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          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/330/792 [1]</TD>
            <TD>Radial velocity in Draco (Kleyna+, 2002)</TD>
            <TD>We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude V~19.5 with a mean velocity precision of ~2km/s. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792#1</TD>
            <TD>2011-09-14T19:47:41Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/330/792</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/792</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/330/792 [2]</TD>
            <TD>Radial velocity in Draco (Kleyna+, 2002)</TD>
            <TD>We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude V~19.5 with a mean velocity precision of ~2km/s. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792#2</TD>
            <TD>2011-09-14T19:47:41Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/330/792&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/792</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/330/792 [stars]</TD>
            <TD>Radial velocity in Draco (Kleyna+, 2002)</TD>
            <TD>We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude V~19.5 with a mean velocity precision of ~2km/s. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792#stars</TD>
            <TD>2011-09-14T19:47:41Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/330/792&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/792</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/330/792 [1]</TD>
            <TD>Radial velocity in Draco (Kleyna+, 2002)</TD>
            <TD>We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude V~19.5 with a mean velocity precision of ~2km/s. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792#1</TD>
            <TD>2011-09-14T19:47:41Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/330/792</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/792</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/330/792 [2]</TD>
            <TD>Radial velocity in Draco (Kleyna+, 2002)</TD>
            <TD>We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude V~19.5 with a mean velocity precision of ~2km/s. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792#2</TD>
            <TD>2011-09-14T19:47:41Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/330/792&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/792</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/330/792 [stars]</TD>
            <TD>Radial velocity in Draco (Kleyna+, 2002)</TD>
            <TD>We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude V~19.5 with a mean velocity precision of ~2km/s. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792#stars</TD>
            <TD>2011-09-14T19:47:41Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/330/792&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/792</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/330/792 [1]</TD>
            <TD>Radial velocity in Draco (Kleyna+, 2002)</TD>
            <TD>We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude V~19.5 with a mean velocity precision of ~2km/s. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792#1</TD>
            <TD>2011-09-14T19:47:41Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/330/792</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/792</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/330/792 [2]</TD>
            <TD>Radial velocity in Draco (Kleyna+, 2002)</TD>
            <TD>We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude V~19.5 with a mean velocity precision of ~2km/s. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792#2</TD>
            <TD>2011-09-14T19:47:41Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/330/792&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/792</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/330/792 [stars]</TD>
            <TD>Radial velocity in Draco (Kleyna+, 2002)</TD>
            <TD>We present stellar radial velocity data for the Draco dwarf spheroidal (dSph) galaxy obtained using the AF2/WYFFOS instrument combination on the William Herschel Telescope. Our data set consists of 186 member stars, 159 of which have good quality velocities, extending to a magnitude V~19.5 with a mean velocity precision of ~2km/s. As this survey is based on a high-precision photometric target list, it contains many more Draco members at large radii. For the first time, this allows a robust determination of the radial behaviour of the velocity dispersion in a dSph.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792#stars</TD>
            <TD>2011-09-14T19:47:41Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/792</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/330/792&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/792</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/420/873 [1]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#1</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/420/873</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/420/873 [2]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#2</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/420/873&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/420/873 [table1]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#table1</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/420/873&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/420/873 [table2]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#table2</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/420/873&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/420/873 [1]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#1</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/420/873</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/420/873 [2]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#2</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/420/873&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/420/873 [table1]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#table1</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/420/873&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/420/873 [table2]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#table2</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/420/873&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/420/873 [1]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#1</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/420/873</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/420/873 [2]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#2</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/420/873&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/420/873 [table1]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#table1</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/420/873&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/420/873 [table2]</TD>
            <TD>Properties of isolated disk galaxies (Varela+, 2004)</TD>
            <TD>We present a new sample of northern isolated galaxies, which are defined by the physical criterion that they were not affected by other galaxies in their evolution during the last few Gyr. To find them we used the logarithmic ratio, f, between inner and tidal forces acting upon the candidate galaxy by a possible perturber.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873#table2</TD>
            <TD>2011-09-14T19:48:52Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/873</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/420/873&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/873</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/333/100 [1]</TD>
            <TD>Radio galaxies in the 2dFGRS (Magliocchetti+, 2002)</TD>
            <TD>We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey (&lt;VII/226&gt;) to study the properties of local radio sources with S&gt;=1mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey(&lt;VIII/71&gt;) , corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9h 48min&lt;=RA&lt;=14h 32min and -2.77{deg}&lt;=DE&lt;=2.25{deg} (2000), down to a magnitude limit b_J_=19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100#1</TD>
            <TD>2011-09-14T19:47:38Z</TD>
            <TD>#AGN#Galaxies#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/333/100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/333/100 [2]</TD>
            <TD>Radio galaxies in the 2dFGRS (Magliocchetti+, 2002)</TD>
            <TD>We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey (&lt;VII/226&gt;) to study the properties of local radio sources with S&gt;=1mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey(&lt;VIII/71&gt;) , corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9h 48min&lt;=RA&lt;=14h 32min and -2.77{deg}&lt;=DE&lt;=2.25{deg} (2000), down to a magnitude limit b_J_=19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100#2</TD>
            <TD>2011-09-14T19:47:38Z</TD>
            <TD>#AGN#Galaxies#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/333/100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/333/100 [table23]</TD>
            <TD>Radio galaxies in the 2dFGRS (Magliocchetti+, 2002)</TD>
            <TD>We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey (&lt;VII/226&gt;) to study the properties of local radio sources with S&gt;=1mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey(&lt;VIII/71&gt;) , corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9h 48min&lt;=RA&lt;=14h 32min and -2.77{deg}&lt;=DE&lt;=2.25{deg} (2000), down to a magnitude limit b_J_=19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100#table23</TD>
            <TD>2011-09-14T19:47:38Z</TD>
            <TD>#AGN#Galaxies#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/333/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/100</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>EIGA</TD>
            <TD>The Extended IRAS Galaxy Atlas</TD>
            <TD>The Extended IRAS Galaxy Atlas (EIGA) is an extension of the original IRAS Galaxy Atlas (IGA) to b = 6.7 deg.. High resolution images at 60 microns and 100 microns have been produced to match the latitude coverage of radio continuum observations obtained as part of the Canadian Galactic Plane Survey (CGPS). Also associated with the EIGA and IGA is the Mid-Infrared Galaxy Atlas (MIGA).</TD>
            <TD>NASA/IPAC Infrared Science Archive</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://irsa.ipac/EIGA#1</TD>
            <TD>2007-04-11T08:52:38Z</TD>
            <TD>##</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://irsa.ipac/EIGA</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://irsa.ipac.caltech.edu/cgi-bin/Atlas/nph-atlas?mission=EIGA&amp;hdr_location=%5CEIGADataPath%5C&amp;SIAP_ACTIVE=1&amp;collection_desc=The+Extended+IRAS+Galaxy+Atlas+%28EIGA%29&amp;</TD>
            <TD />
            <TD>300</TD>
            <TD>ivo://irsa.ipac/IRSA</TD>
            <TD>http://irsa.ipac.caltech.edu/data/EIGA</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>MIGA</TD>
            <TD>The Mid-Infrared Galaxy Atlas</TD>
            <TD>The Mid-Infrared Galaxy Atlas (MIGA) is a high resolution image atlas of the Galactic plane at 12 microns and 25 microns, it has been produced using the HIRES processed infrared data from the IRAS satellite. It is a counterpart to the far-infrared IRAS Galaxy Atlas (IGA) and the Extended IRAS Galaxy Atlas (EIGA).</TD>
            <TD>NASA/IPAC Infrared Science Archive</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://irsa.ipac/MIGA#1</TD>
            <TD>2007-04-11T08:52:38Z</TD>
            <TD>##</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://irsa.ipac/MIGA</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://irsa.ipac.caltech.edu/cgi-bin/Atlas/nph-atlas?mission=MIGA&amp;hdr_location=%5CMIGADataPath%5C&amp;SIAP_ACTIVE=1&amp;collection_desc=The+Mid-Infrared+Galaxy+Atlas+%28MIGA%29&amp;</TD>
            <TD />
            <TD>3000</TD>
            <TD>ivo://irsa.ipac</TD>
            <TD>http://irsa.ipac.caltech.edu/data/MIGA</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>USNO-B1</TD>
            <TD>USNO-B1 Catalogue</TD>
            <TD>USNO-B is an all-sky catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,042,618,261 objects derived from 3,643,201,733 separate observations. The data were obtained from scans of 7435 Schmidt plates taken for the various sky surveys during the last 50 years. USNO-B1.0 is believed to provide all-sky coverage, completeness down to V=21, 0.2" astrometric accuracy at J2000, 0.3 mag photometric accuracy in up to five colors, and 85% accuracy for distinguishing stars from nonstellar objects. A brief discussion of various issues is given here, but the actual data are available from the US Naval Observatory Web site and others.</TD>
            <TD>United States Naval Observatory, Flagstaff Station</TD>
            <TD>#Optical#</TD>
            <TD>ivo://fs.usno/cat/usnob#1</TD>
            <TD>2007-04-11T08:52:38Z</TD>
            <TD>#astrometric catalogue#optical astronomy#finding charts#photographic images#</TD>
            <TD>#Catalog#</TD>
            <TD>#Secondary Education#Community College#University#Research#Amateur#</TD>
            <TD />
            <TD />
            <TD>ivo://fs.usno/cat/usnob</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://www.nofs.navy.mil/cgi-bin/vo_cone.cgi?CAT=USNO-B1&amp;</TD>
            <TD>1.0</TD>
            <TD>100000</TD>
            <TD>ivo://fs.usno/org</TD>
            <TD>http://www.nofs.navy.mil/data/fchpix</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/405/99 [1]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#1</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/405/99</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/405/99 [2]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#2</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/405/99&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/405/99 [table3]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#table3</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/405/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/405/99 [table2]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#table2</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/405/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/405/99 [table1]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#table1</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/405/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/405/99 [1]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#1</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/405/99</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/405/99 [2]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#2</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/405/99&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/405/99 [table3]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#table3</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/405/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/405/99 [table2]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#table2</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/405/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/405/99 [table1]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#table1</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/405/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/405/99 [1]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#1</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/405/99</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/405/99 [2]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#2</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/405/99&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/405/99 [table3]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#table3</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/405/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/405/99 [table2]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#table2</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/405/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/405/99 [table1]</TD>
            <TD>LSB galaxies in near-infrared. I. (Monnier-Ragaigne+, 2003)</TD>
            <TD>A sample of about 3800 Low Surface Brightness (LSB) galaxies was selected using the all-sky near-infrared (J, H and Ks-band) 2MASS survey. The selected objects have a mean central surface brightness within a 5" radius around their centre fainter than 18mag/arcsec^2^ in the Ks band, making them the lowest surface brightness galaxies detected by 2MASS. A description is given of the relevant properties of the 2MASS survey and the LSB galaxy selection procedure, as well as of basic photometric properties of the selected objects. The latter properties are compared to those of other samples of galaxies, of both LSBs and "classical'' high surface brightness (HSB) objects, which were selected in the optical. The 2MASS LSBs have a B_Tc_-K_T_ colour colour which is on average 0.9mag bluer than that of HSBs from the NGC. The 2MASS sample does not appear to contain a significant population of red objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99#table1</TD>
            <TD>2011-09-14T20:02:24Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/405/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/405/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/405/99</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/369/1334 [1]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#1</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/369/1334</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/369/1334 [2]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#2</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1334 [galaxies]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#galaxies</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1334 [catalog]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#catalog</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1334 [table4]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#table4</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/369/1334 [1]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#1</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/369/1334</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/369/1334 [2]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#2</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1334 [galaxies]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#galaxies</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1334 [catalog]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#catalog</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1334 [table4]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#table4</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/369/1334 [1]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#1</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/369/1334</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/369/1334 [2]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#2</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1334 [galaxies]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#galaxies</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1334 [catalog]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#catalog</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1334 [table4]</TD>
            <TD>FSVS Cluster Catalogue (Sochting+, 2006)</TD>
            <TD>We describe a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semiparametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by colour discrimination. The sample covers a wide range of richness, has a density of ~28 clusters/deg^2^, and spans a range of estimated redshifts of 0.05&lt;z&lt;0.9 with mean &lt;z&gt;=0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be {sigma}~0.03. Containing over 100 clusters with z&gt;0.6, the catalogue contributes substantially to the current total of optically selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programmes. The construction of this FSVS Cluster Catalogue completes a fundamental component of our continuing programmes to investigate the environments of quasars and the chemical evolution of galaxies. We publish here the list of all clusters with their basic parameters, and discuss some illustrative examples in more detail. The full FSVS Cluster Catalogue, together with images and lists of member galaxies etc., will be issued as part of the 'NOAO (National Optical Astronomy Observatories) data products', and accessible at http://www.noao.edu/dpp/ . We describe the format of these data and access to them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334#table4</TD>
            <TD>2011-09-14T20:02:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1334</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1334&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1334</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/354/823 [1]</TD>
            <TD>HII region catalogue of NGC 3359 (Rozas+, 2000)</TD>
            <TD>From an H-{alpha} image of the spiral barred galaxy NGC 3359, an HII region catalogue is composed. The catalogue comprises the position, mean radius and the calibrated H-alpha luminosity of each HII region. The observations of the image of NGC 3359 in H-{alpha} were carried out in February 1996, on the Isaac Newton telescope in La Palma in the context of the BARS international time project of the Canary Islands Observatories. A CCD TeK-7 detector was used with a projected pixel size of 0.59".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823#1</TD>
            <TD>2011-09-14T20:03:47Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/354/823</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/354/823</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/354/823 [2]</TD>
            <TD>HII region catalogue of NGC 3359 (Rozas+, 2000)</TD>
            <TD>From an H-{alpha} image of the spiral barred galaxy NGC 3359, an HII region catalogue is composed. The catalogue comprises the position, mean radius and the calibrated H-alpha luminosity of each HII region. The observations of the image of NGC 3359 in H-{alpha} were carried out in February 1996, on the Isaac Newton telescope in La Palma in the context of the BARS international time project of the Canary Islands Observatories. A CCD TeK-7 detector was used with a projected pixel size of 0.59".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823#2</TD>
            <TD>2011-09-14T20:03:47Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/354/823&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/354/823</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/354/823 [catalog]</TD>
            <TD>HII region catalogue of NGC 3359 (Rozas+, 2000)</TD>
            <TD>From an H-{alpha} image of the spiral barred galaxy NGC 3359, an HII region catalogue is composed. The catalogue comprises the position, mean radius and the calibrated H-alpha luminosity of each HII region. The observations of the image of NGC 3359 in H-{alpha} were carried out in February 1996, on the Isaac Newton telescope in La Palma in the context of the BARS international time project of the Canary Islands Observatories. A CCD TeK-7 detector was used with a projected pixel size of 0.59".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823#catalog</TD>
            <TD>2011-09-14T20:03:47Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/354/823&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/354/823</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/354/823 [1]</TD>
            <TD>HII region catalogue of NGC 3359 (Rozas+, 2000)</TD>
            <TD>From an H-{alpha} image of the spiral barred galaxy NGC 3359, an HII region catalogue is composed. The catalogue comprises the position, mean radius and the calibrated H-alpha luminosity of each HII region. The observations of the image of NGC 3359 in H-{alpha} were carried out in February 1996, on the Isaac Newton telescope in La Palma in the context of the BARS international time project of the Canary Islands Observatories. A CCD TeK-7 detector was used with a projected pixel size of 0.59".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823#1</TD>
            <TD>2011-09-14T20:03:47Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/354/823</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/354/823</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/354/823 [2]</TD>
            <TD>HII region catalogue of NGC 3359 (Rozas+, 2000)</TD>
            <TD>From an H-{alpha} image of the spiral barred galaxy NGC 3359, an HII region catalogue is composed. The catalogue comprises the position, mean radius and the calibrated H-alpha luminosity of each HII region. The observations of the image of NGC 3359 in H-{alpha} were carried out in February 1996, on the Isaac Newton telescope in La Palma in the context of the BARS international time project of the Canary Islands Observatories. A CCD TeK-7 detector was used with a projected pixel size of 0.59".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823#2</TD>
            <TD>2011-09-14T20:03:47Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/354/823&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/354/823</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/354/823 [catalog]</TD>
            <TD>HII region catalogue of NGC 3359 (Rozas+, 2000)</TD>
            <TD>From an H-{alpha} image of the spiral barred galaxy NGC 3359, an HII region catalogue is composed. The catalogue comprises the position, mean radius and the calibrated H-alpha luminosity of each HII region. The observations of the image of NGC 3359 in H-{alpha} were carried out in February 1996, on the Isaac Newton telescope in La Palma in the context of the BARS international time project of the Canary Islands Observatories. A CCD TeK-7 detector was used with a projected pixel size of 0.59".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823#catalog</TD>
            <TD>2011-09-14T20:03:47Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/354/823&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/354/823</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>IGA</TD>
            <TD>The IRAS Galaxy Atlas</TD>
            <TD>The IRAS Galaxy Atlas (IGA) is a high resolution image atlas of the Galactic plane at 60 and 100 microns, it has been produced using the IRAS satellite data. The HIRES program was developed by the Infrared Processing and Analysis Center (IPAC) to produce high resolution (~ 1 arcmin) images from IRAS data using the Maximum Correlation Method (H.H. Aumann, J.W. Fowler and M. Melnyk, 1990, Astronomical Journal, 99, 1674).</TD>
            <TD>NASA/IPAC Infrared Science Archive</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://irsa.ipac/IGA#1</TD>
            <TD>2007-04-11T08:52:38Z</TD>
            <TD>##</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://irsa.ipac/IGA</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://irsa.ipac.caltech.edu/cgi-bin/Atlas/nph-atlas?mission=IGA&amp;hdr_location=%5CIGADataPath%5C&amp;SIAP_ACTIVE=1&amp;collection_desc=The+IRAS+Galaxy+Atlas+%28IGA%29&amp;</TD>
            <TD />
            <TD>3000</TD>
            <TD>ivo://irsa.ipac/IRSA</TD>
            <TD>http://irsa.ipac.caltech.edu/data/IGA</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/354/823 [1]</TD>
            <TD>HII region catalogue of NGC 3359 (Rozas+, 2000)</TD>
            <TD>From an H-{alpha} image of the spiral barred galaxy NGC 3359, an HII region catalogue is composed. The catalogue comprises the position, mean radius and the calibrated H-alpha luminosity of each HII region. The observations of the image of NGC 3359 in H-{alpha} were carried out in February 1996, on the Isaac Newton telescope in La Palma in the context of the BARS international time project of the Canary Islands Observatories. A CCD TeK-7 detector was used with a projected pixel size of 0.59".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823#1</TD>
            <TD>2011-09-14T20:03:47Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/354/823</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/354/823</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/354/823 [2]</TD>
            <TD>HII region catalogue of NGC 3359 (Rozas+, 2000)</TD>
            <TD>From an H-{alpha} image of the spiral barred galaxy NGC 3359, an HII region catalogue is composed. The catalogue comprises the position, mean radius and the calibrated H-alpha luminosity of each HII region. The observations of the image of NGC 3359 in H-{alpha} were carried out in February 1996, on the Isaac Newton telescope in La Palma in the context of the BARS international time project of the Canary Islands Observatories. A CCD TeK-7 detector was used with a projected pixel size of 0.59".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823#2</TD>
            <TD>2011-09-14T20:03:47Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/354/823&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/354/823</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/354/823 [catalog]</TD>
            <TD>HII region catalogue of NGC 3359 (Rozas+, 2000)</TD>
            <TD>From an H-{alpha} image of the spiral barred galaxy NGC 3359, an HII region catalogue is composed. The catalogue comprises the position, mean radius and the calibrated H-alpha luminosity of each HII region. The observations of the image of NGC 3359 in H-{alpha} were carried out in February 1996, on the Isaac Newton telescope in La Palma in the context of the BARS international time project of the Canary Islands Observatories. A CCD TeK-7 detector was used with a projected pixel size of 0.59".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823#catalog</TD>
            <TD>2011-09-14T20:03:47Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/354/823</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/354/823&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/354/823</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/435/781 [1]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#1</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/435/781</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/435/781 [2]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#2</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/435/781&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/435/781 [table5]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#table5</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/435/781&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/435/781 [table3]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#table3</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/435/781&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/435/781 [1]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#1</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/435/781</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/435/781 [2]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#2</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/435/781&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/435/781 [table5]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#table5</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/435/781&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/435/781 [table3]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#table3</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/435/781&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/333/100 [1]</TD>
            <TD>Radio galaxies in the 2dFGRS (Magliocchetti+, 2002)</TD>
            <TD>We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey (&lt;VII/226&gt;) to study the properties of local radio sources with S&gt;=1mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey(&lt;VIII/71&gt;) , corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9h 48min&lt;=RA&lt;=14h 32min and -2.77{deg}&lt;=DE&lt;=2.25{deg} (2000), down to a magnitude limit b_J_=19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100#1</TD>
            <TD>2011-09-14T19:47:38Z</TD>
            <TD>#AGN#Galaxies#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/333/100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/333/100 [2]</TD>
            <TD>Radio galaxies in the 2dFGRS (Magliocchetti+, 2002)</TD>
            <TD>We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey (&lt;VII/226&gt;) to study the properties of local radio sources with S&gt;=1mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey(&lt;VIII/71&gt;) , corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9h 48min&lt;=RA&lt;=14h 32min and -2.77{deg}&lt;=DE&lt;=2.25{deg} (2000), down to a magnitude limit b_J_=19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100#2</TD>
            <TD>2011-09-14T19:47:38Z</TD>
            <TD>#AGN#Galaxies#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/333/100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/333/100 [table23]</TD>
            <TD>Radio galaxies in the 2dFGRS (Magliocchetti+, 2002)</TD>
            <TD>We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey (&lt;VII/226&gt;) to study the properties of local radio sources with S&gt;=1mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey(&lt;VIII/71&gt;) , corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9h 48min&lt;=RA&lt;=14h 32min and -2.77{deg}&lt;=DE&lt;=2.25{deg} (2000), down to a magnitude limit b_J_=19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100#table23</TD>
            <TD>2011-09-14T19:47:38Z</TD>
            <TD>#AGN#Galaxies#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/333/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/100</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/435/781 [1]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#1</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/435/781</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/435/781 [2]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#2</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/435/781&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/435/781 [table5]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#table5</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/435/781&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/435/781 [table3]</TD>
            <TD>Redshifts of galaxies in 21 EIS cluster fields (Olsen+, 2005)</TD>
            <TD>We have carried out an investigation of the properties of low redshift EIS clusters using both spectroscopy and imaging data. We present new redshifts for 738 galaxies in 21 ESO Imaging Survey (EIS) Cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space and to identify groups/clusters of galaxies corresponding to the original EIS matched filter cluster candidates. In this way we spectroscopically confirm 20 of the 21 cluster candidates with a matched-filter estimated redshift z_MF_=0.2. We have now obtained spectroscopic redshifts for 34 EIS cluster candidates with z_MF_=0.2 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;. Of those we spectroscopically confirm 32 with redshifts ranging from z=0.064 to 0.283. We find that: 1) the velocity dispersions of the systems range from sigma_v_&lt;=130km/s to sigma_v_=1200km/s, typical of galaxy groups to rich clusters; 2) richnesses corresponding to Abell classes R&lt;=1; and 3) concentration indices ranging from C=0.2 to C=1.2. From the analysis of the colours of the galaxy populations we find that 53% of the spectroscopically confirmed systems have a "significant" red sequence. These systems are on average richer and have higher velocity dispersions. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781#table3</TD>
            <TD>2011-09-14T20:04:04Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/781</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/435/781&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/781</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/333/100 [1]</TD>
            <TD>Radio galaxies in the 2dFGRS (Magliocchetti+, 2002)</TD>
            <TD>We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey (&lt;VII/226&gt;) to study the properties of local radio sources with S&gt;=1mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey(&lt;VIII/71&gt;) , corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9h 48min&lt;=RA&lt;=14h 32min and -2.77{deg}&lt;=DE&lt;=2.25{deg} (2000), down to a magnitude limit b_J_=19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100#1</TD>
            <TD>2011-09-14T19:47:38Z</TD>
            <TD>#AGN#Galaxies#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/333/100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/333/100 [2]</TD>
            <TD>Radio galaxies in the 2dFGRS (Magliocchetti+, 2002)</TD>
            <TD>We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey (&lt;VII/226&gt;) to study the properties of local radio sources with S&gt;=1mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey(&lt;VIII/71&gt;) , corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9h 48min&lt;=RA&lt;=14h 32min and -2.77{deg}&lt;=DE&lt;=2.25{deg} (2000), down to a magnitude limit b_J_=19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100#2</TD>
            <TD>2011-09-14T19:47:38Z</TD>
            <TD>#AGN#Galaxies#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/333/100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/333/100 [table23]</TD>
            <TD>Radio galaxies in the 2dFGRS (Magliocchetti+, 2002)</TD>
            <TD>We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey (&lt;VII/226&gt;) to study the properties of local radio sources with S&gt;=1mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey(&lt;VIII/71&gt;) , corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9h 48min&lt;=RA&lt;=14h 32min and -2.77{deg}&lt;=DE&lt;=2.25{deg} (2000), down to a magnitude limit b_J_=19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100#table23</TD>
            <TD>2011-09-14T19:47:38Z</TD>
            <TD>#AGN#Galaxies#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/333/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/100</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/464/573 [1]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#1</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/464/573</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/464/573 [2]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#2</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/464/573&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table4]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table4</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table1]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table1</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table3]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table3</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table2]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table2</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table5]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table5</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
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            <TD>#Research#</TD>
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            <TD>25-Jan-2007</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/704 [1]</TD>
            <TD>Low surface brightness galaxies in SDSS (Kniazev+, 2004)</TD>
            <TD>In this paper we present results of a pilot study to use imaging data from the Sloan Digital Sky Survey (SDSS) to search for low surface brightness (LSB) galaxies. For our pilot study we use a test sample of 92 galaxies from the Impey et al. catalog distributed over 93 SDSS fields of the Early Data Release (EDR, &lt;J/AJ/123/567&gt;). Many galaxies from the test sample are either LSB or dwarf galaxies. To deal with the SDSS data most effectively, a new photometry software was created, which is described in this paper. We present the results of the selection algorithms applied to these 93 EDR fields. Two galaxies from the Impey et al. (1996, &lt;J/ApJS/105/209&gt;) test sample are very likely artifacts, as confirmed by follow-up imaging. With our algorithms we were able to recover 87 of the 90 remaining test sample galaxies, implying a detection rate of ~96.5%. The three missed galaxies fall too close to very bright stars or galaxies. In addition, 42 new galaxies with parameters similar to the test sample objects were found in these EDR fields (i.e.,~47% additional galaxies). We present the main photometric parameters of all identified galaxies and carry out first statistical comparisons. We tested the quality of our photometry by comparing the magnitudes for our test sample galaxies and other bright galaxies with values from the literature. All these tests yielded consistent results. We briefly discuss a few unusual galaxies found in our pilot study, including an LSB galaxy with a two-component disk and 10 new giant LSB galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704#1</TD>
            <TD>2011-09-14T19:47:48Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/704</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/704</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/704 [2]</TD>
            <TD>Low surface brightness galaxies in SDSS (Kniazev+, 2004)</TD>
            <TD>In this paper we present results of a pilot study to use imaging data from the Sloan Digital Sky Survey (SDSS) to search for low surface brightness (LSB) galaxies. For our pilot study we use a test sample of 92 galaxies from the Impey et al. catalog distributed over 93 SDSS fields of the Early Data Release (EDR, &lt;J/AJ/123/567&gt;). Many galaxies from the test sample are either LSB or dwarf galaxies. To deal with the SDSS data most effectively, a new photometry software was created, which is described in this paper. We present the results of the selection algorithms applied to these 93 EDR fields. Two galaxies from the Impey et al. (1996, &lt;J/ApJS/105/209&gt;) test sample are very likely artifacts, as confirmed by follow-up imaging. With our algorithms we were able to recover 87 of the 90 remaining test sample galaxies, implying a detection rate of ~96.5%. The three missed galaxies fall too close to very bright stars or galaxies. In addition, 42 new galaxies with parameters similar to the test sample objects were found in these EDR fields (i.e.,~47% additional galaxies). We present the main photometric parameters of all identified galaxies and carry out first statistical comparisons. We tested the quality of our photometry by comparing the magnitudes for our test sample galaxies and other bright galaxies with values from the literature. All these tests yielded consistent results. We briefly discuss a few unusual galaxies found in our pilot study, including an LSB galaxy with a two-component disk and 10 new giant LSB galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704#2</TD>
            <TD>2011-09-14T19:47:48Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>19-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/704&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/704</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/704 [catalog]</TD>
            <TD>Low surface brightness galaxies in SDSS (Kniazev+, 2004)</TD>
            <TD>In this paper we present results of a pilot study to use imaging data from the Sloan Digital Sky Survey (SDSS) to search for low surface brightness (LSB) galaxies. For our pilot study we use a test sample of 92 galaxies from the Impey et al. catalog distributed over 93 SDSS fields of the Early Data Release (EDR, &lt;J/AJ/123/567&gt;). Many galaxies from the test sample are either LSB or dwarf galaxies. To deal with the SDSS data most effectively, a new photometry software was created, which is described in this paper. We present the results of the selection algorithms applied to these 93 EDR fields. Two galaxies from the Impey et al. (1996, &lt;J/ApJS/105/209&gt;) test sample are very likely artifacts, as confirmed by follow-up imaging. With our algorithms we were able to recover 87 of the 90 remaining test sample galaxies, implying a detection rate of ~96.5%. The three missed galaxies fall too close to very bright stars or galaxies. In addition, 42 new galaxies with parameters similar to the test sample objects were found in these EDR fields (i.e.,~47% additional galaxies). We present the main photometric parameters of all identified galaxies and carry out first statistical comparisons. We tested the quality of our photometry by comparing the magnitudes for our test sample galaxies and other bright galaxies with values from the literature. All these tests yielded consistent results. We briefly discuss a few unusual galaxies found in our pilot study, including an LSB galaxy with a two-component disk and 10 new giant LSB galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704#catalog</TD>
            <TD>2011-09-14T19:47:48Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>19-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/704&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/704</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/448/893 [1]</TD>
            <TD>Photometry and lines of (z~0.2-1.0) galaxies (Lamareille+, 2006)</TD>
            <TD>We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range 0.2&lt;z&lt;1.0 with a peak around 0.2&lt;=z&lt;=0.4. The analysis is based on medium resolution (Rs=500-600), optical spectra obtained at VLT and Keck. The targets are mostly "Canada-France Redshift Survey" (&lt;VII/225&gt;) emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the "Gemini Deep Deep Survey" (&lt;J/AJ/127/2455&gt;) public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893#1</TD>
            <TD>2011-09-14T19:49:01Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/448/893</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/893</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/448/893 [2]</TD>
            <TD>Photometry and lines of (z~0.2-1.0) galaxies (Lamareille+, 2006)</TD>
            <TD>We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range 0.2&lt;z&lt;1.0 with a peak around 0.2&lt;=z&lt;=0.4. The analysis is based on medium resolution (Rs=500-600), optical spectra obtained at VLT and Keck. The targets are mostly "Canada-France Redshift Survey" (&lt;VII/225&gt;) emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the "Gemini Deep Deep Survey" (&lt;J/AJ/127/2455&gt;) public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893#2</TD>
            <TD>2011-09-14T19:49:01Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>08-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893</TD>
            <TD />
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/448/893&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/893</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/448/893 [lcl05]</TD>
            <TD>Photometry and lines of (z~0.2-1.0) galaxies (Lamareille+, 2006)</TD>
            <TD>We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range 0.2&lt;z&lt;1.0 with a peak around 0.2&lt;=z&lt;=0.4. The analysis is based on medium resolution (Rs=500-600), optical spectra obtained at VLT and Keck. The targets are mostly "Canada-France Redshift Survey" (&lt;VII/225&gt;) emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the "Gemini Deep Deep Survey" (&lt;J/AJ/127/2455&gt;) public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893#lcl05</TD>
            <TD>2011-09-14T19:49:01Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/448/893&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/893</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/704 [1]</TD>
            <TD>Low surface brightness galaxies in SDSS (Kniazev+, 2004)</TD>
            <TD>In this paper we present results of a pilot study to use imaging data from the Sloan Digital Sky Survey (SDSS) to search for low surface brightness (LSB) galaxies. For our pilot study we use a test sample of 92 galaxies from the Impey et al. catalog distributed over 93 SDSS fields of the Early Data Release (EDR, &lt;J/AJ/123/567&gt;). Many galaxies from the test sample are either LSB or dwarf galaxies. To deal with the SDSS data most effectively, a new photometry software was created, which is described in this paper. We present the results of the selection algorithms applied to these 93 EDR fields. Two galaxies from the Impey et al. (1996, &lt;J/ApJS/105/209&gt;) test sample are very likely artifacts, as confirmed by follow-up imaging. With our algorithms we were able to recover 87 of the 90 remaining test sample galaxies, implying a detection rate of ~96.5%. The three missed galaxies fall too close to very bright stars or galaxies. In addition, 42 new galaxies with parameters similar to the test sample objects were found in these EDR fields (i.e.,~47% additional galaxies). We present the main photometric parameters of all identified galaxies and carry out first statistical comparisons. We tested the quality of our photometry by comparing the magnitudes for our test sample galaxies and other bright galaxies with values from the literature. All these tests yielded consistent results. We briefly discuss a few unusual galaxies found in our pilot study, including an LSB galaxy with a two-component disk and 10 new giant LSB galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704#1</TD>
            <TD>2011-09-14T19:47:48Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/704</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/704</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/704 [2]</TD>
            <TD>Low surface brightness galaxies in SDSS (Kniazev+, 2004)</TD>
            <TD>In this paper we present results of a pilot study to use imaging data from the Sloan Digital Sky Survey (SDSS) to search for low surface brightness (LSB) galaxies. For our pilot study we use a test sample of 92 galaxies from the Impey et al. catalog distributed over 93 SDSS fields of the Early Data Release (EDR, &lt;J/AJ/123/567&gt;). Many galaxies from the test sample are either LSB or dwarf galaxies. To deal with the SDSS data most effectively, a new photometry software was created, which is described in this paper. We present the results of the selection algorithms applied to these 93 EDR fields. Two galaxies from the Impey et al. (1996, &lt;J/ApJS/105/209&gt;) test sample are very likely artifacts, as confirmed by follow-up imaging. With our algorithms we were able to recover 87 of the 90 remaining test sample galaxies, implying a detection rate of ~96.5%. The three missed galaxies fall too close to very bright stars or galaxies. In addition, 42 new galaxies with parameters similar to the test sample objects were found in these EDR fields (i.e.,~47% additional galaxies). We present the main photometric parameters of all identified galaxies and carry out first statistical comparisons. We tested the quality of our photometry by comparing the magnitudes for our test sample galaxies and other bright galaxies with values from the literature. All these tests yielded consistent results. We briefly discuss a few unusual galaxies found in our pilot study, including an LSB galaxy with a two-component disk and 10 new giant LSB galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704#2</TD>
            <TD>2011-09-14T19:47:48Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/704&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/704</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/704 [catalog]</TD>
            <TD>Low surface brightness galaxies in SDSS (Kniazev+, 2004)</TD>
            <TD>In this paper we present results of a pilot study to use imaging data from the Sloan Digital Sky Survey (SDSS) to search for low surface brightness (LSB) galaxies. For our pilot study we use a test sample of 92 galaxies from the Impey et al. catalog distributed over 93 SDSS fields of the Early Data Release (EDR, &lt;J/AJ/123/567&gt;). Many galaxies from the test sample are either LSB or dwarf galaxies. To deal with the SDSS data most effectively, a new photometry software was created, which is described in this paper. We present the results of the selection algorithms applied to these 93 EDR fields. Two galaxies from the Impey et al. (1996, &lt;J/ApJS/105/209&gt;) test sample are very likely artifacts, as confirmed by follow-up imaging. With our algorithms we were able to recover 87 of the 90 remaining test sample galaxies, implying a detection rate of ~96.5%. The three missed galaxies fall too close to very bright stars or galaxies. In addition, 42 new galaxies with parameters similar to the test sample objects were found in these EDR fields (i.e.,~47% additional galaxies). We present the main photometric parameters of all identified galaxies and carry out first statistical comparisons. We tested the quality of our photometry by comparing the magnitudes for our test sample galaxies and other bright galaxies with values from the literature. All these tests yielded consistent results. We briefly discuss a few unusual galaxies found in our pilot study, including an LSB galaxy with a two-component disk and 10 new giant LSB galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704#catalog</TD>
            <TD>2011-09-14T19:47:48Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/704</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/704&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/704</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/464/573 [1]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
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            <TD>HTTP Request</TD>
            <TD>J/A+A/464/573 [2]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table4]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table1]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table3]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table2]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
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            <TD>J/A+A/464/573 [table5]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/127/704 [1]</TD>
            <TD>Low surface brightness galaxies in SDSS (Kniazev+, 2004)</TD>
            <TD>In this paper we present results of a pilot study to use imaging data from the Sloan Digital Sky Survey (SDSS) to search for low surface brightness (LSB) galaxies. For our pilot study we use a test sample of 92 galaxies from the Impey et al. catalog distributed over 93 SDSS fields of the Early Data Release (EDR, &lt;J/AJ/123/567&gt;). Many galaxies from the test sample are either LSB or dwarf galaxies. To deal with the SDSS data most effectively, a new photometry software was created, which is described in this paper. We present the results of the selection algorithms applied to these 93 EDR fields. Two galaxies from the Impey et al. (1996, &lt;J/ApJS/105/209&gt;) test sample are very likely artifacts, as confirmed by follow-up imaging. With our algorithms we were able to recover 87 of the 90 remaining test sample galaxies, implying a detection rate of ~96.5%. The three missed galaxies fall too close to very bright stars or galaxies. In addition, 42 new galaxies with parameters similar to the test sample objects were found in these EDR fields (i.e.,~47% additional galaxies). We present the main photometric parameters of all identified galaxies and carry out first statistical comparisons. We tested the quality of our photometry by comparing the magnitudes for our test sample galaxies and other bright galaxies with values from the literature. All these tests yielded consistent results. We briefly discuss a few unusual galaxies found in our pilot study, including an LSB galaxy with a two-component disk and 10 new giant LSB galaxies.</TD>
            <TD>CDS</TD>
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            <TD>J/AJ/127/704 [2]</TD>
            <TD>Low surface brightness galaxies in SDSS (Kniazev+, 2004)</TD>
            <TD>In this paper we present results of a pilot study to use imaging data from the Sloan Digital Sky Survey (SDSS) to search for low surface brightness (LSB) galaxies. For our pilot study we use a test sample of 92 galaxies from the Impey et al. catalog distributed over 93 SDSS fields of the Early Data Release (EDR, &lt;J/AJ/123/567&gt;). Many galaxies from the test sample are either LSB or dwarf galaxies. To deal with the SDSS data most effectively, a new photometry software was created, which is described in this paper. We present the results of the selection algorithms applied to these 93 EDR fields. Two galaxies from the Impey et al. (1996, &lt;J/ApJS/105/209&gt;) test sample are very likely artifacts, as confirmed by follow-up imaging. With our algorithms we were able to recover 87 of the 90 remaining test sample galaxies, implying a detection rate of ~96.5%. The three missed galaxies fall too close to very bright stars or galaxies. In addition, 42 new galaxies with parameters similar to the test sample objects were found in these EDR fields (i.e.,~47% additional galaxies). We present the main photometric parameters of all identified galaxies and carry out first statistical comparisons. We tested the quality of our photometry by comparing the magnitudes for our test sample galaxies and other bright galaxies with values from the literature. All these tests yielded consistent results. We briefly discuss a few unusual galaxies found in our pilot study, including an LSB galaxy with a two-component disk and 10 new giant LSB galaxies.</TD>
            <TD>CDS</TD>
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            <TD>J/AJ/127/704 [catalog]</TD>
            <TD>Low surface brightness galaxies in SDSS (Kniazev+, 2004)</TD>
            <TD>In this paper we present results of a pilot study to use imaging data from the Sloan Digital Sky Survey (SDSS) to search for low surface brightness (LSB) galaxies. For our pilot study we use a test sample of 92 galaxies from the Impey et al. catalog distributed over 93 SDSS fields of the Early Data Release (EDR, &lt;J/AJ/123/567&gt;). Many galaxies from the test sample are either LSB or dwarf galaxies. To deal with the SDSS data most effectively, a new photometry software was created, which is described in this paper. We present the results of the selection algorithms applied to these 93 EDR fields. Two galaxies from the Impey et al. (1996, &lt;J/ApJS/105/209&gt;) test sample are very likely artifacts, as confirmed by follow-up imaging. With our algorithms we were able to recover 87 of the 90 remaining test sample galaxies, implying a detection rate of ~96.5%. The three missed galaxies fall too close to very bright stars or galaxies. In addition, 42 new galaxies with parameters similar to the test sample objects were found in these EDR fields (i.e.,~47% additional galaxies). We present the main photometric parameters of all identified galaxies and carry out first statistical comparisons. We tested the quality of our photometry by comparing the magnitudes for our test sample galaxies and other bright galaxies with values from the literature. All these tests yielded consistent results. We briefly discuss a few unusual galaxies found in our pilot study, including an LSB galaxy with a two-component disk and 10 new giant LSB galaxies.</TD>
            <TD>CDS</TD>
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            <TD>J/A+A/464/573 [1]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/464/573 [2]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#2</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/464/573&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table4]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table4</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table1]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table1</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table3]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table3</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table2]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table2</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/573 [table5]</TD>
            <TD>VI photometry of 5 open clusters (Carraro+, 2007)</TD>
            <TD>The stellar populations in the outer Galactic disk are a subject of wide interest nowadays. To contribute to a better picture of this part of the Galaxy, we have studied the nature of five marginally investigated star clusters (Collinder 74, Berkeley 27, Haffner 8, NGC 2509, and VdB-Hagen4) by means of accurate CCD photometry in the V and I passbands. These clusters are in fact located in the third Galactic quadrant. We aim to obtain the basic parameters of these objects, which in some cases are still disputed in the literature. In the case of VdB-Hagen 4 we provide the first estimate of its fundamental parameters, while for Haffner 8 we present the first CCD photometry. The analysis is based on the comparison between field star decontaminated color-magnitude diagrams and stellar models. Particular care is devoted to the the assessment of the data quality and the statistical field star decontamination. The Padova library of stellar isochrones is adopted in this study. The analysis we carried out allowed us to solve a few inconsistencies in the literature regarding Haffner 8 and NGC 2509. Collinder 74 is found to be significantly older than reported before. VdB-Hagen 4 is a young open cluster located more than 20kpc from the Galactic center. Such an extreme distance is compatible with the cluster belonging to the Norma-Cygnus arm.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573#table5</TD>
            <TD>2011-09-14T20:04:20Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
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            <TD>#Research#</TD>
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            <TD>25-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/573</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/918 [1]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918#1</TD>
            <TD>2011-09-14T19:48:03Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/918</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/918</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/918 [2]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918#2</TD>
            <TD>2011-09-14T19:48:03Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/918&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/918</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/918 [sculptor]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918#sculptor</TD>
            <TD>2011-09-14T19:48:03Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/918&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/918</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/918 [ngc6822]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918#ngc6822</TD>
            <TD>2011-09-14T19:48:03Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/918&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/918</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/918 [fornax]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918#fornax</TD>
            <TD>2011-09-14T19:48:03Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/918</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/918&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/918</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/448/893 [1]</TD>
            <TD>Photometry and lines of (z~0.2-1.0) galaxies (Lamareille+, 2006)</TD>
            <TD>We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range 0.2&lt;z&lt;1.0 with a peak around 0.2&lt;=z&lt;=0.4. The analysis is based on medium resolution (Rs=500-600), optical spectra obtained at VLT and Keck. The targets are mostly "Canada-France Redshift Survey" (&lt;VII/225&gt;) emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the "Gemini Deep Deep Survey" (&lt;J/AJ/127/2455&gt;) public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893#1</TD>
            <TD>2011-09-14T19:49:01Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/448/893</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/893</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/448/893 [2]</TD>
            <TD>Photometry and lines of (z~0.2-1.0) galaxies (Lamareille+, 2006)</TD>
            <TD>We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range 0.2&lt;z&lt;1.0 with a peak around 0.2&lt;=z&lt;=0.4. The analysis is based on medium resolution (Rs=500-600), optical spectra obtained at VLT and Keck. The targets are mostly "Canada-France Redshift Survey" (&lt;VII/225&gt;) emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the "Gemini Deep Deep Survey" (&lt;J/AJ/127/2455&gt;) public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893#2</TD>
            <TD>2011-09-14T19:49:01Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/448/893&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/893</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/448/893 [lcl05]</TD>
            <TD>Photometry and lines of (z~0.2-1.0) galaxies (Lamareille+, 2006)</TD>
            <TD>We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range 0.2&lt;z&lt;1.0 with a peak around 0.2&lt;=z&lt;=0.4. The analysis is based on medium resolution (Rs=500-600), optical spectra obtained at VLT and Keck. The targets are mostly "Canada-France Redshift Survey" (&lt;VII/225&gt;) emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the "Gemini Deep Deep Survey" (&lt;J/AJ/127/2455&gt;) public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893#lcl05</TD>
            <TD>2011-09-14T19:49:01Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/448/893&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/893</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/161/271 [1]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#1</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/161/271</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/161/271 [2]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#2</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table5]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table5</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table4]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table4</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table6]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table6</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table3]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table3</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/161/271 [1]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#1</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/161/271</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/161/271 [2]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#2</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table5]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table5</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table4]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table4</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table6]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table6</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table3]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table3</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
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            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
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            <TD>30-Jan-2002</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/918</TD>
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            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/918 [2]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
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            <TD>J/MNRAS/327/918 [sculptor]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T19:48:03Z</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/327/918 [ngc6822]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
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            <TD>30-Jan-2002</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>J/MNRAS/327/918 [fornax]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Web Page</TD>
            <TD>J/MNRAS/327/918 [1]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/918</TD>
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            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/918 [2]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/918&amp;</TD>
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            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/327/918 [sculptor]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
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            <TD>#Optical#</TD>
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            <TD>ConeSearch</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/327/918 [ngc6822]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>J/MNRAS/327/918 [fornax]</TD>
            <TD>CaII in extragalactic red giants (Tolstoy+, 2001)</TD>
            <TD>Spectroscopic abundance determinations for stars spanning a Hubble time in age are necessary in order to determine unambiguously the evolutionary histories of galaxies. Using FORS1 in multi-object spectroscopy mode on ANTU (UT1) at the ESO VLT on Paranal, we have obtained near-infrared spectra from which we have measured the equivalent widths of the two strongest Ca II triplet lines to determine metal abundances for a sample of red giant branch stars, selected from ESO NTT optical (I, V-I) photometry of three nearby Local Group galaxies: the Sculptor dwarf spheroidal, the Fornax dwarf spheroidal and the dwarf irregular NGC 6822. The summed equivalent width of the two strongest lines in the Ca II triplet absorption-line feature, centred at 8500{AA}, can be readily converted into an [Fe/H] abundance using the previously established calibrations by Armandroff &amp; Da Costa (1991AJ....101.1329A) and Rutledge, Hesser &amp; Stetson (1997, Cat. &lt;J/PASP/109/883&gt;). We have measured metallicities for 37 stars in Sculptor, 32 stars in Fornax and 23 stars in NGC 6822, yielding more precise estimates of the metallicity distribution functions for these galaxies than it is possible to obtain photometrically. In the case of NGC 6822, this is the first direct measurement of the abundances of the intermediate-age and old stellar populations. We find metallicity spreads in each galaxy which are broadly consistent with the photometric width of the red giant branch, although the abundances of individual stars do not always appear to correspond to their colour. This is almost certainly predominantly due to a highly variable star formation rate with time in these galaxies, which results in a non-uniform, non-globular-cluster-like evolution of the Ca/Fe ratio.</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/161/271 [1]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#1</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/161/271</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/161/271 [2]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#2</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table5]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table5</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table4]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table4</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table6]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table6</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/271 [table3]</TD>
            <TD>The X-ray binary population in M33. I (Grimm+, 2005)</TD>
            <TD>In this paper we present the source list for three Chandra observations of the Local Group galaxy M33. The observations are centered on the nucleus and on the star-forming region NGC 604. We detect a total of 261 sources in an area of 0.2{deg}^2^ down to a flux limit of 3x10^-16^ergs/s/cm^2^, which corresponds to a luminosity of 2x10^34^ergs/s at a distance of 840kpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271#table3</TD>
            <TD>2011-09-14T20:04:51Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/271</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/446/839 [1]</TD>
            <TD>H{alpha} surface photometry in nearby clusters (Gavazzi+, 2006)</TD>
            <TD>We present the H{alpha} imaging observations of 273 late-type galaxies in the nearby rich galaxy clusters Virgo, A 1367, Coma, Cancer, Hercules and in the Great Wall, carried out primarily with the 2.1m telescope of the San Pedro Martir Observatory (SPM) and with the ESO/3.6m telescope. We derived the H{alpha}+[NII] fluxes and equivalent widths. The H{alpha} survey reached completion for an optically selected sample of nearby galaxies in and outside rich clusters. Taking advantage of the completeness of the data set, the dependence of H{alpha} properties on the Hubble type was determined for late-type galaxies in the Virgo cluster. Differences in the gaseous content partly account for the large scatter of the H{alpha} EW within each Hubble-type class. We studied the radial distributions of the H{alpha} EW around Coma+A 1367 and the Virgo clusters in two luminosity bins. Luminous galaxies show a decrease in their average H{alpha} EW in the inner ~1 virial radius, while low-luminosity galaxies do not show this trend. Description:</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839#1</TD>
            <TD>2011-09-14T19:48:22Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/446/839</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/446/839</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/446/839 [2]</TD>
            <TD>H{alpha} surface photometry in nearby clusters (Gavazzi+, 2006)</TD>
            <TD>We present the H{alpha} imaging observations of 273 late-type galaxies in the nearby rich galaxy clusters Virgo, A 1367, Coma, Cancer, Hercules and in the Great Wall, carried out primarily with the 2.1m telescope of the San Pedro Martir Observatory (SPM) and with the ESO/3.6m telescope. We derived the H{alpha}+[NII] fluxes and equivalent widths. The H{alpha} survey reached completion for an optically selected sample of nearby galaxies in and outside rich clusters. Taking advantage of the completeness of the data set, the dependence of H{alpha} properties on the Hubble type was determined for late-type galaxies in the Virgo cluster. Differences in the gaseous content partly account for the large scatter of the H{alpha} EW within each Hubble-type class. We studied the radial distributions of the H{alpha} EW around Coma+A 1367 and the Virgo clusters in two luminosity bins. Luminous galaxies show a decrease in their average H{alpha} EW in the inner ~1 virial radius, while low-luminosity galaxies do not show this trend. Description:</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839#2</TD>
            <TD>2011-09-14T19:48:22Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/446/839&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/446/839</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/446/839 [table1]</TD>
            <TD>H{alpha} surface photometry in nearby clusters (Gavazzi+, 2006)</TD>
            <TD>We present the H{alpha} imaging observations of 273 late-type galaxies in the nearby rich galaxy clusters Virgo, A 1367, Coma, Cancer, Hercules and in the Great Wall, carried out primarily with the 2.1m telescope of the San Pedro Martir Observatory (SPM) and with the ESO/3.6m telescope. We derived the H{alpha}+[NII] fluxes and equivalent widths. The H{alpha} survey reached completion for an optically selected sample of nearby galaxies in and outside rich clusters. Taking advantage of the completeness of the data set, the dependence of H{alpha} properties on the Hubble type was determined for late-type galaxies in the Virgo cluster. Differences in the gaseous content partly account for the large scatter of the H{alpha} EW within each Hubble-type class. We studied the radial distributions of the H{alpha} EW around Coma+A 1367 and the Virgo clusters in two luminosity bins. Luminous galaxies show a decrease in their average H{alpha} EW in the inner ~1 virial radius, while low-luminosity galaxies do not show this trend. Description:</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839#table1</TD>
            <TD>2011-09-14T19:48:22Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/446/839&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/446/839</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/114/298 [1]</TD>
            <TD>BVI photometry in NGC 300 (Pietrzynski+, 2002)</TD>
            <TD>Based on 13 nights of observations of four fields in NGC 300, we have set up an extensive sequence of stars with accurate BVI photometry covering a relatively large (25'x25') region centered on this galaxy. This sequence of standard stars is very useful for calibrating the photometry of variable stars and other objects in NGC 300 and other galaxies obtained from wide-field mosaic images. Our standard-star list contains B, V, and I measurements for 390 stars. The accuracy of the zero points in the V filter and B-V color is better than 0.02mag, and about 0.03mag for the V-I color. We found very good agreement between our measurements and those previously obtained by Walker for 26 stars near NGC 300.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298#1</TD>
            <TD>2011-09-14T20:04:53Z</TD>
            <TD>#Photometry#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/114/298</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/298</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/114/298 [2]</TD>
            <TD>BVI photometry in NGC 300 (Pietrzynski+, 2002)</TD>
            <TD>Based on 13 nights of observations of four fields in NGC 300, we have set up an extensive sequence of stars with accurate BVI photometry covering a relatively large (25'x25') region centered on this galaxy. This sequence of standard stars is very useful for calibrating the photometry of variable stars and other objects in NGC 300 and other galaxies obtained from wide-field mosaic images. Our standard-star list contains B, V, and I measurements for 390 stars. The accuracy of the zero points in the V filter and B-V color is better than 0.02mag, and about 0.03mag for the V-I color. We found very good agreement between our measurements and those previously obtained by Walker for 26 stars near NGC 300.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298#2</TD>
            <TD>2011-09-14T20:04:53Z</TD>
            <TD>#Photometry#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/114/298&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/298</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/114/298 [table4]</TD>
            <TD>BVI photometry in NGC 300 (Pietrzynski+, 2002)</TD>
            <TD>Based on 13 nights of observations of four fields in NGC 300, we have set up an extensive sequence of stars with accurate BVI photometry covering a relatively large (25'x25') region centered on this galaxy. This sequence of standard stars is very useful for calibrating the photometry of variable stars and other objects in NGC 300 and other galaxies obtained from wide-field mosaic images. Our standard-star list contains B, V, and I measurements for 390 stars. The accuracy of the zero points in the V filter and B-V color is better than 0.02mag, and about 0.03mag for the V-I color. We found very good agreement between our measurements and those previously obtained by Walker for 26 stars near NGC 300.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298#table4</TD>
            <TD>2011-09-14T20:04:53Z</TD>
            <TD>#Photometry#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/114/298&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/298</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/448/893 [1]</TD>
            <TD>Photometry and lines of (z~0.2-1.0) galaxies (Lamareille+, 2006)</TD>
            <TD>We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range 0.2&lt;z&lt;1.0 with a peak around 0.2&lt;=z&lt;=0.4. The analysis is based on medium resolution (Rs=500-600), optical spectra obtained at VLT and Keck. The targets are mostly "Canada-France Redshift Survey" (&lt;VII/225&gt;) emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the "Gemini Deep Deep Survey" (&lt;J/AJ/127/2455&gt;) public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893#1</TD>
            <TD>2011-09-14T19:49:01Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/448/893</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/893</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/448/893 [2]</TD>
            <TD>Photometry and lines of (z~0.2-1.0) galaxies (Lamareille+, 2006)</TD>
            <TD>We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range 0.2&lt;z&lt;1.0 with a peak around 0.2&lt;=z&lt;=0.4. The analysis is based on medium resolution (Rs=500-600), optical spectra obtained at VLT and Keck. The targets are mostly "Canada-France Redshift Survey" (&lt;VII/225&gt;) emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the "Gemini Deep Deep Survey" (&lt;J/AJ/127/2455&gt;) public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893#2</TD>
            <TD>2011-09-14T19:49:01Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/448/893&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/893</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/448/893 [lcl05]</TD>
            <TD>Photometry and lines of (z~0.2-1.0) galaxies (Lamareille+, 2006)</TD>
            <TD>We present the spectrophotometric properties of a sample of 141 emission-line galaxies at redshifts in the range 0.2&lt;z&lt;1.0 with a peak around 0.2&lt;=z&lt;=0.4. The analysis is based on medium resolution (Rs=500-600), optical spectra obtained at VLT and Keck. The targets are mostly "Canada-France Redshift Survey" (&lt;VII/225&gt;) emission-line galaxies, with the addition of field galaxies randomly selected behind lensing clusters. We complement this sample with galaxy spectra from the "Gemini Deep Deep Survey" (&lt;J/AJ/127/2455&gt;) public data release. We have computed absolute magnitudes of the galaxies and measured the line fluxes and equivalent widths of the main emission/absorption lines. The last two have been measured after careful subtraction of the fitted stellar continuum using the platefit software originally developed for the SDSS and adapted to our data. We present a careful comparison of this software with the results of manual measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893#lcl05</TD>
            <TD>2011-09-14T19:49:01Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/893</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/448/893&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/893</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/446/839 [1]</TD>
            <TD>H{alpha} surface photometry in nearby clusters (Gavazzi+, 2006)</TD>
            <TD>We present the H{alpha} imaging observations of 273 late-type galaxies in the nearby rich galaxy clusters Virgo, A 1367, Coma, Cancer, Hercules and in the Great Wall, carried out primarily with the 2.1m telescope of the San Pedro Martir Observatory (SPM) and with the ESO/3.6m telescope. We derived the H{alpha}+[NII] fluxes and equivalent widths. The H{alpha} survey reached completion for an optically selected sample of nearby galaxies in and outside rich clusters. Taking advantage of the completeness of the data set, the dependence of H{alpha} properties on the Hubble type was determined for late-type galaxies in the Virgo cluster. Differences in the gaseous content partly account for the large scatter of the H{alpha} EW within each Hubble-type class. We studied the radial distributions of the H{alpha} EW around Coma+A 1367 and the Virgo clusters in two luminosity bins. Luminous galaxies show a decrease in their average H{alpha} EW in the inner ~1 virial radius, while low-luminosity galaxies do not show this trend. Description:</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839#1</TD>
            <TD>2011-09-14T19:48:22Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/446/839</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/446/839</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/446/839 [2]</TD>
            <TD>H{alpha} surface photometry in nearby clusters (Gavazzi+, 2006)</TD>
            <TD>We present the H{alpha} imaging observations of 273 late-type galaxies in the nearby rich galaxy clusters Virgo, A 1367, Coma, Cancer, Hercules and in the Great Wall, carried out primarily with the 2.1m telescope of the San Pedro Martir Observatory (SPM) and with the ESO/3.6m telescope. We derived the H{alpha}+[NII] fluxes and equivalent widths. The H{alpha} survey reached completion for an optically selected sample of nearby galaxies in and outside rich clusters. Taking advantage of the completeness of the data set, the dependence of H{alpha} properties on the Hubble type was determined for late-type galaxies in the Virgo cluster. Differences in the gaseous content partly account for the large scatter of the H{alpha} EW within each Hubble-type class. We studied the radial distributions of the H{alpha} EW around Coma+A 1367 and the Virgo clusters in two luminosity bins. Luminous galaxies show a decrease in their average H{alpha} EW in the inner ~1 virial radius, while low-luminosity galaxies do not show this trend. Description:</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839#2</TD>
            <TD>2011-09-14T19:48:22Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/446/839&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/446/839</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/446/839 [table1]</TD>
            <TD>H{alpha} surface photometry in nearby clusters (Gavazzi+, 2006)</TD>
            <TD>We present the H{alpha} imaging observations of 273 late-type galaxies in the nearby rich galaxy clusters Virgo, A 1367, Coma, Cancer, Hercules and in the Great Wall, carried out primarily with the 2.1m telescope of the San Pedro Martir Observatory (SPM) and with the ESO/3.6m telescope. We derived the H{alpha}+[NII] fluxes and equivalent widths. The H{alpha} survey reached completion for an optically selected sample of nearby galaxies in and outside rich clusters. Taking advantage of the completeness of the data set, the dependence of H{alpha} properties on the Hubble type was determined for late-type galaxies in the Virgo cluster. Differences in the gaseous content partly account for the large scatter of the H{alpha} EW within each Hubble-type class. We studied the radial distributions of the H{alpha} EW around Coma+A 1367 and the Virgo clusters in two luminosity bins. Luminous galaxies show a decrease in their average H{alpha} EW in the inner ~1 virial radius, while low-luminosity galaxies do not show this trend. Description:</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839#table1</TD>
            <TD>2011-09-14T19:48:22Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/446/839&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/446/839</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/114/298 [1]</TD>
            <TD>BVI photometry in NGC 300 (Pietrzynski+, 2002)</TD>
            <TD>Based on 13 nights of observations of four fields in NGC 300, we have set up an extensive sequence of stars with accurate BVI photometry covering a relatively large (25'x25') region centered on this galaxy. This sequence of standard stars is very useful for calibrating the photometry of variable stars and other objects in NGC 300 and other galaxies obtained from wide-field mosaic images. Our standard-star list contains B, V, and I measurements for 390 stars. The accuracy of the zero points in the V filter and B-V color is better than 0.02mag, and about 0.03mag for the V-I color. We found very good agreement between our measurements and those previously obtained by Walker for 26 stars near NGC 300.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298#1</TD>
            <TD>2011-09-14T20:04:53Z</TD>
            <TD>#Photometry#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/114/298</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/298</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/114/298 [2]</TD>
            <TD>BVI photometry in NGC 300 (Pietrzynski+, 2002)</TD>
            <TD>Based on 13 nights of observations of four fields in NGC 300, we have set up an extensive sequence of stars with accurate BVI photometry covering a relatively large (25'x25') region centered on this galaxy. This sequence of standard stars is very useful for calibrating the photometry of variable stars and other objects in NGC 300 and other galaxies obtained from wide-field mosaic images. Our standard-star list contains B, V, and I measurements for 390 stars. The accuracy of the zero points in the V filter and B-V color is better than 0.02mag, and about 0.03mag for the V-I color. We found very good agreement between our measurements and those previously obtained by Walker for 26 stars near NGC 300.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298#2</TD>
            <TD>2011-09-14T20:04:53Z</TD>
            <TD>#Photometry#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/114/298&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/298</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/114/298 [table4]</TD>
            <TD>BVI photometry in NGC 300 (Pietrzynski+, 2002)</TD>
            <TD>Based on 13 nights of observations of four fields in NGC 300, we have set up an extensive sequence of stars with accurate BVI photometry covering a relatively large (25'x25') region centered on this galaxy. This sequence of standard stars is very useful for calibrating the photometry of variable stars and other objects in NGC 300 and other galaxies obtained from wide-field mosaic images. Our standard-star list contains B, V, and I measurements for 390 stars. The accuracy of the zero points in the V filter and B-V color is better than 0.02mag, and about 0.03mag for the V-I color. We found very good agreement between our measurements and those previously obtained by Walker for 26 stars near NGC 300.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298#table4</TD>
            <TD>2011-09-14T20:04:53Z</TD>
            <TD>#Photometry#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/114/298&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/298</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/373/1203 [1]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#1</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/373/1203</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/373/1203 [2]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#2</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/373/1203&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/373/1203 [KR]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#KR</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/373/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/373/1203 [table5]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#table5</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/373/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/446/839 [1]</TD>
            <TD>H{alpha} surface photometry in nearby clusters (Gavazzi+, 2006)</TD>
            <TD>We present the H{alpha} imaging observations of 273 late-type galaxies in the nearby rich galaxy clusters Virgo, A 1367, Coma, Cancer, Hercules and in the Great Wall, carried out primarily with the 2.1m telescope of the San Pedro Martir Observatory (SPM) and with the ESO/3.6m telescope. We derived the H{alpha}+[NII] fluxes and equivalent widths. The H{alpha} survey reached completion for an optically selected sample of nearby galaxies in and outside rich clusters. Taking advantage of the completeness of the data set, the dependence of H{alpha} properties on the Hubble type was determined for late-type galaxies in the Virgo cluster. Differences in the gaseous content partly account for the large scatter of the H{alpha} EW within each Hubble-type class. We studied the radial distributions of the H{alpha} EW around Coma+A 1367 and the Virgo clusters in two luminosity bins. Luminous galaxies show a decrease in their average H{alpha} EW in the inner ~1 virial radius, while low-luminosity galaxies do not show this trend. Description:</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839#1</TD>
            <TD>2011-09-14T19:48:22Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/446/839</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/446/839</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/446/839 [2]</TD>
            <TD>H{alpha} surface photometry in nearby clusters (Gavazzi+, 2006)</TD>
            <TD>We present the H{alpha} imaging observations of 273 late-type galaxies in the nearby rich galaxy clusters Virgo, A 1367, Coma, Cancer, Hercules and in the Great Wall, carried out primarily with the 2.1m telescope of the San Pedro Martir Observatory (SPM) and with the ESO/3.6m telescope. We derived the H{alpha}+[NII] fluxes and equivalent widths. The H{alpha} survey reached completion for an optically selected sample of nearby galaxies in and outside rich clusters. Taking advantage of the completeness of the data set, the dependence of H{alpha} properties on the Hubble type was determined for late-type galaxies in the Virgo cluster. Differences in the gaseous content partly account for the large scatter of the H{alpha} EW within each Hubble-type class. We studied the radial distributions of the H{alpha} EW around Coma+A 1367 and the Virgo clusters in two luminosity bins. Luminous galaxies show a decrease in their average H{alpha} EW in the inner ~1 virial radius, while low-luminosity galaxies do not show this trend. Description:</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839#2</TD>
            <TD>2011-09-14T19:48:22Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/446/839&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/446/839</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/446/839 [table1]</TD>
            <TD>H{alpha} surface photometry in nearby clusters (Gavazzi+, 2006)</TD>
            <TD>We present the H{alpha} imaging observations of 273 late-type galaxies in the nearby rich galaxy clusters Virgo, A 1367, Coma, Cancer, Hercules and in the Great Wall, carried out primarily with the 2.1m telescope of the San Pedro Martir Observatory (SPM) and with the ESO/3.6m telescope. We derived the H{alpha}+[NII] fluxes and equivalent widths. The H{alpha} survey reached completion for an optically selected sample of nearby galaxies in and outside rich clusters. Taking advantage of the completeness of the data set, the dependence of H{alpha} properties on the Hubble type was determined for late-type galaxies in the Virgo cluster. Differences in the gaseous content partly account for the large scatter of the H{alpha} EW within each Hubble-type class. We studied the radial distributions of the H{alpha} EW around Coma+A 1367 and the Virgo clusters in two luminosity bins. Luminous galaxies show a decrease in their average H{alpha} EW in the inner ~1 virial radius, while low-luminosity galaxies do not show this trend. Description:</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839#table1</TD>
            <TD>2011-09-14T19:48:22Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/446/839</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/446/839&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/446/839</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/114/298 [1]</TD>
            <TD>BVI photometry in NGC 300 (Pietrzynski+, 2002)</TD>
            <TD>Based on 13 nights of observations of four fields in NGC 300, we have set up an extensive sequence of stars with accurate BVI photometry covering a relatively large (25'x25') region centered on this galaxy. This sequence of standard stars is very useful for calibrating the photometry of variable stars and other objects in NGC 300 and other galaxies obtained from wide-field mosaic images. Our standard-star list contains B, V, and I measurements for 390 stars. The accuracy of the zero points in the V filter and B-V color is better than 0.02mag, and about 0.03mag for the V-I color. We found very good agreement between our measurements and those previously obtained by Walker for 26 stars near NGC 300.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298#1</TD>
            <TD>2011-09-14T20:04:53Z</TD>
            <TD>#Photometry#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/114/298</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/298</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/114/298 [2]</TD>
            <TD>BVI photometry in NGC 300 (Pietrzynski+, 2002)</TD>
            <TD>Based on 13 nights of observations of four fields in NGC 300, we have set up an extensive sequence of stars with accurate BVI photometry covering a relatively large (25'x25') region centered on this galaxy. This sequence of standard stars is very useful for calibrating the photometry of variable stars and other objects in NGC 300 and other galaxies obtained from wide-field mosaic images. Our standard-star list contains B, V, and I measurements for 390 stars. The accuracy of the zero points in the V filter and B-V color is better than 0.02mag, and about 0.03mag for the V-I color. We found very good agreement between our measurements and those previously obtained by Walker for 26 stars near NGC 300.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298#2</TD>
            <TD>2011-09-14T20:04:53Z</TD>
            <TD>#Photometry#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/114/298&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/298</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/114/298 [table4]</TD>
            <TD>BVI photometry in NGC 300 (Pietrzynski+, 2002)</TD>
            <TD>Based on 13 nights of observations of four fields in NGC 300, we have set up an extensive sequence of stars with accurate BVI photometry covering a relatively large (25'x25') region centered on this galaxy. This sequence of standard stars is very useful for calibrating the photometry of variable stars and other objects in NGC 300 and other galaxies obtained from wide-field mosaic images. Our standard-star list contains B, V, and I measurements for 390 stars. The accuracy of the zero points in the V filter and B-V color is better than 0.02mag, and about 0.03mag for the V-I color. We found very good agreement between our measurements and those previously obtained by Walker for 26 stars near NGC 300.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298#table4</TD>
            <TD>2011-09-14T20:04:53Z</TD>
            <TD>#Photometry#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/298</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/114/298&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/298</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/599/1006 [1]</TD>
            <TD>DEEP Groth Strip Survey. VII. (Kobulnicky+, 2003)</TD>
            <TD>Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26&lt;z&lt;0.82. These galaxies comprise a small subset selected from among 693 objects in the DGSS. They are chosen for chemical analysis by virtue of having the strongest emission lines. Oxygen abundances relative to hydrogen are in the range 8.4&lt;12+log(O/H)&lt;9.0 with typical internal plus systematic measurement uncertainties of 0.17dex. The 64 DGSS galaxies collectively exhibit an increase in metallicity with B-band luminosity, i.e., an L-Z relation like that seen among local galaxies. Using the DGSS sample and local galaxy samples for comparison, we searched for a "second parameter" that might explain some of the dispersion seen in the L-Z relation. Parameters such as galaxy color, emission-line equivalent width, and effective radius were explored but found to be uncorrelated with residuals from the mean L-Z relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006#1</TD>
            <TD>2011-09-14T19:53:36Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/599/1006</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/599/1006</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/599/1006 [2]</TD>
            <TD>DEEP Groth Strip Survey. VII. (Kobulnicky+, 2003)</TD>
            <TD>Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26&lt;z&lt;0.82. These galaxies comprise a small subset selected from among 693 objects in the DGSS. They are chosen for chemical analysis by virtue of having the strongest emission lines. Oxygen abundances relative to hydrogen are in the range 8.4&lt;12+log(O/H)&lt;9.0 with typical internal plus systematic measurement uncertainties of 0.17dex. The 64 DGSS galaxies collectively exhibit an increase in metallicity with B-band luminosity, i.e., an L-Z relation like that seen among local galaxies. Using the DGSS sample and local galaxy samples for comparison, we searched for a "second parameter" that might explain some of the dispersion seen in the L-Z relation. Parameters such as galaxy color, emission-line equivalent width, and effective radius were explored but found to be uncorrelated with residuals from the mean L-Z relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006#2</TD>
            <TD>2011-09-14T19:53:36Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/599/1006&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/599/1006</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/599/1006 [table1]</TD>
            <TD>DEEP Groth Strip Survey. VII. (Kobulnicky+, 2003)</TD>
            <TD>Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26&lt;z&lt;0.82. These galaxies comprise a small subset selected from among 693 objects in the DGSS. They are chosen for chemical analysis by virtue of having the strongest emission lines. Oxygen abundances relative to hydrogen are in the range 8.4&lt;12+log(O/H)&lt;9.0 with typical internal plus systematic measurement uncertainties of 0.17dex. The 64 DGSS galaxies collectively exhibit an increase in metallicity with B-band luminosity, i.e., an L-Z relation like that seen among local galaxies. Using the DGSS sample and local galaxy samples for comparison, we searched for a "second parameter" that might explain some of the dispersion seen in the L-Z relation. Parameters such as galaxy color, emission-line equivalent width, and effective radius were explored but found to be uncorrelated with residuals from the mean L-Z relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006#table1</TD>
            <TD>2011-09-14T19:53:36Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/599/1006&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/599/1006</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/448/983 [1]</TD>
            <TD>VIJsKs photometry in AM 1339-445 and AM1343-452 (Rejkuba+, 2006)</TD>
            <TD>The catalogues of the upper red giant stars in AM 1339-445 and AM 1343-452 are based on ground-based observations obtained in near-IR Js and Ks bands with ISAAC at VLT and on space-based archival optical V and I data from WFPC2 at HST. The Ks observations were taken in two different epochs. The combined optical and near-IR catalogues contain all the stellar sources detected both in ISAAC array and WF3 chip of the WFPC2, which was centered on each galaxy. Table 2 lists V, I, Js and the average Ks magnitudes of 275 stars in AM 1339-445. Table 3 lists V, I, Js and the average Ks magnitudes of 190 stars in AM 1343-452. The magnitudes have not been corrected for extinction. For each magnitude we list magnitude errors as given by photometric packages, HSTphot and DAOPHOT, used to obtain optical and near-IR photometry, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/983#1</TD>
            <TD>2011-09-14T19:49:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/983</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/448/983</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/983</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/448/983 [2]</TD>
            <TD>VIJsKs photometry in AM 1339-445 and AM1343-452 (Rejkuba+, 2006)</TD>
            <TD>The catalogues of the upper red giant stars in AM 1339-445 and AM 1343-452 are based on ground-based observations obtained in near-IR Js and Ks bands with ISAAC at VLT and on space-based archival optical V and I data from WFPC2 at HST. The Ks observations were taken in two different epochs. The combined optical and near-IR catalogues contain all the stellar sources detected both in ISAAC array and WF3 chip of the WFPC2, which was centered on each galaxy. Table 2 lists V, I, Js and the average Ks magnitudes of 275 stars in AM 1339-445. Table 3 lists V, I, Js and the average Ks magnitudes of 190 stars in AM 1343-452. The magnitudes have not been corrected for extinction. For each magnitude we list magnitude errors as given by photometric packages, HSTphot and DAOPHOT, used to obtain optical and near-IR photometry, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/983#2</TD>
            <TD>2011-09-14T19:49:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/983</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/448/983&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/983</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/373/1203 [1]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#1</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/373/1203</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/373/1203 [2]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#2</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/373/1203&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/373/1203 [KR]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#KR</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/373/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/373/1203 [table5]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#table5</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/373/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/599/1006 [1]</TD>
            <TD>DEEP Groth Strip Survey. VII. (Kobulnicky+, 2003)</TD>
            <TD>Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26&lt;z&lt;0.82. These galaxies comprise a small subset selected from among 693 objects in the DGSS. They are chosen for chemical analysis by virtue of having the strongest emission lines. Oxygen abundances relative to hydrogen are in the range 8.4&lt;12+log(O/H)&lt;9.0 with typical internal plus systematic measurement uncertainties of 0.17dex. The 64 DGSS galaxies collectively exhibit an increase in metallicity with B-band luminosity, i.e., an L-Z relation like that seen among local galaxies. Using the DGSS sample and local galaxy samples for comparison, we searched for a "second parameter" that might explain some of the dispersion seen in the L-Z relation. Parameters such as galaxy color, emission-line equivalent width, and effective radius were explored but found to be uncorrelated with residuals from the mean L-Z relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006#1</TD>
            <TD>2011-09-14T19:53:36Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/599/1006</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/599/1006</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/599/1006 [2]</TD>
            <TD>DEEP Groth Strip Survey. VII. (Kobulnicky+, 2003)</TD>
            <TD>Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26&lt;z&lt;0.82. These galaxies comprise a small subset selected from among 693 objects in the DGSS. They are chosen for chemical analysis by virtue of having the strongest emission lines. Oxygen abundances relative to hydrogen are in the range 8.4&lt;12+log(O/H)&lt;9.0 with typical internal plus systematic measurement uncertainties of 0.17dex. The 64 DGSS galaxies collectively exhibit an increase in metallicity with B-band luminosity, i.e., an L-Z relation like that seen among local galaxies. Using the DGSS sample and local galaxy samples for comparison, we searched for a "second parameter" that might explain some of the dispersion seen in the L-Z relation. Parameters such as galaxy color, emission-line equivalent width, and effective radius were explored but found to be uncorrelated with residuals from the mean L-Z relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006#2</TD>
            <TD>2011-09-14T19:53:36Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/599/1006&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/599/1006</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/599/1006 [table1]</TD>
            <TD>DEEP Groth Strip Survey. VII. (Kobulnicky+, 2003)</TD>
            <TD>Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26&lt;z&lt;0.82. These galaxies comprise a small subset selected from among 693 objects in the DGSS. They are chosen for chemical analysis by virtue of having the strongest emission lines. Oxygen abundances relative to hydrogen are in the range 8.4&lt;12+log(O/H)&lt;9.0 with typical internal plus systematic measurement uncertainties of 0.17dex. The 64 DGSS galaxies collectively exhibit an increase in metallicity with B-band luminosity, i.e., an L-Z relation like that seen among local galaxies. Using the DGSS sample and local galaxy samples for comparison, we searched for a "second parameter" that might explain some of the dispersion seen in the L-Z relation. Parameters such as galaxy color, emission-line equivalent width, and effective radius were explored but found to be uncorrelated with residuals from the mean L-Z relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006#table1</TD>
            <TD>2011-09-14T19:53:36Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/599/1006&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/599/1006</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/448/983 [1]</TD>
            <TD>VIJsKs photometry in AM 1339-445 and AM1343-452 (Rejkuba+, 2006)</TD>
            <TD>The catalogues of the upper red giant stars in AM 1339-445 and AM 1343-452 are based on ground-based observations obtained in near-IR Js and Ks bands with ISAAC at VLT and on space-based archival optical V and I data from WFPC2 at HST. The Ks observations were taken in two different epochs. The combined optical and near-IR catalogues contain all the stellar sources detected both in ISAAC array and WF3 chip of the WFPC2, which was centered on each galaxy. Table 2 lists V, I, Js and the average Ks magnitudes of 275 stars in AM 1339-445. Table 3 lists V, I, Js and the average Ks magnitudes of 190 stars in AM 1343-452. The magnitudes have not been corrected for extinction. For each magnitude we list magnitude errors as given by photometric packages, HSTphot and DAOPHOT, used to obtain optical and near-IR photometry, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/983#1</TD>
            <TD>2011-09-14T19:49:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/983</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/448/983</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/983</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/448/983 [2]</TD>
            <TD>VIJsKs photometry in AM 1339-445 and AM1343-452 (Rejkuba+, 2006)</TD>
            <TD>The catalogues of the upper red giant stars in AM 1339-445 and AM 1343-452 are based on ground-based observations obtained in near-IR Js and Ks bands with ISAAC at VLT and on space-based archival optical V and I data from WFPC2 at HST. The Ks observations were taken in two different epochs. The combined optical and near-IR catalogues contain all the stellar sources detected both in ISAAC array and WF3 chip of the WFPC2, which was centered on each galaxy. Table 2 lists V, I, Js and the average Ks magnitudes of 275 stars in AM 1339-445. Table 3 lists V, I, Js and the average Ks magnitudes of 190 stars in AM 1343-452. The magnitudes have not been corrected for extinction. For each magnitude we list magnitude errors as given by photometric packages, HSTphot and DAOPHOT, used to obtain optical and near-IR photometry, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/983#2</TD>
            <TD>2011-09-14T19:49:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/448/983</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/448/983&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/448/983</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/373/1203 [1]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#1</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/373/1203</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/373/1203 [2]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#2</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/373/1203&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/373/1203 [KR]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#KR</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/373/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/373/1203 [table5]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz (Kerton, 2006)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to reexamine radio sources listed in the Kallas and Reich (1980A&amp;AS...42..227K) catalogue. A sample of point sources with flat or rising spectra between 408 and 1420MHz has been compiled, and within this sample likely Gigahertz Peaked Spectrum sources have been identified.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203#table5</TD>
            <TD>2011-09-14T20:02:18Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/373/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/373/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/373/1203</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/599/1006 [1]</TD>
            <TD>DEEP Groth Strip Survey. VII. (Kobulnicky+, 2003)</TD>
            <TD>Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26&lt;z&lt;0.82. These galaxies comprise a small subset selected from among 693 objects in the DGSS. They are chosen for chemical analysis by virtue of having the strongest emission lines. Oxygen abundances relative to hydrogen are in the range 8.4&lt;12+log(O/H)&lt;9.0 with typical internal plus systematic measurement uncertainties of 0.17dex. The 64 DGSS galaxies collectively exhibit an increase in metallicity with B-band luminosity, i.e., an L-Z relation like that seen among local galaxies. Using the DGSS sample and local galaxy samples for comparison, we searched for a "second parameter" that might explain some of the dispersion seen in the L-Z relation. Parameters such as galaxy color, emission-line equivalent width, and effective radius were explored but found to be uncorrelated with residuals from the mean L-Z relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006#1</TD>
            <TD>2011-09-14T19:53:36Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/599/1006</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/599/1006</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/599/1006 [2]</TD>
            <TD>DEEP Groth Strip Survey. VII. (Kobulnicky+, 2003)</TD>
            <TD>Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26&lt;z&lt;0.82. These galaxies comprise a small subset selected from among 693 objects in the DGSS. They are chosen for chemical analysis by virtue of having the strongest emission lines. Oxygen abundances relative to hydrogen are in the range 8.4&lt;12+log(O/H)&lt;9.0 with typical internal plus systematic measurement uncertainties of 0.17dex. The 64 DGSS galaxies collectively exhibit an increase in metallicity with B-band luminosity, i.e., an L-Z relation like that seen among local galaxies. Using the DGSS sample and local galaxy samples for comparison, we searched for a "second parameter" that might explain some of the dispersion seen in the L-Z relation. Parameters such as galaxy color, emission-line equivalent width, and effective radius were explored but found to be uncorrelated with residuals from the mean L-Z relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006#2</TD>
            <TD>2011-09-14T19:53:36Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/599/1006&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/599/1006</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/599/1006 [table1]</TD>
            <TD>DEEP Groth Strip Survey. VII. (Kobulnicky+, 2003)</TD>
            <TD>Using spectroscopic data from the Deep Extragalactic Evolutionary Probe Groth Strip Survey (DGSS), we analyze the gas-phase oxygen abundances in the warm ionized medium for 64 emission-line field galaxies in the redshift range 0.26&lt;z&lt;0.82. These galaxies comprise a small subset selected from among 693 objects in the DGSS. They are chosen for chemical analysis by virtue of having the strongest emission lines. Oxygen abundances relative to hydrogen are in the range 8.4&lt;12+log(O/H)&lt;9.0 with typical internal plus systematic measurement uncertainties of 0.17dex. The 64 DGSS galaxies collectively exhibit an increase in metallicity with B-band luminosity, i.e., an L-Z relation like that seen among local galaxies. Using the DGSS sample and local galaxy samples for comparison, we searched for a "second parameter" that might explain some of the dispersion seen in the L-Z relation. Parameters such as galaxy color, emission-line equivalent width, and effective radius were explored but found to be uncorrelated with residuals from the mean L-Z relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006#table1</TD>
            <TD>2011-09-14T19:53:36Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/599/1006</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/599/1006&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/599/1006</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/335/673 [1]</TD>
            <TD>DA white dwarfs in 2dF QSO Redshift Survey (Vennes+, 2002)</TD>
            <TD>We report the spectroscopic identification of close to 1000 hydrogen-rich (DA) white dwarfs discovered in the course of the Anglo-Australian 2dF QSO Redshift Survey (2QZ, Cat. &lt;VII/223&gt;). We measured the atmospheric parameters of a subsample of 201 stars based on good-quality Balmer line spectra and we determine the 2QZ population characteristics. Over ten per cent of the sample are potential ZZ Ceti variables. We estimate the DA white dwarf birthrate (b_DA_=0.5-1.0x10^-12^/yr/pc^3^) and the scale-height (h=220-300pc) of the population in the thin disc of the Galaxy by combining information acquired in the Palomar-Green, AAT-UVX and new 2QZ surveys. White dwarfs appear related to G and late-F progenitors. A catalogue of 201 DA white dwarfs is presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673#1</TD>
            <TD>2011-09-14T19:53:42Z</TD>
            <TD>#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/335/673</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/335/673</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/335/673 [2]</TD>
            <TD>DA white dwarfs in 2dF QSO Redshift Survey (Vennes+, 2002)</TD>
            <TD>We report the spectroscopic identification of close to 1000 hydrogen-rich (DA) white dwarfs discovered in the course of the Anglo-Australian 2dF QSO Redshift Survey (2QZ, Cat. &lt;VII/223&gt;). We measured the atmospheric parameters of a subsample of 201 stars based on good-quality Balmer line spectra and we determine the 2QZ population characteristics. Over ten per cent of the sample are potential ZZ Ceti variables. We estimate the DA white dwarf birthrate (b_DA_=0.5-1.0x10^-12^/yr/pc^3^) and the scale-height (h=220-300pc) of the population in the thin disc of the Galaxy by combining information acquired in the Palomar-Green, AAT-UVX and new 2QZ surveys. White dwarfs appear related to G and late-F progenitors. A catalogue of 201 DA white dwarfs is presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673#2</TD>
            <TD>2011-09-14T19:53:42Z</TD>
            <TD>#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/335/673&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/335/673</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/335/673 [tablea1]</TD>
            <TD>DA white dwarfs in 2dF QSO Redshift Survey (Vennes+, 2002)</TD>
            <TD>We report the spectroscopic identification of close to 1000 hydrogen-rich (DA) white dwarfs discovered in the course of the Anglo-Australian 2dF QSO Redshift Survey (2QZ, Cat. &lt;VII/223&gt;). We measured the atmospheric parameters of a subsample of 201 stars based on good-quality Balmer line spectra and we determine the 2QZ population characteristics. Over ten per cent of the sample are potential ZZ Ceti variables. We estimate the DA white dwarf birthrate (b_DA_=0.5-1.0x10^-12^/yr/pc^3^) and the scale-height (h=220-300pc) of the population in the thin disc of the Galaxy by combining information acquired in the Palomar-Green, AAT-UVX and new 2QZ surveys. White dwarfs appear related to G and late-F progenitors. A catalogue of 201 DA white dwarfs is presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673#tablea1</TD>
            <TD>2011-09-14T19:53:42Z</TD>
            <TD>#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/335/673&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/335/673</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/335/673 [1]</TD>
            <TD>DA white dwarfs in 2dF QSO Redshift Survey (Vennes+, 2002)</TD>
            <TD>We report the spectroscopic identification of close to 1000 hydrogen-rich (DA) white dwarfs discovered in the course of the Anglo-Australian 2dF QSO Redshift Survey (2QZ, Cat. &lt;VII/223&gt;). We measured the atmospheric parameters of a subsample of 201 stars based on good-quality Balmer line spectra and we determine the 2QZ population characteristics. Over ten per cent of the sample are potential ZZ Ceti variables. We estimate the DA white dwarf birthrate (b_DA_=0.5-1.0x10^-12^/yr/pc^3^) and the scale-height (h=220-300pc) of the population in the thin disc of the Galaxy by combining information acquired in the Palomar-Green, AAT-UVX and new 2QZ surveys. White dwarfs appear related to G and late-F progenitors. A catalogue of 201 DA white dwarfs is presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673#1</TD>
            <TD>2011-09-14T19:53:42Z</TD>
            <TD>#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/335/673</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/335/673</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/335/673 [2]</TD>
            <TD>DA white dwarfs in 2dF QSO Redshift Survey (Vennes+, 2002)</TD>
            <TD>We report the spectroscopic identification of close to 1000 hydrogen-rich (DA) white dwarfs discovered in the course of the Anglo-Australian 2dF QSO Redshift Survey (2QZ, Cat. &lt;VII/223&gt;). We measured the atmospheric parameters of a subsample of 201 stars based on good-quality Balmer line spectra and we determine the 2QZ population characteristics. Over ten per cent of the sample are potential ZZ Ceti variables. We estimate the DA white dwarf birthrate (b_DA_=0.5-1.0x10^-12^/yr/pc^3^) and the scale-height (h=220-300pc) of the population in the thin disc of the Galaxy by combining information acquired in the Palomar-Green, AAT-UVX and new 2QZ surveys. White dwarfs appear related to G and late-F progenitors. A catalogue of 201 DA white dwarfs is presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673#2</TD>
            <TD>2011-09-14T19:53:42Z</TD>
            <TD>#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/335/673&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/335/673</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/335/673 [tablea1]</TD>
            <TD>DA white dwarfs in 2dF QSO Redshift Survey (Vennes+, 2002)</TD>
            <TD>We report the spectroscopic identification of close to 1000 hydrogen-rich (DA) white dwarfs discovered in the course of the Anglo-Australian 2dF QSO Redshift Survey (2QZ, Cat. &lt;VII/223&gt;). We measured the atmospheric parameters of a subsample of 201 stars based on good-quality Balmer line spectra and we determine the 2QZ population characteristics. Over ten per cent of the sample are potential ZZ Ceti variables. We estimate the DA white dwarf birthrate (b_DA_=0.5-1.0x10^-12^/yr/pc^3^) and the scale-height (h=220-300pc) of the population in the thin disc of the Galaxy by combining information acquired in the Palomar-Green, AAT-UVX and new 2QZ surveys. White dwarfs appear related to G and late-F progenitors. A catalogue of 201 DA white dwarfs is presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673#tablea1</TD>
            <TD>2011-09-14T19:53:42Z</TD>
            <TD>#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/335/673&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/335/673</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/449/425 [1]</TD>
            <TD>Optical identification of ROSAT-FSC sources (Mickaelian+, 2006)</TD>
            <TD>The Byurakan/Hamburg/ROSAT Catalogue (BHRC) of the optical identifications of X-ray sources is presented. The BHRC includes all 2791 sources from the ROSAT-FSC (&lt;IX/29&gt;) with |b|&gt;30, DEC&gt;0 and ROSAT count rate CR&gt;0.04cts/s. The optical identifications were carried out by means of the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, and other available data. We managed to identify 97% of sources (2696 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups etc.), and 304 have ambiguous identifications. The table gives all available multiwavelength data for the identified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425#1</TD>
            <TD>2011-09-14T19:53:44Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/449/425</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/425</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/449/425 [2]</TD>
            <TD>Optical identification of ROSAT-FSC sources (Mickaelian+, 2006)</TD>
            <TD>The Byurakan/Hamburg/ROSAT Catalogue (BHRC) of the optical identifications of X-ray sources is presented. The BHRC includes all 2791 sources from the ROSAT-FSC (&lt;IX/29&gt;) with |b|&gt;30, DEC&gt;0 and ROSAT count rate CR&gt;0.04cts/s. The optical identifications were carried out by means of the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, and other available data. We managed to identify 97% of sources (2696 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups etc.), and 304 have ambiguous identifications. The table gives all available multiwavelength data for the identified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425#2</TD>
            <TD>2011-09-14T19:53:44Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/449/425&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/425</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/449/425 [table1]</TD>
            <TD>Optical identification of ROSAT-FSC sources (Mickaelian+, 2006)</TD>
            <TD>The Byurakan/Hamburg/ROSAT Catalogue (BHRC) of the optical identifications of X-ray sources is presented. The BHRC includes all 2791 sources from the ROSAT-FSC (&lt;IX/29&gt;) with |b|&gt;30, DEC&gt;0 and ROSAT count rate CR&gt;0.04cts/s. The optical identifications were carried out by means of the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, and other available data. We managed to identify 97% of sources (2696 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups etc.), and 304 have ambiguous identifications. The table gives all available multiwavelength data for the identified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425#table1</TD>
            <TD>2011-09-14T19:53:44Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/449/425&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/425</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/335/673 [1]</TD>
            <TD>DA white dwarfs in 2dF QSO Redshift Survey (Vennes+, 2002)</TD>
            <TD>We report the spectroscopic identification of close to 1000 hydrogen-rich (DA) white dwarfs discovered in the course of the Anglo-Australian 2dF QSO Redshift Survey (2QZ, Cat. &lt;VII/223&gt;). We measured the atmospheric parameters of a subsample of 201 stars based on good-quality Balmer line spectra and we determine the 2QZ population characteristics. Over ten per cent of the sample are potential ZZ Ceti variables. We estimate the DA white dwarf birthrate (b_DA_=0.5-1.0x10^-12^/yr/pc^3^) and the scale-height (h=220-300pc) of the population in the thin disc of the Galaxy by combining information acquired in the Palomar-Green, AAT-UVX and new 2QZ surveys. White dwarfs appear related to G and late-F progenitors. A catalogue of 201 DA white dwarfs is presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673#1</TD>
            <TD>2011-09-14T19:53:42Z</TD>
            <TD>#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/335/673</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/335/673</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/335/673 [2]</TD>
            <TD>DA white dwarfs in 2dF QSO Redshift Survey (Vennes+, 2002)</TD>
            <TD>We report the spectroscopic identification of close to 1000 hydrogen-rich (DA) white dwarfs discovered in the course of the Anglo-Australian 2dF QSO Redshift Survey (2QZ, Cat. &lt;VII/223&gt;). We measured the atmospheric parameters of a subsample of 201 stars based on good-quality Balmer line spectra and we determine the 2QZ population characteristics. Over ten per cent of the sample are potential ZZ Ceti variables. We estimate the DA white dwarf birthrate (b_DA_=0.5-1.0x10^-12^/yr/pc^3^) and the scale-height (h=220-300pc) of the population in the thin disc of the Galaxy by combining information acquired in the Palomar-Green, AAT-UVX and new 2QZ surveys. White dwarfs appear related to G and late-F progenitors. A catalogue of 201 DA white dwarfs is presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673#2</TD>
            <TD>2011-09-14T19:53:42Z</TD>
            <TD>#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/335/673&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/335/673</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/335/673 [tablea1]</TD>
            <TD>DA white dwarfs in 2dF QSO Redshift Survey (Vennes+, 2002)</TD>
            <TD>We report the spectroscopic identification of close to 1000 hydrogen-rich (DA) white dwarfs discovered in the course of the Anglo-Australian 2dF QSO Redshift Survey (2QZ, Cat. &lt;VII/223&gt;). We measured the atmospheric parameters of a subsample of 201 stars based on good-quality Balmer line spectra and we determine the 2QZ population characteristics. Over ten per cent of the sample are potential ZZ Ceti variables. We estimate the DA white dwarf birthrate (b_DA_=0.5-1.0x10^-12^/yr/pc^3^) and the scale-height (h=220-300pc) of the population in the thin disc of the Galaxy by combining information acquired in the Palomar-Green, AAT-UVX and new 2QZ surveys. White dwarfs appear related to G and late-F progenitors. A catalogue of 201 DA white dwarfs is presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673#tablea1</TD>
            <TD>2011-09-14T19:53:42Z</TD>
            <TD>#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/335/673</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/335/673&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/335/673</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/449/425 [1]</TD>
            <TD>Optical identification of ROSAT-FSC sources (Mickaelian+, 2006)</TD>
            <TD>The Byurakan/Hamburg/ROSAT Catalogue (BHRC) of the optical identifications of X-ray sources is presented. The BHRC includes all 2791 sources from the ROSAT-FSC (&lt;IX/29&gt;) with |b|&gt;30, DEC&gt;0 and ROSAT count rate CR&gt;0.04cts/s. The optical identifications were carried out by means of the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, and other available data. We managed to identify 97% of sources (2696 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups etc.), and 304 have ambiguous identifications. The table gives all available multiwavelength data for the identified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425#1</TD>
            <TD>2011-09-14T19:53:44Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/449/425</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/425</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/449/425 [2]</TD>
            <TD>Optical identification of ROSAT-FSC sources (Mickaelian+, 2006)</TD>
            <TD>The Byurakan/Hamburg/ROSAT Catalogue (BHRC) of the optical identifications of X-ray sources is presented. The BHRC includes all 2791 sources from the ROSAT-FSC (&lt;IX/29&gt;) with |b|&gt;30, DEC&gt;0 and ROSAT count rate CR&gt;0.04cts/s. The optical identifications were carried out by means of the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, and other available data. We managed to identify 97% of sources (2696 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups etc.), and 304 have ambiguous identifications. The table gives all available multiwavelength data for the identified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425#2</TD>
            <TD>2011-09-14T19:53:44Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/449/425&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/425</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/449/425 [table1]</TD>
            <TD>Optical identification of ROSAT-FSC sources (Mickaelian+, 2006)</TD>
            <TD>The Byurakan/Hamburg/ROSAT Catalogue (BHRC) of the optical identifications of X-ray sources is presented. The BHRC includes all 2791 sources from the ROSAT-FSC (&lt;IX/29&gt;) with |b|&gt;30, DEC&gt;0 and ROSAT count rate CR&gt;0.04cts/s. The optical identifications were carried out by means of the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, and other available data. We managed to identify 97% of sources (2696 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups etc.), and 304 have ambiguous identifications. The table gives all available multiwavelength data for the identified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425#table1</TD>
            <TD>2011-09-14T19:53:44Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/449/425&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/425</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/62 [1]</TD>
            <TD>Catalog of double nucleus disk galaxies (Gimeno+, 2004)</TD>
            <TD>We have compiled a catalog of disk galaxies that have a double nucleus, through systematic examination of existing catalogs and publications. The Catalog of Double Nucleus Disk Galaxies includes 107 objects, together with their basic data. The aim of the catalog is to provide a more systematic and homogeneous basis for the study of the relevance of galaxy interactions and minor mergers in the formation of these double nuclei. We have also investigated possible correlations between geometric and photometric parameters of the double nuclei and their host galaxies. The preliminary results indicate the presence of several significant correlations that should be considered in any theoretical scenario describing minor mergers and disk galaxy evolution</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62#1</TD>
            <TD>2011-09-14T20:02:48Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/62</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/62</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/62 [2]</TD>
            <TD>Catalog of double nucleus disk galaxies (Gimeno+, 2004)</TD>
            <TD>We have compiled a catalog of disk galaxies that have a double nucleus, through systematic examination of existing catalogs and publications. The Catalog of Double Nucleus Disk Galaxies includes 107 objects, together with their basic data. The aim of the catalog is to provide a more systematic and homogeneous basis for the study of the relevance of galaxy interactions and minor mergers in the formation of these double nuclei. We have also investigated possible correlations between geometric and photometric parameters of the double nuclei and their host galaxies. The preliminary results indicate the presence of several significant correlations that should be considered in any theoretical scenario describing minor mergers and disk galaxy evolution</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62#2</TD>
            <TD>2011-09-14T20:02:48Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/62&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/62 [table1]</TD>
            <TD>Catalog of double nucleus disk galaxies (Gimeno+, 2004)</TD>
            <TD>We have compiled a catalog of disk galaxies that have a double nucleus, through systematic examination of existing catalogs and publications. The Catalog of Double Nucleus Disk Galaxies includes 107 objects, together with their basic data. The aim of the catalog is to provide a more systematic and homogeneous basis for the study of the relevance of galaxy interactions and minor mergers in the formation of these double nuclei. We have also investigated possible correlations between geometric and photometric parameters of the double nuclei and their host galaxies. The preliminary results indicate the presence of several significant correlations that should be considered in any theoretical scenario describing minor mergers and disk galaxy evolution</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62#table1</TD>
            <TD>2011-09-14T20:02:48Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/62</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/62 [1]</TD>
            <TD>Catalog of double nucleus disk galaxies (Gimeno+, 2004)</TD>
            <TD>We have compiled a catalog of disk galaxies that have a double nucleus, through systematic examination of existing catalogs and publications. The Catalog of Double Nucleus Disk Galaxies includes 107 objects, together with their basic data. The aim of the catalog is to provide a more systematic and homogeneous basis for the study of the relevance of galaxy interactions and minor mergers in the formation of these double nuclei. We have also investigated possible correlations between geometric and photometric parameters of the double nuclei and their host galaxies. The preliminary results indicate the presence of several significant correlations that should be considered in any theoretical scenario describing minor mergers and disk galaxy evolution</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62#1</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/128/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/62</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/62</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/62 [2]</TD>
            <TD>Catalog of double nucleus disk galaxies (Gimeno+, 2004)</TD>
            <TD>We have compiled a catalog of disk galaxies that have a double nucleus, through systematic examination of existing catalogs and publications. The Catalog of Double Nucleus Disk Galaxies includes 107 objects, together with their basic data. The aim of the catalog is to provide a more systematic and homogeneous basis for the study of the relevance of galaxy interactions and minor mergers in the formation of these double nuclei. We have also investigated possible correlations between geometric and photometric parameters of the double nuclei and their host galaxies. The preliminary results indicate the presence of several significant correlations that should be considered in any theoretical scenario describing minor mergers and disk galaxy evolution</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T20:02:48Z</TD>
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            <TD>22-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/62&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/62 [table1]</TD>
            <TD>Catalog of double nucleus disk galaxies (Gimeno+, 2004)</TD>
            <TD>We have compiled a catalog of disk galaxies that have a double nucleus, through systematic examination of existing catalogs and publications. The Catalog of Double Nucleus Disk Galaxies includes 107 objects, together with their basic data. The aim of the catalog is to provide a more systematic and homogeneous basis for the study of the relevance of galaxy interactions and minor mergers in the formation of these double nuclei. We have also investigated possible correlations between geometric and photometric parameters of the double nuclei and their host galaxies. The preliminary results indicate the presence of several significant correlations that should be considered in any theoretical scenario describing minor mergers and disk galaxy evolution</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62#table1</TD>
            <TD>2011-09-14T20:02:48Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
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            <TD>22-Jan-2007</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/62</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/459/85 [1]</TD>
            <TD>O/H and gas densities in star-forming galaxies (Nagao+, 2006)</TD>
            <TD>Generally the gas metallicity in distant galaxies can only be inferred by using a few prominent emission lines. Various theoretical models have been used to predict the relationship between emission line fluxes and metallicity, suggesting that some line ratios can be used as diagnostics of the gas metallicity in galaxies. However, accurate empirical calibrations of these emission line flux ratios from real galaxy spectra spanning a wide metallicity range are still lacking. In this paper we provide such empirical calibrations by using the combination of two sets of spectroscopic data: one consisting of low-metallicity galaxies with a measurement of [O III]{lambda}4363 taken from the literature, including spectra from the Sloan Digital Sky Survey (SDSS), and the other one consisting of galaxies in the SDSS database whose gas metallicity has been determined from various strong emission lines in their spectra. This combined data set constitutes the largest sample of galaxies with information on the gas metallicity available so far and spanning the widest metallicity range. By using these data we obtain accurate empirical relations between gas metallicity and several emission line diagnostics, including the R23 parameter, the [NII]{lambda}6584/H{alpha} and [O III]{lambda}5007/[NII]{lambda}6584 ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85#1</TD>
            <TD>2011-09-14T20:06:10Z</TD>
            <TD>#Abundances#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/459/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/459/85 [2]</TD>
            <TD>O/H and gas densities in star-forming galaxies (Nagao+, 2006)</TD>
            <TD>Generally the gas metallicity in distant galaxies can only be inferred by using a few prominent emission lines. Various theoretical models have been used to predict the relationship between emission line fluxes and metallicity, suggesting that some line ratios can be used as diagnostics of the gas metallicity in galaxies. However, accurate empirical calibrations of these emission line flux ratios from real galaxy spectra spanning a wide metallicity range are still lacking. In this paper we provide such empirical calibrations by using the combination of two sets of spectroscopic data: one consisting of low-metallicity galaxies with a measurement of [O III]{lambda}4363 taken from the literature, including spectra from the Sloan Digital Sky Survey (SDSS), and the other one consisting of galaxies in the SDSS database whose gas metallicity has been determined from various strong emission lines in their spectra. This combined data set constitutes the largest sample of galaxies with information on the gas metallicity available so far and spanning the widest metallicity range. By using these data we obtain accurate empirical relations between gas metallicity and several emission line diagnostics, including the R23 parameter, the [NII]{lambda}6584/H{alpha} and [O III]{lambda}5007/[NII]{lambda}6584 ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85#2</TD>
            <TD>2011-09-14T20:06:10Z</TD>
            <TD>#Abundances#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/459/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/85</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/459/85 [table1]</TD>
            <TD>O/H and gas densities in star-forming galaxies (Nagao+, 2006)</TD>
            <TD>Generally the gas metallicity in distant galaxies can only be inferred by using a few prominent emission lines. Various theoretical models have been used to predict the relationship between emission line fluxes and metallicity, suggesting that some line ratios can be used as diagnostics of the gas metallicity in galaxies. However, accurate empirical calibrations of these emission line flux ratios from real galaxy spectra spanning a wide metallicity range are still lacking. In this paper we provide such empirical calibrations by using the combination of two sets of spectroscopic data: one consisting of low-metallicity galaxies with a measurement of [O III]{lambda}4363 taken from the literature, including spectra from the Sloan Digital Sky Survey (SDSS), and the other one consisting of galaxies in the SDSS database whose gas metallicity has been determined from various strong emission lines in their spectra. This combined data set constitutes the largest sample of galaxies with information on the gas metallicity available so far and spanning the widest metallicity range. By using these data we obtain accurate empirical relations between gas metallicity and several emission line diagnostics, including the R23 parameter, the [NII]{lambda}6584/H{alpha} and [O III]{lambda}5007/[NII]{lambda}6584 ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85#table1</TD>
            <TD>2011-09-14T20:06:10Z</TD>
            <TD>#Abundances#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/459/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/85</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/399/457 [1]</TD>
            <TD>Warps in southern hemisphere galaxies (Sanchez-Saavedra+, 2003)</TD>
            <TD>A catalog of optical warps of galaxies is presented. This can be considered complementary to that reported by Sanchez-Saavedra et al. (1990MNRAS.246..458S), with 42 galaxies in the northern hemisphere, and to that by Reshetnikov &amp; Combes (1999A&amp;AS..138..101R), with 60 optical warps. The limits of the present catalog are: logr_25_&gt;0.60, B_1_&lt;14.5, DE(2000)&lt;0{deg}, -2.5&lt;t.7. Therefore, lenticular galaxies have also been considered. This catalog lists 150 warped galaxies out of a sample of 276 edge-on galaxies and covers the whole southern hemisphere, except the Avoidance Zone. It is therefore very suitable for statistical studies of warps. It also provides a source guide for detailed particular observations. We confirm the large frequency of warped spirals: nearly all galaxies are warped. The frequency and warp angle do not present important differences for the different types of spirals. However, no lenticular warped galaxy has been found within the specified limits. This finding constitutes an important restriction for theoretical models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457#1</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/399/457</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/399/457</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/457</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/399/457 [2]</TD>
            <TD>Warps in southern hemisphere galaxies (Sanchez-Saavedra+, 2003)</TD>
            <TD>A catalog of optical warps of galaxies is presented. This can be considered complementary to that reported by Sanchez-Saavedra et al. (1990MNRAS.246..458S), with 42 galaxies in the northern hemisphere, and to that by Reshetnikov &amp; Combes (1999A&amp;AS..138..101R), with 60 optical warps. The limits of the present catalog are: logr_25_&gt;0.60, B_1_&lt;14.5, DE(2000)&lt;0{deg}, -2.5&lt;t.7. Therefore, lenticular galaxies have also been considered. This catalog lists 150 warped galaxies out of a sample of 276 edge-on galaxies and covers the whole southern hemisphere, except the Avoidance Zone. It is therefore very suitable for statistical studies of warps. It also provides a source guide for detailed particular observations. We confirm the large frequency of warped spirals: nearly all galaxies are warped. The frequency and warp angle do not present important differences for the different types of spirals. However, no lenticular warped galaxy has been found within the specified limits. This finding constitutes an important restriction for theoretical models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457#2</TD>
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            <TD>18-Mar-2003</TD>
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            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/399/457&amp;</TD>
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            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/399/457 [galaxies]</TD>
            <TD>Warps in southern hemisphere galaxies (Sanchez-Saavedra+, 2003)</TD>
            <TD>A catalog of optical warps of galaxies is presented. This can be considered complementary to that reported by Sanchez-Saavedra et al. (1990MNRAS.246..458S), with 42 galaxies in the northern hemisphere, and to that by Reshetnikov &amp; Combes (1999A&amp;AS..138..101R), with 60 optical warps. The limits of the present catalog are: logr_25_&gt;0.60, B_1_&lt;14.5, DE(2000)&lt;0{deg}, -2.5&lt;t.7. Therefore, lenticular galaxies have also been considered. This catalog lists 150 warped galaxies out of a sample of 276 edge-on galaxies and covers the whole southern hemisphere, except the Avoidance Zone. It is therefore very suitable for statistical studies of warps. It also provides a source guide for detailed particular observations. We confirm the large frequency of warped spirals: nearly all galaxies are warped. The frequency and warp angle do not present important differences for the different types of spirals. However, no lenticular warped galaxy has been found within the specified limits. This finding constitutes an important restriction for theoretical models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457#galaxies</TD>
            <TD>2011-09-14T19:55:29Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/457&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/457</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/459/85 [1]</TD>
            <TD>O/H and gas densities in star-forming galaxies (Nagao+, 2006)</TD>
            <TD>Generally the gas metallicity in distant galaxies can only be inferred by using a few prominent emission lines. Various theoretical models have been used to predict the relationship between emission line fluxes and metallicity, suggesting that some line ratios can be used as diagnostics of the gas metallicity in galaxies. However, accurate empirical calibrations of these emission line flux ratios from real galaxy spectra spanning a wide metallicity range are still lacking. In this paper we provide such empirical calibrations by using the combination of two sets of spectroscopic data: one consisting of low-metallicity galaxies with a measurement of [O III]{lambda}4363 taken from the literature, including spectra from the Sloan Digital Sky Survey (SDSS), and the other one consisting of galaxies in the SDSS database whose gas metallicity has been determined from various strong emission lines in their spectra. This combined data set constitutes the largest sample of galaxies with information on the gas metallicity available so far and spanning the widest metallicity range. By using these data we obtain accurate empirical relations between gas metallicity and several emission line diagnostics, including the R23 parameter, the [NII]{lambda}6584/H{alpha} and [O III]{lambda}5007/[NII]{lambda}6584 ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85#1</TD>
            <TD>2011-09-14T20:06:10Z</TD>
            <TD>#Abundances#Interstellar_Medium#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/459/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/85</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/459/85 [2]</TD>
            <TD>O/H and gas densities in star-forming galaxies (Nagao+, 2006)</TD>
            <TD>Generally the gas metallicity in distant galaxies can only be inferred by using a few prominent emission lines. Various theoretical models have been used to predict the relationship between emission line fluxes and metallicity, suggesting that some line ratios can be used as diagnostics of the gas metallicity in galaxies. However, accurate empirical calibrations of these emission line flux ratios from real galaxy spectra spanning a wide metallicity range are still lacking. In this paper we provide such empirical calibrations by using the combination of two sets of spectroscopic data: one consisting of low-metallicity galaxies with a measurement of [O III]{lambda}4363 taken from the literature, including spectra from the Sloan Digital Sky Survey (SDSS), and the other one consisting of galaxies in the SDSS database whose gas metallicity has been determined from various strong emission lines in their spectra. This combined data set constitutes the largest sample of galaxies with information on the gas metallicity available so far and spanning the widest metallicity range. By using these data we obtain accurate empirical relations between gas metallicity and several emission line diagnostics, including the R23 parameter, the [NII]{lambda}6584/H{alpha} and [O III]{lambda}5007/[NII]{lambda}6584 ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85#2</TD>
            <TD>2011-09-14T20:06:10Z</TD>
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            <TD>11-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/459/85&amp;</TD>
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            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/459/85 [table1]</TD>
            <TD>O/H and gas densities in star-forming galaxies (Nagao+, 2006)</TD>
            <TD>Generally the gas metallicity in distant galaxies can only be inferred by using a few prominent emission lines. Various theoretical models have been used to predict the relationship between emission line fluxes and metallicity, suggesting that some line ratios can be used as diagnostics of the gas metallicity in galaxies. However, accurate empirical calibrations of these emission line flux ratios from real galaxy spectra spanning a wide metallicity range are still lacking. In this paper we provide such empirical calibrations by using the combination of two sets of spectroscopic data: one consisting of low-metallicity galaxies with a measurement of [O III]{lambda}4363 taken from the literature, including spectra from the Sloan Digital Sky Survey (SDSS), and the other one consisting of galaxies in the SDSS database whose gas metallicity has been determined from various strong emission lines in their spectra. This combined data set constitutes the largest sample of galaxies with information on the gas metallicity available so far and spanning the widest metallicity range. By using these data we obtain accurate empirical relations between gas metallicity and several emission line diagnostics, including the R23 parameter, the [NII]{lambda}6584/H{alpha} and [O III]{lambda}5007/[NII]{lambda}6584 ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85#table1</TD>
            <TD>2011-09-14T20:06:10Z</TD>
            <TD>#Abundances#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/459/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/399/457 [1]</TD>
            <TD>Warps in southern hemisphere galaxies (Sanchez-Saavedra+, 2003)</TD>
            <TD>A catalog of optical warps of galaxies is presented. This can be considered complementary to that reported by Sanchez-Saavedra et al. (1990MNRAS.246..458S), with 42 galaxies in the northern hemisphere, and to that by Reshetnikov &amp; Combes (1999A&amp;AS..138..101R), with 60 optical warps. The limits of the present catalog are: logr_25_&gt;0.60, B_1_&lt;14.5, DE(2000)&lt;0{deg}, -2.5&lt;t.7. Therefore, lenticular galaxies have also been considered. This catalog lists 150 warped galaxies out of a sample of 276 edge-on galaxies and covers the whole southern hemisphere, except the Avoidance Zone. It is therefore very suitable for statistical studies of warps. It also provides a source guide for detailed particular observations. We confirm the large frequency of warped spirals: nearly all galaxies are warped. The frequency and warp angle do not present important differences for the different types of spirals. However, no lenticular warped galaxy has been found within the specified limits. This finding constitutes an important restriction for theoretical models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457#1</TD>
            <TD>2011-09-14T19:55:29Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/399/457</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/457</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/399/457 [2]</TD>
            <TD>Warps in southern hemisphere galaxies (Sanchez-Saavedra+, 2003)</TD>
            <TD>A catalog of optical warps of galaxies is presented. This can be considered complementary to that reported by Sanchez-Saavedra et al. (1990MNRAS.246..458S), with 42 galaxies in the northern hemisphere, and to that by Reshetnikov &amp; Combes (1999A&amp;AS..138..101R), with 60 optical warps. The limits of the present catalog are: logr_25_&gt;0.60, B_1_&lt;14.5, DE(2000)&lt;0{deg}, -2.5&lt;t.7. Therefore, lenticular galaxies have also been considered. This catalog lists 150 warped galaxies out of a sample of 276 edge-on galaxies and covers the whole southern hemisphere, except the Avoidance Zone. It is therefore very suitable for statistical studies of warps. It also provides a source guide for detailed particular observations. We confirm the large frequency of warped spirals: nearly all galaxies are warped. The frequency and warp angle do not present important differences for the different types of spirals. However, no lenticular warped galaxy has been found within the specified limits. This finding constitutes an important restriction for theoretical models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457#2</TD>
            <TD>2011-09-14T19:55:29Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/399/457&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/457</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/457 [galaxies]</TD>
            <TD>Warps in southern hemisphere galaxies (Sanchez-Saavedra+, 2003)</TD>
            <TD>A catalog of optical warps of galaxies is presented. This can be considered complementary to that reported by Sanchez-Saavedra et al. (1990MNRAS.246..458S), with 42 galaxies in the northern hemisphere, and to that by Reshetnikov &amp; Combes (1999A&amp;AS..138..101R), with 60 optical warps. The limits of the present catalog are: logr_25_&gt;0.60, B_1_&lt;14.5, DE(2000)&lt;0{deg}, -2.5&lt;t.7. Therefore, lenticular galaxies have also been considered. This catalog lists 150 warped galaxies out of a sample of 276 edge-on galaxies and covers the whole southern hemisphere, except the Avoidance Zone. It is therefore very suitable for statistical studies of warps. It also provides a source guide for detailed particular observations. We confirm the large frequency of warped spirals: nearly all galaxies are warped. The frequency and warp angle do not present important differences for the different types of spirals. However, no lenticular warped galaxy has been found within the specified limits. This finding constitutes an important restriction for theoretical models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457#galaxies</TD>
            <TD>2011-09-14T19:55:29Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/457&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/457</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/459/85 [1]</TD>
            <TD>O/H and gas densities in star-forming galaxies (Nagao+, 2006)</TD>
            <TD>Generally the gas metallicity in distant galaxies can only be inferred by using a few prominent emission lines. Various theoretical models have been used to predict the relationship between emission line fluxes and metallicity, suggesting that some line ratios can be used as diagnostics of the gas metallicity in galaxies. However, accurate empirical calibrations of these emission line flux ratios from real galaxy spectra spanning a wide metallicity range are still lacking. In this paper we provide such empirical calibrations by using the combination of two sets of spectroscopic data: one consisting of low-metallicity galaxies with a measurement of [O III]{lambda}4363 taken from the literature, including spectra from the Sloan Digital Sky Survey (SDSS), and the other one consisting of galaxies in the SDSS database whose gas metallicity has been determined from various strong emission lines in their spectra. This combined data set constitutes the largest sample of galaxies with information on the gas metallicity available so far and spanning the widest metallicity range. By using these data we obtain accurate empirical relations between gas metallicity and several emission line diagnostics, including the R23 parameter, the [NII]{lambda}6584/H{alpha} and [O III]{lambda}5007/[NII]{lambda}6584 ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85#1</TD>
            <TD>2011-09-14T20:06:10Z</TD>
            <TD>#Abundances#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/459/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/459/85 [2]</TD>
            <TD>O/H and gas densities in star-forming galaxies (Nagao+, 2006)</TD>
            <TD>Generally the gas metallicity in distant galaxies can only be inferred by using a few prominent emission lines. Various theoretical models have been used to predict the relationship between emission line fluxes and metallicity, suggesting that some line ratios can be used as diagnostics of the gas metallicity in galaxies. However, accurate empirical calibrations of these emission line flux ratios from real galaxy spectra spanning a wide metallicity range are still lacking. In this paper we provide such empirical calibrations by using the combination of two sets of spectroscopic data: one consisting of low-metallicity galaxies with a measurement of [O III]{lambda}4363 taken from the literature, including spectra from the Sloan Digital Sky Survey (SDSS), and the other one consisting of galaxies in the SDSS database whose gas metallicity has been determined from various strong emission lines in their spectra. This combined data set constitutes the largest sample of galaxies with information on the gas metallicity available so far and spanning the widest metallicity range. By using these data we obtain accurate empirical relations between gas metallicity and several emission line diagnostics, including the R23 parameter, the [NII]{lambda}6584/H{alpha} and [O III]{lambda}5007/[NII]{lambda}6584 ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85#2</TD>
            <TD>2011-09-14T20:06:10Z</TD>
            <TD>#Abundances#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/459/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/459/85 [table1]</TD>
            <TD>O/H and gas densities in star-forming galaxies (Nagao+, 2006)</TD>
            <TD>Generally the gas metallicity in distant galaxies can only be inferred by using a few prominent emission lines. Various theoretical models have been used to predict the relationship between emission line fluxes and metallicity, suggesting that some line ratios can be used as diagnostics of the gas metallicity in galaxies. However, accurate empirical calibrations of these emission line flux ratios from real galaxy spectra spanning a wide metallicity range are still lacking. In this paper we provide such empirical calibrations by using the combination of two sets of spectroscopic data: one consisting of low-metallicity galaxies with a measurement of [O III]{lambda}4363 taken from the literature, including spectra from the Sloan Digital Sky Survey (SDSS), and the other one consisting of galaxies in the SDSS database whose gas metallicity has been determined from various strong emission lines in their spectra. This combined data set constitutes the largest sample of galaxies with information on the gas metallicity available so far and spanning the widest metallicity range. By using these data we obtain accurate empirical relations between gas metallicity and several emission line diagnostics, including the R23 parameter, the [NII]{lambda}6584/H{alpha} and [O III]{lambda}5007/[NII]{lambda}6584 ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85#table1</TD>
            <TD>2011-09-14T20:06:10Z</TD>
            <TD>#Abundances#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/459/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/399/457 [1]</TD>
            <TD>Warps in southern hemisphere galaxies (Sanchez-Saavedra+, 2003)</TD>
            <TD>A catalog of optical warps of galaxies is presented. This can be considered complementary to that reported by Sanchez-Saavedra et al. (1990MNRAS.246..458S), with 42 galaxies in the northern hemisphere, and to that by Reshetnikov &amp; Combes (1999A&amp;AS..138..101R), with 60 optical warps. The limits of the present catalog are: logr_25_&gt;0.60, B_1_&lt;14.5, DE(2000)&lt;0{deg}, -2.5&lt;t.7. Therefore, lenticular galaxies have also been considered. This catalog lists 150 warped galaxies out of a sample of 276 edge-on galaxies and covers the whole southern hemisphere, except the Avoidance Zone. It is therefore very suitable for statistical studies of warps. It also provides a source guide for detailed particular observations. We confirm the large frequency of warped spirals: nearly all galaxies are warped. The frequency and warp angle do not present important differences for the different types of spirals. However, no lenticular warped galaxy has been found within the specified limits. This finding constitutes an important restriction for theoretical models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457#1</TD>
            <TD>2011-09-14T19:55:29Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/399/457</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/457</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/399/457 [2]</TD>
            <TD>Warps in southern hemisphere galaxies (Sanchez-Saavedra+, 2003)</TD>
            <TD>A catalog of optical warps of galaxies is presented. This can be considered complementary to that reported by Sanchez-Saavedra et al. (1990MNRAS.246..458S), with 42 galaxies in the northern hemisphere, and to that by Reshetnikov &amp; Combes (1999A&amp;AS..138..101R), with 60 optical warps. The limits of the present catalog are: logr_25_&gt;0.60, B_1_&lt;14.5, DE(2000)&lt;0{deg}, -2.5&lt;t.7. Therefore, lenticular galaxies have also been considered. This catalog lists 150 warped galaxies out of a sample of 276 edge-on galaxies and covers the whole southern hemisphere, except the Avoidance Zone. It is therefore very suitable for statistical studies of warps. It also provides a source guide for detailed particular observations. We confirm the large frequency of warped spirals: nearly all galaxies are warped. The frequency and warp angle do not present important differences for the different types of spirals. However, no lenticular warped galaxy has been found within the specified limits. This finding constitutes an important restriction for theoretical models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457#2</TD>
            <TD>2011-09-14T19:55:29Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/399/457&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/457</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/457 [galaxies]</TD>
            <TD>Warps in southern hemisphere galaxies (Sanchez-Saavedra+, 2003)</TD>
            <TD>A catalog of optical warps of galaxies is presented. This can be considered complementary to that reported by Sanchez-Saavedra et al. (1990MNRAS.246..458S), with 42 galaxies in the northern hemisphere, and to that by Reshetnikov &amp; Combes (1999A&amp;AS..138..101R), with 60 optical warps. The limits of the present catalog are: logr_25_&gt;0.60, B_1_&lt;14.5, DE(2000)&lt;0{deg}, -2.5&lt;t.7. Therefore, lenticular galaxies have also been considered. This catalog lists 150 warped galaxies out of a sample of 276 edge-on galaxies and covers the whole southern hemisphere, except the Avoidance Zone. It is therefore very suitable for statistical studies of warps. It also provides a source guide for detailed particular observations. We confirm the large frequency of warped spirals: nearly all galaxies are warped. The frequency and warp angle do not present important differences for the different types of spirals. However, no lenticular warped galaxy has been found within the specified limits. This finding constitutes an important restriction for theoretical models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457#galaxies</TD>
            <TD>2011-09-14T19:55:29Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/457</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/457&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/457</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>HST.GEMS</TD>
            <TD>HST Galaxy Evolution from Morphology and SEDs</TD>
            <TD>GEMs is a large-area (800 arcmin 2) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the Hubble Space Telescope. Centered on the Chandra Deep Field-South, it covers an area of ~ 28'x28', or about 120 HDF areas, to a depth of MAB(F606W)=28.5(5s) for compact sources. Focusing on the redshift range ~ 0.2&lt;z&lt;1.1, GEMS provides morphologies and structural parameters for nearly 10,000 galaxies where redshift estimates, luminosities, and SEDs exist from COMBO-17.</TD>
            <TD>MAST</TD>
            <TD>#Optical#</TD>
            <TD>ivo://mast.stsci/siap/hst.gems#1</TD>
            <TD>2012-03-08T20:44:09Z</TD>
            <TD>#Optical Astronomy#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1.0</TD>
            <TD>ivo://mast.stsci/siap/hst.gems</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://archive.stsci.edu/siap/search.php?id=gems&amp;</TD>
            <TD />
            <TD>100</TD>
            <TD />
            <TD>http://archive.stsci.edu/prepds/gems/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/467/1003 [1]</TD>
            <TD>Photometry of star clusters in NGC 1380 (Chies-Santos+ 2007)</TD>
            <TD>NGC 1380 is a lenticular galaxy located near the center of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy was previously studied only from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the center of the galaxy. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. A total of about 570 cluster candidates were found down to V=26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks. Likewise for the size distribution. We identified the smaller population as being mainly typical globular clusters, while the more extended objects have small probabilities of being such objects. Different correlations between absolute magnitudes, sizes, colours and location were inferred for these cluster sub-populations. Most extended clusters (Reff&gt;4pc) share similar properties to the diffuse star clusters reported to inhabit luminous early-type galaxies in the Virgo galaxy cluster such as being of low surface brightness and fainter than MV~-8. We also report on a small group of (R_eff_~10pc), -8&lt;MV&lt;-6, red clusters located near the centre of NGC 1380, which may be interpreted as faint fuzzies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003#1</TD>
            <TD>2011-09-14T20:06:26Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/467/1003</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1003</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/467/1003 [2]</TD>
            <TD>Photometry of star clusters in NGC 1380 (Chies-Santos+ 2007)</TD>
            <TD>NGC 1380 is a lenticular galaxy located near the center of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy was previously studied only from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the center of the galaxy. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. A total of about 570 cluster candidates were found down to V=26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks. Likewise for the size distribution. We identified the smaller population as being mainly typical globular clusters, while the more extended objects have small probabilities of being such objects. Different correlations between absolute magnitudes, sizes, colours and location were inferred for these cluster sub-populations. Most extended clusters (Reff&gt;4pc) share similar properties to the diffuse star clusters reported to inhabit luminous early-type galaxies in the Virgo galaxy cluster such as being of low surface brightness and fainter than MV~-8. We also report on a small group of (R_eff_~10pc), -8&lt;MV&lt;-6, red clusters located near the centre of NGC 1380, which may be interpreted as faint fuzzies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003#2</TD>
            <TD>2011-09-14T20:06:26Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/467/1003&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1003</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/467/1003 [table4]</TD>
            <TD>Photometry of star clusters in NGC 1380 (Chies-Santos+ 2007)</TD>
            <TD>NGC 1380 is a lenticular galaxy located near the center of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy was previously studied only from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the center of the galaxy. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. A total of about 570 cluster candidates were found down to V=26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks. Likewise for the size distribution. We identified the smaller population as being mainly typical globular clusters, while the more extended objects have small probabilities of being such objects. Different correlations between absolute magnitudes, sizes, colours and location were inferred for these cluster sub-populations. Most extended clusters (Reff&gt;4pc) share similar properties to the diffuse star clusters reported to inhabit luminous early-type galaxies in the Virgo galaxy cluster such as being of low surface brightness and fainter than MV~-8. We also report on a small group of (R_eff_~10pc), -8&lt;MV&lt;-6, red clusters located near the centre of NGC 1380, which may be interpreted as faint fuzzies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003#table4</TD>
            <TD>2011-09-14T20:06:26Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/467/1003&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1003</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSSDR5</TD>
            <TD>Sloan Digital Sky Survey (DR5)</TD>
            <TD>This node contains data from the fifth data release (DR5) of SDSS. The Sloan Digital Sky Survey is the most ambitious astronomical survey ever undertaken. The survey will map one-quarter of the entire sky in detail, determining the positions and absolute brightnesses of hundreds of millions of celestial objects. It will also measure the distances to more than a million galaxies and quasars. The SDSS addresses fascinating, fundamental questions about the universe. With the survey, astronomers will be able to see the large-scale patterns of galaxies: sheets and voids through the whole universe. Scientists have many ideas about how the universe evolved, and different patterns of large-scale structure point to different theories. The Sloan Digital Sky Survey will tell us which theories are right - or whether we will have to come up with entirely new ideas.</TD>
            <TD>JHU</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/SDSSDR5#1</TD>
            <TD>2012-03-08T20:49:58Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD>#Research#</TD>
            <TD />
            <TD>DR5</TD>
            <TD>ivo://sdss.jhu/openskynode/SDSSDR5</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/SDSSDR5/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD>http://www.sdss.org/dr5</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/467/1003 [1]</TD>
            <TD>Photometry of star clusters in NGC 1380 (Chies-Santos+ 2007)</TD>
            <TD>NGC 1380 is a lenticular galaxy located near the center of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy was previously studied only from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the center of the galaxy. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. A total of about 570 cluster candidates were found down to V=26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks. Likewise for the size distribution. We identified the smaller population as being mainly typical globular clusters, while the more extended objects have small probabilities of being such objects. Different correlations between absolute magnitudes, sizes, colours and location were inferred for these cluster sub-populations. Most extended clusters (Reff&gt;4pc) share similar properties to the diffuse star clusters reported to inhabit luminous early-type galaxies in the Virgo galaxy cluster such as being of low surface brightness and fainter than MV~-8. We also report on a small group of (R_eff_~10pc), -8&lt;MV&lt;-6, red clusters located near the centre of NGC 1380, which may be interpreted as faint fuzzies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003#1</TD>
            <TD>2011-09-14T20:06:26Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/467/1003</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1003</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/467/1003 [2]</TD>
            <TD>Photometry of star clusters in NGC 1380 (Chies-Santos+ 2007)</TD>
            <TD>NGC 1380 is a lenticular galaxy located near the center of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy was previously studied only from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the center of the galaxy. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. A total of about 570 cluster candidates were found down to V=26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks. Likewise for the size distribution. We identified the smaller population as being mainly typical globular clusters, while the more extended objects have small probabilities of being such objects. Different correlations between absolute magnitudes, sizes, colours and location were inferred for these cluster sub-populations. Most extended clusters (Reff&gt;4pc) share similar properties to the diffuse star clusters reported to inhabit luminous early-type galaxies in the Virgo galaxy cluster such as being of low surface brightness and fainter than MV~-8. We also report on a small group of (R_eff_~10pc), -8&lt;MV&lt;-6, red clusters located near the centre of NGC 1380, which may be interpreted as faint fuzzies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003#2</TD>
            <TD>2011-09-14T20:06:26Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/467/1003&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1003</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/467/1003 [table4]</TD>
            <TD>Photometry of star clusters in NGC 1380 (Chies-Santos+ 2007)</TD>
            <TD>NGC 1380 is a lenticular galaxy located near the center of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy was previously studied only from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the center of the galaxy. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. A total of about 570 cluster candidates were found down to V=26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks. Likewise for the size distribution. We identified the smaller population as being mainly typical globular clusters, while the more extended objects have small probabilities of being such objects. Different correlations between absolute magnitudes, sizes, colours and location were inferred for these cluster sub-populations. Most extended clusters (Reff&gt;4pc) share similar properties to the diffuse star clusters reported to inhabit luminous early-type galaxies in the Virgo galaxy cluster such as being of low surface brightness and fainter than MV~-8. We also report on a small group of (R_eff_~10pc), -8&lt;MV&lt;-6, red clusters located near the centre of NGC 1380, which may be interpreted as faint fuzzies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003#table4</TD>
            <TD>2011-09-14T20:06:26Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/467/1003&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1003</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/449/425 [1]</TD>
            <TD>Optical identification of ROSAT-FSC sources (Mickaelian+, 2006)</TD>
            <TD>The Byurakan/Hamburg/ROSAT Catalogue (BHRC) of the optical identifications of X-ray sources is presented. The BHRC includes all 2791 sources from the ROSAT-FSC (&lt;IX/29&gt;) with |b|&gt;30, DEC&gt;0 and ROSAT count rate CR&gt;0.04cts/s. The optical identifications were carried out by means of the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, and other available data. We managed to identify 97% of sources (2696 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups etc.), and 304 have ambiguous identifications. The table gives all available multiwavelength data for the identified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425#1</TD>
            <TD>2011-09-14T19:53:44Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/449/425</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/425</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/449/425 [2]</TD>
            <TD>Optical identification of ROSAT-FSC sources (Mickaelian+, 2006)</TD>
            <TD>The Byurakan/Hamburg/ROSAT Catalogue (BHRC) of the optical identifications of X-ray sources is presented. The BHRC includes all 2791 sources from the ROSAT-FSC (&lt;IX/29&gt;) with |b|&gt;30, DEC&gt;0 and ROSAT count rate CR&gt;0.04cts/s. The optical identifications were carried out by means of the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, and other available data. We managed to identify 97% of sources (2696 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups etc.), and 304 have ambiguous identifications. The table gives all available multiwavelength data for the identified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425#2</TD>
            <TD>2011-09-14T19:53:44Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/449/425&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/425</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/449/425 [table1]</TD>
            <TD>Optical identification of ROSAT-FSC sources (Mickaelian+, 2006)</TD>
            <TD>The Byurakan/Hamburg/ROSAT Catalogue (BHRC) of the optical identifications of X-ray sources is presented. The BHRC includes all 2791 sources from the ROSAT-FSC (&lt;IX/29&gt;) with |b|&gt;30, DEC&gt;0 and ROSAT count rate CR&gt;0.04cts/s. The optical identifications were carried out by means of the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, and other available data. We managed to identify 97% of sources (2696 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups etc.), and 304 have ambiguous identifications. The table gives all available multiwavelength data for the identified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425#table1</TD>
            <TD>2011-09-14T19:53:44Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/425</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/449/425&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/425</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/359/865 [1]</TD>
            <TD>ISOPHOT 170{mu}m Serendipity Survey I. (Stickel+, 2000)</TD>
            <TD>Serendipity slew survey measurements were acquired with the ISOPHOT C200 detector installed on the ISO mission. The C200 detector is a 2x2 pixel array of stressed Ge:Ga with a pixel size of 89.4arcsec, and was used in conjunction with the C160 broad-band filter (reference wavelength 170{mu}m, width 89{mu}m). During the lifetime of the ISO mission, about 550 hours of measurements have been gathered with more than 12000 slews. From the slew data with low (100{mu}m&lt;=15MJy/sr) cirrus background, 115 well-observed sources with a high signal to noise ratio in all detector pixels having a galaxy association were extracted. The 170{mu}m fluxes measured from the Serendipity slews have been put on an absolute flux level by using calibration sources observed additionally with the photometric mapping mode of ISOPHOT. For all but a few galaxies, the 170{mu}m fluxes are determined for the first time, which represents a significant increase in he number of galaxies with measured Far-Infrared (FIR) fluxes beyond the IRAS 100{mu}m limit.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865#1</TD>
            <TD>2011-09-14T20:12:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/359/865</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/865</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/359/865 [2]</TD>
            <TD>ISOPHOT 170{mu}m Serendipity Survey I. (Stickel+, 2000)</TD>
            <TD>Serendipity slew survey measurements were acquired with the ISOPHOT C200 detector installed on the ISO mission. The C200 detector is a 2x2 pixel array of stressed Ge:Ga with a pixel size of 89.4arcsec, and was used in conjunction with the C160 broad-band filter (reference wavelength 170{mu}m, width 89{mu}m). During the lifetime of the ISO mission, about 550 hours of measurements have been gathered with more than 12000 slews. From the slew data with low (100{mu}m&lt;=15MJy/sr) cirrus background, 115 well-observed sources with a high signal to noise ratio in all detector pixels having a galaxy association were extracted. The 170{mu}m fluxes measured from the Serendipity slews have been put on an absolute flux level by using calibration sources observed additionally with the photometric mapping mode of ISOPHOT. For all but a few galaxies, the 170{mu}m fluxes are determined for the first time, which represents a significant increase in he number of galaxies with measured Far-Infrared (FIR) fluxes beyond the IRAS 100{mu}m limit.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865#2</TD>
            <TD>2011-09-14T20:12:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/359/865&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/865</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/359/865 [table4]</TD>
            <TD>ISOPHOT 170{mu}m Serendipity Survey I. (Stickel+, 2000)</TD>
            <TD>Serendipity slew survey measurements were acquired with the ISOPHOT C200 detector installed on the ISO mission. The C200 detector is a 2x2 pixel array of stressed Ge:Ga with a pixel size of 89.4arcsec, and was used in conjunction with the C160 broad-band filter (reference wavelength 170{mu}m, width 89{mu}m). During the lifetime of the ISO mission, about 550 hours of measurements have been gathered with more than 12000 slews. From the slew data with low (100{mu}m&lt;=15MJy/sr) cirrus background, 115 well-observed sources with a high signal to noise ratio in all detector pixels having a galaxy association were extracted. The 170{mu}m fluxes measured from the Serendipity slews have been put on an absolute flux level by using calibration sources observed additionally with the photometric mapping mode of ISOPHOT. For all but a few galaxies, the 170{mu}m fluxes are determined for the first time, which represents a significant increase in he number of galaxies with measured Far-Infrared (FIR) fluxes beyond the IRAS 100{mu}m limit.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865#table4</TD>
            <TD>2011-09-14T20:12:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/359/865&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/865</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/467/1003 [1]</TD>
            <TD>Photometry of star clusters in NGC 1380 (Chies-Santos+ 2007)</TD>
            <TD>NGC 1380 is a lenticular galaxy located near the center of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy was previously studied only from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the center of the galaxy. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. A total of about 570 cluster candidates were found down to V=26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks. Likewise for the size distribution. We identified the smaller population as being mainly typical globular clusters, while the more extended objects have small probabilities of being such objects. Different correlations between absolute magnitudes, sizes, colours and location were inferred for these cluster sub-populations. Most extended clusters (Reff&gt;4pc) share similar properties to the diffuse star clusters reported to inhabit luminous early-type galaxies in the Virgo galaxy cluster such as being of low surface brightness and fainter than MV~-8. We also report on a small group of (R_eff_~10pc), -8&lt;MV&lt;-6, red clusters located near the centre of NGC 1380, which may be interpreted as faint fuzzies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003#1</TD>
            <TD>2011-09-14T20:06:26Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/467/1003</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1003</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/467/1003 [2]</TD>
            <TD>Photometry of star clusters in NGC 1380 (Chies-Santos+ 2007)</TD>
            <TD>NGC 1380 is a lenticular galaxy located near the center of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy was previously studied only from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the center of the galaxy. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. A total of about 570 cluster candidates were found down to V=26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks. Likewise for the size distribution. We identified the smaller population as being mainly typical globular clusters, while the more extended objects have small probabilities of being such objects. Different correlations between absolute magnitudes, sizes, colours and location were inferred for these cluster sub-populations. Most extended clusters (Reff&gt;4pc) share similar properties to the diffuse star clusters reported to inhabit luminous early-type galaxies in the Virgo galaxy cluster such as being of low surface brightness and fainter than MV~-8. We also report on a small group of (R_eff_~10pc), -8&lt;MV&lt;-6, red clusters located near the centre of NGC 1380, which may be interpreted as faint fuzzies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003#2</TD>
            <TD>2011-09-14T20:06:26Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/467/1003&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1003</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/467/1003 [table4]</TD>
            <TD>Photometry of star clusters in NGC 1380 (Chies-Santos+ 2007)</TD>
            <TD>NGC 1380 is a lenticular galaxy located near the center of the Fornax Cluster, northeast of NGC 1399. The globular cluster system of this galaxy was previously studied only from the ground. Recent studies of similar early-type galaxies, specially lenticular ones, reveal the existence of star clusters that apparently break up the traditional open/globular cluster dichotomy. With higher quality photometry from HST/WFPC2 we study the star clusters in NGC 1380, measuring their magnitudes, colours, sizes and projected distances from the center of the galaxy. We used deep archival HST/WFPC2 in the B and V bands. We built colour magnitude diagrams from which we selected a sample of cluster candidates. We also analysed their colour distribution and measured their sizes. Based on their location in the luminosity-size diagram we estimated probabilities of them being typical globular clusters as those found in the Galaxy. A total of about 570 cluster candidates were found down to V=26.5. We measured sizes for approximately 200 of them. The observed colour distribution has three apparent peaks. Likewise for the size distribution. We identified the smaller population as being mainly typical globular clusters, while the more extended objects have small probabilities of being such objects. Different correlations between absolute magnitudes, sizes, colours and location were inferred for these cluster sub-populations. Most extended clusters (Reff&gt;4pc) share similar properties to the diffuse star clusters reported to inhabit luminous early-type galaxies in the Virgo galaxy cluster such as being of low surface brightness and fainter than MV~-8. We also report on a small group of (R_eff_~10pc), -8&lt;MV&lt;-6, red clusters located near the centre of NGC 1380, which may be interpreted as faint fuzzies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003#table4</TD>
            <TD>2011-09-14T20:06:26Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1003</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/467/1003&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1003</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/359/865 [1]</TD>
            <TD>ISOPHOT 170{mu}m Serendipity Survey I. (Stickel+, 2000)</TD>
            <TD>Serendipity slew survey measurements were acquired with the ISOPHOT C200 detector installed on the ISO mission. The C200 detector is a 2x2 pixel array of stressed Ge:Ga with a pixel size of 89.4arcsec, and was used in conjunction with the C160 broad-band filter (reference wavelength 170{mu}m, width 89{mu}m). During the lifetime of the ISO mission, about 550 hours of measurements have been gathered with more than 12000 slews. From the slew data with low (100{mu}m&lt;=15MJy/sr) cirrus background, 115 well-observed sources with a high signal to noise ratio in all detector pixels having a galaxy association were extracted. The 170{mu}m fluxes measured from the Serendipity slews have been put on an absolute flux level by using calibration sources observed additionally with the photometric mapping mode of ISOPHOT. For all but a few galaxies, the 170{mu}m fluxes are determined for the first time, which represents a significant increase in he number of galaxies with measured Far-Infrared (FIR) fluxes beyond the IRAS 100{mu}m limit.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865#1</TD>
            <TD>2011-09-14T20:12:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/359/865</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/865</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/359/865 [2]</TD>
            <TD>ISOPHOT 170{mu}m Serendipity Survey I. (Stickel+, 2000)</TD>
            <TD>Serendipity slew survey measurements were acquired with the ISOPHOT C200 detector installed on the ISO mission. The C200 detector is a 2x2 pixel array of stressed Ge:Ga with a pixel size of 89.4arcsec, and was used in conjunction with the C160 broad-band filter (reference wavelength 170{mu}m, width 89{mu}m). During the lifetime of the ISO mission, about 550 hours of measurements have been gathered with more than 12000 slews. From the slew data with low (100{mu}m&lt;=15MJy/sr) cirrus background, 115 well-observed sources with a high signal to noise ratio in all detector pixels having a galaxy association were extracted. The 170{mu}m fluxes measured from the Serendipity slews have been put on an absolute flux level by using calibration sources observed additionally with the photometric mapping mode of ISOPHOT. For all but a few galaxies, the 170{mu}m fluxes are determined for the first time, which represents a significant increase in he number of galaxies with measured Far-Infrared (FIR) fluxes beyond the IRAS 100{mu}m limit.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865#2</TD>
            <TD>2011-09-14T20:12:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/359/865&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/865</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/359/865 [table4]</TD>
            <TD>ISOPHOT 170{mu}m Serendipity Survey I. (Stickel+, 2000)</TD>
            <TD>Serendipity slew survey measurements were acquired with the ISOPHOT C200 detector installed on the ISO mission. The C200 detector is a 2x2 pixel array of stressed Ge:Ga with a pixel size of 89.4arcsec, and was used in conjunction with the C160 broad-band filter (reference wavelength 170{mu}m, width 89{mu}m). During the lifetime of the ISO mission, about 550 hours of measurements have been gathered with more than 12000 slews. From the slew data with low (100{mu}m&lt;=15MJy/sr) cirrus background, 115 well-observed sources with a high signal to noise ratio in all detector pixels having a galaxy association were extracted. The 170{mu}m fluxes measured from the Serendipity slews have been put on an absolute flux level by using calibration sources observed additionally with the photometric mapping mode of ISOPHOT. For all but a few galaxies, the 170{mu}m fluxes are determined for the first time, which represents a significant increase in he number of galaxies with measured Far-Infrared (FIR) fluxes beyond the IRAS 100{mu}m limit.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865#table4</TD>
            <TD>2011-09-14T20:12:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/359/865&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/865</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/1559 [1]</TD>
            <TD>Diameters of Galactic open star clusters (van den Bergh+, 2006)</TD>
            <TD>The present paper presents a tabulation of data on all 600 Galactic open clusters for which it is currently possible to calculate linear diameters. As expected, the youngest "clusters", with ages &lt;15Myr, contain a significant (&gt;=20%) admixture of associations. Among intermediate-age clusters, with ages in the range 15Myr to 1.5Gyr, the median cluster diameter is found to increase with age. Small, compact clusters are rare among objects with ages &gt;1.5Gyr. Open clusters with ages &gt;1Gyr appear to form what might be termed a "cluster thick disk", part of which consists of objects that were probably captured gravitationally by the main body of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559#1</TD>
            <TD>2011-09-14T20:11:05Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/1559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/1559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/1559 [2]</TD>
            <TD>Diameters of Galactic open star clusters (van den Bergh+, 2006)</TD>
            <TD>The present paper presents a tabulation of data on all 600 Galactic open clusters for which it is currently possible to calculate linear diameters. As expected, the youngest "clusters", with ages &lt;15Myr, contain a significant (&gt;=20%) admixture of associations. Among intermediate-age clusters, with ages in the range 15Myr to 1.5Gyr, the median cluster diameter is found to increase with age. Small, compact clusters are rare among objects with ages &gt;1.5Gyr. Open clusters with ages &gt;1Gyr appear to form what might be termed a "cluster thick disk", part of which consists of objects that were probably captured gravitationally by the main body of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559#2</TD>
            <TD>2011-09-14T20:11:05Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/1559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/1559</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/1559 [table1]</TD>
            <TD>Diameters of Galactic open star clusters (van den Bergh+, 2006)</TD>
            <TD>The present paper presents a tabulation of data on all 600 Galactic open clusters for which it is currently possible to calculate linear diameters. As expected, the youngest "clusters", with ages &lt;15Myr, contain a significant (&gt;=20%) admixture of associations. Among intermediate-age clusters, with ages in the range 15Myr to 1.5Gyr, the median cluster diameter is found to increase with age. Small, compact clusters are rare among objects with ages &gt;1.5Gyr. Open clusters with ages &gt;1Gyr appear to form what might be termed a "cluster thick disk", part of which consists of objects that were probably captured gravitationally by the main body of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559#table1</TD>
            <TD>2011-09-14T20:11:05Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/1559&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/1559</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/359/865 [1]</TD>
            <TD>ISOPHOT 170{mu}m Serendipity Survey I. (Stickel+, 2000)</TD>
            <TD>Serendipity slew survey measurements were acquired with the ISOPHOT C200 detector installed on the ISO mission. The C200 detector is a 2x2 pixel array of stressed Ge:Ga with a pixel size of 89.4arcsec, and was used in conjunction with the C160 broad-band filter (reference wavelength 170{mu}m, width 89{mu}m). During the lifetime of the ISO mission, about 550 hours of measurements have been gathered with more than 12000 slews. From the slew data with low (100{mu}m&lt;=15MJy/sr) cirrus background, 115 well-observed sources with a high signal to noise ratio in all detector pixels having a galaxy association were extracted. The 170{mu}m fluxes measured from the Serendipity slews have been put on an absolute flux level by using calibration sources observed additionally with the photometric mapping mode of ISOPHOT. For all but a few galaxies, the 170{mu}m fluxes are determined for the first time, which represents a significant increase in he number of galaxies with measured Far-Infrared (FIR) fluxes beyond the IRAS 100{mu}m limit.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865#1</TD>
            <TD>2011-09-14T20:12:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/359/865</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/865</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/359/865 [2]</TD>
            <TD>ISOPHOT 170{mu}m Serendipity Survey I. (Stickel+, 2000)</TD>
            <TD>Serendipity slew survey measurements were acquired with the ISOPHOT C200 detector installed on the ISO mission. The C200 detector is a 2x2 pixel array of stressed Ge:Ga with a pixel size of 89.4arcsec, and was used in conjunction with the C160 broad-band filter (reference wavelength 170{mu}m, width 89{mu}m). During the lifetime of the ISO mission, about 550 hours of measurements have been gathered with more than 12000 slews. From the slew data with low (100{mu}m&lt;=15MJy/sr) cirrus background, 115 well-observed sources with a high signal to noise ratio in all detector pixels having a galaxy association were extracted. The 170{mu}m fluxes measured from the Serendipity slews have been put on an absolute flux level by using calibration sources observed additionally with the photometric mapping mode of ISOPHOT. For all but a few galaxies, the 170{mu}m fluxes are determined for the first time, which represents a significant increase in he number of galaxies with measured Far-Infrared (FIR) fluxes beyond the IRAS 100{mu}m limit.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865#2</TD>
            <TD>2011-09-14T20:12:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/359/865&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/865</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/359/865 [table4]</TD>
            <TD>ISOPHOT 170{mu}m Serendipity Survey I. (Stickel+, 2000)</TD>
            <TD>Serendipity slew survey measurements were acquired with the ISOPHOT C200 detector installed on the ISO mission. The C200 detector is a 2x2 pixel array of stressed Ge:Ga with a pixel size of 89.4arcsec, and was used in conjunction with the C160 broad-band filter (reference wavelength 170{mu}m, width 89{mu}m). During the lifetime of the ISO mission, about 550 hours of measurements have been gathered with more than 12000 slews. From the slew data with low (100{mu}m&lt;=15MJy/sr) cirrus background, 115 well-observed sources with a high signal to noise ratio in all detector pixels having a galaxy association were extracted. The 170{mu}m fluxes measured from the Serendipity slews have been put on an absolute flux level by using calibration sources observed additionally with the photometric mapping mode of ISOPHOT. For all but a few galaxies, the 170{mu}m fluxes are determined for the first time, which represents a significant increase in he number of galaxies with measured Far-Infrared (FIR) fluxes beyond the IRAS 100{mu}m limit.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865#table4</TD>
            <TD>2011-09-14T20:12:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/865</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/359/865&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/865</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/467/1025 [1]</TD>
            <TD>JHK photometry of Fornax red giant branch (Gullieuszik+, 2007)</TD>
            <TD>The catalogues of the upper red giant branch stars in Fornax dwarf Spheroidal galaxy are obtained from ground-based SOFI@NTT observations. The shallow catalogue is obtained from a mosaic of 16 SOFI fields and covers an area of 18.5x18.5arcmin. The deep catalogue covers an area of 4.5x4.5arcmin.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025#1</TD>
            <TD>2011-09-14T20:13:33Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/467/1025</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1025</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/467/1025 [2]</TD>
            <TD>JHK photometry of Fornax red giant branch (Gullieuszik+, 2007)</TD>
            <TD>The catalogues of the upper red giant branch stars in Fornax dwarf Spheroidal galaxy are obtained from ground-based SOFI@NTT observations. The shallow catalogue is obtained from a mosaic of 16 SOFI fields and covers an area of 18.5x18.5arcmin. The deep catalogue covers an area of 4.5x4.5arcmin.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025#2</TD>
            <TD>2011-09-14T20:13:33Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/467/1025&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1025</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/467/1025 [fornax]</TD>
            <TD>JHK photometry of Fornax red giant branch (Gullieuszik+, 2007)</TD>
            <TD>The catalogues of the upper red giant branch stars in Fornax dwarf Spheroidal galaxy are obtained from ground-based SOFI@NTT observations. The shallow catalogue is obtained from a mosaic of 16 SOFI fields and covers an area of 18.5x18.5arcmin. The deep catalogue covers an area of 4.5x4.5arcmin.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025#fornax</TD>
            <TD>2011-09-14T20:13:33Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/467/1025&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1025</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/1559 [1]</TD>
            <TD>Diameters of Galactic open star clusters (van den Bergh+, 2006)</TD>
            <TD>The present paper presents a tabulation of data on all 600 Galactic open clusters for which it is currently possible to calculate linear diameters. As expected, the youngest "clusters", with ages &lt;15Myr, contain a significant (&gt;=20%) admixture of associations. Among intermediate-age clusters, with ages in the range 15Myr to 1.5Gyr, the median cluster diameter is found to increase with age. Small, compact clusters are rare among objects with ages &gt;1.5Gyr. Open clusters with ages &gt;1Gyr appear to form what might be termed a "cluster thick disk", part of which consists of objects that were probably captured gravitationally by the main body of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559#1</TD>
            <TD>2011-09-14T20:11:05Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/1559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/1559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/1559 [2]</TD>
            <TD>Diameters of Galactic open star clusters (van den Bergh+, 2006)</TD>
            <TD>The present paper presents a tabulation of data on all 600 Galactic open clusters for which it is currently possible to calculate linear diameters. As expected, the youngest "clusters", with ages &lt;15Myr, contain a significant (&gt;=20%) admixture of associations. Among intermediate-age clusters, with ages in the range 15Myr to 1.5Gyr, the median cluster diameter is found to increase with age. Small, compact clusters are rare among objects with ages &gt;1.5Gyr. Open clusters with ages &gt;1Gyr appear to form what might be termed a "cluster thick disk", part of which consists of objects that were probably captured gravitationally by the main body of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559#2</TD>
            <TD>2011-09-14T20:11:05Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/1559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/1559</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/1559 [table1]</TD>
            <TD>Diameters of Galactic open star clusters (van den Bergh+, 2006)</TD>
            <TD>The present paper presents a tabulation of data on all 600 Galactic open clusters for which it is currently possible to calculate linear diameters. As expected, the youngest "clusters", with ages &lt;15Myr, contain a significant (&gt;=20%) admixture of associations. Among intermediate-age clusters, with ages in the range 15Myr to 1.5Gyr, the median cluster diameter is found to increase with age. Small, compact clusters are rare among objects with ages &gt;1.5Gyr. Open clusters with ages &gt;1Gyr appear to form what might be termed a "cluster thick disk", part of which consists of objects that were probably captured gravitationally by the main body of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559#table1</TD>
            <TD>2011-09-14T20:11:05Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/1559&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/1559</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/449/461 [1]</TD>
            <TD>Radial velocities in A2744 (Boschin+, 2006)</TD>
            <TD>Spectroscopic redshifts for 102 galaxies in the central region of the galaxy cluster Abell 2744 are presented. For each galaxy equatorial coordinates and radial velocity are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461#1</TD>
            <TD>2011-09-14T19:53:52Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/449/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/449/461 [2]</TD>
            <TD>Radial velocities in A2744 (Boschin+, 2006)</TD>
            <TD>Spectroscopic redshifts for 102 galaxies in the central region of the galaxy cluster Abell 2744 are presented. For each galaxy equatorial coordinates and radial velocity are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461#2</TD>
            <TD>2011-09-14T19:53:52Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/449/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/449/461 [table1]</TD>
            <TD>Radial velocities in A2744 (Boschin+, 2006)</TD>
            <TD>Spectroscopic redshifts for 102 galaxies in the central region of the galaxy cluster Abell 2744 are presented. For each galaxy equatorial coordinates and radial velocity are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461#table1</TD>
            <TD>2011-09-14T19:53:52Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/449/461&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/461</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/467/1025 [1]</TD>
            <TD>JHK photometry of Fornax red giant branch (Gullieuszik+, 2007)</TD>
            <TD>The catalogues of the upper red giant branch stars in Fornax dwarf Spheroidal galaxy are obtained from ground-based SOFI@NTT observations. The shallow catalogue is obtained from a mosaic of 16 SOFI fields and covers an area of 18.5x18.5arcmin. The deep catalogue covers an area of 4.5x4.5arcmin.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025#1</TD>
            <TD>2011-09-14T20:13:33Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/467/1025</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1025</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/467/1025 [2]</TD>
            <TD>JHK photometry of Fornax red giant branch (Gullieuszik+, 2007)</TD>
            <TD>The catalogues of the upper red giant branch stars in Fornax dwarf Spheroidal galaxy are obtained from ground-based SOFI@NTT observations. The shallow catalogue is obtained from a mosaic of 16 SOFI fields and covers an area of 18.5x18.5arcmin. The deep catalogue covers an area of 4.5x4.5arcmin.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025#2</TD>
            <TD>2011-09-14T20:13:33Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/467/1025&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1025</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/467/1025 [fornax]</TD>
            <TD>JHK photometry of Fornax red giant branch (Gullieuszik+, 2007)</TD>
            <TD>The catalogues of the upper red giant branch stars in Fornax dwarf Spheroidal galaxy are obtained from ground-based SOFI@NTT observations. The shallow catalogue is obtained from a mosaic of 16 SOFI fields and covers an area of 18.5x18.5arcmin. The deep catalogue covers an area of 4.5x4.5arcmin.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025#fornax</TD>
            <TD>2011-09-14T20:13:33Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/467/1025&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1025</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/62 [1]</TD>
            <TD>Catalog of double nucleus disk galaxies (Gimeno+, 2004)</TD>
            <TD>We have compiled a catalog of disk galaxies that have a double nucleus, through systematic examination of existing catalogs and publications. The Catalog of Double Nucleus Disk Galaxies includes 107 objects, together with their basic data. The aim of the catalog is to provide a more systematic and homogeneous basis for the study of the relevance of galaxy interactions and minor mergers in the formation of these double nuclei. We have also investigated possible correlations between geometric and photometric parameters of the double nuclei and their host galaxies. The preliminary results indicate the presence of several significant correlations that should be considered in any theoretical scenario describing minor mergers and disk galaxy evolution</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62#1</TD>
            <TD>2011-09-14T20:02:48Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/62</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/62</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/62 [2]</TD>
            <TD>Catalog of double nucleus disk galaxies (Gimeno+, 2004)</TD>
            <TD>We have compiled a catalog of disk galaxies that have a double nucleus, through systematic examination of existing catalogs and publications. The Catalog of Double Nucleus Disk Galaxies includes 107 objects, together with their basic data. The aim of the catalog is to provide a more systematic and homogeneous basis for the study of the relevance of galaxy interactions and minor mergers in the formation of these double nuclei. We have also investigated possible correlations between geometric and photometric parameters of the double nuclei and their host galaxies. The preliminary results indicate the presence of several significant correlations that should be considered in any theoretical scenario describing minor mergers and disk galaxy evolution</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62#2</TD>
            <TD>2011-09-14T20:02:48Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/62&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/62 [table1]</TD>
            <TD>Catalog of double nucleus disk galaxies (Gimeno+, 2004)</TD>
            <TD>We have compiled a catalog of disk galaxies that have a double nucleus, through systematic examination of existing catalogs and publications. The Catalog of Double Nucleus Disk Galaxies includes 107 objects, together with their basic data. The aim of the catalog is to provide a more systematic and homogeneous basis for the study of the relevance of galaxy interactions and minor mergers in the formation of these double nuclei. We have also investigated possible correlations between geometric and photometric parameters of the double nuclei and their host galaxies. The preliminary results indicate the presence of several significant correlations that should be considered in any theoretical scenario describing minor mergers and disk galaxy evolution</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62#table1</TD>
            <TD>2011-09-14T20:02:48Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/62</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/1559 [1]</TD>
            <TD>Diameters of Galactic open star clusters (van den Bergh+, 2006)</TD>
            <TD>The present paper presents a tabulation of data on all 600 Galactic open clusters for which it is currently possible to calculate linear diameters. As expected, the youngest "clusters", with ages &lt;15Myr, contain a significant (&gt;=20%) admixture of associations. Among intermediate-age clusters, with ages in the range 15Myr to 1.5Gyr, the median cluster diameter is found to increase with age. Small, compact clusters are rare among objects with ages &gt;1.5Gyr. Open clusters with ages &gt;1Gyr appear to form what might be termed a "cluster thick disk", part of which consists of objects that were probably captured gravitationally by the main body of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559#1</TD>
            <TD>2011-09-14T20:11:05Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/1559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/1559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/1559 [2]</TD>
            <TD>Diameters of Galactic open star clusters (van den Bergh+, 2006)</TD>
            <TD>The present paper presents a tabulation of data on all 600 Galactic open clusters for which it is currently possible to calculate linear diameters. As expected, the youngest "clusters", with ages &lt;15Myr, contain a significant (&gt;=20%) admixture of associations. Among intermediate-age clusters, with ages in the range 15Myr to 1.5Gyr, the median cluster diameter is found to increase with age. Small, compact clusters are rare among objects with ages &gt;1.5Gyr. Open clusters with ages &gt;1Gyr appear to form what might be termed a "cluster thick disk", part of which consists of objects that were probably captured gravitationally by the main body of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559#2</TD>
            <TD>2011-09-14T20:11:05Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/1559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/1559</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/1559 [table1]</TD>
            <TD>Diameters of Galactic open star clusters (van den Bergh+, 2006)</TD>
            <TD>The present paper presents a tabulation of data on all 600 Galactic open clusters for which it is currently possible to calculate linear diameters. As expected, the youngest "clusters", with ages &lt;15Myr, contain a significant (&gt;=20%) admixture of associations. Among intermediate-age clusters, with ages in the range 15Myr to 1.5Gyr, the median cluster diameter is found to increase with age. Small, compact clusters are rare among objects with ages &gt;1.5Gyr. Open clusters with ages &gt;1Gyr appear to form what might be termed a "cluster thick disk", part of which consists of objects that were probably captured gravitationally by the main body of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559#table1</TD>
            <TD>2011-09-14T20:11:05Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/1559</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/1559&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/1559</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/449/461 [1]</TD>
            <TD>Radial velocities in A2744 (Boschin+, 2006)</TD>
            <TD>Spectroscopic redshifts for 102 galaxies in the central region of the galaxy cluster Abell 2744 are presented. For each galaxy equatorial coordinates and radial velocity are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461#1</TD>
            <TD>2011-09-14T19:53:52Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/449/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/449/461 [2]</TD>
            <TD>Radial velocities in A2744 (Boschin+, 2006)</TD>
            <TD>Spectroscopic redshifts for 102 galaxies in the central region of the galaxy cluster Abell 2744 are presented. For each galaxy equatorial coordinates and radial velocity are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461#2</TD>
            <TD>2011-09-14T19:53:52Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/449/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/449/461 [table1]</TD>
            <TD>Radial velocities in A2744 (Boschin+, 2006)</TD>
            <TD>Spectroscopic redshifts for 102 galaxies in the central region of the galaxy cluster Abell 2744 are presented. For each galaxy equatorial coordinates and radial velocity are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461#table1</TD>
            <TD>2011-09-14T19:53:52Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/449/461&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/461</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/467/1025 [1]</TD>
            <TD>JHK photometry of Fornax red giant branch (Gullieuszik+, 2007)</TD>
            <TD>The catalogues of the upper red giant branch stars in Fornax dwarf Spheroidal galaxy are obtained from ground-based SOFI@NTT observations. The shallow catalogue is obtained from a mosaic of 16 SOFI fields and covers an area of 18.5x18.5arcmin. The deep catalogue covers an area of 4.5x4.5arcmin.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025#1</TD>
            <TD>2011-09-14T20:13:33Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/467/1025</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1025</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/467/1025 [2]</TD>
            <TD>JHK photometry of Fornax red giant branch (Gullieuszik+, 2007)</TD>
            <TD>The catalogues of the upper red giant branch stars in Fornax dwarf Spheroidal galaxy are obtained from ground-based SOFI@NTT observations. The shallow catalogue is obtained from a mosaic of 16 SOFI fields and covers an area of 18.5x18.5arcmin. The deep catalogue covers an area of 4.5x4.5arcmin.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025#2</TD>
            <TD>2011-09-14T20:13:33Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/467/1025&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1025</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/467/1025 [fornax]</TD>
            <TD>JHK photometry of Fornax red giant branch (Gullieuszik+, 2007)</TD>
            <TD>The catalogues of the upper red giant branch stars in Fornax dwarf Spheroidal galaxy are obtained from ground-based SOFI@NTT observations. The shallow catalogue is obtained from a mosaic of 16 SOFI fields and covers an area of 18.5x18.5arcmin. The deep catalogue covers an area of 4.5x4.5arcmin.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025#fornax</TD>
            <TD>2011-09-14T20:13:33Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/1025</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/467/1025&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/1025</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/166/549 [1]</TD>
            <TD>HST/ACS observations of NGC 346 (Gouliermis+, 2006)</TD>
            <TD>We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V~11 to V~28 mag, including all stellar types from the most massive young stars to faint lower main-sequence and pre-main-sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: the stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete stellar sample of a field about 5'×5' around the most active star-forming region in this galaxy. Considering the importance of these data for various investigations in the area, we provide the full stellar catalog from our photometry. This paper is the first part of an ongoing study to investigate in detail the two dominant stellar systems in the area and their surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549#1</TD>
            <TD>2011-09-14T20:03:06Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/166/549</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/166/549</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/166/549 [2]</TD>
            <TD>HST/ACS observations of NGC 346 (Gouliermis+, 2006)</TD>
            <TD>We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V~11 to V~28 mag, including all stellar types from the most massive young stars to faint lower main-sequence and pre-main-sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: the stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete stellar sample of a field about 5'×5' around the most active star-forming region in this galaxy. Considering the importance of these data for various investigations in the area, we provide the full stellar catalog from our photometry. This paper is the first part of an ongoing study to investigate in detail the two dominant stellar systems in the area and their surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549#2</TD>
            <TD>2011-09-14T20:03:06Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/166/549&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/166/549</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/166/549 [table2]</TD>
            <TD>HST/ACS observations of NGC 346 (Gouliermis+, 2006)</TD>
            <TD>We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V~11 to V~28 mag, including all stellar types from the most massive young stars to faint lower main-sequence and pre-main-sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: the stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete stellar sample of a field about 5'×5' around the most active star-forming region in this galaxy. Considering the importance of these data for various investigations in the area, we provide the full stellar catalog from our photometry. This paper is the first part of an ongoing study to investigate in detail the two dominant stellar systems in the area and their surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549#table2</TD>
            <TD>2011-09-14T20:03:06Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/166/549&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/166/549</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/449/461 [1]</TD>
            <TD>Radial velocities in A2744 (Boschin+, 2006)</TD>
            <TD>Spectroscopic redshifts for 102 galaxies in the central region of the galaxy cluster Abell 2744 are presented. For each galaxy equatorial coordinates and radial velocity are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461#1</TD>
            <TD>2011-09-14T19:53:52Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/449/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/449/461 [2]</TD>
            <TD>Radial velocities in A2744 (Boschin+, 2006)</TD>
            <TD>Spectroscopic redshifts for 102 galaxies in the central region of the galaxy cluster Abell 2744 are presented. For each galaxy equatorial coordinates and radial velocity are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461#2</TD>
            <TD>2011-09-14T19:53:52Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/449/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/449/461 [table1]</TD>
            <TD>Radial velocities in A2744 (Boschin+, 2006)</TD>
            <TD>Spectroscopic redshifts for 102 galaxies in the central region of the galaxy cluster Abell 2744 are presented. For each galaxy equatorial coordinates and radial velocity are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461#table1</TD>
            <TD>2011-09-14T19:53:52Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/449/461</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/449/461&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/449/461</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/468/937 [1]</TD>
            <TD>K-band AO imaging in COSMOS deep field (Huertas-Company+, 2007)</TD>
            <TD>We present the results of an imaging program of distant galaxies (z~0.8) at high spatial resolution (~0.1") aiming at studying their morphological evolution. We observed 7 fields of 1'x1' with the NACO Adaptive Optics system (VLT) in Ks (2.16{mu}m) band with typical V~14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area, in which multi-wavelength photometric and spectroscopic observations are ongoing. High angular-resolution K-band data have the advantage of probing old stellar populations in the rest-frame, enabling a determination of galaxy morphological types unaffected by recent star formation, which are more closely linked to the underlying mass than classical optical morphology studies (HST). Adaptive optics on ground based telescopes is the only method today for obtaining such a high resolution in the K-band, but it suffers from limitations since only small fields are observable and long integration times are necessary.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937#1</TD>
            <TD>2011-09-14T20:14:17Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/468/937</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/937</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/468/937 [2]</TD>
            <TD>K-band AO imaging in COSMOS deep field (Huertas-Company+, 2007)</TD>
            <TD>We present the results of an imaging program of distant galaxies (z~0.8) at high spatial resolution (~0.1") aiming at studying their morphological evolution. We observed 7 fields of 1'x1' with the NACO Adaptive Optics system (VLT) in Ks (2.16{mu}m) band with typical V~14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area, in which multi-wavelength photometric and spectroscopic observations are ongoing. High angular-resolution K-band data have the advantage of probing old stellar populations in the rest-frame, enabling a determination of galaxy morphological types unaffected by recent star formation, which are more closely linked to the underlying mass than classical optical morphology studies (HST). Adaptive optics on ground based telescopes is the only method today for obtaining such a high resolution in the K-band, but it suffers from limitations since only small fields are observable and long integration times are necessary.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937#2</TD>
            <TD>2011-09-14T20:14:17Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/468/937&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/937</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/468/937 [table6]</TD>
            <TD>K-band AO imaging in COSMOS deep field (Huertas-Company+, 2007)</TD>
            <TD>We present the results of an imaging program of distant galaxies (z~0.8) at high spatial resolution (~0.1") aiming at studying their morphological evolution. We observed 7 fields of 1'x1' with the NACO Adaptive Optics system (VLT) in Ks (2.16{mu}m) band with typical V~14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area, in which multi-wavelength photometric and spectroscopic observations are ongoing. High angular-resolution K-band data have the advantage of probing old stellar populations in the rest-frame, enabling a determination of galaxy morphological types unaffected by recent star formation, which are more closely linked to the underlying mass than classical optical morphology studies (HST). Adaptive optics on ground based telescopes is the only method today for obtaining such a high resolution in the K-band, but it suffers from limitations since only small fields are observable and long integration times are necessary.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937#table6</TD>
            <TD>2011-09-14T20:14:17Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/468/937&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/937</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/166/549 [1]</TD>
            <TD>HST/ACS observations of NGC 346 (Gouliermis+, 2006)</TD>
            <TD>We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V~11 to V~28 mag, including all stellar types from the most massive young stars to faint lower main-sequence and pre-main-sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: the stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete stellar sample of a field about 5'×5' around the most active star-forming region in this galaxy. Considering the importance of these data for various investigations in the area, we provide the full stellar catalog from our photometry. This paper is the first part of an ongoing study to investigate in detail the two dominant stellar systems in the area and their surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549#1</TD>
            <TD>2011-09-14T20:03:06Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/166/549</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/166/549</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/166/549 [2]</TD>
            <TD>HST/ACS observations of NGC 346 (Gouliermis+, 2006)</TD>
            <TD>We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V~11 to V~28 mag, including all stellar types from the most massive young stars to faint lower main-sequence and pre-main-sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: the stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete stellar sample of a field about 5'×5' around the most active star-forming region in this galaxy. Considering the importance of these data for various investigations in the area, we provide the full stellar catalog from our photometry. This paper is the first part of an ongoing study to investigate in detail the two dominant stellar systems in the area and their surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549#2</TD>
            <TD>2011-09-14T20:03:06Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/166/549&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/166/549</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/166/549 [table2]</TD>
            <TD>HST/ACS observations of NGC 346 (Gouliermis+, 2006)</TD>
            <TD>We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V~11 to V~28 mag, including all stellar types from the most massive young stars to faint lower main-sequence and pre-main-sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: the stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete stellar sample of a field about 5'×5' around the most active star-forming region in this galaxy. Considering the importance of these data for various investigations in the area, we provide the full stellar catalog from our photometry. This paper is the first part of an ongoing study to investigate in detail the two dominant stellar systems in the area and their surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549#table2</TD>
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            <TD>#Open_Clusters#</TD>
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            <TD>#Research#</TD>
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            <TD>17-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/166/549&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/166/549</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/360/1305 [1]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#1</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/360/1305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/360/1305 [2]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#2</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/360/1305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/360/1305 [table6]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#table6</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/360/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/360/1305 [param]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#param</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/360/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/468/937 [1]</TD>
            <TD>K-band AO imaging in COSMOS deep field (Huertas-Company+, 2007)</TD>
            <TD>We present the results of an imaging program of distant galaxies (z~0.8) at high spatial resolution (~0.1") aiming at studying their morphological evolution. We observed 7 fields of 1'x1' with the NACO Adaptive Optics system (VLT) in Ks (2.16{mu}m) band with typical V~14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area, in which multi-wavelength photometric and spectroscopic observations are ongoing. High angular-resolution K-band data have the advantage of probing old stellar populations in the rest-frame, enabling a determination of galaxy morphological types unaffected by recent star formation, which are more closely linked to the underlying mass than classical optical morphology studies (HST). Adaptive optics on ground based telescopes is the only method today for obtaining such a high resolution in the K-band, but it suffers from limitations since only small fields are observable and long integration times are necessary.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937#1</TD>
            <TD>2011-09-14T20:14:17Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/468/937</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/937</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/468/937 [2]</TD>
            <TD>K-band AO imaging in COSMOS deep field (Huertas-Company+, 2007)</TD>
            <TD>We present the results of an imaging program of distant galaxies (z~0.8) at high spatial resolution (~0.1") aiming at studying their morphological evolution. We observed 7 fields of 1'x1' with the NACO Adaptive Optics system (VLT) in Ks (2.16{mu}m) band with typical V~14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area, in which multi-wavelength photometric and spectroscopic observations are ongoing. High angular-resolution K-band data have the advantage of probing old stellar populations in the rest-frame, enabling a determination of galaxy morphological types unaffected by recent star formation, which are more closely linked to the underlying mass than classical optical morphology studies (HST). Adaptive optics on ground based telescopes is the only method today for obtaining such a high resolution in the K-band, but it suffers from limitations since only small fields are observable and long integration times are necessary.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937#2</TD>
            <TD>2011-09-14T20:14:17Z</TD>
            <TD>#Photometry#Galaxies#</TD>
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            <TD />
            <TD>03-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/468/937&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/937</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/468/937 [table6]</TD>
            <TD>K-band AO imaging in COSMOS deep field (Huertas-Company+, 2007)</TD>
            <TD>We present the results of an imaging program of distant galaxies (z~0.8) at high spatial resolution (~0.1") aiming at studying their morphological evolution. We observed 7 fields of 1'x1' with the NACO Adaptive Optics system (VLT) in Ks (2.16{mu}m) band with typical V~14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area, in which multi-wavelength photometric and spectroscopic observations are ongoing. High angular-resolution K-band data have the advantage of probing old stellar populations in the rest-frame, enabling a determination of galaxy morphological types unaffected by recent star formation, which are more closely linked to the underlying mass than classical optical morphology studies (HST). Adaptive optics on ground based telescopes is the only method today for obtaining such a high resolution in the K-band, but it suffers from limitations since only small fields are observable and long integration times are necessary.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937#table6</TD>
            <TD>2011-09-14T20:14:17Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/468/937&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/937</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/166/549 [1]</TD>
            <TD>HST/ACS observations of NGC 346 (Gouliermis+, 2006)</TD>
            <TD>We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V~11 to V~28 mag, including all stellar types from the most massive young stars to faint lower main-sequence and pre-main-sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: the stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete stellar sample of a field about 5'×5' around the most active star-forming region in this galaxy. Considering the importance of these data for various investigations in the area, we provide the full stellar catalog from our photometry. This paper is the first part of an ongoing study to investigate in detail the two dominant stellar systems in the area and their surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549#1</TD>
            <TD>2011-09-14T20:03:06Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/166/549</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/166/549</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/166/549 [2]</TD>
            <TD>HST/ACS observations of NGC 346 (Gouliermis+, 2006)</TD>
            <TD>We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V~11 to V~28 mag, including all stellar types from the most massive young stars to faint lower main-sequence and pre-main-sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: the stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete stellar sample of a field about 5'×5' around the most active star-forming region in this galaxy. Considering the importance of these data for various investigations in the area, we provide the full stellar catalog from our photometry. This paper is the first part of an ongoing study to investigate in detail the two dominant stellar systems in the area and their surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549#2</TD>
            <TD>2011-09-14T20:03:06Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/166/549&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/166/549</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/166/549 [table2]</TD>
            <TD>HST/ACS observations of NGC 346 (Gouliermis+, 2006)</TD>
            <TD>We present a photometric study of the star-forming region NGC 346 and its surrounding field in the Small Magellanic Cloud, using data taken with the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST). The data set contains both short and long exposures for increased dynamic range, and photometry was performed using the ACS module of the stellar photometry package DOLPHOT. We detected almost 100,000 stars over a magnitude range of V~11 to V~28 mag, including all stellar types from the most massive young stars to faint lower main-sequence and pre-main-sequence stars. We find that this region, which is characterized by a plethora of stellar systems and interesting objects, is an outstanding example of mixed stellar populations. We take into account different features of the color-magnitude diagram of all the detected stars to distinguish the two dominant stellar systems: the stellar association NGC 346 and the old spherical star cluster BS 90. These observations provide a complete stellar sample of a field about 5'×5' around the most active star-forming region in this galaxy. Considering the importance of these data for various investigations in the area, we provide the full stellar catalog from our photometry. This paper is the first part of an ongoing study to investigate in detail the two dominant stellar systems in the area and their surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549#table2</TD>
            <TD>2011-09-14T20:03:06Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/166/549</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/166/549&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/166/549</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/468/937 [1]</TD>
            <TD>K-band AO imaging in COSMOS deep field (Huertas-Company+, 2007)</TD>
            <TD>We present the results of an imaging program of distant galaxies (z~0.8) at high spatial resolution (~0.1") aiming at studying their morphological evolution. We observed 7 fields of 1'x1' with the NACO Adaptive Optics system (VLT) in Ks (2.16{mu}m) band with typical V~14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area, in which multi-wavelength photometric and spectroscopic observations are ongoing. High angular-resolution K-band data have the advantage of probing old stellar populations in the rest-frame, enabling a determination of galaxy morphological types unaffected by recent star formation, which are more closely linked to the underlying mass than classical optical morphology studies (HST). Adaptive optics on ground based telescopes is the only method today for obtaining such a high resolution in the K-band, but it suffers from limitations since only small fields are observable and long integration times are necessary.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937#1</TD>
            <TD>2011-09-14T20:14:17Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/468/937</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/937</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/468/937 [2]</TD>
            <TD>K-band AO imaging in COSMOS deep field (Huertas-Company+, 2007)</TD>
            <TD>We present the results of an imaging program of distant galaxies (z~0.8) at high spatial resolution (~0.1") aiming at studying their morphological evolution. We observed 7 fields of 1'x1' with the NACO Adaptive Optics system (VLT) in Ks (2.16{mu}m) band with typical V~14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area, in which multi-wavelength photometric and spectroscopic observations are ongoing. High angular-resolution K-band data have the advantage of probing old stellar populations in the rest-frame, enabling a determination of galaxy morphological types unaffected by recent star formation, which are more closely linked to the underlying mass than classical optical morphology studies (HST). Adaptive optics on ground based telescopes is the only method today for obtaining such a high resolution in the K-band, but it suffers from limitations since only small fields are observable and long integration times are necessary.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937#2</TD>
            <TD>2011-09-14T20:14:17Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/468/937&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/937</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/468/937 [table6]</TD>
            <TD>K-band AO imaging in COSMOS deep field (Huertas-Company+, 2007)</TD>
            <TD>We present the results of an imaging program of distant galaxies (z~0.8) at high spatial resolution (~0.1") aiming at studying their morphological evolution. We observed 7 fields of 1'x1' with the NACO Adaptive Optics system (VLT) in Ks (2.16{mu}m) band with typical V~14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area, in which multi-wavelength photometric and spectroscopic observations are ongoing. High angular-resolution K-band data have the advantage of probing old stellar populations in the rest-frame, enabling a determination of galaxy morphological types unaffected by recent star formation, which are more closely linked to the underlying mass than classical optical morphology studies (HST). Adaptive optics on ground based telescopes is the only method today for obtaining such a high resolution in the K-band, but it suffers from limitations since only small fields are observable and long integration times are necessary.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937#table6</TD>
            <TD>2011-09-14T20:14:17Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/937</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/468/937&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/937</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/360/1305 [1]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#1</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/360/1305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/360/1305 [2]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#2</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/360/1305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/360/1305 [table6]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#table6</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/360/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/360/1305 [param]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#param</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/360/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/468/807 [1]</TD>
            <TD>Redshifts of galaxies associated with X emission (Mannucci+, 2007)</TD>
            <TD>List of the target galaxies observed with the WHT/AF2/WYFOOS and TNG/DOLORES multi-object spectrographs. For each galaxy, the coordinates, the R-band magnitude, the spectroscopic redshift and the spectral classification are given. Target galaxies have been selected to have R-band magnitudes between 20.0 and 21.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807#1</TD>
            <TD>2011-09-14T20:11:23Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/468/807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/468/807 [2]</TD>
            <TD>Redshifts of galaxies associated with X emission (Mannucci+, 2007)</TD>
            <TD>List of the target galaxies observed with the WHT/AF2/WYFOOS and TNG/DOLORES multi-object spectrographs. For each galaxy, the coordinates, the R-band magnitude, the spectroscopic redshift and the spectral classification are given. Target galaxies have been selected to have R-band magnitudes between 20.0 and 21.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807#2</TD>
            <TD>2011-09-14T20:11:23Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/468/807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/807</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/468/807 [table2]</TD>
            <TD>Redshifts of galaxies associated with X emission (Mannucci+, 2007)</TD>
            <TD>List of the target galaxies observed with the WHT/AF2/WYFOOS and TNG/DOLORES multi-object spectrographs. For each galaxy, the coordinates, the R-band magnitude, the spectroscopic redshift and the spectral classification are given. Target galaxies have been selected to have R-band magnitudes between 20.0 and 21.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807#table2</TD>
            <TD>2011-09-14T20:11:23Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/468/807&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AcA/51/221 [1]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#1</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AcA/51/221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AcA/51/221 [2]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#2</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AcA/51/221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/51/221 [ic1613]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#ic1613</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/51/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/51/221 [table1]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#table1</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/51/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/463/503 [1]</TD>
            <TD>Early-type dwarf galaxies in Fornax cluster (Mieske+, 2007)</TD>
            <TD>Total V-band magnitude, central V-band surface brightness, and V-I colour is presented for a sample of 100 dwarf elliptical galaxy candidates in the central Fornax cluster. We also give the cluster membership flag assigned to each galaxy, based upon distance measurements obtained with the SBF method and on morphological assessment. For most of the sources, the photometric parameters are derived from imaging with the IMACS instrument at the Magellan telescope on Las Campanas Observatory. For some fainter sources the photometric parameters were derived from imaging with the WFCCD camera at the 2.5m du Pont telescope on Las Campanas Observatory. Those sources are specifically indicated in the comments column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503#1</TD>
            <TD>2011-09-14T20:04:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/463/503</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/503</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/463/503 [2]</TD>
            <TD>Early-type dwarf galaxies in Fornax cluster (Mieske+, 2007)</TD>
            <TD>Total V-band magnitude, central V-band surface brightness, and V-I colour is presented for a sample of 100 dwarf elliptical galaxy candidates in the central Fornax cluster. We also give the cluster membership flag assigned to each galaxy, based upon distance measurements obtained with the SBF method and on morphological assessment. For most of the sources, the photometric parameters are derived from imaging with the IMACS instrument at the Magellan telescope on Las Campanas Observatory. For some fainter sources the photometric parameters were derived from imaging with the WFCCD camera at the 2.5m du Pont telescope on Las Campanas Observatory. Those sources are specifically indicated in the comments column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503#2</TD>
            <TD>2011-09-14T20:04:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/463/503&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/503</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/463/503 [table1]</TD>
            <TD>Early-type dwarf galaxies in Fornax cluster (Mieske+, 2007)</TD>
            <TD>Total V-band magnitude, central V-band surface brightness, and V-I colour is presented for a sample of 100 dwarf elliptical galaxy candidates in the central Fornax cluster. We also give the cluster membership flag assigned to each galaxy, based upon distance measurements obtained with the SBF method and on morphological assessment. For most of the sources, the photometric parameters are derived from imaging with the IMACS instrument at the Magellan telescope on Las Campanas Observatory. For some fainter sources the photometric parameters were derived from imaging with the WFCCD camera at the 2.5m du Pont telescope on Las Campanas Observatory. Those sources are specifically indicated in the comments column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503#table1</TD>
            <TD>2011-09-14T20:04:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/463/503&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/503</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/360/1305 [1]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#1</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/360/1305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/360/1305 [2]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#2</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/360/1305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/360/1305 [table6]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#table6</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/360/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/360/1305 [param]</TD>
            <TD>Polarization of extragalactic sources (Roy+, 2005)</TD>
            <TD>We have observed a sample of 64 small-diameter sources towards the central -6&lt;l&lt;6, -2&lt;b&lt;2 of the Galaxy with the aim of studying the Faraday rotation measure near the Galactic Centre region. All the sources were observed at 6- and 3.6-cm wavelengths using the ATCA and the VLA. 59 of these sources are inferred to be extragalactic. The observations presented here constitute the first systematic study of the radio polarization properties of the background sources towards this direction and increase the number of known extragalactic radio sources in this part of the sky by almost an order of magnitude. Based on the morphology, spectral indices and lack of polarized emission, we identify four Galactic HII regions in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305#param</TD>
            <TD>2011-09-14T19:54:56Z</TD>
            <TD>#Polarization#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/360/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/360/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/360/1305</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AcA/51/221 [1]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#1</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AcA/51/221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AcA/51/221 [2]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#2</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AcA/51/221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/51/221 [ic1613]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#ic1613</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/51/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/51/221 [table1]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#table1</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/51/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/463/503 [1]</TD>
            <TD>Early-type dwarf galaxies in Fornax cluster (Mieske+, 2007)</TD>
            <TD>Total V-band magnitude, central V-band surface brightness, and V-I colour is presented for a sample of 100 dwarf elliptical galaxy candidates in the central Fornax cluster. We also give the cluster membership flag assigned to each galaxy, based upon distance measurements obtained with the SBF method and on morphological assessment. For most of the sources, the photometric parameters are derived from imaging with the IMACS instrument at the Magellan telescope on Las Campanas Observatory. For some fainter sources the photometric parameters were derived from imaging with the WFCCD camera at the 2.5m du Pont telescope on Las Campanas Observatory. Those sources are specifically indicated in the comments column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503#1</TD>
            <TD>2011-09-14T20:04:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/463/503</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/503</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/463/503 [2]</TD>
            <TD>Early-type dwarf galaxies in Fornax cluster (Mieske+, 2007)</TD>
            <TD>Total V-band magnitude, central V-band surface brightness, and V-I colour is presented for a sample of 100 dwarf elliptical galaxy candidates in the central Fornax cluster. We also give the cluster membership flag assigned to each galaxy, based upon distance measurements obtained with the SBF method and on morphological assessment. For most of the sources, the photometric parameters are derived from imaging with the IMACS instrument at the Magellan telescope on Las Campanas Observatory. For some fainter sources the photometric parameters were derived from imaging with the WFCCD camera at the 2.5m du Pont telescope on Las Campanas Observatory. Those sources are specifically indicated in the comments column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503#2</TD>
            <TD>2011-09-14T20:04:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/463/503&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/503</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/463/503 [table1]</TD>
            <TD>Early-type dwarf galaxies in Fornax cluster (Mieske+, 2007)</TD>
            <TD>Total V-band magnitude, central V-band surface brightness, and V-I colour is presented for a sample of 100 dwarf elliptical galaxy candidates in the central Fornax cluster. We also give the cluster membership flag assigned to each galaxy, based upon distance measurements obtained with the SBF method and on morphological assessment. For most of the sources, the photometric parameters are derived from imaging with the IMACS instrument at the Magellan telescope on Las Campanas Observatory. For some fainter sources the photometric parameters were derived from imaging with the WFCCD camera at the 2.5m du Pont telescope on Las Campanas Observatory. Those sources are specifically indicated in the comments column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503#table1</TD>
            <TD>2011-09-14T20:04:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/463/503&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/503</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AcA/51/221 [1]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#1</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AcA/51/221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AcA/51/221 [2]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#2</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AcA/51/221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/51/221 [ic1613]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#ic1613</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/51/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/51/221 [table1]</TD>
            <TD>OGLE-II. Cepheids in IC 1613 (Udalski+, 2001)</TD>
            <TD>We present results of the search for Cepheids in the galaxy IC 1613 carried out as a sub-project of the OGLE-II microlensing survey. 138 Cepheids were found in the 14.2'x14.2' region in the center of the galaxy. We present light curves, VI photometry and basic data for all these objects, as well as color-magnitude diagram of the observed field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221#table1</TD>
            <TD>2011-09-14T20:14:39Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AcA/51/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/51/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/51/221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/357/871 [1]</TD>
            <TD>RR Lyrae stars in the Sgr dwarf galaxy (Cseresnjes+, 2000)</TD>
            <TD>The catalog of single-period RR Lyraes is composed of two tables, one for each field: - filed1.dat for variables detected in field 1 (SAG) centered on (l,b)=(6.6{deg}, -10.8{deg}). The photometry of these RR Lyraes is based on a combination of a Kodak Tech-Pan 4415 film with a BG12 filter. - field2.dat for variables detected in field 2 (DUO) centered on (l,b)=(3.1{deg}, -7.1{deg}). The photometry is based on the Bj system. It is important to note that the photometric systems are different between the two fields (see paper I &amp; II for details). The magnitude and amplitude are therefore not directly comparable from one field to another. The RR Lyrae stars of this catalog are almost evenly distributed between the Sagittarius dwarf and the Galaxy. They are easily separated through an histogram of the magnitudes (see Paper I).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871#1</TD>
            <TD>2012-03-01T11:34:18Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/357/871</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/871</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/357/871 [2]</TD>
            <TD>RR Lyrae stars in the Sgr dwarf galaxy (Cseresnjes+, 2000)</TD>
            <TD>The catalog of single-period RR Lyraes is composed of two tables, one for each field: - filed1.dat for variables detected in field 1 (SAG) centered on (l,b)=(6.6{deg}, -10.8{deg}). The photometry of these RR Lyraes is based on a combination of a Kodak Tech-Pan 4415 film with a BG12 filter. - field2.dat for variables detected in field 2 (DUO) centered on (l,b)=(3.1{deg}, -7.1{deg}). The photometry is based on the Bj system. It is important to note that the photometric systems are different between the two fields (see paper I &amp; II for details). The magnitude and amplitude are therefore not directly comparable from one field to another. The RR Lyrae stars of this catalog are almost evenly distributed between the Sagittarius dwarf and the Galaxy. They are easily separated through an histogram of the magnitudes (see Paper I).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871#2</TD>
            <TD>2012-03-01T11:34:18Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/357/871&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/871</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/357/871 [stars]</TD>
            <TD>RR Lyrae stars in the Sgr dwarf galaxy (Cseresnjes+, 2000)</TD>
            <TD>The catalog of single-period RR Lyraes is composed of two tables, one for each field: - filed1.dat for variables detected in field 1 (SAG) centered on (l,b)=(6.6{deg}, -10.8{deg}). The photometry of these RR Lyraes is based on a combination of a Kodak Tech-Pan 4415 film with a BG12 filter. - field2.dat for variables detected in field 2 (DUO) centered on (l,b)=(3.1{deg}, -7.1{deg}). The photometry is based on the Bj system. It is important to note that the photometric systems are different between the two fields (see paper I &amp; II for details). The magnitude and amplitude are therefore not directly comparable from one field to another. The RR Lyrae stars of this catalog are almost evenly distributed between the Sagittarius dwarf and the Galaxy. They are easily separated through an histogram of the magnitudes (see Paper I).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871#stars</TD>
            <TD>2012-03-01T11:34:18Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/357/871&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/871</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/463/503 [1]</TD>
            <TD>Early-type dwarf galaxies in Fornax cluster (Mieske+, 2007)</TD>
            <TD>Total V-band magnitude, central V-band surface brightness, and V-I colour is presented for a sample of 100 dwarf elliptical galaxy candidates in the central Fornax cluster. We also give the cluster membership flag assigned to each galaxy, based upon distance measurements obtained with the SBF method and on morphological assessment. For most of the sources, the photometric parameters are derived from imaging with the IMACS instrument at the Magellan telescope on Las Campanas Observatory. For some fainter sources the photometric parameters were derived from imaging with the WFCCD camera at the 2.5m du Pont telescope on Las Campanas Observatory. Those sources are specifically indicated in the comments column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503#1</TD>
            <TD>2011-09-14T20:04:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/463/503</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/503</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/463/503 [2]</TD>
            <TD>Early-type dwarf galaxies in Fornax cluster (Mieske+, 2007)</TD>
            <TD>Total V-band magnitude, central V-band surface brightness, and V-I colour is presented for a sample of 100 dwarf elliptical galaxy candidates in the central Fornax cluster. We also give the cluster membership flag assigned to each galaxy, based upon distance measurements obtained with the SBF method and on morphological assessment. For most of the sources, the photometric parameters are derived from imaging with the IMACS instrument at the Magellan telescope on Las Campanas Observatory. For some fainter sources the photometric parameters were derived from imaging with the WFCCD camera at the 2.5m du Pont telescope on Las Campanas Observatory. Those sources are specifically indicated in the comments column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503#2</TD>
            <TD>2011-09-14T20:04:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/463/503&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/503</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/463/503 [table1]</TD>
            <TD>Early-type dwarf galaxies in Fornax cluster (Mieske+, 2007)</TD>
            <TD>Total V-band magnitude, central V-band surface brightness, and V-I colour is presented for a sample of 100 dwarf elliptical galaxy candidates in the central Fornax cluster. We also give the cluster membership flag assigned to each galaxy, based upon distance measurements obtained with the SBF method and on morphological assessment. For most of the sources, the photometric parameters are derived from imaging with the IMACS instrument at the Magellan telescope on Las Campanas Observatory. For some fainter sources the photometric parameters were derived from imaging with the WFCCD camera at the 2.5m du Pont telescope on Las Campanas Observatory. Those sources are specifically indicated in the comments column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503#table1</TD>
            <TD>2011-09-14T20:04:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/503</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/463/503&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/503</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/467/73 [1]</TD>
            <TD>3{sigma} hard sample of XMDS survey (Tajer+, 2007)</TD>
            <TD>Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. We selected a sample of 136 X-ray sources detected at a significance of &gt;=3{sigma} in the 2-10keV band (F_2-10_&gt;~10^-14^erg/cm^2^/s) in a ~1deg^2^ area in the XMM Medium Deep Survey (XMDS, Cat. &lt;J/A+A/439/413&gt;). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73#1</TD>
            <TD>2011-09-14T20:14:41Z</TD>
            <TD>#AGN#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/467/73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/467/73 [2]</TD>
            <TD>3{sigma} hard sample of XMDS survey (Tajer+, 2007)</TD>
            <TD>Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. We selected a sample of 136 X-ray sources detected at a significance of &gt;=3{sigma} in the 2-10keV band (F_2-10_&gt;~10^-14^erg/cm^2^/s) in a ~1deg^2^ area in the XMM Medium Deep Survey (XMDS, Cat. &lt;J/A+A/439/413&gt;). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73#2</TD>
            <TD>2011-09-14T20:14:41Z</TD>
            <TD>#AGN#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/467/73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/73</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/467/73 [tablea1]</TD>
            <TD>3{sigma} hard sample of XMDS survey (Tajer+, 2007)</TD>
            <TD>Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. We selected a sample of 136 X-ray sources detected at a significance of &gt;=3{sigma} in the 2-10keV band (F_2-10_&gt;~10^-14^erg/cm^2^/s) in a ~1deg^2^ area in the XMM Medium Deep Survey (XMDS, Cat. &lt;J/A+A/439/413&gt;). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73#tablea1</TD>
            <TD>2011-09-14T20:14:41Z</TD>
            <TD>#AGN#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/467/73&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/357/871 [1]</TD>
            <TD>RR Lyrae stars in the Sgr dwarf galaxy (Cseresnjes+, 2000)</TD>
            <TD>The catalog of single-period RR Lyraes is composed of two tables, one for each field: - filed1.dat for variables detected in field 1 (SAG) centered on (l,b)=(6.6{deg}, -10.8{deg}). The photometry of these RR Lyraes is based on a combination of a Kodak Tech-Pan 4415 film with a BG12 filter. - field2.dat for variables detected in field 2 (DUO) centered on (l,b)=(3.1{deg}, -7.1{deg}). The photometry is based on the Bj system. It is important to note that the photometric systems are different between the two fields (see paper I &amp; II for details). The magnitude and amplitude are therefore not directly comparable from one field to another. The RR Lyrae stars of this catalog are almost evenly distributed between the Sagittarius dwarf and the Galaxy. They are easily separated through an histogram of the magnitudes (see Paper I).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871#1</TD>
            <TD>2012-03-01T11:34:18Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/357/871</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/871</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/357/871 [2]</TD>
            <TD>RR Lyrae stars in the Sgr dwarf galaxy (Cseresnjes+, 2000)</TD>
            <TD>The catalog of single-period RR Lyraes is composed of two tables, one for each field: - filed1.dat for variables detected in field 1 (SAG) centered on (l,b)=(6.6{deg}, -10.8{deg}). The photometry of these RR Lyraes is based on a combination of a Kodak Tech-Pan 4415 film with a BG12 filter. - field2.dat for variables detected in field 2 (DUO) centered on (l,b)=(3.1{deg}, -7.1{deg}). The photometry is based on the Bj system. It is important to note that the photometric systems are different between the two fields (see paper I &amp; II for details). The magnitude and amplitude are therefore not directly comparable from one field to another. The RR Lyrae stars of this catalog are almost evenly distributed between the Sagittarius dwarf and the Galaxy. They are easily separated through an histogram of the magnitudes (see Paper I).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871#2</TD>
            <TD>2012-03-01T11:34:18Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/357/871&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/871</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/357/871 [stars]</TD>
            <TD>RR Lyrae stars in the Sgr dwarf galaxy (Cseresnjes+, 2000)</TD>
            <TD>The catalog of single-period RR Lyraes is composed of two tables, one for each field: - filed1.dat for variables detected in field 1 (SAG) centered on (l,b)=(6.6{deg}, -10.8{deg}). The photometry of these RR Lyraes is based on a combination of a Kodak Tech-Pan 4415 film with a BG12 filter. - field2.dat for variables detected in field 2 (DUO) centered on (l,b)=(3.1{deg}, -7.1{deg}). The photometry is based on the Bj system. It is important to note that the photometric systems are different between the two fields (see paper I &amp; II for details). The magnitude and amplitude are therefore not directly comparable from one field to another. The RR Lyrae stars of this catalog are almost evenly distributed between the Sagittarius dwarf and the Galaxy. They are easily separated through an histogram of the magnitudes (see Paper I).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871#stars</TD>
            <TD>2012-03-01T11:34:18Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/357/871&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/871</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/467/73 [1]</TD>
            <TD>3{sigma} hard sample of XMDS survey (Tajer+, 2007)</TD>
            <TD>Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. We selected a sample of 136 X-ray sources detected at a significance of &gt;=3{sigma} in the 2-10keV band (F_2-10_&gt;~10^-14^erg/cm^2^/s) in a ~1deg^2^ area in the XMM Medium Deep Survey (XMDS, Cat. &lt;J/A+A/439/413&gt;). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73#1</TD>
            <TD>2011-09-14T20:14:41Z</TD>
            <TD>#AGN#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/467/73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/467/73 [2]</TD>
            <TD>3{sigma} hard sample of XMDS survey (Tajer+, 2007)</TD>
            <TD>Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. We selected a sample of 136 X-ray sources detected at a significance of &gt;=3{sigma} in the 2-10keV band (F_2-10_&gt;~10^-14^erg/cm^2^/s) in a ~1deg^2^ area in the XMM Medium Deep Survey (XMDS, Cat. &lt;J/A+A/439/413&gt;). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73#2</TD>
            <TD>2011-09-14T20:14:41Z</TD>
            <TD>#AGN#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/467/73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/73</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/467/73 [tablea1]</TD>
            <TD>3{sigma} hard sample of XMDS survey (Tajer+, 2007)</TD>
            <TD>Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. We selected a sample of 136 X-ray sources detected at a significance of &gt;=3{sigma} in the 2-10keV band (F_2-10_&gt;~10^-14^erg/cm^2^/s) in a ~1deg^2^ area in the XMM Medium Deep Survey (XMDS, Cat. &lt;J/A+A/439/413&gt;). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73#tablea1</TD>
            <TD>2011-09-14T20:14:41Z</TD>
            <TD>#AGN#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/467/73&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/621 [1]</TD>
            <TD>Galaxy morphology in the CFRS (van den Bergh, 2001)</TD>
            <TD>The images of 229 galaxies in the Canada-France Redshift Survey have been classified on the DDO system. These observations were combined with previous classifications of galaxies with known redshifts in the Hubble Deep Field. The combined sample provides homogeneous morphological classifications for 425 galaxies of known redshift. The fraction of all galaxies that are of type E, S0, or E/S0 appears to remain approximately constant at ~17% over the redshift range 0.25&lt;z&lt;1.2. Over the same range, the fraction of irregular (Ir) galaxies increases from ~5% to ~12%. Part of this increase may be due to mild luminosity evolution of Ir galaxies. The frequency of mergers is found to rise by a factor of 2 or 3 over the redshift range covered by the present survey. These results are in qualitative agreement with those obtained previously by Brinchmann et al. (Cat. &lt;J/ApJ/499/112&gt;) using a coarser galaxy classification system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621#1</TD>
            <TD>2011-09-14T20:04:44Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/621</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/621</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/621 [2]</TD>
            <TD>Galaxy morphology in the CFRS (van den Bergh, 2001)</TD>
            <TD>The images of 229 galaxies in the Canada-France Redshift Survey have been classified on the DDO system. These observations were combined with previous classifications of galaxies with known redshifts in the Hubble Deep Field. The combined sample provides homogeneous morphological classifications for 425 galaxies of known redshift. The fraction of all galaxies that are of type E, S0, or E/S0 appears to remain approximately constant at ~17% over the redshift range 0.25&lt;z&lt;1.2. Over the same range, the fraction of irregular (Ir) galaxies increases from ~5% to ~12%. Part of this increase may be due to mild luminosity evolution of Ir galaxies. The frequency of mergers is found to rise by a factor of 2 or 3 over the redshift range covered by the present survey. These results are in qualitative agreement with those obtained previously by Brinchmann et al. (Cat. &lt;J/ApJ/499/112&gt;) using a coarser galaxy classification system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621#2</TD>
            <TD>2011-09-14T20:04:44Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/621&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/621</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/621 [table1]</TD>
            <TD>Galaxy morphology in the CFRS (van den Bergh, 2001)</TD>
            <TD>The images of 229 galaxies in the Canada-France Redshift Survey have been classified on the DDO system. These observations were combined with previous classifications of galaxies with known redshifts in the Hubble Deep Field. The combined sample provides homogeneous morphological classifications for 425 galaxies of known redshift. The fraction of all galaxies that are of type E, S0, or E/S0 appears to remain approximately constant at ~17% over the redshift range 0.25&lt;z&lt;1.2. Over the same range, the fraction of irregular (Ir) galaxies increases from ~5% to ~12%. Part of this increase may be due to mild luminosity evolution of Ir galaxies. The frequency of mergers is found to rise by a factor of 2 or 3 over the redshift range covered by the present survey. These results are in qualitative agreement with those obtained previously by Brinchmann et al. (Cat. &lt;J/ApJ/499/112&gt;) using a coarser galaxy classification system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621#table1</TD>
            <TD>2011-09-14T20:04:44Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/621&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/621</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/467/73 [1]</TD>
            <TD>3{sigma} hard sample of XMDS survey (Tajer+, 2007)</TD>
            <TD>Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. We selected a sample of 136 X-ray sources detected at a significance of &gt;=3{sigma} in the 2-10keV band (F_2-10_&gt;~10^-14^erg/cm^2^/s) in a ~1deg^2^ area in the XMM Medium Deep Survey (XMDS, Cat. &lt;J/A+A/439/413&gt;). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73#1</TD>
            <TD>2011-09-14T20:14:41Z</TD>
            <TD>#AGN#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/467/73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/467/73 [2]</TD>
            <TD>3{sigma} hard sample of XMDS survey (Tajer+, 2007)</TD>
            <TD>Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. We selected a sample of 136 X-ray sources detected at a significance of &gt;=3{sigma} in the 2-10keV band (F_2-10_&gt;~10^-14^erg/cm^2^/s) in a ~1deg^2^ area in the XMM Medium Deep Survey (XMDS, Cat. &lt;J/A+A/439/413&gt;). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73#2</TD>
            <TD>2011-09-14T20:14:41Z</TD>
            <TD>#AGN#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/467/73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/73</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/467/73 [tablea1]</TD>
            <TD>3{sigma} hard sample of XMDS survey (Tajer+, 2007)</TD>
            <TD>Our goal is to probe the populations of obscured and unobscured AGN investigating their optical-IR and X-ray properties as a function of X-ray flux, luminosity and redshift within a hard X-ray selected sample with wide multiwavelength coverage. We selected a sample of 136 X-ray sources detected at a significance of &gt;=3{sigma} in the 2-10keV band (F_2-10_&gt;~10^-14^erg/cm^2^/s) in a ~1deg^2^ area in the XMM Medium Deep Survey (XMDS, Cat. &lt;J/A+A/439/413&gt;). The XMDS area is covered with optical photometry from the VVDS and CFHTLS surveys and infrared Spitzer data from the SWIRE survey. Based on the X-ray luminosity and X-ray to optical ratio, 132 sources are likely AGN, of which 122 have unambiguous optical - IR identification. The observed optical and IR spectral energy distributions of all identified sources are fitted with AGN/galaxy templates in order to classify them and compute photometric redshifts. X-ray spectral analysis is performed individually for sources with a sufficient number of counts and using a stacking technique for subsamples of sources at different flux levels. Hardness ratios are used to estimate X-ray absorption in individual weak sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73#tablea1</TD>
            <TD>2011-09-14T20:14:41Z</TD>
            <TD>#AGN#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/467/73</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/467/73&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/467/73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/357/871 [1]</TD>
            <TD>RR Lyrae stars in the Sgr dwarf galaxy (Cseresnjes+, 2000)</TD>
            <TD>The catalog of single-period RR Lyraes is composed of two tables, one for each field: - filed1.dat for variables detected in field 1 (SAG) centered on (l,b)=(6.6{deg}, -10.8{deg}). The photometry of these RR Lyraes is based on a combination of a Kodak Tech-Pan 4415 film with a BG12 filter. - field2.dat for variables detected in field 2 (DUO) centered on (l,b)=(3.1{deg}, -7.1{deg}). The photometry is based on the Bj system. It is important to note that the photometric systems are different between the two fields (see paper I &amp; II for details). The magnitude and amplitude are therefore not directly comparable from one field to another. The RR Lyrae stars of this catalog are almost evenly distributed between the Sagittarius dwarf and the Galaxy. They are easily separated through an histogram of the magnitudes (see Paper I).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871#1</TD>
            <TD>2012-03-01T11:34:18Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/357/871</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/871</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/357/871 [2]</TD>
            <TD>RR Lyrae stars in the Sgr dwarf galaxy (Cseresnjes+, 2000)</TD>
            <TD>The catalog of single-period RR Lyraes is composed of two tables, one for each field: - filed1.dat for variables detected in field 1 (SAG) centered on (l,b)=(6.6{deg}, -10.8{deg}). The photometry of these RR Lyraes is based on a combination of a Kodak Tech-Pan 4415 film with a BG12 filter. - field2.dat for variables detected in field 2 (DUO) centered on (l,b)=(3.1{deg}, -7.1{deg}). The photometry is based on the Bj system. It is important to note that the photometric systems are different between the two fields (see paper I &amp; II for details). The magnitude and amplitude are therefore not directly comparable from one field to another. The RR Lyrae stars of this catalog are almost evenly distributed between the Sagittarius dwarf and the Galaxy. They are easily separated through an histogram of the magnitudes (see Paper I).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871#2</TD>
            <TD>2012-03-01T11:34:18Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/357/871&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/871</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/357/871 [stars]</TD>
            <TD>RR Lyrae stars in the Sgr dwarf galaxy (Cseresnjes+, 2000)</TD>
            <TD>The catalog of single-period RR Lyraes is composed of two tables, one for each field: - filed1.dat for variables detected in field 1 (SAG) centered on (l,b)=(6.6{deg}, -10.8{deg}). The photometry of these RR Lyraes is based on a combination of a Kodak Tech-Pan 4415 film with a BG12 filter. - field2.dat for variables detected in field 2 (DUO) centered on (l,b)=(3.1{deg}, -7.1{deg}). The photometry is based on the Bj system. It is important to note that the photometric systems are different between the two fields (see paper I &amp; II for details). The magnitude and amplitude are therefore not directly comparable from one field to another. The RR Lyrae stars of this catalog are almost evenly distributed between the Sagittarius dwarf and the Galaxy. They are easily separated through an histogram of the magnitudes (see Paper I).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871#stars</TD>
            <TD>2012-03-01T11:34:18Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/871</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/357/871&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/871</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/621 [1]</TD>
            <TD>Galaxy morphology in the CFRS (van den Bergh, 2001)</TD>
            <TD>The images of 229 galaxies in the Canada-France Redshift Survey have been classified on the DDO system. These observations were combined with previous classifications of galaxies with known redshifts in the Hubble Deep Field. The combined sample provides homogeneous morphological classifications for 425 galaxies of known redshift. The fraction of all galaxies that are of type E, S0, or E/S0 appears to remain approximately constant at ~17% over the redshift range 0.25&lt;z&lt;1.2. Over the same range, the fraction of irregular (Ir) galaxies increases from ~5% to ~12%. Part of this increase may be due to mild luminosity evolution of Ir galaxies. The frequency of mergers is found to rise by a factor of 2 or 3 over the redshift range covered by the present survey. These results are in qualitative agreement with those obtained previously by Brinchmann et al. (Cat. &lt;J/ApJ/499/112&gt;) using a coarser galaxy classification system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621#1</TD>
            <TD>2011-09-14T20:04:44Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/621</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/621</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/621 [2]</TD>
            <TD>Galaxy morphology in the CFRS (van den Bergh, 2001)</TD>
            <TD>The images of 229 galaxies in the Canada-France Redshift Survey have been classified on the DDO system. These observations were combined with previous classifications of galaxies with known redshifts in the Hubble Deep Field. The combined sample provides homogeneous morphological classifications for 425 galaxies of known redshift. The fraction of all galaxies that are of type E, S0, or E/S0 appears to remain approximately constant at ~17% over the redshift range 0.25&lt;z&lt;1.2. Over the same range, the fraction of irregular (Ir) galaxies increases from ~5% to ~12%. Part of this increase may be due to mild luminosity evolution of Ir galaxies. The frequency of mergers is found to rise by a factor of 2 or 3 over the redshift range covered by the present survey. These results are in qualitative agreement with those obtained previously by Brinchmann et al. (Cat. &lt;J/ApJ/499/112&gt;) using a coarser galaxy classification system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621#2</TD>
            <TD>2011-09-14T20:04:44Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/621&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/621</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/621 [table1]</TD>
            <TD>Galaxy morphology in the CFRS (van den Bergh, 2001)</TD>
            <TD>The images of 229 galaxies in the Canada-France Redshift Survey have been classified on the DDO system. These observations were combined with previous classifications of galaxies with known redshifts in the Hubble Deep Field. The combined sample provides homogeneous morphological classifications for 425 galaxies of known redshift. The fraction of all galaxies that are of type E, S0, or E/S0 appears to remain approximately constant at ~17% over the redshift range 0.25&lt;z&lt;1.2. Over the same range, the fraction of irregular (Ir) galaxies increases from ~5% to ~12%. Part of this increase may be due to mild luminosity evolution of Ir galaxies. The frequency of mergers is found to rise by a factor of 2 or 3 over the redshift range covered by the present survey. These results are in qualitative agreement with those obtained previously by Brinchmann et al. (Cat. &lt;J/ApJ/499/112&gt;) using a coarser galaxy classification system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621#table1</TD>
            <TD>2011-09-14T20:04:44Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/621&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/621</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/PASA/18. [1]</TD>
            <TD>FLAIR II spectroscopy of DENIS samples (Mamon+, 2001)</TD>
            <TD>As a pilot survey for the forthcoming 6dF Galaxy Redshift Survey, spectroscopy of galaxies selected in the 1.2 micron J waveband with the DENIS imaging survey was performed at the UKST using the FLAIR II multi-object spectroscope. Sixty-nine galaxy redshifts were obtained in a high galactic latitude field and an additional 12 redshifts in a low galactic latitude (b=-17{deg}), obscured field. This spectroscopic follow-up of NIR selected galaxies illustrates the feasibility of obtaining redshifts with optical spectra on galaxies selected at much longer wavelengths. It validated a very preliminary algorithm for star/galaxy separation for high galactic latitude DENIS objects, with 99% reliability for J&lt;13.9. The FLAIR II redshifts are in excellent agreement with those, previously published, of 20 common galaxies. However, the FLAIR II redshift determinations presented here required substantially longer integration times to achieve 90% completeness than expected from previous optical surveys at comparable depth. This is mainly due to a degradation in overall fibre throughput due to known problems with ageing of the prism- cement-fibre interface with exposure to UV light. In comparison to our high galactic latitude field, our low latitude (high extinction) field required 2.5 times more exposure time for less than 50% of successful redshift measurements. Among the J&lt;=13.9 galaxies with measured redshifts, only 37+/-6% display emission lines, in comparison with 60% of emission line galaxies in optical samples of comparable depth. These galaxies are, on average, half a magnitude bluer in B-J than galaxies of the same luminosity without emission fines. We confirm a previous optically-based result that the fraction of galaxies with emission lines increases rapidly with decreasing galaxy luminosity. The J band luminosity function is estimated. Our high latitude field displays a concentration of galaxies at cz~=38000km/s suggesting a possible supercluster. A radial velocity is reported for a galaxy lying near the projected centre of the Abell 1434 cluster of galaxies, for which no cluster redshift is currently available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232#1</TD>
            <TD>2011-09-14T20:15:03Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/PASA/18.232</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/18.232</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/PASA/18. [2]</TD>
            <TD>FLAIR II spectroscopy of DENIS samples (Mamon+, 2001)</TD>
            <TD>As a pilot survey for the forthcoming 6dF Galaxy Redshift Survey, spectroscopy of galaxies selected in the 1.2 micron J waveband with the DENIS imaging survey was performed at the UKST using the FLAIR II multi-object spectroscope. Sixty-nine galaxy redshifts were obtained in a high galactic latitude field and an additional 12 redshifts in a low galactic latitude (b=-17{deg}), obscured field. This spectroscopic follow-up of NIR selected galaxies illustrates the feasibility of obtaining redshifts with optical spectra on galaxies selected at much longer wavelengths. It validated a very preliminary algorithm for star/galaxy separation for high galactic latitude DENIS objects, with 99% reliability for J&lt;13.9. The FLAIR II redshifts are in excellent agreement with those, previously published, of 20 common galaxies. However, the FLAIR II redshift determinations presented here required substantially longer integration times to achieve 90% completeness than expected from previous optical surveys at comparable depth. This is mainly due to a degradation in overall fibre throughput due to known problems with ageing of the prism- cement-fibre interface with exposure to UV light. In comparison to our high galactic latitude field, our low latitude (high extinction) field required 2.5 times more exposure time for less than 50% of successful redshift measurements. Among the J&lt;=13.9 galaxies with measured redshifts, only 37+/-6% display emission lines, in comparison with 60% of emission line galaxies in optical samples of comparable depth. These galaxies are, on average, half a magnitude bluer in B-J than galaxies of the same luminosity without emission fines. We confirm a previous optically-based result that the fraction of galaxies with emission lines increases rapidly with decreasing galaxy luminosity. The J band luminosity function is estimated. Our high latitude field displays a concentration of galaxies at cz~=38000km/s suggesting a possible supercluster. A radial velocity is reported for a galaxy lying near the projected centre of the Abell 1434 cluster of galaxies, for which no cluster redshift is currently available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232#2</TD>
            <TD>2011-09-14T20:15:03Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/PASA/18.232&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/18.232</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/PASA/18. [tables]</TD>
            <TD>FLAIR II spectroscopy of DENIS samples (Mamon+, 2001)</TD>
            <TD>As a pilot survey for the forthcoming 6dF Galaxy Redshift Survey, spectroscopy of galaxies selected in the 1.2 micron J waveband with the DENIS imaging survey was performed at the UKST using the FLAIR II multi-object spectroscope. Sixty-nine galaxy redshifts were obtained in a high galactic latitude field and an additional 12 redshifts in a low galactic latitude (b=-17{deg}), obscured field. This spectroscopic follow-up of NIR selected galaxies illustrates the feasibility of obtaining redshifts with optical spectra on galaxies selected at much longer wavelengths. It validated a very preliminary algorithm for star/galaxy separation for high galactic latitude DENIS objects, with 99% reliability for J&lt;13.9. The FLAIR II redshifts are in excellent agreement with those, previously published, of 20 common galaxies. However, the FLAIR II redshift determinations presented here required substantially longer integration times to achieve 90% completeness than expected from previous optical surveys at comparable depth. This is mainly due to a degradation in overall fibre throughput due to known problems with ageing of the prism- cement-fibre interface with exposure to UV light. In comparison to our high galactic latitude field, our low latitude (high extinction) field required 2.5 times more exposure time for less than 50% of successful redshift measurements. Among the J&lt;=13.9 galaxies with measured redshifts, only 37+/-6% display emission lines, in comparison with 60% of emission line galaxies in optical samples of comparable depth. These galaxies are, on average, half a magnitude bluer in B-J than galaxies of the same luminosity without emission fines. We confirm a previous optically-based result that the fraction of galaxies with emission lines increases rapidly with decreasing galaxy luminosity. The J band luminosity function is estimated. Our high latitude field displays a concentration of galaxies at cz~=38000km/s suggesting a possible supercluster. A radial velocity is reported for a galaxy lying near the projected centre of the Abell 1434 cluster of galaxies, for which no cluster redshift is currently available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232#tables</TD>
            <TD>2011-09-14T20:15:03Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/PASA/18.232&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/18.232</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/2018 [1]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#1</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/2018</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/2018 [2]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#2</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/2018&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2018 [table1]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#table1</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2018&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2018 [table2]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#table2</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2018&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/PASA/18. [1]</TD>
            <TD>FLAIR II spectroscopy of DENIS samples (Mamon+, 2001)</TD>
            <TD>As a pilot survey for the forthcoming 6dF Galaxy Redshift Survey, spectroscopy of galaxies selected in the 1.2 micron J waveband with the DENIS imaging survey was performed at the UKST using the FLAIR II multi-object spectroscope. Sixty-nine galaxy redshifts were obtained in a high galactic latitude field and an additional 12 redshifts in a low galactic latitude (b=-17{deg}), obscured field. This spectroscopic follow-up of NIR selected galaxies illustrates the feasibility of obtaining redshifts with optical spectra on galaxies selected at much longer wavelengths. It validated a very preliminary algorithm for star/galaxy separation for high galactic latitude DENIS objects, with 99% reliability for J&lt;13.9. The FLAIR II redshifts are in excellent agreement with those, previously published, of 20 common galaxies. However, the FLAIR II redshift determinations presented here required substantially longer integration times to achieve 90% completeness than expected from previous optical surveys at comparable depth. This is mainly due to a degradation in overall fibre throughput due to known problems with ageing of the prism- cement-fibre interface with exposure to UV light. In comparison to our high galactic latitude field, our low latitude (high extinction) field required 2.5 times more exposure time for less than 50% of successful redshift measurements. Among the J&lt;=13.9 galaxies with measured redshifts, only 37+/-6% display emission lines, in comparison with 60% of emission line galaxies in optical samples of comparable depth. These galaxies are, on average, half a magnitude bluer in B-J than galaxies of the same luminosity without emission fines. We confirm a previous optically-based result that the fraction of galaxies with emission lines increases rapidly with decreasing galaxy luminosity. The J band luminosity function is estimated. Our high latitude field displays a concentration of galaxies at cz~=38000km/s suggesting a possible supercluster. A radial velocity is reported for a galaxy lying near the projected centre of the Abell 1434 cluster of galaxies, for which no cluster redshift is currently available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232#1</TD>
            <TD>2011-09-14T20:15:03Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/PASA/18.232</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/18.232</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/PASA/18. [2]</TD>
            <TD>FLAIR II spectroscopy of DENIS samples (Mamon+, 2001)</TD>
            <TD>As a pilot survey for the forthcoming 6dF Galaxy Redshift Survey, spectroscopy of galaxies selected in the 1.2 micron J waveband with the DENIS imaging survey was performed at the UKST using the FLAIR II multi-object spectroscope. Sixty-nine galaxy redshifts were obtained in a high galactic latitude field and an additional 12 redshifts in a low galactic latitude (b=-17{deg}), obscured field. This spectroscopic follow-up of NIR selected galaxies illustrates the feasibility of obtaining redshifts with optical spectra on galaxies selected at much longer wavelengths. It validated a very preliminary algorithm for star/galaxy separation for high galactic latitude DENIS objects, with 99% reliability for J&lt;13.9. The FLAIR II redshifts are in excellent agreement with those, previously published, of 20 common galaxies. However, the FLAIR II redshift determinations presented here required substantially longer integration times to achieve 90% completeness than expected from previous optical surveys at comparable depth. This is mainly due to a degradation in overall fibre throughput due to known problems with ageing of the prism- cement-fibre interface with exposure to UV light. In comparison to our high galactic latitude field, our low latitude (high extinction) field required 2.5 times more exposure time for less than 50% of successful redshift measurements. Among the J&lt;=13.9 galaxies with measured redshifts, only 37+/-6% display emission lines, in comparison with 60% of emission line galaxies in optical samples of comparable depth. These galaxies are, on average, half a magnitude bluer in B-J than galaxies of the same luminosity without emission fines. We confirm a previous optically-based result that the fraction of galaxies with emission lines increases rapidly with decreasing galaxy luminosity. The J band luminosity function is estimated. Our high latitude field displays a concentration of galaxies at cz~=38000km/s suggesting a possible supercluster. A radial velocity is reported for a galaxy lying near the projected centre of the Abell 1434 cluster of galaxies, for which no cluster redshift is currently available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232#2</TD>
            <TD>2011-09-14T20:15:03Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/PASA/18.232&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/18.232</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/PASA/18. [tables]</TD>
            <TD>FLAIR II spectroscopy of DENIS samples (Mamon+, 2001)</TD>
            <TD>As a pilot survey for the forthcoming 6dF Galaxy Redshift Survey, spectroscopy of galaxies selected in the 1.2 micron J waveband with the DENIS imaging survey was performed at the UKST using the FLAIR II multi-object spectroscope. Sixty-nine galaxy redshifts were obtained in a high galactic latitude field and an additional 12 redshifts in a low galactic latitude (b=-17{deg}), obscured field. This spectroscopic follow-up of NIR selected galaxies illustrates the feasibility of obtaining redshifts with optical spectra on galaxies selected at much longer wavelengths. It validated a very preliminary algorithm for star/galaxy separation for high galactic latitude DENIS objects, with 99% reliability for J&lt;13.9. The FLAIR II redshifts are in excellent agreement with those, previously published, of 20 common galaxies. However, the FLAIR II redshift determinations presented here required substantially longer integration times to achieve 90% completeness than expected from previous optical surveys at comparable depth. This is mainly due to a degradation in overall fibre throughput due to known problems with ageing of the prism- cement-fibre interface with exposure to UV light. In comparison to our high galactic latitude field, our low latitude (high extinction) field required 2.5 times more exposure time for less than 50% of successful redshift measurements. Among the J&lt;=13.9 galaxies with measured redshifts, only 37+/-6% display emission lines, in comparison with 60% of emission line galaxies in optical samples of comparable depth. These galaxies are, on average, half a magnitude bluer in B-J than galaxies of the same luminosity without emission fines. We confirm a previous optically-based result that the fraction of galaxies with emission lines increases rapidly with decreasing galaxy luminosity. The J band luminosity function is estimated. Our high latitude field displays a concentration of galaxies at cz~=38000km/s suggesting a possible supercluster. A radial velocity is reported for a galaxy lying near the projected centre of the Abell 1434 cluster of galaxies, for which no cluster redshift is currently available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232#tables</TD>
            <TD>2011-09-14T20:15:03Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/PASA/18.232&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/18.232</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/468/807 [1]</TD>
            <TD>Redshifts of galaxies associated with X emission (Mannucci+, 2007)</TD>
            <TD>List of the target galaxies observed with the WHT/AF2/WYFOOS and TNG/DOLORES multi-object spectrographs. For each galaxy, the coordinates, the R-band magnitude, the spectroscopic redshift and the spectral classification are given. Target galaxies have been selected to have R-band magnitudes between 20.0 and 21.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807#1</TD>
            <TD>2011-09-14T20:11:23Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/468/807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/468/807 [2]</TD>
            <TD>Redshifts of galaxies associated with X emission (Mannucci+, 2007)</TD>
            <TD>List of the target galaxies observed with the WHT/AF2/WYFOOS and TNG/DOLORES multi-object spectrographs. For each galaxy, the coordinates, the R-band magnitude, the spectroscopic redshift and the spectral classification are given. Target galaxies have been selected to have R-band magnitudes between 20.0 and 21.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807#2</TD>
            <TD>2011-09-14T20:11:23Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/468/807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/807</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/468/807 [table2]</TD>
            <TD>Redshifts of galaxies associated with X emission (Mannucci+, 2007)</TD>
            <TD>List of the target galaxies observed with the WHT/AF2/WYFOOS and TNG/DOLORES multi-object spectrographs. For each galaxy, the coordinates, the R-band magnitude, the spectroscopic redshift and the spectral classification are given. Target galaxies have been selected to have R-band magnitudes between 20.0 and 21.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807#table2</TD>
            <TD>2011-09-14T20:11:23Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/468/807&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/2018 [1]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#1</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/2018</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/2018 [2]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#2</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/2018&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2018 [table1]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#table1</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2018&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2018 [table2]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#table2</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2018&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/PASA/18. [1]</TD>
            <TD>FLAIR II spectroscopy of DENIS samples (Mamon+, 2001)</TD>
            <TD>As a pilot survey for the forthcoming 6dF Galaxy Redshift Survey, spectroscopy of galaxies selected in the 1.2 micron J waveband with the DENIS imaging survey was performed at the UKST using the FLAIR II multi-object spectroscope. Sixty-nine galaxy redshifts were obtained in a high galactic latitude field and an additional 12 redshifts in a low galactic latitude (b=-17{deg}), obscured field. This spectroscopic follow-up of NIR selected galaxies illustrates the feasibility of obtaining redshifts with optical spectra on galaxies selected at much longer wavelengths. It validated a very preliminary algorithm for star/galaxy separation for high galactic latitude DENIS objects, with 99% reliability for J&lt;13.9. The FLAIR II redshifts are in excellent agreement with those, previously published, of 20 common galaxies. However, the FLAIR II redshift determinations presented here required substantially longer integration times to achieve 90% completeness than expected from previous optical surveys at comparable depth. This is mainly due to a degradation in overall fibre throughput due to known problems with ageing of the prism- cement-fibre interface with exposure to UV light. In comparison to our high galactic latitude field, our low latitude (high extinction) field required 2.5 times more exposure time for less than 50% of successful redshift measurements. Among the J&lt;=13.9 galaxies with measured redshifts, only 37+/-6% display emission lines, in comparison with 60% of emission line galaxies in optical samples of comparable depth. These galaxies are, on average, half a magnitude bluer in B-J than galaxies of the same luminosity without emission fines. We confirm a previous optically-based result that the fraction of galaxies with emission lines increases rapidly with decreasing galaxy luminosity. The J band luminosity function is estimated. Our high latitude field displays a concentration of galaxies at cz~=38000km/s suggesting a possible supercluster. A radial velocity is reported for a galaxy lying near the projected centre of the Abell 1434 cluster of galaxies, for which no cluster redshift is currently available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232#1</TD>
            <TD>2011-09-14T20:15:03Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/PASA/18.232</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/18.232</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/PASA/18. [2]</TD>
            <TD>FLAIR II spectroscopy of DENIS samples (Mamon+, 2001)</TD>
            <TD>As a pilot survey for the forthcoming 6dF Galaxy Redshift Survey, spectroscopy of galaxies selected in the 1.2 micron J waveband with the DENIS imaging survey was performed at the UKST using the FLAIR II multi-object spectroscope. Sixty-nine galaxy redshifts were obtained in a high galactic latitude field and an additional 12 redshifts in a low galactic latitude (b=-17{deg}), obscured field. This spectroscopic follow-up of NIR selected galaxies illustrates the feasibility of obtaining redshifts with optical spectra on galaxies selected at much longer wavelengths. It validated a very preliminary algorithm for star/galaxy separation for high galactic latitude DENIS objects, with 99% reliability for J&lt;13.9. The FLAIR II redshifts are in excellent agreement with those, previously published, of 20 common galaxies. However, the FLAIR II redshift determinations presented here required substantially longer integration times to achieve 90% completeness than expected from previous optical surveys at comparable depth. This is mainly due to a degradation in overall fibre throughput due to known problems with ageing of the prism- cement-fibre interface with exposure to UV light. In comparison to our high galactic latitude field, our low latitude (high extinction) field required 2.5 times more exposure time for less than 50% of successful redshift measurements. Among the J&lt;=13.9 galaxies with measured redshifts, only 37+/-6% display emission lines, in comparison with 60% of emission line galaxies in optical samples of comparable depth. These galaxies are, on average, half a magnitude bluer in B-J than galaxies of the same luminosity without emission fines. We confirm a previous optically-based result that the fraction of galaxies with emission lines increases rapidly with decreasing galaxy luminosity. The J band luminosity function is estimated. Our high latitude field displays a concentration of galaxies at cz~=38000km/s suggesting a possible supercluster. A radial velocity is reported for a galaxy lying near the projected centre of the Abell 1434 cluster of galaxies, for which no cluster redshift is currently available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232#2</TD>
            <TD>2011-09-14T20:15:03Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/PASA/18.232&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/18.232</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/PASA/18. [tables]</TD>
            <TD>FLAIR II spectroscopy of DENIS samples (Mamon+, 2001)</TD>
            <TD>As a pilot survey for the forthcoming 6dF Galaxy Redshift Survey, spectroscopy of galaxies selected in the 1.2 micron J waveband with the DENIS imaging survey was performed at the UKST using the FLAIR II multi-object spectroscope. Sixty-nine galaxy redshifts were obtained in a high galactic latitude field and an additional 12 redshifts in a low galactic latitude (b=-17{deg}), obscured field. This spectroscopic follow-up of NIR selected galaxies illustrates the feasibility of obtaining redshifts with optical spectra on galaxies selected at much longer wavelengths. It validated a very preliminary algorithm for star/galaxy separation for high galactic latitude DENIS objects, with 99% reliability for J&lt;13.9. The FLAIR II redshifts are in excellent agreement with those, previously published, of 20 common galaxies. However, the FLAIR II redshift determinations presented here required substantially longer integration times to achieve 90% completeness than expected from previous optical surveys at comparable depth. This is mainly due to a degradation in overall fibre throughput due to known problems with ageing of the prism- cement-fibre interface with exposure to UV light. In comparison to our high galactic latitude field, our low latitude (high extinction) field required 2.5 times more exposure time for less than 50% of successful redshift measurements. Among the J&lt;=13.9 galaxies with measured redshifts, only 37+/-6% display emission lines, in comparison with 60% of emission line galaxies in optical samples of comparable depth. These galaxies are, on average, half a magnitude bluer in B-J than galaxies of the same luminosity without emission fines. We confirm a previous optically-based result that the fraction of galaxies with emission lines increases rapidly with decreasing galaxy luminosity. The J band luminosity function is estimated. Our high latitude field displays a concentration of galaxies at cz~=38000km/s suggesting a possible supercluster. A radial velocity is reported for a galaxy lying near the projected centre of the Abell 1434 cluster of galaxies, for which no cluster redshift is currently available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232#tables</TD>
            <TD>2011-09-14T20:15:03Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/18.232</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/PASA/18.232&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/18.232</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/468/807 [1]</TD>
            <TD>Redshifts of galaxies associated with X emission (Mannucci+, 2007)</TD>
            <TD>List of the target galaxies observed with the WHT/AF2/WYFOOS and TNG/DOLORES multi-object spectrographs. For each galaxy, the coordinates, the R-band magnitude, the spectroscopic redshift and the spectral classification are given. Target galaxies have been selected to have R-band magnitudes between 20.0 and 21.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807#1</TD>
            <TD>2011-09-14T20:11:23Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/468/807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/468/807 [2]</TD>
            <TD>Redshifts of galaxies associated with X emission (Mannucci+, 2007)</TD>
            <TD>List of the target galaxies observed with the WHT/AF2/WYFOOS and TNG/DOLORES multi-object spectrographs. For each galaxy, the coordinates, the R-band magnitude, the spectroscopic redshift and the spectral classification are given. Target galaxies have been selected to have R-band magnitudes between 20.0 and 21.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807#2</TD>
            <TD>2011-09-14T20:11:23Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/468/807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/807</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/468/807 [table2]</TD>
            <TD>Redshifts of galaxies associated with X emission (Mannucci+, 2007)</TD>
            <TD>List of the target galaxies observed with the WHT/AF2/WYFOOS and TNG/DOLORES multi-object spectrographs. For each galaxy, the coordinates, the R-band magnitude, the spectroscopic redshift and the spectral classification are given. Target galaxies have been selected to have R-band magnitudes between 20.0 and 21.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807#table2</TD>
            <TD>2011-09-14T20:11:23Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/468/807</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/468/807&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/468/807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/461/81 [1]</TD>
            <TD>Galaxy clusters in the CFHTLS (Olsen+, 2007)</TD>
            <TD>Galaxy cluster candidates for the four Deep fields of the CFHTLS. For each cluster we give a name, position in J2000, estimated redshift and richness, detection significance, number of redshift bins in which the candidate showed a signal, fraction of masked area around the candidate and a visual grade from A (best) to D (worst).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81#1</TD>
            <TD>2011-09-14T20:15:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/461/81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/461/81 [2]</TD>
            <TD>Galaxy clusters in the CFHTLS (Olsen+, 2007)</TD>
            <TD>Galaxy cluster candidates for the four Deep fields of the CFHTLS. For each cluster we give a name, position in J2000, estimated redshift and richness, detection significance, number of redshift bins in which the candidate showed a signal, fraction of masked area around the candidate and a visual grade from A (best) to D (worst).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81#2</TD>
            <TD>2011-09-14T20:15:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/461/81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/461/81 [table3]</TD>
            <TD>Galaxy clusters in the CFHTLS (Olsen+, 2007)</TD>
            <TD>Galaxy cluster candidates for the four Deep fields of the CFHTLS. For each cluster we give a name, position in J2000, estimated redshift and richness, detection significance, number of redshift bins in which the candidate showed a signal, fraction of masked area around the candidate and a visual grade from A (best) to D (worst).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81#table3</TD>
            <TD>2011-09-14T20:15:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/461/81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/84/997 [1]</TD>
            <TD>Abundances of Sr, Y, Zr, Ce and Ba (Mashonkina+, 2007)</TD>
            <TD>Sr, Y, Zr, and Ce abundances are derived for the sample of 74 cool dwarfs and subgiants with the iron abundance [Fe/H] ranged between -2.43 and 0.25. The results are based on LTE (Y, Zr and Ce) and non-LTE (Sr) line formation and line profile analysis of high resolution (40000 and 60000) spectra that have a typical S/N of 50-200. The Zr/Y, Sr/Y, and Sr/Zr ratios in the halo stars form nearly a plateau over the wide metallicity range, -2.43&lt;=[Fe/H]&lt;=0.90, indicating a common origin of Sr, Y, and Zr at the epoch of the halo formation. We find a steep decline of [Zr/Y] in the thick disk stars with increasing Ba abundance. This suggests the reduction of the production rate of Zr compared to that for Y at the active phase of the thick disk formation. The halo and thick disk stars reveal an overabundance of Zr relative to barium that grows with decreasing Ba abundance. There is a clear correlation of the [Zr/Ba] and [Eu/Ba] abundance ratios. Our observational findings for the halo and thick disk do not support the Galaxy chemical evolution models available in the literature and require to improve their predictions. The thin disk stars reveal, on average, solar abundance ratios for (Y,Zr)/Fe, (Y,Zr)/Ba, and Zr/Y. We note a slight decline of Zr/Ba and Zr/Y in these stars with increasing Ba abundance. Our results favour a dominance of the asymptotic giant branch stars in the heavy element enrichment of the interstellar gas over the epoch of the thin disk existence, in agreement with the theory of the main s-process nucleosynthesis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997#1</TD>
            <TD>2011-09-14T20:23:35Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/84/997</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/84/997</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/84/997 [2]</TD>
            <TD>Abundances of Sr, Y, Zr, Ce and Ba (Mashonkina+, 2007)</TD>
            <TD>Sr, Y, Zr, and Ce abundances are derived for the sample of 74 cool dwarfs and subgiants with the iron abundance [Fe/H] ranged between -2.43 and 0.25. The results are based on LTE (Y, Zr and Ce) and non-LTE (Sr) line formation and line profile analysis of high resolution (40000 and 60000) spectra that have a typical S/N of 50-200. The Zr/Y, Sr/Y, and Sr/Zr ratios in the halo stars form nearly a plateau over the wide metallicity range, -2.43&lt;=[Fe/H]&lt;=0.90, indicating a common origin of Sr, Y, and Zr at the epoch of the halo formation. We find a steep decline of [Zr/Y] in the thick disk stars with increasing Ba abundance. This suggests the reduction of the production rate of Zr compared to that for Y at the active phase of the thick disk formation. The halo and thick disk stars reveal an overabundance of Zr relative to barium that grows with decreasing Ba abundance. There is a clear correlation of the [Zr/Ba] and [Eu/Ba] abundance ratios. Our observational findings for the halo and thick disk do not support the Galaxy chemical evolution models available in the literature and require to improve their predictions. The thin disk stars reveal, on average, solar abundance ratios for (Y,Zr)/Fe, (Y,Zr)/Ba, and Zr/Y. We note a slight decline of Zr/Ba and Zr/Y in these stars with increasing Ba abundance. Our results favour a dominance of the asymptotic giant branch stars in the heavy element enrichment of the interstellar gas over the epoch of the thin disk existence, in agreement with the theory of the main s-process nucleosynthesis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997#2</TD>
            <TD>2011-09-14T20:23:35Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/84/997&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/84/997</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AZh/84/997 [abun]</TD>
            <TD>Abundances of Sr, Y, Zr, Ce and Ba (Mashonkina+, 2007)</TD>
            <TD>Sr, Y, Zr, and Ce abundances are derived for the sample of 74 cool dwarfs and subgiants with the iron abundance [Fe/H] ranged between -2.43 and 0.25. The results are based on LTE (Y, Zr and Ce) and non-LTE (Sr) line formation and line profile analysis of high resolution (40000 and 60000) spectra that have a typical S/N of 50-200. The Zr/Y, Sr/Y, and Sr/Zr ratios in the halo stars form nearly a plateau over the wide metallicity range, -2.43&lt;=[Fe/H]&lt;=0.90, indicating a common origin of Sr, Y, and Zr at the epoch of the halo formation. We find a steep decline of [Zr/Y] in the thick disk stars with increasing Ba abundance. This suggests the reduction of the production rate of Zr compared to that for Y at the active phase of the thick disk formation. The halo and thick disk stars reveal an overabundance of Zr relative to barium that grows with decreasing Ba abundance. There is a clear correlation of the [Zr/Ba] and [Eu/Ba] abundance ratios. Our observational findings for the halo and thick disk do not support the Galaxy chemical evolution models available in the literature and require to improve their predictions. The thin disk stars reveal, on average, solar abundance ratios for (Y,Zr)/Fe, (Y,Zr)/Ba, and Zr/Y. We note a slight decline of Zr/Ba and Zr/Y in these stars with increasing Ba abundance. Our results favour a dominance of the asymptotic giant branch stars in the heavy element enrichment of the interstellar gas over the epoch of the thin disk existence, in agreement with the theory of the main s-process nucleosynthesis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997#abun</TD>
            <TD>2011-09-14T20:23:35Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AZh/84/997&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/84/997</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/2018 [1]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#1</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/2018</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/2018 [2]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#2</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/2018&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2018 [table1]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#table1</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2018&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2018 [table2]</TD>
            <TD>Galaxies with large velocity dispersions (Bernardi+, 2006)</TD>
            <TD>We describe the results of a search for galaxies with large (350&gt;=km/s) velocity dispersions. The largest systems we have found appear to be the extremes of the early-type galaxy population: compared to other galaxies with similar luminosities, they have the largest velocity dispersions and the smallest sizes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018#table2</TD>
            <TD>2011-09-14T20:12:38Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2018</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2018&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2018</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/461/81 [1]</TD>
            <TD>Galaxy clusters in the CFHTLS (Olsen+, 2007)</TD>
            <TD>Galaxy cluster candidates for the four Deep fields of the CFHTLS. For each cluster we give a name, position in J2000, estimated redshift and richness, detection significance, number of redshift bins in which the candidate showed a signal, fraction of masked area around the candidate and a visual grade from A (best) to D (worst).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81#1</TD>
            <TD>2011-09-14T20:15:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/461/81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/461/81 [2]</TD>
            <TD>Galaxy clusters in the CFHTLS (Olsen+, 2007)</TD>
            <TD>Galaxy cluster candidates for the four Deep fields of the CFHTLS. For each cluster we give a name, position in J2000, estimated redshift and richness, detection significance, number of redshift bins in which the candidate showed a signal, fraction of masked area around the candidate and a visual grade from A (best) to D (worst).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81#2</TD>
            <TD>2011-09-14T20:15:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/461/81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/461/81 [table3]</TD>
            <TD>Galaxy clusters in the CFHTLS (Olsen+, 2007)</TD>
            <TD>Galaxy cluster candidates for the four Deep fields of the CFHTLS. For each cluster we give a name, position in J2000, estimated redshift and richness, detection significance, number of redshift bins in which the candidate showed a signal, fraction of masked area around the candidate and a visual grade from A (best) to D (worst).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81#table3</TD>
            <TD>2011-09-14T20:15:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/461/81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/84/997 [1]</TD>
            <TD>Abundances of Sr, Y, Zr, Ce and Ba (Mashonkina+, 2007)</TD>
            <TD>Sr, Y, Zr, and Ce abundances are derived for the sample of 74 cool dwarfs and subgiants with the iron abundance [Fe/H] ranged between -2.43 and 0.25. The results are based on LTE (Y, Zr and Ce) and non-LTE (Sr) line formation and line profile analysis of high resolution (40000 and 60000) spectra that have a typical S/N of 50-200. The Zr/Y, Sr/Y, and Sr/Zr ratios in the halo stars form nearly a plateau over the wide metallicity range, -2.43&lt;=[Fe/H]&lt;=0.90, indicating a common origin of Sr, Y, and Zr at the epoch of the halo formation. We find a steep decline of [Zr/Y] in the thick disk stars with increasing Ba abundance. This suggests the reduction of the production rate of Zr compared to that for Y at the active phase of the thick disk formation. The halo and thick disk stars reveal an overabundance of Zr relative to barium that grows with decreasing Ba abundance. There is a clear correlation of the [Zr/Ba] and [Eu/Ba] abundance ratios. Our observational findings for the halo and thick disk do not support the Galaxy chemical evolution models available in the literature and require to improve their predictions. The thin disk stars reveal, on average, solar abundance ratios for (Y,Zr)/Fe, (Y,Zr)/Ba, and Zr/Y. We note a slight decline of Zr/Ba and Zr/Y in these stars with increasing Ba abundance. Our results favour a dominance of the asymptotic giant branch stars in the heavy element enrichment of the interstellar gas over the epoch of the thin disk existence, in agreement with the theory of the main s-process nucleosynthesis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997#1</TD>
            <TD>2011-09-14T20:23:35Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/84/997</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/84/997</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/84/997 [2]</TD>
            <TD>Abundances of Sr, Y, Zr, Ce and Ba (Mashonkina+, 2007)</TD>
            <TD>Sr, Y, Zr, and Ce abundances are derived for the sample of 74 cool dwarfs and subgiants with the iron abundance [Fe/H] ranged between -2.43 and 0.25. The results are based on LTE (Y, Zr and Ce) and non-LTE (Sr) line formation and line profile analysis of high resolution (40000 and 60000) spectra that have a typical S/N of 50-200. The Zr/Y, Sr/Y, and Sr/Zr ratios in the halo stars form nearly a plateau over the wide metallicity range, -2.43&lt;=[Fe/H]&lt;=0.90, indicating a common origin of Sr, Y, and Zr at the epoch of the halo formation. We find a steep decline of [Zr/Y] in the thick disk stars with increasing Ba abundance. This suggests the reduction of the production rate of Zr compared to that for Y at the active phase of the thick disk formation. The halo and thick disk stars reveal an overabundance of Zr relative to barium that grows with decreasing Ba abundance. There is a clear correlation of the [Zr/Ba] and [Eu/Ba] abundance ratios. Our observational findings for the halo and thick disk do not support the Galaxy chemical evolution models available in the literature and require to improve their predictions. The thin disk stars reveal, on average, solar abundance ratios for (Y,Zr)/Fe, (Y,Zr)/Ba, and Zr/Y. We note a slight decline of Zr/Ba and Zr/Y in these stars with increasing Ba abundance. Our results favour a dominance of the asymptotic giant branch stars in the heavy element enrichment of the interstellar gas over the epoch of the thin disk existence, in agreement with the theory of the main s-process nucleosynthesis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997#2</TD>
            <TD>2011-09-14T20:23:35Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/84/997&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/84/997</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AZh/84/997 [abun]</TD>
            <TD>Abundances of Sr, Y, Zr, Ce and Ba (Mashonkina+, 2007)</TD>
            <TD>Sr, Y, Zr, and Ce abundances are derived for the sample of 74 cool dwarfs and subgiants with the iron abundance [Fe/H] ranged between -2.43 and 0.25. The results are based on LTE (Y, Zr and Ce) and non-LTE (Sr) line formation and line profile analysis of high resolution (40000 and 60000) spectra that have a typical S/N of 50-200. The Zr/Y, Sr/Y, and Sr/Zr ratios in the halo stars form nearly a plateau over the wide metallicity range, -2.43&lt;=[Fe/H]&lt;=0.90, indicating a common origin of Sr, Y, and Zr at the epoch of the halo formation. We find a steep decline of [Zr/Y] in the thick disk stars with increasing Ba abundance. This suggests the reduction of the production rate of Zr compared to that for Y at the active phase of the thick disk formation. The halo and thick disk stars reveal an overabundance of Zr relative to barium that grows with decreasing Ba abundance. There is a clear correlation of the [Zr/Ba] and [Eu/Ba] abundance ratios. Our observational findings for the halo and thick disk do not support the Galaxy chemical evolution models available in the literature and require to improve their predictions. The thin disk stars reveal, on average, solar abundance ratios for (Y,Zr)/Fe, (Y,Zr)/Ba, and Zr/Y. We note a slight decline of Zr/Ba and Zr/Y in these stars with increasing Ba abundance. Our results favour a dominance of the asymptotic giant branch stars in the heavy element enrichment of the interstellar gas over the epoch of the thin disk existence, in agreement with the theory of the main s-process nucleosynthesis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997#abun</TD>
            <TD>2011-09-14T20:23:35Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AZh/84/997&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/84/997</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/461/81 [1]</TD>
            <TD>Galaxy clusters in the CFHTLS (Olsen+, 2007)</TD>
            <TD>Galaxy cluster candidates for the four Deep fields of the CFHTLS. For each cluster we give a name, position in J2000, estimated redshift and richness, detection significance, number of redshift bins in which the candidate showed a signal, fraction of masked area around the candidate and a visual grade from A (best) to D (worst).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81#1</TD>
            <TD>2011-09-14T20:15:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/461/81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/461/81 [2]</TD>
            <TD>Galaxy clusters in the CFHTLS (Olsen+, 2007)</TD>
            <TD>Galaxy cluster candidates for the four Deep fields of the CFHTLS. For each cluster we give a name, position in J2000, estimated redshift and richness, detection significance, number of redshift bins in which the candidate showed a signal, fraction of masked area around the candidate and a visual grade from A (best) to D (worst).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81#2</TD>
            <TD>2011-09-14T20:15:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/461/81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/461/81 [table3]</TD>
            <TD>Galaxy clusters in the CFHTLS (Olsen+, 2007)</TD>
            <TD>Galaxy cluster candidates for the four Deep fields of the CFHTLS. For each cluster we give a name, position in J2000, estimated redshift and richness, detection significance, number of redshift bins in which the candidate showed a signal, fraction of masked area around the candidate and a visual grade from A (best) to D (worst).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81#table3</TD>
            <TD>2011-09-14T20:15:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/461/81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/472/121 [1]</TD>
            <TD>AMIGA V. Isolation parameters (Verley+, 2007)</TD>
            <TD>Our starting sample is the Catalogue of Isolated Galaxies (CIG). We used two parameters to estimate the influence exerted by the neighbour galaxies on the CIG galaxy: the local number density of neighbour galaxies and the tidal strength affecting the CIG galaxy. We show that both parameters together provide a comprehensive picture of the environment. For comparison, those parameters have also been derived for galaxies in denser environments such as triplets, groups and clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121#1</TD>
            <TD>2011-09-14T20:15:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/472/121</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/121</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/472/121 [2]</TD>
            <TD>AMIGA V. Isolation parameters (Verley+, 2007)</TD>
            <TD>Our starting sample is the Catalogue of Isolated Galaxies (CIG). We used two parameters to estimate the influence exerted by the neighbour galaxies on the CIG galaxy: the local number density of neighbour galaxies and the tidal strength affecting the CIG galaxy. We show that both parameters together provide a comprehensive picture of the environment. For comparison, those parameters have also been derived for galaxies in denser environments such as triplets, groups and clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121#2</TD>
            <TD>2011-09-14T20:15:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/472/121&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/472/121 [tables]</TD>
            <TD>AMIGA V. Isolation parameters (Verley+, 2007)</TD>
            <TD>Our starting sample is the Catalogue of Isolated Galaxies (CIG). We used two parameters to estimate the influence exerted by the neighbour galaxies on the CIG galaxy: the local number density of neighbour galaxies and the tidal strength affecting the CIG galaxy. We show that both parameters together provide a comprehensive picture of the environment. For comparison, those parameters have also been derived for galaxies in denser environments such as triplets, groups and clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121#tables</TD>
            <TD>2011-09-14T20:15:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/472/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/121</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/84/997 [1]</TD>
            <TD>Abundances of Sr, Y, Zr, Ce and Ba (Mashonkina+, 2007)</TD>
            <TD>Sr, Y, Zr, and Ce abundances are derived for the sample of 74 cool dwarfs and subgiants with the iron abundance [Fe/H] ranged between -2.43 and 0.25. The results are based on LTE (Y, Zr and Ce) and non-LTE (Sr) line formation and line profile analysis of high resolution (40000 and 60000) spectra that have a typical S/N of 50-200. The Zr/Y, Sr/Y, and Sr/Zr ratios in the halo stars form nearly a plateau over the wide metallicity range, -2.43&lt;=[Fe/H]&lt;=0.90, indicating a common origin of Sr, Y, and Zr at the epoch of the halo formation. We find a steep decline of [Zr/Y] in the thick disk stars with increasing Ba abundance. This suggests the reduction of the production rate of Zr compared to that for Y at the active phase of the thick disk formation. The halo and thick disk stars reveal an overabundance of Zr relative to barium that grows with decreasing Ba abundance. There is a clear correlation of the [Zr/Ba] and [Eu/Ba] abundance ratios. Our observational findings for the halo and thick disk do not support the Galaxy chemical evolution models available in the literature and require to improve their predictions. The thin disk stars reveal, on average, solar abundance ratios for (Y,Zr)/Fe, (Y,Zr)/Ba, and Zr/Y. We note a slight decline of Zr/Ba and Zr/Y in these stars with increasing Ba abundance. Our results favour a dominance of the asymptotic giant branch stars in the heavy element enrichment of the interstellar gas over the epoch of the thin disk existence, in agreement with the theory of the main s-process nucleosynthesis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997#1</TD>
            <TD>2011-09-14T20:23:35Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/84/997</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/84/997</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/84/997 [2]</TD>
            <TD>Abundances of Sr, Y, Zr, Ce and Ba (Mashonkina+, 2007)</TD>
            <TD>Sr, Y, Zr, and Ce abundances are derived for the sample of 74 cool dwarfs and subgiants with the iron abundance [Fe/H] ranged between -2.43 and 0.25. The results are based on LTE (Y, Zr and Ce) and non-LTE (Sr) line formation and line profile analysis of high resolution (40000 and 60000) spectra that have a typical S/N of 50-200. The Zr/Y, Sr/Y, and Sr/Zr ratios in the halo stars form nearly a plateau over the wide metallicity range, -2.43&lt;=[Fe/H]&lt;=0.90, indicating a common origin of Sr, Y, and Zr at the epoch of the halo formation. We find a steep decline of [Zr/Y] in the thick disk stars with increasing Ba abundance. This suggests the reduction of the production rate of Zr compared to that for Y at the active phase of the thick disk formation. The halo and thick disk stars reveal an overabundance of Zr relative to barium that grows with decreasing Ba abundance. There is a clear correlation of the [Zr/Ba] and [Eu/Ba] abundance ratios. Our observational findings for the halo and thick disk do not support the Galaxy chemical evolution models available in the literature and require to improve their predictions. The thin disk stars reveal, on average, solar abundance ratios for (Y,Zr)/Fe, (Y,Zr)/Ba, and Zr/Y. We note a slight decline of Zr/Ba and Zr/Y in these stars with increasing Ba abundance. Our results favour a dominance of the asymptotic giant branch stars in the heavy element enrichment of the interstellar gas over the epoch of the thin disk existence, in agreement with the theory of the main s-process nucleosynthesis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997#2</TD>
            <TD>2011-09-14T20:23:35Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/84/997&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/84/997</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AZh/84/997 [abun]</TD>
            <TD>Abundances of Sr, Y, Zr, Ce and Ba (Mashonkina+, 2007)</TD>
            <TD>Sr, Y, Zr, and Ce abundances are derived for the sample of 74 cool dwarfs and subgiants with the iron abundance [Fe/H] ranged between -2.43 and 0.25. The results are based on LTE (Y, Zr and Ce) and non-LTE (Sr) line formation and line profile analysis of high resolution (40000 and 60000) spectra that have a typical S/N of 50-200. The Zr/Y, Sr/Y, and Sr/Zr ratios in the halo stars form nearly a plateau over the wide metallicity range, -2.43&lt;=[Fe/H]&lt;=0.90, indicating a common origin of Sr, Y, and Zr at the epoch of the halo formation. We find a steep decline of [Zr/Y] in the thick disk stars with increasing Ba abundance. This suggests the reduction of the production rate of Zr compared to that for Y at the active phase of the thick disk formation. The halo and thick disk stars reveal an overabundance of Zr relative to barium that grows with decreasing Ba abundance. There is a clear correlation of the [Zr/Ba] and [Eu/Ba] abundance ratios. Our observational findings for the halo and thick disk do not support the Galaxy chemical evolution models available in the literature and require to improve their predictions. The thin disk stars reveal, on average, solar abundance ratios for (Y,Zr)/Fe, (Y,Zr)/Ba, and Zr/Y. We note a slight decline of Zr/Ba and Zr/Y in these stars with increasing Ba abundance. Our results favour a dominance of the asymptotic giant branch stars in the heavy element enrichment of the interstellar gas over the epoch of the thin disk existence, in agreement with the theory of the main s-process nucleosynthesis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997#abun</TD>
            <TD>2011-09-14T20:23:35Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/AZh/84/997</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AZh/84/997&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/84/997</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/472/121 [1]</TD>
            <TD>AMIGA V. Isolation parameters (Verley+, 2007)</TD>
            <TD>Our starting sample is the Catalogue of Isolated Galaxies (CIG). We used two parameters to estimate the influence exerted by the neighbour galaxies on the CIG galaxy: the local number density of neighbour galaxies and the tidal strength affecting the CIG galaxy. We show that both parameters together provide a comprehensive picture of the environment. For comparison, those parameters have also been derived for galaxies in denser environments such as triplets, groups and clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121#1</TD>
            <TD>2011-09-14T20:15:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/472/121</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/121</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/472/121 [2]</TD>
            <TD>AMIGA V. Isolation parameters (Verley+, 2007)</TD>
            <TD>Our starting sample is the Catalogue of Isolated Galaxies (CIG). We used two parameters to estimate the influence exerted by the neighbour galaxies on the CIG galaxy: the local number density of neighbour galaxies and the tidal strength affecting the CIG galaxy. We show that both parameters together provide a comprehensive picture of the environment. For comparison, those parameters have also been derived for galaxies in denser environments such as triplets, groups and clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121#2</TD>
            <TD>2011-09-14T20:15:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/472/121&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/472/121 [tables]</TD>
            <TD>AMIGA V. Isolation parameters (Verley+, 2007)</TD>
            <TD>Our starting sample is the Catalogue of Isolated Galaxies (CIG). We used two parameters to estimate the influence exerted by the neighbour galaxies on the CIG galaxy: the local number density of neighbour galaxies and the tidal strength affecting the CIG galaxy. We show that both parameters together provide a comprehensive picture of the environment. For comparison, those parameters have also been derived for galaxies in denser environments such as triplets, groups and clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121#tables</TD>
            <TD>2011-09-14T20:15:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/472/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/121</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/384/107 [1]</TD>
            <TD>VRIJHK photometry of SN 2002cv (Elias-Rosa+, 2008)</TD>
            <TD>The fact that another SN Ia, SN 2002bo, exploded in the same galaxy a few months before SN 2002cv, makes available pre-discovery optical and near-IR (NIR) data and hence templates for photometric measurements via image subtraction. SN 2002cv was observed for seven months, from day 10.7 to +205.9 relative to I-band maximum light. Here, we present the data collected by four different teams: University of California, Berkeley (USA), Imperial College (UK), Padova Observatory (INAF, Italy) and Teramo Observatory (INAF, Italy).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/107#1</TD>
            <TD>2011-09-14T20:23:50Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/107</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/384/107</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/107</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/384/107 [2]</TD>
            <TD>VRIJHK photometry of SN 2002cv (Elias-Rosa+, 2008)</TD>
            <TD>The fact that another SN Ia, SN 2002bo, exploded in the same galaxy a few months before SN 2002cv, makes available pre-discovery optical and near-IR (NIR) data and hence templates for photometric measurements via image subtraction. SN 2002cv was observed for seven months, from day 10.7 to +205.9 relative to I-band maximum light. Here, we present the data collected by four different teams: University of California, Berkeley (USA), Imperial College (UK), Padova Observatory (INAF, Italy) and Teramo Observatory (INAF, Italy).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/107#2</TD>
            <TD>2011-09-14T20:23:50Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/107</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/384/107&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/107</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/472/121 [1]</TD>
            <TD>AMIGA V. Isolation parameters (Verley+, 2007)</TD>
            <TD>Our starting sample is the Catalogue of Isolated Galaxies (CIG). We used two parameters to estimate the influence exerted by the neighbour galaxies on the CIG galaxy: the local number density of neighbour galaxies and the tidal strength affecting the CIG galaxy. We show that both parameters together provide a comprehensive picture of the environment. For comparison, those parameters have also been derived for galaxies in denser environments such as triplets, groups and clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121#1</TD>
            <TD>2011-09-14T20:15:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/472/121</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/121</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/472/121 [2]</TD>
            <TD>AMIGA V. Isolation parameters (Verley+, 2007)</TD>
            <TD>Our starting sample is the Catalogue of Isolated Galaxies (CIG). We used two parameters to estimate the influence exerted by the neighbour galaxies on the CIG galaxy: the local number density of neighbour galaxies and the tidal strength affecting the CIG galaxy. We show that both parameters together provide a comprehensive picture of the environment. For comparison, those parameters have also been derived for galaxies in denser environments such as triplets, groups and clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121#2</TD>
            <TD>2011-09-14T20:15:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/472/121&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/472/121 [tables]</TD>
            <TD>AMIGA V. Isolation parameters (Verley+, 2007)</TD>
            <TD>Our starting sample is the Catalogue of Isolated Galaxies (CIG). We used two parameters to estimate the influence exerted by the neighbour galaxies on the CIG galaxy: the local number density of neighbour galaxies and the tidal strength affecting the CIG galaxy. We show that both parameters together provide a comprehensive picture of the environment. For comparison, those parameters have also been derived for galaxies in denser environments such as triplets, groups and clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121#tables</TD>
            <TD>2011-09-14T20:15:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/472/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/121</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/384/107 [1]</TD>
            <TD>VRIJHK photometry of SN 2002cv (Elias-Rosa+, 2008)</TD>
            <TD>The fact that another SN Ia, SN 2002bo, exploded in the same galaxy a few months before SN 2002cv, makes available pre-discovery optical and near-IR (NIR) data and hence templates for photometric measurements via image subtraction. SN 2002cv was observed for seven months, from day 10.7 to +205.9 relative to I-band maximum light. Here, we present the data collected by four different teams: University of California, Berkeley (USA), Imperial College (UK), Padova Observatory (INAF, Italy) and Teramo Observatory (INAF, Italy).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/107#1</TD>
            <TD>2011-09-14T20:23:50Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/107</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/384/107</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/107</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/384/107 [2]</TD>
            <TD>VRIJHK photometry of SN 2002cv (Elias-Rosa+, 2008)</TD>
            <TD>The fact that another SN Ia, SN 2002bo, exploded in the same galaxy a few months before SN 2002cv, makes available pre-discovery optical and near-IR (NIR) data and hence templates for photometric measurements via image subtraction. SN 2002cv was observed for seven months, from day 10.7 to +205.9 relative to I-band maximum light. Here, we present the data collected by four different teams: University of California, Berkeley (USA), Imperial College (UK), Padova Observatory (INAF, Italy) and Teramo Observatory (INAF, Italy).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/107#2</TD>
            <TD>2011-09-14T20:23:50Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/107</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/384/107&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/107</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>AGES</TD>
            <TD>Arecibo Galaxy Environment Survey</TD>
            <TD>The Arecibo Galaxy Environment Survey (AGES) is an intermediate depth HI survey with the Arecibo L-band Feed Array (ALFA) multibeam instrument. When completed, it will cover an area of 200 sq. deg. to an integration time of 300 s/beam. Thirteen areas of sky have been selected, covering the full range of environments from the Local Void through isolated galaxies, galaxy pairs and galaxy groups to the Virgo Cluster. The survey products include catalogs with extracted measurements and HI parameters, as well as integrated HI spectral profiles.</TD>
            <TD>AGES consortium</TD>
            <TD>#Radio#</TD>
            <TD>ivo://ages.cardiff/ages_dr1#1</TD>
            <TD>2010-02-19T14:07:03Z</TD>
            <TD>#Galaxies#Neutral Hydrogen#Radio#Arecibo#Sky survey#ALFA#</TD>
            <TD>#Archive#</TD>
            <TD>#University#Research#</TD>
            <TD />
            <TD>1.0</TD>
            <TD>ivo://ages.cardiff/ages_dr1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://www.astro.cf.ac.uk/pub/Luca.Cortese/ages/database/public/query_simple.html</TD>
            <TD />
            <TD />
            <TD />
            <TD>http://www.naic.edu/~ages/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/135/1395 [1]</TD>
            <TD>omega Cen Spitzer photometry (Boyer+, 2008)</TD>
            <TD>This catalog presents photometry of more than 40000 sources in {omega} Centauri at 3.6, 4.5, 5.8, 8, and 24 microns from the Spitzer Space Telescope. The catalog also includes a note indicating whether a source is a candidate galaxy, asymptotic giant branch (AGB) star, anomalous RGB (RGB-a) star, or horizontal branch (HB) star. Membership information from van Leeuwen et al. (2000, &lt;J/A+A/360/472&gt;) is included along with the Leiden identification numbers (LEID). The catalog also includes a note indicating whether a source is super-Ba-rich, CN-rich, and/or is an M-type (M), carbon (C), or post-AGB (P) star, as identified by van Loon et al. (2007MNRAS.382.1353V).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395#1</TD>
            <TD>2011-09-14T20:23:52Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/135/1395</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1395</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/135/1395 [2]</TD>
            <TD>omega Cen Spitzer photometry (Boyer+, 2008)</TD>
            <TD>This catalog presents photometry of more than 40000 sources in {omega} Centauri at 3.6, 4.5, 5.8, 8, and 24 microns from the Spitzer Space Telescope. The catalog also includes a note indicating whether a source is a candidate galaxy, asymptotic giant branch (AGB) star, anomalous RGB (RGB-a) star, or horizontal branch (HB) star. Membership information from van Leeuwen et al. (2000, &lt;J/A+A/360/472&gt;) is included along with the Leiden identification numbers (LEID). The catalog also includes a note indicating whether a source is super-Ba-rich, CN-rich, and/or is an M-type (M), carbon (C), or post-AGB (P) star, as identified by van Loon et al. (2007MNRAS.382.1353V).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395#2</TD>
            <TD>2011-09-14T20:23:52Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/135/1395&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/135/1395 [catalog]</TD>
            <TD>omega Cen Spitzer photometry (Boyer+, 2008)</TD>
            <TD>This catalog presents photometry of more than 40000 sources in {omega} Centauri at 3.6, 4.5, 5.8, 8, and 24 microns from the Spitzer Space Telescope. The catalog also includes a note indicating whether a source is a candidate galaxy, asymptotic giant branch (AGB) star, anomalous RGB (RGB-a) star, or horizontal branch (HB) star. Membership information from van Leeuwen et al. (2000, &lt;J/A+A/360/472&gt;) is included along with the Leiden identification numbers (LEID). The catalog also includes a note indicating whether a source is super-Ba-rich, CN-rich, and/or is an M-type (M), carbon (C), or post-AGB (P) star, as identified by van Loon et al. (2007MNRAS.382.1353V).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395#catalog</TD>
            <TD>2011-09-14T20:23:52Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/135/1395&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>AGES</TD>
            <TD>Arecibo Galaxy Environment Survey</TD>
            <TD>The Arecibo Galaxy Environment Survey (AGES) is an intermediate depth HI survey with the Arecibo L-band Feed Array (ALFA) multibeam instrument. When completed, it will cover an area of 200 sq. deg. to an integration time of 300 s/beam. Thirteen areas of sky have been selected, covering the full range of environments from the Local Void through isolated galaxies, galaxy pairs and galaxy groups to the Virgo Cluster. The survey products include catalogs with extracted measurements and HI parameters, as well as integrated HI spectral profiles.</TD>
            <TD>AGES consortium</TD>
            <TD>#Radio#</TD>
            <TD>ivo://ages.cardiff/ages_conesearch#1</TD>
            <TD>2010-02-19T14:01:44Z</TD>
            <TD>#Galaxies#Neutral Hydrogen#Radio#Arecibo#Sky survey#ALFA#</TD>
            <TD>#Archive#</TD>
            <TD>#University#Research#</TD>
            <TD />
            <TD>1.0</TD>
            <TD>ivo://ages.cardiff/ages_conesearch</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://www.astro.cf.ac.uk/pub/Luca.Cortese/ages/database/public/cone_search.php?</TD>
            <TD>100</TD>
            <TD>200</TD>
            <TD />
            <TD>http://www.naic.edu/~ages/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/135/1395 [1]</TD>
            <TD>omega Cen Spitzer photometry (Boyer+, 2008)</TD>
            <TD>This catalog presents photometry of more than 40000 sources in {omega} Centauri at 3.6, 4.5, 5.8, 8, and 24 microns from the Spitzer Space Telescope. The catalog also includes a note indicating whether a source is a candidate galaxy, asymptotic giant branch (AGB) star, anomalous RGB (RGB-a) star, or horizontal branch (HB) star. Membership information from van Leeuwen et al. (2000, &lt;J/A+A/360/472&gt;) is included along with the Leiden identification numbers (LEID). The catalog also includes a note indicating whether a source is super-Ba-rich, CN-rich, and/or is an M-type (M), carbon (C), or post-AGB (P) star, as identified by van Loon et al. (2007MNRAS.382.1353V).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395#1</TD>
            <TD>2011-09-14T20:23:52Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/135/1395</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1395</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/135/1395 [2]</TD>
            <TD>omega Cen Spitzer photometry (Boyer+, 2008)</TD>
            <TD>This catalog presents photometry of more than 40000 sources in {omega} Centauri at 3.6, 4.5, 5.8, 8, and 24 microns from the Spitzer Space Telescope. The catalog also includes a note indicating whether a source is a candidate galaxy, asymptotic giant branch (AGB) star, anomalous RGB (RGB-a) star, or horizontal branch (HB) star. Membership information from van Leeuwen et al. (2000, &lt;J/A+A/360/472&gt;) is included along with the Leiden identification numbers (LEID). The catalog also includes a note indicating whether a source is super-Ba-rich, CN-rich, and/or is an M-type (M), carbon (C), or post-AGB (P) star, as identified by van Loon et al. (2007MNRAS.382.1353V).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395#2</TD>
            <TD>2011-09-14T20:23:52Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/135/1395&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/135/1395 [catalog]</TD>
            <TD>omega Cen Spitzer photometry (Boyer+, 2008)</TD>
            <TD>This catalog presents photometry of more than 40000 sources in {omega} Centauri at 3.6, 4.5, 5.8, 8, and 24 microns from the Spitzer Space Telescope. The catalog also includes a note indicating whether a source is a candidate galaxy, asymptotic giant branch (AGB) star, anomalous RGB (RGB-a) star, or horizontal branch (HB) star. Membership information from van Leeuwen et al. (2000, &lt;J/A+A/360/472&gt;) is included along with the Leiden identification numbers (LEID). The catalog also includes a note indicating whether a source is super-Ba-rich, CN-rich, and/or is an M-type (M), carbon (C), or post-AGB (P) star, as identified by van Loon et al. (2007MNRAS.382.1353V).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395#catalog</TD>
            <TD>2011-09-14T20:23:52Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/135/1395&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1395</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/82/197 [1]</TD>
            <TD>Mean UV Spectra of Stellar Groups (Fanelli+ 1992)</TD>
            <TD>We present a library of mean ultraviolet stellar energy distributions derived from International Ultraviolet Explorer (IUE) low-resolution spectrophotometry of 216 stars. The library is intended to facilitate interpretation of the composite UV light of stellar populations such as star clusters and galaxies. The spectra cover 1205-3185 Angstroms with a spectral resolution of approximately 6 A. The individual stellar spectra were corrected for interstellar extinction (using the Savage-Mathis law), converted to a common flux scale, and interpolated to a common wavelength scale. Stars were combined into standard groups according to their intrinsic continuum colors, observed UV spectral morphology, MK luminosity class, and metal abundance. The library consists of 56 groups: 21 dwarf (V), 8 subgiant (IV), 16 giant (III), and 11 supergiant (I+II) groups, covering O3-M4 spectral types. A metal-poor sequence is included, containing four dwarf and two giant groups, as is a metal-enhanced sequence with a single dwarf, subgiant, and giant group. More information on the library compilation and descriptions of the behaviour of spectral indices characterizing the continuum and strong absorption features are given in the paper. The spectra themselves (in the uvgroups.fit file) were previously released in the AAS CD-ROM Series Volume VII (1996); see Leitherer et al. "A Database for Galaxy Evolution Modeling" (1996PASP..108..996L).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/82/197#1</TD>
            <TD>2011-09-14T21:15:25Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/82/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/82/197</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/82/197</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/82/197 [2]</TD>
            <TD>Mean UV Spectra of Stellar Groups (Fanelli+ 1992)</TD>
            <TD>We present a library of mean ultraviolet stellar energy distributions derived from International Ultraviolet Explorer (IUE) low-resolution spectrophotometry of 216 stars. The library is intended to facilitate interpretation of the composite UV light of stellar populations such as star clusters and galaxies. The spectra cover 1205-3185 Angstroms with a spectral resolution of approximately 6 A. The individual stellar spectra were corrected for interstellar extinction (using the Savage-Mathis law), converted to a common flux scale, and interpolated to a common wavelength scale. Stars were combined into standard groups according to their intrinsic continuum colors, observed UV spectral morphology, MK luminosity class, and metal abundance. The library consists of 56 groups: 21 dwarf (V), 8 subgiant (IV), 16 giant (III), and 11 supergiant (I+II) groups, covering O3-M4 spectral types. A metal-poor sequence is included, containing four dwarf and two giant groups, as is a metal-enhanced sequence with a single dwarf, subgiant, and giant group. More information on the library compilation and descriptions of the behaviour of spectral indices characterizing the continuum and strong absorption features are given in the paper. The spectra themselves (in the uvgroups.fit file) were previously released in the AAS CD-ROM Series Volume VII (1996); see Leitherer et al. "A Database for Galaxy Evolution Modeling" (1996PASP..108..996L).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/82/197#2</TD>
            <TD>2011-09-14T21:15:25Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/82/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/82/197&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/82/197</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/590/797 [1]</TD>
            <TD>Parameters of galactic globular clusters (Van Den Bregh+, 2003)</TD>
            <TD>The relations between the luminosities M_V_, the metallicities [Fe/H], the Galactocentric radii R, and the central concentration indices c of Galactic globular clusters are discussed. It is found that the most luminous clusters rarely have collapsed cores. The reason for this might be that the core collapse timescales for such populous clusters are greater than the age of the Galaxy. Among those clusters for which the structure has not been modified by core collapse, there is a correlation between central concentration and integrated luminosity, in the sense that the most luminous clusters have the strongest central concentration. The outermost region of the Galaxy with R&gt;10kpc was apparently not able to form metal-rich ([Fe/H]&gt;-1.0) globular clusters, whereas such clusters (of which Ter 7 is the prototype) were able to form in some nearby dwarf spheroidal galaxies. It is not yet clear how the popular hypothesis that globular clusters were initially formed with a single power-law mass spectrum can be reconciled with the observation that both (1) Galactic globular clusters with R&gt;80kpc and (2) the globulars associated with the Sagittarius dwarf appear to have bimodal luminosity functions. Presently available data hint at, but are not yet able to establish, the existence of a radial metallicity gradient for metal-poor globular clusters with [Fe/H]&lt;-1.0.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797#1</TD>
            <TD>2011-09-14T20:13:13Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/590/797</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/590/797</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/590/797 [2]</TD>
            <TD>Parameters of galactic globular clusters (Van Den Bregh+, 2003)</TD>
            <TD>The relations between the luminosities M_V_, the metallicities [Fe/H], the Galactocentric radii R, and the central concentration indices c of Galactic globular clusters are discussed. It is found that the most luminous clusters rarely have collapsed cores. The reason for this might be that the core collapse timescales for such populous clusters are greater than the age of the Galaxy. Among those clusters for which the structure has not been modified by core collapse, there is a correlation between central concentration and integrated luminosity, in the sense that the most luminous clusters have the strongest central concentration. The outermost region of the Galaxy with R&gt;10kpc was apparently not able to form metal-rich ([Fe/H]&gt;-1.0) globular clusters, whereas such clusters (of which Ter 7 is the prototype) were able to form in some nearby dwarf spheroidal galaxies. It is not yet clear how the popular hypothesis that globular clusters were initially formed with a single power-law mass spectrum can be reconciled with the observation that both (1) Galactic globular clusters with R&gt;80kpc and (2) the globulars associated with the Sagittarius dwarf appear to have bimodal luminosity functions. Presently available data hint at, but are not yet able to establish, the existence of a radial metallicity gradient for metal-poor globular clusters with [Fe/H]&lt;-1.0.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797#2</TD>
            <TD>2011-09-14T20:13:13Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/590/797&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/590/797</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/590/797 [table1]</TD>
            <TD>Parameters of galactic globular clusters (Van Den Bregh+, 2003)</TD>
            <TD>The relations between the luminosities M_V_, the metallicities [Fe/H], the Galactocentric radii R, and the central concentration indices c of Galactic globular clusters are discussed. It is found that the most luminous clusters rarely have collapsed cores. The reason for this might be that the core collapse timescales for such populous clusters are greater than the age of the Galaxy. Among those clusters for which the structure has not been modified by core collapse, there is a correlation between central concentration and integrated luminosity, in the sense that the most luminous clusters have the strongest central concentration. The outermost region of the Galaxy with R&gt;10kpc was apparently not able to form metal-rich ([Fe/H]&gt;-1.0) globular clusters, whereas such clusters (of which Ter 7 is the prototype) were able to form in some nearby dwarf spheroidal galaxies. It is not yet clear how the popular hypothesis that globular clusters were initially formed with a single power-law mass spectrum can be reconciled with the observation that both (1) Galactic globular clusters with R&gt;80kpc and (2) the globulars associated with the Sagittarius dwarf appear to have bimodal luminosity functions. Presently available data hint at, but are not yet able to establish, the existence of a radial metallicity gradient for metal-poor globular clusters with [Fe/H]&lt;-1.0.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797#table1</TD>
            <TD>2011-09-14T20:13:13Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/590/797&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/590/797</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/82/197 [1]</TD>
            <TD>Mean UV Spectra of Stellar Groups (Fanelli+ 1992)</TD>
            <TD>We present a library of mean ultraviolet stellar energy distributions derived from International Ultraviolet Explorer (IUE) low-resolution spectrophotometry of 216 stars. The library is intended to facilitate interpretation of the composite UV light of stellar populations such as star clusters and galaxies. The spectra cover 1205-3185 Angstroms with a spectral resolution of approximately 6 A. The individual stellar spectra were corrected for interstellar extinction (using the Savage-Mathis law), converted to a common flux scale, and interpolated to a common wavelength scale. Stars were combined into standard groups according to their intrinsic continuum colors, observed UV spectral morphology, MK luminosity class, and metal abundance. The library consists of 56 groups: 21 dwarf (V), 8 subgiant (IV), 16 giant (III), and 11 supergiant (I+II) groups, covering O3-M4 spectral types. A metal-poor sequence is included, containing four dwarf and two giant groups, as is a metal-enhanced sequence with a single dwarf, subgiant, and giant group. More information on the library compilation and descriptions of the behaviour of spectral indices characterizing the continuum and strong absorption features are given in the paper. The spectra themselves (in the uvgroups.fit file) were previously released in the AAS CD-ROM Series Volume VII (1996); see Leitherer et al. "A Database for Galaxy Evolution Modeling" (1996PASP..108..996L).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/82/197#1</TD>
            <TD>2011-09-14T21:15:25Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/82/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/82/197</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/82/197</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/82/197 [2]</TD>
            <TD>Mean UV Spectra of Stellar Groups (Fanelli+ 1992)</TD>
            <TD>We present a library of mean ultraviolet stellar energy distributions derived from International Ultraviolet Explorer (IUE) low-resolution spectrophotometry of 216 stars. The library is intended to facilitate interpretation of the composite UV light of stellar populations such as star clusters and galaxies. The spectra cover 1205-3185 Angstroms with a spectral resolution of approximately 6 A. The individual stellar spectra were corrected for interstellar extinction (using the Savage-Mathis law), converted to a common flux scale, and interpolated to a common wavelength scale. Stars were combined into standard groups according to their intrinsic continuum colors, observed UV spectral morphology, MK luminosity class, and metal abundance. The library consists of 56 groups: 21 dwarf (V), 8 subgiant (IV), 16 giant (III), and 11 supergiant (I+II) groups, covering O3-M4 spectral types. A metal-poor sequence is included, containing four dwarf and two giant groups, as is a metal-enhanced sequence with a single dwarf, subgiant, and giant group. More information on the library compilation and descriptions of the behaviour of spectral indices characterizing the continuum and strong absorption features are given in the paper. The spectra themselves (in the uvgroups.fit file) were previously released in the AAS CD-ROM Series Volume VII (1996); see Leitherer et al. "A Database for Galaxy Evolution Modeling" (1996PASP..108..996L).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/82/197#2</TD>
            <TD>2011-09-14T21:15:25Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/82/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/82/197&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/82/197</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/135/1395 [1]</TD>
            <TD>omega Cen Spitzer photometry (Boyer+, 2008)</TD>
            <TD>This catalog presents photometry of more than 40000 sources in {omega} Centauri at 3.6, 4.5, 5.8, 8, and 24 microns from the Spitzer Space Telescope. The catalog also includes a note indicating whether a source is a candidate galaxy, asymptotic giant branch (AGB) star, anomalous RGB (RGB-a) star, or horizontal branch (HB) star. Membership information from van Leeuwen et al. (2000, &lt;J/A+A/360/472&gt;) is included along with the Leiden identification numbers (LEID). The catalog also includes a note indicating whether a source is super-Ba-rich, CN-rich, and/or is an M-type (M), carbon (C), or post-AGB (P) star, as identified by van Loon et al. (2007MNRAS.382.1353V).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395#1</TD>
            <TD>2011-09-14T20:23:52Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/135/1395</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1395</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/135/1395 [2]</TD>
            <TD>omega Cen Spitzer photometry (Boyer+, 2008)</TD>
            <TD>This catalog presents photometry of more than 40000 sources in {omega} Centauri at 3.6, 4.5, 5.8, 8, and 24 microns from the Spitzer Space Telescope. The catalog also includes a note indicating whether a source is a candidate galaxy, asymptotic giant branch (AGB) star, anomalous RGB (RGB-a) star, or horizontal branch (HB) star. Membership information from van Leeuwen et al. (2000, &lt;J/A+A/360/472&gt;) is included along with the Leiden identification numbers (LEID). The catalog also includes a note indicating whether a source is super-Ba-rich, CN-rich, and/or is an M-type (M), carbon (C), or post-AGB (P) star, as identified by van Loon et al. (2007MNRAS.382.1353V).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395#2</TD>
            <TD>2011-09-14T20:23:52Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/135/1395&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/135/1395 [catalog]</TD>
            <TD>omega Cen Spitzer photometry (Boyer+, 2008)</TD>
            <TD>This catalog presents photometry of more than 40000 sources in {omega} Centauri at 3.6, 4.5, 5.8, 8, and 24 microns from the Spitzer Space Telescope. The catalog also includes a note indicating whether a source is a candidate galaxy, asymptotic giant branch (AGB) star, anomalous RGB (RGB-a) star, or horizontal branch (HB) star. Membership information from van Leeuwen et al. (2000, &lt;J/A+A/360/472&gt;) is included along with the Leiden identification numbers (LEID). The catalog also includes a note indicating whether a source is super-Ba-rich, CN-rich, and/or is an M-type (M), carbon (C), or post-AGB (P) star, as identified by van Loon et al. (2007MNRAS.382.1353V).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395#catalog</TD>
            <TD>2011-09-14T20:23:52Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1395</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/135/1395&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1395</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/621 [1]</TD>
            <TD>Galaxy morphology in the CFRS (van den Bergh, 2001)</TD>
            <TD>The images of 229 galaxies in the Canada-France Redshift Survey have been classified on the DDO system. These observations were combined with previous classifications of galaxies with known redshifts in the Hubble Deep Field. The combined sample provides homogeneous morphological classifications for 425 galaxies of known redshift. The fraction of all galaxies that are of type E, S0, or E/S0 appears to remain approximately constant at ~17% over the redshift range 0.25&lt;z&lt;1.2. Over the same range, the fraction of irregular (Ir) galaxies increases from ~5% to ~12%. Part of this increase may be due to mild luminosity evolution of Ir galaxies. The frequency of mergers is found to rise by a factor of 2 or 3 over the redshift range covered by the present survey. These results are in qualitative agreement with those obtained previously by Brinchmann et al. (Cat. &lt;J/ApJ/499/112&gt;) using a coarser galaxy classification system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621#1</TD>
            <TD>2011-09-14T20:04:44Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/621</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/621</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/621 [2]</TD>
            <TD>Galaxy morphology in the CFRS (van den Bergh, 2001)</TD>
            <TD>The images of 229 galaxies in the Canada-France Redshift Survey have been classified on the DDO system. These observations were combined with previous classifications of galaxies with known redshifts in the Hubble Deep Field. The combined sample provides homogeneous morphological classifications for 425 galaxies of known redshift. The fraction of all galaxies that are of type E, S0, or E/S0 appears to remain approximately constant at ~17% over the redshift range 0.25&lt;z&lt;1.2. Over the same range, the fraction of irregular (Ir) galaxies increases from ~5% to ~12%. Part of this increase may be due to mild luminosity evolution of Ir galaxies. The frequency of mergers is found to rise by a factor of 2 or 3 over the redshift range covered by the present survey. These results are in qualitative agreement with those obtained previously by Brinchmann et al. (Cat. &lt;J/ApJ/499/112&gt;) using a coarser galaxy classification system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621#2</TD>
            <TD>2011-09-14T20:04:44Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/621&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/621</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/621 [table1]</TD>
            <TD>Galaxy morphology in the CFRS (van den Bergh, 2001)</TD>
            <TD>The images of 229 galaxies in the Canada-France Redshift Survey have been classified on the DDO system. These observations were combined with previous classifications of galaxies with known redshifts in the Hubble Deep Field. The combined sample provides homogeneous morphological classifications for 425 galaxies of known redshift. The fraction of all galaxies that are of type E, S0, or E/S0 appears to remain approximately constant at ~17% over the redshift range 0.25&lt;z&lt;1.2. Over the same range, the fraction of irregular (Ir) galaxies increases from ~5% to ~12%. Part of this increase may be due to mild luminosity evolution of Ir galaxies. The frequency of mergers is found to rise by a factor of 2 or 3 over the redshift range covered by the present survey. These results are in qualitative agreement with those obtained previously by Brinchmann et al. (Cat. &lt;J/ApJ/499/112&gt;) using a coarser galaxy classification system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621#table1</TD>
            <TD>2011-09-14T20:04:44Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/621</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/621&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/621</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>HDFS</TD>
            <TD>The Hubble Deep Field South</TD>
            <TD>A second Hubble Deep Field campaign was carried out between late September and October of 1998. The raw, pipeline calibrated and reprocessed data were released to the community on November 23, 1998. The rationale for undertaking a second deep field campaign followed from the wealth of information that has come out of HDF-N, and from the desire to provide a point of focus for similar studies of the distant universe from southern-hemisphere facilities. The wide public access to the HDF-N data stimulated extensive followup observations across the electromagnetic spectrum, both from major ground-based observatories and from other satellites.</TD>
            <TD>STScI</TD>
            <TD>#Optical#</TD>
            <TD>ivo://archive.stsci.edu/hdfs/SKYNODE#1</TD>
            <TD>2011-09-14T18:11:56Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD />
            <TD />
            <TD>V1.0</TD>
            <TD>ivo://archive.stsci.edu/hdfs/SKYNODE</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://galex.stsci.edu/skynode/ohdfs/nodeb.asmx</TD>
            <TD />
            <TD>0</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/192 [1]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#1</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/192</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/192 [2]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#2</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/192&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/192 [arplist]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#arplist</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/192&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/192 [arpord]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#arpord</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/192&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/192 [1]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#1</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/192</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/192 [2]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#2</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/192&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/192 [arplist]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#arplist</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/192&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/192 [arpord]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#arpord</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/192&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Rosat</TD>
            <TD>Rosat</TD>
            <TD>ROSAT, the ROentgen SATellite, was an X-ray observatory developed through a cooperative program between the Germany, the United States, and the United Kingdom. The satellite was designed and operated by Germany, and was launched by the United States on June 1, 1990. It was turned off on February 12, 1999. Power was supplied through 3 solar panels providing 1 kW of power during Sun-lit parts of the orbit, and through a rechargeable battery during the shadow phase (spacecraft night, up to 40 minutes per orbit).</TD>
            <TD>JHU</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://sdss.jhu/openskynode/Rosat#1</TD>
            <TD>2011-09-14T18:12:01Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD />
            <TD>5</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/Rosat</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/rosat/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/590/797 [1]</TD>
            <TD>Parameters of galactic globular clusters (Van Den Bregh+, 2003)</TD>
            <TD>The relations between the luminosities M_V_, the metallicities [Fe/H], the Galactocentric radii R, and the central concentration indices c of Galactic globular clusters are discussed. It is found that the most luminous clusters rarely have collapsed cores. The reason for this might be that the core collapse timescales for such populous clusters are greater than the age of the Galaxy. Among those clusters for which the structure has not been modified by core collapse, there is a correlation between central concentration and integrated luminosity, in the sense that the most luminous clusters have the strongest central concentration. The outermost region of the Galaxy with R&gt;10kpc was apparently not able to form metal-rich ([Fe/H]&gt;-1.0) globular clusters, whereas such clusters (of which Ter 7 is the prototype) were able to form in some nearby dwarf spheroidal galaxies. It is not yet clear how the popular hypothesis that globular clusters were initially formed with a single power-law mass spectrum can be reconciled with the observation that both (1) Galactic globular clusters with R&gt;80kpc and (2) the globulars associated with the Sagittarius dwarf appear to have bimodal luminosity functions. Presently available data hint at, but are not yet able to establish, the existence of a radial metallicity gradient for metal-poor globular clusters with [Fe/H]&lt;-1.0.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797#1</TD>
            <TD>2011-09-14T20:13:13Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/590/797</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/590/797</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/590/797 [2]</TD>
            <TD>Parameters of galactic globular clusters (Van Den Bregh+, 2003)</TD>
            <TD>The relations between the luminosities M_V_, the metallicities [Fe/H], the Galactocentric radii R, and the central concentration indices c of Galactic globular clusters are discussed. It is found that the most luminous clusters rarely have collapsed cores. The reason for this might be that the core collapse timescales for such populous clusters are greater than the age of the Galaxy. Among those clusters for which the structure has not been modified by core collapse, there is a correlation between central concentration and integrated luminosity, in the sense that the most luminous clusters have the strongest central concentration. The outermost region of the Galaxy with R&gt;10kpc was apparently not able to form metal-rich ([Fe/H]&gt;-1.0) globular clusters, whereas such clusters (of which Ter 7 is the prototype) were able to form in some nearby dwarf spheroidal galaxies. It is not yet clear how the popular hypothesis that globular clusters were initially formed with a single power-law mass spectrum can be reconciled with the observation that both (1) Galactic globular clusters with R&gt;80kpc and (2) the globulars associated with the Sagittarius dwarf appear to have bimodal luminosity functions. Presently available data hint at, but are not yet able to establish, the existence of a radial metallicity gradient for metal-poor globular clusters with [Fe/H]&lt;-1.0.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797#2</TD>
            <TD>2011-09-14T20:13:13Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/590/797&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/590/797</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/590/797 [table1]</TD>
            <TD>Parameters of galactic globular clusters (Van Den Bregh+, 2003)</TD>
            <TD>The relations between the luminosities M_V_, the metallicities [Fe/H], the Galactocentric radii R, and the central concentration indices c of Galactic globular clusters are discussed. It is found that the most luminous clusters rarely have collapsed cores. The reason for this might be that the core collapse timescales for such populous clusters are greater than the age of the Galaxy. Among those clusters for which the structure has not been modified by core collapse, there is a correlation between central concentration and integrated luminosity, in the sense that the most luminous clusters have the strongest central concentration. The outermost region of the Galaxy with R&gt;10kpc was apparently not able to form metal-rich ([Fe/H]&gt;-1.0) globular clusters, whereas such clusters (of which Ter 7 is the prototype) were able to form in some nearby dwarf spheroidal galaxies. It is not yet clear how the popular hypothesis that globular clusters were initially formed with a single power-law mass spectrum can be reconciled with the observation that both (1) Galactic globular clusters with R&gt;80kpc and (2) the globulars associated with the Sagittarius dwarf appear to have bimodal luminosity functions. Presently available data hint at, but are not yet able to establish, the existence of a radial metallicity gradient for metal-poor globular clusters with [Fe/H]&lt;-1.0.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797#table1</TD>
            <TD>2011-09-14T20:13:13Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/590/797&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/590/797</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/192 [1]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#1</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/192</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/192 [2]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#2</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/192&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/192 [arplist]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#arplist</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/192&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/192 [arpord]</TD>
            <TD>Arp's Peculiar Galaxies (Webb 1996)</TD>
            <TD>Halton C. Arp photographed 338 views of notable peculiar galaxies and published them as his 1966 "Atlas of Peculiar Galaxies." Since then, galaxy catalogs have named 585 of the involved galaxies. This contemporary index collects names and characteristics of the involved objects for use by contemporary observers of the historical views.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/192#arpord</TD>
            <TD>2011-09-14T20:31:49Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/192</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/192&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/192</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/590/797 [1]</TD>
            <TD>Parameters of galactic globular clusters (Van Den Bregh+, 2003)</TD>
            <TD>The relations between the luminosities M_V_, the metallicities [Fe/H], the Galactocentric radii R, and the central concentration indices c of Galactic globular clusters are discussed. It is found that the most luminous clusters rarely have collapsed cores. The reason for this might be that the core collapse timescales for such populous clusters are greater than the age of the Galaxy. Among those clusters for which the structure has not been modified by core collapse, there is a correlation between central concentration and integrated luminosity, in the sense that the most luminous clusters have the strongest central concentration. The outermost region of the Galaxy with R&gt;10kpc was apparently not able to form metal-rich ([Fe/H]&gt;-1.0) globular clusters, whereas such clusters (of which Ter 7 is the prototype) were able to form in some nearby dwarf spheroidal galaxies. It is not yet clear how the popular hypothesis that globular clusters were initially formed with a single power-law mass spectrum can be reconciled with the observation that both (1) Galactic globular clusters with R&gt;80kpc and (2) the globulars associated with the Sagittarius dwarf appear to have bimodal luminosity functions. Presently available data hint at, but are not yet able to establish, the existence of a radial metallicity gradient for metal-poor globular clusters with [Fe/H]&lt;-1.0.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/590/797#1</TD>
            <TD>2011-09-14T20:13:13Z</TD>
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            <TD>22-Aug-2007</TD>
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            <TD>WebBrowser</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/590/797 [2]</TD>
            <TD>Parameters of galactic globular clusters (Van Den Bregh+, 2003)</TD>
            <TD>The relations between the luminosities M_V_, the metallicities [Fe/H], the Galactocentric radii R, and the central concentration indices c of Galactic globular clusters are discussed. It is found that the most luminous clusters rarely have collapsed cores. The reason for this might be that the core collapse timescales for such populous clusters are greater than the age of the Galaxy. Among those clusters for which the structure has not been modified by core collapse, there is a correlation between central concentration and integrated luminosity, in the sense that the most luminous clusters have the strongest central concentration. The outermost region of the Galaxy with R&gt;10kpc was apparently not able to form metal-rich ([Fe/H]&gt;-1.0) globular clusters, whereas such clusters (of which Ter 7 is the prototype) were able to form in some nearby dwarf spheroidal galaxies. It is not yet clear how the popular hypothesis that globular clusters were initially formed with a single power-law mass spectrum can be reconciled with the observation that both (1) Galactic globular clusters with R&gt;80kpc and (2) the globulars associated with the Sagittarius dwarf appear to have bimodal luminosity functions. Presently available data hint at, but are not yet able to establish, the existence of a radial metallicity gradient for metal-poor globular clusters with [Fe/H]&lt;-1.0.</TD>
            <TD>CDS</TD>
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            <TD>J/ApJ/590/797 [table1]</TD>
            <TD>Parameters of galactic globular clusters (Van Den Bregh+, 2003)</TD>
            <TD>The relations between the luminosities M_V_, the metallicities [Fe/H], the Galactocentric radii R, and the central concentration indices c of Galactic globular clusters are discussed. It is found that the most luminous clusters rarely have collapsed cores. The reason for this might be that the core collapse timescales for such populous clusters are greater than the age of the Galaxy. Among those clusters for which the structure has not been modified by core collapse, there is a correlation between central concentration and integrated luminosity, in the sense that the most luminous clusters have the strongest central concentration. The outermost region of the Galaxy with R&gt;10kpc was apparently not able to form metal-rich ([Fe/H]&gt;-1.0) globular clusters, whereas such clusters (of which Ter 7 is the prototype) were able to form in some nearby dwarf spheroidal galaxies. It is not yet clear how the popular hypothesis that globular clusters were initially formed with a single power-law mass spectrum can be reconciled with the observation that both (1) Galactic globular clusters with R&gt;80kpc and (2) the globulars associated with the Sagittarius dwarf appear to have bimodal luminosity functions. Presently available data hint at, but are not yet able to establish, the existence of a radial metallicity gradient for metal-poor globular clusters with [Fe/H]&lt;-1.0.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/590/797</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/167/1 [1]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T20:32:37Z</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/167/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/167/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/167/1 [2]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/167/1 [table3]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/167/1&amp;</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJS/167/1 [table4]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/167/1&amp;</TD>
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            <TD>Web Page</TD>
            <TD>J/A+AS/141/449 [1]</TD>
            <TD>Coma cluster early-type galaxies (Mehlert+, 2000)</TD>
            <TD>Table 1 describes the photometric properties (R-band magnitude, effective radius, surface brightness, a_4_, ellipticity) of all 35 Coma cluster galaxies, which are investigated spectroscopically in this work. Besides the galaxy numbers given by Godwin et al. (1983, Cat. &lt;VII/42&gt;, GMP83), we also list the NGC/IC numbers as well as Dressler's numbers given in Dressler et al. (1987ApJ...313...42D, D87). Additionally the galaxy type as well as there distance to the clusters center are given. Table 5 to Table 12 (photom.dat) give the results from surface brightness and isophotal shape analysis (local surface brightness, ellipticity, position angle and Fourier coefficients along the major axis) for 8 galaxies of the sample derived from Kron Cousins R band photometry. Table 13 to Table 47 (kinema.dat) give spatially resolved kinematic parameter (v, sigma, H_3_, H_4_) for all 35 galaxies while in Table 48 to Table 82 (indice1.dat and indice2.dat) we list the radial profiles of the measured line indices (H_beta_, Mg, Fe, NaD) of these galaxies. Table 4 contains the results from the comparison of our mean data within the circular standard aperture (see paper) with the mean values given by Joergensen (1999MNRAS.306..607J, J99).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS.VizieR/J/A+AS/141/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/449</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/449</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/449 [2]</TD>
            <TD>Coma cluster early-type galaxies (Mehlert+, 2000)</TD>
            <TD>Table 1 describes the photometric properties (R-band magnitude, effective radius, surface brightness, a_4_, ellipticity) of all 35 Coma cluster galaxies, which are investigated spectroscopically in this work. Besides the galaxy numbers given by Godwin et al. (1983, Cat. &lt;VII/42&gt;, GMP83), we also list the NGC/IC numbers as well as Dressler's numbers given in Dressler et al. (1987ApJ...313...42D, D87). Additionally the galaxy type as well as there distance to the clusters center are given. Table 5 to Table 12 (photom.dat) give the results from surface brightness and isophotal shape analysis (local surface brightness, ellipticity, position angle and Fourier coefficients along the major axis) for 8 galaxies of the sample derived from Kron Cousins R band photometry. Table 13 to Table 47 (kinema.dat) give spatially resolved kinematic parameter (v, sigma, H_3_, H_4_) for all 35 galaxies while in Table 48 to Table 82 (indice1.dat and indice2.dat) we list the radial profiles of the measured line indices (H_beta_, Mg, Fe, NaD) of these galaxies. Table 4 contains the results from the comparison of our mean data within the circular standard aperture (see paper) with the mean values given by Joergensen (1999MNRAS.306..607J, J99).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>10-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/449&amp;</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/449 [table1]</TD>
            <TD>Coma cluster early-type galaxies (Mehlert+, 2000)</TD>
            <TD>Table 1 describes the photometric properties (R-band magnitude, effective radius, surface brightness, a_4_, ellipticity) of all 35 Coma cluster galaxies, which are investigated spectroscopically in this work. Besides the galaxy numbers given by Godwin et al. (1983, Cat. &lt;VII/42&gt;, GMP83), we also list the NGC/IC numbers as well as Dressler's numbers given in Dressler et al. (1987ApJ...313...42D, D87). Additionally the galaxy type as well as there distance to the clusters center are given. Table 5 to Table 12 (photom.dat) give the results from surface brightness and isophotal shape analysis (local surface brightness, ellipticity, position angle and Fourier coefficients along the major axis) for 8 galaxies of the sample derived from Kron Cousins R band photometry. Table 13 to Table 47 (kinema.dat) give spatially resolved kinematic parameter (v, sigma, H_3_, H_4_) for all 35 galaxies while in Table 48 to Table 82 (indice1.dat and indice2.dat) we list the radial profiles of the measured line indices (H_beta_, Mg, Fe, NaD) of these galaxies. Table 4 contains the results from the comparison of our mean data within the circular standard aperture (see paper) with the mean values given by Joergensen (1999MNRAS.306..607J, J99).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/449&amp;</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/449</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/449 [1]</TD>
            <TD>Coma cluster early-type galaxies (Mehlert+, 2000)</TD>
            <TD>Table 1 describes the photometric properties (R-band magnitude, effective radius, surface brightness, a_4_, ellipticity) of all 35 Coma cluster galaxies, which are investigated spectroscopically in this work. Besides the galaxy numbers given by Godwin et al. (1983, Cat. &lt;VII/42&gt;, GMP83), we also list the NGC/IC numbers as well as Dressler's numbers given in Dressler et al. (1987ApJ...313...42D, D87). Additionally the galaxy type as well as there distance to the clusters center are given. Table 5 to Table 12 (photom.dat) give the results from surface brightness and isophotal shape analysis (local surface brightness, ellipticity, position angle and Fourier coefficients along the major axis) for 8 galaxies of the sample derived from Kron Cousins R band photometry. Table 13 to Table 47 (kinema.dat) give spatially resolved kinematic parameter (v, sigma, H_3_, H_4_) for all 35 galaxies while in Table 48 to Table 82 (indice1.dat and indice2.dat) we list the radial profiles of the measured line indices (H_beta_, Mg, Fe, NaD) of these galaxies. Table 4 contains the results from the comparison of our mean data within the circular standard aperture (see paper) with the mean values given by Joergensen (1999MNRAS.306..607J, J99).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449#1</TD>
            <TD>2011-09-14T20:14:23Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>10-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/449</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/449</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/449 [2]</TD>
            <TD>Coma cluster early-type galaxies (Mehlert+, 2000)</TD>
            <TD>Table 1 describes the photometric properties (R-band magnitude, effective radius, surface brightness, a_4_, ellipticity) of all 35 Coma cluster galaxies, which are investigated spectroscopically in this work. Besides the galaxy numbers given by Godwin et al. (1983, Cat. &lt;VII/42&gt;, GMP83), we also list the NGC/IC numbers as well as Dressler's numbers given in Dressler et al. (1987ApJ...313...42D, D87). Additionally the galaxy type as well as there distance to the clusters center are given. Table 5 to Table 12 (photom.dat) give the results from surface brightness and isophotal shape analysis (local surface brightness, ellipticity, position angle and Fourier coefficients along the major axis) for 8 galaxies of the sample derived from Kron Cousins R band photometry. Table 13 to Table 47 (kinema.dat) give spatially resolved kinematic parameter (v, sigma, H_3_, H_4_) for all 35 galaxies while in Table 48 to Table 82 (indice1.dat and indice2.dat) we list the radial profiles of the measured line indices (H_beta_, Mg, Fe, NaD) of these galaxies. Table 4 contains the results from the comparison of our mean data within the circular standard aperture (see paper) with the mean values given by Joergensen (1999MNRAS.306..607J, J99).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449#2</TD>
            <TD>2011-09-14T20:14:23Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/449&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/449 [table1]</TD>
            <TD>Coma cluster early-type galaxies (Mehlert+, 2000)</TD>
            <TD>Table 1 describes the photometric properties (R-band magnitude, effective radius, surface brightness, a_4_, ellipticity) of all 35 Coma cluster galaxies, which are investigated spectroscopically in this work. Besides the galaxy numbers given by Godwin et al. (1983, Cat. &lt;VII/42&gt;, GMP83), we also list the NGC/IC numbers as well as Dressler's numbers given in Dressler et al. (1987ApJ...313...42D, D87). Additionally the galaxy type as well as there distance to the clusters center are given. Table 5 to Table 12 (photom.dat) give the results from surface brightness and isophotal shape analysis (local surface brightness, ellipticity, position angle and Fourier coefficients along the major axis) for 8 galaxies of the sample derived from Kron Cousins R band photometry. Table 13 to Table 47 (kinema.dat) give spatially resolved kinematic parameter (v, sigma, H_3_, H_4_) for all 35 galaxies while in Table 48 to Table 82 (indice1.dat and indice2.dat) we list the radial profiles of the measured line indices (H_beta_, Mg, Fe, NaD) of these galaxies. Table 4 contains the results from the comparison of our mean data within the circular standard aperture (see paper) with the mean values given by Joergensen (1999MNRAS.306..607J, J99).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449#table1</TD>
            <TD>2011-09-14T20:14:23Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
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            <TD>#Research#</TD>
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            <TD>10-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/449</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/481 [1]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#1</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/481</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/481 [2]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#2</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/481&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/481 [galaxies]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#galaxies</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/481&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/481 [table3]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#table3</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/481&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/449 [1]</TD>
            <TD>Coma cluster early-type galaxies (Mehlert+, 2000)</TD>
            <TD>Table 1 describes the photometric properties (R-band magnitude, effective radius, surface brightness, a_4_, ellipticity) of all 35 Coma cluster galaxies, which are investigated spectroscopically in this work. Besides the galaxy numbers given by Godwin et al. (1983, Cat. &lt;VII/42&gt;, GMP83), we also list the NGC/IC numbers as well as Dressler's numbers given in Dressler et al. (1987ApJ...313...42D, D87). Additionally the galaxy type as well as there distance to the clusters center are given. Table 5 to Table 12 (photom.dat) give the results from surface brightness and isophotal shape analysis (local surface brightness, ellipticity, position angle and Fourier coefficients along the major axis) for 8 galaxies of the sample derived from Kron Cousins R band photometry. Table 13 to Table 47 (kinema.dat) give spatially resolved kinematic parameter (v, sigma, H_3_, H_4_) for all 35 galaxies while in Table 48 to Table 82 (indice1.dat and indice2.dat) we list the radial profiles of the measured line indices (H_beta_, Mg, Fe, NaD) of these galaxies. Table 4 contains the results from the comparison of our mean data within the circular standard aperture (see paper) with the mean values given by Joergensen (1999MNRAS.306..607J, J99).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449#1</TD>
            <TD>2011-09-14T20:14:23Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/449</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/449</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/449 [2]</TD>
            <TD>Coma cluster early-type galaxies (Mehlert+, 2000)</TD>
            <TD>Table 1 describes the photometric properties (R-band magnitude, effective radius, surface brightness, a_4_, ellipticity) of all 35 Coma cluster galaxies, which are investigated spectroscopically in this work. Besides the galaxy numbers given by Godwin et al. (1983, Cat. &lt;VII/42&gt;, GMP83), we also list the NGC/IC numbers as well as Dressler's numbers given in Dressler et al. (1987ApJ...313...42D, D87). Additionally the galaxy type as well as there distance to the clusters center are given. Table 5 to Table 12 (photom.dat) give the results from surface brightness and isophotal shape analysis (local surface brightness, ellipticity, position angle and Fourier coefficients along the major axis) for 8 galaxies of the sample derived from Kron Cousins R band photometry. Table 13 to Table 47 (kinema.dat) give spatially resolved kinematic parameter (v, sigma, H_3_, H_4_) for all 35 galaxies while in Table 48 to Table 82 (indice1.dat and indice2.dat) we list the radial profiles of the measured line indices (H_beta_, Mg, Fe, NaD) of these galaxies. Table 4 contains the results from the comparison of our mean data within the circular standard aperture (see paper) with the mean values given by Joergensen (1999MNRAS.306..607J, J99).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449#2</TD>
            <TD>2011-09-14T20:14:23Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/449&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/449 [table1]</TD>
            <TD>Coma cluster early-type galaxies (Mehlert+, 2000)</TD>
            <TD>Table 1 describes the photometric properties (R-band magnitude, effective radius, surface brightness, a_4_, ellipticity) of all 35 Coma cluster galaxies, which are investigated spectroscopically in this work. Besides the galaxy numbers given by Godwin et al. (1983, Cat. &lt;VII/42&gt;, GMP83), we also list the NGC/IC numbers as well as Dressler's numbers given in Dressler et al. (1987ApJ...313...42D, D87). Additionally the galaxy type as well as there distance to the clusters center are given. Table 5 to Table 12 (photom.dat) give the results from surface brightness and isophotal shape analysis (local surface brightness, ellipticity, position angle and Fourier coefficients along the major axis) for 8 galaxies of the sample derived from Kron Cousins R band photometry. Table 13 to Table 47 (kinema.dat) give spatially resolved kinematic parameter (v, sigma, H_3_, H_4_) for all 35 galaxies while in Table 48 to Table 82 (indice1.dat and indice2.dat) we list the radial profiles of the measured line indices (H_beta_, Mg, Fe, NaD) of these galaxies. Table 4 contains the results from the comparison of our mean data within the circular standard aperture (see paper) with the mean values given by Joergensen (1999MNRAS.306..607J, J99).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449#table1</TD>
            <TD>2011-09-14T20:14:23Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/449</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/167/1 [1]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1#1</TD>
            <TD>2011-09-14T20:32:37Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/167/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/167/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/167/1 [2]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1#2</TD>
            <TD>2011-09-14T20:32:37Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/167/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/167/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/167/1 [table3]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1#table3</TD>
            <TD>2011-09-14T20:32:37Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/167/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/167/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/167/1 [table4]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1#table4</TD>
            <TD>2011-09-14T20:32:37Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/167/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/167/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/472/101 [1]</TD>
            <TD>Chemical evolution of SMC planetary nebulae (Idiart+, 2007)</TD>
            <TD>We investigate the chemical evolution of the Small Magellanic Cloud (SMC) based on abundance data of planetary nebulae (PNe). The main goal is to investigate the time evolution of the oxygen abundance in this galaxy by deriving an age-metallicity relation. Such a relation is of fundamental importance as an observational constraint for chemical evolution models of the SMC. We have used high quality PNe data to derive the properties of the progenitor stars, so that the stellar ages could be estimated. We collected a large number of measured spectral fluxes for each nebula and derived accurate physical parameters and nebular abundances. New spectral data for a sample of SMC PNe obtained between 1999 and 2002 are also presented. These data are used with data available in the literature to improve the accuracy of the fluxes for each spectral line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101#1</TD>
            <TD>2011-09-14T20:15:11Z</TD>
            <TD>#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/472/101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/472/101 [2]</TD>
            <TD>Chemical evolution of SMC planetary nebulae (Idiart+, 2007)</TD>
            <TD>We investigate the chemical evolution of the Small Magellanic Cloud (SMC) based on abundance data of planetary nebulae (PNe). The main goal is to investigate the time evolution of the oxygen abundance in this galaxy by deriving an age-metallicity relation. Such a relation is of fundamental importance as an observational constraint for chemical evolution models of the SMC. We have used high quality PNe data to derive the properties of the progenitor stars, so that the stellar ages could be estimated. We collected a large number of measured spectral fluxes for each nebula and derived accurate physical parameters and nebular abundances. New spectral data for a sample of SMC PNe obtained between 1999 and 2002 are also presented. These data are used with data available in the literature to improve the accuracy of the fluxes for each spectral line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101#2</TD>
            <TD>2011-09-14T20:15:11Z</TD>
            <TD>#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/472/101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/472/101 [table7]</TD>
            <TD>Chemical evolution of SMC planetary nebulae (Idiart+, 2007)</TD>
            <TD>We investigate the chemical evolution of the Small Magellanic Cloud (SMC) based on abundance data of planetary nebulae (PNe). The main goal is to investigate the time evolution of the oxygen abundance in this galaxy by deriving an age-metallicity relation. Such a relation is of fundamental importance as an observational constraint for chemical evolution models of the SMC. We have used high quality PNe data to derive the properties of the progenitor stars, so that the stellar ages could be estimated. We collected a large number of measured spectral fluxes for each nebula and derived accurate physical parameters and nebular abundances. New spectral data for a sample of SMC PNe obtained between 1999 and 2002 are also presented. These data are used with data available in the literature to improve the accuracy of the fluxes for each spectral line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101#table7</TD>
            <TD>2011-09-14T20:15:11Z</TD>
            <TD>#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/472/101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/167/1 [1]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1#1</TD>
            <TD>2011-09-14T20:32:37Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/167/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/167/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/167/1 [2]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1#2</TD>
            <TD>2011-09-14T20:32:37Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/167/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/167/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/167/1 [table3]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1#table3</TD>
            <TD>2011-09-14T20:32:37Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/167/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/167/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/167/1 [table4]</TD>
            <TD>Galaxy groups and clusters from SDSS (Berlind+, 2006)</TD>
            <TD>We identify galaxy groups and clusters in volume-limited samples of the Sloan Digital Sky Survey (SDSS) redshift survey, using a redshift-space friends-of-friends algorithm. We optimize the friends-of-friends linking lengths to recover galaxy systems that occupy the same dark matter halos, using a set of mock catalogs created by populating halos of N-body simulations with galaxies. Extensive tests with these mock catalogs show that no combination of perpendicular and line-of-sight linking lengths is able to yield groups and clusters that simultaneously recover the true halo multiplicity function, projected size distribution, and velocity dispersion. We adopt a linking length combination that yields, for galaxy groups with 10 or more members: a group multiplicity function that is unbiased with respect to the true halo multiplicity function; an unbiased median relation between the multiplicities of groups and their associated halos; a spurious group fraction of less than ~1%; a halo completeness of more than 97%; the correct projected size distribution as a function of multiplicity; and a velocity dispersion distribution that is ~20% too low at all multiplicities. These results hold over a range of mock catalogs that use different input recipes of populating halos with galaxies. We apply our group-finding algorithm to the SDSS data and obtain three group and cluster catalogs for three volume-limited samples that cover 3495.1deg^2^ on the sky, go out to redshifts of 0.1, 0.068, and 0.045, and contain 57138, 37820, and 18895 galaxies, respectively. We correct for incompleteness caused by fiber collisions and survey edges and obtain measurements of the group multiplicity function, with errors calculated from realistic mock catalogs. These multiplicity function measurements provide a key constraint on the relation between galaxy populations and dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1#table4</TD>
            <TD>2011-09-14T20:32:37Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/167/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/167/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/167/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/472/101 [1]</TD>
            <TD>Chemical evolution of SMC planetary nebulae (Idiart+, 2007)</TD>
            <TD>We investigate the chemical evolution of the Small Magellanic Cloud (SMC) based on abundance data of planetary nebulae (PNe). The main goal is to investigate the time evolution of the oxygen abundance in this galaxy by deriving an age-metallicity relation. Such a relation is of fundamental importance as an observational constraint for chemical evolution models of the SMC. We have used high quality PNe data to derive the properties of the progenitor stars, so that the stellar ages could be estimated. We collected a large number of measured spectral fluxes for each nebula and derived accurate physical parameters and nebular abundances. New spectral data for a sample of SMC PNe obtained between 1999 and 2002 are also presented. These data are used with data available in the literature to improve the accuracy of the fluxes for each spectral line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101#1</TD>
            <TD>2011-09-14T20:15:11Z</TD>
            <TD>#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/472/101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/472/101 [2]</TD>
            <TD>Chemical evolution of SMC planetary nebulae (Idiart+, 2007)</TD>
            <TD>We investigate the chemical evolution of the Small Magellanic Cloud (SMC) based on abundance data of planetary nebulae (PNe). The main goal is to investigate the time evolution of the oxygen abundance in this galaxy by deriving an age-metallicity relation. Such a relation is of fundamental importance as an observational constraint for chemical evolution models of the SMC. We have used high quality PNe data to derive the properties of the progenitor stars, so that the stellar ages could be estimated. We collected a large number of measured spectral fluxes for each nebula and derived accurate physical parameters and nebular abundances. New spectral data for a sample of SMC PNe obtained between 1999 and 2002 are also presented. These data are used with data available in the literature to improve the accuracy of the fluxes for each spectral line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101#2</TD>
            <TD>2011-09-14T20:15:11Z</TD>
            <TD>#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/472/101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/472/101 [table7]</TD>
            <TD>Chemical evolution of SMC planetary nebulae (Idiart+, 2007)</TD>
            <TD>We investigate the chemical evolution of the Small Magellanic Cloud (SMC) based on abundance data of planetary nebulae (PNe). The main goal is to investigate the time evolution of the oxygen abundance in this galaxy by deriving an age-metallicity relation. Such a relation is of fundamental importance as an observational constraint for chemical evolution models of the SMC. We have used high quality PNe data to derive the properties of the progenitor stars, so that the stellar ages could be estimated. We collected a large number of measured spectral fluxes for each nebula and derived accurate physical parameters and nebular abundances. New spectral data for a sample of SMC PNe obtained between 1999 and 2002 are also presented. These data are used with data available in the literature to improve the accuracy of the fluxes for each spectral line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101#table7</TD>
            <TD>2011-09-14T20:15:11Z</TD>
            <TD>#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/472/101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/493/913 [1]</TD>
            <TD>Abundances of 9 HB stars in NGC 6352 (Feltzing+, 2009)</TD>
            <TD>Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of alpha-elements in the clusters and the amount of alpha-elements is well known to influence the derivation of ages for globular clusters. We present a study of elemental abundances for alpha and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. We find that NGC 6352 has [Fe/H]=-0.55, is enhanced in the alpha-elements to about +0.2dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B-V)=0.24 and (m-M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913#1</TD>
            <TD>2011-09-14T20:32:53Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/493/913</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/493/913</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/493/913 [2]</TD>
            <TD>Abundances of 9 HB stars in NGC 6352 (Feltzing+, 2009)</TD>
            <TD>Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of alpha-elements in the clusters and the amount of alpha-elements is well known to influence the derivation of ages for globular clusters. We present a study of elemental abundances for alpha and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. We find that NGC 6352 has [Fe/H]=-0.55, is enhanced in the alpha-elements to about +0.2dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B-V)=0.24 and (m-M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913#2</TD>
            <TD>2011-09-14T20:32:53Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/493/913&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/493/913</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/493/913 [table1]</TD>
            <TD>Abundances of 9 HB stars in NGC 6352 (Feltzing+, 2009)</TD>
            <TD>Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of alpha-elements in the clusters and the amount of alpha-elements is well known to influence the derivation of ages for globular clusters. We present a study of elemental abundances for alpha and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. We find that NGC 6352 has [Fe/H]=-0.55, is enhanced in the alpha-elements to about +0.2dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B-V)=0.24 and (m-M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913#table1</TD>
            <TD>2011-09-14T20:32:53Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>23-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/493/913</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/472/101 [1]</TD>
            <TD>Chemical evolution of SMC planetary nebulae (Idiart+, 2007)</TD>
            <TD>We investigate the chemical evolution of the Small Magellanic Cloud (SMC) based on abundance data of planetary nebulae (PNe). The main goal is to investigate the time evolution of the oxygen abundance in this galaxy by deriving an age-metallicity relation. Such a relation is of fundamental importance as an observational constraint for chemical evolution models of the SMC. We have used high quality PNe data to derive the properties of the progenitor stars, so that the stellar ages could be estimated. We collected a large number of measured spectral fluxes for each nebula and derived accurate physical parameters and nebular abundances. New spectral data for a sample of SMC PNe obtained between 1999 and 2002 are also presented. These data are used with data available in the literature to improve the accuracy of the fluxes for each spectral line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101#1</TD>
            <TD>2011-09-14T20:15:11Z</TD>
            <TD>#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/472/101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/472/101 [2]</TD>
            <TD>Chemical evolution of SMC planetary nebulae (Idiart+, 2007)</TD>
            <TD>We investigate the chemical evolution of the Small Magellanic Cloud (SMC) based on abundance data of planetary nebulae (PNe). The main goal is to investigate the time evolution of the oxygen abundance in this galaxy by deriving an age-metallicity relation. Such a relation is of fundamental importance as an observational constraint for chemical evolution models of the SMC. We have used high quality PNe data to derive the properties of the progenitor stars, so that the stellar ages could be estimated. We collected a large number of measured spectral fluxes for each nebula and derived accurate physical parameters and nebular abundances. New spectral data for a sample of SMC PNe obtained between 1999 and 2002 are also presented. These data are used with data available in the literature to improve the accuracy of the fluxes for each spectral line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101#2</TD>
            <TD>2011-09-14T20:15:11Z</TD>
            <TD>#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/472/101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/472/101 [table7]</TD>
            <TD>Chemical evolution of SMC planetary nebulae (Idiart+, 2007)</TD>
            <TD>We investigate the chemical evolution of the Small Magellanic Cloud (SMC) based on abundance data of planetary nebulae (PNe). The main goal is to investigate the time evolution of the oxygen abundance in this galaxy by deriving an age-metallicity relation. Such a relation is of fundamental importance as an observational constraint for chemical evolution models of the SMC. We have used high quality PNe data to derive the properties of the progenitor stars, so that the stellar ages could be estimated. We collected a large number of measured spectral fluxes for each nebula and derived accurate physical parameters and nebular abundances. New spectral data for a sample of SMC PNe obtained between 1999 and 2002 are also presented. These data are used with data available in the literature to improve the accuracy of the fluxes for each spectral line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101#table7</TD>
            <TD>2011-09-14T20:15:11Z</TD>
            <TD>#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/472/101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/472/101&amp;</TD>
            <TD>180</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/472/101</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/493/913 [1]</TD>
            <TD>Abundances of 9 HB stars in NGC 6352 (Feltzing+, 2009)</TD>
            <TD>Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of alpha-elements in the clusters and the amount of alpha-elements is well known to influence the derivation of ages for globular clusters. We present a study of elemental abundances for alpha and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. We find that NGC 6352 has [Fe/H]=-0.55, is enhanced in the alpha-elements to about +0.2dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B-V)=0.24 and (m-M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913#1</TD>
            <TD>2011-09-14T20:32:53Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/493/913</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/493/913</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/493/913 [2]</TD>
            <TD>Abundances of 9 HB stars in NGC 6352 (Feltzing+, 2009)</TD>
            <TD>Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of alpha-elements in the clusters and the amount of alpha-elements is well known to influence the derivation of ages for globular clusters. We present a study of elemental abundances for alpha and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. We find that NGC 6352 has [Fe/H]=-0.55, is enhanced in the alpha-elements to about +0.2dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B-V)=0.24 and (m-M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913#2</TD>
            <TD>2011-09-14T20:32:53Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/493/913&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/493/913</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/493/913 [table1]</TD>
            <TD>Abundances of 9 HB stars in NGC 6352 (Feltzing+, 2009)</TD>
            <TD>Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of alpha-elements in the clusters and the amount of alpha-elements is well known to influence the derivation of ages for globular clusters. We present a study of elemental abundances for alpha and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. We find that NGC 6352 has [Fe/H]=-0.55, is enhanced in the alpha-elements to about +0.2dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B-V)=0.24 and (m-M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913#table1</TD>
            <TD>2011-09-14T20:32:53Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/493/913&amp;</TD>
            <TD>180</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/493/913</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/cgps [1]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/cgps#1</TD>
            <TD>2011-09-14T20:15:27Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/B/cgps</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/cgps</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/cgps</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/cgps [2]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/cgps#2</TD>
            <TD>2011-09-14T20:15:27Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/B/cgps</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/cgps&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/cgps</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/493/913 [1]</TD>
            <TD>Abundances of 9 HB stars in NGC 6352 (Feltzing+, 2009)</TD>
            <TD>Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of alpha-elements in the clusters and the amount of alpha-elements is well known to influence the derivation of ages for globular clusters. We present a study of elemental abundances for alpha and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. We find that NGC 6352 has [Fe/H]=-0.55, is enhanced in the alpha-elements to about +0.2dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B-V)=0.24 and (m-M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913#1</TD>
            <TD>2011-09-14T20:32:53Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/493/913</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/493/913</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/493/913 [2]</TD>
            <TD>Abundances of 9 HB stars in NGC 6352 (Feltzing+, 2009)</TD>
            <TD>Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of alpha-elements in the clusters and the amount of alpha-elements is well known to influence the derivation of ages for globular clusters. We present a study of elemental abundances for alpha and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. We find that NGC 6352 has [Fe/H]=-0.55, is enhanced in the alpha-elements to about +0.2dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B-V)=0.24 and (m-M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913#2</TD>
            <TD>2011-09-14T20:32:53Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/493/913&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/493/913</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/493/913 [table1]</TD>
            <TD>Abundances of 9 HB stars in NGC 6352 (Feltzing+, 2009)</TD>
            <TD>Metal-rich globular clusters provide important tracers of the formation of our Galaxy. Moreover, and not less important, they are very important calibrators for the derivation of properties of extra-galactic metal-rich stellar populations. Nonetheless, only a few of the metal-rich globular clusters in the Milky Way have been studied using high-resolution stellar spectra to derive elemental abundances. Additionally, Rosenberg et al. identified a small group of metal-rich globular clusters that appeared to be about 2 billion years younger than the bulk of the Milky Way globular clusters. However, it is unclear if like is compared with like in this dataset as we do not know the enhancement of alpha-elements in the clusters and the amount of alpha-elements is well known to influence the derivation of ages for globular clusters. We present a study of elemental abundances for alpha and iron-peak elements for nine HB stars in the metal-rich globular cluster NGC 6352. The elemental abundances are based on high-resolution, high signal-to-noise spectra obtained with the UVES spectrograph on VLT. The elemental abundances have been derived using standard LTE calculations and stellar parameters have been derived from the spectra themselves by requiring ionizational as well as excitational equilibrium. We find that NGC 6352 has [Fe/H]=-0.55, is enhanced in the alpha-elements to about +0.2dex for Ca, Si, and Ti relative to Fe. For the iron-peak elements we find solar values. Based on the spectroscopically derived stellar parameters we find that an E(B-V)=0.24 and (m-M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913#table1</TD>
            <TD>2011-09-14T20:32:53Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/493/913</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/493/913&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/493/913</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/cgps [1]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/cgps#1</TD>
            <TD>2011-09-14T20:15:27Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/B/cgps</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/cgps</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/cgps</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/cgps [2]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/cgps#2</TD>
            <TD>2011-09-14T20:15:27Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/B/cgps</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/cgps&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/cgps</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/388/1537 [1]</TD>
            <TD>Galaxy pairs from SDSS-DR2 (McIntosh+, 2008)</TD>
            <TD>We make use of the SDSS DR2 group catalogue (Weinmann et al., 2006MNRAS.366....2W), which was constructed by applying the Yang et al. (2005MNRAS.356.1293Y) halo-based group finder to the New York University Value-Added Galaxy Catalogue (NYU-VAGC, Blanton et al., 2005AJ....129.2562B).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537#1</TD>
            <TD>2011-09-14T20:33:25Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/388/1537</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/388/1537</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/388/1537 [2]</TD>
            <TD>Galaxy pairs from SDSS-DR2 (McIntosh+, 2008)</TD>
            <TD>We make use of the SDSS DR2 group catalogue (Weinmann et al., 2006MNRAS.366....2W), which was constructed by applying the Yang et al. (2005MNRAS.356.1293Y) halo-based group finder to the New York University Value-Added Galaxy Catalogue (NYU-VAGC, Blanton et al., 2005AJ....129.2562B).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537#2</TD>
            <TD>2011-09-14T20:33:25Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/388/1537&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/388/1537</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/388/1537 [mergers]</TD>
            <TD>Galaxy pairs from SDSS-DR2 (McIntosh+, 2008)</TD>
            <TD>We make use of the SDSS DR2 group catalogue (Weinmann et al., 2006MNRAS.366....2W), which was constructed by applying the Yang et al. (2005MNRAS.356.1293Y) halo-based group finder to the New York University Value-Added Galaxy Catalogue (NYU-VAGC, Blanton et al., 2005AJ....129.2562B).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537#mergers</TD>
            <TD>2011-09-14T20:33:25Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/388/1537&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/388/1537</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/cgps [1]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/cgps#1</TD>
            <TD>2011-09-14T20:15:27Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/B/cgps</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/cgps</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/cgps</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/cgps [2]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/cgps#2</TD>
            <TD>2011-09-14T20:15:27Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/B/cgps</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/cgps&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/cgps</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/388/1537 [1]</TD>
            <TD>Galaxy pairs from SDSS-DR2 (McIntosh+, 2008)</TD>
            <TD>We make use of the SDSS DR2 group catalogue (Weinmann et al., 2006MNRAS.366....2W), which was constructed by applying the Yang et al. (2005MNRAS.356.1293Y) halo-based group finder to the New York University Value-Added Galaxy Catalogue (NYU-VAGC, Blanton et al., 2005AJ....129.2562B).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537#1</TD>
            <TD>2011-09-14T20:33:25Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/388/1537</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/388/1537</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/388/1537 [2]</TD>
            <TD>Galaxy pairs from SDSS-DR2 (McIntosh+, 2008)</TD>
            <TD>We make use of the SDSS DR2 group catalogue (Weinmann et al., 2006MNRAS.366....2W), which was constructed by applying the Yang et al. (2005MNRAS.356.1293Y) halo-based group finder to the New York University Value-Added Galaxy Catalogue (NYU-VAGC, Blanton et al., 2005AJ....129.2562B).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537#2</TD>
            <TD>2011-09-14T20:33:25Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/388/1537&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/388/1537</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/388/1537 [mergers]</TD>
            <TD>Galaxy pairs from SDSS-DR2 (McIntosh+, 2008)</TD>
            <TD>We make use of the SDSS DR2 group catalogue (Weinmann et al., 2006MNRAS.366....2W), which was constructed by applying the Yang et al. (2005MNRAS.356.1293Y) halo-based group finder to the New York University Value-Added Galaxy Catalogue (NYU-VAGC, Blanton et al., 2005AJ....129.2562B).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537#mergers</TD>
            <TD>2011-09-14T20:33:25Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/388/1537&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/388/1537</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/157/228 [1]</TD>
            <TD>Catalog of galaxy morphology in four clusters (Saintonge+, 2005)</TD>
            <TD>Hubble Space Telescope (HST) imaging of four rich, X-ray-luminous, galaxy clusters (0.33&lt;z&lt;0.83) is used to produce quantitative morphological measurements for galaxies in their fields. Catalogs of these measurements are presented for 1642 galaxies brighter than F814W(AB)=23.0. Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model. The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component. Cluster membership is determined using a statistical correction for field galaxy contamination, and a mass normalization factor (mass within boundaries of the observed fields) is derived for each cluster. Morphological classes are defined using B/T: disk galaxies have 0&lt;=B/T&lt;=0.4, intermediate galaxies 0.4&lt;B/T&lt;0.8, and bulge-dominated galaxies have 0.8&lt;=B/T&lt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228#1</TD>
            <TD>2011-09-14T20:15:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/157/228</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/228</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/157/228 [2]</TD>
            <TD>Catalog of galaxy morphology in four clusters (Saintonge+, 2005)</TD>
            <TD>Hubble Space Telescope (HST) imaging of four rich, X-ray-luminous, galaxy clusters (0.33&lt;z&lt;0.83) is used to produce quantitative morphological measurements for galaxies in their fields. Catalogs of these measurements are presented for 1642 galaxies brighter than F814W(AB)=23.0. Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model. The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component. Cluster membership is determined using a statistical correction for field galaxy contamination, and a mass normalization factor (mass within boundaries of the observed fields) is derived for each cluster. Morphological classes are defined using B/T: disk galaxies have 0&lt;=B/T&lt;=0.4, intermediate galaxies 0.4&lt;B/T&lt;0.8, and bulge-dominated galaxies have 0.8&lt;=B/T&lt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228#2</TD>
            <TD>2011-09-14T20:15:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/157/228&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/228</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/157/228 [catalog]</TD>
            <TD>Catalog of galaxy morphology in four clusters (Saintonge+, 2005)</TD>
            <TD>Hubble Space Telescope (HST) imaging of four rich, X-ray-luminous, galaxy clusters (0.33&lt;z&lt;0.83) is used to produce quantitative morphological measurements for galaxies in their fields. Catalogs of these measurements are presented for 1642 galaxies brighter than F814W(AB)=23.0. Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model. The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component. Cluster membership is determined using a statistical correction for field galaxy contamination, and a mass normalization factor (mass within boundaries of the observed fields) is derived for each cluster. Morphological classes are defined using B/T: disk galaxies have 0&lt;=B/T&lt;=0.4, intermediate galaxies 0.4&lt;B/T&lt;0.8, and bulge-dominated galaxies have 0.8&lt;=B/T&lt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228#catalog</TD>
            <TD>2011-09-14T20:15:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/157/228&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/228</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/157/228 [1]</TD>
            <TD>Catalog of galaxy morphology in four clusters (Saintonge+, 2005)</TD>
            <TD>Hubble Space Telescope (HST) imaging of four rich, X-ray-luminous, galaxy clusters (0.33&lt;z&lt;0.83) is used to produce quantitative morphological measurements for galaxies in their fields. Catalogs of these measurements are presented for 1642 galaxies brighter than F814W(AB)=23.0. Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model. The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component. Cluster membership is determined using a statistical correction for field galaxy contamination, and a mass normalization factor (mass within boundaries of the observed fields) is derived for each cluster. Morphological classes are defined using B/T: disk galaxies have 0&lt;=B/T&lt;=0.4, intermediate galaxies 0.4&lt;B/T&lt;0.8, and bulge-dominated galaxies have 0.8&lt;=B/T&lt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228#1</TD>
            <TD>2011-09-14T20:15:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/157/228</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/228</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/157/228 [2]</TD>
            <TD>Catalog of galaxy morphology in four clusters (Saintonge+, 2005)</TD>
            <TD>Hubble Space Telescope (HST) imaging of four rich, X-ray-luminous, galaxy clusters (0.33&lt;z&lt;0.83) is used to produce quantitative morphological measurements for galaxies in their fields. Catalogs of these measurements are presented for 1642 galaxies brighter than F814W(AB)=23.0. Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model. The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component. Cluster membership is determined using a statistical correction for field galaxy contamination, and a mass normalization factor (mass within boundaries of the observed fields) is derived for each cluster. Morphological classes are defined using B/T: disk galaxies have 0&lt;=B/T&lt;=0.4, intermediate galaxies 0.4&lt;B/T&lt;0.8, and bulge-dominated galaxies have 0.8&lt;=B/T&lt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228#2</TD>
            <TD>2011-09-14T20:15:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/157/228&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/228</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/157/228 [catalog]</TD>
            <TD>Catalog of galaxy morphology in four clusters (Saintonge+, 2005)</TD>
            <TD>Hubble Space Telescope (HST) imaging of four rich, X-ray-luminous, galaxy clusters (0.33&lt;z&lt;0.83) is used to produce quantitative morphological measurements for galaxies in their fields. Catalogs of these measurements are presented for 1642 galaxies brighter than F814W(AB)=23.0. Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model. The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component. Cluster membership is determined using a statistical correction for field galaxy contamination, and a mass normalization factor (mass within boundaries of the observed fields) is derived for each cluster. Morphological classes are defined using B/T: disk galaxies have 0&lt;=B/T&lt;=0.4, intermediate galaxies 0.4&lt;B/T&lt;0.8, and bulge-dominated galaxies have 0.8&lt;=B/T&lt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228#catalog</TD>
            <TD>2011-09-14T20:15:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/157/228&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/228</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/388/1537 [1]</TD>
            <TD>Galaxy pairs from SDSS-DR2 (McIntosh+, 2008)</TD>
            <TD>We make use of the SDSS DR2 group catalogue (Weinmann et al., 2006MNRAS.366....2W), which was constructed by applying the Yang et al. (2005MNRAS.356.1293Y) halo-based group finder to the New York University Value-Added Galaxy Catalogue (NYU-VAGC, Blanton et al., 2005AJ....129.2562B).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537#1</TD>
            <TD>2011-09-14T20:33:25Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/388/1537</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/388/1537</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/388/1537 [2]</TD>
            <TD>Galaxy pairs from SDSS-DR2 (McIntosh+, 2008)</TD>
            <TD>We make use of the SDSS DR2 group catalogue (Weinmann et al., 2006MNRAS.366....2W), which was constructed by applying the Yang et al. (2005MNRAS.356.1293Y) halo-based group finder to the New York University Value-Added Galaxy Catalogue (NYU-VAGC, Blanton et al., 2005AJ....129.2562B).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537#2</TD>
            <TD>2011-09-14T20:33:25Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/388/1537&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/388/1537</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/388/1537 [mergers]</TD>
            <TD>Galaxy pairs from SDSS-DR2 (McIntosh+, 2008)</TD>
            <TD>We make use of the SDSS DR2 group catalogue (Weinmann et al., 2006MNRAS.366....2W), which was constructed by applying the Yang et al. (2005MNRAS.356.1293Y) halo-based group finder to the New York University Value-Added Galaxy Catalogue (NYU-VAGC, Blanton et al., 2005AJ....129.2562B).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537#mergers</TD>
            <TD>2011-09-14T20:33:25Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/388/1537</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/388/1537&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/388/1537</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/481 [1]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#1</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/481</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/481 [2]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#2</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/481&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/481 [galaxies]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#galaxies</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/481&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/481 [table3]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#table3</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/481&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/157/228 [1]</TD>
            <TD>Catalog of galaxy morphology in four clusters (Saintonge+, 2005)</TD>
            <TD>Hubble Space Telescope (HST) imaging of four rich, X-ray-luminous, galaxy clusters (0.33&lt;z&lt;0.83) is used to produce quantitative morphological measurements for galaxies in their fields. Catalogs of these measurements are presented for 1642 galaxies brighter than F814W(AB)=23.0. Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model. The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component. Cluster membership is determined using a statistical correction for field galaxy contamination, and a mass normalization factor (mass within boundaries of the observed fields) is derived for each cluster. Morphological classes are defined using B/T: disk galaxies have 0&lt;=B/T&lt;=0.4, intermediate galaxies 0.4&lt;B/T&lt;0.8, and bulge-dominated galaxies have 0.8&lt;=B/T&lt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228#1</TD>
            <TD>2011-09-14T20:15:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/157/228</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/228</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/157/228 [2]</TD>
            <TD>Catalog of galaxy morphology in four clusters (Saintonge+, 2005)</TD>
            <TD>Hubble Space Telescope (HST) imaging of four rich, X-ray-luminous, galaxy clusters (0.33&lt;z&lt;0.83) is used to produce quantitative morphological measurements for galaxies in their fields. Catalogs of these measurements are presented for 1642 galaxies brighter than F814W(AB)=23.0. Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model. The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component. Cluster membership is determined using a statistical correction for field galaxy contamination, and a mass normalization factor (mass within boundaries of the observed fields) is derived for each cluster. Morphological classes are defined using B/T: disk galaxies have 0&lt;=B/T&lt;=0.4, intermediate galaxies 0.4&lt;B/T&lt;0.8, and bulge-dominated galaxies have 0.8&lt;=B/T&lt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228#2</TD>
            <TD>2011-09-14T20:15:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/157/228&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/228</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/157/228 [catalog]</TD>
            <TD>Catalog of galaxy morphology in four clusters (Saintonge+, 2005)</TD>
            <TD>Hubble Space Telescope (HST) imaging of four rich, X-ray-luminous, galaxy clusters (0.33&lt;z&lt;0.83) is used to produce quantitative morphological measurements for galaxies in their fields. Catalogs of these measurements are presented for 1642 galaxies brighter than F814W(AB)=23.0. Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model. The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component. Cluster membership is determined using a statistical correction for field galaxy contamination, and a mass normalization factor (mass within boundaries of the observed fields) is derived for each cluster. Morphological classes are defined using B/T: disk galaxies have 0&lt;=B/T&lt;=0.4, intermediate galaxies 0.4&lt;B/T&lt;0.8, and bulge-dominated galaxies have 0.8&lt;=B/T&lt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228#catalog</TD>
            <TD>2011-09-14T20:15:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/228</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/157/228&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/228</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/172/615 [1]</TD>
            <TD>GALFIT result for GEMS galaxies (Haussler+, 2007)</TD>
            <TD>GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800arcmin^2^) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the HST, centered on the CDFS. GALFIT is a two-dimensional galaxy-fitting software package written by Peng et al. (2002AJ....124..266P) designed to extract structural components from galaxy images. GIM2D (Galaxy Image 2D) was written by Luc Simard (2002ApJS..142....1S) as an IRAF package for the quantitative morphological analysis of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615#1</TD>
            <TD>2011-09-14T20:45:28Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/172/615</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/172/615</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/172/615 [2]</TD>
            <TD>GALFIT result for GEMS galaxies (Haussler+, 2007)</TD>
            <TD>GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800arcmin^2^) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the HST, centered on the CDFS. GALFIT is a two-dimensional galaxy-fitting software package written by Peng et al. (2002AJ....124..266P) designed to extract structural components from galaxy images. GIM2D (Galaxy Image 2D) was written by Luc Simard (2002ApJS..142....1S) as an IRAF package for the quantitative morphological analysis of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615#2</TD>
            <TD>2011-09-14T20:45:28Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/172/615&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/172/615</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/172/615 [table9]</TD>
            <TD>GALFIT result for GEMS galaxies (Haussler+, 2007)</TD>
            <TD>GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800arcmin^2^) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the HST, centered on the CDFS. GALFIT is a two-dimensional galaxy-fitting software package written by Peng et al. (2002AJ....124..266P) designed to extract structural components from galaxy images. GIM2D (Galaxy Image 2D) was written by Luc Simard (2002ApJS..142....1S) as an IRAF package for the quantitative morphological analysis of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615#table9</TD>
            <TD>2011-09-14T20:45:28Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/172/615&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/172/615</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/BSAO/57. [1]</TD>
            <TD>2MASS-selected Flat Galaxy Catalog (2MFGC) (Mitronova+, 2004)</TD>
            <TD>An all-sky catalog of 18020 disc-like galaxies is presented. The galaxies are selected from the Extended Source Catalog of the Two Micron All-Sky Survey (XSC 2MASS) basing on their 2MASS axial ratio a/b&gt;=3. The Catalog contains data on magnitudes of a galaxy in the J, H, Ks bands, its axial ratio, positional angle, index of luminosity concentration, as well as identification of the galaxy with the LEDA and the NED databases. Unlike the available optical catalogs, the new 2MFGC catalog seems to be more suitable to study cosmic streaming on a scale of z~0.1. The dipole moment of distribution of the bright (K&lt;11mag) 2MFGC objects (l=227{deg}, b=41{deg} or SGL=90{deg}, SGB=-43{deg}) lies within statistical errors (+/-15{deg}) in the direction of the IRAS dipole and the optical RFGC dipole.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5#1</TD>
            <TD>2011-09-14T21:15:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/BSAO/57.5</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BSAO/57.5</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/BSAO/57. [2]</TD>
            <TD>2MASS-selected Flat Galaxy Catalog (2MFGC) (Mitronova+, 2004)</TD>
            <TD>An all-sky catalog of 18020 disc-like galaxies is presented. The galaxies are selected from the Extended Source Catalog of the Two Micron All-Sky Survey (XSC 2MASS) basing on their 2MASS axial ratio a/b&gt;=3. The Catalog contains data on magnitudes of a galaxy in the J, H, Ks bands, its axial ratio, positional angle, index of luminosity concentration, as well as identification of the galaxy with the LEDA and the NED databases. Unlike the available optical catalogs, the new 2MFGC catalog seems to be more suitable to study cosmic streaming on a scale of z~0.1. The dipole moment of distribution of the bright (K&lt;11mag) 2MFGC objects (l=227{deg}, b=41{deg} or SGL=90{deg}, SGB=-43{deg}) lies within statistical errors (+/-15{deg}) in the direction of the IRAS dipole and the optical RFGC dipole.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5#2</TD>
            <TD>2011-09-14T21:15:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/BSAO/57.5&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BSAO/57.5</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BSAO/57. [catalog]</TD>
            <TD>2MASS-selected Flat Galaxy Catalog (2MFGC) (Mitronova+, 2004)</TD>
            <TD>An all-sky catalog of 18020 disc-like galaxies is presented. The galaxies are selected from the Extended Source Catalog of the Two Micron All-Sky Survey (XSC 2MASS) basing on their 2MASS axial ratio a/b&gt;=3. The Catalog contains data on magnitudes of a galaxy in the J, H, Ks bands, its axial ratio, positional angle, index of luminosity concentration, as well as identification of the galaxy with the LEDA and the NED databases. Unlike the available optical catalogs, the new 2MFGC catalog seems to be more suitable to study cosmic streaming on a scale of z~0.1. The dipole moment of distribution of the bright (K&lt;11mag) 2MFGC objects (l=227{deg}, b=41{deg} or SGL=90{deg}, SGB=-43{deg}) lies within statistical errors (+/-15{deg}) in the direction of the IRAS dipole and the optical RFGC dipole.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5#catalog</TD>
            <TD>2011-09-14T21:15:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BSAO/57.5&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BSAO/57.5</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/172/615 [1]</TD>
            <TD>GALFIT result for GEMS galaxies (Haussler+, 2007)</TD>
            <TD>GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800arcmin^2^) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the HST, centered on the CDFS. GALFIT is a two-dimensional galaxy-fitting software package written by Peng et al. (2002AJ....124..266P) designed to extract structural components from galaxy images. GIM2D (Galaxy Image 2D) was written by Luc Simard (2002ApJS..142....1S) as an IRAF package for the quantitative morphological analysis of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615#1</TD>
            <TD>2011-09-14T20:45:28Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/172/615</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/172/615</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/172/615 [2]</TD>
            <TD>GALFIT result for GEMS galaxies (Haussler+, 2007)</TD>
            <TD>GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800arcmin^2^) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the HST, centered on the CDFS. GALFIT is a two-dimensional galaxy-fitting software package written by Peng et al. (2002AJ....124..266P) designed to extract structural components from galaxy images. GIM2D (Galaxy Image 2D) was written by Luc Simard (2002ApJS..142....1S) as an IRAF package for the quantitative morphological analysis of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615#2</TD>
            <TD>2011-09-14T20:45:28Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/172/615&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/172/615</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/172/615 [table9]</TD>
            <TD>GALFIT result for GEMS galaxies (Haussler+, 2007)</TD>
            <TD>GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800arcmin^2^) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the HST, centered on the CDFS. GALFIT is a two-dimensional galaxy-fitting software package written by Peng et al. (2002AJ....124..266P) designed to extract structural components from galaxy images. GIM2D (Galaxy Image 2D) was written by Luc Simard (2002ApJS..142....1S) as an IRAF package for the quantitative morphological analysis of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615#table9</TD>
            <TD>2011-09-14T20:45:28Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/172/615&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/172/615</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/BSAO/57. [1]</TD>
            <TD>2MASS-selected Flat Galaxy Catalog (2MFGC) (Mitronova+, 2004)</TD>
            <TD>An all-sky catalog of 18020 disc-like galaxies is presented. The galaxies are selected from the Extended Source Catalog of the Two Micron All-Sky Survey (XSC 2MASS) basing on their 2MASS axial ratio a/b&gt;=3. The Catalog contains data on magnitudes of a galaxy in the J, H, Ks bands, its axial ratio, positional angle, index of luminosity concentration, as well as identification of the galaxy with the LEDA and the NED databases. Unlike the available optical catalogs, the new 2MFGC catalog seems to be more suitable to study cosmic streaming on a scale of z~0.1. The dipole moment of distribution of the bright (K&lt;11mag) 2MFGC objects (l=227{deg}, b=41{deg} or SGL=90{deg}, SGB=-43{deg}) lies within statistical errors (+/-15{deg}) in the direction of the IRAS dipole and the optical RFGC dipole.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5#1</TD>
            <TD>2011-09-14T21:15:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/BSAO/57.5</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BSAO/57.5</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/BSAO/57. [2]</TD>
            <TD>2MASS-selected Flat Galaxy Catalog (2MFGC) (Mitronova+, 2004)</TD>
            <TD>An all-sky catalog of 18020 disc-like galaxies is presented. The galaxies are selected from the Extended Source Catalog of the Two Micron All-Sky Survey (XSC 2MASS) basing on their 2MASS axial ratio a/b&gt;=3. The Catalog contains data on magnitudes of a galaxy in the J, H, Ks bands, its axial ratio, positional angle, index of luminosity concentration, as well as identification of the galaxy with the LEDA and the NED databases. Unlike the available optical catalogs, the new 2MFGC catalog seems to be more suitable to study cosmic streaming on a scale of z~0.1. The dipole moment of distribution of the bright (K&lt;11mag) 2MFGC objects (l=227{deg}, b=41{deg} or SGL=90{deg}, SGB=-43{deg}) lies within statistical errors (+/-15{deg}) in the direction of the IRAS dipole and the optical RFGC dipole.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5#2</TD>
            <TD>2011-09-14T21:15:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/BSAO/57.5&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BSAO/57.5</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BSAO/57. [catalog]</TD>
            <TD>2MASS-selected Flat Galaxy Catalog (2MFGC) (Mitronova+, 2004)</TD>
            <TD>An all-sky catalog of 18020 disc-like galaxies is presented. The galaxies are selected from the Extended Source Catalog of the Two Micron All-Sky Survey (XSC 2MASS) basing on their 2MASS axial ratio a/b&gt;=3. The Catalog contains data on magnitudes of a galaxy in the J, H, Ks bands, its axial ratio, positional angle, index of luminosity concentration, as well as identification of the galaxy with the LEDA and the NED databases. Unlike the available optical catalogs, the new 2MFGC catalog seems to be more suitable to study cosmic streaming on a scale of z~0.1. The dipole moment of distribution of the bright (K&lt;11mag) 2MFGC objects (l=227{deg}, b=41{deg} or SGL=90{deg}, SGB=-43{deg}) lies within statistical errors (+/-15{deg}) in the direction of the IRAS dipole and the optical RFGC dipole.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5#catalog</TD>
            <TD>2011-09-14T21:15:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BSAO/57.5&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BSAO/57.5</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/172/615 [1]</TD>
            <TD>GALFIT result for GEMS galaxies (Haussler+, 2007)</TD>
            <TD>GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800arcmin^2^) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the HST, centered on the CDFS. GALFIT is a two-dimensional galaxy-fitting software package written by Peng et al. (2002AJ....124..266P) designed to extract structural components from galaxy images. GIM2D (Galaxy Image 2D) was written by Luc Simard (2002ApJS..142....1S) as an IRAF package for the quantitative morphological analysis of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615#1</TD>
            <TD>2011-09-14T20:45:28Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/172/615</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/172/615</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/172/615 [2]</TD>
            <TD>GALFIT result for GEMS galaxies (Haussler+, 2007)</TD>
            <TD>GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800arcmin^2^) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the HST, centered on the CDFS. GALFIT is a two-dimensional galaxy-fitting software package written by Peng et al. (2002AJ....124..266P) designed to extract structural components from galaxy images. GIM2D (Galaxy Image 2D) was written by Luc Simard (2002ApJS..142....1S) as an IRAF package for the quantitative morphological analysis of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615#2</TD>
            <TD>2011-09-14T20:45:28Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/172/615&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/172/615</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/172/615 [table9]</TD>
            <TD>GALFIT result for GEMS galaxies (Haussler+, 2007)</TD>
            <TD>GEMS (Galaxy Evolution from Morphologies and SEDs) is a large-area (800arcmin^2^) two-color (F606W and F850LP) imaging survey with the Advanced Camera for Surveys on the HST, centered on the CDFS. GALFIT is a two-dimensional galaxy-fitting software package written by Peng et al. (2002AJ....124..266P) designed to extract structural components from galaxy images. GIM2D (Galaxy Image 2D) was written by Luc Simard (2002ApJS..142....1S) as an IRAF package for the quantitative morphological analysis of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615#table9</TD>
            <TD>2011-09-14T20:45:28Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/172/615</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/172/615&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/172/615</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/BSAO/57. [1]</TD>
            <TD>2MASS-selected Flat Galaxy Catalog (2MFGC) (Mitronova+, 2004)</TD>
            <TD>An all-sky catalog of 18020 disc-like galaxies is presented. The galaxies are selected from the Extended Source Catalog of the Two Micron All-Sky Survey (XSC 2MASS) basing on their 2MASS axial ratio a/b&gt;=3. The Catalog contains data on magnitudes of a galaxy in the J, H, Ks bands, its axial ratio, positional angle, index of luminosity concentration, as well as identification of the galaxy with the LEDA and the NED databases. Unlike the available optical catalogs, the new 2MFGC catalog seems to be more suitable to study cosmic streaming on a scale of z~0.1. The dipole moment of distribution of the bright (K&lt;11mag) 2MFGC objects (l=227{deg}, b=41{deg} or SGL=90{deg}, SGB=-43{deg}) lies within statistical errors (+/-15{deg}) in the direction of the IRAS dipole and the optical RFGC dipole.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5#1</TD>
            <TD>2011-09-14T21:15:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/BSAO/57.5</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BSAO/57.5</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/BSAO/57. [2]</TD>
            <TD>2MASS-selected Flat Galaxy Catalog (2MFGC) (Mitronova+, 2004)</TD>
            <TD>An all-sky catalog of 18020 disc-like galaxies is presented. The galaxies are selected from the Extended Source Catalog of the Two Micron All-Sky Survey (XSC 2MASS) basing on their 2MASS axial ratio a/b&gt;=3. The Catalog contains data on magnitudes of a galaxy in the J, H, Ks bands, its axial ratio, positional angle, index of luminosity concentration, as well as identification of the galaxy with the LEDA and the NED databases. Unlike the available optical catalogs, the new 2MFGC catalog seems to be more suitable to study cosmic streaming on a scale of z~0.1. The dipole moment of distribution of the bright (K&lt;11mag) 2MFGC objects (l=227{deg}, b=41{deg} or SGL=90{deg}, SGB=-43{deg}) lies within statistical errors (+/-15{deg}) in the direction of the IRAS dipole and the optical RFGC dipole.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5#2</TD>
            <TD>2011-09-14T21:15:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/BSAO/57.5&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BSAO/57.5</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BSAO/57. [catalog]</TD>
            <TD>2MASS-selected Flat Galaxy Catalog (2MFGC) (Mitronova+, 2004)</TD>
            <TD>An all-sky catalog of 18020 disc-like galaxies is presented. The galaxies are selected from the Extended Source Catalog of the Two Micron All-Sky Survey (XSC 2MASS) basing on their 2MASS axial ratio a/b&gt;=3. The Catalog contains data on magnitudes of a galaxy in the J, H, Ks bands, its axial ratio, positional angle, index of luminosity concentration, as well as identification of the galaxy with the LEDA and the NED databases. Unlike the available optical catalogs, the new 2MFGC catalog seems to be more suitable to study cosmic streaming on a scale of z~0.1. The dipole moment of distribution of the bright (K&lt;11mag) 2MFGC objects (l=227{deg}, b=41{deg} or SGL=90{deg}, SGB=-43{deg}) lies within statistical errors (+/-15{deg}) in the direction of the IRAS dipole and the optical RFGC dipole.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5#catalog</TD>
            <TD>2011-09-14T21:15:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/BSAO/57.5</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BSAO/57.5&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BSAO/57.5</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/169/213 [1]</TD>
            <TD>ACS Fornax Cluster Survey. I. (Jordan+, 2007)</TD>
            <TD>Observations for each of the 43 program galaxies were carried out as part of GO program 10217 between 2004 September and 2005 March. Each galaxy was imaged within a single orbit, using the ACS Wide Field Channel (WFC) mode.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213#1</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/169/213</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/169/213</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/169/213 [2]</TD>
            <TD>ACS Fornax Cluster Survey. I. (Jordan+, 2007)</TD>
            <TD>Observations for each of the 43 program galaxies were carried out as part of GO program 10217 between 2004 September and 2005 March. Each galaxy was imaged within a single orbit, using the ACS Wide Field Channel (WFC) mode.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213#2</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/169/213&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/169/213</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/169/213 [table3]</TD>
            <TD>ACS Fornax Cluster Survey. I. (Jordan+, 2007)</TD>
            <TD>Observations for each of the 43 program galaxies were carried out as part of GO program 10217 between 2004 September and 2005 March. Each galaxy was imaged within a single orbit, using the ACS Wide Field Channel (WFC) mode.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213#table3</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/169/213&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/169/213</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/404/1801 [1]</TD>
            <TD>Horizon MareNostrum cosmological run (Gay+, 2010)</TD>
            <TD>The correlation between the large-scale distribution of galaxies and their spectroscopic properties at z=1.5 is investigated using the Horizon MareNostrum cosmological run. We have extracted a large sample of 105 galaxies from this large hydrodynamical simulation featuring standard galaxy formation physics. Spectral synthesis is applied to these single stellar populations to generate spectra and colours for all galaxies. We use the skeleton as a tracer of the cosmic web and study how our galaxy catalogue depends on the distance to the skeleton. We show that galaxies closer to the skeleton tend to be redder but that the effect is mostly due to the proximity of large haloes at the nodes of the skeleton, rather than the filaments themselves. The virtual catalogues (spectroscopical properties of the MareNostrum galaxies at various redshifts) are available online at http://www.iap.fr/users/pichon/MareNostrum/catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1801#1</TD>
            <TD>2011-09-14T21:15:59Z</TD>
            <TD>#Photometry#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1801</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/404/1801</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1801</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/404/1801 [2]</TD>
            <TD>Horizon MareNostrum cosmological run (Gay+, 2010)</TD>
            <TD>The correlation between the large-scale distribution of galaxies and their spectroscopic properties at z=1.5 is investigated using the Horizon MareNostrum cosmological run. We have extracted a large sample of 105 galaxies from this large hydrodynamical simulation featuring standard galaxy formation physics. Spectral synthesis is applied to these single stellar populations to generate spectra and colours for all galaxies. We use the skeleton as a tracer of the cosmic web and study how our galaxy catalogue depends on the distance to the skeleton. We show that galaxies closer to the skeleton tend to be redder but that the effect is mostly due to the proximity of large haloes at the nodes of the skeleton, rather than the filaments themselves. The virtual catalogues (spectroscopical properties of the MareNostrum galaxies at various redshifts) are available online at http://www.iap.fr/users/pichon/MareNostrum/catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1801#2</TD>
            <TD>2011-09-14T21:15:59Z</TD>
            <TD>#Photometry#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1801</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/404/1801&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1801</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/169/213 [1]</TD>
            <TD>ACS Fornax Cluster Survey. I. (Jordan+, 2007)</TD>
            <TD>Observations for each of the 43 program galaxies were carried out as part of GO program 10217 between 2004 September and 2005 March. Each galaxy was imaged within a single orbit, using the ACS Wide Field Channel (WFC) mode.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213#1</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/169/213</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/169/213</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/169/213 [2]</TD>
            <TD>ACS Fornax Cluster Survey. I. (Jordan+, 2007)</TD>
            <TD>Observations for each of the 43 program galaxies were carried out as part of GO program 10217 between 2004 September and 2005 March. Each galaxy was imaged within a single orbit, using the ACS Wide Field Channel (WFC) mode.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213#2</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/169/213&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/169/213</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/169/213 [table3]</TD>
            <TD>ACS Fornax Cluster Survey. I. (Jordan+, 2007)</TD>
            <TD>Observations for each of the 43 program galaxies were carried out as part of GO program 10217 between 2004 September and 2005 March. Each galaxy was imaged within a single orbit, using the ACS Wide Field Channel (WFC) mode.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213#table3</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/169/213&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/169/213</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/404/1801 [1]</TD>
            <TD>Horizon MareNostrum cosmological run (Gay+, 2010)</TD>
            <TD>The correlation between the large-scale distribution of galaxies and their spectroscopic properties at z=1.5 is investigated using the Horizon MareNostrum cosmological run. We have extracted a large sample of 105 galaxies from this large hydrodynamical simulation featuring standard galaxy formation physics. Spectral synthesis is applied to these single stellar populations to generate spectra and colours for all galaxies. We use the skeleton as a tracer of the cosmic web and study how our galaxy catalogue depends on the distance to the skeleton. We show that galaxies closer to the skeleton tend to be redder but that the effect is mostly due to the proximity of large haloes at the nodes of the skeleton, rather than the filaments themselves. The virtual catalogues (spectroscopical properties of the MareNostrum galaxies at various redshifts) are available online at http://www.iap.fr/users/pichon/MareNostrum/catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1801#1</TD>
            <TD>2011-09-14T21:15:59Z</TD>
            <TD>#Photometry#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1801</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/404/1801</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1801</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/404/1801 [2]</TD>
            <TD>Horizon MareNostrum cosmological run (Gay+, 2010)</TD>
            <TD>The correlation between the large-scale distribution of galaxies and their spectroscopic properties at z=1.5 is investigated using the Horizon MareNostrum cosmological run. We have extracted a large sample of 105 galaxies from this large hydrodynamical simulation featuring standard galaxy formation physics. Spectral synthesis is applied to these single stellar populations to generate spectra and colours for all galaxies. We use the skeleton as a tracer of the cosmic web and study how our galaxy catalogue depends on the distance to the skeleton. We show that galaxies closer to the skeleton tend to be redder but that the effect is mostly due to the proximity of large haloes at the nodes of the skeleton, rather than the filaments themselves. The virtual catalogues (spectroscopical properties of the MareNostrum galaxies at various redshifts) are available online at http://www.iap.fr/users/pichon/MareNostrum/catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1801#2</TD>
            <TD>2011-09-14T21:15:59Z</TD>
            <TD>#Photometry#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1801</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/404/1801&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1801</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/481 [1]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#1</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/481</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/481 [2]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#2</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/481&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/481 [galaxies]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#galaxies</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/481&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/481 [table3]</TD>
            <TD>Near-infrared survey around PKS 1343-601 (Schroeder+, 2007)</TD>
            <TD>The highly obscured radio-bright galaxy PKS 1343-601 at Galactic coordinates of (l,b)=(309.7,+1.8) has been suspected to mark the centre of a hitherto unknown cluster in the wider Great Attractor region. As such it presents an ideal region for a search of galaxies in the near-infrared (NIR) and an in-depth study of their colours as a function of extinction. A visual search of a ~30 square-degree area centred on this radio galaxy on images of the NIR DENIS survey (IJK) revealed 83 galaxies (including two AGNs) and 39 possible candidates. Of these, 49 are also listed in the 2MASS Extended Source Catalog 2MASX. Taking the IRAS/DIRBE extinction values (Schlegel et al., 1998ApJ...500..525S) at face value, the absorption in the optical (AB) ranges from ~2mag to over 100mag across the Galactic Plane. Comparing the detections with other systematic surveys, we conclude that this search is highly complete up to the detection limits of the DENIS survey and certainly surpasses any automatic galaxy finding algorithm applied to crowded areas.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481#table3</TD>
            <TD>2011-09-14T20:06:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/481</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/481&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/481</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/169/213 [1]</TD>
            <TD>ACS Fornax Cluster Survey. I. (Jordan+, 2007)</TD>
            <TD>Observations for each of the 43 program galaxies were carried out as part of GO program 10217 between 2004 September and 2005 March. Each galaxy was imaged within a single orbit, using the ACS Wide Field Channel (WFC) mode.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213#1</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/169/213</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/169/213</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/169/213 [2]</TD>
            <TD>ACS Fornax Cluster Survey. I. (Jordan+, 2007)</TD>
            <TD>Observations for each of the 43 program galaxies were carried out as part of GO program 10217 between 2004 September and 2005 March. Each galaxy was imaged within a single orbit, using the ACS Wide Field Channel (WFC) mode.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213#2</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/169/213&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/169/213</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/169/213 [table3]</TD>
            <TD>ACS Fornax Cluster Survey. I. (Jordan+, 2007)</TD>
            <TD>Observations for each of the 43 program galaxies were carried out as part of GO program 10217 between 2004 September and 2005 March. Each galaxy was imaged within a single orbit, using the ACS Wide Field Channel (WFC) mode.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213#table3</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/169/213</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/169/213&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/169/213</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/479 [1]</TD>
            <TD>IRAC observations of M83 extended UV disk (Dong+, 2008)</TD>
            <TD>Spitzer Infrared Array Camera (IRAC) observations of two fields in the extended UV disk (XUV-disk) of M83 have been recently obtained, ~3R_HII_ away from the center of the galaxy (R_HII_=6.6kpc). Galaxy Evolution Explorer (GALEX) UV images have shown the two fields to host in situ recent star formation. The IRAC images are used in conjunction with GALEX data and new HI imaging from The HI Nearby Galaxy Survey (THINGS) to constrain stellar masses and ages of the UV clumps in the fields, and to relate the local recent star formation to the reservoir of available gas. Multi-wavelength photometry in the UV and mid-IR (MIR) bands of 136 UV clumps (spatial resolution &gt;220pc) identified in the two target fields, together with model fitting of the stellar UV-MIR spectral energy distributions (SEDs), suggests that the clumps cover a range of ages between a few Myr and &gt;1Gyr with a median value around &lt;=100Myr, and have masses in the range 10^3^-3x10^6^M_{sun}_, with a peak ~10^4.7^M_{sun}.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479#1</TD>
            <TD>2011-09-14T21:17:42Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/479</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/479</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/479 [2]</TD>
            <TD>IRAC observations of M83 extended UV disk (Dong+, 2008)</TD>
            <TD>Spitzer Infrared Array Camera (IRAC) observations of two fields in the extended UV disk (XUV-disk) of M83 have been recently obtained, ~3R_HII_ away from the center of the galaxy (R_HII_=6.6kpc). Galaxy Evolution Explorer (GALEX) UV images have shown the two fields to host in situ recent star formation. The IRAC images are used in conjunction with GALEX data and new HI imaging from The HI Nearby Galaxy Survey (THINGS) to constrain stellar masses and ages of the UV clumps in the fields, and to relate the local recent star formation to the reservoir of available gas. Multi-wavelength photometry in the UV and mid-IR (MIR) bands of 136 UV clumps (spatial resolution &gt;220pc) identified in the two target fields, together with model fitting of the stellar UV-MIR spectral energy distributions (SEDs), suggests that the clumps cover a range of ages between a few Myr and &gt;1Gyr with a median value around &lt;=100Myr, and have masses in the range 10^3^-3x10^6^M_{sun}_, with a peak ~10^4.7^M_{sun}.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479#2</TD>
            <TD>2011-09-14T21:17:42Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/479&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/479</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/479 [table23]</TD>
            <TD>IRAC observations of M83 extended UV disk (Dong+, 2008)</TD>
            <TD>Spitzer Infrared Array Camera (IRAC) observations of two fields in the extended UV disk (XUV-disk) of M83 have been recently obtained, ~3R_HII_ away from the center of the galaxy (R_HII_=6.6kpc). Galaxy Evolution Explorer (GALEX) UV images have shown the two fields to host in situ recent star formation. The IRAC images are used in conjunction with GALEX data and new HI imaging from The HI Nearby Galaxy Survey (THINGS) to constrain stellar masses and ages of the UV clumps in the fields, and to relate the local recent star formation to the reservoir of available gas. Multi-wavelength photometry in the UV and mid-IR (MIR) bands of 136 UV clumps (spatial resolution &gt;220pc) identified in the two target fields, together with model fitting of the stellar UV-MIR spectral energy distributions (SEDs), suggests that the clumps cover a range of ages between a few Myr and &gt;1Gyr with a median value around &lt;=100Myr, and have masses in the range 10^3^-3x10^6^M_{sun}_, with a peak ~10^4.7^M_{sun}.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479#table23</TD>
            <TD>2011-09-14T21:17:42Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/479&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/479</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/643 [1]</TD>
            <TD>GALEX UV photometry of M31 Globular Clusters (Rey+, 2007)</TD>
            <TD>The M31 images were obtained as part of the Nearby Galaxy Survey (NGS) carried out by GALEX in two UV bands: FUV (135-175nm) and NUV (175-275nm). Details on the early observations of 14 fields released under the GALEX Release 1 (GR1) can be found in Thilker et al. (2005ApJ...619L..67T) and Paper I (Rey et al., 2005ApJ...619L.119R). We have observed an additional nine GALEX fields in 2004 September-November, which are included in the GALEX Release 2 (GR2).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643#1</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/643</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/643</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/643 [2]</TD>
            <TD>GALEX UV photometry of M31 Globular Clusters (Rey+, 2007)</TD>
            <TD>The M31 images were obtained as part of the Nearby Galaxy Survey (NGS) carried out by GALEX in two UV bands: FUV (135-175nm) and NUV (175-275nm). Details on the early observations of 14 fields released under the GALEX Release 1 (GR1) can be found in Thilker et al. (2005ApJ...619L..67T) and Paper I (Rey et al., 2005ApJ...619L.119R). We have observed an additional nine GALEX fields in 2004 September-November, which are included in the GALEX Release 2 (GR2).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643#2</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/643&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/643</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/173/643 [table2]</TD>
            <TD>GALEX UV photometry of M31 Globular Clusters (Rey+, 2007)</TD>
            <TD>The M31 images were obtained as part of the Nearby Galaxy Survey (NGS) carried out by GALEX in two UV bands: FUV (135-175nm) and NUV (175-275nm). Details on the early observations of 14 fields released under the GALEX Release 1 (GR1) can be found in Thilker et al. (2005ApJ...619L..67T) and Paper I (Rey et al., 2005ApJ...619L.119R). We have observed an additional nine GALEX fields in 2004 September-November, which are included in the GALEX Release 2 (GR2).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643#table2</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/173/643&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/643</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/479 [1]</TD>
            <TD>IRAC observations of M83 extended UV disk (Dong+, 2008)</TD>
            <TD>Spitzer Infrared Array Camera (IRAC) observations of two fields in the extended UV disk (XUV-disk) of M83 have been recently obtained, ~3R_HII_ away from the center of the galaxy (R_HII_=6.6kpc). Galaxy Evolution Explorer (GALEX) UV images have shown the two fields to host in situ recent star formation. The IRAC images are used in conjunction with GALEX data and new HI imaging from The HI Nearby Galaxy Survey (THINGS) to constrain stellar masses and ages of the UV clumps in the fields, and to relate the local recent star formation to the reservoir of available gas. Multi-wavelength photometry in the UV and mid-IR (MIR) bands of 136 UV clumps (spatial resolution &gt;220pc) identified in the two target fields, together with model fitting of the stellar UV-MIR spectral energy distributions (SEDs), suggests that the clumps cover a range of ages between a few Myr and &gt;1Gyr with a median value around &lt;=100Myr, and have masses in the range 10^3^-3x10^6^M_{sun}_, with a peak ~10^4.7^M_{sun}.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479#1</TD>
            <TD>2011-09-14T21:17:42Z</TD>
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            <TD>04-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/479</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/479</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/479 [2]</TD>
            <TD>IRAC observations of M83 extended UV disk (Dong+, 2008)</TD>
            <TD>Spitzer Infrared Array Camera (IRAC) observations of two fields in the extended UV disk (XUV-disk) of M83 have been recently obtained, ~3R_HII_ away from the center of the galaxy (R_HII_=6.6kpc). Galaxy Evolution Explorer (GALEX) UV images have shown the two fields to host in situ recent star formation. The IRAC images are used in conjunction with GALEX data and new HI imaging from The HI Nearby Galaxy Survey (THINGS) to constrain stellar masses and ages of the UV clumps in the fields, and to relate the local recent star formation to the reservoir of available gas. Multi-wavelength photometry in the UV and mid-IR (MIR) bands of 136 UV clumps (spatial resolution &gt;220pc) identified in the two target fields, together with model fitting of the stellar UV-MIR spectral energy distributions (SEDs), suggests that the clumps cover a range of ages between a few Myr and &gt;1Gyr with a median value around &lt;=100Myr, and have masses in the range 10^3^-3x10^6^M_{sun}_, with a peak ~10^4.7^M_{sun}.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479#2</TD>
            <TD>2011-09-14T21:17:42Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/479&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/479</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/479 [table23]</TD>
            <TD>IRAC observations of M83 extended UV disk (Dong+, 2008)</TD>
            <TD>Spitzer Infrared Array Camera (IRAC) observations of two fields in the extended UV disk (XUV-disk) of M83 have been recently obtained, ~3R_HII_ away from the center of the galaxy (R_HII_=6.6kpc). Galaxy Evolution Explorer (GALEX) UV images have shown the two fields to host in situ recent star formation. The IRAC images are used in conjunction with GALEX data and new HI imaging from The HI Nearby Galaxy Survey (THINGS) to constrain stellar masses and ages of the UV clumps in the fields, and to relate the local recent star formation to the reservoir of available gas. Multi-wavelength photometry in the UV and mid-IR (MIR) bands of 136 UV clumps (spatial resolution &gt;220pc) identified in the two target fields, together with model fitting of the stellar UV-MIR spectral energy distributions (SEDs), suggests that the clumps cover a range of ages between a few Myr and &gt;1Gyr with a median value around &lt;=100Myr, and have masses in the range 10^3^-3x10^6^M_{sun}_, with a peak ~10^4.7^M_{sun}.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479#table23</TD>
            <TD>2011-09-14T21:17:42Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/479&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/479</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/643 [1]</TD>
            <TD>GALEX UV photometry of M31 Globular Clusters (Rey+, 2007)</TD>
            <TD>The M31 images were obtained as part of the Nearby Galaxy Survey (NGS) carried out by GALEX in two UV bands: FUV (135-175nm) and NUV (175-275nm). Details on the early observations of 14 fields released under the GALEX Release 1 (GR1) can be found in Thilker et al. (2005ApJ...619L..67T) and Paper I (Rey et al., 2005ApJ...619L.119R). We have observed an additional nine GALEX fields in 2004 September-November, which are included in the GALEX Release 2 (GR2).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643#1</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/643</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/643</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/643 [2]</TD>
            <TD>GALEX UV photometry of M31 Globular Clusters (Rey+, 2007)</TD>
            <TD>The M31 images were obtained as part of the Nearby Galaxy Survey (NGS) carried out by GALEX in two UV bands: FUV (135-175nm) and NUV (175-275nm). Details on the early observations of 14 fields released under the GALEX Release 1 (GR1) can be found in Thilker et al. (2005ApJ...619L..67T) and Paper I (Rey et al., 2005ApJ...619L.119R). We have observed an additional nine GALEX fields in 2004 September-November, which are included in the GALEX Release 2 (GR2).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643#2</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/643&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/643</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/173/643 [table2]</TD>
            <TD>GALEX UV photometry of M31 Globular Clusters (Rey+, 2007)</TD>
            <TD>The M31 images were obtained as part of the Nearby Galaxy Survey (NGS) carried out by GALEX in two UV bands: FUV (135-175nm) and NUV (175-275nm). Details on the early observations of 14 fields released under the GALEX Release 1 (GR1) can be found in Thilker et al. (2005ApJ...619L..67T) and Paper I (Rey et al., 2005ApJ...619L.119R). We have observed an additional nine GALEX fields in 2004 September-November, which are included in the GALEX Release 2 (GR2).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643#table2</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/173/643&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/643</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/479 [1]</TD>
            <TD>IRAC observations of M83 extended UV disk (Dong+, 2008)</TD>
            <TD>Spitzer Infrared Array Camera (IRAC) observations of two fields in the extended UV disk (XUV-disk) of M83 have been recently obtained, ~3R_HII_ away from the center of the galaxy (R_HII_=6.6kpc). Galaxy Evolution Explorer (GALEX) UV images have shown the two fields to host in situ recent star formation. The IRAC images are used in conjunction with GALEX data and new HI imaging from The HI Nearby Galaxy Survey (THINGS) to constrain stellar masses and ages of the UV clumps in the fields, and to relate the local recent star formation to the reservoir of available gas. Multi-wavelength photometry in the UV and mid-IR (MIR) bands of 136 UV clumps (spatial resolution &gt;220pc) identified in the two target fields, together with model fitting of the stellar UV-MIR spectral energy distributions (SEDs), suggests that the clumps cover a range of ages between a few Myr and &gt;1Gyr with a median value around &lt;=100Myr, and have masses in the range 10^3^-3x10^6^M_{sun}_, with a peak ~10^4.7^M_{sun}.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479#1</TD>
            <TD>2011-09-14T21:17:42Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/479</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/479</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/479 [2]</TD>
            <TD>IRAC observations of M83 extended UV disk (Dong+, 2008)</TD>
            <TD>Spitzer Infrared Array Camera (IRAC) observations of two fields in the extended UV disk (XUV-disk) of M83 have been recently obtained, ~3R_HII_ away from the center of the galaxy (R_HII_=6.6kpc). Galaxy Evolution Explorer (GALEX) UV images have shown the two fields to host in situ recent star formation. The IRAC images are used in conjunction with GALEX data and new HI imaging from The HI Nearby Galaxy Survey (THINGS) to constrain stellar masses and ages of the UV clumps in the fields, and to relate the local recent star formation to the reservoir of available gas. Multi-wavelength photometry in the UV and mid-IR (MIR) bands of 136 UV clumps (spatial resolution &gt;220pc) identified in the two target fields, together with model fitting of the stellar UV-MIR spectral energy distributions (SEDs), suggests that the clumps cover a range of ages between a few Myr and &gt;1Gyr with a median value around &lt;=100Myr, and have masses in the range 10^3^-3x10^6^M_{sun}_, with a peak ~10^4.7^M_{sun}.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479#2</TD>
            <TD>2011-09-14T21:17:42Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/479&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/479</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/479 [table23]</TD>
            <TD>IRAC observations of M83 extended UV disk (Dong+, 2008)</TD>
            <TD>Spitzer Infrared Array Camera (IRAC) observations of two fields in the extended UV disk (XUV-disk) of M83 have been recently obtained, ~3R_HII_ away from the center of the galaxy (R_HII_=6.6kpc). Galaxy Evolution Explorer (GALEX) UV images have shown the two fields to host in situ recent star formation. The IRAC images are used in conjunction with GALEX data and new HI imaging from The HI Nearby Galaxy Survey (THINGS) to constrain stellar masses and ages of the UV clumps in the fields, and to relate the local recent star formation to the reservoir of available gas. Multi-wavelength photometry in the UV and mid-IR (MIR) bands of 136 UV clumps (spatial resolution &gt;220pc) identified in the two target fields, together with model fitting of the stellar UV-MIR spectral energy distributions (SEDs), suggests that the clumps cover a range of ages between a few Myr and &gt;1Gyr with a median value around &lt;=100Myr, and have masses in the range 10^3^-3x10^6^M_{sun}_, with a peak ~10^4.7^M_{sun}.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479#table23</TD>
            <TD>2011-09-14T21:17:42Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/479</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/479&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/479</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/329/87 [1]</TD>
            <TD>2dF Galaxy Redshift Survey: galaxy clusters (de Propris+, 2002)</TD>
            <TD>We have carried out a study of known clusters within the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;) observed areas and have identified 431 Abell, 173 APM and 343 EDCC clusters. Precise redshifts, velocity dispersions and new centroids have been measured for the majority of these objects, and this information is used to study the completeness of these catalogues, the level of contamination from foreground and background structures along the cluster's line of sight, the space density of the clusters as a function of redshift, and their velocity dispersion distributions. We find that the Abell and EDCC catalogues are contaminated at the level of about 10 per cent, whereas the APM catalogue suffers only 5 per cent contamination. If we use the original catalogue centroids, the level of contamination rises to approximately 15 per cent for the Abell and EDCC catalogues, showing that the presence of foreground and background groups may alter the richness of clusters in these catalogues. There is a deficiency of clusters at z~0.05 hat may correspond to a large underdensity in the Southern hemisphere. From the cumulative distribution of velocity dispersions for these clusters, we derive a space density of {sigma}&gt;1000km/s clusters of 3.6x10^-6^h^3^/Mpc^3^. This result is used to constrain models for structure formation; our data favour low-density cosmologies, subject to the usual assumptions concerning the shape and normalization of the power spectrum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87#1</TD>
            <TD>2012-09-20T13:52:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/329/87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/329/87 [2]</TD>
            <TD>2dF Galaxy Redshift Survey: galaxy clusters (de Propris+, 2002)</TD>
            <TD>We have carried out a study of known clusters within the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;) observed areas and have identified 431 Abell, 173 APM and 343 EDCC clusters. Precise redshifts, velocity dispersions and new centroids have been measured for the majority of these objects, and this information is used to study the completeness of these catalogues, the level of contamination from foreground and background structures along the cluster's line of sight, the space density of the clusters as a function of redshift, and their velocity dispersion distributions. We find that the Abell and EDCC catalogues are contaminated at the level of about 10 per cent, whereas the APM catalogue suffers only 5 per cent contamination. If we use the original catalogue centroids, the level of contamination rises to approximately 15 per cent for the Abell and EDCC catalogues, showing that the presence of foreground and background groups may alter the richness of clusters in these catalogues. There is a deficiency of clusters at z~0.05 hat may correspond to a large underdensity in the Southern hemisphere. From the cumulative distribution of velocity dispersions for these clusters, we derive a space density of {sigma}&gt;1000km/s clusters of 3.6x10^-6^h^3^/Mpc^3^. This result is used to constrain models for structure formation; our data favour low-density cosmologies, subject to the usual assumptions concerning the shape and normalization of the power spectrum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87#2</TD>
            <TD>2012-09-20T13:52:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/329/87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/329/87 [table1]</TD>
            <TD>2dF Galaxy Redshift Survey: galaxy clusters (de Propris+, 2002)</TD>
            <TD>We have carried out a study of known clusters within the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;) observed areas and have identified 431 Abell, 173 APM and 343 EDCC clusters. Precise redshifts, velocity dispersions and new centroids have been measured for the majority of these objects, and this information is used to study the completeness of these catalogues, the level of contamination from foreground and background structures along the cluster's line of sight, the space density of the clusters as a function of redshift, and their velocity dispersion distributions. We find that the Abell and EDCC catalogues are contaminated at the level of about 10 per cent, whereas the APM catalogue suffers only 5 per cent contamination. If we use the original catalogue centroids, the level of contamination rises to approximately 15 per cent for the Abell and EDCC catalogues, showing that the presence of foreground and background groups may alter the richness of clusters in these catalogues. There is a deficiency of clusters at z~0.05 hat may correspond to a large underdensity in the Southern hemisphere. From the cumulative distribution of velocity dispersions for these clusters, we derive a space density of {sigma}&gt;1000km/s clusters of 3.6x10^-6^h^3^/Mpc^3^. This result is used to constrain models for structure formation; our data favour low-density cosmologies, subject to the usual assumptions concerning the shape and normalization of the power spectrum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87#table1</TD>
            <TD>2012-09-20T13:52:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/329/87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/87</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/329/87 [1]</TD>
            <TD>2dF Galaxy Redshift Survey: galaxy clusters (de Propris+, 2002)</TD>
            <TD>We have carried out a study of known clusters within the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;) observed areas and have identified 431 Abell, 173 APM and 343 EDCC clusters. Precise redshifts, velocity dispersions and new centroids have been measured for the majority of these objects, and this information is used to study the completeness of these catalogues, the level of contamination from foreground and background structures along the cluster's line of sight, the space density of the clusters as a function of redshift, and their velocity dispersion distributions. We find that the Abell and EDCC catalogues are contaminated at the level of about 10 per cent, whereas the APM catalogue suffers only 5 per cent contamination. If we use the original catalogue centroids, the level of contamination rises to approximately 15 per cent for the Abell and EDCC catalogues, showing that the presence of foreground and background groups may alter the richness of clusters in these catalogues. There is a deficiency of clusters at z~0.05 hat may correspond to a large underdensity in the Southern hemisphere. From the cumulative distribution of velocity dispersions for these clusters, we derive a space density of {sigma}&gt;1000km/s clusters of 3.6x10^-6^h^3^/Mpc^3^. This result is used to constrain models for structure formation; our data favour low-density cosmologies, subject to the usual assumptions concerning the shape and normalization of the power spectrum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87#1</TD>
            <TD>2012-09-20T13:52:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/329/87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/329/87 [2]</TD>
            <TD>2dF Galaxy Redshift Survey: galaxy clusters (de Propris+, 2002)</TD>
            <TD>We have carried out a study of known clusters within the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;) observed areas and have identified 431 Abell, 173 APM and 343 EDCC clusters. Precise redshifts, velocity dispersions and new centroids have been measured for the majority of these objects, and this information is used to study the completeness of these catalogues, the level of contamination from foreground and background structures along the cluster's line of sight, the space density of the clusters as a function of redshift, and their velocity dispersion distributions. We find that the Abell and EDCC catalogues are contaminated at the level of about 10 per cent, whereas the APM catalogue suffers only 5 per cent contamination. If we use the original catalogue centroids, the level of contamination rises to approximately 15 per cent for the Abell and EDCC catalogues, showing that the presence of foreground and background groups may alter the richness of clusters in these catalogues. There is a deficiency of clusters at z~0.05 hat may correspond to a large underdensity in the Southern hemisphere. From the cumulative distribution of velocity dispersions for these clusters, we derive a space density of {sigma}&gt;1000km/s clusters of 3.6x10^-6^h^3^/Mpc^3^. This result is used to constrain models for structure formation; our data favour low-density cosmologies, subject to the usual assumptions concerning the shape and normalization of the power spectrum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87#2</TD>
            <TD>2012-09-20T13:52:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/329/87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/329/87 [table1]</TD>
            <TD>2dF Galaxy Redshift Survey: galaxy clusters (de Propris+, 2002)</TD>
            <TD>We have carried out a study of known clusters within the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;) observed areas and have identified 431 Abell, 173 APM and 343 EDCC clusters. Precise redshifts, velocity dispersions and new centroids have been measured for the majority of these objects, and this information is used to study the completeness of these catalogues, the level of contamination from foreground and background structures along the cluster's line of sight, the space density of the clusters as a function of redshift, and their velocity dispersion distributions. We find that the Abell and EDCC catalogues are contaminated at the level of about 10 per cent, whereas the APM catalogue suffers only 5 per cent contamination. If we use the original catalogue centroids, the level of contamination rises to approximately 15 per cent for the Abell and EDCC catalogues, showing that the presence of foreground and background groups may alter the richness of clusters in these catalogues. There is a deficiency of clusters at z~0.05 hat may correspond to a large underdensity in the Southern hemisphere. From the cumulative distribution of velocity dispersions for these clusters, we derive a space density of {sigma}&gt;1000km/s clusters of 3.6x10^-6^h^3^/Mpc^3^. This result is used to constrain models for structure formation; our data favour low-density cosmologies, subject to the usual assumptions concerning the shape and normalization of the power spectrum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87#table1</TD>
            <TD>2012-09-20T13:52:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/329/87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/87</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/329/87 [1]</TD>
            <TD>2dF Galaxy Redshift Survey: galaxy clusters (de Propris+, 2002)</TD>
            <TD>We have carried out a study of known clusters within the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;) observed areas and have identified 431 Abell, 173 APM and 343 EDCC clusters. Precise redshifts, velocity dispersions and new centroids have been measured for the majority of these objects, and this information is used to study the completeness of these catalogues, the level of contamination from foreground and background structures along the cluster's line of sight, the space density of the clusters as a function of redshift, and their velocity dispersion distributions. We find that the Abell and EDCC catalogues are contaminated at the level of about 10 per cent, whereas the APM catalogue suffers only 5 per cent contamination. If we use the original catalogue centroids, the level of contamination rises to approximately 15 per cent for the Abell and EDCC catalogues, showing that the presence of foreground and background groups may alter the richness of clusters in these catalogues. There is a deficiency of clusters at z~0.05 hat may correspond to a large underdensity in the Southern hemisphere. From the cumulative distribution of velocity dispersions for these clusters, we derive a space density of {sigma}&gt;1000km/s clusters of 3.6x10^-6^h^3^/Mpc^3^. This result is used to constrain models for structure formation; our data favour low-density cosmologies, subject to the usual assumptions concerning the shape and normalization of the power spectrum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87#1</TD>
            <TD>2012-09-20T13:52:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/329/87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/329/87 [2]</TD>
            <TD>2dF Galaxy Redshift Survey: galaxy clusters (de Propris+, 2002)</TD>
            <TD>We have carried out a study of known clusters within the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;) observed areas and have identified 431 Abell, 173 APM and 343 EDCC clusters. Precise redshifts, velocity dispersions and new centroids have been measured for the majority of these objects, and this information is used to study the completeness of these catalogues, the level of contamination from foreground and background structures along the cluster's line of sight, the space density of the clusters as a function of redshift, and their velocity dispersion distributions. We find that the Abell and EDCC catalogues are contaminated at the level of about 10 per cent, whereas the APM catalogue suffers only 5 per cent contamination. If we use the original catalogue centroids, the level of contamination rises to approximately 15 per cent for the Abell and EDCC catalogues, showing that the presence of foreground and background groups may alter the richness of clusters in these catalogues. There is a deficiency of clusters at z~0.05 hat may correspond to a large underdensity in the Southern hemisphere. From the cumulative distribution of velocity dispersions for these clusters, we derive a space density of {sigma}&gt;1000km/s clusters of 3.6x10^-6^h^3^/Mpc^3^. This result is used to constrain models for structure formation; our data favour low-density cosmologies, subject to the usual assumptions concerning the shape and normalization of the power spectrum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87#2</TD>
            <TD>2012-09-20T13:52:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/329/87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/329/87 [table1]</TD>
            <TD>2dF Galaxy Redshift Survey: galaxy clusters (de Propris+, 2002)</TD>
            <TD>We have carried out a study of known clusters within the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;) observed areas and have identified 431 Abell, 173 APM and 343 EDCC clusters. Precise redshifts, velocity dispersions and new centroids have been measured for the majority of these objects, and this information is used to study the completeness of these catalogues, the level of contamination from foreground and background structures along the cluster's line of sight, the space density of the clusters as a function of redshift, and their velocity dispersion distributions. We find that the Abell and EDCC catalogues are contaminated at the level of about 10 per cent, whereas the APM catalogue suffers only 5 per cent contamination. If we use the original catalogue centroids, the level of contamination rises to approximately 15 per cent for the Abell and EDCC catalogues, showing that the presence of foreground and background groups may alter the richness of clusters in these catalogues. There is a deficiency of clusters at z~0.05 hat may correspond to a large underdensity in the Southern hemisphere. From the cumulative distribution of velocity dispersions for these clusters, we derive a space density of {sigma}&gt;1000km/s clusters of 3.6x10^-6^h^3^/Mpc^3^. This result is used to constrain models for structure formation; our data favour low-density cosmologies, subject to the usual assumptions concerning the shape and normalization of the power spectrum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87#table1</TD>
            <TD>2012-09-20T13:52:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/329/87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GOODS</TD>
            <TD>The Great Observatories Origins Deep Survey</TD>
            <TD>GOODS North and South Open SkyNode. GOODS aims to unite extremely deep observations from NASA's Great Observatories, the Spitzer Space Telescope, Hubble, and Chandra, ESA's XMM-Newton, and from the most powerful ground-based facilities, to survey the distant universe to the faintest flux limits across the broadest range of wavelengths. GOODS incorporates a Spitzer Space Telescope Legacy Program to carry out the deepest observations with that facility at 3.6 to 24 microns, an HST Treasury Program for deep high-resolution optical imaging. GOODS will survey a total of roughly 320 square arcminutes in two fields centered on the Hubble Deep Field North and the Chandra Deep Field South. The space-based observations will be complemented by ground-based imaging and spectroscopy, including an extensive commitment of ESO and NOAO observing time.</TD>
            <TD>STScI</TD>
            <TD>#Optical#</TD>
            <TD>ivo://archive.stsci.edu/goods/SKYNODE#1</TD>
            <TD>2011-09-14T18:11:55Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD />
            <TD />
            <TD>V1.0</TD>
            <TD>ivo://archive.stsci.edu/goods/SKYNODE</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://galex.stsci.edu/skynode/ogoods/nodeb.asmx</TD>
            <TD />
            <TD>0</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UDF</TD>
            <TD>The Hubble Ultra Deep Field</TD>
            <TD>The ACS Ultra Deep Field (UDF) is a survey carried out using the Advanced Camera for Surveys (ACS) on HST and taking advantage of the Director's Discretionary time. The UDF will consist of a single ultra- deep field (412 orbits in total) within the CDF-S GOODS area. Scientific drivers of the UDF include probing the tail of the reionization epoch, constraining the star formation history of the Universe, probing the faint end of the galaxy luminosity function, and tracking the origin, structure, and merger history of galaxies as they evolve onto and off the Hubble sequence.</TD>
            <TD>STScI</TD>
            <TD>#Optical#</TD>
            <TD>ivo://archive.stsci.edu/udf/SKYNODE#1</TD>
            <TD>2011-09-14T18:11:57Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#Hubble#</TD>
            <TD />
            <TD />
            <TD />
            <TD>V1.0</TD>
            <TD>ivo://archive.stsci.edu/udf/SKYNODE</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://galex.stsci.edu/skynode/oudf/nodeb.asmx</TD>
            <TD />
            <TD>0</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/377/787 [1]</TD>
            <TD>SDSS Luminous Red Galaxies (Barber+, 2007)</TD>
            <TD>The data are taken from the Luminous Red Galaxy sample of the Sloan Digital Sky Survey Data Release 4. From the SDSS spectra we compute the five indices Hbeta, Hgamma_F_, Dn(4000), [MgFe]', [Mg1Fe]'. These are matched indices from a synthetic library of spectra containing 31000 different star formation scenarios. From this we can infer probability distributions for a number of properties, such as age, metallicity, etc. The results are presented here as the 5th, 16th, 50th (median), 86th and 95th percentiles of the relevant distribution. The 4391 LRG properties presented here are chosen from the redshift range 0.15&lt;z&lt;0.4 and require all 5 of the above indices to have well-measured values (i.e. no contamination from skylines, bad pixels) Also given are a number of properties that come directly from the SDSS database, such as redshift, velocity dispersion etc. For the luminosity distance calculation (and subsequent mass estimates), we assume a FRW metric, with omega_m_=0.25, omega_lambda_=0.75 and H_0_=73km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787#1</TD>
            <TD>2011-09-14T20:10:56Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/377/787</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/377/787</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/377/787 [2]</TD>
            <TD>SDSS Luminous Red Galaxies (Barber+, 2007)</TD>
            <TD>The data are taken from the Luminous Red Galaxy sample of the Sloan Digital Sky Survey Data Release 4. From the SDSS spectra we compute the five indices Hbeta, Hgamma_F_, Dn(4000), [MgFe]', [Mg1Fe]'. These are matched indices from a synthetic library of spectra containing 31000 different star formation scenarios. From this we can infer probability distributions for a number of properties, such as age, metallicity, etc. The results are presented here as the 5th, 16th, 50th (median), 86th and 95th percentiles of the relevant distribution. The 4391 LRG properties presented here are chosen from the redshift range 0.15&lt;z&lt;0.4 and require all 5 of the above indices to have well-measured values (i.e. no contamination from skylines, bad pixels) Also given are a number of properties that come directly from the SDSS database, such as redshift, velocity dispersion etc. For the luminosity distance calculation (and subsequent mass estimates), we assume a FRW metric, with omega_m_=0.25, omega_lambda_=0.75 and H_0_=73km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787#2</TD>
            <TD>2011-09-14T20:10:56Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/377/787&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/377/787</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/377/787 [lrgs]</TD>
            <TD>SDSS Luminous Red Galaxies (Barber+, 2007)</TD>
            <TD>The data are taken from the Luminous Red Galaxy sample of the Sloan Digital Sky Survey Data Release 4. From the SDSS spectra we compute the five indices Hbeta, Hgamma_F_, Dn(4000), [MgFe]', [Mg1Fe]'. These are matched indices from a synthetic library of spectra containing 31000 different star formation scenarios. From this we can infer probability distributions for a number of properties, such as age, metallicity, etc. The results are presented here as the 5th, 16th, 50th (median), 86th and 95th percentiles of the relevant distribution. The 4391 LRG properties presented here are chosen from the redshift range 0.15&lt;z&lt;0.4 and require all 5 of the above indices to have well-measured values (i.e. no contamination from skylines, bad pixels) Also given are a number of properties that come directly from the SDSS database, such as redshift, velocity dispersion etc. For the luminosity distance calculation (and subsequent mass estimates), we assume a FRW metric, with omega_m_=0.25, omega_lambda_=0.75 and H_0_=73km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787#lrgs</TD>
            <TD>2011-09-14T20:10:56Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/377/787&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/377/787</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RC3</TD>
            <TD>THIRD REFERENCE CATALOGUE OF BRIGHT GALAXIES</TD>
            <TD>The Third Reference Catalogue of Bright Galaxies (RC3) attempts to be reasonably complete for galaxies having apparent diameters larger than 1' at the D25 isophotal level and total B-band magnitudes BT brighter than about 15.5, with a redshift not in excess of 15,000 km/s, as well as many other objects of interest, such as compact galaxies smaller than 1' or fainter than magnitude 15.5, and those already in RC2 (de Vaucouleurs et al. 1976).</TD>
            <TD>JHU</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/RC3#1</TD>
            <TD>2011-09-14T18:12:01Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD />
            <TD>1</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/RC3</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/rc3/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>TwoDf</TD>
            <TD>2dF Galaxy Redshift Survey</TD>
            <TD>The Two Degree Field system (`2dF') is the AAT's (and arguably the world's) most complex astronomical instrument. It is designed to allow the acquisition of up to 400 simultaneous spectra of objects anywhere within a two degree field on the sky. It consists of a wide field corrector, an atmospheric dispersion compensator, a robot gantry which positions optical fibres to 0.3'' and two spectrographs each of which accepts 200 of the fibres to produce low to medium resolution spectra. A tumbling mechanism with two field plates allows the next field to be configured while the current field is being observed</TD>
            <TD>JHU</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/TwoDf#1</TD>
            <TD>2011-09-14T18:12:02Z</TD>
            <TD>#OpenSkyNode#Spectra#Redshift#</TD>
            <TD />
            <TD />
            <TD>1</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/TwoDf</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/twodf/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/377/787 [1]</TD>
            <TD>SDSS Luminous Red Galaxies (Barber+, 2007)</TD>
            <TD>The data are taken from the Luminous Red Galaxy sample of the Sloan Digital Sky Survey Data Release 4. From the SDSS spectra we compute the five indices Hbeta, Hgamma_F_, Dn(4000), [MgFe]', [Mg1Fe]'. These are matched indices from a synthetic library of spectra containing 31000 different star formation scenarios. From this we can infer probability distributions for a number of properties, such as age, metallicity, etc. The results are presented here as the 5th, 16th, 50th (median), 86th and 95th percentiles of the relevant distribution. The 4391 LRG properties presented here are chosen from the redshift range 0.15&lt;z&lt;0.4 and require all 5 of the above indices to have well-measured values (i.e. no contamination from skylines, bad pixels) Also given are a number of properties that come directly from the SDSS database, such as redshift, velocity dispersion etc. For the luminosity distance calculation (and subsequent mass estimates), we assume a FRW metric, with omega_m_=0.25, omega_lambda_=0.75 and H_0_=73km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787#1</TD>
            <TD>2011-09-14T20:10:56Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/377/787</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/377/787</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/377/787 [2]</TD>
            <TD>SDSS Luminous Red Galaxies (Barber+, 2007)</TD>
            <TD>The data are taken from the Luminous Red Galaxy sample of the Sloan Digital Sky Survey Data Release 4. From the SDSS spectra we compute the five indices Hbeta, Hgamma_F_, Dn(4000), [MgFe]', [Mg1Fe]'. These are matched indices from a synthetic library of spectra containing 31000 different star formation scenarios. From this we can infer probability distributions for a number of properties, such as age, metallicity, etc. The results are presented here as the 5th, 16th, 50th (median), 86th and 95th percentiles of the relevant distribution. The 4391 LRG properties presented here are chosen from the redshift range 0.15&lt;z&lt;0.4 and require all 5 of the above indices to have well-measured values (i.e. no contamination from skylines, bad pixels) Also given are a number of properties that come directly from the SDSS database, such as redshift, velocity dispersion etc. For the luminosity distance calculation (and subsequent mass estimates), we assume a FRW metric, with omega_m_=0.25, omega_lambda_=0.75 and H_0_=73km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787#2</TD>
            <TD>2011-09-14T20:10:56Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/377/787&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/377/787</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/377/787 [lrgs]</TD>
            <TD>SDSS Luminous Red Galaxies (Barber+, 2007)</TD>
            <TD>The data are taken from the Luminous Red Galaxy sample of the Sloan Digital Sky Survey Data Release 4. From the SDSS spectra we compute the five indices Hbeta, Hgamma_F_, Dn(4000), [MgFe]', [Mg1Fe]'. These are matched indices from a synthetic library of spectra containing 31000 different star formation scenarios. From this we can infer probability distributions for a number of properties, such as age, metallicity, etc. The results are presented here as the 5th, 16th, 50th (median), 86th and 95th percentiles of the relevant distribution. The 4391 LRG properties presented here are chosen from the redshift range 0.15&lt;z&lt;0.4 and require all 5 of the above indices to have well-measured values (i.e. no contamination from skylines, bad pixels) Also given are a number of properties that come directly from the SDSS database, such as redshift, velocity dispersion etc. For the luminosity distance calculation (and subsequent mass estimates), we assume a FRW metric, with omega_m_=0.25, omega_lambda_=0.75 and H_0_=73km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787#lrgs</TD>
            <TD>2011-09-14T20:10:56Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/377/787&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/377/787</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/122/109 [1]</TD>
            <TD>Galaxy structural parameters (Takamiya+, 1999)</TD>
            <TD>The evolution of the structure of galaxies as a function of redshift is investigated using two parameters: the metric radius of the galaxy (R_eta_) and the power at high spatial frequencies in the disk of the galaxy (chi). A direct comparison is made between nearby (z~0) and distant (0.2&lt;~z&lt;~1) galaxies by following a fixed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broadband images at ~4500 E observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies, 1996AJ....111..174F). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between ~3000 and ~9000 E (Williams et al., 1997, Cat. &lt;J/AJ/112/1335&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/109#1</TD>
            <TD>2011-09-14T17:51:27Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/122/109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/122/109 [2]</TD>
            <TD>Galaxy structural parameters (Takamiya+, 1999)</TD>
            <TD>The evolution of the structure of galaxies as a function of redshift is investigated using two parameters: the metric radius of the galaxy (R_eta_) and the power at high spatial frequencies in the disk of the galaxy (chi). A direct comparison is made between nearby (z~0) and distant (0.2&lt;~z&lt;~1) galaxies by following a fixed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broadband images at ~4500 E observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies, 1996AJ....111..174F). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between ~3000 and ~9000 E (Williams et al., 1997, Cat. &lt;J/AJ/112/1335&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/109#2</TD>
            <TD>2011-09-14T17:51:27Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/122/109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/377/787 [1]</TD>
            <TD>SDSS Luminous Red Galaxies (Barber+, 2007)</TD>
            <TD>The data are taken from the Luminous Red Galaxy sample of the Sloan Digital Sky Survey Data Release 4. From the SDSS spectra we compute the five indices Hbeta, Hgamma_F_, Dn(4000), [MgFe]', [Mg1Fe]'. These are matched indices from a synthetic library of spectra containing 31000 different star formation scenarios. From this we can infer probability distributions for a number of properties, such as age, metallicity, etc. The results are presented here as the 5th, 16th, 50th (median), 86th and 95th percentiles of the relevant distribution. The 4391 LRG properties presented here are chosen from the redshift range 0.15&lt;z&lt;0.4 and require all 5 of the above indices to have well-measured values (i.e. no contamination from skylines, bad pixels) Also given are a number of properties that come directly from the SDSS database, such as redshift, velocity dispersion etc. For the luminosity distance calculation (and subsequent mass estimates), we assume a FRW metric, with omega_m_=0.25, omega_lambda_=0.75 and H_0_=73km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787#1</TD>
            <TD>2011-09-14T20:10:56Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/377/787</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/377/787</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/377/787 [2]</TD>
            <TD>SDSS Luminous Red Galaxies (Barber+, 2007)</TD>
            <TD>The data are taken from the Luminous Red Galaxy sample of the Sloan Digital Sky Survey Data Release 4. From the SDSS spectra we compute the five indices Hbeta, Hgamma_F_, Dn(4000), [MgFe]', [Mg1Fe]'. These are matched indices from a synthetic library of spectra containing 31000 different star formation scenarios. From this we can infer probability distributions for a number of properties, such as age, metallicity, etc. The results are presented here as the 5th, 16th, 50th (median), 86th and 95th percentiles of the relevant distribution. The 4391 LRG properties presented here are chosen from the redshift range 0.15&lt;z&lt;0.4 and require all 5 of the above indices to have well-measured values (i.e. no contamination from skylines, bad pixels) Also given are a number of properties that come directly from the SDSS database, such as redshift, velocity dispersion etc. For the luminosity distance calculation (and subsequent mass estimates), we assume a FRW metric, with omega_m_=0.25, omega_lambda_=0.75 and H_0_=73km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787#2</TD>
            <TD>2011-09-14T20:10:56Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/377/787&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/377/787</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/377/787 [lrgs]</TD>
            <TD>SDSS Luminous Red Galaxies (Barber+, 2007)</TD>
            <TD>The data are taken from the Luminous Red Galaxy sample of the Sloan Digital Sky Survey Data Release 4. From the SDSS spectra we compute the five indices Hbeta, Hgamma_F_, Dn(4000), [MgFe]', [Mg1Fe]'. These are matched indices from a synthetic library of spectra containing 31000 different star formation scenarios. From this we can infer probability distributions for a number of properties, such as age, metallicity, etc. The results are presented here as the 5th, 16th, 50th (median), 86th and 95th percentiles of the relevant distribution. The 4391 LRG properties presented here are chosen from the redshift range 0.15&lt;z&lt;0.4 and require all 5 of the above indices to have well-measured values (i.e. no contamination from skylines, bad pixels) Also given are a number of properties that come directly from the SDSS database, such as redshift, velocity dispersion etc. For the luminosity distance calculation (and subsequent mass estimates), we assume a FRW metric, with omega_m_=0.25, omega_lambda_=0.75 and H_0_=73km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787#lrgs</TD>
            <TD>2011-09-14T20:10:56Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/377/787</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/377/787&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/377/787</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/122/109 [1]</TD>
            <TD>Galaxy structural parameters (Takamiya+, 1999)</TD>
            <TD>The evolution of the structure of galaxies as a function of redshift is investigated using two parameters: the metric radius of the galaxy (R_eta_) and the power at high spatial frequencies in the disk of the galaxy (chi). A direct comparison is made between nearby (z~0) and distant (0.2&lt;~z&lt;~1) galaxies by following a fixed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broadband images at ~4500 E observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies, 1996AJ....111..174F). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between ~3000 and ~9000 E (Williams et al., 1997, Cat. &lt;J/AJ/112/1335&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/109#1</TD>
            <TD>2011-09-14T17:51:27Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/122/109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/122/109 [2]</TD>
            <TD>Galaxy structural parameters (Takamiya+, 1999)</TD>
            <TD>The evolution of the structure of galaxies as a function of redshift is investigated using two parameters: the metric radius of the galaxy (R_eta_) and the power at high spatial frequencies in the disk of the galaxy (chi). A direct comparison is made between nearby (z~0) and distant (0.2&lt;~z&lt;~1) galaxies by following a fixed range in rest frame wavelengths. The data of the nearby galaxies comprise 136 broadband images at ~4500 E observed with the 0.9 m telescope at Kitt Peak National Observatory (23 galaxies) and selected from the catalog of digital images of Frei et al. (113 galaxies, 1996AJ....111..174F). The high-redshift sample comprises 94 galaxies selected from the Hubble Deep Field (HDF) observations with the Hubble Space Telescope using the Wide Field Planetary Camera 2 in four broad bands that range between ~3000 and ~9000 E (Williams et al., 1997, Cat. &lt;J/AJ/112/1335&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/109#2</TD>
            <TD>2011-09-14T17:51:27Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/122/109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/362/9 [1]</TD>
            <TD>Radio-loud AGN in SDSS (Best+, 2005)</TD>
            <TD>A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS, &lt;VIII/65&gt;) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9% reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000{AA} break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5mJy at 1.4GHz. A full catalogue of positions and radio properties is provided for these sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9#1</TD>
            <TD>2011-09-14T20:10:58Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/362/9</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/362/9</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/362/9 [2]</TD>
            <TD>Radio-loud AGN in SDSS (Best+, 2005)</TD>
            <TD>A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS, &lt;VIII/65&gt;) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9% reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000{AA} break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5mJy at 1.4GHz. A full catalogue of positions and radio properties is provided for these sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9#2</TD>
            <TD>2011-09-14T20:10:58Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/362/9&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/362/9</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/362/9 [table2]</TD>
            <TD>Radio-loud AGN in SDSS (Best+, 2005)</TD>
            <TD>A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS, &lt;VIII/65&gt;) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9% reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000{AA} break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5mJy at 1.4GHz. A full catalogue of positions and radio properties is provided for these sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9#table2</TD>
            <TD>2011-09-14T20:10:58Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/362/9&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/362/9</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/112 [1]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112#1</TD>
            <TD>2011-09-14T17:51:29Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/V/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/112</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/112 [2]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112#2</TD>
            <TD>2011-09-14T17:51:29Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/V/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/112&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/112 [catalog]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
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            <TD>2011-09-14T17:51:29Z</TD>
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            <TD>#Research#</TD>
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            <TD>17-Jul-2002</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>V/112 [1]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112#1</TD>
            <TD>2011-09-14T17:51:29Z</TD>
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            <TD>17-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/V/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/112</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/112 [2]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112#2</TD>
            <TD>2011-09-14T17:51:29Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/V/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/112&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>V/112 [catalog]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112#catalog</TD>
            <TD>2011-09-14T17:51:29Z</TD>
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            <TD>17-Jul-2002</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>V/112 [1]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112#1</TD>
            <TD>2011-09-14T17:51:29Z</TD>
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            <TD>17-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/V/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/112</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/112 [2]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112#2</TD>
            <TD>2011-09-14T17:51:29Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>17-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/V/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/112&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>V/112 [catalog]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>This Catalog of Star-Forming Regions in the Galaxy contains coordinates and fluxes of young objects in the radio and infrared, as well as data on the radial velocities of recombination and molecular lines, for more than three thousand star-forming regions. In addition to photometric and kinematic data, we present information on diffuse and reflecting nebulae, dark and molecular clouds, and other objects related to young stars. The catalog consists of two parts. The main catalog lists star-forming regions in order of Galactic longitude and is supplemented by analogous information for star-forming regions in complexes of dark clouds with large angular sizes that are closest to the Sun. In our preliminary study of the catalog data using a formal classification of the star-forming regions, we subdivided these objects into several classes and characterized them as being populated primarily by massive or low-mass stars at early or late stages of the star-formation process. We also distinguish between relatively nearby and distant complexes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112#catalog</TD>
            <TD>2011-09-14T17:51:29Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/V/112</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/112&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>SDSS-DR5</TD>
            <TD>Sloan Digital Sky Survey (DR5)</TD>
            <TD>The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey</TD>
            <TD>The Johns Hopkins Univer</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/services/DR5CONE#1</TD>
            <TD>2011-09-14T17:51:47Z</TD>
            <TD>#Stars#Survey#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.100000001490116</TD>
            <TD>DR5</TD>
            <TD>ivo://sdss.jhu/services/DR5CONE</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://casjobs.sdss.org/vo/dr5cone/sdssConeSearch.asmx/ConeSearch?</TD>
            <TD>1</TD>
            <TD>5000</TD>
            <TD />
            <TD>http://www.sdss.jhu.edu/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSSDR3</TD>
            <TD>Sloan Digital Sky Survey (DR3)</TD>
            <TD>Simply put, the Sloan Digital Sky Survey is the most ambitious astronomical survey ever undertaken. The survey will map one-quarter of the entire sky in detail, determining the positions and absolute brightnesses of hundreds of millions of celestial objects. It will also measure the distances to more than a million galaxies and quasars. The SDSS addresses fascinating, fundamental questions about the universe. With the survey, astronomers will be able to see the large-scale patterns of galaxies: sheets and voids through the whole universe. Scientists have many ideas about how the universe evolved, and different patterns of large-scale structure point to different theories. The Sloan Digital Sky Survey will tell us which theories are right - or whether we will have to come up with entirely new ideas.</TD>
            <TD>JHU</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/SDSSDR3#1</TD>
            <TD>2011-09-14T18:12:15Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD>#Research#</TD>
            <TD>0.800000011920929</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/SDSSDR3</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes//SDSSDR3/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/362/9 [1]</TD>
            <TD>Radio-loud AGN in SDSS (Best+, 2005)</TD>
            <TD>A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS, &lt;VIII/65&gt;) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9% reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000{AA} break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5mJy at 1.4GHz. A full catalogue of positions and radio properties is provided for these sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9#1</TD>
            <TD>2011-09-14T20:10:58Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/362/9</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/362/9</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/362/9 [2]</TD>
            <TD>Radio-loud AGN in SDSS (Best+, 2005)</TD>
            <TD>A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS, &lt;VIII/65&gt;) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9% reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000{AA} break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5mJy at 1.4GHz. A full catalogue of positions and radio properties is provided for these sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9#2</TD>
            <TD>2011-09-14T20:10:58Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/362/9&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/362/9</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/362/9 [table2]</TD>
            <TD>Radio-loud AGN in SDSS (Best+, 2005)</TD>
            <TD>A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS, &lt;VIII/65&gt;) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9% reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000{AA} break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5mJy at 1.4GHz. A full catalogue of positions and radio properties is provided for these sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9#table2</TD>
            <TD>2011-09-14T20:10:58Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/362/9&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/362/9</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/362/9 [1]</TD>
            <TD>Radio-loud AGN in SDSS (Best+, 2005)</TD>
            <TD>A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS, &lt;VIII/65&gt;) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9% reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000{AA} break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5mJy at 1.4GHz. A full catalogue of positions and radio properties is provided for these sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9#1</TD>
            <TD>2011-09-14T20:10:58Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/362/9</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/362/9</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/362/9 [2]</TD>
            <TD>Radio-loud AGN in SDSS (Best+, 2005)</TD>
            <TD>A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS, &lt;VIII/65&gt;) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9% reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000{AA} break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5mJy at 1.4GHz. A full catalogue of positions and radio properties is provided for these sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9#2</TD>
            <TD>2011-09-14T20:10:58Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/362/9&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/362/9</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/362/9 [table2]</TD>
            <TD>Radio-loud AGN in SDSS (Best+, 2005)</TD>
            <TD>A sample of 2712 radio-luminous galaxies is defined from the second data release of the Sloan Digital Sky Survey (SDSS) by cross-comparing the main spectroscopic galaxy sample with two radio surveys: the National Radio Astronomy Observatories (NRAO) Very Large Array (VLA) Sky Survey (NVSS, &lt;VIII/65&gt;) and the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) survey. The comparison is carried out in a multistage process and makes optimal use of both radio surveys by exploiting the sensitivity of the NVSS to extended and multicomponent radio sources in addition to the high angular resolution of the FIRST images. A radio source sample with 95 per cent completeness and 98.9% reliability is achieved, far better than would be possible for this sample if only one of the surveys was used. The radio source sample is then divided into two classes: radio-loud active galactic nuclei (AGN) and galaxies in which the radio emission is dominated by star formation. The division is based on the location of a galaxy in the plane of 4000{AA} break strength versus radio luminosity per unit stellar mass and provides a sample of 2215 radio-loud AGN and 497 star-forming galaxies brighter than 5mJy at 1.4GHz. A full catalogue of positions and radio properties is provided for these sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9#table2</TD>
            <TD>2011-09-14T20:10:58Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/362/9</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/362/9&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/362/9</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/300/323 [1]</TD>
            <TD>NOT GL survey of multiply imaged quasars (Jaunsen+, 1995)</TD>
            <TD>A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323#1</TD>
            <TD>2011-09-14T18:14:48Z</TD>
            <TD>#Photometry#Gravitational_lensing#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/300/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/300/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/300/323 [2]</TD>
            <TD>NOT GL survey of multiply imaged quasars (Jaunsen+, 1995)</TD>
            <TD>A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323#2</TD>
            <TD>2011-09-14T18:14:48Z</TD>
            <TD>#Photometry#Gravitational_lensing#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/300/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/300/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/300/323 [table1]</TD>
            <TD>NOT GL survey of multiply imaged quasars (Jaunsen+, 1995)</TD>
            <TD>A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323#table1</TD>
            <TD>2011-09-14T18:14:48Z</TD>
            <TD>#Photometry#Gravitational_lensing#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/300/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/300/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/300/323 [1]</TD>
            <TD>NOT GL survey of multiply imaged quasars (Jaunsen+, 1995)</TD>
            <TD>A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323#1</TD>
            <TD>2011-09-14T18:14:48Z</TD>
            <TD>#Photometry#Gravitational_lensing#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/300/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/300/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/300/323 [2]</TD>
            <TD>NOT GL survey of multiply imaged quasars (Jaunsen+, 1995)</TD>
            <TD>A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323#2</TD>
            <TD>2011-09-14T18:14:48Z</TD>
            <TD>#Photometry#Gravitational_lensing#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/300/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/300/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/300/323 [table1]</TD>
            <TD>NOT GL survey of multiply imaged quasars (Jaunsen+, 1995)</TD>
            <TD>A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323#table1</TD>
            <TD>2011-09-14T18:14:48Z</TD>
            <TD>#Photometry#Gravitational_lensing#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/300/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/300/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/451 [1]</TD>
            <TD>Radio continuum spectra of GPS galaxies (Torniainen+, 2007)</TD>
            <TD>Radio continuum spectral properties of a sample of 96 galaxy-type gigahertz-peaked spectrum (GPS) sources are presented. When available, also the redshifts of the sources are listed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451#1</TD>
            <TD>2011-09-14T20:11:31Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/451 [2]</TD>
            <TD>Radio continuum spectra of GPS galaxies (Torniainen+, 2007)</TD>
            <TD>Radio continuum spectral properties of a sample of 96 galaxy-type gigahertz-peaked spectrum (GPS) sources are presented. When available, also the redshifts of the sources are listed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451#2</TD>
            <TD>2011-09-14T20:11:31Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/451 [table2]</TD>
            <TD>Radio continuum spectra of GPS galaxies (Torniainen+, 2007)</TD>
            <TD>Radio continuum spectral properties of a sample of 96 galaxy-type gigahertz-peaked spectrum (GPS) sources are presented. When available, also the redshifts of the sources are listed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451#table2</TD>
            <TD>2011-09-14T20:11:31Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/300/323 [1]</TD>
            <TD>NOT GL survey of multiply imaged quasars (Jaunsen+, 1995)</TD>
            <TD>A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323#1</TD>
            <TD>2011-09-14T18:14:48Z</TD>
            <TD>#Photometry#Gravitational_lensing#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/300/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/300/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/300/323 [2]</TD>
            <TD>NOT GL survey of multiply imaged quasars (Jaunsen+, 1995)</TD>
            <TD>A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323#2</TD>
            <TD>2011-09-14T18:14:48Z</TD>
            <TD>#Photometry#Gravitational_lensing#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/300/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/300/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/300/323 [table1]</TD>
            <TD>NOT GL survey of multiply imaged quasars (Jaunsen+, 1995)</TD>
            <TD>A gravitational lens (GL)-search program, initiated in 1990 at the Nordic Optcal Telescope (NOT), has revealed several possible GL-candidates among a sample of 168 quasars (QSOs), chosen from three lists compiled by C. Hazard, D. Reimers and J. Surdej, respectively. Some of these candidates, selected for having close companions (within 5 arcseconds), were imaged in several filters and their colours compared. Low dispersion spectra of the most promising candidates were also obtained at the NOT and ESO New Technology Telescope (NTT). None of these has proved to be strong candidates of gravitational lensing effects. We present this new sample of QSOs and combine it with previously published optical QSO samples in a statistical analysis to yield constraints on flat cosmologies and galaxy velocity dispersions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323#table1</TD>
            <TD>2011-09-14T18:14:48Z</TD>
            <TD>#Photometry#Gravitational_lensing#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/300/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/300/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/300/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/643 [1]</TD>
            <TD>GALEX UV photometry of M31 Globular Clusters (Rey+, 2007)</TD>
            <TD>The M31 images were obtained as part of the Nearby Galaxy Survey (NGS) carried out by GALEX in two UV bands: FUV (135-175nm) and NUV (175-275nm). Details on the early observations of 14 fields released under the GALEX Release 1 (GR1) can be found in Thilker et al. (2005ApJ...619L..67T) and Paper I (Rey et al., 2005ApJ...619L.119R). We have observed an additional nine GALEX fields in 2004 September-November, which are included in the GALEX Release 2 (GR2).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643#1</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/643</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/643</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/643 [2]</TD>
            <TD>GALEX UV photometry of M31 Globular Clusters (Rey+, 2007)</TD>
            <TD>The M31 images were obtained as part of the Nearby Galaxy Survey (NGS) carried out by GALEX in two UV bands: FUV (135-175nm) and NUV (175-275nm). Details on the early observations of 14 fields released under the GALEX Release 1 (GR1) can be found in Thilker et al. (2005ApJ...619L..67T) and Paper I (Rey et al., 2005ApJ...619L.119R). We have observed an additional nine GALEX fields in 2004 September-November, which are included in the GALEX Release 2 (GR2).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643#2</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/643&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/643</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/173/643 [table2]</TD>
            <TD>GALEX UV photometry of M31 Globular Clusters (Rey+, 2007)</TD>
            <TD>The M31 images were obtained as part of the Nearby Galaxy Survey (NGS) carried out by GALEX in two UV bands: FUV (135-175nm) and NUV (175-275nm). Details on the early observations of 14 fields released under the GALEX Release 1 (GR1) can be found in Thilker et al. (2005ApJ...619L..67T) and Paper I (Rey et al., 2005ApJ...619L.119R). We have observed an additional nine GALEX fields in 2004 September-November, which are included in the GALEX Release 2 (GR2).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643#table2</TD>
            <TD>2011-09-14T20:45:45Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/643</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/173/643&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/643</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/539/577 [1]</TD>
            <TD>Galaxy morphologies in Cl 1358+62 (Fabricant+, 2000)</TD>
            <TD>We describe the morphological composition of a sample of 518 galaxies in the field of Cl 1358+62 at z=0.33, drawn from a large Hubble Space Telescope mosaic covering 53 square arcminutes. The sample is complete to I=22, corresponding to M_V_=-18.5 in the rest frame. The galaxy morphologies have been independently classified by the authors of this paper and by Alan Dressler. Dressler's classifications place our work in context with the previous MORPHS study and allow us to estimate the scatter between different sets of visual classifications. We restrict most of our analysis to the brighter part of the sample, I&lt;21 (M_V_&lt;-19.5), where the scatter between the two sets of classifications is 1 in morphological type.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577#1</TD>
            <TD>2011-09-14T20:23:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/539/577</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/577</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/539/577 [2]</TD>
            <TD>Galaxy morphologies in Cl 1358+62 (Fabricant+, 2000)</TD>
            <TD>We describe the morphological composition of a sample of 518 galaxies in the field of Cl 1358+62 at z=0.33, drawn from a large Hubble Space Telescope mosaic covering 53 square arcminutes. The sample is complete to I=22, corresponding to M_V_=-18.5 in the rest frame. The galaxy morphologies have been independently classified by the authors of this paper and by Alan Dressler. Dressler's classifications place our work in context with the previous MORPHS study and allow us to estimate the scatter between different sets of visual classifications. We restrict most of our analysis to the brighter part of the sample, I&lt;21 (M_V_&lt;-19.5), where the scatter between the two sets of classifications is 1 in morphological type.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577#2</TD>
            <TD>2011-09-14T20:23:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/539/577&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/577</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/539/577 [table2]</TD>
            <TD>Galaxy morphologies in Cl 1358+62 (Fabricant+, 2000)</TD>
            <TD>We describe the morphological composition of a sample of 518 galaxies in the field of Cl 1358+62 at z=0.33, drawn from a large Hubble Space Telescope mosaic covering 53 square arcminutes. The sample is complete to I=22, corresponding to M_V_=-18.5 in the rest frame. The galaxy morphologies have been independently classified by the authors of this paper and by Alan Dressler. Dressler's classifications place our work in context with the previous MORPHS study and allow us to estimate the scatter between different sets of visual classifications. We restrict most of our analysis to the brighter part of the sample, I&lt;21 (M_V_&lt;-19.5), where the scatter between the two sets of classifications is 1 in morphological type.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577#table2</TD>
            <TD>2011-09-14T20:23:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/539/577&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/577</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/315/40 [1]</TD>
            <TD>Photometry of the Tuc dwarf galaxy (Saviane, 1996)</TD>
            <TD>We present V and I CCD photometry for ~360 stars in the recently discovered dwarf galaxy Tucana. The large field investigated and the accurate photometric calibration make our data complementary to the deeper HST photometry. From the I magnitude of the tip of the red giant branch we estimate a distance modulus (m-M)_0_=24.69+/-0.16, corresponding to 870+/-60Kpc, confirming that Tucana is an isolated dwarf spheroidal located almost at the border of the Local Group. From the color of the red giant branch tip and by direct comparison with the giant branches of galactic globular clusters we estimate a metallicity [Fe/H]=-1.8+/-0.2, with no clear indication for a metallicity spread. The color-magnitude diagram indicates that Tucana has had a single star formation burst at the epoch of the Galactic globular cluster star formation. There is no evidence for an intermediate or young stellar population. We derive the V luminosity profile, the surface density profile of resolved stars, and the structural parameters of Tucana, from which we confirm that Tucana participates to the general metallicity-surface brightness-absolute magnitude relations defined by the Galaxy and M31 dwarf spheroidal and dwarf elliptical companions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/315/40#1</TD>
            <TD>2011-09-14T18:15:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/315/40</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/315/40</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/315/40</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/315/40 [2]</TD>
            <TD>Photometry of the Tuc dwarf galaxy (Saviane, 1996)</TD>
            <TD>We present V and I CCD photometry for ~360 stars in the recently discovered dwarf galaxy Tucana. The large field investigated and the accurate photometric calibration make our data complementary to the deeper HST photometry. From the I magnitude of the tip of the red giant branch we estimate a distance modulus (m-M)_0_=24.69+/-0.16, corresponding to 870+/-60Kpc, confirming that Tucana is an isolated dwarf spheroidal located almost at the border of the Local Group. From the color of the red giant branch tip and by direct comparison with the giant branches of galactic globular clusters we estimate a metallicity [Fe/H]=-1.8+/-0.2, with no clear indication for a metallicity spread. The color-magnitude diagram indicates that Tucana has had a single star formation burst at the epoch of the Galactic globular cluster star formation. There is no evidence for an intermediate or young stellar population. We derive the V luminosity profile, the surface density profile of resolved stars, and the structural parameters of Tucana, from which we confirm that Tucana participates to the general metallicity-surface brightness-absolute magnitude relations defined by the Galaxy and M31 dwarf spheroidal and dwarf elliptical companions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/315/40#2</TD>
            <TD>2011-09-14T18:15:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/315/40</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/315/40&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/315/40</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/315/40 [1]</TD>
            <TD>Photometry of the Tuc dwarf galaxy (Saviane, 1996)</TD>
            <TD>We present V and I CCD photometry for ~360 stars in the recently discovered dwarf galaxy Tucana. The large field investigated and the accurate photometric calibration make our data complementary to the deeper HST photometry. From the I magnitude of the tip of the red giant branch we estimate a distance modulus (m-M)_0_=24.69+/-0.16, corresponding to 870+/-60Kpc, confirming that Tucana is an isolated dwarf spheroidal located almost at the border of the Local Group. From the color of the red giant branch tip and by direct comparison with the giant branches of galactic globular clusters we estimate a metallicity [Fe/H]=-1.8+/-0.2, with no clear indication for a metallicity spread. The color-magnitude diagram indicates that Tucana has had a single star formation burst at the epoch of the Galactic globular cluster star formation. There is no evidence for an intermediate or young stellar population. We derive the V luminosity profile, the surface density profile of resolved stars, and the structural parameters of Tucana, from which we confirm that Tucana participates to the general metallicity-surface brightness-absolute magnitude relations defined by the Galaxy and M31 dwarf spheroidal and dwarf elliptical companions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/315/40#1</TD>
            <TD>2011-09-14T18:15:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/315/40</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/315/40</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/315/40</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/315/40 [2]</TD>
            <TD>Photometry of the Tuc dwarf galaxy (Saviane, 1996)</TD>
            <TD>We present V and I CCD photometry for ~360 stars in the recently discovered dwarf galaxy Tucana. The large field investigated and the accurate photometric calibration make our data complementary to the deeper HST photometry. From the I magnitude of the tip of the red giant branch we estimate a distance modulus (m-M)_0_=24.69+/-0.16, corresponding to 870+/-60Kpc, confirming that Tucana is an isolated dwarf spheroidal located almost at the border of the Local Group. From the color of the red giant branch tip and by direct comparison with the giant branches of galactic globular clusters we estimate a metallicity [Fe/H]=-1.8+/-0.2, with no clear indication for a metallicity spread. The color-magnitude diagram indicates that Tucana has had a single star formation burst at the epoch of the Galactic globular cluster star formation. There is no evidence for an intermediate or young stellar population. We derive the V luminosity profile, the surface density profile of resolved stars, and the structural parameters of Tucana, from which we confirm that Tucana participates to the general metallicity-surface brightness-absolute magnitude relations defined by the Galaxy and M31 dwarf spheroidal and dwarf elliptical companions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/315/40#2</TD>
            <TD>2011-09-14T18:15:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/315/40</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/315/40&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/315/40</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/293 [1]</TD>
            <TD>GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)</TD>
            <TD>The Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), is a survey of Galactic Plane central parts made with the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope (SST). It covers approximately 220 square degrees, between galactic longitudes +/-65{deg} and +/-1{deg} in galactic latitude (up to 4.2{deg} in the central parts). The four IRAC bands are centered at approximately 3.6, 4.5, 5.8 and 8.0{mu}m. The GLIMPSE combines the 3 surveys: * GLIMPSE-I covers the longitude ranges |l|=10--65{deg} and the latitude range |b|&lt;=1{deg} (Benjamin et al. 2003PASP..115..953B) * GLIMPSE-II covers the longitude range of |l|&lt;=10{deg}, and a latitude range |b|&lt;=1{deg} from |l|=5--10, |b|&lt;=1.5 for |l|=2--5, and |b|&lt;=2{deg} for |l|&lt;=2. GLIMPSE-II coverage excludes the Galactic center region |l|&lt;=1, |b|&lt;=0.75 observed by the GALCEN GO program (PID=3677). * GLIMPSE-3D adds vertical extensions up to |b|=4.2{deg} near the galactic center, and up to |b|=3{deg} in selected other parts of the Galaxy (+/-10, 18.5, 25, 30, and -15 (345){deg}). GLIMPSE-II had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006). The highly reliable v2.0 GLIMPSEII Catalog (v2.0_GLMIIC) consists of point sources that are detected at least twice in one band and at least once in an adjacent band and a S/N &gt; 5 cut for the band with the two detections. There are also faint and bright flux limits on the Catalog entries. The more complete v2.0 Archive (v2.0_GLMIIA) has less stringent criteria, namely two detections in any bands, those detections having a S/N &gt; 5. The IRAC data were bandmerged with the 2MASS All-Sky Point Source Catalog. See the GLIMPSEII v2.0 Data Products &amp; Data Delivery document for more details. The catalog available from CDS merges the 3 surveys GLIMPSE-I (v2.0), GLIMPSE-II (v2.0), and GLIMPSE-3D; Catalog and Archive records are also merged here. In the regions of overlap between the 3 surveys (e.g. longitude around 10{deg}) preference was given to (1) GLIMPSE-II, as recommended in the GLIMPSE documents of May 2007 (glimpse1_v2.0.pdf) and April 2008 (glimpse2-v2.0.pdf); (2) GLIMPSE-I, and (3) GLIMPSE-3D sources. Sources from different surveys were merged if their position is closer than 0.1arcsec. Documents and a document describing in detail the point source photometry steps, see http://www.astro.wisc.edu/glimpse/docs.html</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/293#1</TD>
            <TD>2011-09-14T20:55:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/II/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/293 [2]</TD>
            <TD>GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)</TD>
            <TD>The Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), is a survey of Galactic Plane central parts made with the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope (SST). It covers approximately 220 square degrees, between galactic longitudes +/-65{deg} and +/-1{deg} in galactic latitude (up to 4.2{deg} in the central parts). The four IRAC bands are centered at approximately 3.6, 4.5, 5.8 and 8.0{mu}m. The GLIMPSE combines the 3 surveys: * GLIMPSE-I covers the longitude ranges |l|=10--65{deg} and the latitude range |b|&lt;=1{deg} (Benjamin et al. 2003PASP..115..953B) * GLIMPSE-II covers the longitude range of |l|&lt;=10{deg}, and a latitude range |b|&lt;=1{deg} from |l|=5--10, |b|&lt;=1.5 for |l|=2--5, and |b|&lt;=2{deg} for |l|&lt;=2. GLIMPSE-II coverage excludes the Galactic center region |l|&lt;=1, |b|&lt;=0.75 observed by the GALCEN GO program (PID=3677). * GLIMPSE-3D adds vertical extensions up to |b|=4.2{deg} near the galactic center, and up to |b|=3{deg} in selected other parts of the Galaxy (+/-10, 18.5, 25, 30, and -15 (345){deg}). GLIMPSE-II had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006). The highly reliable v2.0 GLIMPSEII Catalog (v2.0_GLMIIC) consists of point sources that are detected at least twice in one band and at least once in an adjacent band and a S/N &gt; 5 cut for the band with the two detections. There are also faint and bright flux limits on the Catalog entries. The more complete v2.0 Archive (v2.0_GLMIIA) has less stringent criteria, namely two detections in any bands, those detections having a S/N &gt; 5. The IRAC data were bandmerged with the 2MASS All-Sky Point Source Catalog. See the GLIMPSEII v2.0 Data Products &amp; Data Delivery document for more details. The catalog available from CDS merges the 3 surveys GLIMPSE-I (v2.0), GLIMPSE-II (v2.0), and GLIMPSE-3D; Catalog and Archive records are also merged here. In the regions of overlap between the 3 surveys (e.g. longitude around 10{deg}) preference was given to (1) GLIMPSE-II, as recommended in the GLIMPSE documents of May 2007 (glimpse1_v2.0.pdf) and April 2008 (glimpse2-v2.0.pdf); (2) GLIMPSE-I, and (3) GLIMPSE-3D sources. Sources from different surveys were merged if their position is closer than 0.1arcsec. Documents and a document describing in detail the point source photometry steps, see http://www.astro.wisc.edu/glimpse/docs.html</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/293#2</TD>
            <TD>2011-09-14T20:55:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/II/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/293 [glimpse]</TD>
            <TD>GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)</TD>
            <TD>The Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), is a survey of Galactic Plane central parts made with the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope (SST). It covers approximately 220 square degrees, between galactic longitudes +/-65{deg} and +/-1{deg} in galactic latitude (up to 4.2{deg} in the central parts). The four IRAC bands are centered at approximately 3.6, 4.5, 5.8 and 8.0{mu}m. The GLIMPSE combines the 3 surveys: * GLIMPSE-I covers the longitude ranges |l|=10--65{deg} and the latitude range |b|&lt;=1{deg} (Benjamin et al. 2003PASP..115..953B) * GLIMPSE-II covers the longitude range of |l|&lt;=10{deg}, and a latitude range |b|&lt;=1{deg} from |l|=5--10, |b|&lt;=1.5 for |l|=2--5, and |b|&lt;=2{deg} for |l|&lt;=2. GLIMPSE-II coverage excludes the Galactic center region |l|&lt;=1, |b|&lt;=0.75 observed by the GALCEN GO program (PID=3677). * GLIMPSE-3D adds vertical extensions up to |b|=4.2{deg} near the galactic center, and up to |b|=3{deg} in selected other parts of the Galaxy (+/-10, 18.5, 25, 30, and -15 (345){deg}). GLIMPSE-II had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006). The highly reliable v2.0 GLIMPSEII Catalog (v2.0_GLMIIC) consists of point sources that are detected at least twice in one band and at least once in an adjacent band and a S/N &gt; 5 cut for the band with the two detections. There are also faint and bright flux limits on the Catalog entries. The more complete v2.0 Archive (v2.0_GLMIIA) has less stringent criteria, namely two detections in any bands, those detections having a S/N &gt; 5. The IRAC data were bandmerged with the 2MASS All-Sky Point Source Catalog. See the GLIMPSEII v2.0 Data Products &amp; Data Delivery document for more details. The catalog available from CDS merges the 3 surveys GLIMPSE-I (v2.0), GLIMPSE-II (v2.0), and GLIMPSE-3D; Catalog and Archive records are also merged here. In the regions of overlap between the 3 surveys (e.g. longitude around 10{deg}) preference was given to (1) GLIMPSE-II, as recommended in the GLIMPSE documents of May 2007 (glimpse1_v2.0.pdf) and April 2008 (glimpse2-v2.0.pdf); (2) GLIMPSE-I, and (3) GLIMPSE-3D sources. Sources from different surveys were merged if their position is closer than 0.1arcsec. Documents and a document describing in detail the point source photometry steps, see http://www.astro.wisc.edu/glimpse/docs.html</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/293#glimpse</TD>
            <TD>2011-09-14T20:55:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/II/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/293</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/293 [1]</TD>
            <TD>GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)</TD>
            <TD>The Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), is a survey of Galactic Plane central parts made with the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope (SST). It covers approximately 220 square degrees, between galactic longitudes +/-65{deg} and +/-1{deg} in galactic latitude (up to 4.2{deg} in the central parts). The four IRAC bands are centered at approximately 3.6, 4.5, 5.8 and 8.0{mu}m. The GLIMPSE combines the 3 surveys: * GLIMPSE-I covers the longitude ranges |l|=10--65{deg} and the latitude range |b|&lt;=1{deg} (Benjamin et al. 2003PASP..115..953B) * GLIMPSE-II covers the longitude range of |l|&lt;=10{deg}, and a latitude range |b|&lt;=1{deg} from |l|=5--10, |b|&lt;=1.5 for |l|=2--5, and |b|&lt;=2{deg} for |l|&lt;=2. GLIMPSE-II coverage excludes the Galactic center region |l|&lt;=1, |b|&lt;=0.75 observed by the GALCEN GO program (PID=3677). * GLIMPSE-3D adds vertical extensions up to |b|=4.2{deg} near the galactic center, and up to |b|=3{deg} in selected other parts of the Galaxy (+/-10, 18.5, 25, 30, and -15 (345){deg}). GLIMPSE-II had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006). The highly reliable v2.0 GLIMPSEII Catalog (v2.0_GLMIIC) consists of point sources that are detected at least twice in one band and at least once in an adjacent band and a S/N &gt; 5 cut for the band with the two detections. There are also faint and bright flux limits on the Catalog entries. The more complete v2.0 Archive (v2.0_GLMIIA) has less stringent criteria, namely two detections in any bands, those detections having a S/N &gt; 5. The IRAC data were bandmerged with the 2MASS All-Sky Point Source Catalog. See the GLIMPSEII v2.0 Data Products &amp; Data Delivery document for more details. The catalog available from CDS merges the 3 surveys GLIMPSE-I (v2.0), GLIMPSE-II (v2.0), and GLIMPSE-3D; Catalog and Archive records are also merged here. In the regions of overlap between the 3 surveys (e.g. longitude around 10{deg}) preference was given to (1) GLIMPSE-II, as recommended in the GLIMPSE documents of May 2007 (glimpse1_v2.0.pdf) and April 2008 (glimpse2-v2.0.pdf); (2) GLIMPSE-I, and (3) GLIMPSE-3D sources. Sources from different surveys were merged if their position is closer than 0.1arcsec. Documents and a document describing in detail the point source photometry steps, see http://www.astro.wisc.edu/glimpse/docs.html</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/293#1</TD>
            <TD>2011-09-14T20:55:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/II/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/293 [2]</TD>
            <TD>GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)</TD>
            <TD>The Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), is a survey of Galactic Plane central parts made with the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope (SST). It covers approximately 220 square degrees, between galactic longitudes +/-65{deg} and +/-1{deg} in galactic latitude (up to 4.2{deg} in the central parts). The four IRAC bands are centered at approximately 3.6, 4.5, 5.8 and 8.0{mu}m. The GLIMPSE combines the 3 surveys: * GLIMPSE-I covers the longitude ranges |l|=10--65{deg} and the latitude range |b|&lt;=1{deg} (Benjamin et al. 2003PASP..115..953B) * GLIMPSE-II covers the longitude range of |l|&lt;=10{deg}, and a latitude range |b|&lt;=1{deg} from |l|=5--10, |b|&lt;=1.5 for |l|=2--5, and |b|&lt;=2{deg} for |l|&lt;=2. GLIMPSE-II coverage excludes the Galactic center region |l|&lt;=1, |b|&lt;=0.75 observed by the GALCEN GO program (PID=3677). * GLIMPSE-3D adds vertical extensions up to |b|=4.2{deg} near the galactic center, and up to |b|=3{deg} in selected other parts of the Galaxy (+/-10, 18.5, 25, 30, and -15 (345){deg}). GLIMPSE-II had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006). The highly reliable v2.0 GLIMPSEII Catalog (v2.0_GLMIIC) consists of point sources that are detected at least twice in one band and at least once in an adjacent band and a S/N &gt; 5 cut for the band with the two detections. There are also faint and bright flux limits on the Catalog entries. The more complete v2.0 Archive (v2.0_GLMIIA) has less stringent criteria, namely two detections in any bands, those detections having a S/N &gt; 5. The IRAC data were bandmerged with the 2MASS All-Sky Point Source Catalog. See the GLIMPSEII v2.0 Data Products &amp; Data Delivery document for more details. The catalog available from CDS merges the 3 surveys GLIMPSE-I (v2.0), GLIMPSE-II (v2.0), and GLIMPSE-3D; Catalog and Archive records are also merged here. In the regions of overlap between the 3 surveys (e.g. longitude around 10{deg}) preference was given to (1) GLIMPSE-II, as recommended in the GLIMPSE documents of May 2007 (glimpse1_v2.0.pdf) and April 2008 (glimpse2-v2.0.pdf); (2) GLIMPSE-I, and (3) GLIMPSE-3D sources. Sources from different surveys were merged if their position is closer than 0.1arcsec. Documents and a document describing in detail the point source photometry steps, see http://www.astro.wisc.edu/glimpse/docs.html</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/293#2</TD>
            <TD>2011-09-14T20:55:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/II/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/293 [glimpse]</TD>
            <TD>GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)</TD>
            <TD>The Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), is a survey of Galactic Plane central parts made with the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope (SST). It covers approximately 220 square degrees, between galactic longitudes +/-65{deg} and +/-1{deg} in galactic latitude (up to 4.2{deg} in the central parts). The four IRAC bands are centered at approximately 3.6, 4.5, 5.8 and 8.0{mu}m. The GLIMPSE combines the 3 surveys: * GLIMPSE-I covers the longitude ranges |l|=10--65{deg} and the latitude range |b|&lt;=1{deg} (Benjamin et al. 2003PASP..115..953B) * GLIMPSE-II covers the longitude range of |l|&lt;=10{deg}, and a latitude range |b|&lt;=1{deg} from |l|=5--10, |b|&lt;=1.5 for |l|=2--5, and |b|&lt;=2{deg} for |l|&lt;=2. GLIMPSE-II coverage excludes the Galactic center region |l|&lt;=1, |b|&lt;=0.75 observed by the GALCEN GO program (PID=3677). * GLIMPSE-3D adds vertical extensions up to |b|=4.2{deg} near the galactic center, and up to |b|=3{deg} in selected other parts of the Galaxy (+/-10, 18.5, 25, 30, and -15 (345){deg}). GLIMPSE-II had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006). The highly reliable v2.0 GLIMPSEII Catalog (v2.0_GLMIIC) consists of point sources that are detected at least twice in one band and at least once in an adjacent band and a S/N &gt; 5 cut for the band with the two detections. There are also faint and bright flux limits on the Catalog entries. The more complete v2.0 Archive (v2.0_GLMIIA) has less stringent criteria, namely two detections in any bands, those detections having a S/N &gt; 5. The IRAC data were bandmerged with the 2MASS All-Sky Point Source Catalog. See the GLIMPSEII v2.0 Data Products &amp; Data Delivery document for more details. The catalog available from CDS merges the 3 surveys GLIMPSE-I (v2.0), GLIMPSE-II (v2.0), and GLIMPSE-3D; Catalog and Archive records are also merged here. In the regions of overlap between the 3 surveys (e.g. longitude around 10{deg}) preference was given to (1) GLIMPSE-II, as recommended in the GLIMPSE documents of May 2007 (glimpse1_v2.0.pdf) and April 2008 (glimpse2-v2.0.pdf); (2) GLIMPSE-I, and (3) GLIMPSE-3D sources. Sources from different surveys were merged if their position is closer than 0.1arcsec. Documents and a document describing in detail the point source photometry steps, see http://www.astro.wisc.edu/glimpse/docs.html</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/293#glimpse</TD>
            <TD>2011-09-14T20:55:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/II/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/293</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/318/416 [1]</TD>
            <TD>Radial velocities &amp; photometry of classical Cepheids (Pont+ 1997)</TD>
            <TD>Radial velocities and distances have been measured for a sample of 48 remote classical Cepheids located in the outer disc of the Galaxy (118deg&lt;l&lt;274deg). The distances are determined from BVI photometry, with semi-empirical metallicity corrections calibrated on the Magellanic Clouds. Using these Cepheids as tracers, the rotation curve of the disc is determined between R_0_ and 2R_0_. The result is a flat rotation curve about 30km/s lower than theta_0_, V_rot_=193+/-4km/s for R_0_==8.5kpc and theta_0_=220kms/s assumed, or V_rot_=167+/-4km/s for R_0_=8kpc and theta_0_=200km/s. The possible presence of non-axisymmetric components in the rotation of the outer disc is considered. We find a very small or vanishing value for any radial motion of the LSR or expansion/contraction motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/416#1</TD>
            <TD>2011-09-14T18:15:33Z</TD>
            <TD>#Photometry#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/416</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/318/416</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/318/416</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/318/416 [2]</TD>
            <TD>Radial velocities &amp; photometry of classical Cepheids (Pont+ 1997)</TD>
            <TD>Radial velocities and distances have been measured for a sample of 48 remote classical Cepheids located in the outer disc of the Galaxy (118deg&lt;l&lt;274deg). The distances are determined from BVI photometry, with semi-empirical metallicity corrections calibrated on the Magellanic Clouds. Using these Cepheids as tracers, the rotation curve of the disc is determined between R_0_ and 2R_0_. The result is a flat rotation curve about 30km/s lower than theta_0_, V_rot_=193+/-4km/s for R_0_==8.5kpc and theta_0_=220kms/s assumed, or V_rot_=167+/-4km/s for R_0_=8kpc and theta_0_=200km/s. The possible presence of non-axisymmetric components in the rotation of the outer disc is considered. We find a very small or vanishing value for any radial motion of the LSR or expansion/contraction motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/416#2</TD>
            <TD>2011-09-14T18:15:33Z</TD>
            <TD>#Photometry#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/416</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/318/416&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/318/416</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/318/416 [1]</TD>
            <TD>Radial velocities &amp; photometry of classical Cepheids (Pont+ 1997)</TD>
            <TD>Radial velocities and distances have been measured for a sample of 48 remote classical Cepheids located in the outer disc of the Galaxy (118deg&lt;l&lt;274deg). The distances are determined from BVI photometry, with semi-empirical metallicity corrections calibrated on the Magellanic Clouds. Using these Cepheids as tracers, the rotation curve of the disc is determined between R_0_ and 2R_0_. The result is a flat rotation curve about 30km/s lower than theta_0_, V_rot_=193+/-4km/s for R_0_==8.5kpc and theta_0_=220kms/s assumed, or V_rot_=167+/-4km/s for R_0_=8kpc and theta_0_=200km/s. The possible presence of non-axisymmetric components in the rotation of the outer disc is considered. We find a very small or vanishing value for any radial motion of the LSR or expansion/contraction motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/416#1</TD>
            <TD>2011-09-14T18:15:33Z</TD>
            <TD>#Photometry#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/416</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/318/416</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/318/416</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/318/416 [2]</TD>
            <TD>Radial velocities &amp; photometry of classical Cepheids (Pont+ 1997)</TD>
            <TD>Radial velocities and distances have been measured for a sample of 48 remote classical Cepheids located in the outer disc of the Galaxy (118deg&lt;l&lt;274deg). The distances are determined from BVI photometry, with semi-empirical metallicity corrections calibrated on the Magellanic Clouds. Using these Cepheids as tracers, the rotation curve of the disc is determined between R_0_ and 2R_0_. The result is a flat rotation curve about 30km/s lower than theta_0_, V_rot_=193+/-4km/s for R_0_==8.5kpc and theta_0_=220kms/s assumed, or V_rot_=167+/-4km/s for R_0_=8kpc and theta_0_=200km/s. The possible presence of non-axisymmetric components in the rotation of the outer disc is considered. We find a very small or vanishing value for any radial motion of the LSR or expansion/contraction motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/416#2</TD>
            <TD>2011-09-14T18:15:33Z</TD>
            <TD>#Photometry#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/416</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/318/416&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/318/416</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/757 [1]</TD>
            <TD>Quasar and radio galaxies flux densities (Hoeksta+ 1997)</TD>
            <TD>The tables described below contain the data used in the analysis. The data have been taken from various sources in the literature. The references to the data can be found in the paper. Table 1 contains the data of the 3C radio galaxy sample. Table 2 contains the data of the 3C quasar sample. Table 3 contains the data of the 4C quasar sample. The tables list the name of the object, its redshift, the value of the Q-parameter (ratio between the core and extended flux at 5 GHz observed frequency), and the flux densities at various frequencies.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/757#1</TD>
            <TD>2011-09-14T18:15:42Z</TD>
            <TD>#Galaxies#QSOs#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/757</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/757</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/757</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/757 [2]</TD>
            <TD>Quasar and radio galaxies flux densities (Hoeksta+ 1997)</TD>
            <TD>The tables described below contain the data used in the analysis. The data have been taken from various sources in the literature. The references to the data can be found in the paper. Table 1 contains the data of the 3C radio galaxy sample. Table 2 contains the data of the 3C quasar sample. Table 3 contains the data of the 4C quasar sample. The tables list the name of the object, its redshift, the value of the Q-parameter (ratio between the core and extended flux at 5 GHz observed frequency), and the flux densities at various frequencies.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/757#2</TD>
            <TD>2011-09-14T18:15:42Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/757</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/757&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/757</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/757 [1]</TD>
            <TD>Quasar and radio galaxies flux densities (Hoeksta+ 1997)</TD>
            <TD>The tables described below contain the data used in the analysis. The data have been taken from various sources in the literature. The references to the data can be found in the paper. Table 1 contains the data of the 3C radio galaxy sample. Table 2 contains the data of the 3C quasar sample. Table 3 contains the data of the 4C quasar sample. The tables list the name of the object, its redshift, the value of the Q-parameter (ratio between the core and extended flux at 5 GHz observed frequency), and the flux densities at various frequencies.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/757#1</TD>
            <TD>2011-09-14T18:15:42Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/757</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/757</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/757</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/757 [2]</TD>
            <TD>Quasar and radio galaxies flux densities (Hoeksta+ 1997)</TD>
            <TD>The tables described below contain the data used in the analysis. The data have been taken from various sources in the literature. The references to the data can be found in the paper. Table 1 contains the data of the 3C radio galaxy sample. Table 2 contains the data of the 3C quasar sample. Table 3 contains the data of the 4C quasar sample. The tables list the name of the object, its redshift, the value of the Q-parameter (ratio between the core and extended flux at 5 GHz observed frequency), and the flux densities at various frequencies.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/757#2</TD>
            <TD>2011-09-14T18:15:42Z</TD>
            <TD>#Galaxies#QSOs#</TD>
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            <TD>23-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/757</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/757&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/757</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/116/447 [1]</TD>
            <TD>M31 globulars clusters ellipticities (Staneva+, 1996)</TD>
            <TD>The projected ellipticities and orientations of 173 globular clusters in the Andromeda galaxy have been determined by using isodensity contours and 2D Gaussian fitting techniques. A number of B plates taken with the 2m Ritchey-Chretien-coude reflector of the Bulgarian National Astronomical Observatory were digitized and processed for each cluster. The derived ellipticities and orientations are presented in the form of a catalogue. The projected ellipticities of M 31 GCs lie between 0.03/0.24 with mean value {epsilon}=0.086+/-0.038. It may be concluded that the most globular clusters in the Andromeda galaxy are quite spherical. The derived orientations do not show a preference with respect to the center of M 31. Some correlations of the ellipticity with other clusters parameters are discussed. The ellipticities determined in this work are compared with those in other Local Group galaxies</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/447#1</TD>
            <TD>2011-09-14T18:18:53Z</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/116/447</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/447</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/116/447 [2]</TD>
            <TD>M31 globulars clusters ellipticities (Staneva+, 1996)</TD>
            <TD>The projected ellipticities and orientations of 173 globular clusters in the Andromeda galaxy have been determined by using isodensity contours and 2D Gaussian fitting techniques. A number of B plates taken with the 2m Ritchey-Chretien-coude reflector of the Bulgarian National Astronomical Observatory were digitized and processed for each cluster. The derived ellipticities and orientations are presented in the form of a catalogue. The projected ellipticities of M 31 GCs lie between 0.03/0.24 with mean value {epsilon}=0.086+/-0.038. It may be concluded that the most globular clusters in the Andromeda galaxy are quite spherical. The derived orientations do not show a preference with respect to the center of M 31. Some correlations of the ellipticity with other clusters parameters are discussed. The ellipticities determined in this work are compared with those in other Local Group galaxies</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/447#2</TD>
            <TD>2011-09-14T18:18:53Z</TD>
            <TD>#Globular_Clusters#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/116/447&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/447</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/116/447 [1]</TD>
            <TD>M31 globulars clusters ellipticities (Staneva+, 1996)</TD>
            <TD>The projected ellipticities and orientations of 173 globular clusters in the Andromeda galaxy have been determined by using isodensity contours and 2D Gaussian fitting techniques. A number of B plates taken with the 2m Ritchey-Chretien-coude reflector of the Bulgarian National Astronomical Observatory were digitized and processed for each cluster. The derived ellipticities and orientations are presented in the form of a catalogue. The projected ellipticities of M 31 GCs lie between 0.03/0.24 with mean value {epsilon}=0.086+/-0.038. It may be concluded that the most globular clusters in the Andromeda galaxy are quite spherical. The derived orientations do not show a preference with respect to the center of M 31. Some correlations of the ellipticity with other clusters parameters are discussed. The ellipticities determined in this work are compared with those in other Local Group galaxies</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/447#1</TD>
            <TD>2011-09-14T18:18:53Z</TD>
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            <TD>08-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/116/447</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/447</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/116/447 [2]</TD>
            <TD>M31 globulars clusters ellipticities (Staneva+, 1996)</TD>
            <TD>The projected ellipticities and orientations of 173 globular clusters in the Andromeda galaxy have been determined by using isodensity contours and 2D Gaussian fitting techniques. A number of B plates taken with the 2m Ritchey-Chretien-coude reflector of the Bulgarian National Astronomical Observatory were digitized and processed for each cluster. The derived ellipticities and orientations are presented in the form of a catalogue. The projected ellipticities of M 31 GCs lie between 0.03/0.24 with mean value {epsilon}=0.086+/-0.038. It may be concluded that the most globular clusters in the Andromeda galaxy are quite spherical. The derived orientations do not show a preference with respect to the center of M 31. Some correlations of the ellipticity with other clusters parameters are discussed. The ellipticities determined in this work are compared with those in other Local Group galaxies</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/447#2</TD>
            <TD>2011-09-14T18:18:53Z</TD>
            <TD>#Globular_Clusters#</TD>
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            <TD>08-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/116/447&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/447</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/117/369 [1]</TD>
            <TD>Galaxies in the "zone of avoidance". III. (Lercher+, 1996)</TD>
            <TD>As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg&lt;=l&lt;=130deg, -10deg&lt;=b&lt;=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/369#1</TD>
            <TD>2011-09-14T18:19:01Z</TD>
            <TD>#Stars#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>1996-Feb-01</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/117/369</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/369</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/117/369 [2]</TD>
            <TD>Galaxies in the "zone of avoidance". III. (Lercher+, 1996)</TD>
            <TD>As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg&lt;=l&lt;=130deg, -10deg&lt;=b&lt;=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/369#2</TD>
            <TD>2011-09-14T18:19:01Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Feb-01</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/117/369&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/369</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/369 [table2]</TD>
            <TD>Galaxies in the "zone of avoidance". III. (Lercher+, 1996)</TD>
            <TD>As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg&lt;=l&lt;=130deg, -10deg&lt;=b&lt;=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/369#table2</TD>
            <TD>2011-09-14T18:19:01Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Feb-01</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/369</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/369&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/369</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/117/369 [1]</TD>
            <TD>Galaxies in the "zone of avoidance". III. (Lercher+, 1996)</TD>
            <TD>As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg&lt;=l&lt;=130deg, -10deg&lt;=b&lt;=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/369#1</TD>
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            <TD>ivo://CDS.VizieR/J/A+AS/117/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/117/369</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/369</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/117/369 [2]</TD>
            <TD>Galaxies in the "zone of avoidance". III. (Lercher+, 1996)</TD>
            <TD>As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg&lt;=l&lt;=130deg, -10deg&lt;=b&lt;=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/369#2</TD>
            <TD>2011-09-14T18:19:01Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
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            <TD>1996-Feb-01</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/117/369&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/369</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/369 [table2]</TD>
            <TD>Galaxies in the "zone of avoidance". III. (Lercher+, 1996)</TD>
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            <TD>Web Page</TD>
            <TD>J/A+AS/117/369 [1]</TD>
            <TD>Galaxies in the "zone of avoidance". III. (Lercher+, 1996)</TD>
            <TD>As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg&lt;=l&lt;=130deg, -10deg&lt;=b&lt;=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.</TD>
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            <TD>J/A+AS/117/369 [2]</TD>
            <TD>Galaxies in the "zone of avoidance". III. (Lercher+, 1996)</TD>
            <TD>As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg&lt;=l&lt;=130deg, -10deg&lt;=b&lt;=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.</TD>
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            <TD>Galaxies in the "zone of avoidance". III. (Lercher+, 1996)</TD>
            <TD>As the third part in a series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present a compilation of 1161 galaxies discovered during a systematic search on Palomar Observatory Sky Survey (POSS) red-sensitive prints. The region searched comprises 200 square degrees, at 120deg&lt;=l&lt;=130deg, -10deg&lt;=b&lt;=+10deg. In addition to galactic, equatorial and rectangular coordinates, we list maximum and minimum optical diameters derived from both the red- and blue-sensitive prints, could assign a morphological type to some of the objects and made cross-checks with the IRAS PSC and several radio catalogues. A test for completeness suggests, that our catalogue should be complete down to a limiting galaxy-diameter of 0.35'. An asymmetric distribution of the galaxies with respect to the galactic equator was found and is discussed by comparing it with the locations of optically visible dust clouds and/or the distribution of IR-emitting dust material. A comparison between the distribution of the galaxies and the 100{mu} IRAS intensity maps led to the identification of four possible clusterings. As a byproduct of our galaxy search, two new planetary nebulae, nebulous stars at the position of a strong cold IRAS point source, and a nearby dwarf irregular galaxy could be detected.</TD>
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            <TD>J/AJ/104/92 [1]</TD>
            <TD>HII Regions Properties in M101 (Scowen+ 1992)</TD>
            <TD>Spectrophotometrically calibrated CCD imagery of two overlapping 16 arc min fields in the SAB(rs)cdI galaxy M101 in the emission of H alpha, [O III] lambda 5007, H beta, and [S II] lambda 6723 are used to study various physical properties of the H II region population. Individual H II regions are identified and mapped using an automated algorithm, thus eliminating personal bias in the measurements. Characteristics of the population studied include the H II region luminosity function and radial variations in extinction, [O III]/H beta, O/H, [S II]/H alpha, ionization parameter, and numbers of ionizing photons. In addition, radial and azimuthal variations in the H II surface density are studied in comparison to that of H I and H_2 inferred from radio 21 cm and CO observations. It is demonstrated that the magnitude of trends and ``gradients'' found from such analyses depend on the surface brightness threshold set in defining the H II region boundaries; so results are presented for both low (log S(H alpha) = -15.7 ergs/s/cm^2/arcsec^2; 625 H II regions) and high (-15.0; 248 H II regions) thresholds. Radial gradients in both extinction, C(H beta), and O/H are seen in the H II region population -- with a distinct flattening in the O/H gradient seen in the outer disk beginning at about 10 kpc. The luminosity function of the H II region population found is similar to previous studies, though both the high and low ends are sensitive to the threshold levels set. Other parameters, such as the ionization parameters, luminosities, and size distribution, show no evidence for systematic variations with galactocentric distance. Current star formation processes active in the disk of M101 are analyzed two-dimensionally by comparison of the distribution of ionized and neutral hydrogen. The star formation efficiency shows considerable variation across the disk, suggesting significant spatial variation in the critical density for cloud collapse across the disk of M101 and thus departures from the simple Toomre model.</TD>
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            <TD>HII Regions Properties in M101 (Scowen+ 1992)</TD>
            <TD>Spectrophotometrically calibrated CCD imagery of two overlapping 16 arc min fields in the SAB(rs)cdI galaxy M101 in the emission of H alpha, [O III] lambda 5007, H beta, and [S II] lambda 6723 are used to study various physical properties of the H II region population. Individual H II regions are identified and mapped using an automated algorithm, thus eliminating personal bias in the measurements. Characteristics of the population studied include the H II region luminosity function and radial variations in extinction, [O III]/H beta, O/H, [S II]/H alpha, ionization parameter, and numbers of ionizing photons. In addition, radial and azimuthal variations in the H II surface density are studied in comparison to that of H I and H_2 inferred from radio 21 cm and CO observations. It is demonstrated that the magnitude of trends and ``gradients'' found from such analyses depend on the surface brightness threshold set in defining the H II region boundaries; so results are presented for both low (log S(H alpha) = -15.7 ergs/s/cm^2/arcsec^2; 625 H II regions) and high (-15.0; 248 H II regions) thresholds. Radial gradients in both extinction, C(H beta), and O/H are seen in the H II region population -- with a distinct flattening in the O/H gradient seen in the outer disk beginning at about 10 kpc. The luminosity function of the H II region population found is similar to previous studies, though both the high and low ends are sensitive to the threshold levels set. Other parameters, such as the ionization parameters, luminosities, and size distribution, show no evidence for systematic variations with galactocentric distance. Current star formation processes active in the disk of M101 are analyzed two-dimensionally by comparison of the distribution of ionized and neutral hydrogen. The star formation efficiency shows considerable variation across the disk, suggesting significant spatial variation in the critical density for cloud collapse across the disk of M101 and thus departures from the simple Toomre model.</TD>
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            <TD>HII Regions Properties in M101 (Scowen+ 1992)</TD>
            <TD>Spectrophotometrically calibrated CCD imagery of two overlapping 16 arc min fields in the SAB(rs)cdI galaxy M101 in the emission of H alpha, [O III] lambda 5007, H beta, and [S II] lambda 6723 are used to study various physical properties of the H II region population. Individual H II regions are identified and mapped using an automated algorithm, thus eliminating personal bias in the measurements. Characteristics of the population studied include the H II region luminosity function and radial variations in extinction, [O III]/H beta, O/H, [S II]/H alpha, ionization parameter, and numbers of ionizing photons. In addition, radial and azimuthal variations in the H II surface density are studied in comparison to that of H I and H_2 inferred from radio 21 cm and CO observations. It is demonstrated that the magnitude of trends and ``gradients'' found from such analyses depend on the surface brightness threshold set in defining the H II region boundaries; so results are presented for both low (log S(H alpha) = -15.7 ergs/s/cm^2/arcsec^2; 625 H II regions) and high (-15.0; 248 H II regions) thresholds. Radial gradients in both extinction, C(H beta), and O/H are seen in the H II region population -- with a distinct flattening in the O/H gradient seen in the outer disk beginning at about 10 kpc. The luminosity function of the H II region population found is similar to previous studies, though both the high and low ends are sensitive to the threshold levels set. Other parameters, such as the ionization parameters, luminosities, and size distribution, show no evidence for systematic variations with galactocentric distance. Current star formation processes active in the disk of M101 are analyzed two-dimensionally by comparison of the distribution of ionized and neutral hydrogen. The star formation efficiency shows considerable variation across the disk, suggesting significant spatial variation in the critical density for cloud collapse across the disk of M101 and thus departures from the simple Toomre model.</TD>
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            <TD>HII Regions Properties in M101 (Scowen+ 1992)</TD>
            <TD>Spectrophotometrically calibrated CCD imagery of two overlapping 16 arc min fields in the SAB(rs)cdI galaxy M101 in the emission of H alpha, [O III] lambda 5007, H beta, and [S II] lambda 6723 are used to study various physical properties of the H II region population. Individual H II regions are identified and mapped using an automated algorithm, thus eliminating personal bias in the measurements. Characteristics of the population studied include the H II region luminosity function and radial variations in extinction, [O III]/H beta, O/H, [S II]/H alpha, ionization parameter, and numbers of ionizing photons. In addition, radial and azimuthal variations in the H II surface density are studied in comparison to that of H I and H_2 inferred from radio 21 cm and CO observations. It is demonstrated that the magnitude of trends and ``gradients'' found from such analyses depend on the surface brightness threshold set in defining the H II region boundaries; so results are presented for both low (log S(H alpha) = -15.7 ergs/s/cm^2/arcsec^2; 625 H II regions) and high (-15.0; 248 H II regions) thresholds. Radial gradients in both extinction, C(H beta), and O/H are seen in the H II region population -- with a distinct flattening in the O/H gradient seen in the outer disk beginning at about 10 kpc. The luminosity function of the H II region population found is similar to previous studies, though both the high and low ends are sensitive to the threshold levels set. Other parameters, such as the ionization parameters, luminosities, and size distribution, show no evidence for systematic variations with galactocentric distance. Current star formation processes active in the disk of M101 are analyzed two-dimensionally by comparison of the distribution of ionized and neutral hydrogen. The star formation efficiency shows considerable variation across the disk, suggesting significant spatial variation in the critical density for cloud collapse across the disk of M101 and thus departures from the simple Toomre model.</TD>
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            <TD>J/AJ/104/92 [1]</TD>
            <TD>HII Regions Properties in M101 (Scowen+ 1992)</TD>
            <TD>Spectrophotometrically calibrated CCD imagery of two overlapping 16 arc min fields in the SAB(rs)cdI galaxy M101 in the emission of H alpha, [O III] lambda 5007, H beta, and [S II] lambda 6723 are used to study various physical properties of the H II region population. Individual H II regions are identified and mapped using an automated algorithm, thus eliminating personal bias in the measurements. Characteristics of the population studied include the H II region luminosity function and radial variations in extinction, [O III]/H beta, O/H, [S II]/H alpha, ionization parameter, and numbers of ionizing photons. In addition, radial and azimuthal variations in the H II surface density are studied in comparison to that of H I and H_2 inferred from radio 21 cm and CO observations. It is demonstrated that the magnitude of trends and ``gradients'' found from such analyses depend on the surface brightness threshold set in defining the H II region boundaries; so results are presented for both low (log S(H alpha) = -15.7 ergs/s/cm^2/arcsec^2; 625 H II regions) and high (-15.0; 248 H II regions) thresholds. Radial gradients in both extinction, C(H beta), and O/H are seen in the H II region population -- with a distinct flattening in the O/H gradient seen in the outer disk beginning at about 10 kpc. The luminosity function of the H II region population found is similar to previous studies, though both the high and low ends are sensitive to the threshold levels set. Other parameters, such as the ionization parameters, luminosities, and size distribution, show no evidence for systematic variations with galactocentric distance. Current star formation processes active in the disk of M101 are analyzed two-dimensionally by comparison of the distribution of ionized and neutral hydrogen. The star formation efficiency shows considerable variation across the disk, suggesting significant spatial variation in the critical density for cloud collapse across the disk of M101 and thus departures from the simple Toomre model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/92#1</TD>
            <TD>2011-09-14T18:21:05Z</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/104/92</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/92</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/104/92 [2]</TD>
            <TD>HII Regions Properties in M101 (Scowen+ 1992)</TD>
            <TD>Spectrophotometrically calibrated CCD imagery of two overlapping 16 arc min fields in the SAB(rs)cdI galaxy M101 in the emission of H alpha, [O III] lambda 5007, H beta, and [S II] lambda 6723 are used to study various physical properties of the H II region population. Individual H II regions are identified and mapped using an automated algorithm, thus eliminating personal bias in the measurements. Characteristics of the population studied include the H II region luminosity function and radial variations in extinction, [O III]/H beta, O/H, [S II]/H alpha, ionization parameter, and numbers of ionizing photons. In addition, radial and azimuthal variations in the H II surface density are studied in comparison to that of H I and H_2 inferred from radio 21 cm and CO observations. It is demonstrated that the magnitude of trends and ``gradients'' found from such analyses depend on the surface brightness threshold set in defining the H II region boundaries; so results are presented for both low (log S(H alpha) = -15.7 ergs/s/cm^2/arcsec^2; 625 H II regions) and high (-15.0; 248 H II regions) thresholds. Radial gradients in both extinction, C(H beta), and O/H are seen in the H II region population -- with a distinct flattening in the O/H gradient seen in the outer disk beginning at about 10 kpc. The luminosity function of the H II region population found is similar to previous studies, though both the high and low ends are sensitive to the threshold levels set. Other parameters, such as the ionization parameters, luminosities, and size distribution, show no evidence for systematic variations with galactocentric distance. Current star formation processes active in the disk of M101 are analyzed two-dimensionally by comparison of the distribution of ionized and neutral hydrogen. The star formation efficiency shows considerable variation across the disk, suggesting significant spatial variation in the critical density for cloud collapse across the disk of M101 and thus departures from the simple Toomre model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/92#2</TD>
            <TD>2011-09-14T18:21:05Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1995-Jan-17</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/92</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/104/92&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/92</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/104/92 [table0]</TD>
            <TD>HII Regions Properties in M101 (Scowen+ 1992)</TD>
            <TD>Spectrophotometrically calibrated CCD imagery of two overlapping 16 arc min fields in the SAB(rs)cdI galaxy M101 in the emission of H alpha, [O III] lambda 5007, H beta, and [S II] lambda 6723 are used to study various physical properties of the H II region population. Individual H II regions are identified and mapped using an automated algorithm, thus eliminating personal bias in the measurements. Characteristics of the population studied include the H II region luminosity function and radial variations in extinction, [O III]/H beta, O/H, [S II]/H alpha, ionization parameter, and numbers of ionizing photons. In addition, radial and azimuthal variations in the H II surface density are studied in comparison to that of H I and H_2 inferred from radio 21 cm and CO observations. It is demonstrated that the magnitude of trends and ``gradients'' found from such analyses depend on the surface brightness threshold set in defining the H II region boundaries; so results are presented for both low (log S(H alpha) = -15.7 ergs/s/cm^2/arcsec^2; 625 H II regions) and high (-15.0; 248 H II regions) thresholds. Radial gradients in both extinction, C(H beta), and O/H are seen in the H II region population -- with a distinct flattening in the O/H gradient seen in the outer disk beginning at about 10 kpc. The luminosity function of the H II region population found is similar to previous studies, though both the high and low ends are sensitive to the threshold levels set. Other parameters, such as the ionization parameters, luminosities, and size distribution, show no evidence for systematic variations with galactocentric distance. Current star formation processes active in the disk of M101 are analyzed two-dimensionally by comparison of the distribution of ionized and neutral hydrogen. The star formation efficiency shows considerable variation across the disk, suggesting significant spatial variation in the critical density for cloud collapse across the disk of M101 and thus departures from the simple Toomre model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/92#table0</TD>
            <TD>2011-09-14T18:21:05Z</TD>
            <TD>#Abundances#Galaxies#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1995-Jan-17</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/92</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/104/92&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/92</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>II/293 [1]</TD>
            <TD>GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)</TD>
            <TD>The Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), is a survey of Galactic Plane central parts made with the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope (SST). It covers approximately 220 square degrees, between galactic longitudes +/-65{deg} and +/-1{deg} in galactic latitude (up to 4.2{deg} in the central parts). The four IRAC bands are centered at approximately 3.6, 4.5, 5.8 and 8.0{mu}m. The GLIMPSE combines the 3 surveys: * GLIMPSE-I covers the longitude ranges |l|=10--65{deg} and the latitude range |b|&lt;=1{deg} (Benjamin et al. 2003PASP..115..953B) * GLIMPSE-II covers the longitude range of |l|&lt;=10{deg}, and a latitude range |b|&lt;=1{deg} from |l|=5--10, |b|&lt;=1.5 for |l|=2--5, and |b|&lt;=2{deg} for |l|&lt;=2. GLIMPSE-II coverage excludes the Galactic center region |l|&lt;=1, |b|&lt;=0.75 observed by the GALCEN GO program (PID=3677). * GLIMPSE-3D adds vertical extensions up to |b|=4.2{deg} near the galactic center, and up to |b|=3{deg} in selected other parts of the Galaxy (+/-10, 18.5, 25, 30, and -15 (345){deg}). GLIMPSE-II had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006). The highly reliable v2.0 GLIMPSEII Catalog (v2.0_GLMIIC) consists of point sources that are detected at least twice in one band and at least once in an adjacent band and a S/N &gt; 5 cut for the band with the two detections. There are also faint and bright flux limits on the Catalog entries. The more complete v2.0 Archive (v2.0_GLMIIA) has less stringent criteria, namely two detections in any bands, those detections having a S/N &gt; 5. The IRAC data were bandmerged with the 2MASS All-Sky Point Source Catalog. See the GLIMPSEII v2.0 Data Products &amp; Data Delivery document for more details. The catalog available from CDS merges the 3 surveys GLIMPSE-I (v2.0), GLIMPSE-II (v2.0), and GLIMPSE-3D; Catalog and Archive records are also merged here. In the regions of overlap between the 3 surveys (e.g. longitude around 10{deg}) preference was given to (1) GLIMPSE-II, as recommended in the GLIMPSE documents of May 2007 (glimpse1_v2.0.pdf) and April 2008 (glimpse2-v2.0.pdf); (2) GLIMPSE-I, and (3) GLIMPSE-3D sources. Sources from different surveys were merged if their position is closer than 0.1arcsec. Documents and a document describing in detail the point source photometry steps, see http://www.astro.wisc.edu/glimpse/docs.html</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/293#1</TD>
            <TD>2011-09-14T20:55:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>ivo://CDS.VizieR/II/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/293 [2]</TD>
            <TD>GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)</TD>
            <TD>The Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), is a survey of Galactic Plane central parts made with the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope (SST). It covers approximately 220 square degrees, between galactic longitudes +/-65{deg} and +/-1{deg} in galactic latitude (up to 4.2{deg} in the central parts). The four IRAC bands are centered at approximately 3.6, 4.5, 5.8 and 8.0{mu}m. The GLIMPSE combines the 3 surveys: * GLIMPSE-I covers the longitude ranges |l|=10--65{deg} and the latitude range |b|&lt;=1{deg} (Benjamin et al. 2003PASP..115..953B) * GLIMPSE-II covers the longitude range of |l|&lt;=10{deg}, and a latitude range |b|&lt;=1{deg} from |l|=5--10, |b|&lt;=1.5 for |l|=2--5, and |b|&lt;=2{deg} for |l|&lt;=2. GLIMPSE-II coverage excludes the Galactic center region |l|&lt;=1, |b|&lt;=0.75 observed by the GALCEN GO program (PID=3677). * GLIMPSE-3D adds vertical extensions up to |b|=4.2{deg} near the galactic center, and up to |b|=3{deg} in selected other parts of the Galaxy (+/-10, 18.5, 25, 30, and -15 (345){deg}). GLIMPSE-II had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006). The highly reliable v2.0 GLIMPSEII Catalog (v2.0_GLMIIC) consists of point sources that are detected at least twice in one band and at least once in an adjacent band and a S/N &gt; 5 cut for the band with the two detections. There are also faint and bright flux limits on the Catalog entries. The more complete v2.0 Archive (v2.0_GLMIIA) has less stringent criteria, namely two detections in any bands, those detections having a S/N &gt; 5. The IRAC data were bandmerged with the 2MASS All-Sky Point Source Catalog. See the GLIMPSEII v2.0 Data Products &amp; Data Delivery document for more details. The catalog available from CDS merges the 3 surveys GLIMPSE-I (v2.0), GLIMPSE-II (v2.0), and GLIMPSE-3D; Catalog and Archive records are also merged here. In the regions of overlap between the 3 surveys (e.g. longitude around 10{deg}) preference was given to (1) GLIMPSE-II, as recommended in the GLIMPSE documents of May 2007 (glimpse1_v2.0.pdf) and April 2008 (glimpse2-v2.0.pdf); (2) GLIMPSE-I, and (3) GLIMPSE-3D sources. Sources from different surveys were merged if their position is closer than 0.1arcsec. Documents and a document describing in detail the point source photometry steps, see http://www.astro.wisc.edu/glimpse/docs.html</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/293#2</TD>
            <TD>2011-09-14T20:55:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/II/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/293 [glimpse]</TD>
            <TD>GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)</TD>
            <TD>The Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE), is a survey of Galactic Plane central parts made with the Infrared Array Camera (IRAC) aboard the Spitzer Space Telescope (SST). It covers approximately 220 square degrees, between galactic longitudes +/-65{deg} and +/-1{deg} in galactic latitude (up to 4.2{deg} in the central parts). The four IRAC bands are centered at approximately 3.6, 4.5, 5.8 and 8.0{mu}m. The GLIMPSE combines the 3 surveys: * GLIMPSE-I covers the longitude ranges |l|=10--65{deg} and the latitude range |b|&lt;=1{deg} (Benjamin et al. 2003PASP..115..953B) * GLIMPSE-II covers the longitude range of |l|&lt;=10{deg}, and a latitude range |b|&lt;=1{deg} from |l|=5--10, |b|&lt;=1.5 for |l|=2--5, and |b|&lt;=2{deg} for |l|&lt;=2. GLIMPSE-II coverage excludes the Galactic center region |l|&lt;=1, |b|&lt;=0.75 observed by the GALCEN GO program (PID=3677). * GLIMPSE-3D adds vertical extensions up to |b|=4.2{deg} near the galactic center, and up to |b|=3{deg} in selected other parts of the Galaxy (+/-10, 18.5, 25, 30, and -15 (345){deg}). GLIMPSE-II had two-epoch coverage for a total of three visits on the sky. The observations consisted of two 1.2 second integrations at each position in the first epoch of data taking (September 2005) and a single 1.2 second integration at each position six months later (April 2006). The highly reliable v2.0 GLIMPSEII Catalog (v2.0_GLMIIC) consists of point sources that are detected at least twice in one band and at least once in an adjacent band and a S/N &gt; 5 cut for the band with the two detections. There are also faint and bright flux limits on the Catalog entries. The more complete v2.0 Archive (v2.0_GLMIIA) has less stringent criteria, namely two detections in any bands, those detections having a S/N &gt; 5. The IRAC data were bandmerged with the 2MASS All-Sky Point Source Catalog. See the GLIMPSEII v2.0 Data Products &amp; Data Delivery document for more details. The catalog available from CDS merges the 3 surveys GLIMPSE-I (v2.0), GLIMPSE-II (v2.0), and GLIMPSE-3D; Catalog and Archive records are also merged here. In the regions of overlap between the 3 surveys (e.g. longitude around 10{deg}) preference was given to (1) GLIMPSE-II, as recommended in the GLIMPSE documents of May 2007 (glimpse1_v2.0.pdf) and April 2008 (glimpse2-v2.0.pdf); (2) GLIMPSE-I, and (3) GLIMPSE-3D sources. Sources from different surveys were merged if their position is closer than 0.1arcsec. Documents and a document describing in detail the point source photometry steps, see http://www.astro.wisc.edu/glimpse/docs.html</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/293#glimpse</TD>
            <TD>2011-09-14T20:55:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/II/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/293</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/190/147 [1]</TD>
            <TD>Mid-IR galaxy morphology from S^4^G (Buta+, 2010)</TD>
            <TD>The goals of the S^4^G project are described by Sheth et al. (2010, PASP, submitted).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147#1</TD>
            <TD>2011-09-14T21:03:30Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/190/147</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/190/147</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/190/147 [2]</TD>
            <TD>Mid-IR galaxy morphology from S^4^G (Buta+, 2010)</TD>
            <TD>The goals of the S^4^G project are described by Sheth et al. (2010, PASP, submitted).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147#2</TD>
            <TD>2011-09-14T21:03:30Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/190/147&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/190/147</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/190/147 [table1]</TD>
            <TD>Mid-IR galaxy morphology from S^4^G (Buta+, 2010)</TD>
            <TD>The goals of the S^4^G project are described by Sheth et al. (2010, PASP, submitted).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147#table1</TD>
            <TD>2011-09-14T21:03:30Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/190/147&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/190/147</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/853 [1]</TD>
            <TD>Energy distributions of radio galaxies (Impey+ 1993)</TD>
            <TD>Far-infrared observations of 140 radio galaxies from the 3CR and B2 catalogs are presented. The galaxies span a range of over four order of magnitude in the radio power, from weak nuclear sources in nearby galaxies, to powerful FR II doubled-lobed sources at moderate redshift. Scanned or pointed observations with IRAS detect 38 of the radio galaxies in at least one waveband; 21 are detected at both 60 and 100 {mu}m. The strength of the far-infrared emission is more closely correlated with core radio emission than with total radio emission, and it is independent of the absolute visual magnitude of the host galaxy. The more luminous 3CR galaxies have warmer far infrared emission than the less luminous B2 galaxies. The relationship between radio and far-infrared luminosity is determined in a way that is insensitive to the large number of infrared nondetections. Radio galaxies have far-infrared emission with similar color temperatures to normal ellipticals; however the inferred amounts of cold interstellar material are typical of gas-rich galaxies. Infrared luminous radio galaxies are rare. Only one in 10^5^ ellipticals with M_V_&lt;-17 has a strong enough radio core to have 10^11^ L_Sun_ of far-infrared emission. Indirect arguments indicates that far-infrared emission in radio galaxies represents star formation that is more closely tied to the active nucleus than to the global properties of the galaxy. The far-infrared luminosity function shows good continuity between radio galaxies and radio loud quasars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/853#1</TD>
            <TD>2011-09-14T18:21:14Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/853</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/853</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/853</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/853 [2]</TD>
            <TD>Energy distributions of radio galaxies (Impey+ 1993)</TD>
            <TD>Far-infrared observations of 140 radio galaxies from the 3CR and B2 catalogs are presented. The galaxies span a range of over four order of magnitude in the radio power, from weak nuclear sources in nearby galaxies, to powerful FR II doubled-lobed sources at moderate redshift. Scanned or pointed observations with IRAS detect 38 of the radio galaxies in at least one waveband; 21 are detected at both 60 and 100 {mu}m. The strength of the far-infrared emission is more closely correlated with core radio emission than with total radio emission, and it is independent of the absolute visual magnitude of the host galaxy. The more luminous 3CR galaxies have warmer far infrared emission than the less luminous B2 galaxies. The relationship between radio and far-infrared luminosity is determined in a way that is insensitive to the large number of infrared nondetections. Radio galaxies have far-infrared emission with similar color temperatures to normal ellipticals; however the inferred amounts of cold interstellar material are typical of gas-rich galaxies. Infrared luminous radio galaxies are rare. Only one in 10^5^ ellipticals with M_V_&lt;-17 has a strong enough radio core to have 10^11^ L_Sun_ of far-infrared emission. Indirect arguments indicates that far-infrared emission in radio galaxies represents star formation that is more closely tied to the active nucleus than to the global properties of the galaxy. The far-infrared luminosity function shows good continuity between radio galaxies and radio loud quasars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/853#2</TD>
            <TD>2011-09-14T18:21:14Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/853</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/853&amp;</TD>
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            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/853</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/853 [1]</TD>
            <TD>Energy distributions of radio galaxies (Impey+ 1993)</TD>
            <TD>Far-infrared observations of 140 radio galaxies from the 3CR and B2 catalogs are presented. The galaxies span a range of over four order of magnitude in the radio power, from weak nuclear sources in nearby galaxies, to powerful FR II doubled-lobed sources at moderate redshift. Scanned or pointed observations with IRAS detect 38 of the radio galaxies in at least one waveband; 21 are detected at both 60 and 100 {mu}m. The strength of the far-infrared emission is more closely correlated with core radio emission than with total radio emission, and it is independent of the absolute visual magnitude of the host galaxy. The more luminous 3CR galaxies have warmer far infrared emission than the less luminous B2 galaxies. The relationship between radio and far-infrared luminosity is determined in a way that is insensitive to the large number of infrared nondetections. Radio galaxies have far-infrared emission with similar color temperatures to normal ellipticals; however the inferred amounts of cold interstellar material are typical of gas-rich galaxies. Infrared luminous radio galaxies are rare. Only one in 10^5^ ellipticals with M_V_&lt;-17 has a strong enough radio core to have 10^11^ L_Sun_ of far-infrared emission. Indirect arguments indicates that far-infrared emission in radio galaxies represents star formation that is more closely tied to the active nucleus than to the global properties of the galaxy. The far-infrared luminosity function shows good continuity between radio galaxies and radio loud quasars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/853#1</TD>
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            <TD />
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/853</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/853</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/853 [2]</TD>
            <TD>Energy distributions of radio galaxies (Impey+ 1993)</TD>
            <TD>Far-infrared observations of 140 radio galaxies from the 3CR and B2 catalogs are presented. The galaxies span a range of over four order of magnitude in the radio power, from weak nuclear sources in nearby galaxies, to powerful FR II doubled-lobed sources at moderate redshift. Scanned or pointed observations with IRAS detect 38 of the radio galaxies in at least one waveband; 21 are detected at both 60 and 100 {mu}m. The strength of the far-infrared emission is more closely correlated with core radio emission than with total radio emission, and it is independent of the absolute visual magnitude of the host galaxy. The more luminous 3CR galaxies have warmer far infrared emission than the less luminous B2 galaxies. The relationship between radio and far-infrared luminosity is determined in a way that is insensitive to the large number of infrared nondetections. Radio galaxies have far-infrared emission with similar color temperatures to normal ellipticals; however the inferred amounts of cold interstellar material are typical of gas-rich galaxies. Infrared luminous radio galaxies are rare. Only one in 10^5^ ellipticals with M_V_&lt;-17 has a strong enough radio core to have 10^11^ L_Sun_ of far-infrared emission. Indirect arguments indicates that far-infrared emission in radio galaxies represents star formation that is more closely tied to the active nucleus than to the global properties of the galaxy. The far-infrared luminosity function shows good continuity between radio galaxies and radio loud quasars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/853#2</TD>
            <TD>2011-09-14T18:21:14Z</TD>
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            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/853&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/853</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/190/147 [1]</TD>
            <TD>Mid-IR galaxy morphology from S^4^G (Buta+, 2010)</TD>
            <TD>The goals of the S^4^G project are described by Sheth et al. (2010, PASP, submitted).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147#1</TD>
            <TD>2011-09-14T21:03:30Z</TD>
            <TD>#Galaxies#</TD>
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            <TD />
            <TD>30-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/190/147</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/190/147</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/190/147 [2]</TD>
            <TD>Mid-IR galaxy morphology from S^4^G (Buta+, 2010)</TD>
            <TD>The goals of the S^4^G project are described by Sheth et al. (2010, PASP, submitted).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147#2</TD>
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            <TD>30-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147</TD>
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/190/147&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/190/147</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/190/147 [table1]</TD>
            <TD>Mid-IR galaxy morphology from S^4^G (Buta+, 2010)</TD>
            <TD>The goals of the S^4^G project are described by Sheth et al. (2010, PASP, submitted).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
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            <TD>#Galaxies#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/190/147&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/190/147</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/493 [1]</TD>
            <TD>Globular clusters in M87 (Lee+, 1993)</TD>
            <TD>We present deep integrated Washington CCD photometry of the extremely populous globular cluster system of NGC 4486 (M87) in Virgo. The metallicities of 407 of the best candidates with T1 &lt; 22 have been estimated from the (C-T1) color. These values are internally precise to ~0.15dex and accurate to ~0.25dex. The mean metallicity of the globular clusters is [Fe/H] = -0.86dex, with a formal standard error of the mean of 0.03dex but a more realistic uncertainty of about 0.2dex. This value is higher than that of the corresponding means of the globular clusters in the Galaxy and M31, but similar to those of the globular clusters in NGC 1399 and NGC 5128, as expected from the relative parent galaxy luminosities. Approximately 10% of the clusters exceed solar abundance, similar to the case for the globular clusters in NGC 1399 and NGC 5128. As found by Couture et al. [ApJS, 73, 671 (1990)], there is a large metallicity dispersion at any radius, with a sigma ~ 0.65dex. However, in contrast to their result and that of previous small-field CCD studies, the globular clusters display a marked gradient in both mean (M-T1) and (C-T1) color with galactocentric distance. The mean metallicity decreases by some 0.6dex over the radial extent of the cluster sample. This result is consistent with the early photographic study by Strom et al. [ApJ, 245, 416 (1981)]. The metallicity distribution function is remarkably similar to that of NGC 1399 found by Ostrov et al. [AJ, 105, 1762 (1993)] using the same technique. The two central cluster ellipticals show significant peaks at very similar metallicities, indicating similar formation and enrichment histories. We also find that this structure in the metallicity distribution function persists to radii where the halo light is dominated by the cD envelope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/493#1</TD>
            <TD>2011-09-14T18:21:27Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/493</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/493</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/493 [2]</TD>
            <TD>Globular clusters in M87 (Lee+, 1993)</TD>
            <TD>We present deep integrated Washington CCD photometry of the extremely populous globular cluster system of NGC 4486 (M87) in Virgo. The metallicities of 407 of the best candidates with T1 &lt; 22 have been estimated from the (C-T1) color. These values are internally precise to ~0.15dex and accurate to ~0.25dex. The mean metallicity of the globular clusters is [Fe/H] = -0.86dex, with a formal standard error of the mean of 0.03dex but a more realistic uncertainty of about 0.2dex. This value is higher than that of the corresponding means of the globular clusters in the Galaxy and M31, but similar to those of the globular clusters in NGC 1399 and NGC 5128, as expected from the relative parent galaxy luminosities. Approximately 10% of the clusters exceed solar abundance, similar to the case for the globular clusters in NGC 1399 and NGC 5128. As found by Couture et al. [ApJS, 73, 671 (1990)], there is a large metallicity dispersion at any radius, with a sigma ~ 0.65dex. However, in contrast to their result and that of previous small-field CCD studies, the globular clusters display a marked gradient in both mean (M-T1) and (C-T1) color with galactocentric distance. The mean metallicity decreases by some 0.6dex over the radial extent of the cluster sample. This result is consistent with the early photographic study by Strom et al. [ApJ, 245, 416 (1981)]. The metallicity distribution function is remarkably similar to that of NGC 1399 found by Ostrov et al. [AJ, 105, 1762 (1993)] using the same technique. The two central cluster ellipticals show significant peaks at very similar metallicities, indicating similar formation and enrichment histories. We also find that this structure in the metallicity distribution function persists to radii where the halo light is dominated by the cD envelope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/493#2</TD>
            <TD>2011-09-14T18:21:27Z</TD>
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            <TD>20-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/493&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/493</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/493 [1]</TD>
            <TD>Globular clusters in M87 (Lee+, 1993)</TD>
            <TD>We present deep integrated Washington CCD photometry of the extremely populous globular cluster system of NGC 4486 (M87) in Virgo. The metallicities of 407 of the best candidates with T1 &lt; 22 have been estimated from the (C-T1) color. These values are internally precise to ~0.15dex and accurate to ~0.25dex. The mean metallicity of the globular clusters is [Fe/H] = -0.86dex, with a formal standard error of the mean of 0.03dex but a more realistic uncertainty of about 0.2dex. This value is higher than that of the corresponding means of the globular clusters in the Galaxy and M31, but similar to those of the globular clusters in NGC 1399 and NGC 5128, as expected from the relative parent galaxy luminosities. Approximately 10% of the clusters exceed solar abundance, similar to the case for the globular clusters in NGC 1399 and NGC 5128. As found by Couture et al. [ApJS, 73, 671 (1990)], there is a large metallicity dispersion at any radius, with a sigma ~ 0.65dex. However, in contrast to their result and that of previous small-field CCD studies, the globular clusters display a marked gradient in both mean (M-T1) and (C-T1) color with galactocentric distance. The mean metallicity decreases by some 0.6dex over the radial extent of the cluster sample. This result is consistent with the early photographic study by Strom et al. [ApJ, 245, 416 (1981)]. The metallicity distribution function is remarkably similar to that of NGC 1399 found by Ostrov et al. [AJ, 105, 1762 (1993)] using the same technique. The two central cluster ellipticals show significant peaks at very similar metallicities, indicating similar formation and enrichment histories. We also find that this structure in the metallicity distribution function persists to radii where the halo light is dominated by the cD envelope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/493#1</TD>
            <TD>2011-09-14T18:21:27Z</TD>
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            <TD>20-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/493</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/493</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/493 [2]</TD>
            <TD>Globular clusters in M87 (Lee+, 1993)</TD>
            <TD>We present deep integrated Washington CCD photometry of the extremely populous globular cluster system of NGC 4486 (M87) in Virgo. The metallicities of 407 of the best candidates with T1 &lt; 22 have been estimated from the (C-T1) color. These values are internally precise to ~0.15dex and accurate to ~0.25dex. The mean metallicity of the globular clusters is [Fe/H] = -0.86dex, with a formal standard error of the mean of 0.03dex but a more realistic uncertainty of about 0.2dex. This value is higher than that of the corresponding means of the globular clusters in the Galaxy and M31, but similar to those of the globular clusters in NGC 1399 and NGC 5128, as expected from the relative parent galaxy luminosities. Approximately 10% of the clusters exceed solar abundance, similar to the case for the globular clusters in NGC 1399 and NGC 5128. As found by Couture et al. [ApJS, 73, 671 (1990)], there is a large metallicity dispersion at any radius, with a sigma ~ 0.65dex. However, in contrast to their result and that of previous small-field CCD studies, the globular clusters display a marked gradient in both mean (M-T1) and (C-T1) color with galactocentric distance. The mean metallicity decreases by some 0.6dex over the radial extent of the cluster sample. This result is consistent with the early photographic study by Strom et al. [ApJ, 245, 416 (1981)]. The metallicity distribution function is remarkably similar to that of NGC 1399 found by Ostrov et al. [AJ, 105, 1762 (1993)] using the same technique. The two central cluster ellipticals show significant peaks at very similar metallicities, indicating similar formation and enrichment histories. We also find that this structure in the metallicity distribution function persists to radii where the halo light is dominated by the cD envelope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/493#2</TD>
            <TD>2011-09-14T18:21:27Z</TD>
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            <TD>20-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/493&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/493</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/986 [1]</TD>
            <TD>CMD for And III (Armandroff+, 1993)</TD>
            <TD>The prime focus CCD camera of the KPNO 4 m telescope has been used to image Andromeda III, a dwarf spheroidal galaxy companion to M31, in the V and I bands. The resulting color-magnitude diagram shows a well defined giant branch whose tip luminosity corresponds to that expected for an old metal-poor population at the distance of M31. By comparing these data with the giant branches of metal-poor population at the distance of M31. By comparing these data with the giant branches of Galactic globular clusters, we determine that the abundance of And III is [Fe/H]=-2.0+/-0.15; with this abundance And III lies on the luminosity-abundance relation defined by the Galactic dwarf spheroidal galaxies. There is some evidence for a small (0.16&lt;{sigma}([Fe/H])&lt;0.24) intrinsic abundance dispersion within And III, but we are unable to unambiguously establish its presence. A study of the And III I-band luminosity function yields a distance modulus (m-M)_0_ of 24.4+/-0.2 for this galaxy, and indicates that the fraction of intermediate-age (3 to 10Gyr) population in And III is approximately 10+/-10 percent. In all these aspects And III, like And I, is similar to the Galactic dwarf spheroidal systems, indicating that M31 and the Galaxy provided similar conditions for the evolution of such galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/986#1</TD>
            <TD>2011-09-14T18:21:33Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/986</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/986</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/986</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/986 [2]</TD>
            <TD>CMD for And III (Armandroff+, 1993)</TD>
            <TD>The prime focus CCD camera of the KPNO 4 m telescope has been used to image Andromeda III, a dwarf spheroidal galaxy companion to M31, in the V and I bands. The resulting color-magnitude diagram shows a well defined giant branch whose tip luminosity corresponds to that expected for an old metal-poor population at the distance of M31. By comparing these data with the giant branches of metal-poor population at the distance of M31. By comparing these data with the giant branches of Galactic globular clusters, we determine that the abundance of And III is [Fe/H]=-2.0+/-0.15; with this abundance And III lies on the luminosity-abundance relation defined by the Galactic dwarf spheroidal galaxies. There is some evidence for a small (0.16&lt;{sigma}([Fe/H])&lt;0.24) intrinsic abundance dispersion within And III, but we are unable to unambiguously establish its presence. A study of the And III I-band luminosity function yields a distance modulus (m-M)_0_ of 24.4+/-0.2 for this galaxy, and indicates that the fraction of intermediate-age (3 to 10Gyr) population in And III is approximately 10+/-10 percent. In all these aspects And III, like And I, is similar to the Galactic dwarf spheroidal systems, indicating that M31 and the Galaxy provided similar conditions for the evolution of such galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/986#2</TD>
            <TD>2011-09-14T18:21:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/986</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/986&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/986</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/986 [1]</TD>
            <TD>CMD for And III (Armandroff+, 1993)</TD>
            <TD>The prime focus CCD camera of the KPNO 4 m telescope has been used to image Andromeda III, a dwarf spheroidal galaxy companion to M31, in the V and I bands. The resulting color-magnitude diagram shows a well defined giant branch whose tip luminosity corresponds to that expected for an old metal-poor population at the distance of M31. By comparing these data with the giant branches of metal-poor population at the distance of M31. By comparing these data with the giant branches of Galactic globular clusters, we determine that the abundance of And III is [Fe/H]=-2.0+/-0.15; with this abundance And III lies on the luminosity-abundance relation defined by the Galactic dwarf spheroidal galaxies. There is some evidence for a small (0.16&lt;{sigma}([Fe/H])&lt;0.24) intrinsic abundance dispersion within And III, but we are unable to unambiguously establish its presence. A study of the And III I-band luminosity function yields a distance modulus (m-M)_0_ of 24.4+/-0.2 for this galaxy, and indicates that the fraction of intermediate-age (3 to 10Gyr) population in And III is approximately 10+/-10 percent. In all these aspects And III, like And I, is similar to the Galactic dwarf spheroidal systems, indicating that M31 and the Galaxy provided similar conditions for the evolution of such galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/106/986</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/986</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/986</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/986 [2]</TD>
            <TD>CMD for And III (Armandroff+, 1993)</TD>
            <TD>The prime focus CCD camera of the KPNO 4 m telescope has been used to image Andromeda III, a dwarf spheroidal galaxy companion to M31, in the V and I bands. The resulting color-magnitude diagram shows a well defined giant branch whose tip luminosity corresponds to that expected for an old metal-poor population at the distance of M31. By comparing these data with the giant branches of metal-poor population at the distance of M31. By comparing these data with the giant branches of Galactic globular clusters, we determine that the abundance of And III is [Fe/H]=-2.0+/-0.15; with this abundance And III lies on the luminosity-abundance relation defined by the Galactic dwarf spheroidal galaxies. There is some evidence for a small (0.16&lt;{sigma}([Fe/H])&lt;0.24) intrinsic abundance dispersion within And III, but we are unable to unambiguously establish its presence. A study of the And III I-band luminosity function yields a distance modulus (m-M)_0_ of 24.4+/-0.2 for this galaxy, and indicates that the fraction of intermediate-age (3 to 10Gyr) population in And III is approximately 10+/-10 percent. In all these aspects And III, like And I, is similar to the Galactic dwarf spheroidal systems, indicating that M31 and the Galaxy provided similar conditions for the evolution of such galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/986</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/1086 [1]</TD>
            <TD>VI Photometry in M54 and Sgr Dwarf Galaxy (Sarajedini+ 1995)</TD>
            <TD>We present VI CCD color-magnitude diagrams for the globular cluster M54 and the Sagittarius dwarf galaxy. These are used to derive the following quantities: [Fe/H] = -1.79 +/- 0.08 for M54 and [Fe/H] = -0.52 +/- 0.09 for Sagittarius. We find a metallicity dispersion of +/- 0.16 dex in M54, and we infer the possible existence of a [Fe/H] ~ -1.3 component in Sagittarius, which may have a metallicity dispersion as well. The mean reddening in the direction of M54 is E(B-V) = 0.13 +/- 0.02. The distances to M54 and Sagittarius, determined using their horizontal branch magnitudes, are identical to within the uncertainties of existing RR Lyrae luminosity-abundance relations. This, together with positional and radial velocity arguments, suggests that M54 is physically associated with Sagittarius. We note that M54 is substantially brighter than the globular cluster members of the Fornax dwarf spheroidal galaxy, and that the metal abundance of Sagittarius is quite high for its estimated absolute magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1086</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/1086 [2]</TD>
            <TD>VI Photometry in M54 and Sgr Dwarf Galaxy (Sarajedini+ 1995)</TD>
            <TD>We present VI CCD color-magnitude diagrams for the globular cluster M54 and the Sagittarius dwarf galaxy. These are used to derive the following quantities: [Fe/H] = -1.79 +/- 0.08 for M54 and [Fe/H] = -0.52 +/- 0.09 for Sagittarius. We find a metallicity dispersion of +/- 0.16 dex in M54, and we infer the possible existence of a [Fe/H] ~ -1.3 component in Sagittarius, which may have a metallicity dispersion as well. The mean reddening in the direction of M54 is E(B-V) = 0.13 +/- 0.02. The distances to M54 and Sagittarius, determined using their horizontal branch magnitudes, are identical to within the uncertainties of existing RR Lyrae luminosity-abundance relations. This, together with positional and radial velocity arguments, suggests that M54 is physically associated with Sagittarius. We note that M54 is substantially brighter than the globular cluster members of the Fornax dwarf spheroidal galaxy, and that the metal abundance of Sagittarius is quite high for its estimated absolute magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1086</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/1086 [1]</TD>
            <TD>VI Photometry in M54 and Sgr Dwarf Galaxy (Sarajedini+ 1995)</TD>
            <TD>We present VI CCD color-magnitude diagrams for the globular cluster M54 and the Sagittarius dwarf galaxy. These are used to derive the following quantities: [Fe/H] = -1.79 +/- 0.08 for M54 and [Fe/H] = -0.52 +/- 0.09 for Sagittarius. We find a metallicity dispersion of +/- 0.16 dex in M54, and we infer the possible existence of a [Fe/H] ~ -1.3 component in Sagittarius, which may have a metallicity dispersion as well. The mean reddening in the direction of M54 is E(B-V) = 0.13 +/- 0.02. The distances to M54 and Sagittarius, determined using their horizontal branch magnitudes, are identical to within the uncertainties of existing RR Lyrae luminosity-abundance relations. This, together with positional and radial velocity arguments, suggests that M54 is physically associated with Sagittarius. We note that M54 is substantially brighter than the globular cluster members of the Fornax dwarf spheroidal galaxy, and that the metal abundance of Sagittarius is quite high for its estimated absolute magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1086#1</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/1086</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1086</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/1086 [2]</TD>
            <TD>VI Photometry in M54 and Sgr Dwarf Galaxy (Sarajedini+ 1995)</TD>
            <TD>We present VI CCD color-magnitude diagrams for the globular cluster M54 and the Sagittarius dwarf galaxy. These are used to derive the following quantities: [Fe/H] = -1.79 +/- 0.08 for M54 and [Fe/H] = -0.52 +/- 0.09 for Sagittarius. We find a metallicity dispersion of +/- 0.16 dex in M54, and we infer the possible existence of a [Fe/H] ~ -1.3 component in Sagittarius, which may have a metallicity dispersion as well. The mean reddening in the direction of M54 is E(B-V) = 0.13 +/- 0.02. The distances to M54 and Sagittarius, determined using their horizontal branch magnitudes, are identical to within the uncertainties of existing RR Lyrae luminosity-abundance relations. This, together with positional and radial velocity arguments, suggests that M54 is physically associated with Sagittarius. We note that M54 is substantially brighter than the globular cluster members of the Fornax dwarf spheroidal galaxy, and that the metal abundance of Sagittarius is quite high for its estimated absolute magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/960 [1]</TD>
            <TD>Young star clusters in The Antennae (Whitmore+ 1995)</TD>
            <TD>New high-resolution images of the disks of NGC 4038/4039 obtained with the Wide Field Camera of the Hubble Space Telescope (HST) are presented. NGC 4038/4039, nicknamed "The Antennae," is a prototypical example of a pair of colliding galaxies believed to be at an early stage of a merger. Down to the limiting magnitude of V~23mag, the HST images reveal a population of over 700 blue pointlike objects within the disks. The mean absolute magnitude of these objects is M_V_=-11mag, with the brightest objects reaching M_V_~-15. Their mean apparent color indices are U-V=-0.7mag and V-I=0.8mag on the Johnson UVI passband system, while their mean indices corrected for internal reddening are (U-V)_0_=-1.0mag and (V-I)_0_=0.5. Their mean effective radius, determined from slightly resolved images, is 18pc (for H0=50km/s/Mpc). Based on their luminosities and resolution, most of these objects cannot be individual stars, but are likely young compact star clusters. The brighter ones are similar to the objects found in NGC 1275 and NGC 7252, which appear to be young globular clusters formed during recent galaxy mergers. Based on their U-V and V-I colors, the brightest, bluest clusters of NGC 4038/4039 appear to be less than 10Myr old. Most of these bright clusters are relatively tightly clustered themselves, with typically a dozen individual clusters belonging to a complex identified as a giant H II region from ground-based observations. The cluster luminosity function (LF) is approximately a power law, {Phi}(L)dL is proportional to L^(-1.78+/-0.05)^dL, with no hint of a turnover at fainter magnitudes. This power-law shape agrees with the LF of Magellanic Cloud clusters and Galactic open clusters, but differs from the LF of old globular cluster systems that is typically Gaussian with a FWHM of ~3mag. Possible explanations for this apparent difference include: (1) We have not observed faint enough to see the turnover, (2) the initial LF of star clusters is a power law but the fainter objects dissolve with time, (3) conditions at the present epoch favor the formation of a wide range of cluster masses while conditions at earlier epochs favored the formation of massive clusters, and (4) the NGC 4038/4039 clusters may not evolve into normal globular clusters. Besides the blue clusters, we also find about a dozen extremely red objects with V-I&gt;3.0. The highest number density of these red objects is found in the SE quadrant, where star formation appears to be most recent. We propose that these objects may be very young star clusters still embedded in their placental dust cocoons.</TD>
            <TD>CDS</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/960</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/960</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/960 [2]</TD>
            <TD>Young star clusters in The Antennae (Whitmore+ 1995)</TD>
            <TD>New high-resolution images of the disks of NGC 4038/4039 obtained with the Wide Field Camera of the Hubble Space Telescope (HST) are presented. NGC 4038/4039, nicknamed "The Antennae," is a prototypical example of a pair of colliding galaxies believed to be at an early stage of a merger. Down to the limiting magnitude of V~23mag, the HST images reveal a population of over 700 blue pointlike objects within the disks. The mean absolute magnitude of these objects is M_V_=-11mag, with the brightest objects reaching M_V_~-15. Their mean apparent color indices are U-V=-0.7mag and V-I=0.8mag on the Johnson UVI passband system, while their mean indices corrected for internal reddening are (U-V)_0_=-1.0mag and (V-I)_0_=0.5. Their mean effective radius, determined from slightly resolved images, is 18pc (for H0=50km/s/Mpc). Based on their luminosities and resolution, most of these objects cannot be individual stars, but are likely young compact star clusters. The brighter ones are similar to the objects found in NGC 1275 and NGC 7252, which appear to be young globular clusters formed during recent galaxy mergers. Based on their U-V and V-I colors, the brightest, bluest clusters of NGC 4038/4039 appear to be less than 10Myr old. Most of these bright clusters are relatively tightly clustered themselves, with typically a dozen individual clusters belonging to a complex identified as a giant H II region from ground-based observations. The cluster luminosity function (LF) is approximately a power law, {Phi}(L)dL is proportional to L^(-1.78+/-0.05)^dL, with no hint of a turnover at fainter magnitudes. This power-law shape agrees with the LF of Magellanic Cloud clusters and Galactic open clusters, but differs from the LF of old globular cluster systems that is typically Gaussian with a FWHM of ~3mag. Possible explanations for this apparent difference include: (1) We have not observed faint enough to see the turnover, (2) the initial LF of star clusters is a power law but the fainter objects dissolve with time, (3) conditions at the present epoch favor the formation of a wide range of cluster masses while conditions at earlier epochs favored the formation of massive clusters, and (4) the NGC 4038/4039 clusters may not evolve into normal globular clusters. Besides the blue clusters, we also find about a dozen extremely red objects with V-I&gt;3.0. The highest number density of these red objects is found in the SE quadrant, where star formation appears to be most recent. We propose that these objects may be very young star clusters still embedded in their placental dust cocoons.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/960</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/960 [1]</TD>
            <TD>Young star clusters in The Antennae (Whitmore+ 1995)</TD>
            <TD>New high-resolution images of the disks of NGC 4038/4039 obtained with the Wide Field Camera of the Hubble Space Telescope (HST) are presented. NGC 4038/4039, nicknamed "The Antennae," is a prototypical example of a pair of colliding galaxies believed to be at an early stage of a merger. Down to the limiting magnitude of V~23mag, the HST images reveal a population of over 700 blue pointlike objects within the disks. The mean absolute magnitude of these objects is M_V_=-11mag, with the brightest objects reaching M_V_~-15. Their mean apparent color indices are U-V=-0.7mag and V-I=0.8mag on the Johnson UVI passband system, while their mean indices corrected for internal reddening are (U-V)_0_=-1.0mag and (V-I)_0_=0.5. Their mean effective radius, determined from slightly resolved images, is 18pc (for H0=50km/s/Mpc). Based on their luminosities and resolution, most of these objects cannot be individual stars, but are likely young compact star clusters. The brighter ones are similar to the objects found in NGC 1275 and NGC 7252, which appear to be young globular clusters formed during recent galaxy mergers. Based on their U-V and V-I colors, the brightest, bluest clusters of NGC 4038/4039 appear to be less than 10Myr old. Most of these bright clusters are relatively tightly clustered themselves, with typically a dozen individual clusters belonging to a complex identified as a giant H II region from ground-based observations. The cluster luminosity function (LF) is approximately a power law, {Phi}(L)dL is proportional to L^(-1.78+/-0.05)^dL, with no hint of a turnover at fainter magnitudes. This power-law shape agrees with the LF of Magellanic Cloud clusters and Galactic open clusters, but differs from the LF of old globular cluster systems that is typically Gaussian with a FWHM of ~3mag. Possible explanations for this apparent difference include: (1) We have not observed faint enough to see the turnover, (2) the initial LF of star clusters is a power law but the fainter objects dissolve with time, (3) conditions at the present epoch favor the formation of a wide range of cluster masses while conditions at earlier epochs favored the formation of massive clusters, and (4) the NGC 4038/4039 clusters may not evolve into normal globular clusters. Besides the blue clusters, we also find about a dozen extremely red objects with V-I&gt;3.0. The highest number density of these red objects is found in the SE quadrant, where star formation appears to be most recent. We propose that these objects may be very young star clusters still embedded in their placental dust cocoons.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/960 [2]</TD>
            <TD>Young star clusters in The Antennae (Whitmore+ 1995)</TD>
            <TD>New high-resolution images of the disks of NGC 4038/4039 obtained with the Wide Field Camera of the Hubble Space Telescope (HST) are presented. NGC 4038/4039, nicknamed "The Antennae," is a prototypical example of a pair of colliding galaxies believed to be at an early stage of a merger. Down to the limiting magnitude of V~23mag, the HST images reveal a population of over 700 blue pointlike objects within the disks. The mean absolute magnitude of these objects is M_V_=-11mag, with the brightest objects reaching M_V_~-15. Their mean apparent color indices are U-V=-0.7mag and V-I=0.8mag on the Johnson UVI passband system, while their mean indices corrected for internal reddening are (U-V)_0_=-1.0mag and (V-I)_0_=0.5. Their mean effective radius, determined from slightly resolved images, is 18pc (for H0=50km/s/Mpc). Based on their luminosities and resolution, most of these objects cannot be individual stars, but are likely young compact star clusters. The brighter ones are similar to the objects found in NGC 1275 and NGC 7252, which appear to be young globular clusters formed during recent galaxy mergers. Based on their U-V and V-I colors, the brightest, bluest clusters of NGC 4038/4039 appear to be less than 10Myr old. Most of these bright clusters are relatively tightly clustered themselves, with typically a dozen individual clusters belonging to a complex identified as a giant H II region from ground-based observations. The cluster luminosity function (LF) is approximately a power law, {Phi}(L)dL is proportional to L^(-1.78+/-0.05)^dL, with no hint of a turnover at fainter magnitudes. This power-law shape agrees with the LF of Magellanic Cloud clusters and Galactic open clusters, but differs from the LF of old globular cluster systems that is typically Gaussian with a FWHM of ~3mag. Possible explanations for this apparent difference include: (1) We have not observed faint enough to see the turnover, (2) the initial LF of star clusters is a power law but the fainter objects dissolve with time, (3) conditions at the present epoch favor the formation of a wide range of cluster masses while conditions at earlier epochs favored the formation of massive clusters, and (4) the NGC 4038/4039 clusters may not evolve into normal globular clusters. Besides the blue clusters, we also find about a dozen extremely red objects with V-I&gt;3.0. The highest number density of these red objects is found in the SE quadrant, where star formation appears to be most recent. We propose that these objects may be very young star clusters still embedded in their placental dust cocoons.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/190/147 [1]</TD>
            <TD>Mid-IR galaxy morphology from S^4^G (Buta+, 2010)</TD>
            <TD>The goals of the S^4^G project are described by Sheth et al. (2010, PASP, submitted).</TD>
            <TD>CDS</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/190/147</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/190/147</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/190/147 [2]</TD>
            <TD>Mid-IR galaxy morphology from S^4^G (Buta+, 2010)</TD>
            <TD>The goals of the S^4^G project are described by Sheth et al. (2010, PASP, submitted).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147#2</TD>
            <TD>2011-09-14T21:03:30Z</TD>
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            <TD>30-Sep-2010</TD>
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            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/190/147&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/190/147</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/190/147 [table1]</TD>
            <TD>Mid-IR galaxy morphology from S^4^G (Buta+, 2010)</TD>
            <TD>The goals of the S^4^G project are described by Sheth et al. (2010, PASP, submitted).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147#table1</TD>
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            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/190/147</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/190/147&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/190/147</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1959 [1]</TD>
            <TD>VLA survey of Abell clusters. V. (Ledlow+ 1995)</TD>
            <TD>We present results from a program of optical imaging of 265 radio galaxies in rich clusters. Using isophotal surface photometry, we investigate the optical properties such as the morphology, surface-brightness profiles, surface-brightness/size relationships, ellipticities, and the frequency of nonelliptical isophotes. The results are compared to a "normal" nonradio-selected sample of elliptical galaxies from the same clusters. The goal is to determine if the parent population of FR I radio galaxies can be distinguished optically from radio-quiet galaxies. The results of the analysis are that cluster ellipticals are a very homogeneous class of objects. The optical properties are consistent with a one-parameter family, where the optical luminosity is the fundamental parameter. In all tests considered, radio-loud FR I galaxies cannot be distinguished optically from radio-quiet galaxies selected from the same environment. The local density of nearby companions (&lt;20kpc) and the frequency of morphological peculiarities or tidal interactions are not statistically different between the radio-loud and quiet samples. There is some suggestion from comparison to published samples of non-cluster radio galaxies, that the cluster environment is not condusive to long-lived tidal interactions, and that such events may be more important to galaxy evolution in poor groups and lower density environments. Such events appear to have little influence on the formation of FR I radio galaxies in rich clusters. The results are consistent with the idea that all elliptical galaxies may at some time (or many times) contain powerful (FR I) radio sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1959#1</TD>
            <TD>2011-09-14T18:22:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1959</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1959</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1959 [2]</TD>
            <TD>VLA survey of Abell clusters. V. (Ledlow+ 1995)</TD>
            <TD>We present results from a program of optical imaging of 265 radio galaxies in rich clusters. Using isophotal surface photometry, we investigate the optical properties such as the morphology, surface-brightness profiles, surface-brightness/size relationships, ellipticities, and the frequency of nonelliptical isophotes. The results are compared to a "normal" nonradio-selected sample of elliptical galaxies from the same clusters. The goal is to determine if the parent population of FR I radio galaxies can be distinguished optically from radio-quiet galaxies. The results of the analysis are that cluster ellipticals are a very homogeneous class of objects. The optical properties are consistent with a one-parameter family, where the optical luminosity is the fundamental parameter. In all tests considered, radio-loud FR I galaxies cannot be distinguished optically from radio-quiet galaxies selected from the same environment. The local density of nearby companions (&lt;20kpc) and the frequency of morphological peculiarities or tidal interactions are not statistically different between the radio-loud and quiet samples. There is some suggestion from comparison to published samples of non-cluster radio galaxies, that the cluster environment is not condusive to long-lived tidal interactions, and that such events may be more important to galaxy evolution in poor groups and lower density environments. Such events appear to have little influence on the formation of FR I radio galaxies in rich clusters. The results are consistent with the idea that all elliptical galaxies may at some time (or many times) contain powerful (FR I) radio sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1959#2</TD>
            <TD>2011-09-14T18:22:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1959&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1959</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1959 [1]</TD>
            <TD>VLA survey of Abell clusters. V. (Ledlow+ 1995)</TD>
            <TD>We present results from a program of optical imaging of 265 radio galaxies in rich clusters. Using isophotal surface photometry, we investigate the optical properties such as the morphology, surface-brightness profiles, surface-brightness/size relationships, ellipticities, and the frequency of nonelliptical isophotes. The results are compared to a "normal" nonradio-selected sample of elliptical galaxies from the same clusters. The goal is to determine if the parent population of FR I radio galaxies can be distinguished optically from radio-quiet galaxies. The results of the analysis are that cluster ellipticals are a very homogeneous class of objects. The optical properties are consistent with a one-parameter family, where the optical luminosity is the fundamental parameter. In all tests considered, radio-loud FR I galaxies cannot be distinguished optically from radio-quiet galaxies selected from the same environment. The local density of nearby companions (&lt;20kpc) and the frequency of morphological peculiarities or tidal interactions are not statistically different between the radio-loud and quiet samples. There is some suggestion from comparison to published samples of non-cluster radio galaxies, that the cluster environment is not condusive to long-lived tidal interactions, and that such events may be more important to galaxy evolution in poor groups and lower density environments. Such events appear to have little influence on the formation of FR I radio galaxies in rich clusters. The results are consistent with the idea that all elliptical galaxies may at some time (or many times) contain powerful (FR I) radio sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1959#1</TD>
            <TD>2011-09-14T18:22:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1959</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1959</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1959 [2]</TD>
            <TD>VLA survey of Abell clusters. V. (Ledlow+ 1995)</TD>
            <TD>We present results from a program of optical imaging of 265 radio galaxies in rich clusters. Using isophotal surface photometry, we investigate the optical properties such as the morphology, surface-brightness profiles, surface-brightness/size relationships, ellipticities, and the frequency of nonelliptical isophotes. The results are compared to a "normal" nonradio-selected sample of elliptical galaxies from the same clusters. The goal is to determine if the parent population of FR I radio galaxies can be distinguished optically from radio-quiet galaxies. The results of the analysis are that cluster ellipticals are a very homogeneous class of objects. The optical properties are consistent with a one-parameter family, where the optical luminosity is the fundamental parameter. In all tests considered, radio-loud FR I galaxies cannot be distinguished optically from radio-quiet galaxies selected from the same environment. The local density of nearby companions (&lt;20kpc) and the frequency of morphological peculiarities or tidal interactions are not statistically different between the radio-loud and quiet samples. There is some suggestion from comparison to published samples of non-cluster radio galaxies, that the cluster environment is not condusive to long-lived tidal interactions, and that such events may be more important to galaxy evolution in poor groups and lower density environments. Such events appear to have little influence on the formation of FR I radio galaxies in rich clusters. The results are consistent with the idea that all elliptical galaxies may at some time (or many times) contain powerful (FR I) radio sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1959#2</TD>
            <TD>2011-09-14T18:22:10Z</TD>
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            <TD>26-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1959&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1959</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2131 [1]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131#1</TD>
            <TD>2011-09-14T18:22:12Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2131</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2131</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2131 [2]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131#2</TD>
            <TD>2011-09-14T18:22:12Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2131&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table3s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131#table3s</TD>
            <TD>2011-09-14T18:22:12Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table5s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131#table5s</TD>
            <TD>2011-09-14T18:22:12Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table2s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131#table2s</TD>
            <TD>2011-09-14T18:22:12Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/110/2131 [1]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
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            <TD>J/AJ/110/2131 [2]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table3s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table5s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table2s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table4s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/110/2131 [1]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
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            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2131 [2]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table3s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>J/AJ/110/2131 [table5s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T18:22:12Z</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table2s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2131#table2s</TD>
            <TD>2011-09-14T18:22:12Z</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/110/2131 [table4s]</TD>
            <TD>M/L for Draco and UMi. I. (Armandroff+ 1995)</TD>
            <TD>We have measured 206 radial velocities for 94 probable members in the Ursa Minor dwarf spheroidal galaxy and 167 velocities for 91 probable members in the Draco dwarf spheroidal galaxy. These velocities were obtained using the KPNO 4m telescope with the Hydra multifiber positioner and bench spectrograph in 1992, 1993, and 1994. Both simulations and repeated measurements show that the median uncertainty in these velocities is 4.0km/s. Our velocities are compared with the other major datasets for Draco and Ursa Minor. Aside from a small zero-point difference, there is excellent agreement between the Hydra velocities and the Olszewski et al. MMT echelle velocities. Comparison with the Hargreaves et al. Ursa Minor velocities reveals inconsistencies which we ascribe to underestimated errors in the Hargreaves et al. data. After correcting for zero-point differences, we combine the three major sets of velocities. Our spectra recovered all of the known Carbon (C) stars in Draco and Ursa Minor and revealed one new C star in Draco and two in Ursa Minor. In addition, one star whose velocity is consistent with membership in Ursa Minor has a deep and wide HBeta absorption line in its spectrum. An initial discussion of the kinematics of the two galaxies is presented. The systemic velocities of Draco and Ursa Minor are -293.3+/-1.0 and -274+/-1.0km/s, respectively. Ursa Minor shows apparent rotation about a position angle of 75deg with an amplitude of about 3km/s; the morphological major axis is 53+/-5deg. No such rotation is found in Draco. We find a velocity dispersion of 10.4+/-0.9km/s for Ursa Minor including all stars and 8.8+/-0.8km/s excluding the star with the most extreme velocity. In Draco we find 10.7+/-0.9km/s including all stars and 8.5+/-0.7km/s excluding the three stars with the most extreme velocities. These dispersions are consistent with the dispersions measured in the other two studies and confirm that Draco and Ursa Minor have the largest mass-to-light ratios of any of the dwarf spheroidals.</TD>
            <TD>CDS</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/110/2715 [1]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
            <TD>CDS</TD>
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            <TD>2011-09-14T18:22:16Z</TD>
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            <TD>J/AJ/110/2715 [2]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2715#2</TD>
            <TD>2011-09-14T18:22:16Z</TD>
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            <TD>J/AJ/110/2715 [m33]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
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            <TD>J/AJ/110/2715 [ngc6822]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
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            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
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            <TD>2011-09-14T18:22:16Z</TD>
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            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2715</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2715</TD>
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            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
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            <TD>05-Sep-1996</TD>
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            <TD>J/AJ/110/2715 [m33]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
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            <TD>J/AJ/110/2715 [ngc6822]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
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            <TD>J/AJ/110/2715 [1]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
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            <TD>J/AJ/110/2715 [2]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
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            <TD>J/AJ/110/2715 [m33]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
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            <TD>J/AJ/110/2715 [ngc6822]</TD>
            <TD>UBV photometry in NGC 6822, M31 and M33 (Massey+ 1995)</TD>
            <TD>We investigate the massive star content of the three Local Group galaxies NGC 6822, M31, and M33 using crowded-field CCD UBV photometry in selected regions to identify the most luminous and massive stars. Optical spectroscopy is presented for many of these stars, allowing construction of accurate H-R diagrams and the first meaningful characterization of the massive star populations in these galaxies. The spectral types also allow investigation of the internal reddenings within these systems and provide fine candidates for stellar-wind studies in the UV. The early-type stars identified include O-type in all three systems, and we call attention to a new Luminous Blue Variable candidate in M33. Our spectroscopy of extreme B supergiants (M_V=-7.5) shows the expected changes with metallicity in comparison to similar objects in the Milky Way, LMC, and SMC, although the metal lines in the NGC 6822 stars are considerably weaker than that expected for a metallicity intermediate between that of the LMC and SMC, suggesting that this galaxy is more metal poor than usually supposed. There is considerable internal reddening within all three galaxies, including even the dwarf irregular NGC 6822, where the color excesses show a systematic spatial trend from E(B-V)=0.26 near the edges to 0.45 in the middle. The slope of the reddening curve is normal in NGC 6822 and M33, with E(U-B)/E(B-V)~0.72, but in M31 we find that this ratio is 0.4-0.5 in all three of our fields. We spectroscopically confirm that stars of high mass (&gt;80M_{sun}_) and luminosity (Mbol~-11) are found in M31 and M33. We have not found stars of similar high mass or luminosity in NGC 6822, where the most luminous star present has Mbol=-10 and an inferred mass of 60M_{sun}_. Similarly, none of the OB associations in NGC 6822 are as impressive in terms of the number of massive stars as the rich associations of the Milky Way and Magellanic Clouds. However, OB78 (=NGC 206) and OB48 in M31 both contain 9-15 stars of mass &gt;40M_{sun}_, making them comparable to impressive sites of star formation in the Milky Way and Magellanic Clouds. M33 contains regions that are even more extreme, with M33-OB127 and M33-OB21 containing 20-30 such stars. The low number of very massive stars in NGC 6822 is consistent with the overall star-formation rate inferred by other means, but the M33 results suggest that the formation of high-mass stars may be favored. The massive star content of individual associations would not have been inferred on the basis of Halpha flux, meaning that the nebulae associated with a number of these OB associations are density rather than radiation bounded, probably due to holes blown in the H I. We have also found that the ratio of the number of very massive (&gt;40M_{sun}_) stars to the number of WR stars is constant within all the Local Group galaxies we have studied, suggesting that (a) the effect of metallicity on the evolution of massive stars is subtle if present, and (b) that WR stars make excellent tracers of the massive star populations. The fact that this ratio is roughly 3, rather than the 10 expected given the relative H- and He-burning lifetimes, argues that either our samples are (uniformly?) incomplete or that some fraction of WR stars are H-burning objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2715#ngc6822</TD>
            <TD>2011-09-14T18:22:16Z</TD>
            <TD>#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2715</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2747 [1]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#1</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2747</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2747 [2]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#2</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2747&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2747 [table4]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#table4</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2747&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2747 [table3]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#table3</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2747&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2747 [1]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#1</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2747</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2747 [2]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#2</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2747&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2747 [table4]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#table4</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2747&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2747 [table3]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#table3</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2747&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2747 [1]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#1</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2747</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2747 [2]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#2</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2747&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2747 [table4]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#table4</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2747&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2747 [table3]</TD>
            <TD>Stars in Sculptor dwarf spheroidal galaxy (Schweitzer+ 1995)</TD>
            <TD>Using 26 plates taken over the course of more than half a century, we present proper motions and photometry for 1177 stars in the central region of the Sculptor dwarf spheroidal galaxy, down to a limiting magnitude of V~20.25 at the level of the horizontal branch. The proper-motion cleaned color-magnitude diagram retained a broad giant branch, further supporting an intrinsic spread in metallicity. We determined an absolute proper motion for Sculptor, relative to background galaxies, of mu_alpha=+0.036+/-0.022arcsec/century and mu_delta=0.043+/-0.025arcsec/century after correcting for the LSR and peculiar solar motions. Our proper-motion uncertainty is similar to or smaller than those obtained by different groups for other distant satellites of the Galaxy. When combined with Sculptor's distance and radial velocity, this measurement shows the dwarf spheroidal to have a space velocity of roughly 220+/-125km/s. Although our measurement is less than twice its uncertainty, the direction of Sculptor's motion is significant because it rules out motion along the Magellanic Stream. A 2.5 sigma error allows for motion in a direction toward the Fornax dwarf spheroidal galaxy, so Sculptor remains a possible member of the proposed Fornax-Leo-Sculptor stream.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747#table3</TD>
            <TD>2011-09-14T18:22:18Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2747</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2747&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2747</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/95/1629 [1]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#1</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/95/1629</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/95/1629 [2]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#2</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/95/1629&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/95/1629 [table2]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#table2</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/95/1629&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/95/1629 [table1]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#table1</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/95/1629&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/95/1629 [1]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#1</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/95/1629</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/95/1629 [2]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#2</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/95/1629&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/95/1629 [table2]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#table2</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/95/1629&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/95/1629 [table1]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#table1</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/95/1629&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/95/1629 [1]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#1</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/95/1629</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/95/1629 [2]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#2</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/95/1629&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/95/1629 [table2]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#table2</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/95/1629&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/95/1629 [table1]</TD>
            <TD>[O III] emission in 2 field-galaxy surveys (Moody+ 1988)</TD>
            <TD>We present emission-line strengths for 394 galaxies from the field-galaxy redshift surveys of Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/AJ/83/1549&gt;, KOS) and Kirshner et al. (1983, Cat. &lt;J/AJ/88/1285&gt;, KOSS) as part of a study of the nature of field and void galaxies. These data are 95% complete in their coverage of the [O III]{lambda}{lambda}5007,4959 emission lines. We find that 8.8%+/-1.5% of a J magnitude-limited data set have [O III]{lambda}5007 emission equivalent widths greater than 10A. There is no evidence that the spatial distribution of emission-line galaxies in each field differs from that of galaxies without emission. However, there is a significant increase in the fraction of galaxies with strong [O III] emission in the southern fields of the Kirshner, Oemler, and Schechter (1978, Cat. &lt;J/J/83/1549&gt;) survey as compared with the other survey fields. Our results are consistent with the conclusion that the fraction of galaxies with emission is larger in the Bootes void than in the general field, but tighter constraints on the void normal galaxy population are needed to improve the statistics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629#table1</TD>
            <TD>2011-09-14T18:22:46Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/95/1629</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/95/1629&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/95/1629</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/298/544 [1]</TD>
            <TD>NGC 121 BR photometry (Stryker+ 1985)</TD>
            <TD>The age of the SMC globular cluster NGC 121 is found from main-sequence isochrone fitting to be 12+/-2x10^9^yr if a distance modulus that assumes Mv=+0.6 for the field RR Lyrae variables near the cluster is used. If instead (m-M)o = 19.3, then the cluster age is 9+/-2x10^9^yr. The cluster is known to contain both RR Lyrae variables and a marginal carbon star; comparison with theoretical models indicates no significant inconsistencies in this joint occurrence at either modulus. The color-magnitude diagram for the nearby field also shows a faint, blue main-sequence turnoff and, in contrast to previous Magellanic Cloud field studies, the field lacks any evidence for the existence of a significant intermediate-age component. A new look at the chemical evolution of the Small Magellanic Cloud suggests that, unlike the Galaxy, where the rate of enrichment has been steady after the initial phase, the enrichment in the SMC remained small for a long interval before increasing rapidly sometime in the last 1-2x10^9^yr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/298/544#1</TD>
            <TD>2011-09-14T18:23:01Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/298/544</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/298/544</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/298/544</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/298/544 [2]</TD>
            <TD>NGC 121 BR photometry (Stryker+ 1985)</TD>
            <TD>The age of the SMC globular cluster NGC 121 is found from main-sequence isochrone fitting to be 12+/-2x10^9^yr if a distance modulus that assumes Mv=+0.6 for the field RR Lyrae variables near the cluster is used. If instead (m-M)o = 19.3, then the cluster age is 9+/-2x10^9^yr. The cluster is known to contain both RR Lyrae variables and a marginal carbon star; comparison with theoretical models indicates no significant inconsistencies in this joint occurrence at either modulus. The color-magnitude diagram for the nearby field also shows a faint, blue main-sequence turnoff and, in contrast to previous Magellanic Cloud field studies, the field lacks any evidence for the existence of a significant intermediate-age component. A new look at the chemical evolution of the Small Magellanic Cloud suggests that, unlike the Galaxy, where the rate of enrichment has been steady after the initial phase, the enrichment in the SMC remained small for a long interval before increasing rapidly sometime in the last 1-2x10^9^yr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/298/544#2</TD>
            <TD>2011-09-14T18:23:01Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/298/544</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/298/544&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/298/544</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/298/544 [1]</TD>
            <TD>NGC 121 BR photometry (Stryker+ 1985)</TD>
            <TD>The age of the SMC globular cluster NGC 121 is found from main-sequence isochrone fitting to be 12+/-2x10^9^yr if a distance modulus that assumes Mv=+0.6 for the field RR Lyrae variables near the cluster is used. If instead (m-M)o = 19.3, then the cluster age is 9+/-2x10^9^yr. The cluster is known to contain both RR Lyrae variables and a marginal carbon star; comparison with theoretical models indicates no significant inconsistencies in this joint occurrence at either modulus. The color-magnitude diagram for the nearby field also shows a faint, blue main-sequence turnoff and, in contrast to previous Magellanic Cloud field studies, the field lacks any evidence for the existence of a significant intermediate-age component. A new look at the chemical evolution of the Small Magellanic Cloud suggests that, unlike the Galaxy, where the rate of enrichment has been steady after the initial phase, the enrichment in the SMC remained small for a long interval before increasing rapidly sometime in the last 1-2x10^9^yr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/298/544#1</TD>
            <TD>2011-09-14T18:23:01Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/298/544</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/298/544</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/298/544</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/298/544 [2]</TD>
            <TD>NGC 121 BR photometry (Stryker+ 1985)</TD>
            <TD>The age of the SMC globular cluster NGC 121 is found from main-sequence isochrone fitting to be 12+/-2x10^9^yr if a distance modulus that assumes Mv=+0.6 for the field RR Lyrae variables near the cluster is used. If instead (m-M)o = 19.3, then the cluster age is 9+/-2x10^9^yr. The cluster is known to contain both RR Lyrae variables and a marginal carbon star; comparison with theoretical models indicates no significant inconsistencies in this joint occurrence at either modulus. The color-magnitude diagram for the nearby field also shows a faint, blue main-sequence turnoff and, in contrast to previous Magellanic Cloud field studies, the field lacks any evidence for the existence of a significant intermediate-age component. A new look at the chemical evolution of the Small Magellanic Cloud suggests that, unlike the Galaxy, where the rate of enrichment has been steady after the initial phase, the enrichment in the SMC remained small for a long interval before increasing rapidly sometime in the last 1-2x10^9^yr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/298/544#2</TD>
            <TD>2011-09-14T18:23:01Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/298/544</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/298/544&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/298/544</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/469/629 [1]</TD>
            <TD>UV-brightest stars of M33 and its nucleus (Massey+ 1996)</TD>
            <TD>We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti &amp; Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629#1</TD>
            <TD>2011-09-14T18:23:42Z</TD>
            <TD>#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/469/629</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/469/629</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/469/629 [2]</TD>
            <TD>UV-brightest stars of M33 and its nucleus (Massey+ 1996)</TD>
            <TD>We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti &amp; Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629#2</TD>
            <TD>2011-09-14T18:23:42Z</TD>
            <TD>#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/469/629&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/469/629</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/469/629 [table1]</TD>
            <TD>UV-brightest stars of M33 and its nucleus (Massey+ 1996)</TD>
            <TD>We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti &amp; Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629#table1</TD>
            <TD>2011-09-14T18:23:42Z</TD>
            <TD>#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/469/629&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/469/629</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/469/629 [1]</TD>
            <TD>UV-brightest stars of M33 and its nucleus (Massey+ 1996)</TD>
            <TD>We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti &amp; Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629#1</TD>
            <TD>2011-09-14T18:23:42Z</TD>
            <TD>#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/469/629</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/469/629</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/469/629 [2]</TD>
            <TD>UV-brightest stars of M33 and its nucleus (Massey+ 1996)</TD>
            <TD>We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti &amp; Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629#2</TD>
            <TD>2011-09-14T18:23:42Z</TD>
            <TD>#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/469/629&amp;</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/469/629</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/469/629 [table1]</TD>
            <TD>UV-brightest stars of M33 and its nucleus (Massey+ 1996)</TD>
            <TD>We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti &amp; Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629#table1</TD>
            <TD>2011-09-14T18:23:42Z</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/469/629 [1]</TD>
            <TD>UV-brightest stars of M33 and its nucleus (Massey+ 1996)</TD>
            <TD>We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti &amp; Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629#1</TD>
            <TD>2011-09-14T18:23:42Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/469/629</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/469/629</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/469/629 [2]</TD>
            <TD>UV-brightest stars of M33 and its nucleus (Massey+ 1996)</TD>
            <TD>We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti &amp; Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629#2</TD>
            <TD>2011-09-14T18:23:42Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
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            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/469/629</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/469/629 [table1]</TD>
            <TD>UV-brightest stars of M33 and its nucleus (Massey+ 1996)</TD>
            <TD>We investigate the UV-brightest sources in the nearby galaxy M33. Our catalog of 356 sources is constructed from far-ultraviolet (FUV; 1500A) and near-ultraviolet (NUV; 2400A) images obtained with the Ultraviolet Imaging Telescope (UIT) matched with ground-based UBV data. We find that our survey is limited by the FUV flux and is complete to F_1500=2.5x10^-15ergs/cm^2^/s/A, other than in the most crowded regions; this corresponds roughly to Mbol=-9.2 to -10.0 (or masses of 40-60M_{sun}_), for Teff=50,000{deg} to 10,000{deg}. We use Hubble Space Telescope (HST) WFPC2 images of several M33 fields to conclude that at least one-half of our sample is uncontaminated by unresolved neighbors, at least at the 0.1" (0.4pc) level, a resolution similar to that achieved in the LMC from the ground. Spectral types have been obtained for 131 of our objects. We discuss the spatial distribution of the UIT sources, finding that they provide an excellent tracer of the spiral arm pattern and confirm that star formation continues in the nuclear region to the present day. Our survey has found a large number of O and early B-type supergiants, including stars as early as O6, but the optical spectroscopic sample is dominated by later type B supergiants, as these are the visually brighter. Among the brightest stars (both at 1500A and at V) are the "superluminous" Wolf-Rayet stars first discovered by Conti &amp; Massey in the largest H II regions of M33; these objects are now known to be small groups of stars in modest analog to R136 in 30 Dor. In general, our survey has failed to detect the known W-R stars, as they are too faint, but we did find several new late-type WN stars and composite systems, which are brighter. Two stars of high absolute visual magnitude (M_v~-9.0) are found to be B I + WN binaries, similar to HDE 269546 in the LMC; one of these is multiple at HST resolution. Most interesting, perhaps, is our finding six Ofpe/WN9 "slash" stars, five of them newly discovered. These stars show properties intermediate between those of Of and WN stars and are believed to be a quiescent form of luminous blue variables (LBVs). Our spectroscopy found five additional stars that are spectroscopically similar to the known LBVs of M33. One of these stars has recently been shown to be spectroscopically variable, and we suggest that all of these stars deserve continued scrutiny. The nucleus of M33 is the visually brightest object in our survey, and its UV colors are indicative of a hotter component than its optical photometry or spectral type would suggest. We discuss the possibility that the pointlike nucleus may contain a few interesting hot stars that dominate the light in the UV, and we make the comparison to the cluster of He I emission-line stars found near the center of the Milky Way. We comment on which color-magnitude and color-color plots make the best diagnostic tools for studying the hot, massive star population of a galaxy like M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629#table1</TD>
            <TD>2011-09-14T18:23:42Z</TD>
            <TD>#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/469/629</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/469/629&amp;</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/96/117 [1]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#1</TD>
            <TD>2011-09-14T18:24:19Z</TD>
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            <TD>18-Jun-1996</TD>
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            <TD />
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            <TD>WebBrowser</TD>
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            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/96/117 [2]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#2</TD>
            <TD>2011-09-14T18:24:19Z</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/117 [table4]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#table4</TD>
            <TD>2011-09-14T18:24:19Z</TD>
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            <TD>#Research#</TD>
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            <TD>18-Jun-1996</TD>
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            <TD>ConeSearch</TD>
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/117 [table3]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#table3</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/117 [table5]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#table5</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/96/117 [1]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#1</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/96/117</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/96/117 [2]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#2</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/117 [table4]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#table4</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/117 [table3]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#table3</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/117 [table5]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#table5</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/96/117 [1]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#1</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/96/117</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/96/117 [2]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#2</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/117 [table4]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#table4</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/117 [table3]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#table3</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/117 [table5]</TD>
            <TD>K-Band Galaxy Counts (McLeod+ 1995)</TD>
            <TD>We present new counts of field galaxies from more than 20 arcmin^2 to a limiting magnitude of K = 20 and from 2 arcmin^2 to K = 21.5. At the faintest magnitudes, the counts are slightly higher than those reported previously, though still consistent given the small numbers of galaxies in the two samples.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117#table5</TD>
            <TD>2011-09-14T18:24:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/117</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/159 [1]</TD>
            <TD>Catalogue of galaxies towards the Coma Supercluster (Slezak+ 1988)</TD>
            <TD>The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/159#1</TD>
            <TD>2011-09-14T18:38:57Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1993</TD>
            <TD>ivo://CDS.VizieR/VII/159</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/159</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/159</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/159 [2]</TD>
            <TD>Catalogue of galaxies towards the Coma Supercluster (Slezak+ 1988)</TD>
            <TD>The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/159#2</TD>
            <TD>2011-09-14T18:38:57Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1993</TD>
            <TD>ivo://CDS.VizieR/VII/159</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/159&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/159</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/159 [catalog]</TD>
            <TD>Catalogue of galaxies towards the Coma Supercluster (Slezak+ 1988)</TD>
            <TD>The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/159#catalog</TD>
            <TD>2011-09-14T18:38:57Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1993</TD>
            <TD>ivo://CDS.VizieR/VII/159</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/159&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/159</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Twoqz</TD>
            <TD>2dF QSO Redshift Survey (2QZ)</TD>
            <TD>Using the AAT Two-Degree Field (2dF) to obtain redshifts for &gt; 25000 B &lt; 21 QSOs in two 75° × 5° declination strips in the South Galactic Pole and in an equatorial region at the North Galactic cap. The primary scientific aims of the QSO survey are: (1) to obtain the primordial fluctuation power spectrum out to COBE scales, (2) to determine the rate of QSO clustering evolution in the non-linear and linear regimes and hence obtain new limits on the value of and the bias parameter, (3) to apply a powerful geometric method to measure .</TD>
            <TD>JHU</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/twoqz#1</TD>
            <TD>2011-09-14T18:12:02Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#Redshift#QSO#</TD>
            <TD />
            <TD />
            <TD>1</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/twoqz</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/twoqz/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/159 [1]</TD>
            <TD>Catalogue of galaxies towards the Coma Supercluster (Slezak+ 1988)</TD>
            <TD>The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/159#1</TD>
            <TD>2011-09-14T18:38:57Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1993</TD>
            <TD>ivo://CDS.VizieR/VII/159</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/159</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/159</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/159 [2]</TD>
            <TD>Catalogue of galaxies towards the Coma Supercluster (Slezak+ 1988)</TD>
            <TD>The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/159#2</TD>
            <TD>2011-09-14T18:38:57Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1993</TD>
            <TD>ivo://CDS.VizieR/VII/159</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/159&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/159</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/159 [catalog]</TD>
            <TD>Catalogue of galaxies towards the Coma Supercluster (Slezak+ 1988)</TD>
            <TD>The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/159#catalog</TD>
            <TD>2011-09-14T18:38:57Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1993</TD>
            <TD>ivo://CDS.VizieR/VII/159</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/159&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/159</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS-DR4</TD>
            <TD>Sloan Digitized Sky Survey(DR4)</TD>
            <TD>The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey</TD>
            <TD>The Johns Hopkins Univer</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/services/DR4CONE#1</TD>
            <TD>2011-09-14T18:12:09Z</TD>
            <TD>#Stars#Survey#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.100000001490116</TD>
            <TD>DR4</TD>
            <TD>ivo://sdss.jhu/services/DR4CONE</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://casjobs.sdss.org/vo/dr4cone/sdssConeSearch.asmx/ConeSearch?</TD>
            <TD>1</TD>
            <TD>5000</TD>
            <TD />
            <TD>http://www.sdss.jhu.edu/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/159 [1]</TD>
            <TD>Catalogue of galaxies towards the Coma Supercluster (Slezak+ 1988)</TD>
            <TD>The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/159#1</TD>
            <TD>2011-09-14T18:38:57Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1993</TD>
            <TD>ivo://CDS.VizieR/VII/159</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/159</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/159</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/159 [2]</TD>
            <TD>Catalogue of galaxies towards the Coma Supercluster (Slezak+ 1988)</TD>
            <TD>The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/159#2</TD>
            <TD>2011-09-14T18:38:57Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1993</TD>
            <TD>ivo://CDS.VizieR/VII/159</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/159&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/159</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/159 [catalog]</TD>
            <TD>Catalogue of galaxies towards the Coma Supercluster (Slezak+ 1988)</TD>
            <TD>The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region. This paper concerns the study of a IIIaJ Palomar Schmidt plate of the Eastern end of this filament. We have developed a real time reduction technique, quite similar to that used for the COSMOS machine and performed, in real time, an image segmentation. The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area. All the non-stellar objects were thus identified using the PDS and a morphological type was attributed to the galaxies. Our catalogue gives coordinates, magnitudes (derived from the Zwicky et al. (1961-68) and Nilson (1973) catalogues), area in pixels, and morphological types for 7582 galaxies. A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude. The asymmetry in the distribution of the bright objects between the North-West and the South-East part of the plate found by Fontanelli (1984) is also present for the fainter objects of our catalogue. We have identified galaxy condensations using an image segmentation on the galaxy density map. The parameters, position, axis, and orientation of these condensations have been estimated.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/159#catalog</TD>
            <TD>2011-09-14T18:38:57Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1993</TD>
            <TD>ivo://CDS.VizieR/VII/159</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/159&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/159</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSSDR2</TD>
            <TD>Sloan Digital Sky Survey (DR2)</TD>
            <TD>The Sloan Digital Sky Survey is the most ambitious astronomical survey ever undertaken. The survey will map one-quarter of the entire sky in detail, determining the positions and absolute brightnesses of hundreds of millions of celestial objects. It will also measure the distances to more than a million galaxies and quasars. The SDSS addresses fascinating, fundamental questions about the universe. With the survey, astronomers will be able to see the large-scale patterns of galaxies: sheets and voids through the whole universe. Scientists have many ideas about how the universe evolved, and different patterns of large-scale structure point to different theories. The Sloan Digital Sky Survey will tell us which theories are right - or whether we will have to come up with entirely new ideas.</TD>
            <TD>JHU</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/dr2#1</TD>
            <TD>2011-09-14T17:51:44Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD>#Research#</TD>
            <TD>0.800000011920929</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/dr2</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes//SDSSDR2/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/679/404 [1]</TD>
            <TD>Star clusters in M82 (Mayya+, 2008)</TD>
            <TD>The data were obtained by the Hubble Heritage Team using the ACS Wide Field Channel in 2006 March, and released in fits format. Observations consisted of 96 individual exposures in F435W, F555W, F814W, and F658N filters covering a field of view of 8'x8' centered on the galaxy nucleus, and cover the entire optical disk of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/404#1</TD>
            <TD>2011-09-14T21:03:47Z</TD>
            <TD>#Associations#Extinction#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/679/404</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/404</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/679/404 [2]</TD>
            <TD>Star clusters in M82 (Mayya+, 2008)</TD>
            <TD>The data were obtained by the Hubble Heritage Team using the ACS Wide Field Channel in 2006 March, and released in fits format. Observations consisted of 96 individual exposures in F435W, F555W, F814W, and F658N filters covering a field of view of 8'x8' centered on the galaxy nucleus, and cover the entire optical disk of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/404#2</TD>
            <TD>2011-09-14T21:03:47Z</TD>
            <TD>#Associations#Extinction#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/679/404&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/404</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/126/401 [1]</TD>
            <TD>M 31 Cepheids periods (Magnier+ 1997)</TD>
            <TD>Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (&lt;3%). For V&lt;21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401#1</TD>
            <TD>2011-09-14T18:39:43Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/126/401</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/401</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/126/401 [2]</TD>
            <TD>M 31 Cepheids periods (Magnier+ 1997)</TD>
            <TD>Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (&lt;3%). For V&lt;21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401#2</TD>
            <TD>2011-09-14T18:39:43Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/126/401&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/126/401 [table1]</TD>
            <TD>M 31 Cepheids periods (Magnier+ 1997)</TD>
            <TD>Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (&lt;3%). For V&lt;21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401#table1</TD>
            <TD>2011-09-14T18:39:43Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/126/401&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSSDR4</TD>
            <TD>Sloan Digital Sky Survey (DR4)</TD>
            <TD>The Sloan Digital Sky Survey is the most ambitious astronomical survey ever undertaken. The survey will map one-quarter of the entire sky in detail, determining the positions and absolute brightnesses of hundreds of millions of celestial objects. It will also measure the distances to more than a million galaxies and quasars. The SDSS addresses fascinating, fundamental questions about the universe. With the survey, astronomers will be able to see the large-scale patterns of galaxies: sheets and voids through the whole universe. Scientists have many ideas about how the universe evolved, and different patterns of large-scale structure point to different theories. The Sloan Digital Sky Survey will tell us which theories are right - or whether we will have to come up with entirely new ideas.</TD>
            <TD>JHU</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/SDSSDR4#1</TD>
            <TD>2011-09-14T17:51:51Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD>#Research#</TD>
            <TD>0.800000011920929</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/SDSSDR4</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes//SDSSDR4/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/679/404 [1]</TD>
            <TD>Star clusters in M82 (Mayya+, 2008)</TD>
            <TD>The data were obtained by the Hubble Heritage Team using the ACS Wide Field Channel in 2006 March, and released in fits format. Observations consisted of 96 individual exposures in F435W, F555W, F814W, and F658N filters covering a field of view of 8'x8' centered on the galaxy nucleus, and cover the entire optical disk of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/404#1</TD>
            <TD>2011-09-14T21:03:47Z</TD>
            <TD>#Associations#Extinction#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/679/404</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/404</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/679/404 [2]</TD>
            <TD>Star clusters in M82 (Mayya+, 2008)</TD>
            <TD>The data were obtained by the Hubble Heritage Team using the ACS Wide Field Channel in 2006 March, and released in fits format. Observations consisted of 96 individual exposures in F435W, F555W, F814W, and F658N filters covering a field of view of 8'x8' centered on the galaxy nucleus, and cover the entire optical disk of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/404#2</TD>
            <TD>2011-09-14T21:03:47Z</TD>
            <TD>#Associations#Extinction#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/679/404&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/404</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/126/401 [1]</TD>
            <TD>M 31 Cepheids periods (Magnier+ 1997)</TD>
            <TD>Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (&lt;3%). For V&lt;21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401#1</TD>
            <TD>2011-09-14T18:39:43Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/126/401</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/401</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/126/401 [2]</TD>
            <TD>M 31 Cepheids periods (Magnier+ 1997)</TD>
            <TD>Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (&lt;3%). For V&lt;21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401#2</TD>
            <TD>2011-09-14T18:39:43Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/126/401&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/126/401 [table1]</TD>
            <TD>M 31 Cepheids periods (Magnier+ 1997)</TD>
            <TD>Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (&lt;3%). For V&lt;21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401#table1</TD>
            <TD>2011-09-14T18:39:43Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/126/401&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVDS_F02_DEEP</TD>
            <TD>VVDS-F02 DEEP catalog</TD>
            <TD>This Cone Search service allows to query on the VVDS-F02-DEEP catalog available at http://cencosw.oamp.fr. It comprises data for 8980 objects from the VVDS-F02 Deep field with IAB between 17.5 and 24, and with spectroscopic redshift between 0 and 5. The observations, data processing and redshift measurements have been conducted by the French-Italian team of the VIMOS VLT Deep Survey (VVDS).</TD>
            <TD>INAF-IASF Milano</TD>
            <TD>#Optical#</TD>
            <TD>ivo://obelix.lambrate.inaf.it/vodb/cone/VVDS_F02_DEEP#1</TD>
            <TD>2011-09-14T17:51:57Z</TD>
            <TD>#Galaxy#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1.0</TD>
            <TD>ivo://obelix.lambrate.inaf.it/vodb/cone/VVDS_F02_DEEP</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://obelix.lambrate.inaf.it/vodb/ConeSearch?CAT=VVDS_F02_DEEP&amp;</TD>
            <TD>0</TD>
            <TD>8980</TD>
            <TD />
            <TD>http://cencosw.oamp.fr</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/126/401 [1]</TD>
            <TD>M 31 Cepheids periods (Magnier+ 1997)</TD>
            <TD>Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (&lt;3%). For V&lt;21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401#1</TD>
            <TD>2011-09-14T18:39:43Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/126/401</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/401</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/126/401 [2]</TD>
            <TD>M 31 Cepheids periods (Magnier+ 1997)</TD>
            <TD>Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (&lt;3%). For V&lt;21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401#2</TD>
            <TD>2011-09-14T18:39:43Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/126/401&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/126/401 [table1]</TD>
            <TD>M 31 Cepheids periods (Magnier+ 1997)</TD>
            <TD>Cepheid variables can be used for more than just a distance indicator. Since the age can be determined from the period, they can be used to trace the star formation history of a galaxy. We have identified 130 new Cepheid variable candidates in M 31, particularly along the spiral arm regions in the north-east of the galaxy. These areas had not been searched for Cepheids in the previous study by Baade and collaborators. The contamination of our sample by other types of variables is low (&lt;3%). For V&lt;21, the completeness is =~53%. These Cepheids will be used to explore the star formation history in M 31.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401#table1</TD>
            <TD>2011-09-14T18:39:43Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/401</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/126/401&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS-DR3</TD>
            <TD>Sloan Digital Sky Survey (DR3)</TD>
            <TD>The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey</TD>
            <TD>The Johns Hopkins Univer</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/services/DR3CONE#1</TD>
            <TD>2011-09-14T18:12:21Z</TD>
            <TD>#Stars#Survey#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>DR3</TD>
            <TD>ivo://sdss.jhu/services/DR3CONE</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://casjobs.sdss.org/vo/dr3cone/sdssConeSearch.asmx/ConeSearch?</TD>
            <TD>1</TD>
            <TD>5000</TD>
            <TD />
            <TD>http://www.sdss.jhu.edu/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/289/263 [1]</TD>
            <TD>Galaxy clusters from the APM galaxy survey (Dalton+ 1997)</TD>
            <TD>We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263#1</TD>
            <TD>2011-09-14T18:40:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/289/263</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/289/263 [2]</TD>
            <TD>Galaxy clusters from the APM galaxy survey (Dalton+ 1997)</TD>
            <TD>We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263#2</TD>
            <TD>2011-09-14T18:40:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/289/263&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/289/263 [catalog]</TD>
            <TD>Galaxy clusters from the APM galaxy survey (Dalton+ 1997)</TD>
            <TD>We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263#catalog</TD>
            <TD>2011-09-14T18:40:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/289/263&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/263</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/180 [1]</TD>
            <TD>uvby-beta photometry of metal-poor stars (Schuster+ 1989)</TD>
            <TD>Using the calibrations derived by Schuster and Nissen (=1989A&amp;A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&amp;AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] &lt;= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) &gt; 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/180#1</TD>
            <TD>2011-09-14T18:13:24Z</TD>
            <TD>#Stars#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/II/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/180</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/180</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/180 [2]</TD>
            <TD>uvby-beta photometry of metal-poor stars (Schuster+ 1989)</TD>
            <TD>Using the calibrations derived by Schuster and Nissen (=1989A&amp;A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&amp;AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] &lt;= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) &gt; 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/180#2</TD>
            <TD>2011-09-14T18:13:24Z</TD>
            <TD>#Stars#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/II/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/180&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/180 [table1]</TD>
            <TD>uvby-beta photometry of metal-poor stars (Schuster+ 1989)</TD>
            <TD>Using the calibrations derived by Schuster and Nissen (=1989A&amp;A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&amp;AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] &lt;= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) &gt; 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/180#table1</TD>
            <TD>2011-09-14T18:13:24Z</TD>
            <TD>#Stars#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/II/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/180</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/289/263 [1]</TD>
            <TD>Galaxy clusters from the APM galaxy survey (Dalton+ 1997)</TD>
            <TD>We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263#1</TD>
            <TD>2011-09-14T18:40:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/289/263</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/289/263 [2]</TD>
            <TD>Galaxy clusters from the APM galaxy survey (Dalton+ 1997)</TD>
            <TD>We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263#2</TD>
            <TD>2011-09-14T18:40:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/289/263&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/289/263 [catalog]</TD>
            <TD>Galaxy clusters from the APM galaxy survey (Dalton+ 1997)</TD>
            <TD>We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263#catalog</TD>
            <TD>2011-09-14T18:40:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/289/263&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/263</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/180 [1]</TD>
            <TD>uvby-beta photometry of metal-poor stars (Schuster+ 1989)</TD>
            <TD>Using the calibrations derived by Schuster and Nissen (=1989A&amp;A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&amp;AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] &lt;= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) &gt; 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/180#1</TD>
            <TD>2011-09-14T18:13:24Z</TD>
            <TD>#Stars#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/II/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/180</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/180</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/180 [2]</TD>
            <TD>uvby-beta photometry of metal-poor stars (Schuster+ 1989)</TD>
            <TD>Using the calibrations derived by Schuster and Nissen (=1989A&amp;A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&amp;AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] &lt;= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) &gt; 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/180#2</TD>
            <TD>2011-09-14T18:13:24Z</TD>
            <TD>#Stars#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/II/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/180&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/180 [table1]</TD>
            <TD>uvby-beta photometry of metal-poor stars (Schuster+ 1989)</TD>
            <TD>Using the calibrations derived by Schuster and Nissen (=1989A&amp;A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&amp;AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] &lt;= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) &gt; 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/180#table1</TD>
            <TD>2011-09-14T18:13:24Z</TD>
            <TD>#Stars#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/II/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/180</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/289/263 [1]</TD>
            <TD>Galaxy clusters from the APM galaxy survey (Dalton+ 1997)</TD>
            <TD>We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263#1</TD>
            <TD>2011-09-14T18:40:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/289/263</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/289/263 [2]</TD>
            <TD>Galaxy clusters from the APM galaxy survey (Dalton+ 1997)</TD>
            <TD>We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263#2</TD>
            <TD>2011-09-14T18:40:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/289/263&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/289/263 [catalog]</TD>
            <TD>Galaxy clusters from the APM galaxy survey (Dalton+ 1997)</TD>
            <TD>We describe the construction of catalogues of galaxy clusters from the APM Galaxy survey using an automated algorithm based on Abell-like selection criteria. We investigate the effects of varying several parameters in our selection algorithm, including the magnitude range and radius from the cluster centre used to estimate the cluster richnesses. We quantify the accuracy of the photometric distance estimates by comparing them with measured redshifts, and we investigate the stability and completeness of the resulting catalogues. We find that the angular correlation functions for different cluster catalogues are in good agreement with one another, and are also consistent with the observed amplitude of the spatial correlation function of rich clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263#catalog</TD>
            <TD>2011-09-14T18:40:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/263</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/289/263&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/263</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>GalexFar [1]</TD>
            <TD>Galaxy Explorer All Sky Survey: Far UV</TD>
            <TD>The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682. &lt;p&gt; The &lt;i&gt;SkyView&lt;/i&gt; GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image. &lt;p&gt; As of February 10, 2011 SkyView uses the GR6 data release for the entire sky.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/skyview/galexfar#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/galexfar</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=galexfar&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GalexFar [2]</TD>
            <TD>Galaxy Explorer All Sky Survey: Far UV</TD>
            <TD>The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682. &lt;p&gt; The &lt;i&gt;SkyView&lt;/i&gt; GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image. &lt;p&gt; As of February 10, 2011 SkyView uses the GR6 data release for the entire sky.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/skyview/galexfar#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/galexfar</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/128/459 [1]</TD>
            <TD>BV photometry of irregular galaxies (Makarova+ 1998)</TD>
            <TD>The tables shows the photometry and colour index for the observed galaxy, with the image parameter SHAR. This parameter is a measure of the difference between the observed width of the object and the psf model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/459#1</TD>
            <TD>2011-09-14T18:42:18Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/459</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/128/459</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/459</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/128/459 [2]</TD>
            <TD>BV photometry of irregular galaxies (Makarova+ 1998)</TD>
            <TD>The tables shows the photometry and colour index for the observed galaxy, with the image parameter SHAR. This parameter is a measure of the difference between the observed width of the object and the psf model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/459#2</TD>
            <TD>2011-09-14T18:42:18Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/459</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/128/459&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/459</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/128/459 [1]</TD>
            <TD>BV photometry of irregular galaxies (Makarova+ 1998)</TD>
            <TD>The tables shows the photometry and colour index for the observed galaxy, with the image parameter SHAR. This parameter is a measure of the difference between the observed width of the object and the psf model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/459#1</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/459</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/128/459</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/459</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/128/459 [2]</TD>
            <TD>BV photometry of irregular galaxies (Makarova+ 1998)</TD>
            <TD>The tables shows the photometry and colour index for the observed galaxy, with the image parameter SHAR. This parameter is a measure of the difference between the observed width of the object and the psf model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/459#2</TD>
            <TD>2011-09-14T18:42:18Z</TD>
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            <TD>28-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/459</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/128/459&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/459</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/118/557 [1]</TD>
            <TD>Near-IR photometry of 86 galaxies. II. (de Jong 1996)</TD>
            <TD>In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong &amp; van der Kruit (1994), which comprises 86 galaxies in six passbands.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557#1</TD>
            <TD>2011-09-14T18:42:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/118/557</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/557</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/118/557 [2]</TD>
            <TD>Near-IR photometry of 86 galaxies. II. (de Jong 1996)</TD>
            <TD>In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong &amp; van der Kruit (1994), which comprises 86 galaxies in six passbands.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557#2</TD>
            <TD>2011-09-14T18:42:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/118/557&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/557</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/557 [galaxies]</TD>
            <TD>Near-IR photometry of 86 galaxies. II. (de Jong 1996)</TD>
            <TD>In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong &amp; van der Kruit (1994), which comprises 86 galaxies in six passbands.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557#galaxies</TD>
            <TD>2011-09-14T18:42:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/557&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/557</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/118/557 [1]</TD>
            <TD>Near-IR photometry of 86 galaxies. II. (de Jong 1996)</TD>
            <TD>In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong &amp; van der Kruit (1994), which comprises 86 galaxies in six passbands.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557#1</TD>
            <TD>2011-09-14T18:42:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/118/557</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/557</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/118/557 [2]</TD>
            <TD>Near-IR photometry of 86 galaxies. II. (de Jong 1996)</TD>
            <TD>In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong &amp; van der Kruit (1994), which comprises 86 galaxies in six passbands.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557#2</TD>
            <TD>2011-09-14T18:42:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/118/557&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/557</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/557 [galaxies]</TD>
            <TD>Near-IR photometry of 86 galaxies. II. (de Jong 1996)</TD>
            <TD>In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong &amp; van der Kruit (1994), which comprises 86 galaxies in six passbands.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557#galaxies</TD>
            <TD>2011-09-14T18:42:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/557&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/557</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/118/557 [1]</TD>
            <TD>Near-IR photometry of 86 galaxies. II. (de Jong 1996)</TD>
            <TD>In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong &amp; van der Kruit (1994), which comprises 86 galaxies in six passbands.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557#1</TD>
            <TD>2011-09-14T18:42:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/118/557</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/557</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/118/557 [2]</TD>
            <TD>Near-IR photometry of 86 galaxies. II. (de Jong 1996)</TD>
            <TD>In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong &amp; van der Kruit (1994), which comprises 86 galaxies in six passbands.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557#2</TD>
            <TD>2011-09-14T18:42:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/118/557&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/557</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/557 [galaxies]</TD>
            <TD>Near-IR photometry of 86 galaxies. II. (de Jong 1996)</TD>
            <TD>In this Paper I present a new two-dimensional decomposition technique, which models the surface photometry of a galaxy with an exponential light profile for both bulge and disk and, when necessary, with a Freeman bar. The new technique w as tested for systematic errors on both artificial and real data and compared with widely used one-dimensional decomposition techniques, where the luminosity profile of the galaxy is used. The comparisons indicate that a decomposition of the two-dimensional image of the galaxy with an exponential light profile for both bulge and disk yields the most reproducible and representative bulge and disk parameters. An extensive error analysis was made to determine the reliability of the model parameters. If the model with an exponential bulge profile is a reasonable description of a galaxy, the maximum errors in the derived model parameters are of order 20%. The uncertainties in the model parameters will increase, if the exponential bulge function is replaced by other often used bulge functions as the de Vaucouleurs law. All decomposition methods were applied to the optical and near-infrared data set presented by de Jong &amp; van der Kruit (1994), which comprises 86 galaxies in six passbands.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557#galaxies</TD>
            <TD>2011-09-14T18:42:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/557</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/557&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/557</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/208 [1]</TD>
            <TD>Faint Galaxies at the North Galactic Pole (Infante+ 1995)</TD>
            <TD>The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&amp;A...282..353), Infante (1994A&amp;AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/208#1</TD>
            <TD>2011-09-14T18:42:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/208</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/208</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/208</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/208 [2]</TD>
            <TD>Faint Galaxies at the North Galactic Pole (Infante+ 1995)</TD>
            <TD>The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&amp;A...282..353), Infante (1994A&amp;AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/208#2</TD>
            <TD>2011-09-14T18:42:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/208</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/208&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/208</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/208 [faintgal]</TD>
            <TD>Faint Galaxies at the North Galactic Pole (Infante+ 1995)</TD>
            <TD>The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&amp;A...282..353), Infante (1994A&amp;AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/208&amp;</TD>
            <TD>180</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>VII/208 [1]</TD>
            <TD>Faint Galaxies at the North Galactic Pole (Infante+ 1995)</TD>
            <TD>The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&amp;A...282..353), Infante (1994A&amp;AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)</TD>
            <TD>CDS</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/208</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/208</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/208 [2]</TD>
            <TD>Faint Galaxies at the North Galactic Pole (Infante+ 1995)</TD>
            <TD>The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&amp;A...282..353), Infante (1994A&amp;AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)</TD>
            <TD>CDS</TD>
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            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/208&amp;</TD>
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            <TD>Catalog</TD>
            <TD>VII/208 [faintgal]</TD>
            <TD>Faint Galaxies at the North Galactic Pole (Infante+ 1995)</TD>
            <TD>The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&amp;A...282..353), Infante (1994A&amp;AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)</TD>
            <TD>CDS</TD>
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            <TD>16-Apr-1998</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>VII/208 [1]</TD>
            <TD>Faint Galaxies at the North Galactic Pole (Infante+ 1995)</TD>
            <TD>The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&amp;A...282..353), Infante (1994A&amp;AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)</TD>
            <TD>CDS</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/208</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/208 [2]</TD>
            <TD>Faint Galaxies at the North Galactic Pole (Infante+ 1995)</TD>
            <TD>The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&amp;A...282..353), Infante (1994A&amp;AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/VII/208</TD>
            <TD />
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            <TD>Catalog</TD>
            <TD>VII/208 [faintgal]</TD>
            <TD>Faint Galaxies at the North Galactic Pole (Infante+ 1995)</TD>
            <TD>The North Galactic Pole Canada-France-Hawaii Telescope Catalogue of faint galaxies is made available. We provide positions, photometric and structural parameters for more than 50000 galaxies. The J and F magnitudes were obtained from IIIaJ and IIIaF CFHT prime focus plates respectively. This catalogue have been used in many studies of faint galaxy properties. Galaxy counts, colour distributions and clustering properties of faint galaxies have been obtained with these data. Statistical properties of stars have been studied as well. For details refer to Infante and Pritchet (1992ApJS...83..237I), Pritchet and Infante (1992ApJ...399L..35P), Infante (1994A&amp;A...282..353), Infante (1994A&amp;AS..107..413I) and Infante and Pritchet (1995ApJ...439..565I). The magnitude errors range from: +/-0.3mag at J=24 to less than +/-0.1 at J=20 +/-0.3mag at F=23 to less than +/-0.1 at F=19 The rms uncertainty in the zero points is 0.022 (J) and 0.038 (F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>180</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>VII/100 [1]</TD>
            <TD>MCG Vol.5 (Vorontsov-Velyaminov+, 1974)</TD>
            <TD>The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/VII/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/100 [2]</TD>
            <TD>MCG Vol.5 (Vorontsov-Velyaminov+, 1974)</TD>
            <TD>The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/100#2</TD>
            <TD>2011-09-14T18:43:26Z</TD>
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            <TD>17-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/VII/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/100&amp;</TD>
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            <TD>ivo://CDS</TD>
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          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/100 [catalog]</TD>
            <TD>MCG Vol.5 (Vorontsov-Velyaminov+, 1974)</TD>
            <TD>The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.</TD>
            <TD>CDS</TD>
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            <TD>2011-09-14T18:43:26Z</TD>
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            <TD>17-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/VII/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/100&amp;</TD>
            <TD>180</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/100</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>VII/100 [1]</TD>
            <TD>MCG Vol.5 (Vorontsov-Velyaminov+, 1974)</TD>
            <TD>The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/100#1</TD>
            <TD>2011-09-14T18:43:26Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>17-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/VII/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/100 [2]</TD>
            <TD>MCG Vol.5 (Vorontsov-Velyaminov+, 1974)</TD>
            <TD>The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/100#2</TD>
            <TD>2011-09-14T18:43:26Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>17-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/VII/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/100 [catalog]</TD>
            <TD>MCG Vol.5 (Vorontsov-Velyaminov+, 1974)</TD>
            <TD>The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/100#catalog</TD>
            <TD>2011-09-14T18:43:26Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/VII/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/100</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>GalexFar [1]</TD>
            <TD>Galaxy Explorer All Sky Survey: Far UV</TD>
            <TD>The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682. &lt;p&gt; The &lt;i&gt;SkyView&lt;/i&gt; GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image. &lt;p&gt; As of February 10, 2011 SkyView uses the GR6 data release for the entire sky.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/skyview/galexfar#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/galexfar</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=galexfar&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GalexFar [2]</TD>
            <TD>Galaxy Explorer All Sky Survey: Far UV</TD>
            <TD>The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682. &lt;p&gt; The &lt;i&gt;SkyView&lt;/i&gt; GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image. &lt;p&gt; As of February 10, 2011 SkyView uses the GR6 data release for the entire sky.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/skyview/galexfar#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/galexfar</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/100 [1]</TD>
            <TD>MCG Vol.5 (Vorontsov-Velyaminov+, 1974)</TD>
            <TD>The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/100#1</TD>
            <TD>2011-09-14T18:43:26Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/VII/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/100 [2]</TD>
            <TD>MCG Vol.5 (Vorontsov-Velyaminov+, 1974)</TD>
            <TD>The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/100#2</TD>
            <TD>2011-09-14T18:43:26Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/VII/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/100 [catalog]</TD>
            <TD>MCG Vol.5 (Vorontsov-Velyaminov+, 1974)</TD>
            <TD>The Morphological Catalogue of Galaxies, Volume 5 (Vorontsov-Velyaminov et al. 1974) includes 1637 galaxies, probably no fainter than the fourteenth magnitude. The catalog was based on Palomar Sky Atlas prints and comprises areas from -30 to -45 degrees in declination. In contrast to the earlier four volumes of the catalog, the fifth was based on the red prints of the Sky Survey only. Visual magnitude estimates are thus in the red. Note that in all cases when in other sources the photoelectric B or photographic magnitude of galaxies are encountered, preference to those values has been given over those of Vorontsov-Velyaminov's estimates. All notes to galaxies published in the earlier volume are included here as well (Kogoshvili 1983). In addition, the following data were used from the ESO/Uppsala survey (Lauberts 1982): magnitudes, colors, radial velocities, Hubble types, and galaxy diameters as measured on the ESO(B) atlas plates up to the surface brightness slightly fainter than 25 magnitudes per square arcsec. These maximum major and minor galaxy diameters are provided in the fifth volume in place of the values taken from the UGC catalog in the earlier four volumes. Various data from both the reference Catalog of Bright Galaxies (de Vaucouleurs et al. 1964) and B-V and U-B colors from the General Catalogue of Photoelectric Magnitudes and Colours (Longo et al. 1983) were included. Fields included in the catalog are identification number; zone sign, number, and field number; galaxy number in the field; component or symbolic designation; NGC or IC identification; B1950.0 position, magnitude, magnitude accuracy, and magnitude reference; angular diameters, surface brightness, symbolic description galaxy, morphological type, galaxy type, heliocentric radial velocity; radial velocity corrected for solar motion; rotational velocity, dates of first two supernovae, number of supernovae, number of H II regions, U-B and B-V colors and references, radio flux densities at 178, 780, 1400, 2700, and 5000 MHz; number of nearby cluster; and coded information on membership of the galaxy to double or multiple systems, interaction features, and faint components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/100#catalog</TD>
            <TD>2011-09-14T18:43:26Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/VII/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/100</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/367 [1]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#1</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/367</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/367 [2]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#2</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/367&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/367 [sumcat]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#sumcat</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/367 [catalog]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#catalog</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/367 [1]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#1</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/367</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/367 [2]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#2</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/367&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/367 [sumcat]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#sumcat</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/367 [catalog]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#catalog</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/367 [1]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#1</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/367</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/367 [2]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#2</TD>
            <TD>2011-09-14T18:43:37Z</TD>
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            <TD>#Catalog#</TD>
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            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/367&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/367 [sumcat]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#sumcat</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/367 [catalog]</TD>
            <TD>Virgo Photometry Catalogue (VPC) (Young+ 1998)</TD>
            <TD>The Virgo Photometry Catalogue (VPC) contains independently calibrated surface photometry in the U, B_J_ and R_C_ bands for over 1000 galaxies (including background objects) brighter than B_J25_=19.0 in a 23{deg}^2^ area of the sky centred on R.A., Dec.(1950)= 12h26m, +13{deg}08'. The angular resolution of the photometry varies from band to band and was in each case determined from the FWHM of stellar profiles: 4.75+/-0.1arcsec in the U band, 5.0+/-0.1arcsec in the B_J_ band and 6.0+/-0.1arcsec in the R_C_ band. The photometry was intended for the derivation of accurate magnitudes and colours and is therefore not of high resolution. Stellar contamination of the galaxy sample is minimal, and cannot exceed about 3 faint-end objects in total (i.e. it is less than about 0.25%). Parameters listed for catalogued galaxies include: equatorial coordinates; morphological types; surface-brightness profile parameters (which preserve the majority of the surface photometry information); U, B_J_ and R_C_ isophotal magnitudes; U, B_J_, R_C_ and [transformed] B total magnitudes; (U-B_J_) and (B_J_-R_C_) equal-area colours, apparent angular radii, ellipticities, position angles, heliocentric radial velocities and alternative designations. All total magnitudes and total colours are extrapolated according to the "t" system of Young et al. (1998A&amp;AS..130..173Y). The VPC is based primarily on four UK-Schmidt plates, all of which were scanned using the COSMOS measuring machine at the Royal Observatory Edinburgh. All magnitudes, colours and surface-brightness parameters are derived from numerical integrations of segmented plate-scan data; except for (in 109 cases) saturated and (in 51 cases) inextricably merged images. The latter 51 images are listed in Table 14 (Appendix D) of the original paper, whilst data for the remaining 1129 objects [i.e. including ones for which the VPC photometry is saturated in one or more bands] are listed in the main catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367#catalog</TD>
            <TD>2011-09-14T18:43:37Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:surface#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/367</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/577 [1]</TD>
            <TD>AO 0235+164 BVRI photometry (Takalo+ 1998)</TD>
            <TD>We present the results of the optical and radio monitoring of the BL Lac object AO 0235+164 during a faint state. In both optical and radio bands the source has been observed at the faintest ever recorded levels, reaching V=19.80 and F_22GHz_=0.34Jy. In the optical bands we still see variability with amplitudes up to 1.5 magnitudes on timescales from days to weeks. The radio variability is less dramatic, but in general follows the optical behaviour. A correlation between general trends in the optical and radio behaviour of AO 0235+164 may be recognized in the data from the present monitoring as well as in the historical light curves, suggesting a `base' mechanism responsible for the emission at both frequencies. A good candidate is a synchrotron process in the relativistic jet. Optical flares with no corresponding radio counterparts have been observed too. These events may be interpreted in terms of microlensing by a foreground galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/577#1</TD>
            <TD>2011-09-14T18:43:49Z</TD>
            <TD>#BL_Lac_objects#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/577</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/577</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/577 [2]</TD>
            <TD>AO 0235+164 BVRI photometry (Takalo+ 1998)</TD>
            <TD>We present the results of the optical and radio monitoring of the BL Lac object AO 0235+164 during a faint state. In both optical and radio bands the source has been observed at the faintest ever recorded levels, reaching V=19.80 and F_22GHz_=0.34Jy. In the optical bands we still see variability with amplitudes up to 1.5 magnitudes on timescales from days to weeks. The radio variability is less dramatic, but in general follows the optical behaviour. A correlation between general trends in the optical and radio behaviour of AO 0235+164 may be recognized in the data from the present monitoring as well as in the historical light curves, suggesting a `base' mechanism responsible for the emission at both frequencies. A good candidate is a synchrotron process in the relativistic jet. Optical flares with no corresponding radio counterparts have been observed too. These events may be interpreted in terms of microlensing by a foreground galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/577#2</TD>
            <TD>2011-09-14T18:43:49Z</TD>
            <TD>#BL_Lac_objects#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/577&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/577</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/577 [1]</TD>
            <TD>AO 0235+164 BVRI photometry (Takalo+ 1998)</TD>
            <TD>We present the results of the optical and radio monitoring of the BL Lac object AO 0235+164 during a faint state. In both optical and radio bands the source has been observed at the faintest ever recorded levels, reaching V=19.80 and F_22GHz_=0.34Jy. In the optical bands we still see variability with amplitudes up to 1.5 magnitudes on timescales from days to weeks. The radio variability is less dramatic, but in general follows the optical behaviour. A correlation between general trends in the optical and radio behaviour of AO 0235+164 may be recognized in the data from the present monitoring as well as in the historical light curves, suggesting a `base' mechanism responsible for the emission at both frequencies. A good candidate is a synchrotron process in the relativistic jet. Optical flares with no corresponding radio counterparts have been observed too. These events may be interpreted in terms of microlensing by a foreground galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/577#1</TD>
            <TD>2011-09-14T18:43:49Z</TD>
            <TD>#BL_Lac_objects#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/577</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/577</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/577 [2]</TD>
            <TD>AO 0235+164 BVRI photometry (Takalo+ 1998)</TD>
            <TD>We present the results of the optical and radio monitoring of the BL Lac object AO 0235+164 during a faint state. In both optical and radio bands the source has been observed at the faintest ever recorded levels, reaching V=19.80 and F_22GHz_=0.34Jy. In the optical bands we still see variability with amplitudes up to 1.5 magnitudes on timescales from days to weeks. The radio variability is less dramatic, but in general follows the optical behaviour. A correlation between general trends in the optical and radio behaviour of AO 0235+164 may be recognized in the data from the present monitoring as well as in the historical light curves, suggesting a `base' mechanism responsible for the emission at both frequencies. A good candidate is a synchrotron process in the relativistic jet. Optical flares with no corresponding radio counterparts have been observed too. These events may be interpreted in terms of microlensing by a foreground galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/577#2</TD>
            <TD>2011-09-14T18:43:49Z</TD>
            <TD>#BL_Lac_objects#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/577&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/577</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/335/823 [1]</TD>
            <TD>Evolution models of elliptical galaxies. III. (Tantalo+ 1998)</TD>
            <TD>In this study we present a simple model of elliptical galaxies aimed at interpreting the gradients in colours and narrow band indices observed across these systems. Salient features of the model are the gradients in mass density and star formation and infall of primordial gas aimed at simulating the collapse of a galaxy into the potential well of dark matter. Adopting a multi-zone model we follow in detail the history of star formation, gas consumption, and chemical enrichment of the galaxy and also allow for the occurrence of galactic winds according to the classical supernova (and stellar winds) energy deposit. The outline of the model, the time scale of gas accretion and rate of star formation as a function of the galacto-centric distance in particular, seek to closely mimic the results from Tree-SPH dynamical models. Although some specific ingredients of the model can be questioned from many points of view (of which we are well aware), the model has to be considered as a gross tool for exploring the consequences of different recipes of gas accretion and star formation in which the simple one-zone scheme is abandoned. With the aid of this model we discuss the observational data on the gradients in metallicity, colours, and narrow band indices across elliptical galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/823#1</TD>
            <TD>2011-09-14T18:44:20Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/335/823</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/823</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/335/823 [2]</TD>
            <TD>Evolution models of elliptical galaxies. III. (Tantalo+ 1998)</TD>
            <TD>In this study we present a simple model of elliptical galaxies aimed at interpreting the gradients in colours and narrow band indices observed across these systems. Salient features of the model are the gradients in mass density and star formation and infall of primordial gas aimed at simulating the collapse of a galaxy into the potential well of dark matter. Adopting a multi-zone model we follow in detail the history of star formation, gas consumption, and chemical enrichment of the galaxy and also allow for the occurrence of galactic winds according to the classical supernova (and stellar winds) energy deposit. The outline of the model, the time scale of gas accretion and rate of star formation as a function of the galacto-centric distance in particular, seek to closely mimic the results from Tree-SPH dynamical models. Although some specific ingredients of the model can be questioned from many points of view (of which we are well aware), the model has to be considered as a gross tool for exploring the consequences of different recipes of gas accretion and star formation in which the simple one-zone scheme is abandoned. With the aid of this model we discuss the observational data on the gradients in metallicity, colours, and narrow band indices across elliptical galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/823#2</TD>
            <TD>2011-09-14T18:44:20Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/335/823&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/823</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/335/823 [1]</TD>
            <TD>Evolution models of elliptical galaxies. III. (Tantalo+ 1998)</TD>
            <TD>In this study we present a simple model of elliptical galaxies aimed at interpreting the gradients in colours and narrow band indices observed across these systems. Salient features of the model are the gradients in mass density and star formation and infall of primordial gas aimed at simulating the collapse of a galaxy into the potential well of dark matter. Adopting a multi-zone model we follow in detail the history of star formation, gas consumption, and chemical enrichment of the galaxy and also allow for the occurrence of galactic winds according to the classical supernova (and stellar winds) energy deposit. The outline of the model, the time scale of gas accretion and rate of star formation as a function of the galacto-centric distance in particular, seek to closely mimic the results from Tree-SPH dynamical models. Although some specific ingredients of the model can be questioned from many points of view (of which we are well aware), the model has to be considered as a gross tool for exploring the consequences of different recipes of gas accretion and star formation in which the simple one-zone scheme is abandoned. With the aid of this model we discuss the observational data on the gradients in metallicity, colours, and narrow band indices across elliptical galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/823#1</TD>
            <TD>2011-09-14T18:44:20Z</TD>
            <TD>#Galaxies#Models#</TD>
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            <TD>#Research#</TD>
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            <TD>26-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/335/823</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/823</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/335/823 [2]</TD>
            <TD>Evolution models of elliptical galaxies. III. (Tantalo+ 1998)</TD>
            <TD>In this study we present a simple model of elliptical galaxies aimed at interpreting the gradients in colours and narrow band indices observed across these systems. Salient features of the model are the gradients in mass density and star formation and infall of primordial gas aimed at simulating the collapse of a galaxy into the potential well of dark matter. Adopting a multi-zone model we follow in detail the history of star formation, gas consumption, and chemical enrichment of the galaxy and also allow for the occurrence of galactic winds according to the classical supernova (and stellar winds) energy deposit. The outline of the model, the time scale of gas accretion and rate of star formation as a function of the galacto-centric distance in particular, seek to closely mimic the results from Tree-SPH dynamical models. Although some specific ingredients of the model can be questioned from many points of view (of which we are well aware), the model has to be considered as a gross tool for exploring the consequences of different recipes of gas accretion and star formation in which the simple one-zone scheme is abandoned. With the aid of this model we discuss the observational data on the gradients in metallicity, colours, and narrow band indices across elliptical galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/823#2</TD>
            <TD>2011-09-14T18:44:20Z</TD>
            <TD>#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/823</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/335/823&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/823</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/101/475 [1]</TD>
            <TD>Spectroscopic observations of A3571 (Quintana+, 1993)</TD>
            <TD>Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475#1</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/101/475</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/101/475</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/101/475 [2]</TD>
            <TD>Spectroscopic observations of A3571 (Quintana+, 1993)</TD>
            <TD>Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475#2</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/101/475&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/101/475</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/101/475 [table1]</TD>
            <TD>Spectroscopic observations of A3571 (Quintana+, 1993)</TD>
            <TD>Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475#table1</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/101/475&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/101/475</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/101/475 [1]</TD>
            <TD>Spectroscopic observations of A3571 (Quintana+, 1993)</TD>
            <TD>Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475#1</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/101/475</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/101/475</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/101/475 [2]</TD>
            <TD>Spectroscopic observations of A3571 (Quintana+, 1993)</TD>
            <TD>Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475#2</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/101/475&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/101/475</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/101/475 [table1]</TD>
            <TD>Spectroscopic observations of A3571 (Quintana+, 1993)</TD>
            <TD>Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475#table1</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/101/475&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/101/475</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/101/475 [1]</TD>
            <TD>Spectroscopic observations of A3571 (Quintana+, 1993)</TD>
            <TD>Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475#1</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/101/475</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/101/475</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/101/475 [2]</TD>
            <TD>Spectroscopic observations of A3571 (Quintana+, 1993)</TD>
            <TD>Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475#2</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/101/475&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/101/475</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/101/475 [table1]</TD>
            <TD>Spectroscopic observations of A3571 (Quintana+, 1993)</TD>
            <TD>Spectroscopic data and density counts are presented for this southern cluster, which seems to belong to the outskirts of the Shapley 8 concentration (= A 3558 = SC 1326-311). Using telescopes at the Cerro Tololo Interamerican Observatory and La Silla Observatory a total of 72 galaxy velocities were measured giving a mean redshift of 0.0384 and a global velocity dispersion of 1022 (+99, -77) km/s. A preliminary analysis of velocity and density data suggests the presence of various subgroups. The central core of the cluster is dominated by a very elongated, distorded and diffuse cD galaxy. This cluster may be an example where the cD was formed early in the collapse process of a cluster which has not reached overall virialization yet. The derived X-ray luminosity of ~2x10^44^erg/s in the 2-6keV band places this cluster in the group of strong X-ray cluster sources.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475#table1</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/101/475</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/101/475&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/101/475</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/36 [1]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#1</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/36</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/36 [2]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#2</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/36&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/36 [a3266]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#a3266</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/36 [table1]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#table1</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/36 [1]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#1</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/36</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/36 [2]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#2</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/36&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/36 [a3266]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#a3266</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/36 [table1]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#table1</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/180 [1]</TD>
            <TD>uvby-beta photometry of metal-poor stars (Schuster+ 1989)</TD>
            <TD>Using the calibrations derived by Schuster and Nissen (=1989A&amp;A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&amp;AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] &lt;= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) &gt; 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/180#1</TD>
            <TD>2011-09-14T18:13:24Z</TD>
            <TD>#Stars#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/II/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/180</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/180</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/180 [2]</TD>
            <TD>uvby-beta photometry of metal-poor stars (Schuster+ 1989)</TD>
            <TD>Using the calibrations derived by Schuster and Nissen (=1989A&amp;A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&amp;AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] &lt;= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) &gt; 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/180#2</TD>
            <TD>2011-09-14T18:13:24Z</TD>
            <TD>#Stars#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/II/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/180&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/180 [table1]</TD>
            <TD>uvby-beta photometry of metal-poor stars (Schuster+ 1989)</TD>
            <TD>Using the calibrations derived by Schuster and Nissen (=1989A&amp;A...221...65S), the interstellar color excesses, E(b-y), and the metallicities, [Fe/H], have been determined for the 711 high velocity and metal-poor stars in the catalogue of uvby-beta photometry (=1988A&amp;AS...73..225S). 220 of these listed in table1 turn out to be halo stars according to the criterion [Fe/H] &lt;= -1.0. About 15% of the halo stars have colors that are significantly affected by interstellar reddening, i.e. E(b-y) &gt; 0.025. The distributions in the c0-(b-y)0 diagram of the halo stars grouped according to [Fe/H], have well defined turn-off points. From the Teff values of these points a minimum age of 18-20 Gyr for the halo stars is determined. However, this age may be 2-3 Gyr too high due to a possible systematic error in Teff for the stellar models used. Relative ages of 77 halo stars in the turn-off region of the c0-(b-y)0 diagram are derived using the isochrones VandenBerg and Bell (=1985ApJS...58..561V). Assuming that the O/Fe abundance ratio is constant in halo stars, evidence of a cosmic age scatter of +/-2.5Gyr at a given metallicity is found. Furthermore, the mean age of the halo stars is found to decrease smoothly by about 3 Gyr from [Fe/H]= -2.0 to -1.0. These results suggest that a pressure-supported slow uniform collapse controlled the formation and early evolution of the Galaxy. However, the scenario of Searle and Zinn (=1978ApJ...225..357S) is also compatible with the results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/180#table1</TD>
            <TD>2011-09-14T18:13:24Z</TD>
            <TD>#Stars#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/II/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/180</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>GalexNear [1]</TD>
            <TD>Galaxy Explorer All Sky Survey: Near UV</TD>
            <TD>The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682. &lt;p&gt; The &lt;i&gt;SkyView&lt;/i&gt; GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image. &lt;p&gt; As of February 10, 2011, SkyView uses the GALEX GR6 data release.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/skyview/galexnear#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/galexnear</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=galexnear&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GalexNear [2]</TD>
            <TD>Galaxy Explorer All Sky Survey: Near UV</TD>
            <TD>The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682. &lt;p&gt; The &lt;i&gt;SkyView&lt;/i&gt; GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image. &lt;p&gt; As of February 10, 2011, SkyView uses the GALEX GR6 data release.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/skyview/galexnear#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/galexnear</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/288/413 [1]</TD>
            <TD>Massive stars in I Zw 36 (Deharveng+ 1994)</TD>
            <TD>We have observed the blue dwarf galaxy I Zw 36 with the f/96 relay of the HST Faint Object Camera and have for the first time resolved massive stars, using the broad band filters F175W, F342W, F430W and F480LP. We have measured the fluxes of 143 of these objects and studied their characteristics in color-magnitude diagrams. A few stars may be red supergiants but their contribution to the integrated light is less than 5% in the F430W filter. The F175W-F430W color of the integrated stellar population is redder than expected from the current burst of star formation, suggesting therefore the presence of an older and unresolved underlying population. The ultraviolet measurements combined with synthetic photometry calculations allow us to place the massive stars in a bolometric magnitude vs. temperature diagram. In this diagram, the stars are compared to evolutionary tracks for different stellar masses. The current burst probably has an age less than 12Myr. We infer an Initial Mass Function, with a power-law slope in the range -1.7 to -2.6 for masses M&gt;=20M_{sun}_. This is consistent with most of the values reported for sites of star formation in the Galaxy and the Magellanic Clouds and does not support the view of an IMF flattening at low metallicity.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/288/413#1</TD>
            <TD>2011-09-14T18:14:19Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/288/413</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/288/413</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/288/413</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/288/413 [2]</TD>
            <TD>Massive stars in I Zw 36 (Deharveng+ 1994)</TD>
            <TD>We have observed the blue dwarf galaxy I Zw 36 with the f/96 relay of the HST Faint Object Camera and have for the first time resolved massive stars, using the broad band filters F175W, F342W, F430W and F480LP. We have measured the fluxes of 143 of these objects and studied their characteristics in color-magnitude diagrams. A few stars may be red supergiants but their contribution to the integrated light is less than 5% in the F430W filter. The F175W-F430W color of the integrated stellar population is redder than expected from the current burst of star formation, suggesting therefore the presence of an older and unresolved underlying population. The ultraviolet measurements combined with synthetic photometry calculations allow us to place the massive stars in a bolometric magnitude vs. temperature diagram. In this diagram, the stars are compared to evolutionary tracks for different stellar masses. The current burst probably has an age less than 12Myr. We infer an Initial Mass Function, with a power-law slope in the range -1.7 to -2.6 for masses M&gt;=20M_{sun}_. This is consistent with most of the values reported for sites of star formation in the Galaxy and the Magellanic Clouds and does not support the view of an IMF flattening at low metallicity.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/288/413#2</TD>
            <TD>2011-09-14T18:14:19Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/288/413</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/288/413&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/288/413</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/36 [1]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#1</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/36</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/36 [2]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#2</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/36&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/36 [a3266]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#a3266</TD>
            <TD>2011-09-14T18:45:05Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/36 [table1]</TD>
            <TD>Velocities in Abell 3266 (Quintana+ 1996)</TD>
            <TD>We present 387 velocities covering an area 1.8x1.8{deg}^2^, including 229 new galaxy velocities obtained from 309 spectra, of which 317 appear to be cluster members according to our analysis. Based on this extended velocity sample we reanalyzed the velocity structure of the cluster. We found a strongly decreasing velocity dispersion profile that, as well as the mean velocity, shows significant radial scatter. Inside the 2.5h_50_^-1^Mpc radius, the velocity dispersion has a value of 1306+/-73km/s, while further out than 3h_50_^-1^Mpc it falls below 800km/s. The global dispersion is 1085+/-51km/s. We found a remarkable velocity substructure, which we interpret as a tidal outgoing arm reaching from the center to the northernmost extensions surveyed. The arm could be produced by a recent merger with another cluster, that moved from the front and SW direction and scattered from the main cluster core into the arm. This model allows us to derive an epoch for the collision between the more massive core and the front edge of the incoming cluster of 4x10^9^h_50_^-1^yr ago and of ~2x10^9^h_50_^-1^yr for the merging of both cores. Formation of the dumb-bell is a later merger process of the two BCMs, consistent with theoretical estimates. The collision picture is also consistent with the distorted X-ray image. The very northernmost parts of the arm could, alternatively, be interpreted as ongoing infall of a few outlying loose groups. The suggestion of a faint galaxy system within 400h_50_^-1^kpc, satellite to the central dumb-bell, is maintained in spite of the large central velocity dispersion value; however, confirmation requires data for further compact faint members. From several mass estimators we derived a cluster dynamical mass value of 5x10^15^h_50_^-1^M_{sun}_, but this value should be seen in the merger context described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/36#table1</TD>
            <TD>2011-09-14T18:45:05Z</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJ/475/445 [1]</TD>
            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJ/475/445 [2]</TD>
            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>Catalog</TD>
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>Web Page</TD>
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/475/445</TD>
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/475/445&amp;</TD>
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            <TD>Catalog</TD>
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>Web Page</TD>
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>ivo://CDS.VizieR/J/ApJ/475/445</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/475/445</TD>
            <TD />
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>VIK photometry of faint field galaxies (Moustakas+ 1997)</TD>
            <TD>We combine deep K-band (W. M. Keck Telescope) with V- and I-band (New Technology Telescope) observations of two "blank" high Galactic latitude fields, surveying a total of ~2arcmin^2^. The K-band number-magnitude counts continue to rise above K~22mag, reaching surface densities of few x10^5^deg^-2^. The slope for the galaxy counts is approximately [dlog(N)/dmag].deg^-2^=0.23+/-0.02 over the range 18-23mag. While this slope is consistent with other recent deep K-band surveys, there is a definite scatter in the normalisations by about a factor of 2. In particular, our normalisation is ~2x greater than the galaxy counts reported by Djorgovski et al. in 1995 (1995ApJ...438L..13D). Optical near-infrared color-magnitude and color-color diagrams for all objects detected in the V+I+K image are plotted and discussed in the context of grids of Bruzual-Charlot isochrone synthesis galaxy evolutionary models. The colors of most of the observed galaxies are consistent with a population drawn from a broad redshift distribution. A few galaxies at K~19-20 are red in both colors (V-I&gt;3; I-K&gt;2, consistent with being early-type galaxies having undergone a burst of star formation at z&gt;5 and viewed at z~1. At K&gt;20, we find several (approximately eight) "red outlier" galaxies with I-K&gt;4 and V-I&lt;2.5, whose colors are difficult to mimic by a single evolving or nonevolving stellar population at any redshift unless they either have quite low metallicity or are highly reddened. We compare the data against the evolutionary tracks of second-burst ellipticals and against a grid of models that does not constrain galaxy ages to a particular formation redshift. The red outliers' surface density is several per square arcminute, which is so high that they are probably common objects of low luminosity L&lt;L*. Whether these are low-metallicity, dusty dwarf galaxies, or old galaxies at high redshift, they are curious and merit spectroscopic follow-up.</TD>
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            <TD>J/ApJ/483/745 [1]</TD>
            <TD>NGC 4478 globular clusters (Neilsen+ 1997)</TD>
            <TD>We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre &amp; Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.</TD>
            <TD>CDS</TD>
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            <TD>J/ApJ/483/745 [2]</TD>
            <TD>NGC 4478 globular clusters (Neilsen+ 1997)</TD>
            <TD>We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre &amp; Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.</TD>
            <TD>CDS</TD>
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            <TD>NGC 4478 globular clusters (Neilsen+ 1997)</TD>
            <TD>We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre &amp; Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJ/483/745 [1]</TD>
            <TD>NGC 4478 globular clusters (Neilsen+ 1997)</TD>
            <TD>We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre &amp; Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJ/483/745 [2]</TD>
            <TD>NGC 4478 globular clusters (Neilsen+ 1997)</TD>
            <TD>We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre &amp; Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.</TD>
            <TD>CDS</TD>
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            <TD>NGC 4478 globular clusters (Neilsen+ 1997)</TD>
            <TD>We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre &amp; Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/745#table3</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Web Page</TD>
            <TD>J/A+A/288/413 [1]</TD>
            <TD>Massive stars in I Zw 36 (Deharveng+ 1994)</TD>
            <TD>We have observed the blue dwarf galaxy I Zw 36 with the f/96 relay of the HST Faint Object Camera and have for the first time resolved massive stars, using the broad band filters F175W, F342W, F430W and F480LP. We have measured the fluxes of 143 of these objects and studied their characteristics in color-magnitude diagrams. A few stars may be red supergiants but their contribution to the integrated light is less than 5% in the F430W filter. The F175W-F430W color of the integrated stellar population is redder than expected from the current burst of star formation, suggesting therefore the presence of an older and unresolved underlying population. The ultraviolet measurements combined with synthetic photometry calculations allow us to place the massive stars in a bolometric magnitude vs. temperature diagram. In this diagram, the stars are compared to evolutionary tracks for different stellar masses. The current burst probably has an age less than 12Myr. We infer an Initial Mass Function, with a power-law slope in the range -1.7 to -2.6 for masses M&gt;=20M_{sun}_. This is consistent with most of the values reported for sites of star formation in the Galaxy and the Magellanic Clouds and does not support the view of an IMF flattening at low metallicity.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/288/413#1</TD>
            <TD>2011-09-14T18:14:19Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/288/413</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/288/413</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/288/413</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/288/413 [2]</TD>
            <TD>Massive stars in I Zw 36 (Deharveng+ 1994)</TD>
            <TD>We have observed the blue dwarf galaxy I Zw 36 with the f/96 relay of the HST Faint Object Camera and have for the first time resolved massive stars, using the broad band filters F175W, F342W, F430W and F480LP. We have measured the fluxes of 143 of these objects and studied their characteristics in color-magnitude diagrams. A few stars may be red supergiants but their contribution to the integrated light is less than 5% in the F430W filter. The F175W-F430W color of the integrated stellar population is redder than expected from the current burst of star formation, suggesting therefore the presence of an older and unresolved underlying population. The ultraviolet measurements combined with synthetic photometry calculations allow us to place the massive stars in a bolometric magnitude vs. temperature diagram. In this diagram, the stars are compared to evolutionary tracks for different stellar masses. The current burst probably has an age less than 12Myr. We infer an Initial Mass Function, with a power-law slope in the range -1.7 to -2.6 for masses M&gt;=20M_{sun}_. This is consistent with most of the values reported for sites of star formation in the Galaxy and the Magellanic Clouds and does not support the view of an IMF flattening at low metallicity.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/288/413#2</TD>
            <TD>2011-09-14T18:14:19Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/288/413</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/288/413&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/288/413</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/483/745 [1]</TD>
            <TD>NGC 4478 globular clusters (Neilsen+ 1997)</TD>
            <TD>We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre &amp; Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/745#1</TD>
            <TD>2011-09-14T18:45:59Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/745</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/483/745</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/483/745</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/483/745 [2]</TD>
            <TD>NGC 4478 globular clusters (Neilsen+ 1997)</TD>
            <TD>We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre &amp; Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/745#2</TD>
            <TD>2011-09-14T18:45:59Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/745</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/483/745&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/483/745</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/483/745 [table3]</TD>
            <TD>NGC 4478 globular clusters (Neilsen+ 1997)</TD>
            <TD>We calculate the distance to NGC 4478, a neighbor of the giant Virgo elliptical M87, using the surface brightness fluctuations method on parallel data from the HST WFPC2 camera. The exposures considered were taken through the F814W filter, which approximates the Johnson I, and through the F606W filter, which is effectively a broad V filter. We describe the use of Fourier methods for separation of the fluctuations due to statistical variations in the projected number of stars per pixel (used to determine the distance) from fluctuations from other sources, which include photon noise, foreground stars, cosmic rays, and the variations due to the overall structure of the galaxy. The mean apparent magnitude of stars responsible for the measured fluctuations is m_I_{bar}=29.78+/-0.03, with an additional systematic uncertainty of 0.05mag. Using the latest calibration of Tonry (1997ApJ...475..399T), we obtain a distance of 15.6+/-1.0Mpc, which is consistent with the distance determined through the use of this method in the infrared K band by Pahre &amp; Mould (1994ApJ...433..567P). We discuss the globular cluster (GC) luminosity function and color distribution, based on the ~130 candidates identified in the field. We find a roughly Gaussian luminosity function centered at m_v_=23.82+/-0.38 with {sigma}=1.16+/-0.21. The GC color distribution is also roughly Gaussian, centered at V-I=0.91+/-0.03, with {sigma}=0.20+/-0.03, and it is coincident to within the error bars with the blue peak of the bimodal color distribution found in M87. Comparing our data with recent evaluations of the GC color distribution at two different locations in M87 we find a trend of the red peak disappearing with radial distance. We speculate that this could be understood if the blue portion of the M87 GC population were acquired from its smaller companions. The specific frequency of globular clusters is among the lowest for elliptical galaxies, comparable only to the value found in M32. In both cases this may be a result of tidal truncation by a giant neighbor. This further indicates that clusters have been stripped from NGC 4478 by M87 and likely now are part of its globular cluster population.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/745#table3</TD>
            <TD>2011-09-14T18:45:59Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/745</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/483/745&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/483/745</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/299/347 [1]</TD>
            <TD>IRAS galaxies behind Taurus clouds (Chamaraux+, 1995)</TD>
            <TD>We carried out a complete search for IRAS galaxies in the Taurus molecular cloud region at l=169deg to 177deg and b=-19deg to -12deg. We selected a total number of 36 galaxies and galaxy candidates and looked for the 21-cm H I line in 25 objects; we detected H I emission in five of them including one with previously unknown redshift. The spatial density of IRAS galaxies with cz=4000 to 6000km/s is lower in this region than in the adjacent regions at both sides along galactic longitude, where the Perseus supercluster and the Gemini-Monoceros filament are respectively located.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347#1</TD>
            <TD>2011-09-14T18:14:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/299/347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/299/347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/299/347 [2]</TD>
            <TD>IRAS galaxies behind Taurus clouds (Chamaraux+, 1995)</TD>
            <TD>We carried out a complete search for IRAS galaxies in the Taurus molecular cloud region at l=169deg to 177deg and b=-19deg to -12deg. We selected a total number of 36 galaxies and galaxy candidates and looked for the 21-cm H I line in 25 objects; we detected H I emission in five of them including one with previously unknown redshift. The spatial density of IRAS galaxies with cz=4000 to 6000km/s is lower in this region than in the adjacent regions at both sides along galactic longitude, where the Perseus supercluster and the Gemini-Monoceros filament are respectively located.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347#2</TD>
            <TD>2011-09-14T18:14:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/299/347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/299/347</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/201 [1]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#1</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/201</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/201 [2]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#2</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/201&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/107/201 [fields]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#fields</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/107/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/107/201 [galaxy]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#galaxy</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/107/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/201 [1]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#1</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/201</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/201 [2]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#2</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/201&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/107/201 [fields]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#fields</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/107/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/107/201 [galaxy]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#galaxy</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/107/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/201 [1]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#1</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/201</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/201 [2]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#2</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/201&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/107/201 [fields]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#fields</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/107/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/107/201 [galaxy]</TD>
            <TD>The Stromlo-APM Redshift Survey IV (Loveday+ 1996)</TD>
            <TD>The Stromlo-APM Redshift Survey consists of 1797 galaxies with b(J)&lt;17.15 selected randomly at a rate of 1 in 20 from Automated Plate Measurement (APM) scans. The survey covers a solid angle of 1.3sr (4300 square degrees) in the south galactic cap. Redshifts have been measured for 1790 (99.6%) of the galaxies. The median galaxy recession velocity is 15,300 km/s and so the volume probed is approximately V=1.38 million Mpc^3/h^3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201#galaxy</TD>
            <TD>2011-09-14T18:46:11Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/107/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/201</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/848 [1]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848#1</TD>
            <TD>2011-09-14T18:46:24Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/848</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/848</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/848 [2]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848#2</TD>
            <TD>2011-09-14T18:46:24Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/848&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/848</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/106/848 [table1]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848#table1</TD>
            <TD>2011-09-14T18:46:24Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/106/848&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/848</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/106/848 [table3b]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848#table3b</TD>
            <TD>2011-09-14T18:46:24Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/106/848&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/848</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/848 [1]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848#1</TD>
            <TD>2011-09-14T18:46:24Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/848</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/848</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/848 [2]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848#2</TD>
            <TD>2011-09-14T18:46:24Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/848&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/848</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/106/848 [table1]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848#table1</TD>
            <TD>2011-09-14T18:46:24Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/848</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/106/848 [1]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
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            <TD>J/AJ/106/848 [2]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
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            <TD>J/AJ/106/848 [table1]</TD>
            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
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            <TD>QSO MgII absorption line systems (Drinkwater+, 1993)</TD>
            <TD>The results of a large R-band imaging survey of 71 bright (m(V)&lt;18) quasars are presented. The quasars were chosen from published samples which have intermediate resolution optical spectroscopy available, so the presence of low redshift Mg II absorption lines can be determined. We have searched our data for galaxies close to the line-of-sight to the quasars, which we might be able to identify with the absorption systems. We find a high coincidence between galaxies very near the line-of-sight and quasars showing absorption systems in their spectra, a result consistent with other studies. These galaxies have a mean luminosity of 0.5L_star_ (assuming they lie at the absorption redshift). The distribution of impact parameters between the galaxies and the quasars extends with a flat distribution to large radii (&gt;30h^-1^kpc). This suggests that the absorption systems may not be gravitationally bound to the observed galaxies, but may be part of larger extended systems. We also find a significant number of galaxies near the line-of-sight to the quasar where no absorption is seen in the quasar spectrum. The selection of our quasars is unbiased with respect to galaxies near the line-of-sight, so we can compare the observed number of absorption systems to that predicted by a simple model with a constant covering factor in Mg II absorbing gas within a maximum radius of each detected galaxy. The model is consistent with a covering factor of unity, but allowing for incompleteness in the detection of galaxies, the covering factor is less than unity. The redshifts of the galaxies are required to confirm this result.</TD>
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            <TD>Web Page</TD>
            <TD>II/139B [1]</TD>
            <TD>General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988)</TD>
            <TD>This data set is the machine-readable version of the fourth edition of the General Catalogue of Variable Stars (Kholopov et al. 1985-1988). The machine version contains the same data as in the first three volumes of the printed catalog, but only the data tables without the textual material (introduction, bibliography, remarks) are included. Modifications to the format of the machine version have been made at the Astronomical Data Center in order to effect a completely homogeneous record structure suitable for full machine processing and sorting. The fourth edition of the General Catalogue of Variable Stars supersedes the third edition (Kukarkin et al. 1969-1970), three supplements (Kukarkin et al. 1971, 1974, 1976) containing data for 5401 new variable stars and improved data for many earlier designated variables, and five namelists (62-66) published in the Information Bulletin of Variable Stars (Kukarkin et al. 1976; Kholopov et al. 1978, 1979, 1981a, 1981b), which included only cross identifications for 2619 new variables. This new edition contains data for 28484 individual objects discovered and named by 1982 and located mainly in the Milky Way galaxy. These data are contained in the first three published volumes. The fourth volume of the fourth edition, published in 1990, contains a table of all variables ordered by right ascension and declination (B1950), a table of variables listed by variability type, and an extensive series of cross-identification tables to alternate designations (see &lt;II/172&gt;). The fifth and final volume will contain data for all presently known variables in external galaxies (including the Magellanic Clouds), extragalactic supernovae, and optically variable quasistellar objects and galactic nuclei (see &lt;II/205&gt;). Data contained in the catalog include star identifier, equatorial position (B1950), annual precession, galactic coordinates, type of variability, maximum and minimum magnitudes, epoch of maximum, period, and spectral type. Since extensive modifications have been made to the record structure of the machine version, users are encouraged to carefully study the brief descriptions given in the document. The list of errors published by Durlevich et al. (1994) has been incorporated in this version</TD>
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            <TD>HTTP Request</TD>
            <TD>II/139B [2]</TD>
            <TD>General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988)</TD>
            <TD>This data set is the machine-readable version of the fourth edition of the General Catalogue of Variable Stars (Kholopov et al. 1985-1988). The machine version contains the same data as in the first three volumes of the printed catalog, but only the data tables without the textual material (introduction, bibliography, remarks) are included. Modifications to the format of the machine version have been made at the Astronomical Data Center in order to effect a completely homogeneous record structure suitable for full machine processing and sorting. The fourth edition of the General Catalogue of Variable Stars supersedes the third edition (Kukarkin et al. 1969-1970), three supplements (Kukarkin et al. 1971, 1974, 1976) containing data for 5401 new variable stars and improved data for many earlier designated variables, and five namelists (62-66) published in the Information Bulletin of Variable Stars (Kukarkin et al. 1976; Kholopov et al. 1978, 1979, 1981a, 1981b), which included only cross identifications for 2619 new variables. This new edition contains data for 28484 individual objects discovered and named by 1982 and located mainly in the Milky Way galaxy. These data are contained in the first three published volumes. The fourth volume of the fourth edition, published in 1990, contains a table of all variables ordered by right ascension and declination (B1950), a table of variables listed by variability type, and an extensive series of cross-identification tables to alternate designations (see &lt;II/172&gt;). The fifth and final volume will contain data for all presently known variables in external galaxies (including the Magellanic Clouds), extragalactic supernovae, and optically variable quasistellar objects and galactic nuclei (see &lt;II/205&gt;). Data contained in the catalog include star identifier, equatorial position (B1950), annual precession, galactic coordinates, type of variability, maximum and minimum magnitudes, epoch of maximum, period, and spectral type. Since extensive modifications have been made to the record structure of the machine version, users are encouraged to carefully study the brief descriptions given in the document. The list of errors published by Durlevich et al. (1994) has been incorporated in this version</TD>
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            <TD>General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988)</TD>
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            <TD>II/139B [1]</TD>
            <TD>General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988)</TD>
            <TD>This data set is the machine-readable version of the fourth edition of the General Catalogue of Variable Stars (Kholopov et al. 1985-1988). The machine version contains the same data as in the first three volumes of the printed catalog, but only the data tables without the textual material (introduction, bibliography, remarks) are included. Modifications to the format of the machine version have been made at the Astronomical Data Center in order to effect a completely homogeneous record structure suitable for full machine processing and sorting. The fourth edition of the General Catalogue of Variable Stars supersedes the third edition (Kukarkin et al. 1969-1970), three supplements (Kukarkin et al. 1971, 1974, 1976) containing data for 5401 new variable stars and improved data for many earlier designated variables, and five namelists (62-66) published in the Information Bulletin of Variable Stars (Kukarkin et al. 1976; Kholopov et al. 1978, 1979, 1981a, 1981b), which included only cross identifications for 2619 new variables. This new edition contains data for 28484 individual objects discovered and named by 1982 and located mainly in the Milky Way galaxy. These data are contained in the first three published volumes. The fourth volume of the fourth edition, published in 1990, contains a table of all variables ordered by right ascension and declination (B1950), a table of variables listed by variability type, and an extensive series of cross-identification tables to alternate designations (see &lt;II/172&gt;). The fifth and final volume will contain data for all presently known variables in external galaxies (including the Magellanic Clouds), extragalactic supernovae, and optically variable quasistellar objects and galactic nuclei (see &lt;II/205&gt;). Data contained in the catalog include star identifier, equatorial position (B1950), annual precession, galactic coordinates, type of variability, maximum and minimum magnitudes, epoch of maximum, period, and spectral type. Since extensive modifications have been made to the record structure of the machine version, users are encouraged to carefully study the brief descriptions given in the document. The list of errors published by Durlevich et al. (1994) has been incorporated in this version</TD>
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            <TD>General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988)</TD>
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            <TD>Catalog</TD>
            <TD>II/139B [catalog]</TD>
            <TD>General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988)</TD>
            <TD>This data set is the machine-readable version of the fourth edition of the General Catalogue of Variable Stars (Kholopov et al. 1985-1988). The machine version contains the same data as in the first three volumes of the printed catalog, but only the data tables without the textual material (introduction, bibliography, remarks) are included. Modifications to the format of the machine version have been made at the Astronomical Data Center in order to effect a completely homogeneous record structure suitable for full machine processing and sorting. The fourth edition of the General Catalogue of Variable Stars supersedes the third edition (Kukarkin et al. 1969-1970), three supplements (Kukarkin et al. 1971, 1974, 1976) containing data for 5401 new variable stars and improved data for many earlier designated variables, and five namelists (62-66) published in the Information Bulletin of Variable Stars (Kukarkin et al. 1976; Kholopov et al. 1978, 1979, 1981a, 1981b), which included only cross identifications for 2619 new variables. This new edition contains data for 28484 individual objects discovered and named by 1982 and located mainly in the Milky Way galaxy. These data are contained in the first three published volumes. The fourth volume of the fourth edition, published in 1990, contains a table of all variables ordered by right ascension and declination (B1950), a table of variables listed by variability type, and an extensive series of cross-identification tables to alternate designations (see &lt;II/172&gt;). The fifth and final volume will contain data for all presently known variables in external galaxies (including the Magellanic Clouds), extragalactic supernovae, and optically variable quasistellar objects and galactic nuclei (see &lt;II/205&gt;). Data contained in the catalog include star identifier, equatorial position (B1950), annual precession, galactic coordinates, type of variability, maximum and minimum magnitudes, epoch of maximum, period, and spectral type. Since extensive modifications have been made to the record structure of the machine version, users are encouraged to carefully study the brief descriptions given in the document. The list of errors published by Durlevich et al. (1994) has been incorporated in this version</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/139B#catalog</TD>
            <TD>2011-09-14T18:46:39Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
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            <TD>15-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/139B</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/139B&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/139B</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/139B [1]</TD>
            <TD>General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988)</TD>
            <TD>This data set is the machine-readable version of the fourth edition of the General Catalogue of Variable Stars (Kholopov et al. 1985-1988). The machine version contains the same data as in the first three volumes of the printed catalog, but only the data tables without the textual material (introduction, bibliography, remarks) are included. Modifications to the format of the machine version have been made at the Astronomical Data Center in order to effect a completely homogeneous record structure suitable for full machine processing and sorting. The fourth edition of the General Catalogue of Variable Stars supersedes the third edition (Kukarkin et al. 1969-1970), three supplements (Kukarkin et al. 1971, 1974, 1976) containing data for 5401 new variable stars and improved data for many earlier designated variables, and five namelists (62-66) published in the Information Bulletin of Variable Stars (Kukarkin et al. 1976; Kholopov et al. 1978, 1979, 1981a, 1981b), which included only cross identifications for 2619 new variables. This new edition contains data for 28484 individual objects discovered and named by 1982 and located mainly in the Milky Way galaxy. These data are contained in the first three published volumes. The fourth volume of the fourth edition, published in 1990, contains a table of all variables ordered by right ascension and declination (B1950), a table of variables listed by variability type, and an extensive series of cross-identification tables to alternate designations (see &lt;II/172&gt;). The fifth and final volume will contain data for all presently known variables in external galaxies (including the Magellanic Clouds), extragalactic supernovae, and optically variable quasistellar objects and galactic nuclei (see &lt;II/205&gt;). Data contained in the catalog include star identifier, equatorial position (B1950), annual precession, galactic coordinates, type of variability, maximum and minimum magnitudes, epoch of maximum, period, and spectral type. Since extensive modifications have been made to the record structure of the machine version, users are encouraged to carefully study the brief descriptions given in the document. The list of errors published by Durlevich et al. (1994) has been incorporated in this version</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/139B#1</TD>
            <TD>2011-09-14T18:46:39Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/139B</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/139B</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/139B</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/139B [2]</TD>
            <TD>General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988)</TD>
            <TD>This data set is the machine-readable version of the fourth edition of the General Catalogue of Variable Stars (Kholopov et al. 1985-1988). The machine version contains the same data as in the first three volumes of the printed catalog, but only the data tables without the textual material (introduction, bibliography, remarks) are included. Modifications to the format of the machine version have been made at the Astronomical Data Center in order to effect a completely homogeneous record structure suitable for full machine processing and sorting. The fourth edition of the General Catalogue of Variable Stars supersedes the third edition (Kukarkin et al. 1969-1970), three supplements (Kukarkin et al. 1971, 1974, 1976) containing data for 5401 new variable stars and improved data for many earlier designated variables, and five namelists (62-66) published in the Information Bulletin of Variable Stars (Kukarkin et al. 1976; Kholopov et al. 1978, 1979, 1981a, 1981b), which included only cross identifications for 2619 new variables. This new edition contains data for 28484 individual objects discovered and named by 1982 and located mainly in the Milky Way galaxy. These data are contained in the first three published volumes. The fourth volume of the fourth edition, published in 1990, contains a table of all variables ordered by right ascension and declination (B1950), a table of variables listed by variability type, and an extensive series of cross-identification tables to alternate designations (see &lt;II/172&gt;). The fifth and final volume will contain data for all presently known variables in external galaxies (including the Magellanic Clouds), extragalactic supernovae, and optically variable quasistellar objects and galactic nuclei (see &lt;II/205&gt;). Data contained in the catalog include star identifier, equatorial position (B1950), annual precession, galactic coordinates, type of variability, maximum and minimum magnitudes, epoch of maximum, period, and spectral type. Since extensive modifications have been made to the record structure of the machine version, users are encouraged to carefully study the brief descriptions given in the document. The list of errors published by Durlevich et al. (1994) has been incorporated in this version</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/139B#2</TD>
            <TD>2011-09-14T18:46:39Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/139B</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/139B&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/139B</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/139B [catalog]</TD>
            <TD>General Catalog of Variable Stars, 4th Ed. (GCVS4) (Kholopov+ 1988)</TD>
            <TD>This data set is the machine-readable version of the fourth edition of the General Catalogue of Variable Stars (Kholopov et al. 1985-1988). The machine version contains the same data as in the first three volumes of the printed catalog, but only the data tables without the textual material (introduction, bibliography, remarks) are included. Modifications to the format of the machine version have been made at the Astronomical Data Center in order to effect a completely homogeneous record structure suitable for full machine processing and sorting. The fourth edition of the General Catalogue of Variable Stars supersedes the third edition (Kukarkin et al. 1969-1970), three supplements (Kukarkin et al. 1971, 1974, 1976) containing data for 5401 new variable stars and improved data for many earlier designated variables, and five namelists (62-66) published in the Information Bulletin of Variable Stars (Kukarkin et al. 1976; Kholopov et al. 1978, 1979, 1981a, 1981b), which included only cross identifications for 2619 new variables. This new edition contains data for 28484 individual objects discovered and named by 1982 and located mainly in the Milky Way galaxy. These data are contained in the first three published volumes. The fourth volume of the fourth edition, published in 1990, contains a table of all variables ordered by right ascension and declination (B1950), a table of variables listed by variability type, and an extensive series of cross-identification tables to alternate designations (see &lt;II/172&gt;). The fifth and final volume will contain data for all presently known variables in external galaxies (including the Magellanic Clouds), extragalactic supernovae, and optically variable quasistellar objects and galactic nuclei (see &lt;II/205&gt;). Data contained in the catalog include star identifier, equatorial position (B1950), annual precession, galactic coordinates, type of variability, maximum and minimum magnitudes, epoch of maximum, period, and spectral type. Since extensive modifications have been made to the record structure of the machine version, users are encouraged to carefully study the brief descriptions given in the document. The list of errors published by Durlevich et al. (1994) has been incorporated in this version</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/139B#catalog</TD>
            <TD>2011-09-14T18:46:39Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/139B</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/139B&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/139B</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/133/181 [1]</TD>
            <TD>BVI imaging of 20 irregular galaxies (Makarova+ 1998)</TD>
            <TD>We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_&lt;500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), &gt;=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181#1</TD>
            <TD>2011-09-14T18:47:12Z</TD>
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            <TD>#Research#</TD>
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            <TD>25-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/133/181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/133/181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/133/181 [2]</TD>
            <TD>BVI imaging of 20 irregular galaxies (Makarova+ 1998)</TD>
            <TD>We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_&lt;500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), &gt;=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181#2</TD>
            <TD>2011-09-14T18:47:12Z</TD>
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            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/133/181&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/133/181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/133/181 [list]</TD>
            <TD>BVI imaging of 20 irregular galaxies (Makarova+ 1998)</TD>
            <TD>We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_&lt;500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), &gt;=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181#list</TD>
            <TD>2011-09-14T18:47:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/133/181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/133/181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/133/181 [1]</TD>
            <TD>BVI imaging of 20 irregular galaxies (Makarova+ 1998)</TD>
            <TD>We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_&lt;500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), &gt;=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181#1</TD>
            <TD>2011-09-14T18:47:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>25-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/133/181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/133/181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/133/181 [2]</TD>
            <TD>BVI imaging of 20 irregular galaxies (Makarova+ 1998)</TD>
            <TD>We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_&lt;500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), &gt;=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181#2</TD>
            <TD>2011-09-14T18:47:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>25-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/133/181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/133/181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/133/181 [list]</TD>
            <TD>BVI imaging of 20 irregular galaxies (Makarova+ 1998)</TD>
            <TD>We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_&lt;500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), &gt;=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181#list</TD>
            <TD>2011-09-14T18:47:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/133/181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/133/181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/299/347 [1]</TD>
            <TD>IRAS galaxies behind Taurus clouds (Chamaraux+, 1995)</TD>
            <TD>We carried out a complete search for IRAS galaxies in the Taurus molecular cloud region at l=169deg to 177deg and b=-19deg to -12deg. We selected a total number of 36 galaxies and galaxy candidates and looked for the 21-cm H I line in 25 objects; we detected H I emission in five of them including one with previously unknown redshift. The spatial density of IRAS galaxies with cz=4000 to 6000km/s is lower in this region than in the adjacent regions at both sides along galactic longitude, where the Perseus supercluster and the Gemini-Monoceros filament are respectively located.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347#1</TD>
            <TD>2011-09-14T18:14:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/299/347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/299/347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/299/347 [2]</TD>
            <TD>IRAS galaxies behind Taurus clouds (Chamaraux+, 1995)</TD>
            <TD>We carried out a complete search for IRAS galaxies in the Taurus molecular cloud region at l=169deg to 177deg and b=-19deg to -12deg. We selected a total number of 36 galaxies and galaxy candidates and looked for the 21-cm H I line in 25 objects; we detected H I emission in five of them including one with previously unknown redshift. The spatial density of IRAS galaxies with cz=4000 to 6000km/s is lower in this region than in the adjacent regions at both sides along galactic longitude, where the Perseus supercluster and the Gemini-Monoceros filament are respectively located.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347#2</TD>
            <TD>2011-09-14T18:14:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/299/347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/299/347</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/133/181 [1]</TD>
            <TD>BVI imaging of 20 irregular galaxies (Makarova+ 1998)</TD>
            <TD>We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_&lt;500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), &gt;=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181#1</TD>
            <TD>2011-09-14T18:47:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/133/181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/133/181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/133/181 [2]</TD>
            <TD>BVI imaging of 20 irregular galaxies (Makarova+ 1998)</TD>
            <TD>We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_&lt;500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), &gt;=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181#2</TD>
            <TD>2011-09-14T18:47:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/133/181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/133/181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/133/181 [list]</TD>
            <TD>BVI imaging of 20 irregular galaxies (Makarova+ 1998)</TD>
            <TD>We present B, V and I CCD stellar photometry for a sample of 20 field irregular dwarf galaxies. Their corrected radial velocity is V_0_&lt;500km/s. Most of them have been resolved into stars for the first time. Based on photometry of their brightest blue stars we have derived the following distances: 5.9Mpc (UGC 685), 5.4Mpc (UGC 1281), 7.2Mpc (UGC 3303), 7.0Mpc (UGC 3476), 7.3:Mpc (UGC 3600), 7.2:Mpc (UGC 3698), 7.9Mpc (NGC 2337), 8.6Mpc (UGC 3817), 5.7Mpc (UGC 3860), 5.6Mpc (UGC 4426), &gt;=7.9Mpc (F 565-v1), 7.4:Mpc (UGC 5086), 7.1Mpc (UGC 5272), 5.9Mpc (UGC 5340), 7.1Mpc (UGC 5427), 2.7:Mpc (UGC 5456), 6.6Mpc (NGC 3274), 9.3Mpc (UGC 5889), 5.2Mpc (NGC 5238), and 8.0Mpc (UGC 9405). Our sample exhibits diverse morphological properties evidently caused by their different starburst activity. The galaxy sample has a median integral absolute magnitude M_B_=-14.6 and a median integral colour (B-V)_T_=+0.47. One dwarf, UGC 5340, stands out by its very blue colour, (B-V)_T_=+0.18, and by its high M(HI)/L ratio, as expected for young galaxies. Four objects of the sample are IRAS sources. Being well isolated systems, the considered galaxies may be used to estimate a local value of the Hubble parameter, H=V_0_/D. For half of the sample galaxies their individual H- values are concentrated within [58-68]km/s/Mpc with a median of 65km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181#list</TD>
            <TD>2011-09-14T18:47:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/133/181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/133/181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/133/181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/110/533 [1]</TD>
            <TD>BR photometry of Fornax bright stars (Stetson+ 1998)</TD>
            <TD>We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg^2^ field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533#1</TD>
            <TD>2011-09-14T18:47:26Z</TD>
            <TD>#Stars#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/110/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/110/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/110/533 [2]</TD>
            <TD>BR photometry of Fornax bright stars (Stetson+ 1998)</TD>
            <TD>We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg^2^ field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533#2</TD>
            <TD>2011-09-14T18:47:26Z</TD>
            <TD>#Stars#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/110/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/110/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/110/533 [table1]</TD>
            <TD>BR photometry of Fornax bright stars (Stetson+ 1998)</TD>
            <TD>We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg^2^ field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533#table1</TD>
            <TD>2011-09-14T18:47:26Z</TD>
            <TD>#Stars#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/110/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/110/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/110/533 [1]</TD>
            <TD>BR photometry of Fornax bright stars (Stetson+ 1998)</TD>
            <TD>We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg^2^ field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533#1</TD>
            <TD>2011-09-14T18:47:26Z</TD>
            <TD>#Stars#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/110/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/110/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/110/533 [2]</TD>
            <TD>BR photometry of Fornax bright stars (Stetson+ 1998)</TD>
            <TD>We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg^2^ field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533#2</TD>
            <TD>2011-09-14T18:47:26Z</TD>
            <TD>#Stars#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/110/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/110/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/110/533 [table1]</TD>
            <TD>BR photometry of Fornax bright stars (Stetson+ 1998)</TD>
            <TD>We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg^2^ field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533#table1</TD>
            <TD>2011-09-14T18:47:26Z</TD>
            <TD>#Stars#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/110/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/110/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/299/347 [1]</TD>
            <TD>IRAS galaxies behind Taurus clouds (Chamaraux+, 1995)</TD>
            <TD>We carried out a complete search for IRAS galaxies in the Taurus molecular cloud region at l=169deg to 177deg and b=-19deg to -12deg. We selected a total number of 36 galaxies and galaxy candidates and looked for the 21-cm H I line in 25 objects; we detected H I emission in five of them including one with previously unknown redshift. The spatial density of IRAS galaxies with cz=4000 to 6000km/s is lower in this region than in the adjacent regions at both sides along galactic longitude, where the Perseus supercluster and the Gemini-Monoceros filament are respectively located.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347#1</TD>
            <TD>2011-09-14T18:14:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/299/347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/299/347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/299/347 [2]</TD>
            <TD>IRAS galaxies behind Taurus clouds (Chamaraux+, 1995)</TD>
            <TD>We carried out a complete search for IRAS galaxies in the Taurus molecular cloud region at l=169deg to 177deg and b=-19deg to -12deg. We selected a total number of 36 galaxies and galaxy candidates and looked for the 21-cm H I line in 25 objects; we detected H I emission in five of them including one with previously unknown redshift. The spatial density of IRAS galaxies with cz=4000 to 6000km/s is lower in this region than in the adjacent regions at both sides along galactic longitude, where the Perseus supercluster and the Gemini-Monoceros filament are respectively located.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347#2</TD>
            <TD>2011-09-14T18:14:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/299/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/299/347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/299/347</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/110/533 [1]</TD>
            <TD>BR photometry of Fornax bright stars (Stetson+ 1998)</TD>
            <TD>We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg^2^ field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533#1</TD>
            <TD>2011-09-14T18:47:26Z</TD>
            <TD>#Stars#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/110/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/110/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/110/533 [2]</TD>
            <TD>BR photometry of Fornax bright stars (Stetson+ 1998)</TD>
            <TD>We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg^2^ field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533#2</TD>
            <TD>2011-09-14T18:47:26Z</TD>
            <TD>#Stars#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/110/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/110/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/110/533 [table1]</TD>
            <TD>BR photometry of Fornax bright stars (Stetson+ 1998)</TD>
            <TD>We present accurate photometry on the Johnson B, Kron-Cousins R photometric system for approximately 100,000 stars in a 1/3deg^2^ field centered on the dwarf spheroidal galaxy in Fornax. We identify numerous probable short-period variable stars, blue stars that appear to be the main sequence of a small population with an age of order 108yr, and two distinct types of luminous red star: an extended sequence of primarily carbon stars and a clump of mostly M giants slightly more luminous than the giant-branch tip. The spatial distribution of each of these subpopulations within the Fornax dwarf galaxy is considered.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533#table1</TD>
            <TD>2011-09-14T18:47:26Z</TD>
            <TD>#Stars#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/PASP/110/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/110/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/110/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/309/446 [1]</TD>
            <TD>HII Regions in M51 (Petit+, 1996)</TD>
            <TD>A deeper detection of the spiral structure of the Sbc galaxy M 51 is the main goal of this paper. New UV data in the 2000A range were obtained with a high altitude balloon of the Laboratoire d'Astronomie Spatiale de Marseille and the Observatoire de Geneve, (LAS-OG). The data reveal the location of hot, evolved low-mass stars predominantly along the outside edge of, and down stream from, the spiral arms defined by the string of HII regions. Since these stars have a relatively well-defined age compared to the "mixed" population of stars seen in the arms when observed in visible light, the UV data is well-suited to derive time-scales of spiral arm components. In particular, the relation between spiral structure and star formation, which is at least partly due to the density wave shock mechanism, can be studied from the differential positions of the low-mass stars observed in the UV and the massive stars coexisting with the ionized gas. To facilitate such detailed UV-H{alpha} comparison, we have also carried out new deep integrations, photometry, and accurate mapping of the H{alpha} emission. A catalogue of 478 HII regions in M 51 has been established from the analysis of narrow band H{alpha} images taken with a combination of the Special Astronomical Observatory (SAO) Russian image tube, and the Observatoire de Marseille (OM) focal reducer f/1.5 (9m equivalent focal length) attached at the prime focus of the 6-m telescope of the SAO. The radial and tangential shifts of the main and secondary spiral structures in UV and H{alpha} are also compared with other spiral tracers. The displacements observed in these observations are compatible with a scenario in which the star formation is triggered by the density wave.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/309/446#1</TD>
            <TD>2011-09-14T18:15:04Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/309/446</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/309/446</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/309/446</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/309/446 [2]</TD>
            <TD>HII Regions in M51 (Petit+, 1996)</TD>
            <TD>A deeper detection of the spiral structure of the Sbc galaxy M 51 is the main goal of this paper. New UV data in the 2000A range were obtained with a high altitude balloon of the Laboratoire d'Astronomie Spatiale de Marseille and the Observatoire de Geneve, (LAS-OG). The data reveal the location of hot, evolved low-mass stars predominantly along the outside edge of, and down stream from, the spiral arms defined by the string of HII regions. Since these stars have a relatively well-defined age compared to the "mixed" population of stars seen in the arms when observed in visible light, the UV data is well-suited to derive time-scales of spiral arm components. In particular, the relation between spiral structure and star formation, which is at least partly due to the density wave shock mechanism, can be studied from the differential positions of the low-mass stars observed in the UV and the massive stars coexisting with the ionized gas. To facilitate such detailed UV-H{alpha} comparison, we have also carried out new deep integrations, photometry, and accurate mapping of the H{alpha} emission. A catalogue of 478 HII regions in M 51 has been established from the analysis of narrow band H{alpha} images taken with a combination of the Special Astronomical Observatory (SAO) Russian image tube, and the Observatoire de Marseille (OM) focal reducer f/1.5 (9m equivalent focal length) attached at the prime focus of the 6-m telescope of the SAO. The radial and tangential shifts of the main and secondary spiral structures in UV and H{alpha} are also compared with other spiral tracers. The displacements observed in these observations are compatible with a scenario in which the star formation is triggered by the density wave.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/309/446#2</TD>
            <TD>2011-09-14T18:15:04Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/309/446</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/309/446&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/309/446</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/440/28 [1]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#1</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/440/28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/440/28 [2]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#2</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/440/28 [table7]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#table7</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/440/28 [table1]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#table1</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/440/28 [table6]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#table6</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/440/28 [1]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#1</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/440/28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/440/28 [2]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#2</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/440/28 [table7]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#table7</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/440/28 [table1]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#table1</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/440/28 [table6]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#table6</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/309/446 [1]</TD>
            <TD>HII Regions in M51 (Petit+, 1996)</TD>
            <TD>A deeper detection of the spiral structure of the Sbc galaxy M 51 is the main goal of this paper. New UV data in the 2000A range were obtained with a high altitude balloon of the Laboratoire d'Astronomie Spatiale de Marseille and the Observatoire de Geneve, (LAS-OG). The data reveal the location of hot, evolved low-mass stars predominantly along the outside edge of, and down stream from, the spiral arms defined by the string of HII regions. Since these stars have a relatively well-defined age compared to the "mixed" population of stars seen in the arms when observed in visible light, the UV data is well-suited to derive time-scales of spiral arm components. In particular, the relation between spiral structure and star formation, which is at least partly due to the density wave shock mechanism, can be studied from the differential positions of the low-mass stars observed in the UV and the massive stars coexisting with the ionized gas. To facilitate such detailed UV-H{alpha} comparison, we have also carried out new deep integrations, photometry, and accurate mapping of the H{alpha} emission. A catalogue of 478 HII regions in M 51 has been established from the analysis of narrow band H{alpha} images taken with a combination of the Special Astronomical Observatory (SAO) Russian image tube, and the Observatoire de Marseille (OM) focal reducer f/1.5 (9m equivalent focal length) attached at the prime focus of the 6-m telescope of the SAO. The radial and tangential shifts of the main and secondary spiral structures in UV and H{alpha} are also compared with other spiral tracers. The displacements observed in these observations are compatible with a scenario in which the star formation is triggered by the density wave.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/309/446#1</TD>
            <TD>2011-09-14T18:15:04Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/309/446</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/309/446</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/309/446</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/309/446 [2]</TD>
            <TD>HII Regions in M51 (Petit+, 1996)</TD>
            <TD>A deeper detection of the spiral structure of the Sbc galaxy M 51 is the main goal of this paper. New UV data in the 2000A range were obtained with a high altitude balloon of the Laboratoire d'Astronomie Spatiale de Marseille and the Observatoire de Geneve, (LAS-OG). The data reveal the location of hot, evolved low-mass stars predominantly along the outside edge of, and down stream from, the spiral arms defined by the string of HII regions. Since these stars have a relatively well-defined age compared to the "mixed" population of stars seen in the arms when observed in visible light, the UV data is well-suited to derive time-scales of spiral arm components. In particular, the relation between spiral structure and star formation, which is at least partly due to the density wave shock mechanism, can be studied from the differential positions of the low-mass stars observed in the UV and the massive stars coexisting with the ionized gas. To facilitate such detailed UV-H{alpha} comparison, we have also carried out new deep integrations, photometry, and accurate mapping of the H{alpha} emission. A catalogue of 478 HII regions in M 51 has been established from the analysis of narrow band H{alpha} images taken with a combination of the Special Astronomical Observatory (SAO) Russian image tube, and the Observatoire de Marseille (OM) focal reducer f/1.5 (9m equivalent focal length) attached at the prime focus of the 6-m telescope of the SAO. The radial and tangential shifts of the main and secondary spiral structures in UV and H{alpha} are also compared with other spiral tracers. The displacements observed in these observations are compatible with a scenario in which the star formation is triggered by the density wave.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/309/446#2</TD>
            <TD>2011-09-14T18:15:04Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/309/446</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/309/446&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/309/446</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/440/28 [1]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#1</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/440/28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/440/28 [2]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#2</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/440/28 [table7]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#table7</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/440/28 [table1]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#table1</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/440/28 [table6]</TD>
            <TD>Brightest Cluster Galaxies velocities (Postman+ 1995)</TD>
            <TD>We investigate the use of Brightest Cluster Galaxies (BCGs) as standard candles for measuring galaxy peculiar velocities on large scales. We have obtained precise large-format CCD surface photometry and redshifts for an all-sky, volume-limited (z&lt;=0.05) sample of 119 BCG. We reinvestigate the Hoessel (1980ApJ...241..493H) relationship between the metric luminosity, L_m_, within the central 10h^-1^kpc of the BCGs and the logarithmic slope of the surface brightness profile, {alpha}. The L_m_-{alpha} relationship reduces the cosmic scatter in L_m_ from 0.327mag to 0.244mag, yielding a typical distance accuracy of 17% per BCG. Residuals about the L_m_-{alpha} relationship are independent of BCG luminosity, BCG B-R_c_ color, BCG location within the host cluster, and richness of the host cluster. The metric luminosity is independent of cluster richness even before correcting for its dependence on {alpha}, which provides further evidence for the unique nature of the BCG luminosity function. Indeed, the BCG luminosity function, both before and after application of the {alpha}-correction, is consistent with a single Gaussian distribution. Half the BCGs in the sample show some evidence of small color gradients as a function of radius within their central 50h^-1^kpc regions but with almost equal numbers becoming redder as becoming bluer. However, with the central 10h^-1^kpc the colors are remarkably constant, the mean B-R_c_ color is 1.51 with a dispersion of only 0.06mag. The narrow photometric and color distributions of the BCGs, the lack of "second-parameter" effects, as well as the unique rich cluster environment of BCGs, argue that BCGs are the most homogeneous distance indicators presently available for large-scale structure research.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28#table6</TD>
            <TD>2011-09-14T18:47:45Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/440/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/440/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/440/28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/310/8 [1]</TD>
            <TD>The ESO Nearby Abell Cluster Survey I. (Katgert+, 1996)</TD>
            <TD>We describe the results of the ESO Key-programme on "Structure and Dynamics of Rich Galaxy Clusters" (which we will henceforth refer to as the ESO Nearby Abell Cluster Survey - or ENACS). We discuss the sample of clusters for which data were obtained, and the observational programme of spectroscopy and photometry that we carried out. The final database contains a total of 5634 galaxies in the directions of 107 clusters from the catalogue by Abell, Corwin and Olowin 1989 (ACO hereafter) with richness R&gt;=1 and mean redshifts z&lt;=0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/8#1</TD>
            <TD>2011-09-14T18:15:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/8</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/310/8</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/310/8</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/310/8 [2]</TD>
            <TD>The ESO Nearby Abell Cluster Survey I. (Katgert+, 1996)</TD>
            <TD>We describe the results of the ESO Key-programme on "Structure and Dynamics of Rich Galaxy Clusters" (which we will henceforth refer to as the ESO Nearby Abell Cluster Survey - or ENACS). We discuss the sample of clusters for which data were obtained, and the observational programme of spectroscopy and photometry that we carried out. The final database contains a total of 5634 galaxies in the directions of 107 clusters from the catalogue by Abell, Corwin and Olowin 1989 (ACO hereafter) with richness R&gt;=1 and mean redshifts z&lt;=0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/8#2</TD>
            <TD>2011-09-14T18:15:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/8</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/310/8&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/310/8</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/140 [1]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/140#1</TD>
            <TD>2011-09-14T18:48:00Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>04-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VII/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/140</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/140 [2]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/140#2</TD>
            <TD>2011-09-14T18:48:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VII/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/140&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/140 [vol1]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/140#vol1</TD>
            <TD>2011-09-14T18:48:00Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
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            <TD>04-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VII/140</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/140&amp;</TD>
            <TD>180</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/140 [vol2]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/140#vol2</TD>
            <TD>2011-09-14T18:48:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VII/140</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/140&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/140 [1]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/140#1</TD>
            <TD>2011-09-14T18:48:00Z</TD>
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            <TD />
            <TD>04-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VII/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/140</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/140 [2]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/140#2</TD>
            <TD>2011-09-14T18:48:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VII/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/140&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/140 [vol1]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
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            <TD>2011-09-14T18:48:00Z</TD>
            <TD>#Galaxies#</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/140&amp;</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>VII/140 [vol2]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
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            <TD>2011-09-14T18:48:00Z</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/310/8 [1]</TD>
            <TD>The ESO Nearby Abell Cluster Survey I. (Katgert+, 1996)</TD>
            <TD>We describe the results of the ESO Key-programme on "Structure and Dynamics of Rich Galaxy Clusters" (which we will henceforth refer to as the ESO Nearby Abell Cluster Survey - or ENACS). We discuss the sample of clusters for which data were obtained, and the observational programme of spectroscopy and photometry that we carried out. The final database contains a total of 5634 galaxies in the directions of 107 clusters from the catalogue by Abell, Corwin and Olowin 1989 (ACO hereafter) with richness R&gt;=1 and mean redshifts z&lt;=0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/8#1</TD>
            <TD>2011-09-14T18:15:09Z</TD>
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            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/8</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/310/8</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/310/8</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/310/8 [2]</TD>
            <TD>The ESO Nearby Abell Cluster Survey I. (Katgert+, 1996)</TD>
            <TD>We describe the results of the ESO Key-programme on "Structure and Dynamics of Rich Galaxy Clusters" (which we will henceforth refer to as the ESO Nearby Abell Cluster Survey - or ENACS). We discuss the sample of clusters for which data were obtained, and the observational programme of spectroscopy and photometry that we carried out. The final database contains a total of 5634 galaxies in the directions of 107 clusters from the catalogue by Abell, Corwin and Olowin 1989 (ACO hereafter) with richness R&gt;=1 and mean redshifts z&lt;=0.1.</TD>
            <TD>CDS</TD>
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            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/8</TD>
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/310/8&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/310/8</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/140 [1]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
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            <TD>2011-09-14T18:48:00Z</TD>
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            <TD>ivo://CDS.VizieR/VII/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/140</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/140 [2]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T18:48:00Z</TD>
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            <TD>ivo://CDS.VizieR/VII/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/140&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/140 [vol1]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/140#vol1</TD>
            <TD>2011-09-14T18:48:00Z</TD>
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/140&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>VII/140 [vol2]</TD>
            <TD>Catalog of Galaxies Behind the Milky Way (Saito+ 1990,91)</TD>
            <TD>This catalog, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represents a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1 mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc. Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are shown in the last column. The search was performed by undergraduate students of a galactic astronomy program in Department of Astronomy, Kyoto University, in 1988 and 1989. Since the main researchers changed from the search in 1988 (Vol. 1) to that in 1989 (Vol. 2), a surface brightness level determining the extents of galaxy images somewhat differs between Vol. 1 and Vol. 2, yielding a difference of mean number densities of the detected galaxies between Vol. 1 and Vol. 2. The difference is examined in paper II. The detectability of galaxies, especially of smallest galaxies, increased in the overlap zones of adjacent fields of the Atlas; the effects are discussed in a paper (Yamada and Saito 1991, to appear in Publ. Astron. Soc. Japan, Vol. 43). In spite of such inhomogeneities in search for galaxies, the catalog is useful as a finding list of bright galaxies, peculiar galaxies, and nearby clusters of galaxies in the region behind the Milky Way. The machine-readable version of the catalog has been made through efforts of Mr. Shogo Nishida, Mr. Tadafumi Takata, and Professor Shiro Nishimura. This will be distributed upon request from Astronomical Data Analysis Center of the National Astronomical Observatory of Japan and other astronomical data centers. This work was supported by the Grant-in-Aid for General Scientific Research (01420002) of the Japanese Ministry of Education, Science, and Culture. June 1991 Mamoru Saito</TD>
            <TD>CDS</TD>
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            <TD>2011-09-14T18:48:00Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>04-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VII/140</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/140&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/140</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/318/111 [1]</TD>
            <TD>ROSAT Galactic Plane Survey (Motch+ 1997)</TD>
            <TD>We present the analysis of the point source content of a low galactic latitude region selected from the ROSAT all-sky survey. The test field is centered at l=90, b=0 and has an area of 64.5deg^2^. A total of 128 soft X-ray sources are detected above a maximum likelihood of 8. Catalogue searches and optical follow-up observations show that in this direction of the galactic plane, 85% of the sources brighter than 0.03PSPC are identified with active coronae. F-K type stars represent 67% (+/-13%) of the stellar identifications and M type stars account for 19% (+/-6%). A small but significant number of X-ray sources are associated with A type stars on the basis of positional coincidence. These results together with those of similar optical campaigns demonstrate that the soft X-ray population of the Milky Way is largely dominated by active stars. We show that the density and distribution in flux and spectral type of the active coronae detected in X-rays are consistent with the picture drawn from current stellar population models and age dependent X-ray luminosity functions. The modelling of this population suggests that most of the stars detected by ROSAT in this direction are younger than 1Gyr. This opens the possibility to extract in a novel way large samples of young stars from the ROSAT all-sky survey. The small number of unidentified sources at low X-ray flux put rather strong constraints on the hypothetical X-ray emission from old neutron stars accreting from the interstellar medium. Our observations clearly rule out models which assume no dynamical heating for this population and a total number of N_ns_=10^9^ neutron stars in the Galaxy. If accretion on polar caps is the dominant mode then our upper limit may imply N_ns_=~10^8^. Among the non coronal identifications are three white dwarfs, a Seyfert 1 active nucleus, two early type stars and one cataclysmic variable. We also report the discovery of a Me+WD close binary system with P_orb_=~12 .</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/111#1</TD>
            <TD>2011-09-14T18:15:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/318/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/318/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/318/111 [2]</TD>
            <TD>ROSAT Galactic Plane Survey (Motch+ 1997)</TD>
            <TD>We present the analysis of the point source content of a low galactic latitude region selected from the ROSAT all-sky survey. The test field is centered at l=90, b=0 and has an area of 64.5deg^2^. A total of 128 soft X-ray sources are detected above a maximum likelihood of 8. Catalogue searches and optical follow-up observations show that in this direction of the galactic plane, 85% of the sources brighter than 0.03PSPC are identified with active coronae. F-K type stars represent 67% (+/-13%) of the stellar identifications and M type stars account for 19% (+/-6%). A small but significant number of X-ray sources are associated with A type stars on the basis of positional coincidence. These results together with those of similar optical campaigns demonstrate that the soft X-ray population of the Milky Way is largely dominated by active stars. We show that the density and distribution in flux and spectral type of the active coronae detected in X-rays are consistent with the picture drawn from current stellar population models and age dependent X-ray luminosity functions. The modelling of this population suggests that most of the stars detected by ROSAT in this direction are younger than 1Gyr. This opens the possibility to extract in a novel way large samples of young stars from the ROSAT all-sky survey. The small number of unidentified sources at low X-ray flux put rather strong constraints on the hypothetical X-ray emission from old neutron stars accreting from the interstellar medium. Our observations clearly rule out models which assume no dynamical heating for this population and a total number of N_ns_=10^9^ neutron stars in the Galaxy. If accretion on polar caps is the dominant mode then our upper limit may imply N_ns_=~10^8^. Among the non coronal identifications are three white dwarfs, a Seyfert 1 active nucleus, two early type stars and one cataclysmic variable. We also report the discovery of a Me+WD close binary system with P_orb_=~12 .</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/111#2</TD>
            <TD>2011-09-14T18:15:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/318/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/318/111</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>GalexNear [1]</TD>
            <TD>Galaxy Explorer All Sky Survey: Near UV</TD>
            <TD>The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682. &lt;p&gt; The &lt;i&gt;SkyView&lt;/i&gt; GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image. &lt;p&gt; As of February 10, 2011, SkyView uses the GALEX GR6 data release.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/skyview/galexnear#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/galexnear</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=galexnear&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GalexNear [2]</TD>
            <TD>Galaxy Explorer All Sky Survey: Near UV</TD>
            <TD>The GALEX, Galaxy Explorer, mission was launched by a Pegasus-XL vehicle on April 28 2003 into a 690km altitude, 29 degree inclination, circular orbit with a 98.6 minute period. The GALEX instrument allows imaging and spectroscopic observations to be made in two ultraviolet bands, Far UV (FUV) 1350-1780A and Near UV (NUV) 1770-2730A. The instrument provides simultaneous co-aligned FUV and NUV images with spatial resolution 4.3 and 5.3 arcseconds respectively. Details of the performance of the instrument and detectors can be found in Morrissey et al. (2007) ApJS, 173, 682. &lt;p&gt; The &lt;i&gt;SkyView&lt;/i&gt; GALEX surveys mosaic the intensity images of All-Sky Survey images. For a given pixel only the nearest image is used. Since a given GALEX observation is circular, this maximizes the coverage compared with default image finding algorithms which use the distance from edge of the image. &lt;p&gt; As of February 10, 2011, SkyView uses the GALEX GR6 data release.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/skyview/galexnear#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/galexnear</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/318/111 [1]</TD>
            <TD>ROSAT Galactic Plane Survey (Motch+ 1997)</TD>
            <TD>We present the analysis of the point source content of a low galactic latitude region selected from the ROSAT all-sky survey. The test field is centered at l=90, b=0 and has an area of 64.5deg^2^. A total of 128 soft X-ray sources are detected above a maximum likelihood of 8. Catalogue searches and optical follow-up observations show that in this direction of the galactic plane, 85% of the sources brighter than 0.03PSPC are identified with active coronae. F-K type stars represent 67% (+/-13%) of the stellar identifications and M type stars account for 19% (+/-6%). A small but significant number of X-ray sources are associated with A type stars on the basis of positional coincidence. These results together with those of similar optical campaigns demonstrate that the soft X-ray population of the Milky Way is largely dominated by active stars. We show that the density and distribution in flux and spectral type of the active coronae detected in X-rays are consistent with the picture drawn from current stellar population models and age dependent X-ray luminosity functions. The modelling of this population suggests that most of the stars detected by ROSAT in this direction are younger than 1Gyr. This opens the possibility to extract in a novel way large samples of young stars from the ROSAT all-sky survey. The small number of unidentified sources at low X-ray flux put rather strong constraints on the hypothetical X-ray emission from old neutron stars accreting from the interstellar medium. Our observations clearly rule out models which assume no dynamical heating for this population and a total number of N_ns_=10^9^ neutron stars in the Galaxy. If accretion on polar caps is the dominant mode then our upper limit may imply N_ns_=~10^8^. Among the non coronal identifications are three white dwarfs, a Seyfert 1 active nucleus, two early type stars and one cataclysmic variable. We also report the discovery of a Me+WD close binary system with P_orb_=~12 .</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/111#1</TD>
            <TD>2011-09-14T18:15:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/318/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/318/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/318/111 [2]</TD>
            <TD>ROSAT Galactic Plane Survey (Motch+ 1997)</TD>
            <TD>We present the analysis of the point source content of a low galactic latitude region selected from the ROSAT all-sky survey. The test field is centered at l=90, b=0 and has an area of 64.5deg^2^. A total of 128 soft X-ray sources are detected above a maximum likelihood of 8. Catalogue searches and optical follow-up observations show that in this direction of the galactic plane, 85% of the sources brighter than 0.03PSPC are identified with active coronae. F-K type stars represent 67% (+/-13%) of the stellar identifications and M type stars account for 19% (+/-6%). A small but significant number of X-ray sources are associated with A type stars on the basis of positional coincidence. These results together with those of similar optical campaigns demonstrate that the soft X-ray population of the Milky Way is largely dominated by active stars. We show that the density and distribution in flux and spectral type of the active coronae detected in X-rays are consistent with the picture drawn from current stellar population models and age dependent X-ray luminosity functions. The modelling of this population suggests that most of the stars detected by ROSAT in this direction are younger than 1Gyr. This opens the possibility to extract in a novel way large samples of young stars from the ROSAT all-sky survey. The small number of unidentified sources at low X-ray flux put rather strong constraints on the hypothetical X-ray emission from old neutron stars accreting from the interstellar medium. Our observations clearly rule out models which assume no dynamical heating for this population and a total number of N_ns_=10^9^ neutron stars in the Galaxy. If accretion on polar caps is the dominant mode then our upper limit may imply N_ns_=~10^8^. Among the non coronal identifications are three white dwarfs, a Seyfert 1 active nucleus, two early type stars and one cataclysmic variable. We also report the discovery of a Me+WD close binary system with P_orb_=~12 .</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/111#2</TD>
            <TD>2011-09-14T18:15:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/318/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/318/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/318/111</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/18 [1]</TD>
            <TD>X-ray sources &lt;1 degree from Seyfert galaxies (Radecke 1997)</TD>
            <TD>Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (&lt; about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04&lt;B^o,i^_T_&lt;12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18#1</TD>
            <TD>2011-09-14T18:15:36Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/18 [2]</TD>
            <TD>X-ray sources &lt;1 degree from Seyfert galaxies (Radecke 1997)</TD>
            <TD>Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (&lt; about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04&lt;B^o,i^_T_&lt;12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18#2</TD>
            <TD>2011-09-14T18:15:36Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/319/18 [appena]</TD>
            <TD>X-ray sources &lt;1 degree from Seyfert galaxies (Radecke 1997)</TD>
            <TD>Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (&lt; about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04&lt;B^o,i^_T_&lt;12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18#appena</TD>
            <TD>2011-09-14T18:15:36Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/319/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/18 [1]</TD>
            <TD>X-ray sources &lt;1 degree from Seyfert galaxies (Radecke 1997)</TD>
            <TD>Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (&lt; about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04&lt;B^o,i^_T_&lt;12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18#1</TD>
            <TD>2011-09-14T18:15:36Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/18 [2]</TD>
            <TD>X-ray sources &lt;1 degree from Seyfert galaxies (Radecke 1997)</TD>
            <TD>Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (&lt; about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04&lt;B^o,i^_T_&lt;12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18#2</TD>
            <TD>2011-09-14T18:15:36Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/319/18 [appena]</TD>
            <TD>X-ray sources &lt;1 degree from Seyfert galaxies (Radecke 1997)</TD>
            <TD>Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (&lt; about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04&lt;B^o,i^_T_&lt;12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18#appena</TD>
            <TD>2011-09-14T18:15:36Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/319/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/231 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. V. (Abraham+ 1998)</TD>
            <TD>Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters: MS 1224.7+2007 (z=0.327) and MS 1512.4+3647 (z=0.372) are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations span three contiguous MOS fields in the east-west direction for MS 1512.4+3647, covering a total area of approximately 8.0'x27.3'. A single field of 7.1'x9.0' was obtained for MS 1224.7+2007. Redshifts for 287 galaxies in the MS 1512.4+3647 fields and 75 galaxies in the MS 1224.7+2007 field (primarily ranging in magnitude from r=18-22) were obtained. The spectroscopic information in this paper is supplemented by photometric information for all galaxies in the fields down to Gunn r=21mag. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/231#1</TD>
            <TD>2011-09-14T18:48:07Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/231</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/231</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/231 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. V. (Abraham+ 1998)</TD>
            <TD>Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters: MS 1224.7+2007 (z=0.327) and MS 1512.4+3647 (z=0.372) are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations span three contiguous MOS fields in the east-west direction for MS 1512.4+3647, covering a total area of approximately 8.0'x27.3'. A single field of 7.1'x9.0' was obtained for MS 1224.7+2007. Redshifts for 287 galaxies in the MS 1512.4+3647 fields and 75 galaxies in the MS 1224.7+2007 field (primarily ranging in magnitude from r=18-22) were obtained. The spectroscopic information in this paper is supplemented by photometric information for all galaxies in the fields down to Gunn r=21mag. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/231#2</TD>
            <TD>2011-09-14T18:48:07Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/116/231&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/231</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>GRANAT [1]</TD>
            <TD>GRANAT/SIGMA</TD>
            <TD>The Soviet orbital observatory GRANAT was launched in December 1989 and was operational till November 1998. One of the main instruments of the observatory was the French-Soviet hard X-ray coded mask telescope SIGMA (Paul et al.1 1991, Adv.Space Res., 11, 279). It was the first space telescope that used coded aperture technique for reconstruction of sky images in hard X-rays (35-1300 keV). The angular resolution of the telescope was approximately 12' and the accuracy of a source localization is approximately 2-3'.&lt;p&gt; SIGMA discovered numerious interesting hard X-ray sources including GRS 1758-258, which is located only 40' from bright soft X-ray source GX 5-1. It detected hard X-ray flux from X-ray burster A1742-294, which is very near to bright black hole binary 1E1740.7-2942. SIGMA set an upper limit on the hard X-ray flux of from the central supermassive black hole in our Galaxy.&lt;p&gt; During the period 1990-1998 SIGMA observed more that one quarter of the sky with sensitivity better than 100 mCrab. The Galactic Center region had the deepest exposure ( approximately 9 million sec), with the sensitivity to a source discovery (S/N &amp;amp;gt; ~ 5) or approximately 10 mCrab.&lt;p&gt; A list of all detected sources with references to publications on them is presented in the paper of Revnivtsev et al. 2004, Astr. Lett. v.6. In these survey images (40-100 keV) all performed observations are averaged together. Transient sources that were discovered by SIGMA may not visible in the averaged image. &lt;p&gt; This survey has some features that users should keep in mind. The SIGMA telescope is a complicated instrument and is strongly dominated by the accuracy of the background subtraction. The presence of a very bright source in the field of view of the telescope sometimes can not be fully accounted for and as a result of it some 'ghost' sources can appear. Such features can be seen in the regions near very bright sources like Crab Nebula, Cyg X-1, Nova Per 1992, Nova Mus 1991, Nova Oph 1993, and in the Galactic Center region. In addition to its nominal field of view (~17x17 deg) located around the optical axis of the telescope, SIGMA had another window of relatively high transparency of its shield, approximately 20-30&amp;amp;amp;#176; apart from the optical axis. Becuase of this a very bright sources like Cyg X-1 can cause non zero illumination of the SIGMA detector if they are located approximately 20-30&amp;amp;amp;#176; from the optical axis. The ring-like features caused by this effect, can be seen around Cyg X-1, and Nova Per 1992. &lt;p&gt; The count rate of detected sources (or upper limits) can be roughly translated into mCrab using the fact that that Crab nebula gives the count rate approximately 2.8e&lt;sup&gt;-3&lt;/sup&gt; cnts/s in the units, provided in 'flux' maps</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/skyview/granat#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/granat</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GRANAT [2]</TD>
            <TD>GRANAT/SIGMA</TD>
            <TD>The Soviet orbital observatory GRANAT was launched in December 1989 and was operational till November 1998. One of the main instruments of the observatory was the French-Soviet hard X-ray coded mask telescope SIGMA (Paul et al.1 1991, Adv.Space Res., 11, 279). It was the first space telescope that used coded aperture technique for reconstruction of sky images in hard X-rays (35-1300 keV). The angular resolution of the telescope was approximately 12' and the accuracy of a source localization is approximately 2-3'.&lt;p&gt; SIGMA discovered numerious interesting hard X-ray sources including GRS 1758-258, which is located only 40' from bright soft X-ray source GX 5-1. It detected hard X-ray flux from X-ray burster A1742-294, which is very near to bright black hole binary 1E1740.7-2942. SIGMA set an upper limit on the hard X-ray flux of from the central supermassive black hole in our Galaxy.&lt;p&gt; During the period 1990-1998 SIGMA observed more that one quarter of the sky with sensitivity better than 100 mCrab. The Galactic Center region had the deepest exposure ( approximately 9 million sec), with the sensitivity to a source discovery (S/N &amp;amp;gt; ~ 5) or approximately 10 mCrab.&lt;p&gt; A list of all detected sources with references to publications on them is presented in the paper of Revnivtsev et al. 2004, Astr. Lett. v.6. In these survey images (40-100 keV) all performed observations are averaged together. Transient sources that were discovered by SIGMA may not visible in the averaged image. &lt;p&gt; This survey has some features that users should keep in mind. The SIGMA telescope is a complicated instrument and is strongly dominated by the accuracy of the background subtraction. The presence of a very bright source in the field of view of the telescope sometimes can not be fully accounted for and as a result of it some 'ghost' sources can appear. Such features can be seen in the regions near very bright sources like Crab Nebula, Cyg X-1, Nova Per 1992, Nova Mus 1991, Nova Oph 1993, and in the Galactic Center region. In addition to its nominal field of view (~17x17 deg) located around the optical axis of the telescope, SIGMA had another window of relatively high transparency of its shield, approximately 20-30&amp;amp;amp;#176; apart from the optical axis. Becuase of this a very bright sources like Cyg X-1 can cause non zero illumination of the SIGMA detector if they are located approximately 20-30&amp;amp;amp;#176; from the optical axis. The ring-like features caused by this effect, can be seen around Cyg X-1, and Nova Per 1992. &lt;p&gt; The count rate of detected sources (or upper limits) can be roughly translated into mCrab using the fact that that Crab nebula gives the count rate approximately 2.8e&lt;sup&gt;-3&lt;/sup&gt; cnts/s in the units, provided in 'flux' maps</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/skyview/granat#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
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            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/granat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>GRANAT [1]</TD>
            <TD>GRANAT/SIGMA</TD>
            <TD>The Soviet orbital observatory GRANAT was launched in December 1989 and was operational till November 1998. One of the main instruments of the observatory was the French-Soviet hard X-ray coded mask telescope SIGMA (Paul et al.1 1991, Adv.Space Res., 11, 279). It was the first space telescope that used coded aperture technique for reconstruction of sky images in hard X-rays (35-1300 keV). The angular resolution of the telescope was approximately 12' and the accuracy of a source localization is approximately 2-3'.&lt;p&gt; SIGMA discovered numerious interesting hard X-ray sources including GRS 1758-258, which is located only 40' from bright soft X-ray source GX 5-1. It detected hard X-ray flux from X-ray burster A1742-294, which is very near to bright black hole binary 1E1740.7-2942. SIGMA set an upper limit on the hard X-ray flux of from the central supermassive black hole in our Galaxy.&lt;p&gt; During the period 1990-1998 SIGMA observed more that one quarter of the sky with sensitivity better than 100 mCrab. The Galactic Center region had the deepest exposure ( approximately 9 million sec), with the sensitivity to a source discovery (S/N &amp;amp;gt; ~ 5) or approximately 10 mCrab.&lt;p&gt; A list of all detected sources with references to publications on them is presented in the paper of Revnivtsev et al. 2004, Astr. Lett. v.6. In these survey images (40-100 keV) all performed observations are averaged together. Transient sources that were discovered by SIGMA may not visible in the averaged image. &lt;p&gt; This survey has some features that users should keep in mind. The SIGMA telescope is a complicated instrument and is strongly dominated by the accuracy of the background subtraction. The presence of a very bright source in the field of view of the telescope sometimes can not be fully accounted for and as a result of it some 'ghost' sources can appear. Such features can be seen in the regions near very bright sources like Crab Nebula, Cyg X-1, Nova Per 1992, Nova Mus 1991, Nova Oph 1993, and in the Galactic Center region. In addition to its nominal field of view (~17x17 deg) located around the optical axis of the telescope, SIGMA had another window of relatively high transparency of its shield, approximately 20-30&amp;amp;amp;#176; apart from the optical axis. Becuase of this a very bright sources like Cyg X-1 can cause non zero illumination of the SIGMA detector if they are located approximately 20-30&amp;amp;amp;#176; from the optical axis. The ring-like features caused by this effect, can be seen around Cyg X-1, and Nova Per 1992. &lt;p&gt; The count rate of detected sources (or upper limits) can be roughly translated into mCrab using the fact that that Crab nebula gives the count rate approximately 2.8e&lt;sup&gt;-3&lt;/sup&gt; cnts/s in the units, provided in 'flux' maps</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/skyview/granat#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/granat</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=granat&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GRANAT [2]</TD>
            <TD>GRANAT/SIGMA</TD>
            <TD>The Soviet orbital observatory GRANAT was launched in December 1989 and was operational till November 1998. One of the main instruments of the observatory was the French-Soviet hard X-ray coded mask telescope SIGMA (Paul et al.1 1991, Adv.Space Res., 11, 279). It was the first space telescope that used coded aperture technique for reconstruction of sky images in hard X-rays (35-1300 keV). The angular resolution of the telescope was approximately 12' and the accuracy of a source localization is approximately 2-3'.&lt;p&gt; SIGMA discovered numerious interesting hard X-ray sources including GRS 1758-258, which is located only 40' from bright soft X-ray source GX 5-1. It detected hard X-ray flux from X-ray burster A1742-294, which is very near to bright black hole binary 1E1740.7-2942. SIGMA set an upper limit on the hard X-ray flux of from the central supermassive black hole in our Galaxy.&lt;p&gt; During the period 1990-1998 SIGMA observed more that one quarter of the sky with sensitivity better than 100 mCrab. The Galactic Center region had the deepest exposure ( approximately 9 million sec), with the sensitivity to a source discovery (S/N &amp;amp;gt; ~ 5) or approximately 10 mCrab.&lt;p&gt; A list of all detected sources with references to publications on them is presented in the paper of Revnivtsev et al. 2004, Astr. Lett. v.6. In these survey images (40-100 keV) all performed observations are averaged together. Transient sources that were discovered by SIGMA may not visible in the averaged image. &lt;p&gt; This survey has some features that users should keep in mind. The SIGMA telescope is a complicated instrument and is strongly dominated by the accuracy of the background subtraction. The presence of a very bright source in the field of view of the telescope sometimes can not be fully accounted for and as a result of it some 'ghost' sources can appear. Such features can be seen in the regions near very bright sources like Crab Nebula, Cyg X-1, Nova Per 1992, Nova Mus 1991, Nova Oph 1993, and in the Galactic Center region. In addition to its nominal field of view (~17x17 deg) located around the optical axis of the telescope, SIGMA had another window of relatively high transparency of its shield, approximately 20-30&amp;amp;amp;#176; apart from the optical axis. Becuase of this a very bright sources like Cyg X-1 can cause non zero illumination of the SIGMA detector if they are located approximately 20-30&amp;amp;amp;#176; from the optical axis. The ring-like features caused by this effect, can be seen around Cyg X-1, and Nova Per 1992. &lt;p&gt; The count rate of detected sources (or upper limits) can be roughly translated into mCrab using the fact that that Crab nebula gives the count rate approximately 2.8e&lt;sup&gt;-3&lt;/sup&gt; cnts/s in the units, provided in 'flux' maps</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/skyview/granat#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/231 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. V. (Abraham+ 1998)</TD>
            <TD>Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters: MS 1224.7+2007 (z=0.327) and MS 1512.4+3647 (z=0.372) are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations span three contiguous MOS fields in the east-west direction for MS 1512.4+3647, covering a total area of approximately 8.0'x27.3'. A single field of 7.1'x9.0' was obtained for MS 1224.7+2007. Redshifts for 287 galaxies in the MS 1512.4+3647 fields and 75 galaxies in the MS 1224.7+2007 field (primarily ranging in magnitude from r=18-22) were obtained. The spectroscopic information in this paper is supplemented by photometric information for all galaxies in the fields down to Gunn r=21mag. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/ApJS/116/231#1</TD>
            <TD>2011-09-14T18:48:07Z</TD>
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            <TD>12-Aug-1998</TD>
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            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/231</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/231</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/231 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. V. (Abraham+ 1998)</TD>
            <TD>Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters: MS 1224.7+2007 (z=0.327) and MS 1512.4+3647 (z=0.372) are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations span three contiguous MOS fields in the east-west direction for MS 1512.4+3647, covering a total area of approximately 8.0'x27.3'. A single field of 7.1'x9.0' was obtained for MS 1224.7+2007. Redshifts for 287 galaxies in the MS 1512.4+3647 fields and 75 galaxies in the MS 1224.7+2007 field (primarily ranging in magnitude from r=18-22) were obtained. The spectroscopic information in this paper is supplemented by photometric information for all galaxies in the fields down to Gunn r=21mag. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/231#2</TD>
            <TD>2011-09-14T18:48:07Z</TD>
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            <TD>ivo://CDS.VizieR/J/ApJS/116/231</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/231</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/516 [1]</TD>
            <TD>Gas content of star-forming galaxies (Pflamm-Altenburg+, 2009)</TD>
            <TD>Stars do not form continuously distributed over star-forming galaxies. They form in star clusters of different masses. This nature of clustered star formation is taken into account in the theory of the integrated galactic stellar initial mass function (IGIMF) in which the galaxy-wide initial mass function (IMF) on galaxy-wide scales is calculated by adding all IMFs of young star clusters. For massive stars, the IGIMF is steeper than the universal IMF in star clusters and steepens with decreasing star formation rate (SFR) which is called the IGIMF effect. The current SFR and the total H{alpha} luminosity of galaxies therefore scale nonlinearly in the IGIMF theory compared to the classical case in which the galaxy-wide IMF is assumed to be constant and identical to the IMF in star clusters. Here we apply for the first time the revised SFR-L_H{alpha}_ relation on a sample of local volume star-forming galaxies with measured H{alpha} luminosities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516#1</TD>
            <TD>2012-01-28T12:46:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>09-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516</TD>
            <TD />
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/516</TD>
            <TD />
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/516</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/516 [2]</TD>
            <TD>Gas content of star-forming galaxies (Pflamm-Altenburg+, 2009)</TD>
            <TD>Stars do not form continuously distributed over star-forming galaxies. They form in star clusters of different masses. This nature of clustered star formation is taken into account in the theory of the integrated galactic stellar initial mass function (IGIMF) in which the galaxy-wide initial mass function (IMF) on galaxy-wide scales is calculated by adding all IMFs of young star clusters. For massive stars, the IGIMF is steeper than the universal IMF in star clusters and steepens with decreasing star formation rate (SFR) which is called the IGIMF effect. The current SFR and the total H{alpha} luminosity of galaxies therefore scale nonlinearly in the IGIMF theory compared to the classical case in which the galaxy-wide IMF is assumed to be constant and identical to the IMF in star clusters. Here we apply for the first time the revised SFR-L_H{alpha}_ relation on a sample of local volume star-forming galaxies with measured H{alpha} luminosities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516#2</TD>
            <TD>2012-01-28T12:46:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/516 [table1]</TD>
            <TD>Gas content of star-forming galaxies (Pflamm-Altenburg+, 2009)</TD>
            <TD>Stars do not form continuously distributed over star-forming galaxies. They form in star clusters of different masses. This nature of clustered star formation is taken into account in the theory of the integrated galactic stellar initial mass function (IGIMF) in which the galaxy-wide initial mass function (IMF) on galaxy-wide scales is calculated by adding all IMFs of young star clusters. For massive stars, the IGIMF is steeper than the universal IMF in star clusters and steepens with decreasing star formation rate (SFR) which is called the IGIMF effect. The current SFR and the total H{alpha} luminosity of galaxies therefore scale nonlinearly in the IGIMF theory compared to the classical case in which the galaxy-wide IMF is assumed to be constant and identical to the IMF in star clusters. Here we apply for the first time the revised SFR-L_H{alpha}_ relation on a sample of local volume star-forming galaxies with measured H{alpha} luminosities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516#table1</TD>
            <TD>2012-01-28T12:46:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>180</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/516</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/516 [1]</TD>
            <TD>Gas content of star-forming galaxies (Pflamm-Altenburg+, 2009)</TD>
            <TD>Stars do not form continuously distributed over star-forming galaxies. They form in star clusters of different masses. This nature of clustered star formation is taken into account in the theory of the integrated galactic stellar initial mass function (IGIMF) in which the galaxy-wide initial mass function (IMF) on galaxy-wide scales is calculated by adding all IMFs of young star clusters. For massive stars, the IGIMF is steeper than the universal IMF in star clusters and steepens with decreasing star formation rate (SFR) which is called the IGIMF effect. The current SFR and the total H{alpha} luminosity of galaxies therefore scale nonlinearly in the IGIMF theory compared to the classical case in which the galaxy-wide IMF is assumed to be constant and identical to the IMF in star clusters. Here we apply for the first time the revised SFR-L_H{alpha}_ relation on a sample of local volume star-forming galaxies with measured H{alpha} luminosities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516#1</TD>
            <TD>2012-01-28T12:46:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/516</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/516</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/516 [2]</TD>
            <TD>Gas content of star-forming galaxies (Pflamm-Altenburg+, 2009)</TD>
            <TD>Stars do not form continuously distributed over star-forming galaxies. They form in star clusters of different masses. This nature of clustered star formation is taken into account in the theory of the integrated galactic stellar initial mass function (IGIMF) in which the galaxy-wide initial mass function (IMF) on galaxy-wide scales is calculated by adding all IMFs of young star clusters. For massive stars, the IGIMF is steeper than the universal IMF in star clusters and steepens with decreasing star formation rate (SFR) which is called the IGIMF effect. The current SFR and the total H{alpha} luminosity of galaxies therefore scale nonlinearly in the IGIMF theory compared to the classical case in which the galaxy-wide IMF is assumed to be constant and identical to the IMF in star clusters. Here we apply for the first time the revised SFR-L_H{alpha}_ relation on a sample of local volume star-forming galaxies with measured H{alpha} luminosities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516#2</TD>
            <TD>2012-01-28T12:46:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/516&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/516</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/516 [table1]</TD>
            <TD>Gas content of star-forming galaxies (Pflamm-Altenburg+, 2009)</TD>
            <TD>Stars do not form continuously distributed over star-forming galaxies. They form in star clusters of different masses. This nature of clustered star formation is taken into account in the theory of the integrated galactic stellar initial mass function (IGIMF) in which the galaxy-wide initial mass function (IMF) on galaxy-wide scales is calculated by adding all IMFs of young star clusters. For massive stars, the IGIMF is steeper than the universal IMF in star clusters and steepens with decreasing star formation rate (SFR) which is called the IGIMF effect. The current SFR and the total H{alpha} luminosity of galaxies therefore scale nonlinearly in the IGIMF theory compared to the classical case in which the galaxy-wide IMF is assumed to be constant and identical to the IMF in star clusters. Here we apply for the first time the revised SFR-L_H{alpha}_ relation on a sample of local volume star-forming galaxies with measured H{alpha} luminosities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516#table1</TD>
            <TD>2012-01-28T12:46:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/516&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/516</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/516 [1]</TD>
            <TD>Gas content of star-forming galaxies (Pflamm-Altenburg+, 2009)</TD>
            <TD>Stars do not form continuously distributed over star-forming galaxies. They form in star clusters of different masses. This nature of clustered star formation is taken into account in the theory of the integrated galactic stellar initial mass function (IGIMF) in which the galaxy-wide initial mass function (IMF) on galaxy-wide scales is calculated by adding all IMFs of young star clusters. For massive stars, the IGIMF is steeper than the universal IMF in star clusters and steepens with decreasing star formation rate (SFR) which is called the IGIMF effect. The current SFR and the total H{alpha} luminosity of galaxies therefore scale nonlinearly in the IGIMF theory compared to the classical case in which the galaxy-wide IMF is assumed to be constant and identical to the IMF in star clusters. Here we apply for the first time the revised SFR-L_H{alpha}_ relation on a sample of local volume star-forming galaxies with measured H{alpha} luminosities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516#1</TD>
            <TD>2012-01-28T12:46:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/516</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/516</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/516 [2]</TD>
            <TD>Gas content of star-forming galaxies (Pflamm-Altenburg+, 2009)</TD>
            <TD>Stars do not form continuously distributed over star-forming galaxies. They form in star clusters of different masses. This nature of clustered star formation is taken into account in the theory of the integrated galactic stellar initial mass function (IGIMF) in which the galaxy-wide initial mass function (IMF) on galaxy-wide scales is calculated by adding all IMFs of young star clusters. For massive stars, the IGIMF is steeper than the universal IMF in star clusters and steepens with decreasing star formation rate (SFR) which is called the IGIMF effect. The current SFR and the total H{alpha} luminosity of galaxies therefore scale nonlinearly in the IGIMF theory compared to the classical case in which the galaxy-wide IMF is assumed to be constant and identical to the IMF in star clusters. Here we apply for the first time the revised SFR-L_H{alpha}_ relation on a sample of local volume star-forming galaxies with measured H{alpha} luminosities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516#2</TD>
            <TD>2012-01-28T12:46:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/516&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/516</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/516 [table1]</TD>
            <TD>Gas content of star-forming galaxies (Pflamm-Altenburg+, 2009)</TD>
            <TD>Stars do not form continuously distributed over star-forming galaxies. They form in star clusters of different masses. This nature of clustered star formation is taken into account in the theory of the integrated galactic stellar initial mass function (IGIMF) in which the galaxy-wide initial mass function (IMF) on galaxy-wide scales is calculated by adding all IMFs of young star clusters. For massive stars, the IGIMF is steeper than the universal IMF in star clusters and steepens with decreasing star formation rate (SFR) which is called the IGIMF effect. The current SFR and the total H{alpha} luminosity of galaxies therefore scale nonlinearly in the IGIMF theory compared to the classical case in which the galaxy-wide IMF is assumed to be constant and identical to the IMF in star clusters. Here we apply for the first time the revised SFR-L_H{alpha}_ relation on a sample of local volume star-forming galaxies with measured H{alpha} luminosities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516#table1</TD>
            <TD>2012-01-28T12:46:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/516</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/516&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/516</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/599 [1]</TD>
            <TD>H{alpha} and UV SFR in the local volume (Lee+, 2009)</TD>
            <TD>Using a complete sample of ~300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and H{alpha} nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ~10^-4^M_{sun}_/yr. The data are drawn from the 11Mpc H{alpha} and Ultraviolet Galaxy Survey (11HUGS), which has obtained H{alpha} fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599#1</TD>
            <TD>2012-01-28T15:29:43Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/599</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/599</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/599 [2]</TD>
            <TD>H{alpha} and UV SFR in the local volume (Lee+, 2009)</TD>
            <TD>Using a complete sample of ~300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and H{alpha} nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ~10^-4^M_{sun}_/yr. The data are drawn from the 11Mpc H{alpha} and Ultraviolet Galaxy Survey (11HUGS), which has obtained H{alpha} fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599#2</TD>
            <TD>2012-01-28T15:29:43Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/599&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/599</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/599 [table1]</TD>
            <TD>H{alpha} and UV SFR in the local volume (Lee+, 2009)</TD>
            <TD>Using a complete sample of ~300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and H{alpha} nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ~10^-4^M_{sun}_/yr. The data are drawn from the 11Mpc H{alpha} and Ultraviolet Galaxy Survey (11HUGS), which has obtained H{alpha} fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599#table1</TD>
            <TD>2012-01-28T15:29:43Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/599&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/599</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/599 [1]</TD>
            <TD>H{alpha} and UV SFR in the local volume (Lee+, 2009)</TD>
            <TD>Using a complete sample of ~300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and H{alpha} nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ~10^-4^M_{sun}_/yr. The data are drawn from the 11Mpc H{alpha} and Ultraviolet Galaxy Survey (11HUGS), which has obtained H{alpha} fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599#1</TD>
            <TD>2012-01-28T15:29:43Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/599</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/599</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/599 [2]</TD>
            <TD>H{alpha} and UV SFR in the local volume (Lee+, 2009)</TD>
            <TD>Using a complete sample of ~300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and H{alpha} nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ~10^-4^M_{sun}_/yr. The data are drawn from the 11Mpc H{alpha} and Ultraviolet Galaxy Survey (11HUGS), which has obtained H{alpha} fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599#2</TD>
            <TD>2012-01-28T15:29:43Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/599&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/599</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/599 [table1]</TD>
            <TD>H{alpha} and UV SFR in the local volume (Lee+, 2009)</TD>
            <TD>Using a complete sample of ~300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and H{alpha} nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ~10^-4^M_{sun}_/yr. The data are drawn from the 11Mpc H{alpha} and Ultraviolet Galaxy Survey (11HUGS), which has obtained H{alpha} fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599#table1</TD>
            <TD>2012-01-28T15:29:43Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/599&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/599</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/599 [1]</TD>
            <TD>H{alpha} and UV SFR in the local volume (Lee+, 2009)</TD>
            <TD>Using a complete sample of ~300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and H{alpha} nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ~10^-4^M_{sun}_/yr. The data are drawn from the 11Mpc H{alpha} and Ultraviolet Galaxy Survey (11HUGS), which has obtained H{alpha} fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599#1</TD>
            <TD>2012-01-28T15:29:43Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/599</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/599</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/599 [2]</TD>
            <TD>H{alpha} and UV SFR in the local volume (Lee+, 2009)</TD>
            <TD>Using a complete sample of ~300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and H{alpha} nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ~10^-4^M_{sun}_/yr. The data are drawn from the 11Mpc H{alpha} and Ultraviolet Galaxy Survey (11HUGS), which has obtained H{alpha} fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599#2</TD>
            <TD>2012-01-28T15:29:43Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/599&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/599</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/599 [table1]</TD>
            <TD>H{alpha} and UV SFR in the local volume (Lee+, 2009)</TD>
            <TD>Using a complete sample of ~300 star-forming galaxies within 11Mpc of the Milky Way, we evaluate the consistency between star formation rates (SFRs) inferred from the far ultraviolet (FUV) non-ionizing continuum and H{alpha} nebular emission, assuming standard conversion recipes in which the SFR scales linearly with luminosity at a given wavelength. Our analysis probes SFRs over 5 orders of magnitude, down to ultra-low activities on the order of ~10^-4^M_{sun}_/yr. The data are drawn from the 11Mpc H{alpha} and Ultraviolet Galaxy Survey (11HUGS), which has obtained H{alpha} fluxes from ground-based narrowband imaging, and UV fluxes from imaging with GALEX.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599#table1</TD>
            <TD>2012-01-28T15:29:43Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/599</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/599&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/599</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/18 [1]</TD>
            <TD>X-ray sources &lt;1 degree from Seyfert galaxies (Radecke 1997)</TD>
            <TD>Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (&lt; about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04&lt;B^o,i^_T_&lt;12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18#1</TD>
            <TD>2011-09-14T18:15:36Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/18 [2]</TD>
            <TD>X-ray sources &lt;1 degree from Seyfert galaxies (Radecke 1997)</TD>
            <TD>Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (&lt; about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04&lt;B^o,i^_T_&lt;12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18#2</TD>
            <TD>2011-09-14T18:15:36Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/319/18 [appena]</TD>
            <TD>X-ray sources &lt;1 degree from Seyfert galaxies (Radecke 1997)</TD>
            <TD>Archived PSPC observations of 26 Seyfert galaxies have been analyzed for bright X-ray sources out to the full extent of the field (&lt; about 50'). Of all Seyferts known this represents a sample 88% complete to B_T_=10mag, 74% complete to 11mag and 50% complete to 12mag. Using the same reduction algorithm, 14 fields centered on stars at high galactic latitudes have been used as control fields. Excluding the two brightest Seyferts, a subset of 24 Seyferts with corrected apparent magnitude between 8.04&lt;B^o,i^_T_&lt;12.90mag show a minimum excess of 46 bright X-ray sources generally distributed between 10 and 25' from the target galaxy. The significances of association of these sources with the Seyferts in the median brightness range are as high as 7.4-sigma.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18#appena</TD>
            <TD>2011-09-14T18:15:36Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/319/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/697/506 [1]</TD>
            <TD>Mid-infrared galaxy luminosity function from AGN (Dai+, 2009)</TD>
            <TD>We measured the mid-IR galaxy LFs in the NDWFS Bootes field by combining IRAC photometry from the IRAC Shallow Survey and AGES redshifts. This field is also covered by multiwavelength data in the UV (GALEX; Martin et al. 2005ApJ...619L...1M), optical (NDWFS), z-band (zBootes; Cool 2007ApJS..169...21C), near-IR (NDWFS and FLAMEX; Elston et al., 2006, Cat. J/ApJ/639/816), and far-IR (24um; Soifer et al. 2004AAS...204.4805S), allowing us to use spectral energy distribution (SED) models to type the galaxies and make K-corrections.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/506#1</TD>
            <TD>2012-01-29T13:22:49Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/697/506</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/506</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/697/506 [2]</TD>
            <TD>Mid-infrared galaxy luminosity function from AGN (Dai+, 2009)</TD>
            <TD>We measured the mid-IR galaxy LFs in the NDWFS Bootes field by combining IRAC photometry from the IRAC Shallow Survey and AGES redshifts. This field is also covered by multiwavelength data in the UV (GALEX; Martin et al. 2005ApJ...619L...1M), optical (NDWFS), z-band (zBootes; Cool 2007ApJS..169...21C), near-IR (NDWFS and FLAMEX; Elston et al., 2006, Cat. J/ApJ/639/816), and far-IR (24um; Soifer et al. 2004AAS...204.4805S), allowing us to use spectral energy distribution (SED) models to type the galaxies and make K-corrections.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/506#2</TD>
            <TD>2012-01-29T13:22:49Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/697/506&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/506</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/324/904 [1]</TD>
            <TD>NGC 4151 line-continuum diagram sequences (Malkov+ 1997)</TD>
            <TD>We present the first results of an 8-year spectroscopic monitoring of the Seyfert 1.5 galaxy NGC 4151 carried out with a CCD spectrograph at the 2.6-m Shajn Telescope of the Crimean Astrophysical Observatory in 1988-1995. Total of 202 H{ alpha} region spectra and 154 H{beta} region spectra have formed the data set. A ll spectra were calibrated in flux using the narrow emission lines which were as summed to be constant over the duration of the monitoring program.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/904#1</TD>
            <TD>2011-09-14T18:15:59Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/904</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/324/904</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/324/904</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/324/904 [2]</TD>
            <TD>NGC 4151 line-continuum diagram sequences (Malkov+ 1997)</TD>
            <TD>We present the first results of an 8-year spectroscopic monitoring of the Seyfert 1.5 galaxy NGC 4151 carried out with a CCD spectrograph at the 2.6-m Shajn Telescope of the Crimean Astrophysical Observatory in 1988-1995. Total of 202 H{ alpha} region spectra and 154 H{beta} region spectra have formed the data set. A ll spectra were calibrated in flux using the narrow emission lines which were as summed to be constant over the duration of the monitoring program.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/904#2</TD>
            <TD>2011-09-14T18:15:59Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/904</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/324/904&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/324/904</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/697/506 [1]</TD>
            <TD>Mid-infrared galaxy luminosity function from AGN (Dai+, 2009)</TD>
            <TD>We measured the mid-IR galaxy LFs in the NDWFS Bootes field by combining IRAC photometry from the IRAC Shallow Survey and AGES redshifts. This field is also covered by multiwavelength data in the UV (GALEX; Martin et al. 2005ApJ...619L...1M), optical (NDWFS), z-band (zBootes; Cool 2007ApJS..169...21C), near-IR (NDWFS and FLAMEX; Elston et al., 2006, Cat. J/ApJ/639/816), and far-IR (24um; Soifer et al. 2004AAS...204.4805S), allowing us to use spectral energy distribution (SED) models to type the galaxies and make K-corrections.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/506#1</TD>
            <TD>2012-01-29T13:22:49Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/697/506</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/506</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/697/506 [2]</TD>
            <TD>Mid-infrared galaxy luminosity function from AGN (Dai+, 2009)</TD>
            <TD>We measured the mid-IR galaxy LFs in the NDWFS Bootes field by combining IRAC photometry from the IRAC Shallow Survey and AGES redshifts. This field is also covered by multiwavelength data in the UV (GALEX; Martin et al. 2005ApJ...619L...1M), optical (NDWFS), z-band (zBootes; Cool 2007ApJS..169...21C), near-IR (NDWFS and FLAMEX; Elston et al., 2006, Cat. J/ApJ/639/816), and far-IR (24um; Soifer et al. 2004AAS...204.4805S), allowing us to use spectral energy distribution (SED) models to type the galaxies and make K-corrections.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/506#2</TD>
            <TD>2012-01-29T13:22:49Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/697/506&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/506</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/537/A141 [1]</TD>
            <TD>SN2009E UBVRI light curves (Pastorello+, 2012)</TD>
            <TD>1987A-like events form a rare sub-group of hydrogen-rich core-collapse supernovae that are thought to originate from the explosion of blue supergiant stars. Although SN 1987A is the best known supernova, very few objects of this group have been discovered and, hence, studied. In this paper we investigate the properties of SN 2009E, which exploded in a relatively nearby spiral galaxy (NGC 4141) and that is probably the faintest 1987A-like supernova discovered so far. We also attempt to characterize this subgroup of core-collapse supernovae with the help of the literature and present new data for a few additional objects. The lack of early-time observations from professional telescopes is compensated by frequent follow-up observations performed by a number of amateur astronomers. This allows us to reconstruct a well-sampled light curve for SN 2009E. Spectroscopic observations which started about 2 months after the supernova explosion, highlight significant differences between SN 2009E and the prototypical SN 1987A. Modelling the data of SN 2009E allows us to constrain the explosion parameters and the properties of the progenitor star, and compare the inferred estimates with those available for the similar SNe 1987A and 1998A. The light curve of SN 2009E is less luminous than that of SN 1987A and the other members of this class, and the maximum light curve peak is reached at a slightly later epoch than in SN 1987A. Late-time photometric observations suggest that SN 2009E ejected about 0.04M_{sun}_ of ^56^Ni, which is the smallest ^56^Ni mass in our sample of 1987A-like events. Modelling the observations with a radiation hydrodynamics code, we infer for SN 2009E a kinetic plus thermal energy of about 0.6 foe, an initial radius of ~7x10^12^cm and an ejected mass of ~19M_{sun}_. The photospheric spectra show a number of narrow (v~1800km/s) metal lines, with unusually strong BaII lines. The nebular spectrum displays narrow emission lines of H, NaI, [CaII] and [OI], with the [OI] feature being relatively strong compared to the [CaII] doublet. The overall spectroscopic evolution is reminiscent of that of the faint ^56^Ni-poor type II-plateau supernovae. This suggests that SN 2009E belongs to the low-luminosity, low ^56^Ni mass, low-energy tail in the distribution of the 1987A-like objects in the same manner as SN 1997D and similar events represent the faint tail in the distribution of physical properties for normal type II-plateau supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/537/A141#1</TD>
            <TD>2012-01-24T10:07:23Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/537/A141</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/537/A141</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/537/A141</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/537/A141 [2]</TD>
            <TD>SN2009E UBVRI light curves (Pastorello+, 2012)</TD>
            <TD>1987A-like events form a rare sub-group of hydrogen-rich core-collapse supernovae that are thought to originate from the explosion of blue supergiant stars. Although SN 1987A is the best known supernova, very few objects of this group have been discovered and, hence, studied. In this paper we investigate the properties of SN 2009E, which exploded in a relatively nearby spiral galaxy (NGC 4141) and that is probably the faintest 1987A-like supernova discovered so far. We also attempt to characterize this subgroup of core-collapse supernovae with the help of the literature and present new data for a few additional objects. The lack of early-time observations from professional telescopes is compensated by frequent follow-up observations performed by a number of amateur astronomers. This allows us to reconstruct a well-sampled light curve for SN 2009E. Spectroscopic observations which started about 2 months after the supernova explosion, highlight significant differences between SN 2009E and the prototypical SN 1987A. Modelling the data of SN 2009E allows us to constrain the explosion parameters and the properties of the progenitor star, and compare the inferred estimates with those available for the similar SNe 1987A and 1998A. The light curve of SN 2009E is less luminous than that of SN 1987A and the other members of this class, and the maximum light curve peak is reached at a slightly later epoch than in SN 1987A. Late-time photometric observations suggest that SN 2009E ejected about 0.04M_{sun}_ of ^56^Ni, which is the smallest ^56^Ni mass in our sample of 1987A-like events. Modelling the observations with a radiation hydrodynamics code, we infer for SN 2009E a kinetic plus thermal energy of about 0.6 foe, an initial radius of ~7x10^12^cm and an ejected mass of ~19M_{sun}_. The photospheric spectra show a number of narrow (v~1800km/s) metal lines, with unusually strong BaII lines. The nebular spectrum displays narrow emission lines of H, NaI, [CaII] and [OI], with the [OI] feature being relatively strong compared to the [CaII] doublet. The overall spectroscopic evolution is reminiscent of that of the faint ^56^Ni-poor type II-plateau supernovae. This suggests that SN 2009E belongs to the low-luminosity, low ^56^Ni mass, low-energy tail in the distribution of the 1987A-like objects in the same manner as SN 1997D and similar events represent the faint tail in the distribution of physical properties for normal type II-plateau supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/537/A141#2</TD>
            <TD>2012-01-24T10:07:23Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/537/A141</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/537/A141&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/537/A141</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/537/A141 [1]</TD>
            <TD>SN2009E UBVRI light curves (Pastorello+, 2012)</TD>
            <TD>1987A-like events form a rare sub-group of hydrogen-rich core-collapse supernovae that are thought to originate from the explosion of blue supergiant stars. Although SN 1987A is the best known supernova, very few objects of this group have been discovered and, hence, studied. In this paper we investigate the properties of SN 2009E, which exploded in a relatively nearby spiral galaxy (NGC 4141) and that is probably the faintest 1987A-like supernova discovered so far. We also attempt to characterize this subgroup of core-collapse supernovae with the help of the literature and present new data for a few additional objects. The lack of early-time observations from professional telescopes is compensated by frequent follow-up observations performed by a number of amateur astronomers. This allows us to reconstruct a well-sampled light curve for SN 2009E. Spectroscopic observations which started about 2 months after the supernova explosion, highlight significant differences between SN 2009E and the prototypical SN 1987A. Modelling the data of SN 2009E allows us to constrain the explosion parameters and the properties of the progenitor star, and compare the inferred estimates with those available for the similar SNe 1987A and 1998A. The light curve of SN 2009E is less luminous than that of SN 1987A and the other members of this class, and the maximum light curve peak is reached at a slightly later epoch than in SN 1987A. Late-time photometric observations suggest that SN 2009E ejected about 0.04M_{sun}_ of ^56^Ni, which is the smallest ^56^Ni mass in our sample of 1987A-like events. Modelling the observations with a radiation hydrodynamics code, we infer for SN 2009E a kinetic plus thermal energy of about 0.6 foe, an initial radius of ~7x10^12^cm and an ejected mass of ~19M_{sun}_. The photospheric spectra show a number of narrow (v~1800km/s) metal lines, with unusually strong BaII lines. The nebular spectrum displays narrow emission lines of H, NaI, [CaII] and [OI], with the [OI] feature being relatively strong compared to the [CaII] doublet. The overall spectroscopic evolution is reminiscent of that of the faint ^56^Ni-poor type II-plateau supernovae. This suggests that SN 2009E belongs to the low-luminosity, low ^56^Ni mass, low-energy tail in the distribution of the 1987A-like objects in the same manner as SN 1997D and similar events represent the faint tail in the distribution of physical properties for normal type II-plateau supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/537/A141#1</TD>
            <TD>2012-01-24T10:07:23Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/537/A141</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/537/A141</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/537/A141</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/537/A141 [2]</TD>
            <TD>SN2009E UBVRI light curves (Pastorello+, 2012)</TD>
            <TD>1987A-like events form a rare sub-group of hydrogen-rich core-collapse supernovae that are thought to originate from the explosion of blue supergiant stars. Although SN 1987A is the best known supernova, very few objects of this group have been discovered and, hence, studied. In this paper we investigate the properties of SN 2009E, which exploded in a relatively nearby spiral galaxy (NGC 4141) and that is probably the faintest 1987A-like supernova discovered so far. We also attempt to characterize this subgroup of core-collapse supernovae with the help of the literature and present new data for a few additional objects. The lack of early-time observations from professional telescopes is compensated by frequent follow-up observations performed by a number of amateur astronomers. This allows us to reconstruct a well-sampled light curve for SN 2009E. Spectroscopic observations which started about 2 months after the supernova explosion, highlight significant differences between SN 2009E and the prototypical SN 1987A. Modelling the data of SN 2009E allows us to constrain the explosion parameters and the properties of the progenitor star, and compare the inferred estimates with those available for the similar SNe 1987A and 1998A. The light curve of SN 2009E is less luminous than that of SN 1987A and the other members of this class, and the maximum light curve peak is reached at a slightly later epoch than in SN 1987A. Late-time photometric observations suggest that SN 2009E ejected about 0.04M_{sun}_ of ^56^Ni, which is the smallest ^56^Ni mass in our sample of 1987A-like events. Modelling the observations with a radiation hydrodynamics code, we infer for SN 2009E a kinetic plus thermal energy of about 0.6 foe, an initial radius of ~7x10^12^cm and an ejected mass of ~19M_{sun}_. The photospheric spectra show a number of narrow (v~1800km/s) metal lines, with unusually strong BaII lines. The nebular spectrum displays narrow emission lines of H, NaI, [CaII] and [OI], with the [OI] feature being relatively strong compared to the [CaII] doublet. The overall spectroscopic evolution is reminiscent of that of the faint ^56^Ni-poor type II-plateau supernovae. This suggests that SN 2009E belongs to the low-luminosity, low ^56^Ni mass, low-energy tail in the distribution of the 1987A-like objects in the same manner as SN 1997D and similar events represent the faint tail in the distribution of physical properties for normal type II-plateau supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/537/A141#2</TD>
            <TD>2012-01-24T10:07:23Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/537/A141</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/537/A141&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/537/A141</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS_DR2 [1]</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (DR2)</TD>
            <TD>UKIDSS is the next generation near-infrared sky survey, the successor to 2MASS. UKIDSS began in May 2005 and will survey 7500 square degrees of the Northern sky, extending over both high and low Galactic latitudes, in JHK to K=18.3. This depth is three magnitudes deeper than 2MASS. UKIDSS will be the true near-infrared counterpart to the Sloan survey, and will produce as well a panoramic clear atlas of the Galactic plane. In fact UKIDSS is made up of five surveys and includes two deep extra-Galactic elements, one covering 35 square degrees to K=21, and the other reaching K=23 over 0.77 square degrees. The survey instrument is WFCAM on the UK Infrared Telescope (UKIRT) in Hawaii. WFCAM has four 2048x2048 Rockwell devices, at 94% spacing, as illustrated at the top. The pixel scale of 0.4 arcsec gives an exposed solid angle of 0.21 sq. degs. Four of the principal quarry of UKIDSS are: the coolest and nearest brown dwarfs, high-redshift dusty starburst galaxies, elliptical galaxies and galaxy clusters at redshifts 1?z?2, and the highest-redshift quasars, at z=7. UKIDSS aims to discover the nearest object to the Sun (outside the solar system) as well as some of the farthest known objects in the Universe.</TD>
            <TD>JVO</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://jvo/ukidss/dr2#1</TD>
            <TD>2010-08-17T01:24:27Z</TD>
            <TD>#Infrared Sky Survey#</TD>
            <TD>#Catalog#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>DR2</TD>
            <TD>ivo://jvo/ukidss/dr2</TD>
            <TD />
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://jvo.nao.ac.jp/skynode/services/SkyNodeForUKIDSS</TD>
            <TD />
            <TD />
            <TD />
            <TD>http://www.ukidss.org/index.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS_DR2 [2]</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (DR2)</TD>
            <TD>UKIDSS is the next generation near-infrared sky survey, the successor to 2MASS. UKIDSS began in May 2005 and will survey 7500 square degrees of the Northern sky, extending over both high and low Galactic latitudes, in JHK to K=18.3. This depth is three magnitudes deeper than 2MASS. UKIDSS will be the true near-infrared counterpart to the Sloan survey, and will produce as well a panoramic clear atlas of the Galactic plane. In fact UKIDSS is made up of five surveys and includes two deep extra-Galactic elements, one covering 35 square degrees to K=21, and the other reaching K=23 over 0.77 square degrees. The survey instrument is WFCAM on the UK Infrared Telescope (UKIRT) in Hawaii. WFCAM has four 2048x2048 Rockwell devices, at 94% spacing, as illustrated at the top. The pixel scale of 0.4 arcsec gives an exposed solid angle of 0.21 sq. degs. Four of the principal quarry of UKIDSS are: the coolest and nearest brown dwarfs, high-redshift dusty starburst galaxies, elliptical galaxies and galaxy clusters at redshifts 1?z?2, and the highest-redshift quasars, at z=7. UKIDSS aims to discover the nearest object to the Sun (outside the solar system) as well as some of the farthest known objects in the Universe.</TD>
            <TD>JVO</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://jvo/ukidss/dr2#2</TD>
            <TD>2010-08-17T01:24:27Z</TD>
            <TD>#Infrared Sky Survey#</TD>
            <TD>#Catalog#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>DR2</TD>
            <TD>ivo://jvo/ukidss/dr2</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD>1.0</TD>
            <TD>std</TD>
            <TD>http://jvo.nao.ac.jp/skynode/do/tap/ukidss</TD>
            <TD />
            <TD />
            <TD />
            <TD>http://www.ukidss.org/index.html</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS_DR2 [1]</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (DR2)</TD>
            <TD>UKIDSS is the next generation near-infrared sky survey, the successor to 2MASS. UKIDSS began in May 2005 and will survey 7500 square degrees of the Northern sky, extending over both high and low Galactic latitudes, in JHK to K=18.3. This depth is three magnitudes deeper than 2MASS. UKIDSS will be the true near-infrared counterpart to the Sloan survey, and will produce as well a panoramic clear atlas of the Galactic plane. In fact UKIDSS is made up of five surveys and includes two deep extra-Galactic elements, one covering 35 square degrees to K=21, and the other reaching K=23 over 0.77 square degrees. The survey instrument is WFCAM on the UK Infrared Telescope (UKIRT) in Hawaii. WFCAM has four 2048x2048 Rockwell devices, at 94% spacing, as illustrated at the top. The pixel scale of 0.4 arcsec gives an exposed solid angle of 0.21 sq. degs. Four of the principal quarry of UKIDSS are: the coolest and nearest brown dwarfs, high-redshift dusty starburst galaxies, elliptical galaxies and galaxy clusters at redshifts 1?z?2, and the highest-redshift quasars, at z=7. UKIDSS aims to discover the nearest object to the Sun (outside the solar system) as well as some of the farthest known objects in the Universe.</TD>
            <TD>JVO</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://jvo/ukidss/dr2#1</TD>
            <TD>2010-08-17T01:24:27Z</TD>
            <TD>#Infrared Sky Survey#</TD>
            <TD>#Catalog#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>DR2</TD>
            <TD>ivo://jvo/ukidss/dr2</TD>
            <TD />
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://jvo.nao.ac.jp/skynode/services/SkyNodeForUKIDSS</TD>
            <TD />
            <TD />
            <TD />
            <TD>http://www.ukidss.org/index.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS_DR2 [2]</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (DR2)</TD>
            <TD>UKIDSS is the next generation near-infrared sky survey, the successor to 2MASS. UKIDSS began in May 2005 and will survey 7500 square degrees of the Northern sky, extending over both high and low Galactic latitudes, in JHK to K=18.3. This depth is three magnitudes deeper than 2MASS. UKIDSS will be the true near-infrared counterpart to the Sloan survey, and will produce as well a panoramic clear atlas of the Galactic plane. In fact UKIDSS is made up of five surveys and includes two deep extra-Galactic elements, one covering 35 square degrees to K=21, and the other reaching K=23 over 0.77 square degrees. The survey instrument is WFCAM on the UK Infrared Telescope (UKIRT) in Hawaii. WFCAM has four 2048x2048 Rockwell devices, at 94% spacing, as illustrated at the top. The pixel scale of 0.4 arcsec gives an exposed solid angle of 0.21 sq. degs. Four of the principal quarry of UKIDSS are: the coolest and nearest brown dwarfs, high-redshift dusty starburst galaxies, elliptical galaxies and galaxy clusters at redshifts 1?z?2, and the highest-redshift quasars, at z=7. UKIDSS aims to discover the nearest object to the Sun (outside the solar system) as well as some of the farthest known objects in the Universe.</TD>
            <TD>JVO</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://jvo/ukidss/dr2#2</TD>
            <TD>2010-08-17T01:24:27Z</TD>
            <TD>#Infrared Sky Survey#</TD>
            <TD>#Catalog#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>DR2</TD>
            <TD>ivo://jvo/ukidss/dr2</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD>1.0</TD>
            <TD>std</TD>
            <TD>http://jvo.nao.ac.jp/skynode/do/tap/ukidss</TD>
            <TD />
            <TD />
            <TD />
            <TD>http://www.ukidss.org/index.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [1]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#1</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIDEO DR2 [2]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#2</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/DirectCone?DSACAT=VIDEO_DR2&amp;DSATAB=videoDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [3]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#3</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIDEO DR2 [4]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#4</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [5]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#5</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [6]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#6</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [7]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#7</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [8]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#8</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [9]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#9</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [10]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#10</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIDEO DR2 [11]</TD>
            <TD>VIDEO DR2 - VISTA Deep Extragalactic Observations survey</TD>
            <TD>The VIDEO survey is a 30 sq. degree, Z,Y,J,H,K survey that is specifically designed to enable exploration of the main issues in observational cosmology. It allows galaxy and cluster/structure evolution to be traced as a function of both epoch and environment from the present day out to z=4 and AGN/QSO evolution up to and into the epoch of reionization at z &gt; 6. The multi-band nature of the survey ensures many key science drivers can be tackled using the survey alone, without recourse to data from other wavebands.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa#11</TD>
            <TD>2012-07-17T16:13:45Z</TD>
            <TD>#Observational cosmology, galaxy, cluster, evolution, infrared#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/videoDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/videoDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://arxiv.org/abs/1206.4263</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/324/904 [1]</TD>
            <TD>NGC 4151 line-continuum diagram sequences (Malkov+ 1997)</TD>
            <TD>We present the first results of an 8-year spectroscopic monitoring of the Seyfert 1.5 galaxy NGC 4151 carried out with a CCD spectrograph at the 2.6-m Shajn Telescope of the Crimean Astrophysical Observatory in 1988-1995. Total of 202 H{ alpha} region spectra and 154 H{beta} region spectra have formed the data set. A ll spectra were calibrated in flux using the narrow emission lines which were as summed to be constant over the duration of the monitoring program.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/904#1</TD>
            <TD>2011-09-14T18:15:59Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/904</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/324/904</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/324/904</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/324/904 [2]</TD>
            <TD>NGC 4151 line-continuum diagram sequences (Malkov+ 1997)</TD>
            <TD>We present the first results of an 8-year spectroscopic monitoring of the Seyfert 1.5 galaxy NGC 4151 carried out with a CCD spectrograph at the 2.6-m Shajn Telescope of the Crimean Astrophysical Observatory in 1988-1995. Total of 202 H{ alpha} region spectra and 154 H{beta} region spectra have formed the data set. A ll spectra were calibrated in flux using the narrow emission lines which were as summed to be constant over the duration of the monitoring program.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/904#2</TD>
            <TD>2011-09-14T18:15:59Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/904</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/324/904&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/324/904</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/539/577 [1]</TD>
            <TD>Galaxy morphologies in Cl 1358+62 (Fabricant+, 2000)</TD>
            <TD>We describe the morphological composition of a sample of 518 galaxies in the field of Cl 1358+62 at z=0.33, drawn from a large Hubble Space Telescope mosaic covering 53 square arcminutes. The sample is complete to I=22, corresponding to M_V_=-18.5 in the rest frame. The galaxy morphologies have been independently classified by the authors of this paper and by Alan Dressler. Dressler's classifications place our work in context with the previous MORPHS study and allow us to estimate the scatter between different sets of visual classifications. We restrict most of our analysis to the brighter part of the sample, I&lt;21 (M_V_&lt;-19.5), where the scatter between the two sets of classifications is 1 in morphological type.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577#1</TD>
            <TD>2011-09-14T20:23:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/539/577</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/577</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/539/577 [2]</TD>
            <TD>Galaxy morphologies in Cl 1358+62 (Fabricant+, 2000)</TD>
            <TD>We describe the morphological composition of a sample of 518 galaxies in the field of Cl 1358+62 at z=0.33, drawn from a large Hubble Space Telescope mosaic covering 53 square arcminutes. The sample is complete to I=22, corresponding to M_V_=-18.5 in the rest frame. The galaxy morphologies have been independently classified by the authors of this paper and by Alan Dressler. Dressler's classifications place our work in context with the previous MORPHS study and allow us to estimate the scatter between different sets of visual classifications. We restrict most of our analysis to the brighter part of the sample, I&lt;21 (M_V_&lt;-19.5), where the scatter between the two sets of classifications is 1 in morphological type.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577#2</TD>
            <TD>2011-09-14T20:23:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/539/577&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/577</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/539/577 [table2]</TD>
            <TD>Galaxy morphologies in Cl 1358+62 (Fabricant+, 2000)</TD>
            <TD>We describe the morphological composition of a sample of 518 galaxies in the field of Cl 1358+62 at z=0.33, drawn from a large Hubble Space Telescope mosaic covering 53 square arcminutes. The sample is complete to I=22, corresponding to M_V_=-18.5 in the rest frame. The galaxy morphologies have been independently classified by the authors of this paper and by Alan Dressler. Dressler's classifications place our work in context with the previous MORPHS study and allow us to estimate the scatter between different sets of visual classifications. We restrict most of our analysis to the brighter part of the sample, I&lt;21 (M_V_&lt;-19.5), where the scatter between the two sets of classifications is 1 in morphological type.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577#table2</TD>
            <TD>2011-09-14T20:23:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/539/577&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/577</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/110/131 [1]</TD>
            <TD>Mixed pairs of galaxies. I. (Rampazzo+, 1995)</TD>
            <TD>We present data from a kinematic and photometric study of six mixed pairs. High resolution rotation and velocity dispersion curves, for both gas and stellar components, are presented. Slit orientations were along the major axis of the spiral and, in most of the cases, along the line connecting the galaxy nuclei. B and V luminosity and geometrical profiles and photometric parameters including effective radius and disk scale length are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/131#1</TD>
            <TD>2011-09-14T18:17:42Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/110/131</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/131</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/110/131 [2]</TD>
            <TD>Mixed pairs of galaxies. I. (Rampazzo+, 1995)</TD>
            <TD>We present data from a kinematic and photometric study of six mixed pairs. High resolution rotation and velocity dispersion curves, for both gas and stellar components, are presented. Slit orientations were along the major axis of the spiral and, in most of the cases, along the line connecting the galaxy nuclei. B and V luminosity and geometrical profiles and photometric parameters including effective radius and disk scale length are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/131#2</TD>
            <TD>2011-09-14T18:17:42Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/110/131&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/131</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/539/577 [1]</TD>
            <TD>Galaxy morphologies in Cl 1358+62 (Fabricant+, 2000)</TD>
            <TD>We describe the morphological composition of a sample of 518 galaxies in the field of Cl 1358+62 at z=0.33, drawn from a large Hubble Space Telescope mosaic covering 53 square arcminutes. The sample is complete to I=22, corresponding to M_V_=-18.5 in the rest frame. The galaxy morphologies have been independently classified by the authors of this paper and by Alan Dressler. Dressler's classifications place our work in context with the previous MORPHS study and allow us to estimate the scatter between different sets of visual classifications. We restrict most of our analysis to the brighter part of the sample, I&lt;21 (M_V_&lt;-19.5), where the scatter between the two sets of classifications is 1 in morphological type.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577#1</TD>
            <TD>2011-09-14T20:23:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/539/577</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/577</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/539/577 [2]</TD>
            <TD>Galaxy morphologies in Cl 1358+62 (Fabricant+, 2000)</TD>
            <TD>We describe the morphological composition of a sample of 518 galaxies in the field of Cl 1358+62 at z=0.33, drawn from a large Hubble Space Telescope mosaic covering 53 square arcminutes. The sample is complete to I=22, corresponding to M_V_=-18.5 in the rest frame. The galaxy morphologies have been independently classified by the authors of this paper and by Alan Dressler. Dressler's classifications place our work in context with the previous MORPHS study and allow us to estimate the scatter between different sets of visual classifications. We restrict most of our analysis to the brighter part of the sample, I&lt;21 (M_V_&lt;-19.5), where the scatter between the two sets of classifications is 1 in morphological type.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577#2</TD>
            <TD>2011-09-14T20:23:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/539/577&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/577</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/539/577 [table2]</TD>
            <TD>Galaxy morphologies in Cl 1358+62 (Fabricant+, 2000)</TD>
            <TD>We describe the morphological composition of a sample of 518 galaxies in the field of Cl 1358+62 at z=0.33, drawn from a large Hubble Space Telescope mosaic covering 53 square arcminutes. The sample is complete to I=22, corresponding to M_V_=-18.5 in the rest frame. The galaxy morphologies have been independently classified by the authors of this paper and by Alan Dressler. Dressler's classifications place our work in context with the previous MORPHS study and allow us to estimate the scatter between different sets of visual classifications. We restrict most of our analysis to the brighter part of the sample, I&lt;21 (M_V_&lt;-19.5), where the scatter between the two sets of classifications is 1 in morphological type.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577#table2</TD>
            <TD>2011-09-14T20:23:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/577</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/539/577&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/577</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/500/714 [1]</TD>
            <TD>Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998)</TD>
            <TD>We use a large, multicolor mosaic of HST WFPC2 images to measure the colors and morphologies of 194 spectroscopically confirmed members of the rich galaxy cluster CL 1358+62 at z=0.33. We study the color-magnitude (CM) relation as a function of radius in the cluster to a limit of 4.6' from the center, equivalent to 1.6h^-1^_50_Mpc. The intrinsic scatter in the rest-frame B-V CM relation of the elliptical galaxies is very small, ~0.022mag. The CM relation of the ellipticals does not depend significantly on the distance from the cluster center. In contrast, the CM relation for the S0 galaxies does depend on radius: the S0's in the core follow a CM relation similar to that of the ellipticals, but at large radii (R&gt;0.7h^-1^_50_Mpc) the S0's are systematically bluer and the scatter in the CM relation approximately doubles, to ~0.043mag. The blueing of the S0's at large radii is significant at the 95% confidence level. These results imply that the S0 galaxies in the outer parts of the cluster have formed stars more recently than the S0's in the inner parts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714#1</TD>
            <TD>2011-09-14T20:23:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/500/714</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/714</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/500/714 [2]</TD>
            <TD>Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998)</TD>
            <TD>We use a large, multicolor mosaic of HST WFPC2 images to measure the colors and morphologies of 194 spectroscopically confirmed members of the rich galaxy cluster CL 1358+62 at z=0.33. We study the color-magnitude (CM) relation as a function of radius in the cluster to a limit of 4.6' from the center, equivalent to 1.6h^-1^_50_Mpc. The intrinsic scatter in the rest-frame B-V CM relation of the elliptical galaxies is very small, ~0.022mag. The CM relation of the ellipticals does not depend significantly on the distance from the cluster center. In contrast, the CM relation for the S0 galaxies does depend on radius: the S0's in the core follow a CM relation similar to that of the ellipticals, but at large radii (R&gt;0.7h^-1^_50_Mpc) the S0's are systematically bluer and the scatter in the CM relation approximately doubles, to ~0.043mag. The blueing of the S0's at large radii is significant at the 95% confidence level. These results imply that the S0 galaxies in the outer parts of the cluster have formed stars more recently than the S0's in the inner parts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714#2</TD>
            <TD>2011-09-14T20:23:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/500/714&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/500/714 [table1]</TD>
            <TD>Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998)</TD>
            <TD>We use a large, multicolor mosaic of HST WFPC2 images to measure the colors and morphologies of 194 spectroscopically confirmed members of the rich galaxy cluster CL 1358+62 at z=0.33. We study the color-magnitude (CM) relation as a function of radius in the cluster to a limit of 4.6' from the center, equivalent to 1.6h^-1^_50_Mpc. The intrinsic scatter in the rest-frame B-V CM relation of the elliptical galaxies is very small, ~0.022mag. The CM relation of the ellipticals does not depend significantly on the distance from the cluster center. In contrast, the CM relation for the S0 galaxies does depend on radius: the S0's in the core follow a CM relation similar to that of the ellipticals, but at large radii (R&gt;0.7h^-1^_50_Mpc) the S0's are systematically bluer and the scatter in the CM relation approximately doubles, to ~0.043mag. The blueing of the S0's at large radii is significant at the 95% confidence level. These results imply that the S0 galaxies in the outer parts of the cluster have formed stars more recently than the S0's in the inner parts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714#table1</TD>
            <TD>2011-09-14T20:23:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/500/714&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/500/714 [1]</TD>
            <TD>Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998)</TD>
            <TD>We use a large, multicolor mosaic of HST WFPC2 images to measure the colors and morphologies of 194 spectroscopically confirmed members of the rich galaxy cluster CL 1358+62 at z=0.33. We study the color-magnitude (CM) relation as a function of radius in the cluster to a limit of 4.6' from the center, equivalent to 1.6h^-1^_50_Mpc. The intrinsic scatter in the rest-frame B-V CM relation of the elliptical galaxies is very small, ~0.022mag. The CM relation of the ellipticals does not depend significantly on the distance from the cluster center. In contrast, the CM relation for the S0 galaxies does depend on radius: the S0's in the core follow a CM relation similar to that of the ellipticals, but at large radii (R&gt;0.7h^-1^_50_Mpc) the S0's are systematically bluer and the scatter in the CM relation approximately doubles, to ~0.043mag. The blueing of the S0's at large radii is significant at the 95% confidence level. These results imply that the S0 galaxies in the outer parts of the cluster have formed stars more recently than the S0's in the inner parts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714#1</TD>
            <TD>2011-09-14T20:23:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/500/714</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/714</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/500/714 [2]</TD>
            <TD>Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998)</TD>
            <TD>We use a large, multicolor mosaic of HST WFPC2 images to measure the colors and morphologies of 194 spectroscopically confirmed members of the rich galaxy cluster CL 1358+62 at z=0.33. We study the color-magnitude (CM) relation as a function of radius in the cluster to a limit of 4.6' from the center, equivalent to 1.6h^-1^_50_Mpc. The intrinsic scatter in the rest-frame B-V CM relation of the elliptical galaxies is very small, ~0.022mag. The CM relation of the ellipticals does not depend significantly on the distance from the cluster center. In contrast, the CM relation for the S0 galaxies does depend on radius: the S0's in the core follow a CM relation similar to that of the ellipticals, but at large radii (R&gt;0.7h^-1^_50_Mpc) the S0's are systematically bluer and the scatter in the CM relation approximately doubles, to ~0.043mag. The blueing of the S0's at large radii is significant at the 95% confidence level. These results imply that the S0 galaxies in the outer parts of the cluster have formed stars more recently than the S0's in the inner parts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714#2</TD>
            <TD>2011-09-14T20:23:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/500/714&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/500/714 [table1]</TD>
            <TD>Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998)</TD>
            <TD>We use a large, multicolor mosaic of HST WFPC2 images to measure the colors and morphologies of 194 spectroscopically confirmed members of the rich galaxy cluster CL 1358+62 at z=0.33. We study the color-magnitude (CM) relation as a function of radius in the cluster to a limit of 4.6' from the center, equivalent to 1.6h^-1^_50_Mpc. The intrinsic scatter in the rest-frame B-V CM relation of the elliptical galaxies is very small, ~0.022mag. The CM relation of the ellipticals does not depend significantly on the distance from the cluster center. In contrast, the CM relation for the S0 galaxies does depend on radius: the S0's in the core follow a CM relation similar to that of the ellipticals, but at large radii (R&gt;0.7h^-1^_50_Mpc) the S0's are systematically bluer and the scatter in the CM relation approximately doubles, to ~0.043mag. The blueing of the S0's at large radii is significant at the 95% confidence level. These results imply that the S0 galaxies in the outer parts of the cluster have formed stars more recently than the S0's in the inner parts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714#table1</TD>
            <TD>2011-09-14T20:23:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/500/714&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/714</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/110/131 [1]</TD>
            <TD>Mixed pairs of galaxies. I. (Rampazzo+, 1995)</TD>
            <TD>We present data from a kinematic and photometric study of six mixed pairs. High resolution rotation and velocity dispersion curves, for both gas and stellar components, are presented. Slit orientations were along the major axis of the spiral and, in most of the cases, along the line connecting the galaxy nuclei. B and V luminosity and geometrical profiles and photometric parameters including effective radius and disk scale length are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/131#1</TD>
            <TD>2011-09-14T18:17:42Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/110/131</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/131</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/110/131 [2]</TD>
            <TD>Mixed pairs of galaxies. I. (Rampazzo+, 1995)</TD>
            <TD>We present data from a kinematic and photometric study of six mixed pairs. High resolution rotation and velocity dispersion curves, for both gas and stellar components, are presented. Slit orientations were along the major axis of the spiral and, in most of the cases, along the line connecting the galaxy nuclei. B and V luminosity and geometrical profiles and photometric parameters including effective radius and disk scale length are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/131#2</TD>
            <TD>2011-09-14T18:17:42Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/110/131&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/500/714 [1]</TD>
            <TD>Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998)</TD>
            <TD>We use a large, multicolor mosaic of HST WFPC2 images to measure the colors and morphologies of 194 spectroscopically confirmed members of the rich galaxy cluster CL 1358+62 at z=0.33. We study the color-magnitude (CM) relation as a function of radius in the cluster to a limit of 4.6' from the center, equivalent to 1.6h^-1^_50_Mpc. The intrinsic scatter in the rest-frame B-V CM relation of the elliptical galaxies is very small, ~0.022mag. The CM relation of the ellipticals does not depend significantly on the distance from the cluster center. In contrast, the CM relation for the S0 galaxies does depend on radius: the S0's in the core follow a CM relation similar to that of the ellipticals, but at large radii (R&gt;0.7h^-1^_50_Mpc) the S0's are systematically bluer and the scatter in the CM relation approximately doubles, to ~0.043mag. The blueing of the S0's at large radii is significant at the 95% confidence level. These results imply that the S0 galaxies in the outer parts of the cluster have formed stars more recently than the S0's in the inner parts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714#1</TD>
            <TD>2011-09-14T20:23:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/500/714</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/714</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/500/714 [2]</TD>
            <TD>Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998)</TD>
            <TD>We use a large, multicolor mosaic of HST WFPC2 images to measure the colors and morphologies of 194 spectroscopically confirmed members of the rich galaxy cluster CL 1358+62 at z=0.33. We study the color-magnitude (CM) relation as a function of radius in the cluster to a limit of 4.6' from the center, equivalent to 1.6h^-1^_50_Mpc. The intrinsic scatter in the rest-frame B-V CM relation of the elliptical galaxies is very small, ~0.022mag. The CM relation of the ellipticals does not depend significantly on the distance from the cluster center. In contrast, the CM relation for the S0 galaxies does depend on radius: the S0's in the core follow a CM relation similar to that of the ellipticals, but at large radii (R&gt;0.7h^-1^_50_Mpc) the S0's are systematically bluer and the scatter in the CM relation approximately doubles, to ~0.043mag. The blueing of the S0's at large radii is significant at the 95% confidence level. These results imply that the S0 galaxies in the outer parts of the cluster have formed stars more recently than the S0's in the inner parts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714#2</TD>
            <TD>2011-09-14T20:23:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/500/714&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/500/714 [table1]</TD>
            <TD>Color-magnitude relation in CL 1358+62 (Van Dokkum+ 1998)</TD>
            <TD>We use a large, multicolor mosaic of HST WFPC2 images to measure the colors and morphologies of 194 spectroscopically confirmed members of the rich galaxy cluster CL 1358+62 at z=0.33. We study the color-magnitude (CM) relation as a function of radius in the cluster to a limit of 4.6' from the center, equivalent to 1.6h^-1^_50_Mpc. The intrinsic scatter in the rest-frame B-V CM relation of the elliptical galaxies is very small, ~0.022mag. The CM relation of the ellipticals does not depend significantly on the distance from the cluster center. In contrast, the CM relation for the S0 galaxies does depend on radius: the S0's in the core follow a CM relation similar to that of the ellipticals, but at large radii (R&gt;0.7h^-1^_50_Mpc) the S0's are systematically bluer and the scatter in the CM relation approximately doubles, to ~0.043mag. The blueing of the S0's at large radii is significant at the 95% confidence level. These results imply that the S0 galaxies in the outer parts of the cluster have formed stars more recently than the S0's in the inner parts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714#table1</TD>
            <TD>2011-09-14T20:23:10Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/714</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/500/714&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/714</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/124/559 [1]</TD>
            <TD>VI photometry of dwarf galaxies (Karanchentsev+ 1997)</TD>
            <TD>Tables show the photometry and colour index for the observed galaxy, with the image parameter SHARP. This parameter is a measure of the difference between the observed width of the object and the psf model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/559#1</TD>
            <TD>2011-09-14T18:20:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/124/559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/124/559 [2]</TD>
            <TD>VI photometry of dwarf galaxies (Karanchentsev+ 1997)</TD>
            <TD>Tables show the photometry and colour index for the observed galaxy, with the image parameter SHARP. This parameter is a measure of the difference between the observed width of the object and the psf model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/559#2</TD>
            <TD>2011-09-14T18:20:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/124/559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/559</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>WMAP [1]</TD>
            <TD>WMAP Seven Year Galaxy Removed</TD>
            <TD>These survey represents a combination of the 7-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body. &lt;p&gt; The original data are available at the &lt;http://lambda.gsfc.nasa.gov&gt;LAMBDA archive&lt;/a&gt;. &lt;p&gt; The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the WMAP data. &lt;/p&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/skyview/wmap#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/wmap</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=wmap&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WMAP [2]</TD>
            <TD>WMAP Seven Year Galaxy Removed</TD>
            <TD>These survey represents a combination of the 7-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body. &lt;p&gt; The original data are available at the &lt;http://lambda.gsfc.nasa.gov&gt;LAMBDA archive&lt;/a&gt;. &lt;p&gt; The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the WMAP data. &lt;/p&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/skyview/wmap#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/wmap</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/124/559 [1]</TD>
            <TD>VI photometry of dwarf galaxies (Karanchentsev+ 1997)</TD>
            <TD>Tables show the photometry and colour index for the observed galaxy, with the image parameter SHARP. This parameter is a measure of the difference between the observed width of the object and the psf model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/559#1</TD>
            <TD>2011-09-14T18:20:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/124/559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/124/559 [2]</TD>
            <TD>VI photometry of dwarf galaxies (Karanchentsev+ 1997)</TD>
            <TD>Tables show the photometry and colour index for the observed galaxy, with the image parameter SHARP. This parameter is a measure of the difference between the observed width of the object and the psf model.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/559#2</TD>
            <TD>2011-09-14T18:20:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/124/559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/559</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/125/71 [1]</TD>
            <TD>BVR photometry of 10 ESO/SERC fields (Cunow+ 1997)</TD>
            <TD>For calibration of ESO/SERC survey plates, photometric CCD sequences have been obtained for 10 ESO/SERC fields in the area 10h00m&lt;R.A.&lt;15h30m and -34deg&lt;Decl.&lt;-18deg. In Tables 2 to 20, the catalogue of the CCD sequences is given. It contains B, V and R magnitudes for 117 galaxies and 162 stars with 12.7&lt;V&lt;21.0. Column 2 gives the object type, S for star, G for galaxy. The positions were measured from scans of Schmidt plates with one of the PDS machines at the Astronomisches Institut, Muenster, Germany. Their accuracy is between 0.5 and 1.0arcsec.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71#1</TD>
            <TD>2011-09-14T18:20:32Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/125/71</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/71</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/125/71 [2]</TD>
            <TD>BVR photometry of 10 ESO/SERC fields (Cunow+ 1997)</TD>
            <TD>For calibration of ESO/SERC survey plates, photometric CCD sequences have been obtained for 10 ESO/SERC fields in the area 10h00m&lt;R.A.&lt;15h30m and -34deg&lt;Decl.&lt;-18deg. In Tables 2 to 20, the catalogue of the CCD sequences is given. It contains B, V and R magnitudes for 117 galaxies and 162 stars with 12.7&lt;V&lt;21.0. Column 2 gives the object type, S for star, G for galaxy. The positions were measured from scans of Schmidt plates with one of the PDS machines at the Astronomisches Institut, Muenster, Germany. Their accuracy is between 0.5 and 1.0arcsec.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71#2</TD>
            <TD>2011-09-14T18:20:32Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/125/71&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/71</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/125/71 [tables]</TD>
            <TD>BVR photometry of 10 ESO/SERC fields (Cunow+ 1997)</TD>
            <TD>For calibration of ESO/SERC survey plates, photometric CCD sequences have been obtained for 10 ESO/SERC fields in the area 10h00m&lt;R.A.&lt;15h30m and -34deg&lt;Decl.&lt;-18deg. In Tables 2 to 20, the catalogue of the CCD sequences is given. It contains B, V and R magnitudes for 117 galaxies and 162 stars with 12.7&lt;V&lt;21.0. Column 2 gives the object type, S for star, G for galaxy. The positions were measured from scans of Schmidt plates with one of the PDS machines at the Astronomisches Institut, Muenster, Germany. Their accuracy is between 0.5 and 1.0arcsec.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71#tables</TD>
            <TD>2011-09-14T18:20:32Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/125/71&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/71</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/125/71 [1]</TD>
            <TD>BVR photometry of 10 ESO/SERC fields (Cunow+ 1997)</TD>
            <TD>For calibration of ESO/SERC survey plates, photometric CCD sequences have been obtained for 10 ESO/SERC fields in the area 10h00m&lt;R.A.&lt;15h30m and -34deg&lt;Decl.&lt;-18deg. In Tables 2 to 20, the catalogue of the CCD sequences is given. It contains B, V and R magnitudes for 117 galaxies and 162 stars with 12.7&lt;V&lt;21.0. Column 2 gives the object type, S for star, G for galaxy. The positions were measured from scans of Schmidt plates with one of the PDS machines at the Astronomisches Institut, Muenster, Germany. Their accuracy is between 0.5 and 1.0arcsec.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71#1</TD>
            <TD>2011-09-14T18:20:32Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/125/71</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/71</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/125/71 [2]</TD>
            <TD>BVR photometry of 10 ESO/SERC fields (Cunow+ 1997)</TD>
            <TD>For calibration of ESO/SERC survey plates, photometric CCD sequences have been obtained for 10 ESO/SERC fields in the area 10h00m&lt;R.A.&lt;15h30m and -34deg&lt;Decl.&lt;-18deg. In Tables 2 to 20, the catalogue of the CCD sequences is given. It contains B, V and R magnitudes for 117 galaxies and 162 stars with 12.7&lt;V&lt;21.0. Column 2 gives the object type, S for star, G for galaxy. The positions were measured from scans of Schmidt plates with one of the PDS machines at the Astronomisches Institut, Muenster, Germany. Their accuracy is between 0.5 and 1.0arcsec.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71#2</TD>
            <TD>2011-09-14T18:20:32Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/125/71&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/71</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/125/71 [tables]</TD>
            <TD>BVR photometry of 10 ESO/SERC fields (Cunow+ 1997)</TD>
            <TD>For calibration of ESO/SERC survey plates, photometric CCD sequences have been obtained for 10 ESO/SERC fields in the area 10h00m&lt;R.A.&lt;15h30m and -34deg&lt;Decl.&lt;-18deg. In Tables 2 to 20, the catalogue of the CCD sequences is given. It contains B, V and R magnitudes for 117 galaxies and 162 stars with 12.7&lt;V&lt;21.0. Column 2 gives the object type, S for star, G for galaxy. The positions were measured from scans of Schmidt plates with one of the PDS machines at the Astronomisches Institut, Muenster, Germany. Their accuracy is between 0.5 and 1.0arcsec.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71#tables</TD>
            <TD>2011-09-14T18:20:32Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/125/71&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/71</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>WMAP [1]</TD>
            <TD>WMAP Seven Year Galaxy Removed</TD>
            <TD>These survey represents a combination of the 7-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body. &lt;p&gt; The original data are available at the &lt;http://lambda.gsfc.nasa.gov&gt;LAMBDA archive&lt;/a&gt;. &lt;p&gt; The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the WMAP data. &lt;/p&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/skyview/wmap#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/wmap</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=wmap&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WMAP [2]</TD>
            <TD>WMAP Seven Year Galaxy Removed</TD>
            <TD>These survey represents a combination of the 7-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body. &lt;p&gt; The original data are available at the &lt;http://lambda.gsfc.nasa.gov&gt;LAMBDA archive&lt;/a&gt;. &lt;p&gt; The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the WMAP data. &lt;/p&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/skyview/wmap#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/wmap</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/654/115 [1]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#1</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/654/115</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/654/115 [2]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#2</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/654/115&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/654/115 [table2]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#table2</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/654/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/654/115 [table1]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#table1</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/654/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/654/115 [1]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#1</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/654/115</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/654/115 [2]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#2</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/654/115&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/654/115 [table2]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#table2</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/654/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/654/115 [table1]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#table1</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/654/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/125/71 [1]</TD>
            <TD>BVR photometry of 10 ESO/SERC fields (Cunow+ 1997)</TD>
            <TD>For calibration of ESO/SERC survey plates, photometric CCD sequences have been obtained for 10 ESO/SERC fields in the area 10h00m&lt;R.A.&lt;15h30m and -34deg&lt;Decl.&lt;-18deg. In Tables 2 to 20, the catalogue of the CCD sequences is given. It contains B, V and R magnitudes for 117 galaxies and 162 stars with 12.7&lt;V&lt;21.0. Column 2 gives the object type, S for star, G for galaxy. The positions were measured from scans of Schmidt plates with one of the PDS machines at the Astronomisches Institut, Muenster, Germany. Their accuracy is between 0.5 and 1.0arcsec.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71#1</TD>
            <TD>2011-09-14T18:20:32Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/125/71</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/71</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/125/71 [2]</TD>
            <TD>BVR photometry of 10 ESO/SERC fields (Cunow+ 1997)</TD>
            <TD>For calibration of ESO/SERC survey plates, photometric CCD sequences have been obtained for 10 ESO/SERC fields in the area 10h00m&lt;R.A.&lt;15h30m and -34deg&lt;Decl.&lt;-18deg. In Tables 2 to 20, the catalogue of the CCD sequences is given. It contains B, V and R magnitudes for 117 galaxies and 162 stars with 12.7&lt;V&lt;21.0. Column 2 gives the object type, S for star, G for galaxy. The positions were measured from scans of Schmidt plates with one of the PDS machines at the Astronomisches Institut, Muenster, Germany. Their accuracy is between 0.5 and 1.0arcsec.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71#2</TD>
            <TD>2011-09-14T18:20:32Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/125/71&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/71</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/125/71 [tables]</TD>
            <TD>BVR photometry of 10 ESO/SERC fields (Cunow+ 1997)</TD>
            <TD>For calibration of ESO/SERC survey plates, photometric CCD sequences have been obtained for 10 ESO/SERC fields in the area 10h00m&lt;R.A.&lt;15h30m and -34deg&lt;Decl.&lt;-18deg. In Tables 2 to 20, the catalogue of the CCD sequences is given. It contains B, V and R magnitudes for 117 galaxies and 162 stars with 12.7&lt;V&lt;21.0. Column 2 gives the object type, S for star, G for galaxy. The positions were measured from scans of Schmidt plates with one of the PDS machines at the Astronomisches Institut, Muenster, Germany. Their accuracy is between 0.5 and 1.0arcsec.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71#tables</TD>
            <TD>2011-09-14T18:20:32Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/71</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/125/71&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/71</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/654/115 [1]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#1</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/654/115</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/654/115 [2]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#2</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/654/115&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/654/115 [table2]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#table2</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/654/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/654/115 [table1]</TD>
            <TD>DEEP2 Galaxy Redshift Survey: SDSS QSOs (Coil+, 2007)</TD>
            <TD>We present the clustering of Deep Extragalactic Evolutionary Probe 2 (DEEP2) galaxies at 0.7&lt;z&lt;1.4 around quasars identified using both the Sloan Digital Sky Survey (SDSS) and DEEP2 surveys. We measure the two-point cross-correlation of a sample of 36 optically selected, spectroscopically identified quasars from the SDSS and 16 more found in the DEEP2 survey with the full DEEP2 galaxy sample over scales 0.1h^-1^MPc&lt;r_p_&lt;10h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115#table1</TD>
            <TD>2011-09-14T20:31:56Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/654/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/654/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/654/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/895 [1]</TD>
            <TD>Stars in the Carina dwarf spheroidal galaxy (Koch+, 2006)</TD>
            <TD>Our observations were performed in visitor mode with the FLAMES (Fibre Large Array Multi Element Spectrograph) facility at the Very Large Telescope (VLT) UT2 of the European Southern Observatory on Cerro Paranal in Chile. We observed during 22 nights spread over two semesters in 2003 and 2004.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895#1</TD>
            <TD>2011-09-14T20:33:00Z</TD>
            <TD>#Abundances#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/895</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/895</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/895 [2]</TD>
            <TD>Stars in the Carina dwarf spheroidal galaxy (Koch+, 2006)</TD>
            <TD>Our observations were performed in visitor mode with the FLAMES (Fibre Large Array Multi Element Spectrograph) facility at the Very Large Telescope (VLT) UT2 of the European Southern Observatory on Cerro Paranal in Chile. We observed during 22 nights spread over two semesters in 2003 and 2004.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895#2</TD>
            <TD>2011-09-14T20:33:00Z</TD>
            <TD>#Abundances#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/895&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/895 [table6]</TD>
            <TD>Stars in the Carina dwarf spheroidal galaxy (Koch+, 2006)</TD>
            <TD>Our observations were performed in visitor mode with the FLAMES (Fibre Large Array Multi Element Spectrograph) facility at the Very Large Telescope (VLT) UT2 of the European Southern Observatory on Cerro Paranal in Chile. We observed during 22 nights spread over two semesters in 2003 and 2004.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895#table6</TD>
            <TD>2011-09-14T20:33:00Z</TD>
            <TD>#Abundances#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/895</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/895 [1]</TD>
            <TD>Stars in the Carina dwarf spheroidal galaxy (Koch+, 2006)</TD>
            <TD>Our observations were performed in visitor mode with the FLAMES (Fibre Large Array Multi Element Spectrograph) facility at the Very Large Telescope (VLT) UT2 of the European Southern Observatory on Cerro Paranal in Chile. We observed during 22 nights spread over two semesters in 2003 and 2004.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895#1</TD>
            <TD>2011-09-14T20:33:00Z</TD>
            <TD>#Abundances#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/895</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/895</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/895 [2]</TD>
            <TD>Stars in the Carina dwarf spheroidal galaxy (Koch+, 2006)</TD>
            <TD>Our observations were performed in visitor mode with the FLAMES (Fibre Large Array Multi Element Spectrograph) facility at the Very Large Telescope (VLT) UT2 of the European Southern Observatory on Cerro Paranal in Chile. We observed during 22 nights spread over two semesters in 2003 and 2004.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895#2</TD>
            <TD>2011-09-14T20:33:00Z</TD>
            <TD>#Abundances#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/895&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/895 [table6]</TD>
            <TD>Stars in the Carina dwarf spheroidal galaxy (Koch+, 2006)</TD>
            <TD>Our observations were performed in visitor mode with the FLAMES (Fibre Large Array Multi Element Spectrograph) facility at the Very Large Telescope (VLT) UT2 of the European Southern Observatory on Cerro Paranal in Chile. We observed during 22 nights spread over two semesters in 2003 and 2004.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895#table6</TD>
            <TD>2011-09-14T20:33:00Z</TD>
            <TD>#Abundances#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/895</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/1762 [1]</TD>
            <TD>Globular clusters around NGC 1399 (Ostrov+ 1993)</TD>
            <TD>We have obtained integrated Washington photometry (C,M,T1) of globular cluster candidates in the field of NGC 1399. This galaxy, the dominant object in the Fornax cluster, shares with NGC 4486 (M87) the property of possessing one of the largest known specific frequencies of globulars. Conflicting evidence on the presence of a B-V color gradient as a function of galactocentric distance has been reported for this cluster system. Here we investigate the existence of a gradient using the C-T1 index, which is twice as metallicity sensitive as B-V. A small gradient is detected. This color gradient, in the sense that outer clusters are bluer, amounts to approx. 0.1 mag in C-T1 over a galactocentric range from about 0.5 to 3.5 arcmin, corresponding to a difference of approx. 0.2 dex in metallicity. This confirms qualitatively the B-V gradient suggested by Bridges et al. [AJ, 101, 469 (1991)]. Photometry for 420 globular cluster candidates is presented. Metal abundances internally precise to approx. 0.25 dex and accurate to approx. 0.3 dex have been obtained for some 250 of the best candidates, after statistically subtracting a field contamination estimated at 30%. The mean abundance of -0.9 +/- 0.2 confirms previous indications that the NGC 1399 globular cluster system is, on average, significantly more metal rich than that of the Galaxy, as expected from the relative parent galaxy luminosities. Approximately 10% of the clusters exceed solar abundance, similar to the case for NGC 5128. The signature of possible globular cluster formation in mergers, as suggested by Ashman and Zepf [ApJ, 384, 50 (1992)], is found in the distinct peaks in the metallicity distribution function. However, their prediction (based on a simple theory designed only for application to normal elliptical galaxies and not the more complicated cD galaxies represented by NGC 1399) that the color difference between the clusters and the background halo light monotonically increases with radius is not borne out by the observations. The difference decreases with radius from the center to approx. 2 arcmin; beyond this radius, the difference does appear to increase, however. At all radii, the mean globular cluster abundance is some 0.25-0.5 dex more metal poor than that of the background halo.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/1762#1</TD>
            <TD>2011-09-14T18:21:06Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/1762</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/1762</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/1762</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/1762 [2]</TD>
            <TD>Globular clusters around NGC 1399 (Ostrov+ 1993)</TD>
            <TD>We have obtained integrated Washington photometry (C,M,T1) of globular cluster candidates in the field of NGC 1399. This galaxy, the dominant object in the Fornax cluster, shares with NGC 4486 (M87) the property of possessing one of the largest known specific frequencies of globulars. Conflicting evidence on the presence of a B-V color gradient as a function of galactocentric distance has been reported for this cluster system. Here we investigate the existence of a gradient using the C-T1 index, which is twice as metallicity sensitive as B-V. A small gradient is detected. This color gradient, in the sense that outer clusters are bluer, amounts to approx. 0.1 mag in C-T1 over a galactocentric range from about 0.5 to 3.5 arcmin, corresponding to a difference of approx. 0.2 dex in metallicity. This confirms qualitatively the B-V gradient suggested by Bridges et al. [AJ, 101, 469 (1991)]. Photometry for 420 globular cluster candidates is presented. Metal abundances internally precise to approx. 0.25 dex and accurate to approx. 0.3 dex have been obtained for some 250 of the best candidates, after statistically subtracting a field contamination estimated at 30%. The mean abundance of -0.9 +/- 0.2 confirms previous indications that the NGC 1399 globular cluster system is, on average, significantly more metal rich than that of the Galaxy, as expected from the relative parent galaxy luminosities. Approximately 10% of the clusters exceed solar abundance, similar to the case for NGC 5128. The signature of possible globular cluster formation in mergers, as suggested by Ashman and Zepf [ApJ, 384, 50 (1992)], is found in the distinct peaks in the metallicity distribution function. However, their prediction (based on a simple theory designed only for application to normal elliptical galaxies and not the more complicated cD galaxies represented by NGC 1399) that the color difference between the clusters and the background halo light monotonically increases with radius is not borne out by the observations. The difference decreases with radius from the center to approx. 2 arcmin; beyond this radius, the difference does appear to increase, however. At all radii, the mean globular cluster abundance is some 0.25-0.5 dex more metal poor than that of the background halo.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/1762#2</TD>
            <TD>2011-09-14T18:21:06Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/1762</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/1762&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/1762</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/895 [1]</TD>
            <TD>Stars in the Carina dwarf spheroidal galaxy (Koch+, 2006)</TD>
            <TD>Our observations were performed in visitor mode with the FLAMES (Fibre Large Array Multi Element Spectrograph) facility at the Very Large Telescope (VLT) UT2 of the European Southern Observatory on Cerro Paranal in Chile. We observed during 22 nights spread over two semesters in 2003 and 2004.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895#1</TD>
            <TD>2011-09-14T20:33:00Z</TD>
            <TD>#Abundances#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/895</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/895</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/895 [2]</TD>
            <TD>Stars in the Carina dwarf spheroidal galaxy (Koch+, 2006)</TD>
            <TD>Our observations were performed in visitor mode with the FLAMES (Fibre Large Array Multi Element Spectrograph) facility at the Very Large Telescope (VLT) UT2 of the European Southern Observatory on Cerro Paranal in Chile. We observed during 22 nights spread over two semesters in 2003 and 2004.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895#2</TD>
            <TD>2011-09-14T20:33:00Z</TD>
            <TD>#Abundances#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/895&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/895 [table6]</TD>
            <TD>Stars in the Carina dwarf spheroidal galaxy (Koch+, 2006)</TD>
            <TD>Our observations were performed in visitor mode with the FLAMES (Fibre Large Array Multi Element Spectrograph) facility at the Very Large Telescope (VLT) UT2 of the European Southern Observatory on Cerro Paranal in Chile. We observed during 22 nights spread over two semesters in 2003 and 2004.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895#table6</TD>
            <TD>2011-09-14T20:33:00Z</TD>
            <TD>#Abundances#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/895</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/1762 [1]</TD>
            <TD>Globular clusters around NGC 1399 (Ostrov+ 1993)</TD>
            <TD>We have obtained integrated Washington photometry (C,M,T1) of globular cluster candidates in the field of NGC 1399. This galaxy, the dominant object in the Fornax cluster, shares with NGC 4486 (M87) the property of possessing one of the largest known specific frequencies of globulars. Conflicting evidence on the presence of a B-V color gradient as a function of galactocentric distance has been reported for this cluster system. Here we investigate the existence of a gradient using the C-T1 index, which is twice as metallicity sensitive as B-V. A small gradient is detected. This color gradient, in the sense that outer clusters are bluer, amounts to approx. 0.1 mag in C-T1 over a galactocentric range from about 0.5 to 3.5 arcmin, corresponding to a difference of approx. 0.2 dex in metallicity. This confirms qualitatively the B-V gradient suggested by Bridges et al. [AJ, 101, 469 (1991)]. Photometry for 420 globular cluster candidates is presented. Metal abundances internally precise to approx. 0.25 dex and accurate to approx. 0.3 dex have been obtained for some 250 of the best candidates, after statistically subtracting a field contamination estimated at 30%. The mean abundance of -0.9 +/- 0.2 confirms previous indications that the NGC 1399 globular cluster system is, on average, significantly more metal rich than that of the Galaxy, as expected from the relative parent galaxy luminosities. Approximately 10% of the clusters exceed solar abundance, similar to the case for NGC 5128. The signature of possible globular cluster formation in mergers, as suggested by Ashman and Zepf [ApJ, 384, 50 (1992)], is found in the distinct peaks in the metallicity distribution function. However, their prediction (based on a simple theory designed only for application to normal elliptical galaxies and not the more complicated cD galaxies represented by NGC 1399) that the color difference between the clusters and the background halo light monotonically increases with radius is not borne out by the observations. The difference decreases with radius from the center to approx. 2 arcmin; beyond this radius, the difference does appear to increase, however. At all radii, the mean globular cluster abundance is some 0.25-0.5 dex more metal poor than that of the background halo.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/1762#1</TD>
            <TD>2011-09-14T18:21:06Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/1762</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/1762</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/1762</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/1762 [2]</TD>
            <TD>Globular clusters around NGC 1399 (Ostrov+ 1993)</TD>
            <TD>We have obtained integrated Washington photometry (C,M,T1) of globular cluster candidates in the field of NGC 1399. This galaxy, the dominant object in the Fornax cluster, shares with NGC 4486 (M87) the property of possessing one of the largest known specific frequencies of globulars. Conflicting evidence on the presence of a B-V color gradient as a function of galactocentric distance has been reported for this cluster system. Here we investigate the existence of a gradient using the C-T1 index, which is twice as metallicity sensitive as B-V. A small gradient is detected. This color gradient, in the sense that outer clusters are bluer, amounts to approx. 0.1 mag in C-T1 over a galactocentric range from about 0.5 to 3.5 arcmin, corresponding to a difference of approx. 0.2 dex in metallicity. This confirms qualitatively the B-V gradient suggested by Bridges et al. [AJ, 101, 469 (1991)]. Photometry for 420 globular cluster candidates is presented. Metal abundances internally precise to approx. 0.25 dex and accurate to approx. 0.3 dex have been obtained for some 250 of the best candidates, after statistically subtracting a field contamination estimated at 30%. The mean abundance of -0.9 +/- 0.2 confirms previous indications that the NGC 1399 globular cluster system is, on average, significantly more metal rich than that of the Galaxy, as expected from the relative parent galaxy luminosities. Approximately 10% of the clusters exceed solar abundance, similar to the case for NGC 5128. The signature of possible globular cluster formation in mergers, as suggested by Ashman and Zepf [ApJ, 384, 50 (1992)], is found in the distinct peaks in the metallicity distribution function. However, their prediction (based on a simple theory designed only for application to normal elliptical galaxies and not the more complicated cD galaxies represented by NGC 1399) that the color difference between the clusters and the background halo light monotonically increases with radius is not borne out by the observations. The difference decreases with radius from the center to approx. 2 arcmin; beyond this radius, the difference does appear to increase, however. At all radii, the mean globular cluster abundance is some 0.25-0.5 dex more metal poor than that of the background halo.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/1762#2</TD>
            <TD>2011-09-14T18:21:06Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/1762</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/1762&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/1762</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/659/1176 [1]</TD>
            <TD>Study of bars in 180 spiral galaxies (Marinova+, 2007)</TD>
            <TD>Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176#1</TD>
            <TD>2011-09-14T20:33:17Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/659/1176</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1176</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/659/1176 [2]</TD>
            <TD>Study of bars in 180 spiral galaxies (Marinova+, 2007)</TD>
            <TD>Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176#2</TD>
            <TD>2011-09-14T20:33:17Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/659/1176&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1176</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/659/1176 [table1]</TD>
            <TD>Study of bars in 180 spiral galaxies (Marinova+, 2007)</TD>
            <TD>Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176#table1</TD>
            <TD>2011-09-14T20:33:17Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/659/1176&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1176</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/659/1176 [1]</TD>
            <TD>Study of bars in 180 spiral galaxies (Marinova+, 2007)</TD>
            <TD>Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176#1</TD>
            <TD>2011-09-14T20:33:17Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/659/1176</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1176</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/659/1176 [2]</TD>
            <TD>Study of bars in 180 spiral galaxies (Marinova+, 2007)</TD>
            <TD>Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176#2</TD>
            <TD>2011-09-14T20:33:17Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/659/1176&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1176</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/659/1176 [table1]</TD>
            <TD>Study of bars in 180 spiral galaxies (Marinova+, 2007)</TD>
            <TD>Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176#table1</TD>
            <TD>2011-09-14T20:33:17Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/659/1176&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1176</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/894 [1]</TD>
            <TD>Star formation in DDO 210 and NGC 3109 (Greggio+ 1993)</TD>
            <TD>The method proposed in Paper I [Tosi et al., AJ, 102, 951 (1991)] to study the star formation histories in nearby irregulars is here applied to the galaxies DDO 210 and NGC 3109. To this purpose we have obtained deep CCD photometry of two regions in DDO 210 and three regions in NGC 3109, reaching V = 24 with the required accuracy of Sigma(V) &lt;= 0.1 mag. Major information on the stellar populations, star formation rates, and initial mass functions of these regions in the last 1 Gyr are derived from the comparison of the observational color-magnitude diagrams and luminosity functions, with the corresponding synthetic diagrams and luminosity functions generated by a numerical simulation code based on stellar evolutionary tracks. In general, for both galaxies we find that in the last 1 Gyr the star formation activity has been rather continuous, possibly occurring in long episodes of moderate activity separated by short quiescent periods. According to our models the metallicity should be fairly low (in the range 0.05 &lt;= Z/Zsun &lt;= 0.5) and the initial mass function exponent in the vicinity of Salpeter's value, i.e., slightly flatter than in the solar neighborhood. The studied regions of NGC 3109 appear to contain different stellar populations (i.e., with slightly different metallicity and star formation histories), whereas those of DDO 210 seem to have fairly similar stellar contents, although for this galaxy the interpretation is more uncertain. As a by-product of our method we find that the distance modulus to DDO 210 should be (m-M)0 approx. 28, which places this galaxy beyond the edge of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/894#1</TD>
            <TD>2011-09-14T18:21:15Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/894</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/894</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/894</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/894 [2]</TD>
            <TD>Star formation in DDO 210 and NGC 3109 (Greggio+ 1993)</TD>
            <TD>The method proposed in Paper I [Tosi et al., AJ, 102, 951 (1991)] to study the star formation histories in nearby irregulars is here applied to the galaxies DDO 210 and NGC 3109. To this purpose we have obtained deep CCD photometry of two regions in DDO 210 and three regions in NGC 3109, reaching V = 24 with the required accuracy of Sigma(V) &lt;= 0.1 mag. Major information on the stellar populations, star formation rates, and initial mass functions of these regions in the last 1 Gyr are derived from the comparison of the observational color-magnitude diagrams and luminosity functions, with the corresponding synthetic diagrams and luminosity functions generated by a numerical simulation code based on stellar evolutionary tracks. In general, for both galaxies we find that in the last 1 Gyr the star formation activity has been rather continuous, possibly occurring in long episodes of moderate activity separated by short quiescent periods. According to our models the metallicity should be fairly low (in the range 0.05 &lt;= Z/Zsun &lt;= 0.5) and the initial mass function exponent in the vicinity of Salpeter's value, i.e., slightly flatter than in the solar neighborhood. The studied regions of NGC 3109 appear to contain different stellar populations (i.e., with slightly different metallicity and star formation histories), whereas those of DDO 210 seem to have fairly similar stellar contents, although for this galaxy the interpretation is more uncertain. As a by-product of our method we find that the distance modulus to DDO 210 should be (m-M)0 approx. 28, which places this galaxy beyond the edge of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/894#2</TD>
            <TD>2011-09-14T18:21:15Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/894</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/894&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/894</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/894 [1]</TD>
            <TD>Star formation in DDO 210 and NGC 3109 (Greggio+ 1993)</TD>
            <TD>The method proposed in Paper I [Tosi et al., AJ, 102, 951 (1991)] to study the star formation histories in nearby irregulars is here applied to the galaxies DDO 210 and NGC 3109. To this purpose we have obtained deep CCD photometry of two regions in DDO 210 and three regions in NGC 3109, reaching V = 24 with the required accuracy of Sigma(V) &lt;= 0.1 mag. Major information on the stellar populations, star formation rates, and initial mass functions of these regions in the last 1 Gyr are derived from the comparison of the observational color-magnitude diagrams and luminosity functions, with the corresponding synthetic diagrams and luminosity functions generated by a numerical simulation code based on stellar evolutionary tracks. In general, for both galaxies we find that in the last 1 Gyr the star formation activity has been rather continuous, possibly occurring in long episodes of moderate activity separated by short quiescent periods. According to our models the metallicity should be fairly low (in the range 0.05 &lt;= Z/Zsun &lt;= 0.5) and the initial mass function exponent in the vicinity of Salpeter's value, i.e., slightly flatter than in the solar neighborhood. The studied regions of NGC 3109 appear to contain different stellar populations (i.e., with slightly different metallicity and star formation histories), whereas those of DDO 210 seem to have fairly similar stellar contents, although for this galaxy the interpretation is more uncertain. As a by-product of our method we find that the distance modulus to DDO 210 should be (m-M)0 approx. 28, which places this galaxy beyond the edge of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/894#1</TD>
            <TD>2011-09-14T18:21:15Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/894</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/894</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/894</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/894 [2]</TD>
            <TD>Star formation in DDO 210 and NGC 3109 (Greggio+ 1993)</TD>
            <TD>The method proposed in Paper I [Tosi et al., AJ, 102, 951 (1991)] to study the star formation histories in nearby irregulars is here applied to the galaxies DDO 210 and NGC 3109. To this purpose we have obtained deep CCD photometry of two regions in DDO 210 and three regions in NGC 3109, reaching V = 24 with the required accuracy of Sigma(V) &lt;= 0.1 mag. Major information on the stellar populations, star formation rates, and initial mass functions of these regions in the last 1 Gyr are derived from the comparison of the observational color-magnitude diagrams and luminosity functions, with the corresponding synthetic diagrams and luminosity functions generated by a numerical simulation code based on stellar evolutionary tracks. In general, for both galaxies we find that in the last 1 Gyr the star formation activity has been rather continuous, possibly occurring in long episodes of moderate activity separated by short quiescent periods. According to our models the metallicity should be fairly low (in the range 0.05 &lt;= Z/Zsun &lt;= 0.5) and the initial mass function exponent in the vicinity of Salpeter's value, i.e., slightly flatter than in the solar neighborhood. The studied regions of NGC 3109 appear to contain different stellar populations (i.e., with slightly different metallicity and star formation histories), whereas those of DDO 210 seem to have fairly similar stellar contents, although for this galaxy the interpretation is more uncertain. As a by-product of our method we find that the distance modulus to DDO 210 should be (m-M)0 approx. 28, which places this galaxy beyond the edge of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/894#2</TD>
            <TD>2011-09-14T18:21:15Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/894</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/894&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/894</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/111 [1]</TD>
            <TD>Intrinsic shape of NGC 3379 (Statler, 1994)</TD>
            <TD>Photometric and kinematic data from the literature are combined with new dynamical models to derive the intrinsic shape of the "standard" elliptical galaxy NGC 3379. The parameters that are best constrained are the dynamical triaxiality T (essentially the triaxiality of the total mass distribution) and the short-to-long axis ratio of the light distribution c_L. The inferred shape is given by a Bayesian probability distribution in the (T,c_L) plane. Assuming a uniform prior, the most probable shape is oblate with a flattening of c_L=.87. The distribution is strongly non-Gaussian, however, and the expectation values, &lt;T&gt;=.31, &lt;c_L&gt;=.75, imply a flatter and more triaxial figure. The 68% highest posterior density region allows more triaxial shapes as long as they are fairly round, or flatter shapes as long as they are nearly oblate. These results are essentially unchanged if the galaxy is assumed to rotate about its short axis, or if it is modeled as an S0 with a negligible-mass disk rather than as an elliptical. The suggestion of Capaccioli et al. [ApJ, 371, 535 (1991)] that NGC 3379 is a rather flat, triaxial S0 galaxy is found to be improbable at the 98% level; this conclusion is largely independent of the bulge-to-disk ratio or the relative rotation speeds of the two components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/111#1</TD>
            <TD>2011-09-14T18:21:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/111 [2]</TD>
            <TD>Intrinsic shape of NGC 3379 (Statler, 1994)</TD>
            <TD>Photometric and kinematic data from the literature are combined with new dynamical models to derive the intrinsic shape of the "standard" elliptical galaxy NGC 3379. The parameters that are best constrained are the dynamical triaxiality T (essentially the triaxiality of the total mass distribution) and the short-to-long axis ratio of the light distribution c_L. The inferred shape is given by a Bayesian probability distribution in the (T,c_L) plane. Assuming a uniform prior, the most probable shape is oblate with a flattening of c_L=.87. The distribution is strongly non-Gaussian, however, and the expectation values, &lt;T&gt;=.31, &lt;c_L&gt;=.75, imply a flatter and more triaxial figure. The 68% highest posterior density region allows more triaxial shapes as long as they are fairly round, or flatter shapes as long as they are nearly oblate. These results are essentially unchanged if the galaxy is assumed to rotate about its short axis, or if it is modeled as an S0 with a negligible-mass disk rather than as an elliptical. The suggestion of Capaccioli et al. [ApJ, 371, 535 (1991)] that NGC 3379 is a rather flat, triaxial S0 galaxy is found to be improbable at the 98% level; this conclusion is largely independent of the bulge-to-disk ratio or the relative rotation speeds of the two components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/111#2</TD>
            <TD>2011-09-14T18:21:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/111 [1]</TD>
            <TD>Intrinsic shape of NGC 3379 (Statler, 1994)</TD>
            <TD>Photometric and kinematic data from the literature are combined with new dynamical models to derive the intrinsic shape of the "standard" elliptical galaxy NGC 3379. The parameters that are best constrained are the dynamical triaxiality T (essentially the triaxiality of the total mass distribution) and the short-to-long axis ratio of the light distribution c_L. The inferred shape is given by a Bayesian probability distribution in the (T,c_L) plane. Assuming a uniform prior, the most probable shape is oblate with a flattening of c_L=.87. The distribution is strongly non-Gaussian, however, and the expectation values, &lt;T&gt;=.31, &lt;c_L&gt;=.75, imply a flatter and more triaxial figure. The 68% highest posterior density region allows more triaxial shapes as long as they are fairly round, or flatter shapes as long as they are nearly oblate. These results are essentially unchanged if the galaxy is assumed to rotate about its short axis, or if it is modeled as an S0 with a negligible-mass disk rather than as an elliptical. The suggestion of Capaccioli et al. [ApJ, 371, 535 (1991)] that NGC 3379 is a rather flat, triaxial S0 galaxy is found to be improbable at the 98% level; this conclusion is largely independent of the bulge-to-disk ratio or the relative rotation speeds of the two components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/111#1</TD>
            <TD>2011-09-14T18:21:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/111 [2]</TD>
            <TD>Intrinsic shape of NGC 3379 (Statler, 1994)</TD>
            <TD>Photometric and kinematic data from the literature are combined with new dynamical models to derive the intrinsic shape of the "standard" elliptical galaxy NGC 3379. The parameters that are best constrained are the dynamical triaxiality T (essentially the triaxiality of the total mass distribution) and the short-to-long axis ratio of the light distribution c_L. The inferred shape is given by a Bayesian probability distribution in the (T,c_L) plane. Assuming a uniform prior, the most probable shape is oblate with a flattening of c_L=.87. The distribution is strongly non-Gaussian, however, and the expectation values, &lt;T&gt;=.31, &lt;c_L&gt;=.75, imply a flatter and more triaxial figure. The 68% highest posterior density region allows more triaxial shapes as long as they are fairly round, or flatter shapes as long as they are nearly oblate. These results are essentially unchanged if the galaxy is assumed to rotate about its short axis, or if it is modeled as an S0 with a negligible-mass disk rather than as an elliptical. The suggestion of Capaccioli et al. [ApJ, 371, 535 (1991)] that NGC 3379 is a rather flat, triaxial S0 galaxy is found to be improbable at the 98% level; this conclusion is largely independent of the bulge-to-disk ratio or the relative rotation speeds of the two components.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/111#2</TD>
            <TD>2011-09-14T18:21:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/RMxAA/47 [1]</TD>
            <TD>AGN activity in isolated SDSS galaxies (Coziol+, 2011)</TD>
            <TD>We discuss the nature and origin of the nuclear activity observed in a sample of 292 SDSS narrow-emission-line galaxies, considered to have formed and evolved in isolation. All these galaxies are spiral like and show some kind of nuclear activity. The fraction of Narrow Line AGNs (NLAGNs) and Transition type Objects (TOs; a NLAGN with circumnuclear star formation) is relatively high, amounting to 64% of the galaxies. There is a definite trend for the NLAGNs to appear in early-type spirals, while the star forming galaxies and TOs are found in later-type spirals. We verify that the probability for a galaxy to show an AGN characteristic increases with the bulge mass of the galaxy (Torres-Papaqui et al. 2011), and find evidence that this trend is really a by-product of the morphology, suggesting that the AGN phenomenon is intimately connected with the formation process of the galaxies. Consistent with this interpretation, we establish a strong connection between the astration rate -- the efficiency with which the gas is transformed into stars - the AGN phenomenon, and the gravitational binding energy of the galaxies: the higher the binding energy, the higher the astration rate and the higher the probability to find an AGN. The NLAGNs in our sample are consistent with scaled-down or powered-down versions of quasars and Broad Line AGNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361#1</TD>
            <TD>2011-11-05T21:25:00Z</TD>
            <TD>#Abundances#AGN#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/RMxAA/47.361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/RMxAA/47.361</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/RMxAA/47 [2]</TD>
            <TD>AGN activity in isolated SDSS galaxies (Coziol+, 2011)</TD>
            <TD>We discuss the nature and origin of the nuclear activity observed in a sample of 292 SDSS narrow-emission-line galaxies, considered to have formed and evolved in isolation. All these galaxies are spiral like and show some kind of nuclear activity. The fraction of Narrow Line AGNs (NLAGNs) and Transition type Objects (TOs; a NLAGN with circumnuclear star formation) is relatively high, amounting to 64% of the galaxies. There is a definite trend for the NLAGNs to appear in early-type spirals, while the star forming galaxies and TOs are found in later-type spirals. We verify that the probability for a galaxy to show an AGN characteristic increases with the bulge mass of the galaxy (Torres-Papaqui et al. 2011), and find evidence that this trend is really a by-product of the morphology, suggesting that the AGN phenomenon is intimately connected with the formation process of the galaxies. Consistent with this interpretation, we establish a strong connection between the astration rate -- the efficiency with which the gas is transformed into stars - the AGN phenomenon, and the gravitational binding energy of the galaxies: the higher the binding energy, the higher the astration rate and the higher the probability to find an AGN. The NLAGNs in our sample are consistent with scaled-down or powered-down versions of quasars and Broad Line AGNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361#2</TD>
            <TD>2011-11-05T21:25:00Z</TD>
            <TD>#Abundances#AGN#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/RMxAA/47.361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/RMxAA/47.361</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/RMxAA/47 [nelg]</TD>
            <TD>AGN activity in isolated SDSS galaxies (Coziol+, 2011)</TD>
            <TD>We discuss the nature and origin of the nuclear activity observed in a sample of 292 SDSS narrow-emission-line galaxies, considered to have formed and evolved in isolation. All these galaxies are spiral like and show some kind of nuclear activity. The fraction of Narrow Line AGNs (NLAGNs) and Transition type Objects (TOs; a NLAGN with circumnuclear star formation) is relatively high, amounting to 64% of the galaxies. There is a definite trend for the NLAGNs to appear in early-type spirals, while the star forming galaxies and TOs are found in later-type spirals. We verify that the probability for a galaxy to show an AGN characteristic increases with the bulge mass of the galaxy (Torres-Papaqui et al. 2011), and find evidence that this trend is really a by-product of the morphology, suggesting that the AGN phenomenon is intimately connected with the formation process of the galaxies. Consistent with this interpretation, we establish a strong connection between the astration rate -- the efficiency with which the gas is transformed into stars - the AGN phenomenon, and the gravitational binding energy of the galaxies: the higher the binding energy, the higher the astration rate and the higher the probability to find an AGN. The NLAGNs in our sample are consistent with scaled-down or powered-down versions of quasars and Broad Line AGNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361#nelg</TD>
            <TD>2011-11-05T21:25:00Z</TD>
            <TD>#Abundances#AGN#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/RMxAA/47.361&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/RMxAA/47.361</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/1055 [1]</TD>
            <TD>Globulars of M81 (Perelmuter+ 1995)</TD>
            <TD>We have obtained photometric BVR, morphological, and astrometric information on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 &lt;= V &lt;= 21; it is used here to identify globular cluster candidates in M81 and as a database for a statistical analysis of the system as a whole. The M81 globular cluster system is revealed as a strong surface density excess of ~70 objects within an 11 kpc galactocentric radius. The total population is estimated at N_T = 210 +/- 30 globulars. The spatial, (B-V), and (V-R) distributions are very similar to those of the Milky Way and of M31. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8] and we propose a revised modulus of (m-M)0 = 27.5 +/- 0.3. The globular cluster luminosity function then reaches its maximum at M_V* = -7.5 +/- 0.4, as it does in the galaxy and in M31. There is suggestive evidence that 13 +/- 5 objects are globulars seen through the disk of M81; spectroscopy or high-resolution imaging will resolve this issue. Using the (B-R)0 index to trace [Fe/H], we notice a weak dependence of mean metallicity on galactocentric distance, as observed in the galaxy and in M31. This result argues in favour of in situ globular formation during the continuous collapse and self-enrichment of an early-type spiral host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055#1</TD>
            <TD>2011-09-14T18:21:47Z</TD>
            <TD>#Positional_Data#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/1055</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1055</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/1055 [2]</TD>
            <TD>Globulars of M81 (Perelmuter+ 1995)</TD>
            <TD>We have obtained photometric BVR, morphological, and astrometric information on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 &lt;= V &lt;= 21; it is used here to identify globular cluster candidates in M81 and as a database for a statistical analysis of the system as a whole. The M81 globular cluster system is revealed as a strong surface density excess of ~70 objects within an 11 kpc galactocentric radius. The total population is estimated at N_T = 210 +/- 30 globulars. The spatial, (B-V), and (V-R) distributions are very similar to those of the Milky Way and of M31. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8] and we propose a revised modulus of (m-M)0 = 27.5 +/- 0.3. The globular cluster luminosity function then reaches its maximum at M_V* = -7.5 +/- 0.4, as it does in the galaxy and in M31. There is suggestive evidence that 13 +/- 5 objects are globulars seen through the disk of M81; spectroscopy or high-resolution imaging will resolve this issue. Using the (B-R)0 index to trace [Fe/H], we notice a weak dependence of mean metallicity on galactocentric distance, as observed in the galaxy and in M31. This result argues in favour of in situ globular formation during the continuous collapse and self-enrichment of an early-type spiral host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055#2</TD>
            <TD>2011-09-14T18:21:47Z</TD>
            <TD>#Positional_Data#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/1055&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1055</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/1055 [table6]</TD>
            <TD>Globulars of M81 (Perelmuter+ 1995)</TD>
            <TD>We have obtained photometric BVR, morphological, and astrometric information on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 &lt;= V &lt;= 21; it is used here to identify globular cluster candidates in M81 and as a database for a statistical analysis of the system as a whole. The M81 globular cluster system is revealed as a strong surface density excess of ~70 objects within an 11 kpc galactocentric radius. The total population is estimated at N_T = 210 +/- 30 globulars. The spatial, (B-V), and (V-R) distributions are very similar to those of the Milky Way and of M31. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8] and we propose a revised modulus of (m-M)0 = 27.5 +/- 0.3. The globular cluster luminosity function then reaches its maximum at M_V* = -7.5 +/- 0.4, as it does in the galaxy and in M31. There is suggestive evidence that 13 +/- 5 objects are globulars seen through the disk of M81; spectroscopy or high-resolution imaging will resolve this issue. Using the (B-R)0 index to trace [Fe/H], we notice a weak dependence of mean metallicity on galactocentric distance, as observed in the galaxy and in M31. This result argues in favour of in situ globular formation during the continuous collapse and self-enrichment of an early-type spiral host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055#table6</TD>
            <TD>2011-09-14T18:21:47Z</TD>
            <TD>#Positional_Data#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/1055&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1055</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#1</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#2</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#3</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#4</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#5</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#6</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#7</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#8</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#9</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#10</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#11</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#12</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#13</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#14</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR3 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#15</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#16</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR3 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#17</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#18</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#19</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#20</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#21</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#22</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#23</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR3 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 3</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa#24</TD>
            <TD>2012-07-18T12:22:27Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/6dfdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dfdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/1055 [1]</TD>
            <TD>Globulars of M81 (Perelmuter+ 1995)</TD>
            <TD>We have obtained photometric BVR, morphological, and astrometric information on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 &lt;= V &lt;= 21; it is used here to identify globular cluster candidates in M81 and as a database for a statistical analysis of the system as a whole. The M81 globular cluster system is revealed as a strong surface density excess of ~70 objects within an 11 kpc galactocentric radius. The total population is estimated at N_T = 210 +/- 30 globulars. The spatial, (B-V), and (V-R) distributions are very similar to those of the Milky Way and of M31. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8] and we propose a revised modulus of (m-M)0 = 27.5 +/- 0.3. The globular cluster luminosity function then reaches its maximum at M_V* = -7.5 +/- 0.4, as it does in the galaxy and in M31. There is suggestive evidence that 13 +/- 5 objects are globulars seen through the disk of M81; spectroscopy or high-resolution imaging will resolve this issue. Using the (B-R)0 index to trace [Fe/H], we notice a weak dependence of mean metallicity on galactocentric distance, as observed in the galaxy and in M31. This result argues in favour of in situ globular formation during the continuous collapse and self-enrichment of an early-type spiral host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055#1</TD>
            <TD>2011-09-14T18:21:47Z</TD>
            <TD>#Positional_Data#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/1055</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1055</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/1055 [2]</TD>
            <TD>Globulars of M81 (Perelmuter+ 1995)</TD>
            <TD>We have obtained photometric BVR, morphological, and astrometric information on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 &lt;= V &lt;= 21; it is used here to identify globular cluster candidates in M81 and as a database for a statistical analysis of the system as a whole. The M81 globular cluster system is revealed as a strong surface density excess of ~70 objects within an 11 kpc galactocentric radius. The total population is estimated at N_T = 210 +/- 30 globulars. The spatial, (B-V), and (V-R) distributions are very similar to those of the Milky Way and of M31. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8] and we propose a revised modulus of (m-M)0 = 27.5 +/- 0.3. The globular cluster luminosity function then reaches its maximum at M_V* = -7.5 +/- 0.4, as it does in the galaxy and in M31. There is suggestive evidence that 13 +/- 5 objects are globulars seen through the disk of M81; spectroscopy or high-resolution imaging will resolve this issue. Using the (B-R)0 index to trace [Fe/H], we notice a weak dependence of mean metallicity on galactocentric distance, as observed in the galaxy and in M31. This result argues in favour of in situ globular formation during the continuous collapse and self-enrichment of an early-type spiral host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055#2</TD>
            <TD>2011-09-14T18:21:47Z</TD>
            <TD>#Positional_Data#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/1055&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1055</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/1055 [table6]</TD>
            <TD>Globulars of M81 (Perelmuter+ 1995)</TD>
            <TD>We have obtained photometric BVR, morphological, and astrometric information on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 &lt;= V &lt;= 21; it is used here to identify globular cluster candidates in M81 and as a database for a statistical analysis of the system as a whole. The M81 globular cluster system is revealed as a strong surface density excess of ~70 objects within an 11 kpc galactocentric radius. The total population is estimated at N_T = 210 +/- 30 globulars. The spatial, (B-V), and (V-R) distributions are very similar to those of the Milky Way and of M31. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8] and we propose a revised modulus of (m-M)0 = 27.5 +/- 0.3. The globular cluster luminosity function then reaches its maximum at M_V* = -7.5 +/- 0.4, as it does in the galaxy and in M31. There is suggestive evidence that 13 +/- 5 objects are globulars seen through the disk of M81; spectroscopy or high-resolution imaging will resolve this issue. Using the (B-R)0 index to trace [Fe/H], we notice a weak dependence of mean metallicity on galactocentric distance, as observed in the galaxy and in M31. This result argues in favour of in situ globular formation during the continuous collapse and self-enrichment of an early-type spiral host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055#table6</TD>
            <TD>2011-09-14T18:21:47Z</TD>
            <TD>#Positional_Data#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/1055&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1055</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/RMxAA/47 [1]</TD>
            <TD>AGN activity in isolated SDSS galaxies (Coziol+, 2011)</TD>
            <TD>We discuss the nature and origin of the nuclear activity observed in a sample of 292 SDSS narrow-emission-line galaxies, considered to have formed and evolved in isolation. All these galaxies are spiral like and show some kind of nuclear activity. The fraction of Narrow Line AGNs (NLAGNs) and Transition type Objects (TOs; a NLAGN with circumnuclear star formation) is relatively high, amounting to 64% of the galaxies. There is a definite trend for the NLAGNs to appear in early-type spirals, while the star forming galaxies and TOs are found in later-type spirals. We verify that the probability for a galaxy to show an AGN characteristic increases with the bulge mass of the galaxy (Torres-Papaqui et al. 2011), and find evidence that this trend is really a by-product of the morphology, suggesting that the AGN phenomenon is intimately connected with the formation process of the galaxies. Consistent with this interpretation, we establish a strong connection between the astration rate -- the efficiency with which the gas is transformed into stars - the AGN phenomenon, and the gravitational binding energy of the galaxies: the higher the binding energy, the higher the astration rate and the higher the probability to find an AGN. The NLAGNs in our sample are consistent with scaled-down or powered-down versions of quasars and Broad Line AGNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361#1</TD>
            <TD>2011-11-05T21:25:00Z</TD>
            <TD>#Abundances#AGN#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/RMxAA/47.361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/RMxAA/47.361</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/RMxAA/47 [2]</TD>
            <TD>AGN activity in isolated SDSS galaxies (Coziol+, 2011)</TD>
            <TD>We discuss the nature and origin of the nuclear activity observed in a sample of 292 SDSS narrow-emission-line galaxies, considered to have formed and evolved in isolation. All these galaxies are spiral like and show some kind of nuclear activity. The fraction of Narrow Line AGNs (NLAGNs) and Transition type Objects (TOs; a NLAGN with circumnuclear star formation) is relatively high, amounting to 64% of the galaxies. There is a definite trend for the NLAGNs to appear in early-type spirals, while the star forming galaxies and TOs are found in later-type spirals. We verify that the probability for a galaxy to show an AGN characteristic increases with the bulge mass of the galaxy (Torres-Papaqui et al. 2011), and find evidence that this trend is really a by-product of the morphology, suggesting that the AGN phenomenon is intimately connected with the formation process of the galaxies. Consistent with this interpretation, we establish a strong connection between the astration rate -- the efficiency with which the gas is transformed into stars - the AGN phenomenon, and the gravitational binding energy of the galaxies: the higher the binding energy, the higher the astration rate and the higher the probability to find an AGN. The NLAGNs in our sample are consistent with scaled-down or powered-down versions of quasars and Broad Line AGNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361#2</TD>
            <TD>2011-11-05T21:25:00Z</TD>
            <TD>#Abundances#AGN#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/RMxAA/47.361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/RMxAA/47.361</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/RMxAA/47 [nelg]</TD>
            <TD>AGN activity in isolated SDSS galaxies (Coziol+, 2011)</TD>
            <TD>We discuss the nature and origin of the nuclear activity observed in a sample of 292 SDSS narrow-emission-line galaxies, considered to have formed and evolved in isolation. All these galaxies are spiral like and show some kind of nuclear activity. The fraction of Narrow Line AGNs (NLAGNs) and Transition type Objects (TOs; a NLAGN with circumnuclear star formation) is relatively high, amounting to 64% of the galaxies. There is a definite trend for the NLAGNs to appear in early-type spirals, while the star forming galaxies and TOs are found in later-type spirals. We verify that the probability for a galaxy to show an AGN characteristic increases with the bulge mass of the galaxy (Torres-Papaqui et al. 2011), and find evidence that this trend is really a by-product of the morphology, suggesting that the AGN phenomenon is intimately connected with the formation process of the galaxies. Consistent with this interpretation, we establish a strong connection between the astration rate -- the efficiency with which the gas is transformed into stars - the AGN phenomenon, and the gravitational binding energy of the galaxies: the higher the binding energy, the higher the astration rate and the higher the probability to find an AGN. The NLAGNs in our sample are consistent with scaled-down or powered-down versions of quasars and Broad Line AGNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361#nelg</TD>
            <TD>2011-11-05T21:25:00Z</TD>
            <TD>#Abundances#AGN#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/RMxAA/47.361&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/RMxAA/47.361</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/1055 [1]</TD>
            <TD>Globulars of M81 (Perelmuter+ 1995)</TD>
            <TD>We have obtained photometric BVR, morphological, and astrometric information on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 &lt;= V &lt;= 21; it is used here to identify globular cluster candidates in M81 and as a database for a statistical analysis of the system as a whole. The M81 globular cluster system is revealed as a strong surface density excess of ~70 objects within an 11 kpc galactocentric radius. The total population is estimated at N_T = 210 +/- 30 globulars. The spatial, (B-V), and (V-R) distributions are very similar to those of the Milky Way and of M31. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8] and we propose a revised modulus of (m-M)0 = 27.5 +/- 0.3. The globular cluster luminosity function then reaches its maximum at M_V* = -7.5 +/- 0.4, as it does in the galaxy and in M31. There is suggestive evidence that 13 +/- 5 objects are globulars seen through the disk of M81; spectroscopy or high-resolution imaging will resolve this issue. Using the (B-R)0 index to trace [Fe/H], we notice a weak dependence of mean metallicity on galactocentric distance, as observed in the galaxy and in M31. This result argues in favour of in situ globular formation during the continuous collapse and self-enrichment of an early-type spiral host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055#1</TD>
            <TD>2011-09-14T18:21:47Z</TD>
            <TD>#Positional_Data#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/1055</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1055</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/1055 [2]</TD>
            <TD>Globulars of M81 (Perelmuter+ 1995)</TD>
            <TD>We have obtained photometric BVR, morphological, and astrometric information on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 &lt;= V &lt;= 21; it is used here to identify globular cluster candidates in M81 and as a database for a statistical analysis of the system as a whole. The M81 globular cluster system is revealed as a strong surface density excess of ~70 objects within an 11 kpc galactocentric radius. The total population is estimated at N_T = 210 +/- 30 globulars. The spatial, (B-V), and (V-R) distributions are very similar to those of the Milky Way and of M31. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8] and we propose a revised modulus of (m-M)0 = 27.5 +/- 0.3. The globular cluster luminosity function then reaches its maximum at M_V* = -7.5 +/- 0.4, as it does in the galaxy and in M31. There is suggestive evidence that 13 +/- 5 objects are globulars seen through the disk of M81; spectroscopy or high-resolution imaging will resolve this issue. Using the (B-R)0 index to trace [Fe/H], we notice a weak dependence of mean metallicity on galactocentric distance, as observed in the galaxy and in M31. This result argues in favour of in situ globular formation during the continuous collapse and self-enrichment of an early-type spiral host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055#2</TD>
            <TD>2011-09-14T18:21:47Z</TD>
            <TD>#Positional_Data#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/1055&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1055</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/1055 [table6]</TD>
            <TD>Globulars of M81 (Perelmuter+ 1995)</TD>
            <TD>We have obtained photometric BVR, morphological, and astrometric information on 3774 objects located within a 25' radius of M81. This catalogue is complete for 15 &lt;= V &lt;= 21; it is used here to identify globular cluster candidates in M81 and as a database for a statistical analysis of the system as a whole. The M81 globular cluster system is revealed as a strong surface density excess of ~70 objects within an 11 kpc galactocentric radius. The total population is estimated at N_T = 210 +/- 30 globulars. The spatial, (B-V), and (V-R) distributions are very similar to those of the Milky Way and of M31. Small but significant systematic errors in Madore et al.'s [AJ, 106, 2243 (1993)] photometry could be responsible for an overestimate of the Cepheid distance to M81 [(m-M)0 = 27.8] and we propose a revised modulus of (m-M)0 = 27.5 +/- 0.3. The globular cluster luminosity function then reaches its maximum at M_V* = -7.5 +/- 0.4, as it does in the galaxy and in M31. There is suggestive evidence that 13 +/- 5 objects are globulars seen through the disk of M81; spectroscopy or high-resolution imaging will resolve this issue. Using the (B-R)0 index to trace [Fe/H], we notice a weak dependence of mean metallicity on galactocentric distance, as observed in the galaxy and in M31. This result argues in favour of in situ globular formation during the continuous collapse and self-enrichment of an early-type spiral host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055#table6</TD>
            <TD>2011-09-14T18:21:47Z</TD>
            <TD>#Positional_Data#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1055</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/1055&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1055</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/RMxAA/47 [1]</TD>
            <TD>AGN activity in isolated SDSS galaxies (Coziol+, 2011)</TD>
            <TD>We discuss the nature and origin of the nuclear activity observed in a sample of 292 SDSS narrow-emission-line galaxies, considered to have formed and evolved in isolation. All these galaxies are spiral like and show some kind of nuclear activity. The fraction of Narrow Line AGNs (NLAGNs) and Transition type Objects (TOs; a NLAGN with circumnuclear star formation) is relatively high, amounting to 64% of the galaxies. There is a definite trend for the NLAGNs to appear in early-type spirals, while the star forming galaxies and TOs are found in later-type spirals. We verify that the probability for a galaxy to show an AGN characteristic increases with the bulge mass of the galaxy (Torres-Papaqui et al. 2011), and find evidence that this trend is really a by-product of the morphology, suggesting that the AGN phenomenon is intimately connected with the formation process of the galaxies. Consistent with this interpretation, we establish a strong connection between the astration rate -- the efficiency with which the gas is transformed into stars - the AGN phenomenon, and the gravitational binding energy of the galaxies: the higher the binding energy, the higher the astration rate and the higher the probability to find an AGN. The NLAGNs in our sample are consistent with scaled-down or powered-down versions of quasars and Broad Line AGNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361#1</TD>
            <TD>2011-11-05T21:25:00Z</TD>
            <TD>#Abundances#AGN#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/RMxAA/47.361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/RMxAA/47.361</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/RMxAA/47 [2]</TD>
            <TD>AGN activity in isolated SDSS galaxies (Coziol+, 2011)</TD>
            <TD>We discuss the nature and origin of the nuclear activity observed in a sample of 292 SDSS narrow-emission-line galaxies, considered to have formed and evolved in isolation. All these galaxies are spiral like and show some kind of nuclear activity. The fraction of Narrow Line AGNs (NLAGNs) and Transition type Objects (TOs; a NLAGN with circumnuclear star formation) is relatively high, amounting to 64% of the galaxies. There is a definite trend for the NLAGNs to appear in early-type spirals, while the star forming galaxies and TOs are found in later-type spirals. We verify that the probability for a galaxy to show an AGN characteristic increases with the bulge mass of the galaxy (Torres-Papaqui et al. 2011), and find evidence that this trend is really a by-product of the morphology, suggesting that the AGN phenomenon is intimately connected with the formation process of the galaxies. Consistent with this interpretation, we establish a strong connection between the astration rate -- the efficiency with which the gas is transformed into stars - the AGN phenomenon, and the gravitational binding energy of the galaxies: the higher the binding energy, the higher the astration rate and the higher the probability to find an AGN. The NLAGNs in our sample are consistent with scaled-down or powered-down versions of quasars and Broad Line AGNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361#2</TD>
            <TD>2011-11-05T21:25:00Z</TD>
            <TD>#Abundances#AGN#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/RMxAA/47.361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/RMxAA/47.361</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/RMxAA/47 [nelg]</TD>
            <TD>AGN activity in isolated SDSS galaxies (Coziol+, 2011)</TD>
            <TD>We discuss the nature and origin of the nuclear activity observed in a sample of 292 SDSS narrow-emission-line galaxies, considered to have formed and evolved in isolation. All these galaxies are spiral like and show some kind of nuclear activity. The fraction of Narrow Line AGNs (NLAGNs) and Transition type Objects (TOs; a NLAGN with circumnuclear star formation) is relatively high, amounting to 64% of the galaxies. There is a definite trend for the NLAGNs to appear in early-type spirals, while the star forming galaxies and TOs are found in later-type spirals. We verify that the probability for a galaxy to show an AGN characteristic increases with the bulge mass of the galaxy (Torres-Papaqui et al. 2011), and find evidence that this trend is really a by-product of the morphology, suggesting that the AGN phenomenon is intimately connected with the formation process of the galaxies. Consistent with this interpretation, we establish a strong connection between the astration rate -- the efficiency with which the gas is transformed into stars - the AGN phenomenon, and the gravitational binding energy of the galaxies: the higher the binding energy, the higher the astration rate and the higher the probability to find an AGN. The NLAGNs in our sample are consistent with scaled-down or powered-down versions of quasars and Broad Line AGNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361#nelg</TD>
            <TD>2011-11-05T21:25:00Z</TD>
            <TD>#Abundances#AGN#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/other/RMxAA/47.361</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/RMxAA/47.361&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/RMxAA/47.361</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/212 [1]</TD>
            <TD>BVR photometry of stars in NGC 2366 (Aparicio+ 1995)</TD>
            <TD>The stellar content of the Im galaxy NGC 2366 is discussed on the basis of CCD BVR photometry. The three brightest blue and red stars have been used to estimate its distance, obtaining a value of 2.9pc. The spatial distribution of the young stellar population is discussed in the light of the integrated color indices and the color-magnitude diagrams of different zones of the galaxy. A generalized star formation burst seems to have taken place about 50Myr ago. The youngest stars are preferentially formed in the South-West part of the bar, where the giant H II complex NGC 2363 is located, being younger and bluer. The bar seems to play a role favoring star formation in one of its extremes. Self-propagation however, does not seem to be triggering star formation at large scale. A small region, populated by very young stars has also been found at the East of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/212#1</TD>
            <TD>2011-09-14T18:22:11Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/212</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/212</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/212</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/212 [2]</TD>
            <TD>BVR photometry of stars in NGC 2366 (Aparicio+ 1995)</TD>
            <TD>The stellar content of the Im galaxy NGC 2366 is discussed on the basis of CCD BVR photometry. The three brightest blue and red stars have been used to estimate its distance, obtaining a value of 2.9pc. The spatial distribution of the young stellar population is discussed in the light of the integrated color indices and the color-magnitude diagrams of different zones of the galaxy. A generalized star formation burst seems to have taken place about 50Myr ago. The youngest stars are preferentially formed in the South-West part of the bar, where the giant H II complex NGC 2363 is located, being younger and bluer. The bar seems to play a role favoring star formation in one of its extremes. Self-propagation however, does not seem to be triggering star formation at large scale. A small region, populated by very young stars has also been found at the East of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/212#2</TD>
            <TD>2011-09-14T18:22:11Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/212</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/212&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/212</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/533/A91 [1]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#1</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/533/A91</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/533/A91 [2]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#2</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/533/A91&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/533/A91 [catalog]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#catalog</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/533/A91&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/533/A91 [table1]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#table1</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/533/A91&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/659/1176 [1]</TD>
            <TD>Study of bars in 180 spiral galaxies (Marinova+, 2007)</TD>
            <TD>Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176#1</TD>
            <TD>2011-09-14T20:33:17Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/659/1176</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1176</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/659/1176 [2]</TD>
            <TD>Study of bars in 180 spiral galaxies (Marinova+, 2007)</TD>
            <TD>Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176#2</TD>
            <TD>2011-09-14T20:33:17Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/659/1176&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1176</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/659/1176 [table1]</TD>
            <TD>Study of bars in 180 spiral galaxies (Marinova+, 2007)</TD>
            <TD>Critical insights on galaxy evolution stem from the study of bars. With the advent of HST surveys that trace bars in the rest-frame optical out to z~1, it is critical to provide a reference baseline for bars at z~0 in the optical band. We present results on bars at z~0 in the optical and NIR based on 180 spirals from OSUBSGS (Eskridge et al., 2002, Cat. J/ApJS/143/73).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176#table1</TD>
            <TD>2011-09-14T20:33:17Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1176</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/659/1176&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1176</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/212 [1]</TD>
            <TD>BVR photometry of stars in NGC 2366 (Aparicio+ 1995)</TD>
            <TD>The stellar content of the Im galaxy NGC 2366 is discussed on the basis of CCD BVR photometry. The three brightest blue and red stars have been used to estimate its distance, obtaining a value of 2.9pc. The spatial distribution of the young stellar population is discussed in the light of the integrated color indices and the color-magnitude diagrams of different zones of the galaxy. A generalized star formation burst seems to have taken place about 50Myr ago. The youngest stars are preferentially formed in the South-West part of the bar, where the giant H II complex NGC 2363 is located, being younger and bluer. The bar seems to play a role favoring star formation in one of its extremes. Self-propagation however, does not seem to be triggering star formation at large scale. A small region, populated by very young stars has also been found at the East of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/212#1</TD>
            <TD>2011-09-14T18:22:11Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/212</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/212</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/212</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/212 [2]</TD>
            <TD>BVR photometry of stars in NGC 2366 (Aparicio+ 1995)</TD>
            <TD>The stellar content of the Im galaxy NGC 2366 is discussed on the basis of CCD BVR photometry. The three brightest blue and red stars have been used to estimate its distance, obtaining a value of 2.9pc. The spatial distribution of the young stellar population is discussed in the light of the integrated color indices and the color-magnitude diagrams of different zones of the galaxy. A generalized star formation burst seems to have taken place about 50Myr ago. The youngest stars are preferentially formed in the South-West part of the bar, where the giant H II complex NGC 2363 is located, being younger and bluer. The bar seems to play a role favoring star formation in one of its extremes. Self-propagation however, does not seem to be triggering star formation at large scale. A small region, populated by very young stars has also been found at the East of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/212#2</TD>
            <TD>2011-09-14T18:22:11Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/212</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/212&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/212</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/533/A91 [1]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#1</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/533/A91</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/533/A91 [2]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#2</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/533/A91&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/533/A91 [catalog]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#catalog</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/533/A91&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/533/A91 [table1]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#table1</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/533/A91&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/508/491 [1]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#1</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/508/491</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/508/491 [2]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#2</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/508/491&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/508/491 [table2]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#table2</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/508/491&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/508/491 [table3]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#table3</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/508/491&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2739 [1]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#1</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2739</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2739 [2]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#2</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2739&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2739 [table2]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#table2</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2739&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2739 [table1]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#table1</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2739&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/533/A91 [1]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#1</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/533/A91</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/533/A91 [2]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#2</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/533/A91&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/533/A91 [catalog]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#catalog</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/533/A91&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/533/A91 [table1]</TD>
            <TD>Deep VI imaging in outer regions of M33 (Grossi+, 2011)</TD>
            <TD>V,I stellar photometry in seven fields in the outer regions of M33 corresponding to extended neutral hydrogen clouds found in a recent 21-cm survey of the galaxy. The fields are named as SE1, SE2, SE3, NW4, NW5, NW6, NW7. An additional field named BG at approximately four degrees to the east of the optical centre of M33 was selected to inspect the contamination from background and foreground sources. For each field X, Y position in the V and I frames, equatorial coordinates, V, I magnitudes and corresponding errors are given. The colour magnitude diagrams obtained with this photometry are shown in Figures 2, 3 and 4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91#table1</TD>
            <TD>2011-11-19T12:20:44Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A91</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/533/A91&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2739 [1]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#1</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2739</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2739 [2]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#2</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2739&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2739 [table2]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#table2</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2739&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2739 [table1]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#table1</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2739&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/412/1070 [1]</TD>
            <TD>Synthetic supernova extinction curves (Kawara+, 2011)</TD>
            <TD>Synthetic spectra of stellar populations reddened by dust are modelled to reproduce the data of SST J1604+4304. This is a young IR galaxy at z= 1.135 with the characteristic of ULIRGs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1070#1</TD>
            <TD>2011-11-23T15:15:01Z</TD>
            <TD>#Extinction#Galaxies#Models#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1070</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/412/1070</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1070</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/412/1070 [2]</TD>
            <TD>Synthetic supernova extinction curves (Kawara+, 2011)</TD>
            <TD>Synthetic spectra of stellar populations reddened by dust are modelled to reproduce the data of SST J1604+4304. This is a young IR galaxy at z= 1.135 with the characteristic of ULIRGs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1070#2</TD>
            <TD>2011-11-23T15:15:01Z</TD>
            <TD>#Extinction#Galaxies#Models#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1070</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/412/1070&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1070</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2739 [1]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#1</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2739</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2739 [2]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#2</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2739&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2739 [table2]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#table2</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2739&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2739 [table1]</TD>
            <TD>H-alpha emitting regions in M33 (Calzetti+ 1995)</TD>
            <TD>We report finding charts and accurate positions for 432 compact H{alpha} emitting regions in the Local Group Galaxy M33 (NGC 598), in an effort to isolate candidates for an SS433-like stellar system. The objects were extracted from narrowband images, centered in the rest frame H{alpha} ({lambda}6563A) and in the red continuum at 6100A. The atlas is complete down to V=~20, and includes 279 compact H II regions and 153 line emitting point-like sources. The point-like sources undoubtedly include a variety of objects: very small H II regions, early type stars with intense stellar winds, and Wolf-Rayet stars, but should also contain objects with the characteristics of SS433. This extensive survey of compact H{alpha} regions in M33 is a first step towards the identification of peculiar stellar systems like SS433 in external galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739#table1</TD>
            <TD>2011-09-14T18:22:17Z</TD>
            <TD>#Stars:early-type#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2739</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2739&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/88/1285 [1]</TD>
            <TD>A deep survey of galaxies (Kirshner+ 1983)</TD>
            <TD>We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285#1</TD>
            <TD>2011-09-14T18:22:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/88/1285</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/88/1285</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/88/1285 [2]</TD>
            <TD>A deep survey of galaxies (Kirshner+ 1983)</TD>
            <TD>We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285#2</TD>
            <TD>2011-09-14T18:22:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/88/1285&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/88/1285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/88/1285 [table2]</TD>
            <TD>A deep survey of galaxies (Kirshner+ 1983)</TD>
            <TD>We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285#table2</TD>
            <TD>2011-09-14T18:22:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/88/1285&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/88/1285</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/412/1070 [1]</TD>
            <TD>Synthetic supernova extinction curves (Kawara+, 2011)</TD>
            <TD>Synthetic spectra of stellar populations reddened by dust are modelled to reproduce the data of SST J1604+4304. This is a young IR galaxy at z= 1.135 with the characteristic of ULIRGs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1070#1</TD>
            <TD>2011-11-23T15:15:01Z</TD>
            <TD>#Extinction#Galaxies#Models#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1070</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/412/1070</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1070</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/412/1070 [2]</TD>
            <TD>Synthetic supernova extinction curves (Kawara+, 2011)</TD>
            <TD>Synthetic spectra of stellar populations reddened by dust are modelled to reproduce the data of SST J1604+4304. This is a young IR galaxy at z= 1.135 with the characteristic of ULIRGs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1070#2</TD>
            <TD>2011-11-23T15:15:01Z</TD>
            <TD>#Extinction#Galaxies#Models#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1070</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/412/1070&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1070</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/508/491 [1]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#1</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/508/491</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/508/491 [2]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#2</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/508/491&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/508/491 [table2]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#table2</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/508/491&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/508/491 [table3]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#table3</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/508/491&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/88/1285 [1]</TD>
            <TD>A deep survey of galaxies (Kirshner+ 1983)</TD>
            <TD>We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285#1</TD>
            <TD>2011-09-14T18:22:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/88/1285</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/88/1285</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/88/1285 [2]</TD>
            <TD>A deep survey of galaxies (Kirshner+ 1983)</TD>
            <TD>We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285#2</TD>
            <TD>2011-09-14T18:22:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/88/1285&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/88/1285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/88/1285 [table2]</TD>
            <TD>A deep survey of galaxies (Kirshner+ 1983)</TD>
            <TD>We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285#table2</TD>
            <TD>2011-09-14T18:22:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/88/1285&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/88/1285</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/88/1285 [1]</TD>
            <TD>A deep survey of galaxies (Kirshner+ 1983)</TD>
            <TD>We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285#1</TD>
            <TD>2011-09-14T18:22:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/88/1285</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/88/1285</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/88/1285 [2]</TD>
            <TD>A deep survey of galaxies (Kirshner+ 1983)</TD>
            <TD>We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285#2</TD>
            <TD>2011-09-14T18:22:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/88/1285&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/88/1285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/88/1285 [table2]</TD>
            <TD>A deep survey of galaxies (Kirshner+ 1983)</TD>
            <TD>We present a sample of galaxies in six fields, each of area 2 sq deg, located in the North and South galactic polar caps. Photoelectrically calibrated photographic magnitudes and J-F colors have been determined for 512 galaxies brighter than completeness limits which range from F=16.5 to F=17.2 among the fields. Velocities, with typical accuracies of 150km/s have been obtained for 280 of the brighter galaxies. Using these data and previously published work, we determine the general galaxy luminosity function parameters to be M*_F_=-22.7, {alpha}=-1.25, and the mean visual luminosity density of the universe to be {rho}=2.3x10^8^hL_{sun}_/Mpc^3^. Assuming M/L_v_=300h, this implies {OMEGA}~0.26.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285#table2</TD>
            <TD>2011-09-14T18:22:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/88/1285</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/88/1285&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/88/1285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/508/491 [1]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#1</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/508/491</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/508/491 [2]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#2</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/508/491&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/508/491 [table2]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#table2</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/508/491&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/508/491 [table3]</TD>
            <TD>M101 Cepheids (Stetson+, 1998)</TD>
            <TD>We report on the identification of 255 candidate variable stars in a field located some 1.7' from the center of the late-type spiral galaxy M101 = NGC 5457, based on observations made with the Wide Field and Planetary Camera 2 on board the Hubble Space Telescope. Photometric measurements in the F555W and F814W filters - analyzed independently with the DAOPHOT/ALLFRAME and DoPHOT software suites - have been transformed to the Johnson V and Kron-Cousins I standard magnitude systems. Periods and intensity-averaged mean magnitudes for 61 carefully selected candidate Cepheid variables with periods in the range 10-48 days indicate a reddening-corrected mean distance modulus (m-M)_0_=29.05+/-0.14 (if the true modulus of the Large Magellanic Cloud is 18.50+/-0.10, and if there is no dependence of the period-luminosity relation on metal abundance); results consistent with this are obtained whether or not the sample is expanded to include a larger fraction of the candidates. Applying a metallicity-dependent correction of +0.16+/-0.10mag would increase this estimate to (m-M)_0_= 29.21+/-0.17mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491#table3</TD>
            <TD>2011-09-14T20:33:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/508/491</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/508/491&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/508/491</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/145/245 [1]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#1</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/145/245</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/145/245 [2]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#2</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/145/245&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/245 [table3]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#table3</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/245 [table4]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#table4</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/145/245 [1]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#1</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/145/245</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/145/245 [2]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#2</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/145/245&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/245 [table3]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#table3</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/245 [table4]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#table4</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/383 [1]</TD>
            <TD>Globulars in PGC 6510, PGC 10922, PGC 4287 (Maybhate+, 2009)</TD>
            <TD>The four galaxies were observed as part of Hubble Space Telescope (HST) General Observer program 10227 (PI: Goudfrooij), using the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the filters F475W and F814W. The observations consisted of several long exposures plus a few short ones to guarantee getting an unsaturated galaxy center. The total exposure times were 7874s, 9350s, 8369s, and 21440s in F475W, and 2712s, 3970s, 5908s, and 7300s in F814W for PGC 6510, PGC 10922, PGC 42871, and PGC 6240, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383#1</TD>
            <TD>2011-11-23T17:34:39Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/383</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/383</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/383 [2]</TD>
            <TD>Globulars in PGC 6510, PGC 10922, PGC 4287 (Maybhate+, 2009)</TD>
            <TD>The four galaxies were observed as part of Hubble Space Telescope (HST) General Observer program 10227 (PI: Goudfrooij), using the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the filters F475W and F814W. The observations consisted of several long exposures plus a few short ones to guarantee getting an unsaturated galaxy center. The total exposure times were 7874s, 9350s, 8369s, and 21440s in F475W, and 2712s, 3970s, 5908s, and 7300s in F814W for PGC 6510, PGC 10922, PGC 42871, and PGC 6240, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383#2</TD>
            <TD>2011-11-23T17:34:39Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/383&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/383 [table3]</TD>
            <TD>Globulars in PGC 6510, PGC 10922, PGC 4287 (Maybhate+, 2009)</TD>
            <TD>The four galaxies were observed as part of Hubble Space Telescope (HST) General Observer program 10227 (PI: Goudfrooij), using the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the filters F475W and F814W. The observations consisted of several long exposures plus a few short ones to guarantee getting an unsaturated galaxy center. The total exposure times were 7874s, 9350s, 8369s, and 21440s in F475W, and 2712s, 3970s, 5908s, and 7300s in F814W for PGC 6510, PGC 10922, PGC 42871, and PGC 6240, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383#table3</TD>
            <TD>2011-11-23T17:34:39Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/383</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/384/404 [1]</TD>
            <TD>Redshifts of a nearby rich clusters of galaxies (Postman+ 1992)</TD>
            <TD>We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC &gt;= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404#1</TD>
            <TD>2011-09-14T18:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/384/404</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/384/404</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/384/404 [2]</TD>
            <TD>Redshifts of a nearby rich clusters of galaxies (Postman+ 1992)</TD>
            <TD>We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC &gt;= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404#2</TD>
            <TD>2011-09-14T18:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/384/404&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/384/404</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/384/404 [table1]</TD>
            <TD>Redshifts of a nearby rich clusters of galaxies (Postman+ 1992)</TD>
            <TD>We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC &gt;= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404#table1</TD>
            <TD>2011-09-14T18:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/384/404&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/384/404</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/145/245 [1]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#1</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/145/245</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/145/245 [2]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#2</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/145/245&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/245 [table3]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#table3</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/245 [table4]</TD>
            <TD>SDSS stars in Draco dwarf spheroidal galaxy (Rave+, 2003)</TD>
            <TD>The CCD imaging observations of Draco are taken from SDSS runs 1336 and 1339, which were obtained 2000 April 4 with the SDSS mosaic imaging camera .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245#table4</TD>
            <TD>2011-09-14T20:33:50Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/245</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/383 [1]</TD>
            <TD>Globulars in PGC 6510, PGC 10922, PGC 4287 (Maybhate+, 2009)</TD>
            <TD>The four galaxies were observed as part of Hubble Space Telescope (HST) General Observer program 10227 (PI: Goudfrooij), using the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the filters F475W and F814W. The observations consisted of several long exposures plus a few short ones to guarantee getting an unsaturated galaxy center. The total exposure times were 7874s, 9350s, 8369s, and 21440s in F475W, and 2712s, 3970s, 5908s, and 7300s in F814W for PGC 6510, PGC 10922, PGC 42871, and PGC 6240, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383#1</TD>
            <TD>2011-11-23T17:34:39Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/383</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/383</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/383 [2]</TD>
            <TD>Globulars in PGC 6510, PGC 10922, PGC 4287 (Maybhate+, 2009)</TD>
            <TD>The four galaxies were observed as part of Hubble Space Telescope (HST) General Observer program 10227 (PI: Goudfrooij), using the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the filters F475W and F814W. The observations consisted of several long exposures plus a few short ones to guarantee getting an unsaturated galaxy center. The total exposure times were 7874s, 9350s, 8369s, and 21440s in F475W, and 2712s, 3970s, 5908s, and 7300s in F814W for PGC 6510, PGC 10922, PGC 42871, and PGC 6240, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383#2</TD>
            <TD>2011-11-23T17:34:39Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/383&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/383 [table3]</TD>
            <TD>Globulars in PGC 6510, PGC 10922, PGC 4287 (Maybhate+, 2009)</TD>
            <TD>The four galaxies were observed as part of Hubble Space Telescope (HST) General Observer program 10227 (PI: Goudfrooij), using the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the filters F475W and F814W. The observations consisted of several long exposures plus a few short ones to guarantee getting an unsaturated galaxy center. The total exposure times were 7874s, 9350s, 8369s, and 21440s in F475W, and 2712s, 3970s, 5908s, and 7300s in F814W for PGC 6510, PGC 10922, PGC 42871, and PGC 6240, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383#table3</TD>
            <TD>2011-11-23T17:34:39Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/383</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/384/404 [1]</TD>
            <TD>Redshifts of a nearby rich clusters of galaxies (Postman+ 1992)</TD>
            <TD>We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC &gt;= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404#1</TD>
            <TD>2011-09-14T18:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/384/404</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/384/404</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/384/404 [2]</TD>
            <TD>Redshifts of a nearby rich clusters of galaxies (Postman+ 1992)</TD>
            <TD>We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC &gt;= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404#2</TD>
            <TD>2011-09-14T18:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/384/404&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/384/404</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/384/404 [table1]</TD>
            <TD>Redshifts of a nearby rich clusters of galaxies (Postman+ 1992)</TD>
            <TD>We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC &gt;= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404#table1</TD>
            <TD>2011-09-14T18:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/384/404&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/384/404</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/171/101 [1]</TD>
            <TD>Globular clusters in the ACS Virgo cluster survey (Jordan+, 2007)</TD>
            <TD>A sample of 100 early-type galaxies in the Virgo Cluster was observed for the ACSVCS (Cote et al., 2004ApJS..153..223C). Each galaxy was imaged in F475W (~Sloan g) and F850LP (~Sloan z) bandpasses for a total of 750 and 1210s, respectively, and reductions were performed as described in Jordan et al., 2004ApJS..154..509J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101#1</TD>
            <TD>2011-09-14T20:43:32Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/171/101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/171/101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/171/101 [2]</TD>
            <TD>Globular clusters in the ACS Virgo cluster survey (Jordan+, 2007)</TD>
            <TD>A sample of 100 early-type galaxies in the Virgo Cluster was observed for the ACSVCS (Cote et al., 2004ApJS..153..223C). Each galaxy was imaged in F475W (~Sloan g) and F850LP (~Sloan z) bandpasses for a total of 750 and 1210s, respectively, and reductions were performed as described in Jordan et al., 2004ApJS..154..509J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101#2</TD>
            <TD>2011-09-14T20:43:32Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/171/101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/171/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/171/101 [galaxies]</TD>
            <TD>Globular clusters in the ACS Virgo cluster survey (Jordan+, 2007)</TD>
            <TD>A sample of 100 early-type galaxies in the Virgo Cluster was observed for the ACSVCS (Cote et al., 2004ApJS..153..223C). Each galaxy was imaged in F475W (~Sloan g) and F850LP (~Sloan z) bandpasses for a total of 750 and 1210s, respectively, and reductions were performed as described in Jordan et al., 2004ApJS..154..509J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101#galaxies</TD>
            <TD>2011-09-14T20:43:32Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/171/101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/171/101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/383 [1]</TD>
            <TD>Globulars in PGC 6510, PGC 10922, PGC 4287 (Maybhate+, 2009)</TD>
            <TD>The four galaxies were observed as part of Hubble Space Telescope (HST) General Observer program 10227 (PI: Goudfrooij), using the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the filters F475W and F814W. The observations consisted of several long exposures plus a few short ones to guarantee getting an unsaturated galaxy center. The total exposure times were 7874s, 9350s, 8369s, and 21440s in F475W, and 2712s, 3970s, 5908s, and 7300s in F814W for PGC 6510, PGC 10922, PGC 42871, and PGC 6240, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383#1</TD>
            <TD>2011-11-23T17:34:39Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/383</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/383</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/383 [2]</TD>
            <TD>Globulars in PGC 6510, PGC 10922, PGC 4287 (Maybhate+, 2009)</TD>
            <TD>The four galaxies were observed as part of Hubble Space Telescope (HST) General Observer program 10227 (PI: Goudfrooij), using the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the filters F475W and F814W. The observations consisted of several long exposures plus a few short ones to guarantee getting an unsaturated galaxy center. The total exposure times were 7874s, 9350s, 8369s, and 21440s in F475W, and 2712s, 3970s, 5908s, and 7300s in F814W for PGC 6510, PGC 10922, PGC 42871, and PGC 6240, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383#2</TD>
            <TD>2011-11-23T17:34:39Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/383&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/383 [table3]</TD>
            <TD>Globulars in PGC 6510, PGC 10922, PGC 4287 (Maybhate+, 2009)</TD>
            <TD>The four galaxies were observed as part of Hubble Space Telescope (HST) General Observer program 10227 (PI: Goudfrooij), using the Wide Field Channel (WFC) of the Advanced Camera for Surveys (ACS) with the filters F475W and F814W. The observations consisted of several long exposures plus a few short ones to guarantee getting an unsaturated galaxy center. The total exposure times were 7874s, 9350s, 8369s, and 21440s in F475W, and 2712s, 3970s, 5908s, and 7300s in F814W for PGC 6510, PGC 10922, PGC 42871, and PGC 6240, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383#table3</TD>
            <TD>2011-11-23T17:34:39Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/383</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/384/404 [1]</TD>
            <TD>Redshifts of a nearby rich clusters of galaxies (Postman+ 1992)</TD>
            <TD>We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC &gt;= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404#1</TD>
            <TD>2011-09-14T18:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/384/404</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/384/404</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/384/404 [2]</TD>
            <TD>Redshifts of a nearby rich clusters of galaxies (Postman+ 1992)</TD>
            <TD>We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC &gt;= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404#2</TD>
            <TD>2011-09-14T18:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/384/404&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/384/404</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/384/404 [table1]</TD>
            <TD>Redshifts of a nearby rich clusters of galaxies (Postman+ 1992)</TD>
            <TD>We have acquired redshifts for a complete sample of 351 Abell clusters with tenth-ranked galaxy magnitudes (m_10_) less than or equal to 16.5, including 115 entirely new cluster redshifts. The survey includes all such clusters which lie north of {delta}=-27deg30arcmin and is the largest magnitude-limited redshift survey of rich clusters to date. Analysis of the spatial distribution of these clusters reveals no clustering on scales larger than 75h^-1^Mpc; we do not detect the large supercluster complexes reported by Tully. The correlation length is 20.0(+/-4.3)h^-1^Mpc, consistent with the results from other surveys. The frequency of voids with radii of order 60h^-1^Mpc or less is consistent with the form and amplitude of the observed two-point correlation function. There is no significant difference between the clustering properties of RC = O and RC &gt;= 1 clusters. A percolation analysis yields 23 superclusters, 17 of which are new. The superclusters are not significantly elongated in the radial direction; large-scale peculiar motions are of order 1000 km s^-1^ or less. Dramatically new constraints on the large-scale cluster distribution will require surveys an order of magnitude larger.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404#table1</TD>
            <TD>2011-09-14T18:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/384/404</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/384/404&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/384/404</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/171/101 [1]</TD>
            <TD>Globular clusters in the ACS Virgo cluster survey (Jordan+, 2007)</TD>
            <TD>A sample of 100 early-type galaxies in the Virgo Cluster was observed for the ACSVCS (Cote et al., 2004ApJS..153..223C). Each galaxy was imaged in F475W (~Sloan g) and F850LP (~Sloan z) bandpasses for a total of 750 and 1210s, respectively, and reductions were performed as described in Jordan et al., 2004ApJS..154..509J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101#1</TD>
            <TD>2011-09-14T20:43:32Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/171/101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/171/101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/171/101 [2]</TD>
            <TD>Globular clusters in the ACS Virgo cluster survey (Jordan+, 2007)</TD>
            <TD>A sample of 100 early-type galaxies in the Virgo Cluster was observed for the ACSVCS (Cote et al., 2004ApJS..153..223C). Each galaxy was imaged in F475W (~Sloan g) and F850LP (~Sloan z) bandpasses for a total of 750 and 1210s, respectively, and reductions were performed as described in Jordan et al., 2004ApJS..154..509J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101#2</TD>
            <TD>2011-09-14T20:43:32Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/171/101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/171/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/171/101 [galaxies]</TD>
            <TD>Globular clusters in the ACS Virgo cluster survey (Jordan+, 2007)</TD>
            <TD>A sample of 100 early-type galaxies in the Virgo Cluster was observed for the ACSVCS (Cote et al., 2004ApJS..153..223C). Each galaxy was imaged in F475W (~Sloan g) and F850LP (~Sloan z) bandpasses for a total of 750 and 1210s, respectively, and reductions were performed as described in Jordan et al., 2004ApJS..154..509J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101#galaxies</TD>
            <TD>2011-09-14T20:43:32Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/171/101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/171/101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/406/1318 [1]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#1</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/406/1318</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/406/1318 [2]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#2</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/406/1318&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/406/1318 [macs]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#macs</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/406/1318&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/406/1318 [rcs]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#rcs</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/406/1318&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/405/498 [1]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#1</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/405/498</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/405/498 [2]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#2</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/405/498&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/405/498 [table1b]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#table1b</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/405/498&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/405/498 [table1a]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#table1a</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/405/498&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/171/101 [1]</TD>
            <TD>Globular clusters in the ACS Virgo cluster survey (Jordan+, 2007)</TD>
            <TD>A sample of 100 early-type galaxies in the Virgo Cluster was observed for the ACSVCS (Cote et al., 2004ApJS..153..223C). Each galaxy was imaged in F475W (~Sloan g) and F850LP (~Sloan z) bandpasses for a total of 750 and 1210s, respectively, and reductions were performed as described in Jordan et al., 2004ApJS..154..509J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101#1</TD>
            <TD>2011-09-14T20:43:32Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/171/101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/171/101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/171/101 [2]</TD>
            <TD>Globular clusters in the ACS Virgo cluster survey (Jordan+, 2007)</TD>
            <TD>A sample of 100 early-type galaxies in the Virgo Cluster was observed for the ACSVCS (Cote et al., 2004ApJS..153..223C). Each galaxy was imaged in F475W (~Sloan g) and F850LP (~Sloan z) bandpasses for a total of 750 and 1210s, respectively, and reductions were performed as described in Jordan et al., 2004ApJS..154..509J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101#2</TD>
            <TD>2011-09-14T20:43:32Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/171/101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/171/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/171/101 [galaxies]</TD>
            <TD>Globular clusters in the ACS Virgo cluster survey (Jordan+, 2007)</TD>
            <TD>A sample of 100 early-type galaxies in the Virgo Cluster was observed for the ACSVCS (Cote et al., 2004ApJS..153..223C). Each galaxy was imaged in F475W (~Sloan g) and F850LP (~Sloan z) bandpasses for a total of 750 and 1210s, respectively, and reductions were performed as described in Jordan et al., 2004ApJS..154..509J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101#galaxies</TD>
            <TD>2011-09-14T20:43:32Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/171/101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/171/101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/171/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/406/1318 [1]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#1</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/406/1318</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/406/1318 [2]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#2</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/406/1318&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/406/1318 [macs]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#macs</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/406/1318&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/406/1318 [rcs]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#rcs</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/406/1318&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/405/498 [1]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#1</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/405/498</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/405/498 [2]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#2</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/405/498&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/405/498 [table1b]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#table1b</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/405/498&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/405/498 [table1a]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#table1a</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/405/498&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/671/333 [1]</TD>
            <TD>Aperture photometry in NGC 5194 (Kennicutt+, 2007)</TD>
            <TD>Spitzer MIPS observations of M51a at 24um were obtained on 22 and 23 June 2004, as part of the SINGS Legacy Program. Narrowband images centered at Halpha and continuum R-band images were obtained on 2001 March 28, with the Cassegrain Focus CCD Imager on the 2.1m telescope at Kitt Peak National Observatory, as part of the SINGS ancillary data program. Archival HST/NICMOS images of the central 144", corresponding to the inner ~6kpc of the galaxy, are available in the Pa{alpha} emission line (1.8756 um, F187N narrow-band filter) and the adjacent continuum (F190N narrow-band filter). HI data for M51a have been obtained through The H I Nearby Galaxy Survey (THINGS), a survey dedicated to obtain high-resolution VLA H I imaging for ~35 nearby galaxies. M51 was observed in the VLA D (2004 July 9), C (2004 April 26), and B array (2005 March 5). The CO J=1-0 map of M51a was obtained as part of the BIMA Survey Of Nearby Galaxies (BIMA SONG).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333#1</TD>
            <TD>2011-09-14T20:56:05Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/671/333</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/333</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/671/333 [2]</TD>
            <TD>Aperture photometry in NGC 5194 (Kennicutt+, 2007)</TD>
            <TD>Spitzer MIPS observations of M51a at 24um were obtained on 22 and 23 June 2004, as part of the SINGS Legacy Program. Narrowband images centered at Halpha and continuum R-band images were obtained on 2001 March 28, with the Cassegrain Focus CCD Imager on the 2.1m telescope at Kitt Peak National Observatory, as part of the SINGS ancillary data program. Archival HST/NICMOS images of the central 144", corresponding to the inner ~6kpc of the galaxy, are available in the Pa{alpha} emission line (1.8756 um, F187N narrow-band filter) and the adjacent continuum (F190N narrow-band filter). HI data for M51a have been obtained through The H I Nearby Galaxy Survey (THINGS), a survey dedicated to obtain high-resolution VLA H I imaging for ~35 nearby galaxies. M51 was observed in the VLA D (2004 July 9), C (2004 April 26), and B array (2005 March 5). The CO J=1-0 map of M51a was obtained as part of the BIMA Survey Of Nearby Galaxies (BIMA SONG).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333#2</TD>
            <TD>2011-09-14T20:56:05Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/671/333&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/333</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/671/333 [table1]</TD>
            <TD>Aperture photometry in NGC 5194 (Kennicutt+, 2007)</TD>
            <TD>Spitzer MIPS observations of M51a at 24um were obtained on 22 and 23 June 2004, as part of the SINGS Legacy Program. Narrowband images centered at Halpha and continuum R-band images were obtained on 2001 March 28, with the Cassegrain Focus CCD Imager on the 2.1m telescope at Kitt Peak National Observatory, as part of the SINGS ancillary data program. Archival HST/NICMOS images of the central 144", corresponding to the inner ~6kpc of the galaxy, are available in the Pa{alpha} emission line (1.8756 um, F187N narrow-band filter) and the adjacent continuum (F190N narrow-band filter). HI data for M51a have been obtained through The H I Nearby Galaxy Survey (THINGS), a survey dedicated to obtain high-resolution VLA H I imaging for ~35 nearby galaxies. M51 was observed in the VLA D (2004 July 9), C (2004 April 26), and B array (2005 March 5). The CO J=1-0 map of M51a was obtained as part of the BIMA Survey Of Nearby Galaxies (BIMA SONG).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333#table1</TD>
            <TD>2011-09-14T20:56:05Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/671/333&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/333</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/405/498 [1]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#1</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/405/498</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/405/498 [2]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#2</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/405/498&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/405/498 [table1b]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#table1b</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/405/498&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/405/498 [table1a]</TD>
            <TD>Counts and spectral indices at 8.44GHz (Windhorst+, 1993)</TD>
            <TD>We used the VLA to make deep images of two 7x7' fields at 8.44 GHz with 10" resolution. With an rms noise of 3.2 and 5.1 {micro}Jy, respectively, in the two fields, we compiled a catalog of 82 sources. The normalized differential 8.44 GHz counts are similar to those at 1.41 and 4.86 GHz. All show a similarly steep submillijansky slope, which is only somewhat flatter than that expected for a nonevolving Euclidean population ({gamma}=2.5). Microjansky radio sources at 4.86 GHz have been identified with faint blue galaxies (18&lt;~V&lt;~28 mag). We argue that their expected median redshift is about 0.5-0.75. Hence, cosmological evolution may be needed to explain the steep slope of the microjansky counts. The 8.44 GHz counts must converge with slope {gamma}&lt;2.0 below S(8.44)~300 nJy, or they would exceed the available field galaxy counts down to V~28 mag, and they must permanently converge below S(8.44)~20 nJy, or their integrated sky brightness would distort the observed thermal cosmic background radiation spectrum at centimeter wavelengths. The estimated 31.5 GHz sky brightness from nanojansky to jansky levels is &lt;36 {micro}K (3{sigma}). Even if weak radio sources cluster on scales of degrees as faint galaxies do, their anisotropic contribution to the COBE DMR experiment (with 7deg FWHM-beam) would not exceed ~1.2{micro}K.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498#table1a</TD>
            <TD>2011-09-14T18:23:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/498</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/405/498&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/498</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/406/1318 [1]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#1</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/406/1318</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/406/1318 [2]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#2</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/406/1318&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/406/1318 [macs]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#macs</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/406/1318&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/406/1318 [rcs]</TD>
            <TD>Lensed-arc statistics of galaxy clusters (Horesh+, 2010)</TD>
            <TD>We have compiled from the HST archive a sample of clusters observed with the Advanced Camera for Surveys (ACS). Here we use images of 35 MACS clusters observed with the ACS (GO-09722, GO-10491, GO-10875, PI Ebeling).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318#rcs</TD>
            <TD>2011-12-02T07:33:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1318</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/406/1318&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1318</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/425/122 [1]</TD>
            <TD>IMF from UV stellar photometry (Hill+, 1994)</TD>
            <TD>UV stellar photometry is presented for 1563 stars within a 40' circular field in the LMC, excluding the 10'x10' field centered on R136 investigated earlier by Hill et al. (1993). Magnitudes are computed from images obtained by the Ultraviolet Imaging Telescope in bands centered at 1615A and 2558A. Stellar masses and extinctions are estimated for the stars in associations using the evolutionary models of Schaerer et al. (1993), assuming the age is 4Myr and that the local LMC extinction follows the Fitzpatrick (1985) 30 Dor extinction curve. The estimated slope of the initial mass function (IMF) for massive stars (&gt;15M_{sun}_) within the Lucke and Hodge (LH) associations is {gamma}=-1.08+/-0.2. Initial masses and extinctions for stars not within LH associations are estimated assuming that the stellar age is either 4Myr or half the stellar lifetime, whichever is larger. The estimated slope of the IMF for massive stars not within LH associations is {gamma}=-1.74+/-0.3 (assuming continuous star formation), compared with {gamma}=-1.35, and {gamma}=-1.7+/-0.5, obtained for the Galaxy by Salpeter (1955) and Scalo (1986), respectively, and {gamma}=-1.6 obtained for massive stars in the Galaxy by Garmany, Conti, &amp; Chiosi (1982). The shallower slope of the association IMF suggests that not only is the star formation rate higher in associations, but that the local conditions favor the formation of higher mass stars there. We make no corrections for binaries or incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/425/122#1</TD>
            <TD>2011-09-14T18:23:19Z</TD>
            <TD>#Associations#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/425/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/425/122</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/425/122</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/425/122 [2]</TD>
            <TD>IMF from UV stellar photometry (Hill+, 1994)</TD>
            <TD>UV stellar photometry is presented for 1563 stars within a 40' circular field in the LMC, excluding the 10'x10' field centered on R136 investigated earlier by Hill et al. (1993). Magnitudes are computed from images obtained by the Ultraviolet Imaging Telescope in bands centered at 1615A and 2558A. Stellar masses and extinctions are estimated for the stars in associations using the evolutionary models of Schaerer et al. (1993), assuming the age is 4Myr and that the local LMC extinction follows the Fitzpatrick (1985) 30 Dor extinction curve. The estimated slope of the initial mass function (IMF) for massive stars (&gt;15M_{sun}_) within the Lucke and Hodge (LH) associations is {gamma}=-1.08+/-0.2. Initial masses and extinctions for stars not within LH associations are estimated assuming that the stellar age is either 4Myr or half the stellar lifetime, whichever is larger. The estimated slope of the IMF for massive stars not within LH associations is {gamma}=-1.74+/-0.3 (assuming continuous star formation), compared with {gamma}=-1.35, and {gamma}=-1.7+/-0.5, obtained for the Galaxy by Salpeter (1955) and Scalo (1986), respectively, and {gamma}=-1.6 obtained for massive stars in the Galaxy by Garmany, Conti, &amp; Chiosi (1982). The shallower slope of the association IMF suggests that not only is the star formation rate higher in associations, but that the local conditions favor the formation of higher mass stars there. We make no corrections for binaries or incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/425/122#2</TD>
            <TD>2011-09-14T18:23:19Z</TD>
            <TD>#Associations#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/425/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/425/122&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/425/122</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/412/1741 [1]</TD>
            <TD>Spectroscopic obs. of 3 spiral galaxies (Scarano+, 2011)</TD>
            <TD>The correlation between the breaks in the metallicity distribution and the corotation radius of spiral galaxies has been already advocated in the past and is predicted by a chemodynamical model of our Galaxy that effectively introduces the role of spiral arms in the star formation rate. In this work, we present photometric and spectroscopic observations made with the Gemini Telescope for three of the best candidates of spiral galaxies to have the corotation inside the optical disc: IC 0167, NGC 1042 and NGC 6907. We observed the most intense and well-distributed HII regions of these galaxies, deriving reliable galactocentric distances and oxygen abundances by applying different statistical methods. From these results, we confirm the presence of variations in the gradients of metallicity of these galaxies that are possibly correlated with the corotation resonance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741#1</TD>
            <TD>2011-12-17T11:05:41Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/412/1741</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1741</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/412/1741 [2]</TD>
            <TD>Spectroscopic obs. of 3 spiral galaxies (Scarano+, 2011)</TD>
            <TD>The correlation between the breaks in the metallicity distribution and the corotation radius of spiral galaxies has been already advocated in the past and is predicted by a chemodynamical model of our Galaxy that effectively introduces the role of spiral arms in the star formation rate. In this work, we present photometric and spectroscopic observations made with the Gemini Telescope for three of the best candidates of spiral galaxies to have the corotation inside the optical disc: IC 0167, NGC 1042 and NGC 6907. We observed the most intense and well-distributed HII regions of these galaxies, deriving reliable galactocentric distances and oxygen abundances by applying different statistical methods. From these results, we confirm the presence of variations in the gradients of metallicity of these galaxies that are possibly correlated with the corotation resonance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741#2</TD>
            <TD>2011-12-17T11:05:41Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/412/1741&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/412/1741 [spectro]</TD>
            <TD>Spectroscopic obs. of 3 spiral galaxies (Scarano+, 2011)</TD>
            <TD>The correlation between the breaks in the metallicity distribution and the corotation radius of spiral galaxies has been already advocated in the past and is predicted by a chemodynamical model of our Galaxy that effectively introduces the role of spiral arms in the star formation rate. In this work, we present photometric and spectroscopic observations made with the Gemini Telescope for three of the best candidates of spiral galaxies to have the corotation inside the optical disc: IC 0167, NGC 1042 and NGC 6907. We observed the most intense and well-distributed HII regions of these galaxies, deriving reliable galactocentric distances and oxygen abundances by applying different statistical methods. From these results, we confirm the presence of variations in the gradients of metallicity of these galaxies that are possibly correlated with the corotation resonance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741#spectro</TD>
            <TD>2011-12-17T11:05:41Z</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/412/1741&amp;</TD>
            <TD>180</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/425/122 [1]</TD>
            <TD>IMF from UV stellar photometry (Hill+, 1994)</TD>
            <TD>UV stellar photometry is presented for 1563 stars within a 40' circular field in the LMC, excluding the 10'x10' field centered on R136 investigated earlier by Hill et al. (1993). Magnitudes are computed from images obtained by the Ultraviolet Imaging Telescope in bands centered at 1615A and 2558A. Stellar masses and extinctions are estimated for the stars in associations using the evolutionary models of Schaerer et al. (1993), assuming the age is 4Myr and that the local LMC extinction follows the Fitzpatrick (1985) 30 Dor extinction curve. The estimated slope of the initial mass function (IMF) for massive stars (&gt;15M_{sun}_) within the Lucke and Hodge (LH) associations is {gamma}=-1.08+/-0.2. Initial masses and extinctions for stars not within LH associations are estimated assuming that the stellar age is either 4Myr or half the stellar lifetime, whichever is larger. The estimated slope of the IMF for massive stars not within LH associations is {gamma}=-1.74+/-0.3 (assuming continuous star formation), compared with {gamma}=-1.35, and {gamma}=-1.7+/-0.5, obtained for the Galaxy by Salpeter (1955) and Scalo (1986), respectively, and {gamma}=-1.6 obtained for massive stars in the Galaxy by Garmany, Conti, &amp; Chiosi (1982). The shallower slope of the association IMF suggests that not only is the star formation rate higher in associations, but that the local conditions favor the formation of higher mass stars there. We make no corrections for binaries or incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/425/122#1</TD>
            <TD>2011-09-14T18:23:19Z</TD>
            <TD>#Associations#Positional_Data#</TD>
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            <TD>25-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/425/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/425/122</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/425/122</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/425/122 [2]</TD>
            <TD>IMF from UV stellar photometry (Hill+, 1994)</TD>
            <TD>UV stellar photometry is presented for 1563 stars within a 40' circular field in the LMC, excluding the 10'x10' field centered on R136 investigated earlier by Hill et al. (1993). Magnitudes are computed from images obtained by the Ultraviolet Imaging Telescope in bands centered at 1615A and 2558A. Stellar masses and extinctions are estimated for the stars in associations using the evolutionary models of Schaerer et al. (1993), assuming the age is 4Myr and that the local LMC extinction follows the Fitzpatrick (1985) 30 Dor extinction curve. The estimated slope of the initial mass function (IMF) for massive stars (&gt;15M_{sun}_) within the Lucke and Hodge (LH) associations is {gamma}=-1.08+/-0.2. Initial masses and extinctions for stars not within LH associations are estimated assuming that the stellar age is either 4Myr or half the stellar lifetime, whichever is larger. The estimated slope of the IMF for massive stars not within LH associations is {gamma}=-1.74+/-0.3 (assuming continuous star formation), compared with {gamma}=-1.35, and {gamma}=-1.7+/-0.5, obtained for the Galaxy by Salpeter (1955) and Scalo (1986), respectively, and {gamma}=-1.6 obtained for massive stars in the Galaxy by Garmany, Conti, &amp; Chiosi (1982). The shallower slope of the association IMF suggests that not only is the star formation rate higher in associations, but that the local conditions favor the formation of higher mass stars there. We make no corrections for binaries or incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/425/122#2</TD>
            <TD>2011-09-14T18:23:19Z</TD>
            <TD>#Associations#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/425/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/425/122&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/425/122</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/412/1741 [1]</TD>
            <TD>Spectroscopic obs. of 3 spiral galaxies (Scarano+, 2011)</TD>
            <TD>The correlation between the breaks in the metallicity distribution and the corotation radius of spiral galaxies has been already advocated in the past and is predicted by a chemodynamical model of our Galaxy that effectively introduces the role of spiral arms in the star formation rate. In this work, we present photometric and spectroscopic observations made with the Gemini Telescope for three of the best candidates of spiral galaxies to have the corotation inside the optical disc: IC 0167, NGC 1042 and NGC 6907. We observed the most intense and well-distributed HII regions of these galaxies, deriving reliable galactocentric distances and oxygen abundances by applying different statistical methods. From these results, we confirm the presence of variations in the gradients of metallicity of these galaxies that are possibly correlated with the corotation resonance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741#1</TD>
            <TD>2011-12-17T11:05:41Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/412/1741</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1741</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/412/1741 [2]</TD>
            <TD>Spectroscopic obs. of 3 spiral galaxies (Scarano+, 2011)</TD>
            <TD>The correlation between the breaks in the metallicity distribution and the corotation radius of spiral galaxies has been already advocated in the past and is predicted by a chemodynamical model of our Galaxy that effectively introduces the role of spiral arms in the star formation rate. In this work, we present photometric and spectroscopic observations made with the Gemini Telescope for three of the best candidates of spiral galaxies to have the corotation inside the optical disc: IC 0167, NGC 1042 and NGC 6907. We observed the most intense and well-distributed HII regions of these galaxies, deriving reliable galactocentric distances and oxygen abundances by applying different statistical methods. From these results, we confirm the presence of variations in the gradients of metallicity of these galaxies that are possibly correlated with the corotation resonance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741#2</TD>
            <TD>2011-12-17T11:05:41Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/412/1741&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/412/1741 [spectro]</TD>
            <TD>Spectroscopic obs. of 3 spiral galaxies (Scarano+, 2011)</TD>
            <TD>The correlation between the breaks in the metallicity distribution and the corotation radius of spiral galaxies has been already advocated in the past and is predicted by a chemodynamical model of our Galaxy that effectively introduces the role of spiral arms in the star formation rate. In this work, we present photometric and spectroscopic observations made with the Gemini Telescope for three of the best candidates of spiral galaxies to have the corotation inside the optical disc: IC 0167, NGC 1042 and NGC 6907. We observed the most intense and well-distributed HII regions of these galaxies, deriving reliable galactocentric distances and oxygen abundances by applying different statistical methods. From these results, we confirm the presence of variations in the gradients of metallicity of these galaxies that are possibly correlated with the corotation resonance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741#spectro</TD>
            <TD>2011-12-17T11:05:41Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/412/1741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1741</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/453/48 [1]</TD>
            <TD>VI photometry of HST faint field galaxies (Driver+ 1995)</TD>
            <TD>We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=&lt;Imag&lt;22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)&lt;1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M &amp; 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z&gt;=0.5 at m_I_=21.75mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/48#1</TD>
            <TD>2011-09-14T18:23:31Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/48</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/453/48</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/48</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/453/48 [2]</TD>
            <TD>VI photometry of HST faint field galaxies (Driver+ 1995)</TD>
            <TD>We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=&lt;Imag&lt;22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)&lt;1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M &amp; 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z&gt;=0.5 at m_I_=21.75mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/48#2</TD>
            <TD>2011-09-14T18:23:31Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/48</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/453/48&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/48</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/453/48 [table2]</TD>
            <TD>VI photometry of HST faint field galaxies (Driver+ 1995)</TD>
            <TD>We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=&lt;Imag&lt;22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)&lt;1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M &amp; 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z&gt;=0.5 at m_I_=21.75mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/48#table2</TD>
            <TD>2011-09-14T18:23:31Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/48</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/453/48&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/48</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/412/1741 [1]</TD>
            <TD>Spectroscopic obs. of 3 spiral galaxies (Scarano+, 2011)</TD>
            <TD>The correlation between the breaks in the metallicity distribution and the corotation radius of spiral galaxies has been already advocated in the past and is predicted by a chemodynamical model of our Galaxy that effectively introduces the role of spiral arms in the star formation rate. In this work, we present photometric and spectroscopic observations made with the Gemini Telescope for three of the best candidates of spiral galaxies to have the corotation inside the optical disc: IC 0167, NGC 1042 and NGC 6907. We observed the most intense and well-distributed HII regions of these galaxies, deriving reliable galactocentric distances and oxygen abundances by applying different statistical methods. From these results, we confirm the presence of variations in the gradients of metallicity of these galaxies that are possibly correlated with the corotation resonance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741#1</TD>
            <TD>2011-12-17T11:05:41Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/412/1741</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1741</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/412/1741 [2]</TD>
            <TD>Spectroscopic obs. of 3 spiral galaxies (Scarano+, 2011)</TD>
            <TD>The correlation between the breaks in the metallicity distribution and the corotation radius of spiral galaxies has been already advocated in the past and is predicted by a chemodynamical model of our Galaxy that effectively introduces the role of spiral arms in the star formation rate. In this work, we present photometric and spectroscopic observations made with the Gemini Telescope for three of the best candidates of spiral galaxies to have the corotation inside the optical disc: IC 0167, NGC 1042 and NGC 6907. We observed the most intense and well-distributed HII regions of these galaxies, deriving reliable galactocentric distances and oxygen abundances by applying different statistical methods. From these results, we confirm the presence of variations in the gradients of metallicity of these galaxies that are possibly correlated with the corotation resonance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741#2</TD>
            <TD>2011-12-17T11:05:41Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/412/1741&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/412/1741 [spectro]</TD>
            <TD>Spectroscopic obs. of 3 spiral galaxies (Scarano+, 2011)</TD>
            <TD>The correlation between the breaks in the metallicity distribution and the corotation radius of spiral galaxies has been already advocated in the past and is predicted by a chemodynamical model of our Galaxy that effectively introduces the role of spiral arms in the star formation rate. In this work, we present photometric and spectroscopic observations made with the Gemini Telescope for three of the best candidates of spiral galaxies to have the corotation inside the optical disc: IC 0167, NGC 1042 and NGC 6907. We observed the most intense and well-distributed HII regions of these galaxies, deriving reliable galactocentric distances and oxygen abundances by applying different statistical methods. From these results, we confirm the presence of variations in the gradients of metallicity of these galaxies that are possibly correlated with the corotation resonance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741#spectro</TD>
            <TD>2011-12-17T11:05:41Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/412/1741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1741</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/453/48 [1]</TD>
            <TD>VI photometry of HST faint field galaxies (Driver+ 1995)</TD>
            <TD>We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=&lt;Imag&lt;22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)&lt;1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M &amp; 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z&gt;=0.5 at m_I_=21.75mag.</TD>
            <TD>CDS</TD>
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            <TD />
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            <TD />
            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/453/48</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/48</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/453/48 [2]</TD>
            <TD>VI photometry of HST faint field galaxies (Driver+ 1995)</TD>
            <TD>We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=&lt;Imag&lt;22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)&lt;1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M &amp; 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z&gt;=0.5 at m_I_=21.75mag.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/453/48 [table2]</TD>
            <TD>VI photometry of HST faint field galaxies (Driver+ 1995)</TD>
            <TD>We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=&lt;Imag&lt;22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)&lt;1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M &amp; 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z&gt;=0.5 at m_I_=21.75mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/453/48&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/48</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A96 [1]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#1</TD>
            <TD>2011-12-18T21:18:57Z</TD>
            <TD>#Associations#Galaxies#</TD>
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            <TD>#Research#</TD>
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            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A96</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A96</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A96 [2]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#2</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A96&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A96</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A96 [table1]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
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            <TD>13-Sep-2011</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A96&amp;</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/534/A96 [table2]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A96&amp;</TD>
            <TD>180</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/453/48 [1]</TD>
            <TD>VI photometry of HST faint field galaxies (Driver+ 1995)</TD>
            <TD>We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=&lt;Imag&lt;22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)&lt;1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M &amp; 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z&gt;=0.5 at m_I_=21.75mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T18:23:31Z</TD>
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            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/48</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/453/48</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/48</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/453/48 [2]</TD>
            <TD>VI photometry of HST faint field galaxies (Driver+ 1995)</TD>
            <TD>We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=&lt;Imag&lt;22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)&lt;1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M &amp; 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z&gt;=0.5 at m_I_=21.75mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/48#2</TD>
            <TD>2011-09-14T18:23:31Z</TD>
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            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/48</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/453/48&amp;</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/453/48 [table2]</TD>
            <TD>VI photometry of HST faint field galaxies (Driver+ 1995)</TD>
            <TD>We present a complete morphologically classified sample of 144 faint field galaxies from the HST Medium Deep Survey with 20.0=&lt;Imag&lt;22.0mag. We compare the global properties of the ellipticals and early- and late-type spirals and find a non-negligible fraction (13/144) of compact blue [(V-I)&lt;1.0mag] systems with r^1/4^ profiles. We give the differential galaxy number counts for ellipticals and early-type spirals independently and find that the data are consistent with no-evolution predictions based on conventional flat Schechter luminosity functions (LFs) and a standard cosmology. Conversely, late-type/irregulars show a steeply rising differential number count with slope ({delta}logN/{delta}m)=0.64+/-0.1. No-evolution models based on the Loveday et al. (1992ApJ...390..338L) and Marzke et al. (1994AJ....108..437M &amp; 1994ApJ...428...43M) local luminosity functions underpredict the late-type/irregular counts by 1.0 and 0.5dex, respectively, at Imag=21.75mag. Examination of the irregulars alone shows that ~50% appear inert and the remainder have multiple cores. If the inert galaxies represent a non-evolving late-type population, then a Loveday-like LF ({alpha}=~-1.0) is ruled out for these types, and an LF with a steep faint end ({alpha}=~-1.5) is suggested. If multiple core structure indicates recent star formation, then the observed excess of faint blue field galaxies is likely a result of et evolutionary processes acting on a steep field LF for late-type/irregulars. The evolutionary mechanism is unclear, but 60% of the multiple-core irregulars show close companions. To reconcile a Marzke-like LF with the faint redshift surveys, this evolution must be preferentially occurring in the brightest late-type galaxies with z&gt;=0.5 at m_I_=21.75mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>14-Feb-1997</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/453/48&amp;</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A96 [1]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#1</TD>
            <TD>2011-12-18T21:18:57Z</TD>
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            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A96</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A96</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A96 [2]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#2</TD>
            <TD>2011-12-18T21:18:57Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A96&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A96</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A96 [table1]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#table1</TD>
            <TD>2011-12-18T21:18:57Z</TD>
            <TD>#Associations#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A96&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A96 [table2]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#table2</TD>
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            <TD>#Associations#Galaxies#</TD>
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            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A96&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A96</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/454/788 [1]</TD>
            <TD>Radial velocities and BV photometry of NGC 3201 (Cote+ 1995)</TD>
            <TD>BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5&lt;~R&lt;~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788#1</TD>
            <TD>2011-09-14T18:23:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
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            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/454/788</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/454/788</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/454/788 [2]</TD>
            <TD>Radial velocities and BV photometry of NGC 3201 (Cote+ 1995)</TD>
            <TD>BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5&lt;~R&lt;~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788#2</TD>
            <TD>2011-09-14T18:23:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/454/788&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/454/788</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/454/788 [table3]</TD>
            <TD>Radial velocities and BV photometry of NGC 3201 (Cote+ 1995)</TD>
            <TD>BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5&lt;~R&lt;~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788#table3</TD>
            <TD>2011-09-14T18:23:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/454/788&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/454/788</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A96 [1]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#1</TD>
            <TD>2011-12-18T21:18:57Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A96</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A96</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A96 [2]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#2</TD>
            <TD>2011-12-18T21:18:57Z</TD>
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            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A96&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A96</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A96 [table1]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#table1</TD>
            <TD>2011-12-18T21:18:57Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A96&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A96</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A96 [table2]</TD>
            <TD>Spitzer photometry of YSC in M33 (Sharma+, 2011)</TD>
            <TD>The properties of young stellar clusters (YSCs) in M33, identified from the center out to about twice the size of the bright star-forming disk, are investigated to determine possible spatial and time variations of the star formation process in this Local Group blue galaxy. 915 MIR sources have been extracted from the Spitzer 24um image. Upon inspection of H{alpha} and GALEX images and exclusion of evolved AGB stars, a sample of 648 objects is selected as candidate YSCs and their luminosity function is examined. The spectral energy distribution of each object, based on aperture photometry, is compared with Starburst99 models to derive age, mass and AV of individual clusters. In the analysis we allow for different values of the upper mass cutoff of the stellar initial mass function (IMF), the porosity of the ISM, and the dustiness of HII regions. We also examine the influence of different dust models and include corrections for incompleteness of the IMF.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96#table2</TD>
            <TD>2011-12-18T21:18:57Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A96</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A96&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A96</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/454/788 [1]</TD>
            <TD>Radial velocities and BV photometry of NGC 3201 (Cote+ 1995)</TD>
            <TD>BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5&lt;~R&lt;~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788#1</TD>
            <TD>2011-09-14T18:23:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/454/788</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/454/788</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/454/788 [2]</TD>
            <TD>Radial velocities and BV photometry of NGC 3201 (Cote+ 1995)</TD>
            <TD>BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5&lt;~R&lt;~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788#2</TD>
            <TD>2011-09-14T18:23:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/454/788&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/454/788</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/454/788 [table3]</TD>
            <TD>Radial velocities and BV photometry of NGC 3201 (Cote+ 1995)</TD>
            <TD>BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5&lt;~R&lt;~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788#table3</TD>
            <TD>2011-09-14T18:23:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/454/788&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/454/788</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/454/788 [1]</TD>
            <TD>Radial velocities and BV photometry of NGC 3201 (Cote+ 1995)</TD>
            <TD>BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5&lt;~R&lt;~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788#1</TD>
            <TD>2011-09-14T18:23:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/454/788</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/454/788</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/454/788 [2]</TD>
            <TD>Radial velocities and BV photometry of NGC 3201 (Cote+ 1995)</TD>
            <TD>BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5&lt;~R&lt;~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788#2</TD>
            <TD>2011-09-14T18:23:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/454/788&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/454/788</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/454/788 [table3]</TD>
            <TD>Radial velocities and BV photometry of NGC 3201 (Cote+ 1995)</TD>
            <TD>BV CCD frames have been used to derive surface brightness profiles for NGC 3201 which extend out to ~18'. A total of 857 radial velocities with median precision ~1km/s for 399 member giants have been used to trace the velocity dispersion profile out to 32.1' (the approximate tidal radius determined from fits of single-mass, isotropic King-Michie models to the cluster surface brightness profiles). The median difference in radial velocity for stars on either side of an imaginary axis stepped through the cluster in 1 deg increments shows a statistically significant maximum amplitude of 1.22+/-0.25km/s. We discuss several possible explanations of this result, including (1) cluster rotation, (2) preferential stripping of stars on prograde orbits near the limiting radius, (3) the projection of the cluster space velocity onto the plane of the sky, and (4) a slight drift in the velocity zero point. It is difficult to unambiguously identify the primary cause of the observed structure in the velocity field, however, and we suspect that all of the above processes may play a role. The BV surface brightness profiles and radial velocities have been modeled with both single- and multimass King-Michie models and nonparametric techniques. The corresponding density profiles and M/L profiles show good agreement over the interval 1.5&lt;~R&lt;~10pc, and both approaches suggest a steady rise in M/L with distance from the cluster center. Due to the low cluster luminosity we are unable to place useful constraints on the anisotropy of M/L_B~M/L_V~2.0+/-0.2 for the multimass and nonparametric models, compared to ~1.65+/-0.15 for models having equal-mass stars. Our best-fit, multimass models have mass function slopes of x~0.75+/-0.25, consistent with recent findings that the form of the mass function depends on the position relative to the potential of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788#table3</TD>
            <TD>2011-09-14T18:23:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/454/788</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/454/788&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/454/788</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/532/A127 [1]</TD>
            <TD>Inner Galaxy HII regions (Du+, 2011)</TD>
            <TD>The observations were made on September 2009 to August 2010 with the 25m radio telescope of Nanshan station. One hundred and twenty sources were selected from the IRAS Point Source Catalog. Sixty-one sources were selected from Quireza et al. (2006, Cat. J/ApJS/165/338) and 70 sources were selected from Lockman (1989, Cat. VIII/58).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127#1</TD>
            <TD>2011-12-27T12:05:18Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/532/A127</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/532/A127</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/532/A127 [2]</TD>
            <TD>Inner Galaxy HII regions (Du+, 2011)</TD>
            <TD>The observations were made on September 2009 to August 2010 with the 25m radio telescope of Nanshan station. One hundred and twenty sources were selected from the IRAS Point Source Catalog. Sixty-one sources were selected from Quireza et al. (2006, Cat. J/ApJS/165/338) and 70 sources were selected from Lockman (1989, Cat. VIII/58).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127#2</TD>
            <TD>2011-12-27T12:05:18Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/532/A127&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/532/A127</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/532/A127 [table1]</TD>
            <TD>Inner Galaxy HII regions (Du+, 2011)</TD>
            <TD>The observations were made on September 2009 to August 2010 with the 25m radio telescope of Nanshan station. One hundred and twenty sources were selected from the IRAS Point Source Catalog. Sixty-one sources were selected from Quireza et al. (2006, Cat. J/ApJS/165/338) and 70 sources were selected from Lockman (1989, Cat. VIII/58).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127#table1</TD>
            <TD>2011-12-27T12:05:18Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/532/A127&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/532/A127</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/102/289 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. II. (Yee+, 1996)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of the rich galaxy cluster Abell 2390 (z=0.228) is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. Using five separate fields, the imaging and spectroscopic observations cover a strip of approximately 7.3'x43.2', centered on the cluster. Redshifts for 327 galaxies, primarily ranging in magnitude from r=17 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, geometric, and color selection functions for the redshift sample are discussed and presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/102/289#1</TD>
            <TD>2011-09-14T18:23:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/102/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/102/289</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/102/289</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/102/289 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. II. (Yee+, 1996)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of the rich galaxy cluster Abell 2390 (z=0.228) is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. Using five separate fields, the imaging and spectroscopic observations cover a strip of approximately 7.3'x43.2', centered on the cluster. Redshifts for 327 galaxies, primarily ranging in magnitude from r=17 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, geometric, and color selection functions for the redshift sample are discussed and presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/102/289#2</TD>
            <TD>2011-09-14T18:23:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/102/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/102/289&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/102/289</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/532/A127 [1]</TD>
            <TD>Inner Galaxy HII regions (Du+, 2011)</TD>
            <TD>The observations were made on September 2009 to August 2010 with the 25m radio telescope of Nanshan station. One hundred and twenty sources were selected from the IRAS Point Source Catalog. Sixty-one sources were selected from Quireza et al. (2006, Cat. J/ApJS/165/338) and 70 sources were selected from Lockman (1989, Cat. VIII/58).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127#1</TD>
            <TD>2011-12-27T12:05:18Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/532/A127</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/532/A127</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/532/A127 [2]</TD>
            <TD>Inner Galaxy HII regions (Du+, 2011)</TD>
            <TD>The observations were made on September 2009 to August 2010 with the 25m radio telescope of Nanshan station. One hundred and twenty sources were selected from the IRAS Point Source Catalog. Sixty-one sources were selected from Quireza et al. (2006, Cat. J/ApJS/165/338) and 70 sources were selected from Lockman (1989, Cat. VIII/58).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127#2</TD>
            <TD>2011-12-27T12:05:18Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/532/A127&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/532/A127</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/532/A127 [table1]</TD>
            <TD>Inner Galaxy HII regions (Du+, 2011)</TD>
            <TD>The observations were made on September 2009 to August 2010 with the 25m radio telescope of Nanshan station. One hundred and twenty sources were selected from the IRAS Point Source Catalog. Sixty-one sources were selected from Quireza et al. (2006, Cat. J/ApJS/165/338) and 70 sources were selected from Lockman (1989, Cat. VIII/58).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127#table1</TD>
            <TD>2011-12-27T12:05:18Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/532/A127&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/532/A127</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/102/289 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. II. (Yee+, 1996)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of the rich galaxy cluster Abell 2390 (z=0.228) is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. Using five separate fields, the imaging and spectroscopic observations cover a strip of approximately 7.3'x43.2', centered on the cluster. Redshifts for 327 galaxies, primarily ranging in magnitude from r=17 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, geometric, and color selection functions for the redshift sample are discussed and presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/102/289#1</TD>
            <TD>2011-09-14T18:23:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/102/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/102/289</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/102/289</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/102/289 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. II. (Yee+, 1996)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of the rich galaxy cluster Abell 2390 (z=0.228) is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. Using five separate fields, the imaging and spectroscopic observations cover a strip of approximately 7.3'x43.2', centered on the cluster. Redshifts for 327 galaxies, primarily ranging in magnitude from r=17 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, geometric, and color selection functions for the redshift sample are discussed and presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/102/289#2</TD>
            <TD>2011-09-14T18:23:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/102/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/102/289&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/102/289</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/96/123 [1]</TD>
            <TD>H-magnitudes of spiral galaxies (Tormen+ 1995)</TD>
            <TD>The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, &amp; Corwin 1976, Cat .&lt;VII/112&gt;), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5&lt;=log(A/D_g_)&lt;=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123#1</TD>
            <TD>2011-09-14T18:24:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/96/123</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/123</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/96/123 [2]</TD>
            <TD>H-magnitudes of spiral galaxies (Tormen+ 1995)</TD>
            <TD>The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, &amp; Corwin 1976, Cat .&lt;VII/112&gt;), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5&lt;=log(A/D_g_)&lt;=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123#2</TD>
            <TD>2011-09-14T18:24:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/96/123&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/123 [table4]</TD>
            <TD>H-magnitudes of spiral galaxies (Tormen+ 1995)</TD>
            <TD>The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, &amp; Corwin 1976, Cat .&lt;VII/112&gt;), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5&lt;=log(A/D_g_)&lt;=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123#table4</TD>
            <TD>2011-09-14T18:24:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/532/A127 [1]</TD>
            <TD>Inner Galaxy HII regions (Du+, 2011)</TD>
            <TD>The observations were made on September 2009 to August 2010 with the 25m radio telescope of Nanshan station. One hundred and twenty sources were selected from the IRAS Point Source Catalog. Sixty-one sources were selected from Quireza et al. (2006, Cat. J/ApJS/165/338) and 70 sources were selected from Lockman (1989, Cat. VIII/58).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127#1</TD>
            <TD>2011-12-27T12:05:18Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/532/A127</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/532/A127</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/532/A127 [2]</TD>
            <TD>Inner Galaxy HII regions (Du+, 2011)</TD>
            <TD>The observations were made on September 2009 to August 2010 with the 25m radio telescope of Nanshan station. One hundred and twenty sources were selected from the IRAS Point Source Catalog. Sixty-one sources were selected from Quireza et al. (2006, Cat. J/ApJS/165/338) and 70 sources were selected from Lockman (1989, Cat. VIII/58).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127#2</TD>
            <TD>2011-12-27T12:05:18Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/532/A127&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/532/A127</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/532/A127 [table1]</TD>
            <TD>Inner Galaxy HII regions (Du+, 2011)</TD>
            <TD>The observations were made on September 2009 to August 2010 with the 25m radio telescope of Nanshan station. One hundred and twenty sources were selected from the IRAS Point Source Catalog. Sixty-one sources were selected from Quireza et al. (2006, Cat. J/ApJS/165/338) and 70 sources were selected from Lockman (1989, Cat. VIII/58).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127#table1</TD>
            <TD>2011-12-27T12:05:18Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/532/A127</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/532/A127&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/532/A127</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/96/123 [1]</TD>
            <TD>H-magnitudes of spiral galaxies (Tormen+ 1995)</TD>
            <TD>The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, &amp; Corwin 1976, Cat .&lt;VII/112&gt;), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5&lt;=log(A/D_g_)&lt;=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123#1</TD>
            <TD>2011-09-14T18:24:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/96/123</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/123</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/96/123 [2]</TD>
            <TD>H-magnitudes of spiral galaxies (Tormen+ 1995)</TD>
            <TD>The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, &amp; Corwin 1976, Cat .&lt;VII/112&gt;), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5&lt;=log(A/D_g_)&lt;=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123#2</TD>
            <TD>2011-09-14T18:24:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/96/123&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/123 [table4]</TD>
            <TD>H-magnitudes of spiral galaxies (Tormen+ 1995)</TD>
            <TD>The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, &amp; Corwin 1976, Cat .&lt;VII/112&gt;), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5&lt;=log(A/D_g_)&lt;=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123#table4</TD>
            <TD>2011-09-14T18:24:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [1]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#1</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=SpecObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [2]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#2</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [3]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#3</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [4]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#4</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR5 [5]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#5</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [6]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#6</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR5 [7]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#7</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [8]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#8</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [9]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#9</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [10]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#10</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [11]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#11</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [12]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#12</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [13]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#13</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR5 [14]</TD>
            <TD>SDSS DR5 - Sloan Digital Sky Survey Data Release 5</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR5 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa#14</TD>
            <TD>2012-07-18T12:35:04Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr5/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/692/856 [1]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#1</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/692/856</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/692/856 [2]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#2</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/692/856&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/692/856 [table1]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#table1</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/692/856&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/692/856 [table2]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#table2</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/692/856&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/692/856 [1]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#1</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/692/856</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/692/856 [2]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#2</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/692/856&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/692/856 [table1]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#table1</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/692/856&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/692/856 [table2]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#table2</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/692/856&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/96/123 [1]</TD>
            <TD>H-magnitudes of spiral galaxies (Tormen+ 1995)</TD>
            <TD>The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, &amp; Corwin 1976, Cat .&lt;VII/112&gt;), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5&lt;=log(A/D_g_)&lt;=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123#1</TD>
            <TD>2011-09-14T18:24:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/96/123</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/123</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/96/123 [2]</TD>
            <TD>H-magnitudes of spiral galaxies (Tormen+ 1995)</TD>
            <TD>The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, &amp; Corwin 1976, Cat .&lt;VII/112&gt;), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5&lt;=log(A/D_g_)&lt;=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123#2</TD>
            <TD>2011-09-14T18:24:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/96/123&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/123 [table4]</TD>
            <TD>H-magnitudes of spiral galaxies (Tormen+ 1995)</TD>
            <TD>The H-magnitude aperture data published by the Aaronson et al. collaboration (See references) over a 10 year period is collected into a homogeneous data set of 1731 observations of 665 galaxies. Ninety-six percent of these galaxies have isophotal diameters and axial ratios determined by the Third Reference Catalogue of Bright Galaxies (RC3; de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;), the most self-consistent set of optical data currently available. The precepts governing the optical data in the RC3 are systematically different from those of the Second Reference Catalogue (de Vaucouleurs, de Vaucouleurs, &amp; Corwin 1976, Cat .&lt;VII/112&gt;), which were used by Aaronson et al. for their original analyses of galaxy peculiar motions. This in turn leads to systematic differences in growth curves and fiducial H-magnitudes, prompting the present recalibration of the near-infrared Tully-Fisher relationship. New optically normalized H-magnitude growth curves are defined for galaxies of types S0 to Im, from which new values of fiducial H-magnitude, H^g^_-0.5_, are measured for the 665 galaxies. A series of internal tests show that these four standard growth curves are defined to an accuracy of 0.05mag over the interval 1.5&lt;=log(A/D_g_)&lt;=-0.2. Comparisons with the Aaronson et al. values of diameters, axial ratios, and fiducial H-magnitudes show the expected differences, given the different definitions of these parameters. The values of H^g^_-0.5_ are assigned quality indices: a quality value of 1 indicates an accuracy of less than 0.2mag, quality 2 indicates an accuracy of 0.2-0.35mag, and quality 3 indicates an accuracy of more than 0.35mag. Revised values of corrected H I velocity widths are also given, based on the new set of axial ratios defined by the RC3.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123#table4</TD>
            <TD>2011-09-14T18:24:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/123</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/692/856 [1]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#1</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/692/856</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/692/856 [2]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#2</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/692/856&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/692/856 [table1]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#table1</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/692/856&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/692/856 [table2]</TD>
            <TD>Supermassive black holes masses upper limits (Beifiori+, 2009)</TD>
            <TD>In order to assemble the largest possible sample of homogeneous measurements of the central emission-line width, we queried the HST Science Archive for objects with STIS spectra obtained with the G750M grating through either the 0.1"x52" or the 0.2"x52" slit placed across the galaxy nucleus, most often at random position angles. This is indeed by far the most common configuration in the archive, which always gives us access to the [NII] {lambda}{lambda}6548,6583, H{alpha}, and [SII] {lambda}{lambda}6716,6731 emission lines. Limiting ourselves to galaxies within 100 Mpc to minimize the impact of the stellar potential on our results, we retrieved data for 177 galaxies spanning the whole range of morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856#table2</TD>
            <TD>2012-01-21T07:27:51Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/856</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/692/856&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/856</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/243/390 [1]</TD>
            <TD>Galaxy redshift survey in a Coma strip (Karachentsev+ 1990)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390#1</TD>
            <TD>2011-09-14T18:37:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1994</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/243/390</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/243/390</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/243/390 [2]</TD>
            <TD>Galaxy redshift survey in a Coma strip (Karachentsev+ 1990)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390#2</TD>
            <TD>2011-09-14T18:37:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1994</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/243/390&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/243/390</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/243/390 [table1]</TD>
            <TD>Galaxy redshift survey in a Coma strip (Karachentsev+ 1990)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390#table1</TD>
            <TD>2011-09-14T18:37:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1994</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/243/390&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/243/390</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/729/22 [1]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#1</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/729/22</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/729/22 [2]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#2</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/729/22&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/729/22 [table3]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#table3</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/729/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/729/22 [table2]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#table2</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/729/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/729/22 [1]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#1</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/729/22</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/729/22 [2]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#2</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/729/22&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/729/22 [table3]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#table3</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/729/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/729/22 [table2]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#table2</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/729/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/729/22 [1]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#1</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/729/22</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/729/22 [2]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#2</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/729/22&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/729/22 [table3]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#table3</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/729/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/729/22 [table2]</TD>
            <TD>SEDs of galaxy cluster members (Atlee+, 2011)</TD>
            <TD>We obtained MIR observations with the Spitzer Space Telescope of the X-ray sources identified as members of eight low-redshift galaxy clusters by Martini et al., 2006ApJ...644..116M. Visible wavelength photometry of these clusters were obtained at the 2.5m du Pont telescope at Las Campanas by Martini et al. 2006ApJ...644..116M. MIR observations from the Spitzer Space Telescope were obtained using the IRAC (3.6, 4.5, 5.8, and 8.0um) and MIPS (24um) instruments from Spitzer program 50096 (PI: Martini). Observations were carried out between 2008 November 1 and 2009 April 22. We supplemented these observations with data from the Spitzer archive for Abell 1689 and AC 114.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22#table2</TD>
            <TD>2012-11-12T12:42:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/729/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/729/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/729/22</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/722/566 [1]</TD>
            <TD>Host galaxies of SNe Ia in SDSS-II SN survey (Lampeitl+, 2010)</TD>
            <TD>In this analysis, we use the full data set from the SDSS-II Supernova Survey (Frieman et al. 2008AJ....135..338F). The SDSS-II SN Survey was a dedicated search for transient objects using the SDSS 2.5m telescope and imaging camera to perform repeat imaging of the "Stripe 82" region of the SDSS survey for three months a year from 2005 to 2007. To ensure that our SN sample is more complete, we also include photometric SNe Ia that have a light curve consistent with being a Type Ia, based on the Bayesian light-curve fitting of Sako et al. (2008, Cat. J/AJ/135/348), and a known host galaxy spectroscopic redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566#1</TD>
            <TD>2012-11-12T12:51:51Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/722/566</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/722/566</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/722/566 [2]</TD>
            <TD>Host galaxies of SNe Ia in SDSS-II SN survey (Lampeitl+, 2010)</TD>
            <TD>In this analysis, we use the full data set from the SDSS-II Supernova Survey (Frieman et al. 2008AJ....135..338F). The SDSS-II SN Survey was a dedicated search for transient objects using the SDSS 2.5m telescope and imaging camera to perform repeat imaging of the "Stripe 82" region of the SDSS survey for three months a year from 2005 to 2007. To ensure that our SN sample is more complete, we also include photometric SNe Ia that have a light curve consistent with being a Type Ia, based on the Bayesian light-curve fitting of Sako et al. (2008, Cat. J/AJ/135/348), and a known host galaxy spectroscopic redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566#2</TD>
            <TD>2012-11-12T12:51:51Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/722/566&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/722/566</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/722/566 [table2]</TD>
            <TD>Host galaxies of SNe Ia in SDSS-II SN survey (Lampeitl+, 2010)</TD>
            <TD>In this analysis, we use the full data set from the SDSS-II Supernova Survey (Frieman et al. 2008AJ....135..338F). The SDSS-II SN Survey was a dedicated search for transient objects using the SDSS 2.5m telescope and imaging camera to perform repeat imaging of the "Stripe 82" region of the SDSS survey for three months a year from 2005 to 2007. To ensure that our SN sample is more complete, we also include photometric SNe Ia that have a light curve consistent with being a Type Ia, based on the Bayesian light-curve fitting of Sako et al. (2008, Cat. J/AJ/135/348), and a known host galaxy spectroscopic redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566#table2</TD>
            <TD>2012-11-12T12:51:51Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/722/566&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/722/566</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/243/390 [1]</TD>
            <TD>Galaxy redshift survey in a Coma strip (Karachentsev+ 1990)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390#1</TD>
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            <TD />
            <TD>10-Feb-1994</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/243/390</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/243/390</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/243/390 [2]</TD>
            <TD>Galaxy redshift survey in a Coma strip (Karachentsev+ 1990)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390#2</TD>
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            <TD>10-Feb-1994</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/243/390&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/243/390</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/243/390 [table1]</TD>
            <TD>Galaxy redshift survey in a Coma strip (Karachentsev+ 1990)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390#table1</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1994</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/243/390&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/243/390</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/722/566 [1]</TD>
            <TD>Host galaxies of SNe Ia in SDSS-II SN survey (Lampeitl+, 2010)</TD>
            <TD>In this analysis, we use the full data set from the SDSS-II Supernova Survey (Frieman et al. 2008AJ....135..338F). The SDSS-II SN Survey was a dedicated search for transient objects using the SDSS 2.5m telescope and imaging camera to perform repeat imaging of the "Stripe 82" region of the SDSS survey for three months a year from 2005 to 2007. To ensure that our SN sample is more complete, we also include photometric SNe Ia that have a light curve consistent with being a Type Ia, based on the Bayesian light-curve fitting of Sako et al. (2008, Cat. J/AJ/135/348), and a known host galaxy spectroscopic redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566#1</TD>
            <TD>2012-11-12T12:51:51Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/722/566</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/722/566</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/722/566 [2]</TD>
            <TD>Host galaxies of SNe Ia in SDSS-II SN survey (Lampeitl+, 2010)</TD>
            <TD>In this analysis, we use the full data set from the SDSS-II Supernova Survey (Frieman et al. 2008AJ....135..338F). The SDSS-II SN Survey was a dedicated search for transient objects using the SDSS 2.5m telescope and imaging camera to perform repeat imaging of the "Stripe 82" region of the SDSS survey for three months a year from 2005 to 2007. To ensure that our SN sample is more complete, we also include photometric SNe Ia that have a light curve consistent with being a Type Ia, based on the Bayesian light-curve fitting of Sako et al. (2008, Cat. J/AJ/135/348), and a known host galaxy spectroscopic redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566#2</TD>
            <TD>2012-11-12T12:51:51Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/722/566&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/722/566</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/722/566 [table2]</TD>
            <TD>Host galaxies of SNe Ia in SDSS-II SN survey (Lampeitl+, 2010)</TD>
            <TD>In this analysis, we use the full data set from the SDSS-II Supernova Survey (Frieman et al. 2008AJ....135..338F). The SDSS-II SN Survey was a dedicated search for transient objects using the SDSS 2.5m telescope and imaging camera to perform repeat imaging of the "Stripe 82" region of the SDSS survey for three months a year from 2005 to 2007. To ensure that our SN sample is more complete, we also include photometric SNe Ia that have a light curve consistent with being a Type Ia, based on the Bayesian light-curve fitting of Sako et al. (2008, Cat. J/AJ/135/348), and a known host galaxy spectroscopic redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566#table2</TD>
            <TD>2012-11-12T12:51:51Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/722/566&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/722/566</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/722/566 [1]</TD>
            <TD>Host galaxies of SNe Ia in SDSS-II SN survey (Lampeitl+, 2010)</TD>
            <TD>In this analysis, we use the full data set from the SDSS-II Supernova Survey (Frieman et al. 2008AJ....135..338F). The SDSS-II SN Survey was a dedicated search for transient objects using the SDSS 2.5m telescope and imaging camera to perform repeat imaging of the "Stripe 82" region of the SDSS survey for three months a year from 2005 to 2007. To ensure that our SN sample is more complete, we also include photometric SNe Ia that have a light curve consistent with being a Type Ia, based on the Bayesian light-curve fitting of Sako et al. (2008, Cat. J/AJ/135/348), and a known host galaxy spectroscopic redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566#1</TD>
            <TD>2012-11-12T12:51:51Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/722/566</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/722/566</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/722/566 [2]</TD>
            <TD>Host galaxies of SNe Ia in SDSS-II SN survey (Lampeitl+, 2010)</TD>
            <TD>In this analysis, we use the full data set from the SDSS-II Supernova Survey (Frieman et al. 2008AJ....135..338F). The SDSS-II SN Survey was a dedicated search for transient objects using the SDSS 2.5m telescope and imaging camera to perform repeat imaging of the "Stripe 82" region of the SDSS survey for three months a year from 2005 to 2007. To ensure that our SN sample is more complete, we also include photometric SNe Ia that have a light curve consistent with being a Type Ia, based on the Bayesian light-curve fitting of Sako et al. (2008, Cat. J/AJ/135/348), and a known host galaxy spectroscopic redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566#2</TD>
            <TD>2012-11-12T12:51:51Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/722/566&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/722/566</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/722/566 [table2]</TD>
            <TD>Host galaxies of SNe Ia in SDSS-II SN survey (Lampeitl+, 2010)</TD>
            <TD>In this analysis, we use the full data set from the SDSS-II Supernova Survey (Frieman et al. 2008AJ....135..338F). The SDSS-II SN Survey was a dedicated search for transient objects using the SDSS 2.5m telescope and imaging camera to perform repeat imaging of the "Stripe 82" region of the SDSS survey for three months a year from 2005 to 2007. To ensure that our SN sample is more complete, we also include photometric SNe Ia that have a light curve consistent with being a Type Ia, based on the Bayesian light-curve fitting of Sako et al. (2008, Cat. J/AJ/135/348), and a known host galaxy spectroscopic redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566#table2</TD>
            <TD>2012-11-12T12:51:51Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/722/566</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/722/566&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/722/566</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/243/390 [1]</TD>
            <TD>Galaxy redshift survey in a Coma strip (Karachentsev+ 1990)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390#1</TD>
            <TD>2011-09-14T18:37:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1994</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/243/390</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/243/390</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/243/390 [2]</TD>
            <TD>Galaxy redshift survey in a Coma strip (Karachentsev+ 1990)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390#2</TD>
            <TD>2011-09-14T18:37:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1994</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/243/390&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/243/390</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/243/390 [table1]</TD>
            <TD>Galaxy redshift survey in a Coma strip (Karachentsev+ 1990)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390#table1</TD>
            <TD>2011-09-14T18:37:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1994</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/243/390</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/243/390&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/243/390</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/112A [1]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112A#1</TD>
            <TD>2012-11-12T16:46:08Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/V/112A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/112A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/112A [2]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112A#2</TD>
            <TD>2012-11-12T16:46:08Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/V/112A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/112A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/112A [catalog]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112A#catalog</TD>
            <TD>2012-11-12T16:46:08Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/V/112A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/112A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112A</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/277/125 [1]</TD>
            <TD>Visual search for galaxies in the Galactic Plane (Hau+ 1995)</TD>
            <TD>We have visually examined 12 Palomar red plates for galaxies at low Galactic latitude b, where the Supergalactic Plane (SGP) is crossed by the Galactic Plane (GP), at Galactic longitude l~135deg. The catalogue consists of 2575 galaxy candidates, of which 462 have major axis diameter d&gt;=0.8arcmin (uncorrected for extinction). Galaxy candidates can be identified down to |b|~0deg. One of our galaxy candidates (J24=Dwingeloo 1) has recently been discovered independently at 21cm by Kraan-Korteweg et al. as a nearby galaxy. Comparisons with structures seen in the IRAs and UGC catalogues are made. We compare the success rate of identifying galaxies using the IRAS Point Source Catalogue under different colour selection criteria. The criteria that require both the 60- and 100-{mu}m fluxes to be of high quality have the highest probability of selecting a galaxy (with d&gt;=0.6arcmin), but at the expense of selecting a smaller number of galaxies in total.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125#1</TD>
            <TD>2011-09-14T18:38:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/277/125</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/277/125</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/277/125 [2]</TD>
            <TD>Visual search for galaxies in the Galactic Plane (Hau+ 1995)</TD>
            <TD>We have visually examined 12 Palomar red plates for galaxies at low Galactic latitude b, where the Supergalactic Plane (SGP) is crossed by the Galactic Plane (GP), at Galactic longitude l~135deg. The catalogue consists of 2575 galaxy candidates, of which 462 have major axis diameter d&gt;=0.8arcmin (uncorrected for extinction). Galaxy candidates can be identified down to |b|~0deg. One of our galaxy candidates (J24=Dwingeloo 1) has recently been discovered independently at 21cm by Kraan-Korteweg et al. as a nearby galaxy. Comparisons with structures seen in the IRAs and UGC catalogues are made. We compare the success rate of identifying galaxies using the IRAS Point Source Catalogue under different colour selection criteria. The criteria that require both the 60- and 100-{mu}m fluxes to be of high quality have the highest probability of selecting a galaxy (with d&gt;=0.6arcmin), but at the expense of selecting a smaller number of galaxies in total.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125#2</TD>
            <TD>2011-09-14T18:38:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/277/125&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/277/125</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/277/125 [table6a]</TD>
            <TD>Visual search for galaxies in the Galactic Plane (Hau+ 1995)</TD>
            <TD>We have visually examined 12 Palomar red plates for galaxies at low Galactic latitude b, where the Supergalactic Plane (SGP) is crossed by the Galactic Plane (GP), at Galactic longitude l~135deg. The catalogue consists of 2575 galaxy candidates, of which 462 have major axis diameter d&gt;=0.8arcmin (uncorrected for extinction). Galaxy candidates can be identified down to |b|~0deg. One of our galaxy candidates (J24=Dwingeloo 1) has recently been discovered independently at 21cm by Kraan-Korteweg et al. as a nearby galaxy. Comparisons with structures seen in the IRAs and UGC catalogues are made. We compare the success rate of identifying galaxies using the IRAS Point Source Catalogue under different colour selection criteria. The criteria that require both the 60- and 100-{mu}m fluxes to be of high quality have the highest probability of selecting a galaxy (with d&gt;=0.6arcmin), but at the expense of selecting a smaller number of galaxies in total.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125#table6a</TD>
            <TD>2011-09-14T18:38:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/277/125&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/277/125</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/112A [1]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112A#1</TD>
            <TD>2012-11-12T16:46:08Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/V/112A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/112A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/112A [2]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112A#2</TD>
            <TD>2012-11-12T16:46:08Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/V/112A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/112A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/112A [catalog]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112A#catalog</TD>
            <TD>2012-11-12T16:46:08Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/V/112A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/112A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112A</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/277/125 [1]</TD>
            <TD>Visual search for galaxies in the Galactic Plane (Hau+ 1995)</TD>
            <TD>We have visually examined 12 Palomar red plates for galaxies at low Galactic latitude b, where the Supergalactic Plane (SGP) is crossed by the Galactic Plane (GP), at Galactic longitude l~135deg. The catalogue consists of 2575 galaxy candidates, of which 462 have major axis diameter d&gt;=0.8arcmin (uncorrected for extinction). Galaxy candidates can be identified down to |b|~0deg. One of our galaxy candidates (J24=Dwingeloo 1) has recently been discovered independently at 21cm by Kraan-Korteweg et al. as a nearby galaxy. Comparisons with structures seen in the IRAs and UGC catalogues are made. We compare the success rate of identifying galaxies using the IRAS Point Source Catalogue under different colour selection criteria. The criteria that require both the 60- and 100-{mu}m fluxes to be of high quality have the highest probability of selecting a galaxy (with d&gt;=0.6arcmin), but at the expense of selecting a smaller number of galaxies in total.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125#1</TD>
            <TD>2011-09-14T18:38:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/277/125</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/277/125</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/277/125 [2]</TD>
            <TD>Visual search for galaxies in the Galactic Plane (Hau+ 1995)</TD>
            <TD>We have visually examined 12 Palomar red plates for galaxies at low Galactic latitude b, where the Supergalactic Plane (SGP) is crossed by the Galactic Plane (GP), at Galactic longitude l~135deg. The catalogue consists of 2575 galaxy candidates, of which 462 have major axis diameter d&gt;=0.8arcmin (uncorrected for extinction). Galaxy candidates can be identified down to |b|~0deg. One of our galaxy candidates (J24=Dwingeloo 1) has recently been discovered independently at 21cm by Kraan-Korteweg et al. as a nearby galaxy. Comparisons with structures seen in the IRAs and UGC catalogues are made. We compare the success rate of identifying galaxies using the IRAS Point Source Catalogue under different colour selection criteria. The criteria that require both the 60- and 100-{mu}m fluxes to be of high quality have the highest probability of selecting a galaxy (with d&gt;=0.6arcmin), but at the expense of selecting a smaller number of galaxies in total.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125#2</TD>
            <TD>2011-09-14T18:38:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/277/125&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/277/125</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/277/125 [table6a]</TD>
            <TD>Visual search for galaxies in the Galactic Plane (Hau+ 1995)</TD>
            <TD>We have visually examined 12 Palomar red plates for galaxies at low Galactic latitude b, where the Supergalactic Plane (SGP) is crossed by the Galactic Plane (GP), at Galactic longitude l~135deg. The catalogue consists of 2575 galaxy candidates, of which 462 have major axis diameter d&gt;=0.8arcmin (uncorrected for extinction). Galaxy candidates can be identified down to |b|~0deg. One of our galaxy candidates (J24=Dwingeloo 1) has recently been discovered independently at 21cm by Kraan-Korteweg et al. as a nearby galaxy. Comparisons with structures seen in the IRAs and UGC catalogues are made. We compare the success rate of identifying galaxies using the IRAS Point Source Catalogue under different colour selection criteria. The criteria that require both the 60- and 100-{mu}m fluxes to be of high quality have the highest probability of selecting a galaxy (with d&gt;=0.6arcmin), but at the expense of selecting a smaller number of galaxies in total.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125#table6a</TD>
            <TD>2011-09-14T18:38:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/277/125&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/277/125</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/112A [1]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112A#1</TD>
            <TD>2012-11-12T16:46:08Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/V/112A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/112A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/112A [2]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112A#2</TD>
            <TD>2012-11-12T16:46:08Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/V/112A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/112A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/112A [catalog]</TD>
            <TD>Catalog of Star-Forming Regions in the Galaxy (Avedisova, 2002)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/112A#catalog</TD>
            <TD>2012-11-12T16:46:08Z</TD>
            <TD>#Galaxies#Nebulae#HII_regions#Masers#YSOs#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/V/112A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/112A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/112A</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/277/125 [1]</TD>
            <TD>Visual search for galaxies in the Galactic Plane (Hau+ 1995)</TD>
            <TD>We have visually examined 12 Palomar red plates for galaxies at low Galactic latitude b, where the Supergalactic Plane (SGP) is crossed by the Galactic Plane (GP), at Galactic longitude l~135deg. The catalogue consists of 2575 galaxy candidates, of which 462 have major axis diameter d&gt;=0.8arcmin (uncorrected for extinction). Galaxy candidates can be identified down to |b|~0deg. One of our galaxy candidates (J24=Dwingeloo 1) has recently been discovered independently at 21cm by Kraan-Korteweg et al. as a nearby galaxy. Comparisons with structures seen in the IRAs and UGC catalogues are made. We compare the success rate of identifying galaxies using the IRAS Point Source Catalogue under different colour selection criteria. The criteria that require both the 60- and 100-{mu}m fluxes to be of high quality have the highest probability of selecting a galaxy (with d&gt;=0.6arcmin), but at the expense of selecting a smaller number of galaxies in total.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125#1</TD>
            <TD>2011-09-14T18:38:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/277/125</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/277/125</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/277/125 [2]</TD>
            <TD>Visual search for galaxies in the Galactic Plane (Hau+ 1995)</TD>
            <TD>We have visually examined 12 Palomar red plates for galaxies at low Galactic latitude b, where the Supergalactic Plane (SGP) is crossed by the Galactic Plane (GP), at Galactic longitude l~135deg. The catalogue consists of 2575 galaxy candidates, of which 462 have major axis diameter d&gt;=0.8arcmin (uncorrected for extinction). Galaxy candidates can be identified down to |b|~0deg. One of our galaxy candidates (J24=Dwingeloo 1) has recently been discovered independently at 21cm by Kraan-Korteweg et al. as a nearby galaxy. Comparisons with structures seen in the IRAs and UGC catalogues are made. We compare the success rate of identifying galaxies using the IRAS Point Source Catalogue under different colour selection criteria. The criteria that require both the 60- and 100-{mu}m fluxes to be of high quality have the highest probability of selecting a galaxy (with d&gt;=0.6arcmin), but at the expense of selecting a smaller number of galaxies in total.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125#2</TD>
            <TD>2011-09-14T18:38:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/277/125&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/277/125</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/277/125 [table6a]</TD>
            <TD>Visual search for galaxies in the Galactic Plane (Hau+ 1995)</TD>
            <TD>We have visually examined 12 Palomar red plates for galaxies at low Galactic latitude b, where the Supergalactic Plane (SGP) is crossed by the Galactic Plane (GP), at Galactic longitude l~135deg. The catalogue consists of 2575 galaxy candidates, of which 462 have major axis diameter d&gt;=0.8arcmin (uncorrected for extinction). Galaxy candidates can be identified down to |b|~0deg. One of our galaxy candidates (J24=Dwingeloo 1) has recently been discovered independently at 21cm by Kraan-Korteweg et al. as a nearby galaxy. Comparisons with structures seen in the IRAs and UGC catalogues are made. We compare the success rate of identifying galaxies using the IRAS Point Source Catalogue under different colour selection criteria. The criteria that require both the 60- and 100-{mu}m fluxes to be of high quality have the highest probability of selecting a galaxy (with d&gt;=0.6arcmin), but at the expense of selecting a smaller number of galaxies in total.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125#table6a</TD>
            <TD>2011-09-14T18:38:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/277/125</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/277/125&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/277/125</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/551/852 [1]</TD>
            <TD>FCRAO CO survey of the outer Galaxy (Heyer+, 2001)</TD>
            <TD>A summary of global properties and an evaluation of the equilibrium state of molecular regions in the outer Galaxy are presented from the decomposition of the Five College Radio Astronomy Observatory (FCRAO, see 1998ApJS..115..241H) Outer Galaxy Survey and targeted ^12^CO and ^13^CO observations (at 115GHz) of four giant molecular cloud complexes. The ensemble of identified objects includes both small, isolated clouds and clumps within larger cloud complexes.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852#1</TD>
            <TD>2012-11-16T16:31:27Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/551/852</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/852</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/551/852 [2]</TD>
            <TD>FCRAO CO survey of the outer Galaxy (Heyer+, 2001)</TD>
            <TD>A summary of global properties and an evaluation of the equilibrium state of molecular regions in the outer Galaxy are presented from the decomposition of the Five College Radio Astronomy Observatory (FCRAO, see 1998ApJS..115..241H) Outer Galaxy Survey and targeted ^12^CO and ^13^CO observations (at 115GHz) of four giant molecular cloud complexes. The ensemble of identified objects includes both small, isolated clouds and clumps within larger cloud complexes.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852#2</TD>
            <TD>2012-11-16T16:31:27Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/551/852&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/852</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/551/852 [table1]</TD>
            <TD>FCRAO CO survey of the outer Galaxy (Heyer+, 2001)</TD>
            <TD>A summary of global properties and an evaluation of the equilibrium state of molecular regions in the outer Galaxy are presented from the decomposition of the Five College Radio Astronomy Observatory (FCRAO, see 1998ApJS..115..241H) Outer Galaxy Survey and targeted ^12^CO and ^13^CO observations (at 115GHz) of four giant molecular cloud complexes. The ensemble of identified objects includes both small, isolated clouds and clumps within larger cloud complexes.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852#table1</TD>
            <TD>2012-11-16T16:31:27Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/551/852&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/852</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/157 [1]</TD>
            <TD>The Extended 12um galaxy sample (Rush+ 1993)</TD>
            <TD>The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/157#1</TD>
            <TD>2011-09-14T18:38:56Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Nonstellar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/157</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/157</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/157 [2]</TD>
            <TD>The Extended 12um galaxy sample (Rush+ 1993)</TD>
            <TD>The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/157#2</TD>
            <TD>2011-09-14T18:38:56Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Nonstellar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/157&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/157</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/157 [12micron]</TD>
            <TD>The Extended 12um galaxy sample (Rush+ 1993)</TD>
            <TD>The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/157#12micron</TD>
            <TD>2011-09-14T18:38:56Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Nonstellar#</TD>
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            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/157</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/157&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/157</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/551/852 [1]</TD>
            <TD>FCRAO CO survey of the outer Galaxy (Heyer+, 2001)</TD>
            <TD>A summary of global properties and an evaluation of the equilibrium state of molecular regions in the outer Galaxy are presented from the decomposition of the Five College Radio Astronomy Observatory (FCRAO, see 1998ApJS..115..241H) Outer Galaxy Survey and targeted ^12^CO and ^13^CO observations (at 115GHz) of four giant molecular cloud complexes. The ensemble of identified objects includes both small, isolated clouds and clumps within larger cloud complexes.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852#1</TD>
            <TD>2012-11-16T16:31:27Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/551/852</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/852</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/551/852 [2]</TD>
            <TD>FCRAO CO survey of the outer Galaxy (Heyer+, 2001)</TD>
            <TD>A summary of global properties and an evaluation of the equilibrium state of molecular regions in the outer Galaxy are presented from the decomposition of the Five College Radio Astronomy Observatory (FCRAO, see 1998ApJS..115..241H) Outer Galaxy Survey and targeted ^12^CO and ^13^CO observations (at 115GHz) of four giant molecular cloud complexes. The ensemble of identified objects includes both small, isolated clouds and clumps within larger cloud complexes.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852#2</TD>
            <TD>2012-11-16T16:31:27Z</TD>
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            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852</TD>
            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/551/852&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/852</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/551/852 [table1]</TD>
            <TD>FCRAO CO survey of the outer Galaxy (Heyer+, 2001)</TD>
            <TD>A summary of global properties and an evaluation of the equilibrium state of molecular regions in the outer Galaxy are presented from the decomposition of the Five College Radio Astronomy Observatory (FCRAO, see 1998ApJS..115..241H) Outer Galaxy Survey and targeted ^12^CO and ^13^CO observations (at 115GHz) of four giant molecular cloud complexes. The ensemble of identified objects includes both small, isolated clouds and clumps within larger cloud complexes.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/ApJ/551/852#table1</TD>
            <TD>2012-11-16T16:31:27Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/551/852&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/852</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/157 [1]</TD>
            <TD>The Extended 12um galaxy sample (Rush+ 1993)</TD>
            <TD>The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/157#1</TD>
            <TD>2011-09-14T18:38:56Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Nonstellar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/157</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/157</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/157 [2]</TD>
            <TD>The Extended 12um galaxy sample (Rush+ 1993)</TD>
            <TD>The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/157#2</TD>
            <TD>2011-09-14T18:38:56Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Nonstellar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/157&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/157</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/157 [12micron]</TD>
            <TD>The Extended 12um galaxy sample (Rush+ 1993)</TD>
            <TD>The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
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            <TD>2011-09-14T18:38:56Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Nonstellar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/157</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/157&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/157</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/551/852 [1]</TD>
            <TD>FCRAO CO survey of the outer Galaxy (Heyer+, 2001)</TD>
            <TD>A summary of global properties and an evaluation of the equilibrium state of molecular regions in the outer Galaxy are presented from the decomposition of the Five College Radio Astronomy Observatory (FCRAO, see 1998ApJS..115..241H) Outer Galaxy Survey and targeted ^12^CO and ^13^CO observations (at 115GHz) of four giant molecular cloud complexes. The ensemble of identified objects includes both small, isolated clouds and clumps within larger cloud complexes.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852#1</TD>
            <TD>2012-11-16T16:31:27Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/551/852</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/852</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/551/852 [2]</TD>
            <TD>FCRAO CO survey of the outer Galaxy (Heyer+, 2001)</TD>
            <TD>A summary of global properties and an evaluation of the equilibrium state of molecular regions in the outer Galaxy are presented from the decomposition of the Five College Radio Astronomy Observatory (FCRAO, see 1998ApJS..115..241H) Outer Galaxy Survey and targeted ^12^CO and ^13^CO observations (at 115GHz) of four giant molecular cloud complexes. The ensemble of identified objects includes both small, isolated clouds and clumps within larger cloud complexes.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852#2</TD>
            <TD>2012-11-16T16:31:27Z</TD>
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            <TD>ivo://CDS.VizieR/J/ApJ/551/852</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/551/852&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/852</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/551/852 [table1]</TD>
            <TD>FCRAO CO survey of the outer Galaxy (Heyer+, 2001)</TD>
            <TD>A summary of global properties and an evaluation of the equilibrium state of molecular regions in the outer Galaxy are presented from the decomposition of the Five College Radio Astronomy Observatory (FCRAO, see 1998ApJS..115..241H) Outer Galaxy Survey and targeted ^12^CO and ^13^CO observations (at 115GHz) of four giant molecular cloud complexes. The ensemble of identified objects includes both small, isolated clouds and clumps within larger cloud complexes.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852#table1</TD>
            <TD>2012-11-16T16:31:27Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/852</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/551/852&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/852</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/157 [1]</TD>
            <TD>The Extended 12um galaxy sample (Rush+ 1993)</TD>
            <TD>The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/157#1</TD>
            <TD>2011-09-14T18:38:56Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Nonstellar#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/157</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/157</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/157 [2]</TD>
            <TD>The Extended 12um galaxy sample (Rush+ 1993)</TD>
            <TD>The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/157#2</TD>
            <TD>2011-09-14T18:38:56Z</TD>
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            <TD>#Catalog#</TD>
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            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/157&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/157</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/157 [12micron]</TD>
            <TD>The Extended 12um galaxy sample (Rush+ 1993)</TD>
            <TD>The authors have used the IRAS data to compile a sample of 893 galaxies, including 118 Seyfert galaxies. Please refer to the "12micron.doc" (ascii) or "12micron.tex" (LaTeX) file for complete descriptions.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/157#12micron</TD>
            <TD>2011-09-14T18:38:56Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Nonstellar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/157</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/157&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/157</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/142A [1]</TD>
            <TD>Southern Redshifts Catalogue (Fairall+, 1991)</TD>
            <TD>Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarily lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilities and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/142A#1</TD>
            <TD>2012-11-13T06:47:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/VII/142A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/142A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/142A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/142A [2]</TD>
            <TD>Southern Redshifts Catalogue (Fairall+, 1991)</TD>
            <TD>Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarily lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilities and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.</TD>
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            <TD>Catalog</TD>
            <TD>VII/142A [catalog]</TD>
            <TD>Southern Redshifts Catalogue (Fairall+, 1991)</TD>
            <TD>Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarily lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilities and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2012-11-13T06:47:25Z</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>VII/36 [1]</TD>
            <TD>Galaxy Redshifts (Rood 1980)</TD>
            <TD>The Catalog of Galaxy Redshifts was compiled by Dr. Rood to enter the most accurate redshift for each entry in the Uppsala General Catalog of Galaxies below 15000 km/s, plus some fainter galaxies in the fields of rich clusters, plus some southern galaxies. The catalog is 99 percent complete for declinations north of -2.5deg and blue magnitude (Pmag) brighter than 13. The present documentation is mostly adapted from the "Documentation of the Machine-Readable Version of the Catalog of Galaxy Redshifts" by Theresa A. Nagy and Robert S. Hill, May 1981, prepared for NASA GSFC, Greenbelt, No SSD-T-5069-0013-81.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/VII/36#1</TD>
            <TD>2011-09-14T18:39:12Z</TD>
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            <TD>04-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/VII/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/36</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/36</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/36 [2]</TD>
            <TD>Galaxy Redshifts (Rood 1980)</TD>
            <TD>The Catalog of Galaxy Redshifts was compiled by Dr. Rood to enter the most accurate redshift for each entry in the Uppsala General Catalog of Galaxies below 15000 km/s, plus some fainter galaxies in the fields of rich clusters, plus some southern galaxies. The catalog is 99 percent complete for declinations north of -2.5deg and blue magnitude (Pmag) brighter than 13. The present documentation is mostly adapted from the "Documentation of the Machine-Readable Version of the Catalog of Galaxy Redshifts" by Theresa A. Nagy and Robert S. Hill, May 1981, prepared for NASA GSFC, Greenbelt, No SSD-T-5069-0013-81.</TD>
            <TD>CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>VII/36 [catalog]</TD>
            <TD>Galaxy Redshifts (Rood 1980)</TD>
            <TD>The Catalog of Galaxy Redshifts was compiled by Dr. Rood to enter the most accurate redshift for each entry in the Uppsala General Catalog of Galaxies below 15000 km/s, plus some fainter galaxies in the fields of rich clusters, plus some southern galaxies. The catalog is 99 percent complete for declinations north of -2.5deg and blue magnitude (Pmag) brighter than 13. The present documentation is mostly adapted from the "Documentation of the Machine-Readable Version of the Catalog of Galaxy Redshifts" by Theresa A. Nagy and Robert S. Hill, May 1981, prepared for NASA GSFC, Greenbelt, No SSD-T-5069-0013-81.</TD>
            <TD>CDS</TD>
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/36</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/142A [1]</TD>
            <TD>Southern Redshifts Catalogue (Fairall+, 1991)</TD>
            <TD>Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarily lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilities and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/142A#1</TD>
            <TD>2012-11-13T06:47:25Z</TD>
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            <TD>#Catalog#</TD>
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            <TD>26-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/VII/142A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/142A</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/142A</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/142A [2]</TD>
            <TD>Southern Redshifts Catalogue (Fairall+, 1991)</TD>
            <TD>Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarily lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilities and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/142A#2</TD>
            <TD>2012-11-13T06:47:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/VII/142A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/142A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/142A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/142A [catalog]</TD>
            <TD>Southern Redshifts Catalogue (Fairall+, 1991)</TD>
            <TD>Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarily lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilities and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/142A#catalog</TD>
            <TD>2012-11-13T06:47:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/VII/142A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/142A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/142A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/36 [1]</TD>
            <TD>Galaxy Redshifts (Rood 1980)</TD>
            <TD>The Catalog of Galaxy Redshifts was compiled by Dr. Rood to enter the most accurate redshift for each entry in the Uppsala General Catalog of Galaxies below 15000 km/s, plus some fainter galaxies in the fields of rich clusters, plus some southern galaxies. The catalog is 99 percent complete for declinations north of -2.5deg and blue magnitude (Pmag) brighter than 13. The present documentation is mostly adapted from the "Documentation of the Machine-Readable Version of the Catalog of Galaxy Redshifts" by Theresa A. Nagy and Robert S. Hill, May 1981, prepared for NASA GSFC, Greenbelt, No SSD-T-5069-0013-81.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/36#1</TD>
            <TD>2011-09-14T18:39:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/VII/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/36</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/36</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/36 [2]</TD>
            <TD>Galaxy Redshifts (Rood 1980)</TD>
            <TD>The Catalog of Galaxy Redshifts was compiled by Dr. Rood to enter the most accurate redshift for each entry in the Uppsala General Catalog of Galaxies below 15000 km/s, plus some fainter galaxies in the fields of rich clusters, plus some southern galaxies. The catalog is 99 percent complete for declinations north of -2.5deg and blue magnitude (Pmag) brighter than 13. The present documentation is mostly adapted from the "Documentation of the Machine-Readable Version of the Catalog of Galaxy Redshifts" by Theresa A. Nagy and Robert S. Hill, May 1981, prepared for NASA GSFC, Greenbelt, No SSD-T-5069-0013-81.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/36#2</TD>
            <TD>2011-09-14T18:39:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/VII/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/36&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/36 [catalog]</TD>
            <TD>Galaxy Redshifts (Rood 1980)</TD>
            <TD>The Catalog of Galaxy Redshifts was compiled by Dr. Rood to enter the most accurate redshift for each entry in the Uppsala General Catalog of Galaxies below 15000 km/s, plus some fainter galaxies in the fields of rich clusters, plus some southern galaxies. The catalog is 99 percent complete for declinations north of -2.5deg and blue magnitude (Pmag) brighter than 13. The present documentation is mostly adapted from the "Documentation of the Machine-Readable Version of the Catalog of Galaxy Redshifts" by Theresa A. Nagy and Robert S. Hill, May 1981, prepared for NASA GSFC, Greenbelt, No SSD-T-5069-0013-81.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/36#catalog</TD>
            <TD>2011-09-14T18:39:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/VII/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/36</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/142A [1]</TD>
            <TD>Southern Redshifts Catalogue (Fairall+, 1991)</TD>
            <TD>Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarily lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilities and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/142A#1</TD>
            <TD>2012-11-13T06:47:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/VII/142A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/142A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/142A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/142A [2]</TD>
            <TD>Southern Redshifts Catalogue (Fairall+, 1991)</TD>
            <TD>Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarily lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilities and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/142A#2</TD>
            <TD>2012-11-13T06:47:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/VII/142A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/142A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/142A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/142A [catalog]</TD>
            <TD>Southern Redshifts Catalogue (Fairall+, 1991)</TD>
            <TD>Previous Versions of this Work: 1981 Catalogue "A Simple Source Catalogue of Galaxies south of Declination -17.5 degrees that have been observed spectroscopically" P.J.K. Dobbie and A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 4. 1983 Catalogue "A Catalogue of Galaxies south of Declination -30 degrees that have been observed spectroscopically" A.P. Fairall, L. Lowe and P.J.K. Dobbie, Publ. Dept. Astr. Univ. Cape Town, No. 5. 1983 Plots "The Spatial Distribution of Galaxies in the Southern Sky" H. Winkler, Mon. Not. Astr. Soc. Sthn. Africa, 42, 74. "The Spatial Distribution of Galaxies in the Southern Sky" A.P. Fairall and H. Winkler in "Clusters and Groups of Galaxies", p. 23. F. Mardirossian et al. (Eds.) Reidel, 1984. 1984 Plots "A Southern Redshift Survey - Redshift-Space Distributions of Normal and Active Galaxies South of Declination -30 degrees" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 6. 1985 Catalogue "A Catalogue of Galaxies South of Declination -30 degrees that have been observed spectroscopically (1985 Version)" A.P. Fairall, Publ. Dept. Astr. Univ. Cape Town, No. 7. Machine-Readable Version by Anne C. Raugh (March 1987) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1988 Catalogue and Plots "Southern Redshifts - Catalogue and plots" A.P. Fairall and A. Jones, Publ. Dept. Astr. Univ. Cape Town, No. 10. Machine-Readable Version by Anne C. Raugh (January 1989) distributed by the Astronomical Data Center, NASA Goddard Space Flight Center. 1990 Plots "Large-Scale Structure in the Universe: Plots from the Updated Catalogue of Radial Velocities of Galaxies and the Southern Redshift Catalogue" A.P. Fairall, G.G.C. Palumbo, G. Vettolani, G. Kauffmann, A. Jones and G. Baiesi-Pillastrini, Mon. Not. R. astr. Soc., 247, 21P. Coverage and Completeness: This catalogue was first published in 1981. The present work is an update and extension of the 4th version, completed in January 1988. Since that version, the northern Declination limit has been shifted from -17.5 degrees to the equator, and radio velocities have been included. The new version, including updated references, has just over double the number of galaxies in the previous version. Whilst most of the references are original source papers, the catalogue was founded on the de Vaucouleurs Second Reference Catalogue (Ref 001) to take care of references prior to 1975. In similar fashion, the HI database of Bottinelli et al (Ref 150), published in 1990, has been used to fill in many of the radio velocities. Literature searches have been made covering the main journals up to Apr-Jun 1991. Whilst the aim is to obtain all available redshifts, experience has shown that, inevitably, some references are overlooked, and no claim to completeness can be made. This is particularly applicable to the Declination zone 0 to -17.5 degrees, into which the catalogue has recently been extended. Apologies are made to any author whose work has been unintentionally omitted. The authors would obviously welcome any reports regarding reference coverage. The preparation of a definitive catalogue that includes all sources, with exhaustive searching and detailed checking, is a major task. Its coverage must necessarily lag behind current literature. The present work does not claim to be a definitive work, but its coverage is up to only 3 or 4 months short of its publication. Past versions of this catalogue have been well received, and demand has prompted the preparation of the new version. One of the authors (A.P.F.) is also involved in the preparation of the definitive updated version of the "Catalogue of Radial Velocities of Galaxies" with G.G.C. Palumbo, G. Vettolani and G. Baiesi-Pillastrini, based in Bologna. That catalogue shows all individual measurements for galaxies over the whole sky. A significant fraction of the effort to produce a catalogue of this nature goes to dealing with references that give only designations (not always obvious ones) of galaxies without providing their coordinates - or which give only galactocentric, not heliocentric, velocities. Such references can take a considerable amount of processing, even before they are entered. Authors and referees should appreciate the importance of accurate coordinates (even with obvious NGC galaxies) for identification purposes. The released version of this catalogue is a public version. The full catalogue does include a few hundred addition redshifts (obtained at the South African Astronomical Observatory, in collaboration with L. da Costa and his group) that have not yet been published. Computer Management of the Catalogue: The catalogue is managed in IBM-compatible PCs using dedicated software developed by one of the authors. It allows almost instant access to galaxies at any coordinate position, or within a chosen error box. It offers full editing facilities and can produce ASCII files etc. The procedure for entering a new velocity determination is initiated by typing in (or interactively feeding from a file) the 1950 coordinates. The computer then searches within 1m in R.A. and 2 arcmin in Declination (the generous range in R.A. is to allow for objects close to the pole), so to determine if an entry for the galaxy already exists. The option is then given to decide whether to add a new entry or edit an existing one. One of the features of the software package is the identification of any form of subset of the data - such as all galaxies within a specified range of R.A. and Declination, range of galactic longitude and latitude, specified velocity range or common velocity flag, common reference or common type. Obviously such subsets are not available in this publication, but special requests can be considered. Hardcopy and Computer-readable Versions of this Catalogue: This catalogue is being distributed in two forms. One is a conventional printed version, the other is a weight-reduced version with the catalogue and reference lists compressed onto a computer diskette. The computer-readable version is distributed by the Strasbourg and Goddard data centres.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/142A#catalog</TD>
            <TD>2012-11-13T06:47:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/VII/142A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/142A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/142A</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/671/333 [1]</TD>
            <TD>Aperture photometry in NGC 5194 (Kennicutt+, 2007)</TD>
            <TD>Spitzer MIPS observations of M51a at 24um were obtained on 22 and 23 June 2004, as part of the SINGS Legacy Program. Narrowband images centered at Halpha and continuum R-band images were obtained on 2001 March 28, with the Cassegrain Focus CCD Imager on the 2.1m telescope at Kitt Peak National Observatory, as part of the SINGS ancillary data program. Archival HST/NICMOS images of the central 144", corresponding to the inner ~6kpc of the galaxy, are available in the Pa{alpha} emission line (1.8756 um, F187N narrow-band filter) and the adjacent continuum (F190N narrow-band filter). HI data for M51a have been obtained through The H I Nearby Galaxy Survey (THINGS), a survey dedicated to obtain high-resolution VLA H I imaging for ~35 nearby galaxies. M51 was observed in the VLA D (2004 July 9), C (2004 April 26), and B array (2005 March 5). The CO J=1-0 map of M51a was obtained as part of the BIMA Survey Of Nearby Galaxies (BIMA SONG).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333#1</TD>
            <TD>2011-09-14T20:56:05Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/671/333</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/333</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/671/333 [2]</TD>
            <TD>Aperture photometry in NGC 5194 (Kennicutt+, 2007)</TD>
            <TD>Spitzer MIPS observations of M51a at 24um were obtained on 22 and 23 June 2004, as part of the SINGS Legacy Program. Narrowband images centered at Halpha and continuum R-band images were obtained on 2001 March 28, with the Cassegrain Focus CCD Imager on the 2.1m telescope at Kitt Peak National Observatory, as part of the SINGS ancillary data program. Archival HST/NICMOS images of the central 144", corresponding to the inner ~6kpc of the galaxy, are available in the Pa{alpha} emission line (1.8756 um, F187N narrow-band filter) and the adjacent continuum (F190N narrow-band filter). HI data for M51a have been obtained through The H I Nearby Galaxy Survey (THINGS), a survey dedicated to obtain high-resolution VLA H I imaging for ~35 nearby galaxies. M51 was observed in the VLA D (2004 July 9), C (2004 April 26), and B array (2005 March 5). The CO J=1-0 map of M51a was obtained as part of the BIMA Survey Of Nearby Galaxies (BIMA SONG).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333#2</TD>
            <TD>2011-09-14T20:56:05Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/671/333&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/333</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/671/333 [table1]</TD>
            <TD>Aperture photometry in NGC 5194 (Kennicutt+, 2007)</TD>
            <TD>Spitzer MIPS observations of M51a at 24um were obtained on 22 and 23 June 2004, as part of the SINGS Legacy Program. Narrowband images centered at Halpha and continuum R-band images were obtained on 2001 March 28, with the Cassegrain Focus CCD Imager on the 2.1m telescope at Kitt Peak National Observatory, as part of the SINGS ancillary data program. Archival HST/NICMOS images of the central 144", corresponding to the inner ~6kpc of the galaxy, are available in the Pa{alpha} emission line (1.8756 um, F187N narrow-band filter) and the adjacent continuum (F190N narrow-band filter). HI data for M51a have been obtained through The H I Nearby Galaxy Survey (THINGS), a survey dedicated to obtain high-resolution VLA H I imaging for ~35 nearby galaxies. M51 was observed in the VLA D (2004 July 9), C (2004 April 26), and B array (2005 March 5). The CO J=1-0 map of M51a was obtained as part of the BIMA Survey Of Nearby Galaxies (BIMA SONG).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333#table1</TD>
            <TD>2011-09-14T20:56:05Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/671/333&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/333</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/36 [1]</TD>
            <TD>Galaxy Redshifts (Rood 1980)</TD>
            <TD>The Catalog of Galaxy Redshifts was compiled by Dr. Rood to enter the most accurate redshift for each entry in the Uppsala General Catalog of Galaxies below 15000 km/s, plus some fainter galaxies in the fields of rich clusters, plus some southern galaxies. The catalog is 99 percent complete for declinations north of -2.5deg and blue magnitude (Pmag) brighter than 13. The present documentation is mostly adapted from the "Documentation of the Machine-Readable Version of the Catalog of Galaxy Redshifts" by Theresa A. Nagy and Robert S. Hill, May 1981, prepared for NASA GSFC, Greenbelt, No SSD-T-5069-0013-81.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/36#1</TD>
            <TD>2011-09-14T18:39:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/VII/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/36</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/36</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/36 [2]</TD>
            <TD>Galaxy Redshifts (Rood 1980)</TD>
            <TD>The Catalog of Galaxy Redshifts was compiled by Dr. Rood to enter the most accurate redshift for each entry in the Uppsala General Catalog of Galaxies below 15000 km/s, plus some fainter galaxies in the fields of rich clusters, plus some southern galaxies. The catalog is 99 percent complete for declinations north of -2.5deg and blue magnitude (Pmag) brighter than 13. The present documentation is mostly adapted from the "Documentation of the Machine-Readable Version of the Catalog of Galaxy Redshifts" by Theresa A. Nagy and Robert S. Hill, May 1981, prepared for NASA GSFC, Greenbelt, No SSD-T-5069-0013-81.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/36#2</TD>
            <TD>2011-09-14T18:39:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/VII/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/36&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/36 [catalog]</TD>
            <TD>Galaxy Redshifts (Rood 1980)</TD>
            <TD>The Catalog of Galaxy Redshifts was compiled by Dr. Rood to enter the most accurate redshift for each entry in the Uppsala General Catalog of Galaxies below 15000 km/s, plus some fainter galaxies in the fields of rich clusters, plus some southern galaxies. The catalog is 99 percent complete for declinations north of -2.5deg and blue magnitude (Pmag) brighter than 13. The present documentation is mostly adapted from the "Documentation of the Machine-Readable Version of the Catalog of Galaxy Redshifts" by Theresa A. Nagy and Robert S. Hill, May 1981, prepared for NASA GSFC, Greenbelt, No SSD-T-5069-0013-81.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/36#catalog</TD>
            <TD>2011-09-14T18:39:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1995</TD>
            <TD>ivo://CDS.VizieR/VII/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/151 [1]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#1</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/151</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/151 [2]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#2</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/151&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table2c]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table2c</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table2a]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table2a</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table1a]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table1a</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table1c]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table1c</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table1b]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table1b</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table2b]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table2b</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/70A [1]</TD>
            <TD>Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983)</TD>
            <TD>The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/70A#1</TD>
            <TD>2011-09-14T18:39:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/VII/70A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/70A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/70A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/70A [2]</TD>
            <TD>Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983)</TD>
            <TD>The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/70A#2</TD>
            <TD>2011-09-14T18:39:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/VII/70A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/70A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/70A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/70A [data]</TD>
            <TD>Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983)</TD>
            <TD>The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/70A#data</TD>
            <TD>2011-09-14T18:39:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/VII/70A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/70A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/70A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/70A [1]</TD>
            <TD>Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983)</TD>
            <TD>The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/70A#1</TD>
            <TD>2011-09-14T18:39:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/VII/70A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/70A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/70A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/70A [2]</TD>
            <TD>Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983)</TD>
            <TD>The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/70A#2</TD>
            <TD>2011-09-14T18:39:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/VII/70A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/70A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/70A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/70A [data]</TD>
            <TD>Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983)</TD>
            <TD>The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/70A#data</TD>
            <TD>2011-09-14T18:39:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/VII/70A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/70A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/70A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/671/333 [1]</TD>
            <TD>Aperture photometry in NGC 5194 (Kennicutt+, 2007)</TD>
            <TD>Spitzer MIPS observations of M51a at 24um were obtained on 22 and 23 June 2004, as part of the SINGS Legacy Program. Narrowband images centered at Halpha and continuum R-band images were obtained on 2001 March 28, with the Cassegrain Focus CCD Imager on the 2.1m telescope at Kitt Peak National Observatory, as part of the SINGS ancillary data program. Archival HST/NICMOS images of the central 144", corresponding to the inner ~6kpc of the galaxy, are available in the Pa{alpha} emission line (1.8756 um, F187N narrow-band filter) and the adjacent continuum (F190N narrow-band filter). HI data for M51a have been obtained through The H I Nearby Galaxy Survey (THINGS), a survey dedicated to obtain high-resolution VLA H I imaging for ~35 nearby galaxies. M51 was observed in the VLA D (2004 July 9), C (2004 April 26), and B array (2005 March 5). The CO J=1-0 map of M51a was obtained as part of the BIMA Survey Of Nearby Galaxies (BIMA SONG).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333#1</TD>
            <TD>2011-09-14T20:56:05Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/671/333</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/333</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/671/333 [2]</TD>
            <TD>Aperture photometry in NGC 5194 (Kennicutt+, 2007)</TD>
            <TD>Spitzer MIPS observations of M51a at 24um were obtained on 22 and 23 June 2004, as part of the SINGS Legacy Program. Narrowband images centered at Halpha and continuum R-band images were obtained on 2001 March 28, with the Cassegrain Focus CCD Imager on the 2.1m telescope at Kitt Peak National Observatory, as part of the SINGS ancillary data program. Archival HST/NICMOS images of the central 144", corresponding to the inner ~6kpc of the galaxy, are available in the Pa{alpha} emission line (1.8756 um, F187N narrow-band filter) and the adjacent continuum (F190N narrow-band filter). HI data for M51a have been obtained through The H I Nearby Galaxy Survey (THINGS), a survey dedicated to obtain high-resolution VLA H I imaging for ~35 nearby galaxies. M51 was observed in the VLA D (2004 July 9), C (2004 April 26), and B array (2005 March 5). The CO J=1-0 map of M51a was obtained as part of the BIMA Survey Of Nearby Galaxies (BIMA SONG).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333#2</TD>
            <TD>2011-09-14T20:56:05Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/671/333&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/333</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/671/333 [table1]</TD>
            <TD>Aperture photometry in NGC 5194 (Kennicutt+, 2007)</TD>
            <TD>Spitzer MIPS observations of M51a at 24um were obtained on 22 and 23 June 2004, as part of the SINGS Legacy Program. Narrowband images centered at Halpha and continuum R-band images were obtained on 2001 March 28, with the Cassegrain Focus CCD Imager on the 2.1m telescope at Kitt Peak National Observatory, as part of the SINGS ancillary data program. Archival HST/NICMOS images of the central 144", corresponding to the inner ~6kpc of the galaxy, are available in the Pa{alpha} emission line (1.8756 um, F187N narrow-band filter) and the adjacent continuum (F190N narrow-band filter). HI data for M51a have been obtained through The H I Nearby Galaxy Survey (THINGS), a survey dedicated to obtain high-resolution VLA H I imaging for ~35 nearby galaxies. M51 was observed in the VLA D (2004 July 9), C (2004 April 26), and B array (2005 March 5). The CO J=1-0 map of M51a was obtained as part of the BIMA Survey Of Nearby Galaxies (BIMA SONG).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333#table1</TD>
            <TD>2011-09-14T20:56:05Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/333</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/671/333&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/333</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/70A [1]</TD>
            <TD>Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983)</TD>
            <TD>The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/70A#1</TD>
            <TD>2011-09-14T18:39:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/VII/70A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/70A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/70A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/70A [2]</TD>
            <TD>Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983)</TD>
            <TD>The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/70A#2</TD>
            <TD>2011-09-14T18:39:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/VII/70A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/70A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/70A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/70A [data]</TD>
            <TD>Galaxies Rotation Curves (Baiesi-Pillastrini+ 1983)</TD>
            <TD>The catalog contains all bibliographical information pertaining to rotation curves of external galaxies that have appeared in the astronomical literature up to 1981 December. Information about 271 galaxies is given from 332 papers. The catalog includes galaxy names, morphological types, positions, radial velocities, approximate extent of the rotation curves from the centers of the galaxies, and references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/70A#data</TD>
            <TD>2011-09-14T18:39:20Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/VII/70A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/70A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/70A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/1438 [1]</TD>
            <TD>NGC 205 BVRI photometry (Lee 1996)</TD>
            <TD>BVRI/CCD photometry of ~2,300 stars in the central 2.2'x3.5' area of the dwarf elliptical galaxy NGC205 in the Local Group is presented. The color-magnitude diagrams of NGC 205 show: (1) a blue plume around (B-V)~0.0mag, extending up to V~19.3mag (M_V_~-5.4mag); and (2) a strong asymptotic giant branch (AGB) population, the brightest of which reaches I~19.0mag, 1.5 mag brighter than the tip of the red giant branch. BVRI photometry of three globular clusters (Hubble IV. V, and VI) is also presented. Hubble V is much bluer [(B-V)=0.37] than other globular clusters. This blue color of Hubble V leads to an estimate of the age, ~300Myrs. A V luminosity function for the blue stars has been derived: the logarithmic slope of the luminosity function for -5.7&lt;M_V_&lt;-3.2 is 0.64+/-0.12, which is similar to those of other nearby galaxies. The AGB stars extend to Mbol~-5.7mag, which is ~0.7mag brighter than those in NGC 185. The bolometric luminosity function of the AGB stars in NGC 205 is found to be flatter than that of the similar dwarf elliptical galaxy NGC 185, but similar to that of a bulge field 4' of the nucleus of M31. Surface photometry for the central area within R=50" is presented, showing that the colors get bluer as the galactocentric radius decreases except for the nucleus region within R=1.6" where the colors get redder inward. Star formation history in NGC 205 is briefly discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1438#1</TD>
            <TD>2011-09-14T18:39:36Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1438</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/1438</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1438</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/1438 [2]</TD>
            <TD>NGC 205 BVRI photometry (Lee 1996)</TD>
            <TD>BVRI/CCD photometry of ~2,300 stars in the central 2.2'x3.5' area of the dwarf elliptical galaxy NGC205 in the Local Group is presented. The color-magnitude diagrams of NGC 205 show: (1) a blue plume around (B-V)~0.0mag, extending up to V~19.3mag (M_V_~-5.4mag); and (2) a strong asymptotic giant branch (AGB) population, the brightest of which reaches I~19.0mag, 1.5 mag brighter than the tip of the red giant branch. BVRI photometry of three globular clusters (Hubble IV. V, and VI) is also presented. Hubble V is much bluer [(B-V)=0.37] than other globular clusters. This blue color of Hubble V leads to an estimate of the age, ~300Myrs. A V luminosity function for the blue stars has been derived: the logarithmic slope of the luminosity function for -5.7&lt;M_V_&lt;-3.2 is 0.64+/-0.12, which is similar to those of other nearby galaxies. The AGB stars extend to Mbol~-5.7mag, which is ~0.7mag brighter than those in NGC 185. The bolometric luminosity function of the AGB stars in NGC 205 is found to be flatter than that of the similar dwarf elliptical galaxy NGC 185, but similar to that of a bulge field 4' of the nucleus of M31. Surface photometry for the central area within R=50" is presented, showing that the colors get bluer as the galactocentric radius decreases except for the nucleus region within R=1.6" where the colors get redder inward. Star formation history in NGC 205 is briefly discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1438#2</TD>
            <TD>2011-09-14T18:39:36Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1438</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/1438&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1438</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/151 [1]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#1</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/151</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/151 [2]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#2</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/151&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table2c]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table2c</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table2a]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table2a</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table1a]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table1a</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table1c]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table1c</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table1b]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table1b</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table2b]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table2b</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/1438 [1]</TD>
            <TD>NGC 205 BVRI photometry (Lee 1996)</TD>
            <TD>BVRI/CCD photometry of ~2,300 stars in the central 2.2'x3.5' area of the dwarf elliptical galaxy NGC205 in the Local Group is presented. The color-magnitude diagrams of NGC 205 show: (1) a blue plume around (B-V)~0.0mag, extending up to V~19.3mag (M_V_~-5.4mag); and (2) a strong asymptotic giant branch (AGB) population, the brightest of which reaches I~19.0mag, 1.5 mag brighter than the tip of the red giant branch. BVRI photometry of three globular clusters (Hubble IV. V, and VI) is also presented. Hubble V is much bluer [(B-V)=0.37] than other globular clusters. This blue color of Hubble V leads to an estimate of the age, ~300Myrs. A V luminosity function for the blue stars has been derived: the logarithmic slope of the luminosity function for -5.7&lt;M_V_&lt;-3.2 is 0.64+/-0.12, which is similar to those of other nearby galaxies. The AGB stars extend to Mbol~-5.7mag, which is ~0.7mag brighter than those in NGC 185. The bolometric luminosity function of the AGB stars in NGC 205 is found to be flatter than that of the similar dwarf elliptical galaxy NGC 185, but similar to that of a bulge field 4' of the nucleus of M31. Surface photometry for the central area within R=50" is presented, showing that the colors get bluer as the galactocentric radius decreases except for the nucleus region within R=1.6" where the colors get redder inward. Star formation history in NGC 205 is briefly discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1438#1</TD>
            <TD>2011-09-14T18:39:36Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1438</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/1438</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1438</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/1438 [2]</TD>
            <TD>NGC 205 BVRI photometry (Lee 1996)</TD>
            <TD>BVRI/CCD photometry of ~2,300 stars in the central 2.2'x3.5' area of the dwarf elliptical galaxy NGC205 in the Local Group is presented. The color-magnitude diagrams of NGC 205 show: (1) a blue plume around (B-V)~0.0mag, extending up to V~19.3mag (M_V_~-5.4mag); and (2) a strong asymptotic giant branch (AGB) population, the brightest of which reaches I~19.0mag, 1.5 mag brighter than the tip of the red giant branch. BVRI photometry of three globular clusters (Hubble IV. V, and VI) is also presented. Hubble V is much bluer [(B-V)=0.37] than other globular clusters. This blue color of Hubble V leads to an estimate of the age, ~300Myrs. A V luminosity function for the blue stars has been derived: the logarithmic slope of the luminosity function for -5.7&lt;M_V_&lt;-3.2 is 0.64+/-0.12, which is similar to those of other nearby galaxies. The AGB stars extend to Mbol~-5.7mag, which is ~0.7mag brighter than those in NGC 185. The bolometric luminosity function of the AGB stars in NGC 205 is found to be flatter than that of the similar dwarf elliptical galaxy NGC 185, but similar to that of a bulge field 4' of the nucleus of M31. Surface photometry for the central area within R=50" is presented, showing that the colors get bluer as the galactocentric radius decreases except for the nucleus region within R=1.6" where the colors get redder inward. Star formation history in NGC 205 is briefly discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1438#2</TD>
            <TD>2011-09-14T18:39:36Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1438</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/1438&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1438</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/151 [1]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#1</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/151</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/151 [2]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#2</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/151&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table2c]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table2c</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table2a]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table2a</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table1a]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table1a</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table1c]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table1c</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table1b]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table1b</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/151 [table2b]</TD>
            <TD>Structure Parameters of Galactic Globular Clusters (Webbink 1985)</TD>
            <TD>This catalog contains observed and derived structure parameters for 154 galactic globular clusters, 7 dwarf spheroidal satellites of the Galaxy, and 6 globular clusters in the Fornax dwarf spheroids, respectively, in six different files. Files 1-3 (table1a, table1b, &amp; table1c) list observed parameters, including cluster designation in order of right ascension, equatorial coordinates (B1950), apparent level of the cluster horizontal branch, reddening, subgiant branch color, limiting and core angular radii, ellipticities (only for table1b), integrated magnitude and central surface brightness. Files 4-6 (table2a, table2b, &amp; table2c) contain positional and structural data derived from the observational data of table1. These include, for instance, galactic and galactocentric or Cartesian coordinates, heliocentric and galactocentric distances, or angular and projected linear distances, position angle, metallicity, limiting and core radii, central relaxation time scale, central mass density, central velocity dispersion, and central escape velocity. The references (all columns which label start by r_) are not available in electronic form.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/151#table2b</TD>
            <TD>2012-11-13T06:47:40Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/151</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/409 [1]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#1</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/409</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/409 [2]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#2</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/409&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/409 [table1]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#table1</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/409 [table2]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#table2</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VIII/3 [1]</TD>
            <TD>An Optical Catalogue of Radio Galaxies (Burbidge+ 1979)</TD>
            <TD>This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/3#1</TD>
            <TD>2012-11-13T06:51:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VIII/3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VIII/3</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/3</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIII/3 [2]</TD>
            <TD>An Optical Catalogue of Radio Galaxies (Burbidge+ 1979)</TD>
            <TD>This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/3#2</TD>
            <TD>2012-11-13T06:51:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VIII/3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VIII/3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/3</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIII/3 [catalog]</TD>
            <TD>An Optical Catalogue of Radio Galaxies (Burbidge+ 1979)</TD>
            <TD>This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/3#catalog</TD>
            <TD>2012-11-13T06:51:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VIII/3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VIII/3&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/3</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/409 [1]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#1</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/409</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/409 [2]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#2</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/409&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/409 [table1]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#table1</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/409 [table2]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#table2</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/409 [1]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#1</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/409</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/409 [2]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#2</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/409&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/409 [table1]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#table1</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/409 [table2]</TD>
            <TD>New nearby dwarf galaxy candidates list (Karachentseva+ 1998)</TD>
            <TD>To increase completeness of the distance limited sample of nearby galaxies from the Kraan-Korteweg &amp; Tammann (1979AN....300..181K) catalogue we undertook a search for small companions of larger known galaxies which have corrected radial velocities with in 500km/s. Based primarely on the POSS-II and ESO/SERC films we found 260 nearby dwarf galaxy candidates with angular diameters a&gt;0.5arcmin. More than 50% of the objects were revealed for the first time. As we suppose, a significant part of them (about 30%) may really belong to the Local Volume sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409#table2</TD>
            <TD>2011-09-14T18:39:56Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/409</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VIII/3 [1]</TD>
            <TD>An Optical Catalogue of Radio Galaxies (Burbidge+ 1979)</TD>
            <TD>This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/3#1</TD>
            <TD>2012-11-13T06:51:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VIII/3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VIII/3</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/3</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIII/3 [2]</TD>
            <TD>An Optical Catalogue of Radio Galaxies (Burbidge+ 1979)</TD>
            <TD>This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/3#2</TD>
            <TD>2012-11-13T06:51:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VIII/3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VIII/3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/3</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIII/3 [catalog]</TD>
            <TD>An Optical Catalogue of Radio Galaxies (Burbidge+ 1979)</TD>
            <TD>This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/3#catalog</TD>
            <TD>2012-11-13T06:51:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VIII/3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VIII/3&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/3</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/275/67 [1]</TD>
            <TD>Velocity Field of the outer Galaxy (Brand+ 1993)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/275/67#1</TD>
            <TD>2011-09-14T18:40:29Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/275/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/275/67</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/275/67</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/275/67 [2]</TD>
            <TD>Velocity Field of the outer Galaxy (Brand+ 1993)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/275/67#2</TD>
            <TD>2011-09-14T18:40:29Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/275/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/275/67&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/275/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VIII/3 [1]</TD>
            <TD>An Optical Catalogue of Radio Galaxies (Burbidge+ 1979)</TD>
            <TD>This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/3#1</TD>
            <TD>2012-11-13T06:51:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VIII/3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VIII/3</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/3</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIII/3 [2]</TD>
            <TD>An Optical Catalogue of Radio Galaxies (Burbidge+ 1979)</TD>
            <TD>This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/3#2</TD>
            <TD>2012-11-13T06:51:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VIII/3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VIII/3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/3</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIII/3 [catalog]</TD>
            <TD>An Optical Catalogue of Radio Galaxies (Burbidge+ 1979)</TD>
            <TD>This catalog contains basic optical information on all known radio galaxies (with L[radio] greater than about 10**[41] ergs/s) that had been identified as of 1979 and for which measured redshifts were available. The data include the right ascension and declination (1950); galaxy (optical) type; visual magnitude; photoelectric colors; redshift (z) and the spectral lines on which the redshift measurements were based; coordinate designations; radio flux and frequency; radio spectral index; other names; and the references for the galaxy identification, photometric data, redshift, radio flux, radio spectral index, and radio map number. Note that the ADC version of this catalog differs somewhat from the original printed catalog in that some fields were added or modified and other fields reordered. In addition to the catalog data file itself, two additional files containing the list of references for the catalog are also available. The first reference list is in alphabetical order, and the second is in numerical order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/3#catalog</TD>
            <TD>2012-11-13T06:51:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VIII/3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VIII/3&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/3</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/275/67 [1]</TD>
            <TD>Velocity Field of the outer Galaxy (Brand+ 1993)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/275/67#1</TD>
            <TD>2011-09-14T18:40:29Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/275/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/275/67</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/275/67</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/275/67 [2]</TD>
            <TD>Velocity Field of the outer Galaxy (Brand+ 1993)</TD>
            <TD>(no description available)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/275/67#2</TD>
            <TD>2011-09-14T18:40:29Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/275/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/275/67&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/275/67</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/289/225 [1]</TD>
            <TD>SMC HI shells velocities (Staveley-Smith+ 1997)</TD>
            <TD>We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales &lt;=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size &gt;=0.6{deg}, and should not be used for deriving total H I column densities</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225#1</TD>
            <TD>2011-09-14T18:40:41Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/289/225</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/225</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/289/225 [2]</TD>
            <TD>SMC HI shells velocities (Staveley-Smith+ 1997)</TD>
            <TD>We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales &lt;=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size &gt;=0.6{deg}, and should not be used for deriving total H I column densities</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225#2</TD>
            <TD>2011-09-14T18:40:41Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/289/225&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/225</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/289/225 [table1]</TD>
            <TD>SMC HI shells velocities (Staveley-Smith+ 1997)</TD>
            <TD>We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales &lt;=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size &gt;=0.6{deg}, and should not be used for deriving total H I column densities</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225#table1</TD>
            <TD>2011-09-14T18:40:41Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/289/225&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/225</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/289/225 [1]</TD>
            <TD>SMC HI shells velocities (Staveley-Smith+ 1997)</TD>
            <TD>We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales &lt;=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size &gt;=0.6{deg}, and should not be used for deriving total H I column densities</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225#1</TD>
            <TD>2011-09-14T18:40:41Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/289/225</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/225</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/289/225 [2]</TD>
            <TD>SMC HI shells velocities (Staveley-Smith+ 1997)</TD>
            <TD>We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales &lt;=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size &gt;=0.6{deg}, and should not be used for deriving total H I column densities</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225#2</TD>
            <TD>2011-09-14T18:40:41Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/289/225&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/225</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/289/225 [table1]</TD>
            <TD>SMC HI shells velocities (Staveley-Smith+ 1997)</TD>
            <TD>We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales &lt;=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size &gt;=0.6{deg}, and should not be used for deriving total H I column densities</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225#table1</TD>
            <TD>2011-09-14T18:40:41Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/289/225&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/225</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/394/795 [1]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#1</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/394/795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/394/795 [2]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#2</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/394/795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/394/795 [table1]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#table1</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/394/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/394/795 [variables]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#variables</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/394/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VI/128 [1]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VI/128#1</TD>
            <TD>2012-11-13T07:12:05Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/VI/128</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VI/128</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/128</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VI/128 [2]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VI/128#2</TD>
            <TD>2012-11-13T07:12:05Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/VI/128</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VI/128&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/128</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VI/128 [cgps]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VI/128#cgps</TD>
            <TD>2012-11-13T07:12:05Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/VI/128</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VI/128&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/128</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/289/225 [1]</TD>
            <TD>SMC HI shells velocities (Staveley-Smith+ 1997)</TD>
            <TD>We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales &lt;=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size &gt;=0.6{deg}, and should not be used for deriving total H I column densities</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225#1</TD>
            <TD>2011-09-14T18:40:41Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/289/225</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/225</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/289/225 [2]</TD>
            <TD>SMC HI shells velocities (Staveley-Smith+ 1997)</TD>
            <TD>We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales &lt;=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size &gt;=0.6{deg}, and should not be used for deriving total H I column densities</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225#2</TD>
            <TD>2011-09-14T18:40:41Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/289/225&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/225</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/289/225 [table1]</TD>
            <TD>SMC HI shells velocities (Staveley-Smith+ 1997)</TD>
            <TD>We present the results of a survey of neutral hydrogen emission in the Small Magellanic Cloud (SMC) with the Australia Telescope Compact Array (ATCA). The survey consists of a mosaic of 320 separate pointings of the 375-m array, resulting in a resolution of 1.6arcmin (28pc, for a distance of 60kpc) over a field of 20deg^2^. The rms brightness temperature sensitivity is 1.4K, corresponding to an H I column density sensitivity of 4x^18^cm^-2^ for each velocity channel of width 1.6km/s. The HI distribution is complex and, on scales &lt;=1kpc, appears to be dominated by the effects of expanding H I shells, which are probably driven by the combined effects of supernovae and stellar winds from massive stars. The picture of the SMC that arises from the current data seems to challenge the earlier belief that the SMC consists of two or more spatially separate structures with different systemic velocities. We find that the observed multiple components are, in many cases, caused by the combined effects of the numerous shells and supershells. Altogether, we identify six supershells (defined here as those with radii greater than 300pc) and 495 giant shells. For each of these, we measure positions. radii, velocities and expansion rates, and derive ages and kinetic energy requirements. The apparent age distribution of shells is remarkably narrow, with a mean age of 5.4Myr and an intrinsic dispersion of 2Myr. Southern shells appear to be older, on average, by 2.5Myr. The kinetic energy of the shells is a large fraction of the gravitational binding energy of the SMC, implying that further disintegration of the SMC will occur with time, and especially at the next close passage with the Large Magellanic Cloud (LMC) or the Galaxy, unless the SMC possesses a massive halo. Because of their interferometric nature, the images presented here are insensitive to structures of size &gt;=0.6{deg}, and should not be used for deriving total H I column densities</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225#table1</TD>
            <TD>2011-09-14T18:40:41Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/289/225</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/289/225&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/289/225</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VI/128 [1]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VI/128#1</TD>
            <TD>2012-11-13T07:12:05Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/VI/128</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VI/128</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/128</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VI/128 [2]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VI/128#2</TD>
            <TD>2012-11-13T07:12:05Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/VI/128</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VI/128&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/128</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VI/128 [cgps]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VI/128#cgps</TD>
            <TD>2012-11-13T07:12:05Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/VI/128</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VI/128&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/128</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/330/881 [1]</TD>
            <TD>Radial velocities of Cartwheel Galaxy (Amram+ 1998)</TD>
            <TD>We report on high spectral and spatial resolution kinematic observations of H{alpha} emission from the Cartwheel system obtained with a scanning Fabry-Perot interferometer. Velocity fields for two galaxies were measured, for the main galaxy of the system, the Cartwheel galaxy, and for a spiral companion ~25h^-1^kpc to the north. The velocity field and the rotation curve of the spiral companion shows classical differential rotation and indicates the mass of the galaxy to be in the range 2.9-4.8x10^9^M{sun}. The Cartwheel galaxy contains strong H{alpha} in emission asymmetrically distributed along its outer ring, with some faint emission detected inside it. The velocity field and the rotation curve of the Cartwheel galaxy is clearly dominated by differential rotation although second-order effects cause distortions which can be understood in a scenario where expansion and density-wave motions are also considered. Our best model-fit to the observed velocity field of the Cartwheel galaxy includes three components for the kinematic of its outer ring: a circular velocity of 217km/s, an expansion velocity of 13-30+/-10km/s and a sinusoidal perturbation with an amplitude of 20+/-5km/s. This expansion velocity, lower than found in previous studies, implies that the ring could be older than previously thought. The rotation curve of the Cartwheel galaxy is consistent with a progenitor which had the morphology of a late-type spiral galaxy. Our measurements support the collisional models of ring galaxy formation and should impose strong constraints to simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/881#1</TD>
            <TD>2011-09-14T18:40:45Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/330/881</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/330/881</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/330/881 [2]</TD>
            <TD>Radial velocities of Cartwheel Galaxy (Amram+ 1998)</TD>
            <TD>We report on high spectral and spatial resolution kinematic observations of H{alpha} emission from the Cartwheel system obtained with a scanning Fabry-Perot interferometer. Velocity fields for two galaxies were measured, for the main galaxy of the system, the Cartwheel galaxy, and for a spiral companion ~25h^-1^kpc to the north. The velocity field and the rotation curve of the spiral companion shows classical differential rotation and indicates the mass of the galaxy to be in the range 2.9-4.8x10^9^M{sun}. The Cartwheel galaxy contains strong H{alpha} in emission asymmetrically distributed along its outer ring, with some faint emission detected inside it. The velocity field and the rotation curve of the Cartwheel galaxy is clearly dominated by differential rotation although second-order effects cause distortions which can be understood in a scenario where expansion and density-wave motions are also considered. Our best model-fit to the observed velocity field of the Cartwheel galaxy includes three components for the kinematic of its outer ring: a circular velocity of 217km/s, an expansion velocity of 13-30+/-10km/s and a sinusoidal perturbation with an amplitude of 20+/-5km/s. This expansion velocity, lower than found in previous studies, implies that the ring could be older than previously thought. The rotation curve of the Cartwheel galaxy is consistent with a progenitor which had the morphology of a late-type spiral galaxy. Our measurements support the collisional models of ring galaxy formation and should impose strong constraints to simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/881#2</TD>
            <TD>2011-09-14T18:40:45Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/330/881&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/330/881</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VI/128 [1]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VI/128#1</TD>
            <TD>2012-11-13T07:12:05Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/VI/128</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VI/128</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/128</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VI/128 [2]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VI/128#2</TD>
            <TD>2012-11-13T07:12:05Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/VI/128</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VI/128&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/128</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VI/128 [cgps]</TD>
            <TD>Log of CGPS exposures (Taylor+, 2003-)</TD>
            <TD>The Dominion Radio Astrophysical Observatory at Penticton (HIA/NRC), in collaboration with an international Consortium of astronomers, has begun a high-resolution survey of the atomic hydrogen and radio continuum emission from our Milky Way galaxy. By constructing a mosaic of 190 synthesis fields, the survey will cover Galactic longitudes from L=74.2 to 147.3 degrees and latitudes from B=-3.6 to +5.6 degrees, resolving features as small as 1 arcminute. For each mosaic (1024x1024 pixels), atomic hydrogen observations are presented as a data "cube" with 272 spectral channels having a velocity resolution of 1.3km/s. Stokes I continuum images at 1420MHz and 408MHz are produced, as well as selected Stokes Q, U and V images at 1420MHz. Complementary images in the four IRAS infrared bands and data cubes of CO (J=1-0) emission have also been created as part of the Survey. In addition to the 5x5{deg} mosaics, a series of nine 15x15{deg} mosaics of 408MHz emission, and possibly other lower radio frequencies, will be created. Mosaics are archived as they are processed and released to the Consortium. Archived data are in FITS format, except for the occasional text file. Imaging of the molecular phase of the ISM, traced by the CO molecule, has been realized at the Five College Radio Astronomy Observatory. High-resolution IRAS images of the dust component, seen through its infrared emission, have been completed at far-infrared wavelengths at the California Institute of Technology, and in the mid-infrared at the Canadian Institute for Theoretical Astrophysics at the University of Toronto. Complementary radio continuum images at frequencies below 408MHz are being contributed by the Mullard Radio Astronomy Observatory of the University of Cambridge and at the Beijing Astronomical Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VI/128#cgps</TD>
            <TD>2012-11-13T07:12:05Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/VI/128</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VI/128&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/128</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/330/881 [1]</TD>
            <TD>Radial velocities of Cartwheel Galaxy (Amram+ 1998)</TD>
            <TD>We report on high spectral and spatial resolution kinematic observations of H{alpha} emission from the Cartwheel system obtained with a scanning Fabry-Perot interferometer. Velocity fields for two galaxies were measured, for the main galaxy of the system, the Cartwheel galaxy, and for a spiral companion ~25h^-1^kpc to the north. The velocity field and the rotation curve of the spiral companion shows classical differential rotation and indicates the mass of the galaxy to be in the range 2.9-4.8x10^9^M{sun}. The Cartwheel galaxy contains strong H{alpha} in emission asymmetrically distributed along its outer ring, with some faint emission detected inside it. The velocity field and the rotation curve of the Cartwheel galaxy is clearly dominated by differential rotation although second-order effects cause distortions which can be understood in a scenario where expansion and density-wave motions are also considered. Our best model-fit to the observed velocity field of the Cartwheel galaxy includes three components for the kinematic of its outer ring: a circular velocity of 217km/s, an expansion velocity of 13-30+/-10km/s and a sinusoidal perturbation with an amplitude of 20+/-5km/s. This expansion velocity, lower than found in previous studies, implies that the ring could be older than previously thought. The rotation curve of the Cartwheel galaxy is consistent with a progenitor which had the morphology of a late-type spiral galaxy. Our measurements support the collisional models of ring galaxy formation and should impose strong constraints to simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/881#1</TD>
            <TD>2011-09-14T18:40:45Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/330/881</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/330/881</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/330/881 [2]</TD>
            <TD>Radial velocities of Cartwheel Galaxy (Amram+ 1998)</TD>
            <TD>We report on high spectral and spatial resolution kinematic observations of H{alpha} emission from the Cartwheel system obtained with a scanning Fabry-Perot interferometer. Velocity fields for two galaxies were measured, for the main galaxy of the system, the Cartwheel galaxy, and for a spiral companion ~25h^-1^kpc to the north. The velocity field and the rotation curve of the spiral companion shows classical differential rotation and indicates the mass of the galaxy to be in the range 2.9-4.8x10^9^M{sun}. The Cartwheel galaxy contains strong H{alpha} in emission asymmetrically distributed along its outer ring, with some faint emission detected inside it. The velocity field and the rotation curve of the Cartwheel galaxy is clearly dominated by differential rotation although second-order effects cause distortions which can be understood in a scenario where expansion and density-wave motions are also considered. Our best model-fit to the observed velocity field of the Cartwheel galaxy includes three components for the kinematic of its outer ring: a circular velocity of 217km/s, an expansion velocity of 13-30+/-10km/s and a sinusoidal perturbation with an amplitude of 20+/-5km/s. This expansion velocity, lower than found in previous studies, implies that the ring could be older than previously thought. The rotation curve of the Cartwheel galaxy is consistent with a progenitor which had the morphology of a late-type spiral galaxy. Our measurements support the collisional models of ring galaxy formation and should impose strong constraints to simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/881#2</TD>
            <TD>2011-09-14T18:40:45Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/330/881&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/330/881</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/68/715 [1]</TD>
            <TD>Clark Lake 30.9MHz survey (Kassim, 1988)</TD>
            <TD>The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg&lt;l&lt;59deg, 84deg&lt;l&lt;97deg, and 133deg&lt;l&lt;250deg, with |b|&lt;2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity is confusion-limited and varies from ~ 5Jy/beam in the inner Galaxy to ~ 1-2Jy/beam toward the outer Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715#1</TD>
            <TD>2012-11-13T07:17:25Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/68/715</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/68/715</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/68/715 [2]</TD>
            <TD>Clark Lake 30.9MHz survey (Kassim, 1988)</TD>
            <TD>The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg&lt;l&lt;59deg, 84deg&lt;l&lt;97deg, and 133deg&lt;l&lt;250deg, with |b|&lt;2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity is confusion-limited and varies from ~ 5Jy/beam in the inner Galaxy to ~ 1-2Jy/beam toward the outer Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715#2</TD>
            <TD>2012-11-13T07:17:25Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/68/715&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/68/715</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/68/715 [table4]</TD>
            <TD>Clark Lake 30.9MHz survey (Kassim, 1988)</TD>
            <TD>The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg&lt;l&lt;59deg, 84deg&lt;l&lt;97deg, and 133deg&lt;l&lt;250deg, with |b|&lt;2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity is confusion-limited and varies from ~ 5Jy/beam in the inner Galaxy to ~ 1-2Jy/beam toward the outer Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715#table4</TD>
            <TD>2012-11-13T07:17:25Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/68/715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/68/715</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/19 [1]</TD>
            <TD>MRC/1Jy Radio source survey. I. (McCarthy+ 1996)</TD>
            <TD>This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408&gt;0.95Jy and -30&lt;decl.(1950)&lt;-20, and 9h20m&lt;R.A.(1950)&lt;14h4m or 20h20m&lt;R.A.(1950)&lt;6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19#1</TD>
            <TD>2011-09-14T18:40:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/19 [2]</TD>
            <TD>MRC/1Jy Radio source survey. I. (McCarthy+ 1996)</TD>
            <TD>This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408&gt;0.95Jy and -30&lt;decl.(1950)&lt;-20, and 9h20m&lt;R.A.(1950)&lt;14h4m or 20h20m&lt;R.A.(1950)&lt;6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19#2</TD>
            <TD>2011-09-14T18:40:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/107/19 [table2]</TD>
            <TD>MRC/1Jy Radio source survey. I. (McCarthy+ 1996)</TD>
            <TD>This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408&gt;0.95Jy and -30&lt;decl.(1950)&lt;-20, and 9h20m&lt;R.A.(1950)&lt;14h4m or 20h20m&lt;R.A.(1950)&lt;6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19#table2</TD>
            <TD>2011-09-14T18:40:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/107/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/19 [1]</TD>
            <TD>MRC/1Jy Radio source survey. I. (McCarthy+ 1996)</TD>
            <TD>This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408&gt;0.95Jy and -30&lt;decl.(1950)&lt;-20, and 9h20m&lt;R.A.(1950)&lt;14h4m or 20h20m&lt;R.A.(1950)&lt;6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19#1</TD>
            <TD>2011-09-14T18:40:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/19 [2]</TD>
            <TD>MRC/1Jy Radio source survey. I. (McCarthy+ 1996)</TD>
            <TD>This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408&gt;0.95Jy and -30&lt;decl.(1950)&lt;-20, and 9h20m&lt;R.A.(1950)&lt;14h4m or 20h20m&lt;R.A.(1950)&lt;6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19#2</TD>
            <TD>2011-09-14T18:40:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/107/19 [table2]</TD>
            <TD>MRC/1Jy Radio source survey. I. (McCarthy+ 1996)</TD>
            <TD>This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408&gt;0.95Jy and -30&lt;decl.(1950)&lt;-20, and 9h20m&lt;R.A.(1950)&lt;14h4m or 20h20m&lt;R.A.(1950)&lt;6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19#table2</TD>
            <TD>2011-09-14T18:40:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/107/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/68/715 [1]</TD>
            <TD>Clark Lake 30.9MHz survey (Kassim, 1988)</TD>
            <TD>The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg&lt;l&lt;59deg, 84deg&lt;l&lt;97deg, and 133deg&lt;l&lt;250deg, with |b|&lt;2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity is confusion-limited and varies from ~ 5Jy/beam in the inner Galaxy to ~ 1-2Jy/beam toward the outer Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715#1</TD>
            <TD>2012-11-13T07:17:25Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/68/715</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/68/715</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/68/715 [2]</TD>
            <TD>Clark Lake 30.9MHz survey (Kassim, 1988)</TD>
            <TD>The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg&lt;l&lt;59deg, 84deg&lt;l&lt;97deg, and 133deg&lt;l&lt;250deg, with |b|&lt;2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity is confusion-limited and varies from ~ 5Jy/beam in the inner Galaxy to ~ 1-2Jy/beam toward the outer Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715#2</TD>
            <TD>2012-11-13T07:17:25Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/68/715&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/68/715</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/68/715 [table4]</TD>
            <TD>Clark Lake 30.9MHz survey (Kassim, 1988)</TD>
            <TD>The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg&lt;l&lt;59deg, 84deg&lt;l&lt;97deg, and 133deg&lt;l&lt;250deg, with |b|&lt;2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity is confusion-limited and varies from ~ 5Jy/beam in the inner Galaxy to ~ 1-2Jy/beam toward the outer Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715#table4</TD>
            <TD>2012-11-13T07:17:25Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/68/715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/68/715</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/19 [1]</TD>
            <TD>MRC/1Jy Radio source survey. I. (McCarthy+ 1996)</TD>
            <TD>This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408&gt;0.95Jy and -30&lt;decl.(1950)&lt;-20, and 9h20m&lt;R.A.(1950)&lt;14h4m or 20h20m&lt;R.A.(1950)&lt;6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19#1</TD>
            <TD>2011-09-14T18:40:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/19 [2]</TD>
            <TD>MRC/1Jy Radio source survey. I. (McCarthy+ 1996)</TD>
            <TD>This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408&gt;0.95Jy and -30&lt;decl.(1950)&lt;-20, and 9h20m&lt;R.A.(1950)&lt;14h4m or 20h20m&lt;R.A.(1950)&lt;6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19#2</TD>
            <TD>2011-09-14T18:40:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/107/19 [table2]</TD>
            <TD>MRC/1Jy Radio source survey. I. (McCarthy+ 1996)</TD>
            <TD>This is the first in a series of papers discussing the properties of a complete set of radio sources selected near S408=1Jy. We present optical or infrared identifications for a sample of 452 radio galaxies. The sources were selected from the 408MHz Molonglo Reference Catalog, restricted only by flux density and position on the sky, as follows: S408&gt;0.95Jy and -30&lt;decl.(1950)&lt;-20, and 9h20m&lt;R.A.(1950)&lt;14h4m or 20h20m&lt;R.A.(1950)&lt;6h14m. This complete sample, the MRC/1 Jy survey, contains 558 radio galaxies or quasars, of which six are occulted by bright stars or galaxies and two are multiple confused sources. Of the remaining 550 sources, 527, or 96%, are identified to an r magnitude of 25, and eight additional sources are identified to K=19. Of the 17 unocculted objects that remain unidentified, 15 are sources for which we have either poor radio maps or inadequate optical/IR images. This paper presents finding charts and astrometric positions for the 452 sources that are not identified as either quasars or BL Lacertae objects. Magnitudes in the r passband accurate to typically 0.1mag are given for 353 of the radio galaxy identifications. Redshifts for 268 of the galaxies are also listed; these have been derived from 450 spectroscopic observations. The radio observations, quasar and BL Lac identifications, spectroscopy, and near-IR images will be presented in subsequent papers in this series.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19#table2</TD>
            <TD>2011-09-14T18:40:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/107/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/68/715 [1]</TD>
            <TD>Clark Lake 30.9MHz survey (Kassim, 1988)</TD>
            <TD>The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg&lt;l&lt;59deg, 84deg&lt;l&lt;97deg, and 133deg&lt;l&lt;250deg, with |b|&lt;2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity is confusion-limited and varies from ~ 5Jy/beam in the inner Galaxy to ~ 1-2Jy/beam toward the outer Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715#1</TD>
            <TD>2012-11-13T07:17:25Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/68/715</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/68/715</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/68/715 [2]</TD>
            <TD>Clark Lake 30.9MHz survey (Kassim, 1988)</TD>
            <TD>The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg&lt;l&lt;59deg, 84deg&lt;l&lt;97deg, and 133deg&lt;l&lt;250deg, with |b|&lt;2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity is confusion-limited and varies from ~ 5Jy/beam in the inner Galaxy to ~ 1-2Jy/beam toward the outer Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715#2</TD>
            <TD>2012-11-13T07:17:25Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/68/715&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/68/715</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/68/715 [table4]</TD>
            <TD>Clark Lake 30.9MHz survey (Kassim, 1988)</TD>
            <TD>The Galactic plane has been mapped at 30.9 MHz with the Clark Lake TPT telescope giving unprecedented resolution for such a low frequency. The synthetized beam is 13.0'x11.1' at the zenith. Contour maps and a source list are presented for the regions 350deg&lt;l&lt;59deg, 84deg&lt;l&lt;97deg, and 133deg&lt;l&lt;250deg, with |b|&lt;2deg-3deg. The source list contains integrated flux densities and positions for 702 discrete emission regions. Sensitivity is confusion-limited and varies from ~ 5Jy/beam in the inner Galaxy to ~ 1-2Jy/beam toward the outer Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715#table4</TD>
            <TD>2012-11-13T07:17:25Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1994</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/68/715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/68/715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/68/715</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/327/952 [1]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#1</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/327/952</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/327/952 [2]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#2</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/327/952&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/952 [table5b]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#table5b</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/952&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/952 [table5a]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#table5a</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/952&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/952 [table5c]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#table5c</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/952&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/394/795 [1]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#1</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/394/795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/394/795 [2]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#2</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/394/795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/394/795 [table1]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#table1</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/394/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/394/795 [variables]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#variables</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/394/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [1]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#1</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Galaxy&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [2]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#2</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=Star&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [3]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#3</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR7 [4]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#4</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/DirectCone?DSACAT=SDSS_DR7&amp;DSATAB=PhotoObj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [5]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#5</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR7 [6]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#6</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [7]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#7</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [8]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#8</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [9]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#9</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [10]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#10</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [11]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#11</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [12]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#12</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR7 [13]</TD>
            <TD>SDSS DR7 - Sloan Digital Sky Survey Data Release 7</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR7 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa#13</TD>
            <TD>2012-07-18T12:36:49Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr7/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/126/85 [1]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#1</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/126/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/126/85 [2]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#2</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table8]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table8</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table3]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table3</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table9]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table9</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table10]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table10</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/327/952 [1]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#1</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/327/952</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/327/952 [2]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#2</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/327/952&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/952 [table5b]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#table5b</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/952&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/952 [table5a]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#table5a</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/952&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/952 [table5c]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#table5c</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/952&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/394/795 [1]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#1</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/394/795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/394/795 [2]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#2</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/394/795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/394/795 [table1]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#table1</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/394/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/394/795 [variables]</TD>
            <TD>AGB stars in Fornax dwarf spheroidal galaxy (Whitelock+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (108) increased to 120 %B Observations were made with the SIRIUS camera on the Japanese-SAAO Infrared Survey Facility (IRSF) at Sutherland. Observations were made at about 15 epochs spread over 3yr in the central 4x4 grid</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795#variables</TD>
            <TD>2011-09-14T20:56:21Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/394/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/394/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/394/795</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/126/85 [1]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#1</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/126/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/126/85 [2]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#2</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table8]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table8</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table3]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table3</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table9]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table9</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table10]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table10</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/327/952 [1]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#1</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/327/952</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/327/952 [2]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#2</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/327/952&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/952 [table5b]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#table5b</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/952&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/952 [table5a]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#table5a</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/952&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/952 [table5c]</TD>
            <TD>Centaurus cluster velocities (Stein+ 1997)</TD>
            <TD>Based on the photometric survey of the inner region of the Centaurus cluster (Jerjen &amp; Dressler, 1997, Cat. &lt;J/A+AS/124/1&gt;) we measured redshifts for a deep, surface brightness limited sample of galaxies using the MEFOS multifibre spectrograph at the ESO 3.6m telescope. With the new data set radial velocities for 120 centrally located cluster members become available which is equivalent to 78% of all known cluster galaxies in the region brighter than B_T_=18.5. The relevant aspect of this investigation is that new redshifts for 32 dwarf galaxies have been measured, rising the total number to 48. We investigate the prominent bimodal velocity distribution of Centaurus in more detail, discussing the very different characteristics of the velocity distributions for the main Hubble types E&amp;S0, spirals, Im&amp;BCD, and dE&amp;dS0. The nucleated, bright dwarf ellipticals are the only galaxies with a Gaussian-like distribution centred at 3148+/-98km/s. The remarkable coincidence of this velocity with the mean velocity of Cen 30 and the redshift of NGC 4696 in particular strongly suggests a connection of the dE&amp;dS0s to the gravitational centre of the Centaurus cluster and/or to the cluster dominant E galaxy. The application of statistical tests reveals the existence of a population dwarf galaxies bound to NGC 4696. The dynamical parameters for the two velocity components suggest that Cen 30 is the real Centaurus cluster whereas Cen 45 can only be a loosely bound group of galaxies. This conclusion is followed up with a type-mixture analysis. All results are fully consistent with the cluster-group scenario. Whether Cen 45 is merging with the cluster or is located in the close background remains unclear. We show that the poorness of Cen 45 represents an intrinsic problem which makes it difficult to approach this question.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952#table5c</TD>
            <TD>2011-09-14T18:42:03Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/952</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/952&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/952</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/ocl [1]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#1</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/ocl</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/ocl [2]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#2</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/ocl&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/ocl [clusters]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#clusters</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/ocl&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/ocl [removed]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#removed</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/ocl&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/583 [1]</TD>
            <TD>Hubble Deep Field surface photometry (Fasano+ 1998)</TD>
            <TD>The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, &lt;http://ecf.hq.eso.org&gt;). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. &lt;J/AJ/112/1335&gt;) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de~Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583#1</TD>
            <TD>2011-09-14T18:42:32Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/583</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/583</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/583 [2]</TD>
            <TD>Hubble Deep Field surface photometry (Fasano+ 1998)</TD>
            <TD>The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, &lt;http://ecf.hq.eso.org&gt;). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. &lt;J/AJ/112/1335&gt;) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de~Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583#2</TD>
            <TD>2011-09-14T18:42:32Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/583&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/583</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/129/583 [name]</TD>
            <TD>Hubble Deep Field surface photometry (Fasano+ 1998)</TD>
            <TD>The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, &lt;http://ecf.hq.eso.org&gt;). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. &lt;J/AJ/112/1335&gt;) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de~Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583#name</TD>
            <TD>2011-09-14T18:42:32Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/129/583&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/583</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/126/85 [1]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#1</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/126/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/126/85 [2]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#2</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table8]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table8</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table3]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table3</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table9]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table9</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/85 [table10]</TD>
            <TD>A mid-infrared galaxy atlas (MIGA) (Kerton+, 2000)</TD>
            <TD>A mid-infrared atlas of part of the Galactic plane (75{deg}&lt;l&lt;148{deg}, b=+/-6{deg}) has been constructed using HIRES processed infrared data to provide a mid-infrared data set for the Canadian Galactic Plane Survey (CGPS). The addition of this data set to the CGPS will enable the study of the emission from the smallest components of interstellar dust at an angular resolution comparable to that of the radio, millimeter, and far-infrared data in the CGPS. The Mid-Infrared Galaxy Atlas (MIGA) is a mid-infrared (12 and 25um) counterpart to the far-infrared IRAS Galaxy Atlas (IGA), and consists of resolution enhanced (~0.5' resolution) HIRES images along with ancillary maps. This paper describes the processing and characteristics of the atlas, the cross-band simulation technique used to obtain high-resolution ratio maps, and future plans to extend both the IGA and MIGA.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85#table10</TD>
            <TD>2012-11-13T07:19:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/ocl [1]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#1</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/ocl</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/ocl [2]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#2</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/ocl&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/ocl [clusters]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#clusters</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/ocl&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/ocl [removed]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#removed</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/ocl&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/583 [1]</TD>
            <TD>Hubble Deep Field surface photometry (Fasano+ 1998)</TD>
            <TD>The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, &lt;http://ecf.hq.eso.org&gt;). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. &lt;J/AJ/112/1335&gt;) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de~Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583#1</TD>
            <TD>2011-09-14T18:42:32Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/583</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/583</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/583 [2]</TD>
            <TD>Hubble Deep Field surface photometry (Fasano+ 1998)</TD>
            <TD>The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, &lt;http://ecf.hq.eso.org&gt;). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. &lt;J/AJ/112/1335&gt;) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de~Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583#2</TD>
            <TD>2011-09-14T18:42:32Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/583&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/583</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/129/583 [name]</TD>
            <TD>Hubble Deep Field surface photometry (Fasano+ 1998)</TD>
            <TD>The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, &lt;http://ecf.hq.eso.org&gt;). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. &lt;J/AJ/112/1335&gt;) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de~Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583#name</TD>
            <TD>2011-09-14T18:42:32Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/129/583&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/583</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/130/177 [1]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#1</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/130/177</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/130/177 [2]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#2</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/130/177&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/177 [table3]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#table3</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/177&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/177 [table2]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#table2</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/177&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/ocl [1]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#1</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/ocl</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/ocl [2]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#2</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/ocl&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/ocl [clusters]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#clusters</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/ocl&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/ocl [removed]</TD>
            <TD>Optically visible open clusters and Candidates (Dias+ 2002-2010)</TD>
            <TD>We have compiled a new catalogue of open clusters in the Galaxy which updates the previous catalogues of Lynga (1987, Cat. &lt;VII/92&gt;) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, http://obswww.unige.ch/webda). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogues, have been included. Virtually all the clusters (1629) presently known were included, which represents an increment of about 476 objects relative to the Lynga (1987, Cat. &lt;VII/92&gt;) catalogue. The catalogue is presented in a single table containing all the important data, which makes it easy to use. In total, 99% of the objects have estimates of their apparent diameters, and 38% have distance, E(B-V) and age determinations. Concerning the data on kinematics, 22% have their mean proper motions listed, 14% their mean radial velocities, and 11% have both information simultaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/ocl#removed</TD>
            <TD>2011-09-14T20:56:35Z</TD>
            <TD>#Abundances#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/B/ocl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/ocl&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/ocl</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/583 [1]</TD>
            <TD>Hubble Deep Field surface photometry (Fasano+ 1998)</TD>
            <TD>The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, &lt;http://ecf.hq.eso.org&gt;). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. &lt;J/AJ/112/1335&gt;) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de~Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583#1</TD>
            <TD>2011-09-14T18:42:32Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/583</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/583</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/583 [2]</TD>
            <TD>Hubble Deep Field surface photometry (Fasano+ 1998)</TD>
            <TD>The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, &lt;http://ecf.hq.eso.org&gt;). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. &lt;J/AJ/112/1335&gt;) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de~Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583#2</TD>
            <TD>2011-09-14T18:42:32Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/583&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/583</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/129/583 [name]</TD>
            <TD>Hubble Deep Field surface photometry (Fasano+ 1998)</TD>
            <TD>The detailed surface photometry of a sample of early-type galaxies in the Hubble Deep Field is presented as part of a long-term project aimed to settle strong observational constraints to the theories modelling the evolution of elliptical galaxies from the early stages. The sample has been extracted, in the V_606_ band, from the database provided by the ESO-STECF-HDF Group (Couch, 1996, &lt;http://ecf.hq.eso.org&gt;). The selection criteria involve the total magnitude, the number of pixels detected above the background level and an automatic star/galaxy classifier. Moreover, form visual inspection of the frames, we excluded the galaxies showing unambiguous late-type morphology. The analysis of the luminosity and geometrical profiles, carried out on the 162 candidates obeying our selection criteria, resulted in a list of 99 'bona fide' early-type galaxies, for which accurate total magnitudes and effective radii were computed on the basis of the equivalent luminosity profiles. The comparison with the magnitudes given by Williams et al. (1996, Cat. &lt;J/AJ/112/1335&gt;) indicates that the automated photometry tends to underestimate the total luminosity of the ellipticals. The luminosity profiles of most of galaxies in our sample follow fairly well the de~Vaucouleurs law ('Normal' profiles). However, a relevant fraction of galaxies, even following the r^1/4^ law in the main body light distribution, exhibit in the inner region a flattening of the luminosity profile not attributable to the PSF (`Flat' profiles) or, in some cases, a complex (multi-nucleus) structure (`Merger' profiles). A statistically significant correlation is found between the shapes of the luminosity profiles and the ellipticity distribution. In particular, the average ellipticity of galaxies belonging to the `Flat' and `Merger' classes is significantly higher than that of the `Normal' galaxies. Finally, even taken into account the relevant uncertainty of the outer position angle profiles, the amount of isophotal twisting of HDF ellipticals turns out to be significantly larger with respect to that of the local samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583#name</TD>
            <TD>2011-09-14T18:42:32Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/583</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/129/583&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/583</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/130/177 [1]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#1</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/130/177</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/130/177 [2]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#2</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/130/177&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/177 [table3]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#table3</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/177&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/177 [table2]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#table2</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/177&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>III/88 [1]</TD>
            <TD>Stellar Spectrophotometric Atlas (Gunn+ 1983)</TD>
            <TD>The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/88#1</TD>
            <TD>2011-09-14T21:03:53Z</TD>
            <TD>#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/III/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=III/88</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/88</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>III/88 [2]</TD>
            <TD>Stellar Spectrophotometric Atlas (Gunn+ 1983)</TD>
            <TD>The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/88#2</TD>
            <TD>2011-09-14T21:03:53Z</TD>
            <TD>#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/III/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=III/88&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/88</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>III/88 [atlas]</TD>
            <TD>Stellar Spectrophotometric Atlas (Gunn+ 1983)</TD>
            <TD>The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/88#atlas</TD>
            <TD>2011-09-14T21:03:53Z</TD>
            <TD>#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/III/88</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=III/88&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/88</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/1 [1]</TD>
            <TD>Old Stellar Populations. VI. Absorption-Line (Trager+ 1998)</TD>
            <TD>We present absorption-line strengths on the Lick/IDS line-strength system of 381 galaxies and 38 globular clusters in the 4000--6400 angstrom region. All galaxies were observed at Lick Observatory between 1972 and 1984 with the Cassegrain Image Dissector Scanner spectrograph, making this study one of the largest homogeneous collections of galaxy spectral line data to date. We also present a catalogue of nuclear velocity dispersions used to correct the absorption-line strengths onto the stellar Lick/IDS system. Extensive discussion of both random and systematic errors of the Lick/IDS system is provided. Indices are seen to fall into three families: alpha-element-like indices (including CN, Mg, Na D, and TiO2) that correlate positively with velocity dispersion; Fe-like indices (including Ca, the G band, TiO1, and all Fe indices) that correlate only weakly with velocity dispersion and the alpha indices; and Hbeta which anti-correlates with both velocity dispersion and the alpha indices. C2 4668 seems to be intermediate between the alpha and Fe groups. These groupings probably represent different element abundance families with different nucleosynthesis histories.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1#1</TD>
            <TD>2011-09-14T18:43:50Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/1 [2]</TD>
            <TD>Old Stellar Populations. VI. Absorption-Line (Trager+ 1998)</TD>
            <TD>We present absorption-line strengths on the Lick/IDS line-strength system of 381 galaxies and 38 globular clusters in the 4000--6400 angstrom region. All galaxies were observed at Lick Observatory between 1972 and 1984 with the Cassegrain Image Dissector Scanner spectrograph, making this study one of the largest homogeneous collections of galaxy spectral line data to date. We also present a catalogue of nuclear velocity dispersions used to correct the absorption-line strengths onto the stellar Lick/IDS system. Extensive discussion of both random and systematic errors of the Lick/IDS system is provided. Indices are seen to fall into three families: alpha-element-like indices (including CN, Mg, Na D, and TiO2) that correlate positively with velocity dispersion; Fe-like indices (including Ca, the G band, TiO1, and all Fe indices) that correlate only weakly with velocity dispersion and the alpha indices; and Hbeta which anti-correlates with both velocity dispersion and the alpha indices. C2 4668 seems to be intermediate between the alpha and Fe groups. These groupings probably represent different element abundance families with different nucleosynthesis histories.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1#2</TD>
            <TD>2011-09-14T18:43:50Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/116/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/116/1 [starcat]</TD>
            <TD>Old Stellar Populations. VI. Absorption-Line (Trager+ 1998)</TD>
            <TD>We present absorption-line strengths on the Lick/IDS line-strength system of 381 galaxies and 38 globular clusters in the 4000--6400 angstrom region. All galaxies were observed at Lick Observatory between 1972 and 1984 with the Cassegrain Image Dissector Scanner spectrograph, making this study one of the largest homogeneous collections of galaxy spectral line data to date. We also present a catalogue of nuclear velocity dispersions used to correct the absorption-line strengths onto the stellar Lick/IDS system. Extensive discussion of both random and systematic errors of the Lick/IDS system is provided. Indices are seen to fall into three families: alpha-element-like indices (including CN, Mg, Na D, and TiO2) that correlate positively with velocity dispersion; Fe-like indices (including Ca, the G band, TiO1, and all Fe indices) that correlate only weakly with velocity dispersion and the alpha indices; and Hbeta which anti-correlates with both velocity dispersion and the alpha indices. C2 4668 seems to be intermediate between the alpha and Fe groups. These groupings probably represent different element abundance families with different nucleosynthesis histories.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1#starcat</TD>
            <TD>2011-09-14T18:43:50Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/116/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/130/177 [1]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#1</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/130/177</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/130/177 [2]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#2</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/130/177&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/177 [table3]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#table3</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/177&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/177 [table2]</TD>
            <TD>Arecibo Dual-Beam Survey (Rosenberg+, 2000)</TD>
            <TD>The Arecibo Dual-Beam Survey is a "blind" 21 cm search for galaxies covering ~430deg^2^ of sky. We present the data from the detection survey as well as from the follow-up observations to confirm detections and improve positions and flux measurements. We find 265 galaxies, many of which are extremely low surface brightness. Some of these previously uncatalogued galaxies lie within the zone of avoidance, where they are obscured by the gas and dust in our Galaxy. Eighty-one of these sources are not previously catalogued optically, and there are 11 galaxies that have no associated optical counterpart or are only tentatively associated with faint wisps of nebulosity on the Digitized Sky Survey images. We discuss the properties of the survey, and in particular we make direct determinations of the completeness and reliability of the sample. The behavior of the completeness and its dependencies is essential for determining the H I mass function. We leave the discussion of the mass function for a later paper, but do note that we find many low surface brightness galaxies and seven sources with M_HI_&lt;10^8^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177#table2</TD>
            <TD>2012-11-13T07:19:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/177</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/177&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/177</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>III/88 [1]</TD>
            <TD>Stellar Spectrophotometric Atlas (Gunn+ 1983)</TD>
            <TD>The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/88#1</TD>
            <TD>2011-09-14T21:03:53Z</TD>
            <TD>#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/III/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=III/88</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/88</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>III/88 [2]</TD>
            <TD>Stellar Spectrophotometric Atlas (Gunn+ 1983)</TD>
            <TD>The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/88#2</TD>
            <TD>2011-09-14T21:03:53Z</TD>
            <TD>#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/III/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=III/88&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/88</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>III/88 [atlas]</TD>
            <TD>Stellar Spectrophotometric Atlas (Gunn+ 1983)</TD>
            <TD>The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/88#atlas</TD>
            <TD>2011-09-14T21:03:53Z</TD>
            <TD>#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/III/88</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=III/88&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/88</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/1 [1]</TD>
            <TD>Old Stellar Populations. VI. Absorption-Line (Trager+ 1998)</TD>
            <TD>We present absorption-line strengths on the Lick/IDS line-strength system of 381 galaxies and 38 globular clusters in the 4000--6400 angstrom region. All galaxies were observed at Lick Observatory between 1972 and 1984 with the Cassegrain Image Dissector Scanner spectrograph, making this study one of the largest homogeneous collections of galaxy spectral line data to date. We also present a catalogue of nuclear velocity dispersions used to correct the absorption-line strengths onto the stellar Lick/IDS system. Extensive discussion of both random and systematic errors of the Lick/IDS system is provided. Indices are seen to fall into three families: alpha-element-like indices (including CN, Mg, Na D, and TiO2) that correlate positively with velocity dispersion; Fe-like indices (including Ca, the G band, TiO1, and all Fe indices) that correlate only weakly with velocity dispersion and the alpha indices; and Hbeta which anti-correlates with both velocity dispersion and the alpha indices. C2 4668 seems to be intermediate between the alpha and Fe groups. These groupings probably represent different element abundance families with different nucleosynthesis histories.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1#1</TD>
            <TD>2011-09-14T18:43:50Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/1 [2]</TD>
            <TD>Old Stellar Populations. VI. Absorption-Line (Trager+ 1998)</TD>
            <TD>We present absorption-line strengths on the Lick/IDS line-strength system of 381 galaxies and 38 globular clusters in the 4000--6400 angstrom region. All galaxies were observed at Lick Observatory between 1972 and 1984 with the Cassegrain Image Dissector Scanner spectrograph, making this study one of the largest homogeneous collections of galaxy spectral line data to date. We also present a catalogue of nuclear velocity dispersions used to correct the absorption-line strengths onto the stellar Lick/IDS system. Extensive discussion of both random and systematic errors of the Lick/IDS system is provided. Indices are seen to fall into three families: alpha-element-like indices (including CN, Mg, Na D, and TiO2) that correlate positively with velocity dispersion; Fe-like indices (including Ca, the G band, TiO1, and all Fe indices) that correlate only weakly with velocity dispersion and the alpha indices; and Hbeta which anti-correlates with both velocity dispersion and the alpha indices. C2 4668 seems to be intermediate between the alpha and Fe groups. These groupings probably represent different element abundance families with different nucleosynthesis histories.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1#2</TD>
            <TD>2011-09-14T18:43:50Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/116/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/116/1 [starcat]</TD>
            <TD>Old Stellar Populations. VI. Absorption-Line (Trager+ 1998)</TD>
            <TD>We present absorption-line strengths on the Lick/IDS line-strength system of 381 galaxies and 38 globular clusters in the 4000--6400 angstrom region. All galaxies were observed at Lick Observatory between 1972 and 1984 with the Cassegrain Image Dissector Scanner spectrograph, making this study one of the largest homogeneous collections of galaxy spectral line data to date. We also present a catalogue of nuclear velocity dispersions used to correct the absorption-line strengths onto the stellar Lick/IDS system. Extensive discussion of both random and systematic errors of the Lick/IDS system is provided. Indices are seen to fall into three families: alpha-element-like indices (including CN, Mg, Na D, and TiO2) that correlate positively with velocity dispersion; Fe-like indices (including Ca, the G band, TiO1, and all Fe indices) that correlate only weakly with velocity dispersion and the alpha indices; and Hbeta which anti-correlates with both velocity dispersion and the alpha indices. C2 4668 seems to be intermediate between the alpha and Fe groups. These groupings probably represent different element abundance families with different nucleosynthesis histories.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1#starcat</TD>
            <TD>2011-09-14T18:43:50Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/116/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/130/237 [1]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#1</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/130/237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/130/237 [2]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#2</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/237 [table3]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#table3</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/237 [table1]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#table1</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/237 [table7]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#table7</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>III/88 [1]</TD>
            <TD>Stellar Spectrophotometric Atlas (Gunn+ 1983)</TD>
            <TD>The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/88#1</TD>
            <TD>2011-09-14T21:03:53Z</TD>
            <TD>#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/III/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=III/88</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/88</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>III/88 [2]</TD>
            <TD>Stellar Spectrophotometric Atlas (Gunn+ 1983)</TD>
            <TD>The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/88#2</TD>
            <TD>2011-09-14T21:03:53Z</TD>
            <TD>#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/III/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=III/88&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/88</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>III/88 [atlas]</TD>
            <TD>Stellar Spectrophotometric Atlas (Gunn+ 1983)</TD>
            <TD>The data were obtained with the Oke multichannel scanner on the 5-meter Hale reflector for purposes of synthetizing galaxy spectra, and the digitized atlas contains normalized spectral energy distributions, computed colors, scan line and continuum indices for 175 selected stars covering the complete ranges of spectral type and luminosity class.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/88#atlas</TD>
            <TD>2011-09-14T21:03:53Z</TD>
            <TD>#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/III/88</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=III/88&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/88</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/130/237 [1]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#1</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/130/237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/130/237 [2]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#2</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/237 [table3]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#table3</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/237 [table1]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#table1</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/237 [table7]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#table7</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/1 [1]</TD>
            <TD>Old Stellar Populations. VI. Absorption-Line (Trager+ 1998)</TD>
            <TD>We present absorption-line strengths on the Lick/IDS line-strength system of 381 galaxies and 38 globular clusters in the 4000--6400 angstrom region. All galaxies were observed at Lick Observatory between 1972 and 1984 with the Cassegrain Image Dissector Scanner spectrograph, making this study one of the largest homogeneous collections of galaxy spectral line data to date. We also present a catalogue of nuclear velocity dispersions used to correct the absorption-line strengths onto the stellar Lick/IDS system. Extensive discussion of both random and systematic errors of the Lick/IDS system is provided. Indices are seen to fall into three families: alpha-element-like indices (including CN, Mg, Na D, and TiO2) that correlate positively with velocity dispersion; Fe-like indices (including Ca, the G band, TiO1, and all Fe indices) that correlate only weakly with velocity dispersion and the alpha indices; and Hbeta which anti-correlates with both velocity dispersion and the alpha indices. C2 4668 seems to be intermediate between the alpha and Fe groups. These groupings probably represent different element abundance families with different nucleosynthesis histories.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1#1</TD>
            <TD>2011-09-14T18:43:50Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/1 [2]</TD>
            <TD>Old Stellar Populations. VI. Absorption-Line (Trager+ 1998)</TD>
            <TD>We present absorption-line strengths on the Lick/IDS line-strength system of 381 galaxies and 38 globular clusters in the 4000--6400 angstrom region. All galaxies were observed at Lick Observatory between 1972 and 1984 with the Cassegrain Image Dissector Scanner spectrograph, making this study one of the largest homogeneous collections of galaxy spectral line data to date. We also present a catalogue of nuclear velocity dispersions used to correct the absorption-line strengths onto the stellar Lick/IDS system. Extensive discussion of both random and systematic errors of the Lick/IDS system is provided. Indices are seen to fall into three families: alpha-element-like indices (including CN, Mg, Na D, and TiO2) that correlate positively with velocity dispersion; Fe-like indices (including Ca, the G band, TiO1, and all Fe indices) that correlate only weakly with velocity dispersion and the alpha indices; and Hbeta which anti-correlates with both velocity dispersion and the alpha indices. C2 4668 seems to be intermediate between the alpha and Fe groups. These groupings probably represent different element abundance families with different nucleosynthesis histories.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1#2</TD>
            <TD>2011-09-14T18:43:50Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/116/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/116/1 [starcat]</TD>
            <TD>Old Stellar Populations. VI. Absorption-Line (Trager+ 1998)</TD>
            <TD>We present absorption-line strengths on the Lick/IDS line-strength system of 381 galaxies and 38 globular clusters in the 4000--6400 angstrom region. All galaxies were observed at Lick Observatory between 1972 and 1984 with the Cassegrain Image Dissector Scanner spectrograph, making this study one of the largest homogeneous collections of galaxy spectral line data to date. We also present a catalogue of nuclear velocity dispersions used to correct the absorption-line strengths onto the stellar Lick/IDS system. Extensive discussion of both random and systematic errors of the Lick/IDS system is provided. Indices are seen to fall into three families: alpha-element-like indices (including CN, Mg, Na D, and TiO2) that correlate positively with velocity dispersion; Fe-like indices (including Ca, the G band, TiO1, and all Fe indices) that correlate only weakly with velocity dispersion and the alpha indices; and Hbeta which anti-correlates with both velocity dispersion and the alpha indices. C2 4668 seems to be intermediate between the alpha and Fe groups. These groupings probably represent different element abundance families with different nucleosynthesis histories.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1#starcat</TD>
            <TD>2011-09-14T18:43:50Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/116/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/130/237 [1]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#1</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/130/237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/130/237 [2]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#2</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/237 [table3]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#table3</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/237 [table1]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#table1</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/130/237 [table7]</TD>
            <TD>LCRS loose groups of galaxies (Tucker+, 2000)</TD>
            <TD>A "friends-of-friends" percolation algorithm has been used to extract a catalog of {delta}n/n=80 density enhancements (groups) from the six slices of the Las Campanas Redshift Survey (LCRS). The full catalog contains 1495 groups and includes 35% of the LCRS galaxy sample. A clean sample of 394 groups has been derived by culling groups from the full sample that either are too close to a slice edge, have a crossing time greater than a Hubble time, have a corrected velocity dispersion of zero, or contain a 55"-'orphan' (a galaxy with a mock redshift that was excluded from the original LCRS redshift catalog due to its proximity to another galaxy, i.e., within 55").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237#table7</TD>
            <TD>2012-11-13T07:20:13Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/130/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/130/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/130/237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/297/255 [1]</TD>
            <TD>HII region catalogue of M100 (Knapen, 1998)</TD>
            <TD>From a new mosaic image in the H-{alpha} line of the complete disc of the spiral galaxy M100, a catalogue is composed listing 1948 individual HII regions. For each HII region, the catalogue gives its position relative to the centre of the galaxy, its deprojected distance to the centre, its radius, and its calibrated luminosity. An indication is included as to whether the HII region is located in the arms, between them, or in the circumnuclear star-forming region. The H-{alpha} image of M100 was obtained during two observing runs with the 4.2m WHT on La Palma, using the TAURUS camera in imaging mode. Since the field of view in this setup is limited by the filter size to around 5' diameter, four fields of the galaxy were imaged, two (eastern half of M100) during the night of 27 May 1991, and two (western half) during the night of 14 March 1992. Narrow band redshifted H-{alpha} filters with width of 15{AA} were used for the observations, centred at 6601{AA} for the H-{alpha} line observations (redshifted using the galaxy's systemic velocity of 1571km/s) and at 6577{AA} and 6565{AA} for the continuum. Exposure times were 1200 seconds for both the on-line and the continuum image on the first night, and 2x900 seconds on the second night. An EEV CCD chip was used during both observing runs, with a projected pixel size of 0.279arcsec, and a size of 1180x1280 pixels.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/255#1</TD>
            <TD>2011-09-14T18:44:19Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jul-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/255</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/297/255</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/255</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/297/255 [2]</TD>
            <TD>HII region catalogue of M100 (Knapen, 1998)</TD>
            <TD>From a new mosaic image in the H-{alpha} line of the complete disc of the spiral galaxy M100, a catalogue is composed listing 1948 individual HII regions. For each HII region, the catalogue gives its position relative to the centre of the galaxy, its deprojected distance to the centre, its radius, and its calibrated luminosity. An indication is included as to whether the HII region is located in the arms, between them, or in the circumnuclear star-forming region. The H-{alpha} image of M100 was obtained during two observing runs with the 4.2m WHT on La Palma, using the TAURUS camera in imaging mode. Since the field of view in this setup is limited by the filter size to around 5' diameter, four fields of the galaxy were imaged, two (eastern half of M100) during the night of 27 May 1991, and two (western half) during the night of 14 March 1992. Narrow band redshifted H-{alpha} filters with width of 15{AA} were used for the observations, centred at 6601{AA} for the H-{alpha} line observations (redshifted using the galaxy's systemic velocity of 1571km/s) and at 6577{AA} and 6565{AA} for the continuum. Exposure times were 1200 seconds for both the on-line and the continuum image on the first night, and 2x900 seconds on the second night. An EEV CCD chip was used during both observing runs, with a projected pixel size of 0.279arcsec, and a size of 1180x1280 pixels.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/255#2</TD>
            <TD>2011-09-14T18:44:19Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jul-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/255</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/297/255&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/255</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/463/1227 [1]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#1</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/463/1227</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/463/1227 [2]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#2</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/463/1227&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/463/1227 [append]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#append</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/463/1227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/463/1227 [appenb]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#appenb</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/463/1227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/297/255 [1]</TD>
            <TD>HII region catalogue of M100 (Knapen, 1998)</TD>
            <TD>From a new mosaic image in the H-{alpha} line of the complete disc of the spiral galaxy M100, a catalogue is composed listing 1948 individual HII regions. For each HII region, the catalogue gives its position relative to the centre of the galaxy, its deprojected distance to the centre, its radius, and its calibrated luminosity. An indication is included as to whether the HII region is located in the arms, between them, or in the circumnuclear star-forming region. The H-{alpha} image of M100 was obtained during two observing runs with the 4.2m WHT on La Palma, using the TAURUS camera in imaging mode. Since the field of view in this setup is limited by the filter size to around 5' diameter, four fields of the galaxy were imaged, two (eastern half of M100) during the night of 27 May 1991, and two (western half) during the night of 14 March 1992. Narrow band redshifted H-{alpha} filters with width of 15{AA} were used for the observations, centred at 6601{AA} for the H-{alpha} line observations (redshifted using the galaxy's systemic velocity of 1571km/s) and at 6577{AA} and 6565{AA} for the continuum. Exposure times were 1200 seconds for both the on-line and the continuum image on the first night, and 2x900 seconds on the second night. An EEV CCD chip was used during both observing runs, with a projected pixel size of 0.279arcsec, and a size of 1180x1280 pixels.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/255#1</TD>
            <TD>2011-09-14T18:44:19Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jul-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/255</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/297/255</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/255</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/297/255 [2]</TD>
            <TD>HII region catalogue of M100 (Knapen, 1998)</TD>
            <TD>From a new mosaic image in the H-{alpha} line of the complete disc of the spiral galaxy M100, a catalogue is composed listing 1948 individual HII regions. For each HII region, the catalogue gives its position relative to the centre of the galaxy, its deprojected distance to the centre, its radius, and its calibrated luminosity. An indication is included as to whether the HII region is located in the arms, between them, or in the circumnuclear star-forming region. The H-{alpha} image of M100 was obtained during two observing runs with the 4.2m WHT on La Palma, using the TAURUS camera in imaging mode. Since the field of view in this setup is limited by the filter size to around 5' diameter, four fields of the galaxy were imaged, two (eastern half of M100) during the night of 27 May 1991, and two (western half) during the night of 14 March 1992. Narrow band redshifted H-{alpha} filters with width of 15{AA} were used for the observations, centred at 6601{AA} for the H-{alpha} line observations (redshifted using the galaxy's systemic velocity of 1571km/s) and at 6577{AA} and 6565{AA} for the continuum. Exposure times were 1200 seconds for both the on-line and the continuum image on the first night, and 2x900 seconds on the second night. An EEV CCD chip was used during both observing runs, with a projected pixel size of 0.279arcsec, and a size of 1180x1280 pixels.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/255#2</TD>
            <TD>2011-09-14T18:44:19Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jul-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/255</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/297/255&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/255</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/463/1227 [1]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#1</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/463/1227</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/463/1227 [2]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#2</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/463/1227&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/463/1227 [append]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#append</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/463/1227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/463/1227 [appenb]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#appenb</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/463/1227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/335/912 [1]</TD>
            <TD>Seyferts in galaxy pairs and groups (Kelm+ 1998)</TD>
            <TD>The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912#1</TD>
            <TD>2011-09-14T18:44:21Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/335/912</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/912</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/335/912 [2]</TD>
            <TD>Seyferts in galaxy pairs and groups (Kelm+ 1998)</TD>
            <TD>The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912#2</TD>
            <TD>2011-09-14T18:44:21Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/335/912&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/912</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/335/912 [tables]</TD>
            <TD>Seyferts in galaxy pairs and groups (Kelm+ 1998)</TD>
            <TD>The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912#tables</TD>
            <TD>2011-09-14T18:44:21Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/335/912&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/912</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/463/1227 [1]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#1</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/463/1227</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/463/1227 [2]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#2</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/463/1227&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/463/1227 [append]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#append</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/463/1227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/463/1227 [appenb]</TD>
            <TD>Catalogue of far-infrared loops in the Galaxy (Konyves+, 2007)</TD>
            <TD>An all-sky survey of loop- and arc-like intensity enhancements has been performed in order to investigate the large-scale structure of the diffuse far-infrared emission. We used maps made of 60 and 100um processed IRAS data (Sky Survey Atlas and dust infrared emission maps) to identify large-scale structures: loops, arcs or cavities, in the far-infrared emission in the Galaxy. Distances were attributed to a subsample of loops using associated objects. We identified 462 far-infrared loops, analyzed their individual FIR properties and their distribution. This data forms the Catalogue of Far-Infrared Loops in the Galaxy. We obtained observational estimates of f_in~30% and f_out~5% for the hot gas volume filling factor of the inward and outward Galactic neighbourhood of the Solar System. We obtained a slope of the power law size luminosity function {beta}=1.37 for low Galactic latitudes in the outer Milky Way. Deviations in the celestial distribution of far-infrared loops clearly indicate, that violent events frequently overwrite the structure of the interstellar matter in the inner Galaxy. Our objects trace out the spiral arm structure of the Galaxy in the neighbourhood of the Sun and their distribution clearly suggests that there is an efficient process that can generate loop-like features at high Galactic latitudes. Power law indices of size luminosity distributions suggest, that the structure of the ISM is ruled by supernovae and stellar winds at low Galactic latitudes while it is governed by supersonic turbulence above the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227#appenb</TD>
            <TD>2012-11-13T13:45:09Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/463/1227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/463/1227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/463/1227</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/335/912 [1]</TD>
            <TD>Seyferts in galaxy pairs and groups (Kelm+ 1998)</TD>
            <TD>The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912#1</TD>
            <TD>2011-09-14T18:44:21Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/335/912</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/912</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/335/912 [2]</TD>
            <TD>Seyferts in galaxy pairs and groups (Kelm+ 1998)</TD>
            <TD>The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912#2</TD>
            <TD>2011-09-14T18:44:21Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/335/912&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/912</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/335/912 [tables]</TD>
            <TD>Seyferts in galaxy pairs and groups (Kelm+ 1998)</TD>
            <TD>The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912#tables</TD>
            <TD>2011-09-14T18:44:21Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/335/912&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/912</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/130/251 [1]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#1</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/130/251</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/130/251 [2]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#2</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/130/251&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/251 [table2]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#table2</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/251&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/251 [table1]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#table1</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/251&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/335/912 [1]</TD>
            <TD>Seyferts in galaxy pairs and groups (Kelm+ 1998)</TD>
            <TD>The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912#1</TD>
            <TD>2011-09-14T18:44:21Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/335/912</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/912</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/335/912 [2]</TD>
            <TD>Seyferts in galaxy pairs and groups (Kelm+ 1998)</TD>
            <TD>The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912#2</TD>
            <TD>2011-09-14T18:44:21Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/335/912&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/912</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/335/912 [tables]</TD>
            <TD>Seyferts in galaxy pairs and groups (Kelm+ 1998)</TD>
            <TD>The occurrence of Seyfert galaxies in 6 samples representative of different cosmological environments (i.e. isolated pairs, compact and loose groups) is analysed. To avoid biases linked to subjective sample selection criteria only canonical samples, taken from the literature, are considered. It is found that the average frequency of Seyferts in all samples, is near 2%. Most Seyferts lying in pairs and compact groups show disturbed morphological appearance, whilst in loose groups disturbed and ``isolated'' Seyferts have roughly the same proportion. Then, within each sample, structures which host a Seyfert are compared to structures which do not. No appreciable differences regarding dynamical properties are found.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912#tables</TD>
            <TD>2011-09-14T18:44:21Z</TD>
            <TD>#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/912</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/335/912&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/912</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/130/251 [1]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#1</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/130/251</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/130/251 [2]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#2</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/130/251&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/251 [table2]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#table2</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/251&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/251 [table1]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#table1</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/251&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/593 [1]</TD>
            <TD>BVRI surface photometry for 14 Sb galaxies (Cunow 1998)</TD>
            <TD>Profiles of surface brightness, ellipticity and position angle obtained from CCD-BVRI images are presented for a sample of 14 spiral galaxies with 13&lt;B_T_&lt;16.1. For these galaxies, exponential disc components were fitted to the profiles. A decrease of disc scalelengths from B to I is found for 13 galaxies, while for one galaxy scalelengths increase from B to I. The scalelength ratios r_D(B)_/r_D(I)_, r_D(V)_/r_D(I)_ and r_D(R)_/r_D(I)_ show a systematic increase with increasing apparent ellipticity. The maximum variation is found for r_D(B)_/r_D(I)_ which is 80% larger for edge-on galaxies than for face-on galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/593#1</TD>
            <TD>2011-09-14T18:44:43Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/593</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/593</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/593 [2]</TD>
            <TD>BVRI surface photometry for 14 Sb galaxies (Cunow 1998)</TD>
            <TD>Profiles of surface brightness, ellipticity and position angle obtained from CCD-BVRI images are presented for a sample of 14 spiral galaxies with 13&lt;B_T_&lt;16.1. For these galaxies, exponential disc components were fitted to the profiles. A decrease of disc scalelengths from B to I is found for 13 galaxies, while for one galaxy scalelengths increase from B to I. The scalelength ratios r_D(B)_/r_D(I)_, r_D(V)_/r_D(I)_ and r_D(R)_/r_D(I)_ show a systematic increase with increasing apparent ellipticity. The maximum variation is found for r_D(B)_/r_D(I)_ which is 80% larger for edge-on galaxies than for face-on galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/593#2</TD>
            <TD>2011-09-14T18:44:43Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/593&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/593</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/130/251 [1]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#1</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/130/251</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/130/251 [2]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#2</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/130/251&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/251 [table2]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#table2</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/251&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/251 [table1]</TD>
            <TD>Star Formation in Early-type galaxies (Longhetti+ 1998)</TD>
            <TD>The paper is the first of a series (Longhetti et al., 1998A&amp;AS..130..267L, 1998b (Paper III) in press) dedicated to the study of the star formation history in early-type galaxies which show fine structures and/or interaction signatures. It presents nuclear line-strength indices for a sample composed of 21 shell galaxies, from the Malin &amp; Carter (1983ApJ...274..534M) southern survey, and 30 members of isolated interacting pairs, from the Reduzzi &amp; Rampazzo (1995ApL....30....1R) catalogue, located in low density environments. The spectral range covers 3700{AA}&lt;{lambda}&lt;5700{AA} at 2.1{AA}FWHM resolution. We measure 16 red ({lambda}&gt;4200{AA}) indices defined by the Lick Group. Measures have been transformed into the Lick-IDS ``standard'' system. The procedure has been tested on a set of 5 elliptical galaxies selected from the Gonzalez (1993, Ph.D. thesis) sample. We derive also three blue ({lambda}&lt;4200) indices, namely {DELTA}(4000{AA}) defined by Hamilton (1985ApJ...297..371H), H+K(CaII) and Hdelta/FeI defined by Rose (1984AJ.....89.1238R, 1985AJ.....90.1927R). Blue indices are correlated to the age of the last starburst occurred in a galaxy (Leonardi &amp; Rose, 1996AJ....111..182L). The indices determination, the estimate of the measurement errors and the correction for the galaxies velocity dispersions are discussed in detail. In the Appendix A we present the indices for a set of hot stars (T&gt;10000K) which may be used for extending, toward high temperatures, Worthey (1992, Ph.D. Thesis) fitting functions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251#table1</TD>
            <TD>2012-11-13T13:53:54Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/251</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/251&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/251</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/593 [1]</TD>
            <TD>BVRI surface photometry for 14 Sb galaxies (Cunow 1998)</TD>
            <TD>Profiles of surface brightness, ellipticity and position angle obtained from CCD-BVRI images are presented for a sample of 14 spiral galaxies with 13&lt;B_T_&lt;16.1. For these galaxies, exponential disc components were fitted to the profiles. A decrease of disc scalelengths from B to I is found for 13 galaxies, while for one galaxy scalelengths increase from B to I. The scalelength ratios r_D(B)_/r_D(I)_, r_D(V)_/r_D(I)_ and r_D(R)_/r_D(I)_ show a systematic increase with increasing apparent ellipticity. The maximum variation is found for r_D(B)_/r_D(I)_ which is 80% larger for edge-on galaxies than for face-on galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/593#1</TD>
            <TD>2011-09-14T18:44:43Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/593</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/593</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/593 [2]</TD>
            <TD>BVRI surface photometry for 14 Sb galaxies (Cunow 1998)</TD>
            <TD>Profiles of surface brightness, ellipticity and position angle obtained from CCD-BVRI images are presented for a sample of 14 spiral galaxies with 13&lt;B_T_&lt;16.1. For these galaxies, exponential disc components were fitted to the profiles. A decrease of disc scalelengths from B to I is found for 13 galaxies, while for one galaxy scalelengths increase from B to I. The scalelength ratios r_D(B)_/r_D(I)_, r_D(V)_/r_D(I)_ and r_D(R)_/r_D(I)_ show a systematic increase with increasing apparent ellipticity. The maximum variation is found for r_D(B)_/r_D(I)_ which is 80% larger for edge-on galaxies than for face-on galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/593#2</TD>
            <TD>2011-09-14T18:44:43Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/593&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/593</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/130/341 [1]</TD>
            <TD>Groups of Galaxies in PPS (Trasarti-Battistoni 1998)</TD>
            <TD>We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra &amp; Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341#1</TD>
            <TD>2012-11-13T13:54:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/130/341</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/341</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/130/341 [2]</TD>
            <TD>Groups of Galaxies in PPS (Trasarti-Battistoni 1998)</TD>
            <TD>We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra &amp; Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341#2</TD>
            <TD>2012-11-13T13:54:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/130/341&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/341</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/341 [table1]</TD>
            <TD>Groups of Galaxies in PPS (Trasarti-Battistoni 1998)</TD>
            <TD>We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra &amp; Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341#table1</TD>
            <TD>2012-11-13T13:54:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/341&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/341</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/97/587 [1]</TD>
            <TD>JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993)</TD>
            <TD>We present K-counts and JHK detailed photometry for a number of stars with K&lt;=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga &amp; Teague, 1992A&amp;AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel &amp; Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K&lt;=+9.0, the disk population may be accounted for by those sources with J-K&lt;=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587#1</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/97/587</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/97/587</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/97/587 [2]</TD>
            <TD>JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993)</TD>
            <TD>We present K-counts and JHK detailed photometry for a number of stars with K&lt;=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga &amp; Teague, 1992A&amp;AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel &amp; Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K&lt;=+9.0, the disk population may be accounted for by those sources with J-K&lt;=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587#2</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/97/587&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/97/587</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/97/587 [table2]</TD>
            <TD>JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993)</TD>
            <TD>We present K-counts and JHK detailed photometry for a number of stars with K&lt;=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga &amp; Teague, 1992A&amp;AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel &amp; Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K&lt;=+9.0, the disk population may be accounted for by those sources with J-K&lt;=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587#table2</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/97/587&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/97/587</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/130/341 [1]</TD>
            <TD>Groups of Galaxies in PPS (Trasarti-Battistoni 1998)</TD>
            <TD>We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra &amp; Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341#1</TD>
            <TD>2012-11-13T13:54:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/130/341</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/341</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/130/341 [2]</TD>
            <TD>Groups of Galaxies in PPS (Trasarti-Battistoni 1998)</TD>
            <TD>We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra &amp; Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341#2</TD>
            <TD>2012-11-13T13:54:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/130/341&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/341</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/341 [table1]</TD>
            <TD>Groups of Galaxies in PPS (Trasarti-Battistoni 1998)</TD>
            <TD>We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra &amp; Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341#table1</TD>
            <TD>2012-11-13T13:54:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/341&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/341</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/97/587 [1]</TD>
            <TD>JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993)</TD>
            <TD>We present K-counts and JHK detailed photometry for a number of stars with K&lt;=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga &amp; Teague, 1992A&amp;AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel &amp; Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K&lt;=+9.0, the disk population may be accounted for by those sources with J-K&lt;=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587#1</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/97/587</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/97/587</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/97/587 [2]</TD>
            <TD>JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993)</TD>
            <TD>We present K-counts and JHK detailed photometry for a number of stars with K&lt;=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga &amp; Teague, 1992A&amp;AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel &amp; Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K&lt;=+9.0, the disk population may be accounted for by those sources with J-K&lt;=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587#2</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/97/587&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/97/587</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/97/587 [table2]</TD>
            <TD>JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993)</TD>
            <TD>We present K-counts and JHK detailed photometry for a number of stars with K&lt;=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga &amp; Teague, 1992A&amp;AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel &amp; Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K&lt;=+9.0, the disk population may be accounted for by those sources with J-K&lt;=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587#table2</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/97/587&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/97/587</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/130/341 [1]</TD>
            <TD>Groups of Galaxies in PPS (Trasarti-Battistoni 1998)</TD>
            <TD>We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra &amp; Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341#1</TD>
            <TD>2012-11-13T13:54:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/130/341</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/341</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/130/341 [2]</TD>
            <TD>Groups of Galaxies in PPS (Trasarti-Battistoni 1998)</TD>
            <TD>We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra &amp; Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341#2</TD>
            <TD>2012-11-13T13:54:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/130/341&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/341</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/341 [table1]</TD>
            <TD>Groups of Galaxies in PPS (Trasarti-Battistoni 1998)</TD>
            <TD>We present a large catalog of galaxy loose groups in the Southern Galactic Hemisphere, selected from the Perseus-Pisces redshift Survey (PPS). Particular care is taken in order to obtain group samples as homogeneous as possible to previously published catalogs. Groups are identified with the adaptive Friends-of-Friends (FoF) algorithm of Huchra &amp; Geller (1982ApJ...257..423H), with suitable normalizations V_0_=350km/s and D_0_=0.231h.Mpc. As a necessary ingredient of FoF algorithms, we obtain the galaxy luminosity function (LF) for PPS. Its Schechter parameters ({alpha}=-1.15+/-0.15, M_*_=-19.3+/-0.1) are in good agreement with similar LF estimates from samples previously used to select groups. The LF normalizations {phi}_*_=0.02h^3^/Mpc^3^ appropriate for PPS yields a density threshold {delta}n/n~180 for the adopted D_0_, apparently rather different from the desired {delta}n/n~80 used in previous studies. We then consider several other link normalizations, and briefly discuss their effect on group properties. We suggest to replace the customarily adopted {delta}n/n parametrization with the more direct D_0_ parametrization. All our catalogs contain N_G_~200 groups, significantly more than in most previous studies where group samples were obtained from galaxy data sets of comparable quality to (but smaller extent than) PPS. The group properties are rather sensitive to the adopted D_0_ and V_0_, but vary little with different redshift corrections, redshift cut-off, and galaxy LF. Loose groups in PPS nicely trace the large scale structure (LSS) in the parent galaxy sample. Physical properties of groups in PPS and in other directly comparable samples are in good agreement. There seems to be a complex interplay among LSS features, FoF grouping procedure, and group properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341#table1</TD>
            <TD>2012-11-13T13:54:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/341</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/341&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/341</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/97/587 [1]</TD>
            <TD>JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993)</TD>
            <TD>We present K-counts and JHK detailed photometry for a number of stars with K&lt;=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga &amp; Teague, 1992A&amp;AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel &amp; Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K&lt;=+9.0, the disk population may be accounted for by those sources with J-K&lt;=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587#1</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/97/587</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/97/587</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/97/587 [2]</TD>
            <TD>JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993)</TD>
            <TD>We present K-counts and JHK detailed photometry for a number of stars with K&lt;=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga &amp; Teague, 1992A&amp;AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel &amp; Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K&lt;=+9.0, the disk population may be accounted for by those sources with J-K&lt;=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587#2</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/97/587&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/97/587</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/97/587 [table2]</TD>
            <TD>JHK photometry of Galactic center stars (Ruelas-Mayorga+ 1993)</TD>
            <TD>We present K-counts and JHK detailed photometry for a number of stars with K&lt;=+9.0 in three clear regions near the galactic centre. These regions are all located approximately at l~0.0 and at latitudes b~-3.5,-4.0 and 4.5 respectively. Their Cumulative Counts Functions (CCF's) are formed, and with the aid of an exponential disk model for the Galaxy they are separated into disk and bulge CCF. As for the case in Baade's Window (BW) (Ruelas-Mayorga &amp; Teague, 1992A&amp;AS...95..379R) the disk is dominant at bright magnitudes whereas the bulge dominates at the faint end of the CCF. The slope of the bulge CCF is steeper than that for the disk in all three cases corroborating the result obtained for BW. The two colour JHK diagram and the K vs J-K diagram for the three regions show that the stellar population in these areas is similar to that studied in BW by us and by Frogel &amp; Whitford (1987ApJ...320..199F). An average value of E(J-K)~0.42mag for the reddening is obtained, which is somewhat larger than that found for BW (0.27). Finally it is shown that at K&lt;=+9.0, the disk population may be accounted for by those sources with J-K&lt;=+1.6 whereas the bulge population presents values for J-K in excess of +1.6.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587#table2</TD>
            <TD>2011-09-14T18:44:50Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/97/587</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/97/587&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/97/587</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1118 [1]</TD>
            <TD>Radial velocities of high-velocity white dwarfs (Silvestri+, 2002)</TD>
            <TD>Radial velocities and complete space motions were measured for 116 white dwarf stars with M dwarf companions (WD+M), including thirteen pairs having "halo-like" velocities. These 116 WD+dM binaries were observed on the 3.5 m telescope at the Apache Point Observatory (APO) on nearly 30 half-nights between 2000 September 4 and 2001 October 20. The APO Double Imaging Spectrograph was used with a 15" slit, yielding a resolution of approximately 2arcsrc/pixel. From the near-solar abundance levels of the M dwarf companions, only one potential stellar halo white dwarf (LP 164-52) was found in the sample, 12 of the 13 high-velocity white dwarfs being actually part of the high-velocity tail of the thick disk rather than the dark matter halo of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118#1</TD>
            <TD>2012-11-13T14:04:49Z</TD>
            <TD>#Multiple_Stars#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1118</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1118</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1118 [2]</TD>
            <TD>Radial velocities of high-velocity white dwarfs (Silvestri+, 2002)</TD>
            <TD>Radial velocities and complete space motions were measured for 116 white dwarf stars with M dwarf companions (WD+M), including thirteen pairs having "halo-like" velocities. These 116 WD+dM binaries were observed on the 3.5 m telescope at the Apache Point Observatory (APO) on nearly 30 half-nights between 2000 September 4 and 2001 October 20. The APO Double Imaging Spectrograph was used with a 15" slit, yielding a resolution of approximately 2arcsrc/pixel. From the near-solar abundance levels of the M dwarf companions, only one potential stellar halo white dwarf (LP 164-52) was found in the sample, 12 of the 13 high-velocity white dwarfs being actually part of the high-velocity tail of the thick disk rather than the dark matter halo of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118#2</TD>
            <TD>2012-11-13T14:04:49Z</TD>
            <TD>#Multiple_Stars#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1118&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1118</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1118 [table1]</TD>
            <TD>Radial velocities of high-velocity white dwarfs (Silvestri+, 2002)</TD>
            <TD>Radial velocities and complete space motions were measured for 116 white dwarf stars with M dwarf companions (WD+M), including thirteen pairs having "halo-like" velocities. These 116 WD+dM binaries were observed on the 3.5 m telescope at the Apache Point Observatory (APO) on nearly 30 half-nights between 2000 September 4 and 2001 October 20. The APO Double Imaging Spectrograph was used with a 15" slit, yielding a resolution of approximately 2arcsrc/pixel. From the near-solar abundance levels of the M dwarf companions, only one potential stellar halo white dwarf (LP 164-52) was found in the sample, 12 of the 13 high-velocity white dwarfs being actually part of the high-velocity tail of the thick disk rather than the dark matter halo of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118#table1</TD>
            <TD>2012-11-13T14:04:49Z</TD>
            <TD>#Multiple_Stars#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1118&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1118</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/62 [1]</TD>
            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
            <TD>A survey of quasar absorbers was conducted using the Infrared Astronomical Satellite (IRAS) database. Quasars with known intervening absorption-line systems and broad absorption line (BAL) QSOs were selected primarily from Junkkarinen et al. (1991ApJS...77..203J). Of the 570 quasars with IRAS data, 52 showed 3{sigma} or better detections in at least one band in SCANPI analysis. The origin of the IRAS flux could be from the absorption-line systems, other galaxies, or the quasar itself. The spectral energy distributions for quasars detected in the absorption-line sample and BAL QSOs were found to be redder than those of two control samples which suggests that some of the IRAS flux may arise in dust associated with the intervening galaxies. IRAS SUPERSCANPI processing was carried out for 77 quasars with known Mg II absorption at Zabs&lt;1 to investigate the ensemble far-infrared properties of these objects. SUPERSCANPI processing evaluates the median flux for many different positions on the sky, resulting in an improvement in the effective sensitivity. A control sample consisting of objects with no Mg II absorption known at Zabs&lt;1 but with the same distribution of absolute V-magnitude, Zem and radio-loud fraction for the background quasars was also processed. The Mg II sample was detected at 3{sigma} or better in all four IRAS bands with a significantly larger flux than the control sample at 60{mu}m and 100{mu}m. If this far-infrared emission is from the absorber galaxies, then the far-infrared luminosity of the composite Mg II absorber was found to be comparable to that of a starbursting galaxy, although such a high star-formation rate is inconsistent with the optical and near-infrared colors of low-redshift Mg II systems. Four of the quasars with individual IRAS detections have intervening galaxies identified with the Mg II absorption-lines. The spectral energy distributions of these galaxies imply far-infrared luminosities in excess of what Arp 220 would give at their redshifts. While all the external evidence suggests that the detection of far-infrared emission from the absorber sample may not be connected to the presence of the Mg II absorber, we discuss future observations which may help explain our results.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/62#1</TD>
            <TD>2011-09-14T18:45:06Z</TD>
            <TD>#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/62</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/62</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/62 [2]</TD>
            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
            <TD>A survey of quasar absorbers was conducted using the Infrared Astronomical Satellite (IRAS) database. Quasars with known intervening absorption-line systems and broad absorption line (BAL) QSOs were selected primarily from Junkkarinen et al. (1991ApJS...77..203J). Of the 570 quasars with IRAS data, 52 showed 3{sigma} or better detections in at least one band in SCANPI analysis. The origin of the IRAS flux could be from the absorption-line systems, other galaxies, or the quasar itself. The spectral energy distributions for quasars detected in the absorption-line sample and BAL QSOs were found to be redder than those of two control samples which suggests that some of the IRAS flux may arise in dust associated with the intervening galaxies. IRAS SUPERSCANPI processing was carried out for 77 quasars with known Mg II absorption at Zabs&lt;1 to investigate the ensemble far-infrared properties of these objects. SUPERSCANPI processing evaluates the median flux for many different positions on the sky, resulting in an improvement in the effective sensitivity. A control sample consisting of objects with no Mg II absorption known at Zabs&lt;1 but with the same distribution of absolute V-magnitude, Zem and radio-loud fraction for the background quasars was also processed. The Mg II sample was detected at 3{sigma} or better in all four IRAS bands with a significantly larger flux than the control sample at 60{mu}m and 100{mu}m. If this far-infrared emission is from the absorber galaxies, then the far-infrared luminosity of the composite Mg II absorber was found to be comparable to that of a starbursting galaxy, although such a high star-formation rate is inconsistent with the optical and near-infrared colors of low-redshift Mg II systems. Four of the quasars with individual IRAS detections have intervening galaxies identified with the Mg II absorption-lines. The spectral energy distributions of these galaxies imply far-infrared luminosities in excess of what Arp 220 would give at their redshifts. While all the external evidence suggests that the detection of far-infrared emission from the absorber sample may not be connected to the presence of the Mg II absorber, we discuss future observations which may help explain our results.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/62#2</TD>
            <TD>2011-09-14T18:45:06Z</TD>
            <TD>#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/62&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/62 [table3]</TD>
            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
            <TD>A survey of quasar absorbers was conducted using the Infrared Astronomical Satellite (IRAS) database. Quasars with known intervening absorption-line systems and broad absorption line (BAL) QSOs were selected primarily from Junkkarinen et al. (1991ApJS...77..203J). Of the 570 quasars with IRAS data, 52 showed 3{sigma} or better detections in at least one band in SCANPI analysis. The origin of the IRAS flux could be from the absorption-line systems, other galaxies, or the quasar itself. The spectral energy distributions for quasars detected in the absorption-line sample and BAL QSOs were found to be redder than those of two control samples which suggests that some of the IRAS flux may arise in dust associated with the intervening galaxies. IRAS SUPERSCANPI processing was carried out for 77 quasars with known Mg II absorption at Zabs&lt;1 to investigate the ensemble far-infrared properties of these objects. SUPERSCANPI processing evaluates the median flux for many different positions on the sky, resulting in an improvement in the effective sensitivity. A control sample consisting of objects with no Mg II absorption known at Zabs&lt;1 but with the same distribution of absolute V-magnitude, Zem and radio-loud fraction for the background quasars was also processed. The Mg II sample was detected at 3{sigma} or better in all four IRAS bands with a significantly larger flux than the control sample at 60{mu}m and 100{mu}m. If this far-infrared emission is from the absorber galaxies, then the far-infrared luminosity of the composite Mg II absorber was found to be comparable to that of a starbursting galaxy, although such a high star-formation rate is inconsistent with the optical and near-infrared colors of low-redshift Mg II systems. Four of the quasars with individual IRAS detections have intervening galaxies identified with the Mg II absorption-lines. The spectral energy distributions of these galaxies imply far-infrared luminosities in excess of what Arp 220 would give at their redshifts. While all the external evidence suggests that the detection of far-infrared emission from the absorber sample may not be connected to the presence of the Mg II absorber, we discuss future observations which may help explain our results.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/62#table3</TD>
            <TD>2011-09-14T18:45:06Z</TD>
            <TD>#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/62 [table4]</TD>
            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
            <TD>A survey of quasar absorbers was conducted using the Infrared Astronomical Satellite (IRAS) database. Quasars with known intervening absorption-line systems and broad absorption line (BAL) QSOs were selected primarily from Junkkarinen et al. (1991ApJS...77..203J). Of the 570 quasars with IRAS data, 52 showed 3{sigma} or better detections in at least one band in SCANPI analysis. The origin of the IRAS flux could be from the absorption-line systems, other galaxies, or the quasar itself. The spectral energy distributions for quasars detected in the absorption-line sample and BAL QSOs were found to be redder than those of two control samples which suggests that some of the IRAS flux may arise in dust associated with the intervening galaxies. IRAS SUPERSCANPI processing was carried out for 77 quasars with known Mg II absorption at Zabs&lt;1 to investigate the ensemble far-infrared properties of these objects. SUPERSCANPI processing evaluates the median flux for many different positions on the sky, resulting in an improvement in the effective sensitivity. A control sample consisting of objects with no Mg II absorption known at Zabs&lt;1 but with the same distribution of absolute V-magnitude, Zem and radio-loud fraction for the background quasars was also processed. The Mg II sample was detected at 3{sigma} or better in all four IRAS bands with a significantly larger flux than the control sample at 60{mu}m and 100{mu}m. If this far-infrared emission is from the absorber galaxies, then the far-infrared luminosity of the composite Mg II absorber was found to be comparable to that of a starbursting galaxy, although such a high star-formation rate is inconsistent with the optical and near-infrared colors of low-redshift Mg II systems. Four of the quasars with individual IRAS detections have intervening galaxies identified with the Mg II absorption-lines. The spectral energy distributions of these galaxies imply far-infrared luminosities in excess of what Arp 220 would give at their redshifts. While all the external evidence suggests that the detection of far-infrared emission from the absorber sample may not be connected to the presence of the Mg II absorber, we discuss future observations which may help explain our results.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/62#table4</TD>
            <TD>2011-09-14T18:45:06Z</TD>
            <TD>#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1118 [1]</TD>
            <TD>Radial velocities of high-velocity white dwarfs (Silvestri+, 2002)</TD>
            <TD>Radial velocities and complete space motions were measured for 116 white dwarf stars with M dwarf companions (WD+M), including thirteen pairs having "halo-like" velocities. These 116 WD+dM binaries were observed on the 3.5 m telescope at the Apache Point Observatory (APO) on nearly 30 half-nights between 2000 September 4 and 2001 October 20. The APO Double Imaging Spectrograph was used with a 15" slit, yielding a resolution of approximately 2arcsrc/pixel. From the near-solar abundance levels of the M dwarf companions, only one potential stellar halo white dwarf (LP 164-52) was found in the sample, 12 of the 13 high-velocity white dwarfs being actually part of the high-velocity tail of the thick disk rather than the dark matter halo of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118#1</TD>
            <TD>2012-11-13T14:04:49Z</TD>
            <TD>#Multiple_Stars#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1118</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1118</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1118 [2]</TD>
            <TD>Radial velocities of high-velocity white dwarfs (Silvestri+, 2002)</TD>
            <TD>Radial velocities and complete space motions were measured for 116 white dwarf stars with M dwarf companions (WD+M), including thirteen pairs having "halo-like" velocities. These 116 WD+dM binaries were observed on the 3.5 m telescope at the Apache Point Observatory (APO) on nearly 30 half-nights between 2000 September 4 and 2001 October 20. The APO Double Imaging Spectrograph was used with a 15" slit, yielding a resolution of approximately 2arcsrc/pixel. From the near-solar abundance levels of the M dwarf companions, only one potential stellar halo white dwarf (LP 164-52) was found in the sample, 12 of the 13 high-velocity white dwarfs being actually part of the high-velocity tail of the thick disk rather than the dark matter halo of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118#2</TD>
            <TD>2012-11-13T14:04:49Z</TD>
            <TD>#Multiple_Stars#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1118&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1118</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1118 [table1]</TD>
            <TD>Radial velocities of high-velocity white dwarfs (Silvestri+, 2002)</TD>
            <TD>Radial velocities and complete space motions were measured for 116 white dwarf stars with M dwarf companions (WD+M), including thirteen pairs having "halo-like" velocities. These 116 WD+dM binaries were observed on the 3.5 m telescope at the Apache Point Observatory (APO) on nearly 30 half-nights between 2000 September 4 and 2001 October 20. The APO Double Imaging Spectrograph was used with a 15" slit, yielding a resolution of approximately 2arcsrc/pixel. From the near-solar abundance levels of the M dwarf companions, only one potential stellar halo white dwarf (LP 164-52) was found in the sample, 12 of the 13 high-velocity white dwarfs being actually part of the high-velocity tail of the thick disk rather than the dark matter halo of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118#table1</TD>
            <TD>2012-11-13T14:04:49Z</TD>
            <TD>#Multiple_Stars#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1118</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1118&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1118</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/62 [1]</TD>
            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
            <TD>A survey of quasar absorbers was conducted using the Infrared Astronomical Satellite (IRAS) database. Quasars with known intervening absorption-line systems and broad absorption line (BAL) QSOs were selected primarily from Junkkarinen et al. (1991ApJS...77..203J). Of the 570 quasars with IRAS data, 52 showed 3{sigma} or better detections in at least one band in SCANPI analysis. The origin of the IRAS flux could be from the absorption-line systems, other galaxies, or the quasar itself. The spectral energy distributions for quasars detected in the absorption-line sample and BAL QSOs were found to be redder than those of two control samples which suggests that some of the IRAS flux may arise in dust associated with the intervening galaxies. IRAS SUPERSCANPI processing was carried out for 77 quasars with known Mg II absorption at Zabs&lt;1 to investigate the ensemble far-infrared properties of these objects. SUPERSCANPI processing evaluates the median flux for many different positions on the sky, resulting in an improvement in the effective sensitivity. A control sample consisting of objects with no Mg II absorption known at Zabs&lt;1 but with the same distribution of absolute V-magnitude, Zem and radio-loud fraction for the background quasars was also processed. The Mg II sample was detected at 3{sigma} or better in all four IRAS bands with a significantly larger flux than the control sample at 60{mu}m and 100{mu}m. If this far-infrared emission is from the absorber galaxies, then the far-infrared luminosity of the composite Mg II absorber was found to be comparable to that of a starbursting galaxy, although such a high star-formation rate is inconsistent with the optical and near-infrared colors of low-redshift Mg II systems. Four of the quasars with individual IRAS detections have intervening galaxies identified with the Mg II absorption-lines. The spectral energy distributions of these galaxies imply far-infrared luminosities in excess of what Arp 220 would give at their redshifts. While all the external evidence suggests that the detection of far-infrared emission from the absorber sample may not be connected to the presence of the Mg II absorber, we discuss future observations which may help explain our results.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/62#1</TD>
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            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
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            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
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            <TD>Radial velocities of high-velocity white dwarfs (Silvestri+, 2002)</TD>
            <TD>Radial velocities and complete space motions were measured for 116 white dwarf stars with M dwarf companions (WD+M), including thirteen pairs having "halo-like" velocities. These 116 WD+dM binaries were observed on the 3.5 m telescope at the Apache Point Observatory (APO) on nearly 30 half-nights between 2000 September 4 and 2001 October 20. The APO Double Imaging Spectrograph was used with a 15" slit, yielding a resolution of approximately 2arcsrc/pixel. From the near-solar abundance levels of the M dwarf companions, only one potential stellar halo white dwarf (LP 164-52) was found in the sample, 12 of the 13 high-velocity white dwarfs being actually part of the high-velocity tail of the thick disk rather than the dark matter halo of the Galaxy.</TD>
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            <TD>Radial velocities of high-velocity white dwarfs (Silvestri+, 2002)</TD>
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            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
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            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
            <TD>A survey of quasar absorbers was conducted using the Infrared Astronomical Satellite (IRAS) database. Quasars with known intervening absorption-line systems and broad absorption line (BAL) QSOs were selected primarily from Junkkarinen et al. (1991ApJS...77..203J). Of the 570 quasars with IRAS data, 52 showed 3{sigma} or better detections in at least one band in SCANPI analysis. The origin of the IRAS flux could be from the absorption-line systems, other galaxies, or the quasar itself. The spectral energy distributions for quasars detected in the absorption-line sample and BAL QSOs were found to be redder than those of two control samples which suggests that some of the IRAS flux may arise in dust associated with the intervening galaxies. IRAS SUPERSCANPI processing was carried out for 77 quasars with known Mg II absorption at Zabs&lt;1 to investigate the ensemble far-infrared properties of these objects. SUPERSCANPI processing evaluates the median flux for many different positions on the sky, resulting in an improvement in the effective sensitivity. A control sample consisting of objects with no Mg II absorption known at Zabs&lt;1 but with the same distribution of absolute V-magnitude, Zem and radio-loud fraction for the background quasars was also processed. The Mg II sample was detected at 3{sigma} or better in all four IRAS bands with a significantly larger flux than the control sample at 60{mu}m and 100{mu}m. If this far-infrared emission is from the absorber galaxies, then the far-infrared luminosity of the composite Mg II absorber was found to be comparable to that of a starbursting galaxy, although such a high star-formation rate is inconsistent with the optical and near-infrared colors of low-redshift Mg II systems. Four of the quasars with individual IRAS detections have intervening galaxies identified with the Mg II absorption-lines. The spectral energy distributions of these galaxies imply far-infrared luminosities in excess of what Arp 220 would give at their redshifts. While all the external evidence suggests that the detection of far-infrared emission from the absorber sample may not be connected to the presence of the Mg II absorber, we discuss future observations which may help explain our results.</TD>
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            <TD>Quasar absorption-line systems (Tanner+ 1996)</TD>
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            <TD>CDS</TD>
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            <TD>ConeSearch</TD>
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            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/62</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/3235 [1]</TD>
            <TD>HIRES atlas of all RBGS galaxies (Surace+, 2004)</TD>
            <TD>We present high-resolution 12, 25, 60, and 100{mu}m images of 106 interacting galaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS, Sanders et al., Cat. &lt;J/AJ/126/1607&gt;), a complete sample of all galaxies having a 60{mu}m flux density greater than 5.24Jy. These systems were selected to have at least two distinguishable galaxies separated by less than three average galactic diameters, and thus we have excluded very widely separated systems and very advanced mergers. Additionally, some systems have been included that are more than three galactic diameters apart, yet have separations less than 4 and are thus likely to suffer from confusion in the RBGS. The new complete survey has the same properties as the prototype survey of Surace et al., 1993AJ....105..864S.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235#1</TD>
            <TD>2012-11-13T14:05:13Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/3235</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3235</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/3235 [2]</TD>
            <TD>HIRES atlas of all RBGS galaxies (Surace+, 2004)</TD>
            <TD>We present high-resolution 12, 25, 60, and 100{mu}m images of 106 interacting galaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS, Sanders et al., Cat. &lt;J/AJ/126/1607&gt;), a complete sample of all galaxies having a 60{mu}m flux density greater than 5.24Jy. These systems were selected to have at least two distinguishable galaxies separated by less than three average galactic diameters, and thus we have excluded very widely separated systems and very advanced mergers. Additionally, some systems have been included that are more than three galactic diameters apart, yet have separations less than 4 and are thus likely to suffer from confusion in the RBGS. The new complete survey has the same properties as the prototype survey of Surace et al., 1993AJ....105..864S.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235#2</TD>
            <TD>2012-11-13T14:05:13Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/3235&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3235</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/3235 [table1]</TD>
            <TD>HIRES atlas of all RBGS galaxies (Surace+, 2004)</TD>
            <TD>We present high-resolution 12, 25, 60, and 100{mu}m images of 106 interacting galaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS, Sanders et al., Cat. &lt;J/AJ/126/1607&gt;), a complete sample of all galaxies having a 60{mu}m flux density greater than 5.24Jy. These systems were selected to have at least two distinguishable galaxies separated by less than three average galactic diameters, and thus we have excluded very widely separated systems and very advanced mergers. Additionally, some systems have been included that are more than three galactic diameters apart, yet have separations less than 4 and are thus likely to suffer from confusion in the RBGS. The new complete survey has the same properties as the prototype survey of Surace et al., 1993AJ....105..864S.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235#table1</TD>
            <TD>2012-11-13T14:05:13Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/3235&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3235</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/109/367 [1]</TD>
            <TD>4C 23.56 field deep imaging (Knopp+ 1997)</TD>
            <TD>We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'&gt;4mag in the field, including two with I-K'&gt;6mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367#1</TD>
            <TD>2011-09-14T18:45:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/109/367</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/367</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/109/367 [2]</TD>
            <TD>4C 23.56 field deep imaging (Knopp+ 1997)</TD>
            <TD>We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'&gt;4mag in the field, including two with I-K'&gt;6mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367#2</TD>
            <TD>2011-09-14T18:45:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/109/367&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/109/367 [table4]</TD>
            <TD>4C 23.56 field deep imaging (Knopp+ 1997)</TD>
            <TD>We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'&gt;4mag in the field, including two with I-K'&gt;6mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367#table4</TD>
            <TD>2011-09-14T18:45:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/109/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/367</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/3235 [1]</TD>
            <TD>HIRES atlas of all RBGS galaxies (Surace+, 2004)</TD>
            <TD>We present high-resolution 12, 25, 60, and 100{mu}m images of 106 interacting galaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS, Sanders et al., Cat. &lt;J/AJ/126/1607&gt;), a complete sample of all galaxies having a 60{mu}m flux density greater than 5.24Jy. These systems were selected to have at least two distinguishable galaxies separated by less than three average galactic diameters, and thus we have excluded very widely separated systems and very advanced mergers. Additionally, some systems have been included that are more than three galactic diameters apart, yet have separations less than 4 and are thus likely to suffer from confusion in the RBGS. The new complete survey has the same properties as the prototype survey of Surace et al., 1993AJ....105..864S.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235#1</TD>
            <TD>2012-11-13T14:05:13Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/3235</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3235</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/3235 [2]</TD>
            <TD>HIRES atlas of all RBGS galaxies (Surace+, 2004)</TD>
            <TD>We present high-resolution 12, 25, 60, and 100{mu}m images of 106 interacting galaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS, Sanders et al., Cat. &lt;J/AJ/126/1607&gt;), a complete sample of all galaxies having a 60{mu}m flux density greater than 5.24Jy. These systems were selected to have at least two distinguishable galaxies separated by less than three average galactic diameters, and thus we have excluded very widely separated systems and very advanced mergers. Additionally, some systems have been included that are more than three galactic diameters apart, yet have separations less than 4 and are thus likely to suffer from confusion in the RBGS. The new complete survey has the same properties as the prototype survey of Surace et al., 1993AJ....105..864S.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235#2</TD>
            <TD>2012-11-13T14:05:13Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/3235&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3235</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/3235 [table1]</TD>
            <TD>HIRES atlas of all RBGS galaxies (Surace+, 2004)</TD>
            <TD>We present high-resolution 12, 25, 60, and 100{mu}m images of 106 interacting galaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS, Sanders et al., Cat. &lt;J/AJ/126/1607&gt;), a complete sample of all galaxies having a 60{mu}m flux density greater than 5.24Jy. These systems were selected to have at least two distinguishable galaxies separated by less than three average galactic diameters, and thus we have excluded very widely separated systems and very advanced mergers. Additionally, some systems have been included that are more than three galactic diameters apart, yet have separations less than 4 and are thus likely to suffer from confusion in the RBGS. The new complete survey has the same properties as the prototype survey of Surace et al., 1993AJ....105..864S.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235#table1</TD>
            <TD>2012-11-13T14:05:13Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/3235&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3235</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/109/367 [1]</TD>
            <TD>4C 23.56 field deep imaging (Knopp+ 1997)</TD>
            <TD>We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'&gt;4mag in the field, including two with I-K'&gt;6mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367#1</TD>
            <TD>2011-09-14T18:45:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/109/367</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/367</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/109/367 [2]</TD>
            <TD>4C 23.56 field deep imaging (Knopp+ 1997)</TD>
            <TD>We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'&gt;4mag in the field, including two with I-K'&gt;6mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367#2</TD>
            <TD>2011-09-14T18:45:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/109/367&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/109/367 [table4]</TD>
            <TD>4C 23.56 field deep imaging (Knopp+ 1997)</TD>
            <TD>We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'&gt;4mag in the field, including two with I-K'&gt;6mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367#table4</TD>
            <TD>2011-09-14T18:45:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/109/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/367</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/3235 [1]</TD>
            <TD>HIRES atlas of all RBGS galaxies (Surace+, 2004)</TD>
            <TD>We present high-resolution 12, 25, 60, and 100{mu}m images of 106 interacting galaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS, Sanders et al., Cat. &lt;J/AJ/126/1607&gt;), a complete sample of all galaxies having a 60{mu}m flux density greater than 5.24Jy. These systems were selected to have at least two distinguishable galaxies separated by less than three average galactic diameters, and thus we have excluded very widely separated systems and very advanced mergers. Additionally, some systems have been included that are more than three galactic diameters apart, yet have separations less than 4 and are thus likely to suffer from confusion in the RBGS. The new complete survey has the same properties as the prototype survey of Surace et al., 1993AJ....105..864S.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235#1</TD>
            <TD>2012-11-13T14:05:13Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/3235</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3235</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/3235 [2]</TD>
            <TD>HIRES atlas of all RBGS galaxies (Surace+, 2004)</TD>
            <TD>We present high-resolution 12, 25, 60, and 100{mu}m images of 106 interacting galaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS, Sanders et al., Cat. &lt;J/AJ/126/1607&gt;), a complete sample of all galaxies having a 60{mu}m flux density greater than 5.24Jy. These systems were selected to have at least two distinguishable galaxies separated by less than three average galactic diameters, and thus we have excluded very widely separated systems and very advanced mergers. Additionally, some systems have been included that are more than three galactic diameters apart, yet have separations less than 4 and are thus likely to suffer from confusion in the RBGS. The new complete survey has the same properties as the prototype survey of Surace et al., 1993AJ....105..864S.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235#2</TD>
            <TD>2012-11-13T14:05:13Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/3235&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3235</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/3235 [table1]</TD>
            <TD>HIRES atlas of all RBGS galaxies (Surace+, 2004)</TD>
            <TD>We present high-resolution 12, 25, 60, and 100{mu}m images of 106 interacting galaxy systems contained in the IRAS Revised Bright Galaxy Sample (RBGS, Sanders et al., Cat. &lt;J/AJ/126/1607&gt;), a complete sample of all galaxies having a 60{mu}m flux density greater than 5.24Jy. These systems were selected to have at least two distinguishable galaxies separated by less than three average galactic diameters, and thus we have excluded very widely separated systems and very advanced mergers. Additionally, some systems have been included that are more than three galactic diameters apart, yet have separations less than 4 and are thus likely to suffer from confusion in the RBGS. The new complete survey has the same properties as the prototype survey of Surace et al., 1993AJ....105..864S.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235#table1</TD>
            <TD>2012-11-13T14:05:13Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3235</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/3235&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3235</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/109/367 [1]</TD>
            <TD>4C 23.56 field deep imaging (Knopp+ 1997)</TD>
            <TD>We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'&gt;4mag in the field, including two with I-K'&gt;6mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367#1</TD>
            <TD>2011-09-14T18:45:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/109/367</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/367</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/109/367 [2]</TD>
            <TD>4C 23.56 field deep imaging (Knopp+ 1997)</TD>
            <TD>We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'&gt;4mag in the field, including two with I-K'&gt;6mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367#2</TD>
            <TD>2011-09-14T18:45:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/109/367&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/109/367 [table4]</TD>
            <TD>4C 23.56 field deep imaging (Knopp+ 1997)</TD>
            <TD>We present deep infrared and optical imaging of a 1.25arcmin^2^ field centered on the giant (~0.5Mpc) high-redshift (z=2.479) ultra-steep-spectrum radio source 4C 23.56. The optical/infrared continuum morphology of the host galaxy is asymmetric, with strong color gradients and an enormous biconical emission-line nebula. The morphology of 4C 23.56 is best described by a dusty galaxy illuminated by a beam from an active galactic nucleus that is scattered into our line of sight. We determine the K' band number counts in the field to a limit of K'=22.5mag and find a marginally significant excess of objects with K'=19-21mag, compared to other K' band surveys. Spectral energy distributions (SEDs) of 117 objects in the field are constructed from aperture photometry in five bands (U', NB, V, I, and K'). From the SEDS we distinguish three subsets of objects as possible candidates for z~2.48 companions: emission-line galaxies, very red galaxies, and flat-spectrum star-forming galaxies. The field has nine candidate objects with line emission in a narrow band centered on the redshifted Ly{alpha} line, compared to an expected number of at most three foreground [O II] emitters that could mimic Ly{alpha} alpha sources. We find a high density of faint, very red objects with I-K'&gt;4mag in the field, including two with I-K'&gt;6mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367#table4</TD>
            <TD>2011-09-14T18:45:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/109/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/53/653 [1]</TD>
            <TD>SSA 22 field NIR imaging (Tamura+, 2001)</TD>
            <TD>Deep narrow- and broad-band near-infrared imaging observations of the central 2'x2' region of the SSA 22 field were made with the near-infrared camera (CISCO) attached to the Subaru Telescope. Using a narrow-band filter centered at 2.033{mu}m, [O III] {lambda}5007 emitters at z~3.06+/-0.02 were searched to examine star-forming activities in an over-density region where a clustering of Lyman Break Galaxies (LBGs) and Lyman {alpha} emitter candidates around z=3.09 was reported, though the targeted redshift is slightly different from that of the peak of the over-density region. Although one emitter candidate at z=3.06 was detected, it is likely to be located at a redshift of between 1 and 2 judged based on multi-band photometry. Another emission-line object was detected in another narrow-band filter (``off band'' filter) centered at 2.120{mu}m, which is identified with a galaxy at z=0.132 (the emission line is Paschen {alpha}). The K'-band imaging data revealed the presence of 12 Extremely Red Objects (EROs) with I_814_-K'&gt;=4. The distribution of the EROs does not seem to coincide with that of Lyman Break Galaxies or Lyman {alpha} emitters at z~3. The magnitudes and colors of the EROs are not consistent with those of passively evolving massive elliptical galaxies at z~3. Candidates for counterparts of the submm sources detected with SCUBA are found; no EROs around the submm sources are found in our magnitude limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653#1</TD>
            <TD>2012-11-13T14:14:57Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/53/653</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/53/653</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/53/653 [2]</TD>
            <TD>SSA 22 field NIR imaging (Tamura+, 2001)</TD>
            <TD>Deep narrow- and broad-band near-infrared imaging observations of the central 2'x2' region of the SSA 22 field were made with the near-infrared camera (CISCO) attached to the Subaru Telescope. Using a narrow-band filter centered at 2.033{mu}m, [O III] {lambda}5007 emitters at z~3.06+/-0.02 were searched to examine star-forming activities in an over-density region where a clustering of Lyman Break Galaxies (LBGs) and Lyman {alpha} emitter candidates around z=3.09 was reported, though the targeted redshift is slightly different from that of the peak of the over-density region. Although one emitter candidate at z=3.06 was detected, it is likely to be located at a redshift of between 1 and 2 judged based on multi-band photometry. Another emission-line object was detected in another narrow-band filter (``off band'' filter) centered at 2.120{mu}m, which is identified with a galaxy at z=0.132 (the emission line is Paschen {alpha}). The K'-band imaging data revealed the presence of 12 Extremely Red Objects (EROs) with I_814_-K'&gt;=4. The distribution of the EROs does not seem to coincide with that of Lyman Break Galaxies or Lyman {alpha} emitters at z~3. The magnitudes and colors of the EROs are not consistent with those of passively evolving massive elliptical galaxies at z~3. Candidates for counterparts of the submm sources detected with SCUBA are found; no EROs around the submm sources are found in our magnitude limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653#2</TD>
            <TD>2012-11-13T14:14:57Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/53/653&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/53/653</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/53/653 [table3]</TD>
            <TD>SSA 22 field NIR imaging (Tamura+, 2001)</TD>
            <TD>Deep narrow- and broad-band near-infrared imaging observations of the central 2'x2' region of the SSA 22 field were made with the near-infrared camera (CISCO) attached to the Subaru Telescope. Using a narrow-band filter centered at 2.033{mu}m, [O III] {lambda}5007 emitters at z~3.06+/-0.02 were searched to examine star-forming activities in an over-density region where a clustering of Lyman Break Galaxies (LBGs) and Lyman {alpha} emitter candidates around z=3.09 was reported, though the targeted redshift is slightly different from that of the peak of the over-density region. Although one emitter candidate at z=3.06 was detected, it is likely to be located at a redshift of between 1 and 2 judged based on multi-band photometry. Another emission-line object was detected in another narrow-band filter (``off band'' filter) centered at 2.120{mu}m, which is identified with a galaxy at z=0.132 (the emission line is Paschen {alpha}). The K'-band imaging data revealed the presence of 12 Extremely Red Objects (EROs) with I_814_-K'&gt;=4. The distribution of the EROs does not seem to coincide with that of Lyman Break Galaxies or Lyman {alpha} emitters at z~3. The magnitudes and colors of the EROs are not consistent with those of passively evolving massive elliptical galaxies at z~3. Candidates for counterparts of the submm sources detected with SCUBA are found; no EROs around the submm sources are found in our magnitude limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653#table3</TD>
            <TD>2012-11-13T14:14:57Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/53/653&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/53/653</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/496/39 [1]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#1</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/496/39</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/496/39 [2]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#2</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/496/39&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/496/39 [table2]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#table2</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/496/39&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/496/39 [table1]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#table1</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/496/39&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/53/653 [1]</TD>
            <TD>SSA 22 field NIR imaging (Tamura+, 2001)</TD>
            <TD>Deep narrow- and broad-band near-infrared imaging observations of the central 2'x2' region of the SSA 22 field were made with the near-infrared camera (CISCO) attached to the Subaru Telescope. Using a narrow-band filter centered at 2.033{mu}m, [O III] {lambda}5007 emitters at z~3.06+/-0.02 were searched to examine star-forming activities in an over-density region where a clustering of Lyman Break Galaxies (LBGs) and Lyman {alpha} emitter candidates around z=3.09 was reported, though the targeted redshift is slightly different from that of the peak of the over-density region. Although one emitter candidate at z=3.06 was detected, it is likely to be located at a redshift of between 1 and 2 judged based on multi-band photometry. Another emission-line object was detected in another narrow-band filter (``off band'' filter) centered at 2.120{mu}m, which is identified with a galaxy at z=0.132 (the emission line is Paschen {alpha}). The K'-band imaging data revealed the presence of 12 Extremely Red Objects (EROs) with I_814_-K'&gt;=4. The distribution of the EROs does not seem to coincide with that of Lyman Break Galaxies or Lyman {alpha} emitters at z~3. The magnitudes and colors of the EROs are not consistent with those of passively evolving massive elliptical galaxies at z~3. Candidates for counterparts of the submm sources detected with SCUBA are found; no EROs around the submm sources are found in our magnitude limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653#1</TD>
            <TD>2012-11-13T14:14:57Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/53/653</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/53/653</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/53/653 [2]</TD>
            <TD>SSA 22 field NIR imaging (Tamura+, 2001)</TD>
            <TD>Deep narrow- and broad-band near-infrared imaging observations of the central 2'x2' region of the SSA 22 field were made with the near-infrared camera (CISCO) attached to the Subaru Telescope. Using a narrow-band filter centered at 2.033{mu}m, [O III] {lambda}5007 emitters at z~3.06+/-0.02 were searched to examine star-forming activities in an over-density region where a clustering of Lyman Break Galaxies (LBGs) and Lyman {alpha} emitter candidates around z=3.09 was reported, though the targeted redshift is slightly different from that of the peak of the over-density region. Although one emitter candidate at z=3.06 was detected, it is likely to be located at a redshift of between 1 and 2 judged based on multi-band photometry. Another emission-line object was detected in another narrow-band filter (``off band'' filter) centered at 2.120{mu}m, which is identified with a galaxy at z=0.132 (the emission line is Paschen {alpha}). The K'-band imaging data revealed the presence of 12 Extremely Red Objects (EROs) with I_814_-K'&gt;=4. The distribution of the EROs does not seem to coincide with that of Lyman Break Galaxies or Lyman {alpha} emitters at z~3. The magnitudes and colors of the EROs are not consistent with those of passively evolving massive elliptical galaxies at z~3. Candidates for counterparts of the submm sources detected with SCUBA are found; no EROs around the submm sources are found in our magnitude limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653#2</TD>
            <TD>2012-11-13T14:14:57Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/53/653&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/53/653</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/53/653 [table3]</TD>
            <TD>SSA 22 field NIR imaging (Tamura+, 2001)</TD>
            <TD>Deep narrow- and broad-band near-infrared imaging observations of the central 2'x2' region of the SSA 22 field were made with the near-infrared camera (CISCO) attached to the Subaru Telescope. Using a narrow-band filter centered at 2.033{mu}m, [O III] {lambda}5007 emitters at z~3.06+/-0.02 were searched to examine star-forming activities in an over-density region where a clustering of Lyman Break Galaxies (LBGs) and Lyman {alpha} emitter candidates around z=3.09 was reported, though the targeted redshift is slightly different from that of the peak of the over-density region. Although one emitter candidate at z=3.06 was detected, it is likely to be located at a redshift of between 1 and 2 judged based on multi-band photometry. Another emission-line object was detected in another narrow-band filter (``off band'' filter) centered at 2.120{mu}m, which is identified with a galaxy at z=0.132 (the emission line is Paschen {alpha}). The K'-band imaging data revealed the presence of 12 Extremely Red Objects (EROs) with I_814_-K'&gt;=4. The distribution of the EROs does not seem to coincide with that of Lyman Break Galaxies or Lyman {alpha} emitters at z~3. The magnitudes and colors of the EROs are not consistent with those of passively evolving massive elliptical galaxies at z~3. Candidates for counterparts of the submm sources detected with SCUBA are found; no EROs around the submm sources are found in our magnitude limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653#table3</TD>
            <TD>2012-11-13T14:14:57Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/53/653&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/53/653</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/496/39 [1]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#1</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/496/39</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/496/39 [2]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#2</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/496/39&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/496/39 [table2]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#table2</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/496/39&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/496/39 [table1]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#table1</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/496/39&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/53/653 [1]</TD>
            <TD>SSA 22 field NIR imaging (Tamura+, 2001)</TD>
            <TD>Deep narrow- and broad-band near-infrared imaging observations of the central 2'x2' region of the SSA 22 field were made with the near-infrared camera (CISCO) attached to the Subaru Telescope. Using a narrow-band filter centered at 2.033{mu}m, [O III] {lambda}5007 emitters at z~3.06+/-0.02 were searched to examine star-forming activities in an over-density region where a clustering of Lyman Break Galaxies (LBGs) and Lyman {alpha} emitter candidates around z=3.09 was reported, though the targeted redshift is slightly different from that of the peak of the over-density region. Although one emitter candidate at z=3.06 was detected, it is likely to be located at a redshift of between 1 and 2 judged based on multi-band photometry. Another emission-line object was detected in another narrow-band filter (``off band'' filter) centered at 2.120{mu}m, which is identified with a galaxy at z=0.132 (the emission line is Paschen {alpha}). The K'-band imaging data revealed the presence of 12 Extremely Red Objects (EROs) with I_814_-K'&gt;=4. The distribution of the EROs does not seem to coincide with that of Lyman Break Galaxies or Lyman {alpha} emitters at z~3. The magnitudes and colors of the EROs are not consistent with those of passively evolving massive elliptical galaxies at z~3. Candidates for counterparts of the submm sources detected with SCUBA are found; no EROs around the submm sources are found in our magnitude limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653#1</TD>
            <TD>2012-11-13T14:14:57Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/53/653</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/53/653</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/53/653 [2]</TD>
            <TD>SSA 22 field NIR imaging (Tamura+, 2001)</TD>
            <TD>Deep narrow- and broad-band near-infrared imaging observations of the central 2'x2' region of the SSA 22 field were made with the near-infrared camera (CISCO) attached to the Subaru Telescope. Using a narrow-band filter centered at 2.033{mu}m, [O III] {lambda}5007 emitters at z~3.06+/-0.02 were searched to examine star-forming activities in an over-density region where a clustering of Lyman Break Galaxies (LBGs) and Lyman {alpha} emitter candidates around z=3.09 was reported, though the targeted redshift is slightly different from that of the peak of the over-density region. Although one emitter candidate at z=3.06 was detected, it is likely to be located at a redshift of between 1 and 2 judged based on multi-band photometry. Another emission-line object was detected in another narrow-band filter (``off band'' filter) centered at 2.120{mu}m, which is identified with a galaxy at z=0.132 (the emission line is Paschen {alpha}). The K'-band imaging data revealed the presence of 12 Extremely Red Objects (EROs) with I_814_-K'&gt;=4. The distribution of the EROs does not seem to coincide with that of Lyman Break Galaxies or Lyman {alpha} emitters at z~3. The magnitudes and colors of the EROs are not consistent with those of passively evolving massive elliptical galaxies at z~3. Candidates for counterparts of the submm sources detected with SCUBA are found; no EROs around the submm sources are found in our magnitude limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653#2</TD>
            <TD>2012-11-13T14:14:57Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/53/653&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/53/653</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/53/653 [table3]</TD>
            <TD>SSA 22 field NIR imaging (Tamura+, 2001)</TD>
            <TD>Deep narrow- and broad-band near-infrared imaging observations of the central 2'x2' region of the SSA 22 field were made with the near-infrared camera (CISCO) attached to the Subaru Telescope. Using a narrow-band filter centered at 2.033{mu}m, [O III] {lambda}5007 emitters at z~3.06+/-0.02 were searched to examine star-forming activities in an over-density region where a clustering of Lyman Break Galaxies (LBGs) and Lyman {alpha} emitter candidates around z=3.09 was reported, though the targeted redshift is slightly different from that of the peak of the over-density region. Although one emitter candidate at z=3.06 was detected, it is likely to be located at a redshift of between 1 and 2 judged based on multi-band photometry. Another emission-line object was detected in another narrow-band filter (``off band'' filter) centered at 2.120{mu}m, which is identified with a galaxy at z=0.132 (the emission line is Paschen {alpha}). The K'-band imaging data revealed the presence of 12 Extremely Red Objects (EROs) with I_814_-K'&gt;=4. The distribution of the EROs does not seem to coincide with that of Lyman Break Galaxies or Lyman {alpha} emitters at z~3. The magnitudes and colors of the EROs are not consistent with those of passively evolving massive elliptical galaxies at z~3. Candidates for counterparts of the submm sources detected with SCUBA are found; no EROs around the submm sources are found in our magnitude limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653#table3</TD>
            <TD>2012-11-13T14:14:57Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/53/653</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/53/653&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/53/653</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/496/39 [1]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#1</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/496/39</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/496/39 [2]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#2</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/496/39&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/496/39 [table2]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#table2</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/496/39&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/496/39 [table1]</TD>
            <TD>Properties of poor groups of galaxies. I. (Zabludoff+ 1998)</TD>
            <TD>We use multifiber spectroscopy of 12 poor groups of galaxies to address (1) whether the groups are bound systems or chance projections of galaxies along the line of sight; (2) why the members of each group have not already merged to form a single galaxy, despite the groups' high galaxy densities, short crossing times, and likely environments for galaxy-galaxy mergers; and (3) how galaxies might evolve in these groups, where the collisional effects of the intragroup gas and the tidal influences of the global potential are weaker than in rich clusters. Each of the 12 groups has fewer than about five cataloged members in the literature. Our sample consists of 1002 galaxy velocities, 280 of which are group members. The groups have mean recessional velocities between 1600 and 7600km/s. Nine groups, including three Hickson compact groups, have the extended X-ray emission characteristic of an intragroup medium (see Paper II, 1998ApJ...496...73M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39#table1</TD>
            <TD>2011-09-14T18:46:00Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/496/39</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/496/39&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/496/39</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/PASA/16. [1]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#1</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/PASA/16.113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/PASA/16. [2]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#2</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/PASA/16.113&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/PASA/16. [table2]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#table2</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/PASA/16.113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/PASA/16. [table3]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#table3</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/PASA/16.113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/103/331 [1]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#1</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/103/331</TD>
            <TD />
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            <TD>ivo://CDS</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJS/103/331 [2]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#2</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/103/331 [table2]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#table2</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/103/331 [table1]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#table1</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/103/331 [table3]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#table3</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/PASA/16. [1]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#1</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/PASA/16.113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/PASA/16. [2]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#2</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/PASA/16.113&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/PASA/16. [table2]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#table2</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/PASA/16.113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/PASA/16. [table3]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#table3</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/PASA/16.113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/103/331 [1]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#1</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/103/331</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/103/331 [2]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#2</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD />
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/103/331&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/103/331 [table2]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#table2</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/103/331 [table1]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#table1</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/103/331 [table3]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#table3</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/PASA/16. [1]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#1</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/PASA/16.113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/PASA/16. [2]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#2</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/PASA/16.113&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/PASA/16. [table2]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#table2</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/PASA/16.113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/PASA/16. [table3]</TD>
            <TD>New structure in Shapley supercluster (Drinkwater+, 1999)</TD>
            <TD>We present new radial velocities for 306 bright (R&lt;16) galaxies in a 77{deg}^2^ region of the Shapley supercluster, measured with the FLAIR-II spectrograph on the UK Schmidt Telescope. The galaxies we measured were uniformly distributed over the survey area, in contrast to previous samples which were concentrated in several rich Abell clusters. Most of the galaxies (230) were members of the Shapley supercluster: they trace out two previously unknown sheets of galaxies linking the Abell clusters of the supercluster. In a 44{deg}^2^ area of the supercluster excluding the Abell clusters, these sheets alone represent an overdensity of a factor of 2.0+/-0.2 compared to a uniform galaxy distribution. The supercluster is not flattened in the Declination direction as has been suggested in previous papers. Within our survey area the new galaxies contribute an additional 50% to the known contents of the Shapley supercluster, with a corresponding increase in its contribution to the motion of the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113#table3</TD>
            <TD>2012-11-13T14:17:54Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/other/PASA/16.113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/PASA/16.113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/PASA/16.113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/103/331 [1]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#1</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/103/331</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/103/331 [2]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#2</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/103/331 [table2]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#table2</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/103/331 [table1]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#table1</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/103/331 [table3]</TD>
            <TD>mJy radio sources at 1.4 GHz (Lu+ 1996)</TD>
            <TD>From the 1.4GHz radio survey of Condon, Dickey, &amp; Salpeter (Cat. &lt;J/AJ/99/1071&gt;) in a region much devoid of rich galaxy clusters at redshifts z&lt;0.43 we selected a "distant" sample of 57 radio sources complete to a 1.4GHz flux density of 35mJy and a "nearby" sample of 36 mostly weaker radio sources which are optically brighter than B~19mag. Our ultimate goals are (1) to study the radio, optical, and near-IR properties of those high-redshift (z~1), moderate-power radio sources in the distant sample and to compare them with that of more powerful radio sources, and (2) to make a comparison of primarily noncluster radio sources in the nearby sample with a companion survey of radio sources in a pair of rich superclusters at z~0.1. In this first paper of a series, we report our new C-array VLA continuum snapshots at 4.86GHz and optical R-band CCD imaging photometry for these two samples and tabulate the observational results on individual sources. Some direct sample statistical properties are also discussed in the paper and summarized as follows: (1) The distant sample: (a) The sample median flux density at 1.4GHz is about 65mJy. (b) The majority (80%) of the sample sources have a steep spectrum between 1.4 and 4.86GHz with a spectral index around 0.9. Nineteen (90%) of the 21 sources that are fully resolved at 4.86 GHz (i.e., angular sizes {theta}&gt;11") have a radio morphology of Fanaroff-Riley (FR) II type. (c) Thirty-seven (88%) of the 42 optically imaged sample sources were optically identified to a limiting R-band magnitude of R~23.5mag. About 15% of the identified radio sources appear to be point sources, and the others are extended galaxies with an appearance similar to nearby elliptical galaxies. (d) Twenty-eight (76%) of the optically identified sources have R&gt;20mag, suggesting that these are probably distant (z&gt;0.8), with a redshift distribution peaking at z~1, where their radio luminosities are about 10 times the break power between the FR I and II classes. (e) We found no strong evidence for the radio and optical axes of the resolved radio sources (i.e., {theta}&gt;5") to be correlated or anticorrelated, nor any evidence for strong clustering around sample radio sources on average. (2) The nearby sample: except for R&lt;15, the sample is dominated by elliptical galaxies with 16&lt;R&lt;18.5mag and a spectral index distribution similar to that of the distant sample. Based on the radial distribution of optical objects around each radio source, we found that the average radio source environment becomes richer from that characteristic of galaxy groups for R&lt;17mag (z&lt;0.2) to that of galaxy groups to clusters at R&gt;18mag (z&gt;0.3) .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331#table3</TD>
            <TD>2011-09-14T18:46:19Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/103/331</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/103/331&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/103/331</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/1323 [1]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#1</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/1323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/1323 [2]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#2</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/1323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/1323 [GCCstars]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#GCCstars</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/1323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/1323 [table4]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#table4</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/1323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/521 [1]</TD>
            <TD>Galaxies redshifts, 210&lt;l&lt;360, |b|&lt;15 (Visvanathan+ 1996)</TD>
            <TD>We have carried out a redshift survey of an IRAS flux-limited (f_60_&gt;0.6) galaxy sample behind the southern Milky Way, 210{deg}&lt;l&lt;360{deg} at |b|&lt;15{deg}. The survey includes redshifts for 951 galaxies, ~500 of which are new. Of these 951 galaxies, 462 are in the zone 5{deg}&lt;b&lt;15{deg} and 353 are in the zone -15{deg}&lt;b&lt;-5{deg}. Though the innermost region of the Milky Way (|b|=5{deg}) remains opaque except in the longitude near 240, the detected galaxies show a high degree of completeness (~70%) in the zones 5{deg}&lt;b&lt;15{deg} and -15{deg}&lt;b&lt;-5{deg}. The cone diagrams exhibiting the detailed distribution of IRAS galaxies in the region 210{deg}&lt;l&lt;360{deg}, |b|&lt;15{deg} shows two clusters in the Puppis region (l=240{deg}, b=-7{deg}, v=2400km/s; l=245{deg}, b=-5{deg}, v=7500km/s), the A3627 cluster (l=325{deg}, b=-7{deg}; v=4500km/s), the S4 cluster (l=280{deg}, b=7{deg}; v=5500km/s), and a possible void at l=245{deg}, v=3000km/s. The region 270{deg}&lt;l&lt;350{deg} is dominated by overdensity of galaxies representing the extension of the Hydra-Centaurus complex in the positive latitudes and the Pavo-Indus complex in the negative latitudes. A velocity histogram of galaxies in the GA region 290{deg}&lt;l&lt;350{deg}, |b|&lt;15{deg}. reveals a substantial overdensity of galaxies in the velocity range 2400-5000km/s. The centroid of this overdensity is located at 4000km/s. The broad increased density of galaxies seen in our data corresponds with the distant concentration seen at 4500km/s in the supergalactic plane survey that covers the same longitude range like ours in l, but a larger range in latitude b (-30{deg} to -10{deg} and +10{deg} to +45{deg}). This lends support to the idea that the overdensity extends all the way from the Centaurus-Hydra complex (l=302{deg}, b=+22{deg}) in the north to the major concentration of the Pavo-Indus supercluster (l=332{deg}, b=-24{deg}) in the south, through the Milky Way. We conclude that the peak of the overdensity responsible for the peculiar velocity field in the local region is possibly situated in the Milky Way itself.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521#1</TD>
            <TD>2011-09-14T18:46:23Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/521 [2]</TD>
            <TD>Galaxies redshifts, 210&lt;l&lt;360, |b|&lt;15 (Visvanathan+ 1996)</TD>
            <TD>We have carried out a redshift survey of an IRAS flux-limited (f_60_&gt;0.6) galaxy sample behind the southern Milky Way, 210{deg}&lt;l&lt;360{deg} at |b|&lt;15{deg}. The survey includes redshifts for 951 galaxies, ~500 of which are new. Of these 951 galaxies, 462 are in the zone 5{deg}&lt;b&lt;15{deg} and 353 are in the zone -15{deg}&lt;b&lt;-5{deg}. Though the innermost region of the Milky Way (|b|=5{deg}) remains opaque except in the longitude near 240, the detected galaxies show a high degree of completeness (~70%) in the zones 5{deg}&lt;b&lt;15{deg} and -15{deg}&lt;b&lt;-5{deg}. The cone diagrams exhibiting the detailed distribution of IRAS galaxies in the region 210{deg}&lt;l&lt;360{deg}, |b|&lt;15{deg} shows two clusters in the Puppis region (l=240{deg}, b=-7{deg}, v=2400km/s; l=245{deg}, b=-5{deg}, v=7500km/s), the A3627 cluster (l=325{deg}, b=-7{deg}; v=4500km/s), the S4 cluster (l=280{deg}, b=7{deg}; v=5500km/s), and a possible void at l=245{deg}, v=3000km/s. The region 270{deg}&lt;l&lt;350{deg} is dominated by overdensity of galaxies representing the extension of the Hydra-Centaurus complex in the positive latitudes and the Pavo-Indus complex in the negative latitudes. A velocity histogram of galaxies in the GA region 290{deg}&lt;l&lt;350{deg}, |b|&lt;15{deg}. reveals a substantial overdensity of galaxies in the velocity range 2400-5000km/s. The centroid of this overdensity is located at 4000km/s. The broad increased density of galaxies seen in our data corresponds with the distant concentration seen at 4500km/s in the supergalactic plane survey that covers the same longitude range like ours in l, but a larger range in latitude b (-30{deg} to -10{deg} and +10{deg} to +45{deg}). This lends support to the idea that the overdensity extends all the way from the Centaurus-Hydra complex (l=302{deg}, b=+22{deg}) in the north to the major concentration of the Pavo-Indus supercluster (l=332{deg}, b=-24{deg}) in the south, through the Milky Way. We conclude that the peak of the overdensity responsible for the peculiar velocity field in the local region is possibly situated in the Milky Way itself.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521#2</TD>
            <TD>2011-09-14T18:46:23Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/1323 [1]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#1</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/1323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/1323 [2]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#2</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/1323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/1323 [GCCstars]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#GCCstars</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/1323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/1323 [table4]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#table4</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/1323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/1323 [1]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#1</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/1323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/1323 [2]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#2</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/1323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/1323 [GCCstars]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#GCCstars</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/1323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/1323 [table4]</TD>
            <TD>Spectroscopy of stars in the Galaxy's nuclear cluster (Do+ 2009)</TD>
            <TD>Near-IR spectra of the central 4" of the Galaxy were obtained between 2007 and 2008 using the OSIRIS integral field spectrograph in conjunction with the LGS AO system on the Keck II telescope. All observations were taken with the narrowband filter Kn3 (2.121-2.229um) centered on the Br{gamma} hydrogen line at 2.1661um, with a pixel scale of 35mas and a spectral resolution of ~3000. With the goal of covering an ~8"x6" area centered on Sgr A*, we divided this region into seven fields (figure 1).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323#table4</TD>
            <TD>2012-04-02T15:30:35Z</TD>
            <TD>#Equivalent_widths#Spectroscopy#Stars:early-type#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/1323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/521 [1]</TD>
            <TD>Galaxies redshifts, 210&lt;l&lt;360, |b|&lt;15 (Visvanathan+ 1996)</TD>
            <TD>We have carried out a redshift survey of an IRAS flux-limited (f_60_&gt;0.6) galaxy sample behind the southern Milky Way, 210{deg}&lt;l&lt;360{deg} at |b|&lt;15{deg}. The survey includes redshifts for 951 galaxies, ~500 of which are new. Of these 951 galaxies, 462 are in the zone 5{deg}&lt;b&lt;15{deg} and 353 are in the zone -15{deg}&lt;b&lt;-5{deg}. Though the innermost region of the Milky Way (|b|=5{deg}) remains opaque except in the longitude near 240, the detected galaxies show a high degree of completeness (~70%) in the zones 5{deg}&lt;b&lt;15{deg} and -15{deg}&lt;b&lt;-5{deg}. The cone diagrams exhibiting the detailed distribution of IRAS galaxies in the region 210{deg}&lt;l&lt;360{deg}, |b|&lt;15{deg} shows two clusters in the Puppis region (l=240{deg}, b=-7{deg}, v=2400km/s; l=245{deg}, b=-5{deg}, v=7500km/s), the A3627 cluster (l=325{deg}, b=-7{deg}; v=4500km/s), the S4 cluster (l=280{deg}, b=7{deg}; v=5500km/s), and a possible void at l=245{deg}, v=3000km/s. The region 270{deg}&lt;l&lt;350{deg} is dominated by overdensity of galaxies representing the extension of the Hydra-Centaurus complex in the positive latitudes and the Pavo-Indus complex in the negative latitudes. A velocity histogram of galaxies in the GA region 290{deg}&lt;l&lt;350{deg}, |b|&lt;15{deg}. reveals a substantial overdensity of galaxies in the velocity range 2400-5000km/s. The centroid of this overdensity is located at 4000km/s. The broad increased density of galaxies seen in our data corresponds with the distant concentration seen at 4500km/s in the supergalactic plane survey that covers the same longitude range like ours in l, but a larger range in latitude b (-30{deg} to -10{deg} and +10{deg} to +45{deg}). This lends support to the idea that the overdensity extends all the way from the Centaurus-Hydra complex (l=302{deg}, b=+22{deg}) in the north to the major concentration of the Pavo-Indus supercluster (l=332{deg}, b=-24{deg}) in the south, through the Milky Way. We conclude that the peak of the overdensity responsible for the peculiar velocity field in the local region is possibly situated in the Milky Way itself.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521#1</TD>
            <TD>2011-09-14T18:46:23Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/521 [2]</TD>
            <TD>Galaxies redshifts, 210&lt;l&lt;360, |b|&lt;15 (Visvanathan+ 1996)</TD>
            <TD>We have carried out a redshift survey of an IRAS flux-limited (f_60_&gt;0.6) galaxy sample behind the southern Milky Way, 210{deg}&lt;l&lt;360{deg} at |b|&lt;15{deg}. The survey includes redshifts for 951 galaxies, ~500 of which are new. Of these 951 galaxies, 462 are in the zone 5{deg}&lt;b&lt;15{deg} and 353 are in the zone -15{deg}&lt;b&lt;-5{deg}. Though the innermost region of the Milky Way (|b|=5{deg}) remains opaque except in the longitude near 240, the detected galaxies show a high degree of completeness (~70%) in the zones 5{deg}&lt;b&lt;15{deg} and -15{deg}&lt;b&lt;-5{deg}. The cone diagrams exhibiting the detailed distribution of IRAS galaxies in the region 210{deg}&lt;l&lt;360{deg}, |b|&lt;15{deg} shows two clusters in the Puppis region (l=240{deg}, b=-7{deg}, v=2400km/s; l=245{deg}, b=-5{deg}, v=7500km/s), the A3627 cluster (l=325{deg}, b=-7{deg}; v=4500km/s), the S4 cluster (l=280{deg}, b=7{deg}; v=5500km/s), and a possible void at l=245{deg}, v=3000km/s. The region 270{deg}&lt;l&lt;350{deg} is dominated by overdensity of galaxies representing the extension of the Hydra-Centaurus complex in the positive latitudes and the Pavo-Indus complex in the negative latitudes. A velocity histogram of galaxies in the GA region 290{deg}&lt;l&lt;350{deg}, |b|&lt;15{deg}. reveals a substantial overdensity of galaxies in the velocity range 2400-5000km/s. The centroid of this overdensity is located at 4000km/s. The broad increased density of galaxies seen in our data corresponds with the distant concentration seen at 4500km/s in the supergalactic plane survey that covers the same longitude range like ours in l, but a larger range in latitude b (-30{deg} to -10{deg} and +10{deg} to +45{deg}). This lends support to the idea that the overdensity extends all the way from the Centaurus-Hydra complex (l=302{deg}, b=+22{deg}) in the north to the major concentration of the Pavo-Indus supercluster (l=332{deg}, b=-24{deg}) in the south, through the Milky Way. We conclude that the peak of the overdensity responsible for the peculiar velocity field in the local region is possibly situated in the Milky Way itself.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521#2</TD>
            <TD>2011-09-14T18:46:23Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/415/1013 [1]</TD>
            <TD>FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)</TD>
            <TD>We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington &amp; Scott 1965MmRAS..69..183P; Gower, Scott &amp; Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson &amp; Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn &amp; Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin &amp; Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013#1</TD>
            <TD>2012-04-22T15:04:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/415/1013</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/1013</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/415/1013 [2]</TD>
            <TD>FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)</TD>
            <TD>We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington &amp; Scott 1965MmRAS..69..183P; Gower, Scott &amp; Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson &amp; Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn &amp; Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin &amp; Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013#2</TD>
            <TD>2012-04-22T15:04:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/415/1013&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/1013</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/415/1013 [appena]</TD>
            <TD>FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)</TD>
            <TD>We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington &amp; Scott 1965MmRAS..69..183P; Gower, Scott &amp; Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson &amp; Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn &amp; Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin &amp; Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013#appena</TD>
            <TD>2012-04-22T15:04:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/415/1013&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/1013</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/521 [1]</TD>
            <TD>Galaxies redshifts, 210&lt;l&lt;360, |b|&lt;15 (Visvanathan+ 1996)</TD>
            <TD>We have carried out a redshift survey of an IRAS flux-limited (f_60_&gt;0.6) galaxy sample behind the southern Milky Way, 210{deg}&lt;l&lt;360{deg} at |b|&lt;15{deg}. The survey includes redshifts for 951 galaxies, ~500 of which are new. Of these 951 galaxies, 462 are in the zone 5{deg}&lt;b&lt;15{deg} and 353 are in the zone -15{deg}&lt;b&lt;-5{deg}. Though the innermost region of the Milky Way (|b|=5{deg}) remains opaque except in the longitude near 240, the detected galaxies show a high degree of completeness (~70%) in the zones 5{deg}&lt;b&lt;15{deg} and -15{deg}&lt;b&lt;-5{deg}. The cone diagrams exhibiting the detailed distribution of IRAS galaxies in the region 210{deg}&lt;l&lt;360{deg}, |b|&lt;15{deg} shows two clusters in the Puppis region (l=240{deg}, b=-7{deg}, v=2400km/s; l=245{deg}, b=-5{deg}, v=7500km/s), the A3627 cluster (l=325{deg}, b=-7{deg}; v=4500km/s), the S4 cluster (l=280{deg}, b=7{deg}; v=5500km/s), and a possible void at l=245{deg}, v=3000km/s. The region 270{deg}&lt;l&lt;350{deg} is dominated by overdensity of galaxies representing the extension of the Hydra-Centaurus complex in the positive latitudes and the Pavo-Indus complex in the negative latitudes. A velocity histogram of galaxies in the GA region 290{deg}&lt;l&lt;350{deg}, |b|&lt;15{deg}. reveals a substantial overdensity of galaxies in the velocity range 2400-5000km/s. The centroid of this overdensity is located at 4000km/s. The broad increased density of galaxies seen in our data corresponds with the distant concentration seen at 4500km/s in the supergalactic plane survey that covers the same longitude range like ours in l, but a larger range in latitude b (-30{deg} to -10{deg} and +10{deg} to +45{deg}). This lends support to the idea that the overdensity extends all the way from the Centaurus-Hydra complex (l=302{deg}, b=+22{deg}) in the north to the major concentration of the Pavo-Indus supercluster (l=332{deg}, b=-24{deg}) in the south, through the Milky Way. We conclude that the peak of the overdensity responsible for the peculiar velocity field in the local region is possibly situated in the Milky Way itself.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521#1</TD>
            <TD>2011-09-14T18:46:23Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/521 [2]</TD>
            <TD>Galaxies redshifts, 210&lt;l&lt;360, |b|&lt;15 (Visvanathan+ 1996)</TD>
            <TD>We have carried out a redshift survey of an IRAS flux-limited (f_60_&gt;0.6) galaxy sample behind the southern Milky Way, 210{deg}&lt;l&lt;360{deg} at |b|&lt;15{deg}. The survey includes redshifts for 951 galaxies, ~500 of which are new. Of these 951 galaxies, 462 are in the zone 5{deg}&lt;b&lt;15{deg} and 353 are in the zone -15{deg}&lt;b&lt;-5{deg}. Though the innermost region of the Milky Way (|b|=5{deg}) remains opaque except in the longitude near 240, the detected galaxies show a high degree of completeness (~70%) in the zones 5{deg}&lt;b&lt;15{deg} and -15{deg}&lt;b&lt;-5{deg}. The cone diagrams exhibiting the detailed distribution of IRAS galaxies in the region 210{deg}&lt;l&lt;360{deg}, |b|&lt;15{deg} shows two clusters in the Puppis region (l=240{deg}, b=-7{deg}, v=2400km/s; l=245{deg}, b=-5{deg}, v=7500km/s), the A3627 cluster (l=325{deg}, b=-7{deg}; v=4500km/s), the S4 cluster (l=280{deg}, b=7{deg}; v=5500km/s), and a possible void at l=245{deg}, v=3000km/s. The region 270{deg}&lt;l&lt;350{deg} is dominated by overdensity of galaxies representing the extension of the Hydra-Centaurus complex in the positive latitudes and the Pavo-Indus complex in the negative latitudes. A velocity histogram of galaxies in the GA region 290{deg}&lt;l&lt;350{deg}, |b|&lt;15{deg}. reveals a substantial overdensity of galaxies in the velocity range 2400-5000km/s. The centroid of this overdensity is located at 4000km/s. The broad increased density of galaxies seen in our data corresponds with the distant concentration seen at 4500km/s in the supergalactic plane survey that covers the same longitude range like ours in l, but a larger range in latitude b (-30{deg} to -10{deg} and +10{deg} to +45{deg}). This lends support to the idea that the overdensity extends all the way from the Centaurus-Hydra complex (l=302{deg}, b=+22{deg}) in the north to the major concentration of the Pavo-Indus supercluster (l=332{deg}, b=-24{deg}) in the south, through the Milky Way. We conclude that the peak of the overdensity responsible for the peculiar velocity field in the local region is possibly situated in the Milky Way itself.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521#2</TD>
            <TD>2011-09-14T18:46:23Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/415/1013 [1]</TD>
            <TD>FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)</TD>
            <TD>We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington &amp; Scott 1965MmRAS..69..183P; Gower, Scott &amp; Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson &amp; Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn &amp; Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin &amp; Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013#1</TD>
            <TD>2012-04-22T15:04:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/415/1013</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/1013</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/415/1013 [2]</TD>
            <TD>FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)</TD>
            <TD>We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington &amp; Scott 1965MmRAS..69..183P; Gower, Scott &amp; Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson &amp; Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn &amp; Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin &amp; Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013#2</TD>
            <TD>2012-04-22T15:04:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/415/1013&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/1013</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/415/1013 [appena]</TD>
            <TD>FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)</TD>
            <TD>We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington &amp; Scott 1965MmRAS..69..183P; Gower, Scott &amp; Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson &amp; Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn &amp; Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin &amp; Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013#appena</TD>
            <TD>2012-04-22T15:04:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/415/1013&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/1013</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/211 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. IV. (Yee+ 1998)</TD>
            <TD>Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters, MS 1358.4+6245 (z=0.328) and MS 1008.1-1224 (z=0.306), are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a mosaic of three MOS fields in the north-south direction of a total area of approximately 23.3'x9.0' for MS 1358.4+6245 and a single field of 7.9'x9.0' for MS 1008.1-1224. Redshifts for 361 galaxies, primarily ranging in magnitude from r=20 to r=22, and Gunn r and g photometry for 3015 galaxies to r=24mag were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/211#1</TD>
            <TD>2011-09-14T18:48:06Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/211 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. IV. (Yee+ 1998)</TD>
            <TD>Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters, MS 1358.4+6245 (z=0.328) and MS 1008.1-1224 (z=0.306), are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a mosaic of three MOS fields in the north-south direction of a total area of approximately 23.3'x9.0' for MS 1358.4+6245 and a single field of 7.9'x9.0' for MS 1008.1-1224. Redshifts for 361 galaxies, primarily ranging in magnitude from r=20 to r=22, and Gunn r and g photometry for 3015 galaxies to r=24mag were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/211#2</TD>
            <TD>2011-09-14T18:48:06Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/116/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/211</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/415/1013 [1]</TD>
            <TD>FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)</TD>
            <TD>We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington &amp; Scott 1965MmRAS..69..183P; Gower, Scott &amp; Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson &amp; Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn &amp; Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin &amp; Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013#1</TD>
            <TD>2012-04-22T15:04:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/415/1013</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/1013</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/415/1013 [2]</TD>
            <TD>FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)</TD>
            <TD>We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington &amp; Scott 1965MmRAS..69..183P; Gower, Scott &amp; Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson &amp; Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn &amp; Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin &amp; Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013#2</TD>
            <TD>2012-04-22T15:04:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/415/1013&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/1013</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/415/1013 [appena]</TD>
            <TD>FR II radio galaxies in SDSS (Koziel-Wierzbowska+, 2011)</TD>
            <TD>We limited our search to radio sources present in the Cambridge Catalogues of Radio Sources: * 3C (Edge et al. 1959MmRAS..68...37E, Bennett 1962MmRAS..68..163B, Cat. VIII/1); * 4C (Pilkington &amp; Scott 1965MmRAS..69..183P; Gower, Scott &amp; Wills 1967MmRAS..71...49G, Cat. VIII/4); * 5C (Pearson 1975, Cat. J/MNRAS/171/475; Pearson &amp; Kus 1978, J/MNRAS/182/273; Benn et al. 1982, J/MNRAS/200/747; Benn &amp; Kenderdine 1991MNRAS.251..253B, Cat. VIII/30; Benn 1995, Cat. J/MNRAS/272/699); * 6C (Baldwin et al. 1985MNRAS.217..717B, Cat. VIII/18; Hales, Baldwin &amp; Warner 1988MNRAS.234..919H, Cat. VIII/21, 1993MNRAS.263...25H, Cat. VIII/25; Hales et al. 1990MNRAS.246..256H, Cat. VIII/22, 1991MNRAS.251...46H, Cat. VIII/23, 1993MNRAS.262.1057H, Cat. VIII/24); * 7C (Hales et al. 2007MNRAS.382.1639H, Cat. VIII/84); * 8C (Rees 1990MNRAS.244..233R, Hales et al. 1995MNRAS.274..447H, Cat. VIII/31) and * 9C (Waldram et al. 2003, Cat. J/MNRAS/342/915), and using the SDSS CrossID we cross-identified them with the sample of 926246 galaxies from the SDSS DR7 main galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013#appena</TD>
            <TD>2012-04-22T15:04:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/1013</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/415/1013&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/1013</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/211 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. IV. (Yee+ 1998)</TD>
            <TD>Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters, MS 1358.4+6245 (z=0.328) and MS 1008.1-1224 (z=0.306), are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a mosaic of three MOS fields in the north-south direction of a total area of approximately 23.3'x9.0' for MS 1358.4+6245 and a single field of 7.9'x9.0' for MS 1008.1-1224. Redshifts for 361 galaxies, primarily ranging in magnitude from r=20 to r=22, and Gunn r and g photometry for 3015 galaxies to r=24mag were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/211#1</TD>
            <TD>2011-09-14T18:48:06Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/211 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. IV. (Yee+ 1998)</TD>
            <TD>Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters, MS 1358.4+6245 (z=0.328) and MS 1008.1-1224 (z=0.306), are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a mosaic of three MOS fields in the north-south direction of a total area of approximately 23.3'x9.0' for MS 1358.4+6245 and a single field of 7.9'x9.0' for MS 1008.1-1224. Redshifts for 361 galaxies, primarily ranging in magnitude from r=20 to r=22, and Gunn r and g photometry for 3015 galaxies to r=24mag were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/211#2</TD>
            <TD>2011-09-14T18:48:06Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/116/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/211</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/23 [1]</TD>
            <TD>IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)</TD>
            <TD>The original galaxy cluster sample is from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al. 2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used the 2MASS archive and previous literature to determine the locations of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the GALEX object identifiers for each BCG detected and the Astronomical Observing Request (AOR) numbers from the Spitzer archive observations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23#1</TD>
            <TD>2012-04-29T16:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/23</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/23</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/23 [2]</TD>
            <TD>IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)</TD>
            <TD>The original galaxy cluster sample is from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al. 2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used the 2MASS archive and previous literature to determine the locations of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the GALEX object identifiers for each BCG detected and the Astronomical Observing Request (AOR) numbers from the Spitzer archive observations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23#2</TD>
            <TD>2012-04-29T16:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/23&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/23</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/23 [table2]</TD>
            <TD>IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)</TD>
            <TD>The original galaxy cluster sample is from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al. 2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used the 2MASS archive and previous literature to determine the locations of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the GALEX object identifiers for each BCG detected and the Astronomical Observing Request (AOR) numbers from the Spitzer archive observations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23#table2</TD>
            <TD>2012-04-29T16:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/23&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/23</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/23 [1]</TD>
            <TD>IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)</TD>
            <TD>The original galaxy cluster sample is from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al. 2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used the 2MASS archive and previous literature to determine the locations of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the GALEX object identifiers for each BCG detected and the Astronomical Observing Request (AOR) numbers from the Spitzer archive observations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23#1</TD>
            <TD>2012-04-29T16:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/23</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/23</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/23 [2]</TD>
            <TD>IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)</TD>
            <TD>The original galaxy cluster sample is from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al. 2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used the 2MASS archive and previous literature to determine the locations of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the GALEX object identifiers for each BCG detected and the Astronomical Observing Request (AOR) numbers from the Spitzer archive observations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23#2</TD>
            <TD>2012-04-29T16:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/23&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/23</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/23 [table2]</TD>
            <TD>IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)</TD>
            <TD>The original galaxy cluster sample is from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al. 2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used the 2MASS archive and previous literature to determine the locations of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the GALEX object identifiers for each BCG detected and the Astronomical Observing Request (AOR) numbers from the Spitzer archive observations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23#table2</TD>
            <TD>2012-04-29T16:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/23&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/23</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/115/1 [1]</TD>
            <TD>MX northern Abell cluster redshift survey (Slinglendy+ 1998)</TD>
            <TD>The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, &amp; Olowin catalogs (Cat. &lt;VII/110&gt;) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R&gt;=1 Abell cluster fields with m_10_&lt;=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1#1</TD>
            <TD>2011-09-14T18:48:30Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/115/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/115/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/115/1 [2]</TD>
            <TD>MX northern Abell cluster redshift survey (Slinglendy+ 1998)</TD>
            <TD>The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, &amp; Olowin catalogs (Cat. &lt;VII/110&gt;) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R&gt;=1 Abell cluster fields with m_10_&lt;=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1#2</TD>
            <TD>2011-09-14T18:48:30Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/115/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/115/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/115/1 [table2]</TD>
            <TD>MX northern Abell cluster redshift survey (Slinglendy+ 1998)</TD>
            <TD>The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, &amp; Olowin catalogs (Cat. &lt;VII/110&gt;) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R&gt;=1 Abell cluster fields with m_10_&lt;=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1#table2</TD>
            <TD>2011-09-14T18:48:30Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/115/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/115/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/23 [1]</TD>
            <TD>IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)</TD>
            <TD>The original galaxy cluster sample is from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al. 2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used the 2MASS archive and previous literature to determine the locations of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the GALEX object identifiers for each BCG detected and the Astronomical Observing Request (AOR) numbers from the Spitzer archive observations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23#1</TD>
            <TD>2012-04-29T16:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/23</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/23</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/23 [2]</TD>
            <TD>IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)</TD>
            <TD>The original galaxy cluster sample is from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al. 2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used the 2MASS archive and previous literature to determine the locations of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the GALEX object identifiers for each BCG detected and the Astronomical Observing Request (AOR) numbers from the Spitzer archive observations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23#2</TD>
            <TD>2012-04-29T16:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/23&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/23</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/23 [table2]</TD>
            <TD>IR and UV star formation in ACCEPT BCGs (Hoffer+, 2012)</TD>
            <TD>The original galaxy cluster sample is from the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) database (Cavagnolo et al. 2009, Cat. J/ApJS/182/12), which includes 239 galaxy clusters. We used the 2MASS archive and previous literature to determine the locations of the BCGs in these galaxy clusters (Table 2). Table 2 also gives the GALEX object identifiers for each BCG detected and the Astronomical Observing Request (AOR) numbers from the Spitzer archive observations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23#table2</TD>
            <TD>2012-04-29T16:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/23</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/23&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/23</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/192/6 [1]</TD>
            <TD>A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)</TD>
            <TD>The Local Volume galaxies that were targeted for GALEX imaging were mainly selected from the sample given in Kennicutt et al. (Paper I, 2008, Cat. J/ApJS/178/247). The ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009ApJS..183...67D), which has obtained HST ACS and WFPC2 imaging for a ~4Mpc volume-limited sample, contains about 20 low-luminosity and/or early-type galaxies that were not already included in Paper I, and GALEX data were also obtained for these objects. Observations of the 11HUGS GALEX Legacy program (GI1_047, GI4_095) galaxies have also been extended into the infrared using the Spitzer Space Telescope as part of the Local Volume Legacy survey (Dale et al. 2009ApJ...703..517D).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6#1</TD>
            <TD>2011-09-14T21:18:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/192/6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/192/6 [2]</TD>
            <TD>A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)</TD>
            <TD>The Local Volume galaxies that were targeted for GALEX imaging were mainly selected from the sample given in Kennicutt et al. (Paper I, 2008, Cat. J/ApJS/178/247). The ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009ApJS..183...67D), which has obtained HST ACS and WFPC2 imaging for a ~4Mpc volume-limited sample, contains about 20 low-luminosity and/or early-type galaxies that were not already included in Paper I, and GALEX data were also obtained for these objects. Observations of the 11HUGS GALEX Legacy program (GI1_047, GI4_095) galaxies have also been extended into the infrared using the Spitzer Space Telescope as part of the Local Volume Legacy survey (Dale et al. 2009ApJ...703..517D).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6#2</TD>
            <TD>2011-09-14T21:18:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/192/6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/6 [sample]</TD>
            <TD>A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)</TD>
            <TD>The Local Volume galaxies that were targeted for GALEX imaging were mainly selected from the sample given in Kennicutt et al. (Paper I, 2008, Cat. J/ApJS/178/247). The ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009ApJS..183...67D), which has obtained HST ACS and WFPC2 imaging for a ~4Mpc volume-limited sample, contains about 20 low-luminosity and/or early-type galaxies that were not already included in Paper I, and GALEX data were also obtained for these objects. Observations of the 11HUGS GALEX Legacy program (GI1_047, GI4_095) galaxies have also been extended into the infrared using the Spitzer Space Telescope as part of the Local Volume Legacy survey (Dale et al. 2009ApJ...703..517D).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6#sample</TD>
            <TD>2011-09-14T21:18:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/115/1 [1]</TD>
            <TD>MX northern Abell cluster redshift survey (Slinglendy+ 1998)</TD>
            <TD>The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, &amp; Olowin catalogs (Cat. &lt;VII/110&gt;) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R&gt;=1 Abell cluster fields with m_10_&lt;=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1#1</TD>
            <TD>2011-09-14T18:48:30Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/115/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/115/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/115/1 [2]</TD>
            <TD>MX northern Abell cluster redshift survey (Slinglendy+ 1998)</TD>
            <TD>The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, &amp; Olowin catalogs (Cat. &lt;VII/110&gt;) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R&gt;=1 Abell cluster fields with m_10_&lt;=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1#2</TD>
            <TD>2011-09-14T18:48:30Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/115/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/115/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/115/1 [table2]</TD>
            <TD>MX northern Abell cluster redshift survey (Slinglendy+ 1998)</TD>
            <TD>The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, &amp; Olowin catalogs (Cat. &lt;VII/110&gt;) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R&gt;=1 Abell cluster fields with m_10_&lt;=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1#table2</TD>
            <TD>2011-09-14T18:48:30Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/115/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/115/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/115/1 [1]</TD>
            <TD>MX northern Abell cluster redshift survey (Slinglendy+ 1998)</TD>
            <TD>The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, &amp; Olowin catalogs (Cat. &lt;VII/110&gt;) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R&gt;=1 Abell cluster fields with m_10_&lt;=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1#1</TD>
            <TD>2011-09-14T18:48:30Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/115/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/115/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/115/1 [2]</TD>
            <TD>MX northern Abell cluster redshift survey (Slinglendy+ 1998)</TD>
            <TD>The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, &amp; Olowin catalogs (Cat. &lt;VII/110&gt;) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R&gt;=1 Abell cluster fields with m_10_&lt;=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1#2</TD>
            <TD>2011-09-14T18:48:30Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/115/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/115/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/115/1 [table2]</TD>
            <TD>MX northern Abell cluster redshift survey (Slinglendy+ 1998)</TD>
            <TD>The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, &amp; Olowin catalogs (Cat. &lt;VII/110&gt;) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R&gt;=1 Abell cluster fields with m_10_&lt;=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1#table2</TD>
            <TD>2011-09-14T18:48:30Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/115/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/115/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/115/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/714/1096 [1]</TD>
            <TD>Galactic planetary nebulae (Stanghellini+, 2010)</TD>
            <TD>In this paper, we use the Magellanic Cloud-calibrated Galactic PN distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to examine the population of PNe in our Galaxy. We extend the Perinotto et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the abundances published more recently, and calculate the metallicity gradients for the different populations, and homogeneously classify the Galactic PN morphology for further insight on population selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096#1</TD>
            <TD>2012-06-10T14:22:44Z</TD>
            <TD>#Abundances#Stars#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/714/1096</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1096</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/714/1096 [2]</TD>
            <TD>Galactic planetary nebulae (Stanghellini+, 2010)</TD>
            <TD>In this paper, we use the Magellanic Cloud-calibrated Galactic PN distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to examine the population of PNe in our Galaxy. We extend the Perinotto et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the abundances published more recently, and calculate the metallicity gradients for the different populations, and homogeneously classify the Galactic PN morphology for further insight on population selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096#2</TD>
            <TD>2012-06-10T14:22:44Z</TD>
            <TD>#Abundances#Stars#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/714/1096&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1096</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/714/1096 [table1]</TD>
            <TD>Galactic planetary nebulae (Stanghellini+, 2010)</TD>
            <TD>In this paper, we use the Magellanic Cloud-calibrated Galactic PN distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to examine the population of PNe in our Galaxy. We extend the Perinotto et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the abundances published more recently, and calculate the metallicity gradients for the different populations, and homogeneously classify the Galactic PN morphology for further insight on population selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096#table1</TD>
            <TD>2012-06-10T14:22:44Z</TD>
            <TD>#Abundances#Stars#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/714/1096&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1096</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>HST.M51</TD>
            <TD>HST ACS mosaic images of M51</TD>
            <TD>In January 2005, the Hubble Heritage Team obtained a large 4-color mosaic image of the Whirlpool Galaxy NGC 5194 (M51), and its companion NGC 5195, with the Advanced Camera for Surveys (ACS) onboard the Hubble Space Telescope (HST observing program 10452, PI: Steven V. W. Beckwith). A six-pointing ACS WFC mosaic of the galaxy pair M51 was obtained in four filters: B, V, I, and H-alpha.</TD>
            <TD>MAST</TD>
            <TD>#Optical#</TD>
            <TD>ivo://mast.stsci/siap/hst.m51#1</TD>
            <TD>2012-02-02T21:01:19Z</TD>
            <TD>#Optical Astronomy#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0500000007450581</TD>
            <TD>1.0</TD>
            <TD>ivo://mast.stsci/siap/hst.m51</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://archive.stsci.edu/siap/search.php?id=m51&amp;</TD>
            <TD />
            <TD>100</TD>
            <TD />
            <TD>http://archive.stsci.edu/prepds/m51/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/714/1096 [1]</TD>
            <TD>Galactic planetary nebulae (Stanghellini+, 2010)</TD>
            <TD>In this paper, we use the Magellanic Cloud-calibrated Galactic PN distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to examine the population of PNe in our Galaxy. We extend the Perinotto et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the abundances published more recently, and calculate the metallicity gradients for the different populations, and homogeneously classify the Galactic PN morphology for further insight on population selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096#1</TD>
            <TD>2012-06-10T14:22:44Z</TD>
            <TD>#Abundances#Stars#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/714/1096</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1096</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/714/1096 [2]</TD>
            <TD>Galactic planetary nebulae (Stanghellini+, 2010)</TD>
            <TD>In this paper, we use the Magellanic Cloud-calibrated Galactic PN distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to examine the population of PNe in our Galaxy. We extend the Perinotto et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the abundances published more recently, and calculate the metallicity gradients for the different populations, and homogeneously classify the Galactic PN morphology for further insight on population selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096#2</TD>
            <TD>2012-06-10T14:22:44Z</TD>
            <TD>#Abundances#Stars#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/714/1096&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1096</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/714/1096 [table1]</TD>
            <TD>Galactic planetary nebulae (Stanghellini+, 2010)</TD>
            <TD>In this paper, we use the Magellanic Cloud-calibrated Galactic PN distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to examine the population of PNe in our Galaxy. We extend the Perinotto et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the abundances published more recently, and calculate the metallicity gradients for the different populations, and homogeneously classify the Galactic PN morphology for further insight on population selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096#table1</TD>
            <TD>2012-06-10T14:22:44Z</TD>
            <TD>#Abundances#Stars#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/714/1096&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1096</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/714/1096 [1]</TD>
            <TD>Galactic planetary nebulae (Stanghellini+, 2010)</TD>
            <TD>In this paper, we use the Magellanic Cloud-calibrated Galactic PN distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to examine the population of PNe in our Galaxy. We extend the Perinotto et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the abundances published more recently, and calculate the metallicity gradients for the different populations, and homogeneously classify the Galactic PN morphology for further insight on population selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096#1</TD>
            <TD>2012-06-10T14:22:44Z</TD>
            <TD>#Abundances#Stars#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/714/1096</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1096</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/714/1096 [2]</TD>
            <TD>Galactic planetary nebulae (Stanghellini+, 2010)</TD>
            <TD>In this paper, we use the Magellanic Cloud-calibrated Galactic PN distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to examine the population of PNe in our Galaxy. We extend the Perinotto et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the abundances published more recently, and calculate the metallicity gradients for the different populations, and homogeneously classify the Galactic PN morphology for further insight on population selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096#2</TD>
            <TD>2012-06-10T14:22:44Z</TD>
            <TD>#Abundances#Stars#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/714/1096&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1096</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/714/1096 [table1]</TD>
            <TD>Galactic planetary nebulae (Stanghellini+, 2010)</TD>
            <TD>In this paper, we use the Magellanic Cloud-calibrated Galactic PN distance scale from Stanghellini et al. 2008, Cat. J/ApJ/689/194 to examine the population of PNe in our Galaxy. We extend the Perinotto et al., 2004, Cat. J/MNRAS/349/793, abundance database with all the abundances published more recently, and calculate the metallicity gradients for the different populations, and homogeneously classify the Galactic PN morphology for further insight on population selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096#table1</TD>
            <TD>2012-06-10T14:22:44Z</TD>
            <TD>#Abundances#Stars#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1096</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/714/1096&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1096</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1051 [1]</TD>
            <TD>Carbon-enhanced metal-poor stars in the Galaxy (Placco+, 2010)</TD>
            <TD>We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051#1</TD>
            <TD>2012-06-24T16:27:21Z</TD>
            <TD>#Abundances#Stars#Stars:peculiar#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1051</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1051</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1051 [2]</TD>
            <TD>Carbon-enhanced metal-poor stars in the Galaxy (Placco+, 2010)</TD>
            <TD>We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051#2</TD>
            <TD>2012-06-24T16:27:21Z</TD>
            <TD>#Abundances#Stars#Stars:peculiar#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1051&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1051</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1051 [CEMPstars]</TD>
            <TD>Carbon-enhanced metal-poor stars in the Galaxy (Placco+, 2010)</TD>
            <TD>We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051#CEMPstars</TD>
            <TD>2012-06-24T16:27:21Z</TD>
            <TD>#Abundances#Stars#Stars:peculiar#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1051&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1051</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1051 [1]</TD>
            <TD>Carbon-enhanced metal-poor stars in the Galaxy (Placco+, 2010)</TD>
            <TD>We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051#1</TD>
            <TD>2012-06-24T16:27:21Z</TD>
            <TD>#Abundances#Stars#Stars:peculiar#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1051</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1051</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1051 [2]</TD>
            <TD>Carbon-enhanced metal-poor stars in the Galaxy (Placco+, 2010)</TD>
            <TD>We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051#2</TD>
            <TD>2012-06-24T16:27:21Z</TD>
            <TD>#Abundances#Stars#Stars:peculiar#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1051&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1051</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1051 [CEMPstars]</TD>
            <TD>Carbon-enhanced metal-poor stars in the Galaxy (Placco+, 2010)</TD>
            <TD>We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051#CEMPstars</TD>
            <TD>2012-06-24T16:27:21Z</TD>
            <TD>#Abundances#Stars#Stars:peculiar#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1051&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1051</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1051 [1]</TD>
            <TD>Carbon-enhanced metal-poor stars in the Galaxy (Placco+, 2010)</TD>
            <TD>We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051#1</TD>
            <TD>2012-06-24T16:27:21Z</TD>
            <TD>#Abundances#Stars#Stars:peculiar#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1051</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1051</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1051 [2]</TD>
            <TD>Carbon-enhanced metal-poor stars in the Galaxy (Placco+, 2010)</TD>
            <TD>We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051#2</TD>
            <TD>2012-06-24T16:27:21Z</TD>
            <TD>#Abundances#Stars#Stars:peculiar#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1051&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1051</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1051 [CEMPstars]</TD>
            <TD>Carbon-enhanced metal-poor stars in the Galaxy (Placco+, 2010)</TD>
            <TD>We have developed a new procedure to search for carbon-enhanced metal-poor (CEMP) stars from the Hamburg/ESO (HES) prism-survey plates. This method employs an extended line index for the CH G band, which we demonstrate to have superior performance when compared to the narrower G-band index formerly employed to estimate G-band strengths for these spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051#CEMPstars</TD>
            <TD>2012-06-24T16:27:21Z</TD>
            <TD>#Abundances#Stars#Stars:peculiar#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1051</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1051&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1051</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1212 [1]</TD>
            <TD>SDSS photometry of interacting galaxies (Smith+, 2010)</TD>
            <TD>We have used the Galaxy Evolution Explorer (GALEX) ultraviolet telescope to study stellar populations and star formation morphology in a well-defined sample of 42 nearby optically selected pre-merger interacting galaxy pairs. Galaxy interactions were likely far more common in the early universe than in the present; thus our study provides a nearby well-resolved comparison sample for high-redshift studies. We have combined the GALEX near-ultraviolet (NUV) and far-ultraviolet images with broadband optical maps from the Sloan Digitized Sky Survey to investigate the ages and extinctions of the tidal features and the disks.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212#1</TD>
            <TD>2012-06-24T23:13:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1212</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1212</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1212 [2]</TD>
            <TD>SDSS photometry of interacting galaxies (Smith+, 2010)</TD>
            <TD>We have used the Galaxy Evolution Explorer (GALEX) ultraviolet telescope to study stellar populations and star formation morphology in a well-defined sample of 42 nearby optically selected pre-merger interacting galaxy pairs. Galaxy interactions were likely far more common in the early universe than in the present; thus our study provides a nearby well-resolved comparison sample for high-redshift studies. We have combined the GALEX near-ultraviolet (NUV) and far-ultraviolet images with broadband optical maps from the Sloan Digitized Sky Survey to investigate the ages and extinctions of the tidal features and the disks.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212#2</TD>
            <TD>2012-06-24T23:13:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1212&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1212</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1212 [table3]</TD>
            <TD>SDSS photometry of interacting galaxies (Smith+, 2010)</TD>
            <TD>We have used the Galaxy Evolution Explorer (GALEX) ultraviolet telescope to study stellar populations and star formation morphology in a well-defined sample of 42 nearby optically selected pre-merger interacting galaxy pairs. Galaxy interactions were likely far more common in the early universe than in the present; thus our study provides a nearby well-resolved comparison sample for high-redshift studies. We have combined the GALEX near-ultraviolet (NUV) and far-ultraviolet images with broadband optical maps from the Sloan Digitized Sky Survey to investigate the ages and extinctions of the tidal features and the disks.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212#table3</TD>
            <TD>2012-06-24T23:13:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1212&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1212</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1212 [1]</TD>
            <TD>SDSS photometry of interacting galaxies (Smith+, 2010)</TD>
            <TD>We have used the Galaxy Evolution Explorer (GALEX) ultraviolet telescope to study stellar populations and star formation morphology in a well-defined sample of 42 nearby optically selected pre-merger interacting galaxy pairs. Galaxy interactions were likely far more common in the early universe than in the present; thus our study provides a nearby well-resolved comparison sample for high-redshift studies. We have combined the GALEX near-ultraviolet (NUV) and far-ultraviolet images with broadband optical maps from the Sloan Digitized Sky Survey to investigate the ages and extinctions of the tidal features and the disks.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212#1</TD>
            <TD>2012-06-24T23:13:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1212</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1212</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1212 [2]</TD>
            <TD>SDSS photometry of interacting galaxies (Smith+, 2010)</TD>
            <TD>We have used the Galaxy Evolution Explorer (GALEX) ultraviolet telescope to study stellar populations and star formation morphology in a well-defined sample of 42 nearby optically selected pre-merger interacting galaxy pairs. Galaxy interactions were likely far more common in the early universe than in the present; thus our study provides a nearby well-resolved comparison sample for high-redshift studies. We have combined the GALEX near-ultraviolet (NUV) and far-ultraviolet images with broadband optical maps from the Sloan Digitized Sky Survey to investigate the ages and extinctions of the tidal features and the disks.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212#2</TD>
            <TD>2012-06-24T23:13:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1212&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1212</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1212 [table3]</TD>
            <TD>SDSS photometry of interacting galaxies (Smith+, 2010)</TD>
            <TD>We have used the Galaxy Evolution Explorer (GALEX) ultraviolet telescope to study stellar populations and star formation morphology in a well-defined sample of 42 nearby optically selected pre-merger interacting galaxy pairs. Galaxy interactions were likely far more common in the early universe than in the present; thus our study provides a nearby well-resolved comparison sample for high-redshift studies. We have combined the GALEX near-ultraviolet (NUV) and far-ultraviolet images with broadband optical maps from the Sloan Digitized Sky Survey to investigate the ages and extinctions of the tidal features and the disks.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212#table3</TD>
            <TD>2012-06-24T23:13:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1212&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1212</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1212 [1]</TD>
            <TD>SDSS photometry of interacting galaxies (Smith+, 2010)</TD>
            <TD>We have used the Galaxy Evolution Explorer (GALEX) ultraviolet telescope to study stellar populations and star formation morphology in a well-defined sample of 42 nearby optically selected pre-merger interacting galaxy pairs. Galaxy interactions were likely far more common in the early universe than in the present; thus our study provides a nearby well-resolved comparison sample for high-redshift studies. We have combined the GALEX near-ultraviolet (NUV) and far-ultraviolet images with broadband optical maps from the Sloan Digitized Sky Survey to investigate the ages and extinctions of the tidal features and the disks.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212#1</TD>
            <TD>2012-06-24T23:13:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1212</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1212</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1212 [2]</TD>
            <TD>SDSS photometry of interacting galaxies (Smith+, 2010)</TD>
            <TD>We have used the Galaxy Evolution Explorer (GALEX) ultraviolet telescope to study stellar populations and star formation morphology in a well-defined sample of 42 nearby optically selected pre-merger interacting galaxy pairs. Galaxy interactions were likely far more common in the early universe than in the present; thus our study provides a nearby well-resolved comparison sample for high-redshift studies. We have combined the GALEX near-ultraviolet (NUV) and far-ultraviolet images with broadband optical maps from the Sloan Digitized Sky Survey to investigate the ages and extinctions of the tidal features and the disks.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212#2</TD>
            <TD>2012-06-24T23:13:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1212&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1212</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1212 [table3]</TD>
            <TD>SDSS photometry of interacting galaxies (Smith+, 2010)</TD>
            <TD>We have used the Galaxy Evolution Explorer (GALEX) ultraviolet telescope to study stellar populations and star formation morphology in a well-defined sample of 42 nearby optically selected pre-merger interacting galaxy pairs. Galaxy interactions were likely far more common in the early universe than in the present; thus our study provides a nearby well-resolved comparison sample for high-redshift studies. We have combined the GALEX near-ultraviolet (NUV) and far-ultraviolet images with broadband optical maps from the Sloan Digitized Sky Survey to investigate the ages and extinctions of the tidal features and the disks.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212#table3</TD>
            <TD>2012-06-24T23:13:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1212</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1212&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1212</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Spectra</TD>
            <TD>VVDS_F02_DEEP</TD>
            <TD>VVDS-F02 DEEP spectra</TD>
            <TD>This SSA (v1.0 prototype) service allows to access the VVDS-F02-DEEP spectra available at http://cencosw.oamp.fr in a VO compliant format. It comprises spectra for 8980 objects from the VVDS-F02 Deep field with IAB between 17.5 and 24, and with spectroscopic redshift between 0 and 5. The observations and data processing have been conducted by the French-Italian team of the VIMOS VLT Deep Survey (VVDS).</TD>
            <TD>INAF-IASF Milano</TD>
            <TD>#Optical#</TD>
            <TD>ivo://obelix.lambrate.inaf.it/vodb/ssa/VVDS_F02_DEEP#1</TD>
            <TD>2008-04-15T20:18:49Z</TD>
            <TD>#Galaxy#Spectroscopy#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>v1.0</TD>
            <TD>ivo://obelix.lambrate.inaf.it/vodb/ssa/VVDS_F02_DEEP</TD>
            <TD>SimpleSpectralAccess</TD>
            <TD>ivo://ivoa.net/std/SSA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD>0.5</TD>
            <TD>std</TD>
            <TD>http://obelix.lambrate.inaf.it/vodb/SSA?CAT=VVDS_F02_DEEP&amp;</TD>
            <TD>360.0</TD>
            <TD>10000</TD>
            <TD />
            <TD>http://cencosw.oamp.fr</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/339/913 [1]</TD>
            <TD>Two distant massive clusters of galaxies (Edge+, 2003)</TD>
            <TD>We discuss the radio, optical, and X-ray properties of two newly discovered, very X-ray luminous, distant clusters of galaxies. Both systems were noted as cluster candidates in a cross-correlation of data from the WENSS (&lt;VIII/162&gt;) radio survey and the ROSAT All-Sky Survey (&lt;IX/10&gt;). Follow-up observations performed by us and the Massive Cluster Survey (MACS) team confirmed both sources as distant galaxy clusters. The first cluster, MACS J0717.5+3745 at a redshift of z=0.5548, contains a very extended, steep-spectrum radio source offset from the cluster core, making it the most distant radio relic known. The second cluster, MACS J1621.3+3810 at z=0.465, is a strong cooling flow with a relatively weak central radio source. We present results from ROSAT High-Resolution Imager (HRI, Cat. &lt;IX/28&gt;) observations of both clusters as well as from optical imaging and VLA radio interferometry observations. Our discoveries demonstrate that distant clusters can be efficiently identified in a relatively shallow X-ray survey, that radio/X-ray selection is efficient, and that both cooling flow and non-cooling flow clusters are selected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913#1</TD>
            <TD>2011-09-14T19:47:28Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/339/913</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/913</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/339/913 [2]</TD>
            <TD>Two distant massive clusters of galaxies (Edge+, 2003)</TD>
            <TD>We discuss the radio, optical, and X-ray properties of two newly discovered, very X-ray luminous, distant clusters of galaxies. Both systems were noted as cluster candidates in a cross-correlation of data from the WENSS (&lt;VIII/162&gt;) radio survey and the ROSAT All-Sky Survey (&lt;IX/10&gt;). Follow-up observations performed by us and the Massive Cluster Survey (MACS) team confirmed both sources as distant galaxy clusters. The first cluster, MACS J0717.5+3745 at a redshift of z=0.5548, contains a very extended, steep-spectrum radio source offset from the cluster core, making it the most distant radio relic known. The second cluster, MACS J1621.3+3810 at z=0.465, is a strong cooling flow with a relatively weak central radio source. We present results from ROSAT High-Resolution Imager (HRI, Cat. &lt;IX/28&gt;) observations of both clusters as well as from optical imaging and VLA radio interferometry observations. Our discoveries demonstrate that distant clusters can be efficiently identified in a relatively shallow X-ray survey, that radio/X-ray selection is efficient, and that both cooling flow and non-cooling flow clusters are selected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913#2</TD>
            <TD>2011-09-14T19:47:28Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/339/913&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/913</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/339/913 [table2]</TD>
            <TD>Two distant massive clusters of galaxies (Edge+, 2003)</TD>
            <TD>We discuss the radio, optical, and X-ray properties of two newly discovered, very X-ray luminous, distant clusters of galaxies. Both systems were noted as cluster candidates in a cross-correlation of data from the WENSS (&lt;VIII/162&gt;) radio survey and the ROSAT All-Sky Survey (&lt;IX/10&gt;). Follow-up observations performed by us and the Massive Cluster Survey (MACS) team confirmed both sources as distant galaxy clusters. The first cluster, MACS J0717.5+3745 at a redshift of z=0.5548, contains a very extended, steep-spectrum radio source offset from the cluster core, making it the most distant radio relic known. The second cluster, MACS J1621.3+3810 at z=0.465, is a strong cooling flow with a relatively weak central radio source. We present results from ROSAT High-Resolution Imager (HRI, Cat. &lt;IX/28&gt;) observations of both clusters as well as from optical imaging and VLA radio interferometry observations. Our discoveries demonstrate that distant clusters can be efficiently identified in a relatively shallow X-ray survey, that radio/X-ray selection is efficient, and that both cooling flow and non-cooling flow clusters are selected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913#table2</TD>
            <TD>2011-09-14T19:47:28Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/339/913&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/913</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/339/913 [1]</TD>
            <TD>Two distant massive clusters of galaxies (Edge+, 2003)</TD>
            <TD>We discuss the radio, optical, and X-ray properties of two newly discovered, very X-ray luminous, distant clusters of galaxies. Both systems were noted as cluster candidates in a cross-correlation of data from the WENSS (&lt;VIII/162&gt;) radio survey and the ROSAT All-Sky Survey (&lt;IX/10&gt;). Follow-up observations performed by us and the Massive Cluster Survey (MACS) team confirmed both sources as distant galaxy clusters. The first cluster, MACS J0717.5+3745 at a redshift of z=0.5548, contains a very extended, steep-spectrum radio source offset from the cluster core, making it the most distant radio relic known. The second cluster, MACS J1621.3+3810 at z=0.465, is a strong cooling flow with a relatively weak central radio source. We present results from ROSAT High-Resolution Imager (HRI, Cat. &lt;IX/28&gt;) observations of both clusters as well as from optical imaging and VLA radio interferometry observations. Our discoveries demonstrate that distant clusters can be efficiently identified in a relatively shallow X-ray survey, that radio/X-ray selection is efficient, and that both cooling flow and non-cooling flow clusters are selected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913#1</TD>
            <TD>2011-09-14T19:47:28Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/339/913</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/913</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/339/913 [2]</TD>
            <TD>Two distant massive clusters of galaxies (Edge+, 2003)</TD>
            <TD>We discuss the radio, optical, and X-ray properties of two newly discovered, very X-ray luminous, distant clusters of galaxies. Both systems were noted as cluster candidates in a cross-correlation of data from the WENSS (&lt;VIII/162&gt;) radio survey and the ROSAT All-Sky Survey (&lt;IX/10&gt;). Follow-up observations performed by us and the Massive Cluster Survey (MACS) team confirmed both sources as distant galaxy clusters. The first cluster, MACS J0717.5+3745 at a redshift of z=0.5548, contains a very extended, steep-spectrum radio source offset from the cluster core, making it the most distant radio relic known. The second cluster, MACS J1621.3+3810 at z=0.465, is a strong cooling flow with a relatively weak central radio source. We present results from ROSAT High-Resolution Imager (HRI, Cat. &lt;IX/28&gt;) observations of both clusters as well as from optical imaging and VLA radio interferometry observations. Our discoveries demonstrate that distant clusters can be efficiently identified in a relatively shallow X-ray survey, that radio/X-ray selection is efficient, and that both cooling flow and non-cooling flow clusters are selected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913#2</TD>
            <TD>2011-09-14T19:47:28Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/339/913&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/913</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/339/913 [table2]</TD>
            <TD>Two distant massive clusters of galaxies (Edge+, 2003)</TD>
            <TD>We discuss the radio, optical, and X-ray properties of two newly discovered, very X-ray luminous, distant clusters of galaxies. Both systems were noted as cluster candidates in a cross-correlation of data from the WENSS (&lt;VIII/162&gt;) radio survey and the ROSAT All-Sky Survey (&lt;IX/10&gt;). Follow-up observations performed by us and the Massive Cluster Survey (MACS) team confirmed both sources as distant galaxy clusters. The first cluster, MACS J0717.5+3745 at a redshift of z=0.5548, contains a very extended, steep-spectrum radio source offset from the cluster core, making it the most distant radio relic known. The second cluster, MACS J1621.3+3810 at z=0.465, is a strong cooling flow with a relatively weak central radio source. We present results from ROSAT High-Resolution Imager (HRI, Cat. &lt;IX/28&gt;) observations of both clusters as well as from optical imaging and VLA radio interferometry observations. Our discoveries demonstrate that distant clusters can be efficiently identified in a relatively shallow X-ray survey, that radio/X-ray selection is efficient, and that both cooling flow and non-cooling flow clusters are selected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913#table2</TD>
            <TD>2011-09-14T19:47:28Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/339/913&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/913</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/339/913 [1]</TD>
            <TD>Two distant massive clusters of galaxies (Edge+, 2003)</TD>
            <TD>We discuss the radio, optical, and X-ray properties of two newly discovered, very X-ray luminous, distant clusters of galaxies. Both systems were noted as cluster candidates in a cross-correlation of data from the WENSS (&lt;VIII/162&gt;) radio survey and the ROSAT All-Sky Survey (&lt;IX/10&gt;). Follow-up observations performed by us and the Massive Cluster Survey (MACS) team confirmed both sources as distant galaxy clusters. The first cluster, MACS J0717.5+3745 at a redshift of z=0.5548, contains a very extended, steep-spectrum radio source offset from the cluster core, making it the most distant radio relic known. The second cluster, MACS J1621.3+3810 at z=0.465, is a strong cooling flow with a relatively weak central radio source. We present results from ROSAT High-Resolution Imager (HRI, Cat. &lt;IX/28&gt;) observations of both clusters as well as from optical imaging and VLA radio interferometry observations. Our discoveries demonstrate that distant clusters can be efficiently identified in a relatively shallow X-ray survey, that radio/X-ray selection is efficient, and that both cooling flow and non-cooling flow clusters are selected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913#1</TD>
            <TD>2011-09-14T19:47:28Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/339/913</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/913</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/339/913 [2]</TD>
            <TD>Two distant massive clusters of galaxies (Edge+, 2003)</TD>
            <TD>We discuss the radio, optical, and X-ray properties of two newly discovered, very X-ray luminous, distant clusters of galaxies. Both systems were noted as cluster candidates in a cross-correlation of data from the WENSS (&lt;VIII/162&gt;) radio survey and the ROSAT All-Sky Survey (&lt;IX/10&gt;). Follow-up observations performed by us and the Massive Cluster Survey (MACS) team confirmed both sources as distant galaxy clusters. The first cluster, MACS J0717.5+3745 at a redshift of z=0.5548, contains a very extended, steep-spectrum radio source offset from the cluster core, making it the most distant radio relic known. The second cluster, MACS J1621.3+3810 at z=0.465, is a strong cooling flow with a relatively weak central radio source. We present results from ROSAT High-Resolution Imager (HRI, Cat. &lt;IX/28&gt;) observations of both clusters as well as from optical imaging and VLA radio interferometry observations. Our discoveries demonstrate that distant clusters can be efficiently identified in a relatively shallow X-ray survey, that radio/X-ray selection is efficient, and that both cooling flow and non-cooling flow clusters are selected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913#2</TD>
            <TD>2011-09-14T19:47:28Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/339/913&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/913</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/339/913 [table2]</TD>
            <TD>Two distant massive clusters of galaxies (Edge+, 2003)</TD>
            <TD>We discuss the radio, optical, and X-ray properties of two newly discovered, very X-ray luminous, distant clusters of galaxies. Both systems were noted as cluster candidates in a cross-correlation of data from the WENSS (&lt;VIII/162&gt;) radio survey and the ROSAT All-Sky Survey (&lt;IX/10&gt;). Follow-up observations performed by us and the Massive Cluster Survey (MACS) team confirmed both sources as distant galaxy clusters. The first cluster, MACS J0717.5+3745 at a redshift of z=0.5548, contains a very extended, steep-spectrum radio source offset from the cluster core, making it the most distant radio relic known. The second cluster, MACS J1621.3+3810 at z=0.465, is a strong cooling flow with a relatively weak central radio source. We present results from ROSAT High-Resolution Imager (HRI, Cat. &lt;IX/28&gt;) observations of both clusters as well as from optical imaging and VLA radio interferometry observations. Our discoveries demonstrate that distant clusters can be efficiently identified in a relatively shallow X-ray survey, that radio/X-ray selection is efficient, and that both cooling flow and non-cooling flow clusters are selected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913#table2</TD>
            <TD>2011-09-14T19:47:28Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/913</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/339/913&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/913</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [1]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#1</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VHS DR1 [2]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#2</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/DirectCone?DSACAT=VHS_DR1&amp;DSATAB=vhsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [3]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#3</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VHS DR1 [4]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#4</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [5]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#5</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [6]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#6</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [7]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#7</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [8]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#8</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [9]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#9</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [10]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#10</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VHS DR1 [11]</TD>
            <TD>VHS DR1 - VISTA Hemisphere Survey Data Release 1</TD>
            <TD>The VHS will image the entire ~20 000 square degrees of the Southern Sky, with the exception of the areas already covered by the VIKING and VVV surveys, in J and Ks. The resulting data will be about 4 magnitudes deeper than 2MASS and DENIS. The 5000 square degrees covered by the Dark Energy Survey (DES), another imaging survey scheduled to begin in 2010 at the CTIO 4 metre Blanco telescope, will also be observed in H-band. The area around both of the Galactic Caps will be observed in Y- and H- band as well to be combined with the data from the VST ATLAS survey. The main science drivers of the VHS include: examining low mass and nearby stars, studying the merger history of the Galaxy, measuring the properties of Dark Energy through the examination of large-scale structure to a redshift of ~1, and searches for high redshift quasars.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa#11</TD>
            <TD>2012-07-17T15:37:19Z</TD>
            <TD>#Stars,Survey,Galaxy, low mass stars, dark energy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vhsDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vhsDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.ast.cam.ac.uk/~rgm/vhs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/330/547 [1]</TD>
            <TD>Local galaxy ages and metallicities (Terlevich+, 2002)</TD>
            <TD>We have assembled a catalogue of relative ages, metallicities and abundance ratios for about 150 local galaxies in field, group and cluster environments. The galaxies span morphological types from cD and ellipticals, to late-type spirals. Ages and metallicities were estimated from high-quality published spectral line indices using Worthey &amp; Ottaviani (1997, Cat. &lt;J/ApJS/111/377&gt;) single stellar population evolutionary models. The identification of galaxy age as a fourth parameter in the fundamental plane (Forbes, Ponman &amp; Brown, 1998ApJ...508L..43F) is confirmed by our larger sample of ages. We investigate trends between age and metallicity, and with other physical parameters of the galaxies, such as ellipticity, luminosity and kinematic anisotropy. We demonstrate the existence of a galaxy age-metallicity relation similar to that seen for local galactic disc stars, whereby young galaxies have high metallicity, while old galaxies span a large range in metallicities. We also investigate the influence of environment and morphology on the galaxy age and metallicity, especially the predictions made by semi-analytic hierarchical clustering models (HCM). We confirm that non-cluster ellipticals are indeed younger on average than cluster ellipticals as predicted by the HCM models. However we also find a trend for the more luminous galaxies to have a higher [Mg/Fe] ratio than the lower luminosity galaxies, which is opposite to the expectation from HCM models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547#1</TD>
            <TD>2011-09-14T19:47:42Z</TD>
            <TD>#Abundances#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/330/547</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/547</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/330/547 [2]</TD>
            <TD>Local galaxy ages and metallicities (Terlevich+, 2002)</TD>
            <TD>We have assembled a catalogue of relative ages, metallicities and abundance ratios for about 150 local galaxies in field, group and cluster environments. The galaxies span morphological types from cD and ellipticals, to late-type spirals. Ages and metallicities were estimated from high-quality published spectral line indices using Worthey &amp; Ottaviani (1997, Cat. &lt;J/ApJS/111/377&gt;) single stellar population evolutionary models. The identification of galaxy age as a fourth parameter in the fundamental plane (Forbes, Ponman &amp; Brown, 1998ApJ...508L..43F) is confirmed by our larger sample of ages. We investigate trends between age and metallicity, and with other physical parameters of the galaxies, such as ellipticity, luminosity and kinematic anisotropy. We demonstrate the existence of a galaxy age-metallicity relation similar to that seen for local galactic disc stars, whereby young galaxies have high metallicity, while old galaxies span a large range in metallicities. We also investigate the influence of environment and morphology on the galaxy age and metallicity, especially the predictions made by semi-analytic hierarchical clustering models (HCM). We confirm that non-cluster ellipticals are indeed younger on average than cluster ellipticals as predicted by the HCM models. However we also find a trend for the more luminous galaxies to have a higher [Mg/Fe] ratio than the lower luminosity galaxies, which is opposite to the expectation from HCM models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547#2</TD>
            <TD>2011-09-14T19:47:42Z</TD>
            <TD>#Abundances#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/330/547&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/547</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/330/547 [galaxy]</TD>
            <TD>Local galaxy ages and metallicities (Terlevich+, 2002)</TD>
            <TD>We have assembled a catalogue of relative ages, metallicities and abundance ratios for about 150 local galaxies in field, group and cluster environments. The galaxies span morphological types from cD and ellipticals, to late-type spirals. Ages and metallicities were estimated from high-quality published spectral line indices using Worthey &amp; Ottaviani (1997, Cat. &lt;J/ApJS/111/377&gt;) single stellar population evolutionary models. The identification of galaxy age as a fourth parameter in the fundamental plane (Forbes, Ponman &amp; Brown, 1998ApJ...508L..43F) is confirmed by our larger sample of ages. We investigate trends between age and metallicity, and with other physical parameters of the galaxies, such as ellipticity, luminosity and kinematic anisotropy. We demonstrate the existence of a galaxy age-metallicity relation similar to that seen for local galactic disc stars, whereby young galaxies have high metallicity, while old galaxies span a large range in metallicities. We also investigate the influence of environment and morphology on the galaxy age and metallicity, especially the predictions made by semi-analytic hierarchical clustering models (HCM). We confirm that non-cluster ellipticals are indeed younger on average than cluster ellipticals as predicted by the HCM models. However we also find a trend for the more luminous galaxies to have a higher [Mg/Fe] ratio than the lower luminosity galaxies, which is opposite to the expectation from HCM models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547#galaxy</TD>
            <TD>2011-09-14T19:47:42Z</TD>
            <TD>#Abundances#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/330/547&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/547</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/330/547 [1]</TD>
            <TD>Local galaxy ages and metallicities (Terlevich+, 2002)</TD>
            <TD>We have assembled a catalogue of relative ages, metallicities and abundance ratios for about 150 local galaxies in field, group and cluster environments. The galaxies span morphological types from cD and ellipticals, to late-type spirals. Ages and metallicities were estimated from high-quality published spectral line indices using Worthey &amp; Ottaviani (1997, Cat. &lt;J/ApJS/111/377&gt;) single stellar population evolutionary models. The identification of galaxy age as a fourth parameter in the fundamental plane (Forbes, Ponman &amp; Brown, 1998ApJ...508L..43F) is confirmed by our larger sample of ages. We investigate trends between age and metallicity, and with other physical parameters of the galaxies, such as ellipticity, luminosity and kinematic anisotropy. We demonstrate the existence of a galaxy age-metallicity relation similar to that seen for local galactic disc stars, whereby young galaxies have high metallicity, while old galaxies span a large range in metallicities. We also investigate the influence of environment and morphology on the galaxy age and metallicity, especially the predictions made by semi-analytic hierarchical clustering models (HCM). We confirm that non-cluster ellipticals are indeed younger on average than cluster ellipticals as predicted by the HCM models. However we also find a trend for the more luminous galaxies to have a higher [Mg/Fe] ratio than the lower luminosity galaxies, which is opposite to the expectation from HCM models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547#1</TD>
            <TD>2011-09-14T19:47:42Z</TD>
            <TD>#Abundances#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/330/547</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/547</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/330/547 [2]</TD>
            <TD>Local galaxy ages and metallicities (Terlevich+, 2002)</TD>
            <TD>We have assembled a catalogue of relative ages, metallicities and abundance ratios for about 150 local galaxies in field, group and cluster environments. The galaxies span morphological types from cD and ellipticals, to late-type spirals. Ages and metallicities were estimated from high-quality published spectral line indices using Worthey &amp; Ottaviani (1997, Cat. &lt;J/ApJS/111/377&gt;) single stellar population evolutionary models. The identification of galaxy age as a fourth parameter in the fundamental plane (Forbes, Ponman &amp; Brown, 1998ApJ...508L..43F) is confirmed by our larger sample of ages. We investigate trends between age and metallicity, and with other physical parameters of the galaxies, such as ellipticity, luminosity and kinematic anisotropy. We demonstrate the existence of a galaxy age-metallicity relation similar to that seen for local galactic disc stars, whereby young galaxies have high metallicity, while old galaxies span a large range in metallicities. We also investigate the influence of environment and morphology on the galaxy age and metallicity, especially the predictions made by semi-analytic hierarchical clustering models (HCM). We confirm that non-cluster ellipticals are indeed younger on average than cluster ellipticals as predicted by the HCM models. However we also find a trend for the more luminous galaxies to have a higher [Mg/Fe] ratio than the lower luminosity galaxies, which is opposite to the expectation from HCM models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547#2</TD>
            <TD>2011-09-14T19:47:42Z</TD>
            <TD>#Abundances#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/330/547&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/547</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/330/547 [galaxy]</TD>
            <TD>Local galaxy ages and metallicities (Terlevich+, 2002)</TD>
            <TD>We have assembled a catalogue of relative ages, metallicities and abundance ratios for about 150 local galaxies in field, group and cluster environments. The galaxies span morphological types from cD and ellipticals, to late-type spirals. Ages and metallicities were estimated from high-quality published spectral line indices using Worthey &amp; Ottaviani (1997, Cat. &lt;J/ApJS/111/377&gt;) single stellar population evolutionary models. The identification of galaxy age as a fourth parameter in the fundamental plane (Forbes, Ponman &amp; Brown, 1998ApJ...508L..43F) is confirmed by our larger sample of ages. We investigate trends between age and metallicity, and with other physical parameters of the galaxies, such as ellipticity, luminosity and kinematic anisotropy. We demonstrate the existence of a galaxy age-metallicity relation similar to that seen for local galactic disc stars, whereby young galaxies have high metallicity, while old galaxies span a large range in metallicities. We also investigate the influence of environment and morphology on the galaxy age and metallicity, especially the predictions made by semi-analytic hierarchical clustering models (HCM). We confirm that non-cluster ellipticals are indeed younger on average than cluster ellipticals as predicted by the HCM models. However we also find a trend for the more luminous galaxies to have a higher [Mg/Fe] ratio than the lower luminosity galaxies, which is opposite to the expectation from HCM models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547#galaxy</TD>
            <TD>2011-09-14T19:47:42Z</TD>
            <TD>#Abundances#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/330/547&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/547</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/330/547 [1]</TD>
            <TD>Local galaxy ages and metallicities (Terlevich+, 2002)</TD>
            <TD>We have assembled a catalogue of relative ages, metallicities and abundance ratios for about 150 local galaxies in field, group and cluster environments. The galaxies span morphological types from cD and ellipticals, to late-type spirals. Ages and metallicities were estimated from high-quality published spectral line indices using Worthey &amp; Ottaviani (1997, Cat. &lt;J/ApJS/111/377&gt;) single stellar population evolutionary models. The identification of galaxy age as a fourth parameter in the fundamental plane (Forbes, Ponman &amp; Brown, 1998ApJ...508L..43F) is confirmed by our larger sample of ages. We investigate trends between age and metallicity, and with other physical parameters of the galaxies, such as ellipticity, luminosity and kinematic anisotropy. We demonstrate the existence of a galaxy age-metallicity relation similar to that seen for local galactic disc stars, whereby young galaxies have high metallicity, while old galaxies span a large range in metallicities. We also investigate the influence of environment and morphology on the galaxy age and metallicity, especially the predictions made by semi-analytic hierarchical clustering models (HCM). We confirm that non-cluster ellipticals are indeed younger on average than cluster ellipticals as predicted by the HCM models. However we also find a trend for the more luminous galaxies to have a higher [Mg/Fe] ratio than the lower luminosity galaxies, which is opposite to the expectation from HCM models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547#1</TD>
            <TD>2011-09-14T19:47:42Z</TD>
            <TD>#Abundances#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/330/547</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/547</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/330/547 [2]</TD>
            <TD>Local galaxy ages and metallicities (Terlevich+, 2002)</TD>
            <TD>We have assembled a catalogue of relative ages, metallicities and abundance ratios for about 150 local galaxies in field, group and cluster environments. The galaxies span morphological types from cD and ellipticals, to late-type spirals. Ages and metallicities were estimated from high-quality published spectral line indices using Worthey &amp; Ottaviani (1997, Cat. &lt;J/ApJS/111/377&gt;) single stellar population evolutionary models. The identification of galaxy age as a fourth parameter in the fundamental plane (Forbes, Ponman &amp; Brown, 1998ApJ...508L..43F) is confirmed by our larger sample of ages. We investigate trends between age and metallicity, and with other physical parameters of the galaxies, such as ellipticity, luminosity and kinematic anisotropy. We demonstrate the existence of a galaxy age-metallicity relation similar to that seen for local galactic disc stars, whereby young galaxies have high metallicity, while old galaxies span a large range in metallicities. We also investigate the influence of environment and morphology on the galaxy age and metallicity, especially the predictions made by semi-analytic hierarchical clustering models (HCM). We confirm that non-cluster ellipticals are indeed younger on average than cluster ellipticals as predicted by the HCM models. However we also find a trend for the more luminous galaxies to have a higher [Mg/Fe] ratio than the lower luminosity galaxies, which is opposite to the expectation from HCM models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547#2</TD>
            <TD>2011-09-14T19:47:42Z</TD>
            <TD>#Abundances#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/330/547&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/547</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/330/547 [galaxy]</TD>
            <TD>Local galaxy ages and metallicities (Terlevich+, 2002)</TD>
            <TD>We have assembled a catalogue of relative ages, metallicities and abundance ratios for about 150 local galaxies in field, group and cluster environments. The galaxies span morphological types from cD and ellipticals, to late-type spirals. Ages and metallicities were estimated from high-quality published spectral line indices using Worthey &amp; Ottaviani (1997, Cat. &lt;J/ApJS/111/377&gt;) single stellar population evolutionary models. The identification of galaxy age as a fourth parameter in the fundamental plane (Forbes, Ponman &amp; Brown, 1998ApJ...508L..43F) is confirmed by our larger sample of ages. We investigate trends between age and metallicity, and with other physical parameters of the galaxies, such as ellipticity, luminosity and kinematic anisotropy. We demonstrate the existence of a galaxy age-metallicity relation similar to that seen for local galactic disc stars, whereby young galaxies have high metallicity, while old galaxies span a large range in metallicities. We also investigate the influence of environment and morphology on the galaxy age and metallicity, especially the predictions made by semi-analytic hierarchical clustering models (HCM). We confirm that non-cluster ellipticals are indeed younger on average than cluster ellipticals as predicted by the HCM models. However we also find a trend for the more luminous galaxies to have a higher [Mg/Fe] ratio than the lower luminosity galaxies, which is opposite to the expectation from HCM models.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547#galaxy</TD>
            <TD>2011-09-14T19:47:42Z</TD>
            <TD>#Abundances#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/547</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/330/547&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/547</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/329/227 [1]</TD>
            <TD>2dF Galaxy Redshift Survey. II. (Sadler+, 2002)</TD>
            <TD>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS, Condon 1998, Cat. &lt;VIII/65&gt;) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS, Colless, 2001, Cat. &lt;VII/226&gt;), covering an effective area of 325{deg}^2^ (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications - the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range z=0.005 to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1 Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4 GHz for both active and star-forming galaxies, and derive a local star formation density of 0.022+/-0.004M_{sun}_/yr/Mpc^3^ (H_0_=50km/s/Mpc)</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227#1</TD>
            <TD>2011-09-14T19:47:43Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/329/227</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/227</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/329/227 [2]</TD>
            <TD>2dF Galaxy Redshift Survey. II. (Sadler+, 2002)</TD>
            <TD>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS, Condon 1998, Cat. &lt;VIII/65&gt;) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS, Colless, 2001, Cat. &lt;VII/226&gt;), covering an effective area of 325{deg}^2^ (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications - the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range z=0.005 to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1 Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4 GHz for both active and star-forming galaxies, and derive a local star formation density of 0.022+/-0.004M_{sun}_/yr/Mpc^3^ (H_0_=50km/s/Mpc)</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227#2</TD>
            <TD>2011-09-14T19:47:43Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/329/227&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/329/227 [2dFGRS]</TD>
            <TD>2dF Galaxy Redshift Survey. II. (Sadler+, 2002)</TD>
            <TD>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS, Condon 1998, Cat. &lt;VIII/65&gt;) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS, Colless, 2001, Cat. &lt;VII/226&gt;), covering an effective area of 325{deg}^2^ (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications - the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range z=0.005 to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1 Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4 GHz for both active and star-forming galaxies, and derive a local star formation density of 0.022+/-0.004M_{sun}_/yr/Mpc^3^ (H_0_=50km/s/Mpc)</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227#2dFGRS</TD>
            <TD>2011-09-14T19:47:43Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/329/227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/329/227 [1]</TD>
            <TD>2dF Galaxy Redshift Survey. II. (Sadler+, 2002)</TD>
            <TD>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS, Condon 1998, Cat. &lt;VIII/65&gt;) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS, Colless, 2001, Cat. &lt;VII/226&gt;), covering an effective area of 325{deg}^2^ (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications - the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range z=0.005 to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1 Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4 GHz for both active and star-forming galaxies, and derive a local star formation density of 0.022+/-0.004M_{sun}_/yr/Mpc^3^ (H_0_=50km/s/Mpc)</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227#1</TD>
            <TD>2011-09-14T19:47:43Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/329/227</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/227</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/329/227 [2]</TD>
            <TD>2dF Galaxy Redshift Survey. II. (Sadler+, 2002)</TD>
            <TD>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS, Condon 1998, Cat. &lt;VIII/65&gt;) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS, Colless, 2001, Cat. &lt;VII/226&gt;), covering an effective area of 325{deg}^2^ (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications - the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range z=0.005 to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1 Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4 GHz for both active and star-forming galaxies, and derive a local star formation density of 0.022+/-0.004M_{sun}_/yr/Mpc^3^ (H_0_=50km/s/Mpc)</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227#2</TD>
            <TD>2011-09-14T19:47:43Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/329/227&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/329/227 [2dFGRS]</TD>
            <TD>2dF Galaxy Redshift Survey. II. (Sadler+, 2002)</TD>
            <TD>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS, Condon 1998, Cat. &lt;VIII/65&gt;) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS, Colless, 2001, Cat. &lt;VII/226&gt;), covering an effective area of 325{deg}^2^ (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications - the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range z=0.005 to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1 Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4 GHz for both active and star-forming galaxies, and derive a local star formation density of 0.022+/-0.004M_{sun}_/yr/Mpc^3^ (H_0_=50km/s/Mpc)</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227#2dFGRS</TD>
            <TD>2011-09-14T19:47:43Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/329/227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/329/227 [1]</TD>
            <TD>2dF Galaxy Redshift Survey. II. (Sadler+, 2002)</TD>
            <TD>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS, Condon 1998, Cat. &lt;VIII/65&gt;) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS, Colless, 2001, Cat. &lt;VII/226&gt;), covering an effective area of 325{deg}^2^ (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications - the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range z=0.005 to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1 Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4 GHz for both active and star-forming galaxies, and derive a local star formation density of 0.022+/-0.004M_{sun}_/yr/Mpc^3^ (H_0_=50km/s/Mpc)</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227#1</TD>
            <TD>2011-09-14T19:47:43Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/329/227</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/227</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/329/227 [2]</TD>
            <TD>2dF Galaxy Redshift Survey. II. (Sadler+, 2002)</TD>
            <TD>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS, Condon 1998, Cat. &lt;VIII/65&gt;) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS, Colless, 2001, Cat. &lt;VII/226&gt;), covering an effective area of 325{deg}^2^ (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications - the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range z=0.005 to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1 Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4 GHz for both active and star-forming galaxies, and derive a local star formation density of 0.022+/-0.004M_{sun}_/yr/Mpc^3^ (H_0_=50km/s/Mpc)</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227#2</TD>
            <TD>2011-09-14T19:47:43Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/329/227&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/329/227 [2dFGRS]</TD>
            <TD>2dF Galaxy Redshift Survey. II. (Sadler+, 2002)</TD>
            <TD>We have cross-matched the 1.4-GHz NRAO VLA Sky Survey (NVSS, Condon 1998, Cat. &lt;VIII/65&gt;) with the first 210 fields observed in the 2dF Galaxy Redshift Survey (2dFGRS, Colless, 2001, Cat. &lt;VII/226&gt;), covering an effective area of 325{deg}^2^ (about 20 per cent of the final 2dFGRS area). This yields a set of optical spectra of 912 candidate NVSS counterparts, of which we identify 757 as genuine radio identifications - the largest and most homogeneous set of radio source spectra ever obtained. The 2dFGRS radio sources span the redshift range z=0.005 to 0.438, and are a mixture of active galaxies (60 per cent) and star-forming galaxies (40 per cent). About 25 per cent of the 2dFGRS radio sources are spatially resolved by NVSS, and the sample includes three giant radio galaxies with projected linear size greater than 1 Mpc. The high quality of the 2dF spectra means we can usually distinguish unambiguously between AGN and star-forming galaxies. We make a new determination of the local radio luminosity function at 1.4 GHz for both active and star-forming galaxies, and derive a local star formation density of 0.022+/-0.004M_{sun}_/yr/Mpc^3^ (H_0_=50km/s/Mpc)</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227#2dFGRS</TD>
            <TD>2011-09-14T19:47:43Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/329/227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/328/461 [1]</TD>
            <TD>X-ray luminosities of early-type galaxies (O'Sullivan+, 2001)</TD>
            <TD>We present a catalogue of X-ray luminosities for 401 early-type galaxies, of which 136 are based on newly analysed ROSAT PSPC pointed observations (Cat. &lt;IX/30&gt;). The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. Using this sample we fit the L_X_/L_B_ relation for early-type galaxies and find a best-fit slope for the catalogue of ~2.2. We demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modelled by a single power-law fit. We also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L_(discrete-source-contribution)_/L_B_~29.5erg/s/L_B{sun}_. We compare this result with luminosities from our catalogue. Lastly, we examine the influence of environment on galaxy X-ray luminosity and on the form of the L_X_/L_B_ relation. We conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461#1</TD>
            <TD>2011-09-14T19:47:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/328/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/328/461 [2]</TD>
            <TD>X-ray luminosities of early-type galaxies (O'Sullivan+, 2001)</TD>
            <TD>We present a catalogue of X-ray luminosities for 401 early-type galaxies, of which 136 are based on newly analysed ROSAT PSPC pointed observations (Cat. &lt;IX/30&gt;). The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. Using this sample we fit the L_X_/L_B_ relation for early-type galaxies and find a best-fit slope for the catalogue of ~2.2. We demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modelled by a single power-law fit. We also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L_(discrete-source-contribution)_/L_B_~29.5erg/s/L_B{sun}_. We compare this result with luminosities from our catalogue. Lastly, we examine the influence of environment on galaxy X-ray luminosity and on the form of the L_X_/L_B_ relation. We conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461#2</TD>
            <TD>2011-09-14T19:47:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/328/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/461 [table3]</TD>
            <TD>X-ray luminosities of early-type galaxies (O'Sullivan+, 2001)</TD>
            <TD>We present a catalogue of X-ray luminosities for 401 early-type galaxies, of which 136 are based on newly analysed ROSAT PSPC pointed observations (Cat. &lt;IX/30&gt;). The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. Using this sample we fit the L_X_/L_B_ relation for early-type galaxies and find a best-fit slope for the catalogue of ~2.2. We demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modelled by a single power-law fit. We also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L_(discrete-source-contribution)_/L_B_~29.5erg/s/L_B{sun}_. We compare this result with luminosities from our catalogue. Lastly, we examine the influence of environment on galaxy X-ray luminosity and on the form of the L_X_/L_B_ relation. We conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461#table3</TD>
            <TD>2011-09-14T19:47:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/461&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/328/461 [1]</TD>
            <TD>X-ray luminosities of early-type galaxies (O'Sullivan+, 2001)</TD>
            <TD>We present a catalogue of X-ray luminosities for 401 early-type galaxies, of which 136 are based on newly analysed ROSAT PSPC pointed observations (Cat. &lt;IX/30&gt;). The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. Using this sample we fit the L_X_/L_B_ relation for early-type galaxies and find a best-fit slope for the catalogue of ~2.2. We demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modelled by a single power-law fit. We also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L_(discrete-source-contribution)_/L_B_~29.5erg/s/L_B{sun}_. We compare this result with luminosities from our catalogue. Lastly, we examine the influence of environment on galaxy X-ray luminosity and on the form of the L_X_/L_B_ relation. We conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461#1</TD>
            <TD>2011-09-14T19:47:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/328/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/328/461 [2]</TD>
            <TD>X-ray luminosities of early-type galaxies (O'Sullivan+, 2001)</TD>
            <TD>We present a catalogue of X-ray luminosities for 401 early-type galaxies, of which 136 are based on newly analysed ROSAT PSPC pointed observations (Cat. &lt;IX/30&gt;). The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. Using this sample we fit the L_X_/L_B_ relation for early-type galaxies and find a best-fit slope for the catalogue of ~2.2. We demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modelled by a single power-law fit. We also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L_(discrete-source-contribution)_/L_B_~29.5erg/s/L_B{sun}_. We compare this result with luminosities from our catalogue. Lastly, we examine the influence of environment on galaxy X-ray luminosity and on the form of the L_X_/L_B_ relation. We conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461#2</TD>
            <TD>2011-09-14T19:47:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/328/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/461 [table3]</TD>
            <TD>X-ray luminosities of early-type galaxies (O'Sullivan+, 2001)</TD>
            <TD>We present a catalogue of X-ray luminosities for 401 early-type galaxies, of which 136 are based on newly analysed ROSAT PSPC pointed observations (Cat. &lt;IX/30&gt;). The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. Using this sample we fit the L_X_/L_B_ relation for early-type galaxies and find a best-fit slope for the catalogue of ~2.2. We demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modelled by a single power-law fit. We also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L_(discrete-source-contribution)_/L_B_~29.5erg/s/L_B{sun}_. We compare this result with luminosities from our catalogue. Lastly, we examine the influence of environment on galaxy X-ray luminosity and on the form of the L_X_/L_B_ relation. We conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461#table3</TD>
            <TD>2011-09-14T19:47:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/461&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/328/461 [1]</TD>
            <TD>X-ray luminosities of early-type galaxies (O'Sullivan+, 2001)</TD>
            <TD>We present a catalogue of X-ray luminosities for 401 early-type galaxies, of which 136 are based on newly analysed ROSAT PSPC pointed observations (Cat. &lt;IX/30&gt;). The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. Using this sample we fit the L_X_/L_B_ relation for early-type galaxies and find a best-fit slope for the catalogue of ~2.2. We demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modelled by a single power-law fit. We also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L_(discrete-source-contribution)_/L_B_~29.5erg/s/L_B{sun}_. We compare this result with luminosities from our catalogue. Lastly, we examine the influence of environment on galaxy X-ray luminosity and on the form of the L_X_/L_B_ relation. We conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461#1</TD>
            <TD>2011-09-14T19:47:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/328/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/328/461 [2]</TD>
            <TD>X-ray luminosities of early-type galaxies (O'Sullivan+, 2001)</TD>
            <TD>We present a catalogue of X-ray luminosities for 401 early-type galaxies, of which 136 are based on newly analysed ROSAT PSPC pointed observations (Cat. &lt;IX/30&gt;). The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. Using this sample we fit the L_X_/L_B_ relation for early-type galaxies and find a best-fit slope for the catalogue of ~2.2. We demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modelled by a single power-law fit. We also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L_(discrete-source-contribution)_/L_B_~29.5erg/s/L_B{sun}_. We compare this result with luminosities from our catalogue. Lastly, we examine the influence of environment on galaxy X-ray luminosity and on the form of the L_X_/L_B_ relation. We conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461#2</TD>
            <TD>2011-09-14T19:47:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/328/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/461 [table3]</TD>
            <TD>X-ray luminosities of early-type galaxies (O'Sullivan+, 2001)</TD>
            <TD>We present a catalogue of X-ray luminosities for 401 early-type galaxies, of which 136 are based on newly analysed ROSAT PSPC pointed observations (Cat. &lt;IX/30&gt;). The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. Using this sample we fit the L_X_/L_B_ relation for early-type galaxies and find a best-fit slope for the catalogue of ~2.2. We demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modelled by a single power-law fit. We also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L_(discrete-source-contribution)_/L_B_~29.5erg/s/L_B{sun}_. We compare this result with luminosities from our catalogue. Lastly, we examine the influence of environment on galaxy X-ray luminosity and on the form of the L_X_/L_B_ relation. We conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461#table3</TD>
            <TD>2011-09-14T19:47:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/461</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/461&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/1116 [1]</TD>
            <TD>VI photometry of Sombrero globular clusters (Larsen+, 2001)</TD>
            <TD>We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the "Sombrero" (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the &gt;99 per cent confidence level, with peaks at (V-I)0=0.96+/-0.03 and 1,21+/-0.03. The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ~2pc with the red ones being ~30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116#1</TD>
            <TD>2011-09-14T19:48:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/1116</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1116</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/1116 [2]</TD>
            <TD>VI photometry of Sombrero globular clusters (Larsen+, 2001)</TD>
            <TD>We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the "Sombrero" (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the &gt;99 per cent confidence level, with peaks at (V-I)0=0.96+/-0.03 and 1,21+/-0.03. The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ~2pc with the red ones being ~30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116#2</TD>
            <TD>2011-09-14T19:48:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/1116&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1116</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/1116 [table2]</TD>
            <TD>VI photometry of Sombrero globular clusters (Larsen+, 2001)</TD>
            <TD>We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the "Sombrero" (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the &gt;99 per cent confidence level, with peaks at (V-I)0=0.96+/-0.03 and 1,21+/-0.03. The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ~2pc with the red ones being ~30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116#table2</TD>
            <TD>2011-09-14T19:48:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/1116&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1116</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/1116 [1]</TD>
            <TD>VI photometry of Sombrero globular clusters (Larsen+, 2001)</TD>
            <TD>We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the "Sombrero" (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the &gt;99 per cent confidence level, with peaks at (V-I)0=0.96+/-0.03 and 1,21+/-0.03. The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ~2pc with the red ones being ~30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116#1</TD>
            <TD>2011-09-14T19:48:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/1116</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1116</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/1116 [2]</TD>
            <TD>VI photometry of Sombrero globular clusters (Larsen+, 2001)</TD>
            <TD>We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the "Sombrero" (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the &gt;99 per cent confidence level, with peaks at (V-I)0=0.96+/-0.03 and 1,21+/-0.03. The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ~2pc with the red ones being ~30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116#2</TD>
            <TD>2011-09-14T19:48:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/1116&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1116</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/1116 [table2]</TD>
            <TD>VI photometry of Sombrero globular clusters (Larsen+, 2001)</TD>
            <TD>We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the "Sombrero" (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the &gt;99 per cent confidence level, with peaks at (V-I)0=0.96+/-0.03 and 1,21+/-0.03. The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ~2pc with the red ones being ~30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116#table2</TD>
            <TD>2011-09-14T19:48:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/1116&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1116</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/1116 [1]</TD>
            <TD>VI photometry of Sombrero globular clusters (Larsen+, 2001)</TD>
            <TD>We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the "Sombrero" (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the &gt;99 per cent confidence level, with peaks at (V-I)0=0.96+/-0.03 and 1,21+/-0.03. The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ~2pc with the red ones being ~30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116#1</TD>
            <TD>2011-09-14T19:48:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/1116</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1116</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/1116 [2]</TD>
            <TD>VI photometry of Sombrero globular clusters (Larsen+, 2001)</TD>
            <TD>We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the "Sombrero" (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the &gt;99 per cent confidence level, with peaks at (V-I)0=0.96+/-0.03 and 1,21+/-0.03. The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ~2pc with the red ones being ~30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116#2</TD>
            <TD>2011-09-14T19:48:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/1116&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1116</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/1116 [table2]</TD>
            <TD>VI photometry of Sombrero globular clusters (Larsen+, 2001)</TD>
            <TD>We explore the rich globular cluster (GC) system of the nearby Sa galaxy M104, the "Sombrero" (NGC 4594), using archive Wide Field Planetary Camera 2 data. The GC colour distribution is found to be bimodal at the &gt;99 per cent confidence level, with peaks at (V-I)0=0.96+/-0.03 and 1,21+/-0.03. The inferred metallicities are very similar to those of GCs in our Galaxy and M31. However, the Sombrero reveals a much enhanced number of red (metal-rich) GCs compared to other well-studied spirals. Because the Sombrero is dominated by a huge bulge and only has a modest disc, we associate the two subpopulations with the halo and bulge components, respectively. Thus our analysis supports the view that the metal-rich GCs in spirals are associated with the bulge rather than with the disc. The Sombrero GCs have typical effective (half-light) radii of ~2pc with the red ones being ~30 per cent smaller than the blue ones. We identify many similarities between the GC system of the Sombrero and those of both late-type spirals and early-type galaxies. Thus both the GC system and the Hubble type of the Sombrero galaxy appear to be intermediate in their nature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116#table2</TD>
            <TD>2011-09-14T19:48:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1116</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/1116&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1116</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [1]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#1</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVV DR1 [2]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#2</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/DirectCone?DSACAT=VVV_DR1&amp;DSATAB=vvvDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [3]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#3</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VVV DR1 [4]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#4</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [5]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#5</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [6]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#6</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [7]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#7</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [8]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#8</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [9]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#9</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [10]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#10</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VVV DR1 [11]</TD>
            <TD>VVV DR1 - VISTA Variables in the Via Lactea survey</TD>
            <TD>The VVV survey will perform wide FOV multi-epoch observations of the Galaxy's bulge and part of the disk, providing the astronomical public community with a high resolution 3-D (or 4-D if you include the time dimension) map of the bulge.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa#11</TD>
            <TD>2012-07-17T15:36:05Z</TD>
            <TD>#Infrared, survey, Milky Way, bulge#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vvvDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vvvDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://mwm.astro.puc.cl/mw/index.php/Main_Page</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/1004 [1]</TD>
            <TD>Early-type galaxy parameters (Blakeslee+, 2001)</TD>
            <TD>We perform a series of comparisons between distance-independent photometric and spectroscopic properties used in the surface brightness fluctuation (SBF) and fundamental plane (FP) methods of early-type galaxy distance estimation. The data are taken from two recent surveys: the SBF Survey of Galaxy Distances and the Streaming Motions of Abell Clusters (SMAC) FP survey. We derive a relation between (V-I)0 colour and Mg2 index using nearly 200 galaxies and discuss implications for Galactic extinction estimates and early-type galaxy stellar populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004#1</TD>
            <TD>2011-09-14T19:48:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/1004</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1004</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/1004 [2]</TD>
            <TD>Early-type galaxy parameters (Blakeslee+, 2001)</TD>
            <TD>We perform a series of comparisons between distance-independent photometric and spectroscopic properties used in the surface brightness fluctuation (SBF) and fundamental plane (FP) methods of early-type galaxy distance estimation. The data are taken from two recent surveys: the SBF Survey of Galaxy Distances and the Streaming Motions of Abell Clusters (SMAC) FP survey. We derive a relation between (V-I)0 colour and Mg2 index using nearly 200 galaxies and discuss implications for Galactic extinction estimates and early-type galaxy stellar populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004#2</TD>
            <TD>2011-09-14T19:48:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/1004&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1004</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/1004 [table1]</TD>
            <TD>Early-type galaxy parameters (Blakeslee+, 2001)</TD>
            <TD>We perform a series of comparisons between distance-independent photometric and spectroscopic properties used in the surface brightness fluctuation (SBF) and fundamental plane (FP) methods of early-type galaxy distance estimation. The data are taken from two recent surveys: the SBF Survey of Galaxy Distances and the Streaming Motions of Abell Clusters (SMAC) FP survey. We derive a relation between (V-I)0 colour and Mg2 index using nearly 200 galaxies and discuss implications for Galactic extinction estimates and early-type galaxy stellar populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004#table1</TD>
            <TD>2011-09-14T19:48:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/1004&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1004</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/1004 [1]</TD>
            <TD>Early-type galaxy parameters (Blakeslee+, 2001)</TD>
            <TD>We perform a series of comparisons between distance-independent photometric and spectroscopic properties used in the surface brightness fluctuation (SBF) and fundamental plane (FP) methods of early-type galaxy distance estimation. The data are taken from two recent surveys: the SBF Survey of Galaxy Distances and the Streaming Motions of Abell Clusters (SMAC) FP survey. We derive a relation between (V-I)0 colour and Mg2 index using nearly 200 galaxies and discuss implications for Galactic extinction estimates and early-type galaxy stellar populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004#1</TD>
            <TD>2011-09-14T19:48:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/1004</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1004</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/1004 [2]</TD>
            <TD>Early-type galaxy parameters (Blakeslee+, 2001)</TD>
            <TD>We perform a series of comparisons between distance-independent photometric and spectroscopic properties used in the surface brightness fluctuation (SBF) and fundamental plane (FP) methods of early-type galaxy distance estimation. The data are taken from two recent surveys: the SBF Survey of Galaxy Distances and the Streaming Motions of Abell Clusters (SMAC) FP survey. We derive a relation between (V-I)0 colour and Mg2 index using nearly 200 galaxies and discuss implications for Galactic extinction estimates and early-type galaxy stellar populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004#2</TD>
            <TD>2011-09-14T19:48:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/1004&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1004</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/1004 [table1]</TD>
            <TD>Early-type galaxy parameters (Blakeslee+, 2001)</TD>
            <TD>We perform a series of comparisons between distance-independent photometric and spectroscopic properties used in the surface brightness fluctuation (SBF) and fundamental plane (FP) methods of early-type galaxy distance estimation. The data are taken from two recent surveys: the SBF Survey of Galaxy Distances and the Streaming Motions of Abell Clusters (SMAC) FP survey. We derive a relation between (V-I)0 colour and Mg2 index using nearly 200 galaxies and discuss implications for Galactic extinction estimates and early-type galaxy stellar populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004#table1</TD>
            <TD>2011-09-14T19:48:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/1004&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1004</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/1004 [1]</TD>
            <TD>Early-type galaxy parameters (Blakeslee+, 2001)</TD>
            <TD>We perform a series of comparisons between distance-independent photometric and spectroscopic properties used in the surface brightness fluctuation (SBF) and fundamental plane (FP) methods of early-type galaxy distance estimation. The data are taken from two recent surveys: the SBF Survey of Galaxy Distances and the Streaming Motions of Abell Clusters (SMAC) FP survey. We derive a relation between (V-I)0 colour and Mg2 index using nearly 200 galaxies and discuss implications for Galactic extinction estimates and early-type galaxy stellar populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004#1</TD>
            <TD>2011-09-14T19:48:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/1004</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1004</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/1004 [2]</TD>
            <TD>Early-type galaxy parameters (Blakeslee+, 2001)</TD>
            <TD>We perform a series of comparisons between distance-independent photometric and spectroscopic properties used in the surface brightness fluctuation (SBF) and fundamental plane (FP) methods of early-type galaxy distance estimation. The data are taken from two recent surveys: the SBF Survey of Galaxy Distances and the Streaming Motions of Abell Clusters (SMAC) FP survey. We derive a relation between (V-I)0 colour and Mg2 index using nearly 200 galaxies and discuss implications for Galactic extinction estimates and early-type galaxy stellar populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004#2</TD>
            <TD>2011-09-14T19:48:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/1004&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1004</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/1004 [table1]</TD>
            <TD>Early-type galaxy parameters (Blakeslee+, 2001)</TD>
            <TD>We perform a series of comparisons between distance-independent photometric and spectroscopic properties used in the surface brightness fluctuation (SBF) and fundamental plane (FP) methods of early-type galaxy distance estimation. The data are taken from two recent surveys: the SBF Survey of Galaxy Distances and the Streaming Motions of Abell Clusters (SMAC) FP survey. We derive a relation between (V-I)0 colour and Mg2 index using nearly 200 galaxies and discuss implications for Galactic extinction estimates and early-type galaxy stellar populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004#table1</TD>
            <TD>2011-09-14T19:48:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/1004</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/1004&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/1004</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/1516 [1]</TD>
            <TD>MCG pairs and triples of galaxies (De Propris+, 2005)</TD>
            <TD>We derive the number of dynamically close companions per galaxy (N_c_) and their total luminosity (L_c_) for galaxies in the Millennium Galaxy Catalogue (MGC, 2003, Cat. &lt;VII/240&gt;). N_c_ is similar to the fraction of galaxies in close pairs and is directly related to the galaxy merger rate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516#1</TD>
            <TD>2011-09-14T19:48:17Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/1516</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1516</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/1516 [2]</TD>
            <TD>MCG pairs and triples of galaxies (De Propris+, 2005)</TD>
            <TD>We derive the number of dynamically close companions per galaxy (N_c_) and their total luminosity (L_c_) for galaxies in the Millennium Galaxy Catalogue (MGC, 2003, Cat. &lt;VII/240&gt;). N_c_ is similar to the fraction of galaxies in close pairs and is directly related to the galaxy merger rate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516#2</TD>
            <TD>2011-09-14T19:48:17Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/1516&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1516</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/1516 [table1]</TD>
            <TD>MCG pairs and triples of galaxies (De Propris+, 2005)</TD>
            <TD>We derive the number of dynamically close companions per galaxy (N_c_) and their total luminosity (L_c_) for galaxies in the Millennium Galaxy Catalogue (MGC, 2003, Cat. &lt;VII/240&gt;). N_c_ is similar to the fraction of galaxies in close pairs and is directly related to the galaxy merger rate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516#table1</TD>
            <TD>2011-09-14T19:48:17Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/1516&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1516</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/1516 [1]</TD>
            <TD>MCG pairs and triples of galaxies (De Propris+, 2005)</TD>
            <TD>We derive the number of dynamically close companions per galaxy (N_c_) and their total luminosity (L_c_) for galaxies in the Millennium Galaxy Catalogue (MGC, 2003, Cat. &lt;VII/240&gt;). N_c_ is similar to the fraction of galaxies in close pairs and is directly related to the galaxy merger rate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516#1</TD>
            <TD>2011-09-14T19:48:17Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/1516</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1516</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/1516 [2]</TD>
            <TD>MCG pairs and triples of galaxies (De Propris+, 2005)</TD>
            <TD>We derive the number of dynamically close companions per galaxy (N_c_) and their total luminosity (L_c_) for galaxies in the Millennium Galaxy Catalogue (MGC, 2003, Cat. &lt;VII/240&gt;). N_c_ is similar to the fraction of galaxies in close pairs and is directly related to the galaxy merger rate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516#2</TD>
            <TD>2011-09-14T19:48:17Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/1516&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1516</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/1516 [table1]</TD>
            <TD>MCG pairs and triples of galaxies (De Propris+, 2005)</TD>
            <TD>We derive the number of dynamically close companions per galaxy (N_c_) and their total luminosity (L_c_) for galaxies in the Millennium Galaxy Catalogue (MGC, 2003, Cat. &lt;VII/240&gt;). N_c_ is similar to the fraction of galaxies in close pairs and is directly related to the galaxy merger rate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516#table1</TD>
            <TD>2011-09-14T19:48:17Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/1516&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1516</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/1516 [1]</TD>
            <TD>MCG pairs and triples of galaxies (De Propris+, 2005)</TD>
            <TD>We derive the number of dynamically close companions per galaxy (N_c_) and their total luminosity (L_c_) for galaxies in the Millennium Galaxy Catalogue (MGC, 2003, Cat. &lt;VII/240&gt;). N_c_ is similar to the fraction of galaxies in close pairs and is directly related to the galaxy merger rate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516#1</TD>
            <TD>2011-09-14T19:48:17Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/1516</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1516</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/1516 [2]</TD>
            <TD>MCG pairs and triples of galaxies (De Propris+, 2005)</TD>
            <TD>We derive the number of dynamically close companions per galaxy (N_c_) and their total luminosity (L_c_) for galaxies in the Millennium Galaxy Catalogue (MGC, 2003, Cat. &lt;VII/240&gt;). N_c_ is similar to the fraction of galaxies in close pairs and is directly related to the galaxy merger rate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516#2</TD>
            <TD>2011-09-14T19:48:17Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/1516&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1516</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/1516 [table1]</TD>
            <TD>MCG pairs and triples of galaxies (De Propris+, 2005)</TD>
            <TD>We derive the number of dynamically close companions per galaxy (N_c_) and their total luminosity (L_c_) for galaxies in the Millennium Galaxy Catalogue (MGC, 2003, Cat. &lt;VII/240&gt;). N_c_ is similar to the fraction of galaxies in close pairs and is directly related to the galaxy merger rate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516#table1</TD>
            <TD>2011-09-14T19:48:17Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1516</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/1516&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1516</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/408/905 [1]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#1</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/408/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/408/905 [2]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#2</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/408/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/408/905 [table1]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#table1</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/408/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/408/905 [tableb]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#tableb</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/408/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/408/905 [1]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#1</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/408/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/408/905 [2]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#2</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/408/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/408/905 [table1]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#table1</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/408/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/408/905 [tableb]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#tableb</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/408/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/408/905 [1]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#1</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/408/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/408/905 [2]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#2</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/408/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/408/905 [table1]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#table1</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/408/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/408/905 [tableb]</TD>
            <TD>Very Luminous Galaxies (Cappi+, 2003)</TD>
            <TD>Three VLGs were selected from our catalogue of VLGs (see Table 1 of Paper I, Cappi et al., 1998A&amp;A...335..779C), while a fourth galaxy satisfying the VLG definition was selected from the CfA catalogue (see Geller &amp; Huchra, 1989Sci...246..897G); the 4 VLG fields were observed at OHP. Other 15 VLG fields were extracted from the 2dFGRS public catalogue (Cat. &lt;VII/226&gt;), which has an overlap with the SSRS2 (Cat. &lt;J/AJ/116/1&gt;). While partially imposed by observational constraints (see below), our selection is random with respect to the VLG properties, and should be representative of the whole sample. In fact, one third of the selected VLGs are early-type galaxies, a fraction consistent with that of the total sample published in Paper I, Cappi et al. (1998A&amp;A...335..779C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905#tableb</TD>
            <TD>2011-09-14T19:54:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/408/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/408/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/408/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1529 [1]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#1</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1529</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1529 [2]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#2</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1927]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1927</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2666]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2666</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1749]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1749</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2067]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2067</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2089]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2089</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1691]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1691</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2079]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2079</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a779]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a779</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1767]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1767</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2199]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2199</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1837]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1837</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1529 [1]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#1</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1529</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1529 [2]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#2</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1927]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1927</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2666]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2666</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1749]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1749</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2067]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2067</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2089]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2089</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1691]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1691</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2079]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2079</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a779]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a779</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1767]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1767</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2199]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2199</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1837]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1837</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1529 [1]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#1</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1529</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1529 [2]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#2</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1927]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1927</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2666]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2666</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1749]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1749</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2067]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2067</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2089]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2089</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1691]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1691</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2079]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2079</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a779]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a779</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1767]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1767</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a2199]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a2199</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1529 [a1837]</TD>
            <TD>cD clusters of galaxies. III. (Hill+, 1998)</TD>
            <TD>We present the final observational data for a spectroscopic study of a sample of cD galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cD galaxies. In this paper we present redshifts for 762 galaxies in the fields of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529#a1837</TD>
            <TD>2011-09-14T19:55:09Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/88/423 [1]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#1</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/88/423</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/88/423 [2]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#2</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/88/423 [table3]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#table3</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/88/423 [table2]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#table2</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/88/423 [table1]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#table1</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/88/423 [1]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#1</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/88/423</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/88/423 [2]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#2</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/88/423 [table3]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#table3</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/88/423 [table2]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#table2</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/88/423 [table1]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#table1</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/88/423 [1]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#1</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/88/423</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/88/423 [2]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#2</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/88/423 [table3]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#table3</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/88/423 [table2]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#table2</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/88/423 [table1]</TD>
            <TD>PNe in NGC 5128 (Hui+ 1993)</TD>
            <TD>We present a catalog of planetary nebulae in the nearest giant elliptical galaxy NGC 5128. The catalog consists of positions and [O III]{lambda}5007 magnitudes for 785 planetary nebulae. This is the second largest catalog of planetaries, next only to that of the Milky Way. We also list the coordinates of 32 bright stars from the Guide Star Catalog and 80 additional reference stars in the survey fields for astrometric reference during future observations. The positions of the planetary nebulae are accurate to 0.2" with respect to the Guide Star Catalog in right ascension or declination.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423#table1</TD>
            <TD>2011-09-14T19:55:27Z</TD>
            <TD>#Positional_Data#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/88/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/88/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/88/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/699/L43 [1]</TD>
            <TD>FIRST-NVSS-SDSS AGN sample catalog (Smolcic+, 2009)</TD>
            <TD>Radio outflows of active galactic nuclei (AGNs) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently, it has been suggested that the two major radio AGN populations-the powerful high-excitation, and the weak low-excitation radio AGNs (HERAGN and LERAGN, respectively)-represent two earlier and later stages of massive galaxy buildup. To test this, here we make use of a local (0.04&lt;z&lt;0.1) sample of ~500 radio AGNs with available optical spectroscopy, drawn from the FIRST, NVSS, SDSS, and 3CRR surveys.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43#1</TD>
            <TD>2012-02-18T17:22:40Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/699/L43</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/699/L43</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/699/L43 [2]</TD>
            <TD>FIRST-NVSS-SDSS AGN sample catalog (Smolcic+, 2009)</TD>
            <TD>Radio outflows of active galactic nuclei (AGNs) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently, it has been suggested that the two major radio AGN populations-the powerful high-excitation, and the weak low-excitation radio AGNs (HERAGN and LERAGN, respectively)-represent two earlier and later stages of massive galaxy buildup. To test this, here we make use of a local (0.04&lt;z&lt;0.1) sample of ~500 radio AGNs with available optical spectroscopy, drawn from the FIRST, NVSS, SDSS, and 3CRR surveys.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43#2</TD>
            <TD>2012-02-18T17:22:40Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/699/L43&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/699/L43</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/699/L43 [catalog]</TD>
            <TD>FIRST-NVSS-SDSS AGN sample catalog (Smolcic+, 2009)</TD>
            <TD>Radio outflows of active galactic nuclei (AGNs) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently, it has been suggested that the two major radio AGN populations-the powerful high-excitation, and the weak low-excitation radio AGNs (HERAGN and LERAGN, respectively)-represent two earlier and later stages of massive galaxy buildup. To test this, here we make use of a local (0.04&lt;z&lt;0.1) sample of ~500 radio AGNs with available optical spectroscopy, drawn from the FIRST, NVSS, SDSS, and 3CRR surveys.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43#catalog</TD>
            <TD>2012-02-18T17:22:40Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/699/L43&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/699/L43</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/699/L43 [1]</TD>
            <TD>FIRST-NVSS-SDSS AGN sample catalog (Smolcic+, 2009)</TD>
            <TD>Radio outflows of active galactic nuclei (AGNs) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently, it has been suggested that the two major radio AGN populations-the powerful high-excitation, and the weak low-excitation radio AGNs (HERAGN and LERAGN, respectively)-represent two earlier and later stages of massive galaxy buildup. To test this, here we make use of a local (0.04&lt;z&lt;0.1) sample of ~500 radio AGNs with available optical spectroscopy, drawn from the FIRST, NVSS, SDSS, and 3CRR surveys.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43#1</TD>
            <TD>2012-02-18T17:22:40Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/699/L43</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/699/L43</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/699/L43 [2]</TD>
            <TD>FIRST-NVSS-SDSS AGN sample catalog (Smolcic+, 2009)</TD>
            <TD>Radio outflows of active galactic nuclei (AGNs) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently, it has been suggested that the two major radio AGN populations-the powerful high-excitation, and the weak low-excitation radio AGNs (HERAGN and LERAGN, respectively)-represent two earlier and later stages of massive galaxy buildup. To test this, here we make use of a local (0.04&lt;z&lt;0.1) sample of ~500 radio AGNs with available optical spectroscopy, drawn from the FIRST, NVSS, SDSS, and 3CRR surveys.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43#2</TD>
            <TD>2012-02-18T17:22:40Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/699/L43&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/699/L43</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/699/L43 [catalog]</TD>
            <TD>FIRST-NVSS-SDSS AGN sample catalog (Smolcic+, 2009)</TD>
            <TD>Radio outflows of active galactic nuclei (AGNs) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently, it has been suggested that the two major radio AGN populations-the powerful high-excitation, and the weak low-excitation radio AGNs (HERAGN and LERAGN, respectively)-represent two earlier and later stages of massive galaxy buildup. To test this, here we make use of a local (0.04&lt;z&lt;0.1) sample of ~500 radio AGNs with available optical spectroscopy, drawn from the FIRST, NVSS, SDSS, and 3CRR surveys.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43#catalog</TD>
            <TD>2012-02-18T17:22:40Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/699/L43&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/699/L43</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/699/L43 [1]</TD>
            <TD>FIRST-NVSS-SDSS AGN sample catalog (Smolcic+, 2009)</TD>
            <TD>Radio outflows of active galactic nuclei (AGNs) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently, it has been suggested that the two major radio AGN populations-the powerful high-excitation, and the weak low-excitation radio AGNs (HERAGN and LERAGN, respectively)-represent two earlier and later stages of massive galaxy buildup. To test this, here we make use of a local (0.04&lt;z&lt;0.1) sample of ~500 radio AGNs with available optical spectroscopy, drawn from the FIRST, NVSS, SDSS, and 3CRR surveys.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43#1</TD>
            <TD>2012-02-18T17:22:40Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/699/L43</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/699/L43</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/699/L43 [2]</TD>
            <TD>FIRST-NVSS-SDSS AGN sample catalog (Smolcic+, 2009)</TD>
            <TD>Radio outflows of active galactic nuclei (AGNs) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently, it has been suggested that the two major radio AGN populations-the powerful high-excitation, and the weak low-excitation radio AGNs (HERAGN and LERAGN, respectively)-represent two earlier and later stages of massive galaxy buildup. To test this, here we make use of a local (0.04&lt;z&lt;0.1) sample of ~500 radio AGNs with available optical spectroscopy, drawn from the FIRST, NVSS, SDSS, and 3CRR surveys.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43#2</TD>
            <TD>2012-02-18T17:22:40Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/699/L43&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/699/L43</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/699/L43 [catalog]</TD>
            <TD>FIRST-NVSS-SDSS AGN sample catalog (Smolcic+, 2009)</TD>
            <TD>Radio outflows of active galactic nuclei (AGNs) are invoked in cosmological models as a key feedback mechanism in the latest phases of massive galaxy formation. Recently, it has been suggested that the two major radio AGN populations-the powerful high-excitation, and the weak low-excitation radio AGNs (HERAGN and LERAGN, respectively)-represent two earlier and later stages of massive galaxy buildup. To test this, here we make use of a local (0.04&lt;z&lt;0.1) sample of ~500 radio AGNs with available optical spectroscopy, drawn from the FIRST, NVSS, SDSS, and 3CRR surveys.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43#catalog</TD>
            <TD>2012-02-18T17:22:40Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/699/L43</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/699/L43&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/699/L43</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>HST.STAGES</TD>
            <TD>Space Telescope A901/902 Galaxy Evolution Survey (STAGES)</TD>
            <TD>STAGES is a large area (0.5x0.5 degree) survey of the complex Abell 901(a,b)/902 multiple-cluster system at z=0.165. An 80-tile imaging mosaic in F606W was conducted in HST cycle 13 with the HST/ACS instrument.</TD>
            <TD>MAST</TD>
            <TD>#Optical#</TD>
            <TD>ivo://mast.stsci/siap/stages#1</TD>
            <TD>2012-03-08T20:47:21Z</TD>
            <TD>#Galaxy Evolution#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1.0</TD>
            <TD>ivo://mast.stsci/siap/stages</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://archive.stsci.edu/siap/search.php?id=stages&amp;</TD>
            <TD />
            <TD>163</TD>
            <TD />
            <TD>http://archive.stsci.edu/prepds/stages/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/702/178 [1]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#1</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/702/178</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/702/178 [2]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#2</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [table6]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#table6</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [green]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#green</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [YSOcand]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#YSOcand</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [table5]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#table5</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [maser]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#maser</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [table1]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#table1</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/702/178 [1]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#1</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/702/178</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/702/178 [2]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#2</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [table6]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#table6</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [green]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#green</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [YSOcand]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#YSOcand</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [table5]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#table5</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [maser]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#maser</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [table1]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#table1</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/702/178 [1]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#1</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/702/178</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/702/178 [2]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#2</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [table6]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#table6</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [green]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#green</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [YSOcand]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#YSOcand</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [table5]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#table5</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [maser]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#maser</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/178 [table1]</TD>
            <TD>YSOs in the central 400pc of the Galaxy (Yusef-Zadeh+, 2009)</TD>
            <TD>The source photometry was based on the 24um catalog compiled by Hinz et al. (2009, Cat. J/ApJS/181/227). Our data are complemented by the Spitzer Legacy program MIPS Inner Galactic Plane Survey (MIPSGAL) which observed 220degrees^2^ of the inner Galactic plane at 24 and 70um (Carey et al. 2009PASP..121...76C). In order to obtain more complete SEDs of some of the high latitude 24um sources that show excess emission at 4.5um, we selected a total of nine such sources distributed at high Galactic latitudes within our survey. These sources were observed separately with MIPS at 70um between 2007 September 21 and 23. We obtained 32 overlapping images at 20cm from two surveys: Yusef-Zadeh et al. 2004, Cat. J/ApJS/155/421 and Law et al. 2008, Cat. J/ApJS/177/255. C. C. Lang et al. (2011ASPC..439...53L) have completed a 6cm survey of the Galactic center region with a uniform uv coverage. We have used this data set to measure the fluxes of several point sources in the G359.43+0.02 cluster.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178#table1</TD>
            <TD>2012-03-12T12:58:25Z</TD>
            <TD>#YSOs#Masses#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/461/397 [1]</TD>
            <TD>RASS-SDSS galaxy cluster survey. V. (Popesso+, 2007)</TD>
            <TD>In this paper we consider a large sample of optically selected clusters, in order to elucidate the physical reasons for the existence of X-ray underluminous clusters. For this purpose we analyzed the correlations of the X-ray and optical properties of a sample of 137 spectroscopically confirmed Abell clusters in the SDSS database. We searched for the X-ray counterpart of each cluster in the ROSAT All Sky Survey. We find that 40% of our clusters have a marginal X-ray detection or remain undetected in X-rays. These clusters appear too X-ray faint on average for their mass as determined by velocity dispersion; i.e. they do not follow the scaling relation between X-ray luminosity and virial mass traced by the other clusters. On the other hand, they do follow the general scaling relation between optical luminosity and virial mass. We refer to these clusters as the X-ray-underluminous Abell clusters (AXU clusters, for short) and designate as "normal" the X-ray detected Abell systems. We separately examined the distributions and properties of the galaxy populations of the normal and the AXU clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397#1</TD>
            <TD>2011-09-14T20:13:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/461/397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/461/397 [2]</TD>
            <TD>RASS-SDSS galaxy cluster survey. V. (Popesso+, 2007)</TD>
            <TD>In this paper we consider a large sample of optically selected clusters, in order to elucidate the physical reasons for the existence of X-ray underluminous clusters. For this purpose we analyzed the correlations of the X-ray and optical properties of a sample of 137 spectroscopically confirmed Abell clusters in the SDSS database. We searched for the X-ray counterpart of each cluster in the ROSAT All Sky Survey. We find that 40% of our clusters have a marginal X-ray detection or remain undetected in X-rays. These clusters appear too X-ray faint on average for their mass as determined by velocity dispersion; i.e. they do not follow the scaling relation between X-ray luminosity and virial mass traced by the other clusters. On the other hand, they do follow the general scaling relation between optical luminosity and virial mass. We refer to these clusters as the X-ray-underluminous Abell clusters (AXU clusters, for short) and designate as "normal" the X-ray detected Abell systems. We separately examined the distributions and properties of the galaxy populations of the normal and the AXU clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397#2</TD>
            <TD>2011-09-14T20:13:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/461/397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/461/397 [tablea1]</TD>
            <TD>RASS-SDSS galaxy cluster survey. V. (Popesso+, 2007)</TD>
            <TD>In this paper we consider a large sample of optically selected clusters, in order to elucidate the physical reasons for the existence of X-ray underluminous clusters. For this purpose we analyzed the correlations of the X-ray and optical properties of a sample of 137 spectroscopically confirmed Abell clusters in the SDSS database. We searched for the X-ray counterpart of each cluster in the ROSAT All Sky Survey. We find that 40% of our clusters have a marginal X-ray detection or remain undetected in X-rays. These clusters appear too X-ray faint on average for their mass as determined by velocity dispersion; i.e. they do not follow the scaling relation between X-ray luminosity and virial mass traced by the other clusters. On the other hand, they do follow the general scaling relation between optical luminosity and virial mass. We refer to these clusters as the X-ray-underluminous Abell clusters (AXU clusters, for short) and designate as "normal" the X-ray detected Abell systems. We separately examined the distributions and properties of the galaxy populations of the normal and the AXU clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397#tablea1</TD>
            <TD>2011-09-14T20:13:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/461/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/461/397 [1]</TD>
            <TD>RASS-SDSS galaxy cluster survey. V. (Popesso+, 2007)</TD>
            <TD>In this paper we consider a large sample of optically selected clusters, in order to elucidate the physical reasons for the existence of X-ray underluminous clusters. For this purpose we analyzed the correlations of the X-ray and optical properties of a sample of 137 spectroscopically confirmed Abell clusters in the SDSS database. We searched for the X-ray counterpart of each cluster in the ROSAT All Sky Survey. We find that 40% of our clusters have a marginal X-ray detection or remain undetected in X-rays. These clusters appear too X-ray faint on average for their mass as determined by velocity dispersion; i.e. they do not follow the scaling relation between X-ray luminosity and virial mass traced by the other clusters. On the other hand, they do follow the general scaling relation between optical luminosity and virial mass. We refer to these clusters as the X-ray-underluminous Abell clusters (AXU clusters, for short) and designate as "normal" the X-ray detected Abell systems. We separately examined the distributions and properties of the galaxy populations of the normal and the AXU clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397#1</TD>
            <TD>2011-09-14T20:13:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/461/397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/461/397 [2]</TD>
            <TD>RASS-SDSS galaxy cluster survey. V. (Popesso+, 2007)</TD>
            <TD>In this paper we consider a large sample of optically selected clusters, in order to elucidate the physical reasons for the existence of X-ray underluminous clusters. For this purpose we analyzed the correlations of the X-ray and optical properties of a sample of 137 spectroscopically confirmed Abell clusters in the SDSS database. We searched for the X-ray counterpart of each cluster in the ROSAT All Sky Survey. We find that 40% of our clusters have a marginal X-ray detection or remain undetected in X-rays. These clusters appear too X-ray faint on average for their mass as determined by velocity dispersion; i.e. they do not follow the scaling relation between X-ray luminosity and virial mass traced by the other clusters. On the other hand, they do follow the general scaling relation between optical luminosity and virial mass. We refer to these clusters as the X-ray-underluminous Abell clusters (AXU clusters, for short) and designate as "normal" the X-ray detected Abell systems. We separately examined the distributions and properties of the galaxy populations of the normal and the AXU clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397#2</TD>
            <TD>2011-09-14T20:13:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/461/397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/461/397 [tablea1]</TD>
            <TD>RASS-SDSS galaxy cluster survey. V. (Popesso+, 2007)</TD>
            <TD>In this paper we consider a large sample of optically selected clusters, in order to elucidate the physical reasons for the existence of X-ray underluminous clusters. For this purpose we analyzed the correlations of the X-ray and optical properties of a sample of 137 spectroscopically confirmed Abell clusters in the SDSS database. We searched for the X-ray counterpart of each cluster in the ROSAT All Sky Survey. We find that 40% of our clusters have a marginal X-ray detection or remain undetected in X-rays. These clusters appear too X-ray faint on average for their mass as determined by velocity dispersion; i.e. they do not follow the scaling relation between X-ray luminosity and virial mass traced by the other clusters. On the other hand, they do follow the general scaling relation between optical luminosity and virial mass. We refer to these clusters as the X-ray-underluminous Abell clusters (AXU clusters, for short) and designate as "normal" the X-ray detected Abell systems. We separately examined the distributions and properties of the galaxy populations of the normal and the AXU clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397#tablea1</TD>
            <TD>2011-09-14T20:13:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/461/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/461/397 [1]</TD>
            <TD>RASS-SDSS galaxy cluster survey. V. (Popesso+, 2007)</TD>
            <TD>In this paper we consider a large sample of optically selected clusters, in order to elucidate the physical reasons for the existence of X-ray underluminous clusters. For this purpose we analyzed the correlations of the X-ray and optical properties of a sample of 137 spectroscopically confirmed Abell clusters in the SDSS database. We searched for the X-ray counterpart of each cluster in the ROSAT All Sky Survey. We find that 40% of our clusters have a marginal X-ray detection or remain undetected in X-rays. These clusters appear too X-ray faint on average for their mass as determined by velocity dispersion; i.e. they do not follow the scaling relation between X-ray luminosity and virial mass traced by the other clusters. On the other hand, they do follow the general scaling relation between optical luminosity and virial mass. We refer to these clusters as the X-ray-underluminous Abell clusters (AXU clusters, for short) and designate as "normal" the X-ray detected Abell systems. We separately examined the distributions and properties of the galaxy populations of the normal and the AXU clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397#1</TD>
            <TD>2011-09-14T20:13:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/461/397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/461/397 [2]</TD>
            <TD>RASS-SDSS galaxy cluster survey. V. (Popesso+, 2007)</TD>
            <TD>In this paper we consider a large sample of optically selected clusters, in order to elucidate the physical reasons for the existence of X-ray underluminous clusters. For this purpose we analyzed the correlations of the X-ray and optical properties of a sample of 137 spectroscopically confirmed Abell clusters in the SDSS database. We searched for the X-ray counterpart of each cluster in the ROSAT All Sky Survey. We find that 40% of our clusters have a marginal X-ray detection or remain undetected in X-rays. These clusters appear too X-ray faint on average for their mass as determined by velocity dispersion; i.e. they do not follow the scaling relation between X-ray luminosity and virial mass traced by the other clusters. On the other hand, they do follow the general scaling relation between optical luminosity and virial mass. We refer to these clusters as the X-ray-underluminous Abell clusters (AXU clusters, for short) and designate as "normal" the X-ray detected Abell systems. We separately examined the distributions and properties of the galaxy populations of the normal and the AXU clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397#2</TD>
            <TD>2011-09-14T20:13:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/461/397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/461/397 [tablea1]</TD>
            <TD>RASS-SDSS galaxy cluster survey. V. (Popesso+, 2007)</TD>
            <TD>In this paper we consider a large sample of optically selected clusters, in order to elucidate the physical reasons for the existence of X-ray underluminous clusters. For this purpose we analyzed the correlations of the X-ray and optical properties of a sample of 137 spectroscopically confirmed Abell clusters in the SDSS database. We searched for the X-ray counterpart of each cluster in the ROSAT All Sky Survey. We find that 40% of our clusters have a marginal X-ray detection or remain undetected in X-rays. These clusters appear too X-ray faint on average for their mass as determined by velocity dispersion; i.e. they do not follow the scaling relation between X-ray luminosity and virial mass traced by the other clusters. On the other hand, they do follow the general scaling relation between optical luminosity and virial mass. We refer to these clusters as the X-ray-underluminous Abell clusters (AXU clusters, for short) and designate as "normal" the X-ray detected Abell systems. We separately examined the distributions and properties of the galaxy populations of the normal and the AXU clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397#tablea1</TD>
            <TD>2011-09-14T20:13:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/461/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/461/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/461/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [1]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#1</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=twomass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [2]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#2</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisj&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [3]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#3</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=agn2mass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [4]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#4</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=denisi&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [5]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#5</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=nvss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [6]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#6</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=supercos&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [7]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#7</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=rass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [8]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#8</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hipass&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [9]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#9</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=shapley&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [10]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#10</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=spectra&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [11]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#11</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=hes&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [12]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#12</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=sumss&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [13]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#13</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=fsc&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [14]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#14</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=durukst&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>6dF DR2 [15]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#15</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/DirectCone?DSACAT=SixdF&amp;DSATAB=target&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [16]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#16</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>6dF DR2 [17]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#17</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [18]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#18</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [19]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#19</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [20]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#20</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [21]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#21</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [22]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#22</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [23]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#23</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>6dF DR2 [24]</TD>
            <TD>6dF Galaxy Survey Data Release 2</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa#24</TD>
            <TD>2012-07-18T12:22:20Z</TD>
            <TD>#6dF survey galaxy galaxies redshift redshifts 2MASS#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/6df-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6df-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/470/821 [1]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#1</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/470/821</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/470/821 [2]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#2</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/470/821&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table3]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table3</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table1]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table1</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table2]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table2</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table4]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table4</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/470/821 [1]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#1</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/470/821</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/470/821 [2]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#2</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/470/821&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table3]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table3</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table1]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table1</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table2]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table2</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table4]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table4</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/470/821 [1]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#1</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/470/821</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/470/821 [2]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#2</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/470/821&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table3]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table3</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table1]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table1</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table2]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table2</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/470/821 [table4]</TD>
            <TD>BLOX Cluster catalog (Dietrich+, 2007)</TD>
            <TD>Galaxy cluster candidates in the XMM-Newton Follow-Up Survey detected with X-ray, optical matched filter, and weak lensing methods. Table 1 is the list of all cluster candidates in this survey with any method. This table lists the cluster candidates' names, positions, and provides information on which methods led to a detection. Individual detection parameters are given in Table 2 (X-ray), Table 3 (optical matched filter), and Table 4 (weak lensing).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821#table4</TD>
            <TD>2011-09-14T20:14:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/470/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/470/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/470/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/471/573 [1]</TD>
            <TD>JHKs photometry of a new stellar cluster (Yun+, 2007)</TD>
            <TD>We report the discovery of a new young stellar cluster and molecular cloud located in the far outer Galaxy, seen towards IRAS 06361-0142, and we characterise their properties. Near-infrared images obtained with VLT/ISAAC through JHK filters, millimetre line observations of CO(1-0) obtained with SEST, and VLA 6cm continuum maps obtained from archive data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573#1</TD>
            <TD>2011-09-14T20:14:21Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/471/573</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/471/573</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/471/573 [2]</TD>
            <TD>JHKs photometry of a new stellar cluster (Yun+, 2007)</TD>
            <TD>We report the discovery of a new young stellar cluster and molecular cloud located in the far outer Galaxy, seen towards IRAS 06361-0142, and we characterise their properties. Near-infrared images obtained with VLT/ISAAC through JHK filters, millimetre line observations of CO(1-0) obtained with SEST, and VLA 6cm continuum maps obtained from archive data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573#2</TD>
            <TD>2011-09-14T20:14:21Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/471/573&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/471/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/471/573 [table1]</TD>
            <TD>JHKs photometry of a new stellar cluster (Yun+, 2007)</TD>
            <TD>We report the discovery of a new young stellar cluster and molecular cloud located in the far outer Galaxy, seen towards IRAS 06361-0142, and we characterise their properties. Near-infrared images obtained with VLT/ISAAC through JHK filters, millimetre line observations of CO(1-0) obtained with SEST, and VLA 6cm continuum maps obtained from archive data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573#table1</TD>
            <TD>2011-09-14T20:14:21Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/471/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/471/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/471/573 [1]</TD>
            <TD>JHKs photometry of a new stellar cluster (Yun+, 2007)</TD>
            <TD>We report the discovery of a new young stellar cluster and molecular cloud located in the far outer Galaxy, seen towards IRAS 06361-0142, and we characterise their properties. Near-infrared images obtained with VLT/ISAAC through JHK filters, millimetre line observations of CO(1-0) obtained with SEST, and VLA 6cm continuum maps obtained from archive data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573#1</TD>
            <TD>2011-09-14T20:14:21Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/471/573</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/471/573</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/471/573 [2]</TD>
            <TD>JHKs photometry of a new stellar cluster (Yun+, 2007)</TD>
            <TD>We report the discovery of a new young stellar cluster and molecular cloud located in the far outer Galaxy, seen towards IRAS 06361-0142, and we characterise their properties. Near-infrared images obtained with VLT/ISAAC through JHK filters, millimetre line observations of CO(1-0) obtained with SEST, and VLA 6cm continuum maps obtained from archive data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573#2</TD>
            <TD>2011-09-14T20:14:21Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/471/573&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/471/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/471/573 [table1]</TD>
            <TD>JHKs photometry of a new stellar cluster (Yun+, 2007)</TD>
            <TD>We report the discovery of a new young stellar cluster and molecular cloud located in the far outer Galaxy, seen towards IRAS 06361-0142, and we characterise their properties. Near-infrared images obtained with VLT/ISAAC through JHK filters, millimetre line observations of CO(1-0) obtained with SEST, and VLA 6cm continuum maps obtained from archive data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573#table1</TD>
            <TD>2011-09-14T20:14:21Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/471/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/471/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/471/573 [1]</TD>
            <TD>JHKs photometry of a new stellar cluster (Yun+, 2007)</TD>
            <TD>We report the discovery of a new young stellar cluster and molecular cloud located in the far outer Galaxy, seen towards IRAS 06361-0142, and we characterise their properties. Near-infrared images obtained with VLT/ISAAC through JHK filters, millimetre line observations of CO(1-0) obtained with SEST, and VLA 6cm continuum maps obtained from archive data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573#1</TD>
            <TD>2011-09-14T20:14:21Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/471/573</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/471/573</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/471/573 [2]</TD>
            <TD>JHKs photometry of a new stellar cluster (Yun+, 2007)</TD>
            <TD>We report the discovery of a new young stellar cluster and molecular cloud located in the far outer Galaxy, seen towards IRAS 06361-0142, and we characterise their properties. Near-infrared images obtained with VLT/ISAAC through JHK filters, millimetre line observations of CO(1-0) obtained with SEST, and VLA 6cm continuum maps obtained from archive data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573#2</TD>
            <TD>2011-09-14T20:14:21Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/471/573&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/471/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/471/573 [table1]</TD>
            <TD>JHKs photometry of a new stellar cluster (Yun+, 2007)</TD>
            <TD>We report the discovery of a new young stellar cluster and molecular cloud located in the far outer Galaxy, seen towards IRAS 06361-0142, and we characterise their properties. Near-infrared images obtained with VLT/ISAAC through JHK filters, millimetre line observations of CO(1-0) obtained with SEST, and VLA 6cm continuum maps obtained from archive data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573#table1</TD>
            <TD>2011-09-14T20:14:21Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/471/573</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/471/573&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/471/573</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/376/1073 [1]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#1</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/376/1073</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/376/1073 [2]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#2</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/376/1073&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/1073 [cluster]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#cluster</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/1073&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/1073 [tableb1]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#tableb1</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/1073&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/376/1073 [1]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#1</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/376/1073</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/376/1073 [2]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#2</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/376/1073&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/1073 [cluster]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#cluster</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/1073&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/1073 [tableb1]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#tableb1</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/1073&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/376/1073 [1]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#1</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/376/1073</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/376/1073 [2]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#2</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/376/1073&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/1073 [cluster]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#cluster</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/1073&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/1073 [tableb1]</TD>
            <TD>Sunyaev-Zel'dovich effect in galaxy clusters (Zemcov+, 2007)</TD>
            <TD>This work has made use of both JCMT archival data and new JCMT observations. For Cl 0152.7-1357, new JCMT data were obtained on 2003 Sept. 28, 29 and 2003 Oct. 17.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073#tableb1</TD>
            <TD>2011-09-14T20:15:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/1073</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/1073&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/1073</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/374/399 [1]</TD>
            <TD>Infrared star clusters with |b|&lt;20{deg} (Froebrich+, 2007)</TD>
            <TD>We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with |b|&lt;20{deg}. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50 per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399#1</TD>
            <TD>2011-09-14T20:15:43Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/374/399</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/374/399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/374/399 [2]</TD>
            <TD>Infrared star clusters with |b|&lt;20{deg} (Froebrich+, 2007)</TD>
            <TD>We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with |b|&lt;20{deg}. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50 per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399#2</TD>
            <TD>2011-09-14T20:15:43Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/374/399&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/374/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/374/399 [tables]</TD>
            <TD>Infrared star clusters with |b|&lt;20{deg} (Froebrich+, 2007)</TD>
            <TD>We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with |b|&lt;20{deg}. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50 per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399#tables</TD>
            <TD>2011-09-14T20:15:43Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/374/399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/374/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/374/399 [1]</TD>
            <TD>Infrared star clusters with |b|&lt;20{deg} (Froebrich+, 2007)</TD>
            <TD>We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with |b|&lt;20{deg}. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50 per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399#1</TD>
            <TD>2011-09-14T20:15:43Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/374/399</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/374/399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/374/399 [2]</TD>
            <TD>Infrared star clusters with |b|&lt;20{deg} (Froebrich+, 2007)</TD>
            <TD>We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with |b|&lt;20{deg}. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50 per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399#2</TD>
            <TD>2011-09-14T20:15:43Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/374/399&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/374/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/374/399 [tables]</TD>
            <TD>Infrared star clusters with |b|&lt;20{deg} (Froebrich+, 2007)</TD>
            <TD>We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with |b|&lt;20{deg}. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50 per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399#tables</TD>
            <TD>2011-09-14T20:15:43Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/374/399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/374/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [1]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#1</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR3 [2]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#2</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/DirectCone?DSACAT=SDSS_DR3&amp;DSATAB=PhotoPrimary&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [3]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#3</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR3 [4]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#4</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [5]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#5</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [6]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#6</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [7]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#7</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [8]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#8</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [9]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#9</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [10]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#10</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR3 [11]</TD>
            <TD>SDSS DR3 - Sloan Digital Sky Survey Data Release 3</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR3 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa#11</TD>
            <TD>2012-07-18T12:34:44Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr3/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/374/399 [1]</TD>
            <TD>Infrared star clusters with |b|&lt;20{deg} (Froebrich+, 2007)</TD>
            <TD>We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with |b|&lt;20{deg}. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50 per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399#1</TD>
            <TD>2011-09-14T20:15:43Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/374/399</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/374/399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/374/399 [2]</TD>
            <TD>Infrared star clusters with |b|&lt;20{deg} (Froebrich+, 2007)</TD>
            <TD>We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with |b|&lt;20{deg}. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50 per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399#2</TD>
            <TD>2011-09-14T20:15:43Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/374/399&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/374/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/374/399 [tables]</TD>
            <TD>Infrared star clusters with |b|&lt;20{deg} (Froebrich+, 2007)</TD>
            <TD>We used star density maps obtained from the Two-Micron All-Sky Survey (2MASS) to obtain a sample of star clusters in the entire Galactic Plane with |b|&lt;20{deg}. A total of 1788 star cluster candidates are identified in this survey. Among those are 681 previously known open clusters and 86 globular clusters. A statistical analysis indicates that our sample of 1021 new cluster candidates has a contamination of about 50 per cent. Star cluster parameters are obtained by fitting a King profile to the star density. These parameters are used to statistically identify probable new globular cluster candidates in our sample. A detailed investigation of the projected distribution of star clusters in the Galaxy demonstrates that they show a clear tendency to cluster on spatial scales in the order of 12-25pc, a typical size for molecular clouds.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399#tables</TD>
            <TD>2011-09-14T20:15:43Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/374/399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/374/399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/374/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/192/6 [1]</TD>
            <TD>A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)</TD>
            <TD>The Local Volume galaxies that were targeted for GALEX imaging were mainly selected from the sample given in Kennicutt et al. (Paper I, 2008, Cat. J/ApJS/178/247). The ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009ApJS..183...67D), which has obtained HST ACS and WFPC2 imaging for a ~4Mpc volume-limited sample, contains about 20 low-luminosity and/or early-type galaxies that were not already included in Paper I, and GALEX data were also obtained for these objects. Observations of the 11HUGS GALEX Legacy program (GI1_047, GI4_095) galaxies have also been extended into the infrared using the Spitzer Space Telescope as part of the Local Volume Legacy survey (Dale et al. 2009ApJ...703..517D).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6#1</TD>
            <TD>2011-09-14T21:18:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/192/6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/192/6 [2]</TD>
            <TD>A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)</TD>
            <TD>The Local Volume galaxies that were targeted for GALEX imaging were mainly selected from the sample given in Kennicutt et al. (Paper I, 2008, Cat. J/ApJS/178/247). The ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009ApJS..183...67D), which has obtained HST ACS and WFPC2 imaging for a ~4Mpc volume-limited sample, contains about 20 low-luminosity and/or early-type galaxies that were not already included in Paper I, and GALEX data were also obtained for these objects. Observations of the 11HUGS GALEX Legacy program (GI1_047, GI4_095) galaxies have also been extended into the infrared using the Spitzer Space Telescope as part of the Local Volume Legacy survey (Dale et al. 2009ApJ...703..517D).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6#2</TD>
            <TD>2011-09-14T21:18:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/192/6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/6 [sample]</TD>
            <TD>A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)</TD>
            <TD>The Local Volume galaxies that were targeted for GALEX imaging were mainly selected from the sample given in Kennicutt et al. (Paper I, 2008, Cat. J/ApJS/178/247). The ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009ApJS..183...67D), which has obtained HST ACS and WFPC2 imaging for a ~4Mpc volume-limited sample, contains about 20 low-luminosity and/or early-type galaxies that were not already included in Paper I, and GALEX data were also obtained for these objects. Observations of the 11HUGS GALEX Legacy program (GI1_047, GI4_095) galaxies have also been extended into the infrared using the Spitzer Space Telescope as part of the Local Volume Legacy survey (Dale et al. 2009ApJ...703..517D).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6#sample</TD>
            <TD>2011-09-14T21:18:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/679/1144 [1]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#1</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/679/1144</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/679/1144 [2]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#2</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/679/1144 [table1]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#table1</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/679/1144 [table3]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#table3</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/679/1144 [table2]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#table2</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/679/1144 [1]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#1</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/679/1144</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/679/1144 [2]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#2</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/679/1144 [table1]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#table1</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/679/1144 [table3]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#table3</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/679/1144 [table2]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#table2</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/192/6 [1]</TD>
            <TD>A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)</TD>
            <TD>The Local Volume galaxies that were targeted for GALEX imaging were mainly selected from the sample given in Kennicutt et al. (Paper I, 2008, Cat. J/ApJS/178/247). The ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009ApJS..183...67D), which has obtained HST ACS and WFPC2 imaging for a ~4Mpc volume-limited sample, contains about 20 low-luminosity and/or early-type galaxies that were not already included in Paper I, and GALEX data were also obtained for these objects. Observations of the 11HUGS GALEX Legacy program (GI1_047, GI4_095) galaxies have also been extended into the infrared using the Spitzer Space Telescope as part of the Local Volume Legacy survey (Dale et al. 2009ApJ...703..517D).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6#1</TD>
            <TD>2011-09-14T21:18:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/192/6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/192/6 [2]</TD>
            <TD>A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)</TD>
            <TD>The Local Volume galaxies that were targeted for GALEX imaging were mainly selected from the sample given in Kennicutt et al. (Paper I, 2008, Cat. J/ApJS/178/247). The ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009ApJS..183...67D), which has obtained HST ACS and WFPC2 imaging for a ~4Mpc volume-limited sample, contains about 20 low-luminosity and/or early-type galaxies that were not already included in Paper I, and GALEX data were also obtained for these objects. Observations of the 11HUGS GALEX Legacy program (GI1_047, GI4_095) galaxies have also been extended into the infrared using the Spitzer Space Telescope as part of the Local Volume Legacy survey (Dale et al. 2009ApJ...703..517D).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6#2</TD>
            <TD>2011-09-14T21:18:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/192/6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/6 [sample]</TD>
            <TD>A GALEX UV imaging survey of nearby galaxies (Lee+, 2011)</TD>
            <TD>The Local Volume galaxies that were targeted for GALEX imaging were mainly selected from the sample given in Kennicutt et al. (Paper I, 2008, Cat. J/ApJS/178/247). The ACS Nearby Galaxy Survey Treasury (ANGST) program (Dalcanton et al. 2009ApJS..183...67D), which has obtained HST ACS and WFPC2 imaging for a ~4Mpc volume-limited sample, contains about 20 low-luminosity and/or early-type galaxies that were not already included in Paper I, and GALEX data were also obtained for these objects. Observations of the 11HUGS GALEX Legacy program (GI1_047, GI4_095) galaxies have also been extended into the infrared using the Spitzer Space Telescope as part of the Local Volume Legacy survey (Dale et al. 2009ApJ...703..517D).</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6#sample</TD>
            <TD>2011-09-14T21:18:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/392/135 [1]</TD>
            <TD>Galaxy clusters from SDSS (Lopes+, 2009)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135#1</TD>
            <TD>2011-10-13T12:20:35Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/392/135</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/135</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/392/135 [2]</TD>
            <TD>Galaxy clusters from SDSS (Lopes+, 2009)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135#2</TD>
            <TD>2011-10-13T12:20:35Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/392/135&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/135</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/135 [clusters]</TD>
            <TD>Galaxy clusters from SDSS (Lopes+, 2009)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135#clusters</TD>
            <TD>2011-10-13T12:20:35Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/135&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/135</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/392/135 [1]</TD>
            <TD>Galaxy clusters from SDSS (Lopes+, 2009)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135#1</TD>
            <TD>2011-10-13T12:20:35Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/392/135</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/135</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/392/135 [2]</TD>
            <TD>Galaxy clusters from SDSS (Lopes+, 2009)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135#2</TD>
            <TD>2011-10-13T12:20:35Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/392/135&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/135</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/135 [clusters]</TD>
            <TD>Galaxy clusters from SDSS (Lopes+, 2009)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135#clusters</TD>
            <TD>2011-10-13T12:20:35Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/135&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/135</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/392/135 [1]</TD>
            <TD>Galaxy clusters from SDSS (Lopes+, 2009)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135#1</TD>
            <TD>2011-10-13T12:20:35Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/392/135</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/135</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/392/135 [2]</TD>
            <TD>Galaxy clusters from SDSS (Lopes+, 2009)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135#2</TD>
            <TD>2011-10-13T12:20:35Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/392/135&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/135</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/135 [clusters]</TD>
            <TD>Galaxy clusters from SDSS (Lopes+, 2009)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135#clusters</TD>
            <TD>2011-10-13T12:20:35Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/135</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/135&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/135</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/179 [1]</TD>
            <TD>AGNs in the Extended Groth Strip Survey (Ramos Almeida+, 2009)</TD>
            <TD>We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179#1</TD>
            <TD>2011-10-19T15:56:43Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/179</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/179</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/179 [2]</TD>
            <TD>AGNs in the Extended Groth Strip Survey (Ramos Almeida+, 2009)</TD>
            <TD>We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179#2</TD>
            <TD>2011-10-19T15:56:43Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/179&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/179</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/179 [sample]</TD>
            <TD>AGNs in the Extended Groth Strip Survey (Ramos Almeida+, 2009)</TD>
            <TD>We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179#sample</TD>
            <TD>2011-10-19T15:56:43Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/179&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/179</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/679/1144 [1]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#1</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/679/1144</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/679/1144 [2]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#2</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/679/1144 [table1]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#table1</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/679/1144 [table3]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#table3</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/679/1144 [table2]</TD>
            <TD>Galaxy clusters in LOS to background QSOs. I. (Lopez+, 2008)</TD>
            <TD>Low-resolution optical spectroscopic follow-up observations of the quasar candidates from the X-ray sample were carried out with the Wide Field Reimaging CCD Camera in long-slit grism mode on the du Pont telescope at Las Campanas Observatory on 2006 March 30 and September 15-16. High-resolution spectroscopy was obtained using the MIKE spectrograph on the Las Campanas Clay 6.5m telescope. We obtained 18 quasar spectra in three runs on 2006 March 18-19 and September 23-24 and 29-30 (see table 1).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144#table2</TD>
            <TD>2011-09-14T21:15:23Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/679/1144</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/679/1144&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/679/1144</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR6 [1]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#1</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/DirectCone?DSACAT=SDSS_DR5&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [2]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#2</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR6 [3]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#3</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [4]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#4</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [5]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#5</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [6]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#6</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [7]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#7</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [8]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#8</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [9]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#9</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR6 [10]</TD>
            <TD>SDSS DR6 SEGUE - Sloan Digital Sky Survey Data Release 6</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR6 SEGUE hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data. This database does not include the entire DR6 release, only the SEGUE portion.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa#10</TD>
            <TD>2012-07-18T12:36:37Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr6/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/684/1143 [1]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#1</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/684/1143</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/684/1143 [2]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#2</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/684/1143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/1143 [table1]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#table1</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/1143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/1143 [table2]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#table2</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/1143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/684/1143 [1]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#1</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/684/1143</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/684/1143 [2]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#2</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/684/1143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/1143 [table1]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#table1</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/1143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/1143 [table2]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#table2</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/1143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/684/1143 [1]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#1</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/684/1143</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/684/1143 [2]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#2</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/684/1143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/1143 [table1]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#table1</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/1143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/1143 [table2]</TD>
            <TD>BHB candidates in the Milky Way (Xue+, 2008)</TD>
            <TD>We derive new constraints on the mass of the Milky Way's dark matter halo, based on 2401 rigorously selected blue horizontal-branch halo stars from SDSS DR6. This sample enables construction of the full line-of-sight velocity distribution at different galactocentric radii. To interpret these distributions, we compare them to matched mock observations drawn from two different cosmological galaxy formation simulations designed to resemble the Milky Way. This procedure results in an estimate of the Milky Way's circular velocity curve to ~60kpc, which is found to be slightly falling from the adopted value of 220km/s at the Sun's location, and implies M(&lt;60kpc)=(4.0+/-0.7)x10^11^M_{sun}_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143#table2</TD>
            <TD>2011-09-14T21:15:24Z</TD>
            <TD>#Abundances#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/1143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/1143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/1143</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/410/166 [1]</TD>
            <TD>Morphological types from Galaxy Zoo 1 (Lintott+, 2011)</TD>
            <TD>++++Lrecl of file 'table3.dat' (87) increased to 105 %B Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166#1</TD>
            <TD>2011-09-14T21:17:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/410/166</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/166</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/410/166 [2]</TD>
            <TD>Morphological types from Galaxy Zoo 1 (Lintott+, 2011)</TD>
            <TD>++++Lrecl of file 'table3.dat' (87) increased to 105 %B Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166#2</TD>
            <TD>2011-09-14T21:17:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/410/166&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/166</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/410/166 [galaxies]</TD>
            <TD>Morphological types from Galaxy Zoo 1 (Lintott+, 2011)</TD>
            <TD>++++Lrecl of file 'table3.dat' (87) increased to 105 %B Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166#galaxies</TD>
            <TD>2011-09-14T21:17:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/410/166&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/166</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/410/166 [1]</TD>
            <TD>Morphological types from Galaxy Zoo 1 (Lintott+, 2011)</TD>
            <TD>++++Lrecl of file 'table3.dat' (87) increased to 105 %B Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166#1</TD>
            <TD>2011-09-14T21:17:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/410/166</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/166</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/410/166 [2]</TD>
            <TD>Morphological types from Galaxy Zoo 1 (Lintott+, 2011)</TD>
            <TD>++++Lrecl of file 'table3.dat' (87) increased to 105 %B Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166#2</TD>
            <TD>2011-09-14T21:17:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/410/166&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/166</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/410/166 [galaxies]</TD>
            <TD>Morphological types from Galaxy Zoo 1 (Lintott+, 2011)</TD>
            <TD>++++Lrecl of file 'table3.dat' (87) increased to 105 %B Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166#galaxies</TD>
            <TD>2011-09-14T21:17:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/410/166&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/166</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/410/166 [1]</TD>
            <TD>Morphological types from Galaxy Zoo 1 (Lintott+, 2011)</TD>
            <TD>++++Lrecl of file 'table3.dat' (87) increased to 105 %B Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166#1</TD>
            <TD>2011-09-14T21:17:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/410/166</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/166</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/410/166 [2]</TD>
            <TD>Morphological types from Galaxy Zoo 1 (Lintott+, 2011)</TD>
            <TD>++++Lrecl of file 'table3.dat' (87) increased to 105 %B Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166#2</TD>
            <TD>2011-09-14T21:17:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/410/166&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/166</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/410/166 [galaxies]</TD>
            <TD>Morphological types from Galaxy Zoo 1 (Lintott+, 2011)</TD>
            <TD>++++Lrecl of file 'table3.dat' (87) increased to 105 %B Morphology is a powerful indicator of a galaxy's dynamical and merger history. It is strongly correlated with many physical parameters, including mass, star formation history and the distribution of mass. The Galaxy Zoo project collected simple morphological classifications of nearly 900000 galaxies drawn from the Sloan Digital Sky Survey, contributed by hundreds of thousands of volunteers. This large number of classifications allows us to exclude classifier error, and measure the influence of subtle biases inherent in morphological classification. This paper presents the data collected by the project, alongside measures of classification accuracy and bias. The data are now publicly available and full catalogues can be downloaded in electronic format from http://data.galaxyzoo.org .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166#galaxies</TD>
            <TD>2011-09-14T21:17:46Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/166</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/410/166&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/166</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS-DR1</TD>
            <TD>Sloan Digitized Sky Survey(DR1)</TD>
            <TD>The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey</TD>
            <TD>The Johns Hopkins Univer</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/services/DR1CONE#1</TD>
            <TD>2011-09-14T18:11:54Z</TD>
            <TD>#Stars#Survey#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>DR1</TD>
            <TD>ivo://sdss.jhu/services/DR1CONE</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyserver.sdss.org/vo/dr1cone/sdssConeSearch.asmx/ConeSearch?</TD>
            <TD>1</TD>
            <TD>5000</TD>
            <TD />
            <TD>http://www.sdss.jhu.edu/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAS</TD>
            <TD>Infrared Astronomical Satellite</TD>
            <TD>Infrared Astronomical Satellite OpenSkyNode The Infrared Astronomical Satellite (IRAS) was a joint project of the US, UK and the Netherlands. The IRAS mission performed an unbiased, sensitive all sky survey at 12, 25, 60 and 100 µm. IRAS increased the number of cataloged astronomical sources by about 70%, detecting about 350,000 infrared sources. IRAS discoveries included a disk of dust grains around the star Vega, six new comets, and very strong infrared emission from interacting galaxies as well as wisps of warm dust called infrared cirrus which could be found in almost every direction of space. IRAS also revealed for the first time the core of our galaxy, the Milky Way</TD>
            <TD>JHU</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://sdss.jhu/openskynode/IRAS#1</TD>
            <TD>2011-09-14T18:12:03Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD />
            <TD>15</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/IRAS</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/iras/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NVSS</TD>
            <TD>NRAO/VLA Sky Survey</TD>
            <TD>The NRAO VLA Sky Survey (NVSS) is a 1.4 GHz continuum survey covering the entire sky north of -40 deg declination. A detailed description appears in the 1998 May issue of The Astronomical Journal (Condon, J. J., Cotton, W. D., Greisen, E. W., Yin, Q. F., Perley, R. A., Taylor, G. B., &amp; Broderick, J. J. 1998, AJ, 115, 1693). The principal NVSS data products are: A set of 2326 continuum image ``cubes,'' each covering 4 deg X 4 deg with three planes containing the Stokes I, Q, and U images. These images were made with a relatively large restoring beam (45 arcsec FWHM) to yield the high surface-brightness sensitivity needed for completeness and photometric accuracy. Their rms brightness fluctuations are about 0.45 mJy/beam = 0.14 K (Stokes I) and 0.29 mJy/beam = 0.09 K (Stokes Q and U). The rms uncertainties in right ascension and declination vary from &lt; 1 arcsec for relatively strong (S &gt; 15 mJy) point sources to 7 arcsec for the faintest (S = 2.3 mJy) detectable sources. The completene</TD>
            <TD>JHU</TD>
            <TD>#Radio#</TD>
            <TD>ivo://sdss.jhu/openskynode/NVSS#1</TD>
            <TD>2011-09-14T18:12:04Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#Radio#</TD>
            <TD />
            <TD />
            <TD>5</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/NVSS</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/nvss/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PSCz</TD>
            <TD>IRAS PSCz Redshift Survey Catalog</TD>
            <TD>The Infrared Astronomical Satellite Point Source Catalog Redshift Survey is a redshift survey of IRAS galaxies to 0.6 Jy. It contains 15,411 galaxies (14,677 with redshifts) over 84% of the sky.</TD>
            <TD>JHU</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://sdss.jhu/openskynode/PSCZ#1</TD>
            <TD>2011-09-14T18:12:04Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD />
            <TD>1</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/PSCZ</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/pscz/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [1]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#1</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=PhotoObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS DR8 [2]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#2</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/DirectCone?DSACAT=SDSS_DR8&amp;DSATAB=SpecObjAll&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [3]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#3</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>SDSS DR8 [4]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#4</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [5]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#5</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [6]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#6</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [7]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#7</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [8]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#8</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [9]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#9</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [10]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#10</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSS DR8 [11]</TD>
            <TD>SDSS DR8 - Sloan Digital Sky Survey Data Release 8</TD>
            <TD>This is an AstroGrid Dataset Access installation of the Sloan Digital Sky Survey (SDSS) DR8 hosted by the Wide Field Astronomy Unit (WFAU), University of Edinburgh. WFAU would like to thank John Hopkins University and the University of Chicago for permission to host the data.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa#11</TD>
            <TD>2012-07-18T12:37:33Z</TD>
            <TD>#Stars,Survey,Galaxy#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/sdssdr8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/sdssdr8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.sdss.org/dr8/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GALEX</TD>
            <TD>Galaxy Evolution Explorer</TD>
            <TD>The Galaxy Evolution Explorer (GALEX), a NASA Small Explorer mission, is performing the first all-sky, deep imaging and spectroscopic ultraviolet surveys in space. The prime goal of GALEX is to study star formation in galaxies and its evolution with time.</TD>
            <TD>Space Telescope Science Institute</TD>
            <TD>#UV#</TD>
            <TD>ivo://archive.stsci.edu/cone/galex#1</TD>
            <TD>2011-09-14T17:51:41Z</TD>
            <TD>#Cosmology#Galaxies#Star Formation#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>V1.0</TD>
            <TD>ivo://archive.stsci.edu/cone/galex</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://galex.stsci.edu/gxWS/ConeSearch/gxConeSearch.aspx?</TD>
            <TD>1</TD>
            <TD>0</TD>
            <TD />
            <TD>http://galex.stsci.edu</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>GALEX</TD>
            <TD>Galaxy Evolution Explorer</TD>
            <TD>The Galaxy Evolution Explorer (GALEX), a NASA Small Explorer mission, is performing the first all-sky, deep imaging and spectroscopic ultraviolet surveys in space. The prime goal of GALEX is to study star formation in galaxies and its evolution with time.</TD>
            <TD>Space Telescope Science Institute</TD>
            <TD>#UV#</TD>
            <TD>ivo://archive.stsci.edu/siap/galex#1</TD>
            <TD>2011-09-14T17:51:42Z</TD>
            <TD>#Cosmology#Galaxies#Star Formation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>V1.0</TD>
            <TD>ivo://archive.stsci.edu/siap/galex</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://galex.stsci.edu/gxWS/SIAP/gxSIAP.aspx?</TD>
            <TD />
            <TD>0</TD>
            <TD />
            <TD>http://galex.stsci.edu</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS-DR2</TD>
            <TD>Sloan Digitized Sky Survey(DR2)</TD>
            <TD>The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey</TD>
            <TD>The Johns Hopkins University</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/services/DR2CONE#1</TD>
            <TD>2011-09-14T17:51:43Z</TD>
            <TD>#Stars#Survey#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>DR2</TD>
            <TD>ivo://sdss.jhu/services/DR2CONE</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyserver.sdss.org/vo/dr2cone/sdssConeSearch.asmx/ConeSearch?</TD>
            <TD>1</TD>
            <TD>5000</TD>
            <TD />
            <TD>http://www.sdss.jhu.edu/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>TWOMASS</TD>
            <TD>Two Micron All Sky Survey</TD>
            <TD>The Two Micron All Sky Survey (2MASS) project is designed to close the gap between our current technical capability and our knowledge of the near-infrared sky. In addition to providing a context for the interpretation of results obtained at infrared and other wavelengths, 2MASS is providing direct answers to immediate questions on the large- scale structure of the Milky Way and the Local Universe. The optimal use of the next generation of infrared space missions, such as HST/NICMOS, the Space Infrared Telescope Facility (SIRTF), and the Next Generation Space Telescope (NGST), as well as powerful ground- based facilities, such as Keck I, Keck II, and Gemini, require a new census with vastly improved sensitivity and astrometric accuracy than that previously available. To achieve these goals, 2MASS has uniformly scanned the entire sky in three near-infrared bands to detect and characterize point sources brighter than about 1 mJy in each band, with signal-to-noise ratio (SNR) greater tha</TD>
            <TD>JHU</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://sdss.jhu/skynode/2mass#1</TD>
            <TD>2011-09-14T17:51:54Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD />
            <TD>0.800000011920929</TD>
            <TD />
            <TD>ivo://sdss.jhu/skynode/2mass</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/TWOMASS/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [1]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#1</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [2]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#2</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [3]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#3</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [4]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#4</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [5]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#5</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [6]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#6</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [7]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#7</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [8]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#8</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [9]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#9</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR2 [10]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#10</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/DirectCone?DSACAT=UKIDSS_DR2&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [11]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#11</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR2 [12]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#12</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [13]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#13</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [14]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#14</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [15]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#15</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [16]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#16</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [17]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#17</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [18]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#18</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR2 [19]</TD>
            <TD>UKIDSS DR2 - UKIRT Infrared Deep Sky Survey Data Release 2</TD>
            <TD>This DSA hosts data release 2 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa#19</TD>
            <TD>2012-07-18T12:41:11Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VVDS_CDFS</TD>
            <TD>VIMOS VLT Deep Survey around the Chandra Deep Field South (CDFS)</TD>
            <TD>This Cone Search service allows to query on the VVDS-CDFS catalog available at http://cencosw.oamp.fr.</TD>
            <TD>INAF-IASF Milano</TD>
            <TD>#Optical#</TD>
            <TD>ivo://obelix.lambrate.inaf.it/vodb/CONE_CDFS#1</TD>
            <TD>2011-09-14T17:51:55Z</TD>
            <TD>#Galaxy#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://obelix.lambrate.inaf.it/vodb/CONE_CDFS</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://obelix.lambrate.inaf.it/vodb/ConeSearch?CAT=CDFS&amp;</TD>
            <TD>0</TD>
            <TD>1599</TD>
            <TD />
            <TD>http://cencosw.oamp.fr</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/96/175 [1]</TD>
            <TD>Kinematics of Metal-Poor Stars (Beers+ 1995)</TD>
            <TD>We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] &lt;= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 &lt;= [Fe/H] &lt;= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage &amp; Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] &lt;= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 &lt;= [Fe/H] &lt;= -0.6 and |z| &lt;= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] &lt;= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 &lt;= [Fe/H] &lt;= -1.5 and [Fe/H] &lt;= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r &gt; 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175#1</TD>
            <TD>2011-09-14T18:37:28Z</TD>
            <TD>#Abundances#Positional_Data#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/96/175</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/175</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/96/175 [2]</TD>
            <TD>Kinematics of Metal-Poor Stars (Beers+ 1995)</TD>
            <TD>We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] &lt;= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 &lt;= [Fe/H] &lt;= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage &amp; Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] &lt;= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 &lt;= [Fe/H] &lt;= -0.6 and |z| &lt;= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] &lt;= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 &lt;= [Fe/H] &lt;= -1.5 and [Fe/H] &lt;= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r &gt; 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175#2</TD>
            <TD>2011-09-14T18:37:28Z</TD>
            <TD>#Abundances#Positional_Data#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/96/175&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/175</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/175 [table2]</TD>
            <TD>Kinematics of Metal-Poor Stars (Beers+ 1995)</TD>
            <TD>We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] &lt;= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 &lt;= [Fe/H] &lt;= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage &amp; Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] &lt;= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 &lt;= [Fe/H] &lt;= -0.6 and |z| &lt;= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] &lt;= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 &lt;= [Fe/H] &lt;= -1.5 and [Fe/H] &lt;= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r &gt; 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175#table2</TD>
            <TD>2011-09-14T18:37:28Z</TD>
            <TD>#Abundances#Positional_Data#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/175&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/175</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/96/175 [1]</TD>
            <TD>Kinematics of Metal-Poor Stars (Beers+ 1995)</TD>
            <TD>We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] &lt;= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 &lt;= [Fe/H] &lt;= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage &amp; Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] &lt;= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 &lt;= [Fe/H] &lt;= -0.6 and |z| &lt;= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] &lt;= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 &lt;= [Fe/H] &lt;= -1.5 and [Fe/H] &lt;= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r &gt; 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175#1</TD>
            <TD>2011-09-14T18:37:28Z</TD>
            <TD>#Abundances#Positional_Data#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/96/175</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/175</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/96/175 [2]</TD>
            <TD>Kinematics of Metal-Poor Stars (Beers+ 1995)</TD>
            <TD>We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] &lt;= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 &lt;= [Fe/H] &lt;= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage &amp; Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] &lt;= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 &lt;= [Fe/H] &lt;= -0.6 and |z| &lt;= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] &lt;= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 &lt;= [Fe/H] &lt;= -1.5 and [Fe/H] &lt;= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r &gt; 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175#2</TD>
            <TD>2011-09-14T18:37:28Z</TD>
            <TD>#Abundances#Positional_Data#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/96/175&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/175</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/175 [table2]</TD>
            <TD>Kinematics of Metal-Poor Stars (Beers+ 1995)</TD>
            <TD>We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] &lt;= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 &lt;= [Fe/H] &lt;= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage &amp; Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] &lt;= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 &lt;= [Fe/H] &lt;= -0.6 and |z| &lt;= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] &lt;= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 &lt;= [Fe/H] &lt;= -1.5 and [Fe/H] &lt;= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r &gt; 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175#table2</TD>
            <TD>2011-09-14T18:37:28Z</TD>
            <TD>#Abundances#Positional_Data#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/175&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/175</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/96/175 [1]</TD>
            <TD>Kinematics of Metal-Poor Stars (Beers+ 1995)</TD>
            <TD>We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] &lt;= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 &lt;= [Fe/H] &lt;= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage &amp; Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] &lt;= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 &lt;= [Fe/H] &lt;= -0.6 and |z| &lt;= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] &lt;= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 &lt;= [Fe/H] &lt;= -1.5 and [Fe/H] &lt;= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r &gt; 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175#1</TD>
            <TD>2011-09-14T18:37:28Z</TD>
            <TD>#Abundances#Positional_Data#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/96/175</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/175</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/96/175 [2]</TD>
            <TD>Kinematics of Metal-Poor Stars (Beers+ 1995)</TD>
            <TD>We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] &lt;= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 &lt;= [Fe/H] &lt;= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage &amp; Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] &lt;= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 &lt;= [Fe/H] &lt;= -0.6 and |z| &lt;= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] &lt;= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 &lt;= [Fe/H] &lt;= -1.5 and [Fe/H] &lt;= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r &gt; 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175#2</TD>
            <TD>2011-09-14T18:37:28Z</TD>
            <TD>#Abundances#Positional_Data#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/96/175&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/175</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/96/175 [table2]</TD>
            <TD>Kinematics of Metal-Poor Stars (Beers+ 1995)</TD>
            <TD>We discuss the kinematic properties of a sample of 1936 Galactic stars, selected without kinematic bias, and with abundances [Fe/H] &lt;= -0.6. The stars selected for this study all have measured radial velocities, and the majority have abundances determined from spectroscopic and narrow-/intermediate-band photometric techniques. In contrast to previous examinations of the kinematics of the metal-poor stars in the Galaxy, our sample contains large numbers of stars that are located at distances in excess of 1 kpc from the Galactic plane. Thus, a much clearer picture of the nature of the metal-deficient populations in the Galaxy can now be drawn. Our present data can be well described in terms of a two-component kinematic model consisting of a thick disk, rotating at roughly 200 km/s (independent of metal abundance), and an essentially nonrotating halo. The kinematics of these two components suggest a very broad overlap in metallicity; the thick disk is shown to possess an extremely metal-weak tail, extending to abundances even lower than previously reported, down to at least [Fe/H] ~ -2.0. A "minimal-assumptions" maximum-likelihood model is used to show that below [Fe/H] = -1.5 roughly 30% of stars in the solar neighbourhood can be kinematically associated with the thick disk. Over the metallicity interval -1.6 &lt;= [Fe/H] &lt;= -1.0, the thick-disk proportion rises to 60%. This fraction is only slightly smaller than contribution of thick-disk stars derived by Morrison, Flynn, and Freeman in the same metallicity interval (80%). Our confirmation that significant numbers of stars with thick-disk-like kinematics exist in the solar neighbourhood at arbitrarily low metal abundance suggests that previous disagreements about the correlation of population rotation velocities and metal abundance (e.g. Sandage &amp; Fouts vs. Norris) may be due primarily to the selection criteria employed, and the resulting different contribution of metal-weak thick-disk stars to the respective data sets. The non-Gaussian nature of the velocity distribution of extremely metal-poor stars ([Fe/H] &lt;= -1.5) in the directions of the Galactic poles reported by previous workers can also be understood as a consequence of the overlap between a cold metal-weak thick-disk population and a hot halo population. A maximum-likelihood technique has been developed in order to estimate the velocity ellipsoids of the thick-disk and halo components of the Galaxy. From the 349 stars in our sample with -1.0 &lt;= [Fe/H] &lt;= -0.6 and |z| &lt;= 1 kpc, the velocity ellipsoid of the thick disk is (sigma_U, sigma_V, sigma_W) = (63 +/- 7, 42 +/- 4, 38 +/- 4) km/s. These values are in remarkably good accord with the predicted thick-disk velocity ellipsoid obtained by Quinn, Hernquist, and Fullagar from simulations of a satellite-merger formation scenario. Based on this velocity ellipsoid, a radial scale length for thick-disk stars of h_R = 4.7 +/- 0.5 kpc is obtained, larger than reported by Morrison, and similar to the value obtained for the old-disk population. However, the apparent equality of sigma_V and sigma_W is evidence that the thick disk is kinematically distinct from the old-disk population, where sigma_V:sigma_W ~ 2^{1/2}:1. We find a substantially smaller asymmetric-drift velocity gradient for presumed thick-disk stars (delta Vrot/delta |z| = -13 +/- 6 km/s/kpc) than reported by Majewski (delta Vrot/delta |z| = -21 +/- 1 km/s/kpc). From 887 stars in our sample with [Fe/H] &lt;= -1.5 the local velocity ellipsoid of the halo is (sigma_r, sigma_phi, sigma_theta) = (153 +/- 10, 93 +/- 18, 107 +/- 7) km/s, that is, strongly radially peaked, as indicated by previous studies. We find little difference in the velocity ellipsoids of this sample when it is split into two roughly equal pieces with -2.2 &lt;= [Fe/H] &lt;= -1.5 and [Fe/H] &lt;= -2.2, which indicates a lack of radial metallicity gradient in the halo, as found from studies of the Galactic globular cluster system. The velocity ellipsoid obtained from the small number of stars in our sample with Galactocentric distances r &gt; 10 kpc (N = 61) is (sigma_r, sigma_phi, sigma_theta) = (115 +/- 18, 138 +/- 78, 110 +/- 24) km/s, much less radially elongated than found for the local sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175#table2</TD>
            <TD>2011-09-14T18:37:28Z</TD>
            <TD>#Abundances#Positional_Data#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/96/175</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/96/175&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/96/175</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>I/129 [1]</TD>
            <TD>Parallaxes and Proper Motions near SGP (Murray+ 1986)</TD>
            <TD>The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/129#1</TD>
            <TD>2011-09-14T18:12:49Z</TD>
            <TD>#Parallaxes#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/I/129</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=I/129</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/129</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>I/129 [2]</TD>
            <TD>Parallaxes and Proper Motions near SGP (Murray+ 1986)</TD>
            <TD>The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/129#2</TD>
            <TD>2011-09-14T18:12:49Z</TD>
            <TD>#Parallaxes#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/I/129</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=I/129&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>I/129 [catalog]</TD>
            <TD>Parallaxes and Proper Motions near SGP (Murray+ 1986)</TD>
            <TD>The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/129#catalog</TD>
            <TD>2011-09-14T18:12:49Z</TD>
            <TD>#Parallaxes#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/I/129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=I/129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>I/129 [1]</TD>
            <TD>Parallaxes and Proper Motions near SGP (Murray+ 1986)</TD>
            <TD>The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/129#1</TD>
            <TD>2011-09-14T18:12:49Z</TD>
            <TD>#Parallaxes#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/I/129</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=I/129</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/129</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>I/129 [2]</TD>
            <TD>Parallaxes and Proper Motions near SGP (Murray+ 1986)</TD>
            <TD>The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/129#2</TD>
            <TD>2011-09-14T18:12:49Z</TD>
            <TD>#Parallaxes#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/I/129</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=I/129&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>I/129 [catalog]</TD>
            <TD>Parallaxes and Proper Motions near SGP (Murray+ 1986)</TD>
            <TD>The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/129#catalog</TD>
            <TD>2011-09-14T18:12:49Z</TD>
            <TD>#Parallaxes#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/I/129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=I/129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>I/129 [1]</TD>
            <TD>Parallaxes and Proper Motions near SGP (Murray+ 1986)</TD>
            <TD>The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/129#1</TD>
            <TD>2011-09-14T18:12:49Z</TD>
            <TD>#Parallaxes#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/I/129</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=I/129</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/129</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>I/129 [2]</TD>
            <TD>Parallaxes and Proper Motions near SGP (Murray+ 1986)</TD>
            <TD>The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/129#2</TD>
            <TD>2011-09-14T18:12:49Z</TD>
            <TD>#Parallaxes#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/I/129</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=I/129&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>I/129 [catalog]</TD>
            <TD>Parallaxes and Proper Motions near SGP (Murray+ 1986)</TD>
            <TD>The catalog contains 6125 stars brighter than B=17.5, V=17.0 in the south galactic cap. The data have been obtained using the UK Schmidt telescope between 1975 and 1981. The plates were measured on the GALAXY machine at RGO. External errors of the parallaxes range between -/+0.012 and -/+0.017 arcsec according to magnitude. Internal proper motion errors range from -/+0.006 and -/+0.008 arcsec. In addition to the positions, proper motions, and parallaxes, the photometric data include B and V.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/129#catalog</TD>
            <TD>2011-09-14T18:12:49Z</TD>
            <TD>#Parallaxes#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Nov-1995</TD>
            <TD>ivo://CDS.VizieR/I/129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=I/129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/211 [1]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#1</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/211 [2]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#2</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/211 [spectro]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#spectro</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/211 [catalog]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#catalog</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/211 [ircam]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#ircam</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/211 [1]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#1</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/211 [2]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#2</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/211 [spectro]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#spectro</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/211 [catalog]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#catalog</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/211 [ircam]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#ircam</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/211 [1]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#1</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/211 [2]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#2</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/211 [spectro]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#spectro</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/211 [catalog]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#catalog</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/211 [ircam]</TD>
            <TD>K-band survey in high galactic latitude (Glazebrook+ 1994)</TD>
            <TD>The survey is a high galactic latitude, large area (552 square arcmin) blank-field sample to a 5{sigma} limit of K=17.3mag. Star-galaxy discrimination is performed. The infrared observations were made over the period 1987-1988, using the infrared camera IRCAM at the 3.8m UKIRTelescope at Mauna Kea, Hawai. The pixel size is 1.2arcsec. The redshift survey (spectro.dat) concerns 124 galaxies of the survey, and was carried out on the Anglo-Australian telescope and the William Herschel telescope at La Palma over the period 1990-1992, with a multi-fibre spectrograph for the brighter objects (R&lt;19), long and multi-slit spectrographs for fainter objects.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/211#ircam</TD>
            <TD>2011-09-14T18:13:33Z</TD>
            <TD>#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/II/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/303/893 [1]</TD>
            <TD>Planetary nebulae with WR-type nuclei (Gorny+, 1995)</TD>
            <TD>A recent systematic search of Wolf-Rayet features in the spectra of Galactic planetary nebulae has increased the list of objects that are known to have WR-type nuclei to about 50. We have compared their nebular properties with those of the other planetary nebulae in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/893#1</TD>
            <TD>2011-09-14T18:14:53Z</TD>
            <TD>#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/893</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/303/893</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/893</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/303/893 [2]</TD>
            <TD>Planetary nebulae with WR-type nuclei (Gorny+, 1995)</TD>
            <TD>A recent systematic search of Wolf-Rayet features in the spectra of Galactic planetary nebulae has increased the list of objects that are known to have WR-type nuclei to about 50. We have compared their nebular properties with those of the other planetary nebulae in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/893#2</TD>
            <TD>2011-09-14T18:14:53Z</TD>
            <TD>#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/893</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/303/893&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/893</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/303/893 [1]</TD>
            <TD>Planetary nebulae with WR-type nuclei (Gorny+, 1995)</TD>
            <TD>A recent systematic search of Wolf-Rayet features in the spectra of Galactic planetary nebulae has increased the list of objects that are known to have WR-type nuclei to about 50. We have compared their nebular properties with those of the other planetary nebulae in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/893#1</TD>
            <TD>2011-09-14T18:14:53Z</TD>
            <TD>#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/893</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/303/893</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/893</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/303/893 [2]</TD>
            <TD>Planetary nebulae with WR-type nuclei (Gorny+, 1995)</TD>
            <TD>A recent systematic search of Wolf-Rayet features in the spectra of Galactic planetary nebulae has increased the list of objects that are known to have WR-type nuclei to about 50. We have compared their nebular properties with those of the other planetary nebulae in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/893#2</TD>
            <TD>2011-09-14T18:14:53Z</TD>
            <TD>#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/893</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/303/893&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/893</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/314/43 [1]</TD>
            <TD>NGC 5548 Profile variability (Kollatschny+ 1996)</TD>
            <TD>Optical emission line intensities of the variable Seyfert 1 galaxy NGC 5548 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/314/43#1</TD>
            <TD>2011-09-14T18:15:23Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/314/43</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/314/43</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/314/43</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/314/43 [2]</TD>
            <TD>NGC 5548 Profile variability (Kollatschny+ 1996)</TD>
            <TD>Optical emission line intensities of the variable Seyfert 1 galaxy NGC 5548 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/314/43#2</TD>
            <TD>2011-09-14T18:15:23Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/314/43</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/314/43&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/314/43</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/314/43 [1]</TD>
            <TD>NGC 5548 Profile variability (Kollatschny+ 1996)</TD>
            <TD>Optical emission line intensities of the variable Seyfert 1 galaxy NGC 5548 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/314/43#1</TD>
            <TD>2011-09-14T18:15:23Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/314/43</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/314/43</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/314/43</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/314/43 [2]</TD>
            <TD>NGC 5548 Profile variability (Kollatschny+ 1996)</TD>
            <TD>Optical emission line intensities of the variable Seyfert 1 galaxy NGC 5548 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/314/43#2</TD>
            <TD>2011-09-14T18:15:23Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/314/43</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/314/43&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/314/43</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [1]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#1</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [2]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#2</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [3]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#3</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [4]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#4</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [5]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#5</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [6]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#6</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [7]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#7</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [8]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#8</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [9]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#9</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR1 [10]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#10</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/DirectCone?DSACAT=UKIDSS_DR1&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [11]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#11</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR1 [12]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#12</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [13]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#13</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [14]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#14</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [15]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#15</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [16]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#16</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [17]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#17</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [18]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#18</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR1 [19]</TD>
            <TD>UKIDSS DR1 - UKIRT Infrared Deep Sky Survey Data Release 1</TD>
            <TD>This DSA hosts data release 1 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa#19</TD>
            <TD>2012-07-18T12:40:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/110/19 [1]</TD>
            <TD>Kinematical observations of pairs of galaxies (Davoust+ 1995)</TD>
            <TD>We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19#1</TD>
            <TD>2011-09-14T18:17:44Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/110/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/110/19 [2]</TD>
            <TD>Kinematical observations of pairs of galaxies (Davoust+ 1995)</TD>
            <TD>We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19#2</TD>
            <TD>2011-09-14T18:17:44Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/110/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/110/19 [table2]</TD>
            <TD>Kinematical observations of pairs of galaxies (Davoust+ 1995)</TD>
            <TD>We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19#table2</TD>
            <TD>2011-09-14T18:17:44Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/110/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/110/19 [1]</TD>
            <TD>Kinematical observations of pairs of galaxies (Davoust+ 1995)</TD>
            <TD>We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19#1</TD>
            <TD>2011-09-14T18:17:44Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/110/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/110/19 [2]</TD>
            <TD>Kinematical observations of pairs of galaxies (Davoust+ 1995)</TD>
            <TD>We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19#2</TD>
            <TD>2011-09-14T18:17:44Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/110/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/110/19 [table2]</TD>
            <TD>Kinematical observations of pairs of galaxies (Davoust+ 1995)</TD>
            <TD>We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19#table2</TD>
            <TD>2011-09-14T18:17:44Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/110/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/110/19 [1]</TD>
            <TD>Kinematical observations of pairs of galaxies (Davoust+ 1995)</TD>
            <TD>We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19#1</TD>
            <TD>2011-09-14T18:17:44Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/110/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/110/19 [2]</TD>
            <TD>Kinematical observations of pairs of galaxies (Davoust+ 1995)</TD>
            <TD>We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19#2</TD>
            <TD>2011-09-14T18:17:44Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/110/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/110/19 [table2]</TD>
            <TD>Kinematical observations of pairs of galaxies (Davoust+ 1995)</TD>
            <TD>We present new radial velocities for 203 galaxies in 105 pairs and 2 triplets. The majority are close pairs of early-type galaxies; there are also pairs including a giant spiral galaxy (generally M51 type), and a few are wide pairs of early-type galaxies. Most velocities were measured from the absorption lines in the region of Mgb; emission-line velocities are also given for 22 galaxies. The velocity of one component only was measured in 13 (generally hierarchical) pairs. Velocity dispersions were measured for a subsample of 18 close pairs of early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19#table2</TD>
            <TD>2011-09-14T18:17:44Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/110/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/119/391 [1]</TD>
            <TD>Gunn photometry of seven clusters of galaxies (Molinari+ 1996)</TD>
            <TD>Gunn g, r, i photometry for the 7 clusters MRC0254-274, Cl0317+15, MS0418.3-3 844, Cl1141-283, A1689, A3594, S0781B is presented. For each cluster we derived the spatial distribution properties obtaining the core radius and the concentration parameters. Color properties of the cluster galaxy population are also briefly discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/119/391#1</TD>
            <TD>2011-09-14T18:19:21Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/119/391</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/119/391</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/119/391</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/119/391 [2]</TD>
            <TD>Gunn photometry of seven clusters of galaxies (Molinari+ 1996)</TD>
            <TD>Gunn g, r, i photometry for the 7 clusters MRC0254-274, Cl0317+15, MS0418.3-3 844, Cl1141-283, A1689, A3594, S0781B is presented. For each cluster we derived the spatial distribution properties obtaining the core radius and the concentration parameters. Color properties of the cluster galaxy population are also briefly discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/119/391#2</TD>
            <TD>2011-09-14T18:19:21Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/119/391</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/119/391&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/119/391</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/119/391 [1]</TD>
            <TD>Gunn photometry of seven clusters of galaxies (Molinari+ 1996)</TD>
            <TD>Gunn g, r, i photometry for the 7 clusters MRC0254-274, Cl0317+15, MS0418.3-3 844, Cl1141-283, A1689, A3594, S0781B is presented. For each cluster we derived the spatial distribution properties obtaining the core radius and the concentration parameters. Color properties of the cluster galaxy population are also briefly discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/119/391#1</TD>
            <TD>2011-09-14T18:19:21Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/119/391</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/119/391</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/119/391</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/119/391 [2]</TD>
            <TD>Gunn photometry of seven clusters of galaxies (Molinari+ 1996)</TD>
            <TD>Gunn g, r, i photometry for the 7 clusters MRC0254-274, Cl0317+15, MS0418.3-3 844, Cl1141-283, A1689, A3594, S0781B is presented. For each cluster we derived the spatial distribution properties obtaining the core radius and the concentration parameters. Color properties of the cluster galaxy population are also briefly discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/119/391#2</TD>
            <TD>2011-09-14T18:19:21Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/119/391</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/119/391&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/119/391</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/124/283 [1]</TD>
            <TD>BR magnitude and redshift of A1300 (Pierre+ 1997)</TD>
            <TD>We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15&lt;=z&lt;=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283#1</TD>
            <TD>2011-09-14T18:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/124/283</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/283</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/124/283 [2]</TD>
            <TD>BR magnitude and redshift of A1300 (Pierre+ 1997)</TD>
            <TD>We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15&lt;=z&lt;=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283#2</TD>
            <TD>2011-09-14T18:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/124/283&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/283</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/124/283 [table4]</TD>
            <TD>BR magnitude and redshift of A1300 (Pierre+ 1997)</TD>
            <TD>We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15&lt;=z&lt;=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283#table4</TD>
            <TD>2011-09-14T18:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/124/283&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/283</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/124/283 [1]</TD>
            <TD>BR magnitude and redshift of A1300 (Pierre+ 1997)</TD>
            <TD>We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15&lt;=z&lt;=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283#1</TD>
            <TD>2011-09-14T18:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/124/283</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/283</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/124/283 [2]</TD>
            <TD>BR magnitude and redshift of A1300 (Pierre+ 1997)</TD>
            <TD>We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15&lt;=z&lt;=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283#2</TD>
            <TD>2011-09-14T18:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/124/283&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/283</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/124/283 [table4]</TD>
            <TD>BR magnitude and redshift of A1300 (Pierre+ 1997)</TD>
            <TD>We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15&lt;=z&lt;=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283#table4</TD>
            <TD>2011-09-14T18:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/124/283&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/283</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/124/283 [1]</TD>
            <TD>BR magnitude and redshift of A1300 (Pierre+ 1997)</TD>
            <TD>We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15&lt;=z&lt;=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283#1</TD>
            <TD>2011-09-14T18:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/124/283</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/283</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/124/283 [2]</TD>
            <TD>BR magnitude and redshift of A1300 (Pierre+ 1997)</TD>
            <TD>We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15&lt;=z&lt;=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283#2</TD>
            <TD>2011-09-14T18:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/124/283&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/283</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/124/283 [table4]</TD>
            <TD>BR magnitude and redshift of A1300 (Pierre+ 1997)</TD>
            <TD>We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15&lt;=z&lt;=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283#table4</TD>
            <TD>2011-09-14T18:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/283</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/124/283&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/283</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/100/1091 [1]</TD>
            <TD>UBR photometry of 39 elliptical galaxies (Peletier+ 1990)</TD>
            <TD>We have obtained U,B, and R CCD surface photometry for a sample of 39 elliptical galaxies. For each galaxy we have determined the surface brightness profile, U-R and B-R color profiles, and the ellipticity and position angle profiles, all as function of major axis radius, using a two-dimensional ellipse fitting program. In addition, we have derived the sin and cos(3.theta) and 4.theta terms that describe the high-order deviations of the B and R isophotes from ellipses. While it is very common for ellipticals to display measurable 3.theta and 4.theta terms, the amplitudes of these terms rarely exceed 0.5%. The isophotes of elliptical galaxies are very well characterized by ellipses. The surface brightness and color profiles are given to radii at which the error in the profile reaches 0.1 mag from the uncertainty in the brightness of the night sky. We have carried out a series of simulations of the effects of seeing on luminosity and ellipticity profiles, to determine the radius beyond which the errors in our data from seeing are less than 0.05 mag and 0.02 in ellipticity. Measurable effects of seeing extend to surprisingly large radii, as much as 5-10 seeing radii, depending upon the ellipticity of the galaxy and the form of the surface brightness profile. Ellipticity and position angle profiles are usually the same in all passbands with no indication that the contours of constant color are more or less flattened than the isophotes, i.e., the isochromes and isophotes have the same shapes, but the insensitivity of the ellipticity to differences between these properties makes this a weak argument. The high-order terms, particularly the 3.theta terms, appear to be sensitive diagnostics for the existence of dust in ellipticals. We find that all the galaxies in this sample either become bluer in B-R and U-R with increasing radius or are of constant color. Mean values for the logarithmic gradients in color are -0.09 mag/arcsec2 per dex in radius in B-R, and -0.20 mag/arcsec2 per dex in radius in U-R. These color changes are consistent with a decrease in the [Fe/H] of approximately 0.20 per decade in radius. Surprisingly, there is no correlation of color gradient with luminosity. It is striking, however, that the lowest luminosity galaxies in the sample (i.e., those with M(B) &gt; -20) do not show any color gradients. They have boxy isophotes, and are also rotationally flattened. While these properties may be related to the fact that they are companions of larger ellipsoidal systems, it could provide an important clue to the formation of ellipticals. Low luminosity ellipticals that are not close companions to giant ellipticals need to be studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/100/1091#1</TD>
            <TD>2011-09-14T18:20:55Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/100/1091</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/100/1091</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/100/1091</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/100/1091 [2]</TD>
            <TD>UBR photometry of 39 elliptical galaxies (Peletier+ 1990)</TD>
            <TD>We have obtained U,B, and R CCD surface photometry for a sample of 39 elliptical galaxies. For each galaxy we have determined the surface brightness profile, U-R and B-R color profiles, and the ellipticity and position angle profiles, all as function of major axis radius, using a two-dimensional ellipse fitting program. In addition, we have derived the sin and cos(3.theta) and 4.theta terms that describe the high-order deviations of the B and R isophotes from ellipses. While it is very common for ellipticals to display measurable 3.theta and 4.theta terms, the amplitudes of these terms rarely exceed 0.5%. The isophotes of elliptical galaxies are very well characterized by ellipses. The surface brightness and color profiles are given to radii at which the error in the profile reaches 0.1 mag from the uncertainty in the brightness of the night sky. We have carried out a series of simulations of the effects of seeing on luminosity and ellipticity profiles, to determine the radius beyond which the errors in our data from seeing are less than 0.05 mag and 0.02 in ellipticity. Measurable effects of seeing extend to surprisingly large radii, as much as 5-10 seeing radii, depending upon the ellipticity of the galaxy and the form of the surface brightness profile. Ellipticity and position angle profiles are usually the same in all passbands with no indication that the contours of constant color are more or less flattened than the isophotes, i.e., the isochromes and isophotes have the same shapes, but the insensitivity of the ellipticity to differences between these properties makes this a weak argument. The high-order terms, particularly the 3.theta terms, appear to be sensitive diagnostics for the existence of dust in ellipticals. We find that all the galaxies in this sample either become bluer in B-R and U-R with increasing radius or are of constant color. Mean values for the logarithmic gradients in color are -0.09 mag/arcsec2 per dex in radius in B-R, and -0.20 mag/arcsec2 per dex in radius in U-R. These color changes are consistent with a decrease in the [Fe/H] of approximately 0.20 per decade in radius. Surprisingly, there is no correlation of color gradient with luminosity. It is striking, however, that the lowest luminosity galaxies in the sample (i.e., those with M(B) &gt; -20) do not show any color gradients. They have boxy isophotes, and are also rotationally flattened. While these properties may be related to the fact that they are companions of larger ellipsoidal systems, it could provide an important clue to the formation of ellipticals. Low luminosity ellipticals that are not close companions to giant ellipticals need to be studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/100/1091#2</TD>
            <TD>2011-09-14T18:20:55Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/100/1091</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/100/1091&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/100/1091</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/100/1091 [1]</TD>
            <TD>UBR photometry of 39 elliptical galaxies (Peletier+ 1990)</TD>
            <TD>We have obtained U,B, and R CCD surface photometry for a sample of 39 elliptical galaxies. For each galaxy we have determined the surface brightness profile, U-R and B-R color profiles, and the ellipticity and position angle profiles, all as function of major axis radius, using a two-dimensional ellipse fitting program. In addition, we have derived the sin and cos(3.theta) and 4.theta terms that describe the high-order deviations of the B and R isophotes from ellipses. While it is very common for ellipticals to display measurable 3.theta and 4.theta terms, the amplitudes of these terms rarely exceed 0.5%. The isophotes of elliptical galaxies are very well characterized by ellipses. The surface brightness and color profiles are given to radii at which the error in the profile reaches 0.1 mag from the uncertainty in the brightness of the night sky. We have carried out a series of simulations of the effects of seeing on luminosity and ellipticity profiles, to determine the radius beyond which the errors in our data from seeing are less than 0.05 mag and 0.02 in ellipticity. Measurable effects of seeing extend to surprisingly large radii, as much as 5-10 seeing radii, depending upon the ellipticity of the galaxy and the form of the surface brightness profile. Ellipticity and position angle profiles are usually the same in all passbands with no indication that the contours of constant color are more or less flattened than the isophotes, i.e., the isochromes and isophotes have the same shapes, but the insensitivity of the ellipticity to differences between these properties makes this a weak argument. The high-order terms, particularly the 3.theta terms, appear to be sensitive diagnostics for the existence of dust in ellipticals. We find that all the galaxies in this sample either become bluer in B-R and U-R with increasing radius or are of constant color. Mean values for the logarithmic gradients in color are -0.09 mag/arcsec2 per dex in radius in B-R, and -0.20 mag/arcsec2 per dex in radius in U-R. These color changes are consistent with a decrease in the [Fe/H] of approximately 0.20 per decade in radius. Surprisingly, there is no correlation of color gradient with luminosity. It is striking, however, that the lowest luminosity galaxies in the sample (i.e., those with M(B) &gt; -20) do not show any color gradients. They have boxy isophotes, and are also rotationally flattened. While these properties may be related to the fact that they are companions of larger ellipsoidal systems, it could provide an important clue to the formation of ellipticals. Low luminosity ellipticals that are not close companions to giant ellipticals need to be studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/100/1091#1</TD>
            <TD>2011-09-14T18:20:55Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/100/1091</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/100/1091</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/100/1091</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/100/1091 [2]</TD>
            <TD>UBR photometry of 39 elliptical galaxies (Peletier+ 1990)</TD>
            <TD>We have obtained U,B, and R CCD surface photometry for a sample of 39 elliptical galaxies. For each galaxy we have determined the surface brightness profile, U-R and B-R color profiles, and the ellipticity and position angle profiles, all as function of major axis radius, using a two-dimensional ellipse fitting program. In addition, we have derived the sin and cos(3.theta) and 4.theta terms that describe the high-order deviations of the B and R isophotes from ellipses. While it is very common for ellipticals to display measurable 3.theta and 4.theta terms, the amplitudes of these terms rarely exceed 0.5%. The isophotes of elliptical galaxies are very well characterized by ellipses. The surface brightness and color profiles are given to radii at which the error in the profile reaches 0.1 mag from the uncertainty in the brightness of the night sky. We have carried out a series of simulations of the effects of seeing on luminosity and ellipticity profiles, to determine the radius beyond which the errors in our data from seeing are less than 0.05 mag and 0.02 in ellipticity. Measurable effects of seeing extend to surprisingly large radii, as much as 5-10 seeing radii, depending upon the ellipticity of the galaxy and the form of the surface brightness profile. Ellipticity and position angle profiles are usually the same in all passbands with no indication that the contours of constant color are more or less flattened than the isophotes, i.e., the isochromes and isophotes have the same shapes, but the insensitivity of the ellipticity to differences between these properties makes this a weak argument. The high-order terms, particularly the 3.theta terms, appear to be sensitive diagnostics for the existence of dust in ellipticals. We find that all the galaxies in this sample either become bluer in B-R and U-R with increasing radius or are of constant color. Mean values for the logarithmic gradients in color are -0.09 mag/arcsec2 per dex in radius in B-R, and -0.20 mag/arcsec2 per dex in radius in U-R. These color changes are consistent with a decrease in the [Fe/H] of approximately 0.20 per decade in radius. Surprisingly, there is no correlation of color gradient with luminosity. It is striking, however, that the lowest luminosity galaxies in the sample (i.e., those with M(B) &gt; -20) do not show any color gradients. They have boxy isophotes, and are also rotationally flattened. While these properties may be related to the fact that they are companions of larger ellipsoidal systems, it could provide an important clue to the formation of ellipticals. Low luminosity ellipticals that are not close companions to giant ellipticals need to be studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/100/1091#2</TD>
            <TD>2011-09-14T18:20:55Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/100/1091</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/100/1091&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/100/1091</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/35 [1]</TD>
            <TD>Montreal Blue Galaxy Survey (Coziol+ 1993)</TD>
            <TD>We describe and present the first results of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of our survey shows that the bulk of our UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey. We expect to find approximately 500 UV-bright galaxies in the 7000 sq. deg. of The MCT Survey with b &lt; -40 deg. As we go further south, a large number of bright new objects will be discovered.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35#1</TD>
            <TD>2011-09-14T18:21:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/35</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/35</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/35 [2]</TD>
            <TD>Montreal Blue Galaxy Survey (Coziol+ 1993)</TD>
            <TD>We describe and present the first results of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of our survey shows that the bulk of our UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey. We expect to find approximately 500 UV-bright galaxies in the 7000 sq. deg. of The MCT Survey with b &lt; -40 deg. As we go further south, a large number of bright new objects will be discovered.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35#2</TD>
            <TD>2011-09-14T18:21:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/35&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/105/35 [table1]</TD>
            <TD>Montreal Blue Galaxy Survey (Coziol+ 1993)</TD>
            <TD>We describe and present the first results of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of our survey shows that the bulk of our UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey. We expect to find approximately 500 UV-bright galaxies in the 7000 sq. deg. of The MCT Survey with b &lt; -40 deg. As we go further south, a large number of bright new objects will be discovered.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35#table1</TD>
            <TD>2011-09-14T18:21:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/105/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/35 [1]</TD>
            <TD>Montreal Blue Galaxy Survey (Coziol+ 1993)</TD>
            <TD>We describe and present the first results of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of our survey shows that the bulk of our UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey. We expect to find approximately 500 UV-bright galaxies in the 7000 sq. deg. of The MCT Survey with b &lt; -40 deg. As we go further south, a large number of bright new objects will be discovered.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35#1</TD>
            <TD>2011-09-14T18:21:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/35</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/35</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/35 [2]</TD>
            <TD>Montreal Blue Galaxy Survey (Coziol+ 1993)</TD>
            <TD>We describe and present the first results of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of our survey shows that the bulk of our UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey. We expect to find approximately 500 UV-bright galaxies in the 7000 sq. deg. of The MCT Survey with b &lt; -40 deg. As we go further south, a large number of bright new objects will be discovered.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35#2</TD>
            <TD>2011-09-14T18:21:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/35&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/105/35 [table1]</TD>
            <TD>Montreal Blue Galaxy Survey (Coziol+ 1993)</TD>
            <TD>We describe and present the first results of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of our survey shows that the bulk of our UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey. We expect to find approximately 500 UV-bright galaxies in the 7000 sq. deg. of The MCT Survey with b &lt; -40 deg. As we go further south, a large number of bright new objects will be discovered.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35#table1</TD>
            <TD>2011-09-14T18:21:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/105/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/35 [1]</TD>
            <TD>Montreal Blue Galaxy Survey (Coziol+ 1993)</TD>
            <TD>We describe and present the first results of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of our survey shows that the bulk of our UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey. We expect to find approximately 500 UV-bright galaxies in the 7000 sq. deg. of The MCT Survey with b &lt; -40 deg. As we go further south, a large number of bright new objects will be discovered.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35#1</TD>
            <TD>2011-09-14T18:21:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/35</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/35</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/35 [2]</TD>
            <TD>Montreal Blue Galaxy Survey (Coziol+ 1993)</TD>
            <TD>We describe and present the first results of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of our survey shows that the bulk of our UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey. We expect to find approximately 500 UV-bright galaxies in the 7000 sq. deg. of The MCT Survey with b &lt; -40 deg. As we go further south, a large number of bright new objects will be discovered.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35#2</TD>
            <TD>2011-09-14T18:21:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/35&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/105/35 [table1]</TD>
            <TD>Montreal Blue Galaxy Survey (Coziol+ 1993)</TD>
            <TD>We describe and present the first results of a UV-bright galaxy survey using the Montreal-Cambridge-Tololo (MCT) plate collection. Visual inspection of 57 CTIO Curtis Schmidt plates, covering more than 1300 sq. deg., has resulted in the identification of 95 UV-bright galaxies brighter than B = 15.5. Even though 80% of these objects are IRAS sources, barely 20% have their nature already established. The initial result of our survey shows that the bulk of our UV-bright candidates are narrow emission-line galaxies commonly known as starburst or HII galaxies. The fraction of AGNs found is somewhat less than 10%, but comparable to what has been found by the Markarian survey. We expect to find approximately 500 UV-bright galaxies in the 7000 sq. deg. of The MCT Survey with b &lt; -40 deg. As we go further south, a large number of bright new objects will be discovered.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35#table1</TD>
            <TD>2011-09-14T18:21:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/105/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/35</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/393 [1]</TD>
            <TD>Small Drift Scan Survey Galaxies Northern Sky (Kent+ 1993)</TD>
            <TD>One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393#1</TD>
            <TD>2011-09-14T18:21:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/393</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/393</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/393 [2]</TD>
            <TD>Small Drift Scan Survey Galaxies Northern Sky (Kent+ 1993)</TD>
            <TD>One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393#2</TD>
            <TD>2011-09-14T18:21:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/393&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/393</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/105/393 [table]</TD>
            <TD>Small Drift Scan Survey Galaxies Northern Sky (Kent+ 1993)</TD>
            <TD>One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393#table</TD>
            <TD>2011-09-14T18:21:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/105/393&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/393</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/393 [1]</TD>
            <TD>Small Drift Scan Survey Galaxies Northern Sky (Kent+ 1993)</TD>
            <TD>One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393#1</TD>
            <TD>2011-09-14T18:21:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/393</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/393</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/393 [2]</TD>
            <TD>Small Drift Scan Survey Galaxies Northern Sky (Kent+ 1993)</TD>
            <TD>One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393#2</TD>
            <TD>2011-09-14T18:21:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/393&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/393</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/105/393 [table]</TD>
            <TD>Small Drift Scan Survey Galaxies Northern Sky (Kent+ 1993)</TD>
            <TD>One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393#table</TD>
            <TD>2011-09-14T18:21:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/105/393&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/393</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/105/393 [1]</TD>
            <TD>Small Drift Scan Survey Galaxies Northern Sky (Kent+ 1993)</TD>
            <TD>One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393#1</TD>
            <TD>2011-09-14T18:21:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/105/393</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/393</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/105/393 [2]</TD>
            <TD>Small Drift Scan Survey Galaxies Northern Sky (Kent+ 1993)</TD>
            <TD>One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393#2</TD>
            <TD>2011-09-14T18:21:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/105/393&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/393</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/105/393 [table]</TD>
            <TD>Small Drift Scan Survey Galaxies Northern Sky (Kent+ 1993)</TD>
            <TD>One key problem of galaxy surveys using photographic plates is an accurate magnitude calibration. Moreover sensitivity and vignetting variations across the plate, need to be removed. The drift-scan technique is a viable alternative: in this observing mode the telescope tracking is stopped and the CCD is clocked at the sidereal rate. CCD columns are aligned in the east-west direction. The CCD is read continuously, building up an image of a strip of the sky. Data were reduced in the standard manner, but replacing bias with drift dark (CCD is operating in drift scan mode with the shutter closed). Flatfields were obtained from median averaging sets of data frames. Astrometry was done using stars whose position was known from the Guide Star Catalog. The galaxy-star classification was done using the east-west FWHM. Then every candidate galaxy was visually inspected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393#table</TD>
            <TD>2011-09-14T18:21:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/105/393</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/105/393&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/105/393</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/107/2093 [1]</TD>
            <TD>DL Cas (Gieren+, 1994)</TD>
            <TD>As an eight-day Cepheid which is both a component of a spectroscopic binary and a member of the open cluster NGC 129, DL Cas is potentially a very accurate calibrator of the period-luminosity (PL) relation and Cepheid mass. From 160 high-precision (sigma&lt;1.5km/s) radial velocity observations made with the CORAVEL and DAO spectrometers - including 67 new unpublished data - we have obtained both the orbital and pulsational velocity curves of this binary Cepheid. This body of RV data makes DL Cas one of the best observed Cepheids in our galaxy. Our analysis yields an orbital period of 684.4+/-0.4days which confirms DL Cas as one of the shortest-period binaries containing a Cepheid. We derive new precise orbital elements which replace earlier preliminary values found by Harris et al. Isochrone fitting to the V,B-V data points of Turner et al. yields an age of NGC 129 of (7.6+/-0.4)x10^7^yr and a Cepheid mass of 5.6M_{sun}_. Evidence from age, a possible period change, and strip crossing times suggest that DL Cas is a solar-abundance star making its third (redward) crossing through the Cepheid instability strip. Existing observational constraints from our mass function of the DL Cas system and an IUE spectrum suggest that the companion is a main sequence star in the mass range from 2.6 to 5.6M_{sun}_. We use the pulsational velocity curve and published photometry to derive the distance and mean radius of DL Cas with the surface brightness method, finding values of 2034+/-110pc and 66.0+/-3.5R_{sun}_, respectively. The radius we derive indicates that DL Cas is a fundamental-mode pulsator, removing any possible ambiguity in mode identification. The distance corresponds to a mean absolute visual magnitude of &lt;Mv&gt;=-4.2+/-0.3mag whose error is dominated by the uncertainty of the absorption correction. Since our very precise distance contributes only 0.12mag to the error in &lt;Mv&gt;, improved reddening studies of NGC 129 would make DL Cas a very tight calibrator of the PL relation. Our value of the gamma velocity of the DL Cas system is identical to the mean radial velocity of the stars in NGC 129, strengthening the case for cluster membership. However, our distance for DL Cas, and thus for NGC 129, is significantly larger than the 1670+/-13pc obtained by Turner et al. from ZAMS fitting of the cluster. Possible causes for this discrepancy, and their implications for Cepheid distance scale calibrations, are discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/107/2093#1</TD>
            <TD>2011-09-14T18:21:37Z</TD>
            <TD>#Binaries:spectroscopic#Open_Clusters#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/107/2093</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/107/2093</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/107/2093</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/107/2093 [2]</TD>
            <TD>DL Cas (Gieren+, 1994)</TD>
            <TD>As an eight-day Cepheid which is both a component of a spectroscopic binary and a member of the open cluster NGC 129, DL Cas is potentially a very accurate calibrator of the period-luminosity (PL) relation and Cepheid mass. From 160 high-precision (sigma&lt;1.5km/s) radial velocity observations made with the CORAVEL and DAO spectrometers - including 67 new unpublished data - we have obtained both the orbital and pulsational velocity curves of this binary Cepheid. This body of RV data makes DL Cas one of the best observed Cepheids in our galaxy. Our analysis yields an orbital period of 684.4+/-0.4days which confirms DL Cas as one of the shortest-period binaries containing a Cepheid. We derive new precise orbital elements which replace earlier preliminary values found by Harris et al. Isochrone fitting to the V,B-V data points of Turner et al. yields an age of NGC 129 of (7.6+/-0.4)x10^7^yr and a Cepheid mass of 5.6M_{sun}_. Evidence from age, a possible period change, and strip crossing times suggest that DL Cas is a solar-abundance star making its third (redward) crossing through the Cepheid instability strip. Existing observational constraints from our mass function of the DL Cas system and an IUE spectrum suggest that the companion is a main sequence star in the mass range from 2.6 to 5.6M_{sun}_. We use the pulsational velocity curve and published photometry to derive the distance and mean radius of DL Cas with the surface brightness method, finding values of 2034+/-110pc and 66.0+/-3.5R_{sun}_, respectively. The radius we derive indicates that DL Cas is a fundamental-mode pulsator, removing any possible ambiguity in mode identification. The distance corresponds to a mean absolute visual magnitude of &lt;Mv&gt;=-4.2+/-0.3mag whose error is dominated by the uncertainty of the absorption correction. Since our very precise distance contributes only 0.12mag to the error in &lt;Mv&gt;, improved reddening studies of NGC 129 would make DL Cas a very tight calibrator of the PL relation. Our value of the gamma velocity of the DL Cas system is identical to the mean radial velocity of the stars in NGC 129, strengthening the case for cluster membership. However, our distance for DL Cas, and thus for NGC 129, is significantly larger than the 1670+/-13pc obtained by Turner et al. from ZAMS fitting of the cluster. Possible causes for this discrepancy, and their implications for Cepheid distance scale calibrations, are discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/107/2093#2</TD>
            <TD>2011-09-14T18:21:37Z</TD>
            <TD>#Binaries:spectroscopic#Open_Clusters#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/107/2093</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/107/2093&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/107/2093</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/107/2093 [1]</TD>
            <TD>DL Cas (Gieren+, 1994)</TD>
            <TD>As an eight-day Cepheid which is both a component of a spectroscopic binary and a member of the open cluster NGC 129, DL Cas is potentially a very accurate calibrator of the period-luminosity (PL) relation and Cepheid mass. From 160 high-precision (sigma&lt;1.5km/s) radial velocity observations made with the CORAVEL and DAO spectrometers - including 67 new unpublished data - we have obtained both the orbital and pulsational velocity curves of this binary Cepheid. This body of RV data makes DL Cas one of the best observed Cepheids in our galaxy. Our analysis yields an orbital period of 684.4+/-0.4days which confirms DL Cas as one of the shortest-period binaries containing a Cepheid. We derive new precise orbital elements which replace earlier preliminary values found by Harris et al. Isochrone fitting to the V,B-V data points of Turner et al. yields an age of NGC 129 of (7.6+/-0.4)x10^7^yr and a Cepheid mass of 5.6M_{sun}_. Evidence from age, a possible period change, and strip crossing times suggest that DL Cas is a solar-abundance star making its third (redward) crossing through the Cepheid instability strip. Existing observational constraints from our mass function of the DL Cas system and an IUE spectrum suggest that the companion is a main sequence star in the mass range from 2.6 to 5.6M_{sun}_. We use the pulsational velocity curve and published photometry to derive the distance and mean radius of DL Cas with the surface brightness method, finding values of 2034+/-110pc and 66.0+/-3.5R_{sun}_, respectively. The radius we derive indicates that DL Cas is a fundamental-mode pulsator, removing any possible ambiguity in mode identification. The distance corresponds to a mean absolute visual magnitude of &lt;Mv&gt;=-4.2+/-0.3mag whose error is dominated by the uncertainty of the absorption correction. Since our very precise distance contributes only 0.12mag to the error in &lt;Mv&gt;, improved reddening studies of NGC 129 would make DL Cas a very tight calibrator of the PL relation. Our value of the gamma velocity of the DL Cas system is identical to the mean radial velocity of the stars in NGC 129, strengthening the case for cluster membership. However, our distance for DL Cas, and thus for NGC 129, is significantly larger than the 1670+/-13pc obtained by Turner et al. from ZAMS fitting of the cluster. Possible causes for this discrepancy, and their implications for Cepheid distance scale calibrations, are discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/107/2093#1</TD>
            <TD>2011-09-14T18:21:37Z</TD>
            <TD>#Binaries:spectroscopic#Open_Clusters#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/107/2093</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/107/2093</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/107/2093</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/107/2093 [2]</TD>
            <TD>DL Cas (Gieren+, 1994)</TD>
            <TD>As an eight-day Cepheid which is both a component of a spectroscopic binary and a member of the open cluster NGC 129, DL Cas is potentially a very accurate calibrator of the period-luminosity (PL) relation and Cepheid mass. From 160 high-precision (sigma&lt;1.5km/s) radial velocity observations made with the CORAVEL and DAO spectrometers - including 67 new unpublished data - we have obtained both the orbital and pulsational velocity curves of this binary Cepheid. This body of RV data makes DL Cas one of the best observed Cepheids in our galaxy. Our analysis yields an orbital period of 684.4+/-0.4days which confirms DL Cas as one of the shortest-period binaries containing a Cepheid. We derive new precise orbital elements which replace earlier preliminary values found by Harris et al. Isochrone fitting to the V,B-V data points of Turner et al. yields an age of NGC 129 of (7.6+/-0.4)x10^7^yr and a Cepheid mass of 5.6M_{sun}_. Evidence from age, a possible period change, and strip crossing times suggest that DL Cas is a solar-abundance star making its third (redward) crossing through the Cepheid instability strip. Existing observational constraints from our mass function of the DL Cas system and an IUE spectrum suggest that the companion is a main sequence star in the mass range from 2.6 to 5.6M_{sun}_. We use the pulsational velocity curve and published photometry to derive the distance and mean radius of DL Cas with the surface brightness method, finding values of 2034+/-110pc and 66.0+/-3.5R_{sun}_, respectively. The radius we derive indicates that DL Cas is a fundamental-mode pulsator, removing any possible ambiguity in mode identification. The distance corresponds to a mean absolute visual magnitude of &lt;Mv&gt;=-4.2+/-0.3mag whose error is dominated by the uncertainty of the absorption correction. Since our very precise distance contributes only 0.12mag to the error in &lt;Mv&gt;, improved reddening studies of NGC 129 would make DL Cas a very tight calibrator of the PL relation. Our value of the gamma velocity of the DL Cas system is identical to the mean radial velocity of the stars in NGC 129, strengthening the case for cluster membership. However, our distance for DL Cas, and thus for NGC 129, is significantly larger than the 1670+/-13pc obtained by Turner et al. from ZAMS fitting of the cluster. Possible causes for this discrepancy, and their implications for Cepheid distance scale calibrations, are discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/107/2093#2</TD>
            <TD>2011-09-14T18:21:37Z</TD>
            <TD>#Binaries:spectroscopic#Open_Clusters#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/107/2093</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/107/2093&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/107/2093</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1032 [1]</TD>
            <TD>APM elliptical galaxies radial velocities (Muriel+ 1995)</TD>
            <TD>We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032#1</TD>
            <TD>2011-09-14T18:22:04Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1032</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1032</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1032 [2]</TD>
            <TD>APM elliptical galaxies radial velocities (Muriel+ 1995)</TD>
            <TD>We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032#2</TD>
            <TD>2011-09-14T18:22:04Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1032&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1032</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/1032 [table1]</TD>
            <TD>APM elliptical galaxies radial velocities (Muriel+ 1995)</TD>
            <TD>We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032#table1</TD>
            <TD>2011-09-14T18:22:04Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/1032&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1032</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [1]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#1</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [2]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#2</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [3]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#3</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [4]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#4</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [5]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#5</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [6]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#6</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [7]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#7</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [8]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#8</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [9]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#9</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR6 [10]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#10</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/DirectCone?DSACAT=UKIDSS_DR6&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [11]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#11</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR6 [12]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#12</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [13]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#13</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [14]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#14</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [15]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#15</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [16]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#16</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [17]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#17</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [18]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#18</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR6 [19]</TD>
            <TD>UKIDSS DR6 - UKIRT Infrared Deep Sky Survey Data Release 6</TD>
            <TD>This DSA hosts data release 6 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Galactic Plane Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa#19</TD>
            <TD>2012-07-18T12:46:08Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 6</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR6-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR6-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1032 [1]</TD>
            <TD>APM elliptical galaxies radial velocities (Muriel+ 1995)</TD>
            <TD>We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032#1</TD>
            <TD>2011-09-14T18:22:04Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1032</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1032</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1032 [2]</TD>
            <TD>APM elliptical galaxies radial velocities (Muriel+ 1995)</TD>
            <TD>We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032#2</TD>
            <TD>2011-09-14T18:22:04Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1032&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1032</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/1032 [table1]</TD>
            <TD>APM elliptical galaxies radial velocities (Muriel+ 1995)</TD>
            <TD>We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032#table1</TD>
            <TD>2011-09-14T18:22:04Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/1032&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1032</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1032 [1]</TD>
            <TD>APM elliptical galaxies radial velocities (Muriel+ 1995)</TD>
            <TD>We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032#1</TD>
            <TD>2011-09-14T18:22:04Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1032</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1032</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1032 [2]</TD>
            <TD>APM elliptical galaxies radial velocities (Muriel+ 1995)</TD>
            <TD>We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032#2</TD>
            <TD>2011-09-14T18:22:04Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1032&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1032</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/1032 [table1]</TD>
            <TD>APM elliptical galaxies radial velocities (Muriel+ 1995)</TD>
            <TD>We present 292 new redshifts of elliptical galaxies selected from the APM Bright Galaxy Survey. We use these data together with published redshifts and bj apparent magnitudes from the APM Bright Galaxy Survey in order to estimate the shape of the Luminosity Function of a total sample of 535 ellipticals. We use the Maximum Likelihood method for the determination of the best fitting parameters {alpha} and M^*^ of a Schechter Function. In order to provide tests for systematics and suitable error estimates we apply Monte Carlo techniques which are also used to deal with incompleteness effects in the data. In agreement with other authors our results indicate a relative lack of low luminosity ellipticals compared to other morphological types. The best fitting shape parameters derived are {alpha}=0.20+/-0.25 and M^*^_Bj_=-20.0+/-0.3. We do not find evidence for a dependence of these parameters on environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032#table1</TD>
            <TD>2011-09-14T18:22:04Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1032</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/1032&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1032</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1141 [1]</TD>
            <TD>Variables in the Sagittarius dSph (Mateo+ 1995)</TD>
            <TD>We present time-series CCD photometry of a field in the newly discovered dwarf spheroidal galaxy in Sagittarius (hereafter Sgr), and of a nearby control field. These data, which consist of VI images obtained during the 1994 OGLE season, were used to identify and study variable stars in both fields. We discovered ten variable stars in the Sgr field, nine of which have light curves and periods consistent with RR Lyr stars or anomalous Cepheids. The control field contains four short-period contact eclipsing binaries, but no pulsating variables. The variables in the Sgr field include a bright RR Lyr star that is almost certainly located in front of Sgr in the galactic bulge, a short-period contact binary located near or within Sgr, and a short-period pulsating star that may either be a foreground halo RR Lyr star or an anomalous Cepheid within Sgr. The seven remaining variables in the Sgr field are RR Lyr stars with very similar mean apparent magnitudes; we conclude that they are members of Sgr. We estimate the total number of RR Lyr stars in Sgr to be 1930+/-730 if M(V,Sgr)=-13, or 310+/-120 if M(V,Sgr)=-11. The frequency of pulsating variables in Sgr is consistent with earlier conclusions that the galaxy consists of a predominant old (age&gt;~10Gyr) population.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1141#1</TD>
            <TD>2011-09-14T18:22:06Z</TD>
            <TD>#Photometry#Gravitational_lensing#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1141</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1141</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1141</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1141 [2]</TD>
            <TD>Variables in the Sagittarius dSph (Mateo+ 1995)</TD>
            <TD>We present time-series CCD photometry of a field in the newly discovered dwarf spheroidal galaxy in Sagittarius (hereafter Sgr), and of a nearby control field. These data, which consist of VI images obtained during the 1994 OGLE season, were used to identify and study variable stars in both fields. We discovered ten variable stars in the Sgr field, nine of which have light curves and periods consistent with RR Lyr stars or anomalous Cepheids. The control field contains four short-period contact eclipsing binaries, but no pulsating variables. The variables in the Sgr field include a bright RR Lyr star that is almost certainly located in front of Sgr in the galactic bulge, a short-period contact binary located near or within Sgr, and a short-period pulsating star that may either be a foreground halo RR Lyr star or an anomalous Cepheid within Sgr. The seven remaining variables in the Sgr field are RR Lyr stars with very similar mean apparent magnitudes; we conclude that they are members of Sgr. We estimate the total number of RR Lyr stars in Sgr to be 1930+/-730 if M(V,Sgr)=-13, or 310+/-120 if M(V,Sgr)=-11. The frequency of pulsating variables in Sgr is consistent with earlier conclusions that the galaxy consists of a predominant old (age&gt;~10Gyr) population.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1141#2</TD>
            <TD>2011-09-14T18:22:06Z</TD>
            <TD>#Photometry#Gravitational_lensing#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1141</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1141&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1141</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1141 [1]</TD>
            <TD>Variables in the Sagittarius dSph (Mateo+ 1995)</TD>
            <TD>We present time-series CCD photometry of a field in the newly discovered dwarf spheroidal galaxy in Sagittarius (hereafter Sgr), and of a nearby control field. These data, which consist of VI images obtained during the 1994 OGLE season, were used to identify and study variable stars in both fields. We discovered ten variable stars in the Sgr field, nine of which have light curves and periods consistent with RR Lyr stars or anomalous Cepheids. The control field contains four short-period contact eclipsing binaries, but no pulsating variables. The variables in the Sgr field include a bright RR Lyr star that is almost certainly located in front of Sgr in the galactic bulge, a short-period contact binary located near or within Sgr, and a short-period pulsating star that may either be a foreground halo RR Lyr star or an anomalous Cepheid within Sgr. The seven remaining variables in the Sgr field are RR Lyr stars with very similar mean apparent magnitudes; we conclude that they are members of Sgr. We estimate the total number of RR Lyr stars in Sgr to be 1930+/-730 if M(V,Sgr)=-13, or 310+/-120 if M(V,Sgr)=-11. The frequency of pulsating variables in Sgr is consistent with earlier conclusions that the galaxy consists of a predominant old (age&gt;~10Gyr) population.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1141#1</TD>
            <TD>2011-09-14T18:22:06Z</TD>
            <TD>#Photometry#Gravitational_lensing#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1141</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1141</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1141</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1141 [2]</TD>
            <TD>Variables in the Sagittarius dSph (Mateo+ 1995)</TD>
            <TD>We present time-series CCD photometry of a field in the newly discovered dwarf spheroidal galaxy in Sagittarius (hereafter Sgr), and of a nearby control field. These data, which consist of VI images obtained during the 1994 OGLE season, were used to identify and study variable stars in both fields. We discovered ten variable stars in the Sgr field, nine of which have light curves and periods consistent with RR Lyr stars or anomalous Cepheids. The control field contains four short-period contact eclipsing binaries, but no pulsating variables. The variables in the Sgr field include a bright RR Lyr star that is almost certainly located in front of Sgr in the galactic bulge, a short-period contact binary located near or within Sgr, and a short-period pulsating star that may either be a foreground halo RR Lyr star or an anomalous Cepheid within Sgr. The seven remaining variables in the Sgr field are RR Lyr stars with very similar mean apparent magnitudes; we conclude that they are members of Sgr. We estimate the total number of RR Lyr stars in Sgr to be 1930+/-730 if M(V,Sgr)=-13, or 310+/-120 if M(V,Sgr)=-11. The frequency of pulsating variables in Sgr is consistent with earlier conclusions that the galaxy consists of a predominant old (age&gt;~10Gyr) population.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1141#2</TD>
            <TD>2011-09-14T18:22:06Z</TD>
            <TD>#Photometry#Gravitational_lensing#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1141</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1141&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1141</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1649 [1]</TD>
            <TD>VI photometry near the M33 nucleus (Mighell+ 1995)</TD>
            <TD>We have studied the stellar populations near the nucleus of the nearby spiral galaxy M33 using archival observations of the Hubble Space Telescope Planetary Camera in the F555W and F785LP passbands. The I vs (V-I) color-magnitude diagram reveals a young stellar population with a blue main sequence and red supergiants, and stars in a blue loop that are Cepheid candidates. An old red giant branch is clearly visible, with a break at I=20.7mag which is, within the observational errors, identical to the giant branch termination point of the Mould &amp; Kristian (1986ApJ...305..591M) halo field. However, red giants are seen up to I=19.5mag, and many bright red giants are undetected in the V band. We find evidence for a wide abundance spread of at least 1.5dex from metal-poor (~M15) to metal-rich (&gt;=47Tucanae) in the Population II stars, in sharp contrast to the M33 halo field of Mould &amp; Kristian (1986ApJ...305..591M) which is metal-poor (~M92) with a narrow abundance range. We show that the various stellar populations have different spatial distributions. The Population II stars are more centrally concentrated than the Population I stars. The red giants brighter than I=20.7 (the termination point for a Galactic globular cluster giant branch) are found to be more centrally concentrated than the (presumably) old red giants. The most-centrally concentrated bright Population II giants are probably associated with the many bright red giants that are undetected in the V band. These infrared-bright giants were probably created in an intermediate-age burst of star formation that took place well after the formation of the oldest halo stars but long before the recent burst of star formation seen in nearby OB associations. This stellar population probably corresponds to the bulge identified in the infrared H band by Minniti et al. (1993ApJ...410L..79M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1649#1</TD>
            <TD>2011-09-14T18:22:08Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1649</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1649</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1649</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1649 [2]</TD>
            <TD>VI photometry near the M33 nucleus (Mighell+ 1995)</TD>
            <TD>We have studied the stellar populations near the nucleus of the nearby spiral galaxy M33 using archival observations of the Hubble Space Telescope Planetary Camera in the F555W and F785LP passbands. The I vs (V-I) color-magnitude diagram reveals a young stellar population with a blue main sequence and red supergiants, and stars in a blue loop that are Cepheid candidates. An old red giant branch is clearly visible, with a break at I=20.7mag which is, within the observational errors, identical to the giant branch termination point of the Mould &amp; Kristian (1986ApJ...305..591M) halo field. However, red giants are seen up to I=19.5mag, and many bright red giants are undetected in the V band. We find evidence for a wide abundance spread of at least 1.5dex from metal-poor (~M15) to metal-rich (&gt;=47Tucanae) in the Population II stars, in sharp contrast to the M33 halo field of Mould &amp; Kristian (1986ApJ...305..591M) which is metal-poor (~M92) with a narrow abundance range. We show that the various stellar populations have different spatial distributions. The Population II stars are more centrally concentrated than the Population I stars. The red giants brighter than I=20.7 (the termination point for a Galactic globular cluster giant branch) are found to be more centrally concentrated than the (presumably) old red giants. The most-centrally concentrated bright Population II giants are probably associated with the many bright red giants that are undetected in the V band. These infrared-bright giants were probably created in an intermediate-age burst of star formation that took place well after the formation of the oldest halo stars but long before the recent burst of star formation seen in nearby OB associations. This stellar population probably corresponds to the bulge identified in the infrared H band by Minniti et al. (1993ApJ...410L..79M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1649#2</TD>
            <TD>2011-09-14T18:22:08Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1649</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1649&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1649</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1649 [1]</TD>
            <TD>VI photometry near the M33 nucleus (Mighell+ 1995)</TD>
            <TD>We have studied the stellar populations near the nucleus of the nearby spiral galaxy M33 using archival observations of the Hubble Space Telescope Planetary Camera in the F555W and F785LP passbands. The I vs (V-I) color-magnitude diagram reveals a young stellar population with a blue main sequence and red supergiants, and stars in a blue loop that are Cepheid candidates. An old red giant branch is clearly visible, with a break at I=20.7mag which is, within the observational errors, identical to the giant branch termination point of the Mould &amp; Kristian (1986ApJ...305..591M) halo field. However, red giants are seen up to I=19.5mag, and many bright red giants are undetected in the V band. We find evidence for a wide abundance spread of at least 1.5dex from metal-poor (~M15) to metal-rich (&gt;=47Tucanae) in the Population II stars, in sharp contrast to the M33 halo field of Mould &amp; Kristian (1986ApJ...305..591M) which is metal-poor (~M92) with a narrow abundance range. We show that the various stellar populations have different spatial distributions. The Population II stars are more centrally concentrated than the Population I stars. The red giants brighter than I=20.7 (the termination point for a Galactic globular cluster giant branch) are found to be more centrally concentrated than the (presumably) old red giants. The most-centrally concentrated bright Population II giants are probably associated with the many bright red giants that are undetected in the V band. These infrared-bright giants were probably created in an intermediate-age burst of star formation that took place well after the formation of the oldest halo stars but long before the recent burst of star formation seen in nearby OB associations. This stellar population probably corresponds to the bulge identified in the infrared H band by Minniti et al. (1993ApJ...410L..79M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1649#1</TD>
            <TD>2011-09-14T18:22:08Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1649</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1649</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1649</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1649 [2]</TD>
            <TD>VI photometry near the M33 nucleus (Mighell+ 1995)</TD>
            <TD>We have studied the stellar populations near the nucleus of the nearby spiral galaxy M33 using archival observations of the Hubble Space Telescope Planetary Camera in the F555W and F785LP passbands. The I vs (V-I) color-magnitude diagram reveals a young stellar population with a blue main sequence and red supergiants, and stars in a blue loop that are Cepheid candidates. An old red giant branch is clearly visible, with a break at I=20.7mag which is, within the observational errors, identical to the giant branch termination point of the Mould &amp; Kristian (1986ApJ...305..591M) halo field. However, red giants are seen up to I=19.5mag, and many bright red giants are undetected in the V band. We find evidence for a wide abundance spread of at least 1.5dex from metal-poor (~M15) to metal-rich (&gt;=47Tucanae) in the Population II stars, in sharp contrast to the M33 halo field of Mould &amp; Kristian (1986ApJ...305..591M) which is metal-poor (~M92) with a narrow abundance range. We show that the various stellar populations have different spatial distributions. The Population II stars are more centrally concentrated than the Population I stars. The red giants brighter than I=20.7 (the termination point for a Galactic globular cluster giant branch) are found to be more centrally concentrated than the (presumably) old red giants. The most-centrally concentrated bright Population II giants are probably associated with the many bright red giants that are undetected in the V band. These infrared-bright giants were probably created in an intermediate-age burst of star formation that took place well after the formation of the oldest halo stars but long before the recent burst of star formation seen in nearby OB associations. This stellar population probably corresponds to the bulge identified in the infrared H band by Minniti et al. (1993ApJ...410L..79M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1649#2</TD>
            <TD>2011-09-14T18:22:08Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1649</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1649&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1649</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/2559 [1]</TD>
            <TD>Supergiants in NGC 672 (Sohn+ 1996)</TD>
            <TD>V, R, and I CCD images are used to investigate the photometric properties and spatial distribution of supergiants in the nearby interacting galaxy NGC 672. Not counting stars imbedded in H II regions, our sample consists of 237 objects. The (V-R,V-I) two-color diagram indicates that the majority of these stars have spectral types between A-K. Statistical tests show that the outer region of NGC 672 contains a redder population of supergiants than the inner region. Comparisons with theoretical evolutionary tracks indicate that the majority of the supergiants in NGC 672 have progenitor masses between 15M_{sun}_ and 25M_{sun}_, and that the inner regions contain stars that are more massive than in the outer disk, indicating that an age gradient is present. The luminosity functions in all three bandpasses follow power laws, and the exponent in V=0.79+/-0.06, in good agreement with other galaxies. The brightest red supergiants occur at V~22.0, from which we derive a distance modulus of 29.5, corresponding to 7.9(+1.0)(-0.9)Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2559#1</TD>
            <TD>2011-09-14T18:22:35Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/2559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/2559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/2559 [2]</TD>
            <TD>Supergiants in NGC 672 (Sohn+ 1996)</TD>
            <TD>V, R, and I CCD images are used to investigate the photometric properties and spatial distribution of supergiants in the nearby interacting galaxy NGC 672. Not counting stars imbedded in H II regions, our sample consists of 237 objects. The (V-R,V-I) two-color diagram indicates that the majority of these stars have spectral types between A-K. Statistical tests show that the outer region of NGC 672 contains a redder population of supergiants than the inner region. Comparisons with theoretical evolutionary tracks indicate that the majority of the supergiants in NGC 672 have progenitor masses between 15M_{sun}_ and 25M_{sun}_, and that the inner regions contain stars that are more massive than in the outer disk, indicating that an age gradient is present. The luminosity functions in all three bandpasses follow power laws, and the exponent in V=0.79+/-0.06, in good agreement with other galaxies. The brightest red supergiants occur at V~22.0, from which we derive a distance modulus of 29.5, corresponding to 7.9(+1.0)(-0.9)Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2559#2</TD>
            <TD>2011-09-14T18:22:35Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/2559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/2559</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/2559 [1]</TD>
            <TD>Supergiants in NGC 672 (Sohn+ 1996)</TD>
            <TD>V, R, and I CCD images are used to investigate the photometric properties and spatial distribution of supergiants in the nearby interacting galaxy NGC 672. Not counting stars imbedded in H II regions, our sample consists of 237 objects. The (V-R,V-I) two-color diagram indicates that the majority of these stars have spectral types between A-K. Statistical tests show that the outer region of NGC 672 contains a redder population of supergiants than the inner region. Comparisons with theoretical evolutionary tracks indicate that the majority of the supergiants in NGC 672 have progenitor masses between 15M_{sun}_ and 25M_{sun}_, and that the inner regions contain stars that are more massive than in the outer disk, indicating that an age gradient is present. The luminosity functions in all three bandpasses follow power laws, and the exponent in V=0.79+/-0.06, in good agreement with other galaxies. The brightest red supergiants occur at V~22.0, from which we derive a distance modulus of 29.5, corresponding to 7.9(+1.0)(-0.9)Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2559#1</TD>
            <TD>2011-09-14T18:22:35Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/2559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/2559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/2559 [2]</TD>
            <TD>Supergiants in NGC 672 (Sohn+ 1996)</TD>
            <TD>V, R, and I CCD images are used to investigate the photometric properties and spatial distribution of supergiants in the nearby interacting galaxy NGC 672. Not counting stars imbedded in H II regions, our sample consists of 237 objects. The (V-R,V-I) two-color diagram indicates that the majority of these stars have spectral types between A-K. Statistical tests show that the outer region of NGC 672 contains a redder population of supergiants than the inner region. Comparisons with theoretical evolutionary tracks indicate that the majority of the supergiants in NGC 672 have progenitor masses between 15M_{sun}_ and 25M_{sun}_, and that the inner regions contain stars that are more massive than in the outer disk, indicating that an age gradient is present. The luminosity functions in all three bandpasses follow power laws, and the exponent in V=0.79+/-0.06, in good agreement with other galaxies. The brightest red supergiants occur at V~22.0, from which we derive a distance modulus of 29.5, corresponding to 7.9(+1.0)(-0.9)Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2559#2</TD>
            <TD>2011-09-14T18:22:35Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/2559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/2559</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/96/1884 [1]</TD>
            <TD>BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)</TD>
            <TD>We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884#1</TD>
            <TD>2011-09-14T18:22:48Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/96/1884</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/96/1884</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/96/1884 [2]</TD>
            <TD>BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)</TD>
            <TD>We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884#2</TD>
            <TD>2011-09-14T18:22:48Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/96/1884&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/96/1884</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/96/1884 [table1]</TD>
            <TD>BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)</TD>
            <TD>We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884#table1</TD>
            <TD>2011-09-14T18:22:48Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/96/1884&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/96/1884</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/96/1884 [1]</TD>
            <TD>BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)</TD>
            <TD>We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884#1</TD>
            <TD>2011-09-14T18:22:48Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
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            <TD>HTTP Request</TD>
            <TD>J/AJ/96/1884 [2]</TD>
            <TD>BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)</TD>
            <TD>We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/96/1884 [table1]</TD>
            <TD>BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)</TD>
            <TD>We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/96/1884 [1]</TD>
            <TD>BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)</TD>
            <TD>We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884#1</TD>
            <TD>2011-09-14T18:22:48Z</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/96/1884</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/96/1884 [2]</TD>
            <TD>BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)</TD>
            <TD>We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884#2</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/96/1884 [table1]</TD>
            <TD>BVRJHK photometry of M31 red supergiants (Humphreys+ 1988)</TD>
            <TD>We have surveyed M31 for its most luminous red stars; 300 candidates were found distributed across the face of the galaxy. JHK infrared photometry was observed for 57 of the candidates, and far-red (6800-8800A) spectra were also obtained for 45 stars. We have used the strength of the Ca II triplet (~8500A) and the J-H and H-K colors as luminosity discriminants to separate the supergiants from the foreground dwarfs. With these criteria, 23 probable late-type supergiants were identified. We discuss their distribution and relative numbers of the red supergiants in comparison with the known WR stars in M31. Accurate extinction and infrared (K=2.2{mu}m) and bolometric luminosities are also derived from the infrared photometry. We find that although visually bright red supergiants (M_V_=-8mag) exist in M31, the most luminous (M_bol_) red supergiants are not found in the relative numbers we would expect in a galaxy of its size and mass. It is probable that the rate of massive-star formation is less in M31, an Sb type spiral, than has been observed in the Sc spirals and irregulars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/96/1884#table1</TD>
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            <TD>ParamHTTP</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/353/494 [1]</TD>
            <TD>JHKL photometry on Galactic bulge M Giants (Frogel+, 1990)</TD>
            <TD>JHKL colors and CO and H2O indices are presented for an unbiased sample of about 250 M giants drawn from complete surveys for such stars along the minor axis of the Galaxy at latitudes between -3deg and -12deg. Magnitudes at 10 {mu}m and narrow-band near-infrared colors for some of these stars are also given. At constant J-K the mean CO index of the bulge M giants weakens monotonically with increasing latitude. From the relation between CO and [Fe/H] established for star clusters, this would correspond to a decrease of ~0.4 dex in the mean [Fe/H] between the -3deg and -12deg fields, from somewhat greater to somewhat less than solar. These values are consistent with abundances derived from optical color-magnitude diagrams. Despite these high [Fe/H] values, the ridgelines of the color-magnitude diagrams for all fields lie between those of 47 Tucanae and M3. There is a mild blueward shift with increasing latitude seen in the integrated mean J-K colors of the fields. A steady progression with latitude in the mean (J-H, H-K) relation for the bulge M giants is observed. For the -12deg field it is significantly displaced from the one for local field giants and overlaps that for globular cluster stars; for the -3deg field it is displaced by about the same amount, but on the opposite side of the field giant relation. Dispersions about this relation and the mean (CO, J-K) relation for the M giants in each field are comparable in size to the measuring uncertainties alone, but in a given field the displacements of individual stars from these two mean relations are statistically correlated. We attribute this correlation to a spread in metallicity within each field but note that this spread is smaller than the total metallicity range over all fields. In addition, metallicity-related effects result in J-H getting bluer with increasing metallicity in stars of similar temperature. The bolometric luminosity function of the nonvariable M giants is nearly independent of latitude. All show a sharp cutoff at Mbol&lt;=-4.2; such a cutoff could be a good extragalactic distance indicator for bulgelike stellar populations. The reddest (J-K&gt;=-1.35) and most luminous stars are found only in the low-latitude windows; all are M7-M9 giants, long-period variables (LPVs), or both. Except for these reddest stars, the ratio at a given color of M7-M9 giants to earlier type giants is independent of latitude. Only when stars of all colors in a spectral group are considered is the rapid falloff seen in the ratio of M7-M9 giants respect to earlier types. The bulge LPVs have &lt;Mbol&gt; = -4.2. Since this is nearly the same as for LPVs in globular clusters, it does not require an age for the bulge population significantly younger than that of globular clusters. Their spatial distribution is similar to that of the reddest late M giants. The LPVs with the reddest colors, attributed to the most extensive circumstellar dust shells, are found in the lowest latitude fields. Most of the bulge IRAS sources in the fields studied can be identified with these LPVs or with the brightest nonvariable M giants; many of the latter are probably foreground objects. The reddest IRAS sources are at the lowest latitudes and have the coolest [12-25]{mu}m colors. The bulge IRAS sources do not appear to represent a different or more luminous class of objects than the optically identified M giants. Five different estimators of the surface brightness and surface density between latitudes -3deg and -12deg have a power-law dependence on radius with exponent between -2.5 and -3.4. The value of the exponent depends on the metallicity of the estimator: the most metal-rich objects have the steepest falloff. However, even the smallest exponent, which characterizes the total light and mass distribution, places the bulge among the most spatially concentrated of those measured by Kent for a sample of 22 Sb-Sc galaxies. Thus the mass distribution within the inner 1.5 kpc of the Galaxy is quite sharply peaked.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/353/494#1</TD>
            <TD>2011-09-14T18:23:05Z</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/353/494</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/353/494</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/353/494 [2]</TD>
            <TD>JHKL photometry on Galactic bulge M Giants (Frogel+, 1990)</TD>
            <TD>JHKL colors and CO and H2O indices are presented for an unbiased sample of about 250 M giants drawn from complete surveys for such stars along the minor axis of the Galaxy at latitudes between -3deg and -12deg. Magnitudes at 10 {mu}m and narrow-band near-infrared colors for some of these stars are also given. At constant J-K the mean CO index of the bulge M giants weakens monotonically with increasing latitude. From the relation between CO and [Fe/H] established for star clusters, this would correspond to a decrease of ~0.4 dex in the mean [Fe/H] between the -3deg and -12deg fields, from somewhat greater to somewhat less than solar. These values are consistent with abundances derived from optical color-magnitude diagrams. Despite these high [Fe/H] values, the ridgelines of the color-magnitude diagrams for all fields lie between those of 47 Tucanae and M3. There is a mild blueward shift with increasing latitude seen in the integrated mean J-K colors of the fields. A steady progression with latitude in the mean (J-H, H-K) relation for the bulge M giants is observed. For the -12deg field it is significantly displaced from the one for local field giants and overlaps that for globular cluster stars; for the -3deg field it is displaced by about the same amount, but on the opposite side of the field giant relation. Dispersions about this relation and the mean (CO, J-K) relation for the M giants in each field are comparable in size to the measuring uncertainties alone, but in a given field the displacements of individual stars from these two mean relations are statistically correlated. We attribute this correlation to a spread in metallicity within each field but note that this spread is smaller than the total metallicity range over all fields. In addition, metallicity-related effects result in J-H getting bluer with increasing metallicity in stars of similar temperature. The bolometric luminosity function of the nonvariable M giants is nearly independent of latitude. All show a sharp cutoff at Mbol&lt;=-4.2; such a cutoff could be a good extragalactic distance indicator for bulgelike stellar populations. The reddest (J-K&gt;=-1.35) and most luminous stars are found only in the low-latitude windows; all are M7-M9 giants, long-period variables (LPVs), or both. Except for these reddest stars, the ratio at a given color of M7-M9 giants to earlier type giants is independent of latitude. Only when stars of all colors in a spectral group are considered is the rapid falloff seen in the ratio of M7-M9 giants respect to earlier types. The bulge LPVs have &lt;Mbol&gt; = -4.2. Since this is nearly the same as for LPVs in globular clusters, it does not require an age for the bulge population significantly younger than that of globular clusters. Their spatial distribution is similar to that of the reddest late M giants. The LPVs with the reddest colors, attributed to the most extensive circumstellar dust shells, are found in the lowest latitude fields. Most of the bulge IRAS sources in the fields studied can be identified with these LPVs or with the brightest nonvariable M giants; many of the latter are probably foreground objects. The reddest IRAS sources are at the lowest latitudes and have the coolest [12-25]{mu}m colors. The bulge IRAS sources do not appear to represent a different or more luminous class of objects than the optically identified M giants. Five different estimators of the surface brightness and surface density between latitudes -3deg and -12deg have a power-law dependence on radius with exponent between -2.5 and -3.4. The value of the exponent depends on the metallicity of the estimator: the most metal-rich objects have the steepest falloff. However, even the smallest exponent, which characterizes the total light and mass distribution, places the bulge among the most spatially concentrated of those measured by Kent for a sample of 22 Sb-Sc galaxies. Thus the mass distribution within the inner 1.5 kpc of the Galaxy is quite sharply peaked.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/353/494#2</TD>
            <TD>2011-09-14T18:23:05Z</TD>
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            <TD>ParamHTTP</TD>
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          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/353/494 [1]</TD>
            <TD>JHKL photometry on Galactic bulge M Giants (Frogel+, 1990)</TD>
            <TD>JHKL colors and CO and H2O indices are presented for an unbiased sample of about 250 M giants drawn from complete surveys for such stars along the minor axis of the Galaxy at latitudes between -3deg and -12deg. Magnitudes at 10 {mu}m and narrow-band near-infrared colors for some of these stars are also given. At constant J-K the mean CO index of the bulge M giants weakens monotonically with increasing latitude. From the relation between CO and [Fe/H] established for star clusters, this would correspond to a decrease of ~0.4 dex in the mean [Fe/H] between the -3deg and -12deg fields, from somewhat greater to somewhat less than solar. These values are consistent with abundances derived from optical color-magnitude diagrams. Despite these high [Fe/H] values, the ridgelines of the color-magnitude diagrams for all fields lie between those of 47 Tucanae and M3. There is a mild blueward shift with increasing latitude seen in the integrated mean J-K colors of the fields. A steady progression with latitude in the mean (J-H, H-K) relation for the bulge M giants is observed. For the -12deg field it is significantly displaced from the one for local field giants and overlaps that for globular cluster stars; for the -3deg field it is displaced by about the same amount, but on the opposite side of the field giant relation. Dispersions about this relation and the mean (CO, J-K) relation for the M giants in each field are comparable in size to the measuring uncertainties alone, but in a given field the displacements of individual stars from these two mean relations are statistically correlated. We attribute this correlation to a spread in metallicity within each field but note that this spread is smaller than the total metallicity range over all fields. In addition, metallicity-related effects result in J-H getting bluer with increasing metallicity in stars of similar temperature. The bolometric luminosity function of the nonvariable M giants is nearly independent of latitude. All show a sharp cutoff at Mbol&lt;=-4.2; such a cutoff could be a good extragalactic distance indicator for bulgelike stellar populations. The reddest (J-K&gt;=-1.35) and most luminous stars are found only in the low-latitude windows; all are M7-M9 giants, long-period variables (LPVs), or both. Except for these reddest stars, the ratio at a given color of M7-M9 giants to earlier type giants is independent of latitude. Only when stars of all colors in a spectral group are considered is the rapid falloff seen in the ratio of M7-M9 giants respect to earlier types. The bulge LPVs have &lt;Mbol&gt; = -4.2. Since this is nearly the same as for LPVs in globular clusters, it does not require an age for the bulge population significantly younger than that of globular clusters. Their spatial distribution is similar to that of the reddest late M giants. The LPVs with the reddest colors, attributed to the most extensive circumstellar dust shells, are found in the lowest latitude fields. Most of the bulge IRAS sources in the fields studied can be identified with these LPVs or with the brightest nonvariable M giants; many of the latter are probably foreground objects. The reddest IRAS sources are at the lowest latitudes and have the coolest [12-25]{mu}m colors. The bulge IRAS sources do not appear to represent a different or more luminous class of objects than the optically identified M giants. Five different estimators of the surface brightness and surface density between latitudes -3deg and -12deg have a power-law dependence on radius with exponent between -2.5 and -3.4. The value of the exponent depends on the metallicity of the estimator: the most metal-rich objects have the steepest falloff. However, even the smallest exponent, which characterizes the total light and mass distribution, places the bulge among the most spatially concentrated of those measured by Kent for a sample of 22 Sb-Sc galaxies. Thus the mass distribution within the inner 1.5 kpc of the Galaxy is quite sharply peaked.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/353/494#1</TD>
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            <TD />
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/353/494</TD>
            <TD />
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/353/494 [2]</TD>
            <TD>JHKL photometry on Galactic bulge M Giants (Frogel+, 1990)</TD>
            <TD>JHKL colors and CO and H2O indices are presented for an unbiased sample of about 250 M giants drawn from complete surveys for such stars along the minor axis of the Galaxy at latitudes between -3deg and -12deg. Magnitudes at 10 {mu}m and narrow-band near-infrared colors for some of these stars are also given. At constant J-K the mean CO index of the bulge M giants weakens monotonically with increasing latitude. From the relation between CO and [Fe/H] established for star clusters, this would correspond to a decrease of ~0.4 dex in the mean [Fe/H] between the -3deg and -12deg fields, from somewhat greater to somewhat less than solar. These values are consistent with abundances derived from optical color-magnitude diagrams. Despite these high [Fe/H] values, the ridgelines of the color-magnitude diagrams for all fields lie between those of 47 Tucanae and M3. There is a mild blueward shift with increasing latitude seen in the integrated mean J-K colors of the fields. A steady progression with latitude in the mean (J-H, H-K) relation for the bulge M giants is observed. For the -12deg field it is significantly displaced from the one for local field giants and overlaps that for globular cluster stars; for the -3deg field it is displaced by about the same amount, but on the opposite side of the field giant relation. Dispersions about this relation and the mean (CO, J-K) relation for the M giants in each field are comparable in size to the measuring uncertainties alone, but in a given field the displacements of individual stars from these two mean relations are statistically correlated. We attribute this correlation to a spread in metallicity within each field but note that this spread is smaller than the total metallicity range over all fields. In addition, metallicity-related effects result in J-H getting bluer with increasing metallicity in stars of similar temperature. The bolometric luminosity function of the nonvariable M giants is nearly independent of latitude. All show a sharp cutoff at Mbol&lt;=-4.2; such a cutoff could be a good extragalactic distance indicator for bulgelike stellar populations. The reddest (J-K&gt;=-1.35) and most luminous stars are found only in the low-latitude windows; all are M7-M9 giants, long-period variables (LPVs), or both. Except for these reddest stars, the ratio at a given color of M7-M9 giants to earlier type giants is independent of latitude. Only when stars of all colors in a spectral group are considered is the rapid falloff seen in the ratio of M7-M9 giants respect to earlier types. The bulge LPVs have &lt;Mbol&gt; = -4.2. Since this is nearly the same as for LPVs in globular clusters, it does not require an age for the bulge population significantly younger than that of globular clusters. Their spatial distribution is similar to that of the reddest late M giants. The LPVs with the reddest colors, attributed to the most extensive circumstellar dust shells, are found in the lowest latitude fields. Most of the bulge IRAS sources in the fields studied can be identified with these LPVs or with the brightest nonvariable M giants; many of the latter are probably foreground objects. The reddest IRAS sources are at the lowest latitudes and have the coolest [12-25]{mu}m colors. The bulge IRAS sources do not appear to represent a different or more luminous class of objects than the optically identified M giants. Five different estimators of the surface brightness and surface density between latitudes -3deg and -12deg have a power-law dependence on radius with exponent between -2.5 and -3.4. The value of the exponent depends on the metallicity of the estimator: the most metal-rich objects have the steepest falloff. However, even the smallest exponent, which characterizes the total light and mass distribution, places the bulge among the most spatially concentrated of those measured by Kent for a sample of 22 Sb-Sc galaxies. Thus the mass distribution within the inner 1.5 kpc of the Galaxy is quite sharply peaked.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/353/494#2</TD>
            <TD>2011-09-14T18:23:05Z</TD>
            <TD>#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/353/494</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/353/494&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/353/494</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
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            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/438/181 [1]</TD>
            <TD>Observations of H II Regions in M81 (Hill+ 1995)</TD>
            <TD>Images of the type Sab spiral galaxy M81 were obtained in far-UV and near-UV bands by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Spacelab mission of 1990 December. Magnitudes in the two UV bands are determined for 52 H II regions from the catalog of Petit, Sivan, &amp; Karachentsev (1988A&amp;AS...74..475P). Fluxes of the H-alpha and H-beta emission lines are determined from CCD images. Extinctions for the brightest H II regions are determined from observed Balmer decrements. Fainter H II regions are assigned the average of published radio-H-alpha extinctions for several bright H II regions. The radiative transfer models of Witt, Thronson, &amp; Capuano (1992, ApJ, 393, 611) are shown to predict a relationship between Balmer Decrement and H-alpha extinction consistent with observed line and radio fluxes for the brightest 7 H II regions and are used to estimate the UV extinction. Ratios of Lyman continuum flux (computed from the extinction corrected H-alpha flux) to the extinction corrected far-UV flux are compared with ratios predicted by model spectra computed for IMF slope equal to -1.0 and stellar masses ranging from 5 to 120 Msun. Ages and masses are estimated by comparing the H-alpha and far-UV fluxes and their ratio with the models. The total of the estimated stellar masses for the 52 H II regions is 1.4x10^5^ Msun. The star-formation rate inferred for M81 from the observed UV and H-alpha fluxes is low for a spiral galaxy at ~0.13 Msun/yr, but consistent with the low star-formation rates obtained by Kennicutt (1983ApJ...272...54K) and Caldwell et al. (1991ApJ...370..526C) for early-type spirals.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/438/181#1</TD>
            <TD>2011-09-14T18:23:21Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/438/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/438/181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/438/181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/438/181 [2]</TD>
            <TD>Observations of H II Regions in M81 (Hill+ 1995)</TD>
            <TD>Images of the type Sab spiral galaxy M81 were obtained in far-UV and near-UV bands by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Spacelab mission of 1990 December. Magnitudes in the two UV bands are determined for 52 H II regions from the catalog of Petit, Sivan, &amp; Karachentsev (1988A&amp;AS...74..475P). Fluxes of the H-alpha and H-beta emission lines are determined from CCD images. Extinctions for the brightest H II regions are determined from observed Balmer decrements. Fainter H II regions are assigned the average of published radio-H-alpha extinctions for several bright H II regions. The radiative transfer models of Witt, Thronson, &amp; Capuano (1992, ApJ, 393, 611) are shown to predict a relationship between Balmer Decrement and H-alpha extinction consistent with observed line and radio fluxes for the brightest 7 H II regions and are used to estimate the UV extinction. Ratios of Lyman continuum flux (computed from the extinction corrected H-alpha flux) to the extinction corrected far-UV flux are compared with ratios predicted by model spectra computed for IMF slope equal to -1.0 and stellar masses ranging from 5 to 120 Msun. Ages and masses are estimated by comparing the H-alpha and far-UV fluxes and their ratio with the models. The total of the estimated stellar masses for the 52 H II regions is 1.4x10^5^ Msun. The star-formation rate inferred for M81 from the observed UV and H-alpha fluxes is low for a spiral galaxy at ~0.13 Msun/yr, but consistent with the low star-formation rates obtained by Kennicutt (1983ApJ...272...54K) and Caldwell et al. (1991ApJ...370..526C) for early-type spirals.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/438/181#2</TD>
            <TD>2011-09-14T18:23:21Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/438/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/438/181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/438/181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/438/181 [1]</TD>
            <TD>Observations of H II Regions in M81 (Hill+ 1995)</TD>
            <TD>Images of the type Sab spiral galaxy M81 were obtained in far-UV and near-UV bands by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Spacelab mission of 1990 December. Magnitudes in the two UV bands are determined for 52 H II regions from the catalog of Petit, Sivan, &amp; Karachentsev (1988A&amp;AS...74..475P). Fluxes of the H-alpha and H-beta emission lines are determined from CCD images. Extinctions for the brightest H II regions are determined from observed Balmer decrements. Fainter H II regions are assigned the average of published radio-H-alpha extinctions for several bright H II regions. The radiative transfer models of Witt, Thronson, &amp; Capuano (1992, ApJ, 393, 611) are shown to predict a relationship between Balmer Decrement and H-alpha extinction consistent with observed line and radio fluxes for the brightest 7 H II regions and are used to estimate the UV extinction. Ratios of Lyman continuum flux (computed from the extinction corrected H-alpha flux) to the extinction corrected far-UV flux are compared with ratios predicted by model spectra computed for IMF slope equal to -1.0 and stellar masses ranging from 5 to 120 Msun. Ages and masses are estimated by comparing the H-alpha and far-UV fluxes and their ratio with the models. The total of the estimated stellar masses for the 52 H II regions is 1.4x10^5^ Msun. The star-formation rate inferred for M81 from the observed UV and H-alpha fluxes is low for a spiral galaxy at ~0.13 Msun/yr, but consistent with the low star-formation rates obtained by Kennicutt (1983ApJ...272...54K) and Caldwell et al. (1991ApJ...370..526C) for early-type spirals.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/438/181#1</TD>
            <TD>2011-09-14T18:23:21Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/438/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/438/181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/438/181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/438/181 [2]</TD>
            <TD>Observations of H II Regions in M81 (Hill+ 1995)</TD>
            <TD>Images of the type Sab spiral galaxy M81 were obtained in far-UV and near-UV bands by the Ultraviolet Imaging Telescope (UIT) during the Astro-1 Spacelab mission of 1990 December. Magnitudes in the two UV bands are determined for 52 H II regions from the catalog of Petit, Sivan, &amp; Karachentsev (1988A&amp;AS...74..475P). Fluxes of the H-alpha and H-beta emission lines are determined from CCD images. Extinctions for the brightest H II regions are determined from observed Balmer decrements. Fainter H II regions are assigned the average of published radio-H-alpha extinctions for several bright H II regions. The radiative transfer models of Witt, Thronson, &amp; Capuano (1992, ApJ, 393, 611) are shown to predict a relationship between Balmer Decrement and H-alpha extinction consistent with observed line and radio fluxes for the brightest 7 H II regions and are used to estimate the UV extinction. Ratios of Lyman continuum flux (computed from the extinction corrected H-alpha flux) to the extinction corrected far-UV flux are compared with ratios predicted by model spectra computed for IMF slope equal to -1.0 and stellar masses ranging from 5 to 120 Msun. Ages and masses are estimated by comparing the H-alpha and far-UV fluxes and their ratio with the models. The total of the estimated stellar masses for the 52 H II regions is 1.4x10^5^ Msun. The star-formation rate inferred for M81 from the observed UV and H-alpha fluxes is low for a spiral galaxy at ~0.13 Msun/yr, but consistent with the low star-formation rates obtained by Kennicutt (1983ApJ...272...54K) and Caldwell et al. (1991ApJ...370..526C) for early-type spirals.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/438/181#2</TD>
            <TD>2011-09-14T18:23:21Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/438/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/438/181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/438/181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/458/455 [1]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#1</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/458/455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/458/455 [2]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#2</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/458/455 [table7]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#table7</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/458/455 [table6]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#table6</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/458/455 [table3]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#table3</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/458/455 [1]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#1</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/458/455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/458/455 [2]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#2</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/458/455 [table7]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#table7</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/458/455 [table6]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#table6</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/458/455 [table3]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#table3</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/458/455 [1]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#1</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/458/455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/458/455 [2]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#2</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/458/455 [table7]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#table7</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/458/455 [table6]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#table6</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/458/455 [table3]</TD>
            <TD>M 104 planetary nebulae (Ford+ 1996)</TD>
            <TD>We used the CTIO 4m telescope to make a complete and kinematically unbiased survey of M104 (NGC 4594; the Sombrero galaxy) for planetary nebulae (i.e., stars) out to 16 kpc. We present the positions and monochromatic [O III] lambda 5007 magnitudes of 294 planetaries, and use the observed planetary nebula luminosity function (PNLF) to measure a distance of 8.9+/-0.6Mpc to the galaxy. The luminosity-specific PN number lambda 2.5 in the halo of M104 is approximately 21.7x10^-9^L_{sun}_, which for its color (B-V)=0.95, is comparable to the values in other galaxies. We use the PNLF distance to M104 to compare its luminosity to the luminosities of the brightest galaxies in the Virgo Cluster, finding that if M104 were in the Virgo Cluster, it would be the third brightest galaxy. We combined the PNLF distance and the observed velocity corrected for Virgo infall to calculate a Hubble constant H_0_=91+/-8km/s/Mpc. We also used the PNLF distances to the NGC 1023 group, the Leo group, the Virgo Cluster, and the Fornax Cluster to derive Hubble constants corrected for Virgo infall. The values of H_0_ for M104, the NGC 1023 group, the Virgo Cluster, and the Fornax Cluster are in excellent agreement, suggesting that the PNLF distances and Schechter's linear infall model provide a self-consistent representation of the Hubble expansion and Virgo infall within most regions of the local supercluster. The unweighted mean of the four values is H_0_=84+/-4. The value of H_0_ derived for the Leo group differs by four standard deviations from the mean of the other four measurements. We conclude that there may be large peculiar motions in the spatially extended Leo spur.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455#table3</TD>
            <TD>2011-09-14T18:23:36Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/458/455</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/458/455&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/458/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/459/110 [1]</TD>
            <TD>Line strengths and gradients in S0 galaxies (Fisher+ 1996)</TD>
            <TD>Line strengths and their gradients in Mg, Fe, and HBeta have been determined for a sample of 20 S0 galaxies in order to study the stellar populations of their bulges and disks and to investigate their relationship to elliptical galaxies. Data are also presented for the elliptical galaxy NGC 1700 and the E/S0 NGC 3585. We find that S0 galaxies generally follow a similar, though possibly steeper, relationship between central Mg_2 line strength and central velocity dispersion as found for elliptical galaxies. The S0 galaxies show no dependence between Fe line strengths and central velocity dispersion -- similar to the behavior observed in elliptical galaxies. The central Mg/Fe ratios in the luminous S0 galaxies show an overabundance of Mg to Fe with respect to solar element ratios. The magnitudes of the Mg and Fe line-strength gradients within the galaxies are found to be correlated, i.e., objects with steep Mg gradients have correspondingly large Fe gradients. We infer bulge and disk gradients for the nine most edge-on galaxies for which we have both major- and minor-axis profiles. The metal line strengths decrease with radius along the major and minor axes in the bulge-dominated central regions. At larger radii, however, the major-axis metal line strength profiles flatten while the minor-axis bulge profiles fall to lower values. Representative color maps in B-R are presented that display a separation between bulge and disk colors corresponding to the metal line strength profiles. Based on our Mg_2 profiles, the average metal gradient found in the disks of our sub-sample is Delta[Fe/H]/Delta(r/h)=-0.08+/-0.06, which corresponds to a reduction in the mean metallicity of the disk stellar population by &lt;~15% per disk scale length (h). These shallow metallicity gradients are approximately a factor of 2-3 smaller than those derived for the disks of late-type spiral galaxies from H II regions and are consistent with previous investigations that showed a trend for disk metallicity gradients to decrease toward earlier Hubble types. As inferred from our Mg and Fe line strengths, the mean size of the bulge metallicity gradients is Delta[Fe/H]/Delta(log r)=-0.7+/-0.4, which is steeper than typical elliptical galaxy gradients. Our findings do not support formation scenarios in which bulges formed either from heated disk material at late times after disk formation or through dissipationless stellar merging, as neither process includes mechanisms for producing the observed metallicity gradients. Our observations are better explained in terms of formation via dissipative collapse (or merging) at early times.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/459/110#1</TD>
            <TD>2011-09-14T18:23:37Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/459/110</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/459/110</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/459/110</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/459/110 [2]</TD>
            <TD>Line strengths and gradients in S0 galaxies (Fisher+ 1996)</TD>
            <TD>Line strengths and their gradients in Mg, Fe, and HBeta have been determined for a sample of 20 S0 galaxies in order to study the stellar populations of their bulges and disks and to investigate their relationship to elliptical galaxies. Data are also presented for the elliptical galaxy NGC 1700 and the E/S0 NGC 3585. We find that S0 galaxies generally follow a similar, though possibly steeper, relationship between central Mg_2 line strength and central velocity dispersion as found for elliptical galaxies. The S0 galaxies show no dependence between Fe line strengths and central velocity dispersion -- similar to the behavior observed in elliptical galaxies. The central Mg/Fe ratios in the luminous S0 galaxies show an overabundance of Mg to Fe with respect to solar element ratios. The magnitudes of the Mg and Fe line-strength gradients within the galaxies are found to be correlated, i.e., objects with steep Mg gradients have correspondingly large Fe gradients. We infer bulge and disk gradients for the nine most edge-on galaxies for which we have both major- and minor-axis profiles. The metal line strengths decrease with radius along the major and minor axes in the bulge-dominated central regions. At larger radii, however, the major-axis metal line strength profiles flatten while the minor-axis bulge profiles fall to lower values. Representative color maps in B-R are presented that display a separation between bulge and disk colors corresponding to the metal line strength profiles. Based on our Mg_2 profiles, the average metal gradient found in the disks of our sub-sample is Delta[Fe/H]/Delta(r/h)=-0.08+/-0.06, which corresponds to a reduction in the mean metallicity of the disk stellar population by &lt;~15% per disk scale length (h). These shallow metallicity gradients are approximately a factor of 2-3 smaller than those derived for the disks of late-type spiral galaxies from H II regions and are consistent with previous investigations that showed a trend for disk metallicity gradients to decrease toward earlier Hubble types. As inferred from our Mg and Fe line strengths, the mean size of the bulge metallicity gradients is Delta[Fe/H]/Delta(log r)=-0.7+/-0.4, which is steeper than typical elliptical galaxy gradients. Our findings do not support formation scenarios in which bulges formed either from heated disk material at late times after disk formation or through dissipationless stellar merging, as neither process includes mechanisms for producing the observed metallicity gradients. Our observations are better explained in terms of formation via dissipative collapse (or merging) at early times.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/459/110#2</TD>
            <TD>2011-09-14T18:23:37Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/459/110</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/459/110&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/459/110</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/459/110 [1]</TD>
            <TD>Line strengths and gradients in S0 galaxies (Fisher+ 1996)</TD>
            <TD>Line strengths and their gradients in Mg, Fe, and HBeta have been determined for a sample of 20 S0 galaxies in order to study the stellar populations of their bulges and disks and to investigate their relationship to elliptical galaxies. Data are also presented for the elliptical galaxy NGC 1700 and the E/S0 NGC 3585. We find that S0 galaxies generally follow a similar, though possibly steeper, relationship between central Mg_2 line strength and central velocity dispersion as found for elliptical galaxies. The S0 galaxies show no dependence between Fe line strengths and central velocity dispersion -- similar to the behavior observed in elliptical galaxies. The central Mg/Fe ratios in the luminous S0 galaxies show an overabundance of Mg to Fe with respect to solar element ratios. The magnitudes of the Mg and Fe line-strength gradients within the galaxies are found to be correlated, i.e., objects with steep Mg gradients have correspondingly large Fe gradients. We infer bulge and disk gradients for the nine most edge-on galaxies for which we have both major- and minor-axis profiles. The metal line strengths decrease with radius along the major and minor axes in the bulge-dominated central regions. At larger radii, however, the major-axis metal line strength profiles flatten while the minor-axis bulge profiles fall to lower values. Representative color maps in B-R are presented that display a separation between bulge and disk colors corresponding to the metal line strength profiles. Based on our Mg_2 profiles, the average metal gradient found in the disks of our sub-sample is Delta[Fe/H]/Delta(r/h)=-0.08+/-0.06, which corresponds to a reduction in the mean metallicity of the disk stellar population by &lt;~15% per disk scale length (h). These shallow metallicity gradients are approximately a factor of 2-3 smaller than those derived for the disks of late-type spiral galaxies from H II regions and are consistent with previous investigations that showed a trend for disk metallicity gradients to decrease toward earlier Hubble types. As inferred from our Mg and Fe line strengths, the mean size of the bulge metallicity gradients is Delta[Fe/H]/Delta(log r)=-0.7+/-0.4, which is steeper than typical elliptical galaxy gradients. Our findings do not support formation scenarios in which bulges formed either from heated disk material at late times after disk formation or through dissipationless stellar merging, as neither process includes mechanisms for producing the observed metallicity gradients. Our observations are better explained in terms of formation via dissipative collapse (or merging) at early times.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/459/110#1</TD>
            <TD>2011-09-14T18:23:37Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/459/110</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/459/110</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/459/110</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/459/110 [2]</TD>
            <TD>Line strengths and gradients in S0 galaxies (Fisher+ 1996)</TD>
            <TD>Line strengths and their gradients in Mg, Fe, and HBeta have been determined for a sample of 20 S0 galaxies in order to study the stellar populations of their bulges and disks and to investigate their relationship to elliptical galaxies. Data are also presented for the elliptical galaxy NGC 1700 and the E/S0 NGC 3585. We find that S0 galaxies generally follow a similar, though possibly steeper, relationship between central Mg_2 line strength and central velocity dispersion as found for elliptical galaxies. The S0 galaxies show no dependence between Fe line strengths and central velocity dispersion -- similar to the behavior observed in elliptical galaxies. The central Mg/Fe ratios in the luminous S0 galaxies show an overabundance of Mg to Fe with respect to solar element ratios. The magnitudes of the Mg and Fe line-strength gradients within the galaxies are found to be correlated, i.e., objects with steep Mg gradients have correspondingly large Fe gradients. We infer bulge and disk gradients for the nine most edge-on galaxies for which we have both major- and minor-axis profiles. The metal line strengths decrease with radius along the major and minor axes in the bulge-dominated central regions. At larger radii, however, the major-axis metal line strength profiles flatten while the minor-axis bulge profiles fall to lower values. Representative color maps in B-R are presented that display a separation between bulge and disk colors corresponding to the metal line strength profiles. Based on our Mg_2 profiles, the average metal gradient found in the disks of our sub-sample is Delta[Fe/H]/Delta(r/h)=-0.08+/-0.06, which corresponds to a reduction in the mean metallicity of the disk stellar population by &lt;~15% per disk scale length (h). These shallow metallicity gradients are approximately a factor of 2-3 smaller than those derived for the disks of late-type spiral galaxies from H II regions and are consistent with previous investigations that showed a trend for disk metallicity gradients to decrease toward earlier Hubble types. As inferred from our Mg and Fe line strengths, the mean size of the bulge metallicity gradients is Delta[Fe/H]/Delta(log r)=-0.7+/-0.4, which is steeper than typical elliptical galaxy gradients. Our findings do not support formation scenarios in which bulges formed either from heated disk material at late times after disk formation or through dissipationless stellar merging, as neither process includes mechanisms for producing the observed metallicity gradients. Our observations are better explained in terms of formation via dissipative collapse (or merging) at early times.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/459/110#2</TD>
            <TD>2011-09-14T18:23:37Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/459/110</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/459/110&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/459/110</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/105/93 [1]</TD>
            <TD>H II Regions in Nearby Seyfert Galaxies (Evans+ 1996)</TD>
            <TD>Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93#1</TD>
            <TD>2011-09-14T18:23:53Z</TD>
            <TD>#Seyfert_Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/105/93</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/93</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/105/93 [2]</TD>
            <TD>H II Regions in Nearby Seyfert Galaxies (Evans+ 1996)</TD>
            <TD>Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93#2</TD>
            <TD>2011-09-14T18:23:53Z</TD>
            <TD>#Seyfert_Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/105/93&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/93</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/105/93 [table2]</TD>
            <TD>H II Regions in Nearby Seyfert Galaxies (Evans+ 1996)</TD>
            <TD>Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93#table2</TD>
            <TD>2011-09-14T18:23:53Z</TD>
            <TD>#Seyfert_Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/105/93&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/93</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [1]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#1</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [2]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#2</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [3]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#3</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [4]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#4</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [5]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#5</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [6]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#6</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [7]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#7</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [8]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#8</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [9]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#9</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR7 [10]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#10</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/DirectCone?DSACAT=UKIDSS_DR7&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [11]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#11</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR7 [12]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#12</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [13]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#13</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [14]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#14</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [15]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#15</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [16]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#16</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [17]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#17</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [18]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#18</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR7 [19]</TD>
            <TD>UKIDSS DR7 - UKIRT Infrared Deep Sky Survey Data Release 7</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from three of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey. The Galactic Plane Survey will be available in march 2012. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa#19</TD>
            <TD>2012-07-18T12:47:40Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 7</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR7-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR7-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/105/93 [1]</TD>
            <TD>H II Regions in Nearby Seyfert Galaxies (Evans+ 1996)</TD>
            <TD>Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93#1</TD>
            <TD>2011-09-14T18:23:53Z</TD>
            <TD>#Seyfert_Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/105/93</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/93</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/105/93 [2]</TD>
            <TD>H II Regions in Nearby Seyfert Galaxies (Evans+ 1996)</TD>
            <TD>Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93#2</TD>
            <TD>2011-09-14T18:23:53Z</TD>
            <TD>#Seyfert_Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/105/93&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/93</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/105/93 [table2]</TD>
            <TD>H II Regions in Nearby Seyfert Galaxies (Evans+ 1996)</TD>
            <TD>Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93#table2</TD>
            <TD>2011-09-14T18:23:53Z</TD>
            <TD>#Seyfert_Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/105/93&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/93</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/543/A156 [1]</TD>
            <TD>Milky Way global survey of star clusters (Kharchenko+, 2012)</TD>
            <TD>An all-sky target list of 3784 entries with initial cluster parameters was compiled from sources available in the literature. As the primary source we used the data from the Catalogue of Open Cluster Data (COCD, Kharchenko et al. 2005a,b, Cat. J/A+A/438/1163, J/A+A/440/403). For further optical clusters the data were taken from the Dias et al. (2002, Cat. B/ocl) list (Version 3.1, 24/nov/2010). Known associations were retrieved from Melnik &amp; Dambis (2009, Cat. J/MNRAS/400/518). For clusters detected in the NIR the information came from Bica et al. (2003b, Cat. J/A+A/404/223), Dutra et al. (2003, Cat. J/A+A/400/533), Froebrich et al. (2007, Cat. J/MNRAS/374/399). Globular clusters were selected from the catalogue by Harris (1996) (edition 2010, 2010arXiv1012.3224H). Additionally, we incorporated supplementary data on embedded clusters from Bica et al. (2003a, Cat. J/A+A/397/177), Lada &amp; Lada (2003ARA&amp;A..41...57L) and on stars in associations from Humphreys (1978, Cat. V/44). The basic stellar data were taken from the all-sky catalogue 2MAst (2Mass with Astrometry), that was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010, Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). Additionally, we incorporated data on radial velocities from Kharchenko et al. (2007, Cat. III/254) and spectral types from ASCC-2.5 (Kharchenko &amp; Roeser 2009, Cat. I/280). Around each object from our target list we defined a circular area with a radius of ra=r2+radd where r2 is cluster radius, and radd=0.3{deg}. In these areas we selected in 2MAst only those stars with flags Rflg (the 2nd triple of the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars with the best quality detections in photometric and astrometric data. There are 871 targets in the 2nd Galaxy quadrant, we confirmed 650 open clusters and/or associations. These 650 sky areas contain about 11.2 mln 2MAst stars with best quality detections in photometric and astrometric data. We selected 30387 most probable members located in the central cluster regions and determined - with a homogeneous method/pipeline - angular sizes of the main morphological parts, heliocentric distances, colour-excesses, mean proper motions, sometimes radial velocities, ages, tidal parameters. There are 4 globular clusters in the 2nd quadrant, they are listed in index_q2.dat, but the data for globular clusters will be submitted to the CDS as a separate catalogue. We present for the 2nd quadrant of the Milky Way: The Catalogue of the MWSC Data with: Catalogue of parameters for confirmed clusters; Index (full list) of MWSC objects; Notes (full object list with notes); Inside each list the entries are ordered by MWSC number (i.e. right ascension J2000 from the target list). The Catalogues of the MWSC Stars in 650 circular sky areas with classified clusters. Files are ordered by MWSC number order; inside each sky area the entries are ordered by Ks magnitudes. The Atlas of MWSC diagrams. In the Atlas the Cluster pages are ordered by MWSC number.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156#1</TD>
            <TD>2012-07-27T09:53:20Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/543/A156</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A156</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/543/A156 [2]</TD>
            <TD>Milky Way global survey of star clusters (Kharchenko+, 2012)</TD>
            <TD>An all-sky target list of 3784 entries with initial cluster parameters was compiled from sources available in the literature. As the primary source we used the data from the Catalogue of Open Cluster Data (COCD, Kharchenko et al. 2005a,b, Cat. J/A+A/438/1163, J/A+A/440/403). For further optical clusters the data were taken from the Dias et al. (2002, Cat. B/ocl) list (Version 3.1, 24/nov/2010). Known associations were retrieved from Melnik &amp; Dambis (2009, Cat. J/MNRAS/400/518). For clusters detected in the NIR the information came from Bica et al. (2003b, Cat. J/A+A/404/223), Dutra et al. (2003, Cat. J/A+A/400/533), Froebrich et al. (2007, Cat. J/MNRAS/374/399). Globular clusters were selected from the catalogue by Harris (1996) (edition 2010, 2010arXiv1012.3224H). Additionally, we incorporated supplementary data on embedded clusters from Bica et al. (2003a, Cat. J/A+A/397/177), Lada &amp; Lada (2003ARA&amp;A..41...57L) and on stars in associations from Humphreys (1978, Cat. V/44). The basic stellar data were taken from the all-sky catalogue 2MAst (2Mass with Astrometry), that was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010, Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). Additionally, we incorporated data on radial velocities from Kharchenko et al. (2007, Cat. III/254) and spectral types from ASCC-2.5 (Kharchenko &amp; Roeser 2009, Cat. I/280). Around each object from our target list we defined a circular area with a radius of ra=r2+radd where r2 is cluster radius, and radd=0.3{deg}. In these areas we selected in 2MAst only those stars with flags Rflg (the 2nd triple of the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars with the best quality detections in photometric and astrometric data. There are 871 targets in the 2nd Galaxy quadrant, we confirmed 650 open clusters and/or associations. These 650 sky areas contain about 11.2 mln 2MAst stars with best quality detections in photometric and astrometric data. We selected 30387 most probable members located in the central cluster regions and determined - with a homogeneous method/pipeline - angular sizes of the main morphological parts, heliocentric distances, colour-excesses, mean proper motions, sometimes radial velocities, ages, tidal parameters. There are 4 globular clusters in the 2nd quadrant, they are listed in index_q2.dat, but the data for globular clusters will be submitted to the CDS as a separate catalogue. We present for the 2nd quadrant of the Milky Way: The Catalogue of the MWSC Data with: Catalogue of parameters for confirmed clusters; Index (full list) of MWSC objects; Notes (full object list with notes); Inside each list the entries are ordered by MWSC number (i.e. right ascension J2000 from the target list). The Catalogues of the MWSC Stars in 650 circular sky areas with classified clusters. Files are ordered by MWSC number order; inside each sky area the entries are ordered by Ks magnitudes. The Atlas of MWSC diagrams. In the Atlas the Cluster pages are ordered by MWSC number.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156#2</TD>
            <TD>2012-07-27T09:53:20Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/543/A156&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A156</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/543/A156 [catal_q2]</TD>
            <TD>Milky Way global survey of star clusters (Kharchenko+, 2012)</TD>
            <TD>An all-sky target list of 3784 entries with initial cluster parameters was compiled from sources available in the literature. As the primary source we used the data from the Catalogue of Open Cluster Data (COCD, Kharchenko et al. 2005a,b, Cat. J/A+A/438/1163, J/A+A/440/403). For further optical clusters the data were taken from the Dias et al. (2002, Cat. B/ocl) list (Version 3.1, 24/nov/2010). Known associations were retrieved from Melnik &amp; Dambis (2009, Cat. J/MNRAS/400/518). For clusters detected in the NIR the information came from Bica et al. (2003b, Cat. J/A+A/404/223), Dutra et al. (2003, Cat. J/A+A/400/533), Froebrich et al. (2007, Cat. J/MNRAS/374/399). Globular clusters were selected from the catalogue by Harris (1996) (edition 2010, 2010arXiv1012.3224H). Additionally, we incorporated supplementary data on embedded clusters from Bica et al. (2003a, Cat. J/A+A/397/177), Lada &amp; Lada (2003ARA&amp;A..41...57L) and on stars in associations from Humphreys (1978, Cat. V/44). The basic stellar data were taken from the all-sky catalogue 2MAst (2Mass with Astrometry), that was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010, Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). Additionally, we incorporated data on radial velocities from Kharchenko et al. (2007, Cat. III/254) and spectral types from ASCC-2.5 (Kharchenko &amp; Roeser 2009, Cat. I/280). Around each object from our target list we defined a circular area with a radius of ra=r2+radd where r2 is cluster radius, and radd=0.3{deg}. In these areas we selected in 2MAst only those stars with flags Rflg (the 2nd triple of the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars with the best quality detections in photometric and astrometric data. There are 871 targets in the 2nd Galaxy quadrant, we confirmed 650 open clusters and/or associations. These 650 sky areas contain about 11.2 mln 2MAst stars with best quality detections in photometric and astrometric data. We selected 30387 most probable members located in the central cluster regions and determined - with a homogeneous method/pipeline - angular sizes of the main morphological parts, heliocentric distances, colour-excesses, mean proper motions, sometimes radial velocities, ages, tidal parameters. There are 4 globular clusters in the 2nd quadrant, they are listed in index_q2.dat, but the data for globular clusters will be submitted to the CDS as a separate catalogue. We present for the 2nd quadrant of the Milky Way: The Catalogue of the MWSC Data with: Catalogue of parameters for confirmed clusters; Index (full list) of MWSC objects; Notes (full object list with notes); Inside each list the entries are ordered by MWSC number (i.e. right ascension J2000 from the target list). The Catalogues of the MWSC Stars in 650 circular sky areas with classified clusters. Files are ordered by MWSC number order; inside each sky area the entries are ordered by Ks magnitudes. The Atlas of MWSC diagrams. In the Atlas the Cluster pages are ordered by MWSC number.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156#catal_q2</TD>
            <TD>2012-07-27T09:53:20Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/543/A156&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A156</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/543/A156 [1]</TD>
            <TD>Milky Way global survey of star clusters (Kharchenko+, 2012)</TD>
            <TD>An all-sky target list of 3784 entries with initial cluster parameters was compiled from sources available in the literature. As the primary source we used the data from the Catalogue of Open Cluster Data (COCD, Kharchenko et al. 2005a,b, Cat. J/A+A/438/1163, J/A+A/440/403). For further optical clusters the data were taken from the Dias et al. (2002, Cat. B/ocl) list (Version 3.1, 24/nov/2010). Known associations were retrieved from Melnik &amp; Dambis (2009, Cat. J/MNRAS/400/518). For clusters detected in the NIR the information came from Bica et al. (2003b, Cat. J/A+A/404/223), Dutra et al. (2003, Cat. J/A+A/400/533), Froebrich et al. (2007, Cat. J/MNRAS/374/399). Globular clusters were selected from the catalogue by Harris (1996) (edition 2010, 2010arXiv1012.3224H). Additionally, we incorporated supplementary data on embedded clusters from Bica et al. (2003a, Cat. J/A+A/397/177), Lada &amp; Lada (2003ARA&amp;A..41...57L) and on stars in associations from Humphreys (1978, Cat. V/44). The basic stellar data were taken from the all-sky catalogue 2MAst (2Mass with Astrometry), that was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010, Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). Additionally, we incorporated data on radial velocities from Kharchenko et al. (2007, Cat. III/254) and spectral types from ASCC-2.5 (Kharchenko &amp; Roeser 2009, Cat. I/280). Around each object from our target list we defined a circular area with a radius of ra=r2+radd where r2 is cluster radius, and radd=0.3{deg}. In these areas we selected in 2MAst only those stars with flags Rflg (the 2nd triple of the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars with the best quality detections in photometric and astrometric data. There are 871 targets in the 2nd Galaxy quadrant, we confirmed 650 open clusters and/or associations. These 650 sky areas contain about 11.2 mln 2MAst stars with best quality detections in photometric and astrometric data. We selected 30387 most probable members located in the central cluster regions and determined - with a homogeneous method/pipeline - angular sizes of the main morphological parts, heliocentric distances, colour-excesses, mean proper motions, sometimes radial velocities, ages, tidal parameters. There are 4 globular clusters in the 2nd quadrant, they are listed in index_q2.dat, but the data for globular clusters will be submitted to the CDS as a separate catalogue. We present for the 2nd quadrant of the Milky Way: The Catalogue of the MWSC Data with: Catalogue of parameters for confirmed clusters; Index (full list) of MWSC objects; Notes (full object list with notes); Inside each list the entries are ordered by MWSC number (i.e. right ascension J2000 from the target list). The Catalogues of the MWSC Stars in 650 circular sky areas with classified clusters. Files are ordered by MWSC number order; inside each sky area the entries are ordered by Ks magnitudes. The Atlas of MWSC diagrams. In the Atlas the Cluster pages are ordered by MWSC number.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156#1</TD>
            <TD>2012-07-27T09:53:20Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/543/A156</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A156</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/543/A156 [2]</TD>
            <TD>Milky Way global survey of star clusters (Kharchenko+, 2012)</TD>
            <TD>An all-sky target list of 3784 entries with initial cluster parameters was compiled from sources available in the literature. As the primary source we used the data from the Catalogue of Open Cluster Data (COCD, Kharchenko et al. 2005a,b, Cat. J/A+A/438/1163, J/A+A/440/403). For further optical clusters the data were taken from the Dias et al. (2002, Cat. B/ocl) list (Version 3.1, 24/nov/2010). Known associations were retrieved from Melnik &amp; Dambis (2009, Cat. J/MNRAS/400/518). For clusters detected in the NIR the information came from Bica et al. (2003b, Cat. J/A+A/404/223), Dutra et al. (2003, Cat. J/A+A/400/533), Froebrich et al. (2007, Cat. J/MNRAS/374/399). Globular clusters were selected from the catalogue by Harris (1996) (edition 2010, 2010arXiv1012.3224H). Additionally, we incorporated supplementary data on embedded clusters from Bica et al. (2003a, Cat. J/A+A/397/177), Lada &amp; Lada (2003ARA&amp;A..41...57L) and on stars in associations from Humphreys (1978, Cat. V/44). The basic stellar data were taken from the all-sky catalogue 2MAst (2Mass with Astrometry), that was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010, Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). Additionally, we incorporated data on radial velocities from Kharchenko et al. (2007, Cat. III/254) and spectral types from ASCC-2.5 (Kharchenko &amp; Roeser 2009, Cat. I/280). Around each object from our target list we defined a circular area with a radius of ra=r2+radd where r2 is cluster radius, and radd=0.3{deg}. In these areas we selected in 2MAst only those stars with flags Rflg (the 2nd triple of the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars with the best quality detections in photometric and astrometric data. There are 871 targets in the 2nd Galaxy quadrant, we confirmed 650 open clusters and/or associations. These 650 sky areas contain about 11.2 mln 2MAst stars with best quality detections in photometric and astrometric data. We selected 30387 most probable members located in the central cluster regions and determined - with a homogeneous method/pipeline - angular sizes of the main morphological parts, heliocentric distances, colour-excesses, mean proper motions, sometimes radial velocities, ages, tidal parameters. There are 4 globular clusters in the 2nd quadrant, they are listed in index_q2.dat, but the data for globular clusters will be submitted to the CDS as a separate catalogue. We present for the 2nd quadrant of the Milky Way: The Catalogue of the MWSC Data with: Catalogue of parameters for confirmed clusters; Index (full list) of MWSC objects; Notes (full object list with notes); Inside each list the entries are ordered by MWSC number (i.e. right ascension J2000 from the target list). The Catalogues of the MWSC Stars in 650 circular sky areas with classified clusters. Files are ordered by MWSC number order; inside each sky area the entries are ordered by Ks magnitudes. The Atlas of MWSC diagrams. In the Atlas the Cluster pages are ordered by MWSC number.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156#2</TD>
            <TD>2012-07-27T09:53:20Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/543/A156&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A156</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/543/A156 [catal_q2]</TD>
            <TD>Milky Way global survey of star clusters (Kharchenko+, 2012)</TD>
            <TD>An all-sky target list of 3784 entries with initial cluster parameters was compiled from sources available in the literature. As the primary source we used the data from the Catalogue of Open Cluster Data (COCD, Kharchenko et al. 2005a,b, Cat. J/A+A/438/1163, J/A+A/440/403). For further optical clusters the data were taken from the Dias et al. (2002, Cat. B/ocl) list (Version 3.1, 24/nov/2010). Known associations were retrieved from Melnik &amp; Dambis (2009, Cat. J/MNRAS/400/518). For clusters detected in the NIR the information came from Bica et al. (2003b, Cat. J/A+A/404/223), Dutra et al. (2003, Cat. J/A+A/400/533), Froebrich et al. (2007, Cat. J/MNRAS/374/399). Globular clusters were selected from the catalogue by Harris (1996) (edition 2010, 2010arXiv1012.3224H). Additionally, we incorporated supplementary data on embedded clusters from Bica et al. (2003a, Cat. J/A+A/397/177), Lada &amp; Lada (2003ARA&amp;A..41...57L) and on stars in associations from Humphreys (1978, Cat. V/44). The basic stellar data were taken from the all-sky catalogue 2MAst (2Mass with Astrometry), that was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010, Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). Additionally, we incorporated data on radial velocities from Kharchenko et al. (2007, Cat. III/254) and spectral types from ASCC-2.5 (Kharchenko &amp; Roeser 2009, Cat. I/280). Around each object from our target list we defined a circular area with a radius of ra=r2+radd where r2 is cluster radius, and radd=0.3{deg}. In these areas we selected in 2MAst only those stars with flags Rflg (the 2nd triple of the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars with the best quality detections in photometric and astrometric data. There are 871 targets in the 2nd Galaxy quadrant, we confirmed 650 open clusters and/or associations. These 650 sky areas contain about 11.2 mln 2MAst stars with best quality detections in photometric and astrometric data. We selected 30387 most probable members located in the central cluster regions and determined - with a homogeneous method/pipeline - angular sizes of the main morphological parts, heliocentric distances, colour-excesses, mean proper motions, sometimes radial velocities, ages, tidal parameters. There are 4 globular clusters in the 2nd quadrant, they are listed in index_q2.dat, but the data for globular clusters will be submitted to the CDS as a separate catalogue. We present for the 2nd quadrant of the Milky Way: The Catalogue of the MWSC Data with: Catalogue of parameters for confirmed clusters; Index (full list) of MWSC objects; Notes (full object list with notes); Inside each list the entries are ordered by MWSC number (i.e. right ascension J2000 from the target list). The Catalogues of the MWSC Stars in 650 circular sky areas with classified clusters. Files are ordered by MWSC number order; inside each sky area the entries are ordered by Ks magnitudes. The Atlas of MWSC diagrams. In the Atlas the Cluster pages are ordered by MWSC number.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156#catal_q2</TD>
            <TD>2012-07-27T09:53:20Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/543/A156&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A156</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/105/93 [1]</TD>
            <TD>H II Regions in Nearby Seyfert Galaxies (Evans+ 1996)</TD>
            <TD>Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93#1</TD>
            <TD>2011-09-14T18:23:53Z</TD>
            <TD>#Seyfert_Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/105/93</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/93</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/105/93 [2]</TD>
            <TD>H II Regions in Nearby Seyfert Galaxies (Evans+ 1996)</TD>
            <TD>Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93#2</TD>
            <TD>2011-09-14T18:23:53Z</TD>
            <TD>#Seyfert_Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/105/93&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/93</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/105/93 [table2]</TD>
            <TD>H II Regions in Nearby Seyfert Galaxies (Evans+ 1996)</TD>
            <TD>Continuum-subtracted Halpha images of 17 nearby Seyfert galaxies are presented. The images are calibrated astrometrically using the Hubble Space Telescope Guide Star Catalog reference frame. For each galaxy, an inventory of H II regions detected using the COSMOS image classifier and centroider is provided. Salient features of each galaxy are described, including the distribution of the H II regions with reference to the galaxy morphology. Relevant abundance data from the literature are noted for each object. These images will find use as finding charts for follow-up spectrophotometric investigations of abundances, abundance gradients, and kinematics of H II regions in active galaxies, and for detailed studies of H II region populations in these objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93#table2</TD>
            <TD>2011-09-14T18:23:53Z</TD>
            <TD>#Seyfert_Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/93</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/105/93&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/93</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/543/A156 [1]</TD>
            <TD>Milky Way global survey of star clusters (Kharchenko+, 2012)</TD>
            <TD>An all-sky target list of 3784 entries with initial cluster parameters was compiled from sources available in the literature. As the primary source we used the data from the Catalogue of Open Cluster Data (COCD, Kharchenko et al. 2005a,b, Cat. J/A+A/438/1163, J/A+A/440/403). For further optical clusters the data were taken from the Dias et al. (2002, Cat. B/ocl) list (Version 3.1, 24/nov/2010). Known associations were retrieved from Melnik &amp; Dambis (2009, Cat. J/MNRAS/400/518). For clusters detected in the NIR the information came from Bica et al. (2003b, Cat. J/A+A/404/223), Dutra et al. (2003, Cat. J/A+A/400/533), Froebrich et al. (2007, Cat. J/MNRAS/374/399). Globular clusters were selected from the catalogue by Harris (1996) (edition 2010, 2010arXiv1012.3224H). Additionally, we incorporated supplementary data on embedded clusters from Bica et al. (2003a, Cat. J/A+A/397/177), Lada &amp; Lada (2003ARA&amp;A..41...57L) and on stars in associations from Humphreys (1978, Cat. V/44). The basic stellar data were taken from the all-sky catalogue 2MAst (2Mass with Astrometry), that was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010, Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). Additionally, we incorporated data on radial velocities from Kharchenko et al. (2007, Cat. III/254) and spectral types from ASCC-2.5 (Kharchenko &amp; Roeser 2009, Cat. I/280). Around each object from our target list we defined a circular area with a radius of ra=r2+radd where r2 is cluster radius, and radd=0.3{deg}. In these areas we selected in 2MAst only those stars with flags Rflg (the 2nd triple of the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars with the best quality detections in photometric and astrometric data. There are 871 targets in the 2nd Galaxy quadrant, we confirmed 650 open clusters and/or associations. These 650 sky areas contain about 11.2 mln 2MAst stars with best quality detections in photometric and astrometric data. We selected 30387 most probable members located in the central cluster regions and determined - with a homogeneous method/pipeline - angular sizes of the main morphological parts, heliocentric distances, colour-excesses, mean proper motions, sometimes radial velocities, ages, tidal parameters. There are 4 globular clusters in the 2nd quadrant, they are listed in index_q2.dat, but the data for globular clusters will be submitted to the CDS as a separate catalogue. We present for the 2nd quadrant of the Milky Way: The Catalogue of the MWSC Data with: Catalogue of parameters for confirmed clusters; Index (full list) of MWSC objects; Notes (full object list with notes); Inside each list the entries are ordered by MWSC number (i.e. right ascension J2000 from the target list). The Catalogues of the MWSC Stars in 650 circular sky areas with classified clusters. Files are ordered by MWSC number order; inside each sky area the entries are ordered by Ks magnitudes. The Atlas of MWSC diagrams. In the Atlas the Cluster pages are ordered by MWSC number.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156#1</TD>
            <TD>2012-07-27T09:53:20Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/543/A156</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A156</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/543/A156 [2]</TD>
            <TD>Milky Way global survey of star clusters (Kharchenko+, 2012)</TD>
            <TD>An all-sky target list of 3784 entries with initial cluster parameters was compiled from sources available in the literature. As the primary source we used the data from the Catalogue of Open Cluster Data (COCD, Kharchenko et al. 2005a,b, Cat. J/A+A/438/1163, J/A+A/440/403). For further optical clusters the data were taken from the Dias et al. (2002, Cat. B/ocl) list (Version 3.1, 24/nov/2010). Known associations were retrieved from Melnik &amp; Dambis (2009, Cat. J/MNRAS/400/518). For clusters detected in the NIR the information came from Bica et al. (2003b, Cat. J/A+A/404/223), Dutra et al. (2003, Cat. J/A+A/400/533), Froebrich et al. (2007, Cat. J/MNRAS/374/399). Globular clusters were selected from the catalogue by Harris (1996) (edition 2010, 2010arXiv1012.3224H). Additionally, we incorporated supplementary data on embedded clusters from Bica et al. (2003a, Cat. J/A+A/397/177), Lada &amp; Lada (2003ARA&amp;A..41...57L) and on stars in associations from Humphreys (1978, Cat. V/44). The basic stellar data were taken from the all-sky catalogue 2MAst (2Mass with Astrometry), that was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010, Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). Additionally, we incorporated data on radial velocities from Kharchenko et al. (2007, Cat. III/254) and spectral types from ASCC-2.5 (Kharchenko &amp; Roeser 2009, Cat. I/280). Around each object from our target list we defined a circular area with a radius of ra=r2+radd where r2 is cluster radius, and radd=0.3{deg}. In these areas we selected in 2MAst only those stars with flags Rflg (the 2nd triple of the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars with the best quality detections in photometric and astrometric data. There are 871 targets in the 2nd Galaxy quadrant, we confirmed 650 open clusters and/or associations. These 650 sky areas contain about 11.2 mln 2MAst stars with best quality detections in photometric and astrometric data. We selected 30387 most probable members located in the central cluster regions and determined - with a homogeneous method/pipeline - angular sizes of the main morphological parts, heliocentric distances, colour-excesses, mean proper motions, sometimes radial velocities, ages, tidal parameters. There are 4 globular clusters in the 2nd quadrant, they are listed in index_q2.dat, but the data for globular clusters will be submitted to the CDS as a separate catalogue. We present for the 2nd quadrant of the Milky Way: The Catalogue of the MWSC Data with: Catalogue of parameters for confirmed clusters; Index (full list) of MWSC objects; Notes (full object list with notes); Inside each list the entries are ordered by MWSC number (i.e. right ascension J2000 from the target list). The Catalogues of the MWSC Stars in 650 circular sky areas with classified clusters. Files are ordered by MWSC number order; inside each sky area the entries are ordered by Ks magnitudes. The Atlas of MWSC diagrams. In the Atlas the Cluster pages are ordered by MWSC number.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156#2</TD>
            <TD>2012-07-27T09:53:20Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/543/A156&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A156</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/543/A156 [catal_q2]</TD>
            <TD>Milky Way global survey of star clusters (Kharchenko+, 2012)</TD>
            <TD>An all-sky target list of 3784 entries with initial cluster parameters was compiled from sources available in the literature. As the primary source we used the data from the Catalogue of Open Cluster Data (COCD, Kharchenko et al. 2005a,b, Cat. J/A+A/438/1163, J/A+A/440/403). For further optical clusters the data were taken from the Dias et al. (2002, Cat. B/ocl) list (Version 3.1, 24/nov/2010). Known associations were retrieved from Melnik &amp; Dambis (2009, Cat. J/MNRAS/400/518). For clusters detected in the NIR the information came from Bica et al. (2003b, Cat. J/A+A/404/223), Dutra et al. (2003, Cat. J/A+A/400/533), Froebrich et al. (2007, Cat. J/MNRAS/374/399). Globular clusters were selected from the catalogue by Harris (1996) (edition 2010, 2010arXiv1012.3224H). Additionally, we incorporated supplementary data on embedded clusters from Bica et al. (2003a, Cat. J/A+A/397/177), Lada &amp; Lada (2003ARA&amp;A..41...57L) and on stars in associations from Humphreys (1978, Cat. V/44). The basic stellar data were taken from the all-sky catalogue 2MAst (2Mass with Astrometry), that was extracted from the all-sky catalogues PPMXL (Roeser et al. 2010, Cat. I/317) and 2MASS (Cutri et al. 2003, Cat. II/246). Additionally, we incorporated data on radial velocities from Kharchenko et al. (2007, Cat. III/254) and spectral types from ASCC-2.5 (Kharchenko &amp; Roeser 2009, Cat. I/280). Around each object from our target list we defined a circular area with a radius of ra=r2+radd where r2 is cluster radius, and radd=0.3{deg}. In these areas we selected in 2MAst only those stars with flags Rflg (the 2nd triple of the flags in 2MASS) set to 1, 2, or 3 in each band, i.e. the stars with the best quality detections in photometric and astrometric data. There are 871 targets in the 2nd Galaxy quadrant, we confirmed 650 open clusters and/or associations. These 650 sky areas contain about 11.2 mln 2MAst stars with best quality detections in photometric and astrometric data. We selected 30387 most probable members located in the central cluster regions and determined - with a homogeneous method/pipeline - angular sizes of the main morphological parts, heliocentric distances, colour-excesses, mean proper motions, sometimes radial velocities, ages, tidal parameters. There are 4 globular clusters in the 2nd quadrant, they are listed in index_q2.dat, but the data for globular clusters will be submitted to the CDS as a separate catalogue. We present for the 2nd quadrant of the Milky Way: The Catalogue of the MWSC Data with: Catalogue of parameters for confirmed clusters; Index (full list) of MWSC objects; Notes (full object list with notes); Inside each list the entries are ordered by MWSC number (i.e. right ascension J2000 from the target list). The Catalogues of the MWSC Stars in 650 circular sky areas with classified clusters. Files are ordered by MWSC number order; inside each sky area the entries are ordered by Ks magnitudes. The Atlas of MWSC diagrams. In the Atlas the Cluster pages are ordered by MWSC number.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156#catal_q2</TD>
            <TD>2012-07-27T09:53:20Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A156</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/543/A156&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A156</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/281 [1]</TD>
            <TD>Atlas of hot, luminous stars at 2 microns (Hanson+ 1996)</TD>
            <TD>We present 2um (K band) spectra of 180 well-studied, optically visible, luminous stars. Most of the stars are of OB spectral type, but we have also included a number of Oe and Be stars, OBN and OBC stars, cool hypergiant stars, and high-mass X-ray binary stars. Our aim in studying normal OB stars is to develop an empirical relationship between 2um spectral features of these massive stars and their stellar temperature and luminosity. We find the system of lines between 2.0 and 2.2um is particulary good for differentiating the early- and mid-O type stars. In the late-O and early-B stars, differentiation becomes more difficult, as the features show only moderate changes. We have developed a spectral classification system for the K band to be used to estimate effective temperatures of O and early-B stars. We demonstrate that K-band spectroscopy is superior in estimating the temperature of hot, luminous stars than the traditional methods of using infrared or even optical photometric colors alone. The only requirements are that adequate resolution (R&gt;1000) and signal-to-noise (S/N~70) be achieved. With our classification system, stars behind large amounts of visible extinction, such as young, heavily reddened H II regions throughout our Galaxy, may be identified and studied for the first time through 2um spectroscopy. Emission lines are commonly seen in the K-band spectra of supergiant stars, however, the OBN supergiants, which have a higher ratio of some processed materials at their surface, may be more likely to show line emission, especially the He I singlet transition at 2.058um. This has led us to propose an evolutionary scenario for some of the Galactic center He I emission-line stars, which evokes rotational mixing (Maeder 1987A&amp;A...178..159M; Langer 1992A&amp;A...265L..17L) to explain both the strong line emission and high luminosity of these mysterious sources. We have compared our spectroscopic database with the most recent stellar atmosphere models. We are encouraged by the good match between the model line profiles at 2um of Schaerer et al. (1996A&amp;A...312..475S) and those observed in OB stars. Finally, we include a thorough discussion of the observational and reduction methods employed to obtain the spectra shown in this atlas for the benefit of those wishing to obtain similar, classification-quality, near-infrared spectra.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/281#1</TD>
            <TD>2011-09-14T18:23:54Z</TD>
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            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/281</TD>
            <TD />
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/281</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/281</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/281 [2]</TD>
            <TD>Atlas of hot, luminous stars at 2 microns (Hanson+ 1996)</TD>
            <TD>We present 2um (K band) spectra of 180 well-studied, optically visible, luminous stars. Most of the stars are of OB spectral type, but we have also included a number of Oe and Be stars, OBN and OBC stars, cool hypergiant stars, and high-mass X-ray binary stars. Our aim in studying normal OB stars is to develop an empirical relationship between 2um spectral features of these massive stars and their stellar temperature and luminosity. We find the system of lines between 2.0 and 2.2um is particulary good for differentiating the early- and mid-O type stars. In the late-O and early-B stars, differentiation becomes more difficult, as the features show only moderate changes. We have developed a spectral classification system for the K band to be used to estimate effective temperatures of O and early-B stars. We demonstrate that K-band spectroscopy is superior in estimating the temperature of hot, luminous stars than the traditional methods of using infrared or even optical photometric colors alone. The only requirements are that adequate resolution (R&gt;1000) and signal-to-noise (S/N~70) be achieved. With our classification system, stars behind large amounts of visible extinction, such as young, heavily reddened H II regions throughout our Galaxy, may be identified and studied for the first time through 2um spectroscopy. Emission lines are commonly seen in the K-band spectra of supergiant stars, however, the OBN supergiants, which have a higher ratio of some processed materials at their surface, may be more likely to show line emission, especially the He I singlet transition at 2.058um. This has led us to propose an evolutionary scenario for some of the Galactic center He I emission-line stars, which evokes rotational mixing (Maeder 1987A&amp;A...178..159M; Langer 1992A&amp;A...265L..17L) to explain both the strong line emission and high luminosity of these mysterious sources. We have compared our spectroscopic database with the most recent stellar atmosphere models. We are encouraged by the good match between the model line profiles at 2um of Schaerer et al. (1996A&amp;A...312..475S) and those observed in OB stars. Finally, we include a thorough discussion of the observational and reduction methods employed to obtain the spectra shown in this atlas for the benefit of those wishing to obtain similar, classification-quality, near-infrared spectra.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/281#2</TD>
            <TD>2011-09-14T18:23:54Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
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            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/281</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/281&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/281</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/542/A66 [1]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#1</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/542/A66</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/542/A66 [2]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#2</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
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          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/542/A66 [YSOs]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#YSOs</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/542/A66 [table3]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#table3</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/542/A66 [table2]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#table2</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/542/A66&amp;</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/281 [1]</TD>
            <TD>Atlas of hot, luminous stars at 2 microns (Hanson+ 1996)</TD>
            <TD>We present 2um (K band) spectra of 180 well-studied, optically visible, luminous stars. Most of the stars are of OB spectral type, but we have also included a number of Oe and Be stars, OBN and OBC stars, cool hypergiant stars, and high-mass X-ray binary stars. Our aim in studying normal OB stars is to develop an empirical relationship between 2um spectral features of these massive stars and their stellar temperature and luminosity. We find the system of lines between 2.0 and 2.2um is particulary good for differentiating the early- and mid-O type stars. In the late-O and early-B stars, differentiation becomes more difficult, as the features show only moderate changes. We have developed a spectral classification system for the K band to be used to estimate effective temperatures of O and early-B stars. We demonstrate that K-band spectroscopy is superior in estimating the temperature of hot, luminous stars than the traditional methods of using infrared or even optical photometric colors alone. The only requirements are that adequate resolution (R&gt;1000) and signal-to-noise (S/N~70) be achieved. With our classification system, stars behind large amounts of visible extinction, such as young, heavily reddened H II regions throughout our Galaxy, may be identified and studied for the first time through 2um spectroscopy. Emission lines are commonly seen in the K-band spectra of supergiant stars, however, the OBN supergiants, which have a higher ratio of some processed materials at their surface, may be more likely to show line emission, especially the He I singlet transition at 2.058um. This has led us to propose an evolutionary scenario for some of the Galactic center He I emission-line stars, which evokes rotational mixing (Maeder 1987A&amp;A...178..159M; Langer 1992A&amp;A...265L..17L) to explain both the strong line emission and high luminosity of these mysterious sources. We have compared our spectroscopic database with the most recent stellar atmosphere models. We are encouraged by the good match between the model line profiles at 2um of Schaerer et al. (1996A&amp;A...312..475S) and those observed in OB stars. Finally, we include a thorough discussion of the observational and reduction methods employed to obtain the spectra shown in this atlas for the benefit of those wishing to obtain similar, classification-quality, near-infrared spectra.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/281#1</TD>
            <TD>2011-09-14T18:23:54Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/281</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/281</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/281</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/281 [2]</TD>
            <TD>Atlas of hot, luminous stars at 2 microns (Hanson+ 1996)</TD>
            <TD>We present 2um (K band) spectra of 180 well-studied, optically visible, luminous stars. Most of the stars are of OB spectral type, but we have also included a number of Oe and Be stars, OBN and OBC stars, cool hypergiant stars, and high-mass X-ray binary stars. Our aim in studying normal OB stars is to develop an empirical relationship between 2um spectral features of these massive stars and their stellar temperature and luminosity. We find the system of lines between 2.0 and 2.2um is particulary good for differentiating the early- and mid-O type stars. In the late-O and early-B stars, differentiation becomes more difficult, as the features show only moderate changes. We have developed a spectral classification system for the K band to be used to estimate effective temperatures of O and early-B stars. We demonstrate that K-band spectroscopy is superior in estimating the temperature of hot, luminous stars than the traditional methods of using infrared or even optical photometric colors alone. The only requirements are that adequate resolution (R&gt;1000) and signal-to-noise (S/N~70) be achieved. With our classification system, stars behind large amounts of visible extinction, such as young, heavily reddened H II regions throughout our Galaxy, may be identified and studied for the first time through 2um spectroscopy. Emission lines are commonly seen in the K-band spectra of supergiant stars, however, the OBN supergiants, which have a higher ratio of some processed materials at their surface, may be more likely to show line emission, especially the He I singlet transition at 2.058um. This has led us to propose an evolutionary scenario for some of the Galactic center He I emission-line stars, which evokes rotational mixing (Maeder 1987A&amp;A...178..159M; Langer 1992A&amp;A...265L..17L) to explain both the strong line emission and high luminosity of these mysterious sources. We have compared our spectroscopic database with the most recent stellar atmosphere models. We are encouraged by the good match between the model line profiles at 2um of Schaerer et al. (1996A&amp;A...312..475S) and those observed in OB stars. Finally, we include a thorough discussion of the observational and reduction methods employed to obtain the spectra shown in this atlas for the benefit of those wishing to obtain similar, classification-quality, near-infrared spectra.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/281#2</TD>
            <TD>2011-09-14T18:23:54Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/281</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/281&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/281</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/542/A66 [1]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#1</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/542/A66</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/542/A66 [2]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#2</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/542/A66 [YSOs]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#YSOs</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/542/A66 [table3]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#table3</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/542/A66 [table2]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#table2</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/273/157 [1]</TD>
            <TD>A faint galaxy survey to B = 24. (Glazebrook+ 1995)</TD>
            <TD>Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5&lt;B&lt;24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z&gt;1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157#1</TD>
            <TD>2011-09-14T18:38:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/273/157</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/273/157</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/273/157 [2]</TD>
            <TD>A faint galaxy survey to B = 24. (Glazebrook+ 1995)</TD>
            <TD>Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5&lt;B&lt;24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z&gt;1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157#2</TD>
            <TD>2011-09-14T18:38:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/273/157&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/273/157</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/273/157 [catalog]</TD>
            <TD>A faint galaxy survey to B = 24. (Glazebrook+ 1995)</TD>
            <TD>Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5&lt;B&lt;24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z&gt;1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157#catalog</TD>
            <TD>2011-09-14T18:38:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/273/157&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/273/157</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/542/A66 [1]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#1</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/542/A66</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/542/A66 [2]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#2</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/542/A66 [YSOs]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#YSOs</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/542/A66 [table3]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#table3</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/542/A66 [table2]</TD>
            <TD>YSOs in 9 LMC star forming regions (Carlson+, 2012)</TD>
            <TD>We introduce a new set of selection criteria for the identification of infrared bright young stellar object (YSO) candidates and apply them to nine HII regions in the Large Magellanic Cloud (LMC), focusing particularly on lower mass candidates missed by most surveys. Data are from the Spitzer Space Telescope legacy program SAGE (Surveying the Agents of Galaxy Evolution; Meixner et al. 2006, Cat. J/AJ/132/2268, see also II/305), combined with optical photometry from the Magellanic Clouds Photometric Survey (MCPS; Zaritsky et al. 1997AJ....114.1002Z) and near-infrared photometry from the InfraRed Survey Facility (IRSF; Kato et al. 2007, Cat. II/288). We choose regions of diverse physical size, star formation rates (SFRs), and ages. We also cover a wide range of locations and surrounding environments in the LMC. These active star-forming regions are LHA 120-N 11, N 44, N 51, N 105, N 113, N 120, N 144, N 160, and N 206. Some have been well-studied (e.g., N11, N44, N160) in the past, while others (e.g., N51, N144) have received little attention. We identify 1045 YSO candidates, including 918 never before identified and 127 matching previous candidate lists. We characterize the evolutionary stage and physical properties of each candidate using the spectral energy distribution (SED) fitter of Robitaille et al. (2007ApJS..169..328R) and estimate mass functions and SFRs for each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66#table2</TD>
            <TD>2012-08-15T07:57:00Z</TD>
            <TD>#Stars#Photometry:wide-band#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/542/A66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/542/A66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/542/A66</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/273/157 [1]</TD>
            <TD>A faint galaxy survey to B = 24. (Glazebrook+ 1995)</TD>
            <TD>Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5&lt;B&lt;24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z&gt;1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157#1</TD>
            <TD>2011-09-14T18:38:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/273/157</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/273/157</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/273/157 [2]</TD>
            <TD>A faint galaxy survey to B = 24. (Glazebrook+ 1995)</TD>
            <TD>Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5&lt;B&lt;24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z&gt;1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157#2</TD>
            <TD>2011-09-14T18:38:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/273/157&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/273/157</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/273/157 [catalog]</TD>
            <TD>A faint galaxy survey to B = 24. (Glazebrook+ 1995)</TD>
            <TD>Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5&lt;B&lt;24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z&gt;1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157#catalog</TD>
            <TD>2011-09-14T18:38:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/273/157&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/273/157</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/411/2009 [1]</TD>
            <TD>H narrow-band imaging of XMMU J2235.3-2557 (Bauer+, 2011)</TD>
            <TD>We obtained observations of the XMMU J2235.3-2557 galaxy cluster with the Near InfraRed Imager and Spectrometer (NIRI) on Gemini North. The data presented in this paper originate from the Gemini programme GN-2007B-Q-79, observed in queue mode in the period from UT 2007 July 11 to UT 2007 September 30.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009#1</TD>
            <TD>2012-08-22T09:06:37Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/411/2009</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2009</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/411/2009 [2]</TD>
            <TD>H narrow-band imaging of XMMU J2235.3-2557 (Bauer+, 2011)</TD>
            <TD>We obtained observations of the XMMU J2235.3-2557 galaxy cluster with the Near InfraRed Imager and Spectrometer (NIRI) on Gemini North. The data presented in this paper originate from the Gemini programme GN-2007B-Q-79, observed in queue mode in the period from UT 2007 July 11 to UT 2007 September 30.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009#2</TD>
            <TD>2012-08-22T09:06:37Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/411/2009&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2009</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/2009 [table1]</TD>
            <TD>H narrow-band imaging of XMMU J2235.3-2557 (Bauer+, 2011)</TD>
            <TD>We obtained observations of the XMMU J2235.3-2557 galaxy cluster with the Near InfraRed Imager and Spectrometer (NIRI) on Gemini North. The data presented in this paper originate from the Gemini programme GN-2007B-Q-79, observed in queue mode in the period from UT 2007 July 11 to UT 2007 September 30.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009#table1</TD>
            <TD>2012-08-22T09:06:37Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/2009&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2009</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/273/157 [1]</TD>
            <TD>A faint galaxy survey to B = 24. (Glazebrook+ 1995)</TD>
            <TD>Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5&lt;B&lt;24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z&gt;1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157#1</TD>
            <TD>2011-09-14T18:38:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/273/157</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/273/157</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/273/157 [2]</TD>
            <TD>A faint galaxy survey to B = 24. (Glazebrook+ 1995)</TD>
            <TD>Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5&lt;B&lt;24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z&gt;1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157#2</TD>
            <TD>2011-09-14T18:38:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/273/157&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/273/157</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/273/157 [catalog]</TD>
            <TD>A faint galaxy survey to B = 24. (Glazebrook+ 1995)</TD>
            <TD>Using the multi-slit LDSS-2 spectrograph on the William Herschel Telescope we have completed a redshift survey in the magnitude range 22.5&lt;B&lt;24 which produced 73 redshifts representing a 73% complete sample uniformly selected from four deep fields at high galactic latitude. The survey extends to z&gt;1 and includes the highest redshift galaxy (z=1.108) yet discovered in a field sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157#catalog</TD>
            <TD>2011-09-14T18:38:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/273/157</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/273/157&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/273/157</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/411/2009 [1]</TD>
            <TD>H narrow-band imaging of XMMU J2235.3-2557 (Bauer+, 2011)</TD>
            <TD>We obtained observations of the XMMU J2235.3-2557 galaxy cluster with the Near InfraRed Imager and Spectrometer (NIRI) on Gemini North. The data presented in this paper originate from the Gemini programme GN-2007B-Q-79, observed in queue mode in the period from UT 2007 July 11 to UT 2007 September 30.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009#1</TD>
            <TD>2012-08-22T09:06:37Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/411/2009</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2009</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/411/2009 [2]</TD>
            <TD>H narrow-band imaging of XMMU J2235.3-2557 (Bauer+, 2011)</TD>
            <TD>We obtained observations of the XMMU J2235.3-2557 galaxy cluster with the Near InfraRed Imager and Spectrometer (NIRI) on Gemini North. The data presented in this paper originate from the Gemini programme GN-2007B-Q-79, observed in queue mode in the period from UT 2007 July 11 to UT 2007 September 30.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009#2</TD>
            <TD>2012-08-22T09:06:37Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/411/2009&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2009</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/2009 [table1]</TD>
            <TD>H narrow-band imaging of XMMU J2235.3-2557 (Bauer+, 2011)</TD>
            <TD>We obtained observations of the XMMU J2235.3-2557 galaxy cluster with the Near InfraRed Imager and Spectrometer (NIRI) on Gemini North. The data presented in this paper originate from the Gemini programme GN-2007B-Q-79, observed in queue mode in the period from UT 2007 July 11 to UT 2007 September 30.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009#table1</TD>
            <TD>2012-08-22T09:06:37Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/2009&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2009</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/275/591 [1]</TD>
            <TD>Outer regions of Galactic Bulge (Ibata+, 1995)</TD>
            <TD>Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591#1</TD>
            <TD>2011-09-14T18:38:03Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/275/591</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/275/591</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/275/591 [2]</TD>
            <TD>Outer regions of Galactic Bulge (Ibata+, 1995)</TD>
            <TD>Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591#2</TD>
            <TD>2011-09-14T18:38:03Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/275/591&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/275/591</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/275/591 [main]</TD>
            <TD>Outer regions of Galactic Bulge (Ibata+, 1995)</TD>
            <TD>Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591#main</TD>
            <TD>2011-09-14T18:38:03Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/275/591&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/275/591</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/411/2009 [1]</TD>
            <TD>H narrow-band imaging of XMMU J2235.3-2557 (Bauer+, 2011)</TD>
            <TD>We obtained observations of the XMMU J2235.3-2557 galaxy cluster with the Near InfraRed Imager and Spectrometer (NIRI) on Gemini North. The data presented in this paper originate from the Gemini programme GN-2007B-Q-79, observed in queue mode in the period from UT 2007 July 11 to UT 2007 September 30.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009#1</TD>
            <TD>2012-08-22T09:06:37Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/411/2009</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2009</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/411/2009 [2]</TD>
            <TD>H narrow-band imaging of XMMU J2235.3-2557 (Bauer+, 2011)</TD>
            <TD>We obtained observations of the XMMU J2235.3-2557 galaxy cluster with the Near InfraRed Imager and Spectrometer (NIRI) on Gemini North. The data presented in this paper originate from the Gemini programme GN-2007B-Q-79, observed in queue mode in the period from UT 2007 July 11 to UT 2007 September 30.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009#2</TD>
            <TD>2012-08-22T09:06:37Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/411/2009&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2009</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/2009 [table1]</TD>
            <TD>H narrow-band imaging of XMMU J2235.3-2557 (Bauer+, 2011)</TD>
            <TD>We obtained observations of the XMMU J2235.3-2557 galaxy cluster with the Near InfraRed Imager and Spectrometer (NIRI) on Gemini North. The data presented in this paper originate from the Gemini programme GN-2007B-Q-79, observed in queue mode in the period from UT 2007 July 11 to UT 2007 September 30.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009#table1</TD>
            <TD>2012-08-22T09:06:37Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2009</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/2009&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2009</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/275/591 [1]</TD>
            <TD>Outer regions of Galactic Bulge (Ibata+, 1995)</TD>
            <TD>Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591#1</TD>
            <TD>2011-09-14T18:38:03Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/275/591</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/275/591</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/275/591 [2]</TD>
            <TD>Outer regions of Galactic Bulge (Ibata+, 1995)</TD>
            <TD>Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591#2</TD>
            <TD>2011-09-14T18:38:03Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/275/591&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/275/591</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/275/591 [main]</TD>
            <TD>Outer regions of Galactic Bulge (Ibata+, 1995)</TD>
            <TD>Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591#main</TD>
            <TD>2011-09-14T18:38:03Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/275/591&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/275/591</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/275/591 [1]</TD>
            <TD>Outer regions of Galactic Bulge (Ibata+, 1995)</TD>
            <TD>Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591#1</TD>
            <TD>2011-09-14T18:38:03Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/275/591</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/275/591</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/275/591 [2]</TD>
            <TD>Outer regions of Galactic Bulge (Ibata+, 1995)</TD>
            <TD>Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591#2</TD>
            <TD>2011-09-14T18:38:03Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/275/591&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/275/591</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/275/591 [main]</TD>
            <TD>Outer regions of Galactic Bulge (Ibata+, 1995)</TD>
            <TD>Digitized UK Schmidt plate photometry, calibrated with CCD photometry, is obtained in 18 regions over the Bulge. Stars are selected for spectroscopic follow-up from with a carefully chosen colour-magnitude window, optimized for efficient detection of bulge K giants. Some 1500 stellar spectra are obtained with the AAT AUTOFIB facility. We derive a radial velocity and metallicity for each star, and quantify the uncertainties in these measurements. Luminosity classification is derived both by visual classification and by using an automated routine based on Principal Component Analysis. There are two basic results from this survey: the discovery of the Sagittarius dwarf galaxy described by Ibata, Gilmore and Irwin (1994Natur.370..194I), and a study of the Galactic Bulge by Ibata and Gilmore (1995MNRAS.275..605I) The catalogue contains coordinates, photometry, radial velocities, luminosity classification and chemical abundances for approximately 1500 stars in lines of sight towards the Galactic Bulge. A detailed description of the selection of these stars, the methods used to derive the data, and the reliability of the data, is presented in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591#main</TD>
            <TD>2011-09-14T18:38:03Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/275/591</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/275/591&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/275/591</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/535/A4 [1]</TD>
            <TD>X-ray galaxy clusters study (Reichert+, 2011)</TD>
            <TD>A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution from the combined data sets. We study in particular the most important scaling relations connecting X-ray luminosity, temperature, and cluster mass (M-T, L_X_-T, and M-L_X_) combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP) that adds new leverage to efficiently constrain the scaling relations at high redshift.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4#1</TD>
            <TD>2012-08-22T09:09:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/535/A4</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A4</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/535/A4 [2]</TD>
            <TD>X-ray galaxy clusters study (Reichert+, 2011)</TD>
            <TD>A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution from the combined data sets. We study in particular the most important scaling relations connecting X-ray luminosity, temperature, and cluster mass (M-T, L_X_-T, and M-L_X_) combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP) that adds new leverage to efficiently constrain the scaling relations at high redshift.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4#2</TD>
            <TD>2012-08-22T09:09:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/535/A4&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A4</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/535/A4 [tablea1]</TD>
            <TD>X-ray galaxy clusters study (Reichert+, 2011)</TD>
            <TD>A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution from the combined data sets. We study in particular the most important scaling relations connecting X-ray luminosity, temperature, and cluster mass (M-T, L_X_-T, and M-L_X_) combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP) that adds new leverage to efficiently constrain the scaling relations at high redshift.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4#tablea1</TD>
            <TD>2012-08-22T09:09:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/535/A4&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A4</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/535/A4 [1]</TD>
            <TD>X-ray galaxy clusters study (Reichert+, 2011)</TD>
            <TD>A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution from the combined data sets. We study in particular the most important scaling relations connecting X-ray luminosity, temperature, and cluster mass (M-T, L_X_-T, and M-L_X_) combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP) that adds new leverage to efficiently constrain the scaling relations at high redshift.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4#1</TD>
            <TD>2012-08-22T09:09:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/535/A4</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A4</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/535/A4 [2]</TD>
            <TD>X-ray galaxy clusters study (Reichert+, 2011)</TD>
            <TD>A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution from the combined data sets. We study in particular the most important scaling relations connecting X-ray luminosity, temperature, and cluster mass (M-T, L_X_-T, and M-L_X_) combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP) that adds new leverage to efficiently constrain the scaling relations at high redshift.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4#2</TD>
            <TD>2012-08-22T09:09:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/535/A4&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A4</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/535/A4 [tablea1]</TD>
            <TD>X-ray galaxy clusters study (Reichert+, 2011)</TD>
            <TD>A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution from the combined data sets. We study in particular the most important scaling relations connecting X-ray luminosity, temperature, and cluster mass (M-T, L_X_-T, and M-L_X_) combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP) that adds new leverage to efficiently constrain the scaling relations at high redshift.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4#tablea1</TD>
            <TD>2012-08-22T09:09:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/535/A4&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A4</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/13 [1]</TD>
            <TD>Globular-Cluster Catalog (Arp 1965)</TD>
            <TD>This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/13#1</TD>
            <TD>2011-09-14T18:38:54Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/VII/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/13</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/13</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/13 [2]</TD>
            <TD>Globular-Cluster Catalog (Arp 1965)</TD>
            <TD>This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/13#2</TD>
            <TD>2011-09-14T18:38:54Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/VII/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/13&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/13 [catalog]</TD>
            <TD>Globular-Cluster Catalog (Arp 1965)</TD>
            <TD>This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/13#catalog</TD>
            <TD>2011-09-14T18:38:54Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/VII/13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/13</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/535/A4 [1]</TD>
            <TD>X-ray galaxy clusters study (Reichert+, 2011)</TD>
            <TD>A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution from the combined data sets. We study in particular the most important scaling relations connecting X-ray luminosity, temperature, and cluster mass (M-T, L_X_-T, and M-L_X_) combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP) that adds new leverage to efficiently constrain the scaling relations at high redshift.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4#1</TD>
            <TD>2012-08-22T09:09:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/535/A4</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A4</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/535/A4 [2]</TD>
            <TD>X-ray galaxy clusters study (Reichert+, 2011)</TD>
            <TD>A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution from the combined data sets. We study in particular the most important scaling relations connecting X-ray luminosity, temperature, and cluster mass (M-T, L_X_-T, and M-L_X_) combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP) that adds new leverage to efficiently constrain the scaling relations at high redshift.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4#2</TD>
            <TD>2012-08-22T09:09:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/535/A4&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A4</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/535/A4 [tablea1]</TD>
            <TD>X-ray galaxy clusters study (Reichert+, 2011)</TD>
            <TD>A precise understanding of the relations between observable X-ray properties of galaxy clusters and cluster mass is a vital part of the application of X-ray galaxy cluster surveys to test cosmological models. An understanding of how these relations evolve with redshift is just emerging from a number of observational data sets. The current literature provides a diverse and inhomogeneous picture of scaling relation evolution. We attempt to transform these results and the data on recently discovered distant clusters into an updated and consistent framework, and provide an overall view of scaling relation evolution from the combined data sets. We study in particular the most important scaling relations connecting X-ray luminosity, temperature, and cluster mass (M-T, L_X_-T, and M-L_X_) combining 14 published data sets supplemented with recently published data of distant clusters and new results from follow-up observations of the XMM-Newton Distant Cluster Project (XDCP) that adds new leverage to efficiently constrain the scaling relations at high redshift.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4#tablea1</TD>
            <TD>2012-08-22T09:09:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A4</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/535/A4&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A4</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/13 [1]</TD>
            <TD>Globular-Cluster Catalog (Arp 1965)</TD>
            <TD>This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/13#1</TD>
            <TD>2011-09-14T18:38:54Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/VII/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/13</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/13</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/13 [2]</TD>
            <TD>Globular-Cluster Catalog (Arp 1965)</TD>
            <TD>This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/13#2</TD>
            <TD>2011-09-14T18:38:54Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/VII/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/13&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/13 [catalog]</TD>
            <TD>Globular-Cluster Catalog (Arp 1965)</TD>
            <TD>This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/13#catalog</TD>
            <TD>2011-09-14T18:38:54Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/VII/13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/533 [1]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#1</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/533 [2]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#2</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/533 [table6]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#table6</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/533 [AGNcand]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#AGNcand</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/13 [1]</TD>
            <TD>Globular-Cluster Catalog (Arp 1965)</TD>
            <TD>This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/13#1</TD>
            <TD>2011-09-14T18:38:54Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/VII/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/13</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/13</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/13 [2]</TD>
            <TD>Globular-Cluster Catalog (Arp 1965)</TD>
            <TD>This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/13#2</TD>
            <TD>2011-09-14T18:38:54Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/VII/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/13&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/13 [catalog]</TD>
            <TD>Globular-Cluster Catalog (Arp 1965)</TD>
            <TD>This catalog is the Globular Cluster Catalog published by Halton C. Arp in 1965 as part of a review paper on globular Clusters. The review focused on the slightly more than a hundred roughly spherical star clusters that have integrated color indices between B-V = 0.6 an 0.8 mag and intrinsic magnitudes between Mbol = -4 and -10 mag. They are distributed about the center of the galaxy. Such clusters contain stars that are very old and metal poor. The catalog improves upon the earlier publication by Mrs. Hogg (1959). An estimate of the completeness of the catalog is 98 percent complete for galactic latitudes above b(II)=8 degrees and 94 percent complete for low latitudes for concentration classes less than XI. This catalog lists for all 119 clusters: the NGC number, or other ID, the name, the position in equatorial and galactic coordinates, the concentration class, galactic absorption, diameter at 0.9, magnitude of 25-st brightest star, distance modulus, galactic radius, x, y, and z positions, total brightness, apparent and intrinsic colors, spectral type and radial velocity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/13#catalog</TD>
            <TD>2011-09-14T18:38:54Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/VII/13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/13</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/533 [1]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#1</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/533 [2]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#2</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/533 [table6]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#table6</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/533 [AGNcand]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#AGNcand</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/190 [1]</TD>
            <TD>Zwicky Galaxy Catalog (Zwicky+ 1968)</TD>
            <TD>This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley &amp; Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zwi_gal.ori and zwi_gal.add. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/190#1</TD>
            <TD>2011-09-14T18:39:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Mar-06</TD>
            <TD>ivo://CDS.VizieR/VII/190</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/190</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/190</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/190 [2]</TD>
            <TD>Zwicky Galaxy Catalog (Zwicky+ 1968)</TD>
            <TD>This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley &amp; Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zwi_gal.ori and zwi_gal.add. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/190#2</TD>
            <TD>2011-09-14T18:39:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Mar-06</TD>
            <TD>ivo://CDS.VizieR/VII/190</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/190&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/190</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/190 [zg_ori]</TD>
            <TD>Zwicky Galaxy Catalog (Zwicky+ 1968)</TD>
            <TD>This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley &amp; Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zwi_gal.ori and zwi_gal.add. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/190#zg_ori</TD>
            <TD>2011-09-14T18:39:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Mar-06</TD>
            <TD>ivo://CDS.VizieR/VII/190</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/190&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/190</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/533 [1]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#1</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/533 [2]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#2</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/533 [table6]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#table6</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/533 [AGNcand]</TD>
            <TD>Morphologies of selected AGN (Griffith+, 2010)</TD>
            <TD>The cornerstone data set for the COSMOS survey is its wide-field HST Advanced Camera for Surveys (ACS) imaging (Scoville et al. 2007ApJS..172...38S). With 583 single-orbit HST ACS F814W (I band; hereafter I814) observations, it is the largest contiguous HST imaging survey to date. The VLA-COSMOS large project (Schinnerer et al., 2007, Cat. J/ApJS/172/46) acquired deep, uniform 1.4GHz data over the entire COSMOS field using the A-array configuration of the Very Large Array (VLA). The XMM-Newton COSMOS survey (Hasinger et al., 2007, Cat. J/ApJS/172/29; Cappelluti et al., 2009, Cat. J/A+A/497/635) acquired deep X-ray data over the entire COSMOS HST ACS field. The S-COSMOS survey (Sanders et al., 2007ApJS..172...86S) is a Spitzer Legacy program which carried out a uniformly deep survey of the full COSMOS field in seven mid-IR bands (3.6, 4.5, 5.8, 8.0, 24, 70, and 160um). The Advanced Camera for Surveys General Catalog2 (ACS-GC) data (R.L. Griffith et al., 2012ApJS..200....9G) was constructed to study the evolution of galaxy morphologies over a wide range of look-back times. The ACS-GC uniformly analyzes the largest HST ACS imaging surveys (AEGIS, GEMS, GOODS-S, GOODS-N, and COSMOS) using the GALAPAGOS code.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533#AGNcand</TD>
            <TD>2012-08-22T12:10:41Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/190 [1]</TD>
            <TD>Zwicky Galaxy Catalog (Zwicky+ 1968)</TD>
            <TD>This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley &amp; Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zwi_gal.ori and zwi_gal.add. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/190#1</TD>
            <TD>2011-09-14T18:39:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Mar-06</TD>
            <TD>ivo://CDS.VizieR/VII/190</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/190</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/190</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/190 [2]</TD>
            <TD>Zwicky Galaxy Catalog (Zwicky+ 1968)</TD>
            <TD>This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley &amp; Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zwi_gal.ori and zwi_gal.add. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/190#2</TD>
            <TD>2011-09-14T18:39:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Mar-06</TD>
            <TD>ivo://CDS.VizieR/VII/190</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/190&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/190</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/190 [zg_ori]</TD>
            <TD>Zwicky Galaxy Catalog (Zwicky+ 1968)</TD>
            <TD>This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley &amp; Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zwi_gal.ori and zwi_gal.add. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/190#zg_ori</TD>
            <TD>2011-09-14T18:39:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Mar-06</TD>
            <TD>ivo://CDS.VizieR/VII/190</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/190&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/190</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/1043 [1]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#1</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/1043</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/1043 [2]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#2</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/1043&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1043 [table2]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#table2</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1043&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1043 [table1]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#table1</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1043&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/190 [1]</TD>
            <TD>Zwicky Galaxy Catalog (Zwicky+ 1968)</TD>
            <TD>This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley &amp; Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zwi_gal.ori and zwi_gal.add. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/190#1</TD>
            <TD>2011-09-14T18:39:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Mar-06</TD>
            <TD>ivo://CDS.VizieR/VII/190</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/190</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/190</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/190 [2]</TD>
            <TD>Zwicky Galaxy Catalog (Zwicky+ 1968)</TD>
            <TD>This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley &amp; Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zwi_gal.ori and zwi_gal.add. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/190#2</TD>
            <TD>2011-09-14T18:39:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Mar-06</TD>
            <TD>ivo://CDS.VizieR/VII/190</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/190&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/190</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/190 [zg_ori]</TD>
            <TD>Zwicky Galaxy Catalog (Zwicky+ 1968)</TD>
            <TD>This document describes a computer version of that part of the CGCG (Zwicky et al. 1961-68) containing all the alphanumeric information for galaxies. All known errors found by Zwicky and many others are corrected as well as erroneous quotations from other catalogs (Shapley &amp; Ames 1932, Bigay 1951, Pettit 1954, Humason et al. 1956, Holmberg 1958). It is an illusion to consider all the errors are found. There are some misprints even in the most extended list of misprints (Paturel et al. 1991). We have compiled two files: zwi_gal.ori and zwi_gal.add. The first one contains the original information from CGCG for galaxies. The second one contains the data from above mentioned other catalogs given in CGCG. We have made no attempts to supply the catalog with any new information. A detailed comparison with the machine-readable version of Zwicky galaxies prepared by R.S. Hill (NSSDC ADC #7049 or CDS VII/49) was performed. Our version contains more data on individual galaxies - designation, description, magnitudes, velocity. All galaxies in the Coma center are included. However Hill's version contains data for Zwicky fields, Palomar Sky Survey plate number as well as Mead-Luyten-Palomar number. There are 27837 different galaxies and 29418 entries in CGCG.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/190#zg_ori</TD>
            <TD>2011-09-14T18:39:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1996-Mar-06</TD>
            <TD>ivo://CDS.VizieR/VII/190</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/190&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/190</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/1043 [1]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#1</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/1043</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/1043 [2]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#2</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/1043&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1043 [table2]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#table2</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1043&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1043 [table1]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#table1</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1043&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/193 [1]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#1</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/193 [2]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#2</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/193 [zbig]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#zbig</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/193 [zcat]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#zcat</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/179 [1]</TD>
            <TD>AGNs in the Extended Groth Strip Survey (Ramos Almeida+, 2009)</TD>
            <TD>We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179#1</TD>
            <TD>2011-10-19T15:56:43Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/179</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/179</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/179 [2]</TD>
            <TD>AGNs in the Extended Groth Strip Survey (Ramos Almeida+, 2009)</TD>
            <TD>We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179#2</TD>
            <TD>2011-10-19T15:56:43Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/179&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/179</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/179 [sample]</TD>
            <TD>AGNs in the Extended Groth Strip Survey (Ramos Almeida+, 2009)</TD>
            <TD>We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179#sample</TD>
            <TD>2011-10-19T15:56:43Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/179&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/179</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/1043 [1]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#1</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/1043</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/1043 [2]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#2</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/1043&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1043 [table2]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#table2</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1043&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1043 [table1]</TD>
            <TD>Globular clusters in M31 and the Galaxy (van den Bergh+, 2010)</TD>
            <TD>The Milky Way system and the Andromeda galaxy experienced radically different evolutionary histories. Nevertheless, it is found that these two galaxies ended up with globular cluster systems in which individual clusters have indistinguishable distributions of half-light radii. Furthermore, globulars in both M31 and the Galaxy are found to have radii that are independent of their luminosities. In this respect, globular clusters differ drastically from early-type galaxies in which half-light radius and luminosity are tightly correlated. Metal-rich globular clusters in M31 occupy a slightly larger volume than do those in the Galaxy. The specific globular cluster frequency in the Andromeda galaxy is found to be significantly higher than it is in the Milky Way system. The present discussion is based on the 107 Galactic globular clusters, and 200 putative globulars in M31, for which UBV photometry was available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043#table1</TD>
            <TD>2012-08-22T12:13:24Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1043</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1043&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1043</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/544/A104 [1]</TD>
            <TD>Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)</TD>
            <TD>The target selection strategy, mask design procedure and observations are similar to those adopted for the EDisCS spectroscopy, described in detail in Halliday et al. (2004, Cat. J/A+A/427/397) and Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target selection was based on the available VLT/FORS2 optical photometry (White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR photometry (Aragon-Salamanca et al., in preparation). The optical data cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph field-of-view. The NIR data cover a somewhat smaller region of 4.2'x5.4'. Spectroscopic observations were completed using the FORS2 spectrograph (cf. Appenzeller et al., 1998Msngr..94....1A) on the VLT, during one observing run in March 2008, comprised of 3 half-nights. A high-efficiency grism was used (grism 600RI+19, {lambda}_central_=6780{AA}, resolution FWHM~6{AA}). The exposure time was 1800 seconds per frame, for a total of 8 frames per mask. A total of 3 masks were observed, for a total of 94 slits (33 slits in mask 1 and 2 and 28 slits in mask 3). The reduction was performed using an "improved sky subtraction", whose properties and advantages have been largely described and discussed in Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). Galaxy redshifts were measured from the reduced 1D spectra, using emission lines where possible, as done in Poggianti et al. (2006ApJ...642..188P). In addition, when possible, we also measured the equivalent width of [OII] and H{delta}. Note that for star-forming galaxies the H{delta} absorption line may be affected by emission in-filling. We have not attempted to correct for this effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104#1</TD>
            <TD>2012-08-22T18:00:56Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/544/A104</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A104</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/544/A104 [2]</TD>
            <TD>Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)</TD>
            <TD>The target selection strategy, mask design procedure and observations are similar to those adopted for the EDisCS spectroscopy, described in detail in Halliday et al. (2004, Cat. J/A+A/427/397) and Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target selection was based on the available VLT/FORS2 optical photometry (White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR photometry (Aragon-Salamanca et al., in preparation). The optical data cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph field-of-view. The NIR data cover a somewhat smaller region of 4.2'x5.4'. Spectroscopic observations were completed using the FORS2 spectrograph (cf. Appenzeller et al., 1998Msngr..94....1A) on the VLT, during one observing run in March 2008, comprised of 3 half-nights. A high-efficiency grism was used (grism 600RI+19, {lambda}_central_=6780{AA}, resolution FWHM~6{AA}). The exposure time was 1800 seconds per frame, for a total of 8 frames per mask. A total of 3 masks were observed, for a total of 94 slits (33 slits in mask 1 and 2 and 28 slits in mask 3). The reduction was performed using an "improved sky subtraction", whose properties and advantages have been largely described and discussed in Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). Galaxy redshifts were measured from the reduced 1D spectra, using emission lines where possible, as done in Poggianti et al. (2006ApJ...642..188P). In addition, when possible, we also measured the equivalent width of [OII] and H{delta}. Note that for star-forming galaxies the H{delta} absorption line may be affected by emission in-filling. We have not attempted to correct for this effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104#2</TD>
            <TD>2012-08-22T18:00:56Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/544/A104&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/544/A104 [table1]</TD>
            <TD>Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)</TD>
            <TD>The target selection strategy, mask design procedure and observations are similar to those adopted for the EDisCS spectroscopy, described in detail in Halliday et al. (2004, Cat. J/A+A/427/397) and Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target selection was based on the available VLT/FORS2 optical photometry (White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR photometry (Aragon-Salamanca et al., in preparation). The optical data cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph field-of-view. The NIR data cover a somewhat smaller region of 4.2'x5.4'. Spectroscopic observations were completed using the FORS2 spectrograph (cf. Appenzeller et al., 1998Msngr..94....1A) on the VLT, during one observing run in March 2008, comprised of 3 half-nights. A high-efficiency grism was used (grism 600RI+19, {lambda}_central_=6780{AA}, resolution FWHM~6{AA}). The exposure time was 1800 seconds per frame, for a total of 8 frames per mask. A total of 3 masks were observed, for a total of 94 slits (33 slits in mask 1 and 2 and 28 slits in mask 3). The reduction was performed using an "improved sky subtraction", whose properties and advantages have been largely described and discussed in Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). Galaxy redshifts were measured from the reduced 1D spectra, using emission lines where possible, as done in Poggianti et al. (2006ApJ...642..188P). In addition, when possible, we also measured the equivalent width of [OII] and H{delta}. Note that for star-forming galaxies the H{delta} absorption line may be affected by emission in-filling. We have not attempted to correct for this effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104#table1</TD>
            <TD>2012-08-22T18:00:56Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/544/A104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A104</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/193 [1]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#1</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/193 [2]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#2</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/193 [zbig]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#zbig</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/193 [zcat]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#zcat</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/544/A104 [1]</TD>
            <TD>Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)</TD>
            <TD>The target selection strategy, mask design procedure and observations are similar to those adopted for the EDisCS spectroscopy, described in detail in Halliday et al. (2004, Cat. J/A+A/427/397) and Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target selection was based on the available VLT/FORS2 optical photometry (White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR photometry (Aragon-Salamanca et al., in preparation). The optical data cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph field-of-view. The NIR data cover a somewhat smaller region of 4.2'x5.4'. Spectroscopic observations were completed using the FORS2 spectrograph (cf. Appenzeller et al., 1998Msngr..94....1A) on the VLT, during one observing run in March 2008, comprised of 3 half-nights. A high-efficiency grism was used (grism 600RI+19, {lambda}_central_=6780{AA}, resolution FWHM~6{AA}). The exposure time was 1800 seconds per frame, for a total of 8 frames per mask. A total of 3 masks were observed, for a total of 94 slits (33 slits in mask 1 and 2 and 28 slits in mask 3). The reduction was performed using an "improved sky subtraction", whose properties and advantages have been largely described and discussed in Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). Galaxy redshifts were measured from the reduced 1D spectra, using emission lines where possible, as done in Poggianti et al. (2006ApJ...642..188P). In addition, when possible, we also measured the equivalent width of [OII] and H{delta}. Note that for star-forming galaxies the H{delta} absorption line may be affected by emission in-filling. We have not attempted to correct for this effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104#1</TD>
            <TD>2012-08-22T18:00:56Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/544/A104</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A104</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/544/A104 [2]</TD>
            <TD>Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)</TD>
            <TD>The target selection strategy, mask design procedure and observations are similar to those adopted for the EDisCS spectroscopy, described in detail in Halliday et al. (2004, Cat. J/A+A/427/397) and Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target selection was based on the available VLT/FORS2 optical photometry (White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR photometry (Aragon-Salamanca et al., in preparation). The optical data cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph field-of-view. The NIR data cover a somewhat smaller region of 4.2'x5.4'. Spectroscopic observations were completed using the FORS2 spectrograph (cf. Appenzeller et al., 1998Msngr..94....1A) on the VLT, during one observing run in March 2008, comprised of 3 half-nights. A high-efficiency grism was used (grism 600RI+19, {lambda}_central_=6780{AA}, resolution FWHM~6{AA}). The exposure time was 1800 seconds per frame, for a total of 8 frames per mask. A total of 3 masks were observed, for a total of 94 slits (33 slits in mask 1 and 2 and 28 slits in mask 3). The reduction was performed using an "improved sky subtraction", whose properties and advantages have been largely described and discussed in Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). Galaxy redshifts were measured from the reduced 1D spectra, using emission lines where possible, as done in Poggianti et al. (2006ApJ...642..188P). In addition, when possible, we also measured the equivalent width of [OII] and H{delta}. Note that for star-forming galaxies the H{delta} absorption line may be affected by emission in-filling. We have not attempted to correct for this effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104#2</TD>
            <TD>2012-08-22T18:00:56Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/544/A104&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/544/A104 [table1]</TD>
            <TD>Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)</TD>
            <TD>The target selection strategy, mask design procedure and observations are similar to those adopted for the EDisCS spectroscopy, described in detail in Halliday et al. (2004, Cat. J/A+A/427/397) and Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target selection was based on the available VLT/FORS2 optical photometry (White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR photometry (Aragon-Salamanca et al., in preparation). The optical data cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph field-of-view. The NIR data cover a somewhat smaller region of 4.2'x5.4'. Spectroscopic observations were completed using the FORS2 spectrograph (cf. Appenzeller et al., 1998Msngr..94....1A) on the VLT, during one observing run in March 2008, comprised of 3 half-nights. A high-efficiency grism was used (grism 600RI+19, {lambda}_central_=6780{AA}, resolution FWHM~6{AA}). The exposure time was 1800 seconds per frame, for a total of 8 frames per mask. A total of 3 masks were observed, for a total of 94 slits (33 slits in mask 1 and 2 and 28 slits in mask 3). The reduction was performed using an "improved sky subtraction", whose properties and advantages have been largely described and discussed in Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). Galaxy redshifts were measured from the reduced 1D spectra, using emission lines where possible, as done in Poggianti et al. (2006ApJ...642..188P). In addition, when possible, we also measured the equivalent width of [OII] and H{delta}. Note that for star-forming galaxies the H{delta} absorption line may be affected by emission in-filling. We have not attempted to correct for this effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104#table1</TD>
            <TD>2012-08-22T18:00:56Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/544/A104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A104</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/193 [1]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#1</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/193 [2]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#2</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/193 [zbig]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#zbig</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/193 [zcat]</TD>
            <TD>The CfA Redshift Catalogue, Version June 1995 (Huchra+ 1995)</TD>
            <TD>The catalog (files zcat.dat and zbig.dat) incorporates much of the latest velocity data from the Whipple Observatory and other sources as well as velocities from earlier compilations such as the Second Reference Catalogue of de Vaucouleurs, de Vaucouleurs, and Corwin; the Index of Galaxy Spectra of Gisler and Friel, and the Catalogue of Radial Velocities of Galaxies of Palumbo, Tanzella-Nitti, and Vettolani. The data included here are BT magnitudes and a few UGC numbers with increased "accuracy" in the velocity source information. The following separate tables contain selected objects from the CfA Redshift Survey: - the first CfA Redsdhift Survey (Huchra et al., 1983ApJS...52...89H); this catalogue contains 2395 galaxies, a number slightly smaller than the published number of 2399, since there have been small corrections to the magnitudes for multiple galaxies. This version has had new morphological types added by me as well as POSS diameters measured for those galaxies that were not in the UGC or did not have UGC diameters. - the first slice of the second CfA redshift survey (Huchra et al., 1990ApJS...72..433H) - the second slice of the CfA redshift survey (Huchra et al., 1995ApJS...99..391H) See the complete description in 'zcom.tex' (in plain TeX), or zcom.txt (plain ascii)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/193#zcat</TD>
            <TD>2011-09-14T18:39:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/544/A104 [1]</TD>
            <TD>Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)</TD>
            <TD>The target selection strategy, mask design procedure and observations are similar to those adopted for the EDisCS spectroscopy, described in detail in Halliday et al. (2004, Cat. J/A+A/427/397) and Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target selection was based on the available VLT/FORS2 optical photometry (White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR photometry (Aragon-Salamanca et al., in preparation). The optical data cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph field-of-view. The NIR data cover a somewhat smaller region of 4.2'x5.4'. Spectroscopic observations were completed using the FORS2 spectrograph (cf. Appenzeller et al., 1998Msngr..94....1A) on the VLT, during one observing run in March 2008, comprised of 3 half-nights. A high-efficiency grism was used (grism 600RI+19, {lambda}_central_=6780{AA}, resolution FWHM~6{AA}). The exposure time was 1800 seconds per frame, for a total of 8 frames per mask. A total of 3 masks were observed, for a total of 94 slits (33 slits in mask 1 and 2 and 28 slits in mask 3). The reduction was performed using an "improved sky subtraction", whose properties and advantages have been largely described and discussed in Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). Galaxy redshifts were measured from the reduced 1D spectra, using emission lines where possible, as done in Poggianti et al. (2006ApJ...642..188P). In addition, when possible, we also measured the equivalent width of [OII] and H{delta}. Note that for star-forming galaxies the H{delta} absorption line may be affected by emission in-filling. We have not attempted to correct for this effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104#1</TD>
            <TD>2012-08-22T18:00:56Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/544/A104</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A104</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/544/A104 [2]</TD>
            <TD>Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)</TD>
            <TD>The target selection strategy, mask design procedure and observations are similar to those adopted for the EDisCS spectroscopy, described in detail in Halliday et al. (2004, Cat. J/A+A/427/397) and Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target selection was based on the available VLT/FORS2 optical photometry (White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR photometry (Aragon-Salamanca et al., in preparation). The optical data cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph field-of-view. The NIR data cover a somewhat smaller region of 4.2'x5.4'. Spectroscopic observations were completed using the FORS2 spectrograph (cf. Appenzeller et al., 1998Msngr..94....1A) on the VLT, during one observing run in March 2008, comprised of 3 half-nights. A high-efficiency grism was used (grism 600RI+19, {lambda}_central_=6780{AA}, resolution FWHM~6{AA}). The exposure time was 1800 seconds per frame, for a total of 8 frames per mask. A total of 3 masks were observed, for a total of 94 slits (33 slits in mask 1 and 2 and 28 slits in mask 3). The reduction was performed using an "improved sky subtraction", whose properties and advantages have been largely described and discussed in Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). Galaxy redshifts were measured from the reduced 1D spectra, using emission lines where possible, as done in Poggianti et al. (2006ApJ...642..188P). In addition, when possible, we also measured the equivalent width of [OII] and H{delta}. Note that for star-forming galaxies the H{delta} absorption line may be affected by emission in-filling. We have not attempted to correct for this effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104#2</TD>
            <TD>2012-08-22T18:00:56Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/544/A104&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/544/A104 [table1]</TD>
            <TD>Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)</TD>
            <TD>The target selection strategy, mask design procedure and observations are similar to those adopted for the EDisCS spectroscopy, described in detail in Halliday et al. (2004, Cat. J/A+A/427/397) and Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target selection was based on the available VLT/FORS2 optical photometry (White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR photometry (Aragon-Salamanca et al., in preparation). The optical data cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph field-of-view. The NIR data cover a somewhat smaller region of 4.2'x5.4'. Spectroscopic observations were completed using the FORS2 spectrograph (cf. Appenzeller et al., 1998Msngr..94....1A) on the VLT, during one observing run in March 2008, comprised of 3 half-nights. A high-efficiency grism was used (grism 600RI+19, {lambda}_central_=6780{AA}, resolution FWHM~6{AA}). The exposure time was 1800 seconds per frame, for a total of 8 frames per mask. A total of 3 masks were observed, for a total of 94 slits (33 slits in mask 1 and 2 and 28 slits in mask 3). The reduction was performed using an "improved sky subtraction", whose properties and advantages have been largely described and discussed in Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). Galaxy redshifts were measured from the reduced 1D spectra, using emission lines where possible, as done in Poggianti et al. (2006ApJ...642..188P). In addition, when possible, we also measured the equivalent width of [OII] and H{delta}. Note that for star-forming galaxies the H{delta} absorption line may be affected by emission in-filling. We have not attempted to correct for this effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104#table1</TD>
            <TD>2012-08-22T18:00:56Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/544/A104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A104</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/204 [1]</TD>
            <TD>Galaxy properties at NGP (Odewahn+ 1995)</TD>
            <TD>A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/204#1</TD>
            <TD>2011-09-14T18:39:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/204</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/204</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/204 [2]</TD>
            <TD>Galaxy properties at NGP (Odewahn+ 1995)</TD>
            <TD>A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/204#2</TD>
            <TD>2011-09-14T18:39:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/204&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/204</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/204 [catalog]</TD>
            <TD>Galaxy properties at NGP (Odewahn+ 1995)</TD>
            <TD>A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/204#catalog</TD>
            <TD>2011-09-14T18:39:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/204</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/204&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/204</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/711/928 [1]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#1</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/711/928</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/711/928 [2]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#2</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [lae]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#lae</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [galex]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#galex</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [table14]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#table14</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [deimos]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#deimos</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/204 [1]</TD>
            <TD>Galaxy properties at NGP (Odewahn+ 1995)</TD>
            <TD>A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/204#1</TD>
            <TD>2011-09-14T18:39:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/204</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/204</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/204 [2]</TD>
            <TD>Galaxy properties at NGP (Odewahn+ 1995)</TD>
            <TD>A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/204#2</TD>
            <TD>2011-09-14T18:39:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/204&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/204</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/204 [catalog]</TD>
            <TD>Galaxy properties at NGP (Odewahn+ 1995)</TD>
            <TD>A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/204#catalog</TD>
            <TD>2011-09-14T18:39:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/204</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/204&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/204</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/711/928 [1]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#1</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/711/928</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/711/928 [2]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#2</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [lae]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#lae</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [galex]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#galex</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [table14]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#table14</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [deimos]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#deimos</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/204 [1]</TD>
            <TD>Galaxy properties at NGP (Odewahn+ 1995)</TD>
            <TD>A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/204#1</TD>
            <TD>2011-09-14T18:39:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/204</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/204</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/204 [2]</TD>
            <TD>Galaxy properties at NGP (Odewahn+ 1995)</TD>
            <TD>A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/204#2</TD>
            <TD>2011-09-14T18:39:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/204&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/204</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/204 [catalog]</TD>
            <TD>Galaxy properties at NGP (Odewahn+ 1995)</TD>
            <TD>A two-color study of the galaxies detected on POSS-I in a 289deg^2^ region centered on the North Galactic Pole is presented. We use a variety of mapping techniques to characterize the large-scale spatial distribution of galaxies. The depth and sample size of this new survey allows, for the first time, the isolation of large photometric subsamples of galaxies in high- and low-density environments on the scale of superclusters. Our principal finding is a statistically significant difference between the mean photometric properties of these subsamples in the sense that galaxies in the high-density Coma and filament environments have redded colors and larger concentration indices than galaxies drawn from low-density interfilament regions. These results are in agreement with the known morphology-density relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/204#catalog</TD>
            <TD>2011-09-14T18:39:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/204</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/204&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/204</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/711/928 [1]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#1</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/711/928</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/711/928 [2]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#2</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [lae]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#lae</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [galex]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#galex</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [table14]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#table14</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/928 [deimos]</TD>
            <TD>Low-redshift Ly{alpha} galaxies from GALEX (Cowie+, 2010)</TD>
            <TD>For each targeted field, we obtained the one- and two-dimensional spectra of all the sources with GALEX grism observations from the Multimission Archive at STScI (MAST). The FUV spectra cover a wavelength range of approximately 1300-1800{AA} at a resolution of ~10{AA}, and the NUV spectra cover a wavelength range of approximately 1850-3000{AA} at a resolution of ~25{AA}. The final Ly{alpha} selected samples are summarized in Tables 2-10. We made optical spectroscopic follow-up observations with the DEIMOS spectrograph on the Keck II 10 m telescope. We obtained observations of 39 sources randomly chosen from our GALEX candidate Ly{alpha} Galaxy sample, 38 of which lie in the redshift interval z=0.195-0.44 and one in the redshift interval z=0.65-1.25 (Table 11), 15 sources randomly chosen from our GALEX AGN sample (Table 12), and 124 sources randomly chosen from our GALEX spectroscopic sample without UV spectral identifications. For the latter, we summarize only the 47 sources found to lie in the redshift interval z=0.195-0.44 (Table 13).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928#deimos</TD>
            <TD>2012-08-23T08:36:21Z</TD>
            <TD>#AGN#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/928</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/928&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/928</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/287/293 [1]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#1</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/287/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/287/293 [2]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#2</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/287/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/287/293 [table1]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#table1</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/287/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/287/293 [tab2-8]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#tab2-8</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/287/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/37 [1]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#1</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/37</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/37 [2]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#2</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/37&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/37 [table1]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#table1</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/37 [table2]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#table2</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/287/293 [1]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#1</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/287/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/287/293 [2]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#2</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/287/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/287/293 [table1]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#table1</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/287/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/287/293 [tab2-8]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#tab2-8</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/287/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/287/293 [1]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#1</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/287/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/287/293 [2]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#2</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/287/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/287/293 [table1]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#table1</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/287/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/287/293 [tab2-8]</TD>
            <TD>BR photometry of EUVE sources (Maoz+ 1997)</TD>
            <TD>Most of the sources detected in the extreme ultraviolet (EUV; 100-600{AA}) by the ROSAT/WFC and EUVE all-sky surveys have been identified with active late-type stars and hot white dwarfs that are near enough to the Earth to escape absorption by interstellar gas. However, about 15 per cent of EUV sources are as yet unidentified with any optical counterparts. We examine whether the unidentified EUV sources may consist of the same population of late-type stars and white dwarfs. We present B and R photometry of stars in the fields of seven of the unidentified EUV sources. We detect in the optical the entire main-sequence and white dwarf population out to the greatest distances where they could still avoid absorption. We use colour-magnitude diagrams to demonstrate that, in most of the fields, none of the observed stars has the colours and magnitudes of late-type dwarfs at distances less than 100pc. Similarly, none of the observed stars is a white dwarf within 500pc that is hot enough to be a EUV emitter. The unidentified EUV sources we study are not detected in X-rays, while cataclysmic variables, X-ray binaries, and active galactic nuclei generally are. We conclude that some of the EUV sources may be a new class of nearby objects, which are either very faint at optical bands or which mimic the colours and magnitudes of distant late-type stars or cool white dwarfs. One candidate for optically faint objects is isolated old neutron stars, slowly accreting interstellar matter. Such neutron stars are expected to be abundant in the Galaxy, and have not been unambiguously detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293#tab2-8</TD>
            <TD>2011-09-14T18:39:53Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/287/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/37 [1]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#1</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/37</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/37 [2]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#2</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/37&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/37 [table1]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#table1</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/37 [table2]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#table2</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/179 [1]</TD>
            <TD>AGNs in the Extended Groth Strip Survey (Ramos Almeida+, 2009)</TD>
            <TD>We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179#1</TD>
            <TD>2011-10-19T15:56:43Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/179</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/179</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/179 [2]</TD>
            <TD>AGNs in the Extended Groth Strip Survey (Ramos Almeida+, 2009)</TD>
            <TD>We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179#2</TD>
            <TD>2011-10-19T15:56:43Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/179&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/179</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/179 [sample]</TD>
            <TD>AGNs in the Extended Groth Strip Survey (Ramos Almeida+, 2009)</TD>
            <TD>We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179#sample</TD>
            <TD>2011-10-19T15:56:43Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/179</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/179&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/179</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/471/L5 [1]</TD>
            <TD>Redshift clustering in the Hubble Deep Field (Cohen+ 1996)</TD>
            <TD>We present initial results from a redshift survey carried out with the low-resolution imaging spectrograph on the 10m W. M. Keck Telescope in the Hubble Deep Field. In the redshift distribution of the 140 extragalactic objects in this sample, we find six strong peaks with velocity dispersions of ~400km/s. The areal density of objects within a particular peak, while it may be nonuniform, does not show evidence for strong central concentration. These peaks have characteristics (velocity dispersions, density enhancements, spacing, and spatial extent) similar to those seen in a comparable redshift survey in a different high Galactic latitude field (Cohen and coworkers), confirming that the structures are generic. They are probably the high-redshift counterparts of huge galaxy structures ("walls") observed locally.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5#1</TD>
            <TD>2011-09-14T18:39:54Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/471/L5</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/L5</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/471/L5 [2]</TD>
            <TD>Redshift clustering in the Hubble Deep Field (Cohen+ 1996)</TD>
            <TD>We present initial results from a redshift survey carried out with the low-resolution imaging spectrograph on the 10m W. M. Keck Telescope in the Hubble Deep Field. In the redshift distribution of the 140 extragalactic objects in this sample, we find six strong peaks with velocity dispersions of ~400km/s. The areal density of objects within a particular peak, while it may be nonuniform, does not show evidence for strong central concentration. These peaks have characteristics (velocity dispersions, density enhancements, spacing, and spatial extent) similar to those seen in a comparable redshift survey in a different high Galactic latitude field (Cohen and coworkers), confirming that the structures are generic. They are probably the high-redshift counterparts of huge galaxy structures ("walls") observed locally.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5#2</TD>
            <TD>2011-09-14T18:39:54Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/471/L5&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/L5</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/471/L5 [table1]</TD>
            <TD>Redshift clustering in the Hubble Deep Field (Cohen+ 1996)</TD>
            <TD>We present initial results from a redshift survey carried out with the low-resolution imaging spectrograph on the 10m W. M. Keck Telescope in the Hubble Deep Field. In the redshift distribution of the 140 extragalactic objects in this sample, we find six strong peaks with velocity dispersions of ~400km/s. The areal density of objects within a particular peak, while it may be nonuniform, does not show evidence for strong central concentration. These peaks have characteristics (velocity dispersions, density enhancements, spacing, and spatial extent) similar to those seen in a comparable redshift survey in a different high Galactic latitude field (Cohen and coworkers), confirming that the structures are generic. They are probably the high-redshift counterparts of huge galaxy structures ("walls") observed locally.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5#table1</TD>
            <TD>2011-09-14T18:39:54Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/471/L5&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/L5</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/37 [1]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#1</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/37</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/37 [2]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#2</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/37&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/37 [table1]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#table1</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/37 [table2]</TD>
            <TD>GALEX catalog of star clusters in M31 (Kang+, 2012)</TD>
            <TD>We construct a new compiled catalog of star clusters in M31 carefully considering three previously published catalogs: RBC version 4 (v4; see also Galleti et al., 2004, Cat. J/A+A/416/917), Caldwell et al. (2009, Cat. J/AJ/137/94, 2011AJ....141...61C), and Peacock et al. (2010, Cat. J/MNRAS/402/803). In this paper, we only consider 700 star clusters that are classified as confirmed star clusters at least in one of the three catalogs. We used UV images from the Nearby Galaxy Survey (NGS) obtained by GALEX in two UV bands: far-ultraviolet (FUV; 1350-1750{AA}) and near-ultraviolet (NUV; 1750-2750{AA}). A total of 23 images (about 17deg^2^) have covered most of the disk and halo of M31. The details of the GALEX observations for M31 are presented in Rey et al. (2005ApJ...619L.119R, 2007, Cat. J/ApJS/173/643).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37#table2</TD>
            <TD>2012-09-07T23:08:15Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/471/L5 [1]</TD>
            <TD>Redshift clustering in the Hubble Deep Field (Cohen+ 1996)</TD>
            <TD>We present initial results from a redshift survey carried out with the low-resolution imaging spectrograph on the 10m W. M. Keck Telescope in the Hubble Deep Field. In the redshift distribution of the 140 extragalactic objects in this sample, we find six strong peaks with velocity dispersions of ~400km/s. The areal density of objects within a particular peak, while it may be nonuniform, does not show evidence for strong central concentration. These peaks have characteristics (velocity dispersions, density enhancements, spacing, and spatial extent) similar to those seen in a comparable redshift survey in a different high Galactic latitude field (Cohen and coworkers), confirming that the structures are generic. They are probably the high-redshift counterparts of huge galaxy structures ("walls") observed locally.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5#1</TD>
            <TD>2011-09-14T18:39:54Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/471/L5</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/L5</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/471/L5 [2]</TD>
            <TD>Redshift clustering in the Hubble Deep Field (Cohen+ 1996)</TD>
            <TD>We present initial results from a redshift survey carried out with the low-resolution imaging spectrograph on the 10m W. M. Keck Telescope in the Hubble Deep Field. In the redshift distribution of the 140 extragalactic objects in this sample, we find six strong peaks with velocity dispersions of ~400km/s. The areal density of objects within a particular peak, while it may be nonuniform, does not show evidence for strong central concentration. These peaks have characteristics (velocity dispersions, density enhancements, spacing, and spatial extent) similar to those seen in a comparable redshift survey in a different high Galactic latitude field (Cohen and coworkers), confirming that the structures are generic. They are probably the high-redshift counterparts of huge galaxy structures ("walls") observed locally.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5#2</TD>
            <TD>2011-09-14T18:39:54Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/471/L5&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/L5</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/471/L5 [table1]</TD>
            <TD>Redshift clustering in the Hubble Deep Field (Cohen+ 1996)</TD>
            <TD>We present initial results from a redshift survey carried out with the low-resolution imaging spectrograph on the 10m W. M. Keck Telescope in the Hubble Deep Field. In the redshift distribution of the 140 extragalactic objects in this sample, we find six strong peaks with velocity dispersions of ~400km/s. The areal density of objects within a particular peak, while it may be nonuniform, does not show evidence for strong central concentration. These peaks have characteristics (velocity dispersions, density enhancements, spacing, and spatial extent) similar to those seen in a comparable redshift survey in a different high Galactic latitude field (Cohen and coworkers), confirming that the structures are generic. They are probably the high-redshift counterparts of huge galaxy structures ("walls") observed locally.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5#table1</TD>
            <TD>2011-09-14T18:39:54Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/471/L5&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/L5</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/471/L5 [1]</TD>
            <TD>Redshift clustering in the Hubble Deep Field (Cohen+ 1996)</TD>
            <TD>We present initial results from a redshift survey carried out with the low-resolution imaging spectrograph on the 10m W. M. Keck Telescope in the Hubble Deep Field. In the redshift distribution of the 140 extragalactic objects in this sample, we find six strong peaks with velocity dispersions of ~400km/s. The areal density of objects within a particular peak, while it may be nonuniform, does not show evidence for strong central concentration. These peaks have characteristics (velocity dispersions, density enhancements, spacing, and spatial extent) similar to those seen in a comparable redshift survey in a different high Galactic latitude field (Cohen and coworkers), confirming that the structures are generic. They are probably the high-redshift counterparts of huge galaxy structures ("walls") observed locally.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5#1</TD>
            <TD>2011-09-14T18:39:54Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/471/L5</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/L5</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/471/L5 [2]</TD>
            <TD>Redshift clustering in the Hubble Deep Field (Cohen+ 1996)</TD>
            <TD>We present initial results from a redshift survey carried out with the low-resolution imaging spectrograph on the 10m W. M. Keck Telescope in the Hubble Deep Field. In the redshift distribution of the 140 extragalactic objects in this sample, we find six strong peaks with velocity dispersions of ~400km/s. The areal density of objects within a particular peak, while it may be nonuniform, does not show evidence for strong central concentration. These peaks have characteristics (velocity dispersions, density enhancements, spacing, and spatial extent) similar to those seen in a comparable redshift survey in a different high Galactic latitude field (Cohen and coworkers), confirming that the structures are generic. They are probably the high-redshift counterparts of huge galaxy structures ("walls") observed locally.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5#2</TD>
            <TD>2011-09-14T18:39:54Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/471/L5&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/L5</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/471/L5 [table1]</TD>
            <TD>Redshift clustering in the Hubble Deep Field (Cohen+ 1996)</TD>
            <TD>We present initial results from a redshift survey carried out with the low-resolution imaging spectrograph on the 10m W. M. Keck Telescope in the Hubble Deep Field. In the redshift distribution of the 140 extragalactic objects in this sample, we find six strong peaks with velocity dispersions of ~400km/s. The areal density of objects within a particular peak, while it may be nonuniform, does not show evidence for strong central concentration. These peaks have characteristics (velocity dispersions, density enhancements, spacing, and spatial extent) similar to those seen in a comparable redshift survey in a different high Galactic latitude field (Cohen and coworkers), confirming that the structures are generic. They are probably the high-redshift counterparts of huge galaxy structures ("walls") observed locally.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5#table1</TD>
            <TD>2011-09-14T18:39:54Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/L5</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/471/L5&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/L5</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/iram [1]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#1</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/iram</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/iram [2]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#2</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/iram&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/iram [30m]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#30m</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/iram&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/iram [pdbi]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#pdbi</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/iram&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/iram [1]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#1</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/iram</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/iram [2]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#2</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/iram&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/iram [30m]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#30m</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/iram&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/iram [pdbi]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#pdbi</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/iram&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/483/826 [1]</TD>
            <TD>BVI CCD photometry of Berkeley 17 (Phelps 1997)</TD>
            <TD>Faint magnitude BVI CCD photometry of the central region of the old open cluster Berkeley 17 (Be 17) has been undertaken to investigate the claim that it is the oldest open cluster yet discovered (Phelps, Janes, &amp; Montgomery, 1994AJ....107.1079P). This study reveals Be 17 to have a metallicity -0.30&lt;=[Fe/H]&lt;=0.00; a reddening 0.52&lt;=E(B-V)&lt;=0.68 or 0.61&lt;=E(V-I)&lt;=0.71; a distance modulus, (m-M)_0_=12.15+/-0.10, corresponding to a distance of 2.7+/-0.1kpc; a diameter of ~10pc; a minimum mass of 400 Msun; and an age of 10-13Gyr. With an adopted age of 12(+1)(-2)Gyr, these results suggest that Be 17 is indeed the oldest open cluster yet discovered. The inferred old age for Be 17 indicates that the cluster is an important one for studies of the differences between open and globular clusters, the transition from the halo/thick disk to the thin disk of the Galaxy, and even for establishing the minimum age of the universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/826#1</TD>
            <TD>2011-09-14T18:41:40Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/826</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/483/826</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/483/826</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/483/826 [2]</TD>
            <TD>BVI CCD photometry of Berkeley 17 (Phelps 1997)</TD>
            <TD>Faint magnitude BVI CCD photometry of the central region of the old open cluster Berkeley 17 (Be 17) has been undertaken to investigate the claim that it is the oldest open cluster yet discovered (Phelps, Janes, &amp; Montgomery, 1994AJ....107.1079P). This study reveals Be 17 to have a metallicity -0.30&lt;=[Fe/H]&lt;=0.00; a reddening 0.52&lt;=E(B-V)&lt;=0.68 or 0.61&lt;=E(V-I)&lt;=0.71; a distance modulus, (m-M)_0_=12.15+/-0.10, corresponding to a distance of 2.7+/-0.1kpc; a diameter of ~10pc; a minimum mass of 400 Msun; and an age of 10-13Gyr. With an adopted age of 12(+1)(-2)Gyr, these results suggest that Be 17 is indeed the oldest open cluster yet discovered. The inferred old age for Be 17 indicates that the cluster is an important one for studies of the differences between open and globular clusters, the transition from the halo/thick disk to the thin disk of the Galaxy, and even for establishing the minimum age of the universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/826#2</TD>
            <TD>2011-09-14T18:41:40Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/826</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/483/826&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/483/826</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/iram [1]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#1</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/iram</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/iram [2]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#2</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/iram&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/iram [30m]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#30m</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/iram&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/iram [pdbi]</TD>
            <TD>IRAM Observation Logs 1991-2010 (IRAM 1991-2012)</TD>
            <TD>The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: The 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure site, and summarizes the observations made there between December 1990 and October 2010. The observations log of the 30-m single-dish telescope covers the period 2009-01-01 to 2010-12-31. This log was produced using a header archive, a collaborative effort between IRAM and IAA/CSIC.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/iram#pdbi</TD>
            <TD>2012-10-23T14:39:48Z</TD>
            <TD>#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/B/iram</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/iram&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/iram</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/545/A16 [1]</TD>
            <TD>Halpha3. Catalog and SFR in Virgo cluster (Gavazzi+, 2012)</TD>
            <TD>We present H{alpha}3 (acronym for H{alpha}-{alpha}{alpha}), an H{alpha} narrow-band imaging survey of ~400 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local Supercluster, including the Virgo cluster. By using hydrogen recombination lines as a tracer of recent star formation, we aim to investigate the relationships between atomic neutral gas and newly formed stars in different environments (cluster and field), morphological types (spirals and dwarfs), and over a wide range of stellar masses (~10^7.5^-10^11.5^M_{sun}_). We image in H{alpha}+[NII] all the galaxies that contain more than 10^7^M_{sun}_ of neutral atomic hydrogen in the sky region 11h&lt;R.A.&lt;16h ; 4{deg}&lt;Dec.&lt;16{deg}; 350&lt;cz&lt;2000km/s using the San Pedro Martir 2m telescope. This survey provides a complete census of the star formation in HI rich galaxies of the local universe. We present the properties of the galaxy sample, together with H{alpha} fluxes and equivalent widths. We find an excellent agreement between the fluxes determined from our images in apertures of 3-arcsec diameter and the fluxes derived from the SDSS spectral database. From the H{alpha} fluxes corrected for galactic and internal extinction and for [NII] contamination we derive the global star formation rates (SFRs).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16#1</TD>
            <TD>2012-12-02T22:38:01Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/545/A16</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/545/A16</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/545/A16 [2]</TD>
            <TD>Halpha3. Catalog and SFR in Virgo cluster (Gavazzi+, 2012)</TD>
            <TD>We present H{alpha}3 (acronym for H{alpha}-{alpha}{alpha}), an H{alpha} narrow-band imaging survey of ~400 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local Supercluster, including the Virgo cluster. By using hydrogen recombination lines as a tracer of recent star formation, we aim to investigate the relationships between atomic neutral gas and newly formed stars in different environments (cluster and field), morphological types (spirals and dwarfs), and over a wide range of stellar masses (~10^7.5^-10^11.5^M_{sun}_). We image in H{alpha}+[NII] all the galaxies that contain more than 10^7^M_{sun}_ of neutral atomic hydrogen in the sky region 11h&lt;R.A.&lt;16h ; 4{deg}&lt;Dec.&lt;16{deg}; 350&lt;cz&lt;2000km/s using the San Pedro Martir 2m telescope. This survey provides a complete census of the star formation in HI rich galaxies of the local universe. We present the properties of the galaxy sample, together with H{alpha} fluxes and equivalent widths. We find an excellent agreement between the fluxes determined from our images in apertures of 3-arcsec diameter and the fluxes derived from the SDSS spectral database. From the H{alpha} fluxes corrected for galactic and internal extinction and for [NII] contamination we derive the global star formation rates (SFRs).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16#2</TD>
            <TD>2012-12-02T22:38:01Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/545/A16&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/545/A16</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/545/A16 [alpha3]</TD>
            <TD>Halpha3. Catalog and SFR in Virgo cluster (Gavazzi+, 2012)</TD>
            <TD>We present H{alpha}3 (acronym for H{alpha}-{alpha}{alpha}), an H{alpha} narrow-band imaging survey of ~400 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local Supercluster, including the Virgo cluster. By using hydrogen recombination lines as a tracer of recent star formation, we aim to investigate the relationships between atomic neutral gas and newly formed stars in different environments (cluster and field), morphological types (spirals and dwarfs), and over a wide range of stellar masses (~10^7.5^-10^11.5^M_{sun}_). We image in H{alpha}+[NII] all the galaxies that contain more than 10^7^M_{sun}_ of neutral atomic hydrogen in the sky region 11h&lt;R.A.&lt;16h ; 4{deg}&lt;Dec.&lt;16{deg}; 350&lt;cz&lt;2000km/s using the San Pedro Martir 2m telescope. This survey provides a complete census of the star formation in HI rich galaxies of the local universe. We present the properties of the galaxy sample, together with H{alpha} fluxes and equivalent widths. We find an excellent agreement between the fluxes determined from our images in apertures of 3-arcsec diameter and the fluxes derived from the SDSS spectral database. From the H{alpha} fluxes corrected for galactic and internal extinction and for [NII] contamination we derive the global star formation rates (SFRs).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16#alpha3</TD>
            <TD>2012-12-02T22:38:01Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/545/A16&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/545/A16</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/545/A16 [1]</TD>
            <TD>Halpha3. Catalog and SFR in Virgo cluster (Gavazzi+, 2012)</TD>
            <TD>We present H{alpha}3 (acronym for H{alpha}-{alpha}{alpha}), an H{alpha} narrow-band imaging survey of ~400 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local Supercluster, including the Virgo cluster. By using hydrogen recombination lines as a tracer of recent star formation, we aim to investigate the relationships between atomic neutral gas and newly formed stars in different environments (cluster and field), morphological types (spirals and dwarfs), and over a wide range of stellar masses (~10^7.5^-10^11.5^M_{sun}_). We image in H{alpha}+[NII] all the galaxies that contain more than 10^7^M_{sun}_ of neutral atomic hydrogen in the sky region 11h&lt;R.A.&lt;16h ; 4{deg}&lt;Dec.&lt;16{deg}; 350&lt;cz&lt;2000km/s using the San Pedro Martir 2m telescope. This survey provides a complete census of the star formation in HI rich galaxies of the local universe. We present the properties of the galaxy sample, together with H{alpha} fluxes and equivalent widths. We find an excellent agreement between the fluxes determined from our images in apertures of 3-arcsec diameter and the fluxes derived from the SDSS spectral database. From the H{alpha} fluxes corrected for galactic and internal extinction and for [NII] contamination we derive the global star formation rates (SFRs).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16#1</TD>
            <TD>2012-12-02T22:38:01Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/545/A16</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/545/A16</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/545/A16 [2]</TD>
            <TD>Halpha3. Catalog and SFR in Virgo cluster (Gavazzi+, 2012)</TD>
            <TD>We present H{alpha}3 (acronym for H{alpha}-{alpha}{alpha}), an H{alpha} narrow-band imaging survey of ~400 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local Supercluster, including the Virgo cluster. By using hydrogen recombination lines as a tracer of recent star formation, we aim to investigate the relationships between atomic neutral gas and newly formed stars in different environments (cluster and field), morphological types (spirals and dwarfs), and over a wide range of stellar masses (~10^7.5^-10^11.5^M_{sun}_). We image in H{alpha}+[NII] all the galaxies that contain more than 10^7^M_{sun}_ of neutral atomic hydrogen in the sky region 11h&lt;R.A.&lt;16h ; 4{deg}&lt;Dec.&lt;16{deg}; 350&lt;cz&lt;2000km/s using the San Pedro Martir 2m telescope. This survey provides a complete census of the star formation in HI rich galaxies of the local universe. We present the properties of the galaxy sample, together with H{alpha} fluxes and equivalent widths. We find an excellent agreement between the fluxes determined from our images in apertures of 3-arcsec diameter and the fluxes derived from the SDSS spectral database. From the H{alpha} fluxes corrected for galactic and internal extinction and for [NII] contamination we derive the global star formation rates (SFRs).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16#2</TD>
            <TD>2012-12-02T22:38:01Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/545/A16&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/545/A16</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/545/A16 [alpha3]</TD>
            <TD>Halpha3. Catalog and SFR in Virgo cluster (Gavazzi+, 2012)</TD>
            <TD>We present H{alpha}3 (acronym for H{alpha}-{alpha}{alpha}), an H{alpha} narrow-band imaging survey of ~400 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local Supercluster, including the Virgo cluster. By using hydrogen recombination lines as a tracer of recent star formation, we aim to investigate the relationships between atomic neutral gas and newly formed stars in different environments (cluster and field), morphological types (spirals and dwarfs), and over a wide range of stellar masses (~10^7.5^-10^11.5^M_{sun}_). We image in H{alpha}+[NII] all the galaxies that contain more than 10^7^M_{sun}_ of neutral atomic hydrogen in the sky region 11h&lt;R.A.&lt;16h ; 4{deg}&lt;Dec.&lt;16{deg}; 350&lt;cz&lt;2000km/s using the San Pedro Martir 2m telescope. This survey provides a complete census of the star formation in HI rich galaxies of the local universe. We present the properties of the galaxy sample, together with H{alpha} fluxes and equivalent widths. We find an excellent agreement between the fluxes determined from our images in apertures of 3-arcsec diameter and the fluxes derived from the SDSS spectral database. From the H{alpha} fluxes corrected for galactic and internal extinction and for [NII] contamination we derive the global star formation rates (SFRs).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16#alpha3</TD>
            <TD>2012-12-02T22:38:01Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/545/A16&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/545/A16</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/545/A16 [1]</TD>
            <TD>Halpha3. Catalog and SFR in Virgo cluster (Gavazzi+, 2012)</TD>
            <TD>We present H{alpha}3 (acronym for H{alpha}-{alpha}{alpha}), an H{alpha} narrow-band imaging survey of ~400 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local Supercluster, including the Virgo cluster. By using hydrogen recombination lines as a tracer of recent star formation, we aim to investigate the relationships between atomic neutral gas and newly formed stars in different environments (cluster and field), morphological types (spirals and dwarfs), and over a wide range of stellar masses (~10^7.5^-10^11.5^M_{sun}_). We image in H{alpha}+[NII] all the galaxies that contain more than 10^7^M_{sun}_ of neutral atomic hydrogen in the sky region 11h&lt;R.A.&lt;16h ; 4{deg}&lt;Dec.&lt;16{deg}; 350&lt;cz&lt;2000km/s using the San Pedro Martir 2m telescope. This survey provides a complete census of the star formation in HI rich galaxies of the local universe. We present the properties of the galaxy sample, together with H{alpha} fluxes and equivalent widths. We find an excellent agreement between the fluxes determined from our images in apertures of 3-arcsec diameter and the fluxes derived from the SDSS spectral database. From the H{alpha} fluxes corrected for galactic and internal extinction and for [NII] contamination we derive the global star formation rates (SFRs).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16#1</TD>
            <TD>2012-12-02T22:38:01Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/545/A16</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/545/A16</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/545/A16 [2]</TD>
            <TD>Halpha3. Catalog and SFR in Virgo cluster (Gavazzi+, 2012)</TD>
            <TD>We present H{alpha}3 (acronym for H{alpha}-{alpha}{alpha}), an H{alpha} narrow-band imaging survey of ~400 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local Supercluster, including the Virgo cluster. By using hydrogen recombination lines as a tracer of recent star formation, we aim to investigate the relationships between atomic neutral gas and newly formed stars in different environments (cluster and field), morphological types (spirals and dwarfs), and over a wide range of stellar masses (~10^7.5^-10^11.5^M_{sun}_). We image in H{alpha}+[NII] all the galaxies that contain more than 10^7^M_{sun}_ of neutral atomic hydrogen in the sky region 11h&lt;R.A.&lt;16h ; 4{deg}&lt;Dec.&lt;16{deg}; 350&lt;cz&lt;2000km/s using the San Pedro Martir 2m telescope. This survey provides a complete census of the star formation in HI rich galaxies of the local universe. We present the properties of the galaxy sample, together with H{alpha} fluxes and equivalent widths. We find an excellent agreement between the fluxes determined from our images in apertures of 3-arcsec diameter and the fluxes derived from the SDSS spectral database. From the H{alpha} fluxes corrected for galactic and internal extinction and for [NII] contamination we derive the global star formation rates (SFRs).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16#2</TD>
            <TD>2012-12-02T22:38:01Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/545/A16&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/545/A16</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/545/A16 [alpha3]</TD>
            <TD>Halpha3. Catalog and SFR in Virgo cluster (Gavazzi+, 2012)</TD>
            <TD>We present H{alpha}3 (acronym for H{alpha}-{alpha}{alpha}), an H{alpha} narrow-band imaging survey of ~400 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local Supercluster, including the Virgo cluster. By using hydrogen recombination lines as a tracer of recent star formation, we aim to investigate the relationships between atomic neutral gas and newly formed stars in different environments (cluster and field), morphological types (spirals and dwarfs), and over a wide range of stellar masses (~10^7.5^-10^11.5^M_{sun}_). We image in H{alpha}+[NII] all the galaxies that contain more than 10^7^M_{sun}_ of neutral atomic hydrogen in the sky region 11h&lt;R.A.&lt;16h ; 4{deg}&lt;Dec.&lt;16{deg}; 350&lt;cz&lt;2000km/s using the San Pedro Martir 2m telescope. This survey provides a complete census of the star formation in HI rich galaxies of the local universe. We present the properties of the galaxy sample, together with H{alpha} fluxes and equivalent widths. We find an excellent agreement between the fluxes determined from our images in apertures of 3-arcsec diameter and the fluxes derived from the SDSS spectral database. From the H{alpha} fluxes corrected for galactic and internal extinction and for [NII] contamination we derive the global star formation rates (SFRs).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16#alpha3</TD>
            <TD>2012-12-02T22:38:01Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/545/A16</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/545/A16&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/545/A16</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/427/2047 [1]</TD>
            <TD>Formation of cD Galaxies and their Clusters (Tovmassian+ 2012)</TD>
            <TD>For 128 Abell clusters selected as hosting a cD galaxy as well as having a minimum number of members with measured reshifts, we extracted the K_s_tot magnitude from 2MASS for the cD galaxy and the 2nd-brightest member of the cluster. Depending on the magnitude difference between these two galaxies we subdivide the sample into 71 clusters with a dominant cD (BM I), 22 clusters of intermediate type, and 35 clusters with a non-dominant cD (NBMI). The table contains cluster name, mean redshift, number of members with redshift, difference in K_s_tot magnitude between the cD galaxy and the 2nd-brightest cluster member, the absolute K_s_tot magnitude of the cD galaxy, the Abell count, the cluster velocity dispersion, the peculiar velocity of the cD galaxy, and the names in NED of the cD galaxy and the 2nd-brightest galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047#1</TD>
            <TD>2012-12-30T10:42:39Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/427/2047</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/427/2047</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/427/2047 [2]</TD>
            <TD>Formation of cD Galaxies and their Clusters (Tovmassian+ 2012)</TD>
            <TD>For 128 Abell clusters selected as hosting a cD galaxy as well as having a minimum number of members with measured reshifts, we extracted the K_s_tot magnitude from 2MASS for the cD galaxy and the 2nd-brightest member of the cluster. Depending on the magnitude difference between these two galaxies we subdivide the sample into 71 clusters with a dominant cD (BM I), 22 clusters of intermediate type, and 35 clusters with a non-dominant cD (NBMI). The table contains cluster name, mean redshift, number of members with redshift, difference in K_s_tot magnitude between the cD galaxy and the 2nd-brightest cluster member, the absolute K_s_tot magnitude of the cD galaxy, the Abell count, the cluster velocity dispersion, the peculiar velocity of the cD galaxy, and the names in NED of the cD galaxy and the 2nd-brightest galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047#2</TD>
            <TD>2012-12-30T10:42:39Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/427/2047&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/427/2047</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/427/2047 [table1]</TD>
            <TD>Formation of cD Galaxies and their Clusters (Tovmassian+ 2012)</TD>
            <TD>For 128 Abell clusters selected as hosting a cD galaxy as well as having a minimum number of members with measured reshifts, we extracted the K_s_tot magnitude from 2MASS for the cD galaxy and the 2nd-brightest member of the cluster. Depending on the magnitude difference between these two galaxies we subdivide the sample into 71 clusters with a dominant cD (BM I), 22 clusters of intermediate type, and 35 clusters with a non-dominant cD (NBMI). The table contains cluster name, mean redshift, number of members with redshift, difference in K_s_tot magnitude between the cD galaxy and the 2nd-brightest cluster member, the absolute K_s_tot magnitude of the cD galaxy, the Abell count, the cluster velocity dispersion, the peculiar velocity of the cD galaxy, and the names in NED of the cD galaxy and the 2nd-brightest galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047#table1</TD>
            <TD>2012-12-30T10:42:39Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/427/2047&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/427/2047</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/427/2047 [1]</TD>
            <TD>Formation of cD Galaxies and their Clusters (Tovmassian+ 2012)</TD>
            <TD>For 128 Abell clusters selected as hosting a cD galaxy as well as having a minimum number of members with measured reshifts, we extracted the K_s_tot magnitude from 2MASS for the cD galaxy and the 2nd-brightest member of the cluster. Depending on the magnitude difference between these two galaxies we subdivide the sample into 71 clusters with a dominant cD (BM I), 22 clusters of intermediate type, and 35 clusters with a non-dominant cD (NBMI). The table contains cluster name, mean redshift, number of members with redshift, difference in K_s_tot magnitude between the cD galaxy and the 2nd-brightest cluster member, the absolute K_s_tot magnitude of the cD galaxy, the Abell count, the cluster velocity dispersion, the peculiar velocity of the cD galaxy, and the names in NED of the cD galaxy and the 2nd-brightest galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047#1</TD>
            <TD>2012-12-30T10:42:39Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/427/2047</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/427/2047</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/427/2047 [2]</TD>
            <TD>Formation of cD Galaxies and their Clusters (Tovmassian+ 2012)</TD>
            <TD>For 128 Abell clusters selected as hosting a cD galaxy as well as having a minimum number of members with measured reshifts, we extracted the K_s_tot magnitude from 2MASS for the cD galaxy and the 2nd-brightest member of the cluster. Depending on the magnitude difference between these two galaxies we subdivide the sample into 71 clusters with a dominant cD (BM I), 22 clusters of intermediate type, and 35 clusters with a non-dominant cD (NBMI). The table contains cluster name, mean redshift, number of members with redshift, difference in K_s_tot magnitude between the cD galaxy and the 2nd-brightest cluster member, the absolute K_s_tot magnitude of the cD galaxy, the Abell count, the cluster velocity dispersion, the peculiar velocity of the cD galaxy, and the names in NED of the cD galaxy and the 2nd-brightest galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047#2</TD>
            <TD>2012-12-30T10:42:39Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/427/2047&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/427/2047</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/427/2047 [table1]</TD>
            <TD>Formation of cD Galaxies and their Clusters (Tovmassian+ 2012)</TD>
            <TD>For 128 Abell clusters selected as hosting a cD galaxy as well as having a minimum number of members with measured reshifts, we extracted the K_s_tot magnitude from 2MASS for the cD galaxy and the 2nd-brightest member of the cluster. Depending on the magnitude difference between these two galaxies we subdivide the sample into 71 clusters with a dominant cD (BM I), 22 clusters of intermediate type, and 35 clusters with a non-dominant cD (NBMI). The table contains cluster name, mean redshift, number of members with redshift, difference in K_s_tot magnitude between the cD galaxy and the 2nd-brightest cluster member, the absolute K_s_tot magnitude of the cD galaxy, the Abell count, the cluster velocity dispersion, the peculiar velocity of the cD galaxy, and the names in NED of the cD galaxy and the 2nd-brightest galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047#table1</TD>
            <TD>2012-12-30T10:42:39Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/427/2047&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/427/2047</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/483/826 [1]</TD>
            <TD>BVI CCD photometry of Berkeley 17 (Phelps 1997)</TD>
            <TD>Faint magnitude BVI CCD photometry of the central region of the old open cluster Berkeley 17 (Be 17) has been undertaken to investigate the claim that it is the oldest open cluster yet discovered (Phelps, Janes, &amp; Montgomery, 1994AJ....107.1079P). This study reveals Be 17 to have a metallicity -0.30&lt;=[Fe/H]&lt;=0.00; a reddening 0.52&lt;=E(B-V)&lt;=0.68 or 0.61&lt;=E(V-I)&lt;=0.71; a distance modulus, (m-M)_0_=12.15+/-0.10, corresponding to a distance of 2.7+/-0.1kpc; a diameter of ~10pc; a minimum mass of 400 Msun; and an age of 10-13Gyr. With an adopted age of 12(+1)(-2)Gyr, these results suggest that Be 17 is indeed the oldest open cluster yet discovered. The inferred old age for Be 17 indicates that the cluster is an important one for studies of the differences between open and globular clusters, the transition from the halo/thick disk to the thin disk of the Galaxy, and even for establishing the minimum age of the universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/826#1</TD>
            <TD>2011-09-14T18:41:40Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/826</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/483/826</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/483/826</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/483/826 [2]</TD>
            <TD>BVI CCD photometry of Berkeley 17 (Phelps 1997)</TD>
            <TD>Faint magnitude BVI CCD photometry of the central region of the old open cluster Berkeley 17 (Be 17) has been undertaken to investigate the claim that it is the oldest open cluster yet discovered (Phelps, Janes, &amp; Montgomery, 1994AJ....107.1079P). This study reveals Be 17 to have a metallicity -0.30&lt;=[Fe/H]&lt;=0.00; a reddening 0.52&lt;=E(B-V)&lt;=0.68 or 0.61&lt;=E(V-I)&lt;=0.71; a distance modulus, (m-M)_0_=12.15+/-0.10, corresponding to a distance of 2.7+/-0.1kpc; a diameter of ~10pc; a minimum mass of 400 Msun; and an age of 10-13Gyr. With an adopted age of 12(+1)(-2)Gyr, these results suggest that Be 17 is indeed the oldest open cluster yet discovered. The inferred old age for Be 17 indicates that the cluster is an important one for studies of the differences between open and globular clusters, the transition from the halo/thick disk to the thin disk of the Galaxy, and even for establishing the minimum age of the universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/826#2</TD>
            <TD>2011-09-14T18:41:40Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/483/826</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/483/826&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/483/826</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/427/2047 [1]</TD>
            <TD>Formation of cD Galaxies and their Clusters (Tovmassian+ 2012)</TD>
            <TD>For 128 Abell clusters selected as hosting a cD galaxy as well as having a minimum number of members with measured reshifts, we extracted the K_s_tot magnitude from 2MASS for the cD galaxy and the 2nd-brightest member of the cluster. Depending on the magnitude difference between these two galaxies we subdivide the sample into 71 clusters with a dominant cD (BM I), 22 clusters of intermediate type, and 35 clusters with a non-dominant cD (NBMI). The table contains cluster name, mean redshift, number of members with redshift, difference in K_s_tot magnitude between the cD galaxy and the 2nd-brightest cluster member, the absolute K_s_tot magnitude of the cD galaxy, the Abell count, the cluster velocity dispersion, the peculiar velocity of the cD galaxy, and the names in NED of the cD galaxy and the 2nd-brightest galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047#1</TD>
            <TD>2012-12-30T10:42:39Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/427/2047</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/427/2047</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/427/2047 [2]</TD>
            <TD>Formation of cD Galaxies and their Clusters (Tovmassian+ 2012)</TD>
            <TD>For 128 Abell clusters selected as hosting a cD galaxy as well as having a minimum number of members with measured reshifts, we extracted the K_s_tot magnitude from 2MASS for the cD galaxy and the 2nd-brightest member of the cluster. Depending on the magnitude difference between these two galaxies we subdivide the sample into 71 clusters with a dominant cD (BM I), 22 clusters of intermediate type, and 35 clusters with a non-dominant cD (NBMI). The table contains cluster name, mean redshift, number of members with redshift, difference in K_s_tot magnitude between the cD galaxy and the 2nd-brightest cluster member, the absolute K_s_tot magnitude of the cD galaxy, the Abell count, the cluster velocity dispersion, the peculiar velocity of the cD galaxy, and the names in NED of the cD galaxy and the 2nd-brightest galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047#2</TD>
            <TD>2012-12-30T10:42:39Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/427/2047&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/427/2047</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/427/2047 [table1]</TD>
            <TD>Formation of cD Galaxies and their Clusters (Tovmassian+ 2012)</TD>
            <TD>For 128 Abell clusters selected as hosting a cD galaxy as well as having a minimum number of members with measured reshifts, we extracted the K_s_tot magnitude from 2MASS for the cD galaxy and the 2nd-brightest member of the cluster. Depending on the magnitude difference between these two galaxies we subdivide the sample into 71 clusters with a dominant cD (BM I), 22 clusters of intermediate type, and 35 clusters with a non-dominant cD (NBMI). The table contains cluster name, mean redshift, number of members with redshift, difference in K_s_tot magnitude between the cD galaxy and the 2nd-brightest cluster member, the absolute K_s_tot magnitude of the cD galaxy, the Abell count, the cluster velocity dispersion, the peculiar velocity of the cD galaxy, and the names in NED of the cD galaxy and the 2nd-brightest galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047#table1</TD>
            <TD>2012-12-30T10:42:39Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/427/2047</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/427/2047&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/427/2047</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/548/A129 [1]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#1</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/548/A129</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/548/A129 [2]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#2</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A129 [n6822_0]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#n6822_0</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A129 [n6822_b]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#n6822_b</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A129 [n6822_a]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#n6822_a</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/548/A129 [1]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#1</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/548/A129</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/548/A129 [2]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#2</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A129 [n6822_0]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#n6822_0</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A129 [n6822_b]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#n6822_b</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A129 [n6822_a]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#n6822_a</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/541/A118 [1]</TD>
            <TD>AGN-Host Galaxy Connection (Povic+, 2012)</TD>
            <TD>Table presents the X-ray properties of all 1121 objects, including fluxes in six selected energy bands, and public available optical data for X-ray counterparts. X-ray flux in X/O flux ratio is the sum of fluxes in (0.5-2keV) and (2-4.5keV) bands, while the optical flux corresponds to R band. The represented hardness ratio was set using the same X-ray bands. Photometric redshifts and K-corrections were measured using the photometric information in five optical (Furusawa et al., 2008, Cat. J/ApJS/176/1), three NIR (Hewett et al., 2006MNRAS.367..454H; Hodgkin et al., 2009MNRAS.394..675H), and four MIR IRAC (SWIRE survey) bands. Morphological classification was obtained using the galSVM code (Huertas-Company et al., 2008A&amp;A...478..971H, 2009A&amp;A...497..743H), one of the new methods useful especially when dealing with high-redshift sources and low-resolution data. With galSVM we obtained the mean surface brightness, asymmetry, concentration index, Gini, Smoothness, M20 moment of light, and two probabilities p1 and p2 that the galaxy belongs to early- (E, S0, S0/Sa) or late-type, respectively. Stellarity and elongation parameters were obtained with SExtractor. All objects with stellarity parameter greater or equal to 0.9 were considered as compact in this work. We included in our analysis for early-type objects only those sources with p1 probabilities greater or equal to 0.75, and for late-type objects all sources with probabilities p2 greater than 0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118#1</TD>
            <TD>2012-07-15T21:26:32Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/541/A118</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/541/A118</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/541/A118 [2]</TD>
            <TD>AGN-Host Galaxy Connection (Povic+, 2012)</TD>
            <TD>Table presents the X-ray properties of all 1121 objects, including fluxes in six selected energy bands, and public available optical data for X-ray counterparts. X-ray flux in X/O flux ratio is the sum of fluxes in (0.5-2keV) and (2-4.5keV) bands, while the optical flux corresponds to R band. The represented hardness ratio was set using the same X-ray bands. Photometric redshifts and K-corrections were measured using the photometric information in five optical (Furusawa et al., 2008, Cat. J/ApJS/176/1), three NIR (Hewett et al., 2006MNRAS.367..454H; Hodgkin et al., 2009MNRAS.394..675H), and four MIR IRAC (SWIRE survey) bands. Morphological classification was obtained using the galSVM code (Huertas-Company et al., 2008A&amp;A...478..971H, 2009A&amp;A...497..743H), one of the new methods useful especially when dealing with high-redshift sources and low-resolution data. With galSVM we obtained the mean surface brightness, asymmetry, concentration index, Gini, Smoothness, M20 moment of light, and two probabilities p1 and p2 that the galaxy belongs to early- (E, S0, S0/Sa) or late-type, respectively. Stellarity and elongation parameters were obtained with SExtractor. All objects with stellarity parameter greater or equal to 0.9 were considered as compact in this work. We included in our analysis for early-type objects only those sources with p1 probabilities greater or equal to 0.75, and for late-type objects all sources with probabilities p2 greater than 0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118#2</TD>
            <TD>2012-07-15T21:26:32Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/541/A118&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/541/A118</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/541/A118 [tablea1]</TD>
            <TD>AGN-Host Galaxy Connection (Povic+, 2012)</TD>
            <TD>Table presents the X-ray properties of all 1121 objects, including fluxes in six selected energy bands, and public available optical data for X-ray counterparts. X-ray flux in X/O flux ratio is the sum of fluxes in (0.5-2keV) and (2-4.5keV) bands, while the optical flux corresponds to R band. The represented hardness ratio was set using the same X-ray bands. Photometric redshifts and K-corrections were measured using the photometric information in five optical (Furusawa et al., 2008, Cat. J/ApJS/176/1), three NIR (Hewett et al., 2006MNRAS.367..454H; Hodgkin et al., 2009MNRAS.394..675H), and four MIR IRAC (SWIRE survey) bands. Morphological classification was obtained using the galSVM code (Huertas-Company et al., 2008A&amp;A...478..971H, 2009A&amp;A...497..743H), one of the new methods useful especially when dealing with high-redshift sources and low-resolution data. With galSVM we obtained the mean surface brightness, asymmetry, concentration index, Gini, Smoothness, M20 moment of light, and two probabilities p1 and p2 that the galaxy belongs to early- (E, S0, S0/Sa) or late-type, respectively. Stellarity and elongation parameters were obtained with SExtractor. All objects with stellarity parameter greater or equal to 0.9 were considered as compact in this work. We included in our analysis for early-type objects only those sources with p1 probabilities greater or equal to 0.75, and for late-type objects all sources with probabilities p2 greater than 0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118#tablea1</TD>
            <TD>2012-07-15T21:26:32Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/541/A118&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/541/A118</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [1]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#1</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [2]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#2</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [3]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#3</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [4]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#4</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [5]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#5</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [6]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#6</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [7]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#7</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [8]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#8</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [9]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#9</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR3 [10]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#10</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/DirectCone?DSACAT=UKIDSS_DR3&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [11]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#11</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR3 [12]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#12</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [13]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#13</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [14]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#14</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [15]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#15</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [16]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#16</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [17]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#17</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [18]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#18</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR3 [19]</TD>
            <TD>UKIDSS DR3 - UKIRT Infrared Deep Sky Survey Data Release 3</TD>
            <TD>This DSA hosts data release 3 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from the five UKIDSS surveys: Large Area Survey, Galactic Plane Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey (see the www.ukidss.org for survey descriptions).</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa#19</TD>
            <TD>2012-07-18T12:41:51Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 3</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR3-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR3-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/491/L31 [1]</TD>
            <TD>TMGS star positions (Garzon+ 1997)</TD>
            <TD>We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31#1</TD>
            <TD>2011-09-14T18:41:42Z</TD>
            <TD>#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/491/L31</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/L31</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/491/L31 [2]</TD>
            <TD>TMGS star positions (Garzon+ 1997)</TD>
            <TD>We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31#2</TD>
            <TD>2011-09-14T18:41:42Z</TD>
            <TD>#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/491/L31&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/L31</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/491/L31 [table1]</TD>
            <TD>TMGS star positions (Garzon+ 1997)</TD>
            <TD>We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31#table1</TD>
            <TD>2011-09-14T18:41:42Z</TD>
            <TD>#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/491/L31&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/L31</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/2268 [1]</TD>
            <TD>SAGE calibration stars (Meixner+, 2006)</TD>
            <TD>We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7{deg}x7{deg}) using the IRAC (3.6, 4.5, 5.8, and 8um) and MIPS (24, 70, and 160um) instruments on board the Spitzer Space Telescope in the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, these agents being the interstellar medium (ISM) and stars in the LMC. This paper provides an overview of the SAGE Legacy project, including observing strategy, data processing, and initial results. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability. The SAGE data are nonproprietary. The data processing includes IRAC and MIPS pipelines and a database for mining the point-source catalogs, which will be released to the community in support of Spitzer proposal cycles 4 and 5. We present initial results on the epoch 1 data for a region near N79 and N83. The MIPS 70 and 160um images of the diffuse dust emission of the N79/N83 region reveal a similar distribution to the gas emissions, especially the HI 21cm emission.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268#1</TD>
            <TD>2012-08-15T07:31:42Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/2268</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/2268</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/2268 [2]</TD>
            <TD>SAGE calibration stars (Meixner+, 2006)</TD>
            <TD>We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7{deg}x7{deg}) using the IRAC (3.6, 4.5, 5.8, and 8um) and MIPS (24, 70, and 160um) instruments on board the Spitzer Space Telescope in the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, these agents being the interstellar medium (ISM) and stars in the LMC. This paper provides an overview of the SAGE Legacy project, including observing strategy, data processing, and initial results. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability. The SAGE data are nonproprietary. The data processing includes IRAC and MIPS pipelines and a database for mining the point-source catalogs, which will be released to the community in support of Spitzer proposal cycles 4 and 5. We present initial results on the epoch 1 data for a region near N79 and N83. The MIPS 70 and 160um images of the diffuse dust emission of the N79/N83 region reveal a similar distribution to the gas emissions, especially the HI 21cm emission.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268#2</TD>
            <TD>2012-08-15T07:31:42Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/2268&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/2268</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/2268 [table3]</TD>
            <TD>SAGE calibration stars (Meixner+, 2006)</TD>
            <TD>We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7{deg}x7{deg}) using the IRAC (3.6, 4.5, 5.8, and 8um) and MIPS (24, 70, and 160um) instruments on board the Spitzer Space Telescope in the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, these agents being the interstellar medium (ISM) and stars in the LMC. This paper provides an overview of the SAGE Legacy project, including observing strategy, data processing, and initial results. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability. The SAGE data are nonproprietary. The data processing includes IRAC and MIPS pipelines and a database for mining the point-source catalogs, which will be released to the community in support of Spitzer proposal cycles 4 and 5. We present initial results on the epoch 1 data for a region near N79 and N83. The MIPS 70 and 160um images of the diffuse dust emission of the N79/N83 region reveal a similar distribution to the gas emissions, especially the HI 21cm emission.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268#table3</TD>
            <TD>2012-08-15T07:31:42Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/2268&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/2268</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/548/A129 [1]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#1</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/548/A129</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/548/A129 [2]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#2</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A129 [n6822_0]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#n6822_0</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A129 [n6822_b]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#n6822_b</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A129 [n6822_a]</TD>
            <TD>HST photometry in NGC 6822 (Fusco+, 2012)</TD>
            <TD>We performed HST photometry on three fields in the south-east region of NGC 6822 galaxy. The resulting catalogues contain ~140,000, ~42,000, ~12,000 stars, from the innermost to the outermost field. Data were calibrated using the VEGAMAG system. Data are stored in three files, one for each field: central field: n6822_0.dat middle field: n6822_a.dat outer field: n6822_b.dat</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129#n6822_a</TD>
            <TD>2012-12-06T07:54:24Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A129</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/491/L31 [1]</TD>
            <TD>TMGS star positions (Garzon+ 1997)</TD>
            <TD>We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31#1</TD>
            <TD>2011-09-14T18:41:42Z</TD>
            <TD>#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/491/L31</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/L31</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/491/L31 [2]</TD>
            <TD>TMGS star positions (Garzon+ 1997)</TD>
            <TD>We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31#2</TD>
            <TD>2011-09-14T18:41:42Z</TD>
            <TD>#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/491/L31&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/L31</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/491/L31 [table1]</TD>
            <TD>TMGS star positions (Garzon+ 1997)</TD>
            <TD>We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31#table1</TD>
            <TD>2011-09-14T18:41:42Z</TD>
            <TD>#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/491/L31&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/L31</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/491/L31 [1]</TD>
            <TD>TMGS star positions (Garzon+ 1997)</TD>
            <TD>We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31#1</TD>
            <TD>2011-09-14T18:41:42Z</TD>
            <TD>#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/491/L31</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/L31</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/491/L31 [2]</TD>
            <TD>TMGS star positions (Garzon+ 1997)</TD>
            <TD>We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31#2</TD>
            <TD>2011-09-14T18:41:42Z</TD>
            <TD>#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/491/L31&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/L31</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/491/L31 [table1]</TD>
            <TD>TMGS star positions (Garzon+ 1997)</TD>
            <TD>We present an analysis of the optical spectroscopy of 58 stars in the Galactic plane at l=27deg, where a prominent excess in the flux distribution and star counts have been observed in several spectral regions, in particular in the Two-Micron Galactic Survey (TMGS) catalog. The sources were selected from the TMGS to have a K magnitude brighter than +5mag and to be within 2deg of the Galactic plane. More than 60% of the spectra correspond to stars of luminosity class I, and a significant proportion of the remainder are very late and fast-evolving giants. This very high concentration of young sources points to the existence of a major star formation region in the Galactic plane, located just inside the assumed origin of the Scutum spiral arm. Such regions can form because of the concentrations of shocked gas where a galactic bar meets a spiral arm, as is observed at the ends of the bars of face-on external galaxies. Thus, the presence of a massive star formation region is very strong supporting evidence for the presence of a bar in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31#table1</TD>
            <TD>2011-09-14T18:41:42Z</TD>
            <TD>#Positional_Data#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/L31</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/491/L31&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/L31</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/541/A118 [1]</TD>
            <TD>AGN-Host Galaxy Connection (Povic+, 2012)</TD>
            <TD>Table presents the X-ray properties of all 1121 objects, including fluxes in six selected energy bands, and public available optical data for X-ray counterparts. X-ray flux in X/O flux ratio is the sum of fluxes in (0.5-2keV) and (2-4.5keV) bands, while the optical flux corresponds to R band. The represented hardness ratio was set using the same X-ray bands. Photometric redshifts and K-corrections were measured using the photometric information in five optical (Furusawa et al., 2008, Cat. J/ApJS/176/1), three NIR (Hewett et al., 2006MNRAS.367..454H; Hodgkin et al., 2009MNRAS.394..675H), and four MIR IRAC (SWIRE survey) bands. Morphological classification was obtained using the galSVM code (Huertas-Company et al., 2008A&amp;A...478..971H, 2009A&amp;A...497..743H), one of the new methods useful especially when dealing with high-redshift sources and low-resolution data. With galSVM we obtained the mean surface brightness, asymmetry, concentration index, Gini, Smoothness, M20 moment of light, and two probabilities p1 and p2 that the galaxy belongs to early- (E, S0, S0/Sa) or late-type, respectively. Stellarity and elongation parameters were obtained with SExtractor. All objects with stellarity parameter greater or equal to 0.9 were considered as compact in this work. We included in our analysis for early-type objects only those sources with p1 probabilities greater or equal to 0.75, and for late-type objects all sources with probabilities p2 greater than 0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118#1</TD>
            <TD>2012-07-15T21:26:32Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/541/A118</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/541/A118</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/541/A118 [2]</TD>
            <TD>AGN-Host Galaxy Connection (Povic+, 2012)</TD>
            <TD>Table presents the X-ray properties of all 1121 objects, including fluxes in six selected energy bands, and public available optical data for X-ray counterparts. X-ray flux in X/O flux ratio is the sum of fluxes in (0.5-2keV) and (2-4.5keV) bands, while the optical flux corresponds to R band. The represented hardness ratio was set using the same X-ray bands. Photometric redshifts and K-corrections were measured using the photometric information in five optical (Furusawa et al., 2008, Cat. J/ApJS/176/1), three NIR (Hewett et al., 2006MNRAS.367..454H; Hodgkin et al., 2009MNRAS.394..675H), and four MIR IRAC (SWIRE survey) bands. Morphological classification was obtained using the galSVM code (Huertas-Company et al., 2008A&amp;A...478..971H, 2009A&amp;A...497..743H), one of the new methods useful especially when dealing with high-redshift sources and low-resolution data. With galSVM we obtained the mean surface brightness, asymmetry, concentration index, Gini, Smoothness, M20 moment of light, and two probabilities p1 and p2 that the galaxy belongs to early- (E, S0, S0/Sa) or late-type, respectively. Stellarity and elongation parameters were obtained with SExtractor. All objects with stellarity parameter greater or equal to 0.9 were considered as compact in this work. We included in our analysis for early-type objects only those sources with p1 probabilities greater or equal to 0.75, and for late-type objects all sources with probabilities p2 greater than 0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118#2</TD>
            <TD>2012-07-15T21:26:32Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/541/A118&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/541/A118</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/541/A118 [tablea1]</TD>
            <TD>AGN-Host Galaxy Connection (Povic+, 2012)</TD>
            <TD>Table presents the X-ray properties of all 1121 objects, including fluxes in six selected energy bands, and public available optical data for X-ray counterparts. X-ray flux in X/O flux ratio is the sum of fluxes in (0.5-2keV) and (2-4.5keV) bands, while the optical flux corresponds to R band. The represented hardness ratio was set using the same X-ray bands. Photometric redshifts and K-corrections were measured using the photometric information in five optical (Furusawa et al., 2008, Cat. J/ApJS/176/1), three NIR (Hewett et al., 2006MNRAS.367..454H; Hodgkin et al., 2009MNRAS.394..675H), and four MIR IRAC (SWIRE survey) bands. Morphological classification was obtained using the galSVM code (Huertas-Company et al., 2008A&amp;A...478..971H, 2009A&amp;A...497..743H), one of the new methods useful especially when dealing with high-redshift sources and low-resolution data. With galSVM we obtained the mean surface brightness, asymmetry, concentration index, Gini, Smoothness, M20 moment of light, and two probabilities p1 and p2 that the galaxy belongs to early- (E, S0, S0/Sa) or late-type, respectively. Stellarity and elongation parameters were obtained with SExtractor. All objects with stellarity parameter greater or equal to 0.9 were considered as compact in this work. We included in our analysis for early-type objects only those sources with p1 probabilities greater or equal to 0.75, and for late-type objects all sources with probabilities p2 greater than 0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118#tablea1</TD>
            <TD>2012-07-15T21:26:32Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/541/A118&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/541/A118</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/455 [1]</TD>
            <TD>Dwarf galaxy candidates around interacting galaxies (Deeg+ 1998)</TD>
            <TD>The tables list positions, sizes and photometry in V and R band of extended objects found in fields, which include a nearby interacting galaxy. The tables' filenames are a combination of the table number and the interacting galaxy's name. The column-descriptions of all tables are identical, expect that the positional offsets refer to different reference positions in each table, given in Note (2). These reference positions are in the center of the interacting galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/455#1</TD>
            <TD>2011-09-14T18:42:29Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/455 [2]</TD>
            <TD>Dwarf galaxy candidates around interacting galaxies (Deeg+ 1998)</TD>
            <TD>The tables list positions, sizes and photometry in V and R band of extended objects found in fields, which include a nearby interacting galaxy. The tables' filenames are a combination of the table number and the interacting galaxy's name. The column-descriptions of all tables are identical, expect that the positional offsets refer to different reference positions in each table, given in Note (2). These reference positions are in the center of the interacting galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/455#2</TD>
            <TD>2011-09-14T18:42:29Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ARXA [1]</TD>
            <TD>Atlas of Radio/X-Ray Associations (ARXA)</TD>
            <TD>The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: &lt;pre&gt; Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. &lt;/pre&gt; Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt;). Questions or comments on ARXA may be directed to eric@flesch.org. See also: &lt;pre&gt; APM home page &lt;a href="http://www.ast.cam.ac.uk/~apmcat"&gt;http://www.ast.cam.ac.uk/~apmcat&lt;/a&gt; USNO-A home page &lt;a href="http://www.nofs.navy.mil/"&gt;http://www.nofs.navy.mil/&lt;/a&gt; NVSS home page &lt;a href="http://www.cv.nrao.edu/nvss/"&gt;http://www.cv.nrao.edu/nvss/&lt;/a&gt; FIRST home page &lt;a href="http://sundog.stsci.edu/"&gt;http://sundog.stsci.edu/&lt;/a&gt; SUMSS home page &lt;a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html"&gt;http://www.astrop.physics.usyd.edu.au/SUMSS/index.html&lt;/a&gt; XMM-Newton home page &lt;a href="http://xmmssc-www.star.le.ac.uk"&gt;http://xmmssc-www.star.le.ac.uk&lt;/a&gt; HRI &amp; PSPC home page &lt;a href="http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php"&gt;http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php&lt;/a&gt; WGA home page &lt;a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html"&gt;http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html&lt;/a&gt; RASS-FSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc&lt;/a&gt; RASS-BSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc&lt;/a&gt; Chandra home page &lt;a href="http://chandra.harvard.edu"&gt;http://chandra.harvard.edu&lt;/a&gt; XAssist home page &lt;a href="http://xassist.pha.jhu.edu/zope/xassist"&gt;http://xassist.pha.jhu.edu/zope/xassist&lt;/a&gt; (XMMX &amp; CXOX sources are from XAssist) &lt;/pre&gt; If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arxa#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arxa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=arxa&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/arxa.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ARXA [2]</TD>
            <TD>Atlas of Radio/X-Ray Associations (ARXA)</TD>
            <TD>The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: &lt;pre&gt; Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. &lt;/pre&gt; Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt;). Questions or comments on ARXA may be directed to eric@flesch.org. See also: &lt;pre&gt; APM home page &lt;a href="http://www.ast.cam.ac.uk/~apmcat"&gt;http://www.ast.cam.ac.uk/~apmcat&lt;/a&gt; USNO-A home page &lt;a href="http://www.nofs.navy.mil/"&gt;http://www.nofs.navy.mil/&lt;/a&gt; NVSS home page &lt;a href="http://www.cv.nrao.edu/nvss/"&gt;http://www.cv.nrao.edu/nvss/&lt;/a&gt; FIRST home page &lt;a href="http://sundog.stsci.edu/"&gt;http://sundog.stsci.edu/&lt;/a&gt; SUMSS home page &lt;a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html"&gt;http://www.astrop.physics.usyd.edu.au/SUMSS/index.html&lt;/a&gt; XMM-Newton home page &lt;a href="http://xmmssc-www.star.le.ac.uk"&gt;http://xmmssc-www.star.le.ac.uk&lt;/a&gt; HRI &amp; PSPC home page &lt;a href="http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php"&gt;http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php&lt;/a&gt; WGA home page &lt;a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html"&gt;http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html&lt;/a&gt; RASS-FSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc&lt;/a&gt; RASS-BSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc&lt;/a&gt; Chandra home page &lt;a href="http://chandra.harvard.edu"&gt;http://chandra.harvard.edu&lt;/a&gt; XAssist home page &lt;a href="http://xassist.pha.jhu.edu/zope/xassist"&gt;http://xassist.pha.jhu.edu/zope/xassist&lt;/a&gt; (XMMX &amp; CXOX sources are from XAssist) &lt;/pre&gt; If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arxa#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arxa</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=arxa&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/arxa.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ARXA [3]</TD>
            <TD>Atlas of Radio/X-Ray Associations (ARXA)</TD>
            <TD>The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: &lt;pre&gt; Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. &lt;/pre&gt; Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt;). Questions or comments on ARXA may be directed to eric@flesch.org. See also: &lt;pre&gt; APM home page &lt;a href="http://www.ast.cam.ac.uk/~apmcat"&gt;http://www.ast.cam.ac.uk/~apmcat&lt;/a&gt; USNO-A home page &lt;a href="http://www.nofs.navy.mil/"&gt;http://www.nofs.navy.mil/&lt;/a&gt; NVSS home page &lt;a href="http://www.cv.nrao.edu/nvss/"&gt;http://www.cv.nrao.edu/nvss/&lt;/a&gt; FIRST home page &lt;a href="http://sundog.stsci.edu/"&gt;http://sundog.stsci.edu/&lt;/a&gt; SUMSS home page &lt;a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html"&gt;http://www.astrop.physics.usyd.edu.au/SUMSS/index.html&lt;/a&gt; XMM-Newton home page &lt;a href="http://xmmssc-www.star.le.ac.uk"&gt;http://xmmssc-www.star.le.ac.uk&lt;/a&gt; HRI &amp; PSPC home page &lt;a href="http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php"&gt;http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php&lt;/a&gt; WGA home page &lt;a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html"&gt;http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html&lt;/a&gt; RASS-FSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc&lt;/a&gt; RASS-BSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc&lt;/a&gt; Chandra home page &lt;a href="http://chandra.harvard.edu"&gt;http://chandra.harvard.edu&lt;/a&gt; XAssist home page &lt;a href="http://xassist.pha.jhu.edu/zope/xassist"&gt;http://xassist.pha.jhu.edu/zope/xassist&lt;/a&gt; (XMMX &amp; CXOX sources are from XAssist) &lt;/pre&gt; If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arxa#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arxa</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_arxa&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/arxa.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/541/A118 [1]</TD>
            <TD>AGN-Host Galaxy Connection (Povic+, 2012)</TD>
            <TD>Table presents the X-ray properties of all 1121 objects, including fluxes in six selected energy bands, and public available optical data for X-ray counterparts. X-ray flux in X/O flux ratio is the sum of fluxes in (0.5-2keV) and (2-4.5keV) bands, while the optical flux corresponds to R band. The represented hardness ratio was set using the same X-ray bands. Photometric redshifts and K-corrections were measured using the photometric information in five optical (Furusawa et al., 2008, Cat. J/ApJS/176/1), three NIR (Hewett et al., 2006MNRAS.367..454H; Hodgkin et al., 2009MNRAS.394..675H), and four MIR IRAC (SWIRE survey) bands. Morphological classification was obtained using the galSVM code (Huertas-Company et al., 2008A&amp;A...478..971H, 2009A&amp;A...497..743H), one of the new methods useful especially when dealing with high-redshift sources and low-resolution data. With galSVM we obtained the mean surface brightness, asymmetry, concentration index, Gini, Smoothness, M20 moment of light, and two probabilities p1 and p2 that the galaxy belongs to early- (E, S0, S0/Sa) or late-type, respectively. Stellarity and elongation parameters were obtained with SExtractor. All objects with stellarity parameter greater or equal to 0.9 were considered as compact in this work. We included in our analysis for early-type objects only those sources with p1 probabilities greater or equal to 0.75, and for late-type objects all sources with probabilities p2 greater than 0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118#1</TD>
            <TD>2012-07-15T21:26:32Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/541/A118</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/541/A118</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/541/A118 [2]</TD>
            <TD>AGN-Host Galaxy Connection (Povic+, 2012)</TD>
            <TD>Table presents the X-ray properties of all 1121 objects, including fluxes in six selected energy bands, and public available optical data for X-ray counterparts. X-ray flux in X/O flux ratio is the sum of fluxes in (0.5-2keV) and (2-4.5keV) bands, while the optical flux corresponds to R band. The represented hardness ratio was set using the same X-ray bands. Photometric redshifts and K-corrections were measured using the photometric information in five optical (Furusawa et al., 2008, Cat. J/ApJS/176/1), three NIR (Hewett et al., 2006MNRAS.367..454H; Hodgkin et al., 2009MNRAS.394..675H), and four MIR IRAC (SWIRE survey) bands. Morphological classification was obtained using the galSVM code (Huertas-Company et al., 2008A&amp;A...478..971H, 2009A&amp;A...497..743H), one of the new methods useful especially when dealing with high-redshift sources and low-resolution data. With galSVM we obtained the mean surface brightness, asymmetry, concentration index, Gini, Smoothness, M20 moment of light, and two probabilities p1 and p2 that the galaxy belongs to early- (E, S0, S0/Sa) or late-type, respectively. Stellarity and elongation parameters were obtained with SExtractor. All objects with stellarity parameter greater or equal to 0.9 were considered as compact in this work. We included in our analysis for early-type objects only those sources with p1 probabilities greater or equal to 0.75, and for late-type objects all sources with probabilities p2 greater than 0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118#2</TD>
            <TD>2012-07-15T21:26:32Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/541/A118&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/541/A118</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/541/A118 [tablea1]</TD>
            <TD>AGN-Host Galaxy Connection (Povic+, 2012)</TD>
            <TD>Table presents the X-ray properties of all 1121 objects, including fluxes in six selected energy bands, and public available optical data for X-ray counterparts. X-ray flux in X/O flux ratio is the sum of fluxes in (0.5-2keV) and (2-4.5keV) bands, while the optical flux corresponds to R band. The represented hardness ratio was set using the same X-ray bands. Photometric redshifts and K-corrections were measured using the photometric information in five optical (Furusawa et al., 2008, Cat. J/ApJS/176/1), three NIR (Hewett et al., 2006MNRAS.367..454H; Hodgkin et al., 2009MNRAS.394..675H), and four MIR IRAC (SWIRE survey) bands. Morphological classification was obtained using the galSVM code (Huertas-Company et al., 2008A&amp;A...478..971H, 2009A&amp;A...497..743H), one of the new methods useful especially when dealing with high-redshift sources and low-resolution data. With galSVM we obtained the mean surface brightness, asymmetry, concentration index, Gini, Smoothness, M20 moment of light, and two probabilities p1 and p2 that the galaxy belongs to early- (E, S0, S0/Sa) or late-type, respectively. Stellarity and elongation parameters were obtained with SExtractor. All objects with stellarity parameter greater or equal to 0.9 were considered as compact in this work. We included in our analysis for early-type objects only those sources with p1 probabilities greater or equal to 0.75, and for late-type objects all sources with probabilities p2 greater than 0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118#tablea1</TD>
            <TD>2012-07-15T21:26:32Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/541/A118</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/541/A118&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/541/A118</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/455 [1]</TD>
            <TD>Dwarf galaxy candidates around interacting galaxies (Deeg+ 1998)</TD>
            <TD>The tables list positions, sizes and photometry in V and R band of extended objects found in fields, which include a nearby interacting galaxy. The tables' filenames are a combination of the table number and the interacting galaxy's name. The column-descriptions of all tables are identical, expect that the positional offsets refer to different reference positions in each table, given in Note (2). These reference positions are in the center of the interacting galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/455#1</TD>
            <TD>2011-09-14T18:42:29Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/455 [2]</TD>
            <TD>Dwarf galaxy candidates around interacting galaxies (Deeg+ 1998)</TD>
            <TD>The tables list positions, sizes and photometry in V and R band of extended objects found in fields, which include a nearby interacting galaxy. The tables' filenames are a combination of the table number and the interacting galaxy's name. The column-descriptions of all tables are identical, expect that the positional offsets refer to different reference positions in each table, given in Note (2). These reference positions are in the center of the interacting galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/455#2</TD>
            <TD>2011-09-14T18:42:29Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/455</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ARXA [1]</TD>
            <TD>Atlas of Radio/X-Ray Associations (ARXA)</TD>
            <TD>The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: &lt;pre&gt; Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. &lt;/pre&gt; Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt;). Questions or comments on ARXA may be directed to eric@flesch.org. See also: &lt;pre&gt; APM home page &lt;a href="http://www.ast.cam.ac.uk/~apmcat"&gt;http://www.ast.cam.ac.uk/~apmcat&lt;/a&gt; USNO-A home page &lt;a href="http://www.nofs.navy.mil/"&gt;http://www.nofs.navy.mil/&lt;/a&gt; NVSS home page &lt;a href="http://www.cv.nrao.edu/nvss/"&gt;http://www.cv.nrao.edu/nvss/&lt;/a&gt; FIRST home page &lt;a href="http://sundog.stsci.edu/"&gt;http://sundog.stsci.edu/&lt;/a&gt; SUMSS home page &lt;a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html"&gt;http://www.astrop.physics.usyd.edu.au/SUMSS/index.html&lt;/a&gt; XMM-Newton home page &lt;a href="http://xmmssc-www.star.le.ac.uk"&gt;http://xmmssc-www.star.le.ac.uk&lt;/a&gt; HRI &amp; PSPC home page &lt;a href="http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php"&gt;http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php&lt;/a&gt; WGA home page &lt;a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html"&gt;http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html&lt;/a&gt; RASS-FSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc&lt;/a&gt; RASS-BSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc&lt;/a&gt; Chandra home page &lt;a href="http://chandra.harvard.edu"&gt;http://chandra.harvard.edu&lt;/a&gt; XAssist home page &lt;a href="http://xassist.pha.jhu.edu/zope/xassist"&gt;http://xassist.pha.jhu.edu/zope/xassist&lt;/a&gt; (XMMX &amp; CXOX sources are from XAssist) &lt;/pre&gt; If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arxa#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arxa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=arxa&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/arxa.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ARXA [2]</TD>
            <TD>Atlas of Radio/X-Ray Associations (ARXA)</TD>
            <TD>The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: &lt;pre&gt; Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. &lt;/pre&gt; Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt;). Questions or comments on ARXA may be directed to eric@flesch.org. See also: &lt;pre&gt; APM home page &lt;a href="http://www.ast.cam.ac.uk/~apmcat"&gt;http://www.ast.cam.ac.uk/~apmcat&lt;/a&gt; USNO-A home page &lt;a href="http://www.nofs.navy.mil/"&gt;http://www.nofs.navy.mil/&lt;/a&gt; NVSS home page &lt;a href="http://www.cv.nrao.edu/nvss/"&gt;http://www.cv.nrao.edu/nvss/&lt;/a&gt; FIRST home page &lt;a href="http://sundog.stsci.edu/"&gt;http://sundog.stsci.edu/&lt;/a&gt; SUMSS home page &lt;a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html"&gt;http://www.astrop.physics.usyd.edu.au/SUMSS/index.html&lt;/a&gt; XMM-Newton home page &lt;a href="http://xmmssc-www.star.le.ac.uk"&gt;http://xmmssc-www.star.le.ac.uk&lt;/a&gt; HRI &amp; PSPC home page &lt;a href="http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php"&gt;http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php&lt;/a&gt; WGA home page &lt;a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html"&gt;http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html&lt;/a&gt; RASS-FSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc&lt;/a&gt; RASS-BSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc&lt;/a&gt; Chandra home page &lt;a href="http://chandra.harvard.edu"&gt;http://chandra.harvard.edu&lt;/a&gt; XAssist home page &lt;a href="http://xassist.pha.jhu.edu/zope/xassist"&gt;http://xassist.pha.jhu.edu/zope/xassist&lt;/a&gt; (XMMX &amp; CXOX sources are from XAssist) &lt;/pre&gt; If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arxa#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arxa</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=arxa&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/arxa.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ARXA [3]</TD>
            <TD>Atlas of Radio/X-Ray Associations (ARXA)</TD>
            <TD>The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: &lt;pre&gt; Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. &lt;/pre&gt; Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt;). Questions or comments on ARXA may be directed to eric@flesch.org. See also: &lt;pre&gt; APM home page &lt;a href="http://www.ast.cam.ac.uk/~apmcat"&gt;http://www.ast.cam.ac.uk/~apmcat&lt;/a&gt; USNO-A home page &lt;a href="http://www.nofs.navy.mil/"&gt;http://www.nofs.navy.mil/&lt;/a&gt; NVSS home page &lt;a href="http://www.cv.nrao.edu/nvss/"&gt;http://www.cv.nrao.edu/nvss/&lt;/a&gt; FIRST home page &lt;a href="http://sundog.stsci.edu/"&gt;http://sundog.stsci.edu/&lt;/a&gt; SUMSS home page &lt;a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html"&gt;http://www.astrop.physics.usyd.edu.au/SUMSS/index.html&lt;/a&gt; XMM-Newton home page &lt;a href="http://xmmssc-www.star.le.ac.uk"&gt;http://xmmssc-www.star.le.ac.uk&lt;/a&gt; HRI &amp; PSPC home page &lt;a href="http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php"&gt;http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php&lt;/a&gt; WGA home page &lt;a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html"&gt;http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html&lt;/a&gt; RASS-FSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc&lt;/a&gt; RASS-BSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc&lt;/a&gt; Chandra home page &lt;a href="http://chandra.harvard.edu"&gt;http://chandra.harvard.edu&lt;/a&gt; XAssist home page &lt;a href="http://xassist.pha.jhu.edu/zope/xassist"&gt;http://xassist.pha.jhu.edu/zope/xassist&lt;/a&gt; (XMMX &amp; CXOX sources are from XAssist) &lt;/pre&gt; If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arxa#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arxa</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_arxa&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/arxa.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ARXA [1]</TD>
            <TD>Atlas of Radio/X-Ray Associations (ARXA)</TD>
            <TD>The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: &lt;pre&gt; Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. &lt;/pre&gt; Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt;). Questions or comments on ARXA may be directed to eric@flesch.org. See also: &lt;pre&gt; APM home page &lt;a href="http://www.ast.cam.ac.uk/~apmcat"&gt;http://www.ast.cam.ac.uk/~apmcat&lt;/a&gt; USNO-A home page &lt;a href="http://www.nofs.navy.mil/"&gt;http://www.nofs.navy.mil/&lt;/a&gt; NVSS home page &lt;a href="http://www.cv.nrao.edu/nvss/"&gt;http://www.cv.nrao.edu/nvss/&lt;/a&gt; FIRST home page &lt;a href="http://sundog.stsci.edu/"&gt;http://sundog.stsci.edu/&lt;/a&gt; SUMSS home page &lt;a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html"&gt;http://www.astrop.physics.usyd.edu.au/SUMSS/index.html&lt;/a&gt; XMM-Newton home page &lt;a href="http://xmmssc-www.star.le.ac.uk"&gt;http://xmmssc-www.star.le.ac.uk&lt;/a&gt; HRI &amp; PSPC home page &lt;a href="http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php"&gt;http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php&lt;/a&gt; WGA home page &lt;a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html"&gt;http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html&lt;/a&gt; RASS-FSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc&lt;/a&gt; RASS-BSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc&lt;/a&gt; Chandra home page &lt;a href="http://chandra.harvard.edu"&gt;http://chandra.harvard.edu&lt;/a&gt; XAssist home page &lt;a href="http://xassist.pha.jhu.edu/zope/xassist"&gt;http://xassist.pha.jhu.edu/zope/xassist&lt;/a&gt; (XMMX &amp; CXOX sources are from XAssist) &lt;/pre&gt; If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arxa#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arxa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=arxa&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/arxa.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ARXA [2]</TD>
            <TD>Atlas of Radio/X-Ray Associations (ARXA)</TD>
            <TD>The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: &lt;pre&gt; Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. &lt;/pre&gt; Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt;). Questions or comments on ARXA may be directed to eric@flesch.org. See also: &lt;pre&gt; APM home page &lt;a href="http://www.ast.cam.ac.uk/~apmcat"&gt;http://www.ast.cam.ac.uk/~apmcat&lt;/a&gt; USNO-A home page &lt;a href="http://www.nofs.navy.mil/"&gt;http://www.nofs.navy.mil/&lt;/a&gt; NVSS home page &lt;a href="http://www.cv.nrao.edu/nvss/"&gt;http://www.cv.nrao.edu/nvss/&lt;/a&gt; FIRST home page &lt;a href="http://sundog.stsci.edu/"&gt;http://sundog.stsci.edu/&lt;/a&gt; SUMSS home page &lt;a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html"&gt;http://www.astrop.physics.usyd.edu.au/SUMSS/index.html&lt;/a&gt; XMM-Newton home page &lt;a href="http://xmmssc-www.star.le.ac.uk"&gt;http://xmmssc-www.star.le.ac.uk&lt;/a&gt; HRI &amp; PSPC home page &lt;a href="http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php"&gt;http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php&lt;/a&gt; WGA home page &lt;a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html"&gt;http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html&lt;/a&gt; RASS-FSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc&lt;/a&gt; RASS-BSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc&lt;/a&gt; Chandra home page &lt;a href="http://chandra.harvard.edu"&gt;http://chandra.harvard.edu&lt;/a&gt; XAssist home page &lt;a href="http://xassist.pha.jhu.edu/zope/xassist"&gt;http://xassist.pha.jhu.edu/zope/xassist&lt;/a&gt; (XMMX &amp; CXOX sources are from XAssist) &lt;/pre&gt; If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arxa#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arxa</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=arxa&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/arxa.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ARXA [3]</TD>
            <TD>Atlas of Radio/X-Ray Associations (ARXA)</TD>
            <TD>The Atlas of Radio/X-Ray Associations (ARXA) is a compendium of all cataloged or APM/USNO-A optical objects which are found to be associated with XMM-Newton, Chandra, RASS, HRI, PSPC or WGACAT X-ray detections, or with NVSS, FIRST or SUMSS radio detections. All detections are listed, plus double radio lobes where found. The source number counts are: &lt;pre&gt; Optical objects - 602,570. NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778. Chandra associations - 32,951. ROSAT RASS - 47,486. ROSAT HRI - 15,523. ROSAT PSPC - 35,607. WGA - 24,226. &lt;/pre&gt; Each optical object is given as one entry in this catalog, containing the sky coordinates, the object name (from the literature where available), APM and USNO-A sourced red and blue photometry, redshift, the source catalogs for the name and redshift, the calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. This catalog supersedes the previous similar compilation by the same author, the Quasars.org (QORG) Catalog, called QORGCAT in the HEASARC's Browse (see &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt;). Questions or comments on ARXA may be directed to eric@flesch.org. See also: &lt;pre&gt; APM home page &lt;a href="http://www.ast.cam.ac.uk/~apmcat"&gt;http://www.ast.cam.ac.uk/~apmcat&lt;/a&gt; USNO-A home page &lt;a href="http://www.nofs.navy.mil/"&gt;http://www.nofs.navy.mil/&lt;/a&gt; NVSS home page &lt;a href="http://www.cv.nrao.edu/nvss/"&gt;http://www.cv.nrao.edu/nvss/&lt;/a&gt; FIRST home page &lt;a href="http://sundog.stsci.edu/"&gt;http://sundog.stsci.edu/&lt;/a&gt; SUMSS home page &lt;a href="http://www.astrop.physics.usyd.edu.au/SUMSS/index.html"&gt;http://www.astrop.physics.usyd.edu.au/SUMSS/index.html&lt;/a&gt; XMM-Newton home page &lt;a href="http://xmmssc-www.star.le.ac.uk"&gt;http://xmmssc-www.star.le.ac.uk&lt;/a&gt; HRI &amp; PSPC home page &lt;a href="http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php"&gt;http://www.mpe.mpg.de/xray/wave/rosat/rra/index.php&lt;/a&gt; WGA home page &lt;a href="http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html"&gt;http://wgacat.gsfc.nasa.gov/wgacat/wgacat.html&lt;/a&gt; RASS-FSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-fsc&lt;/a&gt; RASS-BSC home page &lt;a href="http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc"&gt;http://www.xray.mpe.mpg.de/rosat/survey/rass-bsc&lt;/a&gt; Chandra home page &lt;a href="http://chandra.harvard.edu"&gt;http://chandra.harvard.edu&lt;/a&gt; XAssist home page &lt;a href="http://xassist.pha.jhu.edu/zope/xassist"&gt;http://xassist.pha.jhu.edu/zope/xassist&lt;/a&gt; (XMMX &amp; CXOX sources are from XAssist) &lt;/pre&gt; If using this catalog in published research, please add a small mention in the acknowledgements. This table is based on research which made use of the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with NASA.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arxa#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arxa</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_arxa&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/arxa.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/113/905 [1]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#1</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/113/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/113/905 [2]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#2</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/113/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/113/905 [table3]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#table3</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/113/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/113/905 [table2]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#table2</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/113/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/113/905 [table1]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#table1</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/113/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>BAXGalClus [1]</TD>
            <TD>BAX X-Ray Galaxy Clusters and Groups Catalog</TD>
            <TD>This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt; for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt;) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/baxgalclus#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/baxgalclus</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=baxgalclus&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/baxgalclus.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>BAXGalClus [2]</TD>
            <TD>BAX X-Ray Galaxy Clusters and Groups Catalog</TD>
            <TD>This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt; for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt;) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/baxgalclus#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/baxgalclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=baxgalclus&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/baxgalclus.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>BAXGalClus [3]</TD>
            <TD>BAX X-Ray Galaxy Clusters and Groups Catalog</TD>
            <TD>This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt; for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt;) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/baxgalclus#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/baxgalclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_baxgalclus&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/baxgalclus.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/113/905 [1]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#1</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/113/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/113/905 [2]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#2</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/113/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/113/905 [table3]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#table3</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/113/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/113/905 [table2]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#table2</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/113/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/113/905 [table1]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#table1</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/113/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>BAXGalClus [1]</TD>
            <TD>BAX X-Ray Galaxy Clusters and Groups Catalog</TD>
            <TD>This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt; for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt;) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/baxgalclus#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/baxgalclus</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=baxgalclus&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/baxgalclus.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>BAXGalClus [2]</TD>
            <TD>BAX X-Ray Galaxy Clusters and Groups Catalog</TD>
            <TD>This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt; for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt;) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/baxgalclus#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/baxgalclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=baxgalclus&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/baxgalclus.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>BAXGalClus [3]</TD>
            <TD>BAX X-Ray Galaxy Clusters and Groups Catalog</TD>
            <TD>This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt; for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt;) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/baxgalclus#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/baxgalclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_baxgalclus&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/baxgalclus.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/113/905 [1]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#1</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/113/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/113/905 [2]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#2</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/113/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/113/905 [table3]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#table3</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/113/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/113/905 [table2]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#table2</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/113/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/113/905 [table1]</TD>
            <TD>HI observations of galaxies (Pantoja+ 1997)</TD>
            <TD>We present H I 21-cm line observations of 543 galaxies at low galactic latitude in the Galactic Anticenter region of the Zone of Avoidance (4h&lt;={alpha}&lt;=8h, 0{deg}=&lt;{delta}=&lt;37{deg}). The sample comprises 147 catalogued objects (from UGC, CGCG, MCG, and IRAS) still missing a redshift measurement and a list of 369 objects selected from an extensive optical compilation of galaxy candidates in this area. The spectra were acquired using the 305-m Arecibo telescope and cover a velocity range from -350 to +13800km/s at a resolution of about 16km/s. 196 galaxies were detected,59 of the catalogued ones and 137 from the optical compilation. The H I derived properties are presented, as is a discussion regarding the redshift distribution in this region. Our data seem to be consistent with a link across the Zone of Avoidance between the Pisces-Perseus supercluster and Abell 569.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905#table1</TD>
            <TD>2011-09-14T18:43:18Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/113/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>BAXGalClus [1]</TD>
            <TD>BAX X-Ray Galaxy Clusters and Groups Catalog</TD>
            <TD>This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt; for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt;) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/baxgalclus#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/baxgalclus</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=baxgalclus&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/baxgalclus.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>BAXGalClus [2]</TD>
            <TD>BAX X-Ray Galaxy Clusters and Groups Catalog</TD>
            <TD>This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt; for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt;) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/baxgalclus#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/baxgalclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=baxgalclus&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/baxgalclus.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>BAXGalClus [3]</TD>
            <TD>BAX X-Ray Galaxy Clusters and Groups Catalog</TD>
            <TD>This table contains the BAX X-Ray Galaxy Clusters and Groups Catalog. BAX (`Base de Donnees Amas de Galaxies X': see &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt; for more details) is a multi-wavelength database dedicated to X-ray clusters and groups of galaxies which allows detailed information retrieval. BAX is designed to support astronomical research by providing access to published measurements of the main physical quantities and to the related bibliographic references: basic data stored in the database are cluster/group identifiers, equatorial coordinates, redshift, flux, X-ray luminosity (in the ROSAT band) and temperature, and (in the online version at &lt;a href="http://bax.ast.obs-mip.fr/"&gt;http://bax.ast.obs-mip.fr/&lt;/a&gt;) links to additional linked parameters (in X-rays, such as spatial profile parameters, as well as SZ parameters of the hot gas, lensing measurements, and data at other wavelengths, such as the optical and radio bands). The clusters and groups in the online BAX database can be queried by the basic parameters as well as the linked parameters or combinations of these. The authors expect BAX to become an important tool for the astronomical community. BAX will optimize various aspects of the scientific analysis of X-ray clusters and groups of galaxies, from proposal planning to data collection, interpretation and publication, from both ground based facilities like MEGACAM (CFHT), VIRMOS (VLT) and from space missions like XMM-Newton, Chandra and Planck.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/baxgalclus#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/baxgalclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_baxgalclus&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/baxgalclus.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/2268 [1]</TD>
            <TD>SAGE calibration stars (Meixner+, 2006)</TD>
            <TD>We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7{deg}x7{deg}) using the IRAC (3.6, 4.5, 5.8, and 8um) and MIPS (24, 70, and 160um) instruments on board the Spitzer Space Telescope in the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, these agents being the interstellar medium (ISM) and stars in the LMC. This paper provides an overview of the SAGE Legacy project, including observing strategy, data processing, and initial results. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability. The SAGE data are nonproprietary. The data processing includes IRAC and MIPS pipelines and a database for mining the point-source catalogs, which will be released to the community in support of Spitzer proposal cycles 4 and 5. We present initial results on the epoch 1 data for a region near N79 and N83. The MIPS 70 and 160um images of the diffuse dust emission of the N79/N83 region reveal a similar distribution to the gas emissions, especially the HI 21cm emission.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268#1</TD>
            <TD>2012-08-15T07:31:42Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/2268</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/2268</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/2268 [2]</TD>
            <TD>SAGE calibration stars (Meixner+, 2006)</TD>
            <TD>We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7{deg}x7{deg}) using the IRAC (3.6, 4.5, 5.8, and 8um) and MIPS (24, 70, and 160um) instruments on board the Spitzer Space Telescope in the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, these agents being the interstellar medium (ISM) and stars in the LMC. This paper provides an overview of the SAGE Legacy project, including observing strategy, data processing, and initial results. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability. The SAGE data are nonproprietary. The data processing includes IRAC and MIPS pipelines and a database for mining the point-source catalogs, which will be released to the community in support of Spitzer proposal cycles 4 and 5. We present initial results on the epoch 1 data for a region near N79 and N83. The MIPS 70 and 160um images of the diffuse dust emission of the N79/N83 region reveal a similar distribution to the gas emissions, especially the HI 21cm emission.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268#2</TD>
            <TD>2012-08-15T07:31:42Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/2268&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/2268</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/2268 [table3]</TD>
            <TD>SAGE calibration stars (Meixner+, 2006)</TD>
            <TD>We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7{deg}x7{deg}) using the IRAC (3.6, 4.5, 5.8, and 8um) and MIPS (24, 70, and 160um) instruments on board the Spitzer Space Telescope in the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, these agents being the interstellar medium (ISM) and stars in the LMC. This paper provides an overview of the SAGE Legacy project, including observing strategy, data processing, and initial results. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability. The SAGE data are nonproprietary. The data processing includes IRAC and MIPS pipelines and a database for mining the point-source catalogs, which will be released to the community in support of Spitzer proposal cycles 4 and 5. We present initial results on the epoch 1 data for a region near N79 and N83. The MIPS 70 and 160um images of the diffuse dust emission of the N79/N83 region reveal a similar distribution to the gas emissions, especially the HI 21cm emission.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268#table3</TD>
            <TD>2012-08-15T07:31:42Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/2268&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/2268</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/334/609 [1]</TD>
            <TD>Carbon stars IR photometry (Guglielmo+ 1998)</TD>
            <TD>We present JHKL photometry of a sample of 150 IRAS stars in the third and fourth galactic quadrant with |b|&lt;2{deg} selected according to their IRAS colour (0.160&lt;=[12-25]&lt;=1.156). We identify 27 carbon star candidates using the [12-25] vs. K-L two-colour diagram method. Among them, 10 are listed in the Stephenson's catalogue of carbon stars and 17 are new infrared carbon stars (IRCS) candidates. Their distances are found to be larger than 3kpc. These data are combined with previous data to study the space distribution of IRCS. The number density seems to be independent of the galactocentric distance (R) toward the Galactic Center and to decrease exponentially toward the anticenter. At the present stage, it is not possible to disentangle effects such as incompleteness of the sample, different space distribution law and dependence of the luminosity on metallicity. In particular, we suggest that the apparent scarcity of IRCS in the central direction of the Galaxy (R&lt;5kpc) might be due to a selection effect. From the available data, we have found no IRCS within 1kpc of the Galactic Center.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/334/609#1</TD>
            <TD>2011-09-14T18:43:47Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/334/609</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/334/609</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/334/609</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/334/609 [2]</TD>
            <TD>Carbon stars IR photometry (Guglielmo+ 1998)</TD>
            <TD>We present JHKL photometry of a sample of 150 IRAS stars in the third and fourth galactic quadrant with |b|&lt;2{deg} selected according to their IRAS colour (0.160&lt;=[12-25]&lt;=1.156). We identify 27 carbon star candidates using the [12-25] vs. K-L two-colour diagram method. Among them, 10 are listed in the Stephenson's catalogue of carbon stars and 17 are new infrared carbon stars (IRCS) candidates. Their distances are found to be larger than 3kpc. These data are combined with previous data to study the space distribution of IRCS. The number density seems to be independent of the galactocentric distance (R) toward the Galactic Center and to decrease exponentially toward the anticenter. At the present stage, it is not possible to disentangle effects such as incompleteness of the sample, different space distribution law and dependence of the luminosity on metallicity. In particular, we suggest that the apparent scarcity of IRCS in the central direction of the Galaxy (R&lt;5kpc) might be due to a selection effect. From the available data, we have found no IRCS within 1kpc of the Galactic Center.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/334/609#2</TD>
            <TD>2011-09-14T18:43:47Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/334/609</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/334/609&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/334/609</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHESSCAT [1]</TD>
            <TD>ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog</TD>
            <TD>The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L_X-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L_H-alpha/L_bol. The quantities L_H-alpha/L_bol and L_X/L_bol are linearly related below L_X/L_bol ~ 3 x 10&lt;sup&gt;-4&lt;/sup&gt;, while L_H-alpha/L_bol appears to turn over at larger L_X/L_bol values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chesscat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chesscat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chesscat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chesscat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHESSCAT [2]</TD>
            <TD>ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog</TD>
            <TD>The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L_X-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L_H-alpha/L_bol. The quantities L_H-alpha/L_bol and L_X/L_bol are linearly related below L_X/L_bol ~ 3 x 10&lt;sup&gt;-4&lt;/sup&gt;, while L_H-alpha/L_bol appears to turn over at larger L_X/L_bol values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chesscat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chesscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chesscat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chesscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHESSCAT [3]</TD>
            <TD>ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog</TD>
            <TD>The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L_X-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L_H-alpha/L_bol. The quantities L_H-alpha/L_bol and L_X/L_bol are linearly related below L_X/L_bol ~ 3 x 10&lt;sup&gt;-4&lt;/sup&gt;, while L_H-alpha/L_bol appears to turn over at larger L_X/L_bol values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chesscat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chesscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chesscat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chesscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/334/609 [1]</TD>
            <TD>Carbon stars IR photometry (Guglielmo+ 1998)</TD>
            <TD>We present JHKL photometry of a sample of 150 IRAS stars in the third and fourth galactic quadrant with |b|&lt;2{deg} selected according to their IRAS colour (0.160&lt;=[12-25]&lt;=1.156). We identify 27 carbon star candidates using the [12-25] vs. K-L two-colour diagram method. Among them, 10 are listed in the Stephenson's catalogue of carbon stars and 17 are new infrared carbon stars (IRCS) candidates. Their distances are found to be larger than 3kpc. These data are combined with previous data to study the space distribution of IRCS. The number density seems to be independent of the galactocentric distance (R) toward the Galactic Center and to decrease exponentially toward the anticenter. At the present stage, it is not possible to disentangle effects such as incompleteness of the sample, different space distribution law and dependence of the luminosity on metallicity. In particular, we suggest that the apparent scarcity of IRCS in the central direction of the Galaxy (R&lt;5kpc) might be due to a selection effect. From the available data, we have found no IRCS within 1kpc of the Galactic Center.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/334/609#1</TD>
            <TD>2011-09-14T18:43:47Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/334/609</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/334/609</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/334/609</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/334/609 [2]</TD>
            <TD>Carbon stars IR photometry (Guglielmo+ 1998)</TD>
            <TD>We present JHKL photometry of a sample of 150 IRAS stars in the third and fourth galactic quadrant with |b|&lt;2{deg} selected according to their IRAS colour (0.160&lt;=[12-25]&lt;=1.156). We identify 27 carbon star candidates using the [12-25] vs. K-L two-colour diagram method. Among them, 10 are listed in the Stephenson's catalogue of carbon stars and 17 are new infrared carbon stars (IRCS) candidates. Their distances are found to be larger than 3kpc. These data are combined with previous data to study the space distribution of IRCS. The number density seems to be independent of the galactocentric distance (R) toward the Galactic Center and to decrease exponentially toward the anticenter. At the present stage, it is not possible to disentangle effects such as incompleteness of the sample, different space distribution law and dependence of the luminosity on metallicity. In particular, we suggest that the apparent scarcity of IRCS in the central direction of the Galaxy (R&lt;5kpc) might be due to a selection effect. From the available data, we have found no IRCS within 1kpc of the Galactic Center.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/334/609#2</TD>
            <TD>2011-09-14T18:43:47Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/334/609</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/334/609&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/334/609</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHESSCAT [1]</TD>
            <TD>ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog</TD>
            <TD>The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L_X-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L_H-alpha/L_bol. The quantities L_H-alpha/L_bol and L_X/L_bol are linearly related below L_X/L_bol ~ 3 x 10&lt;sup&gt;-4&lt;/sup&gt;, while L_H-alpha/L_bol appears to turn over at larger L_X/L_bol values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chesscat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chesscat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chesscat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chesscat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHESSCAT [2]</TD>
            <TD>ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog</TD>
            <TD>The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L_X-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L_H-alpha/L_bol. The quantities L_H-alpha/L_bol and L_X/L_bol are linearly related below L_X/L_bol ~ 3 x 10&lt;sup&gt;-4&lt;/sup&gt;, while L_H-alpha/L_bol appears to turn over at larger L_X/L_bol values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chesscat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chesscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chesscat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chesscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHESSCAT [3]</TD>
            <TD>ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog</TD>
            <TD>The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L_X-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L_H-alpha/L_bol. The quantities L_H-alpha/L_bol and L_X/L_bol are linearly related below L_X/L_bol ~ 3 x 10&lt;sup&gt;-4&lt;/sup&gt;, while L_H-alpha/L_bol appears to turn over at larger L_X/L_bol values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chesscat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chesscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chesscat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chesscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/2268 [1]</TD>
            <TD>SAGE calibration stars (Meixner+, 2006)</TD>
            <TD>We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7{deg}x7{deg}) using the IRAC (3.6, 4.5, 5.8, and 8um) and MIPS (24, 70, and 160um) instruments on board the Spitzer Space Telescope in the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, these agents being the interstellar medium (ISM) and stars in the LMC. This paper provides an overview of the SAGE Legacy project, including observing strategy, data processing, and initial results. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability. The SAGE data are nonproprietary. The data processing includes IRAC and MIPS pipelines and a database for mining the point-source catalogs, which will be released to the community in support of Spitzer proposal cycles 4 and 5. We present initial results on the epoch 1 data for a region near N79 and N83. The MIPS 70 and 160um images of the diffuse dust emission of the N79/N83 region reveal a similar distribution to the gas emissions, especially the HI 21cm emission.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268#1</TD>
            <TD>2012-08-15T07:31:42Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/2268</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/2268</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/2268 [2]</TD>
            <TD>SAGE calibration stars (Meixner+, 2006)</TD>
            <TD>We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7{deg}x7{deg}) using the IRAC (3.6, 4.5, 5.8, and 8um) and MIPS (24, 70, and 160um) instruments on board the Spitzer Space Telescope in the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, these agents being the interstellar medium (ISM) and stars in the LMC. This paper provides an overview of the SAGE Legacy project, including observing strategy, data processing, and initial results. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability. The SAGE data are nonproprietary. The data processing includes IRAC and MIPS pipelines and a database for mining the point-source catalogs, which will be released to the community in support of Spitzer proposal cycles 4 and 5. We present initial results on the epoch 1 data for a region near N79 and N83. The MIPS 70 and 160um images of the diffuse dust emission of the N79/N83 region reveal a similar distribution to the gas emissions, especially the HI 21cm emission.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268#2</TD>
            <TD>2012-08-15T07:31:42Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/2268&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/2268</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/2268 [table3]</TD>
            <TD>SAGE calibration stars (Meixner+, 2006)</TD>
            <TD>We are performing a uniform and unbiased imaging survey of the Large Magellanic Cloud (LMC; ~7{deg}x7{deg}) using the IRAC (3.6, 4.5, 5.8, and 8um) and MIPS (24, 70, and 160um) instruments on board the Spitzer Space Telescope in the Surveying the Agents of a Galaxy's Evolution (SAGE) survey, these agents being the interstellar medium (ISM) and stars in the LMC. This paper provides an overview of the SAGE Legacy project, including observing strategy, data processing, and initial results. The observing strategy includes two epochs in 2005, separated by 3 months, that both mitigate instrumental artifacts and constrain source variability. The SAGE data are nonproprietary. The data processing includes IRAC and MIPS pipelines and a database for mining the point-source catalogs, which will be released to the community in support of Spitzer proposal cycles 4 and 5. We present initial results on the epoch 1 data for a region near N79 and N83. The MIPS 70 and 160um images of the diffuse dust emission of the N79/N83 region reveal a similar distribution to the gas emissions, especially the HI 21cm emission.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268#table3</TD>
            <TD>2012-08-15T07:31:42Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/2268</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/2268&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/2268</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHESSCAT [1]</TD>
            <TD>ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog</TD>
            <TD>The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L_X-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L_H-alpha/L_bol. The quantities L_H-alpha/L_bol and L_X/L_bol are linearly related below L_X/L_bol ~ 3 x 10&lt;sup&gt;-4&lt;/sup&gt;, while L_H-alpha/L_bol appears to turn over at larger L_X/L_bol values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chesscat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chesscat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chesscat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chesscat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHESSCAT [2]</TD>
            <TD>ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog</TD>
            <TD>The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L_X-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L_H-alpha/L_bol. The quantities L_H-alpha/L_bol and L_X/L_bol are linearly related below L_X/L_bol ~ 3 x 10&lt;sup&gt;-4&lt;/sup&gt;, while L_H-alpha/L_bol appears to turn over at larger L_X/L_bol values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chesscat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chesscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chesscat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chesscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHESSCAT [3]</TD>
            <TD>ChaMP Extended Stellar Survey (ChESS) X-Ray Catalog</TD>
            <TD>The ChaMP Extended Stellar Survey (ChESS) X-ray catalog contains 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS). The authors used morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create this catalog, from a sample of 2121 matched ChaMP/SDSS sources. Their cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in their final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. New spectral classifications and H-alpha measurements are presented for an additional 79 stars. The catalog is dominated by main-sequence stars; the authors estimate the fraction of giants in ChESS to be ~10%. They identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. They derive distances from ~10 to 2000 pc for the stars in the catalog using photometric parallax relations appropriate for dwarfs on the main sequence and calculate their X-ray and bolometric luminosities. These stars lie in a unique space in the L_X-distance plane, filling the gap between the nearby stars identified as counterparts to sources in the ROSAT All Sky Survey and the more distant stars detected in deep Chandra and XMM-Newton surveys. For 36 newly identified X-ray-emitting M stars, the authors calculated L_H-alpha/L_bol. The quantities L_H-alpha/L_bol and L_X/L_bol are linearly related below L_X/L_bol ~ 3 x 10&lt;sup&gt;-4&lt;/sup&gt;, while L_H-alpha/L_bol appears to turn over at larger L_X/L_bol values. Stars with reliable SDSS photometry have an ~0.1 mag blue excess in u-g, likely due to increased chromospheric continuum emission. Photometric metallicity estimates suggest that the sample is evenly split between the young and old disk populations of the Galaxy; the lowest activity sources belong to the old disk population, a clear signature of the decay of magnetic activity with age.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chesscat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chesscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chesscat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chesscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/95/401 [1]</TD>
            <TD>Clusters of galaxies position angles (Plionis 1994)</TD>
            <TD>The position angles of a large number of Abell and Shectman clusters, identified in the Lick map as surface galaxy-density enhancements, are estimated. I determine the major axis orientation of a total of 637 clusters, of which 448 are Shectman clusters (202 of which are also Abell clusters) and 189 are Abell clusters not originally detected by Shectman due to his adopted density threshold. Using published redshifts for 277 of these clusters I have detected strong nearest neighbor alignments over scales up to ~15h^-1^Mpc at a&gt;~2.5-3{sigma} significance level, while quite weak alignments are detected even up to ~60h^-1^Mpc. A more significant alignment signal (~4{sigma}) is detected among all neighbors residing in superclusters and having separations &lt;~ 10h^-1^Mpc. Again, weaker but significant alignments are found when larger separations are considered. Since my cluster sample is neither volume limited nor redshift complete (which would have tended to wash out any real alignment signal), the alignments detected should reflect a real and possibly a stronger underline effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/401#1</TD>
            <TD>2011-09-14T18:44:17Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/95/401</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/95/401</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/95/401 [2]</TD>
            <TD>Clusters of galaxies position angles (Plionis 1994)</TD>
            <TD>The position angles of a large number of Abell and Shectman clusters, identified in the Lick map as surface galaxy-density enhancements, are estimated. I determine the major axis orientation of a total of 637 clusters, of which 448 are Shectman clusters (202 of which are also Abell clusters) and 189 are Abell clusters not originally detected by Shectman due to his adopted density threshold. Using published redshifts for 277 of these clusters I have detected strong nearest neighbor alignments over scales up to ~15h^-1^Mpc at a&gt;~2.5-3{sigma} significance level, while quite weak alignments are detected even up to ~60h^-1^Mpc. A more significant alignment signal (~4{sigma}) is detected among all neighbors residing in superclusters and having separations &lt;~ 10h^-1^Mpc. Again, weaker but significant alignments are found when larger separations are considered. Since my cluster sample is neither volume limited nor redshift complete (which would have tended to wash out any real alignment signal), the alignments detected should reflect a real and possibly a stronger underline effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/401#2</TD>
            <TD>2011-09-14T18:44:17Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/95/401&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/95/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ELAISS1OID [1]</TD>
            <TD>ELAIS S1 Field X-Ray Source Optical/IR Identifications Catalog</TD>
            <TD>This table contains the optical identifications and a multi-band catalog of a sample of 478 X-ray sources detected in the XMM-Newton and Chandra surveys of the central 0.6 deg&lt;sup&gt;2&lt;/sup&gt; of the ELAIS-S1 field. The most likely optical/infrared counterpart of each X-ray source was identified using the chance coincidence probability in the R and IRAC 3.6 micron bands.This method was complemented by the precise positions obtained through Chandra observations. The authors were able to associate a counterpart to each X-ray source in the catalogue. Approximately 94% of them are detected in the R band, while the remaining are blank fields in the optical down to R ~ 24.5, but have a near-infrared counterpart detected by IRAC within 6 arcsec of the XMM-Newton centroid. The multi-band catalog, produced using the positions of the identified optical counterparts, contains photometry in ten photometric bands, from B to the MIPS 24 micron band. The spectroscopic follow-up allowed us to determine the redshift and classification for 237 sources (~ 50% of the sample) brighter than R = 24. The spectroscopic redshifts were complemented by reliable photometric redshifts for 68 sources. The authors classified 47% of the sources with spectroscopic redshift as broad-line active galactic nuclei (BL AGNs) with z = 0.1-3.5, while sources without broad-lines (NOT BL AGNs) are about 46% of the spectroscopic sample and are found up to z = 2.6. The remaining fraction is represented by extended X-ray sources and stars. The authors spectroscopically identified 11 type 2 QSOs among the sources with F(2-10 keV)/F(R) &gt; 8, with redshift between 0.9 and 2.6, high 2-10 keV luminosity (log L(2-10 keV) &gt;= 43.8 erg/s) and hard X-ray colors suggesting large absorbing columns at the rest frame (log N_H up to 23.6 cm&lt;sup&gt;-2&lt;/sup&gt;). BL AGNs show on average blue optical-to-near-infrared colors, softer X-ray colors and X-ray-to-optical colors typical of optically selected AGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray flux ratio and span a wider range of X-ray-to-optical colors. On average the Spectral Energy Distributions (SEDs) of high-luminosity BL AGNs resemble the power-law typical of unobscured AGNs. The SEDs of NOT BLAGNs are dominated by the galaxy emission in the optical/near-infrared, and show a rise in the mid-infrared which suggests the presence of an obscured active nucleus. The authours have used the infrared-to-optical colors and near-infrared SEDs to infer the properties of the AGN host galaxies. Identifications and photometric parameters for 478 sources detected by XMM-Newton in the ELAIS-S1 field are given. For each source, the X-ray positions and fluxes, optical position and photometry, Spitzer IRAC and MIPS 24 micron positions and fluxes, spectroscopic redshift where available, photometric redshift and SED shape classification are given.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiss1oid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiss1oid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=elaiss1oid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/elaiss1oid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ELAISS1OID [2]</TD>
            <TD>ELAIS S1 Field X-Ray Source Optical/IR Identifications Catalog</TD>
            <TD>This table contains the optical identifications and a multi-band catalog of a sample of 478 X-ray sources detected in the XMM-Newton and Chandra surveys of the central 0.6 deg&lt;sup&gt;2&lt;/sup&gt; of the ELAIS-S1 field. The most likely optical/infrared counterpart of each X-ray source was identified using the chance coincidence probability in the R and IRAC 3.6 micron bands.This method was complemented by the precise positions obtained through Chandra observations. The authors were able to associate a counterpart to each X-ray source in the catalogue. Approximately 94% of them are detected in the R band, while the remaining are blank fields in the optical down to R ~ 24.5, but have a near-infrared counterpart detected by IRAC within 6 arcsec of the XMM-Newton centroid. The multi-band catalog, produced using the positions of the identified optical counterparts, contains photometry in ten photometric bands, from B to the MIPS 24 micron band. The spectroscopic follow-up allowed us to determine the redshift and classification for 237 sources (~ 50% of the sample) brighter than R = 24. The spectroscopic redshifts were complemented by reliable photometric redshifts for 68 sources. The authors classified 47% of the sources with spectroscopic redshift as broad-line active galactic nuclei (BL AGNs) with z = 0.1-3.5, while sources without broad-lines (NOT BL AGNs) are about 46% of the spectroscopic sample and are found up to z = 2.6. The remaining fraction is represented by extended X-ray sources and stars. The authors spectroscopically identified 11 type 2 QSOs among the sources with F(2-10 keV)/F(R) &gt; 8, with redshift between 0.9 and 2.6, high 2-10 keV luminosity (log L(2-10 keV) &gt;= 43.8 erg/s) and hard X-ray colors suggesting large absorbing columns at the rest frame (log N_H up to 23.6 cm&lt;sup&gt;-2&lt;/sup&gt;). BL AGNs show on average blue optical-to-near-infrared colors, softer X-ray colors and X-ray-to-optical colors typical of optically selected AGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray flux ratio and span a wider range of X-ray-to-optical colors. On average the Spectral Energy Distributions (SEDs) of high-luminosity BL AGNs resemble the power-law typical of unobscured AGNs. The SEDs of NOT BLAGNs are dominated by the galaxy emission in the optical/near-infrared, and show a rise in the mid-infrared which suggests the presence of an obscured active nucleus. The authours have used the infrared-to-optical colors and near-infrared SEDs to infer the properties of the AGN host galaxies. Identifications and photometric parameters for 478 sources detected by XMM-Newton in the ELAIS-S1 field are given. For each source, the X-ray positions and fluxes, optical position and photometry, Spitzer IRAC and MIPS 24 micron positions and fluxes, spectroscopic redshift where available, photometric redshift and SED shape classification are given.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiss1oid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>ELAISS1OID [3]</TD>
            <TD>ELAIS S1 Field X-Ray Source Optical/IR Identifications Catalog</TD>
            <TD>This table contains the optical identifications and a multi-band catalog of a sample of 478 X-ray sources detected in the XMM-Newton and Chandra surveys of the central 0.6 deg&lt;sup&gt;2&lt;/sup&gt; of the ELAIS-S1 field. The most likely optical/infrared counterpart of each X-ray source was identified using the chance coincidence probability in the R and IRAC 3.6 micron bands.This method was complemented by the precise positions obtained through Chandra observations. The authors were able to associate a counterpart to each X-ray source in the catalogue. Approximately 94% of them are detected in the R band, while the remaining are blank fields in the optical down to R ~ 24.5, but have a near-infrared counterpart detected by IRAC within 6 arcsec of the XMM-Newton centroid. The multi-band catalog, produced using the positions of the identified optical counterparts, contains photometry in ten photometric bands, from B to the MIPS 24 micron band. The spectroscopic follow-up allowed us to determine the redshift and classification for 237 sources (~ 50% of the sample) brighter than R = 24. The spectroscopic redshifts were complemented by reliable photometric redshifts for 68 sources. The authors classified 47% of the sources with spectroscopic redshift as broad-line active galactic nuclei (BL AGNs) with z = 0.1-3.5, while sources without broad-lines (NOT BL AGNs) are about 46% of the spectroscopic sample and are found up to z = 2.6. The remaining fraction is represented by extended X-ray sources and stars. The authors spectroscopically identified 11 type 2 QSOs among the sources with F(2-10 keV)/F(R) &gt; 8, with redshift between 0.9 and 2.6, high 2-10 keV luminosity (log L(2-10 keV) &gt;= 43.8 erg/s) and hard X-ray colors suggesting large absorbing columns at the rest frame (log N_H up to 23.6 cm&lt;sup&gt;-2&lt;/sup&gt;). BL AGNs show on average blue optical-to-near-infrared colors, softer X-ray colors and X-ray-to-optical colors typical of optically selected AGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray flux ratio and span a wider range of X-ray-to-optical colors. On average the Spectral Energy Distributions (SEDs) of high-luminosity BL AGNs resemble the power-law typical of unobscured AGNs. The SEDs of NOT BLAGNs are dominated by the galaxy emission in the optical/near-infrared, and show a rise in the mid-infrared which suggests the presence of an obscured active nucleus. The authours have used the infrared-to-optical colors and near-infrared SEDs to infer the properties of the AGN host galaxies. Identifications and photometric parameters for 478 sources detected by XMM-Newton in the ELAIS-S1 field are given. For each source, the X-ray positions and fluxes, optical position and photometry, Spitzer IRAC and MIPS 24 micron positions and fluxes, spectroscopic redshift where available, photometric redshift and SED shape classification are given.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_elaiss1oid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJS/199/34 [1]</TD>
            <TD>Clusters of galaxies in SDSS-III (Wen+, 2012)</TD>
            <TD>Wen et al. (2009, Cat. J/ApJS/183/197) identified 39668 galaxy clusters from the SDSS DR6 by the discrimination of member galaxies of clusters using photometric redshifts of galaxies. Wen &amp; Han (2011ApJ...734...68W) improved the method and successfully identified the high-redshift clusters from the deep fields of the Canada-France-Hawaii Telescope (CFHT) Wide survey, the CHFT Deep survey, the Cosmic Evolution Survey, and the Spitzer Wide-area InfraRed Extragalactic survey. Here, we follow and improve the algorithm to identify clusters from SDSS-III (SDSS Data Release 8; Aihara et al. 2011ApJS..193...29A, see Cat. II/306).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34#1</TD>
            <TD>2012-08-22T15:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>14-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/34</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/34</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/34 [2]</TD>
            <TD>Clusters of galaxies in SDSS-III (Wen+, 2012)</TD>
            <TD>Wen et al. (2009, Cat. J/ApJS/183/197) identified 39668 galaxy clusters from the SDSS DR6 by the discrimination of member galaxies of clusters using photometric redshifts of galaxies. Wen &amp; Han (2011ApJ...734...68W) improved the method and successfully identified the high-redshift clusters from the deep fields of the Canada-France-Hawaii Telescope (CFHT) Wide survey, the CHFT Deep survey, the Cosmic Evolution Survey, and the Spitzer Wide-area InfraRed Extragalactic survey. Here, we follow and improve the algorithm to identify clusters from SDSS-III (SDSS Data Release 8; Aihara et al. 2011ApJS..193...29A, see Cat. II/306).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34#2</TD>
            <TD>2012-08-22T15:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
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            <TD>#Research#</TD>
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            <TD>14-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34</TD>
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            <TD>J/ApJS/199/34 [table1]</TD>
            <TD>Clusters of galaxies in SDSS-III (Wen+, 2012)</TD>
            <TD>Wen et al. (2009, Cat. J/ApJS/183/197) identified 39668 galaxy clusters from the SDSS DR6 by the discrimination of member galaxies of clusters using photometric redshifts of galaxies. Wen &amp; Han (2011ApJ...734...68W) improved the method and successfully identified the high-redshift clusters from the deep fields of the Canada-France-Hawaii Telescope (CFHT) Wide survey, the CHFT Deep survey, the Cosmic Evolution Survey, and the Spitzer Wide-area InfraRed Extragalactic survey. Here, we follow and improve the algorithm to identify clusters from SDSS-III (SDSS Data Release 8; Aihara et al. 2011ApJS..193...29A, see Cat. II/306).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34#table1</TD>
            <TD>2012-08-22T15:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>14-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/34</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/95/401 [1]</TD>
            <TD>Clusters of galaxies position angles (Plionis 1994)</TD>
            <TD>The position angles of a large number of Abell and Shectman clusters, identified in the Lick map as surface galaxy-density enhancements, are estimated. I determine the major axis orientation of a total of 637 clusters, of which 448 are Shectman clusters (202 of which are also Abell clusters) and 189 are Abell clusters not originally detected by Shectman due to his adopted density threshold. Using published redshifts for 277 of these clusters I have detected strong nearest neighbor alignments over scales up to ~15h^-1^Mpc at a&gt;~2.5-3{sigma} significance level, while quite weak alignments are detected even up to ~60h^-1^Mpc. A more significant alignment signal (~4{sigma}) is detected among all neighbors residing in superclusters and having separations &lt;~ 10h^-1^Mpc. Again, weaker but significant alignments are found when larger separations are considered. Since my cluster sample is neither volume limited nor redshift complete (which would have tended to wash out any real alignment signal), the alignments detected should reflect a real and possibly a stronger underline effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/401#1</TD>
            <TD>2011-09-14T18:44:17Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/401</TD>
            <TD />
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            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/95/401</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/95/401</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/95/401 [2]</TD>
            <TD>Clusters of galaxies position angles (Plionis 1994)</TD>
            <TD>The position angles of a large number of Abell and Shectman clusters, identified in the Lick map as surface galaxy-density enhancements, are estimated. I determine the major axis orientation of a total of 637 clusters, of which 448 are Shectman clusters (202 of which are also Abell clusters) and 189 are Abell clusters not originally detected by Shectman due to his adopted density threshold. Using published redshifts for 277 of these clusters I have detected strong nearest neighbor alignments over scales up to ~15h^-1^Mpc at a&gt;~2.5-3{sigma} significance level, while quite weak alignments are detected even up to ~60h^-1^Mpc. A more significant alignment signal (~4{sigma}) is detected among all neighbors residing in superclusters and having separations &lt;~ 10h^-1^Mpc. Again, weaker but significant alignments are found when larger separations are considered. Since my cluster sample is neither volume limited nor redshift complete (which would have tended to wash out any real alignment signal), the alignments detected should reflect a real and possibly a stronger underline effect.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/401#2</TD>
            <TD>2011-09-14T18:44:17Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/401</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/95/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ELAISS1OID [1]</TD>
            <TD>ELAIS S1 Field X-Ray Source Optical/IR Identifications Catalog</TD>
            <TD>This table contains the optical identifications and a multi-band catalog of a sample of 478 X-ray sources detected in the XMM-Newton and Chandra surveys of the central 0.6 deg&lt;sup&gt;2&lt;/sup&gt; of the ELAIS-S1 field. The most likely optical/infrared counterpart of each X-ray source was identified using the chance coincidence probability in the R and IRAC 3.6 micron bands.This method was complemented by the precise positions obtained through Chandra observations. The authors were able to associate a counterpart to each X-ray source in the catalogue. Approximately 94% of them are detected in the R band, while the remaining are blank fields in the optical down to R ~ 24.5, but have a near-infrared counterpart detected by IRAC within 6 arcsec of the XMM-Newton centroid. The multi-band catalog, produced using the positions of the identified optical counterparts, contains photometry in ten photometric bands, from B to the MIPS 24 micron band. The spectroscopic follow-up allowed us to determine the redshift and classification for 237 sources (~ 50% of the sample) brighter than R = 24. The spectroscopic redshifts were complemented by reliable photometric redshifts for 68 sources. The authors classified 47% of the sources with spectroscopic redshift as broad-line active galactic nuclei (BL AGNs) with z = 0.1-3.5, while sources without broad-lines (NOT BL AGNs) are about 46% of the spectroscopic sample and are found up to z = 2.6. The remaining fraction is represented by extended X-ray sources and stars. The authors spectroscopically identified 11 type 2 QSOs among the sources with F(2-10 keV)/F(R) &gt; 8, with redshift between 0.9 and 2.6, high 2-10 keV luminosity (log L(2-10 keV) &gt;= 43.8 erg/s) and hard X-ray colors suggesting large absorbing columns at the rest frame (log N_H up to 23.6 cm&lt;sup&gt;-2&lt;/sup&gt;). BL AGNs show on average blue optical-to-near-infrared colors, softer X-ray colors and X-ray-to-optical colors typical of optically selected AGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray flux ratio and span a wider range of X-ray-to-optical colors. On average the Spectral Energy Distributions (SEDs) of high-luminosity BL AGNs resemble the power-law typical of unobscured AGNs. The SEDs of NOT BLAGNs are dominated by the galaxy emission in the optical/near-infrared, and show a rise in the mid-infrared which suggests the presence of an obscured active nucleus. The authours have used the infrared-to-optical colors and near-infrared SEDs to infer the properties of the AGN host galaxies. Identifications and photometric parameters for 478 sources detected by XMM-Newton in the ELAIS-S1 field are given. For each source, the X-ray positions and fluxes, optical position and photometry, Spitzer IRAC and MIPS 24 micron positions and fluxes, spectroscopic redshift where available, photometric redshift and SED shape classification are given.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiss1oid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiss1oid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>ELAISS1OID [2]</TD>
            <TD>ELAIS S1 Field X-Ray Source Optical/IR Identifications Catalog</TD>
            <TD>This table contains the optical identifications and a multi-band catalog of a sample of 478 X-ray sources detected in the XMM-Newton and Chandra surveys of the central 0.6 deg&lt;sup&gt;2&lt;/sup&gt; of the ELAIS-S1 field. The most likely optical/infrared counterpart of each X-ray source was identified using the chance coincidence probability in the R and IRAC 3.6 micron bands.This method was complemented by the precise positions obtained through Chandra observations. The authors were able to associate a counterpart to each X-ray source in the catalogue. Approximately 94% of them are detected in the R band, while the remaining are blank fields in the optical down to R ~ 24.5, but have a near-infrared counterpart detected by IRAC within 6 arcsec of the XMM-Newton centroid. The multi-band catalog, produced using the positions of the identified optical counterparts, contains photometry in ten photometric bands, from B to the MIPS 24 micron band. The spectroscopic follow-up allowed us to determine the redshift and classification for 237 sources (~ 50% of the sample) brighter than R = 24. The spectroscopic redshifts were complemented by reliable photometric redshifts for 68 sources. The authors classified 47% of the sources with spectroscopic redshift as broad-line active galactic nuclei (BL AGNs) with z = 0.1-3.5, while sources without broad-lines (NOT BL AGNs) are about 46% of the spectroscopic sample and are found up to z = 2.6. The remaining fraction is represented by extended X-ray sources and stars. The authors spectroscopically identified 11 type 2 QSOs among the sources with F(2-10 keV)/F(R) &gt; 8, with redshift between 0.9 and 2.6, high 2-10 keV luminosity (log L(2-10 keV) &gt;= 43.8 erg/s) and hard X-ray colors suggesting large absorbing columns at the rest frame (log N_H up to 23.6 cm&lt;sup&gt;-2&lt;/sup&gt;). BL AGNs show on average blue optical-to-near-infrared colors, softer X-ray colors and X-ray-to-optical colors typical of optically selected AGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray flux ratio and span a wider range of X-ray-to-optical colors. On average the Spectral Energy Distributions (SEDs) of high-luminosity BL AGNs resemble the power-law typical of unobscured AGNs. The SEDs of NOT BLAGNs are dominated by the galaxy emission in the optical/near-infrared, and show a rise in the mid-infrared which suggests the presence of an obscured active nucleus. The authours have used the infrared-to-optical colors and near-infrared SEDs to infer the properties of the AGN host galaxies. Identifications and photometric parameters for 478 sources detected by XMM-Newton in the ELAIS-S1 field are given. For each source, the X-ray positions and fluxes, optical position and photometry, Spitzer IRAC and MIPS 24 micron positions and fluxes, spectroscopic redshift where available, photometric redshift and SED shape classification are given.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiss1oid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/elaiss1oid</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/elaiss1oid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ELAISS1OID [3]</TD>
            <TD>ELAIS S1 Field X-Ray Source Optical/IR Identifications Catalog</TD>
            <TD>This table contains the optical identifications and a multi-band catalog of a sample of 478 X-ray sources detected in the XMM-Newton and Chandra surveys of the central 0.6 deg&lt;sup&gt;2&lt;/sup&gt; of the ELAIS-S1 field. The most likely optical/infrared counterpart of each X-ray source was identified using the chance coincidence probability in the R and IRAC 3.6 micron bands.This method was complemented by the precise positions obtained through Chandra observations. The authors were able to associate a counterpart to each X-ray source in the catalogue. Approximately 94% of them are detected in the R band, while the remaining are blank fields in the optical down to R ~ 24.5, but have a near-infrared counterpart detected by IRAC within 6 arcsec of the XMM-Newton centroid. The multi-band catalog, produced using the positions of the identified optical counterparts, contains photometry in ten photometric bands, from B to the MIPS 24 micron band. The spectroscopic follow-up allowed us to determine the redshift and classification for 237 sources (~ 50% of the sample) brighter than R = 24. The spectroscopic redshifts were complemented by reliable photometric redshifts for 68 sources. The authors classified 47% of the sources with spectroscopic redshift as broad-line active galactic nuclei (BL AGNs) with z = 0.1-3.5, while sources without broad-lines (NOT BL AGNs) are about 46% of the spectroscopic sample and are found up to z = 2.6. The remaining fraction is represented by extended X-ray sources and stars. The authors spectroscopically identified 11 type 2 QSOs among the sources with F(2-10 keV)/F(R) &gt; 8, with redshift between 0.9 and 2.6, high 2-10 keV luminosity (log L(2-10 keV) &gt;= 43.8 erg/s) and hard X-ray colors suggesting large absorbing columns at the rest frame (log N_H up to 23.6 cm&lt;sup&gt;-2&lt;/sup&gt;). BL AGNs show on average blue optical-to-near-infrared colors, softer X-ray colors and X-ray-to-optical colors typical of optically selected AGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray flux ratio and span a wider range of X-ray-to-optical colors. On average the Spectral Energy Distributions (SEDs) of high-luminosity BL AGNs resemble the power-law typical of unobscured AGNs. The SEDs of NOT BLAGNs are dominated by the galaxy emission in the optical/near-infrared, and show a rise in the mid-infrared which suggests the presence of an obscured active nucleus. The authours have used the infrared-to-optical colors and near-infrared SEDs to infer the properties of the AGN host galaxies. Identifications and photometric parameters for 478 sources detected by XMM-Newton in the ELAIS-S1 field are given. For each source, the X-ray positions and fluxes, optical position and photometry, Spitzer IRAC and MIPS 24 micron positions and fluxes, spectroscopic redshift where available, photometric redshift and SED shape classification are given.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiss1oid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/elaiss1oid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_elaiss1oid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/elaiss1oid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/99/784 [1]</TD>
            <TD>IR photometry of LMC long-period variables (Hughes+ 1990)</TD>
            <TD>Infrared JHK photometry and visual spectra have been obtained for a large sample of long-period variables (LPVs) in the Large Magellanic Cloud (LMC). Various aspects of the asymptotic giant branch (AGB) evolution of LPVs are discussed using these data. The birth/death rate of LPVs of different ages in the LMC is compared with the birth rates of appropriate samples of planetary nebulae clump stars, Cepheids, and OH/IR stars. It appears that there are much fewer large-amplitude LPVs per unit galactic stellar mass in the LMC than in the Galaxy. We suggest that this may be due to the fact that the evolved intermediate-age AGB stars in the LMC often turn into carbon stars, which tend to have smaller pulsation amplitudes than M stars. There is also a major discrepancy between the number of LPVs in the LMC (and in the Galaxy) and the number predicted by the theories of AGB evolution, pulsation, and mass loss. A distance modulus to the LMC of 18.66+0.05 is derived by comparing the LMC LPVs with P~200days with the 47 Tucanae Mira variables in the (K, logP) plane. The (K, logP) relation is also used to examine the tilt of the LMC populations of old and intermediate-age stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/784#1</TD>
            <TD>2011-09-14T18:45:01Z</TD>
            <TD>#Spectral_Classification#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/784</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/99/784</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/784</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/99/784 [2]</TD>
            <TD>IR photometry of LMC long-period variables (Hughes+ 1990)</TD>
            <TD>Infrared JHK photometry and visual spectra have been obtained for a large sample of long-period variables (LPVs) in the Large Magellanic Cloud (LMC). Various aspects of the asymptotic giant branch (AGB) evolution of LPVs are discussed using these data. The birth/death rate of LPVs of different ages in the LMC is compared with the birth rates of appropriate samples of planetary nebulae clump stars, Cepheids, and OH/IR stars. It appears that there are much fewer large-amplitude LPVs per unit galactic stellar mass in the LMC than in the Galaxy. We suggest that this may be due to the fact that the evolved intermediate-age AGB stars in the LMC often turn into carbon stars, which tend to have smaller pulsation amplitudes than M stars. There is also a major discrepancy between the number of LPVs in the LMC (and in the Galaxy) and the number predicted by the theories of AGB evolution, pulsation, and mass loss. A distance modulus to the LMC of 18.66+0.05 is derived by comparing the LMC LPVs with P~200days with the 47 Tucanae Mira variables in the (K, logP) plane. The (K, logP) relation is also used to examine the tilt of the LMC populations of old and intermediate-age stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/784#2</TD>
            <TD>2011-09-14T18:45:01Z</TD>
            <TD>#Spectral_Classification#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/784</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/99/784&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/784</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ELAISS1OID [1]</TD>
            <TD>ELAIS S1 Field X-Ray Source Optical/IR Identifications Catalog</TD>
            <TD>This table contains the optical identifications and a multi-band catalog of a sample of 478 X-ray sources detected in the XMM-Newton and Chandra surveys of the central 0.6 deg&lt;sup&gt;2&lt;/sup&gt; of the ELAIS-S1 field. The most likely optical/infrared counterpart of each X-ray source was identified using the chance coincidence probability in the R and IRAC 3.6 micron bands.This method was complemented by the precise positions obtained through Chandra observations. The authors were able to associate a counterpart to each X-ray source in the catalogue. Approximately 94% of them are detected in the R band, while the remaining are blank fields in the optical down to R ~ 24.5, but have a near-infrared counterpart detected by IRAC within 6 arcsec of the XMM-Newton centroid. The multi-band catalog, produced using the positions of the identified optical counterparts, contains photometry in ten photometric bands, from B to the MIPS 24 micron band. The spectroscopic follow-up allowed us to determine the redshift and classification for 237 sources (~ 50% of the sample) brighter than R = 24. The spectroscopic redshifts were complemented by reliable photometric redshifts for 68 sources. The authors classified 47% of the sources with spectroscopic redshift as broad-line active galactic nuclei (BL AGNs) with z = 0.1-3.5, while sources without broad-lines (NOT BL AGNs) are about 46% of the spectroscopic sample and are found up to z = 2.6. The remaining fraction is represented by extended X-ray sources and stars. The authors spectroscopically identified 11 type 2 QSOs among the sources with F(2-10 keV)/F(R) &gt; 8, with redshift between 0.9 and 2.6, high 2-10 keV luminosity (log L(2-10 keV) &gt;= 43.8 erg/s) and hard X-ray colors suggesting large absorbing columns at the rest frame (log N_H up to 23.6 cm&lt;sup&gt;-2&lt;/sup&gt;). BL AGNs show on average blue optical-to-near-infrared colors, softer X-ray colors and X-ray-to-optical colors typical of optically selected AGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray flux ratio and span a wider range of X-ray-to-optical colors. On average the Spectral Energy Distributions (SEDs) of high-luminosity BL AGNs resemble the power-law typical of unobscured AGNs. The SEDs of NOT BLAGNs are dominated by the galaxy emission in the optical/near-infrared, and show a rise in the mid-infrared which suggests the presence of an obscured active nucleus. The authours have used the infrared-to-optical colors and near-infrared SEDs to infer the properties of the AGN host galaxies. Identifications and photometric parameters for 478 sources detected by XMM-Newton in the ELAIS-S1 field are given. For each source, the X-ray positions and fluxes, optical position and photometry, Spitzer IRAC and MIPS 24 micron positions and fluxes, spectroscopic redshift where available, photometric redshift and SED shape classification are given.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiss1oid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiss1oid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=elaiss1oid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/elaiss1oid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ELAISS1OID [2]</TD>
            <TD>ELAIS S1 Field X-Ray Source Optical/IR Identifications Catalog</TD>
            <TD>This table contains the optical identifications and a multi-band catalog of a sample of 478 X-ray sources detected in the XMM-Newton and Chandra surveys of the central 0.6 deg&lt;sup&gt;2&lt;/sup&gt; of the ELAIS-S1 field. The most likely optical/infrared counterpart of each X-ray source was identified using the chance coincidence probability in the R and IRAC 3.6 micron bands.This method was complemented by the precise positions obtained through Chandra observations. The authors were able to associate a counterpart to each X-ray source in the catalogue. Approximately 94% of them are detected in the R band, while the remaining are blank fields in the optical down to R ~ 24.5, but have a near-infrared counterpart detected by IRAC within 6 arcsec of the XMM-Newton centroid. The multi-band catalog, produced using the positions of the identified optical counterparts, contains photometry in ten photometric bands, from B to the MIPS 24 micron band. The spectroscopic follow-up allowed us to determine the redshift and classification for 237 sources (~ 50% of the sample) brighter than R = 24. The spectroscopic redshifts were complemented by reliable photometric redshifts for 68 sources. The authors classified 47% of the sources with spectroscopic redshift as broad-line active galactic nuclei (BL AGNs) with z = 0.1-3.5, while sources without broad-lines (NOT BL AGNs) are about 46% of the spectroscopic sample and are found up to z = 2.6. The remaining fraction is represented by extended X-ray sources and stars. The authors spectroscopically identified 11 type 2 QSOs among the sources with F(2-10 keV)/F(R) &gt; 8, with redshift between 0.9 and 2.6, high 2-10 keV luminosity (log L(2-10 keV) &gt;= 43.8 erg/s) and hard X-ray colors suggesting large absorbing columns at the rest frame (log N_H up to 23.6 cm&lt;sup&gt;-2&lt;/sup&gt;). BL AGNs show on average blue optical-to-near-infrared colors, softer X-ray colors and X-ray-to-optical colors typical of optically selected AGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray flux ratio and span a wider range of X-ray-to-optical colors. On average the Spectral Energy Distributions (SEDs) of high-luminosity BL AGNs resemble the power-law typical of unobscured AGNs. The SEDs of NOT BLAGNs are dominated by the galaxy emission in the optical/near-infrared, and show a rise in the mid-infrared which suggests the presence of an obscured active nucleus. The authours have used the infrared-to-optical colors and near-infrared SEDs to infer the properties of the AGN host galaxies. Identifications and photometric parameters for 478 sources detected by XMM-Newton in the ELAIS-S1 field are given. For each source, the X-ray positions and fluxes, optical position and photometry, Spitzer IRAC and MIPS 24 micron positions and fluxes, spectroscopic redshift where available, photometric redshift and SED shape classification are given.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiss1oid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiss1oid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=elaiss1oid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/elaiss1oid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ELAISS1OID [3]</TD>
            <TD>ELAIS S1 Field X-Ray Source Optical/IR Identifications Catalog</TD>
            <TD>This table contains the optical identifications and a multi-band catalog of a sample of 478 X-ray sources detected in the XMM-Newton and Chandra surveys of the central 0.6 deg&lt;sup&gt;2&lt;/sup&gt; of the ELAIS-S1 field. The most likely optical/infrared counterpart of each X-ray source was identified using the chance coincidence probability in the R and IRAC 3.6 micron bands.This method was complemented by the precise positions obtained through Chandra observations. The authors were able to associate a counterpart to each X-ray source in the catalogue. Approximately 94% of them are detected in the R band, while the remaining are blank fields in the optical down to R ~ 24.5, but have a near-infrared counterpart detected by IRAC within 6 arcsec of the XMM-Newton centroid. The multi-band catalog, produced using the positions of the identified optical counterparts, contains photometry in ten photometric bands, from B to the MIPS 24 micron band. The spectroscopic follow-up allowed us to determine the redshift and classification for 237 sources (~ 50% of the sample) brighter than R = 24. The spectroscopic redshifts were complemented by reliable photometric redshifts for 68 sources. The authors classified 47% of the sources with spectroscopic redshift as broad-line active galactic nuclei (BL AGNs) with z = 0.1-3.5, while sources without broad-lines (NOT BL AGNs) are about 46% of the spectroscopic sample and are found up to z = 2.6. The remaining fraction is represented by extended X-ray sources and stars. The authors spectroscopically identified 11 type 2 QSOs among the sources with F(2-10 keV)/F(R) &gt; 8, with redshift between 0.9 and 2.6, high 2-10 keV luminosity (log L(2-10 keV) &gt;= 43.8 erg/s) and hard X-ray colors suggesting large absorbing columns at the rest frame (log N_H up to 23.6 cm&lt;sup&gt;-2&lt;/sup&gt;). BL AGNs show on average blue optical-to-near-infrared colors, softer X-ray colors and X-ray-to-optical colors typical of optically selected AGNs. Conversely, narrow-line sources show redder optical colors, harder X-ray flux ratio and span a wider range of X-ray-to-optical colors. On average the Spectral Energy Distributions (SEDs) of high-luminosity BL AGNs resemble the power-law typical of unobscured AGNs. The SEDs of NOT BLAGNs are dominated by the galaxy emission in the optical/near-infrared, and show a rise in the mid-infrared which suggests the presence of an obscured active nucleus. The authours have used the infrared-to-optical colors and near-infrared SEDs to infer the properties of the AGN host galaxies. Identifications and photometric parameters for 478 sources detected by XMM-Newton in the ELAIS-S1 field are given. For each source, the X-ray positions and fluxes, optical position and photometry, Spitzer IRAC and MIPS 24 micron positions and fluxes, spectroscopic redshift where available, photometric redshift and SED shape classification are given.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiss1oid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiss1oid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_elaiss1oid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/elaiss1oid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/99/784 [1]</TD>
            <TD>IR photometry of LMC long-period variables (Hughes+ 1990)</TD>
            <TD>Infrared JHK photometry and visual spectra have been obtained for a large sample of long-period variables (LPVs) in the Large Magellanic Cloud (LMC). Various aspects of the asymptotic giant branch (AGB) evolution of LPVs are discussed using these data. The birth/death rate of LPVs of different ages in the LMC is compared with the birth rates of appropriate samples of planetary nebulae clump stars, Cepheids, and OH/IR stars. It appears that there are much fewer large-amplitude LPVs per unit galactic stellar mass in the LMC than in the Galaxy. We suggest that this may be due to the fact that the evolved intermediate-age AGB stars in the LMC often turn into carbon stars, which tend to have smaller pulsation amplitudes than M stars. There is also a major discrepancy between the number of LPVs in the LMC (and in the Galaxy) and the number predicted by the theories of AGB evolution, pulsation, and mass loss. A distance modulus to the LMC of 18.66+0.05 is derived by comparing the LMC LPVs with P~200days with the 47 Tucanae Mira variables in the (K, logP) plane. The (K, logP) relation is also used to examine the tilt of the LMC populations of old and intermediate-age stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/784#1</TD>
            <TD>2011-09-14T18:45:01Z</TD>
            <TD>#Spectral_Classification#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/784</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/99/784</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/784</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/99/784 [2]</TD>
            <TD>IR photometry of LMC long-period variables (Hughes+ 1990)</TD>
            <TD>Infrared JHK photometry and visual spectra have been obtained for a large sample of long-period variables (LPVs) in the Large Magellanic Cloud (LMC). Various aspects of the asymptotic giant branch (AGB) evolution of LPVs are discussed using these data. The birth/death rate of LPVs of different ages in the LMC is compared with the birth rates of appropriate samples of planetary nebulae clump stars, Cepheids, and OH/IR stars. It appears that there are much fewer large-amplitude LPVs per unit galactic stellar mass in the LMC than in the Galaxy. We suggest that this may be due to the fact that the evolved intermediate-age AGB stars in the LMC often turn into carbon stars, which tend to have smaller pulsation amplitudes than M stars. There is also a major discrepancy between the number of LPVs in the LMC (and in the Galaxy) and the number predicted by the theories of AGB evolution, pulsation, and mass loss. A distance modulus to the LMC of 18.66+0.05 is derived by comparing the LMC LPVs with P~200days with the 47 Tucanae Mira variables in the (K, logP) plane. The (K, logP) relation is also used to examine the tilt of the LMC populations of old and intermediate-age stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/784#2</TD>
            <TD>2011-09-14T18:45:01Z</TD>
            <TD>#Spectral_Classification#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/784</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/99/784&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/784</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ETGALCXO [1]</TD>
            <TD>Early-Type Galaxies Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L_X). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L_GC&lt;sup&gt;Alpha&lt;/sup&gt; Z_Fe&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33+/-0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau_L and the duty cycle is F_d, their results imply ~ 1.5(Tau_L/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F_d&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminoaities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D_25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D_25 restriction should mitigate against contamination by background AGNs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalcxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalcxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=etgalcxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/etgalcxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ETGALCXO [2]</TD>
            <TD>Early-Type Galaxies Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L_X). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L_GC&lt;sup&gt;Alpha&lt;/sup&gt; Z_Fe&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33+/-0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau_L and the duty cycle is F_d, their results imply ~ 1.5(Tau_L/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F_d&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminoaities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D_25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D_25 restriction should mitigate against contamination by background AGNs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalcxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=etgalcxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/etgalcxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ETGALCXO [3]</TD>
            <TD>Early-Type Galaxies Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L_X). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L_GC&lt;sup&gt;Alpha&lt;/sup&gt; Z_Fe&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33+/-0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau_L and the duty cycle is F_d, their results imply ~ 1.5(Tau_L/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F_d&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminoaities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D_25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D_25 restriction should mitigate against contamination by background AGNs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalcxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_etgalcxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/etgalcxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ETGALCXO [1]</TD>
            <TD>Early-Type Galaxies Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L_X). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L_GC&lt;sup&gt;Alpha&lt;/sup&gt; Z_Fe&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33+/-0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau_L and the duty cycle is F_d, their results imply ~ 1.5(Tau_L/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F_d&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminoaities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D_25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D_25 restriction should mitigate against contamination by background AGNs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalcxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalcxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=etgalcxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/etgalcxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ETGALCXO [2]</TD>
            <TD>Early-Type Galaxies Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L_X). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L_GC&lt;sup&gt;Alpha&lt;/sup&gt; Z_Fe&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33+/-0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau_L and the duty cycle is F_d, their results imply ~ 1.5(Tau_L/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F_d&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminoaities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D_25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D_25 restriction should mitigate against contamination by background AGNs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalcxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=etgalcxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/etgalcxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ETGALCXO [3]</TD>
            <TD>Early-Type Galaxies Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L_X). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L_GC&lt;sup&gt;Alpha&lt;/sup&gt; Z_Fe&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33+/-0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau_L and the duty cycle is F_d, their results imply ~ 1.5(Tau_L/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F_d&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminoaities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D_25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D_25 restriction should mitigate against contamination by background AGNs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalcxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_etgalcxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/etgalcxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/34 [1]</TD>
            <TD>Clusters of galaxies in SDSS-III (Wen+, 2012)</TD>
            <TD>Wen et al. (2009, Cat. J/ApJS/183/197) identified 39668 galaxy clusters from the SDSS DR6 by the discrimination of member galaxies of clusters using photometric redshifts of galaxies. Wen &amp; Han (2011ApJ...734...68W) improved the method and successfully identified the high-redshift clusters from the deep fields of the Canada-France-Hawaii Telescope (CFHT) Wide survey, the CHFT Deep survey, the Cosmic Evolution Survey, and the Spitzer Wide-area InfraRed Extragalactic survey. Here, we follow and improve the algorithm to identify clusters from SDSS-III (SDSS Data Release 8; Aihara et al. 2011ApJS..193...29A, see Cat. II/306).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34#1</TD>
            <TD>2012-08-22T15:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/34</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/34</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/34 [2]</TD>
            <TD>Clusters of galaxies in SDSS-III (Wen+, 2012)</TD>
            <TD>Wen et al. (2009, Cat. J/ApJS/183/197) identified 39668 galaxy clusters from the SDSS DR6 by the discrimination of member galaxies of clusters using photometric redshifts of galaxies. Wen &amp; Han (2011ApJ...734...68W) improved the method and successfully identified the high-redshift clusters from the deep fields of the Canada-France-Hawaii Telescope (CFHT) Wide survey, the CHFT Deep survey, the Cosmic Evolution Survey, and the Spitzer Wide-area InfraRed Extragalactic survey. Here, we follow and improve the algorithm to identify clusters from SDSS-III (SDSS Data Release 8; Aihara et al. 2011ApJS..193...29A, see Cat. II/306).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34#2</TD>
            <TD>2012-08-22T15:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/34&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/34</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/34 [table1]</TD>
            <TD>Clusters of galaxies in SDSS-III (Wen+, 2012)</TD>
            <TD>Wen et al. (2009, Cat. J/ApJS/183/197) identified 39668 galaxy clusters from the SDSS DR6 by the discrimination of member galaxies of clusters using photometric redshifts of galaxies. Wen &amp; Han (2011ApJ...734...68W) improved the method and successfully identified the high-redshift clusters from the deep fields of the Canada-France-Hawaii Telescope (CFHT) Wide survey, the CHFT Deep survey, the Cosmic Evolution Survey, and the Spitzer Wide-area InfraRed Extragalactic survey. Here, we follow and improve the algorithm to identify clusters from SDSS-III (SDSS Data Release 8; Aihara et al. 2011ApJS..193...29A, see Cat. II/306).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34#table1</TD>
            <TD>2012-08-22T15:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/34&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/34</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/173 [1]</TD>
            <TD>BVR photometry of NGC 6822 (Marconi+ 1995)</TD>
            <TD>Our proposed method to study the star-formation histories in nearby irregulars is here applied to NGC 6822. To this purpose we have obtained accurate CCD photometry of three regions in the galaxy, reaching V=23.5 with the required accuracy of {sigma}_BVR_&lt;=0.1mag. Major information on the stellar populations, star-formation rates, and initial mass functions of these regions in the last 1Gyr are derived from the comparison of the observational color-magnitude diagrams and luminosity functions with the corresponding synthetic diagrams and luminosity functions generated by a numerical simulation code based on stellar evolutionary tracks. We find that in the last 1Gyr the star-formation activity has been rather continuous, possibly occurring in long episodes of moderate activity separated by short quiescent periods, and that the initial mass function exponent a is in the vicinity of Salpeter's value, i.e., slightly flatter than in the solar neighborhood. The studied regions of NGC 6822 appear to contain different stellar populations. The preferred star formation regime for region A is a continuous activity coupled with a moderately flat {alpha}. For region C, instead, our best models suggest a discontinuous star formation and a moderately steep {alpha}. NGC 6822 is the last object of our original sample of five nearby irregulars. We can then draw the scenario resulting from this sample: most of the observed fields appear to have experienced a gasping regime of star formation, with average exponent {alpha}=2.35 for the initial mass function. Despite their small sizes, the majority of the sample galaxies contain different stellar populations in different regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/173#1</TD>
            <TD>2011-09-14T18:45:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/173</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/173</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/173 [2]</TD>
            <TD>BVR photometry of NGC 6822 (Marconi+ 1995)</TD>
            <TD>Our proposed method to study the star-formation histories in nearby irregulars is here applied to NGC 6822. To this purpose we have obtained accurate CCD photometry of three regions in the galaxy, reaching V=23.5 with the required accuracy of {sigma}_BVR_&lt;=0.1mag. Major information on the stellar populations, star-formation rates, and initial mass functions of these regions in the last 1Gyr are derived from the comparison of the observational color-magnitude diagrams and luminosity functions with the corresponding synthetic diagrams and luminosity functions generated by a numerical simulation code based on stellar evolutionary tracks. We find that in the last 1Gyr the star-formation activity has been rather continuous, possibly occurring in long episodes of moderate activity separated by short quiescent periods, and that the initial mass function exponent a is in the vicinity of Salpeter's value, i.e., slightly flatter than in the solar neighborhood. The studied regions of NGC 6822 appear to contain different stellar populations. The preferred star formation regime for region A is a continuous activity coupled with a moderately flat {alpha}. For region C, instead, our best models suggest a discontinuous star formation and a moderately steep {alpha}. NGC 6822 is the last object of our original sample of five nearby irregulars. We can then draw the scenario resulting from this sample: most of the observed fields appear to have experienced a gasping regime of star formation, with average exponent {alpha}=2.35 for the initial mass function. Despite their small sizes, the majority of the sample galaxies contain different stellar populations in different regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/173#2</TD>
            <TD>2011-09-14T18:45:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/173&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/173</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ETGALCXO [1]</TD>
            <TD>Early-Type Galaxies Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L_X). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L_GC&lt;sup&gt;Alpha&lt;/sup&gt; Z_Fe&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33+/-0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau_L and the duty cycle is F_d, their results imply ~ 1.5(Tau_L/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F_d&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminoaities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D_25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D_25 restriction should mitigate against contamination by background AGNs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalcxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalcxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=etgalcxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/etgalcxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ETGALCXO [2]</TD>
            <TD>Early-Type Galaxies Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L_X). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L_GC&lt;sup&gt;Alpha&lt;/sup&gt; Z_Fe&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33+/-0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau_L and the duty cycle is F_d, their results imply ~ 1.5(Tau_L/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F_d&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminoaities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D_25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D_25 restriction should mitigate against contamination by background AGNs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalcxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=etgalcxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/etgalcxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ETGALCXO [3]</TD>
            <TD>Early-Type Galaxies Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a Chandra survey of low-mass X-ray binaries (LMXBs) in 24 early-type galaxies. Correcting for detection incompleteness, the X-ray luminosity function (XLF) of each galaxy is consistent with a power law with negative logarithmic differential slope, Beta, ~ 2.0. However, Beta strongly correlates with incompleteness, indicating the XLF flattens at low X-ray luminosity (L_X). The composite XLF is well fitted by a power law with a break at (2.21 [+0.65,-0.56]) x 10&lt;sup&gt;38&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; and Beta = 1.40 [+0.10,-0.13] and = 2.84 [+0.39,-0.30] below and above it, respectively. The break is close to the Eddington limit for a 1.4 solar-mass neutron star, but the XLF shape rules out its representing the division between neutron star and black hole systems. Although the XLFs are similar, the authors find evidence of some variation between galaxies. The high-L_X XLF slope does not correlate with age, but may correlate with [Alpha/Fe]. Considering only LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;, matching the LMXBs with globular clusters (GCs) identified in HST observations of 19 of the galaxies, the authors find the probability a GC hosts an LMXB is proportional to L_GC&lt;sup&gt;Alpha&lt;/sup&gt; Z_Fe&lt;sup&gt;Gamma&lt;/sup&gt; where Alpha = 1.01 +/- 0.19 and Gamma = 0.33+/-0.11. Correcting for GC luminosity and color effects, and detection incompleteness, they find no evidence that the fraction of LMXBs with L_X &gt; 10&lt;sup&gt;37&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in GCs (40%), or the fraction of GCs hosting LMXBs (~ 6.5%) varies between galaxies. The spatial distribution of LMXBs resembles that of GCs, and the specific frequency of LMXBs is proportional to the GC specific luminosity, consistent with the hypothesis that all LMXBs form in GCs. If the LMXB lifetime is Tau_L and the duty cycle is F_d, their results imply ~ 1.5(Tau_L/10&lt;sup&gt;8&lt;/sup&gt; yr)&lt;sup&gt;-1&lt;/sup&gt; F_d&lt;sup&gt;-1&lt;/sup&gt; LMXBs are formed per gigayear per GC, and they place an upper limit of one active LMXB in the field per 3.4 x 10&lt;sup&gt;9&lt;/sup&gt; solar luminoaities of V-band luminosity. This table contains 1194 X-ray point sources that were detected within the B-band 25th magnitude ellipse D_25 (as listed in the de Vaucouleurs et al. Catalog of Bright Galaxies) of 24 early-type galaxies observed by Chandra (listed in Table 1 of the reference paper). The D_25 restriction should mitigate against contamination by background AGNs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalcxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_etgalcxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/etgalcxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/173 [1]</TD>
            <TD>BVR photometry of NGC 6822 (Marconi+ 1995)</TD>
            <TD>Our proposed method to study the star-formation histories in nearby irregulars is here applied to NGC 6822. To this purpose we have obtained accurate CCD photometry of three regions in the galaxy, reaching V=23.5 with the required accuracy of {sigma}_BVR_&lt;=0.1mag. Major information on the stellar populations, star-formation rates, and initial mass functions of these regions in the last 1Gyr are derived from the comparison of the observational color-magnitude diagrams and luminosity functions with the corresponding synthetic diagrams and luminosity functions generated by a numerical simulation code based on stellar evolutionary tracks. We find that in the last 1Gyr the star-formation activity has been rather continuous, possibly occurring in long episodes of moderate activity separated by short quiescent periods, and that the initial mass function exponent a is in the vicinity of Salpeter's value, i.e., slightly flatter than in the solar neighborhood. The studied regions of NGC 6822 appear to contain different stellar populations. The preferred star formation regime for region A is a continuous activity coupled with a moderately flat {alpha}. For region C, instead, our best models suggest a discontinuous star formation and a moderately steep {alpha}. NGC 6822 is the last object of our original sample of five nearby irregulars. We can then draw the scenario resulting from this sample: most of the observed fields appear to have experienced a gasping regime of star formation, with average exponent {alpha}=2.35 for the initial mass function. Despite their small sizes, the majority of the sample galaxies contain different stellar populations in different regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/173#1</TD>
            <TD>2011-09-14T18:45:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/173</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/173</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/173 [2]</TD>
            <TD>BVR photometry of NGC 6822 (Marconi+ 1995)</TD>
            <TD>Our proposed method to study the star-formation histories in nearby irregulars is here applied to NGC 6822. To this purpose we have obtained accurate CCD photometry of three regions in the galaxy, reaching V=23.5 with the required accuracy of {sigma}_BVR_&lt;=0.1mag. Major information on the stellar populations, star-formation rates, and initial mass functions of these regions in the last 1Gyr are derived from the comparison of the observational color-magnitude diagrams and luminosity functions with the corresponding synthetic diagrams and luminosity functions generated by a numerical simulation code based on stellar evolutionary tracks. We find that in the last 1Gyr the star-formation activity has been rather continuous, possibly occurring in long episodes of moderate activity separated by short quiescent periods, and that the initial mass function exponent a is in the vicinity of Salpeter's value, i.e., slightly flatter than in the solar neighborhood. The studied regions of NGC 6822 appear to contain different stellar populations. The preferred star formation regime for region A is a continuous activity coupled with a moderately flat {alpha}. For region C, instead, our best models suggest a discontinuous star formation and a moderately steep {alpha}. NGC 6822 is the last object of our original sample of five nearby irregulars. We can then draw the scenario resulting from this sample: most of the observed fields appear to have experienced a gasping regime of star formation, with average exponent {alpha}=2.35 for the initial mass function. Despite their small sizes, the majority of the sample galaxies contain different stellar populations in different regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/173#2</TD>
            <TD>2011-09-14T18:45:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/173&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/173</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>FSVSClusGR [1]</TD>
            <TD>Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups</TD>
            <TD>The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups contains a a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semi-parametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by color discrimination. The sample covers a wide range of richness, has a density of ~28 clusters per square degree, and spans a range of estimated redshifts of 0.05 &lt; z &lt; 0.9 with mean &lt;z&gt; = 0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be sigma ~ 0.03. Containing over 100 clusters with z &gt; 0.6, the catalog contributes substantially to the current total of optically-selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programs. The construction of this FSVS Cluster Catalogue completes a fundamental component of the authors' continuing program to investigate the environments of quasars and the chemical evolution of galaxies. The present table contains the list of all clusters with their basic parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/fsvsclustr#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/fsvsclustr</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=fsvsclustr&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/fsvsclustr.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>FSVSClusGR [2]</TD>
            <TD>Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups</TD>
            <TD>The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups contains a a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semi-parametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by color discrimination. The sample covers a wide range of richness, has a density of ~28 clusters per square degree, and spans a range of estimated redshifts of 0.05 &lt; z &lt; 0.9 with mean &lt;z&gt; = 0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be sigma ~ 0.03. Containing over 100 clusters with z &gt; 0.6, the catalog contributes substantially to the current total of optically-selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programs. The construction of this FSVS Cluster Catalogue completes a fundamental component of the authors' continuing program to investigate the environments of quasars and the chemical evolution of galaxies. The present table contains the list of all clusters with their basic parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/fsvsclustr#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/fsvsclustr</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=fsvsclustr&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/fsvsclustr.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>FSVSClusGR [3]</TD>
            <TD>Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups</TD>
            <TD>The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups contains a a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semi-parametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by color discrimination. The sample covers a wide range of richness, has a density of ~28 clusters per square degree, and spans a range of estimated redshifts of 0.05 &lt; z &lt; 0.9 with mean &lt;z&gt; = 0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be sigma ~ 0.03. Containing over 100 clusters with z &gt; 0.6, the catalog contributes substantially to the current total of optically-selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programs. The construction of this FSVS Cluster Catalogue completes a fundamental component of the authors' continuing program to investigate the environments of quasars and the chemical evolution of galaxies. The present table contains the list of all clusters with their basic parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/fsvsclustr#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/fsvsclustr</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_fsvsclustr&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/fsvsclustr.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/480/568 [1]</TD>
            <TD>RK photometry in 3C 336 field (Steidel+ 1997)</TD>
            <TD>We present very deep WFPC2 images and FOS spectroscopy from the Hubble Space Telescope (HST) together with numerous supporting ground-based observations of the field of the quasar 3C 336 (z_em_=0.927). The observations are designed to investigate the nature of galaxies producing metal-line absorption systems in the spectrum of the QSO. Along a single line of sight, we find at least six metal-line absorption systems (of which three are newly discovered) ranging in redshift from 0.317 to 0.892. Through an extensive program of optical and IR imaging, QSO spectroscopy, and faint galaxy spectroscopy, we have identified five of the six metal-line absorption systems with luminous (L_K_&gt;=0.1L^*^_K_) galaxies. These have morphologies ranging from very late-type spiral to S0, and they exhibit a wide range of inclination and position angles with respect to the QSO sight line. The only unidentified absorber, despite our intensive search, is a damped Lyman-{alpha} system at z_abs_=0.656. Analysis of the absorption spectrum suggests that the metal abundances ([Fe/H]=-1.2) in this system are similar to those in damped systems at z~2 and to the two other damped systems for which abundances have been determined at z&lt;1. The absorption line system must either be associated with an underluminous, late-type spiral galaxy, which we find at a projected disk impact parameter of ~120h^-1^kpc, or with an as yet unseen, extremely faint galaxy (L&lt;0.05L^*^_K_) near the QSO sight line that eludes detection despite our deep HST and high-resolution ground-based near-IR images. We have found no examples of intrinsically faint galaxies (L&lt;0.1L^*^) at small impact parameters that might have been missed as absorber candidates in our previous ground-based imaging and spectroscopic programs on Mg II absorbing galaxies. We have, however, identified several intrinsically faint galaxies within ~50h^-1^kpc of the QSO sight line that do not produce detectable metal-line absorption. There are no bright galaxies (L&gt;0.1L_K_) within 50h^-1^kpc that do not produce detectable metal lines (of Mg II {lambda}{lambda}2796, 2803 and/or C IV {lambda}{lambda}1548, 1550) in the QSO spectrum. All of these results generally support the inferences we have previously reached from a larger survey for absorption-selected galaxies at z&lt;1. There are several other galaxies with redshifts near that of 3C 336, suggesting that the QSO is situated in an overdense region, perhaps a galaxy cluster. Previously published reports of a cluster around 3C 336 were largely misled by the presence of many foreground galaxies seen in projection near the QSO. It is possible that a reported measurement of weak shear gravitational lensing in this field may be produced by the QSO cluster itself, since there appear to be no other groups or clusters in the foreground. We find no evidence for a normal, bright QSO host galaxy, although there are several faint objects very close to the quasar and at similar redshift that might either be companions or part of a disorganized QSO host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/480/568#1</TD>
            <TD>2011-09-14T18:45:17Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/480/568</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/480/568</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/480/568</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/480/568 [2]</TD>
            <TD>RK photometry in 3C 336 field (Steidel+ 1997)</TD>
            <TD>We present very deep WFPC2 images and FOS spectroscopy from the Hubble Space Telescope (HST) together with numerous supporting ground-based observations of the field of the quasar 3C 336 (z_em_=0.927). The observations are designed to investigate the nature of galaxies producing metal-line absorption systems in the spectrum of the QSO. Along a single line of sight, we find at least six metal-line absorption systems (of which three are newly discovered) ranging in redshift from 0.317 to 0.892. Through an extensive program of optical and IR imaging, QSO spectroscopy, and faint galaxy spectroscopy, we have identified five of the six metal-line absorption systems with luminous (L_K_&gt;=0.1L^*^_K_) galaxies. These have morphologies ranging from very late-type spiral to S0, and they exhibit a wide range of inclination and position angles with respect to the QSO sight line. The only unidentified absorber, despite our intensive search, is a damped Lyman-{alpha} system at z_abs_=0.656. Analysis of the absorption spectrum suggests that the metal abundances ([Fe/H]=-1.2) in this system are similar to those in damped systems at z~2 and to the two other damped systems for which abundances have been determined at z&lt;1. The absorption line system must either be associated with an underluminous, late-type spiral galaxy, which we find at a projected disk impact parameter of ~120h^-1^kpc, or with an as yet unseen, extremely faint galaxy (L&lt;0.05L^*^_K_) near the QSO sight line that eludes detection despite our deep HST and high-resolution ground-based near-IR images. We have found no examples of intrinsically faint galaxies (L&lt;0.1L^*^) at small impact parameters that might have been missed as absorber candidates in our previous ground-based imaging and spectroscopic programs on Mg II absorbing galaxies. We have, however, identified several intrinsically faint galaxies within ~50h^-1^kpc of the QSO sight line that do not produce detectable metal-line absorption. There are no bright galaxies (L&gt;0.1L_K_) within 50h^-1^kpc that do not produce detectable metal lines (of Mg II {lambda}{lambda}2796, 2803 and/or C IV {lambda}{lambda}1548, 1550) in the QSO spectrum. All of these results generally support the inferences we have previously reached from a larger survey for absorption-selected galaxies at z&lt;1. There are several other galaxies with redshifts near that of 3C 336, suggesting that the QSO is situated in an overdense region, perhaps a galaxy cluster. Previously published reports of a cluster around 3C 336 were largely misled by the presence of many foreground galaxies seen in projection near the QSO. It is possible that a reported measurement of weak shear gravitational lensing in this field may be produced by the QSO cluster itself, since there appear to be no other groups or clusters in the foreground. We find no evidence for a normal, bright QSO host galaxy, although there are several faint objects very close to the quasar and at similar redshift that might either be companions or part of a disorganized QSO host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/480/568#2</TD>
            <TD>2011-09-14T18:45:17Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/480/568</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/480/568&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/480/568</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>FSVSClusGR [1]</TD>
            <TD>Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups</TD>
            <TD>The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups contains a a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semi-parametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by color discrimination. The sample covers a wide range of richness, has a density of ~28 clusters per square degree, and spans a range of estimated redshifts of 0.05 &lt; z &lt; 0.9 with mean &lt;z&gt; = 0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be sigma ~ 0.03. Containing over 100 clusters with z &gt; 0.6, the catalog contributes substantially to the current total of optically-selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programs. The construction of this FSVS Cluster Catalogue completes a fundamental component of the authors' continuing program to investigate the environments of quasars and the chemical evolution of galaxies. The present table contains the list of all clusters with their basic parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/fsvsclustr#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Cluster#</TD>
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            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/fsvsclustr</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>180</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/fsvsclustr.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>FSVSClusGR [2]</TD>
            <TD>Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups</TD>
            <TD>The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups contains a a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semi-parametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by color discrimination. The sample covers a wide range of richness, has a density of ~28 clusters per square degree, and spans a range of estimated redshifts of 0.05 &lt; z &lt; 0.9 with mean &lt;z&gt; = 0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be sigma ~ 0.03. Containing over 100 clusters with z &gt; 0.6, the catalog contributes substantially to the current total of optically-selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programs. The construction of this FSVS Cluster Catalogue completes a fundamental component of the authors' continuing program to investigate the environments of quasars and the chemical evolution of galaxies. The present table contains the list of all clusters with their basic parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/fsvsclustr#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0833333333333333333</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=fsvsclustr&amp;</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/fsvsclustr.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>FSVSClusGR [3]</TD>
            <TD>Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups</TD>
            <TD>The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups contains a a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semi-parametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by color discrimination. The sample covers a wide range of richness, has a density of ~28 clusters per square degree, and spans a range of estimated redshifts of 0.05 &lt; z &lt; 0.9 with mean &lt;z&gt; = 0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be sigma ~ 0.03. Containing over 100 clusters with z &gt; 0.6, the catalog contributes substantially to the current total of optically-selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programs. The construction of this FSVS Cluster Catalogue completes a fundamental component of the authors' continuing program to investigate the environments of quasars and the chemical evolution of galaxies. The present table contains the list of all clusters with their basic parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>ivo://nasa.heasarc/fsvsclustr#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_fsvsclustr&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/fsvsclustr.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/480/568 [1]</TD>
            <TD>RK photometry in 3C 336 field (Steidel+ 1997)</TD>
            <TD>We present very deep WFPC2 images and FOS spectroscopy from the Hubble Space Telescope (HST) together with numerous supporting ground-based observations of the field of the quasar 3C 336 (z_em_=0.927). The observations are designed to investigate the nature of galaxies producing metal-line absorption systems in the spectrum of the QSO. Along a single line of sight, we find at least six metal-line absorption systems (of which three are newly discovered) ranging in redshift from 0.317 to 0.892. Through an extensive program of optical and IR imaging, QSO spectroscopy, and faint galaxy spectroscopy, we have identified five of the six metal-line absorption systems with luminous (L_K_&gt;=0.1L^*^_K_) galaxies. These have morphologies ranging from very late-type spiral to S0, and they exhibit a wide range of inclination and position angles with respect to the QSO sight line. The only unidentified absorber, despite our intensive search, is a damped Lyman-{alpha} system at z_abs_=0.656. Analysis of the absorption spectrum suggests that the metal abundances ([Fe/H]=-1.2) in this system are similar to those in damped systems at z~2 and to the two other damped systems for which abundances have been determined at z&lt;1. The absorption line system must either be associated with an underluminous, late-type spiral galaxy, which we find at a projected disk impact parameter of ~120h^-1^kpc, or with an as yet unseen, extremely faint galaxy (L&lt;0.05L^*^_K_) near the QSO sight line that eludes detection despite our deep HST and high-resolution ground-based near-IR images. We have found no examples of intrinsically faint galaxies (L&lt;0.1L^*^) at small impact parameters that might have been missed as absorber candidates in our previous ground-based imaging and spectroscopic programs on Mg II absorbing galaxies. We have, however, identified several intrinsically faint galaxies within ~50h^-1^kpc of the QSO sight line that do not produce detectable metal-line absorption. There are no bright galaxies (L&gt;0.1L_K_) within 50h^-1^kpc that do not produce detectable metal lines (of Mg II {lambda}{lambda}2796, 2803 and/or C IV {lambda}{lambda}1548, 1550) in the QSO spectrum. All of these results generally support the inferences we have previously reached from a larger survey for absorption-selected galaxies at z&lt;1. There are several other galaxies with redshifts near that of 3C 336, suggesting that the QSO is situated in an overdense region, perhaps a galaxy cluster. Previously published reports of a cluster around 3C 336 were largely misled by the presence of many foreground galaxies seen in projection near the QSO. It is possible that a reported measurement of weak shear gravitational lensing in this field may be produced by the QSO cluster itself, since there appear to be no other groups or clusters in the foreground. We find no evidence for a normal, bright QSO host galaxy, although there are several faint objects very close to the quasar and at similar redshift that might either be companions or part of a disorganized QSO host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/480/568#1</TD>
            <TD>2011-09-14T18:45:17Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/480/568</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/480/568</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/480/568</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/480/568 [2]</TD>
            <TD>RK photometry in 3C 336 field (Steidel+ 1997)</TD>
            <TD>We present very deep WFPC2 images and FOS spectroscopy from the Hubble Space Telescope (HST) together with numerous supporting ground-based observations of the field of the quasar 3C 336 (z_em_=0.927). The observations are designed to investigate the nature of galaxies producing metal-line absorption systems in the spectrum of the QSO. Along a single line of sight, we find at least six metal-line absorption systems (of which three are newly discovered) ranging in redshift from 0.317 to 0.892. Through an extensive program of optical and IR imaging, QSO spectroscopy, and faint galaxy spectroscopy, we have identified five of the six metal-line absorption systems with luminous (L_K_&gt;=0.1L^*^_K_) galaxies. These have morphologies ranging from very late-type spiral to S0, and they exhibit a wide range of inclination and position angles with respect to the QSO sight line. The only unidentified absorber, despite our intensive search, is a damped Lyman-{alpha} system at z_abs_=0.656. Analysis of the absorption spectrum suggests that the metal abundances ([Fe/H]=-1.2) in this system are similar to those in damped systems at z~2 and to the two other damped systems for which abundances have been determined at z&lt;1. The absorption line system must either be associated with an underluminous, late-type spiral galaxy, which we find at a projected disk impact parameter of ~120h^-1^kpc, or with an as yet unseen, extremely faint galaxy (L&lt;0.05L^*^_K_) near the QSO sight line that eludes detection despite our deep HST and high-resolution ground-based near-IR images. We have found no examples of intrinsically faint galaxies (L&lt;0.1L^*^) at small impact parameters that might have been missed as absorber candidates in our previous ground-based imaging and spectroscopic programs on Mg II absorbing galaxies. We have, however, identified several intrinsically faint galaxies within ~50h^-1^kpc of the QSO sight line that do not produce detectable metal-line absorption. There are no bright galaxies (L&gt;0.1L_K_) within 50h^-1^kpc that do not produce detectable metal lines (of Mg II {lambda}{lambda}2796, 2803 and/or C IV {lambda}{lambda}1548, 1550) in the QSO spectrum. All of these results generally support the inferences we have previously reached from a larger survey for absorption-selected galaxies at z&lt;1. There are several other galaxies with redshifts near that of 3C 336, suggesting that the QSO is situated in an overdense region, perhaps a galaxy cluster. Previously published reports of a cluster around 3C 336 were largely misled by the presence of many foreground galaxies seen in projection near the QSO. It is possible that a reported measurement of weak shear gravitational lensing in this field may be produced by the QSO cluster itself, since there appear to be no other groups or clusters in the foreground. We find no evidence for a normal, bright QSO host galaxy, although there are several faint objects very close to the quasar and at similar redshift that might either be companions or part of a disorganized QSO host.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/480/568#2</TD>
            <TD>2011-09-14T18:45:17Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>08-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/480/568</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/480/568</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>FSVSClusGR [1]</TD>
            <TD>Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups</TD>
            <TD>The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups contains a a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semi-parametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by color discrimination. The sample covers a wide range of richness, has a density of ~28 clusters per square degree, and spans a range of estimated redshifts of 0.05 &lt; z &lt; 0.9 with mean &lt;z&gt; = 0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be sigma ~ 0.03. Containing over 100 clusters with z &gt; 0.6, the catalog contributes substantially to the current total of optically-selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programs. The construction of this FSVS Cluster Catalogue completes a fundamental component of the authors' continuing program to investigate the environments of quasars and the chemical evolution of galaxies. The present table contains the list of all clusters with their basic parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/fsvsclustr#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0833333333333333333</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=fsvsclustr&amp;</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/fsvsclustr.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>FSVSClusGR [2]</TD>
            <TD>Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups</TD>
            <TD>The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups contains a a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semi-parametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by color discrimination. The sample covers a wide range of richness, has a density of ~28 clusters per square degree, and spans a range of estimated redshifts of 0.05 &lt; z &lt; 0.9 with mean &lt;z&gt; = 0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be sigma ~ 0.03. Containing over 100 clusters with z &gt; 0.6, the catalog contributes substantially to the current total of optically-selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programs. The construction of this FSVS Cluster Catalogue completes a fundamental component of the authors' continuing program to investigate the environments of quasars and the chemical evolution of galaxies. The present table contains the list of all clusters with their basic parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/fsvsclustr#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Cluster#</TD>
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            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/fsvsclustr</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=fsvsclustr&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/fsvsclustr.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>FSVSClusGR [3]</TD>
            <TD>Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups</TD>
            <TD>The Faint Sky Variability Survey Catalog of Galaxy Clusters and Rich Groups contains a a large sample of 598 galaxy clusters and rich groups discovered in the data of the Faint Sky Variability Survey (FSVS). The clusters have been identified using a fully automated, semi-parametric technique based on a maximum likelihood approach applied to Voronoi tessellation, and enhanced by color discrimination. The sample covers a wide range of richness, has a density of ~28 clusters per square degree, and spans a range of estimated redshifts of 0.05 &lt; z &lt; 0.9 with mean &lt;z&gt; = 0.345. Assuming the presence of a cluster red sequence, the uncertainty of the estimated cluster redshifts is assessed to be sigma ~ 0.03. Containing over 100 clusters with z &gt; 0.6, the catalog contributes substantially to the current total of optically-selected, intermediate-redshift clusters, and complements the existing, usually X-ray selected, samples. The FSVS fields are accessible for observation throughout the whole year, making them particularly suited for large follow-up programs. The construction of this FSVS Cluster Catalogue completes a fundamental component of the authors' continuing program to investigate the environments of quasars and the chemical evolution of galaxies. The present table contains the list of all clusters with their basic parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/fsvsclustr#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/fsvsclustr</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_fsvsclustr&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/fsvsclustr.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/34 [1]</TD>
            <TD>Clusters of galaxies in SDSS-III (Wen+, 2012)</TD>
            <TD>Wen et al. (2009, Cat. J/ApJS/183/197) identified 39668 galaxy clusters from the SDSS DR6 by the discrimination of member galaxies of clusters using photometric redshifts of galaxies. Wen &amp; Han (2011ApJ...734...68W) improved the method and successfully identified the high-redshift clusters from the deep fields of the Canada-France-Hawaii Telescope (CFHT) Wide survey, the CHFT Deep survey, the Cosmic Evolution Survey, and the Spitzer Wide-area InfraRed Extragalactic survey. Here, we follow and improve the algorithm to identify clusters from SDSS-III (SDSS Data Release 8; Aihara et al. 2011ApJS..193...29A, see Cat. II/306).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34#1</TD>
            <TD>2012-08-22T15:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/34</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/34</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/34 [2]</TD>
            <TD>Clusters of galaxies in SDSS-III (Wen+, 2012)</TD>
            <TD>Wen et al. (2009, Cat. J/ApJS/183/197) identified 39668 galaxy clusters from the SDSS DR6 by the discrimination of member galaxies of clusters using photometric redshifts of galaxies. Wen &amp; Han (2011ApJ...734...68W) improved the method and successfully identified the high-redshift clusters from the deep fields of the Canada-France-Hawaii Telescope (CFHT) Wide survey, the CHFT Deep survey, the Cosmic Evolution Survey, and the Spitzer Wide-area InfraRed Extragalactic survey. Here, we follow and improve the algorithm to identify clusters from SDSS-III (SDSS Data Release 8; Aihara et al. 2011ApJS..193...29A, see Cat. II/306).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34#2</TD>
            <TD>2012-08-22T15:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/34&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/34</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/34 [table1]</TD>
            <TD>Clusters of galaxies in SDSS-III (Wen+, 2012)</TD>
            <TD>Wen et al. (2009, Cat. J/ApJS/183/197) identified 39668 galaxy clusters from the SDSS DR6 by the discrimination of member galaxies of clusters using photometric redshifts of galaxies. Wen &amp; Han (2011ApJ...734...68W) improved the method and successfully identified the high-redshift clusters from the deep fields of the Canada-France-Hawaii Telescope (CFHT) Wide survey, the CHFT Deep survey, the Cosmic Evolution Survey, and the Spitzer Wide-area InfraRed Extragalactic survey. Here, we follow and improve the algorithm to identify clusters from SDSS-III (SDSS Data Release 8; Aihara et al. 2011ApJS..193...29A, see Cat. II/306).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34#table1</TD>
            <TD>2012-08-22T15:20:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/34</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/34&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/34</TD>
          </TR>
          <TR>
            <TD>CatalogService</TD>
            <TD>GCVS/X-gal</TD>
            <TD>General Catalog of Variable Stars (GCVS4.2): Extragalactic Variables</TD>
            <TD>The General Catalog of Variable Stars (GCVS) is the only reference source on all known variable stars. This database is based on the electronically-readable version as distributed by the Sternberg Astronomical Institute and Institute of Astronomy (Russian Acad. Sci.), Moscow. It is the catalog of extragalactic variable stars, an updated version of the list contained in the GCVS (4th edition), Volume V. The total number of entries in this database is 10979 variable stars in 35 stellar systems (including the Magellanic Clouds, the Andromeda Galaxy, etc.). These variables include 144 stars now considered to be non-members of the galaxies in whose fields they lie, and 92 more stars that are possible non-members. The present improved electronic version of the GCVS 4th Edition, Volumes I-V, combined with the Name-Lists of Variable Stars Nos. 67 - 77, is also available from the Sternberg Institute via anonymous ftp to &lt;a href="ftp://ftp.sai.msu.su/pub/groups/cluster/gcvs/gcvs/"&gt;ftp://ftp.sai.msu.su/pub/groups/cluster/gcvs/gcvs/&lt;/a&gt; and more information is available via the Web at &lt;a href="http://www.sai.msu.su/groups/cluster/gcvs/gcvs/"&gt;http://www.sai.msu.su/groups/cluster/gcvs/gcvs/&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/gcvsegvars</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Extragalactic Variable Star#</TD>
            <TD>#Catalog#</TD>
            <TD>#University#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gcvsegvars</TD>
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/gcvsegvars.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/123/115 [1]</TD>
            <TD>Variables stars in Palomar-Groningen field 3 (Ng+ 1997)</TD>
            <TD>A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&amp;AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115#1</TD>
            <TD>2011-09-14T18:45:32Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/123/115</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/115</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/123/115 [2]</TD>
            <TD>Variables stars in Palomar-Groningen field 3 (Ng+ 1997)</TD>
            <TD>A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&amp;AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115#2</TD>
            <TD>2011-09-14T18:45:32Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/123/115&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/123/115 [table1]</TD>
            <TD>Variables stars in Palomar-Groningen field 3 (Ng+ 1997)</TD>
            <TD>A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&amp;AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115#table1</TD>
            <TD>2011-09-14T18:45:32Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/123/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GLXSDSSQSO [1]</TD>
            <TD>GALEX/SDSS Quasar Catalog</TD>
            <TD>This table contains the result of an analysis of the broad-band UV and optical properties of z ~&lt; 3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles and listed in this table, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7 arcseconds. Most of the DR3 sample quasars are detected in the near-UV until z ~ 1.7, with the near-UV detection fraction dropping to ~50% by z ~ 2. Statistical tests performed on the distributions of nondetections indicate that the optically selected quasars missed in the UV tend to be optically faint or at high redshift. The GALEX positions are shown to be consistent with the SDSS astrometry to within an rms scatter of 0.6 - 0.7 arcsecs in each coordinate, and the empirically determined photometric errors from multiepoch GALEX observations significantly exceed the Poissonian errors quoted in the GR1 object catalogs. The UV-detected quasars are well separated from stars in UV-optical color-color space, with the UV-optical relative colors suggesting a marginally detected population of reddened objects due to absorption along the line of sight or dust associated with the quasar. The resulting spectral energy distributions (SEDs) cover ~350 - 9000 Angstroms (rest frame), where the overall median SED peaks near the Lyman-Alpha emission line, as found in other UV quasar studies. The large sample size allows the authors to construct median SEDs in small bins of redshift and luminosity, and they find that the median SED becomes harder (bluer) at UV wavelengths for quasars with lower continuum luminosity. The detected UV-optical flux as a function of redshift is qualitatively consistent with attenuation by intervening Lyman-absorbing clouds.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqso#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Quasar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqso</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=glxsdssqso&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqso.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GLXSDSSQSO [2]</TD>
            <TD>GALEX/SDSS Quasar Catalog</TD>
            <TD>This table contains the result of an analysis of the broad-band UV and optical properties of z ~&lt; 3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles and listed in this table, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7 arcseconds. Most of the DR3 sample quasars are detected in the near-UV until z ~ 1.7, with the near-UV detection fraction dropping to ~50% by z ~ 2. Statistical tests performed on the distributions of nondetections indicate that the optically selected quasars missed in the UV tend to be optically faint or at high redshift. The GALEX positions are shown to be consistent with the SDSS astrometry to within an rms scatter of 0.6 - 0.7 arcsecs in each coordinate, and the empirically determined photometric errors from multiepoch GALEX observations significantly exceed the Poissonian errors quoted in the GR1 object catalogs. The UV-detected quasars are well separated from stars in UV-optical color-color space, with the UV-optical relative colors suggesting a marginally detected population of reddened objects due to absorption along the line of sight or dust associated with the quasar. The resulting spectral energy distributions (SEDs) cover ~350 - 9000 Angstroms (rest frame), where the overall median SED peaks near the Lyman-Alpha emission line, as found in other UV quasar studies. The large sample size allows the authors to construct median SEDs in small bins of redshift and luminosity, and they find that the median SED becomes harder (bluer) at UV wavelengths for quasars with lower continuum luminosity. The detected UV-optical flux as a function of redshift is qualitatively consistent with attenuation by intervening Lyman-absorbing clouds.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqso#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Quasar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqso</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=glxsdssqso&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqso.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GLXSDSSQSO [3]</TD>
            <TD>GALEX/SDSS Quasar Catalog</TD>
            <TD>This table contains the result of an analysis of the broad-band UV and optical properties of z ~&lt; 3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles and listed in this table, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7 arcseconds. Most of the DR3 sample quasars are detected in the near-UV until z ~ 1.7, with the near-UV detection fraction dropping to ~50% by z ~ 2. Statistical tests performed on the distributions of nondetections indicate that the optically selected quasars missed in the UV tend to be optically faint or at high redshift. The GALEX positions are shown to be consistent with the SDSS astrometry to within an rms scatter of 0.6 - 0.7 arcsecs in each coordinate, and the empirically determined photometric errors from multiepoch GALEX observations significantly exceed the Poissonian errors quoted in the GR1 object catalogs. The UV-detected quasars are well separated from stars in UV-optical color-color space, with the UV-optical relative colors suggesting a marginally detected population of reddened objects due to absorption along the line of sight or dust associated with the quasar. The resulting spectral energy distributions (SEDs) cover ~350 - 9000 Angstroms (rest frame), where the overall median SED peaks near the Lyman-Alpha emission line, as found in other UV quasar studies. The large sample size allows the authors to construct median SEDs in small bins of redshift and luminosity, and they find that the median SED becomes harder (bluer) at UV wavelengths for quasars with lower continuum luminosity. The detected UV-optical flux as a function of redshift is qualitatively consistent with attenuation by intervening Lyman-absorbing clouds.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqso#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Quasar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqso</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_glxsdssqso&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqso.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GLXSDSSQSO [1]</TD>
            <TD>GALEX/SDSS Quasar Catalog</TD>
            <TD>This table contains the result of an analysis of the broad-band UV and optical properties of z ~&lt; 3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles and listed in this table, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7 arcseconds. Most of the DR3 sample quasars are detected in the near-UV until z ~ 1.7, with the near-UV detection fraction dropping to ~50% by z ~ 2. Statistical tests performed on the distributions of nondetections indicate that the optically selected quasars missed in the UV tend to be optically faint or at high redshift. The GALEX positions are shown to be consistent with the SDSS astrometry to within an rms scatter of 0.6 - 0.7 arcsecs in each coordinate, and the empirically determined photometric errors from multiepoch GALEX observations significantly exceed the Poissonian errors quoted in the GR1 object catalogs. The UV-detected quasars are well separated from stars in UV-optical color-color space, with the UV-optical relative colors suggesting a marginally detected population of reddened objects due to absorption along the line of sight or dust associated with the quasar. The resulting spectral energy distributions (SEDs) cover ~350 - 9000 Angstroms (rest frame), where the overall median SED peaks near the Lyman-Alpha emission line, as found in other UV quasar studies. The large sample size allows the authors to construct median SEDs in small bins of redshift and luminosity, and they find that the median SED becomes harder (bluer) at UV wavelengths for quasars with lower continuum luminosity. The detected UV-optical flux as a function of redshift is qualitatively consistent with attenuation by intervening Lyman-absorbing clouds.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqso#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Quasar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqso</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=glxsdssqso&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqso.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GLXSDSSQSO [2]</TD>
            <TD>GALEX/SDSS Quasar Catalog</TD>
            <TD>This table contains the result of an analysis of the broad-band UV and optical properties of z ~&lt; 3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles and listed in this table, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7 arcseconds. Most of the DR3 sample quasars are detected in the near-UV until z ~ 1.7, with the near-UV detection fraction dropping to ~50% by z ~ 2. Statistical tests performed on the distributions of nondetections indicate that the optically selected quasars missed in the UV tend to be optically faint or at high redshift. The GALEX positions are shown to be consistent with the SDSS astrometry to within an rms scatter of 0.6 - 0.7 arcsecs in each coordinate, and the empirically determined photometric errors from multiepoch GALEX observations significantly exceed the Poissonian errors quoted in the GR1 object catalogs. The UV-detected quasars are well separated from stars in UV-optical color-color space, with the UV-optical relative colors suggesting a marginally detected population of reddened objects due to absorption along the line of sight or dust associated with the quasar. The resulting spectral energy distributions (SEDs) cover ~350 - 9000 Angstroms (rest frame), where the overall median SED peaks near the Lyman-Alpha emission line, as found in other UV quasar studies. The large sample size allows the authors to construct median SEDs in small bins of redshift and luminosity, and they find that the median SED becomes harder (bluer) at UV wavelengths for quasars with lower continuum luminosity. The detected UV-optical flux as a function of redshift is qualitatively consistent with attenuation by intervening Lyman-absorbing clouds.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqso#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Quasar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqso</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=glxsdssqso&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqso.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GLXSDSSQSO [3]</TD>
            <TD>GALEX/SDSS Quasar Catalog</TD>
            <TD>This table contains the result of an analysis of the broad-band UV and optical properties of z ~&lt; 3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles and listed in this table, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7 arcseconds. Most of the DR3 sample quasars are detected in the near-UV until z ~ 1.7, with the near-UV detection fraction dropping to ~50% by z ~ 2. Statistical tests performed on the distributions of nondetections indicate that the optically selected quasars missed in the UV tend to be optically faint or at high redshift. The GALEX positions are shown to be consistent with the SDSS astrometry to within an rms scatter of 0.6 - 0.7 arcsecs in each coordinate, and the empirically determined photometric errors from multiepoch GALEX observations significantly exceed the Poissonian errors quoted in the GR1 object catalogs. The UV-detected quasars are well separated from stars in UV-optical color-color space, with the UV-optical relative colors suggesting a marginally detected population of reddened objects due to absorption along the line of sight or dust associated with the quasar. The resulting spectral energy distributions (SEDs) cover ~350 - 9000 Angstroms (rest frame), where the overall median SED peaks near the Lyman-Alpha emission line, as found in other UV quasar studies. The large sample size allows the authors to construct median SEDs in small bins of redshift and luminosity, and they find that the median SED becomes harder (bluer) at UV wavelengths for quasars with lower continuum luminosity. The detected UV-optical flux as a function of redshift is qualitatively consistent with attenuation by intervening Lyman-absorbing clouds.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqso#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Quasar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqso</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_glxsdssqso&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqso.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/123/115 [1]</TD>
            <TD>Variables stars in Palomar-Groningen field 3 (Ng+ 1997)</TD>
            <TD>A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&amp;AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115#1</TD>
            <TD>2011-09-14T18:45:32Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/123/115</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/115</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/123/115 [2]</TD>
            <TD>Variables stars in Palomar-Groningen field 3 (Ng+ 1997)</TD>
            <TD>A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&amp;AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115#2</TD>
            <TD>2011-09-14T18:45:32Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/123/115&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/123/115 [table1]</TD>
            <TD>Variables stars in Palomar-Groningen field 3 (Ng+ 1997)</TD>
            <TD>A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&amp;AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115#table1</TD>
            <TD>2011-09-14T18:45:32Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/123/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/115</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/701/1965 [1]</TD>
            <TD>Radial dust properties of SINGS galaxies (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies. Eighteen SINGS galaxies were not suitable for our purposes and were excluded from the present study. Nearly all SINGS galaxies have been observed in the far-UV (FUV; {lambda}_eff_=151.6nm) and near-UV (NUV; {lambda}_eff_=226.7nm) by GALEX (see Table 1). The reader is referred to Paper I (2009, Cat. J/ApJ/703/1569) for a more detailed description of the Spitzer data used here. Mid- and far-IR observations of the SINGS sample were carried out using the Spitzer Space Telescope (IRAC and MIPS). The HI Nearby Galaxy Survey (THINGS; Walter et al. 2008, Cat. J/AJ/136/2563) used the Very Large Array (VLA) to map HI 21cm line emission from 34 nearby (D&lt;15Mpc) galaxies, most of which were also targets of SINGS and the GALEX Nearby Galaxies Survey.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965#1</TD>
            <TD>2011-11-02T21:20:55Z</TD>
            <TD>#Extinction#Galaxies#Interstellar_Medium#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/701/1965</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1965</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/701/1965 [2]</TD>
            <TD>Radial dust properties of SINGS galaxies (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies. Eighteen SINGS galaxies were not suitable for our purposes and were excluded from the present study. Nearly all SINGS galaxies have been observed in the far-UV (FUV; {lambda}_eff_=151.6nm) and near-UV (NUV; {lambda}_eff_=226.7nm) by GALEX (see Table 1). The reader is referred to Paper I (2009, Cat. J/ApJ/703/1569) for a more detailed description of the Spitzer data used here. Mid- and far-IR observations of the SINGS sample were carried out using the Spitzer Space Telescope (IRAC and MIPS). The HI Nearby Galaxy Survey (THINGS; Walter et al. 2008, Cat. J/AJ/136/2563) used the Very Large Array (VLA) to map HI 21cm line emission from 34 nearby (D&lt;15Mpc) galaxies, most of which were also targets of SINGS and the GALEX Nearby Galaxies Survey.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965#2</TD>
            <TD>2011-11-02T21:20:55Z</TD>
            <TD>#Extinction#Galaxies#Interstellar_Medium#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/701/1965&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1965</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1965 [table1]</TD>
            <TD>Radial dust properties of SINGS galaxies (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies. Eighteen SINGS galaxies were not suitable for our purposes and were excluded from the present study. Nearly all SINGS galaxies have been observed in the far-UV (FUV; {lambda}_eff_=151.6nm) and near-UV (NUV; {lambda}_eff_=226.7nm) by GALEX (see Table 1). The reader is referred to Paper I (2009, Cat. J/ApJ/703/1569) for a more detailed description of the Spitzer data used here. Mid- and far-IR observations of the SINGS sample were carried out using the Spitzer Space Telescope (IRAC and MIPS). The HI Nearby Galaxy Survey (THINGS; Walter et al. 2008, Cat. J/AJ/136/2563) used the Very Large Array (VLA) to map HI 21cm line emission from 34 nearby (D&lt;15Mpc) galaxies, most of which were also targets of SINGS and the GALEX Nearby Galaxies Survey.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965#table1</TD>
            <TD>2011-11-02T21:20:55Z</TD>
            <TD>#Extinction#Galaxies#Interstellar_Medium#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1965&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1965</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/701/1965 [1]</TD>
            <TD>Radial dust properties of SINGS galaxies (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies. Eighteen SINGS galaxies were not suitable for our purposes and were excluded from the present study. Nearly all SINGS galaxies have been observed in the far-UV (FUV; {lambda}_eff_=151.6nm) and near-UV (NUV; {lambda}_eff_=226.7nm) by GALEX (see Table 1). The reader is referred to Paper I (2009, Cat. J/ApJ/703/1569) for a more detailed description of the Spitzer data used here. Mid- and far-IR observations of the SINGS sample were carried out using the Spitzer Space Telescope (IRAC and MIPS). The HI Nearby Galaxy Survey (THINGS; Walter et al. 2008, Cat. J/AJ/136/2563) used the Very Large Array (VLA) to map HI 21cm line emission from 34 nearby (D&lt;15Mpc) galaxies, most of which were also targets of SINGS and the GALEX Nearby Galaxies Survey.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965#1</TD>
            <TD>2011-11-02T21:20:55Z</TD>
            <TD>#Extinction#Galaxies#Interstellar_Medium#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/701/1965</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1965</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/701/1965 [2]</TD>
            <TD>Radial dust properties of SINGS galaxies (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies. Eighteen SINGS galaxies were not suitable for our purposes and were excluded from the present study. Nearly all SINGS galaxies have been observed in the far-UV (FUV; {lambda}_eff_=151.6nm) and near-UV (NUV; {lambda}_eff_=226.7nm) by GALEX (see Table 1). The reader is referred to Paper I (2009, Cat. J/ApJ/703/1569) for a more detailed description of the Spitzer data used here. Mid- and far-IR observations of the SINGS sample were carried out using the Spitzer Space Telescope (IRAC and MIPS). The HI Nearby Galaxy Survey (THINGS; Walter et al. 2008, Cat. J/AJ/136/2563) used the Very Large Array (VLA) to map HI 21cm line emission from 34 nearby (D&lt;15Mpc) galaxies, most of which were also targets of SINGS and the GALEX Nearby Galaxies Survey.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965#2</TD>
            <TD>2011-11-02T21:20:55Z</TD>
            <TD>#Extinction#Galaxies#Interstellar_Medium#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/701/1965&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1965</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1965 [table1]</TD>
            <TD>Radial dust properties of SINGS galaxies (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies. Eighteen SINGS galaxies were not suitable for our purposes and were excluded from the present study. Nearly all SINGS galaxies have been observed in the far-UV (FUV; {lambda}_eff_=151.6nm) and near-UV (NUV; {lambda}_eff_=226.7nm) by GALEX (see Table 1). The reader is referred to Paper I (2009, Cat. J/ApJ/703/1569) for a more detailed description of the Spitzer data used here. Mid- and far-IR observations of the SINGS sample were carried out using the Spitzer Space Telescope (IRAC and MIPS). The HI Nearby Galaxy Survey (THINGS; Walter et al. 2008, Cat. J/AJ/136/2563) used the Very Large Array (VLA) to map HI 21cm line emission from 34 nearby (D&lt;15Mpc) galaxies, most of which were also targets of SINGS and the GALEX Nearby Galaxies Survey.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965#table1</TD>
            <TD>2011-11-02T21:20:55Z</TD>
            <TD>#Extinction#Galaxies#Interstellar_Medium#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1965&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1965</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/701/1965 [1]</TD>
            <TD>Radial dust properties of SINGS galaxies (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies. Eighteen SINGS galaxies were not suitable for our purposes and were excluded from the present study. Nearly all SINGS galaxies have been observed in the far-UV (FUV; {lambda}_eff_=151.6nm) and near-UV (NUV; {lambda}_eff_=226.7nm) by GALEX (see Table 1). The reader is referred to Paper I (2009, Cat. J/ApJ/703/1569) for a more detailed description of the Spitzer data used here. Mid- and far-IR observations of the SINGS sample were carried out using the Spitzer Space Telescope (IRAC and MIPS). The HI Nearby Galaxy Survey (THINGS; Walter et al. 2008, Cat. J/AJ/136/2563) used the Very Large Array (VLA) to map HI 21cm line emission from 34 nearby (D&lt;15Mpc) galaxies, most of which were also targets of SINGS and the GALEX Nearby Galaxies Survey.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965#1</TD>
            <TD>2011-11-02T21:20:55Z</TD>
            <TD>#Extinction#Galaxies#Interstellar_Medium#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/701/1965</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1965</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/701/1965 [2]</TD>
            <TD>Radial dust properties of SINGS galaxies (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies. Eighteen SINGS galaxies were not suitable for our purposes and were excluded from the present study. Nearly all SINGS galaxies have been observed in the far-UV (FUV; {lambda}_eff_=151.6nm) and near-UV (NUV; {lambda}_eff_=226.7nm) by GALEX (see Table 1). The reader is referred to Paper I (2009, Cat. J/ApJ/703/1569) for a more detailed description of the Spitzer data used here. Mid- and far-IR observations of the SINGS sample were carried out using the Spitzer Space Telescope (IRAC and MIPS). The HI Nearby Galaxy Survey (THINGS; Walter et al. 2008, Cat. J/AJ/136/2563) used the Very Large Array (VLA) to map HI 21cm line emission from 34 nearby (D&lt;15Mpc) galaxies, most of which were also targets of SINGS and the GALEX Nearby Galaxies Survey.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965#2</TD>
            <TD>2011-11-02T21:20:55Z</TD>
            <TD>#Extinction#Galaxies#Interstellar_Medium#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/701/1965&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1965</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1965 [table1]</TD>
            <TD>Radial dust properties of SINGS galaxies (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies. Eighteen SINGS galaxies were not suitable for our purposes and were excluded from the present study. Nearly all SINGS galaxies have been observed in the far-UV (FUV; {lambda}_eff_=151.6nm) and near-UV (NUV; {lambda}_eff_=226.7nm) by GALEX (see Table 1). The reader is referred to Paper I (2009, Cat. J/ApJ/703/1569) for a more detailed description of the Spitzer data used here. Mid- and far-IR observations of the SINGS sample were carried out using the Spitzer Space Telescope (IRAC and MIPS). The HI Nearby Galaxy Survey (THINGS; Walter et al. 2008, Cat. J/AJ/136/2563) used the Very Large Array (VLA) to map HI 21cm line emission from 34 nearby (D&lt;15Mpc) galaxies, most of which were also targets of SINGS and the GALEX Nearby Galaxies Survey.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965#table1</TD>
            <TD>2011-11-02T21:20:55Z</TD>
            <TD>#Extinction#Galaxies#Interstellar_Medium#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1965</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1965&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1965</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/1569 [1]</TD>
            <TD>Radial distribution in SINGS galaxies. I. (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies selected to cover the range in morphological-type, luminosity and FIR/optical luminosity observed in the local universe. The GALEX mission has observed nearly all SINGS galaxies in the FUV and the near-UV. Optical images for the SINGS galaxies were taken at the Kitt Peak National Observatory (KPNO) 2.1m telescope and the Cerro Tololo Inter-American Observatory (CTIO) 1.5m telescope, using Harris BVRI filters. We finally opted for using images from the Sloan Digital Sky Survey (SDSS-DR6; Adelman-McCarthy et al. 2008, Cat. II/282; superseded by II/294) for as many galaxies as possible. Since the SINGS galaxies are too large to fit into a single Two Micron All Sky Survey (2MASS) scan, the corresponding mosaics were retrieved from the 2MASS Large Galaxy Atlas (LGA; Jarrett et al. 2003AJ....125..525J). Mid-IR images at 3.6, 4.5, 5.8, and 8.0um were obtained using the Infrared Array Camera (IRAC) on board Spitzer and MIPS for 24, 70 and 160um.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569#1</TD>
            <TD>2011-11-02T22:39:19Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/1569</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1569</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/1569 [2]</TD>
            <TD>Radial distribution in SINGS galaxies. I. (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies selected to cover the range in morphological-type, luminosity and FIR/optical luminosity observed in the local universe. The GALEX mission has observed nearly all SINGS galaxies in the FUV and the near-UV. Optical images for the SINGS galaxies were taken at the Kitt Peak National Observatory (KPNO) 2.1m telescope and the Cerro Tololo Inter-American Observatory (CTIO) 1.5m telescope, using Harris BVRI filters. We finally opted for using images from the Sloan Digital Sky Survey (SDSS-DR6; Adelman-McCarthy et al. 2008, Cat. II/282; superseded by II/294) for as many galaxies as possible. Since the SINGS galaxies are too large to fit into a single Two Micron All Sky Survey (2MASS) scan, the corresponding mosaics were retrieved from the 2MASS Large Galaxy Atlas (LGA; Jarrett et al. 2003AJ....125..525J). Mid-IR images at 3.6, 4.5, 5.8, and 8.0um were obtained using the Infrared Array Camera (IRAC) on board Spitzer and MIPS for 24, 70 and 160um.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569#2</TD>
            <TD>2011-11-02T22:39:19Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/1569&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1569</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/1569 [table1]</TD>
            <TD>Radial distribution in SINGS galaxies. I. (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies selected to cover the range in morphological-type, luminosity and FIR/optical luminosity observed in the local universe. The GALEX mission has observed nearly all SINGS galaxies in the FUV and the near-UV. Optical images for the SINGS galaxies were taken at the Kitt Peak National Observatory (KPNO) 2.1m telescope and the Cerro Tololo Inter-American Observatory (CTIO) 1.5m telescope, using Harris BVRI filters. We finally opted for using images from the Sloan Digital Sky Survey (SDSS-DR6; Adelman-McCarthy et al. 2008, Cat. II/282; superseded by II/294) for as many galaxies as possible. Since the SINGS galaxies are too large to fit into a single Two Micron All Sky Survey (2MASS) scan, the corresponding mosaics were retrieved from the 2MASS Large Galaxy Atlas (LGA; Jarrett et al. 2003AJ....125..525J). Mid-IR images at 3.6, 4.5, 5.8, and 8.0um were obtained using the Infrared Array Camera (IRAC) on board Spitzer and MIPS for 24, 70 and 160um.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569#table1</TD>
            <TD>2011-11-02T22:39:19Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/1569&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1569</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/1569 [1]</TD>
            <TD>Radial distribution in SINGS galaxies. I. (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies selected to cover the range in morphological-type, luminosity and FIR/optical luminosity observed in the local universe. The GALEX mission has observed nearly all SINGS galaxies in the FUV and the near-UV. Optical images for the SINGS galaxies were taken at the Kitt Peak National Observatory (KPNO) 2.1m telescope and the Cerro Tololo Inter-American Observatory (CTIO) 1.5m telescope, using Harris BVRI filters. We finally opted for using images from the Sloan Digital Sky Survey (SDSS-DR6; Adelman-McCarthy et al. 2008, Cat. II/282; superseded by II/294) for as many galaxies as possible. Since the SINGS galaxies are too large to fit into a single Two Micron All Sky Survey (2MASS) scan, the corresponding mosaics were retrieved from the 2MASS Large Galaxy Atlas (LGA; Jarrett et al. 2003AJ....125..525J). Mid-IR images at 3.6, 4.5, 5.8, and 8.0um were obtained using the Infrared Array Camera (IRAC) on board Spitzer and MIPS for 24, 70 and 160um.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569#1</TD>
            <TD>2011-11-02T22:39:19Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/1569</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1569</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/1569 [2]</TD>
            <TD>Radial distribution in SINGS galaxies. I. (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies selected to cover the range in morphological-type, luminosity and FIR/optical luminosity observed in the local universe. The GALEX mission has observed nearly all SINGS galaxies in the FUV and the near-UV. Optical images for the SINGS galaxies were taken at the Kitt Peak National Observatory (KPNO) 2.1m telescope and the Cerro Tololo Inter-American Observatory (CTIO) 1.5m telescope, using Harris BVRI filters. We finally opted for using images from the Sloan Digital Sky Survey (SDSS-DR6; Adelman-McCarthy et al. 2008, Cat. II/282; superseded by II/294) for as many galaxies as possible. Since the SINGS galaxies are too large to fit into a single Two Micron All Sky Survey (2MASS) scan, the corresponding mosaics were retrieved from the 2MASS Large Galaxy Atlas (LGA; Jarrett et al. 2003AJ....125..525J). Mid-IR images at 3.6, 4.5, 5.8, and 8.0um were obtained using the Infrared Array Camera (IRAC) on board Spitzer and MIPS for 24, 70 and 160um.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569#2</TD>
            <TD>2011-11-02T22:39:19Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/1569&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1569</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/1569 [table1]</TD>
            <TD>Radial distribution in SINGS galaxies. I. (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies selected to cover the range in morphological-type, luminosity and FIR/optical luminosity observed in the local universe. The GALEX mission has observed nearly all SINGS galaxies in the FUV and the near-UV. Optical images for the SINGS galaxies were taken at the Kitt Peak National Observatory (KPNO) 2.1m telescope and the Cerro Tololo Inter-American Observatory (CTIO) 1.5m telescope, using Harris BVRI filters. We finally opted for using images from the Sloan Digital Sky Survey (SDSS-DR6; Adelman-McCarthy et al. 2008, Cat. II/282; superseded by II/294) for as many galaxies as possible. Since the SINGS galaxies are too large to fit into a single Two Micron All Sky Survey (2MASS) scan, the corresponding mosaics were retrieved from the 2MASS Large Galaxy Atlas (LGA; Jarrett et al. 2003AJ....125..525J). Mid-IR images at 3.6, 4.5, 5.8, and 8.0um were obtained using the Infrared Array Camera (IRAC) on board Spitzer and MIPS for 24, 70 and 160um.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569#table1</TD>
            <TD>2011-11-02T22:39:19Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/1569&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1569</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/1569 [1]</TD>
            <TD>Radial distribution in SINGS galaxies. I. (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies selected to cover the range in morphological-type, luminosity and FIR/optical luminosity observed in the local universe. The GALEX mission has observed nearly all SINGS galaxies in the FUV and the near-UV. Optical images for the SINGS galaxies were taken at the Kitt Peak National Observatory (KPNO) 2.1m telescope and the Cerro Tololo Inter-American Observatory (CTIO) 1.5m telescope, using Harris BVRI filters. We finally opted for using images from the Sloan Digital Sky Survey (SDSS-DR6; Adelman-McCarthy et al. 2008, Cat. II/282; superseded by II/294) for as many galaxies as possible. Since the SINGS galaxies are too large to fit into a single Two Micron All Sky Survey (2MASS) scan, the corresponding mosaics were retrieved from the 2MASS Large Galaxy Atlas (LGA; Jarrett et al. 2003AJ....125..525J). Mid-IR images at 3.6, 4.5, 5.8, and 8.0um were obtained using the Infrared Array Camera (IRAC) on board Spitzer and MIPS for 24, 70 and 160um.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569#1</TD>
            <TD>2011-11-02T22:39:19Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/1569</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1569</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/1569 [2]</TD>
            <TD>Radial distribution in SINGS galaxies. I. (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies selected to cover the range in morphological-type, luminosity and FIR/optical luminosity observed in the local universe. The GALEX mission has observed nearly all SINGS galaxies in the FUV and the near-UV. Optical images for the SINGS galaxies were taken at the Kitt Peak National Observatory (KPNO) 2.1m telescope and the Cerro Tololo Inter-American Observatory (CTIO) 1.5m telescope, using Harris BVRI filters. We finally opted for using images from the Sloan Digital Sky Survey (SDSS-DR6; Adelman-McCarthy et al. 2008, Cat. II/282; superseded by II/294) for as many galaxies as possible. Since the SINGS galaxies are too large to fit into a single Two Micron All Sky Survey (2MASS) scan, the corresponding mosaics were retrieved from the 2MASS Large Galaxy Atlas (LGA; Jarrett et al. 2003AJ....125..525J). Mid-IR images at 3.6, 4.5, 5.8, and 8.0um were obtained using the Infrared Array Camera (IRAC) on board Spitzer and MIPS for 24, 70 and 160um.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569#2</TD>
            <TD>2011-11-02T22:39:19Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/1569&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1569</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/1569 [table1]</TD>
            <TD>Radial distribution in SINGS galaxies. I. (Munoz-Mateos+, 2009)</TD>
            <TD>The SINGS sample (Kennicutt et al. 2003PASP..115..928K) consists of 75 nearby galaxies selected to cover the range in morphological-type, luminosity and FIR/optical luminosity observed in the local universe. The GALEX mission has observed nearly all SINGS galaxies in the FUV and the near-UV. Optical images for the SINGS galaxies were taken at the Kitt Peak National Observatory (KPNO) 2.1m telescope and the Cerro Tololo Inter-American Observatory (CTIO) 1.5m telescope, using Harris BVRI filters. We finally opted for using images from the Sloan Digital Sky Survey (SDSS-DR6; Adelman-McCarthy et al. 2008, Cat. II/282; superseded by II/294) for as many galaxies as possible. Since the SINGS galaxies are too large to fit into a single Two Micron All Sky Survey (2MASS) scan, the corresponding mosaics were retrieved from the 2MASS Large Galaxy Atlas (LGA; Jarrett et al. 2003AJ....125..525J). Mid-IR images at 3.6, 4.5, 5.8, and 8.0um were obtained using the Infrared Array Camera (IRAC) on board Spitzer and MIPS for 24, 70 and 160um.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569#table1</TD>
            <TD>2011-11-02T22:39:19Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/1569</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/1569&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/1569</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/514/A3 [1]</TD>
            <TD>Star-galaxy separation in AKARI FIS All-Sky Survey (Pollo+, 2010)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3#1</TD>
            <TD>2012-10-18T11:16:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/514/A3</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A3</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/514/A3 [2]</TD>
            <TD>Star-galaxy separation in AKARI FIS All-Sky Survey (Pollo+, 2010)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3#2</TD>
            <TD>2012-10-18T11:16:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/514/A3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A3</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A3 [catalog]</TD>
            <TD>Star-galaxy separation in AKARI FIS All-Sky Survey (Pollo+, 2010)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3#catalog</TD>
            <TD>2012-10-18T11:16:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A3&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A3</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/533/A52 [1]</TD>
            <TD>X-ray monitoring of M31 novae (Henze+, 2011)</TD>
            <TD>Context. Classical novae (CNe) represent the major class of supersoft X-ray sources (SSSs) in the central region of the galaxy M31. We performed a dedicated monitoring of the M31 central region with XMM-Newton and Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009, respectively, to find SSS counterparts of CNe, determine the duration of their SSS phase, and derive physical outburst parameters. We systematically searched our data for X-ray counterparts of CNe, determined their X-ray light curves and characterised their spectra using blackbody fits and white dwarf (WD) atmosphere models. Additionally, we determined luminosity upper limits for all previously known X-ray emitting novae that are not detected any more and for all CNe in our field of view with optical outbursts between one year before the start of the X-ray monitoring (Oct 2006) and its end (Feb 2009).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52#1</TD>
            <TD>2011-11-04T14:21:21Z</TD>
            <TD>#Galaxies#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/533/A52</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A52</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/533/A52 [2]</TD>
            <TD>X-ray monitoring of M31 novae (Henze+, 2011)</TD>
            <TD>Context. Classical novae (CNe) represent the major class of supersoft X-ray sources (SSSs) in the central region of the galaxy M31. We performed a dedicated monitoring of the M31 central region with XMM-Newton and Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009, respectively, to find SSS counterparts of CNe, determine the duration of their SSS phase, and derive physical outburst parameters. We systematically searched our data for X-ray counterparts of CNe, determined their X-ray light curves and characterised their spectra using blackbody fits and white dwarf (WD) atmosphere models. Additionally, we determined luminosity upper limits for all previously known X-ray emitting novae that are not detected any more and for all CNe in our field of view with optical outbursts between one year before the start of the X-ray monitoring (Oct 2006) and its end (Feb 2009).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52#2</TD>
            <TD>2011-11-04T14:21:21Z</TD>
            <TD>#Galaxies#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/533/A52&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A52</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/533/A52 [table9]</TD>
            <TD>X-ray monitoring of M31 novae (Henze+, 2011)</TD>
            <TD>Context. Classical novae (CNe) represent the major class of supersoft X-ray sources (SSSs) in the central region of the galaxy M31. We performed a dedicated monitoring of the M31 central region with XMM-Newton and Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009, respectively, to find SSS counterparts of CNe, determine the duration of their SSS phase, and derive physical outburst parameters. We systematically searched our data for X-ray counterparts of CNe, determined their X-ray light curves and characterised their spectra using blackbody fits and white dwarf (WD) atmosphere models. Additionally, we determined luminosity upper limits for all previously known X-ray emitting novae that are not detected any more and for all CNe in our field of view with optical outbursts between one year before the start of the X-ray monitoring (Oct 2006) and its end (Feb 2009).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52#table9</TD>
            <TD>2011-11-04T14:21:21Z</TD>
            <TD>#Galaxies#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/533/A52&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A52</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/514/A3 [1]</TD>
            <TD>Star-galaxy separation in AKARI FIS All-Sky Survey (Pollo+, 2010)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3#1</TD>
            <TD>2012-10-18T11:16:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/514/A3</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A3</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/514/A3 [2]</TD>
            <TD>Star-galaxy separation in AKARI FIS All-Sky Survey (Pollo+, 2010)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3#2</TD>
            <TD>2012-10-18T11:16:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/514/A3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A3</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A3 [catalog]</TD>
            <TD>Star-galaxy separation in AKARI FIS All-Sky Survey (Pollo+, 2010)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3#catalog</TD>
            <TD>2012-10-18T11:16:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A3&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A3</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/533/A52 [1]</TD>
            <TD>X-ray monitoring of M31 novae (Henze+, 2011)</TD>
            <TD>Context. Classical novae (CNe) represent the major class of supersoft X-ray sources (SSSs) in the central region of the galaxy M31. We performed a dedicated monitoring of the M31 central region with XMM-Newton and Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009, respectively, to find SSS counterparts of CNe, determine the duration of their SSS phase, and derive physical outburst parameters. We systematically searched our data for X-ray counterparts of CNe, determined their X-ray light curves and characterised their spectra using blackbody fits and white dwarf (WD) atmosphere models. Additionally, we determined luminosity upper limits for all previously known X-ray emitting novae that are not detected any more and for all CNe in our field of view with optical outbursts between one year before the start of the X-ray monitoring (Oct 2006) and its end (Feb 2009).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52#1</TD>
            <TD>2011-11-04T14:21:21Z</TD>
            <TD>#Galaxies#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/533/A52</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A52</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/533/A52 [2]</TD>
            <TD>X-ray monitoring of M31 novae (Henze+, 2011)</TD>
            <TD>Context. Classical novae (CNe) represent the major class of supersoft X-ray sources (SSSs) in the central region of the galaxy M31. We performed a dedicated monitoring of the M31 central region with XMM-Newton and Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009, respectively, to find SSS counterparts of CNe, determine the duration of their SSS phase, and derive physical outburst parameters. We systematically searched our data for X-ray counterparts of CNe, determined their X-ray light curves and characterised their spectra using blackbody fits and white dwarf (WD) atmosphere models. Additionally, we determined luminosity upper limits for all previously known X-ray emitting novae that are not detected any more and for all CNe in our field of view with optical outbursts between one year before the start of the X-ray monitoring (Oct 2006) and its end (Feb 2009).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52#2</TD>
            <TD>2011-11-04T14:21:21Z</TD>
            <TD>#Galaxies#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/533/A52&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A52</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/533/A52 [table9]</TD>
            <TD>X-ray monitoring of M31 novae (Henze+, 2011)</TD>
            <TD>Context. Classical novae (CNe) represent the major class of supersoft X-ray sources (SSSs) in the central region of the galaxy M31. We performed a dedicated monitoring of the M31 central region with XMM-Newton and Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009, respectively, to find SSS counterparts of CNe, determine the duration of their SSS phase, and derive physical outburst parameters. We systematically searched our data for X-ray counterparts of CNe, determined their X-ray light curves and characterised their spectra using blackbody fits and white dwarf (WD) atmosphere models. Additionally, we determined luminosity upper limits for all previously known X-ray emitting novae that are not detected any more and for all CNe in our field of view with optical outbursts between one year before the start of the X-ray monitoring (Oct 2006) and its end (Feb 2009).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52#table9</TD>
            <TD>2011-11-04T14:21:21Z</TD>
            <TD>#Galaxies#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/533/A52&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A52</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/514/A3 [1]</TD>
            <TD>Star-galaxy separation in AKARI FIS All-Sky Survey (Pollo+, 2010)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3#1</TD>
            <TD>2012-10-18T11:16:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/514/A3</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A3</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/514/A3 [2]</TD>
            <TD>Star-galaxy separation in AKARI FIS All-Sky Survey (Pollo+, 2010)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3#2</TD>
            <TD>2012-10-18T11:16:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/514/A3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A3</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A3 [catalog]</TD>
            <TD>Star-galaxy separation in AKARI FIS All-Sky Survey (Pollo+, 2010)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3#catalog</TD>
            <TD>2012-10-18T11:16:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A3&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A3</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/533/A52 [1]</TD>
            <TD>X-ray monitoring of M31 novae (Henze+, 2011)</TD>
            <TD>Context. Classical novae (CNe) represent the major class of supersoft X-ray sources (SSSs) in the central region of the galaxy M31. We performed a dedicated monitoring of the M31 central region with XMM-Newton and Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009, respectively, to find SSS counterparts of CNe, determine the duration of their SSS phase, and derive physical outburst parameters. We systematically searched our data for X-ray counterparts of CNe, determined their X-ray light curves and characterised their spectra using blackbody fits and white dwarf (WD) atmosphere models. Additionally, we determined luminosity upper limits for all previously known X-ray emitting novae that are not detected any more and for all CNe in our field of view with optical outbursts between one year before the start of the X-ray monitoring (Oct 2006) and its end (Feb 2009).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52#1</TD>
            <TD>2011-11-04T14:21:21Z</TD>
            <TD>#Galaxies#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/533/A52</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A52</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/533/A52 [2]</TD>
            <TD>X-ray monitoring of M31 novae (Henze+, 2011)</TD>
            <TD>Context. Classical novae (CNe) represent the major class of supersoft X-ray sources (SSSs) in the central region of the galaxy M31. We performed a dedicated monitoring of the M31 central region with XMM-Newton and Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009, respectively, to find SSS counterparts of CNe, determine the duration of their SSS phase, and derive physical outburst parameters. We systematically searched our data for X-ray counterparts of CNe, determined their X-ray light curves and characterised their spectra using blackbody fits and white dwarf (WD) atmosphere models. Additionally, we determined luminosity upper limits for all previously known X-ray emitting novae that are not detected any more and for all CNe in our field of view with optical outbursts between one year before the start of the X-ray monitoring (Oct 2006) and its end (Feb 2009).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52#2</TD>
            <TD>2011-11-04T14:21:21Z</TD>
            <TD>#Galaxies#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/533/A52&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A52</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/533/A52 [table9]</TD>
            <TD>X-ray monitoring of M31 novae (Henze+, 2011)</TD>
            <TD>Context. Classical novae (CNe) represent the major class of supersoft X-ray sources (SSSs) in the central region of the galaxy M31. We performed a dedicated monitoring of the M31 central region with XMM-Newton and Chandra between Nov 2007 and Feb 2008 and between Nov 2008 and Feb 2009, respectively, to find SSS counterparts of CNe, determine the duration of their SSS phase, and derive physical outburst parameters. We systematically searched our data for X-ray counterparts of CNe, determined their X-ray light curves and characterised their spectra using blackbody fits and white dwarf (WD) atmosphere models. Additionally, we determined luminosity upper limits for all previously known X-ray emitting novae that are not detected any more and for all CNe in our field of view with optical outbursts between one year before the start of the X-ray monitoring (Oct 2006) and its end (Feb 2009).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52#table9</TD>
            <TD>2011-11-04T14:21:21Z</TD>
            <TD>#Galaxies#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A52</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/533/A52&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A52</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GLXSDSSQSO [1]</TD>
            <TD>GALEX/SDSS Quasar Catalog</TD>
            <TD>This table contains the result of an analysis of the broad-band UV and optical properties of z ~&lt; 3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles and listed in this table, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7 arcseconds. Most of the DR3 sample quasars are detected in the near-UV until z ~ 1.7, with the near-UV detection fraction dropping to ~50% by z ~ 2. Statistical tests performed on the distributions of nondetections indicate that the optically selected quasars missed in the UV tend to be optically faint or at high redshift. The GALEX positions are shown to be consistent with the SDSS astrometry to within an rms scatter of 0.6 - 0.7 arcsecs in each coordinate, and the empirically determined photometric errors from multiepoch GALEX observations significantly exceed the Poissonian errors quoted in the GR1 object catalogs. The UV-detected quasars are well separated from stars in UV-optical color-color space, with the UV-optical relative colors suggesting a marginally detected population of reddened objects due to absorption along the line of sight or dust associated with the quasar. The resulting spectral energy distributions (SEDs) cover ~350 - 9000 Angstroms (rest frame), where the overall median SED peaks near the Lyman-Alpha emission line, as found in other UV quasar studies. The large sample size allows the authors to construct median SEDs in small bins of redshift and luminosity, and they find that the median SED becomes harder (bluer) at UV wavelengths for quasars with lower continuum luminosity. The detected UV-optical flux as a function of redshift is qualitatively consistent with attenuation by intervening Lyman-absorbing clouds.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqso#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Quasar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqso</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=glxsdssqso&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqso.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GLXSDSSQSO [2]</TD>
            <TD>GALEX/SDSS Quasar Catalog</TD>
            <TD>This table contains the result of an analysis of the broad-band UV and optical properties of z ~&lt; 3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles and listed in this table, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7 arcseconds. Most of the DR3 sample quasars are detected in the near-UV until z ~ 1.7, with the near-UV detection fraction dropping to ~50% by z ~ 2. Statistical tests performed on the distributions of nondetections indicate that the optically selected quasars missed in the UV tend to be optically faint or at high redshift. The GALEX positions are shown to be consistent with the SDSS astrometry to within an rms scatter of 0.6 - 0.7 arcsecs in each coordinate, and the empirically determined photometric errors from multiepoch GALEX observations significantly exceed the Poissonian errors quoted in the GR1 object catalogs. The UV-detected quasars are well separated from stars in UV-optical color-color space, with the UV-optical relative colors suggesting a marginally detected population of reddened objects due to absorption along the line of sight or dust associated with the quasar. The resulting spectral energy distributions (SEDs) cover ~350 - 9000 Angstroms (rest frame), where the overall median SED peaks near the Lyman-Alpha emission line, as found in other UV quasar studies. The large sample size allows the authors to construct median SEDs in small bins of redshift and luminosity, and they find that the median SED becomes harder (bluer) at UV wavelengths for quasars with lower continuum luminosity. The detected UV-optical flux as a function of redshift is qualitatively consistent with attenuation by intervening Lyman-absorbing clouds.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqso#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Quasar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqso</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=glxsdssqso&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqso.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GLXSDSSQSO [3]</TD>
            <TD>GALEX/SDSS Quasar Catalog</TD>
            <TD>This table contains the result of an analysis of the broad-band UV and optical properties of z ~&lt; 3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles and listed in this table, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7 arcseconds. Most of the DR3 sample quasars are detected in the near-UV until z ~ 1.7, with the near-UV detection fraction dropping to ~50% by z ~ 2. Statistical tests performed on the distributions of nondetections indicate that the optically selected quasars missed in the UV tend to be optically faint or at high redshift. The GALEX positions are shown to be consistent with the SDSS astrometry to within an rms scatter of 0.6 - 0.7 arcsecs in each coordinate, and the empirically determined photometric errors from multiepoch GALEX observations significantly exceed the Poissonian errors quoted in the GR1 object catalogs. The UV-detected quasars are well separated from stars in UV-optical color-color space, with the UV-optical relative colors suggesting a marginally detected population of reddened objects due to absorption along the line of sight or dust associated with the quasar. The resulting spectral energy distributions (SEDs) cover ~350 - 9000 Angstroms (rest frame), where the overall median SED peaks near the Lyman-Alpha emission line, as found in other UV quasar studies. The large sample size allows the authors to construct median SEDs in small bins of redshift and luminosity, and they find that the median SED becomes harder (bluer) at UV wavelengths for quasars with lower continuum luminosity. The detected UV-optical flux as a function of redshift is qualitatively consistent with attenuation by intervening Lyman-absorbing clouds.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqso#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Quasar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqso</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_glxsdssqso&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqso.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/4795 [1]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#1</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/4795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/4795 [2]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#2</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4795 [table3]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#table3</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4795 [table2]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#table2</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4795 [table1]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#table1</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/123/115 [1]</TD>
            <TD>Variables stars in Palomar-Groningen field 3 (Ng+ 1997)</TD>
            <TD>A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&amp;AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115#1</TD>
            <TD>2011-09-14T18:45:32Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/123/115</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/115</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/123/115 [2]</TD>
            <TD>Variables stars in Palomar-Groningen field 3 (Ng+ 1997)</TD>
            <TD>A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&amp;AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115#2</TD>
            <TD>2011-09-14T18:45:32Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/123/115&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/123/115 [table1]</TD>
            <TD>Variables stars in Palomar-Groningen field 3 (Ng+ 1997)</TD>
            <TD>A catalogue is presented with variable (RR Lyrae, semiregular and Mira) stars located inside field #3 (PG3) of the Palomar-Groningen Survey at the outer edge of the Sagittarius dwarf galaxy. One of the semiregular variables is a carbon star, comparable with those found by Azzopardi et al. (1991A&amp;AS...88..265A). Serendipity provides the suggestion, that their carbon stars might not be located inside, but behind the bulge on the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115#table1</TD>
            <TD>2011-09-14T18:45:32Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/123/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/115</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/123/529 [1]</TD>
            <TD>UV-excess quasar candidates around NGC 450 (Gosset+ 1997)</TD>
            <TD>We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529#1</TD>
            <TD>2011-09-14T18:45:47Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/123/529</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/529</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/123/529 [2]</TD>
            <TD>UV-excess quasar candidates around NGC 450 (Gosset+ 1997)</TD>
            <TD>We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529#2</TD>
            <TD>2011-09-14T18:45:47Z</TD>
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            <TD>02-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/123/529&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/529</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/123/529 [table6]</TD>
            <TD>UV-excess quasar candidates around NGC 450 (Gosset+ 1997)</TD>
            <TD>We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529#table6</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/123/529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/529</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/4795 [1]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#1</TD>
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            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/4795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/4795 [2]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#2</TD>
            <TD>2011-11-16T16:27:25Z</TD>
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            <TD>#Catalog#</TD>
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            <TD />
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            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4795 [table3]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#table3</TD>
            <TD>2011-11-16T16:27:25Z</TD>
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            <TD>23-Oct-2011</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4795 [table2]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#table2</TD>
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            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4795 [table1]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#table1</TD>
            <TD>2011-11-16T16:27:25Z</TD>
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            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>Hickson Group [1]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Catalog</TD>
            <TD>The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcg#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcg</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=hcg&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcg.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Hickson Group [2]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Catalog</TD>
            <TD>The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcg#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hcg&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Hickson Group [3]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Catalog</TD>
            <TD>The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcg#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hcg&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/123/529 [1]</TD>
            <TD>UV-excess quasar candidates around NGC 450 (Gosset+ 1997)</TD>
            <TD>We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529#1</TD>
            <TD>2011-09-14T18:45:47Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/123/529</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/529</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/123/529 [2]</TD>
            <TD>UV-excess quasar candidates around NGC 450 (Gosset+ 1997)</TD>
            <TD>We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529#2</TD>
            <TD>2011-09-14T18:45:47Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/123/529&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/123/529 [table6]</TD>
            <TD>UV-excess quasar candidates around NGC 450 (Gosset+ 1997)</TD>
            <TD>We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529#table6</TD>
            <TD>2011-09-14T18:45:47Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/123/529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/529</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/1975 [1]</TD>
            <TD>Normal spiral galaxies optical and UV photometry (Smith+, 2010)</TD>
            <TD>We compare the UV-optical colors of a well-defined set of optically selected pre-merger interacting galaxy pairs with those of normal spirals. The shorter wavelength colors show a larger dispersion for the interacting galaxies than for the spirals. This result can best be explained by higher star formation rates on average in the interacting galaxies, combined with higher extinctions on average. This is consistent with earlier studies which found that the star formation in interacting galaxies tends to be more centrally concentrated than in normal spirals, perhaps due to gas being driven into the center by the interaction. As noted in earlier studies, there is a large variation from galaxy to galaxy in the implied star formation rates of the interacting galaxies, with some galaxies having enhanced rates but others being fairly quiescent.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975#1</TD>
            <TD>2012-10-23T13:47:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/1975</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1975</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/1975 [2]</TD>
            <TD>Normal spiral galaxies optical and UV photometry (Smith+, 2010)</TD>
            <TD>We compare the UV-optical colors of a well-defined set of optically selected pre-merger interacting galaxy pairs with those of normal spirals. The shorter wavelength colors show a larger dispersion for the interacting galaxies than for the spirals. This result can best be explained by higher star formation rates on average in the interacting galaxies, combined with higher extinctions on average. This is consistent with earlier studies which found that the star formation in interacting galaxies tends to be more centrally concentrated than in normal spirals, perhaps due to gas being driven into the center by the interaction. As noted in earlier studies, there is a large variation from galaxy to galaxy in the implied star formation rates of the interacting galaxies, with some galaxies having enhanced rates but others being fairly quiescent.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975#2</TD>
            <TD>2012-10-23T13:47:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/1975&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1975</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1975 [table1]</TD>
            <TD>Normal spiral galaxies optical and UV photometry (Smith+, 2010)</TD>
            <TD>We compare the UV-optical colors of a well-defined set of optically selected pre-merger interacting galaxy pairs with those of normal spirals. The shorter wavelength colors show a larger dispersion for the interacting galaxies than for the spirals. This result can best be explained by higher star formation rates on average in the interacting galaxies, combined with higher extinctions on average. This is consistent with earlier studies which found that the star formation in interacting galaxies tends to be more centrally concentrated than in normal spirals, perhaps due to gas being driven into the center by the interaction. As noted in earlier studies, there is a large variation from galaxy to galaxy in the implied star formation rates of the interacting galaxies, with some galaxies having enhanced rates but others being fairly quiescent.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975#table1</TD>
            <TD>2012-10-23T13:47:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1975&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1975</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Hickson Group [1]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Catalog</TD>
            <TD>The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcg#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcg</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=hcg&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcg.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Hickson Group [2]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Catalog</TD>
            <TD>The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcg#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hcg&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Hickson Group [3]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Catalog</TD>
            <TD>The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcg#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hcg&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/123/529 [1]</TD>
            <TD>UV-excess quasar candidates around NGC 450 (Gosset+ 1997)</TD>
            <TD>We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529#1</TD>
            <TD>2011-09-14T18:45:47Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/123/529</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/529</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/123/529 [2]</TD>
            <TD>UV-excess quasar candidates around NGC 450 (Gosset+ 1997)</TD>
            <TD>We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529#2</TD>
            <TD>2011-09-14T18:45:47Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/123/529&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/529</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/123/529 [table6]</TD>
            <TD>UV-excess quasar candidates around NGC 450 (Gosset+ 1997)</TD>
            <TD>We describe the results of a survey for moderately bright quasars performed in a 20.6-square-degree field around the galaxy NGC 450. The quasar candidates we re-selected on the basis of their ultraviolet excess: by comparative visual inspection of the double image of each single object on a U/B dual-exposure Schmidt photographic plate, 95 primary and 45 secondary quasar candidates were selected on the basis of their U image being too bright. The spectroscopic identification of the primary candidates led to the discovery of 59 bona fide quasars (out of which 6 were previously known). The Palomar Schmidt plate was digitised using the MAMA measuring machine and the outcoming data reduced using ad hoc procedures. A photometric calibration allowed us to derive values for the limiting magnitudes and for the U-B index selection threshold of the survey. A catalogue containing 60 quasars is presented with accurate positions, magnitudes and additional information such as redshifts. We studied the spatial distribution of the objects and detected, for the quasars of our sample, a significant deviation from randomness in the form of a propensity to cluster in pairs on the celestial sphere with a typical scale of about 10arcmin. We also formally detected a tendency towards a 3-D clustering, but this result is induced by a single pair of quasars. A forthcoming paper will deal with a similar work performed in a field around NGC 520; the latter field is located directly to the North of the present one and slightly overlaps it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529#table6</TD>
            <TD>2011-09-14T18:45:47Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/123/529</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/123/529&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/123/529</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/4795 [1]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#1</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/4795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/4795 [2]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#2</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4795 [table3]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#table3</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4795 [table2]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#table2</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4795 [table1]</TD>
            <TD>Dynamical state of brightest cluster galaxies (Coziol+, 2009)</TD>
            <TD>A large sample of Abell clusters of galaxies, selected for the likely presence of a dominant galaxy, is used to study the dynamical properties of the brightest cluster members (BCMs). From visual inspection of Digitized Sky Survey images combined with redshift information we identify 1426 candidate BCMs located in 1221 different redshift components associated with 1169 different Abell clusters. This is the largest sample published so far of such galaxies. From our own morphological classification we find that ~92% of the BCMs in our sample are early-type galaxies and 48% are of cD type. We confirm what was previously observed based on much smaller samples, namely, that a large fraction of BCMs have significant peculiar velocities. From a subsample of 452 clusters having at least 10 measured radial velocities, we estimate a median BCM peculiar velocity of 32% of their host clusters' radial velocity dispersion. This suggests that most BCMs are not at rest in the potential well of their clusters. This phenomenon is common to galaxy clusters in our sample, and not a special trait of clusters hosting cD galaxies. We show that the peculiar velocity of the BCM is independent of cluster richness and only slightly dependent on the Bautz-Morgan type. We also find a weak trend for the peculiar velocity to rise with the cluster velocity dispersion. The strongest dependence is with the morphological type of the BCM: cD galaxies tend to have lower relative peculiar velocities than elliptical galaxies. This result points to a connection between the formation of the BCMs and that of their clusters. Our data are qualitatively consistent with the merging-groups scenario, where BCMs in clusters formed first in smaller subsystems comparable to compact groups of galaxies. In this scenario, clusters would have formed recently from the mergers of many such groups and would still be in a dynamically unrelaxed state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795#table1</TD>
            <TD>2011-11-16T16:27:25Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Hickson Group [1]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Catalog</TD>
            <TD>The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcg#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcg</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=hcg&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcg.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Hickson Group [2]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Catalog</TD>
            <TD>The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcg#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hcg&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Hickson Group [3]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Catalog</TD>
            <TD>The HCG database table is based on the Hickson Catalog, which is a list of 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Dynamical parameters which were derived for 92 of the 100 groups are also included in the database. (Note that the Hubble constant was assumed to be Ho = 100 km/s/Mpc.) This database table essentially contains the information given in Table 1 of Hickson, P. (1982, ApJ, 255, 382) and Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353). Consequently, the information on individual galaxies in the Hickson groups that is also given in these references, e.g., in Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCG database table; however, the latter data can be found in the related HEASARC database table HCGGALAXY.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcg#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hcg&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/73/661 [1]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#1</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/73/661</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/73/661 [2]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#2</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/73/661&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/73/661 [table2]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#table2</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/73/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/73/661 [table1]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#table1</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/73/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/702/506 [1]</TD>
            <TD>The Clowes-Campusano LQG Survey. I. (Haberzettl+, 2009)</TD>
            <TD>We observed part of the Clowes-Campusano Large Quasar Group (CCLQG), it contains at least 18 bright quasars at 1.2&lt;z&lt;1.5 and a spatial overdensity of 3 for B_J_&lt;=20.0mag (Clowes &amp; Campusano 1991, Cat. J/MNRAS/249/218). The CCLQG covers ~2.5degx5deg (~120x240h^-2^Mpc^2^) and is 590h^-1^Mpc deep. For this study we have imaged two slightly overlapping 1.2deg fields within the CCLQG in the far-UV ({lambda}_eff_=1538.6{AA}) and near-UV ({lambda}_eff_=2315.7{AA}) filter bands, using the UV satellite GALEX (Galaxy Evolution Explorer). The observations were part of the Guest Investigator program, cycle 1 (October 2004 - September 2005) proposal 35.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506#1</TD>
            <TD>2011-11-20T12:09:51Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/702/506</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/506</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/702/506 [2]</TD>
            <TD>The Clowes-Campusano LQG Survey. I. (Haberzettl+, 2009)</TD>
            <TD>We observed part of the Clowes-Campusano Large Quasar Group (CCLQG), it contains at least 18 bright quasars at 1.2&lt;z&lt;1.5 and a spatial overdensity of 3 for B_J_&lt;=20.0mag (Clowes &amp; Campusano 1991, Cat. J/MNRAS/249/218). The CCLQG covers ~2.5degx5deg (~120x240h^-2^Mpc^2^) and is 590h^-1^Mpc deep. For this study we have imaged two slightly overlapping 1.2deg fields within the CCLQG in the far-UV ({lambda}_eff_=1538.6{AA}) and near-UV ({lambda}_eff_=2315.7{AA}) filter bands, using the UV satellite GALEX (Galaxy Evolution Explorer). The observations were part of the Guest Investigator program, cycle 1 (October 2004 - September 2005) proposal 35.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506#2</TD>
            <TD>2011-11-20T12:09:51Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/702/506&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/506</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/506 [table2]</TD>
            <TD>The Clowes-Campusano LQG Survey. I. (Haberzettl+, 2009)</TD>
            <TD>We observed part of the Clowes-Campusano Large Quasar Group (CCLQG), it contains at least 18 bright quasars at 1.2&lt;z&lt;1.5 and a spatial overdensity of 3 for B_J_&lt;=20.0mag (Clowes &amp; Campusano 1991, Cat. J/MNRAS/249/218). The CCLQG covers ~2.5degx5deg (~120x240h^-2^Mpc^2^) and is 590h^-1^Mpc deep. For this study we have imaged two slightly overlapping 1.2deg fields within the CCLQG in the far-UV ({lambda}_eff_=1538.6{AA}) and near-UV ({lambda}_eff_=2315.7{AA}) filter bands, using the UV satellite GALEX (Galaxy Evolution Explorer). The observations were part of the Guest Investigator program, cycle 1 (October 2004 - September 2005) proposal 35.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506#table2</TD>
            <TD>2011-11-20T12:09:51Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/506&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/506</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>HM XRB [1]</TD>
            <TD>Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)</TD>
            <TD>This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz&lt;/a&gt; Individual notes on each HMXB are available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/hmxbcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hmxbcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=hmxbcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/hmxbcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>HM XRB [2]</TD>
            <TD>Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)</TD>
            <TD>This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz&lt;/a&gt; Individual notes on each HMXB are available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/hmxbcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hmxbcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/hmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>HM XRB [3]</TD>
            <TD>Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)</TD>
            <TD>This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz&lt;/a&gt; Individual notes on each HMXB are available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/hmxbcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hmxbcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/hmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/702/506 [1]</TD>
            <TD>The Clowes-Campusano LQG Survey. I. (Haberzettl+, 2009)</TD>
            <TD>We observed part of the Clowes-Campusano Large Quasar Group (CCLQG), it contains at least 18 bright quasars at 1.2&lt;z&lt;1.5 and a spatial overdensity of 3 for B_J_&lt;=20.0mag (Clowes &amp; Campusano 1991, Cat. J/MNRAS/249/218). The CCLQG covers ~2.5degx5deg (~120x240h^-2^Mpc^2^) and is 590h^-1^Mpc deep. For this study we have imaged two slightly overlapping 1.2deg fields within the CCLQG in the far-UV ({lambda}_eff_=1538.6{AA}) and near-UV ({lambda}_eff_=2315.7{AA}) filter bands, using the UV satellite GALEX (Galaxy Evolution Explorer). The observations were part of the Guest Investigator program, cycle 1 (October 2004 - September 2005) proposal 35.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506#1</TD>
            <TD>2011-11-20T12:09:51Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/702/506</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/506</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/702/506 [2]</TD>
            <TD>The Clowes-Campusano LQG Survey. I. (Haberzettl+, 2009)</TD>
            <TD>We observed part of the Clowes-Campusano Large Quasar Group (CCLQG), it contains at least 18 bright quasars at 1.2&lt;z&lt;1.5 and a spatial overdensity of 3 for B_J_&lt;=20.0mag (Clowes &amp; Campusano 1991, Cat. J/MNRAS/249/218). The CCLQG covers ~2.5degx5deg (~120x240h^-2^Mpc^2^) and is 590h^-1^Mpc deep. For this study we have imaged two slightly overlapping 1.2deg fields within the CCLQG in the far-UV ({lambda}_eff_=1538.6{AA}) and near-UV ({lambda}_eff_=2315.7{AA}) filter bands, using the UV satellite GALEX (Galaxy Evolution Explorer). The observations were part of the Guest Investigator program, cycle 1 (October 2004 - September 2005) proposal 35.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506#2</TD>
            <TD>2011-11-20T12:09:51Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/702/506&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/506</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/506 [table2]</TD>
            <TD>The Clowes-Campusano LQG Survey. I. (Haberzettl+, 2009)</TD>
            <TD>We observed part of the Clowes-Campusano Large Quasar Group (CCLQG), it contains at least 18 bright quasars at 1.2&lt;z&lt;1.5 and a spatial overdensity of 3 for B_J_&lt;=20.0mag (Clowes &amp; Campusano 1991, Cat. J/MNRAS/249/218). The CCLQG covers ~2.5degx5deg (~120x240h^-2^Mpc^2^) and is 590h^-1^Mpc deep. For this study we have imaged two slightly overlapping 1.2deg fields within the CCLQG in the far-UV ({lambda}_eff_=1538.6{AA}) and near-UV ({lambda}_eff_=2315.7{AA}) filter bands, using the UV satellite GALEX (Galaxy Evolution Explorer). The observations were part of the Guest Investigator program, cycle 1 (October 2004 - September 2005) proposal 35.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506#table2</TD>
            <TD>2011-11-20T12:09:51Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/506&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/506</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>HM XRB [1]</TD>
            <TD>Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)</TD>
            <TD>This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz&lt;/a&gt; Individual notes on each HMXB are available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/hmxbcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hmxbcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=hmxbcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/hmxbcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>HM XRB [2]</TD>
            <TD>Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)</TD>
            <TD>This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz&lt;/a&gt; Individual notes on each HMXB are available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/hmxbcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hmxbcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/hmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>HM XRB [3]</TD>
            <TD>Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)</TD>
            <TD>This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz&lt;/a&gt; Individual notes on each HMXB are available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/hmxbcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hmxbcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/hmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/1975 [1]</TD>
            <TD>Normal spiral galaxies optical and UV photometry (Smith+, 2010)</TD>
            <TD>We compare the UV-optical colors of a well-defined set of optically selected pre-merger interacting galaxy pairs with those of normal spirals. The shorter wavelength colors show a larger dispersion for the interacting galaxies than for the spirals. This result can best be explained by higher star formation rates on average in the interacting galaxies, combined with higher extinctions on average. This is consistent with earlier studies which found that the star formation in interacting galaxies tends to be more centrally concentrated than in normal spirals, perhaps due to gas being driven into the center by the interaction. As noted in earlier studies, there is a large variation from galaxy to galaxy in the implied star formation rates of the interacting galaxies, with some galaxies having enhanced rates but others being fairly quiescent.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975#1</TD>
            <TD>2012-10-23T13:47:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/1975</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1975</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/1975 [2]</TD>
            <TD>Normal spiral galaxies optical and UV photometry (Smith+, 2010)</TD>
            <TD>We compare the UV-optical colors of a well-defined set of optically selected pre-merger interacting galaxy pairs with those of normal spirals. The shorter wavelength colors show a larger dispersion for the interacting galaxies than for the spirals. This result can best be explained by higher star formation rates on average in the interacting galaxies, combined with higher extinctions on average. This is consistent with earlier studies which found that the star formation in interacting galaxies tends to be more centrally concentrated than in normal spirals, perhaps due to gas being driven into the center by the interaction. As noted in earlier studies, there is a large variation from galaxy to galaxy in the implied star formation rates of the interacting galaxies, with some galaxies having enhanced rates but others being fairly quiescent.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975#2</TD>
            <TD>2012-10-23T13:47:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/1975&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1975</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1975 [table1]</TD>
            <TD>Normal spiral galaxies optical and UV photometry (Smith+, 2010)</TD>
            <TD>We compare the UV-optical colors of a well-defined set of optically selected pre-merger interacting galaxy pairs with those of normal spirals. The shorter wavelength colors show a larger dispersion for the interacting galaxies than for the spirals. This result can best be explained by higher star formation rates on average in the interacting galaxies, combined with higher extinctions on average. This is consistent with earlier studies which found that the star formation in interacting galaxies tends to be more centrally concentrated than in normal spirals, perhaps due to gas being driven into the center by the interaction. As noted in earlier studies, there is a large variation from galaxy to galaxy in the implied star formation rates of the interacting galaxies, with some galaxies having enhanced rates but others being fairly quiescent.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975#table1</TD>
            <TD>2012-10-23T13:47:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1975&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1975</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>HM XRB [1]</TD>
            <TD>Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)</TD>
            <TD>This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz&lt;/a&gt; Individual notes on each HMXB are available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/hmxbcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hmxbcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=hmxbcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/hmxbcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>HM XRB [2]</TD>
            <TD>Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)</TD>
            <TD>This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz&lt;/a&gt; Individual notes on each HMXB are available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/hmxbcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hmxbcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/hmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>HM XRB [3]</TD>
            <TD>Catalog of High-Mass X-Ray Binaries in the Galaxy (4th Ed.)</TD>
            <TD>This table contains the 4th edition of the Catalog of High-Mass X-Ray Binaries (HMXBs) in the Galaxy. The catalog contains source name(s), coordinates, finding charts, X-ray luminosities, system parameters, and stellar parameters of the components and other characteristic properties for 114 HMXBs, together with a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is noted. Literature published before 1 October 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/refs.dat.gz&lt;/a&gt; Individual notes on each HMXB are available at the URL &lt;a href="ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz"&gt;ftp://cdsweb.u-strasbg.fr/cats/J/A+A/455/1165/notes.dat.gz&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/hmxbcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hmxbcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/hmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/1975 [1]</TD>
            <TD>Normal spiral galaxies optical and UV photometry (Smith+, 2010)</TD>
            <TD>We compare the UV-optical colors of a well-defined set of optically selected pre-merger interacting galaxy pairs with those of normal spirals. The shorter wavelength colors show a larger dispersion for the interacting galaxies than for the spirals. This result can best be explained by higher star formation rates on average in the interacting galaxies, combined with higher extinctions on average. This is consistent with earlier studies which found that the star formation in interacting galaxies tends to be more centrally concentrated than in normal spirals, perhaps due to gas being driven into the center by the interaction. As noted in earlier studies, there is a large variation from galaxy to galaxy in the implied star formation rates of the interacting galaxies, with some galaxies having enhanced rates but others being fairly quiescent.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975#1</TD>
            <TD>2012-10-23T13:47:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/1975</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1975</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/1975 [2]</TD>
            <TD>Normal spiral galaxies optical and UV photometry (Smith+, 2010)</TD>
            <TD>We compare the UV-optical colors of a well-defined set of optically selected pre-merger interacting galaxy pairs with those of normal spirals. The shorter wavelength colors show a larger dispersion for the interacting galaxies than for the spirals. This result can best be explained by higher star formation rates on average in the interacting galaxies, combined with higher extinctions on average. This is consistent with earlier studies which found that the star formation in interacting galaxies tends to be more centrally concentrated than in normal spirals, perhaps due to gas being driven into the center by the interaction. As noted in earlier studies, there is a large variation from galaxy to galaxy in the implied star formation rates of the interacting galaxies, with some galaxies having enhanced rates but others being fairly quiescent.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975#2</TD>
            <TD>2012-10-23T13:47:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/1975&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1975</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1975 [table1]</TD>
            <TD>Normal spiral galaxies optical and UV photometry (Smith+, 2010)</TD>
            <TD>We compare the UV-optical colors of a well-defined set of optically selected pre-merger interacting galaxy pairs with those of normal spirals. The shorter wavelength colors show a larger dispersion for the interacting galaxies than for the spirals. This result can best be explained by higher star formation rates on average in the interacting galaxies, combined with higher extinctions on average. This is consistent with earlier studies which found that the star formation in interacting galaxies tends to be more centrally concentrated than in normal spirals, perhaps due to gas being driven into the center by the interaction. As noted in earlier studies, there is a large variation from galaxy to galaxy in the implied star formation rates of the interacting galaxies, with some galaxies having enhanced rates but others being fairly quiescent.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975#table1</TD>
            <TD>2012-10-23T13:47:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1975</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1975&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1975</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/73/661 [1]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#1</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/73/661</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/73/661 [2]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#2</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/73/661&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/73/661 [table2]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#table2</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/73/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/73/661 [table1]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#table1</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/73/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/702/506 [1]</TD>
            <TD>The Clowes-Campusano LQG Survey. I. (Haberzettl+, 2009)</TD>
            <TD>We observed part of the Clowes-Campusano Large Quasar Group (CCLQG), it contains at least 18 bright quasars at 1.2&lt;z&lt;1.5 and a spatial overdensity of 3 for B_J_&lt;=20.0mag (Clowes &amp; Campusano 1991, Cat. J/MNRAS/249/218). The CCLQG covers ~2.5degx5deg (~120x240h^-2^Mpc^2^) and is 590h^-1^Mpc deep. For this study we have imaged two slightly overlapping 1.2deg fields within the CCLQG in the far-UV ({lambda}_eff_=1538.6{AA}) and near-UV ({lambda}_eff_=2315.7{AA}) filter bands, using the UV satellite GALEX (Galaxy Evolution Explorer). The observations were part of the Guest Investigator program, cycle 1 (October 2004 - September 2005) proposal 35.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506#1</TD>
            <TD>2011-11-20T12:09:51Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/702/506</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/506</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/702/506 [2]</TD>
            <TD>The Clowes-Campusano LQG Survey. I. (Haberzettl+, 2009)</TD>
            <TD>We observed part of the Clowes-Campusano Large Quasar Group (CCLQG), it contains at least 18 bright quasars at 1.2&lt;z&lt;1.5 and a spatial overdensity of 3 for B_J_&lt;=20.0mag (Clowes &amp; Campusano 1991, Cat. J/MNRAS/249/218). The CCLQG covers ~2.5degx5deg (~120x240h^-2^Mpc^2^) and is 590h^-1^Mpc deep. For this study we have imaged two slightly overlapping 1.2deg fields within the CCLQG in the far-UV ({lambda}_eff_=1538.6{AA}) and near-UV ({lambda}_eff_=2315.7{AA}) filter bands, using the UV satellite GALEX (Galaxy Evolution Explorer). The observations were part of the Guest Investigator program, cycle 1 (October 2004 - September 2005) proposal 35.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506#2</TD>
            <TD>2011-11-20T12:09:51Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/702/506&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/506</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/506 [table2]</TD>
            <TD>The Clowes-Campusano LQG Survey. I. (Haberzettl+, 2009)</TD>
            <TD>We observed part of the Clowes-Campusano Large Quasar Group (CCLQG), it contains at least 18 bright quasars at 1.2&lt;z&lt;1.5 and a spatial overdensity of 3 for B_J_&lt;=20.0mag (Clowes &amp; Campusano 1991, Cat. J/MNRAS/249/218). The CCLQG covers ~2.5degx5deg (~120x240h^-2^Mpc^2^) and is 590h^-1^Mpc deep. For this study we have imaged two slightly overlapping 1.2deg fields within the CCLQG in the far-UV ({lambda}_eff_=1538.6{AA}) and near-UV ({lambda}_eff_=2315.7{AA}) filter bands, using the UV satellite GALEX (Galaxy Evolution Explorer). The observations were part of the Guest Investigator program, cycle 1 (October 2004 - September 2005) proposal 35.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506#table2</TD>
            <TD>2011-11-20T12:09:51Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/506</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/506&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/506</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/544/A73 [1]</TD>
            <TD>BVI photometry of Fornax dSph galaxy (de Boer+, 2012)</TD>
            <TD>Deep optical photometry of the Fornax dSph in the B, V and I filters was obtained using the CTIO 4-m MOSAIC II camera over 9 nights in October 2008 and November 2009. Deep photometry for the outer fields was obtained as part of observing proposal 2008B-0397 (PI M. Mateo) supplemented by deep pointings covering the centre of Fornax as part of observing proposal 2009B-0157 (PI A. Saha). Our observing strategy was to obtain several non-dithered, long (600s) exposures for each pointing, which were stacked together to obtain the deepest photometry possible. Short (10s, 90s) exposures were also obtained, in order to sample the bright stars that are saturated in the deep images. In order to ensure accurate photometric calibration of the data set, several fields were observed in Fornax using the 0.9m CTIO telescope, under photometric conditions. Furthermore, observations were also made of Landolt standard fields (Landolt 1992, Cat II/183; Landolt 2007, Cat. J/AJ/133/2502) covering a range of different airmass and colour. Medium and high resolution spectroscopic observations are available for individual stars on the RGB in Fornax, giving measurements of [Fe/H] and the detailed abundance patterns of individual stars, from Battaglia et al. 2006, Cat. J/A+A/459/423; 2008, Cat. J/MNRAS/383/183); Starkenburg et al. 2010A&amp;A...513A..34S; Letarte et al. 2010, Cat. J/A+A/523/A17</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73#1</TD>
            <TD>2012-10-23T15:18:04Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/544/A73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/544/A73 [2]</TD>
            <TD>BVI photometry of Fornax dSph galaxy (de Boer+, 2012)</TD>
            <TD>Deep optical photometry of the Fornax dSph in the B, V and I filters was obtained using the CTIO 4-m MOSAIC II camera over 9 nights in October 2008 and November 2009. Deep photometry for the outer fields was obtained as part of observing proposal 2008B-0397 (PI M. Mateo) supplemented by deep pointings covering the centre of Fornax as part of observing proposal 2009B-0157 (PI A. Saha). Our observing strategy was to obtain several non-dithered, long (600s) exposures for each pointing, which were stacked together to obtain the deepest photometry possible. Short (10s, 90s) exposures were also obtained, in order to sample the bright stars that are saturated in the deep images. In order to ensure accurate photometric calibration of the data set, several fields were observed in Fornax using the 0.9m CTIO telescope, under photometric conditions. Furthermore, observations were also made of Landolt standard fields (Landolt 1992, Cat II/183; Landolt 2007, Cat. J/AJ/133/2502) covering a range of different airmass and colour. Medium and high resolution spectroscopic observations are available for individual stars on the RGB in Fornax, giving measurements of [Fe/H] and the detailed abundance patterns of individual stars, from Battaglia et al. 2006, Cat. J/A+A/459/423; 2008, Cat. J/MNRAS/383/183); Starkenburg et al. 2010A&amp;A...513A..34S; Letarte et al. 2010, Cat. J/A+A/523/A17</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73#2</TD>
            <TD>2012-10-23T15:18:04Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/544/A73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A73</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/544/A73 [table1]</TD>
            <TD>BVI photometry of Fornax dSph galaxy (de Boer+, 2012)</TD>
            <TD>Deep optical photometry of the Fornax dSph in the B, V and I filters was obtained using the CTIO 4-m MOSAIC II camera over 9 nights in October 2008 and November 2009. Deep photometry for the outer fields was obtained as part of observing proposal 2008B-0397 (PI M. Mateo) supplemented by deep pointings covering the centre of Fornax as part of observing proposal 2009B-0157 (PI A. Saha). Our observing strategy was to obtain several non-dithered, long (600s) exposures for each pointing, which were stacked together to obtain the deepest photometry possible. Short (10s, 90s) exposures were also obtained, in order to sample the bright stars that are saturated in the deep images. In order to ensure accurate photometric calibration of the data set, several fields were observed in Fornax using the 0.9m CTIO telescope, under photometric conditions. Furthermore, observations were also made of Landolt standard fields (Landolt 1992, Cat II/183; Landolt 2007, Cat. J/AJ/133/2502) covering a range of different airmass and colour. Medium and high resolution spectroscopic observations are available for individual stars on the RGB in Fornax, giving measurements of [Fe/H] and the detailed abundance patterns of individual stars, from Battaglia et al. 2006, Cat. J/A+A/459/423; 2008, Cat. J/MNRAS/383/183); Starkenburg et al. 2010A&amp;A...513A..34S; Letarte et al. 2010, Cat. J/A+A/523/A17</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73#table1</TD>
            <TD>2012-10-23T15:18:04Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/544/A73&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/73/661 [1]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#1</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/73/661</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/73/661 [2]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#2</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/73/661&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/73/661 [table2]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#table2</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/73/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/73/661 [table1]</TD>
            <TD>H II regions in M 101 (Hodge+ 1990)</TD>
            <TD>A previous survey of the H II regions in M101 (Hodge and Kennicutt) has been extended by a series of CCD images and image tube plates of the galaxy, approximately tripling the number of known emission regions. This paper provides maps and a catalog of a total of 1264 H II regions in M101.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661#table1</TD>
            <TD>2011-09-14T18:45:49Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/73/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/661</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/702/955 [1]</TD>
            <TD>K-band luminosity function from 2MASX (Devereux+, 2009)</TD>
            <TD>Differential Ks-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall Ks-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the Ks-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at Ks in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955#1</TD>
            <TD>2011-11-20T13:10:27Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/702/955</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/955</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/702/955 [2]</TD>
            <TD>K-band luminosity function from 2MASX (Devereux+, 2009)</TD>
            <TD>Differential Ks-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall Ks-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the Ks-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at Ks in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955#2</TD>
            <TD>2011-11-20T13:10:27Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/702/955&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/955</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/955 [table1]</TD>
            <TD>K-band luminosity function from 2MASX (Devereux+, 2009)</TD>
            <TD>Differential Ks-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall Ks-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the Ks-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at Ks in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955#table1</TD>
            <TD>2011-11-20T13:10:27Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/955&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/955</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/544/A73 [1]</TD>
            <TD>BVI photometry of Fornax dSph galaxy (de Boer+, 2012)</TD>
            <TD>Deep optical photometry of the Fornax dSph in the B, V and I filters was obtained using the CTIO 4-m MOSAIC II camera over 9 nights in October 2008 and November 2009. Deep photometry for the outer fields was obtained as part of observing proposal 2008B-0397 (PI M. Mateo) supplemented by deep pointings covering the centre of Fornax as part of observing proposal 2009B-0157 (PI A. Saha). Our observing strategy was to obtain several non-dithered, long (600s) exposures for each pointing, which were stacked together to obtain the deepest photometry possible. Short (10s, 90s) exposures were also obtained, in order to sample the bright stars that are saturated in the deep images. In order to ensure accurate photometric calibration of the data set, several fields were observed in Fornax using the 0.9m CTIO telescope, under photometric conditions. Furthermore, observations were also made of Landolt standard fields (Landolt 1992, Cat II/183; Landolt 2007, Cat. J/AJ/133/2502) covering a range of different airmass and colour. Medium and high resolution spectroscopic observations are available for individual stars on the RGB in Fornax, giving measurements of [Fe/H] and the detailed abundance patterns of individual stars, from Battaglia et al. 2006, Cat. J/A+A/459/423; 2008, Cat. J/MNRAS/383/183); Starkenburg et al. 2010A&amp;A...513A..34S; Letarte et al. 2010, Cat. J/A+A/523/A17</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73#1</TD>
            <TD>2012-10-23T15:18:04Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/544/A73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/544/A73 [2]</TD>
            <TD>BVI photometry of Fornax dSph galaxy (de Boer+, 2012)</TD>
            <TD>Deep optical photometry of the Fornax dSph in the B, V and I filters was obtained using the CTIO 4-m MOSAIC II camera over 9 nights in October 2008 and November 2009. Deep photometry for the outer fields was obtained as part of observing proposal 2008B-0397 (PI M. Mateo) supplemented by deep pointings covering the centre of Fornax as part of observing proposal 2009B-0157 (PI A. Saha). Our observing strategy was to obtain several non-dithered, long (600s) exposures for each pointing, which were stacked together to obtain the deepest photometry possible. Short (10s, 90s) exposures were also obtained, in order to sample the bright stars that are saturated in the deep images. In order to ensure accurate photometric calibration of the data set, several fields were observed in Fornax using the 0.9m CTIO telescope, under photometric conditions. Furthermore, observations were also made of Landolt standard fields (Landolt 1992, Cat II/183; Landolt 2007, Cat. J/AJ/133/2502) covering a range of different airmass and colour. Medium and high resolution spectroscopic observations are available for individual stars on the RGB in Fornax, giving measurements of [Fe/H] and the detailed abundance patterns of individual stars, from Battaglia et al. 2006, Cat. J/A+A/459/423; 2008, Cat. J/MNRAS/383/183); Starkenburg et al. 2010A&amp;A...513A..34S; Letarte et al. 2010, Cat. J/A+A/523/A17</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73#2</TD>
            <TD>2012-10-23T15:18:04Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/544/A73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A73</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/544/A73 [table1]</TD>
            <TD>BVI photometry of Fornax dSph galaxy (de Boer+, 2012)</TD>
            <TD>Deep optical photometry of the Fornax dSph in the B, V and I filters was obtained using the CTIO 4-m MOSAIC II camera over 9 nights in October 2008 and November 2009. Deep photometry for the outer fields was obtained as part of observing proposal 2008B-0397 (PI M. Mateo) supplemented by deep pointings covering the centre of Fornax as part of observing proposal 2009B-0157 (PI A. Saha). Our observing strategy was to obtain several non-dithered, long (600s) exposures for each pointing, which were stacked together to obtain the deepest photometry possible. Short (10s, 90s) exposures were also obtained, in order to sample the bright stars that are saturated in the deep images. In order to ensure accurate photometric calibration of the data set, several fields were observed in Fornax using the 0.9m CTIO telescope, under photometric conditions. Furthermore, observations were also made of Landolt standard fields (Landolt 1992, Cat II/183; Landolt 2007, Cat. J/AJ/133/2502) covering a range of different airmass and colour. Medium and high resolution spectroscopic observations are available for individual stars on the RGB in Fornax, giving measurements of [Fe/H] and the detailed abundance patterns of individual stars, from Battaglia et al. 2006, Cat. J/A+A/459/423; 2008, Cat. J/MNRAS/383/183); Starkenburg et al. 2010A&amp;A...513A..34S; Letarte et al. 2010, Cat. J/A+A/523/A17</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73#table1</TD>
            <TD>2012-10-23T15:18:04Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/544/A73&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/112/29 [1]</TD>
            <TD>HII regions in southern spiral galaxies (Feinstein 1997)</TD>
            <TD>By using narrow-band filters to measure the H{alpha} flux, a catalog of H II regions in several spiral galaxies was made, consisting of the position and flux of the objects. For each galaxy the H{alpha} luminosity function was derived. From the observed sample, two galaxies were found to have type II luminosity functions. Some simple models were made in order to understand the nature of the luminosity function (both type I and type II). The goal of our work was to simulate how a change of star-forming region, the cluster-mass distribution, or the initial mass function (in an evolutionary environment) can change the shape of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/112/29#1</TD>
            <TD>2011-09-14T18:46:03Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/112/29</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/112/29</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/112/29</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/112/29 [2]</TD>
            <TD>HII regions in southern spiral galaxies (Feinstein 1997)</TD>
            <TD>By using narrow-band filters to measure the H{alpha} flux, a catalog of H II regions in several spiral galaxies was made, consisting of the position and flux of the objects. For each galaxy the H{alpha} luminosity function was derived. From the observed sample, two galaxies were found to have type II luminosity functions. Some simple models were made in order to understand the nature of the luminosity function (both type I and type II). The goal of our work was to simulate how a change of star-forming region, the cluster-mass distribution, or the initial mass function (in an evolutionary environment) can change the shape of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/112/29#2</TD>
            <TD>2011-09-14T18:46:03Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/112/29</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/112/29&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/112/29</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IPCUltrasoft [1]</TD>
            <TD>Einstein IPC Ultrasoft Sources Catalog</TD>
            <TD>A survey of the entire Einstein IPC database (a total of 5934 sources) has been carried out in order to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5 keV). The selection criteria were based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. The selection of sources for this survey was based on the analysis of counts in three broad energy bands defined as C1=0.16-0.56 keV, C2=0.56-1.08 keV, and C3= 1.08-3.5 keV. Ratios of these three bands constituted X-ray 'colors' which in turn were used to estimate the shape of the spectrum over the IPC bandpass. Based on models of X-ray spectra folded through the IPC response function, the following criteria were determined for the selection of ultrasoft sources: C1&gt;0 and R1=C2/C1&lt;0.36. These criteria guarantee an intrinsically soft X-ray spectrum that can be modeled by blackbody temperatures kT&lt;50 keV, power-law spectral indices of &gt;=2, or thermal plasma temperatures T&lt;1 MK (million K). Details of the data analysis can be found in the Thompson et al. (1998) reference.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ipcultsoft#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ipcultsoft</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ipcultsoft&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/ipcultsoft.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IPCUltrasoft [2]</TD>
            <TD>Einstein IPC Ultrasoft Sources Catalog</TD>
            <TD>A survey of the entire Einstein IPC database (a total of 5934 sources) has been carried out in order to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5 keV). The selection criteria were based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. The selection of sources for this survey was based on the analysis of counts in three broad energy bands defined as C1=0.16-0.56 keV, C2=0.56-1.08 keV, and C3= 1.08-3.5 keV. Ratios of these three bands constituted X-ray 'colors' which in turn were used to estimate the shape of the spectrum over the IPC bandpass. Based on models of X-ray spectra folded through the IPC response function, the following criteria were determined for the selection of ultrasoft sources: C1&gt;0 and R1=C2/C1&lt;0.36. These criteria guarantee an intrinsically soft X-ray spectrum that can be modeled by blackbody temperatures kT&lt;50 keV, power-law spectral indices of &gt;=2, or thermal plasma temperatures T&lt;1 MK (million K). Details of the data analysis can be found in the Thompson et al. (1998) reference.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ipcultsoft#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ipcultsoft</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ipcultsoft&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/ipcultsoft.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IPCUltrasoft [3]</TD>
            <TD>Einstein IPC Ultrasoft Sources Catalog</TD>
            <TD>A survey of the entire Einstein IPC database (a total of 5934 sources) has been carried out in order to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5 keV). The selection criteria were based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. The selection of sources for this survey was based on the analysis of counts in three broad energy bands defined as C1=0.16-0.56 keV, C2=0.56-1.08 keV, and C3= 1.08-3.5 keV. Ratios of these three bands constituted X-ray 'colors' which in turn were used to estimate the shape of the spectrum over the IPC bandpass. Based on models of X-ray spectra folded through the IPC response function, the following criteria were determined for the selection of ultrasoft sources: C1&gt;0 and R1=C2/C1&lt;0.36. These criteria guarantee an intrinsically soft X-ray spectrum that can be modeled by blackbody temperatures kT&lt;50 keV, power-law spectral indices of &gt;=2, or thermal plasma temperatures T&lt;1 MK (million K). Details of the data analysis can be found in the Thompson et al. (1998) reference.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ipcultsoft#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ipcultsoft</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ipcultsoft&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/ipcultsoft.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/544/A73 [1]</TD>
            <TD>BVI photometry of Fornax dSph galaxy (de Boer+, 2012)</TD>
            <TD>Deep optical photometry of the Fornax dSph in the B, V and I filters was obtained using the CTIO 4-m MOSAIC II camera over 9 nights in October 2008 and November 2009. Deep photometry for the outer fields was obtained as part of observing proposal 2008B-0397 (PI M. Mateo) supplemented by deep pointings covering the centre of Fornax as part of observing proposal 2009B-0157 (PI A. Saha). Our observing strategy was to obtain several non-dithered, long (600s) exposures for each pointing, which were stacked together to obtain the deepest photometry possible. Short (10s, 90s) exposures were also obtained, in order to sample the bright stars that are saturated in the deep images. In order to ensure accurate photometric calibration of the data set, several fields were observed in Fornax using the 0.9m CTIO telescope, under photometric conditions. Furthermore, observations were also made of Landolt standard fields (Landolt 1992, Cat II/183; Landolt 2007, Cat. J/AJ/133/2502) covering a range of different airmass and colour. Medium and high resolution spectroscopic observations are available for individual stars on the RGB in Fornax, giving measurements of [Fe/H] and the detailed abundance patterns of individual stars, from Battaglia et al. 2006, Cat. J/A+A/459/423; 2008, Cat. J/MNRAS/383/183); Starkenburg et al. 2010A&amp;A...513A..34S; Letarte et al. 2010, Cat. J/A+A/523/A17</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73#1</TD>
            <TD>2012-10-23T15:18:04Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/544/A73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/544/A73 [2]</TD>
            <TD>BVI photometry of Fornax dSph galaxy (de Boer+, 2012)</TD>
            <TD>Deep optical photometry of the Fornax dSph in the B, V and I filters was obtained using the CTIO 4-m MOSAIC II camera over 9 nights in October 2008 and November 2009. Deep photometry for the outer fields was obtained as part of observing proposal 2008B-0397 (PI M. Mateo) supplemented by deep pointings covering the centre of Fornax as part of observing proposal 2009B-0157 (PI A. Saha). Our observing strategy was to obtain several non-dithered, long (600s) exposures for each pointing, which were stacked together to obtain the deepest photometry possible. Short (10s, 90s) exposures were also obtained, in order to sample the bright stars that are saturated in the deep images. In order to ensure accurate photometric calibration of the data set, several fields were observed in Fornax using the 0.9m CTIO telescope, under photometric conditions. Furthermore, observations were also made of Landolt standard fields (Landolt 1992, Cat II/183; Landolt 2007, Cat. J/AJ/133/2502) covering a range of different airmass and colour. Medium and high resolution spectroscopic observations are available for individual stars on the RGB in Fornax, giving measurements of [Fe/H] and the detailed abundance patterns of individual stars, from Battaglia et al. 2006, Cat. J/A+A/459/423; 2008, Cat. J/MNRAS/383/183); Starkenburg et al. 2010A&amp;A...513A..34S; Letarte et al. 2010, Cat. J/A+A/523/A17</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73#2</TD>
            <TD>2012-10-23T15:18:04Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/544/A73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A73</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/544/A73 [table1]</TD>
            <TD>BVI photometry of Fornax dSph galaxy (de Boer+, 2012)</TD>
            <TD>Deep optical photometry of the Fornax dSph in the B, V and I filters was obtained using the CTIO 4-m MOSAIC II camera over 9 nights in October 2008 and November 2009. Deep photometry for the outer fields was obtained as part of observing proposal 2008B-0397 (PI M. Mateo) supplemented by deep pointings covering the centre of Fornax as part of observing proposal 2009B-0157 (PI A. Saha). Our observing strategy was to obtain several non-dithered, long (600s) exposures for each pointing, which were stacked together to obtain the deepest photometry possible. Short (10s, 90s) exposures were also obtained, in order to sample the bright stars that are saturated in the deep images. In order to ensure accurate photometric calibration of the data set, several fields were observed in Fornax using the 0.9m CTIO telescope, under photometric conditions. Furthermore, observations were also made of Landolt standard fields (Landolt 1992, Cat II/183; Landolt 2007, Cat. J/AJ/133/2502) covering a range of different airmass and colour. Medium and high resolution spectroscopic observations are available for individual stars on the RGB in Fornax, giving measurements of [Fe/H] and the detailed abundance patterns of individual stars, from Battaglia et al. 2006, Cat. J/A+A/459/423; 2008, Cat. J/MNRAS/383/183); Starkenburg et al. 2010A&amp;A...513A..34S; Letarte et al. 2010, Cat. J/A+A/523/A17</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73#table1</TD>
            <TD>2012-10-23T15:18:04Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A73</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/544/A73&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/112/29 [1]</TD>
            <TD>HII regions in southern spiral galaxies (Feinstein 1997)</TD>
            <TD>By using narrow-band filters to measure the H{alpha} flux, a catalog of H II regions in several spiral galaxies was made, consisting of the position and flux of the objects. For each galaxy the H{alpha} luminosity function was derived. From the observed sample, two galaxies were found to have type II luminosity functions. Some simple models were made in order to understand the nature of the luminosity function (both type I and type II). The goal of our work was to simulate how a change of star-forming region, the cluster-mass distribution, or the initial mass function (in an evolutionary environment) can change the shape of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/112/29#1</TD>
            <TD>2011-09-14T18:46:03Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/112/29</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/112/29</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/112/29</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/112/29 [2]</TD>
            <TD>HII regions in southern spiral galaxies (Feinstein 1997)</TD>
            <TD>By using narrow-band filters to measure the H{alpha} flux, a catalog of H II regions in several spiral galaxies was made, consisting of the position and flux of the objects. For each galaxy the H{alpha} luminosity function was derived. From the observed sample, two galaxies were found to have type II luminosity functions. Some simple models were made in order to understand the nature of the luminosity function (both type I and type II). The goal of our work was to simulate how a change of star-forming region, the cluster-mass distribution, or the initial mass function (in an evolutionary environment) can change the shape of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/112/29#2</TD>
            <TD>2011-09-14T18:46:03Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/112/29</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/112/29&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/112/29</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/702/955 [1]</TD>
            <TD>K-band luminosity function from 2MASX (Devereux+, 2009)</TD>
            <TD>Differential Ks-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall Ks-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the Ks-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at Ks in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955#1</TD>
            <TD>2011-11-20T13:10:27Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/702/955</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/955</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/702/955 [2]</TD>
            <TD>K-band luminosity function from 2MASX (Devereux+, 2009)</TD>
            <TD>Differential Ks-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall Ks-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the Ks-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at Ks in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955#2</TD>
            <TD>2011-11-20T13:10:27Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/702/955&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/955</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/955 [table1]</TD>
            <TD>K-band luminosity function from 2MASX (Devereux+, 2009)</TD>
            <TD>Differential Ks-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall Ks-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the Ks-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at Ks in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955#table1</TD>
            <TD>2011-11-20T13:10:27Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/955&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/955</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/540/A47 [1]</TD>
            <TD>AMIGA X. Isolated galaxy colors (Fernandez Lorenzo+, 2012)</TD>
            <TD>Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47#1</TD>
            <TD>2012-10-27T17:04:34Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/540/A47</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A47</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/540/A47 [2]</TD>
            <TD>AMIGA X. Isolated galaxy colors (Fernandez Lorenzo+, 2012)</TD>
            <TD>Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47#2</TD>
            <TD>2012-10-27T17:04:34Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/540/A47&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A47</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A47 [table1]</TD>
            <TD>AMIGA X. Isolated galaxy colors (Fernandez Lorenzo+, 2012)</TD>
            <TD>Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47#table1</TD>
            <TD>2012-10-27T17:04:34Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A47&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A47</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/120/257 [1]</TD>
            <TD>Ionized gas velocity in 6 galaxies (Zeilinger+ 1996)</TD>
            <TD>We report observations of the velocity field of the ionized gas in the nearby ellipticals NGC 1453, NGC 2974, NGC 3962, NGC 4636, NGC 6868 and NGC 7097. This is part of an ESO Key Programme intended to derive the mass distribution of elliptical galaxies and to investigate the possible presence of dark matter. All galaxy spectra are characterized by LINER-type emission. The derived gas kinematics confirm the picture of a regular gaseous disk structure with ordered rotation. The gas velocity dispersion profiles decline rapidly from a high central value in the range of =~150 to =~250km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/257#1</TD>
            <TD>2011-09-14T18:46:05Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/120/257</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/257</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/120/257 [2]</TD>
            <TD>Ionized gas velocity in 6 galaxies (Zeilinger+ 1996)</TD>
            <TD>We report observations of the velocity field of the ionized gas in the nearby ellipticals NGC 1453, NGC 2974, NGC 3962, NGC 4636, NGC 6868 and NGC 7097. This is part of an ESO Key Programme intended to derive the mass distribution of elliptical galaxies and to investigate the possible presence of dark matter. All galaxy spectra are characterized by LINER-type emission. The derived gas kinematics confirm the picture of a regular gaseous disk structure with ordered rotation. The gas velocity dispersion profiles decline rapidly from a high central value in the range of =~150 to =~250km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/257#2</TD>
            <TD>2011-09-14T18:46:05Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/120/257&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/257</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/702/955 [1]</TD>
            <TD>K-band luminosity function from 2MASX (Devereux+, 2009)</TD>
            <TD>Differential Ks-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall Ks-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the Ks-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at Ks in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955#1</TD>
            <TD>2011-11-20T13:10:27Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/702/955</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/955</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/702/955 [2]</TD>
            <TD>K-band luminosity function from 2MASX (Devereux+, 2009)</TD>
            <TD>Differential Ks-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall Ks-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the Ks-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at Ks in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955#2</TD>
            <TD>2011-11-20T13:10:27Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/702/955&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/955</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/702/955 [table1]</TD>
            <TD>K-band luminosity function from 2MASX (Devereux+, 2009)</TD>
            <TD>Differential Ks-band luminosity functions (LFs) are presented for a complete sample of 1613 nearby bright galaxies segregated by visible morphology. The LF for late-type spirals follows a power law that rises toward low luminosities whereas the LFs for ellipticals, lenticulars, and bulge-dominated spirals are peaked and decline toward both higher and lower luminosities. Each morphological type (E, S0, S0/a-Sab, Sb-Sbc, Sc-Scd) contributes approximately equally to the overall Ks-band luminosity density of galaxies in the local universe. Type averaged bulge/disk ratios are used to subtract the disk component leading to the prediction that the Ks-band LF for bulges is bimodal with ellipticals dominating the high luminosity peak, comprising 60% of the bulge luminosity density in the local universe with the remaining 40% contributed by lenticulars and the bulges of spirals. Overall, bulges contribute 30% of the galaxy luminosity density at Ks in the local universe with spiral disks making up the remainder. If bulge luminosities indicate central black hole (BH) masses, then our results predict that the BH mass function is also bimodal.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955#table1</TD>
            <TD>2011-11-20T13:10:27Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/702/955</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/702/955&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/702/955</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/540/A47 [1]</TD>
            <TD>AMIGA X. Isolated galaxy colors (Fernandez Lorenzo+, 2012)</TD>
            <TD>Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47#1</TD>
            <TD>2012-10-27T17:04:34Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/540/A47</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A47</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/540/A47 [2]</TD>
            <TD>AMIGA X. Isolated galaxy colors (Fernandez Lorenzo+, 2012)</TD>
            <TD>Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47#2</TD>
            <TD>2012-10-27T17:04:34Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/540/A47&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A47</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A47 [table1]</TD>
            <TD>AMIGA X. Isolated galaxy colors (Fernandez Lorenzo+, 2012)</TD>
            <TD>Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47#table1</TD>
            <TD>2012-10-27T17:04:34Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A47&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A47</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/120/257 [1]</TD>
            <TD>Ionized gas velocity in 6 galaxies (Zeilinger+ 1996)</TD>
            <TD>We report observations of the velocity field of the ionized gas in the nearby ellipticals NGC 1453, NGC 2974, NGC 3962, NGC 4636, NGC 6868 and NGC 7097. This is part of an ESO Key Programme intended to derive the mass distribution of elliptical galaxies and to investigate the possible presence of dark matter. All galaxy spectra are characterized by LINER-type emission. The derived gas kinematics confirm the picture of a regular gaseous disk structure with ordered rotation. The gas velocity dispersion profiles decline rapidly from a high central value in the range of =~150 to =~250km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/257#1</TD>
            <TD>2011-09-14T18:46:05Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/120/257</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/257</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/120/257 [2]</TD>
            <TD>Ionized gas velocity in 6 galaxies (Zeilinger+ 1996)</TD>
            <TD>We report observations of the velocity field of the ionized gas in the nearby ellipticals NGC 1453, NGC 2974, NGC 3962, NGC 4636, NGC 6868 and NGC 7097. This is part of an ESO Key Programme intended to derive the mass distribution of elliptical galaxies and to investigate the possible presence of dark matter. All galaxy spectra are characterized by LINER-type emission. The derived gas kinematics confirm the picture of a regular gaseous disk structure with ordered rotation. The gas velocity dispersion profiles decline rapidly from a high central value in the range of =~150 to =~250km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/257#2</TD>
            <TD>2011-09-14T18:46:05Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/120/257&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/257</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/2376 [1]</TD>
            <TD>Case blue/emission-line galaxies (Salzer+ 1995)</TD>
            <TD>We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376#1</TD>
            <TD>2011-09-14T18:46:21Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/2376</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/2376</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/2376 [2]</TD>
            <TD>Case blue/emission-line galaxies (Salzer+ 1995)</TD>
            <TD>We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376#2</TD>
            <TD>2011-09-14T18:46:21Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/2376&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/2376</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/2376 [table2]</TD>
            <TD>Case blue/emission-line galaxies (Salzer+ 1995)</TD>
            <TD>We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376#table2</TD>
            <TD>2011-09-14T18:46:21Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/2376&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/2376</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IPCUltrasoft [1]</TD>
            <TD>Einstein IPC Ultrasoft Sources Catalog</TD>
            <TD>A survey of the entire Einstein IPC database (a total of 5934 sources) has been carried out in order to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5 keV). The selection criteria were based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. The selection of sources for this survey was based on the analysis of counts in three broad energy bands defined as C1=0.16-0.56 keV, C2=0.56-1.08 keV, and C3= 1.08-3.5 keV. Ratios of these three bands constituted X-ray 'colors' which in turn were used to estimate the shape of the spectrum over the IPC bandpass. Based on models of X-ray spectra folded through the IPC response function, the following criteria were determined for the selection of ultrasoft sources: C1&gt;0 and R1=C2/C1&lt;0.36. These criteria guarantee an intrinsically soft X-ray spectrum that can be modeled by blackbody temperatures kT&lt;50 keV, power-law spectral indices of &gt;=2, or thermal plasma temperatures T&lt;1 MK (million K). Details of the data analysis can be found in the Thompson et al. (1998) reference.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ipcultsoft#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ipcultsoft</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ipcultsoft&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/ipcultsoft.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IPCUltrasoft [2]</TD>
            <TD>Einstein IPC Ultrasoft Sources Catalog</TD>
            <TD>A survey of the entire Einstein IPC database (a total of 5934 sources) has been carried out in order to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5 keV). The selection criteria were based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. The selection of sources for this survey was based on the analysis of counts in three broad energy bands defined as C1=0.16-0.56 keV, C2=0.56-1.08 keV, and C3= 1.08-3.5 keV. Ratios of these three bands constituted X-ray 'colors' which in turn were used to estimate the shape of the spectrum over the IPC bandpass. Based on models of X-ray spectra folded through the IPC response function, the following criteria were determined for the selection of ultrasoft sources: C1&gt;0 and R1=C2/C1&lt;0.36. These criteria guarantee an intrinsically soft X-ray spectrum that can be modeled by blackbody temperatures kT&lt;50 keV, power-law spectral indices of &gt;=2, or thermal plasma temperatures T&lt;1 MK (million K). Details of the data analysis can be found in the Thompson et al. (1998) reference.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ipcultsoft#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ipcultsoft</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ipcultsoft&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/ipcultsoft.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IPCUltrasoft [3]</TD>
            <TD>Einstein IPC Ultrasoft Sources Catalog</TD>
            <TD>A survey of the entire Einstein IPC database (a total of 5934 sources) has been carried out in order to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5 keV). The selection criteria were based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. The selection of sources for this survey was based on the analysis of counts in three broad energy bands defined as C1=0.16-0.56 keV, C2=0.56-1.08 keV, and C3= 1.08-3.5 keV. Ratios of these three bands constituted X-ray 'colors' which in turn were used to estimate the shape of the spectrum over the IPC bandpass. Based on models of X-ray spectra folded through the IPC response function, the following criteria were determined for the selection of ultrasoft sources: C1&gt;0 and R1=C2/C1&lt;0.36. These criteria guarantee an intrinsically soft X-ray spectrum that can be modeled by blackbody temperatures kT&lt;50 keV, power-law spectral indices of &gt;=2, or thermal plasma temperatures T&lt;1 MK (million K). Details of the data analysis can be found in the Thompson et al. (1998) reference.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ipcultsoft#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ipcultsoft</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ipcultsoft&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/ipcultsoft.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/540/A47 [1]</TD>
            <TD>AMIGA X. Isolated galaxy colors (Fernandez Lorenzo+, 2012)</TD>
            <TD>Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47#1</TD>
            <TD>2012-10-27T17:04:34Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/540/A47</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A47</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/540/A47 [2]</TD>
            <TD>AMIGA X. Isolated galaxy colors (Fernandez Lorenzo+, 2012)</TD>
            <TD>Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47#2</TD>
            <TD>2012-10-27T17:04:34Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/540/A47&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A47</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A47 [table1]</TD>
            <TD>AMIGA X. Isolated galaxy colors (Fernandez Lorenzo+, 2012)</TD>
            <TD>Revision of the main properties for all AMIGA galaxies. Because a significant number of new data are available for the sample since the AMIGA project started, apparent magnitudes, morphological types, distances, and optical luminosities for the CIG sample have been updated. In the frame of the Wf4Ever project, the revision of these properties was partially automated by the implementation of scientific workflows that ask for and gather values of some of the properties for all AMIGA galaxies from the HyperLeda catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47#table1</TD>
            <TD>2012-10-27T17:04:34Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A47</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A47&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A47</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/2376 [1]</TD>
            <TD>Case blue/emission-line galaxies (Salzer+ 1995)</TD>
            <TD>We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376#1</TD>
            <TD>2011-09-14T18:46:21Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/2376</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/2376</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/2376 [2]</TD>
            <TD>Case blue/emission-line galaxies (Salzer+ 1995)</TD>
            <TD>We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376#2</TD>
            <TD>2011-09-14T18:46:21Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/2376&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/2376</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/2376 [table2]</TD>
            <TD>Case blue/emission-line galaxies (Salzer+ 1995)</TD>
            <TD>We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376#table2</TD>
            <TD>2011-09-14T18:46:21Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/2376&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/2376</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IPCUltrasoft [1]</TD>
            <TD>Einstein IPC Ultrasoft Sources Catalog</TD>
            <TD>A survey of the entire Einstein IPC database (a total of 5934 sources) has been carried out in order to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5 keV). The selection criteria were based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. The selection of sources for this survey was based on the analysis of counts in three broad energy bands defined as C1=0.16-0.56 keV, C2=0.56-1.08 keV, and C3= 1.08-3.5 keV. Ratios of these three bands constituted X-ray 'colors' which in turn were used to estimate the shape of the spectrum over the IPC bandpass. Based on models of X-ray spectra folded through the IPC response function, the following criteria were determined for the selection of ultrasoft sources: C1&gt;0 and R1=C2/C1&lt;0.36. These criteria guarantee an intrinsically soft X-ray spectrum that can be modeled by blackbody temperatures kT&lt;50 keV, power-law spectral indices of &gt;=2, or thermal plasma temperatures T&lt;1 MK (million K). Details of the data analysis can be found in the Thompson et al. (1998) reference.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ipcultsoft#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ipcultsoft</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ipcultsoft&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/ipcultsoft.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IPCUltrasoft [2]</TD>
            <TD>Einstein IPC Ultrasoft Sources Catalog</TD>
            <TD>A survey of the entire Einstein IPC database (a total of 5934 sources) has been carried out in order to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5 keV). The selection criteria were based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. The selection of sources for this survey was based on the analysis of counts in three broad energy bands defined as C1=0.16-0.56 keV, C2=0.56-1.08 keV, and C3= 1.08-3.5 keV. Ratios of these three bands constituted X-ray 'colors' which in turn were used to estimate the shape of the spectrum over the IPC bandpass. Based on models of X-ray spectra folded through the IPC response function, the following criteria were determined for the selection of ultrasoft sources: C1&gt;0 and R1=C2/C1&lt;0.36. These criteria guarantee an intrinsically soft X-ray spectrum that can be modeled by blackbody temperatures kT&lt;50 keV, power-law spectral indices of &gt;=2, or thermal plasma temperatures T&lt;1 MK (million K). Details of the data analysis can be found in the Thompson et al. (1998) reference.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ipcultsoft#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ipcultsoft</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ipcultsoft&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/ipcultsoft.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IPCUltrasoft [3]</TD>
            <TD>Einstein IPC Ultrasoft Sources Catalog</TD>
            <TD>A survey of the entire Einstein IPC database (a total of 5934 sources) has been carried out in order to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5 keV). The selection criteria were based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. The selection of sources for this survey was based on the analysis of counts in three broad energy bands defined as C1=0.16-0.56 keV, C2=0.56-1.08 keV, and C3= 1.08-3.5 keV. Ratios of these three bands constituted X-ray 'colors' which in turn were used to estimate the shape of the spectrum over the IPC bandpass. Based on models of X-ray spectra folded through the IPC response function, the following criteria were determined for the selection of ultrasoft sources: C1&gt;0 and R1=C2/C1&lt;0.36. These criteria guarantee an intrinsically soft X-ray spectrum that can be modeled by blackbody temperatures kT&lt;50 keV, power-law spectral indices of &gt;=2, or thermal plasma temperatures T&lt;1 MK (million K). Details of the data analysis can be found in the Thompson et al. (1998) reference.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ipcultsoft#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ipcultsoft</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ipcultsoft&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/ipcultsoft.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/2376 [1]</TD>
            <TD>Case blue/emission-line galaxies (Salzer+ 1995)</TD>
            <TD>We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376#1</TD>
            <TD>2011-09-14T18:46:21Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/2376</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/2376</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/2376 [2]</TD>
            <TD>Case blue/emission-line galaxies (Salzer+ 1995)</TD>
            <TD>We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376#2</TD>
            <TD>2011-09-14T18:46:21Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/2376&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/2376</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/2376 [table2]</TD>
            <TD>Case blue/emission-line galaxies (Salzer+ 1995)</TD>
            <TD>We present CCD imaging and spectroscopic data for 176 blue and/or emission-line galaxies from Lists I and II of the Case Northern Sky Survey. Our sample consists of all Case galaxies which lie in the region which overlaps the original Slice of the Universe survey. We use the observational data to investigate the physical properties of the galaxies selected by the surveys to compare with various parameters published in the survey lists, and to investigate the selection characteristics and completeness limit of the survey. The majority of the Case galaxies are energized by regions of active star formation; only 5% of the sample are Seyfert galaxies. The dual selection techniques used (both UV-excess and emission lines) allow the survey to detect star-forming galaxies with a wide range of properties and evolutionary states. In particular, the Case survey selects galaxies with lower levels of activity than most previous surveys. The survey also includes a larger fraction of intermediate and low-luminosity galaxies than would be present in a purely magnitude-limited sample. Although galaxies as faint as m_B_=19 are present in the sample, the completeness limit of the UV-excess selected portion of the survey is closer to m_B_=16. The luminosity function of the Case galaxies is derived and compared with that of the "normal" field galaxies in the same volume of space. The shape of the Case luminosity function is similar to that for the field sample. A surprising result is that 31% of the field galaxy population can be accounted for by galaxies of the type selected in the Case survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376#table2</TD>
            <TD>2011-09-14T18:46:21Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/2376</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/2376&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/2376</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LyngaOpenCl [1]</TD>
            <TD>Lynga Open Clusters Catalog</TD>
            <TD>This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lyngaclust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lyngaclust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lyngaclust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lyngaclust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LyngaOpenCl [2]</TD>
            <TD>Lynga Open Clusters Catalog</TD>
            <TD>This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lyngaclust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lyngaclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lyngaclust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lyngaclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LyngaOpenCl [3]</TD>
            <TD>Lynga Open Clusters Catalog</TD>
            <TD>This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lyngaclust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lyngaclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lyngaclust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lyngaclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/544/A81 [1]</TD>
            <TD>Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)</TD>
            <TD>The measurements of apparent magnitudes, diameters (D_25_), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81#1</TD>
            <TD>2012-10-28T21:55:37Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/544/A81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/544/A81 [2]</TD>
            <TD>Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)</TD>
            <TD>The measurements of apparent magnitudes, diameters (D_25_), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81#2</TD>
            <TD>2012-10-28T21:55:37Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/544/A81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/544/A81 [snsdss]</TD>
            <TD>Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)</TD>
            <TD>The measurements of apparent magnitudes, diameters (D_25_), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81#snsdss</TD>
            <TD>2012-10-28T21:55:37Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/544/A81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/470/724 [1]</TD>
            <TD>Abell 576 galaxies magnitude and velocities (Mohr+ 1996)</TD>
            <TD>We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_&lt;17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_&gt;4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724#1</TD>
            <TD>2011-09-14T18:46:22Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/470/724</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/470/724</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/470/724 [2]</TD>
            <TD>Abell 576 galaxies magnitude and velocities (Mohr+ 1996)</TD>
            <TD>We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_&lt;17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_&gt;4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724#2</TD>
            <TD>2011-09-14T18:46:22Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/470/724&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/470/724</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/470/724 [table1]</TD>
            <TD>Abell 576 galaxies magnitude and velocities (Mohr+ 1996)</TD>
            <TD>We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_&lt;17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_&gt;4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724#table1</TD>
            <TD>2011-09-14T18:46:22Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/470/724&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/470/724</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LyngaOpenCl [1]</TD>
            <TD>Lynga Open Clusters Catalog</TD>
            <TD>This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lyngaclust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lyngaclust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lyngaclust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lyngaclust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LyngaOpenCl [2]</TD>
            <TD>Lynga Open Clusters Catalog</TD>
            <TD>This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lyngaclust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lyngaclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lyngaclust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lyngaclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LyngaOpenCl [3]</TD>
            <TD>Lynga Open Clusters Catalog</TD>
            <TD>This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lyngaclust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lyngaclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lyngaclust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lyngaclust.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LyngaOpenCl [1]</TD>
            <TD>Lynga Open Clusters Catalog</TD>
            <TD>This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lyngaclust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lyngaclust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lyngaclust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lyngaclust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LyngaOpenCl [2]</TD>
            <TD>Lynga Open Clusters Catalog</TD>
            <TD>This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lyngaclust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lyngaclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lyngaclust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lyngaclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LyngaOpenCl [3]</TD>
            <TD>Lynga Open Clusters Catalog</TD>
            <TD>This is a catalog of open cluster data, as compiled by Gosta Lynga, Lund Observatory. The aim of this catalog is to give salient data for all known open star clusters in our galaxy. As far as possible only published data values have been quoted; for some of the parameters, these values have been slected from references which can be obtained from the HEASARC. This data in part results from the merging of the data resulting from a joint project between K. Janes, C. Duke and Lynga, herein refered to as JDL data. The aim of that project was to discuss properties of the open cluster system by using existing data and by taking their accuracy into proper regard. Thus the data were assessed, mostly by Janes, weight assigned and weighted mean values derived of reddenings, turn-off colors and distances.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lyngaclust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lyngaclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lyngaclust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lyngaclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/470/724 [1]</TD>
            <TD>Abell 576 galaxies magnitude and velocities (Mohr+ 1996)</TD>
            <TD>We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_&lt;17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_&gt;4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724#1</TD>
            <TD>2011-09-14T18:46:22Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/470/724</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/470/724</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/470/724 [2]</TD>
            <TD>Abell 576 galaxies magnitude and velocities (Mohr+ 1996)</TD>
            <TD>We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_&lt;17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_&gt;4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724#2</TD>
            <TD>2011-09-14T18:46:22Z</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJ/470/724 [table1]</TD>
            <TD>Abell 576 galaxies magnitude and velocities (Mohr+ 1996)</TD>
            <TD>We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_&lt;17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_&gt;4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.</TD>
            <TD>CDS</TD>
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            <TD>Catalog</TD>
            <TD>M31XMM2 [1]</TD>
            <TD>M31 XMM-Newton Spectral Survey X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L_X interval 37.0 &lt;~ log L_X erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L_X ~1.4 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the observed population is statistically dominated by the point source population of M 31.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>M31XMM2 [2]</TD>
            <TD>M31 XMM-Newton Spectral Survey X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L_X interval 37.0 &lt;~ log L_X erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L_X ~1.4 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the observed population is statistically dominated by the point source population of M 31.</TD>
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            <TD>Web Page</TD>
            <TD>M31XMM2 [3]</TD>
            <TD>M31 XMM-Newton Spectral Survey X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L_X interval 37.0 &lt;~ log L_X erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L_X ~1.4 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the observed population is statistically dominated by the point source population of M 31.</TD>
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            <TD>M31 XMM-Newton Spectral Survey X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L_X interval 37.0 &lt;~ log L_X erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L_X ~1.4 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the observed population is statistically dominated by the point source population of M 31.</TD>
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            <TD>HTTP Request</TD>
            <TD>M31XMM2 [2]</TD>
            <TD>M31 XMM-Newton Spectral Survey X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L_X interval 37.0 &lt;~ log L_X erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L_X ~1.4 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the observed population is statistically dominated by the point source population of M 31.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>M31XMM2 [3]</TD>
            <TD>M31 XMM-Newton Spectral Survey X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L_X interval 37.0 &lt;~ log L_X erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L_X ~1.4 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the observed population is statistically dominated by the point source population of M 31.</TD>
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            <TD>J/ApJ/470/724 [1]</TD>
            <TD>Abell 576 galaxies magnitude and velocities (Mohr+ 1996)</TD>
            <TD>We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_&lt;17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_&gt;4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T18:46:22Z</TD>
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            <TD>30-Sep-1997</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJ/470/724 [2]</TD>
            <TD>Abell 576 galaxies magnitude and velocities (Mohr+ 1996)</TD>
            <TD>We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_&lt;17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_&gt;4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.</TD>
            <TD>CDS</TD>
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            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/470/724&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/470/724</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/470/724 [table1]</TD>
            <TD>Abell 576 galaxies magnitude and velocities (Mohr+ 1996)</TD>
            <TD>We analyse the galaxy population and dynamics of the galaxy cluster A576; the observational constraints include 281 redshifts (230 new), R-band CCD galaxy photometry over a 2h^-1^Mpcx2h^-1^Mpc region centered on the cluster, an Einstein IPC X-ray image, and an Einstein MPC X-ray spectrum. We focus on an 86% complete magnitude-limited sample (R_23.5_&lt;17) of 169 cluster galaxies. The cluster galaxies with emission lines in their spectra have a larger velocity dispersion and are significantly less clustered on this 2h^-1^Mpc scale than galaxies without emission lines. We show that excluding the emission-line galaxies from the cluster sample decreases the velocity dispersion by 18% and the virial mass estimate by a factor of 2. The central cluster region contains a non-emission galaxy population and an intracluster medium which is significantly cooler ({sigma}_core_=387^+250^_-105_km/s and T_X_=1.6-0.3/+0.4keV at 90% confidence) than the global populations ({sigma}=977^+124^_-96_km/s for the non-emission population and T_X_&gt;4keV at 90% confidence). Because (1) the low-dispersion galaxy population is no more luminous than the global population and (2) the evidence for a cooling flow is weak, we suggest that the core of A576 may contain the remnants of a lower mass subcluster. We examine the cluster mass, baryon fraction, and luminosity function. The cluster virial mass varies significantly depending on the galaxy sample used. Consistency between the hydrostatic and virial estimators can be achieved if (1) the gas temperature at r~1h^-1^Mpc is T_X_~8keV (the best-fit value) and (2) several velocity outliers are excluded from the virial calculation. Although the best-fit Schechter function parameters and the ratio of galaxy to gas mass in A576 are typical of other clusters, the baryon fraction is relatively low. Using the consistent cluster binding mass, we show that the gas mass fraction is ~3h^-3/2^% and the baryon fraction is ~4%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724#table1</TD>
            <TD>2011-09-14T18:46:22Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/470/724</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/470/724&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/470/724</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M31XMM2 [1]</TD>
            <TD>M31 XMM-Newton Spectral Survey X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L_X interval 37.0 &lt;~ log L_X erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L_X ~1.4 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the observed population is statistically dominated by the point source population of M 31.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmm2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmm2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m31xmm2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmm2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M31XMM2 [2]</TD>
            <TD>M31 XMM-Newton Spectral Survey X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L_X interval 37.0 &lt;~ log L_X erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L_X ~1.4 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the observed population is statistically dominated by the point source population of M 31.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmm2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmm2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m31xmm2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmm2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M31XMM2 [3]</TD>
            <TD>M31 XMM-Newton Spectral Survey X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of a complete spectral survey of the X-ray point sources detected in five XMM-Newton observations along the major axis of M 31 but avoiding the central bulge, aimed at establishing the population characteristics of X-ray sources in this galaxy. One observation of each disc field of M 31 was taken using the EPIC pn and MOS cameras on XMM-Newton in January and June 2002. The authors obtained background-subtracted spectra and lightcurves for each of the 335 X-ray point sources detected across the five observations from 2002. They also correlate their source list with those of earlier X-ray surveys and radio, optical and infra-red catalogs. Sources with more than 50 source counts are individually spectrally fit in order to create the most accurate luminosity functions of M 31 to date. Based on the spectral fitting of these sources with a power law model, the authors observe a broad range of best-fit photon index. From this distribution of best-fit index, they identify 16 strong high mass X-ray binary system candidates in M 31. They show the first cumulative luminosity functions created using the best-fit spectral model to each source with more than 50 source counts in the disc of M 31. The cumulative luminosity functions show a distinct flattening in the X-ray luminosity L_X interval 37.0 &lt;~ log L_X erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;~ 37.5. Such a feature may also be present in the X-ray populations of several other galaxies, but at a much lower statistical significance. The authors investigate the number of AGN present in their source list and find that, above L_X ~1.4 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, the observed population is statistically dominated by the point source population of M 31.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmm2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmm2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m31xmm2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmm2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/99/1071 [1]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#1</TD>
            <TD>2011-09-14T18:46:53Z</TD>
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            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/99/1071</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/99/1071 [2]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#2</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/99/1071&amp;</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table2]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table2</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
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            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table1]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table1</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>9999</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table3]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table3</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table4]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table4</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/99/1071 [1]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#1</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/99/1071</TD>
            <TD />
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/99/1071 [2]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#2</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table2]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table2</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table1]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table1</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table3]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table3</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table4]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table4</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMM/M33 [1]</TD>
            <TD>XMM-Newton M33 Survey Catalog</TD>
            <TD>This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 10^35 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmmxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmmxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33xmmxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmmxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMM/M33 [2]</TD>
            <TD>XMM-Newton M33 Survey Catalog</TD>
            <TD>This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 10^35 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmmxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33xmmxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMM/M33 [3]</TD>
            <TD>XMM-Newton M33 Survey Catalog</TD>
            <TD>This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 10^35 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmmxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33xmmxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/99/1071 [1]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#1</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/99/1071</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/99/1071 [2]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#2</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table2]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table2</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table1]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table1</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table3]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table3</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1071 [table4]</TD>
            <TD>1.4 GHz source survey (Condon+ 1990)</TD>
            <TD>We report on 1.4GHz continuum observations for 56 contiguous VLA fields, using the D configuration, in a region devoid of nearby, rich galaxy clusters (at z&lt;0.4). 354 continuum sources are tabulated, with fluxes down to about 1.5mJy, in an area of about 12degres^+2^. Only about seven of the 354 radio sources are associated with known rich galaxy clusters at z&gt;0.4 (tabulated by Gunn, Hoessel, and Oke, 1986ApJ...306...30G). We compare source positions with those from an optical catalog (generated from a POSS plate with the use of the Minnesota Automated Plate Scanner) and find mild correlations on angular scales of order 1arcmin. This suggests some association of radio sources with galaxy groups (sizes of order 200 kpc) at redshifts of order z~0.1, even though there are no rich galaxy clusters in this redshift range.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071#table4</TD>
            <TD>2011-09-14T18:46:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMM/M33 [1]</TD>
            <TD>XMM-Newton M33 Survey Catalog</TD>
            <TD>This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 10^35 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmmxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmmxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33xmmxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmmxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMM/M33 [2]</TD>
            <TD>XMM-Newton M33 Survey Catalog</TD>
            <TD>This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 10^35 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmmxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33xmmxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMM/M33 [3]</TD>
            <TD>XMM-Newton M33 Survey Catalog</TD>
            <TD>This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 10^35 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmmxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33xmmxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/106/463 [1]</TD>
            <TD>SiO maser sources (Jiang+ 1996)</TD>
            <TD>The observations in the 28SiO J=1-0 v=1, J=1-0 v=2 lines and the 29SiO J=1-0, v=0 lines were simultaneously made toward 181 color-selected IRAS sources in the outer disk of the Galaxy (at longitudes between 90 deg and 250 deg). The 28SiO lines were detected in 63 sources (56 new) and the 29SiO line in 11 sources (9 new). Most of the detections are optically variable stars, mainly Mira-type variables and a few semiregular variables. The detection rate (35%) is much lower than that of the bulge survey performed by the same observational system - the 45m telescope at Nobeyama Radio Observatory. The lower detection rate of SiO maser emission is partly attributed to the increase of contaminations by stars with C-rich circumstellar envelopes and young stellar objects in the outer disk sample. The kinematical implications of the observational results are also discussed. The luminosity distances to the SiO maser sources are estimated from their IRAS fluxes at 12um and colors. By combining the SiO radial velocity and the luminosity distance, the rotation curve of the outer Galactic disk is found to be slightly falling within the Galactocentric distance between 8.5 and 12kpc. The sources located within 20deg from the Galactic anticenter direction are used to check for a peculiar motion of the local standard of rest.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463#1</TD>
            <TD>2011-09-14T18:47:41Z</TD>
            <TD>#Masers#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/106/463</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/106/463</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/106/463 [2]</TD>
            <TD>SiO maser sources (Jiang+ 1996)</TD>
            <TD>The observations in the 28SiO J=1-0 v=1, J=1-0 v=2 lines and the 29SiO J=1-0, v=0 lines were simultaneously made toward 181 color-selected IRAS sources in the outer disk of the Galaxy (at longitudes between 90 deg and 250 deg). The 28SiO lines were detected in 63 sources (56 new) and the 29SiO line in 11 sources (9 new). Most of the detections are optically variable stars, mainly Mira-type variables and a few semiregular variables. The detection rate (35%) is much lower than that of the bulge survey performed by the same observational system - the 45m telescope at Nobeyama Radio Observatory. The lower detection rate of SiO maser emission is partly attributed to the increase of contaminations by stars with C-rich circumstellar envelopes and young stellar objects in the outer disk sample. The kinematical implications of the observational results are also discussed. The luminosity distances to the SiO maser sources are estimated from their IRAS fluxes at 12um and colors. By combining the SiO radial velocity and the luminosity distance, the rotation curve of the outer Galactic disk is found to be slightly falling within the Galactocentric distance between 8.5 and 12kpc. The sources located within 20deg from the Galactic anticenter direction are used to check for a peculiar motion of the local standard of rest.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463#2</TD>
            <TD>2011-09-14T18:47:41Z</TD>
            <TD>#Masers#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/106/463&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/106/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMM/M33 [1]</TD>
            <TD>XMM-Newton M33 Survey Catalog</TD>
            <TD>This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 10^35 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmmxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmmxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33xmmxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmmxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMM/M33 [2]</TD>
            <TD>XMM-Newton M33 Survey Catalog</TD>
            <TD>This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 10^35 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmmxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33xmmxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMM/M33 [3]</TD>
            <TD>XMM-Newton M33 Survey Catalog</TD>
            <TD>This table contains a source catalog based om XMM-Newton observations of the nearby galaxy M 33. In an XMM-Newton raster observation of this bright Local Group spiral galaxy, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity limit of 10^35 erg/s, more than a factor of 10 deeper than earlier ROSAT observations. European Photon Imaging Camera (EPIC) hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. The authors correlated these newly detected X-ray sources with earlier M 33 X-ray catalogs and information from optical, infra-red and radio wavelengths. As M 33 sources, theydetect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations, 175 to 210 background sources are expected in this field. This indicates that about half of the sources which were detected are actually within M 33.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmmxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33xmmxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/106/463 [1]</TD>
            <TD>SiO maser sources (Jiang+ 1996)</TD>
            <TD>The observations in the 28SiO J=1-0 v=1, J=1-0 v=2 lines and the 29SiO J=1-0, v=0 lines were simultaneously made toward 181 color-selected IRAS sources in the outer disk of the Galaxy (at longitudes between 90 deg and 250 deg). The 28SiO lines were detected in 63 sources (56 new) and the 29SiO line in 11 sources (9 new). Most of the detections are optically variable stars, mainly Mira-type variables and a few semiregular variables. The detection rate (35%) is much lower than that of the bulge survey performed by the same observational system - the 45m telescope at Nobeyama Radio Observatory. The lower detection rate of SiO maser emission is partly attributed to the increase of contaminations by stars with C-rich circumstellar envelopes and young stellar objects in the outer disk sample. The kinematical implications of the observational results are also discussed. The luminosity distances to the SiO maser sources are estimated from their IRAS fluxes at 12um and colors. By combining the SiO radial velocity and the luminosity distance, the rotation curve of the outer Galactic disk is found to be slightly falling within the Galactocentric distance between 8.5 and 12kpc. The sources located within 20deg from the Galactic anticenter direction are used to check for a peculiar motion of the local standard of rest.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463#1</TD>
            <TD>2011-09-14T18:47:41Z</TD>
            <TD>#Masers#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/106/463</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/106/463</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/106/463 [2]</TD>
            <TD>SiO maser sources (Jiang+ 1996)</TD>
            <TD>The observations in the 28SiO J=1-0 v=1, J=1-0 v=2 lines and the 29SiO J=1-0, v=0 lines were simultaneously made toward 181 color-selected IRAS sources in the outer disk of the Galaxy (at longitudes between 90 deg and 250 deg). The 28SiO lines were detected in 63 sources (56 new) and the 29SiO line in 11 sources (9 new). Most of the detections are optically variable stars, mainly Mira-type variables and a few semiregular variables. The detection rate (35%) is much lower than that of the bulge survey performed by the same observational system - the 45m telescope at Nobeyama Radio Observatory. The lower detection rate of SiO maser emission is partly attributed to the increase of contaminations by stars with C-rich circumstellar envelopes and young stellar objects in the outer disk sample. The kinematical implications of the observational results are also discussed. The luminosity distances to the SiO maser sources are estimated from their IRAS fluxes at 12um and colors. By combining the SiO radial velocity and the luminosity distance, the rotation curve of the outer Galactic disk is found to be slightly falling within the Galactocentric distance between 8.5 and 12kpc. The sources located within 20deg from the Galactic anticenter direction are used to check for a peculiar motion of the local standard of rest.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463#2</TD>
            <TD>2011-09-14T18:47:41Z</TD>
            <TD>#Masers#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/106/463&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/106/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MARKARIAN2 [1]</TD>
            <TD>Markarian Galaxies Optical Database</TD>
            <TD>A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=markarian2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MARKARIAN2 [2]</TD>
            <TD>Markarian Galaxies Optical Database</TD>
            <TD>A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=markarian2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MARKARIAN2 [3]</TD>
            <TD>Markarian Galaxies Optical Database</TD>
            <TD>A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_markarian2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/106/463 [1]</TD>
            <TD>SiO maser sources (Jiang+ 1996)</TD>
            <TD>The observations in the 28SiO J=1-0 v=1, J=1-0 v=2 lines and the 29SiO J=1-0, v=0 lines were simultaneously made toward 181 color-selected IRAS sources in the outer disk of the Galaxy (at longitudes between 90 deg and 250 deg). The 28SiO lines were detected in 63 sources (56 new) and the 29SiO line in 11 sources (9 new). Most of the detections are optically variable stars, mainly Mira-type variables and a few semiregular variables. The detection rate (35%) is much lower than that of the bulge survey performed by the same observational system - the 45m telescope at Nobeyama Radio Observatory. The lower detection rate of SiO maser emission is partly attributed to the increase of contaminations by stars with C-rich circumstellar envelopes and young stellar objects in the outer disk sample. The kinematical implications of the observational results are also discussed. The luminosity distances to the SiO maser sources are estimated from their IRAS fluxes at 12um and colors. By combining the SiO radial velocity and the luminosity distance, the rotation curve of the outer Galactic disk is found to be slightly falling within the Galactocentric distance between 8.5 and 12kpc. The sources located within 20deg from the Galactic anticenter direction are used to check for a peculiar motion of the local standard of rest.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463#1</TD>
            <TD>2011-09-14T18:47:41Z</TD>
            <TD>#Masers#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/106/463</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/106/463</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/106/463 [2]</TD>
            <TD>SiO maser sources (Jiang+ 1996)</TD>
            <TD>The observations in the 28SiO J=1-0 v=1, J=1-0 v=2 lines and the 29SiO J=1-0, v=0 lines were simultaneously made toward 181 color-selected IRAS sources in the outer disk of the Galaxy (at longitudes between 90 deg and 250 deg). The 28SiO lines were detected in 63 sources (56 new) and the 29SiO line in 11 sources (9 new). Most of the detections are optically variable stars, mainly Mira-type variables and a few semiregular variables. The detection rate (35%) is much lower than that of the bulge survey performed by the same observational system - the 45m telescope at Nobeyama Radio Observatory. The lower detection rate of SiO maser emission is partly attributed to the increase of contaminations by stars with C-rich circumstellar envelopes and young stellar objects in the outer disk sample. The kinematical implications of the observational results are also discussed. The luminosity distances to the SiO maser sources are estimated from their IRAS fluxes at 12um and colors. By combining the SiO radial velocity and the luminosity distance, the rotation curve of the outer Galactic disk is found to be slightly falling within the Galactocentric distance between 8.5 and 12kpc. The sources located within 20deg from the Galactic anticenter direction are used to check for a peculiar motion of the local standard of rest.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463#2</TD>
            <TD>2011-09-14T18:47:41Z</TD>
            <TD>#Masers#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/106/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/106/463&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/106/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MARKARIAN2 [1]</TD>
            <TD>Markarian Galaxies Optical Database</TD>
            <TD>A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=markarian2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MARKARIAN2 [2]</TD>
            <TD>Markarian Galaxies Optical Database</TD>
            <TD>A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=markarian2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MARKARIAN2 [3]</TD>
            <TD>Markarian Galaxies Optical Database</TD>
            <TD>A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_markarian2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/874 [1]</TD>
            <TD>Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)</TD>
            <TD>We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 &lt;= M/L_B(0) &lt;= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874#1</TD>
            <TD>2011-09-14T18:48:10Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/874</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/874</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/874 [2]</TD>
            <TD>Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)</TD>
            <TD>We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 &lt;= M/L_B(0) &lt;= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874#2</TD>
            <TD>2011-09-14T18:48:10Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/874&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/874</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/874 [table2]</TD>
            <TD>Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)</TD>
            <TD>We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 &lt;= M/L_B(0) &lt;= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874#table2</TD>
            <TD>2011-09-14T18:48:10Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/874&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/874</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MARKARIAN2 [1]</TD>
            <TD>Markarian Galaxies Optical Database</TD>
            <TD>A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=markarian2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MARKARIAN2 [2]</TD>
            <TD>Markarian Galaxies Optical Database</TD>
            <TD>A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=markarian2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MARKARIAN2 [3]</TD>
            <TD>Markarian Galaxies Optical Database</TD>
            <TD>A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_markarian2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/874 [1]</TD>
            <TD>Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)</TD>
            <TD>We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 &lt;= M/L_B(0) &lt;= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874#1</TD>
            <TD>2011-09-14T18:48:10Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/874</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/874</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/874 [2]</TD>
            <TD>Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)</TD>
            <TD>We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 &lt;= M/L_B(0) &lt;= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874#2</TD>
            <TD>2011-09-14T18:48:10Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/874&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/874</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/874 [table2]</TD>
            <TD>Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)</TD>
            <TD>We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 &lt;= M/L_B(0) &lt;= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874#table2</TD>
            <TD>2011-09-14T18:48:10Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/874&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/874</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4636CXO [1]</TD>
            <TD>NGC 4636 Chandra X-Ray Point Source Catalog</TD>
            <TD>This catalog lists the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling ~193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, the authors detected 318 individual point sources. For their analysis, they used a subset of 277 detections with &gt;= net 10 counts (a limiting luminosity of approximately 1.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV band, outside the central 1.5 arcminutes bright galaxy core). This table contains this subset of 277 X-ray sources. The authors discuss the radial distribution of the point sources. Between 1.5 and 6 arcminutes from the center, 25% of the sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% to be low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6 arcminutes, background sources (AGN) will dominate the point sources. The authors explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, ~10% of the sources in each observation show significant short-term variability. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope Alpha = 1.14 +/- 0.03. The authors do not detect, but estimate an upper limit of ~4.5 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the current X-ray luminosity of, the historical supernova SN1939A. They find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1.5 to 6 arcminutes of the galaxy center, 48 of the 129 X-ray point sources (37%) with &gt;=10 net counts are matched with GC candidates. Since they expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, the authors find that ~70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. The authors do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;= L_x &lt;= 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4636cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4636cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4636cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4636cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4636CXO [2]</TD>
            <TD>NGC 4636 Chandra X-Ray Point Source Catalog</TD>
            <TD>This catalog lists the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling ~193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, the authors detected 318 individual point sources. For their analysis, they used a subset of 277 detections with &gt;= net 10 counts (a limiting luminosity of approximately 1.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV band, outside the central 1.5 arcminutes bright galaxy core). This table contains this subset of 277 X-ray sources. The authors discuss the radial distribution of the point sources. Between 1.5 and 6 arcminutes from the center, 25% of the sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% to be low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6 arcminutes, background sources (AGN) will dominate the point sources. The authors explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, ~10% of the sources in each observation show significant short-term variability. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope Alpha = 1.14 +/- 0.03. The authors do not detect, but estimate an upper limit of ~4.5 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the current X-ray luminosity of, the historical supernova SN1939A. They find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1.5 to 6 arcminutes of the galaxy center, 48 of the 129 X-ray point sources (37%) with &gt;=10 net counts are matched with GC candidates. Since they expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, the authors find that ~70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. The authors do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;= L_x &lt;= 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4636cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4636cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4636cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4636cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4636CXO [3]</TD>
            <TD>NGC 4636 Chandra X-Ray Point Source Catalog</TD>
            <TD>This catalog lists the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling ~193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, the authors detected 318 individual point sources. For their analysis, they used a subset of 277 detections with &gt;= net 10 counts (a limiting luminosity of approximately 1.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV band, outside the central 1.5 arcminutes bright galaxy core). This table contains this subset of 277 X-ray sources. The authors discuss the radial distribution of the point sources. Between 1.5 and 6 arcminutes from the center, 25% of the sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% to be low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6 arcminutes, background sources (AGN) will dominate the point sources. The authors explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, ~10% of the sources in each observation show significant short-term variability. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope Alpha = 1.14 +/- 0.03. The authors do not detect, but estimate an upper limit of ~4.5 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the current X-ray luminosity of, the historical supernova SN1939A. They find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1.5 to 6 arcminutes of the galaxy center, 48 of the 129 X-ray point sources (37%) with &gt;=10 net counts are matched with GC candidates. Since they expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, the authors find that ~70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. The authors do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;= L_x &lt;= 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4636cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4636cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4636cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4636cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/874 [1]</TD>
            <TD>Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)</TD>
            <TD>We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 &lt;= M/L_B(0) &lt;= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874#1</TD>
            <TD>2011-09-14T18:48:10Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/874</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/874</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/874 [2]</TD>
            <TD>Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)</TD>
            <TD>We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 &lt;= M/L_B(0) &lt;= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874#2</TD>
            <TD>2011-09-14T18:48:10Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/874&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/874</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/874 [table2]</TD>
            <TD>Kinematics of MKW and AWM Poor Clusters (Beers+ 1995)</TD>
            <TD>We report 472 new redshifts for 416 galaxies in the regions of the 23 poor clusters of galaxies originally identified by Morgan, Kayser, and White, and Albert, White and Morgan. Eighteen of the poor clusters now have 10 or more available redshifts within 1.5h^-1 Mpc of the central galaxy; 11 clusters have at least 20 available redshifts. Based on the 21 clusters for which we have sufficient velocity information, the median velocity scale is 336 km/s, a factor of 2 smaller than found for rich clusters. Several of the poor clusters exhibit complex velocity distributions due to the presence of nearby clumps of galaxies. We check on the velocity of the dominant galaxy in each poor cluster relative to the remaining cluster members. Significantly high relative velocities of the dominant galaxy are found in only 4 of 21 poor clusters, 3 of which we suspect are due to contamination of the parent velocity distribution. Several statistical tests indicate that the D/cD galaxies are at the kinematic centers of the parent poor cluster velocity distributions. Mass-to-light ratios for 13 of the 15 poor clusters for which we have the required data are in the range 50 &lt;= M/L_B(0) &lt;= 200 Msun/Lsun. The complex nature of the regions surrounding many of the poor clusters suggests that these groupings may represent an early epoch of cluster formation. For example, the poor clusters MKW7 and MKW8 are shown to be gravitationally bound and likely to merge to form a richer cluster within the next several Gyrs. Eight of the nine other poor clusters for which simple two-body dynamical models can be carried out are consistent with being bound to other clumps in their vicinity. Additional complex systems with more than two gravitationally bound clumps are observed among the poor clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874#table2</TD>
            <TD>2011-09-14T18:48:10Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/874</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/874&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/874</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>LGA</TD>
            <TD>2MASS Large Galaxy Atlas</TD>
            <TD>The high sensitivity and angular resolution of the 2MASS Large Galaxy Atlas (LGA) images allows closer inspection of diverse stellar populations, large-scale structures such as spirals, bulges, warps and bars, star formation regions and evolution of galaxies. This image atlas represents the first uniform, all-sky, view of galaxies as seen in the near-infrared wavelength window that is most sensitive to the dominant mass component of galaxies.</TD>
            <TD>NASA/IPAC Infrared Science Archive</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://irsa.ipac/LGA#1</TD>
            <TD>2007-04-11T08:52:38Z</TD>
            <TD>##</TD>
            <TD>#Archive#Journal#Project#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://irsa.ipac/LGA</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://irsa.ipac.caltech.edu/cgi-bin/Atlas/nph-atlas?mission=LGA&amp;hdr_location=%5CLGADataPath%5C&amp;SIAP_ACTIVE=1&amp;collection_desc=2MASS+Large+Galaxy+Atlas+%28LGA%29&amp;</TD>
            <TD />
            <TD>200</TD>
            <TD>ivo://irsa.ipac/IRSA</TD>
            <TD>http://irsa.ipac.caltech.edu/data/LGA</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/59 [1]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#1</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/59</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/59 [2]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#2</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/59&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/59 [appendxb]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#appendxb</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/59&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/59 [appendxa]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#appendxa</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/59&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/626/L15 [1]</TD>
            <TD>Templates for photometric redshifts of submm sources (Hunt+, 2005)</TD>
            <TD>There is growing evidence that some star-forming galaxies at z&gt;1 are characterized by high efficiencies and specific star formation rates. In the local universe, these traits are shared by "active" blue compact dwarf galaxies (BCDs) with compact and dense star-forming regions. The spectral energy distributions (SEDs) of these BCDs are dominated by young massive star clusters, embedded in a cocoon of dust. In this Letter, we incorporate these BCD SEDs as templates for two samples of high-redshift galaxy populations selected at submillimeter wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/L15#1</TD>
            <TD>2011-09-14T20:02:06Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/L15</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/626/L15</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/L15</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/626/L15 [2]</TD>
            <TD>Templates for photometric redshifts of submm sources (Hunt+, 2005)</TD>
            <TD>There is growing evidence that some star-forming galaxies at z&gt;1 are characterized by high efficiencies and specific star formation rates. In the local universe, these traits are shared by "active" blue compact dwarf galaxies (BCDs) with compact and dense star-forming regions. The spectral energy distributions (SEDs) of these BCDs are dominated by young massive star clusters, embedded in a cocoon of dust. In this Letter, we incorporate these BCD SEDs as templates for two samples of high-redshift galaxy populations selected at submillimeter wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/L15#2</TD>
            <TD>2011-09-14T20:02:06Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/L15</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/626/L15&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/L15</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/59 [1]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#1</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/59</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/59 [2]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#2</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/59&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/59 [appendxb]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#appendxb</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/59&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/59 [appendxa]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#appendxa</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/59&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/626/L15 [1]</TD>
            <TD>Templates for photometric redshifts of submm sources (Hunt+, 2005)</TD>
            <TD>There is growing evidence that some star-forming galaxies at z&gt;1 are characterized by high efficiencies and specific star formation rates. In the local universe, these traits are shared by "active" blue compact dwarf galaxies (BCDs) with compact and dense star-forming regions. The spectral energy distributions (SEDs) of these BCDs are dominated by young massive star clusters, embedded in a cocoon of dust. In this Letter, we incorporate these BCD SEDs as templates for two samples of high-redshift galaxy populations selected at submillimeter wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/L15#1</TD>
            <TD>2011-09-14T20:02:06Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/L15</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/626/L15</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/L15</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/626/L15 [2]</TD>
            <TD>Templates for photometric redshifts of submm sources (Hunt+, 2005)</TD>
            <TD>There is growing evidence that some star-forming galaxies at z&gt;1 are characterized by high efficiencies and specific star formation rates. In the local universe, these traits are shared by "active" blue compact dwarf galaxies (BCDs) with compact and dense star-forming regions. The spectral energy distributions (SEDs) of these BCDs are dominated by young massive star clusters, embedded in a cocoon of dust. In this Letter, we incorporate these BCD SEDs as templates for two samples of high-redshift galaxy populations selected at submillimeter wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/L15#2</TD>
            <TD>2011-09-14T20:02:06Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/L15</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/626/L15&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/L15</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/59 [1]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#1</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/59</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/59 [2]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#2</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/59&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/59 [appendxb]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#appendxb</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/59&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/59 [appendxa]</TD>
            <TD>The central Fornax Cluster. I. Galaxy photometry (Hilker+ 1999)</TD>
            <TD>In this paper, a photometric catalog is presented of V and I photometry of galaxies in the central regions of the Fornax galaxy cluster. Our 11 CCD fields cover 0.17 square degrees in total. The limiting surface brightness is around 24mag/arcsec^2^, similar to that of Ferguson's (1989, Cat. &lt;VII/180&gt;) catalog, whereas our limiting total magnitude is around V=22mag, about two magnitudes fainter. The photometric properties of more than 870 objects are presented as a catalog (Appendix A). The properties and fit parameters of the surface brightness profiles for a sub-sample are presented in a second catalog (Appendix B). Four new dwarf galaxies are added to Ferguson's catalog. However, we confirm that the dwarf galaxies in Fornax follow a similar surface brightness -- magnitude relation as the Local Group dwarfs. They also follow the color (metallicity) -- magnitude relation seen in other galaxy clusters. A formerly suspected excess of dwarf galaxies surrounding the central giant cD galaxy NGC 1399 can be explained by the superposition of a background cluster at z=0.11 (Hilker et al. 1998, Cat. &lt;J/A+AS/134/75&gt;, Paper II in this series).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59#appendxa</TD>
            <TD>2011-09-14T18:48:26Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/59</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/59&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/59</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/369/1351 [1]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#1</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/369/1351</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/369/1351 [2]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#2</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/369/1351&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1351 [tablea1]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#tablea1</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1351&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1351 [tableb1]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#tableb1</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1351&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/75 [1]</TD>
            <TD>Central Fornax Cluster. II. Galaxy spectroscopy (Hilker+ 1999)</TD>
            <TD>In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. &lt;J/A+AS/134/59&gt;). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. &lt;VII/180&gt;). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75#1</TD>
            <TD>2011-09-14T18:48:27Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/75</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/75</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/75 [2]</TD>
            <TD>Central Fornax Cluster. II. Galaxy spectroscopy (Hilker+ 1999)</TD>
            <TD>In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. &lt;J/A+AS/134/59&gt;). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. &lt;VII/180&gt;). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75#2</TD>
            <TD>2011-09-14T18:48:27Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/75&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/75</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/75 [table2]</TD>
            <TD>Central Fornax Cluster. II. Galaxy spectroscopy (Hilker+ 1999)</TD>
            <TD>In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. &lt;J/A+AS/134/59&gt;). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. &lt;VII/180&gt;). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75#table2</TD>
            <TD>2011-09-14T18:48:27Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/75&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/75</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/369/1351 [1]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#1</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/369/1351</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/369/1351 [2]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#2</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/369/1351&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1351 [tablea1]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#tablea1</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1351&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1351 [tableb1]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#tableb1</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1351&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/75 [1]</TD>
            <TD>Central Fornax Cluster. II. Galaxy spectroscopy (Hilker+ 1999)</TD>
            <TD>In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. &lt;J/A+AS/134/59&gt;). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. &lt;VII/180&gt;). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75#1</TD>
            <TD>2011-09-14T18:48:27Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/75</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/75</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/75 [2]</TD>
            <TD>Central Fornax Cluster. II. Galaxy spectroscopy (Hilker+ 1999)</TD>
            <TD>In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. &lt;J/A+AS/134/59&gt;). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. &lt;VII/180&gt;). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75#2</TD>
            <TD>2011-09-14T18:48:27Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/75&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/75</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/75 [table2]</TD>
            <TD>Central Fornax Cluster. II. Galaxy spectroscopy (Hilker+ 1999)</TD>
            <TD>In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. &lt;J/A+AS/134/59&gt;). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. &lt;VII/180&gt;). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75#table2</TD>
            <TD>2011-09-14T18:48:27Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/75&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/75</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/369/1351 [1]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#1</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/369/1351</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/369/1351 [2]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#2</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/369/1351&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1351 [tablea1]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#tablea1</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1351&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/369/1351 [tableb1]</TD>
            <TD>Velocities in the possible Eridanus group (Brough+, 2006)</TD>
            <TD>We examine a possible supergroup in the direction of the Eridanus constellation using 6dF Galaxy Survey second data release (6dFGS DR2) positions and velocities together with Two-Micron All-Sky Survey and Hyper-Lyon-Meudon Extragalactic DAtabase photometry. We perform a friends-of-friends analysis to determine which galaxies are associated with each substructure before examining the properties of the constituent galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351#tableb1</TD>
            <TD>2011-09-14T20:02:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1351</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/369/1351&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1351</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/75 [1]</TD>
            <TD>Central Fornax Cluster. II. Galaxy spectroscopy (Hilker+ 1999)</TD>
            <TD>In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. &lt;J/A+AS/134/59&gt;). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. &lt;VII/180&gt;). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75#1</TD>
            <TD>2011-09-14T18:48:27Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/75</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/75</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/75 [2]</TD>
            <TD>Central Fornax Cluster. II. Galaxy spectroscopy (Hilker+ 1999)</TD>
            <TD>In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. &lt;J/A+AS/134/59&gt;). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. &lt;VII/180&gt;). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75#2</TD>
            <TD>2011-09-14T18:48:27Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/75&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/75</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/75 [table2]</TD>
            <TD>Central Fornax Cluster. II. Galaxy spectroscopy (Hilker+ 1999)</TD>
            <TD>In this paper, radial velocities of 94 galaxies brighter than about V_tot=20mag in the direction of the central Fornax cluster have been measured. The galaxies have been selected from the photometric catalog of Paper I (Hilker et al., 1998, Cat. &lt;J/A+AS/134/59&gt;). Most of the velocity determinations of the fainter galaxies are based on strong emission lines of late type galaxies. Table 2 of this paper contains the position, magnitude and velocity of all galaxies. Except for 8 Fornax members, all galaxies lie in the background. Among the 8 members, there are 5 nucleated dwarf ellipticals that are already listed in the FCC (Ferguson, 1989, Cat. &lt;VII/180&gt;). Two of the 3 "new" members are very compact and have surface brightnesses comparable to globular clusters, however their luminosities are in the range of dwarf elliptical nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75#table2</TD>
            <TD>2011-09-14T18:48:27Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jun-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/75</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/75&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/75</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/544/A81 [1]</TD>
            <TD>Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)</TD>
            <TD>The measurements of apparent magnitudes, diameters (D_25_), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81#1</TD>
            <TD>2012-10-28T21:55:37Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/544/A81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/544/A81 [2]</TD>
            <TD>Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)</TD>
            <TD>The measurements of apparent magnitudes, diameters (D_25_), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81#2</TD>
            <TD>2012-10-28T21:55:37Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/544/A81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/544/A81 [snsdss]</TD>
            <TD>Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)</TD>
            <TD>The measurements of apparent magnitudes, diameters (D_25_), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81#snsdss</TD>
            <TD>2012-10-28T21:55:37Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/544/A81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/181 [1]</TD>
            <TD>BVI photometry of Whiting 1 (Carraro+, 2007)</TD>
            <TD>Recently Carraro (2005ApJ...621L..61C) drew attention to the remarkable star cluster Whiting 1, showing that it lies at about 40kpc from the Sun and is therefore unquestionably a member of the Galactic halo (l=-60.6{deg}). Its Color Magnitude Diagram (CMD) indicated that Whiting 1 is very young (~5Gyrs) for a globular cluster. It is highly likely that Whiting 1 is originated in a dwarf galaxy that has since been disrupted by the Milky Way. The main purpose of the present study is to better constrain the properties of Whiting 1, and assess whether it belongs to a stellar stream from the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph). Deep CCD photometry in the BVI pass-band obtained with the VLT is used to improve the quality of the CMD, and provide more solid estimates of the cluster distance and age, while high resolution spectra of three evolved stars obtained at Magellan is used to derive the cluster kinematics and analyze its possible membership to the Sgr dSph. We demonstrate that - independently on the Halo model employed - Whiting 1 is part of the trailing stream of the Sgr dSph. We derive a new age estimate of 6.5^+1.0^_-0.5_Gyr, and a smaller heliocentric distance of 29.4^+1.8^_-2.0_kpc. The number of globular clusters confirmed to be members of Sgr dSph is now 6. Among these clusters, Whiting 1 is particularly interesting, being the youngest and one of the most metal rich. The existence of Whiting 1 shows how the Sgr dSph was able to form star clusters for a period at least of 6Gyr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181#1</TD>
            <TD>2011-09-14T20:04:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/181 [2]</TD>
            <TD>BVI photometry of Whiting 1 (Carraro+, 2007)</TD>
            <TD>Recently Carraro (2005ApJ...621L..61C) drew attention to the remarkable star cluster Whiting 1, showing that it lies at about 40kpc from the Sun and is therefore unquestionably a member of the Galactic halo (l=-60.6{deg}). Its Color Magnitude Diagram (CMD) indicated that Whiting 1 is very young (~5Gyrs) for a globular cluster. It is highly likely that Whiting 1 is originated in a dwarf galaxy that has since been disrupted by the Milky Way. The main purpose of the present study is to better constrain the properties of Whiting 1, and assess whether it belongs to a stellar stream from the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph). Deep CCD photometry in the BVI pass-band obtained with the VLT is used to improve the quality of the CMD, and provide more solid estimates of the cluster distance and age, while high resolution spectra of three evolved stars obtained at Magellan is used to derive the cluster kinematics and analyze its possible membership to the Sgr dSph. We demonstrate that - independently on the Halo model employed - Whiting 1 is part of the trailing stream of the Sgr dSph. We derive a new age estimate of 6.5^+1.0^_-0.5_Gyr, and a smaller heliocentric distance of 29.4^+1.8^_-2.0_kpc. The number of globular clusters confirmed to be members of Sgr dSph is now 6. Among these clusters, Whiting 1 is particularly interesting, being the youngest and one of the most metal rich. The existence of Whiting 1 shows how the Sgr dSph was able to form star clusters for a period at least of 6Gyr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181#2</TD>
            <TD>2011-09-14T20:04:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/181 [table1]</TD>
            <TD>BVI photometry of Whiting 1 (Carraro+, 2007)</TD>
            <TD>Recently Carraro (2005ApJ...621L..61C) drew attention to the remarkable star cluster Whiting 1, showing that it lies at about 40kpc from the Sun and is therefore unquestionably a member of the Galactic halo (l=-60.6{deg}). Its Color Magnitude Diagram (CMD) indicated that Whiting 1 is very young (~5Gyrs) for a globular cluster. It is highly likely that Whiting 1 is originated in a dwarf galaxy that has since been disrupted by the Milky Way. The main purpose of the present study is to better constrain the properties of Whiting 1, and assess whether it belongs to a stellar stream from the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph). Deep CCD photometry in the BVI pass-band obtained with the VLT is used to improve the quality of the CMD, and provide more solid estimates of the cluster distance and age, while high resolution spectra of three evolved stars obtained at Magellan is used to derive the cluster kinematics and analyze its possible membership to the Sgr dSph. We demonstrate that - independently on the Halo model employed - Whiting 1 is part of the trailing stream of the Sgr dSph. We derive a new age estimate of 6.5^+1.0^_-0.5_Gyr, and a smaller heliocentric distance of 29.4^+1.8^_-2.0_kpc. The number of globular clusters confirmed to be members of Sgr dSph is now 6. Among these clusters, Whiting 1 is particularly interesting, being the youngest and one of the most metal rich. The existence of Whiting 1 shows how the Sgr dSph was able to form star clusters for a period at least of 6Gyr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181#table1</TD>
            <TD>2011-09-14T20:04:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/544/A81 [1]</TD>
            <TD>Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)</TD>
            <TD>The measurements of apparent magnitudes, diameters (D_25_), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81#1</TD>
            <TD>2012-10-28T21:55:37Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/544/A81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/544/A81 [2]</TD>
            <TD>Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)</TD>
            <TD>The measurements of apparent magnitudes, diameters (D_25_), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81#2</TD>
            <TD>2012-10-28T21:55:37Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/544/A81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/544/A81 [snsdss]</TD>
            <TD>Supernovae and their hosts in the SDSS DR8 (Hakobyan+, 2012)</TD>
            <TD>The measurements of apparent magnitudes, diameters (D_25_), axial ratios (b/a), and position angles (PA) of SN host galaxies were made using the images extracted from the SDSS g-band. For each host galaxy, we analyzed RGB images of the SDSS to accurately measure the position of its nucleus to provide the SDSS name. With these images, we also provide the host galaxy's morphological type, and note if it has a bar, a disturbed disk, and whether it is part of an interacting or merging system. In addition, the SDSS nuclear spectra were analyzed to diagnose the central power source of the galaxies. Special attention was paid to collect accurate data on the spectroscopic classes, coordinates, offsets of SNe, and heliocentric redshifts of the host galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81#snsdss</TD>
            <TD>2012-10-28T21:55:37Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/544/A81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/544/A81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/544/A81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CENACXO [1]</TD>
            <TD>Centaurus A Galaxy Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, 246 individual point sources are detected above a limiting luminosity of ~ 2 * 10^36 ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. Eight foreground stars were identified in these observations, and nine of the sources were identified with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view were detected. The faintest source in this table has 5 counts, which corresponds to a limiting luminosity of ~2.2 x 10^36 erg/s at the center of the field of view. The two observations of Cen A were made with the ACIS-I array (observation IDs were 00316 and 00962) on 1999 December 5 and 2000 May 17, with 35.9 36.5 ks exposures, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cenacxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cenacxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cenacxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cenacxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CENACXO [2]</TD>
            <TD>Centaurus A Galaxy Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, 246 individual point sources are detected above a limiting luminosity of ~ 2 * 10^36 ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. Eight foreground stars were identified in these observations, and nine of the sources were identified with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view were detected. The faintest source in this table has 5 counts, which corresponds to a limiting luminosity of ~2.2 x 10^36 erg/s at the center of the field of view. The two observations of Cen A were made with the ACIS-I array (observation IDs were 00316 and 00962) on 1999 December 5 and 2000 May 17, with 35.9 36.5 ks exposures, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cenacxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cenacxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cenacxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cenacxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CENACXO [3]</TD>
            <TD>Centaurus A Galaxy Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, 246 individual point sources are detected above a limiting luminosity of ~ 2 * 10^36 ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. Eight foreground stars were identified in these observations, and nine of the sources were identified with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view were detected. The faintest source in this table has 5 counts, which corresponds to a limiting luminosity of ~2.2 x 10^36 erg/s at the center of the field of view. The two observations of Cen A were made with the ACIS-I array (observation IDs were 00316 and 00962) on 1999 December 5 and 2000 May 17, with 35.9 36.5 ks exposures, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cenacxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cenacxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cenacxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cenacxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CENACXO [1]</TD>
            <TD>Centaurus A Galaxy Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, 246 individual point sources are detected above a limiting luminosity of ~ 2 * 10^36 ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. Eight foreground stars were identified in these observations, and nine of the sources were identified with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view were detected. The faintest source in this table has 5 counts, which corresponds to a limiting luminosity of ~2.2 x 10^36 erg/s at the center of the field of view. The two observations of Cen A were made with the ACIS-I array (observation IDs were 00316 and 00962) on 1999 December 5 and 2000 May 17, with 35.9 36.5 ks exposures, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cenacxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cenacxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cenacxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cenacxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CENACXO [2]</TD>
            <TD>Centaurus A Galaxy Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, 246 individual point sources are detected above a limiting luminosity of ~ 2 * 10^36 ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. Eight foreground stars were identified in these observations, and nine of the sources were identified with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view were detected. The faintest source in this table has 5 counts, which corresponds to a limiting luminosity of ~2.2 x 10^36 erg/s at the center of the field of view. The two observations of Cen A were made with the ACIS-I array (observation IDs were 00316 and 00962) on 1999 December 5 and 2000 May 17, with 35.9 36.5 ks exposures, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cenacxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cenacxo&amp;</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cenacxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CENACXO [3]</TD>
            <TD>Centaurus A Galaxy Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, 246 individual point sources are detected above a limiting luminosity of ~ 2 * 10^36 ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. Eight foreground stars were identified in these observations, and nine of the sources were identified with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view were detected. The faintest source in this table has 5 counts, which corresponds to a limiting luminosity of ~2.2 x 10^36 erg/s at the center of the field of view. The two observations of Cen A were made with the ACIS-I array (observation IDs were 00316 and 00962) on 1999 December 5 and 2000 May 17, with 35.9 36.5 ks exposures, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cenacxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/cenacxo</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cenacxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cenacxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CENACXO [1]</TD>
            <TD>Centaurus A Galaxy Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, 246 individual point sources are detected above a limiting luminosity of ~ 2 * 10^36 ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. Eight foreground stars were identified in these observations, and nine of the sources were identified with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view were detected. The faintest source in this table has 5 counts, which corresponds to a limiting luminosity of ~2.2 x 10^36 erg/s at the center of the field of view. The two observations of Cen A were made with the ACIS-I array (observation IDs were 00316 and 00962) on 1999 December 5 and 2000 May 17, with 35.9 36.5 ks exposures, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cenacxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cenacxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cenacxo.html</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>CENACXO [2]</TD>
            <TD>Centaurus A Galaxy Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, 246 individual point sources are detected above a limiting luminosity of ~ 2 * 10^36 ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. Eight foreground stars were identified in these observations, and nine of the sources were identified with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view were detected. The faintest source in this table has 5 counts, which corresponds to a limiting luminosity of ~2.2 x 10^36 erg/s at the center of the field of view. The two observations of Cen A were made with the ACIS-I array (observation IDs were 00316 and 00962) on 1999 December 5 and 2000 May 17, with 35.9 36.5 ks exposures, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cenacxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cenacxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CENACXO [3]</TD>
            <TD>Centaurus A Galaxy Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, 246 individual point sources are detected above a limiting luminosity of ~ 2 * 10^36 ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. Eight foreground stars were identified in these observations, and nine of the sources were identified with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view were detected. The faintest source in this table has 5 counts, which corresponds to a limiting luminosity of ~2.2 x 10^36 erg/s at the center of the field of view. The two observations of Cen A were made with the ACIS-I array (observation IDs were 00316 and 00962) on 1999 December 5 and 2000 May 17, with 35.9 36.5 ks exposures, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cenacxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cenacxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cenacxo.html</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>CHAMPLANE [1]</TD>
            <TD>Chandra Multiwavelength Plane Survey Optical ID Catalog</TD>
            <TD>The authors have carried out optical and X-ray spectral analyses on a sample of 136 candidate optical counterparts of X-ray sources found in five Galactic bulge fields included in their Chandra Multiwavelength Plane (ChaMPlane) Survey. They used a combination of optical spectral fitting and quantile X-ray analysis to obtain the hydrogen column density toward each object, and a three-dimensional dust model of the Galaxy to estimate the most probable distance in each case. They present the discovery of a population of stellar coronal emission sources, likely consisting of pre-main-sequence, young main-sequence, and main-sequence stars, as well as a component of active binaries of RS CVn or BY Dra type. They identify one candidate quiescent low-mass X-ray binary with a subgiant companion, but note that this object may also be an RS CVn system. They report the discovery of 3 new X-ray-detected cataclysmic variables (CVs) in the direction of the Galactic center (at distances &lt;~2 kpc). This number is in excess of predictions made with a simple CV model based on a local CV space density of &lt;~10&lt;sup&gt;-5&lt;/sup&gt; pc&lt;sup&gt;-3&lt;/sup&gt;, and a scale height of ~200 pc. They discuss several possible reasons for this observed excess in their paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champlane#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/champlane</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=champlane&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champlane.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHAMPLANE [2]</TD>
            <TD>Chandra Multiwavelength Plane Survey Optical ID Catalog</TD>
            <TD>The authors have carried out optical and X-ray spectral analyses on a sample of 136 candidate optical counterparts of X-ray sources found in five Galactic bulge fields included in their Chandra Multiwavelength Plane (ChaMPlane) Survey. They used a combination of optical spectral fitting and quantile X-ray analysis to obtain the hydrogen column density toward each object, and a three-dimensional dust model of the Galaxy to estimate the most probable distance in each case. They present the discovery of a population of stellar coronal emission sources, likely consisting of pre-main-sequence, young main-sequence, and main-sequence stars, as well as a component of active binaries of RS CVn or BY Dra type. They identify one candidate quiescent low-mass X-ray binary with a subgiant companion, but note that this object may also be an RS CVn system. They report the discovery of 3 new X-ray-detected cataclysmic variables (CVs) in the direction of the Galactic center (at distances &lt;~2 kpc). This number is in excess of predictions made with a simple CV model based on a local CV space density of &lt;~10&lt;sup&gt;-5&lt;/sup&gt; pc&lt;sup&gt;-3&lt;/sup&gt;, and a scale height of ~200 pc. They discuss several possible reasons for this observed excess in their paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champlane#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ParamHTTP</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champlane.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHAMPLANE [3]</TD>
            <TD>Chandra Multiwavelength Plane Survey Optical ID Catalog</TD>
            <TD>The authors have carried out optical and X-ray spectral analyses on a sample of 136 candidate optical counterparts of X-ray sources found in five Galactic bulge fields included in their Chandra Multiwavelength Plane (ChaMPlane) Survey. They used a combination of optical spectral fitting and quantile X-ray analysis to obtain the hydrogen column density toward each object, and a three-dimensional dust model of the Galaxy to estimate the most probable distance in each case. They present the discovery of a population of stellar coronal emission sources, likely consisting of pre-main-sequence, young main-sequence, and main-sequence stars, as well as a component of active binaries of RS CVn or BY Dra type. They identify one candidate quiescent low-mass X-ray binary with a subgiant companion, but note that this object may also be an RS CVn system. They report the discovery of 3 new X-ray-detected cataclysmic variables (CVs) in the direction of the Galactic center (at distances &lt;~2 kpc). This number is in excess of predictions made with a simple CV model based on a local CV space density of &lt;~10&lt;sup&gt;-5&lt;/sup&gt; pc&lt;sup&gt;-3&lt;/sup&gt;, and a scale height of ~200 pc. They discuss several possible reasons for this observed excess in their paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champlane#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_champlane&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champlane.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHAMPLANE [1]</TD>
            <TD>Chandra Multiwavelength Plane Survey Optical ID Catalog</TD>
            <TD>The authors have carried out optical and X-ray spectral analyses on a sample of 136 candidate optical counterparts of X-ray sources found in five Galactic bulge fields included in their Chandra Multiwavelength Plane (ChaMPlane) Survey. They used a combination of optical spectral fitting and quantile X-ray analysis to obtain the hydrogen column density toward each object, and a three-dimensional dust model of the Galaxy to estimate the most probable distance in each case. They present the discovery of a population of stellar coronal emission sources, likely consisting of pre-main-sequence, young main-sequence, and main-sequence stars, as well as a component of active binaries of RS CVn or BY Dra type. They identify one candidate quiescent low-mass X-ray binary with a subgiant companion, but note that this object may also be an RS CVn system. They report the discovery of 3 new X-ray-detected cataclysmic variables (CVs) in the direction of the Galactic center (at distances &lt;~2 kpc). This number is in excess of predictions made with a simple CV model based on a local CV space density of &lt;~10&lt;sup&gt;-5&lt;/sup&gt; pc&lt;sup&gt;-3&lt;/sup&gt;, and a scale height of ~200 pc. They discuss several possible reasons for this observed excess in their paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champlane#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=champlane&amp;</TD>
            <TD>180</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champlane.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHAMPLANE [2]</TD>
            <TD>Chandra Multiwavelength Plane Survey Optical ID Catalog</TD>
            <TD>The authors have carried out optical and X-ray spectral analyses on a sample of 136 candidate optical counterparts of X-ray sources found in five Galactic bulge fields included in their Chandra Multiwavelength Plane (ChaMPlane) Survey. They used a combination of optical spectral fitting and quantile X-ray analysis to obtain the hydrogen column density toward each object, and a three-dimensional dust model of the Galaxy to estimate the most probable distance in each case. They present the discovery of a population of stellar coronal emission sources, likely consisting of pre-main-sequence, young main-sequence, and main-sequence stars, as well as a component of active binaries of RS CVn or BY Dra type. They identify one candidate quiescent low-mass X-ray binary with a subgiant companion, but note that this object may also be an RS CVn system. They report the discovery of 3 new X-ray-detected cataclysmic variables (CVs) in the direction of the Galactic center (at distances &lt;~2 kpc). This number is in excess of predictions made with a simple CV model based on a local CV space density of &lt;~10&lt;sup&gt;-5&lt;/sup&gt; pc&lt;sup&gt;-3&lt;/sup&gt;, and a scale height of ~200 pc. They discuss several possible reasons for this observed excess in their paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
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            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=champlane&amp;</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champlane.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHAMPLANE [3]</TD>
            <TD>Chandra Multiwavelength Plane Survey Optical ID Catalog</TD>
            <TD>The authors have carried out optical and X-ray spectral analyses on a sample of 136 candidate optical counterparts of X-ray sources found in five Galactic bulge fields included in their Chandra Multiwavelength Plane (ChaMPlane) Survey. They used a combination of optical spectral fitting and quantile X-ray analysis to obtain the hydrogen column density toward each object, and a three-dimensional dust model of the Galaxy to estimate the most probable distance in each case. They present the discovery of a population of stellar coronal emission sources, likely consisting of pre-main-sequence, young main-sequence, and main-sequence stars, as well as a component of active binaries of RS CVn or BY Dra type. They identify one candidate quiescent low-mass X-ray binary with a subgiant companion, but note that this object may also be an RS CVn system. They report the discovery of 3 new X-ray-detected cataclysmic variables (CVs) in the direction of the Galactic center (at distances &lt;~2 kpc). This number is in excess of predictions made with a simple CV model based on a local CV space density of &lt;~10&lt;sup&gt;-5&lt;/sup&gt; pc&lt;sup&gt;-3&lt;/sup&gt;, and a scale height of ~200 pc. They discuss several possible reasons for this observed excess in their paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champlane#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/champlane</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_champlane&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champlane.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHAMPLANE [1]</TD>
            <TD>Chandra Multiwavelength Plane Survey Optical ID Catalog</TD>
            <TD>The authors have carried out optical and X-ray spectral analyses on a sample of 136 candidate optical counterparts of X-ray sources found in five Galactic bulge fields included in their Chandra Multiwavelength Plane (ChaMPlane) Survey. They used a combination of optical spectral fitting and quantile X-ray analysis to obtain the hydrogen column density toward each object, and a three-dimensional dust model of the Galaxy to estimate the most probable distance in each case. They present the discovery of a population of stellar coronal emission sources, likely consisting of pre-main-sequence, young main-sequence, and main-sequence stars, as well as a component of active binaries of RS CVn or BY Dra type. They identify one candidate quiescent low-mass X-ray binary with a subgiant companion, but note that this object may also be an RS CVn system. They report the discovery of 3 new X-ray-detected cataclysmic variables (CVs) in the direction of the Galactic center (at distances &lt;~2 kpc). This number is in excess of predictions made with a simple CV model based on a local CV space density of &lt;~10&lt;sup&gt;-5&lt;/sup&gt; pc&lt;sup&gt;-3&lt;/sup&gt;, and a scale height of ~200 pc. They discuss several possible reasons for this observed excess in their paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champlane#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/champlane</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=champlane&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champlane.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHAMPLANE [2]</TD>
            <TD>Chandra Multiwavelength Plane Survey Optical ID Catalog</TD>
            <TD>The authors have carried out optical and X-ray spectral analyses on a sample of 136 candidate optical counterparts of X-ray sources found in five Galactic bulge fields included in their Chandra Multiwavelength Plane (ChaMPlane) Survey. They used a combination of optical spectral fitting and quantile X-ray analysis to obtain the hydrogen column density toward each object, and a three-dimensional dust model of the Galaxy to estimate the most probable distance in each case. They present the discovery of a population of stellar coronal emission sources, likely consisting of pre-main-sequence, young main-sequence, and main-sequence stars, as well as a component of active binaries of RS CVn or BY Dra type. They identify one candidate quiescent low-mass X-ray binary with a subgiant companion, but note that this object may also be an RS CVn system. They report the discovery of 3 new X-ray-detected cataclysmic variables (CVs) in the direction of the Galactic center (at distances &lt;~2 kpc). This number is in excess of predictions made with a simple CV model based on a local CV space density of &lt;~10&lt;sup&gt;-5&lt;/sup&gt; pc&lt;sup&gt;-3&lt;/sup&gt;, and a scale height of ~200 pc. They discuss several possible reasons for this observed excess in their paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champlane#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/champlane</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=champlane&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champlane.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHAMPLANE [3]</TD>
            <TD>Chandra Multiwavelength Plane Survey Optical ID Catalog</TD>
            <TD>The authors have carried out optical and X-ray spectral analyses on a sample of 136 candidate optical counterparts of X-ray sources found in five Galactic bulge fields included in their Chandra Multiwavelength Plane (ChaMPlane) Survey. They used a combination of optical spectral fitting and quantile X-ray analysis to obtain the hydrogen column density toward each object, and a three-dimensional dust model of the Galaxy to estimate the most probable distance in each case. They present the discovery of a population of stellar coronal emission sources, likely consisting of pre-main-sequence, young main-sequence, and main-sequence stars, as well as a component of active binaries of RS CVn or BY Dra type. They identify one candidate quiescent low-mass X-ray binary with a subgiant companion, but note that this object may also be an RS CVn system. They report the discovery of 3 new X-ray-detected cataclysmic variables (CVs) in the direction of the Galactic center (at distances &lt;~2 kpc). This number is in excess of predictions made with a simple CV model based on a local CV space density of &lt;~10&lt;sup&gt;-5&lt;/sup&gt; pc&lt;sup&gt;-3&lt;/sup&gt;, and a scale height of ~200 pc. They discuss several possible reasons for this observed excess in their paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champlane#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/champlane</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_champlane&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champlane.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChanNSPiral [1]</TD>
            <TD>Chandra Nearby Spiral Galaxies Point Source Catalog</TD>
            <TD>Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. This table contains the results from a survey of 11 nearby, nearly face-on spiral galaxies observed with the Chandra X-ray Observatory in 22 observations for a total of 869 ks. The galaxies in this sample are at high Galactic latitude to minimize the absorbing column in the line of site, are nearby to minimize source confusion, and span the Hubble sequence for spirals (types 0-7), allowing insights into the X-ray source population of many diverse systems. More than 820 unique point sources are detected in at least one observation within the D25 ellipses of the galaxies. A minimum of 27% of the sources exhibit detectable long- or short-term variability, indicating a source population dominated by accreting XRBs. 17 ultraluminous X-ray sources are detected, with typical rates per galaxy of 1 or 2. In this table, source lists for the 11 galaxies are presented, along with source counts, fluxes, luminosities, X-ray colors, and variability properties. It should be noted that the X-ray source counts presented in this table are raw, background-subtracted counts, so the count rates in sources from the same galaxy that fall on different CCDs cannot be directly compared. The colors presented have been corrected for the differences between front-illuminated and back-illuminated CCDs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/channsgpsc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/channsgpsc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=channsgpsc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/channsgpsc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChanNSPiral [2]</TD>
            <TD>Chandra Nearby Spiral Galaxies Point Source Catalog</TD>
            <TD>Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. This table contains the results from a survey of 11 nearby, nearly face-on spiral galaxies observed with the Chandra X-ray Observatory in 22 observations for a total of 869 ks. The galaxies in this sample are at high Galactic latitude to minimize the absorbing column in the line of site, are nearby to minimize source confusion, and span the Hubble sequence for spirals (types 0-7), allowing insights into the X-ray source population of many diverse systems. More than 820 unique point sources are detected in at least one observation within the D25 ellipses of the galaxies. A minimum of 27% of the sources exhibit detectable long- or short-term variability, indicating a source population dominated by accreting XRBs. 17 ultraluminous X-ray sources are detected, with typical rates per galaxy of 1 or 2. In this table, source lists for the 11 galaxies are presented, along with source counts, fluxes, luminosities, X-ray colors, and variability properties. It should be noted that the X-ray source counts presented in this table are raw, background-subtracted counts, so the count rates in sources from the same galaxy that fall on different CCDs cannot be directly compared. The colors presented have been corrected for the differences between front-illuminated and back-illuminated CCDs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/channsgpsc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/channsgpsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=channsgpsc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/channsgpsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChanNSPiral [3]</TD>
            <TD>Chandra Nearby Spiral Galaxies Point Source Catalog</TD>
            <TD>Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. This table contains the results from a survey of 11 nearby, nearly face-on spiral galaxies observed with the Chandra X-ray Observatory in 22 observations for a total of 869 ks. The galaxies in this sample are at high Galactic latitude to minimize the absorbing column in the line of site, are nearby to minimize source confusion, and span the Hubble sequence for spirals (types 0-7), allowing insights into the X-ray source population of many diverse systems. More than 820 unique point sources are detected in at least one observation within the D25 ellipses of the galaxies. A minimum of 27% of the sources exhibit detectable long- or short-term variability, indicating a source population dominated by accreting XRBs. 17 ultraluminous X-ray sources are detected, with typical rates per galaxy of 1 or 2. In this table, source lists for the 11 galaxies are presented, along with source counts, fluxes, luminosities, X-ray colors, and variability properties. It should be noted that the X-ray source counts presented in this table are raw, background-subtracted counts, so the count rates in sources from the same galaxy that fall on different CCDs cannot be directly compared. The colors presented have been corrected for the differences between front-illuminated and back-illuminated CCDs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/channsgpsc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/channsgpsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_channsgpsc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/channsgpsc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChanNSPiral [1]</TD>
            <TD>Chandra Nearby Spiral Galaxies Point Source Catalog</TD>
            <TD>Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. This table contains the results from a survey of 11 nearby, nearly face-on spiral galaxies observed with the Chandra X-ray Observatory in 22 observations for a total of 869 ks. The galaxies in this sample are at high Galactic latitude to minimize the absorbing column in the line of site, are nearby to minimize source confusion, and span the Hubble sequence for spirals (types 0-7), allowing insights into the X-ray source population of many diverse systems. More than 820 unique point sources are detected in at least one observation within the D25 ellipses of the galaxies. A minimum of 27% of the sources exhibit detectable long- or short-term variability, indicating a source population dominated by accreting XRBs. 17 ultraluminous X-ray sources are detected, with typical rates per galaxy of 1 or 2. In this table, source lists for the 11 galaxies are presented, along with source counts, fluxes, luminosities, X-ray colors, and variability properties. It should be noted that the X-ray source counts presented in this table are raw, background-subtracted counts, so the count rates in sources from the same galaxy that fall on different CCDs cannot be directly compared. The colors presented have been corrected for the differences between front-illuminated and back-illuminated CCDs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/channsgpsc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/channsgpsc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=channsgpsc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/channsgpsc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChanNSPiral [2]</TD>
            <TD>Chandra Nearby Spiral Galaxies Point Source Catalog</TD>
            <TD>Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. This table contains the results from a survey of 11 nearby, nearly face-on spiral galaxies observed with the Chandra X-ray Observatory in 22 observations for a total of 869 ks. The galaxies in this sample are at high Galactic latitude to minimize the absorbing column in the line of site, are nearby to minimize source confusion, and span the Hubble sequence for spirals (types 0-7), allowing insights into the X-ray source population of many diverse systems. More than 820 unique point sources are detected in at least one observation within the D25 ellipses of the galaxies. A minimum of 27% of the sources exhibit detectable long- or short-term variability, indicating a source population dominated by accreting XRBs. 17 ultraluminous X-ray sources are detected, with typical rates per galaxy of 1 or 2. In this table, source lists for the 11 galaxies are presented, along with source counts, fluxes, luminosities, X-ray colors, and variability properties. It should be noted that the X-ray source counts presented in this table are raw, background-subtracted counts, so the count rates in sources from the same galaxy that fall on different CCDs cannot be directly compared. The colors presented have been corrected for the differences between front-illuminated and back-illuminated CCDs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/channsgpsc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/channsgpsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=channsgpsc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/channsgpsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChanNSPiral [3]</TD>
            <TD>Chandra Nearby Spiral Galaxies Point Source Catalog</TD>
            <TD>Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. This table contains the results from a survey of 11 nearby, nearly face-on spiral galaxies observed with the Chandra X-ray Observatory in 22 observations for a total of 869 ks. The galaxies in this sample are at high Galactic latitude to minimize the absorbing column in the line of site, are nearby to minimize source confusion, and span the Hubble sequence for spirals (types 0-7), allowing insights into the X-ray source population of many diverse systems. More than 820 unique point sources are detected in at least one observation within the D25 ellipses of the galaxies. A minimum of 27% of the sources exhibit detectable long- or short-term variability, indicating a source population dominated by accreting XRBs. 17 ultraluminous X-ray sources are detected, with typical rates per galaxy of 1 or 2. In this table, source lists for the 11 galaxies are presented, along with source counts, fluxes, luminosities, X-ray colors, and variability properties. It should be noted that the X-ray source counts presented in this table are raw, background-subtracted counts, so the count rates in sources from the same galaxy that fall on different CCDs cannot be directly compared. The colors presented have been corrected for the differences between front-illuminated and back-illuminated CCDs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/channsgpsc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/channsgpsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_channsgpsc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/channsgpsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/762 [1]</TD>
            <TD>LAEs at z~4.5 in the LALA Cetus field (Wang+, 2009)</TD>
            <TD>We obtained the narrowband images used to select z~4.5 Ly{alpha} galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)~80{AA}. The central wavelengths are 6559, 6611, 6650, 6692, and 6730{AA} for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in B_W_, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z~4.5 Ly{alpha} emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ~7{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762#1</TD>
            <TD>2012-01-28T15:38:39Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/762</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/762</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/762 [2]</TD>
            <TD>LAEs at z~4.5 in the LALA Cetus field (Wang+, 2009)</TD>
            <TD>We obtained the narrowband images used to select z~4.5 Ly{alpha} galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)~80{AA}. The central wavelengths are 6559, 6611, 6650, 6692, and 6730{AA} for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in B_W_, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z~4.5 Ly{alpha} emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ~7{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762#2</TD>
            <TD>2012-01-28T15:38:39Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/762&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/762</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/762 [table3]</TD>
            <TD>LAEs at z~4.5 in the LALA Cetus field (Wang+, 2009)</TD>
            <TD>We obtained the narrowband images used to select z~4.5 Ly{alpha} galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)~80{AA}. The central wavelengths are 6559, 6611, 6650, 6692, and 6730{AA} for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in B_W_, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z~4.5 Ly{alpha} emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ~7{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762#table3</TD>
            <TD>2012-01-28T15:38:39Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/762&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/762</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/2217 [1]</TD>
            <TD>Lensing measurement of SDSS galaxy clusters. I. (Sheldon+, 2009)</TD>
            <TD>The clusters used in this study are drawn from a superset of the recently released MaxBCG catalog of Koester et al. (2007, Cat. J/ApJ/660/239, 2007ApJ...660..221K). The galaxies used for cluster selection and shear measurement were drawn from the SDSS. The area used for this study is somewhat smaller than the SDSS data release 4 (Adelman-McCarthy et al. 2006, Cat. II/267; superseded by Cat. II/294).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2217#1</TD>
            <TD>2011-12-15T23:03:14Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2217</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/2217</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/2217</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/2217 [2]</TD>
            <TD>Lensing measurement of SDSS galaxy clusters. I. (Sheldon+, 2009)</TD>
            <TD>The clusters used in this study are drawn from a superset of the recently released MaxBCG catalog of Koester et al. (2007, Cat. J/ApJ/660/239, 2007ApJ...660..221K). The galaxies used for cluster selection and shear measurement were drawn from the SDSS. The area used for this study is somewhat smaller than the SDSS data release 4 (Adelman-McCarthy et al. 2006, Cat. II/267; superseded by Cat. II/294).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2217#2</TD>
            <TD>2011-12-15T23:03:14Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2217</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/2217&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/2217</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChanNSPiral [1]</TD>
            <TD>Chandra Nearby Spiral Galaxies Point Source Catalog</TD>
            <TD>Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. This table contains the results from a survey of 11 nearby, nearly face-on spiral galaxies observed with the Chandra X-ray Observatory in 22 observations for a total of 869 ks. The galaxies in this sample are at high Galactic latitude to minimize the absorbing column in the line of site, are nearby to minimize source confusion, and span the Hubble sequence for spirals (types 0-7), allowing insights into the X-ray source population of many diverse systems. More than 820 unique point sources are detected in at least one observation within the D25 ellipses of the galaxies. A minimum of 27% of the sources exhibit detectable long- or short-term variability, indicating a source population dominated by accreting XRBs. 17 ultraluminous X-ray sources are detected, with typical rates per galaxy of 1 or 2. In this table, source lists for the 11 galaxies are presented, along with source counts, fluxes, luminosities, X-ray colors, and variability properties. It should be noted that the X-ray source counts presented in this table are raw, background-subtracted counts, so the count rates in sources from the same galaxy that fall on different CCDs cannot be directly compared. The colors presented have been corrected for the differences between front-illuminated and back-illuminated CCDs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/channsgpsc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/channsgpsc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=channsgpsc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/channsgpsc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChanNSPiral [2]</TD>
            <TD>Chandra Nearby Spiral Galaxies Point Source Catalog</TD>
            <TD>Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. This table contains the results from a survey of 11 nearby, nearly face-on spiral galaxies observed with the Chandra X-ray Observatory in 22 observations for a total of 869 ks. The galaxies in this sample are at high Galactic latitude to minimize the absorbing column in the line of site, are nearby to minimize source confusion, and span the Hubble sequence for spirals (types 0-7), allowing insights into the X-ray source population of many diverse systems. More than 820 unique point sources are detected in at least one observation within the D25 ellipses of the galaxies. A minimum of 27% of the sources exhibit detectable long- or short-term variability, indicating a source population dominated by accreting XRBs. 17 ultraluminous X-ray sources are detected, with typical rates per galaxy of 1 or 2. In this table, source lists for the 11 galaxies are presented, along with source counts, fluxes, luminosities, X-ray colors, and variability properties. It should be noted that the X-ray source counts presented in this table are raw, background-subtracted counts, so the count rates in sources from the same galaxy that fall on different CCDs cannot be directly compared. The colors presented have been corrected for the differences between front-illuminated and back-illuminated CCDs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/channsgpsc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/channsgpsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=channsgpsc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/channsgpsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChanNSPiral [3]</TD>
            <TD>Chandra Nearby Spiral Galaxies Point Source Catalog</TD>
            <TD>Emission from discrete point sources dominates the X-ray luminosity in spiral galaxies. This table contains the results from a survey of 11 nearby, nearly face-on spiral galaxies observed with the Chandra X-ray Observatory in 22 observations for a total of 869 ks. The galaxies in this sample are at high Galactic latitude to minimize the absorbing column in the line of site, are nearby to minimize source confusion, and span the Hubble sequence for spirals (types 0-7), allowing insights into the X-ray source population of many diverse systems. More than 820 unique point sources are detected in at least one observation within the D25 ellipses of the galaxies. A minimum of 27% of the sources exhibit detectable long- or short-term variability, indicating a source population dominated by accreting XRBs. 17 ultraluminous X-ray sources are detected, with typical rates per galaxy of 1 or 2. In this table, source lists for the 11 galaxies are presented, along with source counts, fluxes, luminosities, X-ray colors, and variability properties. It should be noted that the X-ray source counts presented in this table are raw, background-subtracted counts, so the count rates in sources from the same galaxy that fall on different CCDs cannot be directly compared. The colors presented have been corrected for the differences between front-illuminated and back-illuminated CCDs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/channsgpsc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/channsgpsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_channsgpsc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/channsgpsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/2217 [1]</TD>
            <TD>Lensing measurement of SDSS galaxy clusters. I. (Sheldon+, 2009)</TD>
            <TD>The clusters used in this study are drawn from a superset of the recently released MaxBCG catalog of Koester et al. (2007, Cat. J/ApJ/660/239, 2007ApJ...660..221K). The galaxies used for cluster selection and shear measurement were drawn from the SDSS. The area used for this study is somewhat smaller than the SDSS data release 4 (Adelman-McCarthy et al. 2006, Cat. II/267; superseded by Cat. II/294).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2217#1</TD>
            <TD>2011-12-15T23:03:14Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2217</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/2217</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/2217</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/2217 [2]</TD>
            <TD>Lensing measurement of SDSS galaxy clusters. I. (Sheldon+, 2009)</TD>
            <TD>The clusters used in this study are drawn from a superset of the recently released MaxBCG catalog of Koester et al. (2007, Cat. J/ApJ/660/239, 2007ApJ...660..221K). The galaxies used for cluster selection and shear measurement were drawn from the SDSS. The area used for this study is somewhat smaller than the SDSS data release 4 (Adelman-McCarthy et al. 2006, Cat. II/267; superseded by Cat. II/294).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2217#2</TD>
            <TD>2011-12-15T23:03:14Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2217</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/2217&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/2217</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/762 [1]</TD>
            <TD>LAEs at z~4.5 in the LALA Cetus field (Wang+, 2009)</TD>
            <TD>We obtained the narrowband images used to select z~4.5 Ly{alpha} galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)~80{AA}. The central wavelengths are 6559, 6611, 6650, 6692, and 6730{AA} for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in B_W_, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z~4.5 Ly{alpha} emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ~7{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762#1</TD>
            <TD>2012-01-28T15:38:39Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/762</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/762</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/762 [2]</TD>
            <TD>LAEs at z~4.5 in the LALA Cetus field (Wang+, 2009)</TD>
            <TD>We obtained the narrowband images used to select z~4.5 Ly{alpha} galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)~80{AA}. The central wavelengths are 6559, 6611, 6650, 6692, and 6730{AA} for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in B_W_, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z~4.5 Ly{alpha} emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ~7{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762#2</TD>
            <TD>2012-01-28T15:38:39Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/762&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/762</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/762 [table3]</TD>
            <TD>LAEs at z~4.5 in the LALA Cetus field (Wang+, 2009)</TD>
            <TD>We obtained the narrowband images used to select z~4.5 Ly{alpha} galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)~80{AA}. The central wavelengths are 6559, 6611, 6650, 6692, and 6730{AA} for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in B_W_, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z~4.5 Ly{alpha} emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ~7{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762#table3</TD>
            <TD>2012-01-28T15:38:39Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/762&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/762</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChanNGalPSC [1]</TD>
            <TD>Chandra Nearby Galaxies Point Source Catalog</TD>
            <TD>The authors have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies. The properties (e.g., counts in 3 energy bands, hardness ratios and inferred X-ray luminosities) of the 1441 X-ray point sources that were detected in these galaxies are listed in this table. The total point-source X-ray (0.3 - 8.0 keV) luminosity L_XP is found to be well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies, and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP and both the old and the young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass and the star formation rate (SFR).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chpngptsrc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chpngptsrc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chpngptsrc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chpngptsrc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChanNGalPSC [2]</TD>
            <TD>Chandra Nearby Galaxies Point Source Catalog</TD>
            <TD>The authors have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies. The properties (e.g., counts in 3 energy bands, hardness ratios and inferred X-ray luminosities) of the 1441 X-ray point sources that were detected in these galaxies are listed in this table. The total point-source X-ray (0.3 - 8.0 keV) luminosity L_XP is found to be well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies, and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP and both the old and the young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass and the star formation rate (SFR).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chpngptsrc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chpngptsrc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chpngptsrc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chpngptsrc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChanNGalPSC [3]</TD>
            <TD>Chandra Nearby Galaxies Point Source Catalog</TD>
            <TD>The authors have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies. The properties (e.g., counts in 3 energy bands, hardness ratios and inferred X-ray luminosities) of the 1441 X-ray point sources that were detected in these galaxies are listed in this table. The total point-source X-ray (0.3 - 8.0 keV) luminosity L_XP is found to be well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies, and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP and both the old and the young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass and the star formation rate (SFR).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chpngptsrc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chpngptsrc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chpngptsrc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chpngptsrc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/2232 [1]</TD>
            <TD>Weak lensing of SDSS galaxy clusters. III. (Sheldon+, 2009)</TD>
            <TD>In this work we measure the mean M/L's for SDSS groups and clusters drawn from the MaxBCG cluster sample (Koester et al. 2007ApJ...660..221K, 2007, Cat. J/ApJ/660/239). We compare the ensemble mass estimates from the first two papers in this series (Sheldon et al. 2009, Cat. J/ApJ/703/2217; Johnston et al. 2007arXiv0709.1159J) with ensemble measurements of the total light. We measure the mean mass using lensing, and the mean luminosity by correlating the clusters with the surrounding galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2232#1</TD>
            <TD>2011-12-15T23:17:13Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2232</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/2232</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/2232</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/2232 [2]</TD>
            <TD>Weak lensing of SDSS galaxy clusters. III. (Sheldon+, 2009)</TD>
            <TD>In this work we measure the mean M/L's for SDSS groups and clusters drawn from the MaxBCG cluster sample (Koester et al. 2007ApJ...660..221K, 2007, Cat. J/ApJ/660/239). We compare the ensemble mass estimates from the first two papers in this series (Sheldon et al. 2009, Cat. J/ApJ/703/2217; Johnston et al. 2007arXiv0709.1159J) with ensemble measurements of the total light. We measure the mean mass using lensing, and the mean luminosity by correlating the clusters with the surrounding galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2232#2</TD>
            <TD>2011-12-15T23:17:13Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2232</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/2232&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/2232</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/181 [1]</TD>
            <TD>BVI photometry of Whiting 1 (Carraro+, 2007)</TD>
            <TD>Recently Carraro (2005ApJ...621L..61C) drew attention to the remarkable star cluster Whiting 1, showing that it lies at about 40kpc from the Sun and is therefore unquestionably a member of the Galactic halo (l=-60.6{deg}). Its Color Magnitude Diagram (CMD) indicated that Whiting 1 is very young (~5Gyrs) for a globular cluster. It is highly likely that Whiting 1 is originated in a dwarf galaxy that has since been disrupted by the Milky Way. The main purpose of the present study is to better constrain the properties of Whiting 1, and assess whether it belongs to a stellar stream from the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph). Deep CCD photometry in the BVI pass-band obtained with the VLT is used to improve the quality of the CMD, and provide more solid estimates of the cluster distance and age, while high resolution spectra of three evolved stars obtained at Magellan is used to derive the cluster kinematics and analyze its possible membership to the Sgr dSph. We demonstrate that - independently on the Halo model employed - Whiting 1 is part of the trailing stream of the Sgr dSph. We derive a new age estimate of 6.5^+1.0^_-0.5_Gyr, and a smaller heliocentric distance of 29.4^+1.8^_-2.0_kpc. The number of globular clusters confirmed to be members of Sgr dSph is now 6. Among these clusters, Whiting 1 is particularly interesting, being the youngest and one of the most metal rich. The existence of Whiting 1 shows how the Sgr dSph was able to form star clusters for a period at least of 6Gyr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181#1</TD>
            <TD>2011-09-14T20:04:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/181 [2]</TD>
            <TD>BVI photometry of Whiting 1 (Carraro+, 2007)</TD>
            <TD>Recently Carraro (2005ApJ...621L..61C) drew attention to the remarkable star cluster Whiting 1, showing that it lies at about 40kpc from the Sun and is therefore unquestionably a member of the Galactic halo (l=-60.6{deg}). Its Color Magnitude Diagram (CMD) indicated that Whiting 1 is very young (~5Gyrs) for a globular cluster. It is highly likely that Whiting 1 is originated in a dwarf galaxy that has since been disrupted by the Milky Way. The main purpose of the present study is to better constrain the properties of Whiting 1, and assess whether it belongs to a stellar stream from the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph). Deep CCD photometry in the BVI pass-band obtained with the VLT is used to improve the quality of the CMD, and provide more solid estimates of the cluster distance and age, while high resolution spectra of three evolved stars obtained at Magellan is used to derive the cluster kinematics and analyze its possible membership to the Sgr dSph. We demonstrate that - independently on the Halo model employed - Whiting 1 is part of the trailing stream of the Sgr dSph. We derive a new age estimate of 6.5^+1.0^_-0.5_Gyr, and a smaller heliocentric distance of 29.4^+1.8^_-2.0_kpc. The number of globular clusters confirmed to be members of Sgr dSph is now 6. Among these clusters, Whiting 1 is particularly interesting, being the youngest and one of the most metal rich. The existence of Whiting 1 shows how the Sgr dSph was able to form star clusters for a period at least of 6Gyr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181#2</TD>
            <TD>2011-09-14T20:04:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/181 [table1]</TD>
            <TD>BVI photometry of Whiting 1 (Carraro+, 2007)</TD>
            <TD>Recently Carraro (2005ApJ...621L..61C) drew attention to the remarkable star cluster Whiting 1, showing that it lies at about 40kpc from the Sun and is therefore unquestionably a member of the Galactic halo (l=-60.6{deg}). Its Color Magnitude Diagram (CMD) indicated that Whiting 1 is very young (~5Gyrs) for a globular cluster. It is highly likely that Whiting 1 is originated in a dwarf galaxy that has since been disrupted by the Milky Way. The main purpose of the present study is to better constrain the properties of Whiting 1, and assess whether it belongs to a stellar stream from the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph). Deep CCD photometry in the BVI pass-band obtained with the VLT is used to improve the quality of the CMD, and provide more solid estimates of the cluster distance and age, while high resolution spectra of three evolved stars obtained at Magellan is used to derive the cluster kinematics and analyze its possible membership to the Sgr dSph. We demonstrate that - independently on the Halo model employed - Whiting 1 is part of the trailing stream of the Sgr dSph. We derive a new age estimate of 6.5^+1.0^_-0.5_Gyr, and a smaller heliocentric distance of 29.4^+1.8^_-2.0_kpc. The number of globular clusters confirmed to be members of Sgr dSph is now 6. Among these clusters, Whiting 1 is particularly interesting, being the youngest and one of the most metal rich. The existence of Whiting 1 shows how the Sgr dSph was able to form star clusters for a period at least of 6Gyr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181#table1</TD>
            <TD>2011-09-14T20:04:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChanNGalPSC [1]</TD>
            <TD>Chandra Nearby Galaxies Point Source Catalog</TD>
            <TD>The authors have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies. The properties (e.g., counts in 3 energy bands, hardness ratios and inferred X-ray luminosities) of the 1441 X-ray point sources that were detected in these galaxies are listed in this table. The total point-source X-ray (0.3 - 8.0 keV) luminosity L_XP is found to be well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies, and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP and both the old and the young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass and the star formation rate (SFR).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chpngptsrc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chpngptsrc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chpngptsrc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chpngptsrc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChanNGalPSC [2]</TD>
            <TD>Chandra Nearby Galaxies Point Source Catalog</TD>
            <TD>The authors have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies. The properties (e.g., counts in 3 energy bands, hardness ratios and inferred X-ray luminosities) of the 1441 X-ray point sources that were detected in these galaxies are listed in this table. The total point-source X-ray (0.3 - 8.0 keV) luminosity L_XP is found to be well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies, and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP and both the old and the young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass and the star formation rate (SFR).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chpngptsrc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chpngptsrc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chpngptsrc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chpngptsrc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChanNGalPSC [3]</TD>
            <TD>Chandra Nearby Galaxies Point Source Catalog</TD>
            <TD>The authors have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies. The properties (e.g., counts in 3 energy bands, hardness ratios and inferred X-ray luminosities) of the 1441 X-ray point sources that were detected in these galaxies are listed in this table. The total point-source X-ray (0.3 - 8.0 keV) luminosity L_XP is found to be well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies, and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP and both the old and the young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass and the star formation rate (SFR).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chpngptsrc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chpngptsrc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chpngptsrc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chpngptsrc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/2232 [1]</TD>
            <TD>Weak lensing of SDSS galaxy clusters. III. (Sheldon+, 2009)</TD>
            <TD>In this work we measure the mean M/L's for SDSS groups and clusters drawn from the MaxBCG cluster sample (Koester et al. 2007ApJ...660..221K, 2007, Cat. J/ApJ/660/239). We compare the ensemble mass estimates from the first two papers in this series (Sheldon et al. 2009, Cat. J/ApJ/703/2217; Johnston et al. 2007arXiv0709.1159J) with ensemble measurements of the total light. We measure the mean mass using lensing, and the mean luminosity by correlating the clusters with the surrounding galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2232#1</TD>
            <TD>2011-12-15T23:17:13Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2232</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/2232</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/2232</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/2232 [2]</TD>
            <TD>Weak lensing of SDSS galaxy clusters. III. (Sheldon+, 2009)</TD>
            <TD>In this work we measure the mean M/L's for SDSS groups and clusters drawn from the MaxBCG cluster sample (Koester et al. 2007ApJ...660..221K, 2007, Cat. J/ApJ/660/239). We compare the ensemble mass estimates from the first two papers in this series (Sheldon et al. 2009, Cat. J/ApJ/703/2217; Johnston et al. 2007arXiv0709.1159J) with ensemble measurements of the total light. We measure the mean mass using lensing, and the mean luminosity by correlating the clusters with the surrounding galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2232#2</TD>
            <TD>2011-12-15T23:17:13Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/2232</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/2232&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/2232</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChanNGalPSC [1]</TD>
            <TD>Chandra Nearby Galaxies Point Source Catalog</TD>
            <TD>The authors have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies. The properties (e.g., counts in 3 energy bands, hardness ratios and inferred X-ray luminosities) of the 1441 X-ray point sources that were detected in these galaxies are listed in this table. The total point-source X-ray (0.3 - 8.0 keV) luminosity L_XP is found to be well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies, and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP and both the old and the young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass and the star formation rate (SFR).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chpngptsrc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chpngptsrc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chpngptsrc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chpngptsrc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChanNGalPSC [2]</TD>
            <TD>Chandra Nearby Galaxies Point Source Catalog</TD>
            <TD>The authors have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies. The properties (e.g., counts in 3 energy bands, hardness ratios and inferred X-ray luminosities) of the 1441 X-ray point sources that were detected in these galaxies are listed in this table. The total point-source X-ray (0.3 - 8.0 keV) luminosity L_XP is found to be well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies, and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP and both the old and the young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass and the star formation rate (SFR).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chpngptsrc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chpngptsrc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chpngptsrc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chpngptsrc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChanNGalPSC [3]</TD>
            <TD>Chandra Nearby Galaxies Point Source Catalog</TD>
            <TD>The authors have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies. The properties (e.g., counts in 3 energy bands, hardness ratios and inferred X-ray luminosities) of the 1441 X-ray point sources that were detected in these galaxies are listed in this table. The total point-source X-ray (0.3 - 8.0 keV) luminosity L_XP is found to be well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies, and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP and both the old and the young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass and the star formation rate (SFR).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chpngptsrc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chpngptsrc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chpngptsrc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chpngptsrc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CYGOB2CXO2 [1]</TD>
            <TD>Cygnus OB2 Association Chandra X-Ray Point Source Catalog 2</TD>
            <TD>This table contains a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. The authors used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric H-alpha Survey, the Two Micron All Sky Survey (2MASS), and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. 755 (45%) of these objects have six-band r', H-alpha, i', J, H, and K optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source they estimate that their X-ray catalog includes &lt;1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broad-band fluxes, spectral model fits, and optical and near-IR photometry in what is one of the largest X-ray catalogs of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2cxo2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2cxo2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cygob2cxo2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cygob2cxo2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CYGOB2CXO2 [2]</TD>
            <TD>Cygnus OB2 Association Chandra X-Ray Point Source Catalog 2</TD>
            <TD>This table contains a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. The authors used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric H-alpha Survey, the Two Micron All Sky Survey (2MASS), and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. 755 (45%) of these objects have six-band r', H-alpha, i', J, H, and K optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source they estimate that their X-ray catalog includes &lt;1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broad-band fluxes, spectral model fits, and optical and near-IR photometry in what is one of the largest X-ray catalogs of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2cxo2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cygob2cxo2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cygob2cxo2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CYGOB2CXO2 [3]</TD>
            <TD>Cygnus OB2 Association Chandra X-Ray Point Source Catalog 2</TD>
            <TD>This table contains a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. The authors used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric H-alpha Survey, the Two Micron All Sky Survey (2MASS), and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. 755 (45%) of these objects have six-band r', H-alpha, i', J, H, and K optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source they estimate that their X-ray catalog includes &lt;1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broad-band fluxes, spectral model fits, and optical and near-IR photometry in what is one of the largest X-ray catalogs of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2cxo2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cygob2cxo2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cygob2cxo2.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CYGOB2CXO2 [1]</TD>
            <TD>Cygnus OB2 Association Chandra X-Ray Point Source Catalog 2</TD>
            <TD>This table contains a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. The authors used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric H-alpha Survey, the Two Micron All Sky Survey (2MASS), and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. 755 (45%) of these objects have six-band r', H-alpha, i', J, H, and K optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source they estimate that their X-ray catalog includes &lt;1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broad-band fluxes, spectral model fits, and optical and near-IR photometry in what is one of the largest X-ray catalogs of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2cxo2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2cxo2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cygob2cxo2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cygob2cxo2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CYGOB2CXO2 [2]</TD>
            <TD>Cygnus OB2 Association Chandra X-Ray Point Source Catalog 2</TD>
            <TD>This table contains a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. The authors used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric H-alpha Survey, the Two Micron All Sky Survey (2MASS), and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. 755 (45%) of these objects have six-band r', H-alpha, i', J, H, and K optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source they estimate that their X-ray catalog includes &lt;1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broad-band fluxes, spectral model fits, and optical and near-IR photometry in what is one of the largest X-ray catalogs of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2cxo2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cygob2cxo2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cygob2cxo2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CYGOB2CXO2 [3]</TD>
            <TD>Cygnus OB2 Association Chandra X-Ray Point Source Catalog 2</TD>
            <TD>This table contains a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. The authors used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric H-alpha Survey, the Two Micron All Sky Survey (2MASS), and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. 755 (45%) of these objects have six-band r', H-alpha, i', J, H, and K optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source they estimate that their X-ray catalog includes &lt;1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broad-band fluxes, spectral model fits, and optical and near-IR photometry in what is one of the largest X-ray catalogs of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2cxo2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cygob2cxo2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cygob2cxo2.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CYGOB2CXO2 [1]</TD>
            <TD>Cygnus OB2 Association Chandra X-Ray Point Source Catalog 2</TD>
            <TD>This table contains a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. The authors used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric H-alpha Survey, the Two Micron All Sky Survey (2MASS), and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. 755 (45%) of these objects have six-band r', H-alpha, i', J, H, and K optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source they estimate that their X-ray catalog includes &lt;1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broad-band fluxes, spectral model fits, and optical and near-IR photometry in what is one of the largest X-ray catalogs of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2cxo2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2cxo2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cygob2cxo2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cygob2cxo2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CYGOB2CXO2 [2]</TD>
            <TD>Cygnus OB2 Association Chandra X-Ray Point Source Catalog 2</TD>
            <TD>This table contains a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. The authors used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric H-alpha Survey, the Two Micron All Sky Survey (2MASS), and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. 755 (45%) of these objects have six-band r', H-alpha, i', J, H, and K optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source they estimate that their X-ray catalog includes &lt;1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broad-band fluxes, spectral model fits, and optical and near-IR photometry in what is one of the largest X-ray catalogs of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2cxo2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cygob2cxo2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cygob2cxo2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CYGOB2CXO2 [3]</TD>
            <TD>Cygnus OB2 Association Chandra X-Ray Point Source Catalog 2</TD>
            <TD>This table contains a catalog of 1696 X-ray sources detected in the massive star-forming region (SFR) Cygnus OB2 and extracted from two archival Chandra observations of the center of the region. A deep source extraction routine, exploiting the low background rates of Chandra observations was employed to maximize the number of sources extracted. Observations at other wavelengths were used to identify low count-rate sources and remove likely spurious sources. Monte Carlo simulations were also used to assess the authenticity of these sources. X-ray spectra were fitted with thermal plasma models to characterize the objects and X-ray light curves were analyzed to determine their variability. The authors used a Bayesian technique to identify optical or near-IR counterparts for 1501 (89%) of our sources, using deep observations from the INT Photometric H-alpha Survey, the Two Micron All Sky Survey (2MASS), and the UKIRT Infrared Deep Sky Survey-Galactic Plane Survey. 755 (45%) of these objects have six-band r', H-alpha, i', J, H, and K optical and near-IR photometry. From an analysis of the Poisson false-source probabilities for each source they estimate that their X-ray catalog includes &lt;1% of false sources, and an even lower fraction when only sources with optical or near-IR associations are considered. A Monte Carlo simulation of the Bayesian matching scheme allows this method to be compared to more simplified matching techniques and enables the various sources of error to be quantified. The catalog of 1696 objects presented here includes X-ray broad-band fluxes, spectral model fits, and optical and near-IR photometry in what is one of the largest X-ray catalogs of a single SFR to date. The high number of stellar X-ray sources detected from relatively shallow observations confirms the status and importance of Cygnus OB2 as one of our Galaxy's most massive SFRs.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2cxo2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cygob2cxo2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/cygob2cxo2.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>EGRCAT [1]</TD>
            <TD>CGRO/EGRET Revised Catalog of Gamma-Ray Sources</TD>
            <TD>The CGRO/EGRET Revised Catalog of Gamma-Ray Sources (EGR) is a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. The authors used the entire EGRET gamma-ray dataset of reprocessed photons at energies above 100 MeV and new Galactic interstellar emission models based on CO, H I, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. The authors applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue (3EG: Hartman et al. 1999, ApJS, 123, 79, available as the EGRET3 Catalog in Browse). The revised EGRET catalog (EGR) lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalog. The authors do not detect 107 sources discovered previously because additional structure is present in the interstellar background. The vast majority of them were unidentified and marked as possibly extended or confused in the 3EG catalog. In particular, the authors do not confirm most of the 3EG sources associated with the local clouds of the Gould Belt. Alternatively, they have found 30 new sources that have no 3EG counterpart. The new error circles for the confirmed 3EG sources largely overlap the previous ones, but several counterparts of particular interest discussed before, such as Sgr A*, radio galaxies, and several microquasars are now found outside the error circles. The authors cross-correlated the source positions with a large number of radio pulsars, pulsar wind nebulae, supernova remnants, OB associations, blazars and flat radiosources and they found a surprising large number of sources (87) at all latitudes that have no counterpart among the potential gamma-ray emitters. Sources found within a radius of 1.5 PSF FWHM of a very bright source, and/or with very asymmetric TS map contours, are not included in the primary list of EGR sources but are included as EGRc sources herein. The EGRc sources represent significant excesses of photons above the background that may be due to extended sources, or structures not properly modeled in the interstellar emission, or artefacts due to incorrect PSF tails. As noted above, there are 188 sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 1640 entries in the HEASARC's version of the Revised EGRET Catalog, corresponding to 1512 'observations' of the 174 primary gamma-ray sources plus 128 'observations' of the 14 confused sources. Thus, there are an average of about 9 entries for every gamma-ray source.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egrcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egrcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=egrcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egrcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>EGRCAT [2]</TD>
            <TD>CGRO/EGRET Revised Catalog of Gamma-Ray Sources</TD>
            <TD>The CGRO/EGRET Revised Catalog of Gamma-Ray Sources (EGR) is a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. The authors used the entire EGRET gamma-ray dataset of reprocessed photons at energies above 100 MeV and new Galactic interstellar emission models based on CO, H I, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. The authors applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue (3EG: Hartman et al. 1999, ApJS, 123, 79, available as the EGRET3 Catalog in Browse). The revised EGRET catalog (EGR) lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalog. The authors do not detect 107 sources discovered previously because additional structure is present in the interstellar background. The vast majority of them were unidentified and marked as possibly extended or confused in the 3EG catalog. In particular, the authors do not confirm most of the 3EG sources associated with the local clouds of the Gould Belt. Alternatively, they have found 30 new sources that have no 3EG counterpart. The new error circles for the confirmed 3EG sources largely overlap the previous ones, but several counterparts of particular interest discussed before, such as Sgr A*, radio galaxies, and several microquasars are now found outside the error circles. The authors cross-correlated the source positions with a large number of radio pulsars, pulsar wind nebulae, supernova remnants, OB associations, blazars and flat radiosources and they found a surprising large number of sources (87) at all latitudes that have no counterpart among the potential gamma-ray emitters. Sources found within a radius of 1.5 PSF FWHM of a very bright source, and/or with very asymmetric TS map contours, are not included in the primary list of EGR sources but are included as EGRc sources herein. The EGRc sources represent significant excesses of photons above the background that may be due to extended sources, or structures not properly modeled in the interstellar emission, or artefacts due to incorrect PSF tails. As noted above, there are 188 sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 1640 entries in the HEASARC's version of the Revised EGRET Catalog, corresponding to 1512 'observations' of the 174 primary gamma-ray sources plus 128 'observations' of the 14 confused sources. Thus, there are an average of about 9 entries for every gamma-ray source.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egrcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=egrcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>EGRCAT [3]</TD>
            <TD>CGRO/EGRET Revised Catalog of Gamma-Ray Sources</TD>
            <TD>The CGRO/EGRET Revised Catalog of Gamma-Ray Sources (EGR) is a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. The authors used the entire EGRET gamma-ray dataset of reprocessed photons at energies above 100 MeV and new Galactic interstellar emission models based on CO, H I, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. The authors applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue (3EG: Hartman et al. 1999, ApJS, 123, 79, available as the EGRET3 Catalog in Browse). The revised EGRET catalog (EGR) lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalog. The authors do not detect 107 sources discovered previously because additional structure is present in the interstellar background. The vast majority of them were unidentified and marked as possibly extended or confused in the 3EG catalog. In particular, the authors do not confirm most of the 3EG sources associated with the local clouds of the Gould Belt. Alternatively, they have found 30 new sources that have no 3EG counterpart. The new error circles for the confirmed 3EG sources largely overlap the previous ones, but several counterparts of particular interest discussed before, such as Sgr A*, radio galaxies, and several microquasars are now found outside the error circles. The authors cross-correlated the source positions with a large number of radio pulsars, pulsar wind nebulae, supernova remnants, OB associations, blazars and flat radiosources and they found a surprising large number of sources (87) at all latitudes that have no counterpart among the potential gamma-ray emitters. Sources found within a radius of 1.5 PSF FWHM of a very bright source, and/or with very asymmetric TS map contours, are not included in the primary list of EGR sources but are included as EGRc sources herein. The EGRc sources represent significant excesses of photons above the background that may be due to extended sources, or structures not properly modeled in the interstellar emission, or artefacts due to incorrect PSF tails. As noted above, there are 188 sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 1640 entries in the HEASARC's version of the Revised EGRET Catalog, corresponding to 1512 'observations' of the 174 primary gamma-ray sources plus 128 'observations' of the 14 confused sources. Thus, there are an average of about 9 entries for every gamma-ray source.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egrcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_egrcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egrcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>EGRCAT [1]</TD>
            <TD>CGRO/EGRET Revised Catalog of Gamma-Ray Sources</TD>
            <TD>The CGRO/EGRET Revised Catalog of Gamma-Ray Sources (EGR) is a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. The authors used the entire EGRET gamma-ray dataset of reprocessed photons at energies above 100 MeV and new Galactic interstellar emission models based on CO, H I, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. The authors applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue (3EG: Hartman et al. 1999, ApJS, 123, 79, available as the EGRET3 Catalog in Browse). The revised EGRET catalog (EGR) lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalog. The authors do not detect 107 sources discovered previously because additional structure is present in the interstellar background. The vast majority of them were unidentified and marked as possibly extended or confused in the 3EG catalog. In particular, the authors do not confirm most of the 3EG sources associated with the local clouds of the Gould Belt. Alternatively, they have found 30 new sources that have no 3EG counterpart. The new error circles for the confirmed 3EG sources largely overlap the previous ones, but several counterparts of particular interest discussed before, such as Sgr A*, radio galaxies, and several microquasars are now found outside the error circles. The authors cross-correlated the source positions with a large number of radio pulsars, pulsar wind nebulae, supernova remnants, OB associations, blazars and flat radiosources and they found a surprising large number of sources (87) at all latitudes that have no counterpart among the potential gamma-ray emitters. Sources found within a radius of 1.5 PSF FWHM of a very bright source, and/or with very asymmetric TS map contours, are not included in the primary list of EGR sources but are included as EGRc sources herein. The EGRc sources represent significant excesses of photons above the background that may be due to extended sources, or structures not properly modeled in the interstellar emission, or artefacts due to incorrect PSF tails. As noted above, there are 188 sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 1640 entries in the HEASARC's version of the Revised EGRET Catalog, corresponding to 1512 'observations' of the 174 primary gamma-ray sources plus 128 'observations' of the 14 confused sources. Thus, there are an average of about 9 entries for every gamma-ray source.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egrcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egrcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=egrcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egrcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>EGRCAT [2]</TD>
            <TD>CGRO/EGRET Revised Catalog of Gamma-Ray Sources</TD>
            <TD>The CGRO/EGRET Revised Catalog of Gamma-Ray Sources (EGR) is a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. The authors used the entire EGRET gamma-ray dataset of reprocessed photons at energies above 100 MeV and new Galactic interstellar emission models based on CO, H I, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. The authors applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue (3EG: Hartman et al. 1999, ApJS, 123, 79, available as the EGRET3 Catalog in Browse). The revised EGRET catalog (EGR) lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalog. The authors do not detect 107 sources discovered previously because additional structure is present in the interstellar background. The vast majority of them were unidentified and marked as possibly extended or confused in the 3EG catalog. In particular, the authors do not confirm most of the 3EG sources associated with the local clouds of the Gould Belt. Alternatively, they have found 30 new sources that have no 3EG counterpart. The new error circles for the confirmed 3EG sources largely overlap the previous ones, but several counterparts of particular interest discussed before, such as Sgr A*, radio galaxies, and several microquasars are now found outside the error circles. The authors cross-correlated the source positions with a large number of radio pulsars, pulsar wind nebulae, supernova remnants, OB associations, blazars and flat radiosources and they found a surprising large number of sources (87) at all latitudes that have no counterpart among the potential gamma-ray emitters. Sources found within a radius of 1.5 PSF FWHM of a very bright source, and/or with very asymmetric TS map contours, are not included in the primary list of EGR sources but are included as EGRc sources herein. The EGRc sources represent significant excesses of photons above the background that may be due to extended sources, or structures not properly modeled in the interstellar emission, or artefacts due to incorrect PSF tails. As noted above, there are 188 sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 1640 entries in the HEASARC's version of the Revised EGRET Catalog, corresponding to 1512 'observations' of the 174 primary gamma-ray sources plus 128 'observations' of the 14 confused sources. Thus, there are an average of about 9 entries for every gamma-ray source.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egrcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=egrcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>EGRCAT [3]</TD>
            <TD>CGRO/EGRET Revised Catalog of Gamma-Ray Sources</TD>
            <TD>The CGRO/EGRET Revised Catalog of Gamma-Ray Sources (EGR) is a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. The authors used the entire EGRET gamma-ray dataset of reprocessed photons at energies above 100 MeV and new Galactic interstellar emission models based on CO, H I, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. The authors applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue (3EG: Hartman et al. 1999, ApJS, 123, 79, available as the EGRET3 Catalog in Browse). The revised EGRET catalog (EGR) lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalog. The authors do not detect 107 sources discovered previously because additional structure is present in the interstellar background. The vast majority of them were unidentified and marked as possibly extended or confused in the 3EG catalog. In particular, the authors do not confirm most of the 3EG sources associated with the local clouds of the Gould Belt. Alternatively, they have found 30 new sources that have no 3EG counterpart. The new error circles for the confirmed 3EG sources largely overlap the previous ones, but several counterparts of particular interest discussed before, such as Sgr A*, radio galaxies, and several microquasars are now found outside the error circles. The authors cross-correlated the source positions with a large number of radio pulsars, pulsar wind nebulae, supernova remnants, OB associations, blazars and flat radiosources and they found a surprising large number of sources (87) at all latitudes that have no counterpart among the potential gamma-ray emitters. Sources found within a radius of 1.5 PSF FWHM of a very bright source, and/or with very asymmetric TS map contours, are not included in the primary list of EGR sources but are included as EGRc sources herein. The EGRc sources represent significant excesses of photons above the background that may be due to extended sources, or structures not properly modeled in the interstellar emission, or artefacts due to incorrect PSF tails. As noted above, there are 188 sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 1640 entries in the HEASARC's version of the Revised EGRET Catalog, corresponding to 1512 'observations' of the 174 primary gamma-ray sources plus 128 'observations' of the 14 confused sources. Thus, there are an average of about 9 entries for every gamma-ray source.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egrcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_egrcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/762 [1]</TD>
            <TD>LAEs at z~4.5 in the LALA Cetus field (Wang+, 2009)</TD>
            <TD>We obtained the narrowband images used to select z~4.5 Ly{alpha} galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)~80{AA}. The central wavelengths are 6559, 6611, 6650, 6692, and 6730{AA} for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in B_W_, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z~4.5 Ly{alpha} emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ~7{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762#1</TD>
            <TD>2012-01-28T15:38:39Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/762</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/762</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/762 [2]</TD>
            <TD>LAEs at z~4.5 in the LALA Cetus field (Wang+, 2009)</TD>
            <TD>We obtained the narrowband images used to select z~4.5 Ly{alpha} galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)~80{AA}. The central wavelengths are 6559, 6611, 6650, 6692, and 6730{AA} for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in B_W_, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z~4.5 Ly{alpha} emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ~7{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762#2</TD>
            <TD>2012-01-28T15:38:39Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/762&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/762</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/762 [table3]</TD>
            <TD>LAEs at z~4.5 in the LALA Cetus field (Wang+, 2009)</TD>
            <TD>We obtained the narrowband images used to select z~4.5 Ly{alpha} galaxy candidates for this work using CCD cameras at the National Optical Astronomy Observatory's 4m telescopes (the Mayall Telescope at Kitt Peak National Observatory, and the Blanco Telescope at Cerro Tololo Inter-American Observatory). We observed the LALA Cetus field (02:05:20-04:55; J2000.0). In total, we obtained deep narrowband stacks over a 36'x36' field in five distinct but overlapping filters, each with full width at half-maximum (FWHM)~80{AA}. The central wavelengths are 6559, 6611, 6650, 6692, and 6730{AA} for narrowband filters Ha0, Ha4, Ha8, Ha12, and Ha16, respectively. To study the continuum emission properties of our candidates, we used deep broadband images in B_W_, R, I band from the NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey 1999ASPC..193..258J). In 2005 September 3-5, we obtained spectroscopy of 194 candidates z~4.5 Ly{alpha} emitters in the LALA Cetus field using the Inamori-Magellan Areal Camera and Spectrograph (IMACS) on the 6.5m Magellan I Baade Telescope. The spectral resolution is ~7{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762#table3</TD>
            <TD>2012-01-28T15:38:39Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/762</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/762&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/762</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/181 [1]</TD>
            <TD>BVI photometry of Whiting 1 (Carraro+, 2007)</TD>
            <TD>Recently Carraro (2005ApJ...621L..61C) drew attention to the remarkable star cluster Whiting 1, showing that it lies at about 40kpc from the Sun and is therefore unquestionably a member of the Galactic halo (l=-60.6{deg}). Its Color Magnitude Diagram (CMD) indicated that Whiting 1 is very young (~5Gyrs) for a globular cluster. It is highly likely that Whiting 1 is originated in a dwarf galaxy that has since been disrupted by the Milky Way. The main purpose of the present study is to better constrain the properties of Whiting 1, and assess whether it belongs to a stellar stream from the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph). Deep CCD photometry in the BVI pass-band obtained with the VLT is used to improve the quality of the CMD, and provide more solid estimates of the cluster distance and age, while high resolution spectra of three evolved stars obtained at Magellan is used to derive the cluster kinematics and analyze its possible membership to the Sgr dSph. We demonstrate that - independently on the Halo model employed - Whiting 1 is part of the trailing stream of the Sgr dSph. We derive a new age estimate of 6.5^+1.0^_-0.5_Gyr, and a smaller heliocentric distance of 29.4^+1.8^_-2.0_kpc. The number of globular clusters confirmed to be members of Sgr dSph is now 6. Among these clusters, Whiting 1 is particularly interesting, being the youngest and one of the most metal rich. The existence of Whiting 1 shows how the Sgr dSph was able to form star clusters for a period at least of 6Gyr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181#1</TD>
            <TD>2011-09-14T20:04:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/181 [2]</TD>
            <TD>BVI photometry of Whiting 1 (Carraro+, 2007)</TD>
            <TD>Recently Carraro (2005ApJ...621L..61C) drew attention to the remarkable star cluster Whiting 1, showing that it lies at about 40kpc from the Sun and is therefore unquestionably a member of the Galactic halo (l=-60.6{deg}). Its Color Magnitude Diagram (CMD) indicated that Whiting 1 is very young (~5Gyrs) for a globular cluster. It is highly likely that Whiting 1 is originated in a dwarf galaxy that has since been disrupted by the Milky Way. The main purpose of the present study is to better constrain the properties of Whiting 1, and assess whether it belongs to a stellar stream from the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph). Deep CCD photometry in the BVI pass-band obtained with the VLT is used to improve the quality of the CMD, and provide more solid estimates of the cluster distance and age, while high resolution spectra of three evolved stars obtained at Magellan is used to derive the cluster kinematics and analyze its possible membership to the Sgr dSph. We demonstrate that - independently on the Halo model employed - Whiting 1 is part of the trailing stream of the Sgr dSph. We derive a new age estimate of 6.5^+1.0^_-0.5_Gyr, and a smaller heliocentric distance of 29.4^+1.8^_-2.0_kpc. The number of globular clusters confirmed to be members of Sgr dSph is now 6. Among these clusters, Whiting 1 is particularly interesting, being the youngest and one of the most metal rich. The existence of Whiting 1 shows how the Sgr dSph was able to form star clusters for a period at least of 6Gyr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181#2</TD>
            <TD>2011-09-14T20:04:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/181 [table1]</TD>
            <TD>BVI photometry of Whiting 1 (Carraro+, 2007)</TD>
            <TD>Recently Carraro (2005ApJ...621L..61C) drew attention to the remarkable star cluster Whiting 1, showing that it lies at about 40kpc from the Sun and is therefore unquestionably a member of the Galactic halo (l=-60.6{deg}). Its Color Magnitude Diagram (CMD) indicated that Whiting 1 is very young (~5Gyrs) for a globular cluster. It is highly likely that Whiting 1 is originated in a dwarf galaxy that has since been disrupted by the Milky Way. The main purpose of the present study is to better constrain the properties of Whiting 1, and assess whether it belongs to a stellar stream from the Sagittarius Dwarf Spheroidal Galaxy (Sgr dSph). Deep CCD photometry in the BVI pass-band obtained with the VLT is used to improve the quality of the CMD, and provide more solid estimates of the cluster distance and age, while high resolution spectra of three evolved stars obtained at Magellan is used to derive the cluster kinematics and analyze its possible membership to the Sgr dSph. We demonstrate that - independently on the Halo model employed - Whiting 1 is part of the trailing stream of the Sgr dSph. We derive a new age estimate of 6.5^+1.0^_-0.5_Gyr, and a smaller heliocentric distance of 29.4^+1.8^_-2.0_kpc. The number of globular clusters confirmed to be members of Sgr dSph is now 6. Among these clusters, Whiting 1 is particularly interesting, being the youngest and one of the most metal rich. The existence of Whiting 1 shows how the Sgr dSph was able to form star clusters for a period at least of 6Gyr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181#table1</TD>
            <TD>2011-09-14T20:04:33Z</TD>
            <TD>#Globular_Clusters#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>EGRCAT [1]</TD>
            <TD>CGRO/EGRET Revised Catalog of Gamma-Ray Sources</TD>
            <TD>The CGRO/EGRET Revised Catalog of Gamma-Ray Sources (EGR) is a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. The authors used the entire EGRET gamma-ray dataset of reprocessed photons at energies above 100 MeV and new Galactic interstellar emission models based on CO, H I, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. The authors applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue (3EG: Hartman et al. 1999, ApJS, 123, 79, available as the EGRET3 Catalog in Browse). The revised EGRET catalog (EGR) lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalog. The authors do not detect 107 sources discovered previously because additional structure is present in the interstellar background. The vast majority of them were unidentified and marked as possibly extended or confused in the 3EG catalog. In particular, the authors do not confirm most of the 3EG sources associated with the local clouds of the Gould Belt. Alternatively, they have found 30 new sources that have no 3EG counterpart. The new error circles for the confirmed 3EG sources largely overlap the previous ones, but several counterparts of particular interest discussed before, such as Sgr A*, radio galaxies, and several microquasars are now found outside the error circles. The authors cross-correlated the source positions with a large number of radio pulsars, pulsar wind nebulae, supernova remnants, OB associations, blazars and flat radiosources and they found a surprising large number of sources (87) at all latitudes that have no counterpart among the potential gamma-ray emitters. Sources found within a radius of 1.5 PSF FWHM of a very bright source, and/or with very asymmetric TS map contours, are not included in the primary list of EGR sources but are included as EGRc sources herein. The EGRc sources represent significant excesses of photons above the background that may be due to extended sources, or structures not properly modeled in the interstellar emission, or artefacts due to incorrect PSF tails. As noted above, there are 188 sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 1640 entries in the HEASARC's version of the Revised EGRET Catalog, corresponding to 1512 'observations' of the 174 primary gamma-ray sources plus 128 'observations' of the 14 confused sources. Thus, there are an average of about 9 entries for every gamma-ray source.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egrcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egrcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=egrcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egrcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>EGRCAT [2]</TD>
            <TD>CGRO/EGRET Revised Catalog of Gamma-Ray Sources</TD>
            <TD>The CGRO/EGRET Revised Catalog of Gamma-Ray Sources (EGR) is a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. The authors used the entire EGRET gamma-ray dataset of reprocessed photons at energies above 100 MeV and new Galactic interstellar emission models based on CO, H I, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. The authors applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue (3EG: Hartman et al. 1999, ApJS, 123, 79, available as the EGRET3 Catalog in Browse). The revised EGRET catalog (EGR) lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalog. The authors do not detect 107 sources discovered previously because additional structure is present in the interstellar background. The vast majority of them were unidentified and marked as possibly extended or confused in the 3EG catalog. In particular, the authors do not confirm most of the 3EG sources associated with the local clouds of the Gould Belt. Alternatively, they have found 30 new sources that have no 3EG counterpart. The new error circles for the confirmed 3EG sources largely overlap the previous ones, but several counterparts of particular interest discussed before, such as Sgr A*, radio galaxies, and several microquasars are now found outside the error circles. The authors cross-correlated the source positions with a large number of radio pulsars, pulsar wind nebulae, supernova remnants, OB associations, blazars and flat radiosources and they found a surprising large number of sources (87) at all latitudes that have no counterpart among the potential gamma-ray emitters. Sources found within a radius of 1.5 PSF FWHM of a very bright source, and/or with very asymmetric TS map contours, are not included in the primary list of EGR sources but are included as EGRc sources herein. The EGRc sources represent significant excesses of photons above the background that may be due to extended sources, or structures not properly modeled in the interstellar emission, or artefacts due to incorrect PSF tails. As noted above, there are 188 sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 1640 entries in the HEASARC's version of the Revised EGRET Catalog, corresponding to 1512 'observations' of the 174 primary gamma-ray sources plus 128 'observations' of the 14 confused sources. Thus, there are an average of about 9 entries for every gamma-ray source.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egrcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=egrcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>EGRCAT [3]</TD>
            <TD>CGRO/EGRET Revised Catalog of Gamma-Ray Sources</TD>
            <TD>The CGRO/EGRET Revised Catalog of Gamma-Ray Sources (EGR) is a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. The authors used the entire EGRET gamma-ray dataset of reprocessed photons at energies above 100 MeV and new Galactic interstellar emission models based on CO, H I, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. The authors applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue (3EG: Hartman et al. 1999, ApJS, 123, 79, available as the EGRET3 Catalog in Browse). The revised EGRET catalog (EGR) lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalog. The authors do not detect 107 sources discovered previously because additional structure is present in the interstellar background. The vast majority of them were unidentified and marked as possibly extended or confused in the 3EG catalog. In particular, the authors do not confirm most of the 3EG sources associated with the local clouds of the Gould Belt. Alternatively, they have found 30 new sources that have no 3EG counterpart. The new error circles for the confirmed 3EG sources largely overlap the previous ones, but several counterparts of particular interest discussed before, such as Sgr A*, radio galaxies, and several microquasars are now found outside the error circles. The authors cross-correlated the source positions with a large number of radio pulsars, pulsar wind nebulae, supernova remnants, OB associations, blazars and flat radiosources and they found a surprising large number of sources (87) at all latitudes that have no counterpart among the potential gamma-ray emitters. Sources found within a radius of 1.5 PSF FWHM of a very bright source, and/or with very asymmetric TS map contours, are not included in the primary list of EGR sources but are included as EGRc sources herein. The EGRc sources represent significant excesses of photons above the background that may be due to extended sources, or structures not properly modeled in the interstellar emission, or artefacts due to incorrect PSF tails. As noted above, there are 188 sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 1640 entries in the HEASARC's version of the Revised EGRET Catalog, corresponding to 1512 'observations' of the 174 primary gamma-ray sources plus 128 'observations' of the 14 confused sources. Thus, there are an average of about 9 entries for every gamma-ray source.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egrcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_egrcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egrcat.html</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>HST.CLASH</TD>
            <TD>Cluster Lensing And Supernova survey with Hubble (CLASH)</TD>
            <TD>By observing 25 massive galaxy clusters with HST's new panchromatic imaging capabilities (Wide-field Camera 3, WFC3, and the Advanced Camera for Surveys, ACS), CLASH will accomplish its four primary science goals: - Map, with unprecedented accuracy, the distribution of dark matter in galaxy clusters using strong and weak gravitational lensing; - Detect Type Ia supernovae out to redshift z ~ 2, allowing us to test the constancy of dark energy's repulsive force over time and look for any evolutionary effects in the supernovae themselves; - Detect and characterize some of the most distant galaxies yet discovered at z &gt; 7 (when the Universe was younger than 800 million years old - or less than 6% of its current age); - Study the internal structure and evolution of the galaxies in and behind these clusters.</TD>
            <TD>MAST</TD>
            <TD>#Optical#Infrared#UV#</TD>
            <TD>ivo://mast.stsci/clash#1</TD>
            <TD>2012-02-02T21:02:24Z</TD>
            <TD>#infrared astronomy#optical astronomy#ultraviolet astronomy#galaxies#Dark Matter#Supernovae#galatic evolution#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0500000007450581</TD>
            <TD>1.0</TD>
            <TD>ivo://mast.stsci/clash</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://archive.stsci.edu/siap/search.php?id=clash&amp;</TD>
            <TD />
            <TD>72</TD>
            <TD />
            <TD>http://archive.stsci.edu/prepds/clash/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/452/739 [1]</TD>
            <TD>ULX sources and FIRST radio sources (Sanchez-Sutil+, 2006)</TD>
            <TD>We search for ultra luminous X-ray source (ULXs) radio counterparts located in nearby galaxies in order to constrain their physical nature. Our work is based on a systematic cross-identification of the most recent and extensive available ULX catalogues and archival radio data. A catalogue of 70 positional coincidences is reported. Most of them are located within the galaxy nucleus. Among them, we find 11 new cases of non-nuclear ULX sources with possibly associated radio emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739#1</TD>
            <TD>2011-09-14T20:05:15Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/452/739</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/452/739</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/452/739 [2]</TD>
            <TD>ULX sources and FIRST radio sources (Sanchez-Sutil+, 2006)</TD>
            <TD>We search for ultra luminous X-ray source (ULXs) radio counterparts located in nearby galaxies in order to constrain their physical nature. Our work is based on a systematic cross-identification of the most recent and extensive available ULX catalogues and archival radio data. A catalogue of 70 positional coincidences is reported. Most of them are located within the galaxy nucleus. Among them, we find 11 new cases of non-nuclear ULX sources with possibly associated radio emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739#2</TD>
            <TD>2011-09-14T20:05:15Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/452/739&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/452/739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/452/739 [table3]</TD>
            <TD>ULX sources and FIRST radio sources (Sanchez-Sutil+, 2006)</TD>
            <TD>We search for ultra luminous X-ray source (ULXs) radio counterparts located in nearby galaxies in order to constrain their physical nature. Our work is based on a systematic cross-identification of the most recent and extensive available ULX catalogues and archival radio data. A catalogue of 70 positional coincidences is reported. Most of them are located within the galaxy nucleus. Among them, we find 11 new cases of non-nuclear ULX sources with possibly associated radio emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739#table3</TD>
            <TD>2011-09-14T20:05:15Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/452/739&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/452/739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Einstein/OGal [1]</TD>
            <TD>Einstein Survey of Optically Selected Galaxies</TD>
            <TD>The Einstein Survey of Optically Selected Galaxies contains the results of a complete Einstein Imaging Proportional Counter (IPC) X-ray survey of optically-selected galaxies from the Shapley-Ames (S-A) Catalog (CDS Catalog &lt;VII/112&gt;), the Uppsala General Catalog (UGC, CDS Catalog &lt;VII/26&gt;) and the European Southern Observatory (ESO) Catalog (CDS Catalog &lt;VII/115&gt;). Well-defined optical criteria were used to select the galaxies, and X-ray fluxes were measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 galaxies have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of &lt;= 0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F, also available at the HEASARC as a database table called EINGALCAT).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/einopslgal#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/einopslgal</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=einopslgal&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/einopslgal.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Einstein/OGal [2]</TD>
            <TD>Einstein Survey of Optically Selected Galaxies</TD>
            <TD>The Einstein Survey of Optically Selected Galaxies contains the results of a complete Einstein Imaging Proportional Counter (IPC) X-ray survey of optically-selected galaxies from the Shapley-Ames (S-A) Catalog (CDS Catalog &lt;VII/112&gt;), the Uppsala General Catalog (UGC, CDS Catalog &lt;VII/26&gt;) and the European Southern Observatory (ESO) Catalog (CDS Catalog &lt;VII/115&gt;). Well-defined optical criteria were used to select the galaxies, and X-ray fluxes were measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 galaxies have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of &lt;= 0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F, also available at the HEASARC as a database table called EINGALCAT).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/einopslgal#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/einopslgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=einopslgal&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/einopslgal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Einstein/OGal [3]</TD>
            <TD>Einstein Survey of Optically Selected Galaxies</TD>
            <TD>The Einstein Survey of Optically Selected Galaxies contains the results of a complete Einstein Imaging Proportional Counter (IPC) X-ray survey of optically-selected galaxies from the Shapley-Ames (S-A) Catalog (CDS Catalog &lt;VII/112&gt;), the Uppsala General Catalog (UGC, CDS Catalog &lt;VII/26&gt;) and the European Southern Observatory (ESO) Catalog (CDS Catalog &lt;VII/115&gt;). Well-defined optical criteria were used to select the galaxies, and X-ray fluxes were measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 galaxies have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of &lt;= 0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F, also available at the HEASARC as a database table called EINGALCAT).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/einopslgal#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/einopslgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_einopslgal&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/einopslgal.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/452/739 [1]</TD>
            <TD>ULX sources and FIRST radio sources (Sanchez-Sutil+, 2006)</TD>
            <TD>We search for ultra luminous X-ray source (ULXs) radio counterparts located in nearby galaxies in order to constrain their physical nature. Our work is based on a systematic cross-identification of the most recent and extensive available ULX catalogues and archival radio data. A catalogue of 70 positional coincidences is reported. Most of them are located within the galaxy nucleus. Among them, we find 11 new cases of non-nuclear ULX sources with possibly associated radio emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739#1</TD>
            <TD>2011-09-14T20:05:15Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/452/739</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/452/739</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/452/739 [2]</TD>
            <TD>ULX sources and FIRST radio sources (Sanchez-Sutil+, 2006)</TD>
            <TD>We search for ultra luminous X-ray source (ULXs) radio counterparts located in nearby galaxies in order to constrain their physical nature. Our work is based on a systematic cross-identification of the most recent and extensive available ULX catalogues and archival radio data. A catalogue of 70 positional coincidences is reported. Most of them are located within the galaxy nucleus. Among them, we find 11 new cases of non-nuclear ULX sources with possibly associated radio emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739#2</TD>
            <TD>2011-09-14T20:05:15Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/452/739&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/452/739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/452/739 [table3]</TD>
            <TD>ULX sources and FIRST radio sources (Sanchez-Sutil+, 2006)</TD>
            <TD>We search for ultra luminous X-ray source (ULXs) radio counterparts located in nearby galaxies in order to constrain their physical nature. Our work is based on a systematic cross-identification of the most recent and extensive available ULX catalogues and archival radio data. A catalogue of 70 positional coincidences is reported. Most of them are located within the galaxy nucleus. Among them, we find 11 new cases of non-nuclear ULX sources with possibly associated radio emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739#table3</TD>
            <TD>2011-09-14T20:05:15Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/452/739&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/452/739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Einstein/OGal [1]</TD>
            <TD>Einstein Survey of Optically Selected Galaxies</TD>
            <TD>The Einstein Survey of Optically Selected Galaxies contains the results of a complete Einstein Imaging Proportional Counter (IPC) X-ray survey of optically-selected galaxies from the Shapley-Ames (S-A) Catalog (CDS Catalog &lt;VII/112&gt;), the Uppsala General Catalog (UGC, CDS Catalog &lt;VII/26&gt;) and the European Southern Observatory (ESO) Catalog (CDS Catalog &lt;VII/115&gt;). Well-defined optical criteria were used to select the galaxies, and X-ray fluxes were measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 galaxies have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of &lt;= 0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F, also available at the HEASARC as a database table called EINGALCAT).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/einopslgal#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/einopslgal</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=einopslgal&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/einopslgal.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Einstein/OGal [2]</TD>
            <TD>Einstein Survey of Optically Selected Galaxies</TD>
            <TD>The Einstein Survey of Optically Selected Galaxies contains the results of a complete Einstein Imaging Proportional Counter (IPC) X-ray survey of optically-selected galaxies from the Shapley-Ames (S-A) Catalog (CDS Catalog &lt;VII/112&gt;), the Uppsala General Catalog (UGC, CDS Catalog &lt;VII/26&gt;) and the European Southern Observatory (ESO) Catalog (CDS Catalog &lt;VII/115&gt;). Well-defined optical criteria were used to select the galaxies, and X-ray fluxes were measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 galaxies have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of &lt;= 0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F, also available at the HEASARC as a database table called EINGALCAT).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/einopslgal#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/einopslgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=einopslgal&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/einopslgal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Einstein/OGal [3]</TD>
            <TD>Einstein Survey of Optically Selected Galaxies</TD>
            <TD>The Einstein Survey of Optically Selected Galaxies contains the results of a complete Einstein Imaging Proportional Counter (IPC) X-ray survey of optically-selected galaxies from the Shapley-Ames (S-A) Catalog (CDS Catalog &lt;VII/112&gt;), the Uppsala General Catalog (UGC, CDS Catalog &lt;VII/26&gt;) and the European Southern Observatory (ESO) Catalog (CDS Catalog &lt;VII/115&gt;). Well-defined optical criteria were used to select the galaxies, and X-ray fluxes were measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 galaxies have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of &lt;= 0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F, also available at the HEASARC as a database table called EINGALCAT).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/einopslgal#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/einopslgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_einopslgal&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/einopslgal.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/452/739 [1]</TD>
            <TD>ULX sources and FIRST radio sources (Sanchez-Sutil+, 2006)</TD>
            <TD>We search for ultra luminous X-ray source (ULXs) radio counterparts located in nearby galaxies in order to constrain their physical nature. Our work is based on a systematic cross-identification of the most recent and extensive available ULX catalogues and archival radio data. A catalogue of 70 positional coincidences is reported. Most of them are located within the galaxy nucleus. Among them, we find 11 new cases of non-nuclear ULX sources with possibly associated radio emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739#1</TD>
            <TD>2011-09-14T20:05:15Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/452/739</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/452/739</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/452/739 [2]</TD>
            <TD>ULX sources and FIRST radio sources (Sanchez-Sutil+, 2006)</TD>
            <TD>We search for ultra luminous X-ray source (ULXs) radio counterparts located in nearby galaxies in order to constrain their physical nature. Our work is based on a systematic cross-identification of the most recent and extensive available ULX catalogues and archival radio data. A catalogue of 70 positional coincidences is reported. Most of them are located within the galaxy nucleus. Among them, we find 11 new cases of non-nuclear ULX sources with possibly associated radio emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739#2</TD>
            <TD>2011-09-14T20:05:15Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/452/739&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/452/739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/452/739 [table3]</TD>
            <TD>ULX sources and FIRST radio sources (Sanchez-Sutil+, 2006)</TD>
            <TD>We search for ultra luminous X-ray source (ULXs) radio counterparts located in nearby galaxies in order to constrain their physical nature. Our work is based on a systematic cross-identification of the most recent and extensive available ULX catalogues and archival radio data. A catalogue of 70 positional coincidences is reported. Most of them are located within the galaxy nucleus. Among them, we find 11 new cases of non-nuclear ULX sources with possibly associated radio emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739#table3</TD>
            <TD>2011-09-14T20:05:15Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/452/739</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/452/739&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/452/739</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Einstein/OGal [1]</TD>
            <TD>Einstein Survey of Optically Selected Galaxies</TD>
            <TD>The Einstein Survey of Optically Selected Galaxies contains the results of a complete Einstein Imaging Proportional Counter (IPC) X-ray survey of optically-selected galaxies from the Shapley-Ames (S-A) Catalog (CDS Catalog &lt;VII/112&gt;), the Uppsala General Catalog (UGC, CDS Catalog &lt;VII/26&gt;) and the European Southern Observatory (ESO) Catalog (CDS Catalog &lt;VII/115&gt;). Well-defined optical criteria were used to select the galaxies, and X-ray fluxes were measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 galaxies have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of &lt;= 0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F, also available at the HEASARC as a database table called EINGALCAT).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/einopslgal#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/einopslgal</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=einopslgal&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/einopslgal.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Einstein/OGal [2]</TD>
            <TD>Einstein Survey of Optically Selected Galaxies</TD>
            <TD>The Einstein Survey of Optically Selected Galaxies contains the results of a complete Einstein Imaging Proportional Counter (IPC) X-ray survey of optically-selected galaxies from the Shapley-Ames (S-A) Catalog (CDS Catalog &lt;VII/112&gt;), the Uppsala General Catalog (UGC, CDS Catalog &lt;VII/26&gt;) and the European Southern Observatory (ESO) Catalog (CDS Catalog &lt;VII/115&gt;). Well-defined optical criteria were used to select the galaxies, and X-ray fluxes were measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 galaxies have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of &lt;= 0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F, also available at the HEASARC as a database table called EINGALCAT).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/einopslgal#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/einopslgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=einopslgal&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/einopslgal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Einstein/OGal [3]</TD>
            <TD>Einstein Survey of Optically Selected Galaxies</TD>
            <TD>The Einstein Survey of Optically Selected Galaxies contains the results of a complete Einstein Imaging Proportional Counter (IPC) X-ray survey of optically-selected galaxies from the Shapley-Ames (S-A) Catalog (CDS Catalog &lt;VII/112&gt;), the Uppsala General Catalog (UGC, CDS Catalog &lt;VII/26&gt;) and the European Southern Observatory (ESO) Catalog (CDS Catalog &lt;VII/115&gt;). Well-defined optical criteria were used to select the galaxies, and X-ray fluxes were measured at the optically-defined positions. The result is a comprehensive list of X-ray detection and upper limit measurements for 1018 galaxies. Of these, 827 galaxies have either independent distance estimates or radial velocities. Associated optical, redshift, and distance data have been assembled for these galaxies, and their distances come from a combination of directly predicted distances and those predicted from the Faber-Burstein Great Attractor/Virgocentric infall model. The accuracy of the X-ray fluxes has been checked in three different ways; all are consistent with the derived X-ray fluxes being of &lt;= 0.1 dex accuracy. In particular, there is agreement with previously published X-ray fluxes for galaxies in common with a 1991 study by Roberts et al. (1991ApJS...75..751R) and a 1992 study by Fabbiano et al. (1992ApJS...80..531F, also available at the HEASARC as a database table called EINGALCAT).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/einopslgal#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/einopslgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_einopslgal&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/einopslgal.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/1221 [1]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#1</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/1221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/1221 [2]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#2</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/1221 [sogs]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#sogs</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/1221 [catalog]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#catalog</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/1221 [plates]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#plates</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ELAISCXO [1]</TD>
            <TD>ELAIS N1 and N2 Fields Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. This table contains the Chandra source catalogs along with an analysis of source counts and hardness ratios. A total of 233 X-ray point sources were detected in addition to two soft extended sources (not included in this table of point sources), which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which the authors attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. The ELAIS Deep X-ray Survey (EDXS) is being conducted in the northern ELAIS regions N1 and N2. The Chandra data consist of approximately 75 ks exposures in each field. Region N1 was observed on 2000 August 3-4 (Obs_ID 888) and N2 on 2000 August 2-3 (Obs_ID 887). The nominal aimpoints were 16:10:20.11 +54:33:22.3 for N1, and 16:36:46.99 +41:01:33.7 for N2 in J2000.0 coordinates. The ACIS-I chips were used with the addition of the ACIS-S2 and ACIS-S4 chips.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiscxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiscxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=elaiscxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/elaiscxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ELAISCXO [2]</TD>
            <TD>ELAIS N1 and N2 Fields Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. This table contains the Chandra source catalogs along with an analysis of source counts and hardness ratios. A total of 233 X-ray point sources were detected in addition to two soft extended sources (not included in this table of point sources), which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which the authors attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. The ELAIS Deep X-ray Survey (EDXS) is being conducted in the northern ELAIS regions N1 and N2. The Chandra data consist of approximately 75 ks exposures in each field. Region N1 was observed on 2000 August 3-4 (Obs_ID 888) and N2 on 2000 August 2-3 (Obs_ID 887). The nominal aimpoints were 16:10:20.11 +54:33:22.3 for N1, and 16:36:46.99 +41:01:33.7 for N2 in J2000.0 coordinates. The ACIS-I chips were used with the addition of the ACIS-S2 and ACIS-S4 chips.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiscxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiscxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=elaiscxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/elaiscxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ELAISCXO [3]</TD>
            <TD>ELAIS N1 and N2 Fields Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. This table contains the Chandra source catalogs along with an analysis of source counts and hardness ratios. A total of 233 X-ray point sources were detected in addition to two soft extended sources (not included in this table of point sources), which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which the authors attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. The ELAIS Deep X-ray Survey (EDXS) is being conducted in the northern ELAIS regions N1 and N2. The Chandra data consist of approximately 75 ks exposures in each field. Region N1 was observed on 2000 August 3-4 (Obs_ID 888) and N2 on 2000 August 2-3 (Obs_ID 887). The nominal aimpoints were 16:10:20.11 +54:33:22.3 for N1, and 16:36:46.99 +41:01:33.7 for N2 in J2000.0 coordinates. The ACIS-I chips were used with the addition of the ACIS-S2 and ACIS-S4 chips.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiscxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiscxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_elaiscxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/elaiscxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/1221 [1]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#1</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/1221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/1221 [2]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#2</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/1221 [sogs]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#sogs</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/1221 [catalog]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#catalog</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/1221 [plates]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#plates</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ELAISCXO [1]</TD>
            <TD>ELAIS N1 and N2 Fields Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. This table contains the Chandra source catalogs along with an analysis of source counts and hardness ratios. A total of 233 X-ray point sources were detected in addition to two soft extended sources (not included in this table of point sources), which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which the authors attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. The ELAIS Deep X-ray Survey (EDXS) is being conducted in the northern ELAIS regions N1 and N2. The Chandra data consist of approximately 75 ks exposures in each field. Region N1 was observed on 2000 August 3-4 (Obs_ID 888) and N2 on 2000 August 2-3 (Obs_ID 887). The nominal aimpoints were 16:10:20.11 +54:33:22.3 for N1, and 16:36:46.99 +41:01:33.7 for N2 in J2000.0 coordinates. The ACIS-I chips were used with the addition of the ACIS-S2 and ACIS-S4 chips.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiscxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiscxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=elaiscxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/elaiscxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ELAISCXO [2]</TD>
            <TD>ELAIS N1 and N2 Fields Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. This table contains the Chandra source catalogs along with an analysis of source counts and hardness ratios. A total of 233 X-ray point sources were detected in addition to two soft extended sources (not included in this table of point sources), which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which the authors attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. The ELAIS Deep X-ray Survey (EDXS) is being conducted in the northern ELAIS regions N1 and N2. The Chandra data consist of approximately 75 ks exposures in each field. Region N1 was observed on 2000 August 3-4 (Obs_ID 888) and N2 on 2000 August 2-3 (Obs_ID 887). The nominal aimpoints were 16:10:20.11 +54:33:22.3 for N1, and 16:36:46.99 +41:01:33.7 for N2 in J2000.0 coordinates. The ACIS-I chips were used with the addition of the ACIS-S2 and ACIS-S4 chips.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiscxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiscxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=elaiscxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/elaiscxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ELAISCXO [3]</TD>
            <TD>ELAIS N1 and N2 Fields Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. This table contains the Chandra source catalogs along with an analysis of source counts and hardness ratios. A total of 233 X-ray point sources were detected in addition to two soft extended sources (not included in this table of point sources), which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which the authors attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. The ELAIS Deep X-ray Survey (EDXS) is being conducted in the northern ELAIS regions N1 and N2. The Chandra data consist of approximately 75 ks exposures in each field. Region N1 was observed on 2000 August 3-4 (Obs_ID 888) and N2 on 2000 August 2-3 (Obs_ID 887). The nominal aimpoints were 16:10:20.11 +54:33:22.3 for N1, and 16:36:46.99 +41:01:33.7 for N2 in J2000.0 coordinates. The ACIS-I chips were used with the addition of the ACIS-S2 and ACIS-S4 chips.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiscxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiscxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_elaiscxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/elaiscxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/1221 [1]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#1</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/1221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/1221 [2]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#2</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/1221 [sogs]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#sogs</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/1221 [catalog]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#catalog</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/1221 [plates]</TD>
            <TD>Sydney observatory Galactic survey (SOGS) (Fresneau+, 2007)</TD>
            <TD>First Epoch astrometric and radiometric information of a survey in the optical along the Galactic fourth quadrant is archived for further analysis in the time-domain. A photographic survey of 1.9x10^6^ stars down to B-magnitude 14.5+/-0.5 along the galactic meridian l=(330+/-5){deg},-64{deg}&lt;b&lt;-7{deg} and along the galactic equator 272{deg}&lt;l&lt;341{deg},-7{deg}&lt;b&lt;7{deg}, is provided from century old astrographic plates of Sydney Observatory. Stellar candidates to investigate the Galaxy disk kinematics up to a distance of 1kpc from the Sun are tentatively selected. A catalogue of 4.8x10^5^ stars is provided for further investigation of the galactic disk heating by transient spiral wave or by GMC encounter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221#plates</TD>
            <TD>2011-09-14T20:06:01Z</TD>
            <TD>#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/1221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/1221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/1221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A120 [1]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey (Takey+, 2011)</TD>
            <TD>The following table provide the first cluster sample catalogue that comprises 175 clusters of the 2XMMi/SDSS Galaxy Cluster Survey. Among them 139 objects are new X-ray discoveries while the others were previously known as X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120#1</TD>
            <TD>2011-12-27T14:59:22Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A120</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A120</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A120 [2]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey (Takey+, 2011)</TD>
            <TD>The following table provide the first cluster sample catalogue that comprises 175 clusters of the 2XMMi/SDSS Galaxy Cluster Survey. Among them 139 objects are new X-ray discoveries while the others were previously known as X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120#2</TD>
            <TD>2011-12-27T14:59:22Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A120&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A120</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A120 [table2]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey (Takey+, 2011)</TD>
            <TD>The following table provide the first cluster sample catalogue that comprises 175 clusters of the 2XMMi/SDSS Galaxy Cluster Survey. Among them 139 objects are new X-ray discoveries while the others were previously known as X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120#table2</TD>
            <TD>2011-12-27T14:59:22Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A120&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A120</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ELAISCXO [1]</TD>
            <TD>ELAIS N1 and N2 Fields Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. This table contains the Chandra source catalogs along with an analysis of source counts and hardness ratios. A total of 233 X-ray point sources were detected in addition to two soft extended sources (not included in this table of point sources), which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which the authors attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. The ELAIS Deep X-ray Survey (EDXS) is being conducted in the northern ELAIS regions N1 and N2. The Chandra data consist of approximately 75 ks exposures in each field. Region N1 was observed on 2000 August 3-4 (Obs_ID 888) and N2 on 2000 August 2-3 (Obs_ID 887). The nominal aimpoints were 16:10:20.11 +54:33:22.3 for N1, and 16:36:46.99 +41:01:33.7 for N2 in J2000.0 coordinates. The ACIS-I chips were used with the addition of the ACIS-S2 and ACIS-S4 chips.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiscxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiscxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=elaiscxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/elaiscxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ELAISCXO [2]</TD>
            <TD>ELAIS N1 and N2 Fields Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. This table contains the Chandra source catalogs along with an analysis of source counts and hardness ratios. A total of 233 X-ray point sources were detected in addition to two soft extended sources (not included in this table of point sources), which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which the authors attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. The ELAIS Deep X-ray Survey (EDXS) is being conducted in the northern ELAIS regions N1 and N2. The Chandra data consist of approximately 75 ks exposures in each field. Region N1 was observed on 2000 August 3-4 (Obs_ID 888) and N2 on 2000 August 2-3 (Obs_ID 887). The nominal aimpoints were 16:10:20.11 +54:33:22.3 for N1, and 16:36:46.99 +41:01:33.7 for N2 in J2000.0 coordinates. The ACIS-I chips were used with the addition of the ACIS-S2 and ACIS-S4 chips.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiscxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiscxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=elaiscxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/elaiscxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ELAISCXO [3]</TD>
            <TD>ELAIS N1 and N2 Fields Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the results of an analysis of two deep (75 ks) Chandra observations of the European Large Area Infrared Space Observatory (ISO) Survey (ELAIS) fields N1 and N2 as the first results from the ELAIS deep X-ray survey. This survey is being conducted in well-studied regions with extensive multiwavelength coverage. This table contains the Chandra source catalogs along with an analysis of source counts and hardness ratios. A total of 233 X-ray point sources were detected in addition to two soft extended sources (not included in this table of point sources), which are found to be associated with galaxy clusters. An overdensity of sources is found in N1 with 30 per cent more sources than N2, which the authors attribute to large-scale structure. A similar variance is seen between other deep Chandra surveys. The source count statistics reveal an increasing fraction of hard sources at fainter fluxes. The number of galaxy-like counterparts also increases dramatically towards fainter fluxes, consistent with the emergence of a large population of obscured sources. The ELAIS Deep X-ray Survey (EDXS) is being conducted in the northern ELAIS regions N1 and N2. The Chandra data consist of approximately 75 ks exposures in each field. Region N1 was observed on 2000 August 3-4 (Obs_ID 888) and N2 on 2000 August 2-3 (Obs_ID 887). The nominal aimpoints were 16:10:20.11 +54:33:22.3 for N1, and 16:36:46.99 +41:01:33.7 for N2 in J2000.0 coordinates. The ACIS-I chips were used with the addition of the ACIS-S2 and ACIS-S4 chips.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/elaiscxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/elaiscxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_elaiscxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/elaiscxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/372/425 [1]</TD>
            <TD>2dF-SDSS Luminous Red Galaxy Survey, 2SLAQ (Cannon+, 2006)</TD>
            <TD>This version of the catalogue was created as v5.1 on 01 Feb 2006 by Russell Cannon. Essentially the same data were used in the other 2SLAQ LRG papers written in 2006. There is one line for each object observed, sorted by RA. The best available redshift, i.e. the one with the highest reliability parameter Q (or the higher S/N in the case of a tie), is given for objects with two or more observations. Another version of the listing, including repeats, is available from the UQ web site at http://lrg.physics.uq.edu.au. The first 27 columns come from the AAO redshifting code (i.e. the concatenated *z.rz output lists from RDC's version of Will Sutherland's original Zcode). Columns 28 to 35 are from the SDSS input target lists prepared by Daniel Eisenstein. Column 36 contains any notes made during the redshifting or subsequent analysis. The first 34 columns are present for all targets, in a fixed format with leading zeroes where appropriate so that they can be easily read in free format. Column 35 gives the original SDSS run_camcol object names for the 2003 2dF data only and is blank otherwise. Note that this version of the redshift listing uses SDSS DR4 photometry in col. 8 and cols. 31-34 (for all but 10 objects) but retains the original DR1 SDSS positions (as used by 2dF) in cols. 28 and 29. Earlier listings up to and including v4 (available from RDC) gave the DR1 photometry used for 2dF target selection; the differences are very small for &gt;99% of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425#1</TD>
            <TD>2011-09-14T20:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/372/425</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/425</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/372/425 [2]</TD>
            <TD>2dF-SDSS Luminous Red Galaxy Survey, 2SLAQ (Cannon+, 2006)</TD>
            <TD>This version of the catalogue was created as v5.1 on 01 Feb 2006 by Russell Cannon. Essentially the same data were used in the other 2SLAQ LRG papers written in 2006. There is one line for each object observed, sorted by RA. The best available redshift, i.e. the one with the highest reliability parameter Q (or the higher S/N in the case of a tie), is given for objects with two or more observations. Another version of the listing, including repeats, is available from the UQ web site at http://lrg.physics.uq.edu.au. The first 27 columns come from the AAO redshifting code (i.e. the concatenated *z.rz output lists from RDC's version of Will Sutherland's original Zcode). Columns 28 to 35 are from the SDSS input target lists prepared by Daniel Eisenstein. Column 36 contains any notes made during the redshifting or subsequent analysis. The first 34 columns are present for all targets, in a fixed format with leading zeroes where appropriate so that they can be easily read in free format. Column 35 gives the original SDSS run_camcol object names for the 2003 2dF data only and is blank otherwise. Note that this version of the redshift listing uses SDSS DR4 photometry in col. 8 and cols. 31-34 (for all but 10 objects) but retains the original DR1 SDSS positions (as used by 2dF) in cols. 28 and 29. Earlier listings up to and including v4 (available from RDC) gave the DR1 photometry used for 2dF target selection; the differences are very small for &gt;99% of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425#2</TD>
            <TD>2011-09-14T20:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/372/425&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/425</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/372/425 [catalog]</TD>
            <TD>2dF-SDSS Luminous Red Galaxy Survey, 2SLAQ (Cannon+, 2006)</TD>
            <TD>This version of the catalogue was created as v5.1 on 01 Feb 2006 by Russell Cannon. Essentially the same data were used in the other 2SLAQ LRG papers written in 2006. There is one line for each object observed, sorted by RA. The best available redshift, i.e. the one with the highest reliability parameter Q (or the higher S/N in the case of a tie), is given for objects with two or more observations. Another version of the listing, including repeats, is available from the UQ web site at http://lrg.physics.uq.edu.au. The first 27 columns come from the AAO redshifting code (i.e. the concatenated *z.rz output lists from RDC's version of Will Sutherland's original Zcode). Columns 28 to 35 are from the SDSS input target lists prepared by Daniel Eisenstein. Column 36 contains any notes made during the redshifting or subsequent analysis. The first 34 columns are present for all targets, in a fixed format with leading zeroes where appropriate so that they can be easily read in free format. Column 35 gives the original SDSS run_camcol object names for the 2003 2dF data only and is blank otherwise. Note that this version of the redshift listing uses SDSS DR4 photometry in col. 8 and cols. 31-34 (for all but 10 objects) but retains the original DR1 SDSS positions (as used by 2dF) in cols. 28 and 29. Earlier listings up to and including v4 (available from RDC) gave the DR1 photometry used for 2dF target selection; the differences are very small for &gt;99% of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425#catalog</TD>
            <TD>2011-09-14T20:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/372/425&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/425</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A120 [1]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey (Takey+, 2011)</TD>
            <TD>The following table provide the first cluster sample catalogue that comprises 175 clusters of the 2XMMi/SDSS Galaxy Cluster Survey. Among them 139 objects are new X-ray discoveries while the others were previously known as X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120#1</TD>
            <TD>2011-12-27T14:59:22Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A120</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A120</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A120 [2]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey (Takey+, 2011)</TD>
            <TD>The following table provide the first cluster sample catalogue that comprises 175 clusters of the 2XMMi/SDSS Galaxy Cluster Survey. Among them 139 objects are new X-ray discoveries while the others were previously known as X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120#2</TD>
            <TD>2011-12-27T14:59:22Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A120&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A120</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A120 [table2]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey (Takey+, 2011)</TD>
            <TD>The following table provide the first cluster sample catalogue that comprises 175 clusters of the 2XMMi/SDSS Galaxy Cluster Survey. Among them 139 objects are new X-ray discoveries while the others were previously known as X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120#table2</TD>
            <TD>2011-12-27T14:59:22Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A120&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A120</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/372/425 [1]</TD>
            <TD>2dF-SDSS Luminous Red Galaxy Survey, 2SLAQ (Cannon+, 2006)</TD>
            <TD>This version of the catalogue was created as v5.1 on 01 Feb 2006 by Russell Cannon. Essentially the same data were used in the other 2SLAQ LRG papers written in 2006. There is one line for each object observed, sorted by RA. The best available redshift, i.e. the one with the highest reliability parameter Q (or the higher S/N in the case of a tie), is given for objects with two or more observations. Another version of the listing, including repeats, is available from the UQ web site at http://lrg.physics.uq.edu.au. The first 27 columns come from the AAO redshifting code (i.e. the concatenated *z.rz output lists from RDC's version of Will Sutherland's original Zcode). Columns 28 to 35 are from the SDSS input target lists prepared by Daniel Eisenstein. Column 36 contains any notes made during the redshifting or subsequent analysis. The first 34 columns are present for all targets, in a fixed format with leading zeroes where appropriate so that they can be easily read in free format. Column 35 gives the original SDSS run_camcol object names for the 2003 2dF data only and is blank otherwise. Note that this version of the redshift listing uses SDSS DR4 photometry in col. 8 and cols. 31-34 (for all but 10 objects) but retains the original DR1 SDSS positions (as used by 2dF) in cols. 28 and 29. Earlier listings up to and including v4 (available from RDC) gave the DR1 photometry used for 2dF target selection; the differences are very small for &gt;99% of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425#1</TD>
            <TD>2011-09-14T20:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/372/425</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/425</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/372/425 [2]</TD>
            <TD>2dF-SDSS Luminous Red Galaxy Survey, 2SLAQ (Cannon+, 2006)</TD>
            <TD>This version of the catalogue was created as v5.1 on 01 Feb 2006 by Russell Cannon. Essentially the same data were used in the other 2SLAQ LRG papers written in 2006. There is one line for each object observed, sorted by RA. The best available redshift, i.e. the one with the highest reliability parameter Q (or the higher S/N in the case of a tie), is given for objects with two or more observations. Another version of the listing, including repeats, is available from the UQ web site at http://lrg.physics.uq.edu.au. The first 27 columns come from the AAO redshifting code (i.e. the concatenated *z.rz output lists from RDC's version of Will Sutherland's original Zcode). Columns 28 to 35 are from the SDSS input target lists prepared by Daniel Eisenstein. Column 36 contains any notes made during the redshifting or subsequent analysis. The first 34 columns are present for all targets, in a fixed format with leading zeroes where appropriate so that they can be easily read in free format. Column 35 gives the original SDSS run_camcol object names for the 2003 2dF data only and is blank otherwise. Note that this version of the redshift listing uses SDSS DR4 photometry in col. 8 and cols. 31-34 (for all but 10 objects) but retains the original DR1 SDSS positions (as used by 2dF) in cols. 28 and 29. Earlier listings up to and including v4 (available from RDC) gave the DR1 photometry used for 2dF target selection; the differences are very small for &gt;99% of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425#2</TD>
            <TD>2011-09-14T20:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/372/425&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/425</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/372/425 [catalog]</TD>
            <TD>2dF-SDSS Luminous Red Galaxy Survey, 2SLAQ (Cannon+, 2006)</TD>
            <TD>This version of the catalogue was created as v5.1 on 01 Feb 2006 by Russell Cannon. Essentially the same data were used in the other 2SLAQ LRG papers written in 2006. There is one line for each object observed, sorted by RA. The best available redshift, i.e. the one with the highest reliability parameter Q (or the higher S/N in the case of a tie), is given for objects with two or more observations. Another version of the listing, including repeats, is available from the UQ web site at http://lrg.physics.uq.edu.au. The first 27 columns come from the AAO redshifting code (i.e. the concatenated *z.rz output lists from RDC's version of Will Sutherland's original Zcode). Columns 28 to 35 are from the SDSS input target lists prepared by Daniel Eisenstein. Column 36 contains any notes made during the redshifting or subsequent analysis. The first 34 columns are present for all targets, in a fixed format with leading zeroes where appropriate so that they can be easily read in free format. Column 35 gives the original SDSS run_camcol object names for the 2003 2dF data only and is blank otherwise. Note that this version of the redshift listing uses SDSS DR4 photometry in col. 8 and cols. 31-34 (for all but 10 objects) but retains the original DR1 SDSS positions (as used by 2dF) in cols. 28 and 29. Earlier listings up to and including v4 (available from RDC) gave the DR1 photometry used for 2dF target selection; the differences are very small for &gt;99% of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425#catalog</TD>
            <TD>2011-09-14T20:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/372/425&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/425</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A120 [1]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey (Takey+, 2011)</TD>
            <TD>The following table provide the first cluster sample catalogue that comprises 175 clusters of the 2XMMi/SDSS Galaxy Cluster Survey. Among them 139 objects are new X-ray discoveries while the others were previously known as X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120#1</TD>
            <TD>2011-12-27T14:59:22Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A120</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A120</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A120 [2]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey (Takey+, 2011)</TD>
            <TD>The following table provide the first cluster sample catalogue that comprises 175 clusters of the 2XMMi/SDSS Galaxy Cluster Survey. Among them 139 objects are new X-ray discoveries while the others were previously known as X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120#2</TD>
            <TD>2011-12-27T14:59:22Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A120&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A120</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A120 [table2]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey (Takey+, 2011)</TD>
            <TD>The following table provide the first cluster sample catalogue that comprises 175 clusters of the 2XMMi/SDSS Galaxy Cluster Survey. Among them 139 objects are new X-ray discoveries while the others were previously known as X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120#table2</TD>
            <TD>2011-12-27T14:59:22Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A120</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A120&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A120</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GC [1]</TD>
            <TD>Milky Way Globular Clusters Catalog (February 2003 Version)</TD>
            <TD>This is the Catalog of Parameters for Milky Way Globular Clusters (February 2003 Version) that was compiled by William E. Harris of McMaster University. It contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: &lt;a href="http://www.physics.mcmaster.ca/~harris/mwgc.ref"&gt;http://www.physics.mcmaster.ca/~harris/mwgc.ref&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/globclust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/globclust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=globclust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/globclust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GC [2]</TD>
            <TD>Milky Way Globular Clusters Catalog (February 2003 Version)</TD>
            <TD>This is the Catalog of Parameters for Milky Way Globular Clusters (February 2003 Version) that was compiled by William E. Harris of McMaster University. It contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: &lt;a href="http://www.physics.mcmaster.ca/~harris/mwgc.ref"&gt;http://www.physics.mcmaster.ca/~harris/mwgc.ref&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/globclust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/globclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=globclust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/globclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GC [3]</TD>
            <TD>Milky Way Globular Clusters Catalog (February 2003 Version)</TD>
            <TD>This is the Catalog of Parameters for Milky Way Globular Clusters (February 2003 Version) that was compiled by William E. Harris of McMaster University. It contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: &lt;a href="http://www.physics.mcmaster.ca/~harris/mwgc.ref"&gt;http://www.physics.mcmaster.ca/~harris/mwgc.ref&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/globclust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/globclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_globclust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/globclust.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/372/425 [1]</TD>
            <TD>2dF-SDSS Luminous Red Galaxy Survey, 2SLAQ (Cannon+, 2006)</TD>
            <TD>This version of the catalogue was created as v5.1 on 01 Feb 2006 by Russell Cannon. Essentially the same data were used in the other 2SLAQ LRG papers written in 2006. There is one line for each object observed, sorted by RA. The best available redshift, i.e. the one with the highest reliability parameter Q (or the higher S/N in the case of a tie), is given for objects with two or more observations. Another version of the listing, including repeats, is available from the UQ web site at http://lrg.physics.uq.edu.au. The first 27 columns come from the AAO redshifting code (i.e. the concatenated *z.rz output lists from RDC's version of Will Sutherland's original Zcode). Columns 28 to 35 are from the SDSS input target lists prepared by Daniel Eisenstein. Column 36 contains any notes made during the redshifting or subsequent analysis. The first 34 columns are present for all targets, in a fixed format with leading zeroes where appropriate so that they can be easily read in free format. Column 35 gives the original SDSS run_camcol object names for the 2003 2dF data only and is blank otherwise. Note that this version of the redshift listing uses SDSS DR4 photometry in col. 8 and cols. 31-34 (for all but 10 objects) but retains the original DR1 SDSS positions (as used by 2dF) in cols. 28 and 29. Earlier listings up to and including v4 (available from RDC) gave the DR1 photometry used for 2dF target selection; the differences are very small for &gt;99% of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425#1</TD>
            <TD>2011-09-14T20:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/372/425</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/425</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/372/425 [2]</TD>
            <TD>2dF-SDSS Luminous Red Galaxy Survey, 2SLAQ (Cannon+, 2006)</TD>
            <TD>This version of the catalogue was created as v5.1 on 01 Feb 2006 by Russell Cannon. Essentially the same data were used in the other 2SLAQ LRG papers written in 2006. There is one line for each object observed, sorted by RA. The best available redshift, i.e. the one with the highest reliability parameter Q (or the higher S/N in the case of a tie), is given for objects with two or more observations. Another version of the listing, including repeats, is available from the UQ web site at http://lrg.physics.uq.edu.au. The first 27 columns come from the AAO redshifting code (i.e. the concatenated *z.rz output lists from RDC's version of Will Sutherland's original Zcode). Columns 28 to 35 are from the SDSS input target lists prepared by Daniel Eisenstein. Column 36 contains any notes made during the redshifting or subsequent analysis. The first 34 columns are present for all targets, in a fixed format with leading zeroes where appropriate so that they can be easily read in free format. Column 35 gives the original SDSS run_camcol object names for the 2003 2dF data only and is blank otherwise. Note that this version of the redshift listing uses SDSS DR4 photometry in col. 8 and cols. 31-34 (for all but 10 objects) but retains the original DR1 SDSS positions (as used by 2dF) in cols. 28 and 29. Earlier listings up to and including v4 (available from RDC) gave the DR1 photometry used for 2dF target selection; the differences are very small for &gt;99% of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425#2</TD>
            <TD>2011-09-14T20:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/372/425&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/425</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/372/425 [catalog]</TD>
            <TD>2dF-SDSS Luminous Red Galaxy Survey, 2SLAQ (Cannon+, 2006)</TD>
            <TD>This version of the catalogue was created as v5.1 on 01 Feb 2006 by Russell Cannon. Essentially the same data were used in the other 2SLAQ LRG papers written in 2006. There is one line for each object observed, sorted by RA. The best available redshift, i.e. the one with the highest reliability parameter Q (or the higher S/N in the case of a tie), is given for objects with two or more observations. Another version of the listing, including repeats, is available from the UQ web site at http://lrg.physics.uq.edu.au. The first 27 columns come from the AAO redshifting code (i.e. the concatenated *z.rz output lists from RDC's version of Will Sutherland's original Zcode). Columns 28 to 35 are from the SDSS input target lists prepared by Daniel Eisenstein. Column 36 contains any notes made during the redshifting or subsequent analysis. The first 34 columns are present for all targets, in a fixed format with leading zeroes where appropriate so that they can be easily read in free format. Column 35 gives the original SDSS run_camcol object names for the 2003 2dF data only and is blank otherwise. Note that this version of the redshift listing uses SDSS DR4 photometry in col. 8 and cols. 31-34 (for all but 10 objects) but retains the original DR1 SDSS positions (as used by 2dF) in cols. 28 and 29. Earlier listings up to and including v4 (available from RDC) gave the DR1 photometry used for 2dF target selection; the differences are very small for &gt;99% of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425#catalog</TD>
            <TD>2011-09-14T20:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/425</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/372/425&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/425</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/633 [1]</TD>
            <TD>A ROSAT survey of contact binary stars (Geske+, 2006)</TD>
            <TD>Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope (Cat. &lt;J/AJ/131/621&gt;) with X-ray data from the ROSAT All Sky Survey (RASS, Cat. &lt;IX/10&gt;) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633#1</TD>
            <TD>2011-09-14T20:11:00Z</TD>
            <TD>#Binaries:eclipsing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/633</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/633</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/633 [2]</TD>
            <TD>A ROSAT survey of contact binary stars (Geske+, 2006)</TD>
            <TD>Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope (Cat. &lt;J/AJ/131/621&gt;) with X-ray data from the ROSAT All Sky Survey (RASS, Cat. &lt;IX/10&gt;) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633#2</TD>
            <TD>2011-09-14T20:11:00Z</TD>
            <TD>#Binaries:eclipsing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/633&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/633</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/633 [table1]</TD>
            <TD>A ROSAT survey of contact binary stars (Geske+, 2006)</TD>
            <TD>Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope (Cat. &lt;J/AJ/131/621&gt;) with X-ray data from the ROSAT All Sky Survey (RASS, Cat. &lt;IX/10&gt;) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633#table1</TD>
            <TD>2011-09-14T20:11:00Z</TD>
            <TD>#Binaries:eclipsing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/633&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/633</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/633 [1]</TD>
            <TD>A ROSAT survey of contact binary stars (Geske+, 2006)</TD>
            <TD>Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope (Cat. &lt;J/AJ/131/621&gt;) with X-ray data from the ROSAT All Sky Survey (RASS, Cat. &lt;IX/10&gt;) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633#1</TD>
            <TD>2011-09-14T20:11:00Z</TD>
            <TD>#Binaries:eclipsing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/633</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/633</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/633 [2]</TD>
            <TD>A ROSAT survey of contact binary stars (Geske+, 2006)</TD>
            <TD>Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope (Cat. &lt;J/AJ/131/621&gt;) with X-ray data from the ROSAT All Sky Survey (RASS, Cat. &lt;IX/10&gt;) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633#2</TD>
            <TD>2011-09-14T20:11:00Z</TD>
            <TD>#Binaries:eclipsing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/633&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/633</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/633 [table1]</TD>
            <TD>A ROSAT survey of contact binary stars (Geske+, 2006)</TD>
            <TD>Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope (Cat. &lt;J/AJ/131/621&gt;) with X-ray data from the ROSAT All Sky Survey (RASS, Cat. &lt;IX/10&gt;) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633#table1</TD>
            <TD>2011-09-14T20:11:00Z</TD>
            <TD>#Binaries:eclipsing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/633&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/633</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/633 [1]</TD>
            <TD>A ROSAT survey of contact binary stars (Geske+, 2006)</TD>
            <TD>Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope (Cat. &lt;J/AJ/131/621&gt;) with X-ray data from the ROSAT All Sky Survey (RASS, Cat. &lt;IX/10&gt;) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633#1</TD>
            <TD>2011-09-14T20:11:00Z</TD>
            <TD>#Binaries:eclipsing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/633</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/633</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/633 [2]</TD>
            <TD>A ROSAT survey of contact binary stars (Geske+, 2006)</TD>
            <TD>Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope (Cat. &lt;J/AJ/131/621&gt;) with X-ray data from the ROSAT All Sky Survey (RASS, Cat. &lt;IX/10&gt;) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633#2</TD>
            <TD>2011-09-14T20:11:00Z</TD>
            <TD>#Binaries:eclipsing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/633&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/633</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/633 [table1]</TD>
            <TD>A ROSAT survey of contact binary stars (Geske+, 2006)</TD>
            <TD>Contact binary stars are common variable stars that are all believed to emit relatively large fluxes of X-rays. In this work we combine a large new sample of contact binary stars derived from the ROTSE-I telescope (Cat. &lt;J/AJ/131/621&gt;) with X-ray data from the ROSAT All Sky Survey (RASS, Cat. &lt;IX/10&gt;) to estimate the X-ray volume emissivity of contact binary stars in the Galaxy. We obtained X-ray fluxes for 140 contact binaries from the RASS, as well as two additional stars observed by the XMM-Newton observatory.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633#table1</TD>
            <TD>2011-09-14T20:11:00Z</TD>
            <TD>#Binaries:eclipsing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/633</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/633&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/633</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/498/195 [1]</TD>
            <TD>Spectroscopic survey of CL 1358+62 (Fisher+ 1998)</TD>
            <TD>We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195#1</TD>
            <TD>2011-09-14T20:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/498/195</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/498/195</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/498/195 [2]</TD>
            <TD>Spectroscopic survey of CL 1358+62 (Fisher+ 1998)</TD>
            <TD>We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195#2</TD>
            <TD>2011-09-14T20:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/498/195&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/498/195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/498/195 [table1]</TD>
            <TD>Spectroscopic survey of CL 1358+62 (Fisher+ 1998)</TD>
            <TD>We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195#table1</TD>
            <TD>2011-09-14T20:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/498/195&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/498/195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/498/195 [1]</TD>
            <TD>Spectroscopic survey of CL 1358+62 (Fisher+ 1998)</TD>
            <TD>We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195#1</TD>
            <TD>2011-09-14T20:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/498/195</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/498/195</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/498/195 [2]</TD>
            <TD>Spectroscopic survey of CL 1358+62 (Fisher+ 1998)</TD>
            <TD>We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195#2</TD>
            <TD>2011-09-14T20:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/498/195&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/498/195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/498/195 [table1]</TD>
            <TD>Spectroscopic survey of CL 1358+62 (Fisher+ 1998)</TD>
            <TD>We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195#table1</TD>
            <TD>2011-09-14T20:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/498/195&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/498/195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/498/195 [1]</TD>
            <TD>Spectroscopic survey of CL 1358+62 (Fisher+ 1998)</TD>
            <TD>We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195#1</TD>
            <TD>2011-09-14T20:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/498/195</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/498/195</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/498/195 [2]</TD>
            <TD>Spectroscopic survey of CL 1358+62 (Fisher+ 1998)</TD>
            <TD>We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195#2</TD>
            <TD>2011-09-14T20:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/498/195&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/498/195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/498/195 [table1]</TD>
            <TD>Spectroscopic survey of CL 1358+62 (Fisher+ 1998)</TD>
            <TD>We present a spectroscopic survey of the rich X-ray-selected galaxy cluster CL 1358+6245 at z=0.328. When our 173 new multislit spectra of cluster galaxies are combined with data from the literature, we produce a catalog of 232 cluster members in a region 10'x11' (3.5Mpcx3.8Mpc) surrounding the brightest cluster galaxy. These data are used to study the structure and dynamics of the cluster and to examine the radial and velocity distributions as a function of spectral type. We classify the spectral types of the cluster members according to the strengths of the Balmer absorption lines (H{delta}, H{gamma}, and H{beta}) and the [O II] 3727{AA} emission line.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195#table1</TD>
            <TD>2011-09-14T20:23:08Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/498/195</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/498/195&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/498/195</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/463/26 [1]</TD>
            <TD>VI photometry of 29 Cepheids in M101. (Kelson+ 1996)</TD>
            <TD>We report on the discovery of 29 Cepheid variables in the galaxy M101 using the original Wide Field Camera (WFC) and the new Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope. We observed a field in M101 at 17 independent epochs in V (F555W), five epochs in I (F785LP/F814W), and one epoch in B (F439W), with a time interval baseline of 381 days. We have found Cepheids with periods ranging from 10 to 60 days. The data have been calibrated using WFPC2 observations with zero points derived from Omega Cen, Pal 4, and NGC 2419 observations. This calibration has been verified by using the Medium Deep Survey (MDS) WFC photometric zero points, and ground-based secondary standards in V and I. The V calibrations agree to +/-0.06mag, and the I calibrations agree to +/-0.4mag. We have constructed V and I period-luminosity (PL) relations and have derived apparent distance moduli based on a distance modulus for the Large Magellanic Cloud (LMC) of 18.50mag and a reddening of E(B-V)=0.10mag to the LMC Cepheids. Period-residual minimization was used to minimize the effects of Malmquist bias on the period-luminosity relation fitting process. Using a Galactic extinction law and the apparent V and I distance moduli, we have found a mean reddening for the M101 sample of E(B-V)=0.03mag and a true distance modulus to M101 of 29.34+/-0.17mag, corresponding to a distance of 7.4+/-0.6Mpc. The sources of error have been rigorously tracked through an error budget; systematic and random errors contribute roughly equally to the quoted error. The mean gas-phase metal abundances in the LMC and in the M101 outer field are similar so we expect metallicity effects to be minimal. These Cepheids will be used in conjunction with results from a Key Project search for Cepheids in an inner field, where the metallicity is larger by a factor of 5, to probe the effects of abundance on the Cepheid period-luminosity relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/463/26#1</TD>
            <TD>2011-09-14T20:23:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/463/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/463/26</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/463/26</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/463/26 [2]</TD>
            <TD>VI photometry of 29 Cepheids in M101. (Kelson+ 1996)</TD>
            <TD>We report on the discovery of 29 Cepheid variables in the galaxy M101 using the original Wide Field Camera (WFC) and the new Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope. We observed a field in M101 at 17 independent epochs in V (F555W), five epochs in I (F785LP/F814W), and one epoch in B (F439W), with a time interval baseline of 381 days. We have found Cepheids with periods ranging from 10 to 60 days. The data have been calibrated using WFPC2 observations with zero points derived from Omega Cen, Pal 4, and NGC 2419 observations. This calibration has been verified by using the Medium Deep Survey (MDS) WFC photometric zero points, and ground-based secondary standards in V and I. The V calibrations agree to +/-0.06mag, and the I calibrations agree to +/-0.4mag. We have constructed V and I period-luminosity (PL) relations and have derived apparent distance moduli based on a distance modulus for the Large Magellanic Cloud (LMC) of 18.50mag and a reddening of E(B-V)=0.10mag to the LMC Cepheids. Period-residual minimization was used to minimize the effects of Malmquist bias on the period-luminosity relation fitting process. Using a Galactic extinction law and the apparent V and I distance moduli, we have found a mean reddening for the M101 sample of E(B-V)=0.03mag and a true distance modulus to M101 of 29.34+/-0.17mag, corresponding to a distance of 7.4+/-0.6Mpc. The sources of error have been rigorously tracked through an error budget; systematic and random errors contribute roughly equally to the quoted error. The mean gas-phase metal abundances in the LMC and in the M101 outer field are similar so we expect metallicity effects to be minimal. These Cepheids will be used in conjunction with results from a Key Project search for Cepheids in an inner field, where the metallicity is larger by a factor of 5, to probe the effects of abundance on the Cepheid period-luminosity relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/463/26#2</TD>
            <TD>2011-09-14T20:23:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/463/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/463/26&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/463/26</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/463/26 [1]</TD>
            <TD>VI photometry of 29 Cepheids in M101. (Kelson+ 1996)</TD>
            <TD>We report on the discovery of 29 Cepheid variables in the galaxy M101 using the original Wide Field Camera (WFC) and the new Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope. We observed a field in M101 at 17 independent epochs in V (F555W), five epochs in I (F785LP/F814W), and one epoch in B (F439W), with a time interval baseline of 381 days. We have found Cepheids with periods ranging from 10 to 60 days. The data have been calibrated using WFPC2 observations with zero points derived from Omega Cen, Pal 4, and NGC 2419 observations. This calibration has been verified by using the Medium Deep Survey (MDS) WFC photometric zero points, and ground-based secondary standards in V and I. The V calibrations agree to +/-0.06mag, and the I calibrations agree to +/-0.4mag. We have constructed V and I period-luminosity (PL) relations and have derived apparent distance moduli based on a distance modulus for the Large Magellanic Cloud (LMC) of 18.50mag and a reddening of E(B-V)=0.10mag to the LMC Cepheids. Period-residual minimization was used to minimize the effects of Malmquist bias on the period-luminosity relation fitting process. Using a Galactic extinction law and the apparent V and I distance moduli, we have found a mean reddening for the M101 sample of E(B-V)=0.03mag and a true distance modulus to M101 of 29.34+/-0.17mag, corresponding to a distance of 7.4+/-0.6Mpc. The sources of error have been rigorously tracked through an error budget; systematic and random errors contribute roughly equally to the quoted error. The mean gas-phase metal abundances in the LMC and in the M101 outer field are similar so we expect metallicity effects to be minimal. These Cepheids will be used in conjunction with results from a Key Project search for Cepheids in an inner field, where the metallicity is larger by a factor of 5, to probe the effects of abundance on the Cepheid period-luminosity relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/463/26#1</TD>
            <TD>2011-09-14T20:23:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/463/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/463/26</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/463/26</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/463/26 [2]</TD>
            <TD>VI photometry of 29 Cepheids in M101. (Kelson+ 1996)</TD>
            <TD>We report on the discovery of 29 Cepheid variables in the galaxy M101 using the original Wide Field Camera (WFC) and the new Wide Field and Planetary Camera 2 (WFPC2) on the Hubble Space Telescope. We observed a field in M101 at 17 independent epochs in V (F555W), five epochs in I (F785LP/F814W), and one epoch in B (F439W), with a time interval baseline of 381 days. We have found Cepheids with periods ranging from 10 to 60 days. The data have been calibrated using WFPC2 observations with zero points derived from Omega Cen, Pal 4, and NGC 2419 observations. This calibration has been verified by using the Medium Deep Survey (MDS) WFC photometric zero points, and ground-based secondary standards in V and I. The V calibrations agree to +/-0.06mag, and the I calibrations agree to +/-0.4mag. We have constructed V and I period-luminosity (PL) relations and have derived apparent distance moduli based on a distance modulus for the Large Magellanic Cloud (LMC) of 18.50mag and a reddening of E(B-V)=0.10mag to the LMC Cepheids. Period-residual minimization was used to minimize the effects of Malmquist bias on the period-luminosity relation fitting process. Using a Galactic extinction law and the apparent V and I distance moduli, we have found a mean reddening for the M101 sample of E(B-V)=0.03mag and a true distance modulus to M101 of 29.34+/-0.17mag, corresponding to a distance of 7.4+/-0.6Mpc. The sources of error have been rigorously tracked through an error budget; systematic and random errors contribute roughly equally to the quoted error. The mean gas-phase metal abundances in the LMC and in the M101 outer field are similar so we expect metallicity effects to be minimal. These Cepheids will be used in conjunction with results from a Key Project search for Cepheids in an inner field, where the metallicity is larger by a factor of 5, to probe the effects of abundance on the Cepheid period-luminosity relation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/463/26#2</TD>
            <TD>2011-09-14T20:23:33Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/463/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/463/26&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/463/26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/384/1611 [1]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#1</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/384/1611</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/384/1611 [2]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#2</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/384/1611&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/384/1611 [table3]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#table3</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/384/1611&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/384/1611 [table1]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#table1</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/384/1611&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/384/1611 [1]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#1</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/384/1611</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/384/1611 [2]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#2</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/384/1611&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/384/1611 [table3]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#table3</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/384/1611&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/384/1611 [table1]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#table1</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/384/1611&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/384/1611 [1]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#1</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/384/1611</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/384/1611 [2]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#2</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/384/1611&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/384/1611 [table3]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#table3</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/384/1611&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/384/1611 [table1]</TD>
            <TD>Submm observations in gravitational lenses (Knudsen+, 2008)</TD>
            <TD>We have conducted a submillimetre mapping survey of faint, gravitationally lensed sources, where we have targeted 12 galaxy clusters and additionally the New Technology Telescope (NTT) Deep Field. The total area surveyed is 71.5arcmin^2^ in the image plane; correcting for gravitational lensing, the total area surveyed is 40arcmin^2^ in the source plane for a typical source redshift z&gt;&gt;2.5. In the deepest maps, an image plane depth of 1{sigma} rms ~0.8mJy is reached. This survey is the largest survey to date to reach such depths. In total 59 sources were detected, including three multiply imaged sources. The gravitational lensing makes it possible to detect sources with flux density below the blank field confusion limit. The lensing-corrected fluxes range from 0.11 to 19mJy. After correcting for multiplicity, there are 10 sources with fluxes &lt;2mJy of which seven have submJy fluxes, doubling the number of such sources known. Number counts are determined below the confusion limit. At 1mJy, the integrated number count is ~10^4^deg^-2^, and at 0.5mJy it is ~2x10^4^deg^-2^. Based on the number counts, at a source plan flux limit of 0.1mJy, essentially all of the 850-m background emission has been resolved. The dominant contribution (&gt;50 per cent) to the integrated background arises from sources with fluxes S850 between 0.4 and 2.5mJy, while the bright sources S850&gt;6mJy contribute only 10 per cent.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611#table1</TD>
            <TD>2011-09-14T20:31:52Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/1611</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/384/1611&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/1611</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/495/707 [1]</TD>
            <TD>WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)</TD>
            <TD>We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707#1</TD>
            <TD>2011-09-14T20:32:35Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/495/707</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/707</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/495/707 [2]</TD>
            <TD>WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)</TD>
            <TD>We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707#2</TD>
            <TD>2011-09-14T20:32:35Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/495/707&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/707</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/495/707 [table4]</TD>
            <TD>WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)</TD>
            <TD>We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707#table4</TD>
            <TD>2011-09-14T20:32:35Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/495/707&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/707</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/495/707 [1]</TD>
            <TD>WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)</TD>
            <TD>We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707#1</TD>
            <TD>2011-09-14T20:32:35Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/495/707</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/707</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/495/707 [2]</TD>
            <TD>WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)</TD>
            <TD>We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707#2</TD>
            <TD>2011-09-14T20:32:35Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/495/707&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/707</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/495/707 [table4]</TD>
            <TD>WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)</TD>
            <TD>We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707#table4</TD>
            <TD>2011-09-14T20:32:35Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/495/707&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/707</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/495/707 [1]</TD>
            <TD>WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)</TD>
            <TD>We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707#1</TD>
            <TD>2011-09-14T20:32:35Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/495/707</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/707</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/495/707 [2]</TD>
            <TD>WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)</TD>
            <TD>We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707#2</TD>
            <TD>2011-09-14T20:32:35Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/495/707&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/707</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/495/707 [table4]</TD>
            <TD>WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)</TD>
            <TD>We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707#table4</TD>
            <TD>2011-09-14T20:32:35Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/707</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/495/707&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/707</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [1]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#1</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [2]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#2</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [3]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#3</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [4]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#4</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [5]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#5</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [6]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#6</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [7]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#7</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR8 [8]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#8</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/DirectCone?DSACAT=UKIDSS_DR8&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [9]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#9</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR8 [10]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#10</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [11]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#11</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [12]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#12</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [13]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#13</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [14]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#14</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [15]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#15</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [16]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#16</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR8 [17]</TD>
            <TD>UKIDSS DR8 - UKIRT Infrared Deep Sky Survey Data Release 8</TD>
            <TD>This DSA hosts data release 7 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey, and Ultra Deep Survey. The Galactic Plane Survey will be available in August 2013. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa#17</TD>
            <TD>2012-07-18T12:48:27Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 8</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR8-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR8-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/269 [1]</TD>
            <TD>Photometry of NGC 5053 (Sarajedini+ 1995)</TD>
            <TD>We present (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system. Monte- Carlo simulations show that both the RGB and HB are underpopulated relative to those of the metal-poor cluster M15, indicative of the relatively lower total luminosity of NGC 5053. Based on the mean magnitude of stars located at the red and blue edges of the instability strip, we find V(HB) = 16.65 +/- 0.03. At this magnitude, polynomial fits to the cluster RGBs in the two measured colors yield (B-V)_g = 0.71 +/- 0.016 and (V-I)_g = 0.93 +/- 0.016. Using the BVI two-color diagram in a differential manner with respect to M68 and M15 gives a reddening of E(B-V) = 0.06 +/- 0.02 for NGC 5053. We have utilized these quantities to extend the calibration of the simultaneous reddening and metallicity method [Sarajedini, AJ, 107, 618 (1994a)] to [Fe/H] = -2.4. Another feature of the color-magnitude diagram that is evident is the rich population of blue straggler stars (BSSs). We are able to recover 22 of 24 previously known BSSs, and we have added 3 more BSSs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269#1</TD>
            <TD>2012-08-13T22:20:10Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/269</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/269</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/269 [2]</TD>
            <TD>Photometry of NGC 5053 (Sarajedini+ 1995)</TD>
            <TD>We present (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system. Monte- Carlo simulations show that both the RGB and HB are underpopulated relative to those of the metal-poor cluster M15, indicative of the relatively lower total luminosity of NGC 5053. Based on the mean magnitude of stars located at the red and blue edges of the instability strip, we find V(HB) = 16.65 +/- 0.03. At this magnitude, polynomial fits to the cluster RGBs in the two measured colors yield (B-V)_g = 0.71 +/- 0.016 and (V-I)_g = 0.93 +/- 0.016. Using the BVI two-color diagram in a differential manner with respect to M68 and M15 gives a reddening of E(B-V) = 0.06 +/- 0.02 for NGC 5053. We have utilized these quantities to extend the calibration of the simultaneous reddening and metallicity method [Sarajedini, AJ, 107, 618 (1994a)] to [Fe/H] = -2.4. Another feature of the color-magnitude diagram that is evident is the rich population of blue straggler stars (BSSs). We are able to recover 22 of 24 previously known BSSs, and we have added 3 more BSSs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269#2</TD>
            <TD>2012-08-13T22:20:10Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/269&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/269</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/269 [table2]</TD>
            <TD>Photometry of NGC 5053 (Sarajedini+ 1995)</TD>
            <TD>We present (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system. Monte- Carlo simulations show that both the RGB and HB are underpopulated relative to those of the metal-poor cluster M15, indicative of the relatively lower total luminosity of NGC 5053. Based on the mean magnitude of stars located at the red and blue edges of the instability strip, we find V(HB) = 16.65 +/- 0.03. At this magnitude, polynomial fits to the cluster RGBs in the two measured colors yield (B-V)_g = 0.71 +/- 0.016 and (V-I)_g = 0.93 +/- 0.016. Using the BVI two-color diagram in a differential manner with respect to M68 and M15 gives a reddening of E(B-V) = 0.06 +/- 0.02 for NGC 5053. We have utilized these quantities to extend the calibration of the simultaneous reddening and metallicity method [Sarajedini, AJ, 107, 618 (1994a)] to [Fe/H] = -2.4. Another feature of the color-magnitude diagram that is evident is the rich population of blue straggler stars (BSSs). We are able to recover 22 of 24 previously known BSSs, and we have added 3 more BSSs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269#table2</TD>
            <TD>2012-08-13T22:20:10Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/269&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/269</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/66 [1]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66#1</TD>
            <TD>2011-09-14T20:32:58Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/66</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/66</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/66 [2]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66#2</TD>
            <TD>2011-09-14T20:32:58Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/66&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/66 [table1]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66#table1</TD>
            <TD>2011-09-14T20:32:58Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/66 [table2]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66#table2</TD>
            <TD>2011-09-14T20:32:58Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/66</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/269 [1]</TD>
            <TD>Photometry of NGC 5053 (Sarajedini+ 1995)</TD>
            <TD>We present (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system. Monte- Carlo simulations show that both the RGB and HB are underpopulated relative to those of the metal-poor cluster M15, indicative of the relatively lower total luminosity of NGC 5053. Based on the mean magnitude of stars located at the red and blue edges of the instability strip, we find V(HB) = 16.65 +/- 0.03. At this magnitude, polynomial fits to the cluster RGBs in the two measured colors yield (B-V)_g = 0.71 +/- 0.016 and (V-I)_g = 0.93 +/- 0.016. Using the BVI two-color diagram in a differential manner with respect to M68 and M15 gives a reddening of E(B-V) = 0.06 +/- 0.02 for NGC 5053. We have utilized these quantities to extend the calibration of the simultaneous reddening and metallicity method [Sarajedini, AJ, 107, 618 (1994a)] to [Fe/H] = -2.4. Another feature of the color-magnitude diagram that is evident is the rich population of blue straggler stars (BSSs). We are able to recover 22 of 24 previously known BSSs, and we have added 3 more BSSs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269#1</TD>
            <TD>2012-08-13T22:20:10Z</TD>
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            <TD>10-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/269</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/269</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/269 [2]</TD>
            <TD>Photometry of NGC 5053 (Sarajedini+ 1995)</TD>
            <TD>We present (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system. Monte- Carlo simulations show that both the RGB and HB are underpopulated relative to those of the metal-poor cluster M15, indicative of the relatively lower total luminosity of NGC 5053. Based on the mean magnitude of stars located at the red and blue edges of the instability strip, we find V(HB) = 16.65 +/- 0.03. At this magnitude, polynomial fits to the cluster RGBs in the two measured colors yield (B-V)_g = 0.71 +/- 0.016 and (V-I)_g = 0.93 +/- 0.016. Using the BVI two-color diagram in a differential manner with respect to M68 and M15 gives a reddening of E(B-V) = 0.06 +/- 0.02 for NGC 5053. We have utilized these quantities to extend the calibration of the simultaneous reddening and metallicity method [Sarajedini, AJ, 107, 618 (1994a)] to [Fe/H] = -2.4. Another feature of the color-magnitude diagram that is evident is the rich population of blue straggler stars (BSSs). We are able to recover 22 of 24 previously known BSSs, and we have added 3 more BSSs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/269&amp;</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/269 [table2]</TD>
            <TD>Photometry of NGC 5053 (Sarajedini+ 1995)</TD>
            <TD>We present (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system. Monte- Carlo simulations show that both the RGB and HB are underpopulated relative to those of the metal-poor cluster M15, indicative of the relatively lower total luminosity of NGC 5053. Based on the mean magnitude of stars located at the red and blue edges of the instability strip, we find V(HB) = 16.65 +/- 0.03. At this magnitude, polynomial fits to the cluster RGBs in the two measured colors yield (B-V)_g = 0.71 +/- 0.016 and (V-I)_g = 0.93 +/- 0.016. Using the BVI two-color diagram in a differential manner with respect to M68 and M15 gives a reddening of E(B-V) = 0.06 +/- 0.02 for NGC 5053. We have utilized these quantities to extend the calibration of the simultaneous reddening and metallicity method [Sarajedini, AJ, 107, 618 (1994a)] to [Fe/H] = -2.4. Another feature of the color-magnitude diagram that is evident is the rich population of blue straggler stars (BSSs). We are able to recover 22 of 24 previously known BSSs, and we have added 3 more BSSs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/269&amp;</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/121/66 [1]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T20:32:58Z</TD>
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            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/66</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/66</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/66 [2]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66#2</TD>
            <TD>2011-09-14T20:32:58Z</TD>
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            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/121/66 [table1]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66#table1</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/66&amp;</TD>
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            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
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            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/109/269 [1]</TD>
            <TD>Photometry of NGC 5053 (Sarajedini+ 1995)</TD>
            <TD>We present (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system. Monte- Carlo simulations show that both the RGB and HB are underpopulated relative to those of the metal-poor cluster M15, indicative of the relatively lower total luminosity of NGC 5053. Based on the mean magnitude of stars located at the red and blue edges of the instability strip, we find V(HB) = 16.65 +/- 0.03. At this magnitude, polynomial fits to the cluster RGBs in the two measured colors yield (B-V)_g = 0.71 +/- 0.016 and (V-I)_g = 0.93 +/- 0.016. Using the BVI two-color diagram in a differential manner with respect to M68 and M15 gives a reddening of E(B-V) = 0.06 +/- 0.02 for NGC 5053. We have utilized these quantities to extend the calibration of the simultaneous reddening and metallicity method [Sarajedini, AJ, 107, 618 (1994a)] to [Fe/H] = -2.4. Another feature of the color-magnitude diagram that is evident is the rich population of blue straggler stars (BSSs). We are able to recover 22 of 24 previously known BSSs, and we have added 3 more BSSs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269#1</TD>
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            <TD>WebBrowser</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/269 [2]</TD>
            <TD>Photometry of NGC 5053 (Sarajedini+ 1995)</TD>
            <TD>We present (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system. Monte- Carlo simulations show that both the RGB and HB are underpopulated relative to those of the metal-poor cluster M15, indicative of the relatively lower total luminosity of NGC 5053. Based on the mean magnitude of stars located at the red and blue edges of the instability strip, we find V(HB) = 16.65 +/- 0.03. At this magnitude, polynomial fits to the cluster RGBs in the two measured colors yield (B-V)_g = 0.71 +/- 0.016 and (V-I)_g = 0.93 +/- 0.016. Using the BVI two-color diagram in a differential manner with respect to M68 and M15 gives a reddening of E(B-V) = 0.06 +/- 0.02 for NGC 5053. We have utilized these quantities to extend the calibration of the simultaneous reddening and metallicity method [Sarajedini, AJ, 107, 618 (1994a)] to [Fe/H] = -2.4. Another feature of the color-magnitude diagram that is evident is the rich population of blue straggler stars (BSSs). We are able to recover 22 of 24 previously known BSSs, and we have added 3 more BSSs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/269#2</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/109/269 [table2]</TD>
            <TD>Photometry of NGC 5053 (Sarajedini+ 1995)</TD>
            <TD>We present (V,B-V), (V,V-I), and (V,B-I) color-magnitude diagrams for NGC 5053, which is the most metal-poor globular cluster known in the galaxy. The horizontal branch (HB) is predominantly blueward of the RR Lyrae instability strip and the slope of the red giant branch (RGB) is relatively steep, both characteristic of a metal-poor system. Monte- Carlo simulations show that both the RGB and HB are underpopulated relative to those of the metal-poor cluster M15, indicative of the relatively lower total luminosity of NGC 5053. Based on the mean magnitude of stars located at the red and blue edges of the instability strip, we find V(HB) = 16.65 +/- 0.03. At this magnitude, polynomial fits to the cluster RGBs in the two measured colors yield (B-V)_g = 0.71 +/- 0.016 and (V-I)_g = 0.93 +/- 0.016. Using the BVI two-color diagram in a differential manner with respect to M68 and M15 gives a reddening of E(B-V) = 0.06 +/- 0.02 for NGC 5053. We have utilized these quantities to extend the calibration of the simultaneous reddening and metallicity method [Sarajedini, AJ, 107, 618 (1994a)] to [Fe/H] = -2.4. Another feature of the color-magnitude diagram that is evident is the rich population of blue straggler stars (BSSs). We are able to recover 22 of 24 previously known BSSs, and we have added 3 more BSSs.</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
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            <TD>2011-09-14T20:32:58Z</TD>
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            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66</TD>
            <TD />
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            <TD>WebBrowser</TD>
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            <TD>HTTP Request</TD>
            <TD>J/AJ/121/66 [2]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/66&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/66</TD>
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            <TD>J/AJ/121/66 [table1]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66#table1</TD>
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            <TD>26-Feb-2001</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/121/66 [table2]</TD>
            <TD>KISS H{alpha} survey list 1 (Salzer+, 2001)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is a new objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors and is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our red spectral data, which cover the spectral range 6400 to 7200{AA}. In most cases, the detected emission line is H{alpha}. The current survey list covers a 1{deg}-wide strip located at {delta}= 29{deg} 30' (B1950.0) and spanning the right ascension range 12h 15m to 17h 0m. An area of 62.2{deg}^2^ is covered. A total of 1128 candidate emission-line objects have been selected for inclusion in the survey list (18.1{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift and emission-line flux and equivalent width based on measurements of the digital objective-prism spectra. The properties of the KISS emission-line galaxies are examined using the available observational data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/66#table2</TD>
            <TD>2011-09-14T20:32:58Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
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            <TD>26-Feb-2001</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/66&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/66</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/125/459 [1]</TD>
            <TD>Nearby clusters of galaxies properties. III. (Trevese+ 1997)</TD>
            <TD>This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. &lt;J/A+AS/94/327&gt;, Flin et al. 1995, Cat. &lt;J/A+AS/110/313&gt;, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459#1</TD>
            <TD>2012-08-25T22:04:56Z</TD>
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            <TD>08-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/125/459</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/459</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/125/459 [2]</TD>
            <TD>Nearby clusters of galaxies properties. III. (Trevese+ 1997)</TD>
            <TD>This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. &lt;J/A+AS/94/327&gt;, Flin et al. 1995, Cat. &lt;J/A+AS/110/313&gt;, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459#2</TD>
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            <TD>08-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/125/459&amp;</TD>
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            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/A+AS/125/459 [tables]</TD>
            <TD>Nearby clusters of galaxies properties. III. (Trevese+ 1997)</TD>
            <TD>This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. &lt;J/A+AS/94/327&gt;, Flin et al. 1995, Cat. &lt;J/A+AS/110/313&gt;, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459#tables</TD>
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            <TD>08-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/125/459&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/459</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/145/65 [1]</TD>
            <TD>Virgo intracluster planetary nebula candidates (Feldmeier+, 2003)</TD>
            <TD>Intracluster stars - stars outside of individual galaxies - are a sensitive measure of the poorly understood processes of galactic mergers, cluster accretion, and tidal stripping that occur in galaxy clusters. In particular, intracluster planetary nebulae are a useful probe of intracluster light as a whole. We present a catalog of 318 intracluster planetary nebula candidates in the nearby Virgo Cluster of galaxies, taken with the Kitt Peak National Observatory 4m telescope. We detail the automated detection routines developed to search for these candidates and discuss the routines' strengths and weaknesses. We discuss the importance of contamination in the catalog, and the likely causes. We present magnitudes and positions of these candidates, suitable for spectroscopic follow-up observations. Analyses of these candidates are presented in other papers of this series.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65#1</TD>
            <TD>2011-09-14T20:33:38Z</TD>
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            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/145/65</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/65</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/145/65 [2]</TD>
            <TD>Virgo intracluster planetary nebula candidates (Feldmeier+, 2003)</TD>
            <TD>Intracluster stars - stars outside of individual galaxies - are a sensitive measure of the poorly understood processes of galactic mergers, cluster accretion, and tidal stripping that occur in galaxy clusters. In particular, intracluster planetary nebulae are a useful probe of intracluster light as a whole. We present a catalog of 318 intracluster planetary nebula candidates in the nearby Virgo Cluster of galaxies, taken with the Kitt Peak National Observatory 4m telescope. We detail the automated detection routines developed to search for these candidates and discuss the routines' strengths and weaknesses. We discuss the importance of contamination in the catalog, and the likely causes. We present magnitudes and positions of these candidates, suitable for spectroscopic follow-up observations. Analyses of these candidates are presented in other papers of this series.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65#2</TD>
            <TD>2011-09-14T20:33:38Z</TD>
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            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/145/65&amp;</TD>
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            <TD>J/ApJS/145/65 [table6]</TD>
            <TD>Virgo intracluster planetary nebula candidates (Feldmeier+, 2003)</TD>
            <TD>Intracluster stars - stars outside of individual galaxies - are a sensitive measure of the poorly understood processes of galactic mergers, cluster accretion, and tidal stripping that occur in galaxy clusters. In particular, intracluster planetary nebulae are a useful probe of intracluster light as a whole. We present a catalog of 318 intracluster planetary nebula candidates in the nearby Virgo Cluster of galaxies, taken with the Kitt Peak National Observatory 4m telescope. We detail the automated detection routines developed to search for these candidates and discuss the routines' strengths and weaknesses. We discuss the importance of contamination in the catalog, and the likely causes. We present magnitudes and positions of these candidates, suitable for spectroscopic follow-up observations. Analyses of these candidates are presented in other papers of this series.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65#table6</TD>
            <TD>2011-09-14T20:33:38Z</TD>
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            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/65</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/125/459 [1]</TD>
            <TD>Nearby clusters of galaxies properties. III. (Trevese+ 1997)</TD>
            <TD>This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. &lt;J/A+AS/94/327&gt;, Flin et al. 1995, Cat. &lt;J/A+AS/110/313&gt;, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459#1</TD>
            <TD>2012-08-25T22:04:56Z</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/125/459</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/459</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/125/459 [2]</TD>
            <TD>Nearby clusters of galaxies properties. III. (Trevese+ 1997)</TD>
            <TD>This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. &lt;J/A+AS/94/327&gt;, Flin et al. 1995, Cat. &lt;J/A+AS/110/313&gt;, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459#2</TD>
            <TD>2012-08-25T22:04:56Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>08-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/125/459&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/459</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/125/459 [tables]</TD>
            <TD>Nearby clusters of galaxies properties. III. (Trevese+ 1997)</TD>
            <TD>This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. &lt;J/A+AS/94/327&gt;, Flin et al. 1995, Cat. &lt;J/A+AS/110/313&gt;, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459#tables</TD>
            <TD>2012-08-25T22:04:56Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>08-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/125/459&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/459</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/145/65 [1]</TD>
            <TD>Virgo intracluster planetary nebula candidates (Feldmeier+, 2003)</TD>
            <TD>Intracluster stars - stars outside of individual galaxies - are a sensitive measure of the poorly understood processes of galactic mergers, cluster accretion, and tidal stripping that occur in galaxy clusters. In particular, intracluster planetary nebulae are a useful probe of intracluster light as a whole. We present a catalog of 318 intracluster planetary nebula candidates in the nearby Virgo Cluster of galaxies, taken with the Kitt Peak National Observatory 4m telescope. We detail the automated detection routines developed to search for these candidates and discuss the routines' strengths and weaknesses. We discuss the importance of contamination in the catalog, and the likely causes. We present magnitudes and positions of these candidates, suitable for spectroscopic follow-up observations. Analyses of these candidates are presented in other papers of this series.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65#1</TD>
            <TD>2011-09-14T20:33:38Z</TD>
            <TD>#Clusters_of_galaxies#Planetary_Nebulae#</TD>
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            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65</TD>
            <TD />
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/145/65</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/65</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJS/145/65 [2]</TD>
            <TD>Virgo intracluster planetary nebula candidates (Feldmeier+, 2003)</TD>
            <TD>Intracluster stars - stars outside of individual galaxies - are a sensitive measure of the poorly understood processes of galactic mergers, cluster accretion, and tidal stripping that occur in galaxy clusters. In particular, intracluster planetary nebulae are a useful probe of intracluster light as a whole. We present a catalog of 318 intracluster planetary nebula candidates in the nearby Virgo Cluster of galaxies, taken with the Kitt Peak National Observatory 4m telescope. We detail the automated detection routines developed to search for these candidates and discuss the routines' strengths and weaknesses. We discuss the importance of contamination in the catalog, and the likely causes. We present magnitudes and positions of these candidates, suitable for spectroscopic follow-up observations. Analyses of these candidates are presented in other papers of this series.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65#2</TD>
            <TD>2011-09-14T20:33:38Z</TD>
            <TD>#Clusters_of_galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/145/65&amp;</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJS/145/65 [table6]</TD>
            <TD>Virgo intracluster planetary nebula candidates (Feldmeier+, 2003)</TD>
            <TD>Intracluster stars - stars outside of individual galaxies - are a sensitive measure of the poorly understood processes of galactic mergers, cluster accretion, and tidal stripping that occur in galaxy clusters. In particular, intracluster planetary nebulae are a useful probe of intracluster light as a whole. We present a catalog of 318 intracluster planetary nebula candidates in the nearby Virgo Cluster of galaxies, taken with the Kitt Peak National Observatory 4m telescope. We detail the automated detection routines developed to search for these candidates and discuss the routines' strengths and weaknesses. We discuss the importance of contamination in the catalog, and the likely causes. We present magnitudes and positions of these candidates, suitable for spectroscopic follow-up observations. Analyses of these candidates are presented in other papers of this series.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65#table6</TD>
            <TD>2011-09-14T20:33:38Z</TD>
            <TD>#Clusters_of_galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/145/65 [1]</TD>
            <TD>Virgo intracluster planetary nebula candidates (Feldmeier+, 2003)</TD>
            <TD>Intracluster stars - stars outside of individual galaxies - are a sensitive measure of the poorly understood processes of galactic mergers, cluster accretion, and tidal stripping that occur in galaxy clusters. In particular, intracluster planetary nebulae are a useful probe of intracluster light as a whole. We present a catalog of 318 intracluster planetary nebula candidates in the nearby Virgo Cluster of galaxies, taken with the Kitt Peak National Observatory 4m telescope. We detail the automated detection routines developed to search for these candidates and discuss the routines' strengths and weaknesses. We discuss the importance of contamination in the catalog, and the likely causes. We present magnitudes and positions of these candidates, suitable for spectroscopic follow-up observations. Analyses of these candidates are presented in other papers of this series.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65#1</TD>
            <TD>2011-09-14T20:33:38Z</TD>
            <TD>#Clusters_of_galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/145/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/145/65 [2]</TD>
            <TD>Virgo intracluster planetary nebula candidates (Feldmeier+, 2003)</TD>
            <TD>Intracluster stars - stars outside of individual galaxies - are a sensitive measure of the poorly understood processes of galactic mergers, cluster accretion, and tidal stripping that occur in galaxy clusters. In particular, intracluster planetary nebulae are a useful probe of intracluster light as a whole. We present a catalog of 318 intracluster planetary nebula candidates in the nearby Virgo Cluster of galaxies, taken with the Kitt Peak National Observatory 4m telescope. We detail the automated detection routines developed to search for these candidates and discuss the routines' strengths and weaknesses. We discuss the importance of contamination in the catalog, and the likely causes. We present magnitudes and positions of these candidates, suitable for spectroscopic follow-up observations. Analyses of these candidates are presented in other papers of this series.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65#2</TD>
            <TD>2011-09-14T20:33:38Z</TD>
            <TD>#Clusters_of_galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/145/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/65 [table6]</TD>
            <TD>Virgo intracluster planetary nebula candidates (Feldmeier+, 2003)</TD>
            <TD>Intracluster stars - stars outside of individual galaxies - are a sensitive measure of the poorly understood processes of galactic mergers, cluster accretion, and tidal stripping that occur in galaxy clusters. In particular, intracluster planetary nebulae are a useful probe of intracluster light as a whole. We present a catalog of 318 intracluster planetary nebula candidates in the nearby Virgo Cluster of galaxies, taken with the Kitt Peak National Observatory 4m telescope. We detail the automated detection routines developed to search for these candidates and discuss the routines' strengths and weaknesses. We discuss the importance of contamination in the catalog, and the likely causes. We present magnitudes and positions of these candidates, suitable for spectroscopic follow-up observations. Analyses of these candidates are presented in other papers of this series.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65#table6</TD>
            <TD>2011-09-14T20:33:38Z</TD>
            <TD>#Clusters_of_galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/125/459 [1]</TD>
            <TD>Nearby clusters of galaxies properties. III. (Trevese+ 1997)</TD>
            <TD>This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. &lt;J/A+AS/94/327&gt;, Flin et al. 1995, Cat. &lt;J/A+AS/110/313&gt;, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459#1</TD>
            <TD>2012-08-25T22:04:56Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/125/459</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/459</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/125/459 [2]</TD>
            <TD>Nearby clusters of galaxies properties. III. (Trevese+ 1997)</TD>
            <TD>This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. &lt;J/A+AS/94/327&gt;, Flin et al. 1995, Cat. &lt;J/A+AS/110/313&gt;, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459#2</TD>
            <TD>2012-08-25T22:04:56Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/125/459&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/459</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/125/459 [tables]</TD>
            <TD>Nearby clusters of galaxies properties. III. (Trevese+ 1997)</TD>
            <TD>This paper is the third of a series (Trevese et al. 1992, Paper I, Cat. &lt;J/A+AS/94/327&gt;, Flin et al. 1995, Cat. &lt;J/A+AS/110/313&gt;, Paper II, presenting F band photometry, from digitized 48-inch Palomar plates, of the galaxies brighter than m_3_+3 in a clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density. In the present paper we analyze 15 new clusters and provide the absolute alpha and delta coordinates of the galaxies of 8 Abell clusters, studied in pap. I, which were published with relative coordinates only. In the electronic version, the tables of the 8 clusters of pap. I are written in the same format of papers II and III.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459#tables</TD>
            <TD>2012-08-25T22:04:56Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/125/459</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/125/459&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/125/459</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1918 [1]</TD>
            <TD>MX northern Abell cluster redshift survey. II. (Miller+, 2002)</TD>
            <TD>The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10&lt;=17.0. We present 1542 new galaxy redshifts within 117 R&gt;=1 Abell cluster fields that have 16.9&lt;=m10&lt;=17.0, 0h&lt;=RA&lt;=24h, -17{deg}&lt;=DE&lt;=90{deg}, and |b|&gt;=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918#1</TD>
            <TD>2011-09-14T20:34:03Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1918</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1918</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1918 [2]</TD>
            <TD>MX northern Abell cluster redshift survey. II. (Miller+, 2002)</TD>
            <TD>The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10&lt;=17.0. We present 1542 new galaxy redshifts within 117 R&gt;=1 Abell cluster fields that have 16.9&lt;=m10&lt;=17.0, 0h&lt;=RA&lt;=24h, -17{deg}&lt;=DE&lt;=90{deg}, and |b|&gt;=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918#2</TD>
            <TD>2011-09-14T20:34:03Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1918&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1918</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1918 [table1]</TD>
            <TD>MX northern Abell cluster redshift survey. II. (Miller+, 2002)</TD>
            <TD>The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10&lt;=17.0. We present 1542 new galaxy redshifts within 117 R&gt;=1 Abell cluster fields that have 16.9&lt;=m10&lt;=17.0, 0h&lt;=RA&lt;=24h, -17{deg}&lt;=DE&lt;=90{deg}, and |b|&gt;=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918#table1</TD>
            <TD>2011-09-14T20:34:03Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1918&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1918</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/141/88 [1]</TD>
            <TD>Galaxy cluster environments of radio sources (Wing+, 2011)</TD>
            <TD>Using the Sloan Digital Sky Survey (SDSS) and the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) catalogs, we examined the optical environments around double-lobed radio sources. Previous studies have shown that multi-component radio sources exhibiting some degree of bending between components are likely to be found in galaxy clusters. Often this radio emission is associated with a cD-type galaxy at the center of a cluster. We cross-correlated the SDSS and FIRST catalogs and measured the richness of the cluster environments surrounding both bent and straight multi-component radio sources. This led to the discovery and classification of a large number of galaxy clusters out to a redshift of z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88#1</TD>
            <TD>2012-09-07T17:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/141/88</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/141/88</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/141/88 [2]</TD>
            <TD>Galaxy cluster environments of radio sources (Wing+, 2011)</TD>
            <TD>Using the Sloan Digital Sky Survey (SDSS) and the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) catalogs, we examined the optical environments around double-lobed radio sources. Previous studies have shown that multi-component radio sources exhibiting some degree of bending between components are likely to be found in galaxy clusters. Often this radio emission is associated with a cD-type galaxy at the center of a cluster. We cross-correlated the SDSS and FIRST catalogs and measured the richness of the cluster environments surrounding both bent and straight multi-component radio sources. This led to the discovery and classification of a large number of galaxy clusters out to a redshift of z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88#2</TD>
            <TD>2012-09-07T17:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/141/88&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/141/88</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/141/88 [table6]</TD>
            <TD>Galaxy cluster environments of radio sources (Wing+, 2011)</TD>
            <TD>Using the Sloan Digital Sky Survey (SDSS) and the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) catalogs, we examined the optical environments around double-lobed radio sources. Previous studies have shown that multi-component radio sources exhibiting some degree of bending between components are likely to be found in galaxy clusters. Often this radio emission is associated with a cD-type galaxy at the center of a cluster. We cross-correlated the SDSS and FIRST catalogs and measured the richness of the cluster environments surrounding both bent and straight multi-component radio sources. This led to the discovery and classification of a large number of galaxy clusters out to a redshift of z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88#table6</TD>
            <TD>2012-09-07T17:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/141/88&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/141/88</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1918 [1]</TD>
            <TD>MX northern Abell cluster redshift survey. II. (Miller+, 2002)</TD>
            <TD>The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10&lt;=17.0. We present 1542 new galaxy redshifts within 117 R&gt;=1 Abell cluster fields that have 16.9&lt;=m10&lt;=17.0, 0h&lt;=RA&lt;=24h, -17{deg}&lt;=DE&lt;=90{deg}, and |b|&gt;=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918#1</TD>
            <TD>2011-09-14T20:34:03Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1918</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1918</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1918 [2]</TD>
            <TD>MX northern Abell cluster redshift survey. II. (Miller+, 2002)</TD>
            <TD>The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10&lt;=17.0. We present 1542 new galaxy redshifts within 117 R&gt;=1 Abell cluster fields that have 16.9&lt;=m10&lt;=17.0, 0h&lt;=RA&lt;=24h, -17{deg}&lt;=DE&lt;=90{deg}, and |b|&gt;=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918#2</TD>
            <TD>2011-09-14T20:34:03Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1918&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1918</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1918 [table1]</TD>
            <TD>MX northern Abell cluster redshift survey. II. (Miller+, 2002)</TD>
            <TD>The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10&lt;=17.0. We present 1542 new galaxy redshifts within 117 R&gt;=1 Abell cluster fields that have 16.9&lt;=m10&lt;=17.0, 0h&lt;=RA&lt;=24h, -17{deg}&lt;=DE&lt;=90{deg}, and |b|&gt;=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918#table1</TD>
            <TD>2011-09-14T20:34:03Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1918&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1918</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/141/88 [1]</TD>
            <TD>Galaxy cluster environments of radio sources (Wing+, 2011)</TD>
            <TD>Using the Sloan Digital Sky Survey (SDSS) and the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) catalogs, we examined the optical environments around double-lobed radio sources. Previous studies have shown that multi-component radio sources exhibiting some degree of bending between components are likely to be found in galaxy clusters. Often this radio emission is associated with a cD-type galaxy at the center of a cluster. We cross-correlated the SDSS and FIRST catalogs and measured the richness of the cluster environments surrounding both bent and straight multi-component radio sources. This led to the discovery and classification of a large number of galaxy clusters out to a redshift of z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88#1</TD>
            <TD>2012-09-07T17:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/141/88</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/141/88</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/141/88 [2]</TD>
            <TD>Galaxy cluster environments of radio sources (Wing+, 2011)</TD>
            <TD>Using the Sloan Digital Sky Survey (SDSS) and the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) catalogs, we examined the optical environments around double-lobed radio sources. Previous studies have shown that multi-component radio sources exhibiting some degree of bending between components are likely to be found in galaxy clusters. Often this radio emission is associated with a cD-type galaxy at the center of a cluster. We cross-correlated the SDSS and FIRST catalogs and measured the richness of the cluster environments surrounding both bent and straight multi-component radio sources. This led to the discovery and classification of a large number of galaxy clusters out to a redshift of z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88#2</TD>
            <TD>2012-09-07T17:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/141/88&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/141/88</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/141/88 [table6]</TD>
            <TD>Galaxy cluster environments of radio sources (Wing+, 2011)</TD>
            <TD>Using the Sloan Digital Sky Survey (SDSS) and the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) catalogs, we examined the optical environments around double-lobed radio sources. Previous studies have shown that multi-component radio sources exhibiting some degree of bending between components are likely to be found in galaxy clusters. Often this radio emission is associated with a cD-type galaxy at the center of a cluster. We cross-correlated the SDSS and FIRST catalogs and measured the richness of the cluster environments surrounding both bent and straight multi-component radio sources. This led to the discovery and classification of a large number of galaxy clusters out to a redshift of z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88#table6</TD>
            <TD>2012-09-07T17:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/141/88&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/141/88</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1918 [1]</TD>
            <TD>MX northern Abell cluster redshift survey. II. (Miller+, 2002)</TD>
            <TD>The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10&lt;=17.0. We present 1542 new galaxy redshifts within 117 R&gt;=1 Abell cluster fields that have 16.9&lt;=m10&lt;=17.0, 0h&lt;=RA&lt;=24h, -17{deg}&lt;=DE&lt;=90{deg}, and |b|&gt;=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918#1</TD>
            <TD>2011-09-14T20:34:03Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1918</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1918</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1918 [2]</TD>
            <TD>MX northern Abell cluster redshift survey. II. (Miller+, 2002)</TD>
            <TD>The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10&lt;=17.0. We present 1542 new galaxy redshifts within 117 R&gt;=1 Abell cluster fields that have 16.9&lt;=m10&lt;=17.0, 0h&lt;=RA&lt;=24h, -17{deg}&lt;=DE&lt;=90{deg}, and |b|&gt;=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918#2</TD>
            <TD>2011-09-14T20:34:03Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1918&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1918</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1918 [table1]</TD>
            <TD>MX northern Abell cluster redshift survey. II. (Miller+, 2002)</TD>
            <TD>The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10&lt;=17.0. We present 1542 new galaxy redshifts within 117 R&gt;=1 Abell cluster fields that have 16.9&lt;=m10&lt;=17.0, 0h&lt;=RA&lt;=24h, -17{deg}&lt;=DE&lt;=90{deg}, and |b|&gt;=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918#table1</TD>
            <TD>2011-09-14T20:34:03Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1918</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1918&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1918</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/141/88 [1]</TD>
            <TD>Galaxy cluster environments of radio sources (Wing+, 2011)</TD>
            <TD>Using the Sloan Digital Sky Survey (SDSS) and the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) catalogs, we examined the optical environments around double-lobed radio sources. Previous studies have shown that multi-component radio sources exhibiting some degree of bending between components are likely to be found in galaxy clusters. Often this radio emission is associated with a cD-type galaxy at the center of a cluster. We cross-correlated the SDSS and FIRST catalogs and measured the richness of the cluster environments surrounding both bent and straight multi-component radio sources. This led to the discovery and classification of a large number of galaxy clusters out to a redshift of z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88#1</TD>
            <TD>2012-09-07T17:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/141/88</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/141/88</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/141/88 [2]</TD>
            <TD>Galaxy cluster environments of radio sources (Wing+, 2011)</TD>
            <TD>Using the Sloan Digital Sky Survey (SDSS) and the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) catalogs, we examined the optical environments around double-lobed radio sources. Previous studies have shown that multi-component radio sources exhibiting some degree of bending between components are likely to be found in galaxy clusters. Often this radio emission is associated with a cD-type galaxy at the center of a cluster. We cross-correlated the SDSS and FIRST catalogs and measured the richness of the cluster environments surrounding both bent and straight multi-component radio sources. This led to the discovery and classification of a large number of galaxy clusters out to a redshift of z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88#2</TD>
            <TD>2012-09-07T17:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/141/88&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/141/88</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/141/88 [table6]</TD>
            <TD>Galaxy cluster environments of radio sources (Wing+, 2011)</TD>
            <TD>Using the Sloan Digital Sky Survey (SDSS) and the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) catalogs, we examined the optical environments around double-lobed radio sources. Previous studies have shown that multi-component radio sources exhibiting some degree of bending between components are likely to be found in galaxy clusters. Often this radio emission is associated with a cD-type galaxy at the center of a cluster. We cross-correlated the SDSS and FIRST catalogs and measured the richness of the cluster environments surrounding both bent and straight multi-component radio sources. This led to the discovery and classification of a large number of galaxy clusters out to a redshift of z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88#table6</TD>
            <TD>2012-09-07T17:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/141/88</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/141/88&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/141/88</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/385/905 [1]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#1</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/385/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/385/905 [2]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#2</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/385/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/385/905 [table2]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#table2</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/385/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/385/905 [table3]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#table3</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/385/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/418/1409 [1]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#1</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/418/1409</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/418/1409 [2]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#2</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/418/1409&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/418/1409 [tablea1]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#tablea1</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/418/1409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/418/1409 [tablea2]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#tablea2</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/418/1409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/385/905 [1]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#1</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/385/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/385/905 [2]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#2</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/385/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/385/905 [table2]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#table2</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/385/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/385/905 [table3]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#table3</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/385/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/418/1409 [1]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#1</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/418/1409</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/418/1409 [2]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#2</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/418/1409&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/418/1409 [tablea1]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#tablea1</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/418/1409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/418/1409 [tablea2]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#tablea2</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/418/1409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/385/905 [1]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#1</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/385/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/385/905 [2]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#2</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/385/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/385/905 [table2]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#table2</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/385/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/385/905 [table3]</TD>
            <TD>OGLEII high pm stars towards Galactic Centre (Rattenbury+, 2008)</TD>
            <TD>The photometry data base of the second phase of the OGLE microlensing experiment, OGLE-II, is a rich source of information about the kinematics and structure of the Galaxy. In this work, we use the OGLE-II proper motion catalogue to identify candidate stars which have high proper motions. 521 stars with proper motion {mu}&gt;50mas/yr in the OGLE-II proper motion catalogue were cross-identified with stars in the MACHO high proper motion catalogue, and the DEep Near-Infrared Survey and Two-Micron All-Sky Survey infrared photometry catalogues. Photometric distances were computed for stars with colours consistent with G/K- and M-type stars. Six stars were newly identified as possible nearby (&lt;50pc) M dwarfs.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905#table3</TD>
            <TD>2011-09-14T20:45:43Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/385/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/418/1409 [1]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#1</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/418/1409</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/418/1409 [2]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#2</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/418/1409&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/418/1409 [tablea1]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#tablea1</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/418/1409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/418/1409 [tablea2]</TD>
            <TD>Compact groups of galaxies in SDSS DR7 (Mendel+, 2011)</TD>
            <TD>In Paper III (Cat. J/MNRAS/395/255) we describe the photometric selection of CGs from the SDSS Data Release 6 (Adelman-McCarthy et al., 2008, Cat. II/282/), which included imaging of the entire SDSS-II Legacy Survey area. Since that paper, SDSS Data Release 7 (DR7; Abazajian et al., 2009ApJS..182..543A) has provided an additional ~1200deg^2^ of spectroscopic data, completing spectroscopic observations of the SDSS-II Legacy Survey footprint. In what follows we use galaxy catalogues drawn from SDSS DR7 and, where available, supplement the CG samples in Paper III with updated spectroscopic information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409#tablea2</TD>
            <TD>2012-10-19T17:52:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/1409</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/418/1409&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/1409</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/249 [1]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#1</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/249</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/249 [2]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#2</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/249&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/249 [spectra]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#spectra</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/249&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/249 [master]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#master</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/249&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ARCQUINCXO [1]</TD>
            <TD>Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog</TD>
            <TD>The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arcquincxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arcquincxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=arcquincxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/arcquincxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ARCQUINCXO [2]</TD>
            <TD>Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog</TD>
            <TD>The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arcquincxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arcquincxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=arcquincxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/arcquincxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ARCQUINCXO [3]</TD>
            <TD>Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog</TD>
            <TD>The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arcquincxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arcquincxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_arcquincxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/arcquincxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/249 [1]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#1</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/249</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/249 [2]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#2</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/249&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/249 [spectra]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#spectra</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/249&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/249 [master]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#master</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/249&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ARCQUINCXO [1]</TD>
            <TD>Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog</TD>
            <TD>The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arcquincxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arcquincxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=arcquincxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/arcquincxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ARCQUINCXO [2]</TD>
            <TD>Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog</TD>
            <TD>The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arcquincxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arcquincxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=arcquincxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/arcquincxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ARCQUINCXO [3]</TD>
            <TD>Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog</TD>
            <TD>The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arcquincxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arcquincxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_arcquincxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/arcquincxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/249 [1]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#1</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/249</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/249 [2]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#2</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/249&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/249 [spectra]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#spectra</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/249&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/249 [master]</TD>
            <TD>6dF-DR2 Galaxy Survey (Jones+, 2005)</TD>
            <TD>The 6dF Galaxy Survey is measuring around 150000 redshifts and 15000 peculiar velocities from galaxies over the southern sky at |b|&gt;10{deg}. When complete, it will be the largest survey of its kind by more than an order of magnitude. A total of 83014 sources now have their spectra, redshifts, and near-infrared and optical photometry available online and searchable through an Structured Query Language at www.wfau.roe.ac.uk/6dFGS/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/249#master</TD>
            <TD>2011-09-14T20:56:16Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/VII/249</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/249&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/249</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ARCQUINCXO [1]</TD>
            <TD>Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog</TD>
            <TD>The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arcquincxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arcquincxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=arcquincxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/arcquincxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ARCQUINCXO [2]</TD>
            <TD>Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog</TD>
            <TD>The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arcquincxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arcquincxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=arcquincxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/arcquincxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ARCQUINCXO [3]</TD>
            <TD>Arches and Quintuplet Clusters Chandra X-Ray Point Source Catalog</TD>
            <TD>The Galactic centre (GC) provides a unique laboratory for a detailed examination of the interplay between massive star formation and the nuclear environment of our Galaxy. Here are presented some of the results from a 100-ks Chandra Advanced CCD Imaging Spectrometer (ACIS) observation of the Arches and Quintuplet star clusters in the form of a catalog of 244 point-like X-ray sources detected in the observation. The deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/arcquincxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/arcquincxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_arcquincxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/arcquincxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/392/1509 [1]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#1</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/392/1509</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/392/1509 [2]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#2</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/392/1509&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/1509 [table2]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#table2</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/1509&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/1509 [table4]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#table4</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/1509&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>DENIS/I [1]</TD>
            <TD>First DENIS I-band Extragalactic Catalog</TD>
            <TD>This database contains the release of the provisional extragalactic catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS) and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog). It was created using an automatic galaxy recognition program based on a discriminating analysis, the efficiency of which is estimated to be better than 99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star Catalog is about 6 arcseconds. The cross-identification with galaxies available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81, 413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains total I-band magnitude, isophotal diameter, axis ratio, position angle and a rough estimate of the morphological type code for 20620 galaxies. The internal completeness of this catalog reaches a limiting I-band magnitude of 14.5, with a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed in this study.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/denisigal#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/denisigal</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=denisigal&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/denisigal.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>DENIS/I [2]</TD>
            <TD>First DENIS I-band Extragalactic Catalog</TD>
            <TD>This database contains the release of the provisional extragalactic catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS) and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog). It was created using an automatic galaxy recognition program based on a discriminating analysis, the efficiency of which is estimated to be better than 99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star Catalog is about 6 arcseconds. The cross-identification with galaxies available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81, 413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains total I-band magnitude, isophotal diameter, axis ratio, position angle and a rough estimate of the morphological type code for 20620 galaxies. The internal completeness of this catalog reaches a limiting I-band magnitude of 14.5, with a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed in this study.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/denisigal#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/denisigal</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=denisigal&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/denisigal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>DENIS/I [3]</TD>
            <TD>First DENIS I-band Extragalactic Catalog</TD>
            <TD>This database contains the release of the provisional extragalactic catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS) and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog). It was created using an automatic galaxy recognition program based on a discriminating analysis, the efficiency of which is estimated to be better than 99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star Catalog is about 6 arcseconds. The cross-identification with galaxies available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81, 413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains total I-band magnitude, isophotal diameter, axis ratio, position angle and a rough estimate of the morphological type code for 20620 galaxies. The internal completeness of this catalog reaches a limiting I-band magnitude of 14.5, with a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed in this study.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/denisigal#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
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            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/denisigal</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_denisigal&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/denisigal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/392/1509 [1]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#1</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/392/1509</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/392/1509 [2]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#2</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/392/1509&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/1509 [table2]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#table2</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/1509&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/1509 [table4]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#table4</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/1509&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/704/789 [1]</TD>
            <TD>Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)</TD>
            <TD>Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z&lt;0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789#1</TD>
            <TD>2011-12-26T15:01:34Z</TD>
            <TD>#AGN#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/704/789</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/789</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/704/789 [2]</TD>
            <TD>Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)</TD>
            <TD>Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z&lt;0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789#2</TD>
            <TD>2011-12-26T15:01:34Z</TD>
            <TD>#AGN#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/704/789&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/789</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/704/789 [table1]</TD>
            <TD>Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)</TD>
            <TD>Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z&lt;0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789#table1</TD>
            <TD>2011-12-26T15:01:34Z</TD>
            <TD>#AGN#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/704/789&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/789</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/392/1509 [1]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#1</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/392/1509</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/392/1509 [2]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#2</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/392/1509&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/1509 [table2]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#table2</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/1509&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/1509 [table4]</TD>
            <TD>Distribution of AGNs in galaxy clusters (Gilmour+, 2009)</TD>
            <TD>We present an analysis of the X-ray point source populations in 182 Chandra images of galaxy clusters at z&gt;0.1 with exposure time &gt;10ks, as well as 44 non-cluster fields. The analysis of the number and flux of these sources, using a detailed pipeline to predict the distribution of non-cluster sources in each field, reveals an excess of X-ray point sources associated with the galaxy clusters. A sample of 148 galaxy clusters at 0.1&lt;z&lt;0.9 , with no other nearby clusters, shows an excess of 230 cluster sources in total, an average of ~1.5 sources per cluster. The lack of optical data for these clusters limits the physical interpretation of this result, as we cannot calculate the fraction of cluster galaxies hosting X-ray sources. However, the fluxes of the excess sources indicate that over half of them are very likely to be active galactic nuclei (AGN), and the radial distribution shows that they are quite evenly distributed over the central 1Mpc of the cluster, with almost no sources found beyond this radius. We also use this pipeline to successfully reproduce the results of previous studies, particularly the higher density of sources in the central 0.5Mpc of a few cluster fields, but show that these conclusions are not generally valid for this larger sample of clusters. We conclude that some of these differences may be due to the sample properties, such as the size and redshift of the clusters studied, or a lack of publications for cluster fields with no excess sources. This paper also presents the basic X-ray properties of the galaxy clusters, and in subsequent papers in this series the dependence of the AGN population on these cluster properties will be evaluated.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509#table4</TD>
            <TD>2011-09-14T20:56:23Z</TD>
            <TD>#AGN#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/1509</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/1509&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/1509</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>DENIS/I [1]</TD>
            <TD>First DENIS I-band Extragalactic Catalog</TD>
            <TD>This database contains the release of the provisional extragalactic catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS) and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog). It was created using an automatic galaxy recognition program based on a discriminating analysis, the efficiency of which is estimated to be better than 99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star Catalog is about 6 arcseconds. The cross-identification with galaxies available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81, 413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains total I-band magnitude, isophotal diameter, axis ratio, position angle and a rough estimate of the morphological type code for 20620 galaxies. The internal completeness of this catalog reaches a limiting I-band magnitude of 14.5, with a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed in this study.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/denisigal#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/denisigal</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=denisigal&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/denisigal.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>DENIS/I [2]</TD>
            <TD>First DENIS I-band Extragalactic Catalog</TD>
            <TD>This database contains the release of the provisional extragalactic catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS) and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog). It was created using an automatic galaxy recognition program based on a discriminating analysis, the efficiency of which is estimated to be better than 99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star Catalog is about 6 arcseconds. The cross-identification with galaxies available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81, 413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains total I-band magnitude, isophotal diameter, axis ratio, position angle and a rough estimate of the morphological type code for 20620 galaxies. The internal completeness of this catalog reaches a limiting I-band magnitude of 14.5, with a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed in this study.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/denisigal#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/denisigal</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=denisigal&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/denisigal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>DENIS/I [3]</TD>
            <TD>First DENIS I-band Extragalactic Catalog</TD>
            <TD>This database contains the release of the provisional extragalactic catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS) and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog). It was created using an automatic galaxy recognition program based on a discriminating analysis, the efficiency of which is estimated to be better than 99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star Catalog is about 6 arcseconds. The cross-identification with galaxies available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81, 413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains total I-band magnitude, isophotal diameter, axis ratio, position angle and a rough estimate of the morphological type code for 20620 galaxies. The internal completeness of this catalog reaches a limiting I-band magnitude of 14.5, with a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed in this study.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/denisigal#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/denisigal</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_denisigal&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/denisigal.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GC [1]</TD>
            <TD>Milky Way Globular Clusters Catalog (February 2003 Version)</TD>
            <TD>This is the Catalog of Parameters for Milky Way Globular Clusters (February 2003 Version) that was compiled by William E. Harris of McMaster University. It contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: &lt;a href="http://www.physics.mcmaster.ca/~harris/mwgc.ref"&gt;http://www.physics.mcmaster.ca/~harris/mwgc.ref&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/globclust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/globclust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=globclust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/globclust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GC [2]</TD>
            <TD>Milky Way Globular Clusters Catalog (February 2003 Version)</TD>
            <TD>This is the Catalog of Parameters for Milky Way Globular Clusters (February 2003 Version) that was compiled by William E. Harris of McMaster University. It contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: &lt;a href="http://www.physics.mcmaster.ca/~harris/mwgc.ref"&gt;http://www.physics.mcmaster.ca/~harris/mwgc.ref&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/globclust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/globclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=globclust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/globclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GC [3]</TD>
            <TD>Milky Way Globular Clusters Catalog (February 2003 Version)</TD>
            <TD>This is the Catalog of Parameters for Milky Way Globular Clusters (February 2003 Version) that was compiled by William E. Harris of McMaster University. It contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: &lt;a href="http://www.physics.mcmaster.ca/~harris/mwgc.ref"&gt;http://www.physics.mcmaster.ca/~harris/mwgc.ref&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/globclust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/globclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_globclust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/globclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/686/859 [1]</TD>
            <TD>Radio sources at 0.327, 1.4, 4.5, 8.5GHz (Birzan+, 2008)</TD>
            <TD>The sample consists of 22 galaxy clusters, one galaxy group (HCG 62), and one elliptical galaxy (M84). In order to have radio data at 327MHz, 1.4GHz, 4.5GHz, and 8.5GHz, we observed 13 objects that did not have VLA archival data at one or more of these frequencies. The observations that we used for each frequency are given in Appendix A (table 6 and 7).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859#1</TD>
            <TD>2011-09-14T21:13:20Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/686/859</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/859</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/686/859 [2]</TD>
            <TD>Radio sources at 0.327, 1.4, 4.5, 8.5GHz (Birzan+, 2008)</TD>
            <TD>The sample consists of 22 galaxy clusters, one galaxy group (HCG 62), and one elliptical galaxy (M84). In order to have radio data at 327MHz, 1.4GHz, 4.5GHz, and 8.5GHz, we observed 13 objects that did not have VLA archival data at one or more of these frequencies. The observations that we used for each frequency are given in Appendix A (table 6 and 7).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859#2</TD>
            <TD>2011-09-14T21:13:20Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/686/859&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/859</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/859 [table1]</TD>
            <TD>Radio sources at 0.327, 1.4, 4.5, 8.5GHz (Birzan+, 2008)</TD>
            <TD>The sample consists of 22 galaxy clusters, one galaxy group (HCG 62), and one elliptical galaxy (M84). In order to have radio data at 327MHz, 1.4GHz, 4.5GHz, and 8.5GHz, we observed 13 objects that did not have VLA archival data at one or more of these frequencies. The observations that we used for each frequency are given in Appendix A (table 6 and 7).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859#table1</TD>
            <TD>2011-09-14T21:13:20Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/859&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/859</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>DENIS/I [1]</TD>
            <TD>First DENIS I-band Extragalactic Catalog</TD>
            <TD>This database contains the release of the provisional extragalactic catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS) and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog). It was created using an automatic galaxy recognition program based on a discriminating analysis, the efficiency of which is estimated to be better than 99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star Catalog is about 6 arcseconds. The cross-identification with galaxies available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81, 413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains total I-band magnitude, isophotal diameter, axis ratio, position angle and a rough estimate of the morphological type code for 20620 galaxies. The internal completeness of this catalog reaches a limiting I-band magnitude of 14.5, with a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed in this study.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/denisigal#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/denisigal</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=denisigal&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/denisigal.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>DENIS/I [2]</TD>
            <TD>First DENIS I-band Extragalactic Catalog</TD>
            <TD>This database contains the release of the provisional extragalactic catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS) and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog). It was created using an automatic galaxy recognition program based on a discriminating analysis, the efficiency of which is estimated to be better than 99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star Catalog is about 6 arcseconds. The cross-identification with galaxies available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81, 413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains total I-band magnitude, isophotal diameter, axis ratio, position angle and a rough estimate of the morphological type code for 20620 galaxies. The internal completeness of this catalog reaches a limiting I-band magnitude of 14.5, with a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed in this study.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/denisigal#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/denisigal</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=denisigal&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/denisigal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>DENIS/I [3]</TD>
            <TD>First DENIS I-band Extragalactic Catalog</TD>
            <TD>This database contains the release of the provisional extragalactic catalog constructed from the "Deep Near Infrared Southern Sky Survey" (DENIS) and is sometimes referred to as REDCAT (Rapid Extraction from DENIS Catalog). It was created using an automatic galaxy recognition program based on a discriminating analysis, the efficiency of which is estimated to be better than 99%. The nominal accuracy for galaxy coordinates calculated with the Guide Star Catalog is about 6 arcseconds. The cross-identification with galaxies available in the Lyon-Meudon Extragalactic DAtabase (LEDA) allows a calibration of the I-band photometry with the sample of Mathewson et al. (1992, ApJS, 81, 413) and Mathewson and Ford (1996, ApJS, 107, 97). Thus, the catalog contains total I-band magnitude, isophotal diameter, axis ratio, position angle and a rough estimate of the morphological type code for 20620 galaxies. The internal completeness of this catalog reaches a limiting I-band magnitude of 14.5, with a photometric accuracy of 0.18 mag. 25% of the Southern sky has been processed in this study.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/denisigal#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/denisigal</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_denisigal&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/denisigal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/704/789 [1]</TD>
            <TD>Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)</TD>
            <TD>Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z&lt;0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789#1</TD>
            <TD>2011-12-26T15:01:34Z</TD>
            <TD>#AGN#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/704/789</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/789</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/704/789 [2]</TD>
            <TD>Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)</TD>
            <TD>Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z&lt;0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789#2</TD>
            <TD>2011-12-26T15:01:34Z</TD>
            <TD>#AGN#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/704/789&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/789</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/704/789 [table1]</TD>
            <TD>Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)</TD>
            <TD>Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z&lt;0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789#table1</TD>
            <TD>2011-12-26T15:01:34Z</TD>
            <TD>#AGN#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/704/789&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/789</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/686/859 [1]</TD>
            <TD>Radio sources at 0.327, 1.4, 4.5, 8.5GHz (Birzan+, 2008)</TD>
            <TD>The sample consists of 22 galaxy clusters, one galaxy group (HCG 62), and one elliptical galaxy (M84). In order to have radio data at 327MHz, 1.4GHz, 4.5GHz, and 8.5GHz, we observed 13 objects that did not have VLA archival data at one or more of these frequencies. The observations that we used for each frequency are given in Appendix A (table 6 and 7).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859#1</TD>
            <TD>2011-09-14T21:13:20Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/686/859</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/859</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/686/859 [2]</TD>
            <TD>Radio sources at 0.327, 1.4, 4.5, 8.5GHz (Birzan+, 2008)</TD>
            <TD>The sample consists of 22 galaxy clusters, one galaxy group (HCG 62), and one elliptical galaxy (M84). In order to have radio data at 327MHz, 1.4GHz, 4.5GHz, and 8.5GHz, we observed 13 objects that did not have VLA archival data at one or more of these frequencies. The observations that we used for each frequency are given in Appendix A (table 6 and 7).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859#2</TD>
            <TD>2011-09-14T21:13:20Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/686/859&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/859</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/859 [table1]</TD>
            <TD>Radio sources at 0.327, 1.4, 4.5, 8.5GHz (Birzan+, 2008)</TD>
            <TD>The sample consists of 22 galaxy clusters, one galaxy group (HCG 62), and one elliptical galaxy (M84). In order to have radio data at 327MHz, 1.4GHz, 4.5GHz, and 8.5GHz, we observed 13 objects that did not have VLA archival data at one or more of these frequencies. The observations that we used for each frequency are given in Appendix A (table 6 and 7).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859#table1</TD>
            <TD>2011-09-14T21:13:20Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/859&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/859</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ESO/Uppsala [1]</TD>
            <TD>ESO-Uppsala ESO(B) Survey</TD>
            <TD>This database table was derived from information provided in "The ESO/Uppsala Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a passband similar to the Johnson B color. Additional information is available from the HEASARC.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/esouppsala#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/esouppsala</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=esouppsala&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/esouppsala.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ESO/Uppsala [2]</TD>
            <TD>ESO-Uppsala ESO(B) Survey</TD>
            <TD>This database table was derived from information provided in "The ESO/Uppsala Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a passband similar to the Johnson B color. Additional information is available from the HEASARC.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/esouppsala#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/esouppsala</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=esouppsala&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/esouppsala.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ESO/Uppsala [3]</TD>
            <TD>ESO-Uppsala ESO(B) Survey</TD>
            <TD>This database table was derived from information provided in "The ESO/Uppsala Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a passband similar to the Johnson B color. Additional information is available from the HEASARC.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/esouppsala#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/esouppsala</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_esouppsala&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/esouppsala.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/704/789 [1]</TD>
            <TD>Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)</TD>
            <TD>Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z&lt;0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789#1</TD>
            <TD>2011-12-26T15:01:34Z</TD>
            <TD>#AGN#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/704/789</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/789</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/704/789 [2]</TD>
            <TD>Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)</TD>
            <TD>Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z&lt;0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789#2</TD>
            <TD>2011-12-26T15:01:34Z</TD>
            <TD>#AGN#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/704/789&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/789</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/704/789 [table1]</TD>
            <TD>Ultra-luminous infrared galaxies in SDSS-DR6 (Hou+, 2009)</TD>
            <TD>Ultra-luminous infrared galaxies (ULIRGs) are interesting objects with dramatic properties. Many efforts have been made to understand the physics of their luminous infrared emission and evolutionary stages. However, a large ULIRG sample is still needed to study the properties of their central black holes (BHs), the BH-host galaxy relation, and their evolution. We identified 308 ULIRGs from the Sloan Digital Sky Survey Data Release 6, and classified them into the NL ULIRGs (with only narrow emission lines) and the Type I ULIRGs (with broad emission lines). About 56% of ULIRGs in our total sample show interaction features, and this percentage is 79% for redshift z&lt;0.2. Optical identifications of these ULIRGs show that the active galactic nucleus percentage is at least 49%, and the percentage increases with the infrared luminosity. We found 62 Type I ULIRGs, and estimated their BH masses and velocity dispersions from their optical spectra. Together with known Type I ULIRGs in the literature, a sample of 90 Type I ULIRGs enables us to make a statistical study.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789#table1</TD>
            <TD>2011-12-26T15:01:34Z</TD>
            <TD>#AGN#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/789</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/704/789&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/789</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/686/859 [1]</TD>
            <TD>Radio sources at 0.327, 1.4, 4.5, 8.5GHz (Birzan+, 2008)</TD>
            <TD>The sample consists of 22 galaxy clusters, one galaxy group (HCG 62), and one elliptical galaxy (M84). In order to have radio data at 327MHz, 1.4GHz, 4.5GHz, and 8.5GHz, we observed 13 objects that did not have VLA archival data at one or more of these frequencies. The observations that we used for each frequency are given in Appendix A (table 6 and 7).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859#1</TD>
            <TD>2011-09-14T21:13:20Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/686/859</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/859</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/686/859 [2]</TD>
            <TD>Radio sources at 0.327, 1.4, 4.5, 8.5GHz (Birzan+, 2008)</TD>
            <TD>The sample consists of 22 galaxy clusters, one galaxy group (HCG 62), and one elliptical galaxy (M84). In order to have radio data at 327MHz, 1.4GHz, 4.5GHz, and 8.5GHz, we observed 13 objects that did not have VLA archival data at one or more of these frequencies. The observations that we used for each frequency are given in Appendix A (table 6 and 7).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859#2</TD>
            <TD>2011-09-14T21:13:20Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/686/859&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/859</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/859 [table1]</TD>
            <TD>Radio sources at 0.327, 1.4, 4.5, 8.5GHz (Birzan+, 2008)</TD>
            <TD>The sample consists of 22 galaxy clusters, one galaxy group (HCG 62), and one elliptical galaxy (M84). In order to have radio data at 327MHz, 1.4GHz, 4.5GHz, and 8.5GHz, we observed 13 objects that did not have VLA archival data at one or more of these frequencies. The observations that we used for each frequency are given in Appendix A (table 6 and 7).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859#table1</TD>
            <TD>2011-09-14T21:13:20Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/859</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/859&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/859</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ESO/Uppsala [1]</TD>
            <TD>ESO-Uppsala ESO(B) Survey</TD>
            <TD>This database table was derived from information provided in "The ESO/Uppsala Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a passband similar to the Johnson B color. Additional information is available from the HEASARC.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/esouppsala#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/esouppsala</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=esouppsala&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/esouppsala.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ESO/Uppsala [2]</TD>
            <TD>ESO-Uppsala ESO(B) Survey</TD>
            <TD>This database table was derived from information provided in "The ESO/Uppsala Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a passband similar to the Johnson B color. Additional information is available from the HEASARC.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/esouppsala#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/esouppsala</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=esouppsala&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/esouppsala.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ESO/Uppsala [3]</TD>
            <TD>ESO-Uppsala ESO(B) Survey</TD>
            <TD>This database table was derived from information provided in "The ESO/Uppsala Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a passband similar to the Johnson B color. Additional information is available from the HEASARC.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/esouppsala#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/esouppsala</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_esouppsala&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/esouppsala.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/704/898 [1]</TD>
            <TD>Photometry of the Hercules dwarf galaxy (Sand+, 2009)</TD>
            <TD>Observations of Hercules were, with one exception, taken during 2008 May and June during normal operations of the Large Binocular Telescope (LBT), fitted with the red and blue channels of the Large Binocular Camera. The B- and V-band images for the central Hercules field were taken during Science Demonstration Time (SDT) and were presented in Coleman et al. (2007ApJ...668L..43C). When necessary, we adopted SDSS-DR6 photometry directly for stars brighter than and near the saturation limit of a given LBT field (which depends both on the observing conditions and point spread function). In this case, g and r magnitudes are converted to B magnitudes via the relations found by Jordi et al. (2006A&amp;A...460..339J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898#1</TD>
            <TD>2011-12-26T21:12:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/704/898</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/898</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/704/898 [2]</TD>
            <TD>Photometry of the Hercules dwarf galaxy (Sand+, 2009)</TD>
            <TD>Observations of Hercules were, with one exception, taken during 2008 May and June during normal operations of the Large Binocular Telescope (LBT), fitted with the red and blue channels of the Large Binocular Camera. The B- and V-band images for the central Hercules field were taken during Science Demonstration Time (SDT) and were presented in Coleman et al. (2007ApJ...668L..43C). When necessary, we adopted SDSS-DR6 photometry directly for stars brighter than and near the saturation limit of a given LBT field (which depends both on the observing conditions and point spread function). In this case, g and r magnitudes are converted to B magnitudes via the relations found by Jordi et al. (2006A&amp;A...460..339J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898#2</TD>
            <TD>2011-12-26T21:12:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/704/898&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/898</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/704/898 [catalog]</TD>
            <TD>Photometry of the Hercules dwarf galaxy (Sand+, 2009)</TD>
            <TD>Observations of Hercules were, with one exception, taken during 2008 May and June during normal operations of the Large Binocular Telescope (LBT), fitted with the red and blue channels of the Large Binocular Camera. The B- and V-band images for the central Hercules field were taken during Science Demonstration Time (SDT) and were presented in Coleman et al. (2007ApJ...668L..43C). When necessary, we adopted SDSS-DR6 photometry directly for stars brighter than and near the saturation limit of a given LBT field (which depends both on the observing conditions and point spread function). In this case, g and r magnitudes are converted to B magnitudes via the relations found by Jordi et al. (2006A&amp;A...460..339J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898#catalog</TD>
            <TD>2011-12-26T21:12:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/704/898&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/898</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/692/511 [1]</TD>
            <TD>Mergers of luminous early-type galaxies (Wen+, 2009)</TD>
            <TD>Supermassive black hole (SMBH) coalescence in galaxy mergers is believed to be one of the primary sources of very low frequency gravitational waves (GWs). Significant contribution of the GWs comes from mergers of massive galaxies with redshifts z&lt;2. Very few previous studies gave the merger rate of massive galaxies. We selected a large sample (1209) of close pairs of galaxies with projected separations 7&lt;r_p_&lt;50kpc from 87889 luminous early-type galaxies (M_r_&lt;-21.5) from the Sloan Digital Sky Survey Data Release 6. These pairs constitute a complete volume-limited sample in the local universe (z&lt;0.12). Using our newly developed technique, 249 mergers have been identified by searching for interaction features. From them, we found that the merger fraction of luminous early-type galaxies is 0.8%, and the merger rate in the local universe is Rg~(1.0+/-0.4)x10^-5^Mpc^-3^/Gyr with an uncertainty mainly depending on the merging timescale.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511#1</TD>
            <TD>2011-09-14T21:22:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/692/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/692/511 [2]</TD>
            <TD>Mergers of luminous early-type galaxies (Wen+, 2009)</TD>
            <TD>Supermassive black hole (SMBH) coalescence in galaxy mergers is believed to be one of the primary sources of very low frequency gravitational waves (GWs). Significant contribution of the GWs comes from mergers of massive galaxies with redshifts z&lt;2. Very few previous studies gave the merger rate of massive galaxies. We selected a large sample (1209) of close pairs of galaxies with projected separations 7&lt;r_p_&lt;50kpc from 87889 luminous early-type galaxies (M_r_&lt;-21.5) from the Sloan Digital Sky Survey Data Release 6. These pairs constitute a complete volume-limited sample in the local universe (z&lt;0.12). Using our newly developed technique, 249 mergers have been identified by searching for interaction features. From them, we found that the merger fraction of luminous early-type galaxies is 0.8%, and the merger rate in the local universe is Rg~(1.0+/-0.4)x10^-5^Mpc^-3^/Gyr with an uncertainty mainly depending on the merging timescale.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511#2</TD>
            <TD>2011-09-14T21:22:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/692/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/692/511 [table1]</TD>
            <TD>Mergers of luminous early-type galaxies (Wen+, 2009)</TD>
            <TD>Supermassive black hole (SMBH) coalescence in galaxy mergers is believed to be one of the primary sources of very low frequency gravitational waves (GWs). Significant contribution of the GWs comes from mergers of massive galaxies with redshifts z&lt;2. Very few previous studies gave the merger rate of massive galaxies. We selected a large sample (1209) of close pairs of galaxies with projected separations 7&lt;r_p_&lt;50kpc from 87889 luminous early-type galaxies (M_r_&lt;-21.5) from the Sloan Digital Sky Survey Data Release 6. These pairs constitute a complete volume-limited sample in the local universe (z&lt;0.12). Using our newly developed technique, 249 mergers have been identified by searching for interaction features. From them, we found that the merger fraction of luminous early-type galaxies is 0.8%, and the merger rate in the local universe is Rg~(1.0+/-0.4)x10^-5^Mpc^-3^/Gyr with an uncertainty mainly depending on the merging timescale.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511#table1</TD>
            <TD>2011-09-14T21:22:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/692/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/704/898 [1]</TD>
            <TD>Photometry of the Hercules dwarf galaxy (Sand+, 2009)</TD>
            <TD>Observations of Hercules were, with one exception, taken during 2008 May and June during normal operations of the Large Binocular Telescope (LBT), fitted with the red and blue channels of the Large Binocular Camera. The B- and V-band images for the central Hercules field were taken during Science Demonstration Time (SDT) and were presented in Coleman et al. (2007ApJ...668L..43C). When necessary, we adopted SDSS-DR6 photometry directly for stars brighter than and near the saturation limit of a given LBT field (which depends both on the observing conditions and point spread function). In this case, g and r magnitudes are converted to B magnitudes via the relations found by Jordi et al. (2006A&amp;A...460..339J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898#1</TD>
            <TD>2011-12-26T21:12:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/704/898</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/898</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/704/898 [2]</TD>
            <TD>Photometry of the Hercules dwarf galaxy (Sand+, 2009)</TD>
            <TD>Observations of Hercules were, with one exception, taken during 2008 May and June during normal operations of the Large Binocular Telescope (LBT), fitted with the red and blue channels of the Large Binocular Camera. The B- and V-band images for the central Hercules field were taken during Science Demonstration Time (SDT) and were presented in Coleman et al. (2007ApJ...668L..43C). When necessary, we adopted SDSS-DR6 photometry directly for stars brighter than and near the saturation limit of a given LBT field (which depends both on the observing conditions and point spread function). In this case, g and r magnitudes are converted to B magnitudes via the relations found by Jordi et al. (2006A&amp;A...460..339J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898#2</TD>
            <TD>2011-12-26T21:12:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/704/898&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/898</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/704/898 [catalog]</TD>
            <TD>Photometry of the Hercules dwarf galaxy (Sand+, 2009)</TD>
            <TD>Observations of Hercules were, with one exception, taken during 2008 May and June during normal operations of the Large Binocular Telescope (LBT), fitted with the red and blue channels of the Large Binocular Camera. The B- and V-band images for the central Hercules field were taken during Science Demonstration Time (SDT) and were presented in Coleman et al. (2007ApJ...668L..43C). When necessary, we adopted SDSS-DR6 photometry directly for stars brighter than and near the saturation limit of a given LBT field (which depends both on the observing conditions and point spread function). In this case, g and r magnitudes are converted to B magnitudes via the relations found by Jordi et al. (2006A&amp;A...460..339J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898#catalog</TD>
            <TD>2011-12-26T21:12:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/704/898&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/898</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ESO/Uppsala [1]</TD>
            <TD>ESO-Uppsala ESO(B) Survey</TD>
            <TD>This database table was derived from information provided in "The ESO/Uppsala Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a passband similar to the Johnson B color. Additional information is available from the HEASARC.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/esouppsala#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/esouppsala</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=esouppsala&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/esouppsala.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ESO/Uppsala [2]</TD>
            <TD>ESO-Uppsala ESO(B) Survey</TD>
            <TD>This database table was derived from information provided in "The ESO/Uppsala Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a passband similar to the Johnson B color. Additional information is available from the HEASARC.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/esouppsala#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/esouppsala</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=esouppsala&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/esouppsala.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ESO/Uppsala [3]</TD>
            <TD>ESO-Uppsala ESO(B) Survey</TD>
            <TD>This database table was derived from information provided in "The ESO/Uppsala Survey of the ESO(B) Atlas" (ESO/U), which is a joint project undertaken by the European Southern Observatory (ESO) and the Uppsala Observatory to provide a systematic and homogeneous search of the ESO(B) Atlas (also known as the Quick Blue Survey). The ESO(B) Atlas, taken with the ESO 1 m Schmidt telescope at La Silla, Chile, covers 606 fields from -90 to -20 degrees of declination. The fields are similar in size and scale to those of the Palomar Observatory Sky Survey. Unsensitized IIa-O plates and a 2 mm GG385 filter were used to give a passband similar to the Johnson B color. Additional information is available from the HEASARC.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/esouppsala#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/esouppsala</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_esouppsala&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/esouppsala.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/704/898 [1]</TD>
            <TD>Photometry of the Hercules dwarf galaxy (Sand+, 2009)</TD>
            <TD>Observations of Hercules were, with one exception, taken during 2008 May and June during normal operations of the Large Binocular Telescope (LBT), fitted with the red and blue channels of the Large Binocular Camera. The B- and V-band images for the central Hercules field were taken during Science Demonstration Time (SDT) and were presented in Coleman et al. (2007ApJ...668L..43C). When necessary, we adopted SDSS-DR6 photometry directly for stars brighter than and near the saturation limit of a given LBT field (which depends both on the observing conditions and point spread function). In this case, g and r magnitudes are converted to B magnitudes via the relations found by Jordi et al. (2006A&amp;A...460..339J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898#1</TD>
            <TD>2011-12-26T21:12:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/704/898</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/898</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/704/898 [2]</TD>
            <TD>Photometry of the Hercules dwarf galaxy (Sand+, 2009)</TD>
            <TD>Observations of Hercules were, with one exception, taken during 2008 May and June during normal operations of the Large Binocular Telescope (LBT), fitted with the red and blue channels of the Large Binocular Camera. The B- and V-band images for the central Hercules field were taken during Science Demonstration Time (SDT) and were presented in Coleman et al. (2007ApJ...668L..43C). When necessary, we adopted SDSS-DR6 photometry directly for stars brighter than and near the saturation limit of a given LBT field (which depends both on the observing conditions and point spread function). In this case, g and r magnitudes are converted to B magnitudes via the relations found by Jordi et al. (2006A&amp;A...460..339J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898#2</TD>
            <TD>2011-12-26T21:12:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/704/898&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/898</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/704/898 [catalog]</TD>
            <TD>Photometry of the Hercules dwarf galaxy (Sand+, 2009)</TD>
            <TD>Observations of Hercules were, with one exception, taken during 2008 May and June during normal operations of the Large Binocular Telescope (LBT), fitted with the red and blue channels of the Large Binocular Camera. The B- and V-band images for the central Hercules field were taken during Science Demonstration Time (SDT) and were presented in Coleman et al. (2007ApJ...668L..43C). When necessary, we adopted SDSS-DR6 photometry directly for stars brighter than and near the saturation limit of a given LBT field (which depends both on the observing conditions and point spread function). In this case, g and r magnitudes are converted to B magnitudes via the relations found by Jordi et al. (2006A&amp;A...460..339J).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898#catalog</TD>
            <TD>2011-12-26T21:12:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/704/898</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/704/898&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/704/898</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>FAUST [1]</TD>
            <TD>Faust Far-UV Point Source Catalog</TD>
            <TD>This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14 ergs/s/cm^2/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/faust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0666666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/faust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=faust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/faust/faust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>FAUST [2]</TD>
            <TD>Faust Far-UV Point Source Catalog</TD>
            <TD>This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14 ergs/s/cm^2/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/faust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0666666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/faust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=faust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/faust/faust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>FAUST [3]</TD>
            <TD>Faust Far-UV Point Source Catalog</TD>
            <TD>This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14 ergs/s/cm^2/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/faust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0666666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/faust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_faust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/faust/faust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/692/511 [1]</TD>
            <TD>Mergers of luminous early-type galaxies (Wen+, 2009)</TD>
            <TD>Supermassive black hole (SMBH) coalescence in galaxy mergers is believed to be one of the primary sources of very low frequency gravitational waves (GWs). Significant contribution of the GWs comes from mergers of massive galaxies with redshifts z&lt;2. Very few previous studies gave the merger rate of massive galaxies. We selected a large sample (1209) of close pairs of galaxies with projected separations 7&lt;r_p_&lt;50kpc from 87889 luminous early-type galaxies (M_r_&lt;-21.5) from the Sloan Digital Sky Survey Data Release 6. These pairs constitute a complete volume-limited sample in the local universe (z&lt;0.12). Using our newly developed technique, 249 mergers have been identified by searching for interaction features. From them, we found that the merger fraction of luminous early-type galaxies is 0.8%, and the merger rate in the local universe is Rg~(1.0+/-0.4)x10^-5^Mpc^-3^/Gyr with an uncertainty mainly depending on the merging timescale.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511#1</TD>
            <TD>2011-09-14T21:22:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/692/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/692/511 [2]</TD>
            <TD>Mergers of luminous early-type galaxies (Wen+, 2009)</TD>
            <TD>Supermassive black hole (SMBH) coalescence in galaxy mergers is believed to be one of the primary sources of very low frequency gravitational waves (GWs). Significant contribution of the GWs comes from mergers of massive galaxies with redshifts z&lt;2. Very few previous studies gave the merger rate of massive galaxies. We selected a large sample (1209) of close pairs of galaxies with projected separations 7&lt;r_p_&lt;50kpc from 87889 luminous early-type galaxies (M_r_&lt;-21.5) from the Sloan Digital Sky Survey Data Release 6. These pairs constitute a complete volume-limited sample in the local universe (z&lt;0.12). Using our newly developed technique, 249 mergers have been identified by searching for interaction features. From them, we found that the merger fraction of luminous early-type galaxies is 0.8%, and the merger rate in the local universe is Rg~(1.0+/-0.4)x10^-5^Mpc^-3^/Gyr with an uncertainty mainly depending on the merging timescale.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511#2</TD>
            <TD>2011-09-14T21:22:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/692/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/692/511 [table1]</TD>
            <TD>Mergers of luminous early-type galaxies (Wen+, 2009)</TD>
            <TD>Supermassive black hole (SMBH) coalescence in galaxy mergers is believed to be one of the primary sources of very low frequency gravitational waves (GWs). Significant contribution of the GWs comes from mergers of massive galaxies with redshifts z&lt;2. Very few previous studies gave the merger rate of massive galaxies. We selected a large sample (1209) of close pairs of galaxies with projected separations 7&lt;r_p_&lt;50kpc from 87889 luminous early-type galaxies (M_r_&lt;-21.5) from the Sloan Digital Sky Survey Data Release 6. These pairs constitute a complete volume-limited sample in the local universe (z&lt;0.12). Using our newly developed technique, 249 mergers have been identified by searching for interaction features. From them, we found that the merger fraction of luminous early-type galaxies is 0.8%, and the merger rate in the local universe is Rg~(1.0+/-0.4)x10^-5^Mpc^-3^/Gyr with an uncertainty mainly depending on the merging timescale.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511#table1</TD>
            <TD>2011-09-14T21:22:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/692/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/1145 [1]</TD>
            <TD>Galaxy clusters in the COSMOS field (Bellagamba+, 2011)</TD>
            <TD>Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal-to-noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi-band approach which could include not only additional optical bands but also observables with different nature such as X-rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo-z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3{sigma} level including both optical and weak-lensing information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145#1</TD>
            <TD>2012-01-19T16:06:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/1145</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1145</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/1145 [2]</TD>
            <TD>Galaxy clusters in the COSMOS field (Bellagamba+, 2011)</TD>
            <TD>Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal-to-noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi-band approach which could include not only additional optical bands but also observables with different nature such as X-rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo-z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3{sigma} level including both optical and weak-lensing information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145#2</TD>
            <TD>2012-01-19T16:06:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/1145&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1145</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/1145 [tables]</TD>
            <TD>Galaxy clusters in the COSMOS field (Bellagamba+, 2011)</TD>
            <TD>Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal-to-noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi-band approach which could include not only additional optical bands but also observables with different nature such as X-rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo-z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3{sigma} level including both optical and weak-lensing information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145#tables</TD>
            <TD>2012-01-19T16:06:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/1145&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1145</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>FAUST [1]</TD>
            <TD>Faust Far-UV Point Source Catalog</TD>
            <TD>This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14 ergs/s/cm^2/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/faust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0666666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/faust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=faust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/faust/faust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>FAUST [2]</TD>
            <TD>Faust Far-UV Point Source Catalog</TD>
            <TD>This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14 ergs/s/cm^2/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/faust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0666666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/faust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=faust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/faust/faust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>FAUST [3]</TD>
            <TD>Faust Far-UV Point Source Catalog</TD>
            <TD>This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14 ergs/s/cm^2/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/faust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0666666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/faust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_faust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/faust/faust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/1145 [1]</TD>
            <TD>Galaxy clusters in the COSMOS field (Bellagamba+, 2011)</TD>
            <TD>Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal-to-noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi-band approach which could include not only additional optical bands but also observables with different nature such as X-rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo-z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3{sigma} level including both optical and weak-lensing information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145#1</TD>
            <TD>2012-01-19T16:06:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/1145</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1145</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/1145 [2]</TD>
            <TD>Galaxy clusters in the COSMOS field (Bellagamba+, 2011)</TD>
            <TD>Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal-to-noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi-band approach which could include not only additional optical bands but also observables with different nature such as X-rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo-z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3{sigma} level including both optical and weak-lensing information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145#2</TD>
            <TD>2012-01-19T16:06:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/1145&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1145</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/1145 [tables]</TD>
            <TD>Galaxy clusters in the COSMOS field (Bellagamba+, 2011)</TD>
            <TD>Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal-to-noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi-band approach which could include not only additional optical bands but also observables with different nature such as X-rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo-z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3{sigma} level including both optical and weak-lensing information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145#tables</TD>
            <TD>2012-01-19T16:06:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/1145&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1145</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/692/511 [1]</TD>
            <TD>Mergers of luminous early-type galaxies (Wen+, 2009)</TD>
            <TD>Supermassive black hole (SMBH) coalescence in galaxy mergers is believed to be one of the primary sources of very low frequency gravitational waves (GWs). Significant contribution of the GWs comes from mergers of massive galaxies with redshifts z&lt;2. Very few previous studies gave the merger rate of massive galaxies. We selected a large sample (1209) of close pairs of galaxies with projected separations 7&lt;r_p_&lt;50kpc from 87889 luminous early-type galaxies (M_r_&lt;-21.5) from the Sloan Digital Sky Survey Data Release 6. These pairs constitute a complete volume-limited sample in the local universe (z&lt;0.12). Using our newly developed technique, 249 mergers have been identified by searching for interaction features. From them, we found that the merger fraction of luminous early-type galaxies is 0.8%, and the merger rate in the local universe is Rg~(1.0+/-0.4)x10^-5^Mpc^-3^/Gyr with an uncertainty mainly depending on the merging timescale.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511#1</TD>
            <TD>2011-09-14T21:22:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/692/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/692/511 [2]</TD>
            <TD>Mergers of luminous early-type galaxies (Wen+, 2009)</TD>
            <TD>Supermassive black hole (SMBH) coalescence in galaxy mergers is believed to be one of the primary sources of very low frequency gravitational waves (GWs). Significant contribution of the GWs comes from mergers of massive galaxies with redshifts z&lt;2. Very few previous studies gave the merger rate of massive galaxies. We selected a large sample (1209) of close pairs of galaxies with projected separations 7&lt;r_p_&lt;50kpc from 87889 luminous early-type galaxies (M_r_&lt;-21.5) from the Sloan Digital Sky Survey Data Release 6. These pairs constitute a complete volume-limited sample in the local universe (z&lt;0.12). Using our newly developed technique, 249 mergers have been identified by searching for interaction features. From them, we found that the merger fraction of luminous early-type galaxies is 0.8%, and the merger rate in the local universe is Rg~(1.0+/-0.4)x10^-5^Mpc^-3^/Gyr with an uncertainty mainly depending on the merging timescale.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511#2</TD>
            <TD>2011-09-14T21:22:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/692/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/692/511 [table1]</TD>
            <TD>Mergers of luminous early-type galaxies (Wen+, 2009)</TD>
            <TD>Supermassive black hole (SMBH) coalescence in galaxy mergers is believed to be one of the primary sources of very low frequency gravitational waves (GWs). Significant contribution of the GWs comes from mergers of massive galaxies with redshifts z&lt;2. Very few previous studies gave the merger rate of massive galaxies. We selected a large sample (1209) of close pairs of galaxies with projected separations 7&lt;r_p_&lt;50kpc from 87889 luminous early-type galaxies (M_r_&lt;-21.5) from the Sloan Digital Sky Survey Data Release 6. These pairs constitute a complete volume-limited sample in the local universe (z&lt;0.12). Using our newly developed technique, 249 mergers have been identified by searching for interaction features. From them, we found that the merger fraction of luminous early-type galaxies is 0.8%, and the merger rate in the local universe is Rg~(1.0+/-0.4)x10^-5^Mpc^-3^/Gyr with an uncertainty mainly depending on the merging timescale.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511#table1</TD>
            <TD>2011-09-14T21:22:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/692/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>FAUST [1]</TD>
            <TD>Faust Far-UV Point Source Catalog</TD>
            <TD>This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14 ergs/s/cm^2/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/faust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0666666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/faust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=faust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/faust/faust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>FAUST [2]</TD>
            <TD>Faust Far-UV Point Source Catalog</TD>
            <TD>This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14 ergs/s/cm^2/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/faust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0666666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/faust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=faust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/faust/faust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>FAUST [3]</TD>
            <TD>Faust Far-UV Point Source Catalog</TD>
            <TD>This catalog contains a list of the photometric measurements of point sources made by the Far Ultraviolet Space Telescope (FAUST) when it flew on the ATLAS-1 space shuttle mission. The list contains 4660 galactic and extragalactic objects detected in 22 wide-field images of the sky (note that the abstract of the published catalog states that it contains 4698 sources: the reason for this discrepancy is not known to the HEASARC). At the locations surveyed, this catalog reaches a limiting magnitude that is approximately a factor of 10 fainter than the previous UV all-sky survey, TD1. The catalog limit is approximately 1x10^-14 ergs/s/cm^2/Angstrom, although it is not complete to this level. Listed for each object is the position, Far-UV (FUV) flux, the error in this flux, and, where possible, an identification from catalogs of nearby stars and galaxies. These catalogs include the Michigan HD (MHD) and HD Catalogs, the SAO Catalog, the HIPPARCOS Input Catalog (HIC), the Position and Proper Motion (PPM) Catalog, the TD1 Catalog, the McCook and Sion Catalog of white dwarf stars, and the RC3 Catalog of Galaxies. 2239 FAUST sources are identified with objects in the stellar catalogs and 172 with galaxies in the RC3 catalog. The number of sources with incorrect identifications is estimated to be less than 2%. Of the 4660 FUV sources in this catalog, 161 have multiple stellar and/or galaxy counterparts (155 sources have 2 possible counterparts, 4 sources have 3 possible counterparts, 1 source has 4 possible counterparts, and 1 source has 6 possible counterparts), with the 4499 remaining FUV sources having 0 or 1 stellar and/or galaxy counterparts. Hence, there are a grand total of 4831 = (4499 + 155x2 + 4x3 + 1x4 + 1x6) entries in this database, since each entry corresponds to a source/counterpart combination. The HEASARC added a parameter 'multiple_ID' to allow the user to identify sources with multiple possible counterparts. FAUST Sources with multiple counterparts thus have multiple entries in this database, and can be recognized by having multiple_id values greater than 1 (and differing information in the parameter fields that contain the properties of the stellar and/or galaxy counterparts).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/faust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0666666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/faust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_faust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/faust/faust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/1145 [1]</TD>
            <TD>Galaxy clusters in the COSMOS field (Bellagamba+, 2011)</TD>
            <TD>Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal-to-noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi-band approach which could include not only additional optical bands but also observables with different nature such as X-rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo-z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3{sigma} level including both optical and weak-lensing information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145#1</TD>
            <TD>2012-01-19T16:06:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/1145</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1145</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/1145 [2]</TD>
            <TD>Galaxy clusters in the COSMOS field (Bellagamba+, 2011)</TD>
            <TD>Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal-to-noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi-band approach which could include not only additional optical bands but also observables with different nature such as X-rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo-z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3{sigma} level including both optical and weak-lensing information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145#2</TD>
            <TD>2012-01-19T16:06:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/1145&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1145</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/1145 [tables]</TD>
            <TD>Galaxy clusters in the COSMOS field (Bellagamba+, 2011)</TD>
            <TD>Galaxy clusters are usually detected in blind optical surveys via suitable filtering methods. We present an optimal matched filter which maximizes their signal-to-noise ratio by taking advantage of the knowledge we have of their intrinsic physical properties and of the data noise properties. In this paper we restrict our application to galaxy magnitudes, positions and photometric redshifts if available, and we also apply the filter separately to weak lensing data. The method is suitable to be naturally extended to a multi-band approach which could include not only additional optical bands but also observables with different nature such as X-rays. For each detection, the filter provides its significance, an estimate for the richness and for the redshift even if photo-z are not given. The provided analytical error estimate is tested against numerical simulations. We finally apply our method to the COSMOS field and compare the results with previous cluster detections obtained with different methods. Our catalogue contains 27 galaxy clusters with minimal threshold at 3{sigma} level including both optical and weak-lensing information.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145#tables</TD>
            <TD>2012-01-19T16:06:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1145</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/1145&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1145</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/396/818 [1]</TD>
            <TD>Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)</TD>
            <TD>We report the discovery of a population of nearby, blue early-type galaxies with high star formation rates (0.5&lt;SFR&lt;50M_{sun}_/yr). They are identified by their visual morphology as provided by Galaxy Zoo for Sloan Digital Sky Survey Data Release 6 and their u-r colour. We select a volume-limited sample in the redshift range 0.02&lt;z&lt;0.05, corresponding to luminosities of approximately L* and above and with u-r colours significantly bluer than the red sequence. We confirm the early-type morphology of the objects in this sample and investigate their environmental dependence and star formation properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818#1</TD>
            <TD>2011-10-04T09:56:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/396/818</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/396/818</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/396/818 [2]</TD>
            <TD>Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)</TD>
            <TD>We report the discovery of a population of nearby, blue early-type galaxies with high star formation rates (0.5&lt;SFR&lt;50M_{sun}_/yr). They are identified by their visual morphology as provided by Galaxy Zoo for Sloan Digital Sky Survey Data Release 6 and their u-r colour. We select a volume-limited sample in the redshift range 0.02&lt;z&lt;0.05, corresponding to luminosities of approximately L* and above and with u-r colours significantly bluer than the red sequence. We confirm the early-type morphology of the objects in this sample and investigate their environmental dependence and star formation properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818#2</TD>
            <TD>2011-10-04T09:56:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/396/818&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/396/818</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/396/818 [table2]</TD>
            <TD>Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)</TD>
            <TD>We report the discovery of a population of nearby, blue early-type galaxies with high star formation rates (0.5&lt;SFR&lt;50M_{sun}_/yr). They are identified by their visual morphology as provided by Galaxy Zoo for Sloan Digital Sky Survey Data Release 6 and their u-r colour. We select a volume-limited sample in the redshift range 0.02&lt;z&lt;0.05, corresponding to luminosities of approximately L* and above and with u-r colours significantly bluer than the red sequence. We confirm the early-type morphology of the objects in this sample and investigate their environmental dependence and star formation properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818#table2</TD>
            <TD>2011-10-04T09:56:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/396/818&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/396/818</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/419/2095 [1]</TD>
            <TD>HMXBs in nearby galaxies (Mineo+, 2012)</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, LX~~2.6x10^39^SFR. However, the scaling relations still bear a rather large dispersion of rms~0.4dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the D25 ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(LX)~35-40 luminosity range with a moderately significant evidence for a break or cut-off at LX~10^40^erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fX~0.2x(0.1Myr/{tau}x) ({tau}x is the life time of the X-ray active phase). This is about 4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095#1</TD>
            <TD>2012-01-05T20:41:05Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/419/2095</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/419/2095</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/419/2095 [2]</TD>
            <TD>HMXBs in nearby galaxies (Mineo+, 2012)</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, LX~~2.6x10^39^SFR. However, the scaling relations still bear a rather large dispersion of rms~0.4dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the D25 ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(LX)~35-40 luminosity range with a moderately significant evidence for a break or cut-off at LX~10^40^erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fX~0.2x(0.1Myr/{tau}x) ({tau}x is the life time of the X-ray active phase). This is about 4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095#2</TD>
            <TD>2012-01-05T20:41:05Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/419/2095&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/419/2095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/419/2095 [hmxb]</TD>
            <TD>HMXBs in nearby galaxies (Mineo+, 2012)</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, LX~~2.6x10^39^SFR. However, the scaling relations still bear a rather large dispersion of rms~0.4dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the D25 ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(LX)~35-40 luminosity range with a moderately significant evidence for a break or cut-off at LX~10^40^erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fX~0.2x(0.1Myr/{tau}x) ({tau}x is the life time of the X-ray active phase). This is about 4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095#hmxb</TD>
            <TD>2012-01-05T20:41:05Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/419/2095&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/419/2095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>INTIBISASS [1]</TD>
            <TD>INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources</TD>
            <TD>The INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources table contains the results from a paper which is the second in a series devoted to the hard X-ray (17 - 60 keV) whole sky survey which has been performed by the INTEGRAL observatory over its first seven years of observations. This table contains the catalog of detected sources and includes 521 objects, 449 of which exceed a 5-sigma detection threshold on the time-averaged map of the sky, and 53 which were detected in various subsamples of exposures. Among the identified sources with known and suspected natures, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b| &gt; 5 degrees) and Galactic (|b| &lt; 5 degrees) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies. The current INTIBISASS table is based on the data provided in Krivonos et al. (2010: Paper II below) and replaces the earlier version available at the HEASARC from February 2008 to December 2010 which was based on Krivonos et al. (2007).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://nasa.heasarc/intibisass#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisass</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=intibisass&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisass.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>INTIBISASS [2]</TD>
            <TD>INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources</TD>
            <TD>The INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources table contains the results from a paper which is the second in a series devoted to the hard X-ray (17 - 60 keV) whole sky survey which has been performed by the INTEGRAL observatory over its first seven years of observations. This table contains the catalog of detected sources and includes 521 objects, 449 of which exceed a 5-sigma detection threshold on the time-averaged map of the sky, and 53 which were detected in various subsamples of exposures. Among the identified sources with known and suspected natures, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b| &gt; 5 degrees) and Galactic (|b| &lt; 5 degrees) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies. The current INTIBISASS table is based on the data provided in Krivonos et al. (2010: Paper II below) and replaces the earlier version available at the HEASARC from February 2008 to December 2010 which was based on Krivonos et al. (2007).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://nasa.heasarc/intibisass#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisass</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=intibisass&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisass.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>INTIBISASS [3]</TD>
            <TD>INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources</TD>
            <TD>The INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources table contains the results from a paper which is the second in a series devoted to the hard X-ray (17 - 60 keV) whole sky survey which has been performed by the INTEGRAL observatory over its first seven years of observations. This table contains the catalog of detected sources and includes 521 objects, 449 of which exceed a 5-sigma detection threshold on the time-averaged map of the sky, and 53 which were detected in various subsamples of exposures. Among the identified sources with known and suspected natures, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b| &gt; 5 degrees) and Galactic (|b| &lt; 5 degrees) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies. The current INTIBISASS table is based on the data provided in Krivonos et al. (2010: Paper II below) and replaces the earlier version available at the HEASARC from February 2008 to December 2010 which was based on Krivonos et al. (2007).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://nasa.heasarc/intibisass#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_intibisass&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisass.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/419/2095 [1]</TD>
            <TD>HMXBs in nearby galaxies (Mineo+, 2012)</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, LX~~2.6x10^39^SFR. However, the scaling relations still bear a rather large dispersion of rms~0.4dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the D25 ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(LX)~35-40 luminosity range with a moderately significant evidence for a break or cut-off at LX~10^40^erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fX~0.2x(0.1Myr/{tau}x) ({tau}x is the life time of the X-ray active phase). This is about 4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095#1</TD>
            <TD>2012-01-05T20:41:05Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/419/2095</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/419/2095</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/419/2095 [2]</TD>
            <TD>HMXBs in nearby galaxies (Mineo+, 2012)</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, LX~~2.6x10^39^SFR. However, the scaling relations still bear a rather large dispersion of rms~0.4dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the D25 ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(LX)~35-40 luminosity range with a moderately significant evidence for a break or cut-off at LX~10^40^erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fX~0.2x(0.1Myr/{tau}x) ({tau}x is the life time of the X-ray active phase). This is about 4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095#2</TD>
            <TD>2012-01-05T20:41:05Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/419/2095&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/419/2095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/419/2095 [hmxb]</TD>
            <TD>HMXBs in nearby galaxies (Mineo+, 2012)</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, LX~~2.6x10^39^SFR. However, the scaling relations still bear a rather large dispersion of rms~0.4dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the D25 ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(LX)~35-40 luminosity range with a moderately significant evidence for a break or cut-off at LX~10^40^erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fX~0.2x(0.1Myr/{tau}x) ({tau}x is the life time of the X-ray active phase). This is about 4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095#hmxb</TD>
            <TD>2012-01-05T20:41:05Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/419/2095&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/419/2095</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/396/818 [1]</TD>
            <TD>Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)</TD>
            <TD>We report the discovery of a population of nearby, blue early-type galaxies with high star formation rates (0.5&lt;SFR&lt;50M_{sun}_/yr). They are identified by their visual morphology as provided by Galaxy Zoo for Sloan Digital Sky Survey Data Release 6 and their u-r colour. We select a volume-limited sample in the redshift range 0.02&lt;z&lt;0.05, corresponding to luminosities of approximately L* and above and with u-r colours significantly bluer than the red sequence. We confirm the early-type morphology of the objects in this sample and investigate their environmental dependence and star formation properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818#1</TD>
            <TD>2011-10-04T09:56:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/396/818</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/396/818</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/396/818 [2]</TD>
            <TD>Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)</TD>
            <TD>We report the discovery of a population of nearby, blue early-type galaxies with high star formation rates (0.5&lt;SFR&lt;50M_{sun}_/yr). They are identified by their visual morphology as provided by Galaxy Zoo for Sloan Digital Sky Survey Data Release 6 and their u-r colour. We select a volume-limited sample in the redshift range 0.02&lt;z&lt;0.05, corresponding to luminosities of approximately L* and above and with u-r colours significantly bluer than the red sequence. We confirm the early-type morphology of the objects in this sample and investigate their environmental dependence and star formation properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818#2</TD>
            <TD>2011-10-04T09:56:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/396/818&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/396/818</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/396/818 [table2]</TD>
            <TD>Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)</TD>
            <TD>We report the discovery of a population of nearby, blue early-type galaxies with high star formation rates (0.5&lt;SFR&lt;50M_{sun}_/yr). They are identified by their visual morphology as provided by Galaxy Zoo for Sloan Digital Sky Survey Data Release 6 and their u-r colour. We select a volume-limited sample in the redshift range 0.02&lt;z&lt;0.05, corresponding to luminosities of approximately L* and above and with u-r colours significantly bluer than the red sequence. We confirm the early-type morphology of the objects in this sample and investigate their environmental dependence and star formation properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818#table2</TD>
            <TD>2011-10-04T09:56:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/396/818&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/396/818</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/419/2095 [1]</TD>
            <TD>HMXBs in nearby galaxies (Mineo+, 2012)</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, LX~~2.6x10^39^SFR. However, the scaling relations still bear a rather large dispersion of rms~0.4dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the D25 ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(LX)~35-40 luminosity range with a moderately significant evidence for a break or cut-off at LX~10^40^erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fX~0.2x(0.1Myr/{tau}x) ({tau}x is the life time of the X-ray active phase). This is about 4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095#1</TD>
            <TD>2012-01-05T20:41:05Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/419/2095</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/419/2095</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/419/2095 [2]</TD>
            <TD>HMXBs in nearby galaxies (Mineo+, 2012)</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, LX~~2.6x10^39^SFR. However, the scaling relations still bear a rather large dispersion of rms~0.4dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the D25 ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(LX)~35-40 luminosity range with a moderately significant evidence for a break or cut-off at LX~10^40^erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fX~0.2x(0.1Myr/{tau}x) ({tau}x is the life time of the X-ray active phase). This is about 4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095#2</TD>
            <TD>2012-01-05T20:41:05Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/419/2095&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/419/2095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/419/2095 [hmxb]</TD>
            <TD>HMXBs in nearby galaxies (Mineo+, 2012)</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, we study populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, we find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, LX~~2.6x10^39^SFR. However, the scaling relations still bear a rather large dispersion of rms~0.4dex, which we believe is of a physical origin. We present the catalog of 1057 X-ray sources detected within the D25 ellipse for galaxies of our sample and construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(LX)~35-40 luminosity range with a moderately significant evidence for a break or cut-off at LX~10^40^erg/s. As before, we did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. We discuss implications of our results for the theory of binary evolution. In particular we estimate the fraction of compact objects that once upon their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, fX~0.2x(0.1Myr/{tau}x) ({tau}x is the life time of the X-ray active phase). This is about 4 orders of magnitude more frequent than in LMXBs. We also derive constrains on the mass distribution of the secondary star in HMXBs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095#hmxb</TD>
            <TD>2012-01-05T20:41:05Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/419/2095</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/419/2095&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/419/2095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>INTIBISASS [1]</TD>
            <TD>INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources</TD>
            <TD>The INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources table contains the results from a paper which is the second in a series devoted to the hard X-ray (17 - 60 keV) whole sky survey which has been performed by the INTEGRAL observatory over its first seven years of observations. This table contains the catalog of detected sources and includes 521 objects, 449 of which exceed a 5-sigma detection threshold on the time-averaged map of the sky, and 53 which were detected in various subsamples of exposures. Among the identified sources with known and suspected natures, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b| &gt; 5 degrees) and Galactic (|b| &lt; 5 degrees) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies. The current INTIBISASS table is based on the data provided in Krivonos et al. (2010: Paper II below) and replaces the earlier version available at the HEASARC from February 2008 to December 2010 which was based on Krivonos et al. (2007).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://nasa.heasarc/intibisass#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisass</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=intibisass&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisass.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>INTIBISASS [2]</TD>
            <TD>INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources</TD>
            <TD>The INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources table contains the results from a paper which is the second in a series devoted to the hard X-ray (17 - 60 keV) whole sky survey which has been performed by the INTEGRAL observatory over its first seven years of observations. This table contains the catalog of detected sources and includes 521 objects, 449 of which exceed a 5-sigma detection threshold on the time-averaged map of the sky, and 53 which were detected in various subsamples of exposures. Among the identified sources with known and suspected natures, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b| &gt; 5 degrees) and Galactic (|b| &lt; 5 degrees) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies. The current INTIBISASS table is based on the data provided in Krivonos et al. (2010: Paper II below) and replaces the earlier version available at the HEASARC from February 2008 to December 2010 which was based on Krivonos et al. (2007).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://nasa.heasarc/intibisass#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisass</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=intibisass&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisass.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>INTIBISASS [3]</TD>
            <TD>INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources</TD>
            <TD>The INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources table contains the results from a paper which is the second in a series devoted to the hard X-ray (17 - 60 keV) whole sky survey which has been performed by the INTEGRAL observatory over its first seven years of observations. This table contains the catalog of detected sources and includes 521 objects, 449 of which exceed a 5-sigma detection threshold on the time-averaged map of the sky, and 53 which were detected in various subsamples of exposures. Among the identified sources with known and suspected natures, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b| &gt; 5 degrees) and Galactic (|b| &lt; 5 degrees) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies. The current INTIBISASS table is based on the data provided in Krivonos et al. (2010: Paper II below) and replaces the earlier version available at the HEASARC from February 2008 to December 2010 which was based on Krivonos et al. (2007).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://nasa.heasarc/intibisass#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisass</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_intibisass&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisass.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/396/818 [1]</TD>
            <TD>Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)</TD>
            <TD>We report the discovery of a population of nearby, blue early-type galaxies with high star formation rates (0.5&lt;SFR&lt;50M_{sun}_/yr). They are identified by their visual morphology as provided by Galaxy Zoo for Sloan Digital Sky Survey Data Release 6 and their u-r colour. We select a volume-limited sample in the redshift range 0.02&lt;z&lt;0.05, corresponding to luminosities of approximately L* and above and with u-r colours significantly bluer than the red sequence. We confirm the early-type morphology of the objects in this sample and investigate their environmental dependence and star formation properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818#1</TD>
            <TD>2011-10-04T09:56:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/396/818</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/396/818</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/396/818 [2]</TD>
            <TD>Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)</TD>
            <TD>We report the discovery of a population of nearby, blue early-type galaxies with high star formation rates (0.5&lt;SFR&lt;50M_{sun}_/yr). They are identified by their visual morphology as provided by Galaxy Zoo for Sloan Digital Sky Survey Data Release 6 and their u-r colour. We select a volume-limited sample in the redshift range 0.02&lt;z&lt;0.05, corresponding to luminosities of approximately L* and above and with u-r colours significantly bluer than the red sequence. We confirm the early-type morphology of the objects in this sample and investigate their environmental dependence and star formation properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818#2</TD>
            <TD>2011-10-04T09:56:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/396/818&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/396/818</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/396/818 [table2]</TD>
            <TD>Blue early-type galaxies in Galaxy Zoo (Schawinski+, 2009)</TD>
            <TD>We report the discovery of a population of nearby, blue early-type galaxies with high star formation rates (0.5&lt;SFR&lt;50M_{sun}_/yr). They are identified by their visual morphology as provided by Galaxy Zoo for Sloan Digital Sky Survey Data Release 6 and their u-r colour. We select a volume-limited sample in the redshift range 0.02&lt;z&lt;0.05, corresponding to luminosities of approximately L* and above and with u-r colours significantly bluer than the red sequence. We confirm the early-type morphology of the objects in this sample and investigate their environmental dependence and star formation properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818#table2</TD>
            <TD>2011-10-04T09:56:22Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/396/818</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/396/818&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/396/818</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/196/11 [1]</TD>
            <TD>Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)</TD>
            <TD>We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1123718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1mag down to bulge and disk magnitudes of g~19 and r~18.5. We also use and compare three different galaxy fitting models: a pure Sersic model, an n_b_=4 bulge+disk model, and a Sersic (free n_b_) bulge+disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11#1</TD>
            <TD>2012-01-06T04:10:10Z</TD>
            <TD>#Galaxies#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/196/11</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/196/11</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/196/11 [2]</TD>
            <TD>Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)</TD>
            <TD>We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1123718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1mag down to bulge and disk magnitudes of g~19 and r~18.5. We also use and compare three different galaxy fitting models: a pure Sersic model, an n_b_=4 bulge+disk model, and a Sersic (free n_b_) bulge+disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11#2</TD>
            <TD>2012-01-06T04:10:10Z</TD>
            <TD>#Galaxies#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/196/11&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/196/11</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/196/11 [table1]</TD>
            <TD>Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)</TD>
            <TD>We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1123718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1mag down to bulge and disk magnitudes of g~19 and r~18.5. We also use and compare three different galaxy fitting models: a pure Sersic model, an n_b_=4 bulge+disk model, and a Sersic (free n_b_) bulge+disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11#table1</TD>
            <TD>2012-01-06T04:10:10Z</TD>
            <TD>#Galaxies#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/196/11&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/196/11</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>INTIBISASS [1]</TD>
            <TD>INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources</TD>
            <TD>The INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources table contains the results from a paper which is the second in a series devoted to the hard X-ray (17 - 60 keV) whole sky survey which has been performed by the INTEGRAL observatory over its first seven years of observations. This table contains the catalog of detected sources and includes 521 objects, 449 of which exceed a 5-sigma detection threshold on the time-averaged map of the sky, and 53 which were detected in various subsamples of exposures. Among the identified sources with known and suspected natures, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b| &gt; 5 degrees) and Galactic (|b| &lt; 5 degrees) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies. The current INTIBISASS table is based on the data provided in Krivonos et al. (2010: Paper II below) and replaces the earlier version available at the HEASARC from February 2008 to December 2010 which was based on Krivonos et al. (2007).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://nasa.heasarc/intibisass#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisass</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=intibisass&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisass.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>INTIBISASS [2]</TD>
            <TD>INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources</TD>
            <TD>The INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources table contains the results from a paper which is the second in a series devoted to the hard X-ray (17 - 60 keV) whole sky survey which has been performed by the INTEGRAL observatory over its first seven years of observations. This table contains the catalog of detected sources and includes 521 objects, 449 of which exceed a 5-sigma detection threshold on the time-averaged map of the sky, and 53 which were detected in various subsamples of exposures. Among the identified sources with known and suspected natures, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b| &gt; 5 degrees) and Galactic (|b| &lt; 5 degrees) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies. The current INTIBISASS table is based on the data provided in Krivonos et al. (2010: Paper II below) and replaces the earlier version available at the HEASARC from February 2008 to December 2010 which was based on Krivonos et al. (2007).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://nasa.heasarc/intibisass#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisass</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=intibisass&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisass.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>INTIBISASS [3]</TD>
            <TD>INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources</TD>
            <TD>The INTEGRAL IBIS All-Sky Survey of Hard X-Ray Sources table contains the results from a paper which is the second in a series devoted to the hard X-ray (17 - 60 keV) whole sky survey which has been performed by the INTEGRAL observatory over its first seven years of observations. This table contains the catalog of detected sources and includes 521 objects, 449 of which exceed a 5-sigma detection threshold on the time-averaged map of the sky, and 53 which were detected in various subsamples of exposures. Among the identified sources with known and suspected natures, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b| &gt; 5 degrees) and Galactic (|b| &lt; 5 degrees) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies. The current INTIBISASS table is based on the data provided in Krivonos et al. (2010: Paper II below) and replaces the earlier version available at the HEASARC from February 2008 to December 2010 which was based on Krivonos et al. (2007).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://nasa.heasarc/intibisass#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisass</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_intibisass&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisass.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/196/11 [1]</TD>
            <TD>Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)</TD>
            <TD>We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1123718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1mag down to bulge and disk magnitudes of g~19 and r~18.5. We also use and compare three different galaxy fitting models: a pure Sersic model, an n_b_=4 bulge+disk model, and a Sersic (free n_b_) bulge+disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11#1</TD>
            <TD>2012-01-06T04:10:10Z</TD>
            <TD>#Galaxies#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/196/11</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/196/11</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/196/11 [2]</TD>
            <TD>Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)</TD>
            <TD>We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1123718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1mag down to bulge and disk magnitudes of g~19 and r~18.5. We also use and compare three different galaxy fitting models: a pure Sersic model, an n_b_=4 bulge+disk model, and a Sersic (free n_b_) bulge+disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11#2</TD>
            <TD>2012-01-06T04:10:10Z</TD>
            <TD>#Galaxies#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/196/11&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/196/11</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/196/11 [table1]</TD>
            <TD>Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)</TD>
            <TD>We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1123718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1mag down to bulge and disk magnitudes of g~19 and r~18.5. We also use and compare three different galaxy fitting models: a pure Sersic model, an n_b_=4 bulge+disk model, and a Sersic (free n_b_) bulge+disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11#table1</TD>
            <TD>2012-01-06T04:10:10Z</TD>
            <TD>#Galaxies#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/196/11&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/196/11</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A90 [1]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#1</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A90</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A90 [2]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#2</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A90&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A90 [table1]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#table1</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A90&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A90 [table2]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#table2</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A90&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/196/11 [1]</TD>
            <TD>Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)</TD>
            <TD>We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1123718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1mag down to bulge and disk magnitudes of g~19 and r~18.5. We also use and compare three different galaxy fitting models: a pure Sersic model, an n_b_=4 bulge+disk model, and a Sersic (free n_b_) bulge+disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11#1</TD>
            <TD>2012-01-06T04:10:10Z</TD>
            <TD>#Galaxies#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/196/11</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/196/11</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/196/11 [2]</TD>
            <TD>Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)</TD>
            <TD>We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1123718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1mag down to bulge and disk magnitudes of g~19 and r~18.5. We also use and compare three different galaxy fitting models: a pure Sersic model, an n_b_=4 bulge+disk model, and a Sersic (free n_b_) bulge+disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11#2</TD>
            <TD>2012-01-06T04:10:10Z</TD>
            <TD>#Galaxies#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/196/11&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/196/11</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/196/11 [table1]</TD>
            <TD>Bulge+disk decompositions of SDSS galaxies (Simard+, 2011)</TD>
            <TD>We perform two-dimensional, point-spread-function-convolved, bulge+disk decompositions in the g and r bandpasses on a sample of 1123718 galaxies from the Legacy area of the Sloan Digital Sky Survey Data Release Seven. Four different decomposition procedures are investigated which make improvements to sky background determinations and object deblending over the standard SDSS procedures that lead to more robust structural parameters and integrated galaxy magnitudes and colors, especially in crowded environments. We use a set of science-based quality assurance metrics, namely, the disk luminosity-size relation, the galaxy color-magnitude diagram, and the galaxy central (fiber) colors to show the robustness of our structural parameters. The best procedure utilizes simultaneous, two-bandpass decompositions. Bulge and disk photometric errors remain below 0.1mag down to bulge and disk magnitudes of g~19 and r~18.5. We also use and compare three different galaxy fitting models: a pure Sersic model, an n_b_=4 bulge+disk model, and a Sersic (free n_b_) bulge+disk model. The most appropriate model for a given galaxy is determined by the F-test probability. All three catalogs of measured structural parameters, rest-frame magnitudes, and colors are publicly released here.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11#table1</TD>
            <TD>2012-01-06T04:10:10Z</TD>
            <TD>#Galaxies#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Nov-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/196/11</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/196/11&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/196/11</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRASZ [1]</TD>
            <TD>IRAS 1.2-Jy Redshift Survey</TD>
            <TD>This is The Redshift Survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in ApJ Supp 1995, 100, 69. The survey contains 9897 objects selected from the IRAS database according to the following criteria: &lt;pre&gt; F60 &gt; 1.2 Jy; F60^2 &gt; F12 f25; |b| &lt; 5; high source density flag at 60 microns not raised. &lt;/pre&gt; Thus, this database consists of both galaxies and Galaxian contaminants. The sample contains ~5320 galaxies, and 14 objects without identifications at the present time.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/iraszsurv#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iraszsurv</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=iraszsurv&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/iras/iraszsurv.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRASZ [2]</TD>
            <TD>IRAS 1.2-Jy Redshift Survey</TD>
            <TD>This is The Redshift Survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in ApJ Supp 1995, 100, 69. The survey contains 9897 objects selected from the IRAS database according to the following criteria: &lt;pre&gt; F60 &gt; 1.2 Jy; F60^2 &gt; F12 f25; |b| &lt; 5; high source density flag at 60 microns not raised. &lt;/pre&gt; Thus, this database consists of both galaxies and Galaxian contaminants. The sample contains ~5320 galaxies, and 14 objects without identifications at the present time.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/iraszsurv#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iraszsurv</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=iraszsurv&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/iras/iraszsurv.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRASZ [3]</TD>
            <TD>IRAS 1.2-Jy Redshift Survey</TD>
            <TD>This is The Redshift Survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in ApJ Supp 1995, 100, 69. The survey contains 9897 objects selected from the IRAS database according to the following criteria: &lt;pre&gt; F60 &gt; 1.2 Jy; F60^2 &gt; F12 f25; |b| &lt; 5; high source density flag at 60 microns not raised. &lt;/pre&gt; Thus, this database consists of both galaxies and Galaxian contaminants. The sample contains ~5320 galaxies, and 14 objects without identifications at the present time.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/iraszsurv#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iraszsurv</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_iraszsurv&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/iras/iraszsurv.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/180 [1]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#1</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/180</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/180 [2]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#2</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/180&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl4]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl4</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl5]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl5</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p2tbl3]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p2tbl3</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl6]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl6</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p2tbl2]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p2tbl2</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl2]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl2</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl3]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl3</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRASZ [1]</TD>
            <TD>IRAS 1.2-Jy Redshift Survey</TD>
            <TD>This is The Redshift Survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in ApJ Supp 1995, 100, 69. The survey contains 9897 objects selected from the IRAS database according to the following criteria: &lt;pre&gt; F60 &gt; 1.2 Jy; F60^2 &gt; F12 f25; |b| &lt; 5; high source density flag at 60 microns not raised. &lt;/pre&gt; Thus, this database consists of both galaxies and Galaxian contaminants. The sample contains ~5320 galaxies, and 14 objects without identifications at the present time.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/iraszsurv#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iraszsurv</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=iraszsurv&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/iras/iraszsurv.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRASZ [2]</TD>
            <TD>IRAS 1.2-Jy Redshift Survey</TD>
            <TD>This is The Redshift Survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in ApJ Supp 1995, 100, 69. The survey contains 9897 objects selected from the IRAS database according to the following criteria: &lt;pre&gt; F60 &gt; 1.2 Jy; F60^2 &gt; F12 f25; |b| &lt; 5; high source density flag at 60 microns not raised. &lt;/pre&gt; Thus, this database consists of both galaxies and Galaxian contaminants. The sample contains ~5320 galaxies, and 14 objects without identifications at the present time.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/iraszsurv#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iraszsurv</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=iraszsurv&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/iras/iraszsurv.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRASZ [3]</TD>
            <TD>IRAS 1.2-Jy Redshift Survey</TD>
            <TD>This is The Redshift Survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in ApJ Supp 1995, 100, 69. The survey contains 9897 objects selected from the IRAS database according to the following criteria: &lt;pre&gt; F60 &gt; 1.2 Jy; F60^2 &gt; F12 f25; |b| &lt; 5; high source density flag at 60 microns not raised. &lt;/pre&gt; Thus, this database consists of both galaxies and Galaxian contaminants. The sample contains ~5320 galaxies, and 14 objects without identifications at the present time.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/iraszsurv#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iraszsurv</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_iraszsurv&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/iras/iraszsurv.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/180 [1]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#1</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/180</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/180 [2]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#2</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/180&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl4]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl4</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl5]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl5</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p2tbl3]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p2tbl3</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl6]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl6</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p2tbl2]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p2tbl2</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl2]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl2</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl3]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl3</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A90 [1]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#1</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A90</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A90 [2]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#2</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A90&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A90 [table1]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#table1</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A90&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A90 [table2]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#table2</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A90&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/180 [1]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#1</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/180</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/180 [2]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#2</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/180&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl4]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl4</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl5]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl5</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p2tbl3]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p2tbl3</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl6]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl6</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p2tbl2]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p2tbl2</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl2]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl2</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/180 [p3tbl3]</TD>
            <TD>Galaxies in Fornax Cluster and five nearby groups (Ferguson+ 1990)</TD>
            <TD>This catalog represents the combination of results published in two papers: Ferguson, H.C. 1989 A.J. 98, 367 (Paper II) and Ferguson, H.C. and Sandage, A. 1990 A.J. 100, 1 (Paper III). See the Historical Notes section below. Please note that the data from Paper II were previously archived as catalog VII/160. This catalog supersedes that earlier dataset. The following paragraphs describe the data included from the two papers. (Paper II) This paper presents a catalog of 2678 galaxies within an area of nearly 40 deg^2^ centered on the Fornax Cluster at {alpha}=3h35m and {delta}=-35.7deg. The data have been obtained from visual inspection of 26 deep large-scale (10.9arcsec/mm) plates taken with the du Pont 2.5m reflector at the Las Campanas Observatory, and from digital photometry of an ESO/SRC blue survey plate covering roughly the same area of the sky. The catalog is essentially diameter limited, with a limiting diameter of 17arcsec at an isophoto of B_T_ =26.5. Within this survey region, the catalog includes 340 likely cluster members and 2338 likely background galaxies. For cluster members, this listing should be complete to B_T_=18 (corresponding to M_BT_=13.0, assuming a distance modulus of m-M=31.9) and contains likely members down to B_T_=20. Cluster membership is for the most part based on galaxy morphology. By virtue of their low surface brightness, dwarf galaxies in the cluster can be distinguished with a high degree of certainty from background galaxies. Radial velocities are included for 89 galaxies in the survey, providing a reliable indicator of membership in these cases. As additional support for our rejection of background galaxies, we model the spatial distribution of various types of galaxies as the sum of a King model cluster component superimposed on a uniform background. Using maximum-likelyhood fits to these spatial distributions, we find a core radius of 0.7deg. for a King model fit to the cluster, and show that there are few, if any, cluster members contained in the sample of background galaxiesBD (Paper III) Five nearby groups of galaxies have been surveyed using large-scale plates from the 2.5 m duPont Telescope at Las Campanas Observatory. Catalogs of galaxies brighter than B_T_ ~ 20 are presented for the Leo, Dorado, NGC 1400, NGC 5044, and Antlia groups. A total of 1044 galaxies are included, from visual inspection of 14 plates, covering 31deg square. Galaxies have been classified in the extended Hubble system, and group memberships have been assigned based on velocity (where available) and morphology. About half the galaxies listed are likely members of one of the nearby groups. The catalogs are complete to B_T_ ~ 18, although the completeness limits vary slightly from group to group. Based on King model fits to the surface density profiles, the core radii of the groups range from 0.3 to 1 Mpc, and central densities range from 120 to 1900 galaxies Mpc^-3^ brighter than M_BT_ = -12.5. Dynamical analysis indicates that all of the groups of likely to be gravitationally bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/180#p3tbl3</TD>
            <TD>2012-11-13T06:49:39Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/VII/180</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/180&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/180</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRASZ [1]</TD>
            <TD>IRAS 1.2-Jy Redshift Survey</TD>
            <TD>This is The Redshift Survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in ApJ Supp 1995, 100, 69. The survey contains 9897 objects selected from the IRAS database according to the following criteria: &lt;pre&gt; F60 &gt; 1.2 Jy; F60^2 &gt; F12 f25; |b| &lt; 5; high source density flag at 60 microns not raised. &lt;/pre&gt; Thus, this database consists of both galaxies and Galaxian contaminants. The sample contains ~5320 galaxies, and 14 objects without identifications at the present time.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/iraszsurv#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iraszsurv</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=iraszsurv&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/iras/iraszsurv.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRASZ [2]</TD>
            <TD>IRAS 1.2-Jy Redshift Survey</TD>
            <TD>This is The Redshift Survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in ApJ Supp 1995, 100, 69. The survey contains 9897 objects selected from the IRAS database according to the following criteria: &lt;pre&gt; F60 &gt; 1.2 Jy; F60^2 &gt; F12 f25; |b| &lt; 5; high source density flag at 60 microns not raised. &lt;/pre&gt; Thus, this database consists of both galaxies and Galaxian contaminants. The sample contains ~5320 galaxies, and 14 objects without identifications at the present time.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/iraszsurv#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iraszsurv</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=iraszsurv&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/iras/iraszsurv.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRASZ [3]</TD>
            <TD>IRAS 1.2-Jy Redshift Survey</TD>
            <TD>This is The Redshift Survey of Fisher, Huchra, Strauss, Davis, Yahil and Schlegel; the data set is described in full in ApJ 361, 49 (1990). The data for the brighter half are included in ApJ Supp 1992, 83, 29; the data for the fainter half are included in ApJ Supp 1995, 100, 69. The survey contains 9897 objects selected from the IRAS database according to the following criteria: &lt;pre&gt; F60 &gt; 1.2 Jy; F60^2 &gt; F12 f25; |b| &lt; 5; high source density flag at 60 microns not raised. &lt;/pre&gt; Thus, this database consists of both galaxies and Galaxian contaminants. The sample contains ~5320 galaxies, and 14 objects without identifications at the present time.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/iraszsurv#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iraszsurv</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_iraszsurv&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/iras/iraszsurv.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/214 [1]</TD>
            <TD>APS Galaxies in the North Galactic Pole (Cabanela, 1999)</TD>
            <TD>This catalog contains information for 217768 unique objects (all plate overlap duplicates have been eliminated) with major-axis diameters greater than 10 arcseconds in O (blue) and identified as "non-stellar" by the APS. Care has been taken to remove known sources of non-extragalactic contamination including SAO star halos, POSS I ghost images of bright stars, low surface brightness material around bright galaxies, and Galactic globular clusters. This version of the MAPS-NGP galaxy catalog preserves the full resolution of data as stored in the Revised Minnesota Automated Plate Scanner Catalog of the POSS I (a.k.a. StarBase2). For more through documentation of how these image parameters are obtained, you may visit the APS WWW site &lt;http://aps.umn.edu/&gt; or look at some of the references listed at the end of this README file.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/214#1</TD>
            <TD>2012-11-13T06:50:35Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/VII/214</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/214</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/214</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/214 [2]</TD>
            <TD>APS Galaxies in the North Galactic Pole (Cabanela, 1999)</TD>
            <TD>This catalog contains information for 217768 unique objects (all plate overlap duplicates have been eliminated) with major-axis diameters greater than 10 arcseconds in O (blue) and identified as "non-stellar" by the APS. Care has been taken to remove known sources of non-extragalactic contamination including SAO star halos, POSS I ghost images of bright stars, low surface brightness material around bright galaxies, and Galactic globular clusters. This version of the MAPS-NGP galaxy catalog preserves the full resolution of data as stored in the Revised Minnesota Automated Plate Scanner Catalog of the POSS I (a.k.a. StarBase2). For more through documentation of how these image parameters are obtained, you may visit the APS WWW site &lt;http://aps.umn.edu/&gt; or look at some of the references listed at the end of this README file.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/214#2</TD>
            <TD>2012-11-13T06:50:35Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/VII/214</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/214&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/214</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/214 [aps]</TD>
            <TD>APS Galaxies in the North Galactic Pole (Cabanela, 1999)</TD>
            <TD>This catalog contains information for 217768 unique objects (all plate overlap duplicates have been eliminated) with major-axis diameters greater than 10 arcseconds in O (blue) and identified as "non-stellar" by the APS. Care has been taken to remove known sources of non-extragalactic contamination including SAO star halos, POSS I ghost images of bright stars, low surface brightness material around bright galaxies, and Galactic globular clusters. This version of the MAPS-NGP galaxy catalog preserves the full resolution of data as stored in the Revised Minnesota Automated Plate Scanner Catalog of the POSS I (a.k.a. StarBase2). For more through documentation of how these image parameters are obtained, you may visit the APS WWW site &lt;http://aps.umn.edu/&gt; or look at some of the references listed at the end of this README file.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/214#aps</TD>
            <TD>2012-11-13T06:50:35Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/VII/214</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/214&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/214</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A90 [1]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#1</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A90</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A90 [2]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#2</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A90&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A90 [table1]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#table1</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A90&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A90 [table2]</TD>
            <TD>WSRT Virgo HI filament survey (Popping+, 2011)</TD>
            <TD>To obtain the highest possible brightness sensitivity in cross-correlations, the WSRT (Westerbork Synthesis Radio Telescope) was configured to simulate a large filled aperture in projection. Twelve of the 14 WSRT 25m telescopes were positioned at regular intervals of 144m. A deep fully-sampled survey of the galaxy filament joining the Local Group to the Virgo Cluster has been undertaken, extending from 8 to 17h in RA and from -1 to +10 degrees in declination and covering 40MHz of bandwidth with 8km/s resolution.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90#table2</TD>
            <TD>2011-09-18T09:29:01Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A90</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A90&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A90</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/214 [1]</TD>
            <TD>APS Galaxies in the North Galactic Pole (Cabanela, 1999)</TD>
            <TD>This catalog contains information for 217768 unique objects (all plate overlap duplicates have been eliminated) with major-axis diameters greater than 10 arcseconds in O (blue) and identified as "non-stellar" by the APS. Care has been taken to remove known sources of non-extragalactic contamination including SAO star halos, POSS I ghost images of bright stars, low surface brightness material around bright galaxies, and Galactic globular clusters. This version of the MAPS-NGP galaxy catalog preserves the full resolution of data as stored in the Revised Minnesota Automated Plate Scanner Catalog of the POSS I (a.k.a. StarBase2). For more through documentation of how these image parameters are obtained, you may visit the APS WWW site &lt;http://aps.umn.edu/&gt; or look at some of the references listed at the end of this README file.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/214#1</TD>
            <TD>2012-11-13T06:50:35Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/VII/214</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/214</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/214</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/214 [2]</TD>
            <TD>APS Galaxies in the North Galactic Pole (Cabanela, 1999)</TD>
            <TD>This catalog contains information for 217768 unique objects (all plate overlap duplicates have been eliminated) with major-axis diameters greater than 10 arcseconds in O (blue) and identified as "non-stellar" by the APS. Care has been taken to remove known sources of non-extragalactic contamination including SAO star halos, POSS I ghost images of bright stars, low surface brightness material around bright galaxies, and Galactic globular clusters. This version of the MAPS-NGP galaxy catalog preserves the full resolution of data as stored in the Revised Minnesota Automated Plate Scanner Catalog of the POSS I (a.k.a. StarBase2). For more through documentation of how these image parameters are obtained, you may visit the APS WWW site &lt;http://aps.umn.edu/&gt; or look at some of the references listed at the end of this README file.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/214#2</TD>
            <TD>2012-11-13T06:50:35Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/VII/214</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/214&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/214</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/214 [aps]</TD>
            <TD>APS Galaxies in the North Galactic Pole (Cabanela, 1999)</TD>
            <TD>This catalog contains information for 217768 unique objects (all plate overlap duplicates have been eliminated) with major-axis diameters greater than 10 arcseconds in O (blue) and identified as "non-stellar" by the APS. Care has been taken to remove known sources of non-extragalactic contamination including SAO star halos, POSS I ghost images of bright stars, low surface brightness material around bright galaxies, and Galactic globular clusters. This version of the MAPS-NGP galaxy catalog preserves the full resolution of data as stored in the Revised Minnesota Automated Plate Scanner Catalog of the POSS I (a.k.a. StarBase2). For more through documentation of how these image parameters are obtained, you may visit the APS WWW site &lt;http://aps.umn.edu/&gt; or look at some of the references listed at the end of this README file.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/214#aps</TD>
            <TD>2012-11-13T06:50:35Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/VII/214</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/214&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/214</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LMXB [1]</TD>
            <TD>Low-Mass X-Ray Binary Catalog (4th Edition, 2007)</TD>
            <TD>This is the Fourth Edition of the Catalog of Low-mass X-ray Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog has a companion catalog of high-mass X-ray binaries (HMXBs) which is called HMXBCAT in the HEASARC database system). The catalog contains source name(s), coordinates, X-ray flux, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with references to a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties being similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary, this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lmxbcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lmxbcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lmxbcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lmxbcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LMXB [2]</TD>
            <TD>Low-Mass X-Ray Binary Catalog (4th Edition, 2007)</TD>
            <TD>This is the Fourth Edition of the Catalog of Low-mass X-ray Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog has a companion catalog of high-mass X-ray binaries (HMXBs) which is called HMXBCAT in the HEASARC database system). The catalog contains source name(s), coordinates, X-ray flux, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with references to a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties being similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary, this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lmxbcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lmxbcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LMXB [3]</TD>
            <TD>Low-Mass X-Ray Binary Catalog (4th Edition, 2007)</TD>
            <TD>This is the Fourth Edition of the Catalog of Low-mass X-ray Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog has a companion catalog of high-mass X-ray binaries (HMXBs) which is called HMXBCAT in the HEASARC database system). The catalog contains source name(s), coordinates, X-ray flux, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with references to a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties being similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary, this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lmxbcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lmxbcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/214 [1]</TD>
            <TD>APS Galaxies in the North Galactic Pole (Cabanela, 1999)</TD>
            <TD>This catalog contains information for 217768 unique objects (all plate overlap duplicates have been eliminated) with major-axis diameters greater than 10 arcseconds in O (blue) and identified as "non-stellar" by the APS. Care has been taken to remove known sources of non-extragalactic contamination including SAO star halos, POSS I ghost images of bright stars, low surface brightness material around bright galaxies, and Galactic globular clusters. This version of the MAPS-NGP galaxy catalog preserves the full resolution of data as stored in the Revised Minnesota Automated Plate Scanner Catalog of the POSS I (a.k.a. StarBase2). For more through documentation of how these image parameters are obtained, you may visit the APS WWW site &lt;http://aps.umn.edu/&gt; or look at some of the references listed at the end of this README file.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/214#1</TD>
            <TD>2012-11-13T06:50:35Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/VII/214</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/214</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/214</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/214 [2]</TD>
            <TD>APS Galaxies in the North Galactic Pole (Cabanela, 1999)</TD>
            <TD>This catalog contains information for 217768 unique objects (all plate overlap duplicates have been eliminated) with major-axis diameters greater than 10 arcseconds in O (blue) and identified as "non-stellar" by the APS. Care has been taken to remove known sources of non-extragalactic contamination including SAO star halos, POSS I ghost images of bright stars, low surface brightness material around bright galaxies, and Galactic globular clusters. This version of the MAPS-NGP galaxy catalog preserves the full resolution of data as stored in the Revised Minnesota Automated Plate Scanner Catalog of the POSS I (a.k.a. StarBase2). For more through documentation of how these image parameters are obtained, you may visit the APS WWW site &lt;http://aps.umn.edu/&gt; or look at some of the references listed at the end of this README file.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/214#2</TD>
            <TD>2012-11-13T06:50:35Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/VII/214</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/214&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/214</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/214 [aps]</TD>
            <TD>APS Galaxies in the North Galactic Pole (Cabanela, 1999)</TD>
            <TD>This catalog contains information for 217768 unique objects (all plate overlap duplicates have been eliminated) with major-axis diameters greater than 10 arcseconds in O (blue) and identified as "non-stellar" by the APS. Care has been taken to remove known sources of non-extragalactic contamination including SAO star halos, POSS I ghost images of bright stars, low surface brightness material around bright galaxies, and Galactic globular clusters. This version of the MAPS-NGP galaxy catalog preserves the full resolution of data as stored in the Revised Minnesota Automated Plate Scanner Catalog of the POSS I (a.k.a. StarBase2). For more through documentation of how these image parameters are obtained, you may visit the APS WWW site &lt;http://aps.umn.edu/&gt; or look at some of the references listed at the end of this README file.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/214#aps</TD>
            <TD>2012-11-13T06:50:35Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/VII/214</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/214&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/214</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/63/S363 [1]</TD>
            <TD>MOIRCS Deep Survey. VII. (Konishi+, 2011)</TD>
            <TD>We constructed a stellar mass-limited z~1 galaxy sample using the deep catalog of Kajisawa et al. (2009ApJ...702.1393K). The catalog contains 3203 Ks(Vega)&lt;24mag galaxies in 28arcmin^2^ from MOIRCS (Multi-Object InfraRed Camera and Spectrograph) Deep Survey (MODS) ultra-deep image obtained with MOIRCS attached to the Subaru Telescope (Kajisawa et al., 2006PASJ...58..951K). It covers a part of the Great Observatories Origins Deep Survey North (GOODS-N: Giavalisco et al. (2004, Cat. II/261) field including Hubble Deep Field North region (HDF-N).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363#1</TD>
            <TD>2011-09-22T16:09:24Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/63/S363</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/63/S363</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/63/S363 [2]</TD>
            <TD>MOIRCS Deep Survey. VII. (Konishi+, 2011)</TD>
            <TD>We constructed a stellar mass-limited z~1 galaxy sample using the deep catalog of Kajisawa et al. (2009ApJ...702.1393K). The catalog contains 3203 Ks(Vega)&lt;24mag galaxies in 28arcmin^2^ from MOIRCS (Multi-Object InfraRed Camera and Spectrograph) Deep Survey (MODS) ultra-deep image obtained with MOIRCS attached to the Subaru Telescope (Kajisawa et al., 2006PASJ...58..951K). It covers a part of the Great Observatories Origins Deep Survey North (GOODS-N: Giavalisco et al. (2004, Cat. II/261) field including Hubble Deep Field North region (HDF-N).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363#2</TD>
            <TD>2011-09-22T16:09:24Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/63/S363&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/63/S363</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/63/S363 [table2]</TD>
            <TD>MOIRCS Deep Survey. VII. (Konishi+, 2011)</TD>
            <TD>We constructed a stellar mass-limited z~1 galaxy sample using the deep catalog of Kajisawa et al. (2009ApJ...702.1393K). The catalog contains 3203 Ks(Vega)&lt;24mag galaxies in 28arcmin^2^ from MOIRCS (Multi-Object InfraRed Camera and Spectrograph) Deep Survey (MODS) ultra-deep image obtained with MOIRCS attached to the Subaru Telescope (Kajisawa et al., 2006PASJ...58..951K). It covers a part of the Great Observatories Origins Deep Survey North (GOODS-N: Giavalisco et al. (2004, Cat. II/261) field including Hubble Deep Field North region (HDF-N).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363#table2</TD>
            <TD>2011-09-22T16:09:24Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/63/S363&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/63/S363</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LMXB [1]</TD>
            <TD>Low-Mass X-Ray Binary Catalog (4th Edition, 2007)</TD>
            <TD>This is the Fourth Edition of the Catalog of Low-mass X-ray Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog has a companion catalog of high-mass X-ray binaries (HMXBs) which is called HMXBCAT in the HEASARC database system). The catalog contains source name(s), coordinates, X-ray flux, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with references to a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties being similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary, this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lmxbcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lmxbcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lmxbcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lmxbcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LMXB [2]</TD>
            <TD>Low-Mass X-Ray Binary Catalog (4th Edition, 2007)</TD>
            <TD>This is the Fourth Edition of the Catalog of Low-mass X-ray Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog has a companion catalog of high-mass X-ray binaries (HMXBs) which is called HMXBCAT in the HEASARC database system). The catalog contains source name(s), coordinates, X-ray flux, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with references to a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties being similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary, this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lmxbcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lmxbcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LMXB [3]</TD>
            <TD>Low-Mass X-Ray Binary Catalog (4th Edition, 2007)</TD>
            <TD>This is the Fourth Edition of the Catalog of Low-mass X-ray Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog has a companion catalog of high-mass X-ray binaries (HMXBs) which is called HMXBCAT in the HEASARC database system). The catalog contains source name(s), coordinates, X-ray flux, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with references to a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties being similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary, this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lmxbcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lmxbcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/63/S363 [1]</TD>
            <TD>MOIRCS Deep Survey. VII. (Konishi+, 2011)</TD>
            <TD>We constructed a stellar mass-limited z~1 galaxy sample using the deep catalog of Kajisawa et al. (2009ApJ...702.1393K). The catalog contains 3203 Ks(Vega)&lt;24mag galaxies in 28arcmin^2^ from MOIRCS (Multi-Object InfraRed Camera and Spectrograph) Deep Survey (MODS) ultra-deep image obtained with MOIRCS attached to the Subaru Telescope (Kajisawa et al., 2006PASJ...58..951K). It covers a part of the Great Observatories Origins Deep Survey North (GOODS-N: Giavalisco et al. (2004, Cat. II/261) field including Hubble Deep Field North region (HDF-N).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363#1</TD>
            <TD>2011-09-22T16:09:24Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/63/S363</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/63/S363</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/63/S363 [2]</TD>
            <TD>MOIRCS Deep Survey. VII. (Konishi+, 2011)</TD>
            <TD>We constructed a stellar mass-limited z~1 galaxy sample using the deep catalog of Kajisawa et al. (2009ApJ...702.1393K). The catalog contains 3203 Ks(Vega)&lt;24mag galaxies in 28arcmin^2^ from MOIRCS (Multi-Object InfraRed Camera and Spectrograph) Deep Survey (MODS) ultra-deep image obtained with MOIRCS attached to the Subaru Telescope (Kajisawa et al., 2006PASJ...58..951K). It covers a part of the Great Observatories Origins Deep Survey North (GOODS-N: Giavalisco et al. (2004, Cat. II/261) field including Hubble Deep Field North region (HDF-N).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363#2</TD>
            <TD>2011-09-22T16:09:24Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/63/S363&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/63/S363</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/63/S363 [table2]</TD>
            <TD>MOIRCS Deep Survey. VII. (Konishi+, 2011)</TD>
            <TD>We constructed a stellar mass-limited z~1 galaxy sample using the deep catalog of Kajisawa et al. (2009ApJ...702.1393K). The catalog contains 3203 Ks(Vega)&lt;24mag galaxies in 28arcmin^2^ from MOIRCS (Multi-Object InfraRed Camera and Spectrograph) Deep Survey (MODS) ultra-deep image obtained with MOIRCS attached to the Subaru Telescope (Kajisawa et al., 2006PASJ...58..951K). It covers a part of the Great Observatories Origins Deep Survey North (GOODS-N: Giavalisco et al. (2004, Cat. II/261) field including Hubble Deep Field North region (HDF-N).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363#table2</TD>
            <TD>2011-09-22T16:09:24Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/63/S363&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/63/S363</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GC [1]</TD>
            <TD>Milky Way Globular Clusters Catalog (February 2003 Version)</TD>
            <TD>This is the Catalog of Parameters for Milky Way Globular Clusters (February 2003 Version) that was compiled by William E. Harris of McMaster University. It contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: &lt;a href="http://www.physics.mcmaster.ca/~harris/mwgc.ref"&gt;http://www.physics.mcmaster.ca/~harris/mwgc.ref&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/globclust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/globclust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=globclust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/globclust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GC [2]</TD>
            <TD>Milky Way Globular Clusters Catalog (February 2003 Version)</TD>
            <TD>This is the Catalog of Parameters for Milky Way Globular Clusters (February 2003 Version) that was compiled by William E. Harris of McMaster University. It contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: &lt;a href="http://www.physics.mcmaster.ca/~harris/mwgc.ref"&gt;http://www.physics.mcmaster.ca/~harris/mwgc.ref&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/globclust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/globclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=globclust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/globclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GC [3]</TD>
            <TD>Milky Way Globular Clusters Catalog (February 2003 Version)</TD>
            <TD>This is the Catalog of Parameters for Milky Way Globular Clusters (February 2003 Version) that was compiled by William E. Harris of McMaster University. It contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 150 objects that are regarded as globular clusters in the Milky Way galaxy. Please acknowledge the use of this catalog in any published work you derive from it. The proper reference to the literature is the published paper (Harris, W.E. 1996, AJ, 112, 1487) which briefly describes the setup of the catalog. The author would also greatly appreciate receiving any new information, in published or preprint form, which would help him to keep the list up to date (contact W. E. Harris at harris@physics.mcmaster.ca). A full discussion of the sources used in the creation of this catalog and of the parameters that it contains can be found in the file: &lt;a href="http://www.physics.mcmaster.ca/~harris/mwgc.ref"&gt;http://www.physics.mcmaster.ca/~harris/mwgc.ref&lt;/a&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/globclust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/globclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_globclust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/globclust.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LMXB [1]</TD>
            <TD>Low-Mass X-Ray Binary Catalog (4th Edition, 2007)</TD>
            <TD>This is the Fourth Edition of the Catalog of Low-mass X-ray Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog has a companion catalog of high-mass X-ray binaries (HMXBs) which is called HMXBCAT in the HEASARC database system). The catalog contains source name(s), coordinates, X-ray flux, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with references to a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties being similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary, this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lmxbcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lmxbcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lmxbcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lmxbcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LMXB [2]</TD>
            <TD>Low-Mass X-Ray Binary Catalog (4th Edition, 2007)</TD>
            <TD>This is the Fourth Edition of the Catalog of Low-mass X-ray Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog has a companion catalog of high-mass X-ray binaries (HMXBs) which is called HMXBCAT in the HEASARC database system). The catalog contains source name(s), coordinates, X-ray flux, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with references to a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties being similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary, this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lmxbcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lmxbcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LMXB [3]</TD>
            <TD>Low-Mass X-Ray Binary Catalog (4th Edition, 2007)</TD>
            <TD>This is the Fourth Edition of the Catalog of Low-mass X-ray Binaries (LMXBs) in the Galaxy and the Magellanic Clouds. The catalog has a companion catalog of high-mass X-ray binaries (HMXBs) which is called HMXBCAT in the HEASARC database system). The catalog contains source name(s), coordinates, X-ray flux, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with references to a comprehensive selection of the relevant literature. The aim of this catalog is to provide some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identified as low-mass X-ray binaries on the basis of their X-ray properties being similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary, this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lmxbcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star#XRB#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lmxbcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lmxbcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/lmxbcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VIII/29A [1]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#1</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VIII/29A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIII/29A [2]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#2</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VIII/29A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIII/29A [abelclus]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#abelclus</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VIII/29A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIII/29A [table1]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#table1</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VIII/29A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/63/S363 [1]</TD>
            <TD>MOIRCS Deep Survey. VII. (Konishi+, 2011)</TD>
            <TD>We constructed a stellar mass-limited z~1 galaxy sample using the deep catalog of Kajisawa et al. (2009ApJ...702.1393K). The catalog contains 3203 Ks(Vega)&lt;24mag galaxies in 28arcmin^2^ from MOIRCS (Multi-Object InfraRed Camera and Spectrograph) Deep Survey (MODS) ultra-deep image obtained with MOIRCS attached to the Subaru Telescope (Kajisawa et al., 2006PASJ...58..951K). It covers a part of the Great Observatories Origins Deep Survey North (GOODS-N: Giavalisco et al. (2004, Cat. II/261) field including Hubble Deep Field North region (HDF-N).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363#1</TD>
            <TD>2011-09-22T16:09:24Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/63/S363</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/63/S363</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/63/S363 [2]</TD>
            <TD>MOIRCS Deep Survey. VII. (Konishi+, 2011)</TD>
            <TD>We constructed a stellar mass-limited z~1 galaxy sample using the deep catalog of Kajisawa et al. (2009ApJ...702.1393K). The catalog contains 3203 Ks(Vega)&lt;24mag galaxies in 28arcmin^2^ from MOIRCS (Multi-Object InfraRed Camera and Spectrograph) Deep Survey (MODS) ultra-deep image obtained with MOIRCS attached to the Subaru Telescope (Kajisawa et al., 2006PASJ...58..951K). It covers a part of the Great Observatories Origins Deep Survey North (GOODS-N: Giavalisco et al. (2004, Cat. II/261) field including Hubble Deep Field North region (HDF-N).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363#2</TD>
            <TD>2011-09-22T16:09:24Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/63/S363&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/63/S363</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/63/S363 [table2]</TD>
            <TD>MOIRCS Deep Survey. VII. (Konishi+, 2011)</TD>
            <TD>We constructed a stellar mass-limited z~1 galaxy sample using the deep catalog of Kajisawa et al. (2009ApJ...702.1393K). The catalog contains 3203 Ks(Vega)&lt;24mag galaxies in 28arcmin^2^ from MOIRCS (Multi-Object InfraRed Camera and Spectrograph) Deep Survey (MODS) ultra-deep image obtained with MOIRCS attached to the Subaru Telescope (Kajisawa et al., 2006PASJ...58..951K). It covers a part of the Great Observatories Origins Deep Survey North (GOODS-N: Giavalisco et al. (2004, Cat. II/261) field including Hubble Deep Field North region (HDF-N).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363#table2</TD>
            <TD>2011-09-22T16:09:24Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/63/S363</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/63/S363&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/63/S363</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/698/865 [1]</TD>
            <TD>Halo streams in the SDSS-DR7 (Klement+, 2009)</TD>
            <TD>SDSS-I was an imaging and spectroscopic survey that began routine operations in 2000 April and continued through 2005 June. The SDSS, and its extensions, uses a dedicated 2.5m telescope located at the Apache Point Observatory in New Mexico. One of three subsurveys carried out during the first extension of the SDSS, known as SDSS-II, the Sloan Extension for Galactic Understanding and Exploration (SEGUE), ran from 2005 July to 2008 June. SEGUE obtained some 250000 medium-resolution spectra of stars in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865#1</TD>
            <TD>2011-10-18T10:28:11Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/698/865</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/698/865</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/698/865 [2]</TD>
            <TD>Halo streams in the SDSS-DR7 (Klement+, 2009)</TD>
            <TD>SDSS-I was an imaging and spectroscopic survey that began routine operations in 2000 April and continued through 2005 June. The SDSS, and its extensions, uses a dedicated 2.5m telescope located at the Apache Point Observatory in New Mexico. One of three subsurveys carried out during the first extension of the SDSS, known as SDSS-II, the Sloan Extension for Galactic Understanding and Exploration (SEGUE), ran from 2005 July to 2008 June. SEGUE obtained some 250000 medium-resolution spectra of stars in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865#2</TD>
            <TD>2011-10-18T10:28:11Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/698/865&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/698/865</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/698/865 [table3]</TD>
            <TD>Halo streams in the SDSS-DR7 (Klement+, 2009)</TD>
            <TD>SDSS-I was an imaging and spectroscopic survey that began routine operations in 2000 April and continued through 2005 June. The SDSS, and its extensions, uses a dedicated 2.5m telescope located at the Apache Point Observatory in New Mexico. One of three subsurveys carried out during the first extension of the SDSS, known as SDSS-II, the Sloan Extension for Galactic Understanding and Exploration (SEGUE), ran from 2005 July to 2008 June. SEGUE obtained some 250000 medium-resolution spectra of stars in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865#table3</TD>
            <TD>2011-10-18T10:28:11Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/698/865&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/698/865</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMM/M31 [1]</TD>
            <TD>XMM-Newton M31 Survey Source Catalog</TD>
            <TD>This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10^34 erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogues and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmmxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmmxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m31xmmxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmmxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMM/M31 [2]</TD>
            <TD>XMM-Newton M31 Survey Source Catalog</TD>
            <TD>This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10^34 erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogues and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmmxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m31xmmxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMM/M31 [3]</TD>
            <TD>XMM-Newton M31 Survey Source Catalog</TD>
            <TD>This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10^34 erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogues and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmmxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m31xmmxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VIII/29A [1]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#1</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VIII/29A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIII/29A [2]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#2</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VIII/29A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIII/29A [abelclus]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#abelclus</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VIII/29A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIII/29A [table1]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#table1</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VIII/29A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/698/865 [1]</TD>
            <TD>Halo streams in the SDSS-DR7 (Klement+, 2009)</TD>
            <TD>SDSS-I was an imaging and spectroscopic survey that began routine operations in 2000 April and continued through 2005 June. The SDSS, and its extensions, uses a dedicated 2.5m telescope located at the Apache Point Observatory in New Mexico. One of three subsurveys carried out during the first extension of the SDSS, known as SDSS-II, the Sloan Extension for Galactic Understanding and Exploration (SEGUE), ran from 2005 July to 2008 June. SEGUE obtained some 250000 medium-resolution spectra of stars in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865#1</TD>
            <TD>2011-10-18T10:28:11Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/698/865</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/698/865</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/698/865 [2]</TD>
            <TD>Halo streams in the SDSS-DR7 (Klement+, 2009)</TD>
            <TD>SDSS-I was an imaging and spectroscopic survey that began routine operations in 2000 April and continued through 2005 June. The SDSS, and its extensions, uses a dedicated 2.5m telescope located at the Apache Point Observatory in New Mexico. One of three subsurveys carried out during the first extension of the SDSS, known as SDSS-II, the Sloan Extension for Galactic Understanding and Exploration (SEGUE), ran from 2005 July to 2008 June. SEGUE obtained some 250000 medium-resolution spectra of stars in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865#2</TD>
            <TD>2011-10-18T10:28:11Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/698/865&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/698/865</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/698/865 [table3]</TD>
            <TD>Halo streams in the SDSS-DR7 (Klement+, 2009)</TD>
            <TD>SDSS-I was an imaging and spectroscopic survey that began routine operations in 2000 April and continued through 2005 June. The SDSS, and its extensions, uses a dedicated 2.5m telescope located at the Apache Point Observatory in New Mexico. One of three subsurveys carried out during the first extension of the SDSS, known as SDSS-II, the Sloan Extension for Galactic Understanding and Exploration (SEGUE), ran from 2005 July to 2008 June. SEGUE obtained some 250000 medium-resolution spectra of stars in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865#table3</TD>
            <TD>2011-10-18T10:28:11Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/698/865&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/698/865</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VIII/29A [1]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#1</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VIII/29A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIII/29A [2]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#2</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VIII/29A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIII/29A [abelclus]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#abelclus</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VIII/29A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIII/29A [table1]</TD>
            <TD>1400-MHz Survey of 1478 Abell Clusters of Galaxies (Owen+ 1982)</TD>
            <TD>This catalog contains observations of Abell clusters of galaxies which were obtained with the Green Bank 91-m telescope at 1400 MHz with an angular resolution of 10'x11' (RAxDEC). This catalog extends the sample of clusters originally published in Owen (1974AJ.....79..427O). The primary goals of this survey were to observe all Abell (1958ApJS....3..211A, Cat. VII/4) clusters with m10 (magnitude of the tenth brightest galaxy in the cluster) less than or equal to 17.0 and declinations north of -19 degrees, to observe all clusters with richness&gt;=3 regardless of m10, and to obtain observations of a representative sample of the rest of the catalog (m10&gt;=17.0; richness&lt;=2). The abelclus.dat file contains ALL 957 detected sources (also beyond 0.5 corrected Abell radii). It contains 525 sources within 0.5 corrected Abell radii, while the published table1.dat file contains 487 entries corresponding to 485 distinct sources (in 442 clusters). The catalog entries contains the flux density at 1400 MHz, the Abell cluster number, richness class, distance class, m10, redshift estimate (z), corrected Abell cluster radius, right ascension (B1950), declination (B1950), deconvolved major and minor source axis lengths, position angle, and distance of the source from the cluster center.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/VIII/29A#table1</TD>
            <TD>2012-11-13T07:08:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VIII/29A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VIII/29A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VIII/29A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMM/M31 [1]</TD>
            <TD>XMM-Newton M31 Survey Source Catalog</TD>
            <TD>This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10^34 erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogues and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmmxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmmxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m31xmmxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmmxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMM/M31 [2]</TD>
            <TD>XMM-Newton M31 Survey Source Catalog</TD>
            <TD>This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10^34 erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogues and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmmxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m31xmmxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMM/M31 [3]</TD>
            <TD>XMM-Newton M31 Survey Source Catalog</TD>
            <TD>This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10^34 erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogues and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmmxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m31xmmxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/543/178 [1]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#1</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/543/178</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/543/178 [2]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#2</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table3]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table3</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table2]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table2</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table7]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table7</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table4]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table4</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table5]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table5</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table6]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table6</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/698/865 [1]</TD>
            <TD>Halo streams in the SDSS-DR7 (Klement+, 2009)</TD>
            <TD>SDSS-I was an imaging and spectroscopic survey that began routine operations in 2000 April and continued through 2005 June. The SDSS, and its extensions, uses a dedicated 2.5m telescope located at the Apache Point Observatory in New Mexico. One of three subsurveys carried out during the first extension of the SDSS, known as SDSS-II, the Sloan Extension for Galactic Understanding and Exploration (SEGUE), ran from 2005 July to 2008 June. SEGUE obtained some 250000 medium-resolution spectra of stars in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865#1</TD>
            <TD>2011-10-18T10:28:11Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/698/865</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/698/865</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/698/865 [2]</TD>
            <TD>Halo streams in the SDSS-DR7 (Klement+, 2009)</TD>
            <TD>SDSS-I was an imaging and spectroscopic survey that began routine operations in 2000 April and continued through 2005 June. The SDSS, and its extensions, uses a dedicated 2.5m telescope located at the Apache Point Observatory in New Mexico. One of three subsurveys carried out during the first extension of the SDSS, known as SDSS-II, the Sloan Extension for Galactic Understanding and Exploration (SEGUE), ran from 2005 July to 2008 June. SEGUE obtained some 250000 medium-resolution spectra of stars in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865#2</TD>
            <TD>2011-10-18T10:28:11Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/698/865&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/698/865</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/698/865 [table3]</TD>
            <TD>Halo streams in the SDSS-DR7 (Klement+, 2009)</TD>
            <TD>SDSS-I was an imaging and spectroscopic survey that began routine operations in 2000 April and continued through 2005 June. The SDSS, and its extensions, uses a dedicated 2.5m telescope located at the Apache Point Observatory in New Mexico. One of three subsurveys carried out during the first extension of the SDSS, known as SDSS-II, the Sloan Extension for Galactic Understanding and Exploration (SEGUE), ran from 2005 July to 2008 June. SEGUE obtained some 250000 medium-resolution spectra of stars in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865#table3</TD>
            <TD>2011-10-18T10:28:11Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/698/865</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/698/865&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/698/865</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/543/178 [1]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#1</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/543/178</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/543/178 [2]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#2</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table3]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table3</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table2]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table2</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table7]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table7</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table4]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table4</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table5]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table5</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table6]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table6</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMM/M31 [1]</TD>
            <TD>XMM-Newton M31 Survey Source Catalog</TD>
            <TD>This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10^34 erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogues and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmmxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmmxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m31xmmxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmmxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMM/M31 [2]</TD>
            <TD>XMM-Newton M31 Survey Source Catalog</TD>
            <TD>This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10^34 erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogues and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmmxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m31xmmxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMM/M31 [3]</TD>
            <TD>XMM-Newton M31 Survey Source Catalog</TD>
            <TD>This table contains a source catalog based on XMM-Newton observations of the bright Local Group spiral galaxy M 31. In an analysis of XMM archival observations of M 31, the authors studied the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5 keV luminosity of 4.4 x 10^34 erg/s. EPIC hardness ratios and optical and radio information were used to distinguish between different source classes. The survey detected 856 sources in an area of 1.24 square degrees. The authors correlated their sources with earlier M 31 X-ray catalogues and used information from optical, infra-red and radio wavelengths. As sources within M 31, they detected 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys revealed transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which might either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate might be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 are foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources which are not connected with M31. In a second paper, the authors presented an extension to the original 2005 XMM-Newton X-ray source catalog of M 31 which contained 39 newly found sources. These sources have been added to the original 856 sources to make a combined catalog of 895 X-ray sources which is contained herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31xmmxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31xmmxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m31xmmxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31xmmxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/543/178 [1]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#1</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/543/178</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/543/178 [2]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#2</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table3]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table3</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table2]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table2</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table7]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table7</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table4]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table4</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table5]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table5</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/543/178 [table6]</TD>
            <TD>Nearby Optical Galaxy (NOG) sample (Giuricin+, 2000)</TD>
            <TD>In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz&lt;=6000km/s) and magnitude-limited (B&lt;=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|&gt;20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178#table6</TD>
            <TD>2012-11-13T07:13:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/543/178</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/543/178&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/543/178</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/701/508 [1]</TD>
            <TD>5000 AGNs behind the Magellanic clouds (Kozlowski+, 2009)</TD>
            <TD>We combine results from studies of the extragalactic NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey, 1999ASPC..191..111J) Bootes field based on the IRAC Shallow Survey (Eisenhardt et al. 2004ApJS..154...48E), the Spitzer Deep Wide Field Survey (SDWFS; Ashby et al. 2009, Cat J/ApJ/701/428), and the AGN and Galaxy Evolution Survey (AGES; C. S. Kochanek et al. 2009, in prep) with the Spitzer SAGE Survey data (Meixner et al. 2006, Cat. J/AJ/132/2268) and OGLE-III optical survey (Udalski et al. 2008AcA....58...69U, 2008AcA....58...89U, 2008AcA....58..329U) of the LMC to develop a simple method of selecting AGNs in these dense stellar fields.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508#1</TD>
            <TD>2011-10-23T14:43:22Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/701/508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/701/508 [2]</TD>
            <TD>5000 AGNs behind the Magellanic clouds (Kozlowski+, 2009)</TD>
            <TD>We combine results from studies of the extragalactic NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey, 1999ASPC..191..111J) Bootes field based on the IRAC Shallow Survey (Eisenhardt et al. 2004ApJS..154...48E), the Spitzer Deep Wide Field Survey (SDWFS; Ashby et al. 2009, Cat J/ApJ/701/428), and the AGN and Galaxy Evolution Survey (AGES; C. S. Kochanek et al. 2009, in prep) with the Spitzer SAGE Survey data (Meixner et al. 2006, Cat. J/AJ/132/2268) and OGLE-III optical survey (Udalski et al. 2008AcA....58...69U, 2008AcA....58...89U, 2008AcA....58..329U) of the LMC to develop a simple method of selecting AGNs in these dense stellar fields.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508#2</TD>
            <TD>2011-10-23T14:43:22Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/701/508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/508 [agn_mc]</TD>
            <TD>5000 AGNs behind the Magellanic clouds (Kozlowski+, 2009)</TD>
            <TD>We combine results from studies of the extragalactic NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey, 1999ASPC..191..111J) Bootes field based on the IRAC Shallow Survey (Eisenhardt et al. 2004ApJS..154...48E), the Spitzer Deep Wide Field Survey (SDWFS; Ashby et al. 2009, Cat J/ApJ/701/428), and the AGN and Galaxy Evolution Survey (AGES; C. S. Kochanek et al. 2009, in prep) with the Spitzer SAGE Survey data (Meixner et al. 2006, Cat. J/AJ/132/2268) and OGLE-III optical survey (Udalski et al. 2008AcA....58...69U, 2008AcA....58...89U, 2008AcA....58..329U) of the LMC to develop a simple method of selecting AGNs in these dense stellar fields.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508#agn_mc</TD>
            <TD>2011-10-23T14:43:22Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/552/427 [1]</TD>
            <TD>Galaxy groups a intermediate redshifts (Carlberg+, 2001)</TD>
            <TD>A group is defined here as a collection of three or more galaxies, above a fixed minimum luminosity, that meet a set of positional requirements designed to minimize chance associations. Here we specifically seek virialized groups, which are collapsed and hence quite dense compared to groups that are only required to be bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427#1</TD>
            <TD>2012-11-13T07:13:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/552/427</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/552/427</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/552/427 [2]</TD>
            <TD>Galaxy groups a intermediate redshifts (Carlberg+, 2001)</TD>
            <TD>A group is defined here as a collection of three or more galaxies, above a fixed minimum luminosity, that meet a set of positional requirements designed to minimize chance associations. Here we specifically seek virialized groups, which are collapsed and hence quite dense compared to groups that are only required to be bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427#2</TD>
            <TD>2012-11-13T07:13:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/552/427&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/552/427</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/552/427 [table1]</TD>
            <TD>Galaxy groups a intermediate redshifts (Carlberg+, 2001)</TD>
            <TD>A group is defined here as a collection of three or more galaxies, above a fixed minimum luminosity, that meet a set of positional requirements designed to minimize chance associations. Here we specifically seek virialized groups, which are collapsed and hence quite dense compared to groups that are only required to be bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427#table1</TD>
            <TD>2012-11-13T07:13:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/552/427&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/552/427</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M33CHASE [1]</TD>
            <TD>M 33 Chandra ACIS Survey (ChASeM33) Final Source Catalog</TD>
            <TD>This table contains the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers ~70% of the D&lt;sub&gt;25&lt;/sub&gt; isophote (radial extent ~ 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of ~2.4 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up Multiple Mirror Telescope (MMT) spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, in the reference paper, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 were presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and 1.6 x 10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (for an assumed distance D to M33 of 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. The list of all the Chandra ACIS observations that were used in the construction of this source catalog is given in table 2 of the 2011 reference paper. X-ray source properties, such as counts, dns values, and photon fluxes were computed in the following energy bands: &lt;pre&gt; Band Energy Range (keV) 1 0.5 - 8.0 2 0.5 - 2.0 3 2.0 - 8.0 4 0.35- 8.0 5 0.35- 1.1 6 1.1 - 2.6 7 2.6 - 8.0 8 0.35- 2.0 &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33chase#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33chase</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33chase&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33chase.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M33CHASE [2]</TD>
            <TD>M 33 Chandra ACIS Survey (ChASeM33) Final Source Catalog</TD>
            <TD>This table contains the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers ~70% of the D&lt;sub&gt;25&lt;/sub&gt; isophote (radial extent ~ 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of ~2.4 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up Multiple Mirror Telescope (MMT) spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, in the reference paper, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 were presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and 1.6 x 10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (for an assumed distance D to M33 of 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. The list of all the Chandra ACIS observations that were used in the construction of this source catalog is given in table 2 of the 2011 reference paper. X-ray source properties, such as counts, dns values, and photon fluxes were computed in the following energy bands: &lt;pre&gt; Band Energy Range (keV) 1 0.5 - 8.0 2 0.5 - 2.0 3 2.0 - 8.0 4 0.35- 8.0 5 0.35- 1.1 6 1.1 - 2.6 7 2.6 - 8.0 8 0.35- 2.0 &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33chase#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33chase</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33chase&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33chase.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M33CHASE [3]</TD>
            <TD>M 33 Chandra ACIS Survey (ChASeM33) Final Source Catalog</TD>
            <TD>This table contains the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers ~70% of the D&lt;sub&gt;25&lt;/sub&gt; isophote (radial extent ~ 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of ~2.4 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up Multiple Mirror Telescope (MMT) spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, in the reference paper, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 were presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and 1.6 x 10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (for an assumed distance D to M33 of 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. The list of all the Chandra ACIS observations that were used in the construction of this source catalog is given in table 2 of the 2011 reference paper. X-ray source properties, such as counts, dns values, and photon fluxes were computed in the following energy bands: &lt;pre&gt; Band Energy Range (keV) 1 0.5 - 8.0 2 0.5 - 2.0 3 2.0 - 8.0 4 0.35- 8.0 5 0.35- 1.1 6 1.1 - 2.6 7 2.6 - 8.0 8 0.35- 2.0 &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33chase#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33chase</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33chase&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33chase.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/552/427 [1]</TD>
            <TD>Galaxy groups a intermediate redshifts (Carlberg+, 2001)</TD>
            <TD>A group is defined here as a collection of three or more galaxies, above a fixed minimum luminosity, that meet a set of positional requirements designed to minimize chance associations. Here we specifically seek virialized groups, which are collapsed and hence quite dense compared to groups that are only required to be bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427#1</TD>
            <TD>2012-11-13T07:13:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/552/427</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/552/427</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/552/427 [2]</TD>
            <TD>Galaxy groups a intermediate redshifts (Carlberg+, 2001)</TD>
            <TD>A group is defined here as a collection of three or more galaxies, above a fixed minimum luminosity, that meet a set of positional requirements designed to minimize chance associations. Here we specifically seek virialized groups, which are collapsed and hence quite dense compared to groups that are only required to be bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427#2</TD>
            <TD>2012-11-13T07:13:09Z</TD>
            <TD>#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/552/427&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/552/427</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/552/427 [table1]</TD>
            <TD>Galaxy groups a intermediate redshifts (Carlberg+, 2001)</TD>
            <TD>A group is defined here as a collection of three or more galaxies, above a fixed minimum luminosity, that meet a set of positional requirements designed to minimize chance associations. Here we specifically seek virialized groups, which are collapsed and hence quite dense compared to groups that are only required to be bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427#table1</TD>
            <TD>2012-11-13T07:13:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/552/427&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/552/427</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/701/508 [1]</TD>
            <TD>5000 AGNs behind the Magellanic clouds (Kozlowski+, 2009)</TD>
            <TD>We combine results from studies of the extragalactic NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey, 1999ASPC..191..111J) Bootes field based on the IRAC Shallow Survey (Eisenhardt et al. 2004ApJS..154...48E), the Spitzer Deep Wide Field Survey (SDWFS; Ashby et al. 2009, Cat J/ApJ/701/428), and the AGN and Galaxy Evolution Survey (AGES; C. S. Kochanek et al. 2009, in prep) with the Spitzer SAGE Survey data (Meixner et al. 2006, Cat. J/AJ/132/2268) and OGLE-III optical survey (Udalski et al. 2008AcA....58...69U, 2008AcA....58...89U, 2008AcA....58..329U) of the LMC to develop a simple method of selecting AGNs in these dense stellar fields.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508#1</TD>
            <TD>2011-10-23T14:43:22Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/701/508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/701/508 [2]</TD>
            <TD>5000 AGNs behind the Magellanic clouds (Kozlowski+, 2009)</TD>
            <TD>We combine results from studies of the extragalactic NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey, 1999ASPC..191..111J) Bootes field based on the IRAC Shallow Survey (Eisenhardt et al. 2004ApJS..154...48E), the Spitzer Deep Wide Field Survey (SDWFS; Ashby et al. 2009, Cat J/ApJ/701/428), and the AGN and Galaxy Evolution Survey (AGES; C. S. Kochanek et al. 2009, in prep) with the Spitzer SAGE Survey data (Meixner et al. 2006, Cat. J/AJ/132/2268) and OGLE-III optical survey (Udalski et al. 2008AcA....58...69U, 2008AcA....58...89U, 2008AcA....58..329U) of the LMC to develop a simple method of selecting AGNs in these dense stellar fields.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508#2</TD>
            <TD>2011-10-23T14:43:22Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/701/508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/508 [agn_mc]</TD>
            <TD>5000 AGNs behind the Magellanic clouds (Kozlowski+, 2009)</TD>
            <TD>We combine results from studies of the extragalactic NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey, 1999ASPC..191..111J) Bootes field based on the IRAC Shallow Survey (Eisenhardt et al. 2004ApJS..154...48E), the Spitzer Deep Wide Field Survey (SDWFS; Ashby et al. 2009, Cat J/ApJ/701/428), and the AGN and Galaxy Evolution Survey (AGES; C. S. Kochanek et al. 2009, in prep) with the Spitzer SAGE Survey data (Meixner et al. 2006, Cat. J/AJ/132/2268) and OGLE-III optical survey (Udalski et al. 2008AcA....58...69U, 2008AcA....58...89U, 2008AcA....58..329U) of the LMC to develop a simple method of selecting AGNs in these dense stellar fields.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508#agn_mc</TD>
            <TD>2011-10-23T14:43:22Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/552/427 [1]</TD>
            <TD>Galaxy groups a intermediate redshifts (Carlberg+, 2001)</TD>
            <TD>A group is defined here as a collection of three or more galaxies, above a fixed minimum luminosity, that meet a set of positional requirements designed to minimize chance associations. Here we specifically seek virialized groups, which are collapsed and hence quite dense compared to groups that are only required to be bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427#1</TD>
            <TD>2012-11-13T07:13:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/552/427</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/552/427</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/552/427 [2]</TD>
            <TD>Galaxy groups a intermediate redshifts (Carlberg+, 2001)</TD>
            <TD>A group is defined here as a collection of three or more galaxies, above a fixed minimum luminosity, that meet a set of positional requirements designed to minimize chance associations. Here we specifically seek virialized groups, which are collapsed and hence quite dense compared to groups that are only required to be bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427#2</TD>
            <TD>2012-11-13T07:13:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/552/427&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/552/427</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/552/427 [table1]</TD>
            <TD>Galaxy groups a intermediate redshifts (Carlberg+, 2001)</TD>
            <TD>A group is defined here as a collection of three or more galaxies, above a fixed minimum luminosity, that meet a set of positional requirements designed to minimize chance associations. Here we specifically seek virialized groups, which are collapsed and hence quite dense compared to groups that are only required to be bound.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427#table1</TD>
            <TD>2012-11-13T07:13:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/552/427</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/552/427&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/552/427</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M33CHASE [1]</TD>
            <TD>M 33 Chandra ACIS Survey (ChASeM33) Final Source Catalog</TD>
            <TD>This table contains the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers ~70% of the D&lt;sub&gt;25&lt;/sub&gt; isophote (radial extent ~ 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of ~2.4 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up Multiple Mirror Telescope (MMT) spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, in the reference paper, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 were presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and 1.6 x 10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (for an assumed distance D to M33 of 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. The list of all the Chandra ACIS observations that were used in the construction of this source catalog is given in table 2 of the 2011 reference paper. X-ray source properties, such as counts, dns values, and photon fluxes were computed in the following energy bands: &lt;pre&gt; Band Energy Range (keV) 1 0.5 - 8.0 2 0.5 - 2.0 3 2.0 - 8.0 4 0.35- 8.0 5 0.35- 1.1 6 1.1 - 2.6 7 2.6 - 8.0 8 0.35- 2.0 &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33chase#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33chase</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33chase&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33chase.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M33CHASE [2]</TD>
            <TD>M 33 Chandra ACIS Survey (ChASeM33) Final Source Catalog</TD>
            <TD>This table contains the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers ~70% of the D&lt;sub&gt;25&lt;/sub&gt; isophote (radial extent ~ 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of ~2.4 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up Multiple Mirror Telescope (MMT) spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, in the reference paper, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 were presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and 1.6 x 10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (for an assumed distance D to M33 of 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. The list of all the Chandra ACIS observations that were used in the construction of this source catalog is given in table 2 of the 2011 reference paper. X-ray source properties, such as counts, dns values, and photon fluxes were computed in the following energy bands: &lt;pre&gt; Band Energy Range (keV) 1 0.5 - 8.0 2 0.5 - 2.0 3 2.0 - 8.0 4 0.35- 8.0 5 0.35- 1.1 6 1.1 - 2.6 7 2.6 - 8.0 8 0.35- 2.0 &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33chase#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33chase</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33chase&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33chase.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M33CHASE [3]</TD>
            <TD>M 33 Chandra ACIS Survey (ChASeM33) Final Source Catalog</TD>
            <TD>This table contains the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers ~70% of the D&lt;sub&gt;25&lt;/sub&gt; isophote (radial extent ~ 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of ~2.4 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up Multiple Mirror Telescope (MMT) spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, in the reference paper, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 were presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and 1.6 x 10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (for an assumed distance D to M33 of 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. The list of all the Chandra ACIS observations that were used in the construction of this source catalog is given in table 2 of the 2011 reference paper. X-ray source properties, such as counts, dns values, and photon fluxes were computed in the following energy bands: &lt;pre&gt; Band Energy Range (keV) 1 0.5 - 8.0 2 0.5 - 2.0 3 2.0 - 8.0 4 0.35- 8.0 5 0.35- 1.1 6 1.1 - 2.6 7 2.6 - 8.0 8 0.35- 2.0 &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33chase#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33chase</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33chase&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33chase.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/154/553 [1]</TD>
            <TD>Inner galaxy massive star formation regions (Sewilo+, 2004)</TD>
            <TD>The observations were made on 2002 November 1-3, 8-9, and 14 with the Green Bank Telescope (GBT). Seventy-two sources were selected from the IRAS Point Source Catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553#1</TD>
            <TD>2012-11-13T07:21:13Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/154/553</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/154/553</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/154/553 [2]</TD>
            <TD>Inner galaxy massive star formation regions (Sewilo+, 2004)</TD>
            <TD>The observations were made on 2002 November 1-3, 8-9, and 14 with the Green Bank Telescope (GBT). Seventy-two sources were selected from the IRAS Point Source Catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553#2</TD>
            <TD>2012-11-13T07:21:13Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/154/553&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/154/553</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/154/553 [sources]</TD>
            <TD>Inner galaxy massive star formation regions (Sewilo+, 2004)</TD>
            <TD>The observations were made on 2002 November 1-3, 8-9, and 14 with the Green Bank Telescope (GBT). Seventy-two sources were selected from the IRAS Point Source Catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553#sources</TD>
            <TD>2012-11-13T07:21:13Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/154/553&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/154/553</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/701/508 [1]</TD>
            <TD>5000 AGNs behind the Magellanic clouds (Kozlowski+, 2009)</TD>
            <TD>We combine results from studies of the extragalactic NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey, 1999ASPC..191..111J) Bootes field based on the IRAC Shallow Survey (Eisenhardt et al. 2004ApJS..154...48E), the Spitzer Deep Wide Field Survey (SDWFS; Ashby et al. 2009, Cat J/ApJ/701/428), and the AGN and Galaxy Evolution Survey (AGES; C. S. Kochanek et al. 2009, in prep) with the Spitzer SAGE Survey data (Meixner et al. 2006, Cat. J/AJ/132/2268) and OGLE-III optical survey (Udalski et al. 2008AcA....58...69U, 2008AcA....58...89U, 2008AcA....58..329U) of the LMC to develop a simple method of selecting AGNs in these dense stellar fields.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508#1</TD>
            <TD>2011-10-23T14:43:22Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/701/508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/701/508 [2]</TD>
            <TD>5000 AGNs behind the Magellanic clouds (Kozlowski+, 2009)</TD>
            <TD>We combine results from studies of the extragalactic NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey, 1999ASPC..191..111J) Bootes field based on the IRAC Shallow Survey (Eisenhardt et al. 2004ApJS..154...48E), the Spitzer Deep Wide Field Survey (SDWFS; Ashby et al. 2009, Cat J/ApJ/701/428), and the AGN and Galaxy Evolution Survey (AGES; C. S. Kochanek et al. 2009, in prep) with the Spitzer SAGE Survey data (Meixner et al. 2006, Cat. J/AJ/132/2268) and OGLE-III optical survey (Udalski et al. 2008AcA....58...69U, 2008AcA....58...89U, 2008AcA....58..329U) of the LMC to develop a simple method of selecting AGNs in these dense stellar fields.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508#2</TD>
            <TD>2011-10-23T14:43:22Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/701/508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/508 [agn_mc]</TD>
            <TD>5000 AGNs behind the Magellanic clouds (Kozlowski+, 2009)</TD>
            <TD>We combine results from studies of the extragalactic NOAO Deep Wide Field Survey (NDWFS; Jannuzi &amp; Dey, 1999ASPC..191..111J) Bootes field based on the IRAC Shallow Survey (Eisenhardt et al. 2004ApJS..154...48E), the Spitzer Deep Wide Field Survey (SDWFS; Ashby et al. 2009, Cat J/ApJ/701/428), and the AGN and Galaxy Evolution Survey (AGES; C. S. Kochanek et al. 2009, in prep) with the Spitzer SAGE Survey data (Meixner et al. 2006, Cat. J/AJ/132/2268) and OGLE-III optical survey (Udalski et al. 2008AcA....58...69U, 2008AcA....58...89U, 2008AcA....58..329U) of the LMC to develop a simple method of selecting AGNs in these dense stellar fields.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508#agn_mc</TD>
            <TD>2011-10-23T14:43:22Z</TD>
            <TD>#AGN#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/154/553 [1]</TD>
            <TD>Inner galaxy massive star formation regions (Sewilo+, 2004)</TD>
            <TD>The observations were made on 2002 November 1-3, 8-9, and 14 with the Green Bank Telescope (GBT). Seventy-two sources were selected from the IRAS Point Source Catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553#1</TD>
            <TD>2012-11-13T07:21:13Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/154/553</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/154/553</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/154/553 [2]</TD>
            <TD>Inner galaxy massive star formation regions (Sewilo+, 2004)</TD>
            <TD>The observations were made on 2002 November 1-3, 8-9, and 14 with the Green Bank Telescope (GBT). Seventy-two sources were selected from the IRAS Point Source Catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553#2</TD>
            <TD>2012-11-13T07:21:13Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/154/553&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/154/553</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/154/553 [sources]</TD>
            <TD>Inner galaxy massive star formation regions (Sewilo+, 2004)</TD>
            <TD>The observations were made on 2002 November 1-3, 8-9, and 14 with the Green Bank Telescope (GBT). Seventy-two sources were selected from the IRAS Point Source Catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553#sources</TD>
            <TD>2012-11-13T07:21:13Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/154/553&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/154/553</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/2782 [1]</TD>
            <TD>Star formation efficiency in nearby galaxies (Leroy+, 2008)</TD>
            <TD>We assemble maps and radial profiles of the necessary quantities in 23 nearby, star-forming galaxies that we list in order of increasing stellar mass in Table 2. These are galaxies for which we could compile the necessary data, which means the overlap of THINGS, SINGS, the GALEX Nearby Galaxy Survey (NGS), and (for spirals) either BIMA SONG or HERACLES.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782#1</TD>
            <TD>2011-09-12T22:55:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/2782</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2782</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/2782 [2]</TD>
            <TD>Star formation efficiency in nearby galaxies (Leroy+, 2008)</TD>
            <TD>We assemble maps and radial profiles of the necessary quantities in 23 nearby, star-forming galaxies that we list in order of increasing stellar mass in Table 2. These are galaxies for which we could compile the necessary data, which means the overlap of THINGS, SINGS, the GALEX Nearby Galaxy Survey (NGS), and (for spirals) either BIMA SONG or HERACLES.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782#2</TD>
            <TD>2011-09-12T22:55:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/2782&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2782</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/2782 [sample]</TD>
            <TD>Star formation efficiency in nearby galaxies (Leroy+, 2008)</TD>
            <TD>We assemble maps and radial profiles of the necessary quantities in 23 nearby, star-forming galaxies that we list in order of increasing stellar mass in Table 2. These are galaxies for which we could compile the necessary data, which means the overlap of THINGS, SINGS, the GALEX Nearby Galaxy Survey (NGS), and (for spirals) either BIMA SONG or HERACLES.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782#sample</TD>
            <TD>2011-09-12T22:55:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/2782&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2782</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/154/553 [1]</TD>
            <TD>Inner galaxy massive star formation regions (Sewilo+, 2004)</TD>
            <TD>The observations were made on 2002 November 1-3, 8-9, and 14 with the Green Bank Telescope (GBT). Seventy-two sources were selected from the IRAS Point Source Catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553#1</TD>
            <TD>2012-11-13T07:21:13Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/154/553</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/154/553</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/154/553 [2]</TD>
            <TD>Inner galaxy massive star formation regions (Sewilo+, 2004)</TD>
            <TD>The observations were made on 2002 November 1-3, 8-9, and 14 with the Green Bank Telescope (GBT). Seventy-two sources were selected from the IRAS Point Source Catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553#2</TD>
            <TD>2012-11-13T07:21:13Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/154/553&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/154/553</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/154/553 [sources]</TD>
            <TD>Inner galaxy massive star formation regions (Sewilo+, 2004)</TD>
            <TD>The observations were made on 2002 November 1-3, 8-9, and 14 with the Green Bank Telescope (GBT). Seventy-two sources were selected from the IRAS Point Source Catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553#sources</TD>
            <TD>2012-11-13T07:21:13Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/154/553</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/154/553&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/154/553</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M33CHASE [1]</TD>
            <TD>M 33 Chandra ACIS Survey (ChASeM33) Final Source Catalog</TD>
            <TD>This table contains the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers ~70% of the D&lt;sub&gt;25&lt;/sub&gt; isophote (radial extent ~ 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of ~2.4 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up Multiple Mirror Telescope (MMT) spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, in the reference paper, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 were presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and 1.6 x 10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (for an assumed distance D to M33 of 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. The list of all the Chandra ACIS observations that were used in the construction of this source catalog is given in table 2 of the 2011 reference paper. X-ray source properties, such as counts, dns values, and photon fluxes were computed in the following energy bands: &lt;pre&gt; Band Energy Range (keV) 1 0.5 - 8.0 2 0.5 - 2.0 3 2.0 - 8.0 4 0.35- 8.0 5 0.35- 1.1 6 1.1 - 2.6 7 2.6 - 8.0 8 0.35- 2.0 &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33chase#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33chase</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33chase&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33chase.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M33CHASE [2]</TD>
            <TD>M 33 Chandra ACIS Survey (ChASeM33) Final Source Catalog</TD>
            <TD>This table contains the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers ~70% of the D&lt;sub&gt;25&lt;/sub&gt; isophote (radial extent ~ 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of ~2.4 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up Multiple Mirror Telescope (MMT) spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, in the reference paper, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 were presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and 1.6 x 10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (for an assumed distance D to M33 of 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. The list of all the Chandra ACIS observations that were used in the construction of this source catalog is given in table 2 of the 2011 reference paper. X-ray source properties, such as counts, dns values, and photon fluxes were computed in the following energy bands: &lt;pre&gt; Band Energy Range (keV) 1 0.5 - 8.0 2 0.5 - 2.0 3 2.0 - 8.0 4 0.35- 8.0 5 0.35- 1.1 6 1.1 - 2.6 7 2.6 - 8.0 8 0.35- 2.0 &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33chase#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33chase</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33chase&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33chase.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M33CHASE [3]</TD>
            <TD>M 33 Chandra ACIS Survey (ChASeM33) Final Source Catalog</TD>
            <TD>This table contains the final source catalog of the Chandra ACIS Survey of M33 (ChASeM33). With a total exposure time of 1.4 Ms, ChASeM33 covers ~70% of the D&lt;sub&gt;25&lt;/sub&gt; isophote (radial extent ~ 4.0 kpc) of M33 and provides the deepest, most complete, and detailed look at a spiral galaxy in X-rays. The source catalog includes 662 sources, reaches a limiting unabsorbed luminosity of ~2.4 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.35-8.0 keV energy band, and contains source positions, source net counts, fluxes and significances in several energy bands, and information on source variability. The analysis challenges posed by ChASeM33 and the techniques adopted to address these challenges are discussed. To constrain the nature of the detected X-ray source, hardness ratios were constructed and spectra were fit for 254 sources, follow-up Multiple Mirror Telescope (MMT) spectra of 116 sources were acquired, and cross-correlations with previous X-ray catalogs and other multi-wavelength data were generated. Based on this effort, 183 of the 662 ChASeM33 sources could be identified. Finally, in the reference paper, the luminosity function (LF) for the detected point sources as well as the one for the X-ray binaries (XRBs) in M33 were presented. The LFs in the soft band (0.5-2.0 keV) and the hard band (2.0-8.0 keV) have a limiting luminosity at the 90% completeness limit of 4.0 x 10&lt;sup&gt;34&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; and 1.6 x 10&lt;sup&gt;35&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (for an assumed distance D to M33 of 817 kpc), respectively, which is significantly lower than what was reported by previous XRB population studies in galaxies more distant than M33. The resulting distribution is consistent with a dominant population of high-mass XRBs as would be expected for M33. The list of all the Chandra ACIS observations that were used in the construction of this source catalog is given in table 2 of the 2011 reference paper. X-ray source properties, such as counts, dns values, and photon fluxes were computed in the following energy bands: &lt;pre&gt; Band Energy Range (keV) 1 0.5 - 8.0 2 0.5 - 2.0 3 2.0 - 8.0 4 0.35- 8.0 5 0.35- 1.1 6 1.1 - 2.6 7 2.6 - 8.0 8 0.35- 2.0 &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33chase#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33chase</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33chase&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33chase.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/2782 [1]</TD>
            <TD>Star formation efficiency in nearby galaxies (Leroy+, 2008)</TD>
            <TD>We assemble maps and radial profiles of the necessary quantities in 23 nearby, star-forming galaxies that we list in order of increasing stellar mass in Table 2. These are galaxies for which we could compile the necessary data, which means the overlap of THINGS, SINGS, the GALEX Nearby Galaxy Survey (NGS), and (for spirals) either BIMA SONG or HERACLES.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782#1</TD>
            <TD>2011-09-12T22:55:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/2782</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2782</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/2782 [2]</TD>
            <TD>Star formation efficiency in nearby galaxies (Leroy+, 2008)</TD>
            <TD>We assemble maps and radial profiles of the necessary quantities in 23 nearby, star-forming galaxies that we list in order of increasing stellar mass in Table 2. These are galaxies for which we could compile the necessary data, which means the overlap of THINGS, SINGS, the GALEX Nearby Galaxy Survey (NGS), and (for spirals) either BIMA SONG or HERACLES.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782#2</TD>
            <TD>2011-09-12T22:55:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/2782&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2782</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/2782 [sample]</TD>
            <TD>Star formation efficiency in nearby galaxies (Leroy+, 2008)</TD>
            <TD>We assemble maps and radial profiles of the necessary quantities in 23 nearby, star-forming galaxies that we list in order of increasing stellar mass in Table 2. These are galaxies for which we could compile the necessary data, which means the overlap of THINGS, SINGS, the GALEX Nearby Galaxy Survey (NGS), and (for spirals) either BIMA SONG or HERACLES.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782#sample</TD>
            <TD>2011-09-12T22:55:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/2782&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2782</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/297/617 [1]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#1</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/297/617</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/297/617 [2]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#2</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/297/617&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/297/617 [table1]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#table1</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/297/617&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/297/617 [table3]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#table3</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/297/617&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/297/617 [table2]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#table2</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/297/617&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChandraM33 [1]</TD>
            <TD>M 33 Chandra X-Ray Point Source Catalog</TD>
            <TD>This database table contains a source list for three Chandra observations of the Local Group galaxy M33. The observations were centered on the nucleus and on the star-forming region NGC 604. A total of 261 sources were detected in an area of about 0.2 square degrees down to a flux limit of 3 x 10^-16 erg/s/cm^2, which corresponds to a luminosity of ~2 x 10^34 erg/s at a distance of 840 kpc. The luminosity functions of the X-ray sources observed in M33 have been constructed and are consistent with those of other star-forming galaxies, taking into account background contamination. In addtion, the combination of X-ray color analysis and the existence of "blue" optical counterparts stronly indicates that the X-ray point source population in M33 consists of young objects. Above 3 x 10^35 erg/s, there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. Notice that each of the 261 X-ray sources in the source list has 3 entries in this table, one for each separate Chandra observation, making a total of 783 entries. The Chandra datasets from which this source list was compiled are available by &lt;a href="/db-perl/W3Browse/w3query.pl?tablehead=name%3Dheasarc_chanmaster&amp;sortvar=obsid&amp;bparam_obsid=786%3B+1730%3B+2023"&gt;querying CHANMASTER for obsids 786, 1730, and 2023&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33cxoxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33cxoxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33cxoxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33cxoxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChandraM33 [2]</TD>
            <TD>M 33 Chandra X-Ray Point Source Catalog</TD>
            <TD>This database table contains a source list for three Chandra observations of the Local Group galaxy M33. The observations were centered on the nucleus and on the star-forming region NGC 604. A total of 261 sources were detected in an area of about 0.2 square degrees down to a flux limit of 3 x 10^-16 erg/s/cm^2, which corresponds to a luminosity of ~2 x 10^34 erg/s at a distance of 840 kpc. The luminosity functions of the X-ray sources observed in M33 have been constructed and are consistent with those of other star-forming galaxies, taking into account background contamination. In addtion, the combination of X-ray color analysis and the existence of "blue" optical counterparts stronly indicates that the X-ray point source population in M33 consists of young objects. Above 3 x 10^35 erg/s, there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. Notice that each of the 261 X-ray sources in the source list has 3 entries in this table, one for each separate Chandra observation, making a total of 783 entries. The Chandra datasets from which this source list was compiled are available by &lt;a href="/db-perl/W3Browse/w3query.pl?tablehead=name%3Dheasarc_chanmaster&amp;sortvar=obsid&amp;bparam_obsid=786%3B+1730%3B+2023"&gt;querying CHANMASTER for obsids 786, 1730, and 2023&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33cxoxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33cxoxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33cxoxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33cxoxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChandraM33 [3]</TD>
            <TD>M 33 Chandra X-Ray Point Source Catalog</TD>
            <TD>This database table contains a source list for three Chandra observations of the Local Group galaxy M33. The observations were centered on the nucleus and on the star-forming region NGC 604. A total of 261 sources were detected in an area of about 0.2 square degrees down to a flux limit of 3 x 10^-16 erg/s/cm^2, which corresponds to a luminosity of ~2 x 10^34 erg/s at a distance of 840 kpc. The luminosity functions of the X-ray sources observed in M33 have been constructed and are consistent with those of other star-forming galaxies, taking into account background contamination. In addtion, the combination of X-ray color analysis and the existence of "blue" optical counterparts stronly indicates that the X-ray point source population in M33 consists of young objects. Above 3 x 10^35 erg/s, there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. Notice that each of the 261 X-ray sources in the source list has 3 entries in this table, one for each separate Chandra observation, making a total of 783 entries. The Chandra datasets from which this source list was compiled are available by &lt;a href="/db-perl/W3Browse/w3query.pl?tablehead=name%3Dheasarc_chanmaster&amp;sortvar=obsid&amp;bparam_obsid=786%3B+1730%3B+2023"&gt;querying CHANMASTER for obsids 786, 1730, and 2023&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33cxoxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33cxoxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33cxoxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33cxoxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/2782 [1]</TD>
            <TD>Star formation efficiency in nearby galaxies (Leroy+, 2008)</TD>
            <TD>We assemble maps and radial profiles of the necessary quantities in 23 nearby, star-forming galaxies that we list in order of increasing stellar mass in Table 2. These are galaxies for which we could compile the necessary data, which means the overlap of THINGS, SINGS, the GALEX Nearby Galaxy Survey (NGS), and (for spirals) either BIMA SONG or HERACLES.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782#1</TD>
            <TD>2011-09-12T22:55:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/2782</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2782</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/2782 [2]</TD>
            <TD>Star formation efficiency in nearby galaxies (Leroy+, 2008)</TD>
            <TD>We assemble maps and radial profiles of the necessary quantities in 23 nearby, star-forming galaxies that we list in order of increasing stellar mass in Table 2. These are galaxies for which we could compile the necessary data, which means the overlap of THINGS, SINGS, the GALEX Nearby Galaxy Survey (NGS), and (for spirals) either BIMA SONG or HERACLES.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782#2</TD>
            <TD>2011-09-12T22:55:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/2782&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2782</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/2782 [sample]</TD>
            <TD>Star formation efficiency in nearby galaxies (Leroy+, 2008)</TD>
            <TD>We assemble maps and radial profiles of the necessary quantities in 23 nearby, star-forming galaxies that we list in order of increasing stellar mass in Table 2. These are galaxies for which we could compile the necessary data, which means the overlap of THINGS, SINGS, the GALEX Nearby Galaxy Survey (NGS), and (for spirals) either BIMA SONG or HERACLES.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782#sample</TD>
            <TD>2011-09-12T22:55:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2782</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/2782&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2782</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/297/617 [1]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#1</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/297/617</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/297/617 [2]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#2</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/297/617&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/297/617 [table1]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#table1</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/297/617&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/297/617 [table3]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#table3</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/297/617&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/297/617 [table2]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#table2</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/297/617&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/297/617 [1]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#1</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/297/617</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/297/617 [2]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#2</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/297/617&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/297/617 [table1]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#table1</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/297/617&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/297/617 [table3]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#table3</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/297/617&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/297/617 [table2]</TD>
            <TD>Hydra/Antlia extension redshifts (Kraan-Korteweg+, 1995)</TD>
            <TD>Spectroscopic observations have been carried out for galaxies in the Milky Way with the 1.9m telescope of the South African Astronomical Observatory (SAAO). The galaxies were selected from a deep optical galaxy search covering 266deg&lt;~l&lt;~296deg, |b|&lt;~10deg (Kraan-Korteweg 1994). This is in the extension of the Hydra and Antlia clusters and in the approximate direction of the dipole anisotropy in the Cosmic Microwave Background radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617#table2</TD>
            <TD>2012-11-13T13:38:29Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+A/297/617</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/297/617&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/297/617</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Hickson(Gal) [1]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Individual Galaxies Data</TD>
            <TD>The HCGGALAXY database table is based on the Hickson Catalog of Compact Groups, and contains data on 463 galaxies in 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Astrometry, photometry, and morphological types, derived from CCD images, are presented for the 463 galaxies. Radial velocities are given for 457 of the 463 galaxies: more than 84% of the galaxies measured have radial velocities that are within 1000 km/s of the group median velocity. Morphological information derived from either an isophotal analysis or from a visual inspection of images is given for 210 of the 463 galaxies. This database table essentially contains the information given in Table 2 of Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P. (1994, ApJ, 427, 684). Consequently, the information on the properties of the Hickson Compact Groups as units that is also given in some of these references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCGGALXY database table; however, the latter data can be found in the related HEASARC database table HCG.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcggalaxy#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcggalaxy</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=hcggalaxy&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcggalaxy.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Hickson(Gal) [2]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Individual Galaxies Data</TD>
            <TD>The HCGGALAXY database table is based on the Hickson Catalog of Compact Groups, and contains data on 463 galaxies in 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Astrometry, photometry, and morphological types, derived from CCD images, are presented for the 463 galaxies. Radial velocities are given for 457 of the 463 galaxies: more than 84% of the galaxies measured have radial velocities that are within 1000 km/s of the group median velocity. Morphological information derived from either an isophotal analysis or from a visual inspection of images is given for 210 of the 463 galaxies. This database table essentially contains the information given in Table 2 of Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P. (1994, ApJ, 427, 684). Consequently, the information on the properties of the Hickson Compact Groups as units that is also given in some of these references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCGGALXY database table; however, the latter data can be found in the related HEASARC database table HCG.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcggalaxy#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcggalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hcggalaxy&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcggalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Hickson(Gal) [3]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Individual Galaxies Data</TD>
            <TD>The HCGGALAXY database table is based on the Hickson Catalog of Compact Groups, and contains data on 463 galaxies in 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Astrometry, photometry, and morphological types, derived from CCD images, are presented for the 463 galaxies. Radial velocities are given for 457 of the 463 galaxies: more than 84% of the galaxies measured have radial velocities that are within 1000 km/s of the group median velocity. Morphological information derived from either an isophotal analysis or from a visual inspection of images is given for 210 of the 463 galaxies. This database table essentially contains the information given in Table 2 of Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P. (1994, ApJ, 427, 684). Consequently, the information on the properties of the Hickson Compact Groups as units that is also given in some of these references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCGGALXY database table; however, the latter data can be found in the related HEASARC database table HCG.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcggalaxy#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcggalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hcggalaxy&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcggalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/411/1013 [1]</TD>
            <TD>CaII triplet in Sextans dSph galaxy (Battaglia+, 2011)</TD>
            <TD>The spectroscopic observations were carried out at VLT/FLAMES between 2003 and 2004, with the exception of one pointing which was re-observed in 2008 May, during the commissioning of the upgraded Grating Instrument for Radiation Analysis with a Fiber-FedEchelle (GIRAFFE) spectrograph CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013#1</TD>
            <TD>2011-11-26T17:51:11Z</TD>
            <TD>#Abundances#Equivalent_widths#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/411/1013</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/1013</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/411/1013 [2]</TD>
            <TD>CaII triplet in Sextans dSph galaxy (Battaglia+, 2011)</TD>
            <TD>The spectroscopic observations were carried out at VLT/FLAMES between 2003 and 2004, with the exception of one pointing which was re-observed in 2008 May, during the commissioning of the upgraded Grating Instrument for Radiation Analysis with a Fiber-FedEchelle (GIRAFFE) spectrograph CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013#2</TD>
            <TD>2011-11-26T17:51:11Z</TD>
            <TD>#Abundances#Equivalent_widths#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/411/1013&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/1013</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/1013 [table3]</TD>
            <TD>CaII triplet in Sextans dSph galaxy (Battaglia+, 2011)</TD>
            <TD>The spectroscopic observations were carried out at VLT/FLAMES between 2003 and 2004, with the exception of one pointing which was re-observed in 2008 May, during the commissioning of the upgraded Grating Instrument for Radiation Analysis with a Fiber-FedEchelle (GIRAFFE) spectrograph CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013#table3</TD>
            <TD>2011-11-26T17:51:11Z</TD>
            <TD>#Abundances#Equivalent_widths#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/1013&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/1013</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/374/861 [1]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#1</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/374/861</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/374/861 [2]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#2</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/374/861&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/374/861 [tablea3]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#tablea3</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/374/861&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/374/861 [tablea1]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#tablea1</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/374/861&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Hickson(Gal) [1]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Individual Galaxies Data</TD>
            <TD>The HCGGALAXY database table is based on the Hickson Catalog of Compact Groups, and contains data on 463 galaxies in 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Astrometry, photometry, and morphological types, derived from CCD images, are presented for the 463 galaxies. Radial velocities are given for 457 of the 463 galaxies: more than 84% of the galaxies measured have radial velocities that are within 1000 km/s of the group median velocity. Morphological information derived from either an isophotal analysis or from a visual inspection of images is given for 210 of the 463 galaxies. This database table essentially contains the information given in Table 2 of Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P. (1994, ApJ, 427, 684). Consequently, the information on the properties of the Hickson Compact Groups as units that is also given in some of these references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCGGALXY database table; however, the latter data can be found in the related HEASARC database table HCG.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcggalaxy#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcggalaxy</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=hcggalaxy&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcggalaxy.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Hickson(Gal) [2]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Individual Galaxies Data</TD>
            <TD>The HCGGALAXY database table is based on the Hickson Catalog of Compact Groups, and contains data on 463 galaxies in 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Astrometry, photometry, and morphological types, derived from CCD images, are presented for the 463 galaxies. Radial velocities are given for 457 of the 463 galaxies: more than 84% of the galaxies measured have radial velocities that are within 1000 km/s of the group median velocity. Morphological information derived from either an isophotal analysis or from a visual inspection of images is given for 210 of the 463 galaxies. This database table essentially contains the information given in Table 2 of Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P. (1994, ApJ, 427, 684). Consequently, the information on the properties of the Hickson Compact Groups as units that is also given in some of these references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCGGALXY database table; however, the latter data can be found in the related HEASARC database table HCG.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcggalaxy#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcggalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hcggalaxy&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcggalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Hickson(Gal) [3]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Individual Galaxies Data</TD>
            <TD>The HCGGALAXY database table is based on the Hickson Catalog of Compact Groups, and contains data on 463 galaxies in 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Astrometry, photometry, and morphological types, derived from CCD images, are presented for the 463 galaxies. Radial velocities are given for 457 of the 463 galaxies: more than 84% of the galaxies measured have radial velocities that are within 1000 km/s of the group median velocity. Morphological information derived from either an isophotal analysis or from a visual inspection of images is given for 210 of the 463 galaxies. This database table essentially contains the information given in Table 2 of Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P. (1994, ApJ, 427, 684). Consequently, the information on the properties of the Hickson Compact Groups as units that is also given in some of these references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCGGALXY database table; however, the latter data can be found in the related HEASARC database table HCG.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcggalaxy#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcggalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hcggalaxy&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcggalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/411/1013 [1]</TD>
            <TD>CaII triplet in Sextans dSph galaxy (Battaglia+, 2011)</TD>
            <TD>The spectroscopic observations were carried out at VLT/FLAMES between 2003 and 2004, with the exception of one pointing which was re-observed in 2008 May, during the commissioning of the upgraded Grating Instrument for Radiation Analysis with a Fiber-FedEchelle (GIRAFFE) spectrograph CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013#1</TD>
            <TD>2011-11-26T17:51:11Z</TD>
            <TD>#Abundances#Equivalent_widths#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/411/1013</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/1013</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/411/1013 [2]</TD>
            <TD>CaII triplet in Sextans dSph galaxy (Battaglia+, 2011)</TD>
            <TD>The spectroscopic observations were carried out at VLT/FLAMES between 2003 and 2004, with the exception of one pointing which was re-observed in 2008 May, during the commissioning of the upgraded Grating Instrument for Radiation Analysis with a Fiber-FedEchelle (GIRAFFE) spectrograph CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013#2</TD>
            <TD>2011-11-26T17:51:11Z</TD>
            <TD>#Abundances#Equivalent_widths#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/411/1013&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/1013</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/1013 [table3]</TD>
            <TD>CaII triplet in Sextans dSph galaxy (Battaglia+, 2011)</TD>
            <TD>The spectroscopic observations were carried out at VLT/FLAMES between 2003 and 2004, with the exception of one pointing which was re-observed in 2008 May, during the commissioning of the upgraded Grating Instrument for Radiation Analysis with a Fiber-FedEchelle (GIRAFFE) spectrograph CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013#table3</TD>
            <TD>2011-11-26T17:51:11Z</TD>
            <TD>#Abundances#Equivalent_widths#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/1013&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/1013</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChandraM33 [1]</TD>
            <TD>M 33 Chandra X-Ray Point Source Catalog</TD>
            <TD>This database table contains a source list for three Chandra observations of the Local Group galaxy M33. The observations were centered on the nucleus and on the star-forming region NGC 604. A total of 261 sources were detected in an area of about 0.2 square degrees down to a flux limit of 3 x 10^-16 erg/s/cm^2, which corresponds to a luminosity of ~2 x 10^34 erg/s at a distance of 840 kpc. The luminosity functions of the X-ray sources observed in M33 have been constructed and are consistent with those of other star-forming galaxies, taking into account background contamination. In addtion, the combination of X-ray color analysis and the existence of "blue" optical counterparts stronly indicates that the X-ray point source population in M33 consists of young objects. Above 3 x 10^35 erg/s, there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. Notice that each of the 261 X-ray sources in the source list has 3 entries in this table, one for each separate Chandra observation, making a total of 783 entries. The Chandra datasets from which this source list was compiled are available by &lt;a href="/db-perl/W3Browse/w3query.pl?tablehead=name%3Dheasarc_chanmaster&amp;sortvar=obsid&amp;bparam_obsid=786%3B+1730%3B+2023"&gt;querying CHANMASTER for obsids 786, 1730, and 2023&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33cxoxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33cxoxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33cxoxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33cxoxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChandraM33 [2]</TD>
            <TD>M 33 Chandra X-Ray Point Source Catalog</TD>
            <TD>This database table contains a source list for three Chandra observations of the Local Group galaxy M33. The observations were centered on the nucleus and on the star-forming region NGC 604. A total of 261 sources were detected in an area of about 0.2 square degrees down to a flux limit of 3 x 10^-16 erg/s/cm^2, which corresponds to a luminosity of ~2 x 10^34 erg/s at a distance of 840 kpc. The luminosity functions of the X-ray sources observed in M33 have been constructed and are consistent with those of other star-forming galaxies, taking into account background contamination. In addtion, the combination of X-ray color analysis and the existence of "blue" optical counterparts stronly indicates that the X-ray point source population in M33 consists of young objects. Above 3 x 10^35 erg/s, there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. Notice that each of the 261 X-ray sources in the source list has 3 entries in this table, one for each separate Chandra observation, making a total of 783 entries. The Chandra datasets from which this source list was compiled are available by &lt;a href="/db-perl/W3Browse/w3query.pl?tablehead=name%3Dheasarc_chanmaster&amp;sortvar=obsid&amp;bparam_obsid=786%3B+1730%3B+2023"&gt;querying CHANMASTER for obsids 786, 1730, and 2023&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33cxoxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33cxoxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33cxoxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33cxoxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChandraM33 [3]</TD>
            <TD>M 33 Chandra X-Ray Point Source Catalog</TD>
            <TD>This database table contains a source list for three Chandra observations of the Local Group galaxy M33. The observations were centered on the nucleus and on the star-forming region NGC 604. A total of 261 sources were detected in an area of about 0.2 square degrees down to a flux limit of 3 x 10^-16 erg/s/cm^2, which corresponds to a luminosity of ~2 x 10^34 erg/s at a distance of 840 kpc. The luminosity functions of the X-ray sources observed in M33 have been constructed and are consistent with those of other star-forming galaxies, taking into account background contamination. In addtion, the combination of X-ray color analysis and the existence of "blue" optical counterparts stronly indicates that the X-ray point source population in M33 consists of young objects. Above 3 x 10^35 erg/s, there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. Notice that each of the 261 X-ray sources in the source list has 3 entries in this table, one for each separate Chandra observation, making a total of 783 entries. The Chandra datasets from which this source list was compiled are available by &lt;a href="/db-perl/W3Browse/w3query.pl?tablehead=name%3Dheasarc_chanmaster&amp;sortvar=obsid&amp;bparam_obsid=786%3B+1730%3B+2023"&gt;querying CHANMASTER for obsids 786, 1730, and 2023&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33cxoxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33cxoxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33cxoxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33cxoxray.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Hickson(Gal) [1]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Individual Galaxies Data</TD>
            <TD>The HCGGALAXY database table is based on the Hickson Catalog of Compact Groups, and contains data on 463 galaxies in 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Astrometry, photometry, and morphological types, derived from CCD images, are presented for the 463 galaxies. Radial velocities are given for 457 of the 463 galaxies: more than 84% of the galaxies measured have radial velocities that are within 1000 km/s of the group median velocity. Morphological information derived from either an isophotal analysis or from a visual inspection of images is given for 210 of the 463 galaxies. This database table essentially contains the information given in Table 2 of Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P. (1994, ApJ, 427, 684). Consequently, the information on the properties of the Hickson Compact Groups as units that is also given in some of these references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCGGALXY database table; however, the latter data can be found in the related HEASARC database table HCG.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcggalaxy#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcggalaxy</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=hcggalaxy&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcggalaxy.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Hickson(Gal) [2]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Individual Galaxies Data</TD>
            <TD>The HCGGALAXY database table is based on the Hickson Catalog of Compact Groups, and contains data on 463 galaxies in 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Astrometry, photometry, and morphological types, derived from CCD images, are presented for the 463 galaxies. Radial velocities are given for 457 of the 463 galaxies: more than 84% of the galaxies measured have radial velocities that are within 1000 km/s of the group median velocity. Morphological information derived from either an isophotal analysis or from a visual inspection of images is given for 210 of the 463 galaxies. This database table essentially contains the information given in Table 2 of Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P. (1994, ApJ, 427, 684). Consequently, the information on the properties of the Hickson Compact Groups as units that is also given in some of these references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCGGALXY database table; however, the latter data can be found in the related HEASARC database table HCG.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcggalaxy#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcggalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=hcggalaxy&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcggalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Hickson(Gal) [3]</TD>
            <TD>Hickson Compact Groups of Galaxies (HCG) Individual Galaxies Data</TD>
            <TD>The HCGGALAXY database table is based on the Hickson Catalog of Compact Groups, and contains data on 463 galaxies in 100 compact groups of galaxies that were identified by a systematic search of the Palomar Observatory Sky Survey red prints. Each group contains four or more galaxies, has an estimated mean surface brightness brighter than 26.0 magnitude per arcsec^2 and satisfies an isolation criterion. Astrometry, photometry, and morphological types, derived from CCD images, are presented for the 463 galaxies. Radial velocities are given for 457 of the 463 galaxies: more than 84% of the galaxies measured have radial velocities that are within 1000 km/s of the group median velocity. Morphological information derived from either an isophotal analysis or from a visual inspection of images is given for 210 of the 463 galaxies. This database table essentially contains the information given in Table 2 of Hickson, P. et al. (1989, ApJS, 70, 687), Table 2 of Hickson, P. et al. (1992, ApJ, 399, 353), and Table 2 of Mendes de Oliveira, C. and Hickson, P. (1994, ApJ, 427, 684). Consequently, the information on the properties of the Hickson Compact Groups as units that is also given in some of these references, e.g., in Table 3 of Hickson, P. et al. (1992, ApJ, 399, 353), is not in the HCGGALXY database table; however, the latter data can be found in the related HEASARC database table HCG.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/hcggalaxy#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/hcggalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_hcggalaxy&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/hcggalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/374/861 [1]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#1</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/374/861</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/374/861 [2]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#2</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/374/861&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/374/861 [tablea3]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#tablea3</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/374/861&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/374/861 [tablea1]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#tablea1</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/374/861&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChandraM33 [1]</TD>
            <TD>M 33 Chandra X-Ray Point Source Catalog</TD>
            <TD>This database table contains a source list for three Chandra observations of the Local Group galaxy M33. The observations were centered on the nucleus and on the star-forming region NGC 604. A total of 261 sources were detected in an area of about 0.2 square degrees down to a flux limit of 3 x 10^-16 erg/s/cm^2, which corresponds to a luminosity of ~2 x 10^34 erg/s at a distance of 840 kpc. The luminosity functions of the X-ray sources observed in M33 have been constructed and are consistent with those of other star-forming galaxies, taking into account background contamination. In addtion, the combination of X-ray color analysis and the existence of "blue" optical counterparts stronly indicates that the X-ray point source population in M33 consists of young objects. Above 3 x 10^35 erg/s, there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. Notice that each of the 261 X-ray sources in the source list has 3 entries in this table, one for each separate Chandra observation, making a total of 783 entries. The Chandra datasets from which this source list was compiled are available by &lt;a href="/db-perl/W3Browse/w3query.pl?tablehead=name%3Dheasarc_chanmaster&amp;sortvar=obsid&amp;bparam_obsid=786%3B+1730%3B+2023"&gt;querying CHANMASTER for obsids 786, 1730, and 2023&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33cxoxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33cxoxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33cxoxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33cxoxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChandraM33 [2]</TD>
            <TD>M 33 Chandra X-Ray Point Source Catalog</TD>
            <TD>This database table contains a source list for three Chandra observations of the Local Group galaxy M33. The observations were centered on the nucleus and on the star-forming region NGC 604. A total of 261 sources were detected in an area of about 0.2 square degrees down to a flux limit of 3 x 10^-16 erg/s/cm^2, which corresponds to a luminosity of ~2 x 10^34 erg/s at a distance of 840 kpc. The luminosity functions of the X-ray sources observed in M33 have been constructed and are consistent with those of other star-forming galaxies, taking into account background contamination. In addtion, the combination of X-ray color analysis and the existence of "blue" optical counterparts stronly indicates that the X-ray point source population in M33 consists of young objects. Above 3 x 10^35 erg/s, there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. Notice that each of the 261 X-ray sources in the source list has 3 entries in this table, one for each separate Chandra observation, making a total of 783 entries. The Chandra datasets from which this source list was compiled are available by &lt;a href="/db-perl/W3Browse/w3query.pl?tablehead=name%3Dheasarc_chanmaster&amp;sortvar=obsid&amp;bparam_obsid=786%3B+1730%3B+2023"&gt;querying CHANMASTER for obsids 786, 1730, and 2023&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33cxoxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33cxoxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33cxoxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33cxoxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChandraM33 [3]</TD>
            <TD>M 33 Chandra X-Ray Point Source Catalog</TD>
            <TD>This database table contains a source list for three Chandra observations of the Local Group galaxy M33. The observations were centered on the nucleus and on the star-forming region NGC 604. A total of 261 sources were detected in an area of about 0.2 square degrees down to a flux limit of 3 x 10^-16 erg/s/cm^2, which corresponds to a luminosity of ~2 x 10^34 erg/s at a distance of 840 kpc. The luminosity functions of the X-ray sources observed in M33 have been constructed and are consistent with those of other star-forming galaxies, taking into account background contamination. In addtion, the combination of X-ray color analysis and the existence of "blue" optical counterparts stronly indicates that the X-ray point source population in M33 consists of young objects. Above 3 x 10^35 erg/s, there are few X-ray sources in the locus of the X-ray hardness ratio diagram that is generally populated by low-mass X-ray binaries. Notice that each of the 261 X-ray sources in the source list has 3 entries in this table, one for each separate Chandra observation, making a total of 783 entries. The Chandra datasets from which this source list was compiled are available by &lt;a href="/db-perl/W3Browse/w3query.pl?tablehead=name%3Dheasarc_chanmaster&amp;sortvar=obsid&amp;bparam_obsid=786%3B+1730%3B+2023"&gt;querying CHANMASTER for obsids 786, 1730, and 2023&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33cxoxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33cxoxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33cxoxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m33cxoxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/374/861 [1]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#1</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/374/861</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/374/861 [2]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#2</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/374/861&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/374/861 [tablea3]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#tablea3</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/374/861&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/374/861 [tablea1]</TD>
            <TD>Positions of giant radio galaxies (Schoenmakers+ 2001)</TD>
            <TD>In tablea1.dat, we present the WENSS selected candidate GRGs after removing sources identified as non-GRGs on basis of optical data. In tablea2.dat, we present the log of the spectroscopic observations of GRG andidates in our sample. In tablea3.dat, we present properties of the radio cores and the optical identifications of the spectroscopically observed giant radio sources, and of the confirmed giant sources B1144+352, B1245+676 and B1310+451. We provide the name of the radio source in IAU notation, the observation used to determine the radio core position and its flux density and the radio core position in right ascension and declination, respectively, in B1950.0 coordinates. The radio positions have been obtained by fitting a Gaussian in the radio map. We further provide the integrated flux density at 1.4GHz of the radio core, the position of the optical identification in right ascension and declination, respectively, in B1950.0 coordinates, obtained from fitting a Gaussian in the available optical image and the magnitude of the identification in the red (POSS-E) band of the Palomar survey. The magnitudes for sources weaker than 15.0 have been obtained from the APM catalogue and are estimated to be accurate to 0.5 mag. For brighter sources, we have measured the magnitudes directly from the digitized POSS-I frames using the photometric calibration for stars available from the STScI WWW-pages and through the getimage-2.0 plate retrieval software. Typical uncertainties in these values are estimated to be large, at least 1mag. In tablea4.dat, further radio properties of the sources in tablea3.dat. We present the integrated flux density of the source at 325MHz from the Westerbork Northern Sky Survey (WENSS) (unless stated otherwise), the integrated flux density at 1400MHz from the NVSS, the spectral index between 325 and 1400MHz, the redshift of the host galaxy, the angular size of the radio source in arcminutes, the resulting projected linear size in Mpc (using H_0=50km/s/Mpc, q_0_=0.5) and the radio luminosity at an emitted frequency of 325MHz.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861#tablea1</TD>
            <TD>2012-11-13T13:40:23Z</TD>
            <TD>#Positional_Data#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/861</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/374/861&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/861</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/411/1013 [1]</TD>
            <TD>CaII triplet in Sextans dSph galaxy (Battaglia+, 2011)</TD>
            <TD>The spectroscopic observations were carried out at VLT/FLAMES between 2003 and 2004, with the exception of one pointing which was re-observed in 2008 May, during the commissioning of the upgraded Grating Instrument for Radiation Analysis with a Fiber-FedEchelle (GIRAFFE) spectrograph CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013#1</TD>
            <TD>2011-11-26T17:51:11Z</TD>
            <TD>#Abundances#Equivalent_widths#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/411/1013</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/1013</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/411/1013 [2]</TD>
            <TD>CaII triplet in Sextans dSph galaxy (Battaglia+, 2011)</TD>
            <TD>The spectroscopic observations were carried out at VLT/FLAMES between 2003 and 2004, with the exception of one pointing which was re-observed in 2008 May, during the commissioning of the upgraded Grating Instrument for Radiation Analysis with a Fiber-FedEchelle (GIRAFFE) spectrograph CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013#2</TD>
            <TD>2011-11-26T17:51:11Z</TD>
            <TD>#Abundances#Equivalent_widths#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/411/1013&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/1013</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/1013 [table3]</TD>
            <TD>CaII triplet in Sextans dSph galaxy (Battaglia+, 2011)</TD>
            <TD>The spectroscopic observations were carried out at VLT/FLAMES between 2003 and 2004, with the exception of one pointing which was re-observed in 2008 May, during the commissioning of the upgraded Grating Instrument for Radiation Analysis with a Fiber-FedEchelle (GIRAFFE) spectrograph CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013#table3</TD>
            <TD>2011-11-26T17:51:11Z</TD>
            <TD>#Abundances#Equivalent_widths#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/1013</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/1013&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/1013</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/377/801 [1]</TD>
            <TD>Fourth list of the Karachentsev catalog (Huchtmeier+, 2001)</TD>
            <TD>This paper presents HI observations of 165 dwarf galaxy candidates from the Karachentsev catalog of candidates for nearby dwarf galaxies prepared from film copies of POSSII and the ESO/SERC southern extension. Now a total of 601 galaxies from the published Karachentsev catalog have been searched for HI emission. Table 1 lists coordinates and general optical properties while Table 2 presents HI data and some global properties of these galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801#1</TD>
            <TD>2012-11-13T13:40:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/377/801</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/801</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/377/801 [2]</TD>
            <TD>Fourth list of the Karachentsev catalog (Huchtmeier+, 2001)</TD>
            <TD>This paper presents HI observations of 165 dwarf galaxy candidates from the Karachentsev catalog of candidates for nearby dwarf galaxies prepared from film copies of POSSII and the ESO/SERC southern extension. Now a total of 601 galaxies from the published Karachentsev catalog have been searched for HI emission. Table 1 lists coordinates and general optical properties while Table 2 presents HI data and some global properties of these galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801#2</TD>
            <TD>2012-11-13T13:40:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/377/801&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/377/801 [table1]</TD>
            <TD>Fourth list of the Karachentsev catalog (Huchtmeier+, 2001)</TD>
            <TD>This paper presents HI observations of 165 dwarf galaxy candidates from the Karachentsev catalog of candidates for nearby dwarf galaxies prepared from film copies of POSSII and the ESO/SERC southern extension. Now a total of 601 galaxies from the published Karachentsev catalog have been searched for HI emission. Table 1 lists coordinates and general optical properties while Table 2 presents HI data and some global properties of these galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801#table1</TD>
            <TD>2012-11-13T13:40:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/377/801&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M33XMM2 [1]</TD>
            <TD>M33 XMM-Newton X-Ray Variability Source Catalog</TD>
            <TD>This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10^-16 to 1.5 x 10^-11 erg/cm^2/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M33. The relative contribution of the classified XRB and SSS in M33 is now comparable to M31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M33 remains much higher.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmm2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmm2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33xmm2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmm2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M33XMM2 [2]</TD>
            <TD>M33 XMM-Newton X-Ray Variability Source Catalog</TD>
            <TD>This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10^-16 to 1.5 x 10^-11 erg/cm^2/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M33. The relative contribution of the classified XRB and SSS in M33 is now comparable to M31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M33 remains much higher.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmm2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmm2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33xmm2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmm2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M33XMM2 [3]</TD>
            <TD>M33 XMM-Newton X-Ray Variability Source Catalog</TD>
            <TD>This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10^-16 to 1.5 x 10^-11 erg/cm^2/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M33. The relative contribution of the classified XRB and SSS in M33 is now comparable to M31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M33 remains much higher.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmm2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmm2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33xmm2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmm2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/377/801 [1]</TD>
            <TD>Fourth list of the Karachentsev catalog (Huchtmeier+, 2001)</TD>
            <TD>This paper presents HI observations of 165 dwarf galaxy candidates from the Karachentsev catalog of candidates for nearby dwarf galaxies prepared from film copies of POSSII and the ESO/SERC southern extension. Now a total of 601 galaxies from the published Karachentsev catalog have been searched for HI emission. Table 1 lists coordinates and general optical properties while Table 2 presents HI data and some global properties of these galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801#1</TD>
            <TD>2012-11-13T13:40:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>01-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/377/801</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/801</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/377/801 [2]</TD>
            <TD>Fourth list of the Karachentsev catalog (Huchtmeier+, 2001)</TD>
            <TD>This paper presents HI observations of 165 dwarf galaxy candidates from the Karachentsev catalog of candidates for nearby dwarf galaxies prepared from film copies of POSSII and the ESO/SERC southern extension. Now a total of 601 galaxies from the published Karachentsev catalog have been searched for HI emission. Table 1 lists coordinates and general optical properties while Table 2 presents HI data and some global properties of these galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801#2</TD>
            <TD>2012-11-13T13:40:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/377/801&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/377/801 [table1]</TD>
            <TD>Fourth list of the Karachentsev catalog (Huchtmeier+, 2001)</TD>
            <TD>This paper presents HI observations of 165 dwarf galaxy candidates from the Karachentsev catalog of candidates for nearby dwarf galaxies prepared from film copies of POSSII and the ESO/SERC southern extension. Now a total of 601 galaxies from the published Karachentsev catalog have been searched for HI emission. Table 1 lists coordinates and general optical properties while Table 2 presents HI data and some global properties of these galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801#table1</TD>
            <TD>2012-11-13T13:40:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/377/801&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/801</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/3942 [1]</TD>
            <TD>Fossil galaxy groups (La Barbera+, 2009)</TD>
            <TD>We use SDSS-DR4 photometric and spectroscopic data out to redshift z~0.1 combined with ROSAT All Sky Survey X-ray data to produce a sample of 25 fossil groups (FGs), defined as bound systems dominated by a single, luminous elliptical galaxy with extended X-ray emission. We examine possible biases introduced by varying the parameters used to define the sample, and the main pitfalls are also discussed.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942#1</TD>
            <TD>2011-12-03T16:50:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/3942</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/3942</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/3942 [2]</TD>
            <TD>Fossil galaxy groups (La Barbera+, 2009)</TD>
            <TD>We use SDSS-DR4 photometric and spectroscopic data out to redshift z~0.1 combined with ROSAT All Sky Survey X-ray data to produce a sample of 25 fossil groups (FGs), defined as bound systems dominated by a single, luminous elliptical galaxy with extended X-ray emission. We examine possible biases introduced by varying the parameters used to define the sample, and the main pitfalls are also discussed.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942#2</TD>
            <TD>2011-12-03T16:50:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/3942&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/3942</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/3942 [table2]</TD>
            <TD>Fossil galaxy groups (La Barbera+, 2009)</TD>
            <TD>We use SDSS-DR4 photometric and spectroscopic data out to redshift z~0.1 combined with ROSAT All Sky Survey X-ray data to produce a sample of 25 fossil groups (FGs), defined as bound systems dominated by a single, luminous elliptical galaxy with extended X-ray emission. We examine possible biases introduced by varying the parameters used to define the sample, and the main pitfalls are also discussed.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942#table2</TD>
            <TD>2011-12-03T16:50:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/3942&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/3942</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/377/801 [1]</TD>
            <TD>Fourth list of the Karachentsev catalog (Huchtmeier+, 2001)</TD>
            <TD>This paper presents HI observations of 165 dwarf galaxy candidates from the Karachentsev catalog of candidates for nearby dwarf galaxies prepared from film copies of POSSII and the ESO/SERC southern extension. Now a total of 601 galaxies from the published Karachentsev catalog have been searched for HI emission. Table 1 lists coordinates and general optical properties while Table 2 presents HI data and some global properties of these galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801#1</TD>
            <TD>2012-11-13T13:40:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/377/801</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/801</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/377/801 [2]</TD>
            <TD>Fourth list of the Karachentsev catalog (Huchtmeier+, 2001)</TD>
            <TD>This paper presents HI observations of 165 dwarf galaxy candidates from the Karachentsev catalog of candidates for nearby dwarf galaxies prepared from film copies of POSSII and the ESO/SERC southern extension. Now a total of 601 galaxies from the published Karachentsev catalog have been searched for HI emission. Table 1 lists coordinates and general optical properties while Table 2 presents HI data and some global properties of these galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801#2</TD>
            <TD>2012-11-13T13:40:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/377/801&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/377/801 [table1]</TD>
            <TD>Fourth list of the Karachentsev catalog (Huchtmeier+, 2001)</TD>
            <TD>This paper presents HI observations of 165 dwarf galaxy candidates from the Karachentsev catalog of candidates for nearby dwarf galaxies prepared from film copies of POSSII and the ESO/SERC southern extension. Now a total of 601 galaxies from the published Karachentsev catalog have been searched for HI emission. Table 1 lists coordinates and general optical properties while Table 2 presents HI data and some global properties of these galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801#table1</TD>
            <TD>2012-11-13T13:40:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/801</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/377/801&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/801</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>M33XMM2 [1]</TD>
            <TD>M33 XMM-Newton X-Ray Variability Source Catalog</TD>
            <TD>This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10^-16 to 1.5 x 10^-11 erg/cm^2/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M33. The relative contribution of the classified XRB and SSS in M33 is now comparable to M31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M33 remains much higher.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmm2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmm2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33xmm2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmm2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M33XMM2 [2]</TD>
            <TD>M33 XMM-Newton X-Ray Variability Source Catalog</TD>
            <TD>This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10^-16 to 1.5 x 10^-11 erg/cm^2/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M33. The relative contribution of the classified XRB and SSS in M33 is now comparable to M31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M33 remains much higher.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmm2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmm2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33xmm2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmm2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M33XMM2 [3]</TD>
            <TD>M33 XMM-Newton X-Ray Variability Source Catalog</TD>
            <TD>This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10^-16 to 1.5 x 10^-11 erg/cm^2/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M33. The relative contribution of the classified XRB and SSS in M33 is now comparable to M31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M33 remains much higher.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmm2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmm2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33xmm2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmm2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/510/A89 [1]</TD>
            <TD>RMS survey of young massive stars in far-IR (Mottram+, 2010)</TD>
            <TD>Less than 50% of RMS sources are associated with IRAS point sources with detections at 60um and 100um, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89#1</TD>
            <TD>2012-11-13T13:47:01Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/510/A89</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A89</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/510/A89 [2]</TD>
            <TD>RMS survey of young massive stars in far-IR (Mottram+, 2010)</TD>
            <TD>Less than 50% of RMS sources are associated with IRAS point sources with detections at 60um and 100um, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89#2</TD>
            <TD>2012-11-13T13:47:01Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/510/A89&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/510/A89 [table1]</TD>
            <TD>RMS survey of young massive stars in far-IR (Mottram+, 2010)</TD>
            <TD>Less than 50% of RMS sources are associated with IRAS point sources with detections at 60um and 100um, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89#table1</TD>
            <TD>2012-11-13T13:47:01Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/510/A89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M51CXO [1]</TD>
            <TD>M 51 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 10^39 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 10^38 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m51cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m51cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m51cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m51cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M51CXO [2]</TD>
            <TD>M 51 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 10^39 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 10^38 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m51cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m51cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m51cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m51cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M51CXO [3]</TD>
            <TD>M 51 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 10^39 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 10^38 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m51cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m51cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m51cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m51cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M33XMM2 [1]</TD>
            <TD>M33 XMM-Newton X-Ray Variability Source Catalog</TD>
            <TD>This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10^-16 to 1.5 x 10^-11 erg/cm^2/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M33. The relative contribution of the classified XRB and SSS in M33 is now comparable to M31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M33 remains much higher.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmm2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmm2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m33xmm2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmm2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M33XMM2 [2]</TD>
            <TD>M33 XMM-Newton X-Ray Variability Source Catalog</TD>
            <TD>This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10^-16 to 1.5 x 10^-11 erg/cm^2/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M33. The relative contribution of the classified XRB and SSS in M33 is now comparable to M31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M33 remains much higher.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmm2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmm2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m33xmm2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmm2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M33XMM2 [3]</TD>
            <TD>M33 XMM-Newton X-Ray Variability Source Catalog</TD>
            <TD>This table contains the summary results of an analysis of the individual observations (24 archival raster observations) of a deep XMM-Newton survey of the Local Group spiral galaxy M33. The authors detected a total of 350 sources with fluxes (in the 0.2 - 4.5 keV energy band) in the range from 6.7 x 10^-16 to 1.5 x 10^-11 erg/cm^2/s. This comprehensive study considered flux variability, spectral characteristics, and classification of the detected objects. Thirty-nine objects in the catalog are new sources, while 311 were already detected in a previous analysis of most of the same data using combined images. The authors present improved positions of these sources, ans also systematically searched for flux variability on time scales of hours to months or years. The detected variability was then used to classify 8 new X-ray binary candidates in M33. Together with the hardness ratio method and cross-correlation with optical, infrared, and radio data, the authors also classified or confirmed previous classification of 25 supernova remnants and candidates, 2 X-ray binaries, and 11 super-soft source candidates (7 of which are new SSS candidates). In addition, they classified 13 active galactic nuclei and background galaxies, 6 stars, and 23 foreground star candidates in the direction of M33. A further 206 objects are classified as 'hard', approximately half of which are sources intrinsic to M33. The relative contribution of the classified XRB and SSS in M33 is now comparable to M31. The luminosity distribution of SNRs in both spiral galaxies is almost the same, although the number of the detected SNRs in M33 remains much higher.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m33xmm2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m33xmm2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m33xmm2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m33xmm2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/510/A89 [1]</TD>
            <TD>RMS survey of young massive stars in far-IR (Mottram+, 2010)</TD>
            <TD>Less than 50% of RMS sources are associated with IRAS point sources with detections at 60um and 100um, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89#1</TD>
            <TD>2012-11-13T13:47:01Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/510/A89</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A89</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/510/A89 [2]</TD>
            <TD>RMS survey of young massive stars in far-IR (Mottram+, 2010)</TD>
            <TD>Less than 50% of RMS sources are associated with IRAS point sources with detections at 60um and 100um, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89#2</TD>
            <TD>2012-11-13T13:47:01Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/510/A89&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/510/A89 [table1]</TD>
            <TD>RMS survey of young massive stars in far-IR (Mottram+, 2010)</TD>
            <TD>Less than 50% of RMS sources are associated with IRAS point sources with detections at 60um and 100um, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89#table1</TD>
            <TD>2012-11-13T13:47:01Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/510/A89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A89</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/3942 [1]</TD>
            <TD>Fossil galaxy groups (La Barbera+, 2009)</TD>
            <TD>We use SDSS-DR4 photometric and spectroscopic data out to redshift z~0.1 combined with ROSAT All Sky Survey X-ray data to produce a sample of 25 fossil groups (FGs), defined as bound systems dominated by a single, luminous elliptical galaxy with extended X-ray emission. We examine possible biases introduced by varying the parameters used to define the sample, and the main pitfalls are also discussed.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942#1</TD>
            <TD>2011-12-03T16:50:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/3942</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/3942</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/3942 [2]</TD>
            <TD>Fossil galaxy groups (La Barbera+, 2009)</TD>
            <TD>We use SDSS-DR4 photometric and spectroscopic data out to redshift z~0.1 combined with ROSAT All Sky Survey X-ray data to produce a sample of 25 fossil groups (FGs), defined as bound systems dominated by a single, luminous elliptical galaxy with extended X-ray emission. We examine possible biases introduced by varying the parameters used to define the sample, and the main pitfalls are also discussed.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942#2</TD>
            <TD>2011-12-03T16:50:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/3942&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/3942</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/3942 [table2]</TD>
            <TD>Fossil galaxy groups (La Barbera+, 2009)</TD>
            <TD>We use SDSS-DR4 photometric and spectroscopic data out to redshift z~0.1 combined with ROSAT All Sky Survey X-ray data to produce a sample of 25 fossil groups (FGs), defined as bound systems dominated by a single, luminous elliptical galaxy with extended X-ray emission. We examine possible biases introduced by varying the parameters used to define the sample, and the main pitfalls are also discussed.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942#table2</TD>
            <TD>2011-12-03T16:50:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/3942&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/3942</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/510/A89 [1]</TD>
            <TD>RMS survey of young massive stars in far-IR (Mottram+, 2010)</TD>
            <TD>Less than 50% of RMS sources are associated with IRAS point sources with detections at 60um and 100um, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89#1</TD>
            <TD>2012-11-13T13:47:01Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/510/A89</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A89</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/510/A89 [2]</TD>
            <TD>RMS survey of young massive stars in far-IR (Mottram+, 2010)</TD>
            <TD>Less than 50% of RMS sources are associated with IRAS point sources with detections at 60um and 100um, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89#2</TD>
            <TD>2012-11-13T13:47:01Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/510/A89&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/510/A89 [table1]</TD>
            <TD>RMS survey of young massive stars in far-IR (Mottram+, 2010)</TD>
            <TD>Less than 50% of RMS sources are associated with IRAS point sources with detections at 60um and 100um, though the vast majority are visible in Spitzer MIPSGAL or IRAS Galaxy Atlas (IGA) images. However, standard aperture photometry is not appropriate for these data due to crowding of sources and strong spatially variable far-IR background emission in the galactic plane. A new technique using a 2-dimensional fit to the background in an annulus around each source is therefore used to obtain far-IR photometry for young RMS sources.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89#table1</TD>
            <TD>2012-11-13T13:47:01Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/510/A89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M51CXO [1]</TD>
            <TD>M 51 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 10^39 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 10^38 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m51cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m51cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m51cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m51cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M51CXO [2]</TD>
            <TD>M 51 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 10^39 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 10^38 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m51cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m51cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m51cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m51cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M51CXO [3]</TD>
            <TD>M 51 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 10^39 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 10^38 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m51cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m51cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m51cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m51cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/3942 [1]</TD>
            <TD>Fossil galaxy groups (La Barbera+, 2009)</TD>
            <TD>We use SDSS-DR4 photometric and spectroscopic data out to redshift z~0.1 combined with ROSAT All Sky Survey X-ray data to produce a sample of 25 fossil groups (FGs), defined as bound systems dominated by a single, luminous elliptical galaxy with extended X-ray emission. We examine possible biases introduced by varying the parameters used to define the sample, and the main pitfalls are also discussed.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942#1</TD>
            <TD>2011-12-03T16:50:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/3942</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/3942</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/3942 [2]</TD>
            <TD>Fossil galaxy groups (La Barbera+, 2009)</TD>
            <TD>We use SDSS-DR4 photometric and spectroscopic data out to redshift z~0.1 combined with ROSAT All Sky Survey X-ray data to produce a sample of 25 fossil groups (FGs), defined as bound systems dominated by a single, luminous elliptical galaxy with extended X-ray emission. We examine possible biases introduced by varying the parameters used to define the sample, and the main pitfalls are also discussed.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942#2</TD>
            <TD>2011-12-03T16:50:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/3942&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/3942</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/3942 [table2]</TD>
            <TD>Fossil galaxy groups (La Barbera+, 2009)</TD>
            <TD>We use SDSS-DR4 photometric and spectroscopic data out to redshift z~0.1 combined with ROSAT All Sky Survey X-ray data to produce a sample of 25 fossil groups (FGs), defined as bound systems dominated by a single, luminous elliptical galaxy with extended X-ray emission. We examine possible biases introduced by varying the parameters used to define the sample, and the main pitfalls are also discussed.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942#table2</TD>
            <TD>2011-12-03T16:50:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/3942</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/3942&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/3942</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/110/313 [1]</TD>
            <TD>Clusters of galaxies properties. II. (Flin+, 1995)</TD>
            <TD>We present F band photometry, from digitized 48-inch Palomar plates, of 1167 galaxies brighter than m_3_ +3 in 10 Abell clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313#1</TD>
            <TD>2012-11-13T13:52:06Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/110/313</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/313</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/110/313 [2]</TD>
            <TD>Clusters of galaxies properties. II. (Flin+, 1995)</TD>
            <TD>We present F band photometry, from digitized 48-inch Palomar plates, of 1167 galaxies brighter than m_3_ +3 in 10 Abell clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313#2</TD>
            <TD>2012-11-13T13:52:06Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/110/313&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/313</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/110/313 [tables]</TD>
            <TD>Clusters of galaxies properties. II. (Flin+, 1995)</TD>
            <TD>We present F band photometry, from digitized 48-inch Palomar plates, of 1167 galaxies brighter than m_3_ +3 in 10 Abell clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313#tables</TD>
            <TD>2012-11-13T13:52:06Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/110/313&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/313</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M51CXO [1]</TD>
            <TD>M 51 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 10^39 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 10^38 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m51cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m51cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m51cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m51cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M51CXO [2]</TD>
            <TD>M 51 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 10^39 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 10^38 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m51cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m51cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m51cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m51cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M51CXO [3]</TD>
            <TD>M 51 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>This table contains the results of two Chandra observations (separated by 1 year) of the population of X-ray sources in the spiral galaxy M 51 (NGC 5194 and NGC 5195). One hundred and thirteen X-ray sources have been detected in an 8.4' x 8.4'(20.4 x 20.4kpc) region, and 84 and 12 of them project within the disks of NGC 5194 and NGC 5195, respectively. Nine and 28 sources have luminosities exceeding 1 x 10^39 erg/s (ultraluminous X-ray sources or ULXs) and 1 x 10^38 erg/s in the 0.5 - 8 keV band, respectively, assuming that they are associated with M 51. The number of ULXs is much higher than found in most normal spiral and elliptical galaxies. Most of the X-ray sources and all seven of the ULXs in NGC 5194 are located in, or close to, a spiral arm, suggesting a connection with recent star formation. The Chandra observations of M 51 were performed on 2000 June 20 and 2001 June 23 with the ACIS instrument. The background was stable in both observations, and effective exposure times of 14.9 and 26.8ks were obtained for the observations in 2000 and 2001, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m51cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m51cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m51cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m51cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M81CXO [1]</TD>
            <TD>M 81 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 10^36 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m81cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M81CXO [2]</TD>
            <TD>M 81 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 10^36 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m81cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M81CXO [3]</TD>
            <TD>M 81 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 10^36 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m81cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/370 [1]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#1</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/370</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/370 [2]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#2</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/370&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/370 [table1]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#table1</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/370&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/370 [tables]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#tables</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/370&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/110/313 [1]</TD>
            <TD>Clusters of galaxies properties. II. (Flin+, 1995)</TD>
            <TD>We present F band photometry, from digitized 48-inch Palomar plates, of 1167 galaxies brighter than m_3_ +3 in 10 Abell clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313#1</TD>
            <TD>2012-11-13T13:52:06Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/110/313</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/313</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/110/313 [2]</TD>
            <TD>Clusters of galaxies properties. II. (Flin+, 1995)</TD>
            <TD>We present F band photometry, from digitized 48-inch Palomar plates, of 1167 galaxies brighter than m_3_ +3 in 10 Abell clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313#2</TD>
            <TD>2012-11-13T13:52:06Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/110/313&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/313</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/110/313 [tables]</TD>
            <TD>Clusters of galaxies properties. II. (Flin+, 1995)</TD>
            <TD>We present F band photometry, from digitized 48-inch Palomar plates, of 1167 galaxies brighter than m_3_ +3 in 10 Abell clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313#tables</TD>
            <TD>2012-11-13T13:52:06Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/110/313&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/313</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M81CXO [1]</TD>
            <TD>M 81 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 10^36 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m81cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M81CXO [2]</TD>
            <TD>M 81 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 10^36 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ParamHTTP</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M81CXO [3]</TD>
            <TD>M 81 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 10^36 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>ivo://nasa.heasarc/m81cxo</TD>
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            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m81cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/370 [1]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#1</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/370</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/370 [2]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#2</TD>
            <TD>2011-12-11T16:41:30Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/370&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/370 [table1]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#table1</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/370 [tables]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#tables</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/370&amp;</TD>
            <TD>180</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/110/313 [1]</TD>
            <TD>Clusters of galaxies properties. II. (Flin+, 1995)</TD>
            <TD>We present F band photometry, from digitized 48-inch Palomar plates, of 1167 galaxies brighter than m_3_ +3 in 10 Abell clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313#1</TD>
            <TD>2012-11-13T13:52:06Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/110/313</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/313</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/110/313 [2]</TD>
            <TD>Clusters of galaxies properties. II. (Flin+, 1995)</TD>
            <TD>We present F band photometry, from digitized 48-inch Palomar plates, of 1167 galaxies brighter than m_3_ +3 in 10 Abell clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313#2</TD>
            <TD>2012-11-13T13:52:06Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/110/313&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/313</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/110/313 [tables]</TD>
            <TD>Clusters of galaxies properties. II. (Flin+, 1995)</TD>
            <TD>We present F band photometry, from digitized 48-inch Palomar plates, of 1167 galaxies brighter than m_3_ +3 in 10 Abell clusters. For each galaxy, absolute coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide finding charts and contour maps of the galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313#tables</TD>
            <TD>2012-11-13T13:52:06Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/110/313</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/110/313&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/110/313</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M81CXO [1]</TD>
            <TD>M 81 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 10^36 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
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            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m81cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M81CXO [2]</TD>
            <TD>M 81 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 10^36 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m81cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M81CXO [3]</TD>
            <TD>M 81 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>A Chandra X-Ray Observatory ACIS-S imaging observation is used to study the population of X-ray sources in the nearby (3.6 Mpc) Sab galaxy M 81 (NGC 3031). A total of 177 sources are detected, with 124 located within the D_25 isophote to a limiting X-ray luminosity of ~ 3 x 10^36 erg/s. Source positions, count rates, luminosities in the 0.3 - 8.0 keV band, limiting optical magnitudes, and potential counterpart identifications are tabulated. Spectral and timing analysis of the 36 brightest sources are reported, including the low-luminosity active galactic nucleus, SN 1993J, and the Einstein-discovered ultraluminous X-ray source X6. The primary X-ray data set is a 49926 s observation of M81 obtained on 2000 May 7 with the Chandra Advanced CCD Imaging Spectrometer (ACIS) spectroscopy array operating in imaging mode. The X-ray data were reprocessed by the Chandra X-ray Center (CXC) on 2001 January 4. These reprocessed data were used in this work. There are no significant differences between the reprocessed data and the originally distributed data analyzed by Tennant et al. (2001ApJ...549L..43T). The observation was taken in faint timed exposure mode at 3.241 s/frame at a focal plane temperature of -120 C. Standard CXC processing has applied aspect corrections and compensated for spacecraft dither. The primary target, SN 1993J, was located near the nominal aimpoint on the back-illuminated (BI) device S3. The nucleus of M81 lies 2.79' from SN 1993J toward the center of S3 in this observation. Accurate positions of these two objects and two G0 stars located on device S2 were used to identify any offset and to determine absolute locations of the remaining Chandra sources as well as objects in other X-ray images and those obtained at other wavelengths. No offset correction was applied to the Chandra X-ray positions.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo</TD>
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m81cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/703/370 [1]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#1</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/703/370</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/703/370 [2]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#2</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/703/370&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/370 [table1]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#table1</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/370&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/703/370 [tables]</TD>
            <TD>Radio SNRs in nearby galaxies (Chomiuk+, 2009)</TD>
            <TD>We compile radio supernova remnant (SNR) samples from the literature for 19 nearby galaxies ranging from the SMC to Arp 220, and use this data to constrain the SNR luminosity function (LF) at 20cm. We find that radio SNR populations are strikingly similar across galaxies. The LF can be described as a power law with constant index and scaling proportional to a galaxy's star formation rate (SFR). Unlike previous authors, we do not find any dependence of SNR luminosity on a galaxy's global interstellar medium density. The observed correlation between the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be completely explained by statistical effects, wherein galaxies with higher SFR more thoroughly sample the high-luminosity end of the SNR LF. The LF is well fitted by a model of SNR synchrotron emission which includes diffusive shock acceleration and magnetic field amplification, if we assume that all remnants are undergoing adiabatic expansion, the densities of star-forming regions are similar across galaxies, and the efficiency of cosmic ray production is constant.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370#tables</TD>
            <TD>2011-12-11T16:41:30Z</TD>
            <TD>#Galaxies#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/703/370</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/703/370&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/703/370</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/853 [1]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#1</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/853</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/853 [2]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#2</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/853&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/853 [table1b]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#table1b</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/853&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/853 [table1a]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#table1a</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/853&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Markarian [1]</TD>
            <TD>First Byurakan Survey (Markarian) Catalog of UV-Excess Galaxies</TD>
            <TD>A catalog of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processing, the FBS areas, the object selection and classification criteria and also several selection effects are described in the reference. The catalog contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included in the catalog. While compiling the catalog, the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum excesses. In addition, the authors included the objects with numbers 1501-1515. In most cases, they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 48 objects from their lists are not included in the catalog, since they are either stars of our Galaxy or star projections on the galaxies. This catalog presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (apparent magnitude &lt; 16.0). Up to the middle of 1987 redshifts were measured for 1459 out of 1469 objects in the catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=markarian&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Markarian [2]</TD>
            <TD>First Byurakan Survey (Markarian) Catalog of UV-Excess Galaxies</TD>
            <TD>A catalog of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processing, the FBS areas, the object selection and classification criteria and also several selection effects are described in the reference. The catalog contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included in the catalog. While compiling the catalog, the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum excesses. In addition, the authors included the objects with numbers 1501-1515. In most cases, they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 48 objects from their lists are not included in the catalog, since they are either stars of our Galaxy or star projections on the galaxies. This catalog presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (apparent magnitude &lt; 16.0). Up to the middle of 1987 redshifts were measured for 1459 out of 1469 objects in the catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=markarian&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Markarian [3]</TD>
            <TD>First Byurakan Survey (Markarian) Catalog of UV-Excess Galaxies</TD>
            <TD>A catalog of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processing, the FBS areas, the object selection and classification criteria and also several selection effects are described in the reference. The catalog contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included in the catalog. While compiling the catalog, the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum excesses. In addition, the authors included the objects with numbers 1501-1515. In most cases, they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 48 objects from their lists are not included in the catalog, since they are either stars of our Galaxy or star projections on the galaxies. This catalog presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (apparent magnitude &lt; 16.0). Up to the middle of 1987 redshifts were measured for 1459 out of 1469 objects in the catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_markarian&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/198 [1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/198</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/198 [2]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#2</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/198&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91file1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91file1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91cl_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91cl_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82file2]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82file2</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmcl_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmcl_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82file1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82file1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91pp_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91pp_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [egalf1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#egalf1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91cl_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91cl_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmcl_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmcl_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmfile1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmfile1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91pp_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91pp_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [mat_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#mat_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmw_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmw_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82file3]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82file3</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [mat_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#mat_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [matfile1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#matfile1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [wcf_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#wcf_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [cf_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#cf_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [cffile1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#cffile1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [egalf2]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#egalf2</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/853 [1]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#1</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/853</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/853 [2]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#2</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/853&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/853 [table1b]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#table1b</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/853&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/853 [table1a]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#table1a</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/853&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Markarian [1]</TD>
            <TD>First Byurakan Survey (Markarian) Catalog of UV-Excess Galaxies</TD>
            <TD>A catalog of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processing, the FBS areas, the object selection and classification criteria and also several selection effects are described in the reference. The catalog contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included in the catalog. While compiling the catalog, the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum excesses. In addition, the authors included the objects with numbers 1501-1515. In most cases, they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 48 objects from their lists are not included in the catalog, since they are either stars of our Galaxy or star projections on the galaxies. This catalog presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (apparent magnitude &lt; 16.0). Up to the middle of 1987 redshifts were measured for 1459 out of 1469 objects in the catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=markarian&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Markarian [2]</TD>
            <TD>First Byurakan Survey (Markarian) Catalog of UV-Excess Galaxies</TD>
            <TD>A catalog of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processing, the FBS areas, the object selection and classification criteria and also several selection effects are described in the reference. The catalog contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included in the catalog. While compiling the catalog, the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum excesses. In addition, the authors included the objects with numbers 1501-1515. In most cases, they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 48 objects from their lists are not included in the catalog, since they are either stars of our Galaxy or star projections on the galaxies. This catalog presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (apparent magnitude &lt; 16.0). Up to the middle of 1987 redshifts were measured for 1459 out of 1469 objects in the catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=markarian&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Markarian [3]</TD>
            <TD>First Byurakan Survey (Markarian) Catalog of UV-Excess Galaxies</TD>
            <TD>A catalog of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processing, the FBS areas, the object selection and classification criteria and also several selection effects are described in the reference. The catalog contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included in the catalog. While compiling the catalog, the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum excesses. In addition, the authors included the objects with numbers 1501-1515. In most cases, they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 48 objects from their lists are not included in the catalog, since they are either stars of our Galaxy or star projections on the galaxies. This catalog presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (apparent magnitude &lt; 16.0). Up to the middle of 1987 redshifts were measured for 1459 out of 1469 objects in the catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_markarian&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/198 [1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/198</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/198 [2]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#2</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/198&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91file1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91file1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91cl_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91cl_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82file2]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82file2</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmcl_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmcl_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82file1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82file1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91pp_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91pp_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [egalf1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#egalf1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91cl_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91cl_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmcl_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmcl_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmfile1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmfile1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91pp_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91pp_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [mat_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#mat_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmw_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmw_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82file3]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82file3</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [mat_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#mat_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [matfile1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#matfile1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [wcf_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#wcf_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [cf_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#cf_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [cffile1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#cffile1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [egalf2]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#egalf2</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/853 [1]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#1</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/853</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/853 [2]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#2</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/853&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/853 [table1b]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#table1b</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/853&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/853 [table1a]</TD>
            <TD>VLA survey of Abell clusters. IV. (Ledlow+ 1995)</TD>
            <TD>This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parametrized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853#table1a</TD>
            <TD>2012-11-13T14:02:45Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/853</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/853&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/853</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/198 [1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/198</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/198 [2]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#2</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/198&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91file1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91file1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91cl_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91cl_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82file2]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82file2</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmcl_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmcl_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82file1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82file1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91pp_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91pp_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [egalf1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#egalf1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91cl_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91cl_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmcl_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmcl_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmfile1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmfile1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [w91pp_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#w91pp_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [mat_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#mat_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [hmw_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#hmw_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [a82file3]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#a82file3</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [mat_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#mat_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [matfile1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#matfile1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [wcf_g]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#wcf_g</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [cf_s]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#cf_s</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [cffile1]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#cffile1</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/198 [egalf2]</TD>
            <TD>Mark III Catalog of Galaxy Peculiar Velocities (Willick+ 1997)</TD>
            <TD>The Mark III Catalog of Galaxy Peculiar Velocities comprises five different types of data files. 1. Basic Observational and Catalog Data 2. Individual Galaxy TF and Dn-sigma Distances 3. Grouped Spiral Galaxy TF Distances 4. Elliptical Galaxy Distances as in the Mark II 5. Comparison of Spiral Galaxy Distances 1. The Basic Data files are: a. Aaronson et al. Field, (359 galaxies; a82): a82file1.dat, a82file2.dat, a82file3.dat b. Mathewson et al. 1992 (1355 galaxies; mat): matfile1.dat, matfile2.dat, matfile3.dat c. Willick 1991, Perseus-Pisces sample (383 galaxies; w91pp): d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): The basic data for all 539 objects in the w91 sample are given in the following files: w91file1.dat, w91file2.dat, w91file3.dat Some galaxies are duplicates; see below for details. e. Courteau-Faber 1993 (326 galaxies; cf): cffile1.dat, cffile2.dat, cffile3.dat f. Han-Mould et al. 1992+, Cluster galaxy sample (433 galaxies; hmcl): The basic data for all 433 galaxies the the hm sample are given in the following files: hmfile1.dat, hmfile3.dat, hmfile2.dat Some galaxies are duplicates; see below for details. 2. The Individual Spiral Galaxy Distances Files are: (See notes for detailed descriptions of how the w91pp, w91cl, hmcl and cf distance files correspond to the galaxies in the w91file*, hmfile*, and cffile* Basic Data files.) a. Aaronson et al. Field, (359 galaxies; a82): a82_s b. Mathewson et al. 1992 (1355 galaxies; mat): mat_s c. Willick 1991, Perseus-Pisces sample (326 galaxies; w91pp): w91pp_s.dat d. Willick 1991, Cluster galaxy sample (156 galaxies; w91cl): w91cl_s.dat e. Courteau-Faber 1993 (321 galaxies; cf): cf_s.dat f. Han-Mould et al. 1992+, all cluster galaxies (427 galaxies; hmcl): hmcl_s.dat 3. The Grouped Spiral Galaxy Distance Files are: (Note: Group numbers in the wcf group (merged w91pp and cf) data file correspond to those in the w91pp and cf individual galaxy files. The hmw group file (merged w91cl and hmcl, 10 northern clusters only, cf. Willick et al. 1995) does not correspond to any individual galaxy distance file.) a. Aaronson et al. Field, (67 groups; a82): a82_g b. Mathewson et al. 1992 (277 groups; mat): mat_g c. Willick 1991, Perseus-Pisces sample (63 groups; w91pp): w91pp_g d. Willick 1991, Cluster galaxy sample (11 groups; w91cl): w91cl_g e. Courteau-Faber 1993 jointly grouped with Willick 1991 (65 groups; wcf): wcf_g f. Han-Mould et al. 1992+, all cluster galaxies (36 groups; hmcl): hmcl_g g. Combined hmcl and w91cl distances for the 10 northern clusters in common between the two samples (10 groups; hmw): hmw_g 4. Elliptical Galaxy Distance Files are: a. The Basic Data for the Mark II elliptical galaxy data: egalf1.dat b. The grouped data for the Mark II elliptical galaxy data, normalized in distance to the full spiral galaxy sample (a 3.5% revision in distances, such that the new distances are 0.965 times the old): egalf2.dat 5. Comparison of Galaxy Distances: This gives a direct comparison of predicted distance, magnitude and rotation velocity (eta) for 403 galaxies in common to two or more of the six spiral galaxy data sets: six data sets: match</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/VII/198#egalf2</TD>
            <TD>2012-11-16T16:33:32Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1996</TD>
            <TD>ivo://CDS.VizieR/VII/198</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/198&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/198</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Markarian [1]</TD>
            <TD>First Byurakan Survey (Markarian) Catalog of UV-Excess Galaxies</TD>
            <TD>A catalog of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processing, the FBS areas, the object selection and classification criteria and also several selection effects are described in the reference. The catalog contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included in the catalog. While compiling the catalog, the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum excesses. In addition, the authors included the objects with numbers 1501-1515. In most cases, they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 48 objects from their lists are not included in the catalog, since they are either stars of our Galaxy or star projections on the galaxies. This catalog presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (apparent magnitude &lt; 16.0). Up to the middle of 1987 redshifts were measured for 1459 out of 1469 objects in the catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=markarian&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Markarian [2]</TD>
            <TD>First Byurakan Survey (Markarian) Catalog of UV-Excess Galaxies</TD>
            <TD>A catalog of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processing, the FBS areas, the object selection and classification criteria and also several selection effects are described in the reference. The catalog contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included in the catalog. While compiling the catalog, the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum excesses. In addition, the authors included the objects with numbers 1501-1515. In most cases, they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 48 objects from their lists are not included in the catalog, since they are either stars of our Galaxy or star projections on the galaxies. This catalog presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (apparent magnitude &lt; 16.0). Up to the middle of 1987 redshifts were measured for 1459 out of 1469 objects in the catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=markarian&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Markarian [3]</TD>
            <TD>First Byurakan Survey (Markarian) Catalog of UV-Excess Galaxies</TD>
            <TD>A catalog of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the FBS was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processing, the FBS areas, the object selection and classification criteria and also several selection effects are described in the reference. The catalog contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included in the catalog. While compiling the catalog, the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum excesses. In addition, the authors included the objects with numbers 1501-1515. In most cases, they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 48 objects from their lists are not included in the catalog, since they are either stars of our Galaxy or star projections on the galaxies. This catalog presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (apparent magnitude &lt; 16.0). Up to the middle of 1987 redshifts were measured for 1459 out of 1469 objects in the catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#</TD>
            <TD>ivo://nasa.heasarc/markarian#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/markarian</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_markarian&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/markarian.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1993 [1]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#1</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1993</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1993 [2]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#2</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1993&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/1993 [table1b]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#table1b</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/1993&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/1993 [table1a]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#table1a</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/1993&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/165A [1]</TD>
            <TD>Measured Redshifts of Abell Clusters of Galaxies (Andernach 1991)</TD>
            <TD>The 'ACO' catalog (Abell, Corwin and Olowin 1989; Cat. VII/110) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/165A#1</TD>
            <TD>2012-11-13T06:48:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/165A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/165A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/165A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/165A [2]</TD>
            <TD>Measured Redshifts of Abell Clusters of Galaxies (Andernach 1991)</TD>
            <TD>The 'ACO' catalog (Abell, Corwin and Olowin 1989; Cat. VII/110) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/165A#2</TD>
            <TD>2012-11-13T06:48:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/165A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/165A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/165A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/165A [catalog]</TD>
            <TD>Measured Redshifts of Abell Clusters of Galaxies (Andernach 1991)</TD>
            <TD>The 'ACO' catalog (Abell, Corwin and Olowin 1989; Cat. VII/110) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/165A#catalog</TD>
            <TD>2012-11-13T06:48:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/165A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/165A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/165A</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1993 [1]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#1</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1993</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1993 [2]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#2</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1993&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/1993 [table1b]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#table1b</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/1993&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/1993 [table1a]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#table1a</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/1993&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MCG [1]</TD>
            <TD>Morphological Galaxy Catalog</TD>
            <TD>The MCG database contains the "Morphological Catalogue of Galaxies," a compilation of information for approximately 34,000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29,000 galaxies and information on the remaining 5,000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01 (+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are numbered with increasing right ascension. The original goal of the compilation was to be complete for galaxies brighter than magnitude 15.1, but the final catalog lists many objects considerably fainter. Information given in the original printed volumes includes: cross- identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes and intensities of the bright inner region and the entire object, estimated inclination, and coded description (by symbols) of the appearance of the galaxy. Each field is then followed by notes on individual objects. All of the above data except the coded description are included in the machine version, except that special coding (e.g. for uncertainty or source designation) is not present (other than for the NGC/IC cross identifications [added at the Astronomical Data Center for this machine version]). Although the notes are not computerized, the presence of a note in the original is flagged in the machine version Detailed descriptions of modifications, corrections and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional Information section below. In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalog resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/mcg#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcg</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=mcg&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/mcg.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MCG [2]</TD>
            <TD>Morphological Galaxy Catalog</TD>
            <TD>The MCG database contains the "Morphological Catalogue of Galaxies," a compilation of information for approximately 34,000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29,000 galaxies and information on the remaining 5,000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01 (+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are numbered with increasing right ascension. The original goal of the compilation was to be complete for galaxies brighter than magnitude 15.1, but the final catalog lists many objects considerably fainter. Information given in the original printed volumes includes: cross- identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes and intensities of the bright inner region and the entire object, estimated inclination, and coded description (by symbols) of the appearance of the galaxy. Each field is then followed by notes on individual objects. All of the above data except the coded description are included in the machine version, except that special coding (e.g. for uncertainty or source designation) is not present (other than for the NGC/IC cross identifications [added at the Astronomical Data Center for this machine version]). Although the notes are not computerized, the presence of a note in the original is flagged in the machine version Detailed descriptions of modifications, corrections and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional Information section below. In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalog resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/mcg#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=mcg&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/mcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MCG [3]</TD>
            <TD>Morphological Galaxy Catalog</TD>
            <TD>The MCG database contains the "Morphological Catalogue of Galaxies," a compilation of information for approximately 34,000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29,000 galaxies and information on the remaining 5,000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01 (+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are numbered with increasing right ascension. The original goal of the compilation was to be complete for galaxies brighter than magnitude 15.1, but the final catalog lists many objects considerably fainter. Information given in the original printed volumes includes: cross- identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes and intensities of the bright inner region and the entire object, estimated inclination, and coded description (by symbols) of the appearance of the galaxy. Each field is then followed by notes on individual objects. All of the above data except the coded description are included in the machine version, except that special coding (e.g. for uncertainty or source designation) is not present (other than for the NGC/IC cross identifications [added at the Astronomical Data Center for this machine version]). Although the notes are not computerized, the presence of a note in the original is flagged in the machine version Detailed descriptions of modifications, corrections and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional Information section below. In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalog resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/mcg#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_mcg&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/mcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/1993 [1]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#1</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/1993</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/1993 [2]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#2</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/1993&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/1993 [table1b]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#table1b</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/1993&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/1993 [table1a]</TD>
            <TD>IRAS Bright Galaxy Survey. II (Sanders+ 1995)</TD>
            <TD>Complete IRAS Observations and redshifts are reported for all sources identified in the IRAS Bright Galaxy Survey - Part II (hereafter referred to as BGS2). Source positions, radial velocities, optical magnitudes, and total flux densities, peak flux densities, and spatial extents at 12, 25, and 100um are reported for 288 sources having 60um flux densities &gt;5.24Jy, the completeness limit of the original Bright Galaxy Survey [Soifer et al. (1989AJ.....98..766S)], hereafter referred to as BGS1. These new data represent the extension of the IRAS Bright Galaxy Survey to southern declinations, Dec&lt;~-30deg, and low Galactic latitudes, 5deg&lt;|b|&lt;=30deg. Although the sky coverage of the BGS2 (~19935deg^2) is 37% larger than the sky coverage of the BGS1, the number of sources is 8% smaller due primarily to large scale structure in the local distribution of galaxies. Otherwise, the sources in the BGS2 show similar relationships between number counts and flux density as observed for the 313 sources in the BGS1. The BGS2 along with the earlier BGS1, represents the best sample currently available for defining the infrared properties of galaxies in the local (z&lt;~0.1) Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993#table1a</TD>
            <TD>2012-11-13T14:03:25Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/1993</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/1993&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/1993</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/165A [1]</TD>
            <TD>Measured Redshifts of Abell Clusters of Galaxies (Andernach 1991)</TD>
            <TD>The 'ACO' catalog (Abell, Corwin and Olowin 1989; Cat. VII/110) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/165A#1</TD>
            <TD>2012-11-13T06:48:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/165A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/165A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/165A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/165A [2]</TD>
            <TD>Measured Redshifts of Abell Clusters of Galaxies (Andernach 1991)</TD>
            <TD>The 'ACO' catalog (Abell, Corwin and Olowin 1989; Cat. VII/110) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/165A#2</TD>
            <TD>2012-11-13T06:48:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/165A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/165A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/165A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/165A [catalog]</TD>
            <TD>Measured Redshifts of Abell Clusters of Galaxies (Andernach 1991)</TD>
            <TD>The 'ACO' catalog (Abell, Corwin and Olowin 1989; Cat. VII/110) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/165A#catalog</TD>
            <TD>2012-11-13T06:48:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/165A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/165A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/165A</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/352/939 [1]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#1</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/352/939</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/352/939 [2]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#2</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/352/939&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/939 [voids]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#voids</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/939&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/939 [table1]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#table1</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/939&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MCG [1]</TD>
            <TD>Morphological Galaxy Catalog</TD>
            <TD>The MCG database contains the "Morphological Catalogue of Galaxies," a compilation of information for approximately 34,000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29,000 galaxies and information on the remaining 5,000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01 (+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are numbered with increasing right ascension. The original goal of the compilation was to be complete for galaxies brighter than magnitude 15.1, but the final catalog lists many objects considerably fainter. Information given in the original printed volumes includes: cross- identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes and intensities of the bright inner region and the entire object, estimated inclination, and coded description (by symbols) of the appearance of the galaxy. Each field is then followed by notes on individual objects. All of the above data except the coded description are included in the machine version, except that special coding (e.g. for uncertainty or source designation) is not present (other than for the NGC/IC cross identifications [added at the Astronomical Data Center for this machine version]). Although the notes are not computerized, the presence of a note in the original is flagged in the machine version Detailed descriptions of modifications, corrections and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional Information section below. In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalog resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/mcg#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcg</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=mcg&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/mcg.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MCG [2]</TD>
            <TD>Morphological Galaxy Catalog</TD>
            <TD>The MCG database contains the "Morphological Catalogue of Galaxies," a compilation of information for approximately 34,000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29,000 galaxies and information on the remaining 5,000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01 (+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are numbered with increasing right ascension. The original goal of the compilation was to be complete for galaxies brighter than magnitude 15.1, but the final catalog lists many objects considerably fainter. Information given in the original printed volumes includes: cross- identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes and intensities of the bright inner region and the entire object, estimated inclination, and coded description (by symbols) of the appearance of the galaxy. Each field is then followed by notes on individual objects. All of the above data except the coded description are included in the machine version, except that special coding (e.g. for uncertainty or source designation) is not present (other than for the NGC/IC cross identifications [added at the Astronomical Data Center for this machine version]). Although the notes are not computerized, the presence of a note in the original is flagged in the machine version Detailed descriptions of modifications, corrections and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional Information section below. In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalog resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/mcg#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=mcg&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/mcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MCG [3]</TD>
            <TD>Morphological Galaxy Catalog</TD>
            <TD>The MCG database contains the "Morphological Catalogue of Galaxies," a compilation of information for approximately 34,000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29,000 galaxies and information on the remaining 5,000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01 (+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are numbered with increasing right ascension. The original goal of the compilation was to be complete for galaxies brighter than magnitude 15.1, but the final catalog lists many objects considerably fainter. Information given in the original printed volumes includes: cross- identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes and intensities of the bright inner region and the entire object, estimated inclination, and coded description (by symbols) of the appearance of the galaxy. Each field is then followed by notes on individual objects. All of the above data except the coded description are included in the machine version, except that special coding (e.g. for uncertainty or source designation) is not present (other than for the NGC/IC cross identifications [added at the Astronomical Data Center for this machine version]). Although the notes are not computerized, the presence of a note in the original is flagged in the machine version Detailed descriptions of modifications, corrections and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional Information section below. In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalog resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/mcg#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_mcg&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/mcg.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MILLIQUAS [1]</TD>
            <TD>Million Quasars Catalog (MILLIQUAS), Version 3.1 (22 October 2012)</TD>
            <TD>This table contains the Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012). It is a compendium of all type I QSOs, AGN, and BL Lacs in the literature, up to 20 October 2012; completeness is full or nearly so. High-confidence (70+%) photometric SDSS and radio/X-ray associated objects are included, which bring the total number of objects to 1,226,331. Objects have been de-duplicated across catalogs, and the earliest name and best redshift is presented for each. Astrometry is fixed onto a combined APM/USNO-A/SDSS optical background, and is accurate to within 1-2 arcseconds, even for the earliest quasars. Note that close objects and lensed images within 1.5 arcseconds may be represented as single objects. This version has the following changes from the previous edition: &lt;pre&gt; (1) Quasar data brought up to publications as at 20 October 2012, including the new DR9 Quasar catalog (Paris I., 2012,arXiv:1210.5166). &lt;/pre&gt; The contents are relatively simple, each object is shown as one entry with the sky coordinates, its name, red and blue optical magnitudes, PSF class, redshift, and the source catalog for its name and redshift, plus a radio and/or X-ray identifier where applicable. The author's current plans are to keep this updated as a "living" QSO catalog, and to think about formal publication at a later date. Questions/comments/praise/complaints may be directed to Eric Flesch at eric@flesch.org. He requests that, if you use this catalog in published research, that you please add a small mention (acknowledgement). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is &lt;a href="http://www.sdss3.org/"&gt;http://www.sdss3.org/&lt;/a&gt;. Version Log: &lt;pre&gt; 0.1 22Apr09 0.3 6May09 Added a radio identifier and an X-ray identifier. 0.5 11May09 Added 30816 objects from newly calculated associations to XMM, Chandra and SUMSS detections, plus some tweaks. Also added QSO probability % for non-confirmed QSOs. 0.8 22Jun09 Added Chandra Source Catalog 1.0 (2009). 1.0 03Aug09 Extensive de-duplication. XMM Slew Catalog data added. 1.4 20Aug09 Misc fixes in the de-duplications. 1.5 29Aug09 Using XMM Slew Catalog v1.3 2.0 14Jun10 Using XMM Slew Catalog v1.4, XMM3 and XASSIST4. 2.1 17Aug10 Removed 8627 NELGs masquerading as AGN. 2.2 7Jan11 About 10,000 AGNe from the previous edition are now presented as QSOs. 796 AGNe mistakenly expunged in 2.1 have been restored. 2.3 5Mar11 SDSS DR-8 and BOSS targets have been included and the threshold for inclusions of candidates has been raised from 60% to 70%. 2.4 5Jun11 Improved QSO-likelihood calculation for the BOSS targets, so 17% of previously included BOSS targets drop out. Newly included data from several sources (see above). 2.5 20Jul11 Some deduplication of quasars which were discovered prior to 1990, 200 recent NED quasars added, some radio/X-ray associations to USNO-B optical data added. 2.6 10Sep11 The USNO-B catalog has been added and hard-deduplicated against APM and SDSS data to make a background pool of 1.04 billion optical objects. Also, about 12 million orphaned one-color APM objects have been removed. There are consequently improvements in this catalog's optical selections and astrometry without changing the net totals much. XMM Slew 1.5 catalog added. Some further astrometric fixes and deduplications of early quasars. 2.7 5Nov11 New quasar publications to 4 November 2011 were added, and a few fixes on individual objects incorporated. 2.8 29Jan12 Completed the fixes of non-astrometric relic data from the Veron-Cetty &amp; Veron 13th edition. About 150 other fixes. Quasars compilation updated through 27 January 2012. 2.9 2Apr12 Data brought up to publications as of 31 March 2012, about 50 astrometric fixes done, and the new FIRST radio catalog, 12Feb16 version, incorporated. 2.10 6Aug12 Data brought up to publications as of 31 July 2012, including the SDSS-DR9 release, Xassist XMM-Newton and Chandra X-ray data updated to 30 June 2012; as this is a catalog for type I (broad-line) objects, 1870 Seyfert-2s, 532 LINERs, and 6 NELGs were removed, but Bl Lacs were retained as unconstrained emission objects. 3.0 9Sep12 Data brought up to publications as at 31 August 2012. Redshifts are calculated for the XDQSO photometric quasar candidates. Fixed issues with 30 DEEP2 object. Separated out 15 SDSS-DR9 object that had been conflated with others. QSO-AGN separator restored to that used thru v2.9, thus ~5000 QSOs were re-classified as AGNe. AGNe historic names sourced from the Principal Galaxy Catalogue. 3.1 22Oct12 See list of changes above. &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/milliquas#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/milliquas</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=milliquas&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/milliquas.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MILLIQUAS [2]</TD>
            <TD>Million Quasars Catalog (MILLIQUAS), Version 3.1 (22 October 2012)</TD>
            <TD>This table contains the Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012). It is a compendium of all type I QSOs, AGN, and BL Lacs in the literature, up to 20 October 2012; completeness is full or nearly so. High-confidence (70+%) photometric SDSS and radio/X-ray associated objects are included, which bring the total number of objects to 1,226,331. Objects have been de-duplicated across catalogs, and the earliest name and best redshift is presented for each. Astrometry is fixed onto a combined APM/USNO-A/SDSS optical background, and is accurate to within 1-2 arcseconds, even for the earliest quasars. Note that close objects and lensed images within 1.5 arcseconds may be represented as single objects. This version has the following changes from the previous edition: &lt;pre&gt; (1) Quasar data brought up to publications as at 20 October 2012, including the new DR9 Quasar catalog (Paris I., 2012,arXiv:1210.5166). &lt;/pre&gt; The contents are relatively simple, each object is shown as one entry with the sky coordinates, its name, red and blue optical magnitudes, PSF class, redshift, and the source catalog for its name and redshift, plus a radio and/or X-ray identifier where applicable. The author's current plans are to keep this updated as a "living" QSO catalog, and to think about formal publication at a later date. Questions/comments/praise/complaints may be directed to Eric Flesch at eric@flesch.org. He requests that, if you use this catalog in published research, that you please add a small mention (acknowledgement). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is &lt;a href="http://www.sdss3.org/"&gt;http://www.sdss3.org/&lt;/a&gt;. Version Log: &lt;pre&gt; 0.1 22Apr09 0.3 6May09 Added a radio identifier and an X-ray identifier. 0.5 11May09 Added 30816 objects from newly calculated associations to XMM, Chandra and SUMSS detections, plus some tweaks. Also added QSO probability % for non-confirmed QSOs. 0.8 22Jun09 Added Chandra Source Catalog 1.0 (2009). 1.0 03Aug09 Extensive de-duplication. XMM Slew Catalog data added. 1.4 20Aug09 Misc fixes in the de-duplications. 1.5 29Aug09 Using XMM Slew Catalog v1.3 2.0 14Jun10 Using XMM Slew Catalog v1.4, XMM3 and XASSIST4. 2.1 17Aug10 Removed 8627 NELGs masquerading as AGN. 2.2 7Jan11 About 10,000 AGNe from the previous edition are now presented as QSOs. 796 AGNe mistakenly expunged in 2.1 have been restored. 2.3 5Mar11 SDSS DR-8 and BOSS targets have been included and the threshold for inclusions of candidates has been raised from 60% to 70%. 2.4 5Jun11 Improved QSO-likelihood calculation for the BOSS targets, so 17% of previously included BOSS targets drop out. Newly included data from several sources (see above). 2.5 20Jul11 Some deduplication of quasars which were discovered prior to 1990, 200 recent NED quasars added, some radio/X-ray associations to USNO-B optical data added. 2.6 10Sep11 The USNO-B catalog has been added and hard-deduplicated against APM and SDSS data to make a background pool of 1.04 billion optical objects. Also, about 12 million orphaned one-color APM objects have been removed. There are consequently improvements in this catalog's optical selections and astrometry without changing the net totals much. XMM Slew 1.5 catalog added. Some further astrometric fixes and deduplications of early quasars. 2.7 5Nov11 New quasar publications to 4 November 2011 were added, and a few fixes on individual objects incorporated. 2.8 29Jan12 Completed the fixes of non-astrometric relic data from the Veron-Cetty &amp; Veron 13th edition. About 150 other fixes. Quasars compilation updated through 27 January 2012. 2.9 2Apr12 Data brought up to publications as of 31 March 2012, about 50 astrometric fixes done, and the new FIRST radio catalog, 12Feb16 version, incorporated. 2.10 6Aug12 Data brought up to publications as of 31 July 2012, including the SDSS-DR9 release, Xassist XMM-Newton and Chandra X-ray data updated to 30 June 2012; as this is a catalog for type I (broad-line) objects, 1870 Seyfert-2s, 532 LINERs, and 6 NELGs were removed, but Bl Lacs were retained as unconstrained emission objects. 3.0 9Sep12 Data brought up to publications as at 31 August 2012. Redshifts are calculated for the XDQSO photometric quasar candidates. Fixed issues with 30 DEEP2 object. Separated out 15 SDSS-DR9 object that had been conflated with others. QSO-AGN separator restored to that used thru v2.9, thus ~5000 QSOs were re-classified as AGNe. AGNe historic names sourced from the Principal Galaxy Catalogue. 3.1 22Oct12 See list of changes above. &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/milliquas#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/milliquas</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=milliquas&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/milliquas.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MILLIQUAS [3]</TD>
            <TD>Million Quasars Catalog (MILLIQUAS), Version 3.1 (22 October 2012)</TD>
            <TD>This table contains the Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012). It is a compendium of all type I QSOs, AGN, and BL Lacs in the literature, up to 20 October 2012; completeness is full or nearly so. High-confidence (70+%) photometric SDSS and radio/X-ray associated objects are included, which bring the total number of objects to 1,226,331. Objects have been de-duplicated across catalogs, and the earliest name and best redshift is presented for each. Astrometry is fixed onto a combined APM/USNO-A/SDSS optical background, and is accurate to within 1-2 arcseconds, even for the earliest quasars. Note that close objects and lensed images within 1.5 arcseconds may be represented as single objects. This version has the following changes from the previous edition: &lt;pre&gt; (1) Quasar data brought up to publications as at 20 October 2012, including the new DR9 Quasar catalog (Paris I., 2012,arXiv:1210.5166). &lt;/pre&gt; The contents are relatively simple, each object is shown as one entry with the sky coordinates, its name, red and blue optical magnitudes, PSF class, redshift, and the source catalog for its name and redshift, plus a radio and/or X-ray identifier where applicable. The author's current plans are to keep this updated as a "living" QSO catalog, and to think about formal publication at a later date. Questions/comments/praise/complaints may be directed to Eric Flesch at eric@flesch.org. He requests that, if you use this catalog in published research, that you please add a small mention (acknowledgement). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is &lt;a href="http://www.sdss3.org/"&gt;http://www.sdss3.org/&lt;/a&gt;. Version Log: &lt;pre&gt; 0.1 22Apr09 0.3 6May09 Added a radio identifier and an X-ray identifier. 0.5 11May09 Added 30816 objects from newly calculated associations to XMM, Chandra and SUMSS detections, plus some tweaks. Also added QSO probability % for non-confirmed QSOs. 0.8 22Jun09 Added Chandra Source Catalog 1.0 (2009). 1.0 03Aug09 Extensive de-duplication. XMM Slew Catalog data added. 1.4 20Aug09 Misc fixes in the de-duplications. 1.5 29Aug09 Using XMM Slew Catalog v1.3 2.0 14Jun10 Using XMM Slew Catalog v1.4, XMM3 and XASSIST4. 2.1 17Aug10 Removed 8627 NELGs masquerading as AGN. 2.2 7Jan11 About 10,000 AGNe from the previous edition are now presented as QSOs. 796 AGNe mistakenly expunged in 2.1 have been restored. 2.3 5Mar11 SDSS DR-8 and BOSS targets have been included and the threshold for inclusions of candidates has been raised from 60% to 70%. 2.4 5Jun11 Improved QSO-likelihood calculation for the BOSS targets, so 17% of previously included BOSS targets drop out. Newly included data from several sources (see above). 2.5 20Jul11 Some deduplication of quasars which were discovered prior to 1990, 200 recent NED quasars added, some radio/X-ray associations to USNO-B optical data added. 2.6 10Sep11 The USNO-B catalog has been added and hard-deduplicated against APM and SDSS data to make a background pool of 1.04 billion optical objects. Also, about 12 million orphaned one-color APM objects have been removed. There are consequently improvements in this catalog's optical selections and astrometry without changing the net totals much. XMM Slew 1.5 catalog added. Some further astrometric fixes and deduplications of early quasars. 2.7 5Nov11 New quasar publications to 4 November 2011 were added, and a few fixes on individual objects incorporated. 2.8 29Jan12 Completed the fixes of non-astrometric relic data from the Veron-Cetty &amp; Veron 13th edition. About 150 other fixes. Quasars compilation updated through 27 January 2012. 2.9 2Apr12 Data brought up to publications as of 31 March 2012, about 50 astrometric fixes done, and the new FIRST radio catalog, 12Feb16 version, incorporated. 2.10 6Aug12 Data brought up to publications as of 31 July 2012, including the SDSS-DR9 release, Xassist XMM-Newton and Chandra X-ray data updated to 30 June 2012; as this is a catalog for type I (broad-line) objects, 1870 Seyfert-2s, 532 LINERs, and 6 NELGs were removed, but Bl Lacs were retained as unconstrained emission objects. 3.0 9Sep12 Data brought up to publications as at 31 August 2012. Redshifts are calculated for the XDQSO photometric quasar candidates. Fixed issues with 30 DEEP2 object. Separated out 15 SDSS-DR9 object that had been conflated with others. QSO-AGN separator restored to that used thru v2.9, thus ~5000 QSOs were re-classified as AGNe. AGNe historic names sourced from the Principal Galaxy Catalogue. 3.1 22Oct12 See list of changes above. &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/milliquas#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/milliquas</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_milliquas&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/milliquas.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/352/939 [1]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#1</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/352/939</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/352/939 [2]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#2</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/352/939&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/939 [voids]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#voids</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/939&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/939 [table1]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#table1</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/939&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MCG [1]</TD>
            <TD>Morphological Galaxy Catalog</TD>
            <TD>The MCG database contains the "Morphological Catalogue of Galaxies," a compilation of information for approximately 34,000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29,000 galaxies and information on the remaining 5,000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01 (+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are numbered with increasing right ascension. The original goal of the compilation was to be complete for galaxies brighter than magnitude 15.1, but the final catalog lists many objects considerably fainter. Information given in the original printed volumes includes: cross- identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes and intensities of the bright inner region and the entire object, estimated inclination, and coded description (by symbols) of the appearance of the galaxy. Each field is then followed by notes on individual objects. All of the above data except the coded description are included in the machine version, except that special coding (e.g. for uncertainty or source designation) is not present (other than for the NGC/IC cross identifications [added at the Astronomical Data Center for this machine version]). Although the notes are not computerized, the presence of a note in the original is flagged in the machine version Detailed descriptions of modifications, corrections and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional Information section below. In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalog resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/mcg#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcg</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=mcg&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/mcg.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MCG [2]</TD>
            <TD>Morphological Galaxy Catalog</TD>
            <TD>The MCG database contains the "Morphological Catalogue of Galaxies," a compilation of information for approximately 34,000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29,000 galaxies and information on the remaining 5,000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01 (+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are numbered with increasing right ascension. The original goal of the compilation was to be complete for galaxies brighter than magnitude 15.1, but the final catalog lists many objects considerably fainter. Information given in the original printed volumes includes: cross- identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes and intensities of the bright inner region and the entire object, estimated inclination, and coded description (by symbols) of the appearance of the galaxy. Each field is then followed by notes on individual objects. All of the above data except the coded description are included in the machine version, except that special coding (e.g. for uncertainty or source designation) is not present (other than for the NGC/IC cross identifications [added at the Astronomical Data Center for this machine version]). Although the notes are not computerized, the presence of a note in the original is flagged in the machine version Detailed descriptions of modifications, corrections and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional Information section below. In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalog resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/mcg#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=mcg&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/mcg.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MCG [3]</TD>
            <TD>Morphological Galaxy Catalog</TD>
            <TD>The MCG database contains the "Morphological Catalogue of Galaxies," a compilation of information for approximately 34,000 galaxies found and examined on the Palomar Observatory Sky Survey (POSS). Individual identifiers are assigned for about 29,000 galaxies and information on the remaining 5,000 is present in the extensive notes of the published catalogs (Vorontsov-Velyaminov et al. 1962-1968). The catalog is structured according to the POSS zones and is numbered from +15 (corresponding to +90 deg) to +01 (+06 deg zone) and +00 (equatorial zone) to -05 (-30 deg zone); the fields are numbered with increasing right ascension. The original goal of the compilation was to be complete for galaxies brighter than magnitude 15.1, but the final catalog lists many objects considerably fainter. Information given in the original printed volumes includes: cross- identifications to the NGC (Dreyer 1888) and IC (Dreyer 1895, 1908) catalogs, equatorial coordinates for 1950.0, magnitude, estimated sizes and intensities of the bright inner region and the entire object, estimated inclination, and coded description (by symbols) of the appearance of the galaxy. Each field is then followed by notes on individual objects. All of the above data except the coded description are included in the machine version, except that special coding (e.g. for uncertainty or source designation) is not present (other than for the NGC/IC cross identifications [added at the Astronomical Data Center for this machine version]). Although the notes are not computerized, the presence of a note in the original is flagged in the machine version Detailed descriptions of modifications, corrections and the record format are provided for the machine-readable version of the "Morphological Catalogue of Galaxies" (Vorontsov-Velyaminov et al. 1962-68); see the Additional Information section below. In addition to hundreds of individual corrections, a detailed comparison of the machine-readable with the published catalog resulted in the addition of 116 missing objects, the deletion of 10 duplicate records, and a format modification to increase storage efficiency.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/mcg#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcg</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_mcg&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/mcg.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MILLIQUAS [1]</TD>
            <TD>Million Quasars Catalog (MILLIQUAS), Version 3.1 (22 October 2012)</TD>
            <TD>This table contains the Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012). It is a compendium of all type I QSOs, AGN, and BL Lacs in the literature, up to 20 October 2012; completeness is full or nearly so. High-confidence (70+%) photometric SDSS and radio/X-ray associated objects are included, which bring the total number of objects to 1,226,331. Objects have been de-duplicated across catalogs, and the earliest name and best redshift is presented for each. Astrometry is fixed onto a combined APM/USNO-A/SDSS optical background, and is accurate to within 1-2 arcseconds, even for the earliest quasars. Note that close objects and lensed images within 1.5 arcseconds may be represented as single objects. This version has the following changes from the previous edition: &lt;pre&gt; (1) Quasar data brought up to publications as at 20 October 2012, including the new DR9 Quasar catalog (Paris I., 2012,arXiv:1210.5166). &lt;/pre&gt; The contents are relatively simple, each object is shown as one entry with the sky coordinates, its name, red and blue optical magnitudes, PSF class, redshift, and the source catalog for its name and redshift, plus a radio and/or X-ray identifier where applicable. The author's current plans are to keep this updated as a "living" QSO catalog, and to think about formal publication at a later date. Questions/comments/praise/complaints may be directed to Eric Flesch at eric@flesch.org. He requests that, if you use this catalog in published research, that you please add a small mention (acknowledgement). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is &lt;a href="http://www.sdss3.org/"&gt;http://www.sdss3.org/&lt;/a&gt;. Version Log: &lt;pre&gt; 0.1 22Apr09 0.3 6May09 Added a radio identifier and an X-ray identifier. 0.5 11May09 Added 30816 objects from newly calculated associations to XMM, Chandra and SUMSS detections, plus some tweaks. Also added QSO probability % for non-confirmed QSOs. 0.8 22Jun09 Added Chandra Source Catalog 1.0 (2009). 1.0 03Aug09 Extensive de-duplication. XMM Slew Catalog data added. 1.4 20Aug09 Misc fixes in the de-duplications. 1.5 29Aug09 Using XMM Slew Catalog v1.3 2.0 14Jun10 Using XMM Slew Catalog v1.4, XMM3 and XASSIST4. 2.1 17Aug10 Removed 8627 NELGs masquerading as AGN. 2.2 7Jan11 About 10,000 AGNe from the previous edition are now presented as QSOs. 796 AGNe mistakenly expunged in 2.1 have been restored. 2.3 5Mar11 SDSS DR-8 and BOSS targets have been included and the threshold for inclusions of candidates has been raised from 60% to 70%. 2.4 5Jun11 Improved QSO-likelihood calculation for the BOSS targets, so 17% of previously included BOSS targets drop out. Newly included data from several sources (see above). 2.5 20Jul11 Some deduplication of quasars which were discovered prior to 1990, 200 recent NED quasars added, some radio/X-ray associations to USNO-B optical data added. 2.6 10Sep11 The USNO-B catalog has been added and hard-deduplicated against APM and SDSS data to make a background pool of 1.04 billion optical objects. Also, about 12 million orphaned one-color APM objects have been removed. There are consequently improvements in this catalog's optical selections and astrometry without changing the net totals much. XMM Slew 1.5 catalog added. Some further astrometric fixes and deduplications of early quasars. 2.7 5Nov11 New quasar publications to 4 November 2011 were added, and a few fixes on individual objects incorporated. 2.8 29Jan12 Completed the fixes of non-astrometric relic data from the Veron-Cetty &amp; Veron 13th edition. About 150 other fixes. Quasars compilation updated through 27 January 2012. 2.9 2Apr12 Data brought up to publications as of 31 March 2012, about 50 astrometric fixes done, and the new FIRST radio catalog, 12Feb16 version, incorporated. 2.10 6Aug12 Data brought up to publications as of 31 July 2012, including the SDSS-DR9 release, Xassist XMM-Newton and Chandra X-ray data updated to 30 June 2012; as this is a catalog for type I (broad-line) objects, 1870 Seyfert-2s, 532 LINERs, and 6 NELGs were removed, but Bl Lacs were retained as unconstrained emission objects. 3.0 9Sep12 Data brought up to publications as at 31 August 2012. Redshifts are calculated for the XDQSO photometric quasar candidates. Fixed issues with 30 DEEP2 object. Separated out 15 SDSS-DR9 object that had been conflated with others. QSO-AGN separator restored to that used thru v2.9, thus ~5000 QSOs were re-classified as AGNe. AGNe historic names sourced from the Principal Galaxy Catalogue. 3.1 22Oct12 See list of changes above. &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/milliquas#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/milliquas</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=milliquas&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/milliquas.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MILLIQUAS [2]</TD>
            <TD>Million Quasars Catalog (MILLIQUAS), Version 3.1 (22 October 2012)</TD>
            <TD>This table contains the Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012). It is a compendium of all type I QSOs, AGN, and BL Lacs in the literature, up to 20 October 2012; completeness is full or nearly so. High-confidence (70+%) photometric SDSS and radio/X-ray associated objects are included, which bring the total number of objects to 1,226,331. Objects have been de-duplicated across catalogs, and the earliest name and best redshift is presented for each. Astrometry is fixed onto a combined APM/USNO-A/SDSS optical background, and is accurate to within 1-2 arcseconds, even for the earliest quasars. Note that close objects and lensed images within 1.5 arcseconds may be represented as single objects. This version has the following changes from the previous edition: &lt;pre&gt; (1) Quasar data brought up to publications as at 20 October 2012, including the new DR9 Quasar catalog (Paris I., 2012,arXiv:1210.5166). &lt;/pre&gt; The contents are relatively simple, each object is shown as one entry with the sky coordinates, its name, red and blue optical magnitudes, PSF class, redshift, and the source catalog for its name and redshift, plus a radio and/or X-ray identifier where applicable. The author's current plans are to keep this updated as a "living" QSO catalog, and to think about formal publication at a later date. Questions/comments/praise/complaints may be directed to Eric Flesch at eric@flesch.org. He requests that, if you use this catalog in published research, that you please add a small mention (acknowledgement). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is &lt;a href="http://www.sdss3.org/"&gt;http://www.sdss3.org/&lt;/a&gt;. Version Log: &lt;pre&gt; 0.1 22Apr09 0.3 6May09 Added a radio identifier and an X-ray identifier. 0.5 11May09 Added 30816 objects from newly calculated associations to XMM, Chandra and SUMSS detections, plus some tweaks. Also added QSO probability % for non-confirmed QSOs. 0.8 22Jun09 Added Chandra Source Catalog 1.0 (2009). 1.0 03Aug09 Extensive de-duplication. XMM Slew Catalog data added. 1.4 20Aug09 Misc fixes in the de-duplications. 1.5 29Aug09 Using XMM Slew Catalog v1.3 2.0 14Jun10 Using XMM Slew Catalog v1.4, XMM3 and XASSIST4. 2.1 17Aug10 Removed 8627 NELGs masquerading as AGN. 2.2 7Jan11 About 10,000 AGNe from the previous edition are now presented as QSOs. 796 AGNe mistakenly expunged in 2.1 have been restored. 2.3 5Mar11 SDSS DR-8 and BOSS targets have been included and the threshold for inclusions of candidates has been raised from 60% to 70%. 2.4 5Jun11 Improved QSO-likelihood calculation for the BOSS targets, so 17% of previously included BOSS targets drop out. Newly included data from several sources (see above). 2.5 20Jul11 Some deduplication of quasars which were discovered prior to 1990, 200 recent NED quasars added, some radio/X-ray associations to USNO-B optical data added. 2.6 10Sep11 The USNO-B catalog has been added and hard-deduplicated against APM and SDSS data to make a background pool of 1.04 billion optical objects. Also, about 12 million orphaned one-color APM objects have been removed. There are consequently improvements in this catalog's optical selections and astrometry without changing the net totals much. XMM Slew 1.5 catalog added. Some further astrometric fixes and deduplications of early quasars. 2.7 5Nov11 New quasar publications to 4 November 2011 were added, and a few fixes on individual objects incorporated. 2.8 29Jan12 Completed the fixes of non-astrometric relic data from the Veron-Cetty &amp; Veron 13th edition. About 150 other fixes. Quasars compilation updated through 27 January 2012. 2.9 2Apr12 Data brought up to publications as of 31 March 2012, about 50 astrometric fixes done, and the new FIRST radio catalog, 12Feb16 version, incorporated. 2.10 6Aug12 Data brought up to publications as of 31 July 2012, including the SDSS-DR9 release, Xassist XMM-Newton and Chandra X-ray data updated to 30 June 2012; as this is a catalog for type I (broad-line) objects, 1870 Seyfert-2s, 532 LINERs, and 6 NELGs were removed, but Bl Lacs were retained as unconstrained emission objects. 3.0 9Sep12 Data brought up to publications as at 31 August 2012. Redshifts are calculated for the XDQSO photometric quasar candidates. Fixed issues with 30 DEEP2 object. Separated out 15 SDSS-DR9 object that had been conflated with others. QSO-AGN separator restored to that used thru v2.9, thus ~5000 QSOs were re-classified as AGNe. AGNe historic names sourced from the Principal Galaxy Catalogue. 3.1 22Oct12 See list of changes above. &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/milliquas#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/milliquas</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=milliquas&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/milliquas.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MILLIQUAS [3]</TD>
            <TD>Million Quasars Catalog (MILLIQUAS), Version 3.1 (22 October 2012)</TD>
            <TD>This table contains the Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012). It is a compendium of all type I QSOs, AGN, and BL Lacs in the literature, up to 20 October 2012; completeness is full or nearly so. High-confidence (70+%) photometric SDSS and radio/X-ray associated objects are included, which bring the total number of objects to 1,226,331. Objects have been de-duplicated across catalogs, and the earliest name and best redshift is presented for each. Astrometry is fixed onto a combined APM/USNO-A/SDSS optical background, and is accurate to within 1-2 arcseconds, even for the earliest quasars. Note that close objects and lensed images within 1.5 arcseconds may be represented as single objects. This version has the following changes from the previous edition: &lt;pre&gt; (1) Quasar data brought up to publications as at 20 October 2012, including the new DR9 Quasar catalog (Paris I., 2012,arXiv:1210.5166). &lt;/pre&gt; The contents are relatively simple, each object is shown as one entry with the sky coordinates, its name, red and blue optical magnitudes, PSF class, redshift, and the source catalog for its name and redshift, plus a radio and/or X-ray identifier where applicable. The author's current plans are to keep this updated as a "living" QSO catalog, and to think about formal publication at a later date. Questions/comments/praise/complaints may be directed to Eric Flesch at eric@flesch.org. He requests that, if you use this catalog in published research, that you please add a small mention (acknowledgement). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is &lt;a href="http://www.sdss3.org/"&gt;http://www.sdss3.org/&lt;/a&gt;. Version Log: &lt;pre&gt; 0.1 22Apr09 0.3 6May09 Added a radio identifier and an X-ray identifier. 0.5 11May09 Added 30816 objects from newly calculated associations to XMM, Chandra and SUMSS detections, plus some tweaks. Also added QSO probability % for non-confirmed QSOs. 0.8 22Jun09 Added Chandra Source Catalog 1.0 (2009). 1.0 03Aug09 Extensive de-duplication. XMM Slew Catalog data added. 1.4 20Aug09 Misc fixes in the de-duplications. 1.5 29Aug09 Using XMM Slew Catalog v1.3 2.0 14Jun10 Using XMM Slew Catalog v1.4, XMM3 and XASSIST4. 2.1 17Aug10 Removed 8627 NELGs masquerading as AGN. 2.2 7Jan11 About 10,000 AGNe from the previous edition are now presented as QSOs. 796 AGNe mistakenly expunged in 2.1 have been restored. 2.3 5Mar11 SDSS DR-8 and BOSS targets have been included and the threshold for inclusions of candidates has been raised from 60% to 70%. 2.4 5Jun11 Improved QSO-likelihood calculation for the BOSS targets, so 17% of previously included BOSS targets drop out. Newly included data from several sources (see above). 2.5 20Jul11 Some deduplication of quasars which were discovered prior to 1990, 200 recent NED quasars added, some radio/X-ray associations to USNO-B optical data added. 2.6 10Sep11 The USNO-B catalog has been added and hard-deduplicated against APM and SDSS data to make a background pool of 1.04 billion optical objects. Also, about 12 million orphaned one-color APM objects have been removed. There are consequently improvements in this catalog's optical selections and astrometry without changing the net totals much. XMM Slew 1.5 catalog added. Some further astrometric fixes and deduplications of early quasars. 2.7 5Nov11 New quasar publications to 4 November 2011 were added, and a few fixes on individual objects incorporated. 2.8 29Jan12 Completed the fixes of non-astrometric relic data from the Veron-Cetty &amp; Veron 13th edition. About 150 other fixes. Quasars compilation updated through 27 January 2012. 2.9 2Apr12 Data brought up to publications as of 31 March 2012, about 50 astrometric fixes done, and the new FIRST radio catalog, 12Feb16 version, incorporated. 2.10 6Aug12 Data brought up to publications as of 31 July 2012, including the SDSS-DR9 release, Xassist XMM-Newton and Chandra X-ray data updated to 30 June 2012; as this is a catalog for type I (broad-line) objects, 1870 Seyfert-2s, 532 LINERs, and 6 NELGs were removed, but Bl Lacs were retained as unconstrained emission objects. 3.0 9Sep12 Data brought up to publications as at 31 August 2012. Redshifts are calculated for the XDQSO photometric quasar candidates. Fixed issues with 30 DEEP2 object. Separated out 15 SDSS-DR9 object that had been conflated with others. QSO-AGN separator restored to that used thru v2.9, thus ~5000 QSOs were re-classified as AGNe. AGNe historic names sourced from the Principal Galaxy Catalogue. 3.1 22Oct12 See list of changes above. &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/milliquas#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/milliquas</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_milliquas&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/milliquas.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/352/939 [1]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#1</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/352/939</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/352/939 [2]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#2</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/352/939&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/939 [voids]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#voids</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/939&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/939 [table1]</TD>
            <TD>2dFGRS Wiener reconstruction of cosmic web (Erdogdu+, 2004)</TD>
            <TD>The 2dFGRS (&lt;VII/226&gt;), now completed, is selected in the photometric b_J_ band from the Automated Plate Measuring (APM, &lt;J/MNRAS/246/433&gt;) galaxy survey and its subsequent extensions. We use the data obtained prior to 2002 May, when the survey was nearly complete. This includes 221283 unique, reliable galaxy redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939#table1</TD>
            <TD>2012-11-13T14:10:37Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/939</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/939&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/939</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Messier [1]</TD>
            <TD>Messier Nebulae</TD>
            <TD>The Messier Catalog of bright, extended objects was compiled by the comet-hunter Charles Messier in the 18th century. It comprised a list of 110 objects which are mostly brighter than 10th magnitude and have angular sizes from 1 to 100 arcminutes. M 102 is now generally considered to be spurious, and the object so named was actually M 101. Hence this electronic version of the Messier Catalog contains only 109 objects. The objects in the Messier Catalog are predominantly star clusters in our Milky Way galaxy, with 29 of them being globular clusters, 27 open clusters; the rest are spiral galaxies (27), elliptical galaxies (11), diffuse and planetary nebulae (10), and miscellaneous objects (5). All of the objects in the Messier Catalog are north of -35 degrees declination.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/messier#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Nebula#Galaxy#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/messier</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=messier&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/messier.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Messier [2]</TD>
            <TD>Messier Nebulae</TD>
            <TD>The Messier Catalog of bright, extended objects was compiled by the comet-hunter Charles Messier in the 18th century. It comprised a list of 110 objects which are mostly brighter than 10th magnitude and have angular sizes from 1 to 100 arcminutes. M 102 is now generally considered to be spurious, and the object so named was actually M 101. Hence this electronic version of the Messier Catalog contains only 109 objects. The objects in the Messier Catalog are predominantly star clusters in our Milky Way galaxy, with 29 of them being globular clusters, 27 open clusters; the rest are spiral galaxies (27), elliptical galaxies (11), diffuse and planetary nebulae (10), and miscellaneous objects (5). All of the objects in the Messier Catalog are north of -35 degrees declination.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/messier#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Nebula#Galaxy#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/messier</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=messier&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/messier.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Messier [3]</TD>
            <TD>Messier Nebulae</TD>
            <TD>The Messier Catalog of bright, extended objects was compiled by the comet-hunter Charles Messier in the 18th century. It comprised a list of 110 objects which are mostly brighter than 10th magnitude and have angular sizes from 1 to 100 arcminutes. M 102 is now generally considered to be spurious, and the object so named was actually M 101. Hence this electronic version of the Messier Catalog contains only 109 objects. The objects in the Messier Catalog are predominantly star clusters in our Milky Way galaxy, with 29 of them being globular clusters, 27 open clusters; the rest are spiral galaxies (27), elliptical galaxies (11), diffuse and planetary nebulae (10), and miscellaneous objects (5). All of the objects in the Messier Catalog are north of -35 degrees declination.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/messier#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Nebula#Galaxy#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/messier</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_messier&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/messier.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MILLIQUAS [1]</TD>
            <TD>Million Quasars Catalog (MILLIQUAS), Version 3.1 (22 October 2012)</TD>
            <TD>This table contains the Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012). It is a compendium of all type I QSOs, AGN, and BL Lacs in the literature, up to 20 October 2012; completeness is full or nearly so. High-confidence (70+%) photometric SDSS and radio/X-ray associated objects are included, which bring the total number of objects to 1,226,331. Objects have been de-duplicated across catalogs, and the earliest name and best redshift is presented for each. Astrometry is fixed onto a combined APM/USNO-A/SDSS optical background, and is accurate to within 1-2 arcseconds, even for the earliest quasars. Note that close objects and lensed images within 1.5 arcseconds may be represented as single objects. This version has the following changes from the previous edition: &lt;pre&gt; (1) Quasar data brought up to publications as at 20 October 2012, including the new DR9 Quasar catalog (Paris I., 2012,arXiv:1210.5166). &lt;/pre&gt; The contents are relatively simple, each object is shown as one entry with the sky coordinates, its name, red and blue optical magnitudes, PSF class, redshift, and the source catalog for its name and redshift, plus a radio and/or X-ray identifier where applicable. The author's current plans are to keep this updated as a "living" QSO catalog, and to think about formal publication at a later date. Questions/comments/praise/complaints may be directed to Eric Flesch at eric@flesch.org. He requests that, if you use this catalog in published research, that you please add a small mention (acknowledgement). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is &lt;a href="http://www.sdss3.org/"&gt;http://www.sdss3.org/&lt;/a&gt;. Version Log: &lt;pre&gt; 0.1 22Apr09 0.3 6May09 Added a radio identifier and an X-ray identifier. 0.5 11May09 Added 30816 objects from newly calculated associations to XMM, Chandra and SUMSS detections, plus some tweaks. Also added QSO probability % for non-confirmed QSOs. 0.8 22Jun09 Added Chandra Source Catalog 1.0 (2009). 1.0 03Aug09 Extensive de-duplication. XMM Slew Catalog data added. 1.4 20Aug09 Misc fixes in the de-duplications. 1.5 29Aug09 Using XMM Slew Catalog v1.3 2.0 14Jun10 Using XMM Slew Catalog v1.4, XMM3 and XASSIST4. 2.1 17Aug10 Removed 8627 NELGs masquerading as AGN. 2.2 7Jan11 About 10,000 AGNe from the previous edition are now presented as QSOs. 796 AGNe mistakenly expunged in 2.1 have been restored. 2.3 5Mar11 SDSS DR-8 and BOSS targets have been included and the threshold for inclusions of candidates has been raised from 60% to 70%. 2.4 5Jun11 Improved QSO-likelihood calculation for the BOSS targets, so 17% of previously included BOSS targets drop out. Newly included data from several sources (see above). 2.5 20Jul11 Some deduplication of quasars which were discovered prior to 1990, 200 recent NED quasars added, some radio/X-ray associations to USNO-B optical data added. 2.6 10Sep11 The USNO-B catalog has been added and hard-deduplicated against APM and SDSS data to make a background pool of 1.04 billion optical objects. Also, about 12 million orphaned one-color APM objects have been removed. There are consequently improvements in this catalog's optical selections and astrometry without changing the net totals much. XMM Slew 1.5 catalog added. Some further astrometric fixes and deduplications of early quasars. 2.7 5Nov11 New quasar publications to 4 November 2011 were added, and a few fixes on individual objects incorporated. 2.8 29Jan12 Completed the fixes of non-astrometric relic data from the Veron-Cetty &amp; Veron 13th edition. About 150 other fixes. Quasars compilation updated through 27 January 2012. 2.9 2Apr12 Data brought up to publications as of 31 March 2012, about 50 astrometric fixes done, and the new FIRST radio catalog, 12Feb16 version, incorporated. 2.10 6Aug12 Data brought up to publications as of 31 July 2012, including the SDSS-DR9 release, Xassist XMM-Newton and Chandra X-ray data updated to 30 June 2012; as this is a catalog for type I (broad-line) objects, 1870 Seyfert-2s, 532 LINERs, and 6 NELGs were removed, but Bl Lacs were retained as unconstrained emission objects. 3.0 9Sep12 Data brought up to publications as at 31 August 2012. Redshifts are calculated for the XDQSO photometric quasar candidates. Fixed issues with 30 DEEP2 object. Separated out 15 SDSS-DR9 object that had been conflated with others. QSO-AGN separator restored to that used thru v2.9, thus ~5000 QSOs were re-classified as AGNe. AGNe historic names sourced from the Principal Galaxy Catalogue. 3.1 22Oct12 See list of changes above. &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/milliquas#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/milliquas</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=milliquas&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/milliquas.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MILLIQUAS [2]</TD>
            <TD>Million Quasars Catalog (MILLIQUAS), Version 3.1 (22 October 2012)</TD>
            <TD>This table contains the Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012). It is a compendium of all type I QSOs, AGN, and BL Lacs in the literature, up to 20 October 2012; completeness is full or nearly so. High-confidence (70+%) photometric SDSS and radio/X-ray associated objects are included, which bring the total number of objects to 1,226,331. Objects have been de-duplicated across catalogs, and the earliest name and best redshift is presented for each. Astrometry is fixed onto a combined APM/USNO-A/SDSS optical background, and is accurate to within 1-2 arcseconds, even for the earliest quasars. Note that close objects and lensed images within 1.5 arcseconds may be represented as single objects. This version has the following changes from the previous edition: &lt;pre&gt; (1) Quasar data brought up to publications as at 20 October 2012, including the new DR9 Quasar catalog (Paris I., 2012,arXiv:1210.5166). &lt;/pre&gt; The contents are relatively simple, each object is shown as one entry with the sky coordinates, its name, red and blue optical magnitudes, PSF class, redshift, and the source catalog for its name and redshift, plus a radio and/or X-ray identifier where applicable. The author's current plans are to keep this updated as a "living" QSO catalog, and to think about formal publication at a later date. Questions/comments/praise/complaints may be directed to Eric Flesch at eric@flesch.org. He requests that, if you use this catalog in published research, that you please add a small mention (acknowledgement). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is &lt;a href="http://www.sdss3.org/"&gt;http://www.sdss3.org/&lt;/a&gt;. Version Log: &lt;pre&gt; 0.1 22Apr09 0.3 6May09 Added a radio identifier and an X-ray identifier. 0.5 11May09 Added 30816 objects from newly calculated associations to XMM, Chandra and SUMSS detections, plus some tweaks. Also added QSO probability % for non-confirmed QSOs. 0.8 22Jun09 Added Chandra Source Catalog 1.0 (2009). 1.0 03Aug09 Extensive de-duplication. XMM Slew Catalog data added. 1.4 20Aug09 Misc fixes in the de-duplications. 1.5 29Aug09 Using XMM Slew Catalog v1.3 2.0 14Jun10 Using XMM Slew Catalog v1.4, XMM3 and XASSIST4. 2.1 17Aug10 Removed 8627 NELGs masquerading as AGN. 2.2 7Jan11 About 10,000 AGNe from the previous edition are now presented as QSOs. 796 AGNe mistakenly expunged in 2.1 have been restored. 2.3 5Mar11 SDSS DR-8 and BOSS targets have been included and the threshold for inclusions of candidates has been raised from 60% to 70%. 2.4 5Jun11 Improved QSO-likelihood calculation for the BOSS targets, so 17% of previously included BOSS targets drop out. Newly included data from several sources (see above). 2.5 20Jul11 Some deduplication of quasars which were discovered prior to 1990, 200 recent NED quasars added, some radio/X-ray associations to USNO-B optical data added. 2.6 10Sep11 The USNO-B catalog has been added and hard-deduplicated against APM and SDSS data to make a background pool of 1.04 billion optical objects. Also, about 12 million orphaned one-color APM objects have been removed. There are consequently improvements in this catalog's optical selections and astrometry without changing the net totals much. XMM Slew 1.5 catalog added. Some further astrometric fixes and deduplications of early quasars. 2.7 5Nov11 New quasar publications to 4 November 2011 were added, and a few fixes on individual objects incorporated. 2.8 29Jan12 Completed the fixes of non-astrometric relic data from the Veron-Cetty &amp; Veron 13th edition. About 150 other fixes. Quasars compilation updated through 27 January 2012. 2.9 2Apr12 Data brought up to publications as of 31 March 2012, about 50 astrometric fixes done, and the new FIRST radio catalog, 12Feb16 version, incorporated. 2.10 6Aug12 Data brought up to publications as of 31 July 2012, including the SDSS-DR9 release, Xassist XMM-Newton and Chandra X-ray data updated to 30 June 2012; as this is a catalog for type I (broad-line) objects, 1870 Seyfert-2s, 532 LINERs, and 6 NELGs were removed, but Bl Lacs were retained as unconstrained emission objects. 3.0 9Sep12 Data brought up to publications as at 31 August 2012. Redshifts are calculated for the XDQSO photometric quasar candidates. Fixed issues with 30 DEEP2 object. Separated out 15 SDSS-DR9 object that had been conflated with others. QSO-AGN separator restored to that used thru v2.9, thus ~5000 QSOs were re-classified as AGNe. AGNe historic names sourced from the Principal Galaxy Catalogue. 3.1 22Oct12 See list of changes above. &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/milliquas#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/milliquas</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=milliquas&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/milliquas.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MILLIQUAS [3]</TD>
            <TD>Million Quasars Catalog (MILLIQUAS), Version 3.1 (22 October 2012)</TD>
            <TD>This table contains the Million Quasars (MILLIQUAS) Catalog, Version 3.1 (22 October 2012). It is a compendium of all type I QSOs, AGN, and BL Lacs in the literature, up to 20 October 2012; completeness is full or nearly so. High-confidence (70+%) photometric SDSS and radio/X-ray associated objects are included, which bring the total number of objects to 1,226,331. Objects have been de-duplicated across catalogs, and the earliest name and best redshift is presented for each. Astrometry is fixed onto a combined APM/USNO-A/SDSS optical background, and is accurate to within 1-2 arcseconds, even for the earliest quasars. Note that close objects and lensed images within 1.5 arcseconds may be represented as single objects. This version has the following changes from the previous edition: &lt;pre&gt; (1) Quasar data brought up to publications as at 20 October 2012, including the new DR9 Quasar catalog (Paris I., 2012,arXiv:1210.5166). &lt;/pre&gt; The contents are relatively simple, each object is shown as one entry with the sky coordinates, its name, red and blue optical magnitudes, PSF class, redshift, and the source catalog for its name and redshift, plus a radio and/or X-ray identifier where applicable. The author's current plans are to keep this updated as a "living" QSO catalog, and to think about formal publication at a later date. Questions/comments/praise/complaints may be directed to Eric Flesch at eric@flesch.org. He requests that, if you use this catalog in published research, that you please add a small mention (acknowledgement). This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has also made use of data obtained from the Chandra Source Catalog, provided by the Chandra X-ray Center (CXC) as part of the Chandra Data Archive. Funding for SDSS-III has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, and the U.S. Department of Energy. The SDSS-III web site is &lt;a href="http://www.sdss3.org/"&gt;http://www.sdss3.org/&lt;/a&gt;. Version Log: &lt;pre&gt; 0.1 22Apr09 0.3 6May09 Added a radio identifier and an X-ray identifier. 0.5 11May09 Added 30816 objects from newly calculated associations to XMM, Chandra and SUMSS detections, plus some tweaks. Also added QSO probability % for non-confirmed QSOs. 0.8 22Jun09 Added Chandra Source Catalog 1.0 (2009). 1.0 03Aug09 Extensive de-duplication. XMM Slew Catalog data added. 1.4 20Aug09 Misc fixes in the de-duplications. 1.5 29Aug09 Using XMM Slew Catalog v1.3 2.0 14Jun10 Using XMM Slew Catalog v1.4, XMM3 and XASSIST4. 2.1 17Aug10 Removed 8627 NELGs masquerading as AGN. 2.2 7Jan11 About 10,000 AGNe from the previous edition are now presented as QSOs. 796 AGNe mistakenly expunged in 2.1 have been restored. 2.3 5Mar11 SDSS DR-8 and BOSS targets have been included and the threshold for inclusions of candidates has been raised from 60% to 70%. 2.4 5Jun11 Improved QSO-likelihood calculation for the BOSS targets, so 17% of previously included BOSS targets drop out. Newly included data from several sources (see above). 2.5 20Jul11 Some deduplication of quasars which were discovered prior to 1990, 200 recent NED quasars added, some radio/X-ray associations to USNO-B optical data added. 2.6 10Sep11 The USNO-B catalog has been added and hard-deduplicated against APM and SDSS data to make a background pool of 1.04 billion optical objects. Also, about 12 million orphaned one-color APM objects have been removed. There are consequently improvements in this catalog's optical selections and astrometry without changing the net totals much. XMM Slew 1.5 catalog added. Some further astrometric fixes and deduplications of early quasars. 2.7 5Nov11 New quasar publications to 4 November 2011 were added, and a few fixes on individual objects incorporated. 2.8 29Jan12 Completed the fixes of non-astrometric relic data from the Veron-Cetty &amp; Veron 13th edition. About 150 other fixes. Quasars compilation updated through 27 January 2012. 2.9 2Apr12 Data brought up to publications as of 31 March 2012, about 50 astrometric fixes done, and the new FIRST radio catalog, 12Feb16 version, incorporated. 2.10 6Aug12 Data brought up to publications as of 31 July 2012, including the SDSS-DR9 release, Xassist XMM-Newton and Chandra X-ray data updated to 30 June 2012; as this is a catalog for type I (broad-line) objects, 1870 Seyfert-2s, 532 LINERs, and 6 NELGs were removed, but Bl Lacs were retained as unconstrained emission objects. 3.0 9Sep12 Data brought up to publications as at 31 August 2012. Redshifts are calculated for the XDQSO photometric quasar candidates. Fixed issues with 30 DEEP2 object. Separated out 15 SDSS-DR9 object that had been conflated with others. QSO-AGN separator restored to that used thru v2.9, thus ~5000 QSOs were re-classified as AGNe. AGNe historic names sourced from the Principal Galaxy Catalogue. 3.1 22Oct12 See list of changes above. &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/milliquas#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/milliquas</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_milliquas&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/milliquas.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AN/329/801 [1]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#1</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AN/329/801</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AN/329/801 [2]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#2</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AN/329/801&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/329/801 [table1]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#table1</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/329/801&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/329/801 [tablea1]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#tablea1</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/329/801&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Messier [1]</TD>
            <TD>Messier Nebulae</TD>
            <TD>The Messier Catalog of bright, extended objects was compiled by the comet-hunter Charles Messier in the 18th century. It comprised a list of 110 objects which are mostly brighter than 10th magnitude and have angular sizes from 1 to 100 arcminutes. M 102 is now generally considered to be spurious, and the object so named was actually M 101. Hence this electronic version of the Messier Catalog contains only 109 objects. The objects in the Messier Catalog are predominantly star clusters in our Milky Way galaxy, with 29 of them being globular clusters, 27 open clusters; the rest are spiral galaxies (27), elliptical galaxies (11), diffuse and planetary nebulae (10), and miscellaneous objects (5). All of the objects in the Messier Catalog are north of -35 degrees declination.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/messier#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Nebula#Galaxy#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/messier</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=messier&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/messier.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Messier [2]</TD>
            <TD>Messier Nebulae</TD>
            <TD>The Messier Catalog of bright, extended objects was compiled by the comet-hunter Charles Messier in the 18th century. It comprised a list of 110 objects which are mostly brighter than 10th magnitude and have angular sizes from 1 to 100 arcminutes. M 102 is now generally considered to be spurious, and the object so named was actually M 101. Hence this electronic version of the Messier Catalog contains only 109 objects. The objects in the Messier Catalog are predominantly star clusters in our Milky Way galaxy, with 29 of them being globular clusters, 27 open clusters; the rest are spiral galaxies (27), elliptical galaxies (11), diffuse and planetary nebulae (10), and miscellaneous objects (5). All of the objects in the Messier Catalog are north of -35 degrees declination.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/messier#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Nebula#Galaxy#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/messier</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=messier&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/messier.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Messier [3]</TD>
            <TD>Messier Nebulae</TD>
            <TD>The Messier Catalog of bright, extended objects was compiled by the comet-hunter Charles Messier in the 18th century. It comprised a list of 110 objects which are mostly brighter than 10th magnitude and have angular sizes from 1 to 100 arcminutes. M 102 is now generally considered to be spurious, and the object so named was actually M 101. Hence this electronic version of the Messier Catalog contains only 109 objects. The objects in the Messier Catalog are predominantly star clusters in our Milky Way galaxy, with 29 of them being globular clusters, 27 open clusters; the rest are spiral galaxies (27), elliptical galaxies (11), diffuse and planetary nebulae (10), and miscellaneous objects (5). All of the objects in the Messier Catalog are north of -35 degrees declination.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/messier#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Nebula#Galaxy#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/messier</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_messier&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/messier.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC [1]</TD>
            <TD>NGC2000.0: Complete New General Catalog and Index Catalog</TD>
            <TD>NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox 2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine-readble version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation. Information on how to contact Sky Publishing is available at &lt;a href="http://www.shopatsky.com/contact_us"&gt;http://www.shopatsky.com/contact_us&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ngc2000#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Nebula#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2000</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc2000&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/ngc2000.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC [2]</TD>
            <TD>NGC2000.0: Complete New General Catalog and Index Catalog</TD>
            <TD>NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox 2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine-readble version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation. Information on how to contact Sky Publishing is available at &lt;a href="http://www.shopatsky.com/contact_us"&gt;http://www.shopatsky.com/contact_us&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ngc2000#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Nebula#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2000</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc2000&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/ngc2000.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC [3]</TD>
            <TD>NGC2000.0: Complete New General Catalog and Index Catalog</TD>
            <TD>NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox 2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine-readble version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation. Information on how to contact Sky Publishing is available at &lt;a href="http://www.shopatsky.com/contact_us"&gt;http://www.shopatsky.com/contact_us&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ngc2000#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Nebula#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2000</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc2000&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/ngc2000.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AN/329/801 [1]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#1</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AN/329/801</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AN/329/801 [2]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#2</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AN/329/801&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/329/801 [table1]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#table1</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/329/801&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/329/801 [tablea1]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#tablea1</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/329/801&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Messier [1]</TD>
            <TD>Messier Nebulae</TD>
            <TD>The Messier Catalog of bright, extended objects was compiled by the comet-hunter Charles Messier in the 18th century. It comprised a list of 110 objects which are mostly brighter than 10th magnitude and have angular sizes from 1 to 100 arcminutes. M 102 is now generally considered to be spurious, and the object so named was actually M 101. Hence this electronic version of the Messier Catalog contains only 109 objects. The objects in the Messier Catalog are predominantly star clusters in our Milky Way galaxy, with 29 of them being globular clusters, 27 open clusters; the rest are spiral galaxies (27), elliptical galaxies (11), diffuse and planetary nebulae (10), and miscellaneous objects (5). All of the objects in the Messier Catalog are north of -35 degrees declination.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/messier#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Nebula#Galaxy#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/messier</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=messier&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/messier.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Messier [2]</TD>
            <TD>Messier Nebulae</TD>
            <TD>The Messier Catalog of bright, extended objects was compiled by the comet-hunter Charles Messier in the 18th century. It comprised a list of 110 objects which are mostly brighter than 10th magnitude and have angular sizes from 1 to 100 arcminutes. M 102 is now generally considered to be spurious, and the object so named was actually M 101. Hence this electronic version of the Messier Catalog contains only 109 objects. The objects in the Messier Catalog are predominantly star clusters in our Milky Way galaxy, with 29 of them being globular clusters, 27 open clusters; the rest are spiral galaxies (27), elliptical galaxies (11), diffuse and planetary nebulae (10), and miscellaneous objects (5). All of the objects in the Messier Catalog are north of -35 degrees declination.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/messier#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Nebula#Galaxy#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/messier</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=messier&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/messier.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Messier [3]</TD>
            <TD>Messier Nebulae</TD>
            <TD>The Messier Catalog of bright, extended objects was compiled by the comet-hunter Charles Messier in the 18th century. It comprised a list of 110 objects which are mostly brighter than 10th magnitude and have angular sizes from 1 to 100 arcminutes. M 102 is now generally considered to be spurious, and the object so named was actually M 101. Hence this electronic version of the Messier Catalog contains only 109 objects. The objects in the Messier Catalog are predominantly star clusters in our Milky Way galaxy, with 29 of them being globular clusters, 27 open clusters; the rest are spiral galaxies (27), elliptical galaxies (11), diffuse and planetary nebulae (10), and miscellaneous objects (5). All of the objects in the Messier Catalog are north of -35 degrees declination.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/messier#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Nebula#Galaxy#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/messier</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_messier&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/messier.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC [1]</TD>
            <TD>NGC2000.0: Complete New General Catalog and Index Catalog</TD>
            <TD>NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox 2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine-readble version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation. Information on how to contact Sky Publishing is available at &lt;a href="http://www.shopatsky.com/contact_us"&gt;http://www.shopatsky.com/contact_us&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ngc2000#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Nebula#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2000</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc2000&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/ngc2000.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC [2]</TD>
            <TD>NGC2000.0: Complete New General Catalog and Index Catalog</TD>
            <TD>NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox 2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine-readble version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation. Information on how to contact Sky Publishing is available at &lt;a href="http://www.shopatsky.com/contact_us"&gt;http://www.shopatsky.com/contact_us&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ngc2000#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Nebula#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2000</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc2000&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/ngc2000.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC [3]</TD>
            <TD>NGC2000.0: Complete New General Catalog and Index Catalog</TD>
            <TD>NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox 2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine-readble version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation. Information on how to contact Sky Publishing is available at &lt;a href="http://www.shopatsky.com/contact_us"&gt;http://www.shopatsky.com/contact_us&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ngc2000#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Nebula#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2000</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc2000&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/ngc2000.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AN/329/801 [1]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#1</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AN/329/801</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AN/329/801 [2]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#2</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AN/329/801&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/329/801 [table1]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#table1</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/329/801&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/329/801 [tablea1]</TD>
            <TD>Agglomerate of early-type Hipparcos stars (Caballero+, 2008)</TD>
            <TD>We study the spatial structure and sub-structure of regions rich in Hipparcos stars with blue BT-VT colours. These regions, which comprise large stellar complexes, OB associations, and young open clusters, are tracers of on-going star formation in the Galaxy. The DBSCAN (Density-Based Spatial Clustering of Applications with Noise) data clustering algorithm is used to look for spatial overdensities of early-type stars. Once an overdensity, "agglomerate", is identified, we carry out a data and bibliographic compilation of their star member candidates. The actual membership in agglomerate of each early-type star is studied based on its heliocentric distance, proper motion, and previous spectro-photometric information. We identify 35 agglomerates of early-type Hipparcos stars. Most of them are associated to previously known clusters and OB associations. The previously unknown P Puppis agglomerate is subject of a dedicated study with Virtual Observatory tools.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801#tablea1</TD>
            <TD>2012-11-13T14:16:45Z</TD>
            <TD>#Associations#Proper_Motions#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AN/329/801</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/329/801&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/329/801</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC6334CXO [1]</TD>
            <TD>NGC 6334 Chandra X-Ray Point Source Catalog</TD>
            <TD>The full stellar population of NGC 6334, one of the most spectacular regions of massive star formation in the nearby Galaxy, has not been well sampled in past studies. The authors have analyzed a mosaic of two Chandra X-ray Observatory images of the region using sensitive data analysis methods, giving a list of 1607 faint X-ray sources with arcsecond positions and approximate line-of-sight absorption. About 95% of these are expected to be cluster members, most lower mass pre-main-sequence stars. Extrapolating to low X-ray levels, the total stellar population is estimated to be 20,000 - 30,000 pre-main-sequence stars. The X-ray sources show a complicated spatial pattern with ~10 distinct star clusters. The heavily obscured clusters are mostly associated with previously known far-infrared sources and radio H II regions. The lightly obscured clusters are mostly newly identified in the X-ray images. Dozens of likely OB stars are found, both in clusters and dispersed throughout the region, suggesting that star formation in the complex has proceeded over millions of years. A number of extraordinarily heavily absorbed X-ray sources are associated with the active regions of star formation.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc6334cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc6334cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc6334cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc6334cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC6334CXO [2]</TD>
            <TD>NGC 6334 Chandra X-Ray Point Source Catalog</TD>
            <TD>The full stellar population of NGC 6334, one of the most spectacular regions of massive star formation in the nearby Galaxy, has not been well sampled in past studies. The authors have analyzed a mosaic of two Chandra X-ray Observatory images of the region using sensitive data analysis methods, giving a list of 1607 faint X-ray sources with arcsecond positions and approximate line-of-sight absorption. About 95% of these are expected to be cluster members, most lower mass pre-main-sequence stars. Extrapolating to low X-ray levels, the total stellar population is estimated to be 20,000 - 30,000 pre-main-sequence stars. The X-ray sources show a complicated spatial pattern with ~10 distinct star clusters. The heavily obscured clusters are mostly associated with previously known far-infrared sources and radio H II regions. The lightly obscured clusters are mostly newly identified in the X-ray images. Dozens of likely OB stars are found, both in clusters and dispersed throughout the region, suggesting that star formation in the complex has proceeded over millions of years. A number of extraordinarily heavily absorbed X-ray sources are associated with the active regions of star formation.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc6334cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc6334cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc6334cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc6334cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC6334CXO [3]</TD>
            <TD>NGC 6334 Chandra X-Ray Point Source Catalog</TD>
            <TD>The full stellar population of NGC 6334, one of the most spectacular regions of massive star formation in the nearby Galaxy, has not been well sampled in past studies. The authors have analyzed a mosaic of two Chandra X-ray Observatory images of the region using sensitive data analysis methods, giving a list of 1607 faint X-ray sources with arcsecond positions and approximate line-of-sight absorption. About 95% of these are expected to be cluster members, most lower mass pre-main-sequence stars. Extrapolating to low X-ray levels, the total stellar population is estimated to be 20,000 - 30,000 pre-main-sequence stars. The X-ray sources show a complicated spatial pattern with ~10 distinct star clusters. The heavily obscured clusters are mostly associated with previously known far-infrared sources and radio H II regions. The lightly obscured clusters are mostly newly identified in the X-ray images. Dozens of likely OB stars are found, both in clusters and dispersed throughout the region, suggesting that star formation in the complex has proceeded over millions of years. A number of extraordinarily heavily absorbed X-ray sources are associated with the active regions of star formation.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc6334cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc6334cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc6334cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc6334cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC [1]</TD>
            <TD>NGC2000.0: Complete New General Catalog and Index Catalog</TD>
            <TD>NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox 2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine-readble version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation. Information on how to contact Sky Publishing is available at &lt;a href="http://www.shopatsky.com/contact_us"&gt;http://www.shopatsky.com/contact_us&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ngc2000#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Nebula#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2000</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc2000&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/ngc2000.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC [2]</TD>
            <TD>NGC2000.0: Complete New General Catalog and Index Catalog</TD>
            <TD>NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox 2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine-readble version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation. Information on how to contact Sky Publishing is available at &lt;a href="http://www.shopatsky.com/contact_us"&gt;http://www.shopatsky.com/contact_us&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ngc2000#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Nebula#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2000</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc2000&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/ngc2000.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC [3]</TD>
            <TD>NGC2000.0: Complete New General Catalog and Index Catalog</TD>
            <TD>NGC 2000.0 is a modern compilation of the New General Catalogue of Nebulae and Clusters of Stars (NGC), the Index Catalogue (IC), and the Second Index Catalogue compiled by J. L. E. Dreyer (1888, 1895, 1908). The new compilation of these classical catalogs is intended to meet the needs of present-day observers by reporting positions at equinox 2000.0 and by incorporating the corrections reported by Dreyer himself and by a host of other astronomers who have worked with the data and compiled lists of errata. The object types given are those known to modern astronomy. This catalog is copyrighted by Sky Publishing Corporation, which has kindly deposited the machine-readble version in the data centers for permanent archiving and dissemination to astronomers for scientific research purposes only. The data should not be used for commercial purposes without the explicit permission of Sky Publishing Corporation. Information on how to contact Sky Publishing is available at &lt;a href="http://www.shopatsky.com/contact_us"&gt;http://www.shopatsky.com/contact_us&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ngc2000#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Nebula#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2000</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc2000&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/general-catalog/ngc2000.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC6334CXO [1]</TD>
            <TD>NGC 6334 Chandra X-Ray Point Source Catalog</TD>
            <TD>The full stellar population of NGC 6334, one of the most spectacular regions of massive star formation in the nearby Galaxy, has not been well sampled in past studies. The authors have analyzed a mosaic of two Chandra X-ray Observatory images of the region using sensitive data analysis methods, giving a list of 1607 faint X-ray sources with arcsecond positions and approximate line-of-sight absorption. About 95% of these are expected to be cluster members, most lower mass pre-main-sequence stars. Extrapolating to low X-ray levels, the total stellar population is estimated to be 20,000 - 30,000 pre-main-sequence stars. The X-ray sources show a complicated spatial pattern with ~10 distinct star clusters. The heavily obscured clusters are mostly associated with previously known far-infrared sources and radio H II regions. The lightly obscured clusters are mostly newly identified in the X-ray images. Dozens of likely OB stars are found, both in clusters and dispersed throughout the region, suggesting that star formation in the complex has proceeded over millions of years. A number of extraordinarily heavily absorbed X-ray sources are associated with the active regions of star formation.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc6334cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc6334cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc6334cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc6334cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC6334CXO [2]</TD>
            <TD>NGC 6334 Chandra X-Ray Point Source Catalog</TD>
            <TD>The full stellar population of NGC 6334, one of the most spectacular regions of massive star formation in the nearby Galaxy, has not been well sampled in past studies. The authors have analyzed a mosaic of two Chandra X-ray Observatory images of the region using sensitive data analysis methods, giving a list of 1607 faint X-ray sources with arcsecond positions and approximate line-of-sight absorption. About 95% of these are expected to be cluster members, most lower mass pre-main-sequence stars. Extrapolating to low X-ray levels, the total stellar population is estimated to be 20,000 - 30,000 pre-main-sequence stars. The X-ray sources show a complicated spatial pattern with ~10 distinct star clusters. The heavily obscured clusters are mostly associated with previously known far-infrared sources and radio H II regions. The lightly obscured clusters are mostly newly identified in the X-ray images. Dozens of likely OB stars are found, both in clusters and dispersed throughout the region, suggesting that star formation in the complex has proceeded over millions of years. A number of extraordinarily heavily absorbed X-ray sources are associated with the active regions of star formation.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc6334cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc6334cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc6334cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc6334cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC6334CXO [3]</TD>
            <TD>NGC 6334 Chandra X-Ray Point Source Catalog</TD>
            <TD>The full stellar population of NGC 6334, one of the most spectacular regions of massive star formation in the nearby Galaxy, has not been well sampled in past studies. The authors have analyzed a mosaic of two Chandra X-ray Observatory images of the region using sensitive data analysis methods, giving a list of 1607 faint X-ray sources with arcsecond positions and approximate line-of-sight absorption. About 95% of these are expected to be cluster members, most lower mass pre-main-sequence stars. Extrapolating to low X-ray levels, the total stellar population is estimated to be 20,000 - 30,000 pre-main-sequence stars. The X-ray sources show a complicated spatial pattern with ~10 distinct star clusters. The heavily obscured clusters are mostly associated with previously known far-infrared sources and radio H II regions. The lightly obscured clusters are mostly newly identified in the X-ray images. Dozens of likely OB stars are found, both in clusters and dispersed throughout the region, suggesting that star formation in the complex has proceeded over millions of years. A number of extraordinarily heavily absorbed X-ray sources are associated with the active regions of star formation.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc6334cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc6334cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc6334cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc6334cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/411/2770 [1]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#1</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/411/2770</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/411/2770 [2]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#2</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/411/2770&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/2770 [gr5-ais]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#gr5-ais</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/2770&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/2770 [gr5-mis]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#gr5-mis</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/2770&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/165A [1]</TD>
            <TD>Measured Redshifts of Abell Clusters of Galaxies (Andernach 1991)</TD>
            <TD>The 'ACO' catalog (Abell, Corwin and Olowin 1989; Cat. VII/110) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/165A#1</TD>
            <TD>2012-11-13T06:48:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/165A</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/165A</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/165A</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/165A [2]</TD>
            <TD>Measured Redshifts of Abell Clusters of Galaxies (Andernach 1991)</TD>
            <TD>The 'ACO' catalog (Abell, Corwin and Olowin 1989; Cat. VII/110) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/165A#2</TD>
            <TD>2012-11-13T06:48:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/165A</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/165A&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/165A</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/165A [catalog]</TD>
            <TD>Measured Redshifts of Abell Clusters of Galaxies (Andernach 1991)</TD>
            <TD>The 'ACO' catalog (Abell, Corwin and Olowin 1989; Cat. VII/110) that contains 4076 rich (A-) clusters of galaxies and 1174 supplementary (S-) clusters was used to compile this catalog. In the compilation, many papers containing galaxy redshifts were checked for positional coincidences of objects with Abell clusters (typically within one Abell radius). In a total of 1059 ACO clusters a redshift for one or more galaxies were found. These 1059 clusters (records) are sorted by the R.A. (B1950) of their centre. Each record consists of cluster name, cluster centre equatorial coordinates (B1950), Abell richness, distance, Bautz-Morgan class, the magnitude of the tenth-brightest cluster member, cluster measured redshift, the reference code, the Abell radius, and the decimal log of the ratio between measured and estimated redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/165A#catalog</TD>
            <TD>2012-11-13T06:48:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/VII/165A</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/165A&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/165A</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/411/2770 [1]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#1</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/411/2770</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/411/2770 [2]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#2</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/411/2770&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/2770 [gr5-ais]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#gr5-ais</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/2770&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/2770 [gr5-mis]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#gr5-mis</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/2770&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC6334CXO [1]</TD>
            <TD>NGC 6334 Chandra X-Ray Point Source Catalog</TD>
            <TD>The full stellar population of NGC 6334, one of the most spectacular regions of massive star formation in the nearby Galaxy, has not been well sampled in past studies. The authors have analyzed a mosaic of two Chandra X-ray Observatory images of the region using sensitive data analysis methods, giving a list of 1607 faint X-ray sources with arcsecond positions and approximate line-of-sight absorption. About 95% of these are expected to be cluster members, most lower mass pre-main-sequence stars. Extrapolating to low X-ray levels, the total stellar population is estimated to be 20,000 - 30,000 pre-main-sequence stars. The X-ray sources show a complicated spatial pattern with ~10 distinct star clusters. The heavily obscured clusters are mostly associated with previously known far-infrared sources and radio H II regions. The lightly obscured clusters are mostly newly identified in the X-ray images. Dozens of likely OB stars are found, both in clusters and dispersed throughout the region, suggesting that star formation in the complex has proceeded over millions of years. A number of extraordinarily heavily absorbed X-ray sources are associated with the active regions of star formation.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc6334cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc6334cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc6334cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc6334cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC6334CXO [2]</TD>
            <TD>NGC 6334 Chandra X-Ray Point Source Catalog</TD>
            <TD>The full stellar population of NGC 6334, one of the most spectacular regions of massive star formation in the nearby Galaxy, has not been well sampled in past studies. The authors have analyzed a mosaic of two Chandra X-ray Observatory images of the region using sensitive data analysis methods, giving a list of 1607 faint X-ray sources with arcsecond positions and approximate line-of-sight absorption. About 95% of these are expected to be cluster members, most lower mass pre-main-sequence stars. Extrapolating to low X-ray levels, the total stellar population is estimated to be 20,000 - 30,000 pre-main-sequence stars. The X-ray sources show a complicated spatial pattern with ~10 distinct star clusters. The heavily obscured clusters are mostly associated with previously known far-infrared sources and radio H II regions. The lightly obscured clusters are mostly newly identified in the X-ray images. Dozens of likely OB stars are found, both in clusters and dispersed throughout the region, suggesting that star formation in the complex has proceeded over millions of years. A number of extraordinarily heavily absorbed X-ray sources are associated with the active regions of star formation.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc6334cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc6334cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc6334cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc6334cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC6334CXO [3]</TD>
            <TD>NGC 6334 Chandra X-Ray Point Source Catalog</TD>
            <TD>The full stellar population of NGC 6334, one of the most spectacular regions of massive star formation in the nearby Galaxy, has not been well sampled in past studies. The authors have analyzed a mosaic of two Chandra X-ray Observatory images of the region using sensitive data analysis methods, giving a list of 1607 faint X-ray sources with arcsecond positions and approximate line-of-sight absorption. About 95% of these are expected to be cluster members, most lower mass pre-main-sequence stars. Extrapolating to low X-ray levels, the total stellar population is estimated to be 20,000 - 30,000 pre-main-sequence stars. The X-ray sources show a complicated spatial pattern with ~10 distinct star clusters. The heavily obscured clusters are mostly associated with previously known far-infrared sources and radio H II regions. The lightly obscured clusters are mostly newly identified in the X-ray images. Dozens of likely OB stars are found, both in clusters and dispersed throughout the region, suggesting that star formation in the complex has proceeded over millions of years. A number of extraordinarily heavily absorbed X-ray sources are associated with the active regions of star formation.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc6334cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc6334cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc6334cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc6334cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4472CXO [1]</TD>
            <TD>NGC 4472 Chandra X-Ray Point Source Catalog</TD>
            <TD>The Chandra X-Ray Point Source Catalog of the giant elliptical galaxy NGC 4472 contains the results of a Chandra ACIS-S/Hubble Space Telescope (HST) study of the point sources of this Virgo Cluster galaxy. The authors ran WAVDETECT from the CIAO 2.2 software package using wavelet scales from 1 to 16 pixels spaced by factors of 2, setting a false-source probability detection threshold of 10^-6, which should yield an expectation value of slightly less than one false source over the entire ACIS-S chip. They identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. An additional 3 sources are within 8" of the center of the galaxy and appear to be associated either with a weak active galactic nucleus or with brightness enhancements in the hot interstellar gas. One additional source (not included in this table) appears to be a spurious detection, as WAVDETECT assigns it a count rate of 1.5 counts, and visual inspection fails to find evidence of a source at that location. The optical data show 1102 sources whose half-light radii are small enough to be globular cluster candidates, 829 of which also have colors consistent with being globular clusters (with only four in the restricted central 10" region). 30 X-ray sources within 0.7" of an optical source with optical colors consistent with being globular clusters were found. Two additional sources show optical colors outside the globular cluster color range and are likely to be either foreground or background objects. The thirty globular cluster matches are likely to be low-mass X-ray binaries (LMXBs) associated with the globular clusters, while ~ 42 of the X-ray sources have no optical counterparts to V &lt;~ 25 and I &lt;~ 24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and ~ 4% of the globular clusters contain X-ray sources. This HEASARC table contains the X-ray data for the above-mentioned 147 detected X-ray sources, and the correlative optical data for the 30 optical counterparts which have colors consistent with being globular clusters. It does not contain the data from the full list of optical sources which were given in Table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4472cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4472cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4472cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4472cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4472CXO [2]</TD>
            <TD>NGC 4472 Chandra X-Ray Point Source Catalog</TD>
            <TD>The Chandra X-Ray Point Source Catalog of the giant elliptical galaxy NGC 4472 contains the results of a Chandra ACIS-S/Hubble Space Telescope (HST) study of the point sources of this Virgo Cluster galaxy. The authors ran WAVDETECT from the CIAO 2.2 software package using wavelet scales from 1 to 16 pixels spaced by factors of 2, setting a false-source probability detection threshold of 10^-6, which should yield an expectation value of slightly less than one false source over the entire ACIS-S chip. They identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. An additional 3 sources are within 8" of the center of the galaxy and appear to be associated either with a weak active galactic nucleus or with brightness enhancements in the hot interstellar gas. One additional source (not included in this table) appears to be a spurious detection, as WAVDETECT assigns it a count rate of 1.5 counts, and visual inspection fails to find evidence of a source at that location. The optical data show 1102 sources whose half-light radii are small enough to be globular cluster candidates, 829 of which also have colors consistent with being globular clusters (with only four in the restricted central 10" region). 30 X-ray sources within 0.7" of an optical source with optical colors consistent with being globular clusters were found. Two additional sources show optical colors outside the globular cluster color range and are likely to be either foreground or background objects. The thirty globular cluster matches are likely to be low-mass X-ray binaries (LMXBs) associated with the globular clusters, while ~ 42 of the X-ray sources have no optical counterparts to V &lt;~ 25 and I &lt;~ 24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and ~ 4% of the globular clusters contain X-ray sources. This HEASARC table contains the X-ray data for the above-mentioned 147 detected X-ray sources, and the correlative optical data for the 30 optical counterparts which have colors consistent with being globular clusters. It does not contain the data from the full list of optical sources which were given in Table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4472cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4472cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4472cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4472cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4472CXO [3]</TD>
            <TD>NGC 4472 Chandra X-Ray Point Source Catalog</TD>
            <TD>The Chandra X-Ray Point Source Catalog of the giant elliptical galaxy NGC 4472 contains the results of a Chandra ACIS-S/Hubble Space Telescope (HST) study of the point sources of this Virgo Cluster galaxy. The authors ran WAVDETECT from the CIAO 2.2 software package using wavelet scales from 1 to 16 pixels spaced by factors of 2, setting a false-source probability detection threshold of 10^-6, which should yield an expectation value of slightly less than one false source over the entire ACIS-S chip. They identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. An additional 3 sources are within 8" of the center of the galaxy and appear to be associated either with a weak active galactic nucleus or with brightness enhancements in the hot interstellar gas. One additional source (not included in this table) appears to be a spurious detection, as WAVDETECT assigns it a count rate of 1.5 counts, and visual inspection fails to find evidence of a source at that location. The optical data show 1102 sources whose half-light radii are small enough to be globular cluster candidates, 829 of which also have colors consistent with being globular clusters (with only four in the restricted central 10" region). 30 X-ray sources within 0.7" of an optical source with optical colors consistent with being globular clusters were found. Two additional sources show optical colors outside the globular cluster color range and are likely to be either foreground or background objects. The thirty globular cluster matches are likely to be low-mass X-ray binaries (LMXBs) associated with the globular clusters, while ~ 42 of the X-ray sources have no optical counterparts to V &lt;~ 25 and I &lt;~ 24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and ~ 4% of the globular clusters contain X-ray sources. This HEASARC table contains the X-ray data for the above-mentioned 147 detected X-ray sources, and the correlative optical data for the 30 optical counterparts which have colors consistent with being globular clusters. It does not contain the data from the full list of optical sources which were given in Table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4472cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4472cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4472cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4472cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>QuasarOrg [1]</TD>
            <TD>All-Sky Optical Catalog of Radio/X-Ray Sources</TD>
            <TD>The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels &gt;40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt; Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/qorgcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/qorgcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=qorgcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/qorgcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>QuasarOrg [2]</TD>
            <TD>All-Sky Optical Catalog of Radio/X-Ray Sources</TD>
            <TD>The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels &gt;40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt; Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/qorgcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/qorgcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=qorgcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/qorgcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>QuasarOrg [3]</TD>
            <TD>All-Sky Optical Catalog of Radio/X-Ray Sources</TD>
            <TD>The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels &gt;40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt; Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/qorgcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/qorgcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_qorgcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/qorgcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/411/2770 [1]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#1</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/411/2770</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/411/2770 [2]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#2</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/411/2770&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/2770 [gr5-ais]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#gr5-ais</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/2770&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/411/2770 [gr5-mis]</TD>
            <TD>Hot white dwarfs in GALEX-DR5 (Bianchi+, 2011)</TD>
            <TD>We present comprehensive catalogues of hot star candidates in the Milky Way (MW), selected from Galaxy Evolution Explorer (GALEX) far-UV (FUV; 1344-1786{AA}) and near-UV (NUV; 1771-2831{AA}) imaging. The FUV and NUV photometry allows us to extract the hottest stellar objects, in particular hot white dwarfs (WD), which are elusive at other wavelengths because of their high temperatures and faint optical luminosities. We generated catalogues of UV sources from two GALEX's surveys: All-Sky Imaging Survey (AIS; depth AB magnitude ~19.9/20.8 in FUV/NUV) and Medium-depth Imaging Survey (MIS; depth ~22.6/22.7mag). The two catalogues (from GALEX fifth data release) contain 65.3/12.6 million (AIS/MIS) unique UV sources with errorNUV&lt;= 0.5 mag, over 21 435/1579deg^2^. We also constructed subcatalogues of the UV sources with matched optical photometry from Sloan Digital Sky Survey (SDSS; seventh data release): these contain 0.6/0.9 million (AIS/MIS) sources with errors &lt;=0.3mag in both FUV and NUV, excluding sources with multiple optical counterparts, over an area of 7325/1103 deg2. All catalogues are available online. We then selected 28 319 (AIS)/9028 (MIS) matched sources with FUV-NUV&lt;-0.13; this colour cut corresponds to stellar Teff hotter than ~18 000K (the exact value varying with gravity). An additional colour cut of NUV-r&gt;0.1 isolates binaries with largely differing Teffs, and some intruding quasi-stellar objects (QSOs; more numerous at faint magnitudes). Available spectroscopy for a subsample indicates that hot-star candidates with NUV-r&lt;0.1 (mostly 'single' hot stars) have negligible contamination by non-stellar objects. We discuss the distribution of sources in the catalogues, and the effects of error and colour cuts on the samples. The density of hot-star candidates increases from high to low Galactic latitudes, but drops on the MW plane due to dust extinction. Our hot-star counts at all latitudes are better matched by MW models computed with an initial-final mass relation (IFMR) that favours lower final masses. The model analysis indicates that the brightest sample is likely composed of WDs located in the thin disc, at typical distances between 0.15 and 1kpc, while the fainter sample comprises also a fraction of thick disc and halo stars. Proper motion distributions, available only for the bright sample (NUV&lt;18mag), are consistent with the kinematics of a thin-disc population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770#gr5-mis</TD>
            <TD>2011-12-26T22:49:33Z</TD>
            <TD>#Stars#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/411/2770</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/411/2770&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/411/2770</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>QuasarOrg [1]</TD>
            <TD>All-Sky Optical Catalog of Radio/X-Ray Sources</TD>
            <TD>The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels &gt;40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt; Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/qorgcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/qorgcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=qorgcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/qorgcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>QuasarOrg [2]</TD>
            <TD>All-Sky Optical Catalog of Radio/X-Ray Sources</TD>
            <TD>The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels &gt;40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt; Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/qorgcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/qorgcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=qorgcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/qorgcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>QuasarOrg [3]</TD>
            <TD>All-Sky Optical Catalog of Radio/X-Ray Sources</TD>
            <TD>The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels &gt;40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt; Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/qorgcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/qorgcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_qorgcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/qorgcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/198/1 [1]</TD>
            <TD>Photometry catalogs for the Lockman Hole (Fotopoulou+, 2012)</TD>
            <TD>The field has been observed with XMM-Newton in the time period between 2000 April and 2002 December. In the far-ultraviolet (FUV) and the near-ultraviolet (NUV) the Lockman Hole area was observed by the Galaxy Evolution Explorer (GALEX). Here, we consider the magnitude in 3" diameter aperture available in the General Release 4/5 (GR4/5). In the optical wavelengths, our data set consists of a compilation of observations from Large Binocular Telescope (LBT; between 2007 February and 2009 March in 5 bands (U, B, V, Y, and z')), Subaru (between 2001 November and 2002 April in the Rc, Ic, and z' filters), and Sloan Digital Sky Survey (SDSS-DR7). The near-infrared view of our sources is provided by the data release 7 of the UKIRT Infrared Deep Sky Survey (UKIDSS). For the near- to mid-infrared wavelengths we are using observations at 3.6um, 4.5um, 5.8um, and 8.0um from the IRAC.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1#1</TD>
            <TD>2012-03-18T17:10:13Z</TD>
            <TD>#AGN#Photometry#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/198/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/198/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/198/1 [2]</TD>
            <TD>Photometry catalogs for the Lockman Hole (Fotopoulou+, 2012)</TD>
            <TD>The field has been observed with XMM-Newton in the time period between 2000 April and 2002 December. In the far-ultraviolet (FUV) and the near-ultraviolet (NUV) the Lockman Hole area was observed by the Galaxy Evolution Explorer (GALEX). Here, we consider the magnitude in 3" diameter aperture available in the General Release 4/5 (GR4/5). In the optical wavelengths, our data set consists of a compilation of observations from Large Binocular Telescope (LBT; between 2007 February and 2009 March in 5 bands (U, B, V, Y, and z')), Subaru (between 2001 November and 2002 April in the Rc, Ic, and z' filters), and Sloan Digital Sky Survey (SDSS-DR7). The near-infrared view of our sources is provided by the data release 7 of the UKIRT Infrared Deep Sky Survey (UKIDSS). For the near- to mid-infrared wavelengths we are using observations at 3.6um, 4.5um, 5.8um, and 8.0um from the IRAC.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1#2</TD>
            <TD>2012-03-18T17:10:13Z</TD>
            <TD>#AGN#Photometry#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/198/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/198/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/198/1 [lhpc]</TD>
            <TD>Photometry catalogs for the Lockman Hole (Fotopoulou+, 2012)</TD>
            <TD>The field has been observed with XMM-Newton in the time period between 2000 April and 2002 December. In the far-ultraviolet (FUV) and the near-ultraviolet (NUV) the Lockman Hole area was observed by the Galaxy Evolution Explorer (GALEX). Here, we consider the magnitude in 3" diameter aperture available in the General Release 4/5 (GR4/5). In the optical wavelengths, our data set consists of a compilation of observations from Large Binocular Telescope (LBT; between 2007 February and 2009 March in 5 bands (U, B, V, Y, and z')), Subaru (between 2001 November and 2002 April in the Rc, Ic, and z' filters), and Sloan Digital Sky Survey (SDSS-DR7). The near-infrared view of our sources is provided by the data release 7 of the UKIRT Infrared Deep Sky Survey (UKIDSS). For the near- to mid-infrared wavelengths we are using observations at 3.6um, 4.5um, 5.8um, and 8.0um from the IRAC.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1#lhpc</TD>
            <TD>2012-03-18T17:10:13Z</TD>
            <TD>#AGN#Photometry#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/198/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/198/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4472CXO [1]</TD>
            <TD>NGC 4472 Chandra X-Ray Point Source Catalog</TD>
            <TD>The Chandra X-Ray Point Source Catalog of the giant elliptical galaxy NGC 4472 contains the results of a Chandra ACIS-S/Hubble Space Telescope (HST) study of the point sources of this Virgo Cluster galaxy. The authors ran WAVDETECT from the CIAO 2.2 software package using wavelet scales from 1 to 16 pixels spaced by factors of 2, setting a false-source probability detection threshold of 10^-6, which should yield an expectation value of slightly less than one false source over the entire ACIS-S chip. They identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. An additional 3 sources are within 8" of the center of the galaxy and appear to be associated either with a weak active galactic nucleus or with brightness enhancements in the hot interstellar gas. One additional source (not included in this table) appears to be a spurious detection, as WAVDETECT assigns it a count rate of 1.5 counts, and visual inspection fails to find evidence of a source at that location. The optical data show 1102 sources whose half-light radii are small enough to be globular cluster candidates, 829 of which also have colors consistent with being globular clusters (with only four in the restricted central 10" region). 30 X-ray sources within 0.7" of an optical source with optical colors consistent with being globular clusters were found. Two additional sources show optical colors outside the globular cluster color range and are likely to be either foreground or background objects. The thirty globular cluster matches are likely to be low-mass X-ray binaries (LMXBs) associated with the globular clusters, while ~ 42 of the X-ray sources have no optical counterparts to V &lt;~ 25 and I &lt;~ 24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and ~ 4% of the globular clusters contain X-ray sources. This HEASARC table contains the X-ray data for the above-mentioned 147 detected X-ray sources, and the correlative optical data for the 30 optical counterparts which have colors consistent with being globular clusters. It does not contain the data from the full list of optical sources which were given in Table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4472cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4472cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4472cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4472cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4472CXO [2]</TD>
            <TD>NGC 4472 Chandra X-Ray Point Source Catalog</TD>
            <TD>The Chandra X-Ray Point Source Catalog of the giant elliptical galaxy NGC 4472 contains the results of a Chandra ACIS-S/Hubble Space Telescope (HST) study of the point sources of this Virgo Cluster galaxy. The authors ran WAVDETECT from the CIAO 2.2 software package using wavelet scales from 1 to 16 pixels spaced by factors of 2, setting a false-source probability detection threshold of 10^-6, which should yield an expectation value of slightly less than one false source over the entire ACIS-S chip. They identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. An additional 3 sources are within 8" of the center of the galaxy and appear to be associated either with a weak active galactic nucleus or with brightness enhancements in the hot interstellar gas. One additional source (not included in this table) appears to be a spurious detection, as WAVDETECT assigns it a count rate of 1.5 counts, and visual inspection fails to find evidence of a source at that location. The optical data show 1102 sources whose half-light radii are small enough to be globular cluster candidates, 829 of which also have colors consistent with being globular clusters (with only four in the restricted central 10" region). 30 X-ray sources within 0.7" of an optical source with optical colors consistent with being globular clusters were found. Two additional sources show optical colors outside the globular cluster color range and are likely to be either foreground or background objects. The thirty globular cluster matches are likely to be low-mass X-ray binaries (LMXBs) associated with the globular clusters, while ~ 42 of the X-ray sources have no optical counterparts to V &lt;~ 25 and I &lt;~ 24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and ~ 4% of the globular clusters contain X-ray sources. This HEASARC table contains the X-ray data for the above-mentioned 147 detected X-ray sources, and the correlative optical data for the 30 optical counterparts which have colors consistent with being globular clusters. It does not contain the data from the full list of optical sources which were given in Table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4472cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4472cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4472cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4472cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4472CXO [3]</TD>
            <TD>NGC 4472 Chandra X-Ray Point Source Catalog</TD>
            <TD>The Chandra X-Ray Point Source Catalog of the giant elliptical galaxy NGC 4472 contains the results of a Chandra ACIS-S/Hubble Space Telescope (HST) study of the point sources of this Virgo Cluster galaxy. The authors ran WAVDETECT from the CIAO 2.2 software package using wavelet scales from 1 to 16 pixels spaced by factors of 2, setting a false-source probability detection threshold of 10^-6, which should yield an expectation value of slightly less than one false source over the entire ACIS-S chip. They identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. An additional 3 sources are within 8" of the center of the galaxy and appear to be associated either with a weak active galactic nucleus or with brightness enhancements in the hot interstellar gas. One additional source (not included in this table) appears to be a spurious detection, as WAVDETECT assigns it a count rate of 1.5 counts, and visual inspection fails to find evidence of a source at that location. The optical data show 1102 sources whose half-light radii are small enough to be globular cluster candidates, 829 of which also have colors consistent with being globular clusters (with only four in the restricted central 10" region). 30 X-ray sources within 0.7" of an optical source with optical colors consistent with being globular clusters were found. Two additional sources show optical colors outside the globular cluster color range and are likely to be either foreground or background objects. The thirty globular cluster matches are likely to be low-mass X-ray binaries (LMXBs) associated with the globular clusters, while ~ 42 of the X-ray sources have no optical counterparts to V &lt;~ 25 and I &lt;~ 24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and ~ 4% of the globular clusters contain X-ray sources. This HEASARC table contains the X-ray data for the above-mentioned 147 detected X-ray sources, and the correlative optical data for the 30 optical counterparts which have colors consistent with being globular clusters. It does not contain the data from the full list of optical sources which were given in Table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4472cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4472cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4472cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4472cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>QuasarOrg [1]</TD>
            <TD>All-Sky Optical Catalog of Radio/X-Ray Sources</TD>
            <TD>The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels &gt;40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt; Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/qorgcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/qorgcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=qorgcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/qorgcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>QuasarOrg [2]</TD>
            <TD>All-Sky Optical Catalog of Radio/X-Ray Sources</TD>
            <TD>The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels &gt;40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt; Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/qorgcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/qorgcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=qorgcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/qorgcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>QuasarOrg [3]</TD>
            <TD>All-Sky Optical Catalog of Radio/X-Ray Sources</TD>
            <TD>The Quasars.org (QORG) Catalog is an all-sky optical catalog of radio/X-ray sources. The QORG Catalog aligns and overlays the year 2001/2 releases of the ROSAT HRI, RASS, PSPC and WGA X-ray catalogs, the NVSS (2002), FIRST (2003) and SUMSS (2003) radio catalogs, the Veron QSO catalog (2003) and various galaxy/star reference catalogs onto the optical APM and USNO-A catalogs. This catalog displays calculated percentage probabilities for each optical, radio/X-ray associated object of its likelihood of being a quasar, galaxy, star, or erroneous radio/X-ray association. This table contains the main Master QORG catalog (master.dat) and contains all 501,756 radio/X-ray associated optical objects and known quasars which are optically detected in APM/USNO-A. Up to six radio/X-ray catalog identifications are presented for each optical object, plus any double radio lobes (21,498 of these). These are superimposed (and laterally fitted) onto a 670,925,779-object optical background which combines APM and USNO-A data. Other subsets of this master catalog are available at the CDS, including the Free-Lunch catalog, a concise easy-to-read variant of the Master catalog showcasing just one X-ray and/or radio identification for each object, a subset catalog of QSO candidates, and a subset catalog of known QSOs/galaxies/stars. Objects presented in this catalog are those optical APM/USNO-A objects which are associated with X-ray/radio detections, or any optically-found catalogued QSO/AGN/Bl Lac objects, which have confidence levels &gt;40% of being radio/X-ray emitting optical objects. There are 501,756 objects included in all (including 48,285 catalogued quasars), representing the 99.4% coverage of the sky which is available from the APM and USNO-A. Each object is shown as one entry giving the position in equatorial coordinates, red and blue optical magnitudes (recalibrated) and PSF class, calculated probabilities of the object being, separately, a quasar, galaxy, star, or erroneous radio/X-ray association, any radio identification from each of the NVSS, FIRST and SUMSS surveys, including candidate double-lobe detections, any X-ray identification from each of the ROSAT HRI, RASS, PSPC and WGA surveys, including fluxes and field shifts of those identifications, plus, if already catalogued, the object name and redshift where applicable. The QORG catalog and supporting data can be accessed from the catalog home page at &lt;a href="http://quasars.org/qorg-data.htm"&gt;http://quasars.org/qorg-data.htm&lt;/a&gt; Questions or comments on the catalog contents may be directed to the first author Eric Flesch at eric@flesch.org. The authors request that researchers using this catalog make a small acknowledgement of such use in any published papers which thereby result.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/qorgcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/qorgcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_qorgcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/qorgcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/198/1 [1]</TD>
            <TD>Photometry catalogs for the Lockman Hole (Fotopoulou+, 2012)</TD>
            <TD>The field has been observed with XMM-Newton in the time period between 2000 April and 2002 December. In the far-ultraviolet (FUV) and the near-ultraviolet (NUV) the Lockman Hole area was observed by the Galaxy Evolution Explorer (GALEX). Here, we consider the magnitude in 3" diameter aperture available in the General Release 4/5 (GR4/5). In the optical wavelengths, our data set consists of a compilation of observations from Large Binocular Telescope (LBT; between 2007 February and 2009 March in 5 bands (U, B, V, Y, and z')), Subaru (between 2001 November and 2002 April in the Rc, Ic, and z' filters), and Sloan Digital Sky Survey (SDSS-DR7). The near-infrared view of our sources is provided by the data release 7 of the UKIRT Infrared Deep Sky Survey (UKIDSS). For the near- to mid-infrared wavelengths we are using observations at 3.6um, 4.5um, 5.8um, and 8.0um from the IRAC.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1#1</TD>
            <TD>2012-03-18T17:10:13Z</TD>
            <TD>#AGN#Photometry#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/198/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/198/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/198/1 [2]</TD>
            <TD>Photometry catalogs for the Lockman Hole (Fotopoulou+, 2012)</TD>
            <TD>The field has been observed with XMM-Newton in the time period between 2000 April and 2002 December. In the far-ultraviolet (FUV) and the near-ultraviolet (NUV) the Lockman Hole area was observed by the Galaxy Evolution Explorer (GALEX). Here, we consider the magnitude in 3" diameter aperture available in the General Release 4/5 (GR4/5). In the optical wavelengths, our data set consists of a compilation of observations from Large Binocular Telescope (LBT; between 2007 February and 2009 March in 5 bands (U, B, V, Y, and z')), Subaru (between 2001 November and 2002 April in the Rc, Ic, and z' filters), and Sloan Digital Sky Survey (SDSS-DR7). The near-infrared view of our sources is provided by the data release 7 of the UKIRT Infrared Deep Sky Survey (UKIDSS). For the near- to mid-infrared wavelengths we are using observations at 3.6um, 4.5um, 5.8um, and 8.0um from the IRAC.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1#2</TD>
            <TD>2012-03-18T17:10:13Z</TD>
            <TD>#AGN#Photometry#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/198/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/198/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/198/1 [lhpc]</TD>
            <TD>Photometry catalogs for the Lockman Hole (Fotopoulou+, 2012)</TD>
            <TD>The field has been observed with XMM-Newton in the time period between 2000 April and 2002 December. In the far-ultraviolet (FUV) and the near-ultraviolet (NUV) the Lockman Hole area was observed by the Galaxy Evolution Explorer (GALEX). Here, we consider the magnitude in 3" diameter aperture available in the General Release 4/5 (GR4/5). In the optical wavelengths, our data set consists of a compilation of observations from Large Binocular Telescope (LBT; between 2007 February and 2009 March in 5 bands (U, B, V, Y, and z')), Subaru (between 2001 November and 2002 April in the Rc, Ic, and z' filters), and Sloan Digital Sky Survey (SDSS-DR7). The near-infrared view of our sources is provided by the data release 7 of the UKIRT Infrared Deep Sky Survey (UKIDSS). For the near- to mid-infrared wavelengths we are using observations at 3.6um, 4.5um, 5.8um, and 8.0um from the IRAC.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1#lhpc</TD>
            <TD>2012-03-18T17:10:13Z</TD>
            <TD>#AGN#Photometry#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/198/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/198/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4472CXO [1]</TD>
            <TD>NGC 4472 Chandra X-Ray Point Source Catalog</TD>
            <TD>The Chandra X-Ray Point Source Catalog of the giant elliptical galaxy NGC 4472 contains the results of a Chandra ACIS-S/Hubble Space Telescope (HST) study of the point sources of this Virgo Cluster galaxy. The authors ran WAVDETECT from the CIAO 2.2 software package using wavelet scales from 1 to 16 pixels spaced by factors of 2, setting a false-source probability detection threshold of 10^-6, which should yield an expectation value of slightly less than one false source over the entire ACIS-S chip. They identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. An additional 3 sources are within 8" of the center of the galaxy and appear to be associated either with a weak active galactic nucleus or with brightness enhancements in the hot interstellar gas. One additional source (not included in this table) appears to be a spurious detection, as WAVDETECT assigns it a count rate of 1.5 counts, and visual inspection fails to find evidence of a source at that location. The optical data show 1102 sources whose half-light radii are small enough to be globular cluster candidates, 829 of which also have colors consistent with being globular clusters (with only four in the restricted central 10" region). 30 X-ray sources within 0.7" of an optical source with optical colors consistent with being globular clusters were found. Two additional sources show optical colors outside the globular cluster color range and are likely to be either foreground or background objects. The thirty globular cluster matches are likely to be low-mass X-ray binaries (LMXBs) associated with the globular clusters, while ~ 42 of the X-ray sources have no optical counterparts to V &lt;~ 25 and I &lt;~ 24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and ~ 4% of the globular clusters contain X-ray sources. This HEASARC table contains the X-ray data for the above-mentioned 147 detected X-ray sources, and the correlative optical data for the 30 optical counterparts which have colors consistent with being globular clusters. It does not contain the data from the full list of optical sources which were given in Table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4472cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4472cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4472cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4472cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4472CXO [2]</TD>
            <TD>NGC 4472 Chandra X-Ray Point Source Catalog</TD>
            <TD>The Chandra X-Ray Point Source Catalog of the giant elliptical galaxy NGC 4472 contains the results of a Chandra ACIS-S/Hubble Space Telescope (HST) study of the point sources of this Virgo Cluster galaxy. The authors ran WAVDETECT from the CIAO 2.2 software package using wavelet scales from 1 to 16 pixels spaced by factors of 2, setting a false-source probability detection threshold of 10^-6, which should yield an expectation value of slightly less than one false source over the entire ACIS-S chip. They identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. An additional 3 sources are within 8" of the center of the galaxy and appear to be associated either with a weak active galactic nucleus or with brightness enhancements in the hot interstellar gas. One additional source (not included in this table) appears to be a spurious detection, as WAVDETECT assigns it a count rate of 1.5 counts, and visual inspection fails to find evidence of a source at that location. The optical data show 1102 sources whose half-light radii are small enough to be globular cluster candidates, 829 of which also have colors consistent with being globular clusters (with only four in the restricted central 10" region). 30 X-ray sources within 0.7" of an optical source with optical colors consistent with being globular clusters were found. Two additional sources show optical colors outside the globular cluster color range and are likely to be either foreground or background objects. The thirty globular cluster matches are likely to be low-mass X-ray binaries (LMXBs) associated with the globular clusters, while ~ 42 of the X-ray sources have no optical counterparts to V &lt;~ 25 and I &lt;~ 24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and ~ 4% of the globular clusters contain X-ray sources. This HEASARC table contains the X-ray data for the above-mentioned 147 detected X-ray sources, and the correlative optical data for the 30 optical counterparts which have colors consistent with being globular clusters. It does not contain the data from the full list of optical sources which were given in Table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4472cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4472cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4472cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4472cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4472CXO [3]</TD>
            <TD>NGC 4472 Chandra X-Ray Point Source Catalog</TD>
            <TD>The Chandra X-Ray Point Source Catalog of the giant elliptical galaxy NGC 4472 contains the results of a Chandra ACIS-S/Hubble Space Telescope (HST) study of the point sources of this Virgo Cluster galaxy. The authors ran WAVDETECT from the CIAO 2.2 software package using wavelet scales from 1 to 16 pixels spaced by factors of 2, setting a false-source probability detection threshold of 10^-6, which should yield an expectation value of slightly less than one false source over the entire ACIS-S chip. They identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. An additional 3 sources are within 8" of the center of the galaxy and appear to be associated either with a weak active galactic nucleus or with brightness enhancements in the hot interstellar gas. One additional source (not included in this table) appears to be a spurious detection, as WAVDETECT assigns it a count rate of 1.5 counts, and visual inspection fails to find evidence of a source at that location. The optical data show 1102 sources whose half-light radii are small enough to be globular cluster candidates, 829 of which also have colors consistent with being globular clusters (with only four in the restricted central 10" region). 30 X-ray sources within 0.7" of an optical source with optical colors consistent with being globular clusters were found. Two additional sources show optical colors outside the globular cluster color range and are likely to be either foreground or background objects. The thirty globular cluster matches are likely to be low-mass X-ray binaries (LMXBs) associated with the globular clusters, while ~ 42 of the X-ray sources have no optical counterparts to V &lt;~ 25 and I &lt;~ 24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and ~ 4% of the globular clusters contain X-ray sources. This HEASARC table contains the X-ray data for the above-mentioned 147 detected X-ray sources, and the correlative optical data for the 30 optical counterparts which have colors consistent with being globular clusters. It does not contain the data from the full list of optical sources which were given in Table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4472cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4472cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4472cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4472cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PSPC/SMC2 [1]</TD>
            <TD>ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al)</TD>
            <TD>This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, A&amp;AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&amp;AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10^36 erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/smcrosxry2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/smcrosxry2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=smcrosxry2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/smcrosxry2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PSPC/SMC2 [2]</TD>
            <TD>ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al)</TD>
            <TD>This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, A&amp;AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&amp;AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10^36 erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/smcrosxry2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/smcrosxry2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=smcrosxry2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/smcrosxry2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PSPC/SMC2 [3]</TD>
            <TD>ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al)</TD>
            <TD>This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, A&amp;AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&amp;AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10^36 erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/smcrosxry2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/smcrosxry2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_smcrosxry2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/smcrosxry2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/198/1 [1]</TD>
            <TD>Photometry catalogs for the Lockman Hole (Fotopoulou+, 2012)</TD>
            <TD>The field has been observed with XMM-Newton in the time period between 2000 April and 2002 December. In the far-ultraviolet (FUV) and the near-ultraviolet (NUV) the Lockman Hole area was observed by the Galaxy Evolution Explorer (GALEX). Here, we consider the magnitude in 3" diameter aperture available in the General Release 4/5 (GR4/5). In the optical wavelengths, our data set consists of a compilation of observations from Large Binocular Telescope (LBT; between 2007 February and 2009 March in 5 bands (U, B, V, Y, and z')), Subaru (between 2001 November and 2002 April in the Rc, Ic, and z' filters), and Sloan Digital Sky Survey (SDSS-DR7). The near-infrared view of our sources is provided by the data release 7 of the UKIRT Infrared Deep Sky Survey (UKIDSS). For the near- to mid-infrared wavelengths we are using observations at 3.6um, 4.5um, 5.8um, and 8.0um from the IRAC.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1#1</TD>
            <TD>2012-03-18T17:10:13Z</TD>
            <TD>#AGN#Photometry#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/198/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/198/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/198/1 [2]</TD>
            <TD>Photometry catalogs for the Lockman Hole (Fotopoulou+, 2012)</TD>
            <TD>The field has been observed with XMM-Newton in the time period between 2000 April and 2002 December. In the far-ultraviolet (FUV) and the near-ultraviolet (NUV) the Lockman Hole area was observed by the Galaxy Evolution Explorer (GALEX). Here, we consider the magnitude in 3" diameter aperture available in the General Release 4/5 (GR4/5). In the optical wavelengths, our data set consists of a compilation of observations from Large Binocular Telescope (LBT; between 2007 February and 2009 March in 5 bands (U, B, V, Y, and z')), Subaru (between 2001 November and 2002 April in the Rc, Ic, and z' filters), and Sloan Digital Sky Survey (SDSS-DR7). The near-infrared view of our sources is provided by the data release 7 of the UKIRT Infrared Deep Sky Survey (UKIDSS). For the near- to mid-infrared wavelengths we are using observations at 3.6um, 4.5um, 5.8um, and 8.0um from the IRAC.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1#2</TD>
            <TD>2012-03-18T17:10:13Z</TD>
            <TD>#AGN#Photometry#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/198/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/198/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/198/1 [lhpc]</TD>
            <TD>Photometry catalogs for the Lockman Hole (Fotopoulou+, 2012)</TD>
            <TD>The field has been observed with XMM-Newton in the time period between 2000 April and 2002 December. In the far-ultraviolet (FUV) and the near-ultraviolet (NUV) the Lockman Hole area was observed by the Galaxy Evolution Explorer (GALEX). Here, we consider the magnitude in 3" diameter aperture available in the General Release 4/5 (GR4/5). In the optical wavelengths, our data set consists of a compilation of observations from Large Binocular Telescope (LBT; between 2007 February and 2009 March in 5 bands (U, B, V, Y, and z')), Subaru (between 2001 November and 2002 April in the Rc, Ic, and z' filters), and Sloan Digital Sky Survey (SDSS-DR7). The near-infrared view of our sources is provided by the data release 7 of the UKIRT Infrared Deep Sky Survey (UKIDSS). For the near- to mid-infrared wavelengths we are using observations at 3.6um, 4.5um, 5.8um, and 8.0um from the IRAC.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1#lhpc</TD>
            <TD>2012-03-18T17:10:13Z</TD>
            <TD>#AGN#Photometry#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/198/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/198/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/198/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PSPC/SMC2 [1]</TD>
            <TD>ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al)</TD>
            <TD>This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, A&amp;AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&amp;AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10^36 erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/smcrosxry2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/smcrosxry2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=smcrosxry2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/smcrosxry2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PSPC/SMC2 [2]</TD>
            <TD>ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al)</TD>
            <TD>This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, A&amp;AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&amp;AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10^36 erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/smcrosxry2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/smcrosxry2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=smcrosxry2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/smcrosxry2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PSPC/SMC2 [3]</TD>
            <TD>ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al)</TD>
            <TD>This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, A&amp;AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&amp;AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10^36 erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/smcrosxry2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/smcrosxry2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_smcrosxry2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/smcrosxry2.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4649CXO [1]</TD>
            <TD>NGC 4649 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>The authors performed a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649 (M 60). In addition to bright diffuse emission, they resolved 165 discrete sources, most of which are presumably low-mass X-ray binaries (LMXBs). As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 solar mass neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law. NGC 4649 was observed on 2000 April 20 on the ACIS-S3 CCD operated at a temperature of -120 C and with a frame time of 3.2 s. In addition to the S3 chip, the ACIS chips I2, I3, S1, S2, and S4 were also turned on for the duration of the observation. Although a number of serendipitous sources were seen on the other chips, the analysis of NGC 4649 in this paper was based on data from the S3 chip alone. The total exposure for the S3 chip was 36,780 s. The discrete X-ray source population on the ACIS S3 image was determined using a wavelet detection algorithm in the 0.3 - 10.0 keV band, and they were confirmed with a local cell detection method. The authors used the CIAO, WAVDETECT, and CELLDETECT programs. The high spatial resolution of Chandra implies that the sensitivity to point sources is not affected very strongly by the background. Thus, the source detection was done using the entire exposure of 36,780 s, including periods with background flares. The wavelet source detection significance threshold was set at 10^-6, which implies that less than 1 false source (due to a statistical fluctuation in the background) would be detected in the entire S3 image. This significance threshold approximately corresponds to requiring that the source flux be determined to better than 3 sigma.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4649cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4649cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4649cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4649cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4649CXO [2]</TD>
            <TD>NGC 4649 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>The authors performed a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649 (M 60). In addition to bright diffuse emission, they resolved 165 discrete sources, most of which are presumably low-mass X-ray binaries (LMXBs). As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 solar mass neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law. NGC 4649 was observed on 2000 April 20 on the ACIS-S3 CCD operated at a temperature of -120 C and with a frame time of 3.2 s. In addition to the S3 chip, the ACIS chips I2, I3, S1, S2, and S4 were also turned on for the duration of the observation. Although a number of serendipitous sources were seen on the other chips, the analysis of NGC 4649 in this paper was based on data from the S3 chip alone. The total exposure for the S3 chip was 36,780 s. The discrete X-ray source population on the ACIS S3 image was determined using a wavelet detection algorithm in the 0.3 - 10.0 keV band, and they were confirmed with a local cell detection method. The authors used the CIAO, WAVDETECT, and CELLDETECT programs. The high spatial resolution of Chandra implies that the sensitivity to point sources is not affected very strongly by the background. Thus, the source detection was done using the entire exposure of 36,780 s, including periods with background flares. The wavelet source detection significance threshold was set at 10^-6, which implies that less than 1 false source (due to a statistical fluctuation in the background) would be detected in the entire S3 image. This significance threshold approximately corresponds to requiring that the source flux be determined to better than 3 sigma.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4649cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4649cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4649cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4649cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4649CXO [3]</TD>
            <TD>NGC 4649 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>The authors performed a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649 (M 60). In addition to bright diffuse emission, they resolved 165 discrete sources, most of which are presumably low-mass X-ray binaries (LMXBs). As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 solar mass neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law. NGC 4649 was observed on 2000 April 20 on the ACIS-S3 CCD operated at a temperature of -120 C and with a frame time of 3.2 s. In addition to the S3 chip, the ACIS chips I2, I3, S1, S2, and S4 were also turned on for the duration of the observation. Although a number of serendipitous sources were seen on the other chips, the analysis of NGC 4649 in this paper was based on data from the S3 chip alone. The total exposure for the S3 chip was 36,780 s. The discrete X-ray source population on the ACIS S3 image was determined using a wavelet detection algorithm in the 0.3 - 10.0 keV band, and they were confirmed with a local cell detection method. The authors used the CIAO, WAVDETECT, and CELLDETECT programs. The high spatial resolution of Chandra implies that the sensitivity to point sources is not affected very strongly by the background. Thus, the source detection was done using the entire exposure of 36,780 s, including periods with background flares. The wavelet source detection significance threshold was set at 10^-6, which implies that less than 1 false source (due to a statistical fluctuation in the background) would be detected in the entire S3 image. This significance threshold approximately corresponds to requiring that the source flux be determined to better than 3 sigma.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4649cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4649cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4649cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4649cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/635/560 [1]</TD>
            <TD>New star clusters discovered in the GLIMPSE survey (Mercer+ 2005)</TD>
            <TD>A systematic and automated search of the extensive GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) mid-infrared survey data of the inner Galaxy was carried out to uncover new star clusters. This search has yielded 59 new clusters. Using our automated search algorithm, these clusters were identified as significant localized overdensities in the GLIMPSE point-source catalog (GLMC) and archive (GLMA). Subsequent visual inspection of the GLIMPSE image mosaics confirmed the existence of these clusters plus an additional 33 heavily embedded clusters missed by our detection algorithm, for a total of 92 newly discovered clusters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560#1</TD>
            <TD>2012-11-13T07:13:49Z</TD>
            <TD>#Associations#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/635/560</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/635/560</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/635/560 [2]</TD>
            <TD>New star clusters discovered in the GLIMPSE survey (Mercer+ 2005)</TD>
            <TD>A systematic and automated search of the extensive GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) mid-infrared survey data of the inner Galaxy was carried out to uncover new star clusters. This search has yielded 59 new clusters. Using our automated search algorithm, these clusters were identified as significant localized overdensities in the GLIMPSE point-source catalog (GLMC) and archive (GLMA). Subsequent visual inspection of the GLIMPSE image mosaics confirmed the existence of these clusters plus an additional 33 heavily embedded clusters missed by our detection algorithm, for a total of 92 newly discovered clusters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560#2</TD>
            <TD>2012-11-13T07:13:49Z</TD>
            <TD>#Associations#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/635/560&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/635/560</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/635/560 [table1]</TD>
            <TD>New star clusters discovered in the GLIMPSE survey (Mercer+ 2005)</TD>
            <TD>A systematic and automated search of the extensive GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) mid-infrared survey data of the inner Galaxy was carried out to uncover new star clusters. This search has yielded 59 new clusters. Using our automated search algorithm, these clusters were identified as significant localized overdensities in the GLIMPSE point-source catalog (GLMC) and archive (GLMA). Subsequent visual inspection of the GLIMPSE image mosaics confirmed the existence of these clusters plus an additional 33 heavily embedded clusters missed by our detection algorithm, for a total of 92 newly discovered clusters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560#table1</TD>
            <TD>2012-11-13T07:13:49Z</TD>
            <TD>#Associations#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/635/560&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/635/560</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PSPC/SMC2 [1]</TD>
            <TD>ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al)</TD>
            <TD>This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, A&amp;AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&amp;AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10^36 erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/smcrosxry2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/smcrosxry2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=smcrosxry2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/smcrosxry2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PSPC/SMC2 [2]</TD>
            <TD>ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al)</TD>
            <TD>This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, A&amp;AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&amp;AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10^36 erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/smcrosxry2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/smcrosxry2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=smcrosxry2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/smcrosxry2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PSPC/SMC2 [3]</TD>
            <TD>ROSAT PSPC Catalog of SMC X-Ray Sources (Haberl et al)</TD>
            <TD>This is a catalogue of 517 discrete X-ray sources in a 6 degree by 6 degree field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, A&amp;AS, 139, 277). The authors followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. In Table 7 of the paper from which this catalog is taken (Haberl et al. 2000, A&amp;AS, 142, 41), for 158 of these 517 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in the ROSAT PSPC observations; most of them with luminosities below 10^36 erg/s, suggesting that the fraction of high-luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/smcrosxry2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/smcrosxry2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_smcrosxry2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/smcrosxry2.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4649CXO [1]</TD>
            <TD>NGC 4649 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>The authors performed a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649 (M 60). In addition to bright diffuse emission, they resolved 165 discrete sources, most of which are presumably low-mass X-ray binaries (LMXBs). As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 solar mass neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law. NGC 4649 was observed on 2000 April 20 on the ACIS-S3 CCD operated at a temperature of -120 C and with a frame time of 3.2 s. In addition to the S3 chip, the ACIS chips I2, I3, S1, S2, and S4 were also turned on for the duration of the observation. Although a number of serendipitous sources were seen on the other chips, the analysis of NGC 4649 in this paper was based on data from the S3 chip alone. The total exposure for the S3 chip was 36,780 s. The discrete X-ray source population on the ACIS S3 image was determined using a wavelet detection algorithm in the 0.3 - 10.0 keV band, and they were confirmed with a local cell detection method. The authors used the CIAO, WAVDETECT, and CELLDETECT programs. The high spatial resolution of Chandra implies that the sensitivity to point sources is not affected very strongly by the background. Thus, the source detection was done using the entire exposure of 36,780 s, including periods with background flares. The wavelet source detection significance threshold was set at 10^-6, which implies that less than 1 false source (due to a statistical fluctuation in the background) would be detected in the entire S3 image. This significance threshold approximately corresponds to requiring that the source flux be determined to better than 3 sigma.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4649cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4649cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4649cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4649cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4649CXO [2]</TD>
            <TD>NGC 4649 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>The authors performed a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649 (M 60). In addition to bright diffuse emission, they resolved 165 discrete sources, most of which are presumably low-mass X-ray binaries (LMXBs). As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 solar mass neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law. NGC 4649 was observed on 2000 April 20 on the ACIS-S3 CCD operated at a temperature of -120 C and with a frame time of 3.2 s. In addition to the S3 chip, the ACIS chips I2, I3, S1, S2, and S4 were also turned on for the duration of the observation. Although a number of serendipitous sources were seen on the other chips, the analysis of NGC 4649 in this paper was based on data from the S3 chip alone. The total exposure for the S3 chip was 36,780 s. The discrete X-ray source population on the ACIS S3 image was determined using a wavelet detection algorithm in the 0.3 - 10.0 keV band, and they were confirmed with a local cell detection method. The authors used the CIAO, WAVDETECT, and CELLDETECT programs. The high spatial resolution of Chandra implies that the sensitivity to point sources is not affected very strongly by the background. Thus, the source detection was done using the entire exposure of 36,780 s, including periods with background flares. The wavelet source detection significance threshold was set at 10^-6, which implies that less than 1 false source (due to a statistical fluctuation in the background) would be detected in the entire S3 image. This significance threshold approximately corresponds to requiring that the source flux be determined to better than 3 sigma.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4649cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4649cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4649cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4649cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4649CXO [3]</TD>
            <TD>NGC 4649 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>The authors performed a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649 (M 60). In addition to bright diffuse emission, they resolved 165 discrete sources, most of which are presumably low-mass X-ray binaries (LMXBs). As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 solar mass neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law. NGC 4649 was observed on 2000 April 20 on the ACIS-S3 CCD operated at a temperature of -120 C and with a frame time of 3.2 s. In addition to the S3 chip, the ACIS chips I2, I3, S1, S2, and S4 were also turned on for the duration of the observation. Although a number of serendipitous sources were seen on the other chips, the analysis of NGC 4649 in this paper was based on data from the S3 chip alone. The total exposure for the S3 chip was 36,780 s. The discrete X-ray source population on the ACIS S3 image was determined using a wavelet detection algorithm in the 0.3 - 10.0 keV band, and they were confirmed with a local cell detection method. The authors used the CIAO, WAVDETECT, and CELLDETECT programs. The high spatial resolution of Chandra implies that the sensitivity to point sources is not affected very strongly by the background. Thus, the source detection was done using the entire exposure of 36,780 s, including periods with background flares. The wavelet source detection significance threshold was set at 10^-6, which implies that less than 1 false source (due to a statistical fluctuation in the background) would be detected in the entire S3 image. This significance threshold approximately corresponds to requiring that the source flux be determined to better than 3 sigma.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4649cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4649cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4649cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4649cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/635/560 [1]</TD>
            <TD>New star clusters discovered in the GLIMPSE survey (Mercer+ 2005)</TD>
            <TD>A systematic and automated search of the extensive GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) mid-infrared survey data of the inner Galaxy was carried out to uncover new star clusters. This search has yielded 59 new clusters. Using our automated search algorithm, these clusters were identified as significant localized overdensities in the GLIMPSE point-source catalog (GLMC) and archive (GLMA). Subsequent visual inspection of the GLIMPSE image mosaics confirmed the existence of these clusters plus an additional 33 heavily embedded clusters missed by our detection algorithm, for a total of 92 newly discovered clusters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560#1</TD>
            <TD>2012-11-13T07:13:49Z</TD>
            <TD>#Associations#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/635/560</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/635/560</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/635/560 [2]</TD>
            <TD>New star clusters discovered in the GLIMPSE survey (Mercer+ 2005)</TD>
            <TD>A systematic and automated search of the extensive GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) mid-infrared survey data of the inner Galaxy was carried out to uncover new star clusters. This search has yielded 59 new clusters. Using our automated search algorithm, these clusters were identified as significant localized overdensities in the GLIMPSE point-source catalog (GLMC) and archive (GLMA). Subsequent visual inspection of the GLIMPSE image mosaics confirmed the existence of these clusters plus an additional 33 heavily embedded clusters missed by our detection algorithm, for a total of 92 newly discovered clusters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560#2</TD>
            <TD>2012-11-13T07:13:49Z</TD>
            <TD>#Associations#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/635/560&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/635/560</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/635/560 [table1]</TD>
            <TD>New star clusters discovered in the GLIMPSE survey (Mercer+ 2005)</TD>
            <TD>A systematic and automated search of the extensive GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) mid-infrared survey data of the inner Galaxy was carried out to uncover new star clusters. This search has yielded 59 new clusters. Using our automated search algorithm, these clusters were identified as significant localized overdensities in the GLIMPSE point-source catalog (GLMC) and archive (GLMA). Subsequent visual inspection of the GLIMPSE image mosaics confirmed the existence of these clusters plus an additional 33 heavily embedded clusters missed by our detection algorithm, for a total of 92 newly discovered clusters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560#table1</TD>
            <TD>2012-11-13T07:13:49Z</TD>
            <TD>#Associations#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/635/560&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/635/560</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4649CXO [1]</TD>
            <TD>NGC 4649 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>The authors performed a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649 (M 60). In addition to bright diffuse emission, they resolved 165 discrete sources, most of which are presumably low-mass X-ray binaries (LMXBs). As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 solar mass neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law. NGC 4649 was observed on 2000 April 20 on the ACIS-S3 CCD operated at a temperature of -120 C and with a frame time of 3.2 s. In addition to the S3 chip, the ACIS chips I2, I3, S1, S2, and S4 were also turned on for the duration of the observation. Although a number of serendipitous sources were seen on the other chips, the analysis of NGC 4649 in this paper was based on data from the S3 chip alone. The total exposure for the S3 chip was 36,780 s. The discrete X-ray source population on the ACIS S3 image was determined using a wavelet detection algorithm in the 0.3 - 10.0 keV band, and they were confirmed with a local cell detection method. The authors used the CIAO, WAVDETECT, and CELLDETECT programs. The high spatial resolution of Chandra implies that the sensitivity to point sources is not affected very strongly by the background. Thus, the source detection was done using the entire exposure of 36,780 s, including periods with background flares. The wavelet source detection significance threshold was set at 10^-6, which implies that less than 1 false source (due to a statistical fluctuation in the background) would be detected in the entire S3 image. This significance threshold approximately corresponds to requiring that the source flux be determined to better than 3 sigma.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4649cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4649cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4649cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4649cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4649CXO [2]</TD>
            <TD>NGC 4649 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>The authors performed a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649 (M 60). In addition to bright diffuse emission, they resolved 165 discrete sources, most of which are presumably low-mass X-ray binaries (LMXBs). As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 solar mass neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law. NGC 4649 was observed on 2000 April 20 on the ACIS-S3 CCD operated at a temperature of -120 C and with a frame time of 3.2 s. In addition to the S3 chip, the ACIS chips I2, I3, S1, S2, and S4 were also turned on for the duration of the observation. Although a number of serendipitous sources were seen on the other chips, the analysis of NGC 4649 in this paper was based on data from the S3 chip alone. The total exposure for the S3 chip was 36,780 s. The discrete X-ray source population on the ACIS S3 image was determined using a wavelet detection algorithm in the 0.3 - 10.0 keV band, and they were confirmed with a local cell detection method. The authors used the CIAO, WAVDETECT, and CELLDETECT programs. The high spatial resolution of Chandra implies that the sensitivity to point sources is not affected very strongly by the background. Thus, the source detection was done using the entire exposure of 36,780 s, including periods with background flares. The wavelet source detection significance threshold was set at 10^-6, which implies that less than 1 false source (due to a statistical fluctuation in the background) would be detected in the entire S3 image. This significance threshold approximately corresponds to requiring that the source flux be determined to better than 3 sigma.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4649cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4649cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4649cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4649cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4649CXO [3]</TD>
            <TD>NGC 4649 Chandra X-Ray Discrete Source Catalog</TD>
            <TD>The authors performed a Chandra X-ray observation of the X-ray bright E2 elliptical galaxy NGC 4649 (M 60). In addition to bright diffuse emission, they resolved 165 discrete sources, most of which are presumably low-mass X-ray binaries (LMXBs). As found in previous studies, the luminosity function of the resolved sources is well-fitted by a broken power law. In NGC 4697 and NGC 1553, the break luminosity was comparable to the Eddington luminosity of a 1.4 solar mass neutron star. One possible interpretation of this result is that those sources with luminosities above the break are accreting black holes and those below are mainly accreting neutron stars. The total X-ray spectrum of the resolved sources is well fitted by a hard power law. NGC 4649 was observed on 2000 April 20 on the ACIS-S3 CCD operated at a temperature of -120 C and with a frame time of 3.2 s. In addition to the S3 chip, the ACIS chips I2, I3, S1, S2, and S4 were also turned on for the duration of the observation. Although a number of serendipitous sources were seen on the other chips, the analysis of NGC 4649 in this paper was based on data from the S3 chip alone. The total exposure for the S3 chip was 36,780 s. The discrete X-ray source population on the ACIS S3 image was determined using a wavelet detection algorithm in the 0.3 - 10.0 keV band, and they were confirmed with a local cell detection method. The authors used the CIAO, WAVDETECT, and CELLDETECT programs. The high spatial resolution of Chandra implies that the sensitivity to point sources is not affected very strongly by the background. Thus, the source detection was done using the entire exposure of 36,780 s, including periods with background flares. The wavelet source detection significance threshold was set at 10^-6, which implies that less than 1 false source (due to a statistical fluctuation in the background) would be detected in the entire S3 image. This significance threshold approximately corresponds to requiring that the source flux be determined to better than 3 sigma.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4649cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4649cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4649cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4649cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UGC [1]</TD>
            <TD>Uppsala General Catalog of Galaxies</TD>
            <TD>The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ugc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ugc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ugc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/ugc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UGC [2]</TD>
            <TD>Uppsala General Catalog of Galaxies</TD>
            <TD>The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ugc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ugc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ugc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/ugc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>UGC [3]</TD>
            <TD>Uppsala General Catalog of Galaxies</TD>
            <TD>The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ugc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ugc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ugc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/ugc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/1364 [1]</TD>
            <TD>SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)</TD>
            <TD>The observations of the SINS H{alpha} sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R~1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R~2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364#1</TD>
            <TD>2012-05-30T15:02:16Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/1364</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/1364</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/1364 [2]</TD>
            <TD>SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)</TD>
            <TD>The observations of the SINS H{alpha} sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R~1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R~2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364#2</TD>
            <TD>2012-05-30T15:02:16Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/1364&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/1364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/1364 [table1]</TD>
            <TD>SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)</TD>
            <TD>The observations of the SINS H{alpha} sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R~1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R~2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364#table1</TD>
            <TD>2012-05-30T15:02:16Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/1364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/1364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>OpenCluster [1]</TD>
            <TD>New Optically Visible Open Clusters and Candidates Catalog</TD>
            <TD>This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, CDS Cat. VII/92, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, &lt;a href="http://www.univie.ac.at/webda/"&gt;http://www.univie.ac.at/webda/&lt;/a&gt;). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects relative to the Lynga Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/openclust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/openclust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=openclust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/openclust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>OpenCluster [2]</TD>
            <TD>New Optically Visible Open Clusters and Candidates Catalog</TD>
            <TD>This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, CDS Cat. VII/92, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, &lt;a href="http://www.univie.ac.at/webda/"&gt;http://www.univie.ac.at/webda/&lt;/a&gt;). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects relative to the Lynga Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/openclust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/openclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=openclust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/openclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>OpenCluster [3]</TD>
            <TD>New Optically Visible Open Clusters and Candidates Catalog</TD>
            <TD>This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, CDS Cat. VII/92, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, &lt;a href="http://www.univie.ac.at/webda/"&gt;http://www.univie.ac.at/webda/&lt;/a&gt;). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects relative to the Lynga Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/openclust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/openclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_openclust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/openclust.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UGC [1]</TD>
            <TD>Uppsala General Catalog of Galaxies</TD>
            <TD>The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ugc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ugc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ugc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/ugc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UGC [2]</TD>
            <TD>Uppsala General Catalog of Galaxies</TD>
            <TD>The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ugc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ugc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ugc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/ugc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>UGC [3]</TD>
            <TD>Uppsala General Catalog of Galaxies</TD>
            <TD>The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ugc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ugc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ugc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/ugc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/1364 [1]</TD>
            <TD>SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)</TD>
            <TD>The observations of the SINS H{alpha} sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R~1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R~2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364#1</TD>
            <TD>2012-05-30T15:02:16Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/1364</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/1364</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/1364 [2]</TD>
            <TD>SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)</TD>
            <TD>The observations of the SINS H{alpha} sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R~1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R~2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364#2</TD>
            <TD>2012-05-30T15:02:16Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/1364&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/1364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/1364 [table1]</TD>
            <TD>SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)</TD>
            <TD>The observations of the SINS H{alpha} sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R~1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R~2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364#table1</TD>
            <TD>2012-05-30T15:02:16Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/1364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/1364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UGC [1]</TD>
            <TD>Uppsala General Catalog of Galaxies</TD>
            <TD>The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ugc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ugc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ugc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/ugc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UGC [2]</TD>
            <TD>Uppsala General Catalog of Galaxies</TD>
            <TD>The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ugc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ugc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ugc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/ugc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>UGC [3]</TD>
            <TD>Uppsala General Catalog of Galaxies</TD>
            <TD>The Uppsala General Catalogue of Galaxies (UGC) is an essentially complete catalog of galaxies to a limiting diameter of 1.0 arcminute and/or to a limiting apparent magnitude of 14.5 on the blue prints of the Palomar Observatory Sky Survey (POSS). Coverage is limited to the sky north of declination -02.5 degrees. Galaxies smaller than 1.0 arcminute in diameter but brighter than 14.5 mag may be included from the Catalogue of Galaxies and of Clusters of Galaxies (CGCG, Zwicky et al. 1961-1968); all such galaxies in the CGCG are included in the UGC. The galaxies are numbered in order of their 1950 right ascension values. The catalog contains descriptions of the galaxies and their surrounding areas, plus conventional system classifications and position angles for flattened galaxies. Galaxy diameters on both the blue and red POSS prints are included and the classifications and descriptions are given in such a way as to provide as accurate an account as possible of the appearance of the galaxies on the prints. Only the data portion of the published UGC is included in the machine-readable version, notice. For additional details regarding the classifications, measurement of apparent magnitudes, and data content, the source reference should be consulted.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/ugc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ugc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ugc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/ugc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/706/1364 [1]</TD>
            <TD>SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)</TD>
            <TD>The observations of the SINS H{alpha} sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R~1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R~2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364#1</TD>
            <TD>2012-05-30T15:02:16Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/706/1364</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/1364</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/706/1364 [2]</TD>
            <TD>SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)</TD>
            <TD>The observations of the SINS H{alpha} sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R~1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R~2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364#2</TD>
            <TD>2012-05-30T15:02:16Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/706/1364&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/1364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/706/1364 [table1]</TD>
            <TD>SINS survey of high-redshift galaxies (Forster Schreiber+, 2009)</TD>
            <TD>The observations of the SINS H{alpha} sample were carried out with SINFONI mounted at the Cassegrain focus of the VLT UT4 telescope. SINFONI consists of the near-IR cryogenic integral field spectrometer SPIFFI and of a curvature-sensor adaptive optics (AO) module called MACAO. The nominal FWHM spectral resolution for the pixel scales relevant to our SINS observations are as follows: R~1900, 2900, and 4500 for J, H, and K at 125mas/pixel, and R~2700 and 5000 at 50mas/pixel. The data were collected during 24 observing campaigns between 2003 March and 2008 July, as part of Guest Instrument and MPE guaranteed time observations. In addition, data of several GMASS ("Galaxy Mass Assembly ultra-deep Spectroscopic Survey"; J.D. Kurk et al., 2009Msngr.135...40K) targets were obtained under normal program allocations as part of a collaboration between the SINS and GMASS teams.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364#table1</TD>
            <TD>2012-05-30T15:02:16Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/706/1364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/706/1364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/706/1364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>OpenCluster [1]</TD>
            <TD>New Optically Visible Open Clusters and Candidates Catalog</TD>
            <TD>This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, CDS Cat. VII/92, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, &lt;a href="http://www.univie.ac.at/webda/"&gt;http://www.univie.ac.at/webda/&lt;/a&gt;). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects relative to the Lynga Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/openclust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/openclust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=openclust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/openclust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>OpenCluster [2]</TD>
            <TD>New Optically Visible Open Clusters and Candidates Catalog</TD>
            <TD>This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, CDS Cat. VII/92, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, &lt;a href="http://www.univie.ac.at/webda/"&gt;http://www.univie.ac.at/webda/&lt;/a&gt;). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects relative to the Lynga Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/openclust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/openclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=openclust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/openclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>OpenCluster [3]</TD>
            <TD>New Optically Visible Open Clusters and Candidates Catalog</TD>
            <TD>This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, CDS Cat. VII/92, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, &lt;a href="http://www.univie.ac.at/webda/"&gt;http://www.univie.ac.at/webda/&lt;/a&gt;). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects relative to the Lynga Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/openclust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/openclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_openclust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/openclust.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WBL [1]</TD>
            <TD>WBL Individual Galaxies Data Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wblgalaxy#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wblgalaxy</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=wblgalaxy&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wblgalaxy.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WBL [2]</TD>
            <TD>WBL Individual Galaxies Data Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wblgalaxy#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wblgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=wblgalaxy&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wblgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WBL [3]</TD>
            <TD>WBL Individual Galaxies Data Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wblgalaxy#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wblgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_wblgalaxy&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wblgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AcA/61/285 [1]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#1</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AcA/61/285</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AcA/61/285 [2]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#2</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AcA/61/285&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/61/285 [catcep]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#catcep</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/61/285&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/61/285 [catt2cep]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#catt2cep</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/61/285&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>OpenCluster [1]</TD>
            <TD>New Optically Visible Open Clusters and Candidates Catalog</TD>
            <TD>This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, CDS Cat. VII/92, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, &lt;a href="http://www.univie.ac.at/webda/"&gt;http://www.univie.ac.at/webda/&lt;/a&gt;). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects relative to the Lynga Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/openclust#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/openclust</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=openclust&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/openclust.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>OpenCluster [2]</TD>
            <TD>New Optically Visible Open Clusters and Candidates Catalog</TD>
            <TD>This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, CDS Cat. VII/92, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, &lt;a href="http://www.univie.ac.at/webda/"&gt;http://www.univie.ac.at/webda/&lt;/a&gt;). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects relative to the Lynga Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/openclust#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/openclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=openclust&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/openclust.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>OpenCluster [3]</TD>
            <TD>New Optically Visible Open Clusters and Candidates Catalog</TD>
            <TD>This is a new catalog of open clusters in the Galaxy which updates the previous catalogs of Lynga (1987, CDS Cat. VII/92, the HEASARC Browse table now called LYNGACLUST) and of Mermilliod (1995, in Information and On-Line Data in Astronomy, ed. D. Egret &amp; M. A. Albrecht (Dordrecht: Kluwer), 127) (included in the WEBDA database, &lt;a href="http://www.univie.ac.at/webda/"&gt;http://www.univie.ac.at/webda/&lt;/a&gt;). New objects and new data, in particular, data on kinematics (proper motions) that were not present in the old catalogs, have been included. Virtually all of the clusters presently known are included, which represents a large increase in the number of objects relative to the Lynga Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/openclust#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.5</TD>
            <TD />
            <TD>ivo://nasa.heasarc/openclust</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_openclust&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/openclust.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WBL [1]</TD>
            <TD>WBL Individual Galaxies Data Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wblgalaxy#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wblgalaxy</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=wblgalaxy&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wblgalaxy.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WBL [2]</TD>
            <TD>WBL Individual Galaxies Data Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wblgalaxy#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wblgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=wblgalaxy&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wblgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WBL [3]</TD>
            <TD>WBL Individual Galaxies Data Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wblgalaxy#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wblgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_wblgalaxy&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wblgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AcA/61/285 [1]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#1</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AcA/61/285</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AcA/61/285 [2]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#2</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AcA/61/285&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/61/285 [catcep]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#catcep</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/61/285&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/61/285 [catt2cep]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#catt2cep</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/61/285&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASS6DFGS [1]</TD>
            <TD>ROSAT All-Sky Survey/6dF Galaxy Survey Catalog of X-Ray Selected AGN</TD>
            <TD>This table contains a catalog of 3405 X-ray sources from the ROSAT All Sky Survey (RASS) Bright Source Catalog which fall within the area covered by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct s&lt;sup&gt;-1&lt;/sup&gt; in the X-ray and covers the area of sky with Declination &lt; 0 degrees and |b| &gt; 10 degrees. The RASS-6dFGS sample was one of the additional target catalogs of the 6dFGS and as a result the authors obtained optical spectra for 2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts with a median redshift of z = 0.16 (excluding the Galactic sources). For the optically bright sources (b_J &lt;= 17.5) in the observed sample, over 90% have reliable redshifts. The catalog mainly comprises quasi-stellar objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of the sources with reliable redshifts, the majority are type 1 active galactic nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and 13% are stars. The authors also identify a small number of optically faint, very low redshift, compact objects which fall outside the general trend in the b_J - z plane. The RASS-6dFGS catalog complements a number of Northern hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and furthermore, in the same region of sky (-40 degrees &lt; Declination &lt; 0 degrees) reveals an additional 561 sources that were not identified as part of that sample. The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky Survey (SUMSS) catalogues and find that the detection rate changes with redshift. At redshifts larger than 1 virtually all of these sources have radio counterparts and with a median flux density of 1.15 Jy, they are much stronger than the median flux density of 28.6 mJy for the full sample. The authors attribute this to the fact that the X-ray flux of these objects is being boosted by a jet component, possibly Doppler boosted, that is only present in radio-loud AGN. The RASS-6dFGS sample provides a large set of homogeneous optical spectra ideal for future studies of X-ray emitting AGN.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rass6dfgs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rass6dfgs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rass6dfgs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass6dfgs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASS6DFGS [2]</TD>
            <TD>ROSAT All-Sky Survey/6dF Galaxy Survey Catalog of X-Ray Selected AGN</TD>
            <TD>This table contains a catalog of 3405 X-ray sources from the ROSAT All Sky Survey (RASS) Bright Source Catalog which fall within the area covered by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct s&lt;sup&gt;-1&lt;/sup&gt; in the X-ray and covers the area of sky with Declination &lt; 0 degrees and |b| &gt; 10 degrees. The RASS-6dFGS sample was one of the additional target catalogs of the 6dFGS and as a result the authors obtained optical spectra for 2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts with a median redshift of z = 0.16 (excluding the Galactic sources). For the optically bright sources (b_J &lt;= 17.5) in the observed sample, over 90% have reliable redshifts. The catalog mainly comprises quasi-stellar objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of the sources with reliable redshifts, the majority are type 1 active galactic nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and 13% are stars. The authors also identify a small number of optically faint, very low redshift, compact objects which fall outside the general trend in the b_J - z plane. The RASS-6dFGS catalog complements a number of Northern hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and furthermore, in the same region of sky (-40 degrees &lt; Declination &lt; 0 degrees) reveals an additional 561 sources that were not identified as part of that sample. The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky Survey (SUMSS) catalogues and find that the detection rate changes with redshift. At redshifts larger than 1 virtually all of these sources have radio counterparts and with a median flux density of 1.15 Jy, they are much stronger than the median flux density of 28.6 mJy for the full sample. The authors attribute this to the fact that the X-ray flux of these objects is being boosted by a jet component, possibly Doppler boosted, that is only present in radio-loud AGN. The RASS-6dFGS sample provides a large set of homogeneous optical spectra ideal for future studies of X-ray emitting AGN.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rass6dfgs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rass6dfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rass6dfgs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass6dfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASS6DFGS [3]</TD>
            <TD>ROSAT All-Sky Survey/6dF Galaxy Survey Catalog of X-Ray Selected AGN</TD>
            <TD>This table contains a catalog of 3405 X-ray sources from the ROSAT All Sky Survey (RASS) Bright Source Catalog which fall within the area covered by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct s&lt;sup&gt;-1&lt;/sup&gt; in the X-ray and covers the area of sky with Declination &lt; 0 degrees and |b| &gt; 10 degrees. The RASS-6dFGS sample was one of the additional target catalogs of the 6dFGS and as a result the authors obtained optical spectra for 2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts with a median redshift of z = 0.16 (excluding the Galactic sources). For the optically bright sources (b_J &lt;= 17.5) in the observed sample, over 90% have reliable redshifts. The catalog mainly comprises quasi-stellar objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of the sources with reliable redshifts, the majority are type 1 active galactic nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and 13% are stars. The authors also identify a small number of optically faint, very low redshift, compact objects which fall outside the general trend in the b_J - z plane. The RASS-6dFGS catalog complements a number of Northern hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and furthermore, in the same region of sky (-40 degrees &lt; Declination &lt; 0 degrees) reveals an additional 561 sources that were not identified as part of that sample. The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky Survey (SUMSS) catalogues and find that the detection rate changes with redshift. At redshifts larger than 1 virtually all of these sources have radio counterparts and with a median flux density of 1.15 Jy, they are much stronger than the median flux density of 28.6 mJy for the full sample. The authors attribute this to the fact that the X-ray flux of these objects is being boosted by a jet component, possibly Doppler boosted, that is only present in radio-loud AGN. The RASS-6dFGS sample provides a large set of homogeneous optical spectra ideal for future studies of X-ray emitting AGN.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rass6dfgs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rass6dfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rass6dfgs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass6dfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/635/560 [1]</TD>
            <TD>New star clusters discovered in the GLIMPSE survey (Mercer+ 2005)</TD>
            <TD>A systematic and automated search of the extensive GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) mid-infrared survey data of the inner Galaxy was carried out to uncover new star clusters. This search has yielded 59 new clusters. Using our automated search algorithm, these clusters were identified as significant localized overdensities in the GLIMPSE point-source catalog (GLMC) and archive (GLMA). Subsequent visual inspection of the GLIMPSE image mosaics confirmed the existence of these clusters plus an additional 33 heavily embedded clusters missed by our detection algorithm, for a total of 92 newly discovered clusters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560#1</TD>
            <TD>2012-11-13T07:13:49Z</TD>
            <TD>#Associations#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/635/560</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/635/560</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/635/560 [2]</TD>
            <TD>New star clusters discovered in the GLIMPSE survey (Mercer+ 2005)</TD>
            <TD>A systematic and automated search of the extensive GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) mid-infrared survey data of the inner Galaxy was carried out to uncover new star clusters. This search has yielded 59 new clusters. Using our automated search algorithm, these clusters were identified as significant localized overdensities in the GLIMPSE point-source catalog (GLMC) and archive (GLMA). Subsequent visual inspection of the GLIMPSE image mosaics confirmed the existence of these clusters plus an additional 33 heavily embedded clusters missed by our detection algorithm, for a total of 92 newly discovered clusters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560#2</TD>
            <TD>2012-11-13T07:13:49Z</TD>
            <TD>#Associations#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/635/560&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/635/560</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/635/560 [table1]</TD>
            <TD>New star clusters discovered in the GLIMPSE survey (Mercer+ 2005)</TD>
            <TD>A systematic and automated search of the extensive GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) mid-infrared survey data of the inner Galaxy was carried out to uncover new star clusters. This search has yielded 59 new clusters. Using our automated search algorithm, these clusters were identified as significant localized overdensities in the GLIMPSE point-source catalog (GLMC) and archive (GLMA). Subsequent visual inspection of the GLIMPSE image mosaics confirmed the existence of these clusters plus an additional 33 heavily embedded clusters missed by our detection algorithm, for a total of 92 newly discovered clusters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560#table1</TD>
            <TD>2012-11-13T07:13:49Z</TD>
            <TD>#Associations#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/635/560</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/635/560&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/635/560</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASS6DFGS [1]</TD>
            <TD>ROSAT All-Sky Survey/6dF Galaxy Survey Catalog of X-Ray Selected AGN</TD>
            <TD>This table contains a catalog of 3405 X-ray sources from the ROSAT All Sky Survey (RASS) Bright Source Catalog which fall within the area covered by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct s&lt;sup&gt;-1&lt;/sup&gt; in the X-ray and covers the area of sky with Declination &lt; 0 degrees and |b| &gt; 10 degrees. The RASS-6dFGS sample was one of the additional target catalogs of the 6dFGS and as a result the authors obtained optical spectra for 2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts with a median redshift of z = 0.16 (excluding the Galactic sources). For the optically bright sources (b_J &lt;= 17.5) in the observed sample, over 90% have reliable redshifts. The catalog mainly comprises quasi-stellar objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of the sources with reliable redshifts, the majority are type 1 active galactic nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and 13% are stars. The authors also identify a small number of optically faint, very low redshift, compact objects which fall outside the general trend in the b_J - z plane. The RASS-6dFGS catalog complements a number of Northern hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and furthermore, in the same region of sky (-40 degrees &lt; Declination &lt; 0 degrees) reveals an additional 561 sources that were not identified as part of that sample. The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky Survey (SUMSS) catalogues and find that the detection rate changes with redshift. At redshifts larger than 1 virtually all of these sources have radio counterparts and with a median flux density of 1.15 Jy, they are much stronger than the median flux density of 28.6 mJy for the full sample. The authors attribute this to the fact that the X-ray flux of these objects is being boosted by a jet component, possibly Doppler boosted, that is only present in radio-loud AGN. The RASS-6dFGS sample provides a large set of homogeneous optical spectra ideal for future studies of X-ray emitting AGN.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rass6dfgs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rass6dfgs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rass6dfgs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass6dfgs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASS6DFGS [2]</TD>
            <TD>ROSAT All-Sky Survey/6dF Galaxy Survey Catalog of X-Ray Selected AGN</TD>
            <TD>This table contains a catalog of 3405 X-ray sources from the ROSAT All Sky Survey (RASS) Bright Source Catalog which fall within the area covered by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct s&lt;sup&gt;-1&lt;/sup&gt; in the X-ray and covers the area of sky with Declination &lt; 0 degrees and |b| &gt; 10 degrees. The RASS-6dFGS sample was one of the additional target catalogs of the 6dFGS and as a result the authors obtained optical spectra for 2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts with a median redshift of z = 0.16 (excluding the Galactic sources). For the optically bright sources (b_J &lt;= 17.5) in the observed sample, over 90% have reliable redshifts. The catalog mainly comprises quasi-stellar objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of the sources with reliable redshifts, the majority are type 1 active galactic nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and 13% are stars. The authors also identify a small number of optically faint, very low redshift, compact objects which fall outside the general trend in the b_J - z plane. The RASS-6dFGS catalog complements a number of Northern hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and furthermore, in the same region of sky (-40 degrees &lt; Declination &lt; 0 degrees) reveals an additional 561 sources that were not identified as part of that sample. The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky Survey (SUMSS) catalogues and find that the detection rate changes with redshift. At redshifts larger than 1 virtually all of these sources have radio counterparts and with a median flux density of 1.15 Jy, they are much stronger than the median flux density of 28.6 mJy for the full sample. The authors attribute this to the fact that the X-ray flux of these objects is being boosted by a jet component, possibly Doppler boosted, that is only present in radio-loud AGN. The RASS-6dFGS sample provides a large set of homogeneous optical spectra ideal for future studies of X-ray emitting AGN.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rass6dfgs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rass6dfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rass6dfgs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass6dfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASS6DFGS [3]</TD>
            <TD>ROSAT All-Sky Survey/6dF Galaxy Survey Catalog of X-Ray Selected AGN</TD>
            <TD>This table contains a catalog of 3405 X-ray sources from the ROSAT All Sky Survey (RASS) Bright Source Catalog which fall within the area covered by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct s&lt;sup&gt;-1&lt;/sup&gt; in the X-ray and covers the area of sky with Declination &lt; 0 degrees and |b| &gt; 10 degrees. The RASS-6dFGS sample was one of the additional target catalogs of the 6dFGS and as a result the authors obtained optical spectra for 2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts with a median redshift of z = 0.16 (excluding the Galactic sources). For the optically bright sources (b_J &lt;= 17.5) in the observed sample, over 90% have reliable redshifts. The catalog mainly comprises quasi-stellar objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of the sources with reliable redshifts, the majority are type 1 active galactic nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and 13% are stars. The authors also identify a small number of optically faint, very low redshift, compact objects which fall outside the general trend in the b_J - z plane. The RASS-6dFGS catalog complements a number of Northern hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and furthermore, in the same region of sky (-40 degrees &lt; Declination &lt; 0 degrees) reveals an additional 561 sources that were not identified as part of that sample. The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky Survey (SUMSS) catalogues and find that the detection rate changes with redshift. At redshifts larger than 1 virtually all of these sources have radio counterparts and with a median flux density of 1.15 Jy, they are much stronger than the median flux density of 28.6 mJy for the full sample. The authors attribute this to the fact that the X-ray flux of these objects is being boosted by a jet component, possibly Doppler boosted, that is only present in radio-loud AGN. The RASS-6dFGS sample provides a large set of homogeneous optical spectra ideal for future studies of X-ray emitting AGN.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rass6dfgs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rass6dfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rass6dfgs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass6dfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AcA/61/285 [1]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#1</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AcA/61/285</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AcA/61/285 [2]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#2</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AcA/61/285&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/61/285 [catcep]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#catcep</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/61/285&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AcA/61/285 [catt2cep]</TD>
            <TD>VI light curves of Galactic Bulge Cepheids (Soszynski+, 2011)</TD>
            <TD>The fourteenth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains Cepheid variables detected in the OGLE-II and OGLE-III fields toward the Galactic bulge. The catalog is divided into two main categories: 32 classical Cepheids (21 single-mode fundamental-mode F, four first-overtone 1O, two double-mode F/1O, three double-mode 1O/2O and two triple-mode 1O/2O/3O pulsators) and 335 type II Cepheids (156 BL Her, 128 W Vir and 51 RV Tau stars). Six of the type II Cepheids likely belong to the Sagittarius Dwarf Spheroidal Galaxy. The catalog data include the time-series photometry collected in the course of the OGLE survey, observational parameters of the stars, finding charts, and cross-identifications with the General Catalogue of Variable Stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285#catt2cep</TD>
            <TD>2012-06-11T05:01:31Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/AcA/61/285</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AcA/61/285&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/61/285</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/61/667 [1]</TD>
            <TD>Kinematics of Galactic old population (Norris 1986)</TD>
            <TD>A catalog is presented of some 1200 Galactic objects which have radial velocities and abundances [Fe/H]&lt;=-0.6. These data have been analyzed to yield information on the kinematic properties of the older populations of the Galaxy and on the interdependence between kinematics and abundance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667#1</TD>
            <TD>2012-11-13T07:16:33Z</TD>
            <TD>#Abundances#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/61/667</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/61/667</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/61/667 [2]</TD>
            <TD>Kinematics of Galactic old population (Norris 1986)</TD>
            <TD>A catalog is presented of some 1200 Galactic objects which have radial velocities and abundances [Fe/H]&lt;=-0.6. These data have been analyzed to yield information on the kinematic properties of the older populations of the Galaxy and on the interdependence between kinematics and abundance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667#2</TD>
            <TD>2012-11-13T07:16:33Z</TD>
            <TD>#Abundances#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/61/667&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/61/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/61/667 [table1]</TD>
            <TD>Kinematics of Galactic old population (Norris 1986)</TD>
            <TD>A catalog is presented of some 1200 Galactic objects which have radial velocities and abundances [Fe/H]&lt;=-0.6. These data have been analyzed to yield information on the kinematic properties of the older populations of the Galaxy and on the interdependence between kinematics and abundance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667#table1</TD>
            <TD>2012-11-13T07:16:33Z</TD>
            <TD>#Abundances#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/61/667&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/61/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASS6DFGS [1]</TD>
            <TD>ROSAT All-Sky Survey/6dF Galaxy Survey Catalog of X-Ray Selected AGN</TD>
            <TD>This table contains a catalog of 3405 X-ray sources from the ROSAT All Sky Survey (RASS) Bright Source Catalog which fall within the area covered by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct s&lt;sup&gt;-1&lt;/sup&gt; in the X-ray and covers the area of sky with Declination &lt; 0 degrees and |b| &gt; 10 degrees. The RASS-6dFGS sample was one of the additional target catalogs of the 6dFGS and as a result the authors obtained optical spectra for 2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts with a median redshift of z = 0.16 (excluding the Galactic sources). For the optically bright sources (b_J &lt;= 17.5) in the observed sample, over 90% have reliable redshifts. The catalog mainly comprises quasi-stellar objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of the sources with reliable redshifts, the majority are type 1 active galactic nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and 13% are stars. The authors also identify a small number of optically faint, very low redshift, compact objects which fall outside the general trend in the b_J - z plane. The RASS-6dFGS catalog complements a number of Northern hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and furthermore, in the same region of sky (-40 degrees &lt; Declination &lt; 0 degrees) reveals an additional 561 sources that were not identified as part of that sample. The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky Survey (SUMSS) catalogues and find that the detection rate changes with redshift. At redshifts larger than 1 virtually all of these sources have radio counterparts and with a median flux density of 1.15 Jy, they are much stronger than the median flux density of 28.6 mJy for the full sample. The authors attribute this to the fact that the X-ray flux of these objects is being boosted by a jet component, possibly Doppler boosted, that is only present in radio-loud AGN. The RASS-6dFGS sample provides a large set of homogeneous optical spectra ideal for future studies of X-ray emitting AGN.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rass6dfgs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rass6dfgs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rass6dfgs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass6dfgs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASS6DFGS [2]</TD>
            <TD>ROSAT All-Sky Survey/6dF Galaxy Survey Catalog of X-Ray Selected AGN</TD>
            <TD>This table contains a catalog of 3405 X-ray sources from the ROSAT All Sky Survey (RASS) Bright Source Catalog which fall within the area covered by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct s&lt;sup&gt;-1&lt;/sup&gt; in the X-ray and covers the area of sky with Declination &lt; 0 degrees and |b| &gt; 10 degrees. The RASS-6dFGS sample was one of the additional target catalogs of the 6dFGS and as a result the authors obtained optical spectra for 2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts with a median redshift of z = 0.16 (excluding the Galactic sources). For the optically bright sources (b_J &lt;= 17.5) in the observed sample, over 90% have reliable redshifts. The catalog mainly comprises quasi-stellar objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of the sources with reliable redshifts, the majority are type 1 active galactic nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and 13% are stars. The authors also identify a small number of optically faint, very low redshift, compact objects which fall outside the general trend in the b_J - z plane. The RASS-6dFGS catalog complements a number of Northern hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and furthermore, in the same region of sky (-40 degrees &lt; Declination &lt; 0 degrees) reveals an additional 561 sources that were not identified as part of that sample. The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky Survey (SUMSS) catalogues and find that the detection rate changes with redshift. At redshifts larger than 1 virtually all of these sources have radio counterparts and with a median flux density of 1.15 Jy, they are much stronger than the median flux density of 28.6 mJy for the full sample. The authors attribute this to the fact that the X-ray flux of these objects is being boosted by a jet component, possibly Doppler boosted, that is only present in radio-loud AGN. The RASS-6dFGS sample provides a large set of homogeneous optical spectra ideal for future studies of X-ray emitting AGN.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rass6dfgs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rass6dfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rass6dfgs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass6dfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASS6DFGS [3]</TD>
            <TD>ROSAT All-Sky Survey/6dF Galaxy Survey Catalog of X-Ray Selected AGN</TD>
            <TD>This table contains a catalog of 3405 X-ray sources from the ROSAT All Sky Survey (RASS) Bright Source Catalog which fall within the area covered by the 6dF Galaxy Survey (6dFGS). The catalog is count-rate limited at 0.05 ct s&lt;sup&gt;-1&lt;/sup&gt; in the X-ray and covers the area of sky with Declination &lt; 0 degrees and |b| &gt; 10 degrees. The RASS-6dFGS sample was one of the additional target catalogs of the 6dFGS and as a result the authors obtained optical spectra for 2224 (65 per cent) RASS sources. Of these, 1715 (77%) have reliable redshifts with a median redshift of z = 0.16 (excluding the Galactic sources). For the optically bright sources (b_J &lt;= 17.5) in the observed sample, over 90% have reliable redshifts. The catalog mainly comprises quasi-stellar objects (QSOs) and active galaxies but also includes 238 Galactic sources. Of the sources with reliable redshifts, the majority are type 1 active galactic nuclei (AGN, 69%), while 12% are type 2 AGN, 6% absorption-line galaxies and 13% are stars. The authors also identify a small number of optically faint, very low redshift, compact objects which fall outside the general trend in the b_J - z plane. The RASS-6dFGS catalog complements a number of Northern hemisphere samples, particularly the ROSAT Bright Source Catalogue-NRAO VLA Sky Survey (RBSC-NVSS) sample (Bauer et al. 2000, ApJS, 129, 547), and furthermore, in the same region of sky (-40 degrees &lt; Declination &lt; 0 degrees) reveals an additional 561 sources that were not identified as part of that sample. The authors detect 918 sources (27%) of the RASS-6dFGS sample in the radio using either the 1.4 GHz NVSS or the 843 MHz Sydney University Molonglo Sky Survey (SUMSS) catalogues and find that the detection rate changes with redshift. At redshifts larger than 1 virtually all of these sources have radio counterparts and with a median flux density of 1.15 Jy, they are much stronger than the median flux density of 28.6 mJy for the full sample. The authors attribute this to the fact that the X-ray flux of these objects is being boosted by a jet component, possibly Doppler boosted, that is only present in radio-loud AGN. The RASS-6dFGS sample provides a large set of homogeneous optical spectra ideal for future studies of X-ray emitting AGN.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#Radio#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rass6dfgs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rass6dfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rass6dfgs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rass6dfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/61/667 [1]</TD>
            <TD>Kinematics of Galactic old population (Norris 1986)</TD>
            <TD>A catalog is presented of some 1200 Galactic objects which have radial velocities and abundances [Fe/H]&lt;=-0.6. These data have been analyzed to yield information on the kinematic properties of the older populations of the Galaxy and on the interdependence between kinematics and abundance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667#1</TD>
            <TD>2012-11-13T07:16:33Z</TD>
            <TD>#Abundances#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/61/667</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/61/667</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/61/667 [2]</TD>
            <TD>Kinematics of Galactic old population (Norris 1986)</TD>
            <TD>A catalog is presented of some 1200 Galactic objects which have radial velocities and abundances [Fe/H]&lt;=-0.6. These data have been analyzed to yield information on the kinematic properties of the older populations of the Galaxy and on the interdependence between kinematics and abundance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667#2</TD>
            <TD>2012-11-13T07:16:33Z</TD>
            <TD>#Abundances#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/61/667&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/61/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/61/667 [table1]</TD>
            <TD>Kinematics of Galactic old population (Norris 1986)</TD>
            <TD>A catalog is presented of some 1200 Galactic objects which have radial velocities and abundances [Fe/H]&lt;=-0.6. These data have been analyzed to yield information on the kinematic properties of the older populations of the Galaxy and on the interdependence between kinematics and abundance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667#table1</TD>
            <TD>2012-11-13T07:16:33Z</TD>
            <TD>#Abundances#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/61/667&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/61/667</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/417/2347 [1]</TD>
            <TD>Tully-Fisher relation for SDSS galaxies (Reyes+, 2011)</TD>
            <TD>In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z&lt;0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347#1</TD>
            <TD>2012-07-05T12:27:01Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/417/2347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/417/2347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/417/2347 [2]</TD>
            <TD>Tully-Fisher relation for SDSS galaxies (Reyes+, 2011)</TD>
            <TD>In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z&lt;0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347#2</TD>
            <TD>2012-07-05T12:27:01Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/417/2347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/417/2347</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/417/2347 [sample]</TD>
            <TD>Tully-Fisher relation for SDSS galaxies (Reyes+, 2011)</TD>
            <TD>In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z&lt;0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347#sample</TD>
            <TD>2012-07-05T12:27:01Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/417/2347&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/417/2347</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASS-CALS [1]</TD>
            <TD>ROSAT All-Sky Survey CALS Galaxy Groups Catalog</TD>
            <TD>This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and optical survey of low-mass galaxy groups as of its publication date in 2000. The authors drew 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z = 15.5. They detected 61 groups (23%) as extended X-ray sources. The X-ray detections have a median membership of nine galaxies, a median recession velocity cz = 7250 km/s, a median projected velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) = 3 x 10^42 /h(100)^2 erg/s, where the Hubble constant is H(0) = 100 h(100) km/s/Mpc. The data in this table replace the preliminary analysis of the X-ray data which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat. &lt;J/ApJ/518/69&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rasscals#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Group#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rasscals</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rasscals&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rasscals.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASS-CALS [2]</TD>
            <TD>ROSAT All-Sky Survey CALS Galaxy Groups Catalog</TD>
            <TD>This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and optical survey of low-mass galaxy groups as of its publication date in 2000. The authors drew 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z = 15.5. They detected 61 groups (23%) as extended X-ray sources. The X-ray detections have a median membership of nine galaxies, a median recession velocity cz = 7250 km/s, a median projected velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) = 3 x 10^42 /h(100)^2 erg/s, where the Hubble constant is H(0) = 100 h(100) km/s/Mpc. The data in this table replace the preliminary analysis of the X-ray data which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat. &lt;J/ApJ/518/69&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rasscals#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Group#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rasscals</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rasscals&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rasscals.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASS-CALS [3]</TD>
            <TD>ROSAT All-Sky Survey CALS Galaxy Groups Catalog</TD>
            <TD>This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and optical survey of low-mass galaxy groups as of its publication date in 2000. The authors drew 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z = 15.5. They detected 61 groups (23%) as extended X-ray sources. The X-ray detections have a median membership of nine galaxies, a median recession velocity cz = 7250 km/s, a median projected velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) = 3 x 10^42 /h(100)^2 erg/s, where the Hubble constant is H(0) = 100 h(100) km/s/Mpc. The data in this table replace the preliminary analysis of the X-ray data which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat. &lt;J/ApJ/518/69&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rasscals#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Group#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rasscals</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rasscals&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rasscals.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/417/2347 [1]</TD>
            <TD>Tully-Fisher relation for SDSS galaxies (Reyes+, 2011)</TD>
            <TD>In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z&lt;0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347#1</TD>
            <TD>2012-07-05T12:27:01Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/417/2347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/417/2347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/417/2347 [2]</TD>
            <TD>Tully-Fisher relation for SDSS galaxies (Reyes+, 2011)</TD>
            <TD>In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z&lt;0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347#2</TD>
            <TD>2012-07-05T12:27:01Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/417/2347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/417/2347</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/417/2347 [sample]</TD>
            <TD>Tully-Fisher relation for SDSS galaxies (Reyes+, 2011)</TD>
            <TD>In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z&lt;0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347#sample</TD>
            <TD>2012-07-05T12:27:01Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/417/2347&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/417/2347</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/61/667 [1]</TD>
            <TD>Kinematics of Galactic old population (Norris 1986)</TD>
            <TD>A catalog is presented of some 1200 Galactic objects which have radial velocities and abundances [Fe/H]&lt;=-0.6. These data have been analyzed to yield information on the kinematic properties of the older populations of the Galaxy and on the interdependence between kinematics and abundance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667#1</TD>
            <TD>2012-11-13T07:16:33Z</TD>
            <TD>#Abundances#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/61/667</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/61/667</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/61/667 [2]</TD>
            <TD>Kinematics of Galactic old population (Norris 1986)</TD>
            <TD>A catalog is presented of some 1200 Galactic objects which have radial velocities and abundances [Fe/H]&lt;=-0.6. These data have been analyzed to yield information on the kinematic properties of the older populations of the Galaxy and on the interdependence between kinematics and abundance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667#2</TD>
            <TD>2012-11-13T07:16:33Z</TD>
            <TD>#Abundances#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/61/667&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/61/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/61/667 [table1]</TD>
            <TD>Kinematics of Galactic old population (Norris 1986)</TD>
            <TD>A catalog is presented of some 1200 Galactic objects which have radial velocities and abundances [Fe/H]&lt;=-0.6. These data have been analyzed to yield information on the kinematic properties of the older populations of the Galaxy and on the interdependence between kinematics and abundance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667#table1</TD>
            <TD>2012-11-13T07:16:33Z</TD>
            <TD>#Abundances#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/61/667</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/61/667&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/61/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASS-CALS [1]</TD>
            <TD>ROSAT All-Sky Survey CALS Galaxy Groups Catalog</TD>
            <TD>This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and optical survey of low-mass galaxy groups as of its publication date in 2000. The authors drew 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z = 15.5. They detected 61 groups (23%) as extended X-ray sources. The X-ray detections have a median membership of nine galaxies, a median recession velocity cz = 7250 km/s, a median projected velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) = 3 x 10^42 /h(100)^2 erg/s, where the Hubble constant is H(0) = 100 h(100) km/s/Mpc. The data in this table replace the preliminary analysis of the X-ray data which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat. &lt;J/ApJ/518/69&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rasscals#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Group#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rasscals</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rasscals&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rasscals.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASS-CALS [2]</TD>
            <TD>ROSAT All-Sky Survey CALS Galaxy Groups Catalog</TD>
            <TD>This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and optical survey of low-mass galaxy groups as of its publication date in 2000. The authors drew 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z = 15.5. They detected 61 groups (23%) as extended X-ray sources. The X-ray detections have a median membership of nine galaxies, a median recession velocity cz = 7250 km/s, a median projected velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) = 3 x 10^42 /h(100)^2 erg/s, where the Hubble constant is H(0) = 100 h(100) km/s/Mpc. The data in this table replace the preliminary analysis of the X-ray data which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat. &lt;J/ApJ/518/69&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rasscals#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Group#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rasscals</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rasscals&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rasscals.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASS-CALS [3]</TD>
            <TD>ROSAT All-Sky Survey CALS Galaxy Groups Catalog</TD>
            <TD>This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and optical survey of low-mass galaxy groups as of its publication date in 2000. The authors drew 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z = 15.5. They detected 61 groups (23%) as extended X-ray sources. The X-ray detections have a median membership of nine galaxies, a median recession velocity cz = 7250 km/s, a median projected velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) = 3 x 10^42 /h(100)^2 erg/s, where the Hubble constant is H(0) = 100 h(100) km/s/Mpc. The data in this table replace the preliminary analysis of the X-ray data which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat. &lt;J/ApJ/518/69&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rasscals#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Group#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rasscals</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rasscals&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rasscals.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/91/347 [1]</TD>
            <TD>A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)</TD>
            <TD>We have used the VLA to survey the inner Galaxy (|b|&lt;0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347#1</TD>
            <TD>2012-11-13T07:18:16Z</TD>
            <TD>#HII_regions#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/91/347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/91/347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/91/347 [2]</TD>
            <TD>A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)</TD>
            <TD>We have used the VLA to survey the inner Galaxy (|b|&lt;0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347#2</TD>
            <TD>2012-11-13T07:18:16Z</TD>
            <TD>#HII_regions#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/91/347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/91/347</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/91/347 [table2]</TD>
            <TD>A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)</TD>
            <TD>We have used the VLA to survey the inner Galaxy (|b|&lt;0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347#table2</TD>
            <TD>2012-11-13T07:18:16Z</TD>
            <TD>#HII_regions#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/91/347&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/91/347</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/417/2347 [1]</TD>
            <TD>Tully-Fisher relation for SDSS galaxies (Reyes+, 2011)</TD>
            <TD>In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z&lt;0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347#1</TD>
            <TD>2012-07-05T12:27:01Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/417/2347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/417/2347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/417/2347 [2]</TD>
            <TD>Tully-Fisher relation for SDSS galaxies (Reyes+, 2011)</TD>
            <TD>In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z&lt;0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347#2</TD>
            <TD>2012-07-05T12:27:01Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/417/2347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/417/2347</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/417/2347 [sample]</TD>
            <TD>Tully-Fisher relation for SDSS galaxies (Reyes+, 2011)</TD>
            <TD>In this paper, we derive scaling relations between photometric observable quantities and disc galaxy rotation velocity V_rot_ or Tully-Fisher relations (TFRs). Our methodology is dictated by our purpose of obtaining purely photometric, minimal-scatter estimators of V_rot_ applicable to large galaxy samples from imaging surveys. To achieve this goal, we have constructed a sample of 189 disc galaxies at redshifts z&lt;0.1 with long-slit H{alpha} spectroscopy from Pizagno et al. (2007, Cat. J/AJ/134/945) and new observations. By construction, this sample is a fair subsample of a large, well-defined parent disc sample of ~170000 galaxies selected from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347#sample</TD>
            <TD>2012-07-05T12:27:01Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/417/2347</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/417/2347&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/417/2347</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASS-CALS [1]</TD>
            <TD>ROSAT All-Sky Survey CALS Galaxy Groups Catalog</TD>
            <TD>This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and optical survey of low-mass galaxy groups as of its publication date in 2000. The authors drew 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z = 15.5. They detected 61 groups (23%) as extended X-ray sources. The X-ray detections have a median membership of nine galaxies, a median recession velocity cz = 7250 km/s, a median projected velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) = 3 x 10^42 /h(100)^2 erg/s, where the Hubble constant is H(0) = 100 h(100) km/s/Mpc. The data in this table replace the preliminary analysis of the X-ray data which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat. &lt;J/ApJ/518/69&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rasscals#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Group#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rasscals</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rasscals&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rasscals.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASS-CALS [2]</TD>
            <TD>ROSAT All-Sky Survey CALS Galaxy Groups Catalog</TD>
            <TD>This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and optical survey of low-mass galaxy groups as of its publication date in 2000. The authors drew 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z = 15.5. They detected 61 groups (23%) as extended X-ray sources. The X-ray detections have a median membership of nine galaxies, a median recession velocity cz = 7250 km/s, a median projected velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) = 3 x 10^42 /h(100)^2 erg/s, where the Hubble constant is H(0) = 100 h(100) km/s/Mpc. The data in this table replace the preliminary analysis of the X-ray data which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat. &lt;J/ApJ/518/69&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rasscals#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Group#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rasscals</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rasscals&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rasscals.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASS-CALS [3]</TD>
            <TD>ROSAT All-Sky Survey CALS Galaxy Groups Catalog</TD>
            <TD>This table contains the catalog from the ROSAT All-Sky Survey (RASS) Center for Astrophysics (CfA) Loose Systems, or RASSCALS, the largest X-ray and optical survey of low-mass galaxy groups as of its publication date in 2000. The authors drew 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z = 15.5. They detected 61 groups (23%) as extended X-ray sources. The X-ray detections have a median membership of nine galaxies, a median recession velocity cz = 7250 km/s, a median projected velocity dispersion sigma(p) = 400 km/s, and a median X-ray luminosity L(x) = 3 x 10^42 /h(100)^2 erg/s, where the Hubble constant is H(0) = 100 h(100) km/s/Mpc. The data in this table replace the preliminary analysis of the X-ray data which was presented in Mahdavi et al., 1999, ApJ, 518, 69 (CDS Cat. &lt;J/ApJ/518/69&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rasscals#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy Group#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rasscals</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rasscals&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rasscals.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WBL [1]</TD>
            <TD>WBL Individual Galaxies Data Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wblgalaxy#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wblgalaxy</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=wblgalaxy&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wblgalaxy.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WBL [2]</TD>
            <TD>WBL Individual Galaxies Data Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wblgalaxy#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wblgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=wblgalaxy&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wblgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WBL [3]</TD>
            <TD>WBL Individual Galaxies Data Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the individual galaxies in the poor clusters which ere given in Table 3 of the published catalog, and includes redshifts for the individual galaxies and cross-references to other galaxy catalogs. The WBL table (q.v.) contains the entries for the clusters themselves (given in Table 2 of the published catalog).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wblgalaxy#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wblgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_wblgalaxy&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wblgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/91/347 [1]</TD>
            <TD>A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)</TD>
            <TD>We have used the VLA to survey the inner Galaxy (|b|&lt;0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347#1</TD>
            <TD>2012-11-13T07:18:16Z</TD>
            <TD>#HII_regions#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/91/347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/91/347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/91/347 [2]</TD>
            <TD>A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)</TD>
            <TD>We have used the VLA to survey the inner Galaxy (|b|&lt;0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347#2</TD>
            <TD>2012-11-13T07:18:16Z</TD>
            <TD>#HII_regions#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/91/347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/91/347</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/91/347 [table2]</TD>
            <TD>A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)</TD>
            <TD>We have used the VLA to survey the inner Galaxy (|b|&lt;0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347#table2</TD>
            <TD>2012-11-13T07:18:16Z</TD>
            <TD>#HII_regions#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/91/347&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/91/347</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASSBCS [1]</TD>
            <TD>ROSAT All-Sky Survey Extended Brightest Cluster Sample</TD>
            <TD>This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample (BCS) and the Low-Flux Extension, which together form the Extended BCS (eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS, 301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere (Dec &gt;=0 degrees), at high Galactic latitudes (|b| &gt;= 20 degrees), with measured redshifts z &lt;= 0.3 and X-ray fluxes higher than 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4 keV band. This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS data and is the largest X-ray-selected cluster sample compiled to the publication date (1998). In addition to Abell clusters which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes were computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15% (mean 1-sigma error). The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the original BCS and employing an identical selection procedure, the BCS extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern hemisphere (Dec &gt;=0 degrees) and at high Galactic latitudes (|b| &gt;= 20 degrees). It comprises 99 X-ray-selected clusters of galaxies with measured redshifts z &lt;= 0.3 (as well as eight more at z &gt; 0.3) and total fluxes between 2.8 x 10^-12 and 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4keV band (the latter value being the flux limit of the original BCS). The extension can be combined (as it has been in this HEASARC table) with the main sample published in 1998 to form the homogeneously selected extended BCS (eBCS), the largest and statistically best understood cluster sample to emerge from the RASS to date. The nominal completeness of the combined sample (defined with respect to a power-law fit to the bright end of the BCS log N -log S distribution) is relatively low at 75% (compared with 90% for the high-flux sample of Paper I). However, just as for the original BCS, this incompleteness can be accurately quantified, and thus statistically corrected for, as a function of X-ray luminosity and redshift. In addition to its importance for improved statistical studies of the properties of clusters in the local Universe, the low-flux extension of the BCS is also intended to serve as a finding list for X-ray-bright clusters in the northern hemisphere which the authors hoped will prove useful in the preparation of cluster observations to be made with the next generation of X-ray telescopes such as Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassebcs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassebcs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rassebcs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassebcs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASSBCS [2]</TD>
            <TD>ROSAT All-Sky Survey Extended Brightest Cluster Sample</TD>
            <TD>This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample (BCS) and the Low-Flux Extension, which together form the Extended BCS (eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS, 301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere (Dec &gt;=0 degrees), at high Galactic latitudes (|b| &gt;= 20 degrees), with measured redshifts z &lt;= 0.3 and X-ray fluxes higher than 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4 keV band. This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS data and is the largest X-ray-selected cluster sample compiled to the publication date (1998). In addition to Abell clusters which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes were computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15% (mean 1-sigma error). The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the original BCS and employing an identical selection procedure, the BCS extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern hemisphere (Dec &gt;=0 degrees) and at high Galactic latitudes (|b| &gt;= 20 degrees). It comprises 99 X-ray-selected clusters of galaxies with measured redshifts z &lt;= 0.3 (as well as eight more at z &gt; 0.3) and total fluxes between 2.8 x 10^-12 and 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4keV band (the latter value being the flux limit of the original BCS). The extension can be combined (as it has been in this HEASARC table) with the main sample published in 1998 to form the homogeneously selected extended BCS (eBCS), the largest and statistically best understood cluster sample to emerge from the RASS to date. The nominal completeness of the combined sample (defined with respect to a power-law fit to the bright end of the BCS log N -log S distribution) is relatively low at 75% (compared with 90% for the high-flux sample of Paper I). However, just as for the original BCS, this incompleteness can be accurately quantified, and thus statistically corrected for, as a function of X-ray luminosity and redshift. In addition to its importance for improved statistical studies of the properties of clusters in the local Universe, the low-flux extension of the BCS is also intended to serve as a finding list for X-ray-bright clusters in the northern hemisphere which the authors hoped will prove useful in the preparation of cluster observations to be made with the next generation of X-ray telescopes such as Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassebcs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassebcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rassebcs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassebcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASSBCS [3]</TD>
            <TD>ROSAT All-Sky Survey Extended Brightest Cluster Sample</TD>
            <TD>This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample (BCS) and the Low-Flux Extension, which together form the Extended BCS (eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS, 301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere (Dec &gt;=0 degrees), at high Galactic latitudes (|b| &gt;= 20 degrees), with measured redshifts z &lt;= 0.3 and X-ray fluxes higher than 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4 keV band. This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS data and is the largest X-ray-selected cluster sample compiled to the publication date (1998). In addition to Abell clusters which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes were computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15% (mean 1-sigma error). The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the original BCS and employing an identical selection procedure, the BCS extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern hemisphere (Dec &gt;=0 degrees) and at high Galactic latitudes (|b| &gt;= 20 degrees). It comprises 99 X-ray-selected clusters of galaxies with measured redshifts z &lt;= 0.3 (as well as eight more at z &gt; 0.3) and total fluxes between 2.8 x 10^-12 and 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4keV band (the latter value being the flux limit of the original BCS). The extension can be combined (as it has been in this HEASARC table) with the main sample published in 1998 to form the homogeneously selected extended BCS (eBCS), the largest and statistically best understood cluster sample to emerge from the RASS to date. The nominal completeness of the combined sample (defined with respect to a power-law fit to the bright end of the BCS log N -log S distribution) is relatively low at 75% (compared with 90% for the high-flux sample of Paper I). However, just as for the original BCS, this incompleteness can be accurately quantified, and thus statistically corrected for, as a function of X-ray luminosity and redshift. In addition to its importance for improved statistical studies of the properties of clusters in the local Universe, the low-flux extension of the BCS is also intended to serve as a finding list for X-ray-bright clusters in the northern hemisphere which the authors hoped will prove useful in the preparation of cluster observations to be made with the next generation of X-ray telescopes such as Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassebcs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassebcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rassebcs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassebcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/91/347 [1]</TD>
            <TD>A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)</TD>
            <TD>We have used the VLA to survey the inner Galaxy (|b|&lt;0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347#1</TD>
            <TD>2012-11-13T07:18:16Z</TD>
            <TD>#HII_regions#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/91/347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/91/347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/91/347 [2]</TD>
            <TD>A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)</TD>
            <TD>We have used the VLA to survey the inner Galaxy (|b|&lt;0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347#2</TD>
            <TD>2012-11-13T07:18:16Z</TD>
            <TD>#HII_regions#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/91/347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/91/347</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/91/347 [table2]</TD>
            <TD>A 5-GHz VLA Survey of the Galactic Plane (Becker+ 1994)</TD>
            <TD>We have used the VLA to survey the inner Galaxy (|b|&lt;0.4{deg}, l=350-40{deg}) at 5GHz to a limiting sensitivity of between 2.5 and 10mJy. The survey has resulted in a catalog of 1272 discrete sources (including 100 sources outside the formal survey area) of which we have tentatively identified ~450 as ultracompact H II regions and ~45 as planetary nebulae. Approximately 30% of the radio sources are detected in the IRAS Point Source Catalog. The results confirm a scale height of only 30pc for ultracompact H II regions. We show that source lists generated from the IRAS Point Source Catalog alone suffer serious effects; the combination of the IRAS and radio surveys allows us to produce a much more complete census of the regions of massive star formation in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347#table2</TD>
            <TD>2012-11-13T07:18:16Z</TD>
            <TD>#HII_regions#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/91/347</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/91/347&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/91/347</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1982 [1]</TD>
            <TD>HST UBVI photometry of NGC 3081 inner regions (Buta+, 2004)</TD>
            <TD>The Hubble Space Telescope (HST) observations of NGC 3081 were secured on 2000 June 25 with the Wide Field Planetary Camera 2 (WFPC2). The center of the galaxy was placed near the overlap section between WFPC2 sections WF3 and WF4. Five broadband filters were used to observe the galaxy: F255W, F336W, F439W, F555W, and F814W. The latter four filters are intended to approximate Johnson U, B, V, and Cousins I photometric systems, respectively, while F255W is a mid-ultraviolet filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982#1</TD>
            <TD>2011-09-14T19:47:18Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1982</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1982</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1982 [2]</TD>
            <TD>HST UBVI photometry of NGC 3081 inner regions (Buta+, 2004)</TD>
            <TD>The Hubble Space Telescope (HST) observations of NGC 3081 were secured on 2000 June 25 with the Wide Field Planetary Camera 2 (WFPC2). The center of the galaxy was placed near the overlap section between WFPC2 sections WF3 and WF4. Five broadband filters were used to observe the galaxy: F255W, F336W, F439W, F555W, and F814W. The latter four filters are intended to approximate Johnson U, B, V, and Cousins I photometric systems, respectively, while F255W is a mid-ultraviolet filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982#2</TD>
            <TD>2011-09-14T19:47:18Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1982&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1982</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/1982 [table3]</TD>
            <TD>HST UBVI photometry of NGC 3081 inner regions (Buta+, 2004)</TD>
            <TD>The Hubble Space Telescope (HST) observations of NGC 3081 were secured on 2000 June 25 with the Wide Field Planetary Camera 2 (WFPC2). The center of the galaxy was placed near the overlap section between WFPC2 sections WF3 and WF4. Five broadband filters were used to observe the galaxy: F255W, F336W, F439W, F555W, and F814W. The latter four filters are intended to approximate Johnson U, B, V, and Cousins I photometric systems, respectively, while F255W is a mid-ultraviolet filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982#table3</TD>
            <TD>2011-09-14T19:47:18Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/1982&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1982</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASSBCS [1]</TD>
            <TD>ROSAT All-Sky Survey Extended Brightest Cluster Sample</TD>
            <TD>This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample (BCS) and the Low-Flux Extension, which together form the Extended BCS (eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS, 301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere (Dec &gt;=0 degrees), at high Galactic latitudes (|b| &gt;= 20 degrees), with measured redshifts z &lt;= 0.3 and X-ray fluxes higher than 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4 keV band. This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS data and is the largest X-ray-selected cluster sample compiled to the publication date (1998). In addition to Abell clusters which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes were computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15% (mean 1-sigma error). The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the original BCS and employing an identical selection procedure, the BCS extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern hemisphere (Dec &gt;=0 degrees) and at high Galactic latitudes (|b| &gt;= 20 degrees). It comprises 99 X-ray-selected clusters of galaxies with measured redshifts z &lt;= 0.3 (as well as eight more at z &gt; 0.3) and total fluxes between 2.8 x 10^-12 and 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4keV band (the latter value being the flux limit of the original BCS). The extension can be combined (as it has been in this HEASARC table) with the main sample published in 1998 to form the homogeneously selected extended BCS (eBCS), the largest and statistically best understood cluster sample to emerge from the RASS to date. The nominal completeness of the combined sample (defined with respect to a power-law fit to the bright end of the BCS log N -log S distribution) is relatively low at 75% (compared with 90% for the high-flux sample of Paper I). However, just as for the original BCS, this incompleteness can be accurately quantified, and thus statistically corrected for, as a function of X-ray luminosity and redshift. In addition to its importance for improved statistical studies of the properties of clusters in the local Universe, the low-flux extension of the BCS is also intended to serve as a finding list for X-ray-bright clusters in the northern hemisphere which the authors hoped will prove useful in the preparation of cluster observations to be made with the next generation of X-ray telescopes such as Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassebcs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassebcs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rassebcs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassebcs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASSBCS [2]</TD>
            <TD>ROSAT All-Sky Survey Extended Brightest Cluster Sample</TD>
            <TD>This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample (BCS) and the Low-Flux Extension, which together form the Extended BCS (eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS, 301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere (Dec &gt;=0 degrees), at high Galactic latitudes (|b| &gt;= 20 degrees), with measured redshifts z &lt;= 0.3 and X-ray fluxes higher than 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4 keV band. This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS data and is the largest X-ray-selected cluster sample compiled to the publication date (1998). In addition to Abell clusters which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes were computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15% (mean 1-sigma error). The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the original BCS and employing an identical selection procedure, the BCS extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern hemisphere (Dec &gt;=0 degrees) and at high Galactic latitudes (|b| &gt;= 20 degrees). It comprises 99 X-ray-selected clusters of galaxies with measured redshifts z &lt;= 0.3 (as well as eight more at z &gt; 0.3) and total fluxes between 2.8 x 10^-12 and 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4keV band (the latter value being the flux limit of the original BCS). The extension can be combined (as it has been in this HEASARC table) with the main sample published in 1998 to form the homogeneously selected extended BCS (eBCS), the largest and statistically best understood cluster sample to emerge from the RASS to date. The nominal completeness of the combined sample (defined with respect to a power-law fit to the bright end of the BCS log N -log S distribution) is relatively low at 75% (compared with 90% for the high-flux sample of Paper I). However, just as for the original BCS, this incompleteness can be accurately quantified, and thus statistically corrected for, as a function of X-ray luminosity and redshift. In addition to its importance for improved statistical studies of the properties of clusters in the local Universe, the low-flux extension of the BCS is also intended to serve as a finding list for X-ray-bright clusters in the northern hemisphere which the authors hoped will prove useful in the preparation of cluster observations to be made with the next generation of X-ray telescopes such as Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassebcs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassebcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rassebcs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassebcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASSBCS [3]</TD>
            <TD>ROSAT All-Sky Survey Extended Brightest Cluster Sample</TD>
            <TD>This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample (BCS) and the Low-Flux Extension, which together form the Extended BCS (eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS, 301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere (Dec &gt;=0 degrees), at high Galactic latitudes (|b| &gt;= 20 degrees), with measured redshifts z &lt;= 0.3 and X-ray fluxes higher than 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4 keV band. This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS data and is the largest X-ray-selected cluster sample compiled to the publication date (1998). In addition to Abell clusters which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes were computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15% (mean 1-sigma error). The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the original BCS and employing an identical selection procedure, the BCS extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern hemisphere (Dec &gt;=0 degrees) and at high Galactic latitudes (|b| &gt;= 20 degrees). It comprises 99 X-ray-selected clusters of galaxies with measured redshifts z &lt;= 0.3 (as well as eight more at z &gt; 0.3) and total fluxes between 2.8 x 10^-12 and 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4keV band (the latter value being the flux limit of the original BCS). The extension can be combined (as it has been in this HEASARC table) with the main sample published in 1998 to form the homogeneously selected extended BCS (eBCS), the largest and statistically best understood cluster sample to emerge from the RASS to date. The nominal completeness of the combined sample (defined with respect to a power-law fit to the bright end of the BCS log N -log S distribution) is relatively low at 75% (compared with 90% for the high-flux sample of Paper I). However, just as for the original BCS, this incompleteness can be accurately quantified, and thus statistically corrected for, as a function of X-ray luminosity and redshift. In addition to its importance for improved statistical studies of the properties of clusters in the local Universe, the low-flux extension of the BCS is also intended to serve as a finding list for X-ray-bright clusters in the northern hemisphere which the authors hoped will prove useful in the preparation of cluster observations to be made with the next generation of X-ray telescopes such as Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassebcs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassebcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rassebcs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassebcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/123/79 [1]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#1</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/123/79</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/123/79 [2]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#2</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/123/79&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/123/79 [3eg]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#3eg</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/123/79&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/123/79 [table1]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#table1</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/123/79&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASSBCS [1]</TD>
            <TD>ROSAT All-Sky Survey Extended Brightest Cluster Sample</TD>
            <TD>This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample (BCS) and the Low-Flux Extension, which together form the Extended BCS (eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS, 301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere (Dec &gt;=0 degrees), at high Galactic latitudes (|b| &gt;= 20 degrees), with measured redshifts z &lt;= 0.3 and X-ray fluxes higher than 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4 keV band. This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS data and is the largest X-ray-selected cluster sample compiled to the publication date (1998). In addition to Abell clusters which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes were computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15% (mean 1-sigma error). The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the original BCS and employing an identical selection procedure, the BCS extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern hemisphere (Dec &gt;=0 degrees) and at high Galactic latitudes (|b| &gt;= 20 degrees). It comprises 99 X-ray-selected clusters of galaxies with measured redshifts z &lt;= 0.3 (as well as eight more at z &gt; 0.3) and total fluxes between 2.8 x 10^-12 and 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4keV band (the latter value being the flux limit of the original BCS). The extension can be combined (as it has been in this HEASARC table) with the main sample published in 1998 to form the homogeneously selected extended BCS (eBCS), the largest and statistically best understood cluster sample to emerge from the RASS to date. The nominal completeness of the combined sample (defined with respect to a power-law fit to the bright end of the BCS log N -log S distribution) is relatively low at 75% (compared with 90% for the high-flux sample of Paper I). However, just as for the original BCS, this incompleteness can be accurately quantified, and thus statistically corrected for, as a function of X-ray luminosity and redshift. In addition to its importance for improved statistical studies of the properties of clusters in the local Universe, the low-flux extension of the BCS is also intended to serve as a finding list for X-ray-bright clusters in the northern hemisphere which the authors hoped will prove useful in the preparation of cluster observations to be made with the next generation of X-ray telescopes such as Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassebcs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassebcs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rassebcs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassebcs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASSBCS [2]</TD>
            <TD>ROSAT All-Sky Survey Extended Brightest Cluster Sample</TD>
            <TD>This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample (BCS) and the Low-Flux Extension, which together form the Extended BCS (eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS, 301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere (Dec &gt;=0 degrees), at high Galactic latitudes (|b| &gt;= 20 degrees), with measured redshifts z &lt;= 0.3 and X-ray fluxes higher than 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4 keV band. This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS data and is the largest X-ray-selected cluster sample compiled to the publication date (1998). In addition to Abell clusters which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes were computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15% (mean 1-sigma error). The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the original BCS and employing an identical selection procedure, the BCS extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern hemisphere (Dec &gt;=0 degrees) and at high Galactic latitudes (|b| &gt;= 20 degrees). It comprises 99 X-ray-selected clusters of galaxies with measured redshifts z &lt;= 0.3 (as well as eight more at z &gt; 0.3) and total fluxes between 2.8 x 10^-12 and 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4keV band (the latter value being the flux limit of the original BCS). The extension can be combined (as it has been in this HEASARC table) with the main sample published in 1998 to form the homogeneously selected extended BCS (eBCS), the largest and statistically best understood cluster sample to emerge from the RASS to date. The nominal completeness of the combined sample (defined with respect to a power-law fit to the bright end of the BCS log N -log S distribution) is relatively low at 75% (compared with 90% for the high-flux sample of Paper I). However, just as for the original BCS, this incompleteness can be accurately quantified, and thus statistically corrected for, as a function of X-ray luminosity and redshift. In addition to its importance for improved statistical studies of the properties of clusters in the local Universe, the low-flux extension of the BCS is also intended to serve as a finding list for X-ray-bright clusters in the northern hemisphere which the authors hoped will prove useful in the preparation of cluster observations to be made with the next generation of X-ray telescopes such as Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassebcs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassebcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rassebcs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassebcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASSBCS [3]</TD>
            <TD>ROSAT All-Sky Survey Extended Brightest Cluster Sample</TD>
            <TD>This table contains the ROSAT All-Sky Survey (RASS) Brightest Cluster Sample (BCS) and the Low-Flux Extension, which together form the Extended BCS (eBCS). The main BCS, which was presented in Ebeling et al. (1998, MNRAS, 301, 881; Paper I), is a 90% flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere (Dec &gt;=0 degrees), at high Galactic latitudes (|b| &gt;= 20 degrees), with measured redshifts z &lt;= 0.3 and X-ray fluxes higher than 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4 keV band. This sample, called the ROSAT Brightest Cluster Sample, is selected from RASS data and is the largest X-ray-selected cluster sample compiled to the publication date (1998). In addition to Abell clusters which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes were computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15% (mean 1-sigma error). The low-flux extension of the X-ray-selected ROSAT Brightest Cluster Sample was published in Ebeling et al. (2000, MNRAS, 318, 333; Paper IV). Like the original BCS and employing an identical selection procedure, the BCS extension is compiled from ROSAT All-Sky Survey (RASS) data in the northern hemisphere (Dec &gt;=0 degrees) and at high Galactic latitudes (|b| &gt;= 20 degrees). It comprises 99 X-ray-selected clusters of galaxies with measured redshifts z &lt;= 0.3 (as well as eight more at z &gt; 0.3) and total fluxes between 2.8 x 10^-12 and 4.4 x 10^-12 erg/cm^2/s in the 0.1 - 2.4keV band (the latter value being the flux limit of the original BCS). The extension can be combined (as it has been in this HEASARC table) with the main sample published in 1998 to form the homogeneously selected extended BCS (eBCS), the largest and statistically best understood cluster sample to emerge from the RASS to date. The nominal completeness of the combined sample (defined with respect to a power-law fit to the bright end of the BCS log N -log S distribution) is relatively low at 75% (compared with 90% for the high-flux sample of Paper I). However, just as for the original BCS, this incompleteness can be accurately quantified, and thus statistically corrected for, as a function of X-ray luminosity and redshift. In addition to its importance for improved statistical studies of the properties of clusters in the local Universe, the low-flux extension of the BCS is also intended to serve as a finding list for X-ray-bright clusters in the northern hemisphere which the authors hoped will prove useful in the preparation of cluster observations to be made with the next generation of X-ray telescopes such as Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassebcs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassebcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rassebcs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassebcs.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WBL [1]</TD>
            <TD>WBL Poor Galaxy Clusters Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wbl#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wbl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=wbl&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wbl.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WBL [2]</TD>
            <TD>WBL Poor Galaxy Clusters Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wbl#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wbl</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=wbl&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wbl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WBL [3]</TD>
            <TD>WBL Poor Galaxy Clusters Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wbl#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wbl</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_wbl&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wbl.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASS/GBC [1]</TD>
            <TD>RASS/Green Bank Catalog</TD>
            <TD>5-GHz high-resolution VLA observations of 2,127 radio and X-ray emitting sources found in both the Green Bank (GB) 5-GHz radio catalog and the ROSAT All-Sky Survey (RASS) are presented. This is referred to as the RASS/Green Bank sample: the HEASARC has abbreviated this to RASSGB to conform with the naming convention that we have used for other RASS catalogs (notice the catalog authors use the rather shorter acronym of RGB. Core flux densities and positions accurate to +/- 0.5" are reported, as well as the GB measurements of the total radio emission, for each source. Because of the radio and X-ray selection criteria adopted, this catalog is believed to almost exclusively contain radio- and X-ray-loud active galaxies. These data are used in the paper by Laurent-Muehleisen et al. (1997) that contains the published version of this catalog to derive the core-to-lobe ratio of objects in this sample, and to discuss their core-dominance relative to samples of radio galaxies and BL Lac objects: the authors conclude that this sample is approximately an order of magnitude more core-dominated than the radio galaxy sample, but is more than an order of magnitude less core-dominated than highly-beamed BL Lac objects. The published version of this catalog comprised two main tables, Table 2 and Table 3. Table 2 gave the 5-GHz high resolution radio source properties for the 1861 Rosat/Green Bank sources for which subarcsecond positions and core radio flux densities had been obtained, while Table 3 gave the 5-GHz radio source properties for the 436 Rosat/Green Bank sources for which only low resolution data were obtained. A table of the 83 Rosat/Green Bank sources for which no radio source greater than 5 sigma was observed in the follow-up VLA observations (Table 4 in the paper) is not included in the present HEASARC RASSGB Catalog but is available in our anonymous ftp area at: &lt;pre&gt; &lt;a href="ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/"&gt;ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/&lt;/a&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassgb#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Radio Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassgb</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rassgb&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassgb.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASS/GBC [2]</TD>
            <TD>RASS/Green Bank Catalog</TD>
            <TD>5-GHz high-resolution VLA observations of 2,127 radio and X-ray emitting sources found in both the Green Bank (GB) 5-GHz radio catalog and the ROSAT All-Sky Survey (RASS) are presented. This is referred to as the RASS/Green Bank sample: the HEASARC has abbreviated this to RASSGB to conform with the naming convention that we have used for other RASS catalogs (notice the catalog authors use the rather shorter acronym of RGB. Core flux densities and positions accurate to +/- 0.5" are reported, as well as the GB measurements of the total radio emission, for each source. Because of the radio and X-ray selection criteria adopted, this catalog is believed to almost exclusively contain radio- and X-ray-loud active galaxies. These data are used in the paper by Laurent-Muehleisen et al. (1997) that contains the published version of this catalog to derive the core-to-lobe ratio of objects in this sample, and to discuss their core-dominance relative to samples of radio galaxies and BL Lac objects: the authors conclude that this sample is approximately an order of magnitude more core-dominated than the radio galaxy sample, but is more than an order of magnitude less core-dominated than highly-beamed BL Lac objects. The published version of this catalog comprised two main tables, Table 2 and Table 3. Table 2 gave the 5-GHz high resolution radio source properties for the 1861 Rosat/Green Bank sources for which subarcsecond positions and core radio flux densities had been obtained, while Table 3 gave the 5-GHz radio source properties for the 436 Rosat/Green Bank sources for which only low resolution data were obtained. A table of the 83 Rosat/Green Bank sources for which no radio source greater than 5 sigma was observed in the follow-up VLA observations (Table 4 in the paper) is not included in the present HEASARC RASSGB Catalog but is available in our anonymous ftp area at: &lt;pre&gt; &lt;a href="ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/"&gt;ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/&lt;/a&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassgb#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Radio Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassgb</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rassgb&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassgb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASS/GBC [3]</TD>
            <TD>RASS/Green Bank Catalog</TD>
            <TD>5-GHz high-resolution VLA observations of 2,127 radio and X-ray emitting sources found in both the Green Bank (GB) 5-GHz radio catalog and the ROSAT All-Sky Survey (RASS) are presented. This is referred to as the RASS/Green Bank sample: the HEASARC has abbreviated this to RASSGB to conform with the naming convention that we have used for other RASS catalogs (notice the catalog authors use the rather shorter acronym of RGB. Core flux densities and positions accurate to +/- 0.5" are reported, as well as the GB measurements of the total radio emission, for each source. Because of the radio and X-ray selection criteria adopted, this catalog is believed to almost exclusively contain radio- and X-ray-loud active galaxies. These data are used in the paper by Laurent-Muehleisen et al. (1997) that contains the published version of this catalog to derive the core-to-lobe ratio of objects in this sample, and to discuss their core-dominance relative to samples of radio galaxies and BL Lac objects: the authors conclude that this sample is approximately an order of magnitude more core-dominated than the radio galaxy sample, but is more than an order of magnitude less core-dominated than highly-beamed BL Lac objects. The published version of this catalog comprised two main tables, Table 2 and Table 3. Table 2 gave the 5-GHz high resolution radio source properties for the 1861 Rosat/Green Bank sources for which subarcsecond positions and core radio flux densities had been obtained, while Table 3 gave the 5-GHz radio source properties for the 436 Rosat/Green Bank sources for which only low resolution data were obtained. A table of the 83 Rosat/Green Bank sources for which no radio source greater than 5 sigma was observed in the follow-up VLA observations (Table 4 in the paper) is not included in the present HEASARC RASSGB Catalog but is available in our anonymous ftp area at: &lt;pre&gt; &lt;a href="ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/"&gt;ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/&lt;/a&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassgb#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Radio Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassgb</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rassgb&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassgb.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WBL [1]</TD>
            <TD>WBL Poor Galaxy Clusters Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wbl#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wbl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=wbl&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wbl.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WBL [2]</TD>
            <TD>WBL Poor Galaxy Clusters Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wbl#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wbl</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=wbl&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wbl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WBL [3]</TD>
            <TD>WBL Poor Galaxy Clusters Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wbl#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wbl</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_wbl&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wbl.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASS/GBC [1]</TD>
            <TD>RASS/Green Bank Catalog</TD>
            <TD>5-GHz high-resolution VLA observations of 2,127 radio and X-ray emitting sources found in both the Green Bank (GB) 5-GHz radio catalog and the ROSAT All-Sky Survey (RASS) are presented. This is referred to as the RASS/Green Bank sample: the HEASARC has abbreviated this to RASSGB to conform with the naming convention that we have used for other RASS catalogs (notice the catalog authors use the rather shorter acronym of RGB. Core flux densities and positions accurate to +/- 0.5" are reported, as well as the GB measurements of the total radio emission, for each source. Because of the radio and X-ray selection criteria adopted, this catalog is believed to almost exclusively contain radio- and X-ray-loud active galaxies. These data are used in the paper by Laurent-Muehleisen et al. (1997) that contains the published version of this catalog to derive the core-to-lobe ratio of objects in this sample, and to discuss their core-dominance relative to samples of radio galaxies and BL Lac objects: the authors conclude that this sample is approximately an order of magnitude more core-dominated than the radio galaxy sample, but is more than an order of magnitude less core-dominated than highly-beamed BL Lac objects. The published version of this catalog comprised two main tables, Table 2 and Table 3. Table 2 gave the 5-GHz high resolution radio source properties for the 1861 Rosat/Green Bank sources for which subarcsecond positions and core radio flux densities had been obtained, while Table 3 gave the 5-GHz radio source properties for the 436 Rosat/Green Bank sources for which only low resolution data were obtained. A table of the 83 Rosat/Green Bank sources for which no radio source greater than 5 sigma was observed in the follow-up VLA observations (Table 4 in the paper) is not included in the present HEASARC RASSGB Catalog but is available in our anonymous ftp area at: &lt;pre&gt; &lt;a href="ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/"&gt;ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/&lt;/a&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassgb#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Radio Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassgb</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rassgb&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassgb.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASS/GBC [2]</TD>
            <TD>RASS/Green Bank Catalog</TD>
            <TD>5-GHz high-resolution VLA observations of 2,127 radio and X-ray emitting sources found in both the Green Bank (GB) 5-GHz radio catalog and the ROSAT All-Sky Survey (RASS) are presented. This is referred to as the RASS/Green Bank sample: the HEASARC has abbreviated this to RASSGB to conform with the naming convention that we have used for other RASS catalogs (notice the catalog authors use the rather shorter acronym of RGB. Core flux densities and positions accurate to +/- 0.5" are reported, as well as the GB measurements of the total radio emission, for each source. Because of the radio and X-ray selection criteria adopted, this catalog is believed to almost exclusively contain radio- and X-ray-loud active galaxies. These data are used in the paper by Laurent-Muehleisen et al. (1997) that contains the published version of this catalog to derive the core-to-lobe ratio of objects in this sample, and to discuss their core-dominance relative to samples of radio galaxies and BL Lac objects: the authors conclude that this sample is approximately an order of magnitude more core-dominated than the radio galaxy sample, but is more than an order of magnitude less core-dominated than highly-beamed BL Lac objects. The published version of this catalog comprised two main tables, Table 2 and Table 3. Table 2 gave the 5-GHz high resolution radio source properties for the 1861 Rosat/Green Bank sources for which subarcsecond positions and core radio flux densities had been obtained, while Table 3 gave the 5-GHz radio source properties for the 436 Rosat/Green Bank sources for which only low resolution data were obtained. A table of the 83 Rosat/Green Bank sources for which no radio source greater than 5 sigma was observed in the follow-up VLA observations (Table 4 in the paper) is not included in the present HEASARC RASSGB Catalog but is available in our anonymous ftp area at: &lt;pre&gt; &lt;a href="ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/"&gt;ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/&lt;/a&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassgb#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Radio Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassgb</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rassgb&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassgb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASS/GBC [3]</TD>
            <TD>RASS/Green Bank Catalog</TD>
            <TD>5-GHz high-resolution VLA observations of 2,127 radio and X-ray emitting sources found in both the Green Bank (GB) 5-GHz radio catalog and the ROSAT All-Sky Survey (RASS) are presented. This is referred to as the RASS/Green Bank sample: the HEASARC has abbreviated this to RASSGB to conform with the naming convention that we have used for other RASS catalogs (notice the catalog authors use the rather shorter acronym of RGB. Core flux densities and positions accurate to +/- 0.5" are reported, as well as the GB measurements of the total radio emission, for each source. Because of the radio and X-ray selection criteria adopted, this catalog is believed to almost exclusively contain radio- and X-ray-loud active galaxies. These data are used in the paper by Laurent-Muehleisen et al. (1997) that contains the published version of this catalog to derive the core-to-lobe ratio of objects in this sample, and to discuss their core-dominance relative to samples of radio galaxies and BL Lac objects: the authors conclude that this sample is approximately an order of magnitude more core-dominated than the radio galaxy sample, but is more than an order of magnitude less core-dominated than highly-beamed BL Lac objects. The published version of this catalog comprised two main tables, Table 2 and Table 3. Table 2 gave the 5-GHz high resolution radio source properties for the 1861 Rosat/Green Bank sources for which subarcsecond positions and core radio flux densities had been obtained, while Table 3 gave the 5-GHz radio source properties for the 436 Rosat/Green Bank sources for which only low resolution data were obtained. A table of the 83 Rosat/Green Bank sources for which no radio source greater than 5 sigma was observed in the follow-up VLA observations (Table 4 in the paper) is not included in the present HEASARC RASSGB Catalog but is available in our anonymous ftp area at: &lt;pre&gt; &lt;a href="ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/"&gt;ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/&lt;/a&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassgb#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Radio Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassgb</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rassgb&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassgb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/123/79 [1]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#1</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/123/79</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/123/79 [2]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#2</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/123/79&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/123/79 [3eg]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#3eg</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/123/79&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/123/79 [table1]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#table1</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/123/79&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASS/GBC [1]</TD>
            <TD>RASS/Green Bank Catalog</TD>
            <TD>5-GHz high-resolution VLA observations of 2,127 radio and X-ray emitting sources found in both the Green Bank (GB) 5-GHz radio catalog and the ROSAT All-Sky Survey (RASS) are presented. This is referred to as the RASS/Green Bank sample: the HEASARC has abbreviated this to RASSGB to conform with the naming convention that we have used for other RASS catalogs (notice the catalog authors use the rather shorter acronym of RGB. Core flux densities and positions accurate to +/- 0.5" are reported, as well as the GB measurements of the total radio emission, for each source. Because of the radio and X-ray selection criteria adopted, this catalog is believed to almost exclusively contain radio- and X-ray-loud active galaxies. These data are used in the paper by Laurent-Muehleisen et al. (1997) that contains the published version of this catalog to derive the core-to-lobe ratio of objects in this sample, and to discuss their core-dominance relative to samples of radio galaxies and BL Lac objects: the authors conclude that this sample is approximately an order of magnitude more core-dominated than the radio galaxy sample, but is more than an order of magnitude less core-dominated than highly-beamed BL Lac objects. The published version of this catalog comprised two main tables, Table 2 and Table 3. Table 2 gave the 5-GHz high resolution radio source properties for the 1861 Rosat/Green Bank sources for which subarcsecond positions and core radio flux densities had been obtained, while Table 3 gave the 5-GHz radio source properties for the 436 Rosat/Green Bank sources for which only low resolution data were obtained. A table of the 83 Rosat/Green Bank sources for which no radio source greater than 5 sigma was observed in the follow-up VLA observations (Table 4 in the paper) is not included in the present HEASARC RASSGB Catalog but is available in our anonymous ftp area at: &lt;pre&gt; &lt;a href="ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/"&gt;ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/&lt;/a&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassgb#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Radio Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassgb</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rassgb&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassgb.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASS/GBC [2]</TD>
            <TD>RASS/Green Bank Catalog</TD>
            <TD>5-GHz high-resolution VLA observations of 2,127 radio and X-ray emitting sources found in both the Green Bank (GB) 5-GHz radio catalog and the ROSAT All-Sky Survey (RASS) are presented. This is referred to as the RASS/Green Bank sample: the HEASARC has abbreviated this to RASSGB to conform with the naming convention that we have used for other RASS catalogs (notice the catalog authors use the rather shorter acronym of RGB. Core flux densities and positions accurate to +/- 0.5" are reported, as well as the GB measurements of the total radio emission, for each source. Because of the radio and X-ray selection criteria adopted, this catalog is believed to almost exclusively contain radio- and X-ray-loud active galaxies. These data are used in the paper by Laurent-Muehleisen et al. (1997) that contains the published version of this catalog to derive the core-to-lobe ratio of objects in this sample, and to discuss their core-dominance relative to samples of radio galaxies and BL Lac objects: the authors conclude that this sample is approximately an order of magnitude more core-dominated than the radio galaxy sample, but is more than an order of magnitude less core-dominated than highly-beamed BL Lac objects. The published version of this catalog comprised two main tables, Table 2 and Table 3. Table 2 gave the 5-GHz high resolution radio source properties for the 1861 Rosat/Green Bank sources for which subarcsecond positions and core radio flux densities had been obtained, while Table 3 gave the 5-GHz radio source properties for the 436 Rosat/Green Bank sources for which only low resolution data were obtained. A table of the 83 Rosat/Green Bank sources for which no radio source greater than 5 sigma was observed in the follow-up VLA observations (Table 4 in the paper) is not included in the present HEASARC RASSGB Catalog but is available in our anonymous ftp area at: &lt;pre&gt; &lt;a href="ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/"&gt;ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/&lt;/a&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassgb#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Radio Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassgb</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rassgb&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassgb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASS/GBC [3]</TD>
            <TD>RASS/Green Bank Catalog</TD>
            <TD>5-GHz high-resolution VLA observations of 2,127 radio and X-ray emitting sources found in both the Green Bank (GB) 5-GHz radio catalog and the ROSAT All-Sky Survey (RASS) are presented. This is referred to as the RASS/Green Bank sample: the HEASARC has abbreviated this to RASSGB to conform with the naming convention that we have used for other RASS catalogs (notice the catalog authors use the rather shorter acronym of RGB. Core flux densities and positions accurate to +/- 0.5" are reported, as well as the GB measurements of the total radio emission, for each source. Because of the radio and X-ray selection criteria adopted, this catalog is believed to almost exclusively contain radio- and X-ray-loud active galaxies. These data are used in the paper by Laurent-Muehleisen et al. (1997) that contains the published version of this catalog to derive the core-to-lobe ratio of objects in this sample, and to discuss their core-dominance relative to samples of radio galaxies and BL Lac objects: the authors conclude that this sample is approximately an order of magnitude more core-dominated than the radio galaxy sample, but is more than an order of magnitude less core-dominated than highly-beamed BL Lac objects. The published version of this catalog comprised two main tables, Table 2 and Table 3. Table 2 gave the 5-GHz high resolution radio source properties for the 1861 Rosat/Green Bank sources for which subarcsecond positions and core radio flux densities had been obtained, while Table 3 gave the 5-GHz radio source properties for the 436 Rosat/Green Bank sources for which only low resolution data were obtained. A table of the 83 Rosat/Green Bank sources for which no radio source greater than 5 sigma was observed in the follow-up VLA observations (Table 4 in the paper) is not included in the present HEASARC RASSGB Catalog but is available in our anonymous ftp area at: &lt;pre&gt; &lt;a href="ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/"&gt;ftp://legacy.gsfc.nasa.gov/heasarc/dbase/misc_files/rassgb/&lt;/a&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassgb#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Radio Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassgb</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rassgb&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassgb.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WBL [1]</TD>
            <TD>WBL Poor Galaxy Clusters Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wbl#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wbl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=wbl&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wbl.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WBL [2]</TD>
            <TD>WBL Poor Galaxy Clusters Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wbl#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wbl</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=wbl&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wbl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WBL [3]</TD>
            <TD>WBL Poor Galaxy Clusters Catalog (White et al. 1999)</TD>
            <TD>The Catalog of Nearby Poor Clusters of Galaxies of White et al. (1999), also known as the WBL Catalog, is a catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3 degrees declination. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^(4/3). These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. This table contains the entries for the clusters (given in Table 2 of the published catalog) and includes redshift data (where available) and cross-references to other group and cluster catalogs. The WBLGALAXY table (q.v.) contains the entries for the individual galaxies in the clusters which ere given in Table 3 of the published catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/wbl#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wbl</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_wbl&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/wbl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/123/79 [1]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#1</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/123/79</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/123/79 [2]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#2</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/123/79&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/123/79 [3eg]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#3eg</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/123/79&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/123/79 [table1]</TD>
            <TD>Third EGRET catalog (3EG) (Hartman+, 1999)</TD>
            <TD>The third catalog of high-energy gamma-ray sources detected by the EGRET telescope on the Compton Gamma Ray Observatory (3EG) includes data from 1991 April 22 to 1995 October 3 (cycles 1, 2, 3, and 4 of the mission). In addition to including more data than the second EGRET catalog and its supplement, this catalog uses completely reprocessed data to correct a number of mostly minimal errors and problems. 14 sources (3 from the Supplement) listed in Table 6 below are not appearing in the 3EG. The 271 sources (E&gt;100 MeV) in the catalog include the single 1991 solar flare bright enough to be detected as a source, the Large Magellanic Cloud, five pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources not yet identified firmly with known objects, although potential identifications have been suggested for a number of those. This catalog supersedes the 2EG (Cat. &lt;J/ApJS/101/259&gt;) and its supplement (Cat. &lt;J/ApJS/107/227&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79#table1</TD>
            <TD>2012-11-13T07:19:08Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/123/79</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/123/79&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/123/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROS400GCLS [1]</TD>
            <TD>ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog</TD>
            <TD>This is a catalog of galaxy clusters detected in a new ROSAT PSPC survey. The survey is optimized to sample, at high redshifts, the mass range corresponding to T &gt; 5 keV clusters at z = 0. Technically, our survey is the extension of the 160 square degree survey (160d, the HEASARC Browse table called ROSGALCLUS). The authors use the same detection algorithm, thus preserving the high quality of the resulting sample; the main difference is a significant increase in sky coverage. The new survey covers 397 square degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings, virtually all of the pointed ROSAT data that were suitable for the detection of distant clusters. The search volume for X-ray luminous clusters within z &lt; 1 exceeds that of the entire local universe (z &lt; 0.1). The authors detected 287 extended X-ray sources with fluxes f_x &gt; 1.4 x 10^-13 erg s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically confirmed as galaxy clusters, groups or individual elliptical galaxies. The paper from which this table is extracted provides a description of the input data, the statistical calibration of the survey via Monte Carlo simulations, and the catalog of detected clusters. The authors also therein compare the basic results with those from previous, smaller area surveys and find good agreement for the logN - log S distribution and the local X-ray luminosity function. This sample clearly shows a decrease in the number density for the most luminous clusters at z &gt; 0.3. The comparison of these ROSAT-derived fluxes with the accurate Chandra measurements for a subset of high-redshift clusters demonstrates the validity of the 400 square degree survey's statistical calibration. This Browse table contains the main cluster catalog (Table 4 of the reference paper) which comprises 242 serendipitously detected clusters of galaxies. It does not include 24 clusters within a redshift of 0.01 of the redshift of the target of the ROSAT observation (given in Table 5 of the reference paper), as these latter are not entirely serendipitous, 5 noncluster extended sources (given in Table 6 of the reference paper), nor 16 likely false X-ray detections (given in Table 7 of the reference paper).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ros400gcls#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ros400gcls</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ros400gcls&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/ros400gcls.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROS400GCLS [2]</TD>
            <TD>ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog</TD>
            <TD>This is a catalog of galaxy clusters detected in a new ROSAT PSPC survey. The survey is optimized to sample, at high redshifts, the mass range corresponding to T &gt; 5 keV clusters at z = 0. Technically, our survey is the extension of the 160 square degree survey (160d, the HEASARC Browse table called ROSGALCLUS). The authors use the same detection algorithm, thus preserving the high quality of the resulting sample; the main difference is a significant increase in sky coverage. The new survey covers 397 square degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings, virtually all of the pointed ROSAT data that were suitable for the detection of distant clusters. The search volume for X-ray luminous clusters within z &lt; 1 exceeds that of the entire local universe (z &lt; 0.1). The authors detected 287 extended X-ray sources with fluxes f_x &gt; 1.4 x 10^-13 erg s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically confirmed as galaxy clusters, groups or individual elliptical galaxies. The paper from which this table is extracted provides a description of the input data, the statistical calibration of the survey via Monte Carlo simulations, and the catalog of detected clusters. The authors also therein compare the basic results with those from previous, smaller area surveys and find good agreement for the logN - log S distribution and the local X-ray luminosity function. This sample clearly shows a decrease in the number density for the most luminous clusters at z &gt; 0.3. The comparison of these ROSAT-derived fluxes with the accurate Chandra measurements for a subset of high-redshift clusters demonstrates the validity of the 400 square degree survey's statistical calibration. This Browse table contains the main cluster catalog (Table 4 of the reference paper) which comprises 242 serendipitously detected clusters of galaxies. It does not include 24 clusters within a redshift of 0.01 of the redshift of the target of the ROSAT observation (given in Table 5 of the reference paper), as these latter are not entirely serendipitous, 5 noncluster extended sources (given in Table 6 of the reference paper), nor 16 likely false X-ray detections (given in Table 7 of the reference paper).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ros400gcls#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ros400gcls</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ros400gcls&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/ros400gcls.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROS400GCLS [3]</TD>
            <TD>ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog</TD>
            <TD>This is a catalog of galaxy clusters detected in a new ROSAT PSPC survey. The survey is optimized to sample, at high redshifts, the mass range corresponding to T &gt; 5 keV clusters at z = 0. Technically, our survey is the extension of the 160 square degree survey (160d, the HEASARC Browse table called ROSGALCLUS). The authors use the same detection algorithm, thus preserving the high quality of the resulting sample; the main difference is a significant increase in sky coverage. The new survey covers 397 square degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings, virtually all of the pointed ROSAT data that were suitable for the detection of distant clusters. The search volume for X-ray luminous clusters within z &lt; 1 exceeds that of the entire local universe (z &lt; 0.1). The authors detected 287 extended X-ray sources with fluxes f_x &gt; 1.4 x 10^-13 erg s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically confirmed as galaxy clusters, groups or individual elliptical galaxies. The paper from which this table is extracted provides a description of the input data, the statistical calibration of the survey via Monte Carlo simulations, and the catalog of detected clusters. The authors also therein compare the basic results with those from previous, smaller area surveys and find good agreement for the logN - log S distribution and the local X-ray luminosity function. This sample clearly shows a decrease in the number density for the most luminous clusters at z &gt; 0.3. The comparison of these ROSAT-derived fluxes with the accurate Chandra measurements for a subset of high-redshift clusters demonstrates the validity of the 400 square degree survey's statistical calibration. This Browse table contains the main cluster catalog (Table 4 of the reference paper) which comprises 242 serendipitously detected clusters of galaxies. It does not include 24 clusters within a redshift of 0.01 of the redshift of the target of the ROSAT observation (given in Table 5 of the reference paper), as these latter are not entirely serendipitous, 5 noncluster extended sources (given in Table 6 of the reference paper), nor 16 likely false X-ray detections (given in Table 7 of the reference paper).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ros400gcls#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ros400gcls</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ros400gcls&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/ros400gcls.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SIXDFGS [1]</TD>
            <TD>6dFGS Galaxy Survey Final Redshift Release Catalog</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b| &gt; 10 degrees). Its 136,304 spectra have yielded 110,256 new extragalactic redshifts and a new catalogue of 125,071 galaxies making near-complete samples with limits in (K, H, J, r&lt;sub&gt;F&lt;/sub&gt;, b&lt;sub&gt;J&lt;/sub&gt;) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (radial velocity quality flag Q =3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all). It supersedes the previous DR2 version (CDS Cat. VII/249). The home page of of the 6dFGS database is &lt;a href="http://www-wfau.roe.ac.uk/6dFGS"&gt;http://www-wfau.roe.ac.uk/6dFGS&lt;/a&gt;. Any use of these data should explicitly state that they come from the Final Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS, 399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004, MNRAS, 355, 747).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/sixdfgs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sixdfgs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sixdfgs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sixdfgs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SIXDFGS [2]</TD>
            <TD>6dFGS Galaxy Survey Final Redshift Release Catalog</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b| &gt; 10 degrees). Its 136,304 spectra have yielded 110,256 new extragalactic redshifts and a new catalogue of 125,071 galaxies making near-complete samples with limits in (K, H, J, r&lt;sub&gt;F&lt;/sub&gt;, b&lt;sub&gt;J&lt;/sub&gt;) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (radial velocity quality flag Q =3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all). It supersedes the previous DR2 version (CDS Cat. VII/249). The home page of of the 6dFGS database is &lt;a href="http://www-wfau.roe.ac.uk/6dFGS"&gt;http://www-wfau.roe.ac.uk/6dFGS&lt;/a&gt;. Any use of these data should explicitly state that they come from the Final Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS, 399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004, MNRAS, 355, 747).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/sixdfgs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sixdfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sixdfgs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sixdfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SIXDFGS [3]</TD>
            <TD>6dFGS Galaxy Survey Final Redshift Release Catalog</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b| &gt; 10 degrees). Its 136,304 spectra have yielded 110,256 new extragalactic redshifts and a new catalogue of 125,071 galaxies making near-complete samples with limits in (K, H, J, r&lt;sub&gt;F&lt;/sub&gt;, b&lt;sub&gt;J&lt;/sub&gt;) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (radial velocity quality flag Q =3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all). It supersedes the previous DR2 version (CDS Cat. VII/249). The home page of of the 6dFGS database is &lt;a href="http://www-wfau.roe.ac.uk/6dFGS"&gt;http://www-wfau.roe.ac.uk/6dFGS&lt;/a&gt;. Any use of these data should explicitly state that they come from the Final Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS, 399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004, MNRAS, 355, 747).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/sixdfgs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sixdfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sixdfgs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sixdfgs.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROS400GCLS [1]</TD>
            <TD>ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog</TD>
            <TD>This is a catalog of galaxy clusters detected in a new ROSAT PSPC survey. The survey is optimized to sample, at high redshifts, the mass range corresponding to T &gt; 5 keV clusters at z = 0. Technically, our survey is the extension of the 160 square degree survey (160d, the HEASARC Browse table called ROSGALCLUS). The authors use the same detection algorithm, thus preserving the high quality of the resulting sample; the main difference is a significant increase in sky coverage. The new survey covers 397 square degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings, virtually all of the pointed ROSAT data that were suitable for the detection of distant clusters. The search volume for X-ray luminous clusters within z &lt; 1 exceeds that of the entire local universe (z &lt; 0.1). The authors detected 287 extended X-ray sources with fluxes f_x &gt; 1.4 x 10^-13 erg s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically confirmed as galaxy clusters, groups or individual elliptical galaxies. The paper from which this table is extracted provides a description of the input data, the statistical calibration of the survey via Monte Carlo simulations, and the catalog of detected clusters. The authors also therein compare the basic results with those from previous, smaller area surveys and find good agreement for the logN - log S distribution and the local X-ray luminosity function. This sample clearly shows a decrease in the number density for the most luminous clusters at z &gt; 0.3. The comparison of these ROSAT-derived fluxes with the accurate Chandra measurements for a subset of high-redshift clusters demonstrates the validity of the 400 square degree survey's statistical calibration. This Browse table contains the main cluster catalog (Table 4 of the reference paper) which comprises 242 serendipitously detected clusters of galaxies. It does not include 24 clusters within a redshift of 0.01 of the redshift of the target of the ROSAT observation (given in Table 5 of the reference paper), as these latter are not entirely serendipitous, 5 noncluster extended sources (given in Table 6 of the reference paper), nor 16 likely false X-ray detections (given in Table 7 of the reference paper).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ros400gcls#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ros400gcls</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ros400gcls&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/ros400gcls.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROS400GCLS [2]</TD>
            <TD>ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog</TD>
            <TD>This is a catalog of galaxy clusters detected in a new ROSAT PSPC survey. The survey is optimized to sample, at high redshifts, the mass range corresponding to T &gt; 5 keV clusters at z = 0. Technically, our survey is the extension of the 160 square degree survey (160d, the HEASARC Browse table called ROSGALCLUS). The authors use the same detection algorithm, thus preserving the high quality of the resulting sample; the main difference is a significant increase in sky coverage. The new survey covers 397 square degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings, virtually all of the pointed ROSAT data that were suitable for the detection of distant clusters. The search volume for X-ray luminous clusters within z &lt; 1 exceeds that of the entire local universe (z &lt; 0.1). The authors detected 287 extended X-ray sources with fluxes f_x &gt; 1.4 x 10^-13 erg s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically confirmed as galaxy clusters, groups or individual elliptical galaxies. The paper from which this table is extracted provides a description of the input data, the statistical calibration of the survey via Monte Carlo simulations, and the catalog of detected clusters. The authors also therein compare the basic results with those from previous, smaller area surveys and find good agreement for the logN - log S distribution and the local X-ray luminosity function. This sample clearly shows a decrease in the number density for the most luminous clusters at z &gt; 0.3. The comparison of these ROSAT-derived fluxes with the accurate Chandra measurements for a subset of high-redshift clusters demonstrates the validity of the 400 square degree survey's statistical calibration. This Browse table contains the main cluster catalog (Table 4 of the reference paper) which comprises 242 serendipitously detected clusters of galaxies. It does not include 24 clusters within a redshift of 0.01 of the redshift of the target of the ROSAT observation (given in Table 5 of the reference paper), as these latter are not entirely serendipitous, 5 noncluster extended sources (given in Table 6 of the reference paper), nor 16 likely false X-ray detections (given in Table 7 of the reference paper).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ros400gcls#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ros400gcls</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ros400gcls&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/ros400gcls.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROS400GCLS [3]</TD>
            <TD>ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog</TD>
            <TD>This is a catalog of galaxy clusters detected in a new ROSAT PSPC survey. The survey is optimized to sample, at high redshifts, the mass range corresponding to T &gt; 5 keV clusters at z = 0. Technically, our survey is the extension of the 160 square degree survey (160d, the HEASARC Browse table called ROSGALCLUS). The authors use the same detection algorithm, thus preserving the high quality of the resulting sample; the main difference is a significant increase in sky coverage. The new survey covers 397 square degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings, virtually all of the pointed ROSAT data that were suitable for the detection of distant clusters. The search volume for X-ray luminous clusters within z &lt; 1 exceeds that of the entire local universe (z &lt; 0.1). The authors detected 287 extended X-ray sources with fluxes f_x &gt; 1.4 x 10^-13 erg s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically confirmed as galaxy clusters, groups or individual elliptical galaxies. The paper from which this table is extracted provides a description of the input data, the statistical calibration of the survey via Monte Carlo simulations, and the catalog of detected clusters. The authors also therein compare the basic results with those from previous, smaller area surveys and find good agreement for the logN - log S distribution and the local X-ray luminosity function. This sample clearly shows a decrease in the number density for the most luminous clusters at z &gt; 0.3. The comparison of these ROSAT-derived fluxes with the accurate Chandra measurements for a subset of high-redshift clusters demonstrates the validity of the 400 square degree survey's statistical calibration. This Browse table contains the main cluster catalog (Table 4 of the reference paper) which comprises 242 serendipitously detected clusters of galaxies. It does not include 24 clusters within a redshift of 0.01 of the redshift of the target of the ROSAT observation (given in Table 5 of the reference paper), as these latter are not entirely serendipitous, 5 noncluster extended sources (given in Table 6 of the reference paper), nor 16 likely false X-ray detections (given in Table 7 of the reference paper).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ros400gcls#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ros400gcls</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ros400gcls&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/ros400gcls.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/126/1 [1]</TD>
            <TD>Abell clusters photometry (Quintana+, 2000)</TD>
            <TD>We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, III, and II. We have performed total photometry in the Gunn r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1#1</TD>
            <TD>2012-11-13T07:19:44Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/126/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/126/1 [2]</TD>
            <TD>Abell clusters photometry (Quintana+, 2000)</TD>
            <TD>We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, III, and II. We have performed total photometry in the Gunn r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1#2</TD>
            <TD>2012-11-13T07:19:44Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/126/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/1 [table6]</TD>
            <TD>Abell clusters photometry (Quintana+, 2000)</TD>
            <TD>We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, III, and II. We have performed total photometry in the Gunn r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1#table6</TD>
            <TD>2012-11-13T07:19:44Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROS400GCLS [1]</TD>
            <TD>ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog</TD>
            <TD>This is a catalog of galaxy clusters detected in a new ROSAT PSPC survey. The survey is optimized to sample, at high redshifts, the mass range corresponding to T &gt; 5 keV clusters at z = 0. Technically, our survey is the extension of the 160 square degree survey (160d, the HEASARC Browse table called ROSGALCLUS). The authors use the same detection algorithm, thus preserving the high quality of the resulting sample; the main difference is a significant increase in sky coverage. The new survey covers 397 square degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings, virtually all of the pointed ROSAT data that were suitable for the detection of distant clusters. The search volume for X-ray luminous clusters within z &lt; 1 exceeds that of the entire local universe (z &lt; 0.1). The authors detected 287 extended X-ray sources with fluxes f_x &gt; 1.4 x 10^-13 erg s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically confirmed as galaxy clusters, groups or individual elliptical galaxies. The paper from which this table is extracted provides a description of the input data, the statistical calibration of the survey via Monte Carlo simulations, and the catalog of detected clusters. The authors also therein compare the basic results with those from previous, smaller area surveys and find good agreement for the logN - log S distribution and the local X-ray luminosity function. This sample clearly shows a decrease in the number density for the most luminous clusters at z &gt; 0.3. The comparison of these ROSAT-derived fluxes with the accurate Chandra measurements for a subset of high-redshift clusters demonstrates the validity of the 400 square degree survey's statistical calibration. This Browse table contains the main cluster catalog (Table 4 of the reference paper) which comprises 242 serendipitously detected clusters of galaxies. It does not include 24 clusters within a redshift of 0.01 of the redshift of the target of the ROSAT observation (given in Table 5 of the reference paper), as these latter are not entirely serendipitous, 5 noncluster extended sources (given in Table 6 of the reference paper), nor 16 likely false X-ray detections (given in Table 7 of the reference paper).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ros400gcls#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ros400gcls</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ros400gcls&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/ros400gcls.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROS400GCLS [2]</TD>
            <TD>ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog</TD>
            <TD>This is a catalog of galaxy clusters detected in a new ROSAT PSPC survey. The survey is optimized to sample, at high redshifts, the mass range corresponding to T &gt; 5 keV clusters at z = 0. Technically, our survey is the extension of the 160 square degree survey (160d, the HEASARC Browse table called ROSGALCLUS). The authors use the same detection algorithm, thus preserving the high quality of the resulting sample; the main difference is a significant increase in sky coverage. The new survey covers 397 square degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings, virtually all of the pointed ROSAT data that were suitable for the detection of distant clusters. The search volume for X-ray luminous clusters within z &lt; 1 exceeds that of the entire local universe (z &lt; 0.1). The authors detected 287 extended X-ray sources with fluxes f_x &gt; 1.4 x 10^-13 erg s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically confirmed as galaxy clusters, groups or individual elliptical galaxies. The paper from which this table is extracted provides a description of the input data, the statistical calibration of the survey via Monte Carlo simulations, and the catalog of detected clusters. The authors also therein compare the basic results with those from previous, smaller area surveys and find good agreement for the logN - log S distribution and the local X-ray luminosity function. This sample clearly shows a decrease in the number density for the most luminous clusters at z &gt; 0.3. The comparison of these ROSAT-derived fluxes with the accurate Chandra measurements for a subset of high-redshift clusters demonstrates the validity of the 400 square degree survey's statistical calibration. This Browse table contains the main cluster catalog (Table 4 of the reference paper) which comprises 242 serendipitously detected clusters of galaxies. It does not include 24 clusters within a redshift of 0.01 of the redshift of the target of the ROSAT observation (given in Table 5 of the reference paper), as these latter are not entirely serendipitous, 5 noncluster extended sources (given in Table 6 of the reference paper), nor 16 likely false X-ray detections (given in Table 7 of the reference paper).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ros400gcls#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ros400gcls</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ros400gcls&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/ros400gcls.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROS400GCLS [3]</TD>
            <TD>ROSAT PSPC 400 Square Degree Galaxy Cluster Catalog</TD>
            <TD>This is a catalog of galaxy clusters detected in a new ROSAT PSPC survey. The survey is optimized to sample, at high redshifts, the mass range corresponding to T &gt; 5 keV clusters at z = 0. Technically, our survey is the extension of the 160 square degree survey (160d, the HEASARC Browse table called ROSGALCLUS). The authors use the same detection algorithm, thus preserving the high quality of the resulting sample; the main difference is a significant increase in sky coverage. The new survey covers 397 square degrees and is based on 1610 high Galactic latitude ROSAT PSPC pointings, virtually all of the pointed ROSAT data that were suitable for the detection of distant clusters. The search volume for X-ray luminous clusters within z &lt; 1 exceeds that of the entire local universe (z &lt; 0.1). The authors detected 287 extended X-ray sources with fluxes f_x &gt; 1.4 x 10^-13 erg s^-1 cm^-2 in the 0.5 - 2 keV energy band, of which 266 (93%) are optically confirmed as galaxy clusters, groups or individual elliptical galaxies. The paper from which this table is extracted provides a description of the input data, the statistical calibration of the survey via Monte Carlo simulations, and the catalog of detected clusters. The authors also therein compare the basic results with those from previous, smaller area surveys and find good agreement for the logN - log S distribution and the local X-ray luminosity function. This sample clearly shows a decrease in the number density for the most luminous clusters at z &gt; 0.3. The comparison of these ROSAT-derived fluxes with the accurate Chandra measurements for a subset of high-redshift clusters demonstrates the validity of the 400 square degree survey's statistical calibration. This Browse table contains the main cluster catalog (Table 4 of the reference paper) which comprises 242 serendipitously detected clusters of galaxies. It does not include 24 clusters within a redshift of 0.01 of the redshift of the target of the ROSAT observation (given in Table 5 of the reference paper), as these latter are not entirely serendipitous, 5 noncluster extended sources (given in Table 6 of the reference paper), nor 16 likely false X-ray detections (given in Table 7 of the reference paper).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ros400gcls#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ros400gcls</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ros400gcls&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/ros400gcls.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SIXDFGS [1]</TD>
            <TD>6dFGS Galaxy Survey Final Redshift Release Catalog</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b| &gt; 10 degrees). Its 136,304 spectra have yielded 110,256 new extragalactic redshifts and a new catalogue of 125,071 galaxies making near-complete samples with limits in (K, H, J, r&lt;sub&gt;F&lt;/sub&gt;, b&lt;sub&gt;J&lt;/sub&gt;) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (radial velocity quality flag Q =3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all). It supersedes the previous DR2 version (CDS Cat. VII/249). The home page of of the 6dFGS database is &lt;a href="http://www-wfau.roe.ac.uk/6dFGS"&gt;http://www-wfau.roe.ac.uk/6dFGS&lt;/a&gt;. Any use of these data should explicitly state that they come from the Final Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS, 399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004, MNRAS, 355, 747).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/sixdfgs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sixdfgs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sixdfgs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sixdfgs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SIXDFGS [2]</TD>
            <TD>6dFGS Galaxy Survey Final Redshift Release Catalog</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b| &gt; 10 degrees). Its 136,304 spectra have yielded 110,256 new extragalactic redshifts and a new catalogue of 125,071 galaxies making near-complete samples with limits in (K, H, J, r&lt;sub&gt;F&lt;/sub&gt;, b&lt;sub&gt;J&lt;/sub&gt;) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (radial velocity quality flag Q =3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all). It supersedes the previous DR2 version (CDS Cat. VII/249). The home page of of the 6dFGS database is &lt;a href="http://www-wfau.roe.ac.uk/6dFGS"&gt;http://www-wfau.roe.ac.uk/6dFGS&lt;/a&gt;. Any use of these data should explicitly state that they come from the Final Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS, 399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004, MNRAS, 355, 747).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/sixdfgs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sixdfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sixdfgs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sixdfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SIXDFGS [3]</TD>
            <TD>6dFGS Galaxy Survey Final Redshift Release Catalog</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b| &gt; 10 degrees). Its 136,304 spectra have yielded 110,256 new extragalactic redshifts and a new catalogue of 125,071 galaxies making near-complete samples with limits in (K, H, J, r&lt;sub&gt;F&lt;/sub&gt;, b&lt;sub&gt;J&lt;/sub&gt;) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (radial velocity quality flag Q =3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all). It supersedes the previous DR2 version (CDS Cat. VII/249). The home page of of the 6dFGS database is &lt;a href="http://www-wfau.roe.ac.uk/6dFGS"&gt;http://www-wfau.roe.ac.uk/6dFGS&lt;/a&gt;. Any use of these data should explicitly state that they come from the Final Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS, 399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004, MNRAS, 355, 747).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/sixdfgs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sixdfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sixdfgs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sixdfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/126/1 [1]</TD>
            <TD>Abell clusters photometry (Quintana+, 2000)</TD>
            <TD>We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, III, and II. We have performed total photometry in the Gunn r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1#1</TD>
            <TD>2012-11-13T07:19:44Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/126/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/126/1 [2]</TD>
            <TD>Abell clusters photometry (Quintana+, 2000)</TD>
            <TD>We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, III, and II. We have performed total photometry in the Gunn r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1#2</TD>
            <TD>2012-11-13T07:19:44Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/126/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/1 [table6]</TD>
            <TD>Abell clusters photometry (Quintana+, 2000)</TD>
            <TD>We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, III, and II. We have performed total photometry in the Gunn r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1#table6</TD>
            <TD>2012-11-13T07:19:44Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROSATNEPID [1]</TD>
            <TD>ROSAT North Ecliptic Pole Survey Optical Identifications</TD>
            <TD>This table contains the ROSAT North Ecliptic Pole (NEP) Survey list of optical identifications. The X-ray data around the NEP from the ROSAT All-Sky Survey (RASS) were used to construct a contiguous area survey which consisted of a sample of 445 individual X-ray sources with fluxes more than ~2x10^-14 erg/cm^2/s in the 0.5 - 2.0 keV energy band. The NEP survey is centered at RA= 18hr 00min Dec= +66deg 33', and covers a region of 80.7 square degrees at a moderate Galactic latitude b= 29.8 degrees. Hence, the NEP survey is as deep as and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. The authors identified 99.6% of the sources and determined redshifts for the extragalactic objects. This table contains the optical identifications for the NEP catalog of X-ray sources, including basic X-ray data and properties of the sources. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGN) (~49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (~34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. The data on AGN in this catalog are essentially superceded by the data in the more recent catalog of Mullis et al. (2004, ApJ, 617, 192), available in HEASARC Browse as the ROSNEPOID table (q.v.), in which, inter alia, a corrected count rate to flux conversion and a different cosmology were used.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rosnepoid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rosnepoid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rosnepoid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rosnepoid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROSATNEPID [2]</TD>
            <TD>ROSAT North Ecliptic Pole Survey Optical Identifications</TD>
            <TD>This table contains the ROSAT North Ecliptic Pole (NEP) Survey list of optical identifications. The X-ray data around the NEP from the ROSAT All-Sky Survey (RASS) were used to construct a contiguous area survey which consisted of a sample of 445 individual X-ray sources with fluxes more than ~2x10^-14 erg/cm^2/s in the 0.5 - 2.0 keV energy band. The NEP survey is centered at RA= 18hr 00min Dec= +66deg 33', and covers a region of 80.7 square degrees at a moderate Galactic latitude b= 29.8 degrees. Hence, the NEP survey is as deep as and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. The authors identified 99.6% of the sources and determined redshifts for the extragalactic objects. This table contains the optical identifications for the NEP catalog of X-ray sources, including basic X-ray data and properties of the sources. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGN) (~49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (~34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. The data on AGN in this catalog are essentially superceded by the data in the more recent catalog of Mullis et al. (2004, ApJ, 617, 192), available in HEASARC Browse as the ROSNEPOID table (q.v.), in which, inter alia, a corrected count rate to flux conversion and a different cosmology were used.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rosnepoid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rosnepoid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rosnepoid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rosnepoid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROSATNEPID [3]</TD>
            <TD>ROSAT North Ecliptic Pole Survey Optical Identifications</TD>
            <TD>This table contains the ROSAT North Ecliptic Pole (NEP) Survey list of optical identifications. The X-ray data around the NEP from the ROSAT All-Sky Survey (RASS) were used to construct a contiguous area survey which consisted of a sample of 445 individual X-ray sources with fluxes more than ~2x10^-14 erg/cm^2/s in the 0.5 - 2.0 keV energy band. The NEP survey is centered at RA= 18hr 00min Dec= +66deg 33', and covers a region of 80.7 square degrees at a moderate Galactic latitude b= 29.8 degrees. Hence, the NEP survey is as deep as and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. The authors identified 99.6% of the sources and determined redshifts for the extragalactic objects. This table contains the optical identifications for the NEP catalog of X-ray sources, including basic X-ray data and properties of the sources. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGN) (~49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (~34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. The data on AGN in this catalog are essentially superceded by the data in the more recent catalog of Mullis et al. (2004, ApJ, 617, 192), available in HEASARC Browse as the ROSNEPOID table (q.v.), in which, inter alia, a corrected count rate to flux conversion and a different cosmology were used.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rosnepoid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rosnepoid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rosnepoid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rosnepoid.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SIXDFGS [1]</TD>
            <TD>6dFGS Galaxy Survey Final Redshift Release Catalog</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b| &gt; 10 degrees). Its 136,304 spectra have yielded 110,256 new extragalactic redshifts and a new catalogue of 125,071 galaxies making near-complete samples with limits in (K, H, J, r&lt;sub&gt;F&lt;/sub&gt;, b&lt;sub&gt;J&lt;/sub&gt;) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (radial velocity quality flag Q =3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all). It supersedes the previous DR2 version (CDS Cat. VII/249). The home page of of the 6dFGS database is &lt;a href="http://www-wfau.roe.ac.uk/6dFGS"&gt;http://www-wfau.roe.ac.uk/6dFGS&lt;/a&gt;. Any use of these data should explicitly state that they come from the Final Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS, 399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004, MNRAS, 355, 747).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/sixdfgs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sixdfgs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sixdfgs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sixdfgs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SIXDFGS [2]</TD>
            <TD>6dFGS Galaxy Survey Final Redshift Release Catalog</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b| &gt; 10 degrees). Its 136,304 spectra have yielded 110,256 new extragalactic redshifts and a new catalogue of 125,071 galaxies making near-complete samples with limits in (K, H, J, r&lt;sub&gt;F&lt;/sub&gt;, b&lt;sub&gt;J&lt;/sub&gt;) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (radial velocity quality flag Q =3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all). It supersedes the previous DR2 version (CDS Cat. VII/249). The home page of of the 6dFGS database is &lt;a href="http://www-wfau.roe.ac.uk/6dFGS"&gt;http://www-wfau.roe.ac.uk/6dFGS&lt;/a&gt;. Any use of these data should explicitly state that they come from the Final Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS, 399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004, MNRAS, 355, 747).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/sixdfgs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sixdfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sixdfgs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sixdfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SIXDFGS [3]</TD>
            <TD>6dFGS Galaxy Survey Final Redshift Release Catalog</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b| &gt; 10 degrees). Its 136,304 spectra have yielded 110,256 new extragalactic redshifts and a new catalogue of 125,071 galaxies making near-complete samples with limits in (K, H, J, r&lt;sub&gt;F&lt;/sub&gt;, b&lt;sub&gt;J&lt;/sub&gt;) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (radial velocity quality flag Q =3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124,647 entries in all). It supersedes the previous DR2 version (CDS Cat. VII/249). The home page of of the 6dFGS database is &lt;a href="http://www-wfau.roe.ac.uk/6dFGS"&gt;http://www-wfau.roe.ac.uk/6dFGS&lt;/a&gt;. Any use of these data should explicitly state that they come from the Final Release of 6dFGS and cite both the 6dGS DR3 paper (Jones et al. 2009, MNRAS, 399, 683) as well as the original 6dFGS survey paper (Jones et al. 2004, MNRAS, 355, 747).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/sixdfgs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sixdfgs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sixdfgs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sixdfgs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/126/1 [1]</TD>
            <TD>Abell clusters photometry (Quintana+, 2000)</TD>
            <TD>We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, III, and II. We have performed total photometry in the Gunn r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1#1</TD>
            <TD>2012-11-13T07:19:44Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/126/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/126/1 [2]</TD>
            <TD>Abell clusters photometry (Quintana+, 2000)</TD>
            <TD>We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, III, and II. We have performed total photometry in the Gunn r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1#2</TD>
            <TD>2012-11-13T07:19:44Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/126/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/126/1 [table6]</TD>
            <TD>Abell clusters photometry (Quintana+, 2000)</TD>
            <TD>We present CCD photometry of 209 southern Abell clusters selected according to Bautz-Morgan type I, III, and II. We have performed total photometry in the Gunn r bandpass, classified stars and galaxies, and obtained structural parameters for the images. To estimate the photometric and structural errors on the CCD images and the completeness limits of our photometry, we performed realistic simulations of stars and galaxies and ran our classification algorithms. Here, we present central galaxy counts and metric photometry of the brightest cluster members, for which we give accurate positions, and compare this photometry with values in the literature. A linear magnitude-redshift relation has been derived from the tenth-ranked galaxy in each cluster. Photometric redshifts have been estimated for 57 clusters. We provide either spectroscopic or photometric redshifts for all the clusters in our sample. Further analysis of these data will be presented in further publications.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1#table6</TD>
            <TD>2012-11-13T07:19:44Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/126/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/126/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/126/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROSATNEPID [1]</TD>
            <TD>ROSAT North Ecliptic Pole Survey Optical Identifications</TD>
            <TD>This table contains the ROSAT North Ecliptic Pole (NEP) Survey list of optical identifications. The X-ray data around the NEP from the ROSAT All-Sky Survey (RASS) were used to construct a contiguous area survey which consisted of a sample of 445 individual X-ray sources with fluxes more than ~2x10^-14 erg/cm^2/s in the 0.5 - 2.0 keV energy band. The NEP survey is centered at RA= 18hr 00min Dec= +66deg 33', and covers a region of 80.7 square degrees at a moderate Galactic latitude b= 29.8 degrees. Hence, the NEP survey is as deep as and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. The authors identified 99.6% of the sources and determined redshifts for the extragalactic objects. This table contains the optical identifications for the NEP catalog of X-ray sources, including basic X-ray data and properties of the sources. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGN) (~49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (~34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. The data on AGN in this catalog are essentially superceded by the data in the more recent catalog of Mullis et al. (2004, ApJ, 617, 192), available in HEASARC Browse as the ROSNEPOID table (q.v.), in which, inter alia, a corrected count rate to flux conversion and a different cosmology were used.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rosnepoid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rosnepoid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rosnepoid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rosnepoid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROSATNEPID [2]</TD>
            <TD>ROSAT North Ecliptic Pole Survey Optical Identifications</TD>
            <TD>This table contains the ROSAT North Ecliptic Pole (NEP) Survey list of optical identifications. The X-ray data around the NEP from the ROSAT All-Sky Survey (RASS) were used to construct a contiguous area survey which consisted of a sample of 445 individual X-ray sources with fluxes more than ~2x10^-14 erg/cm^2/s in the 0.5 - 2.0 keV energy band. The NEP survey is centered at RA= 18hr 00min Dec= +66deg 33', and covers a region of 80.7 square degrees at a moderate Galactic latitude b= 29.8 degrees. Hence, the NEP survey is as deep as and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. The authors identified 99.6% of the sources and determined redshifts for the extragalactic objects. This table contains the optical identifications for the NEP catalog of X-ray sources, including basic X-ray data and properties of the sources. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGN) (~49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (~34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. The data on AGN in this catalog are essentially superceded by the data in the more recent catalog of Mullis et al. (2004, ApJ, 617, 192), available in HEASARC Browse as the ROSNEPOID table (q.v.), in which, inter alia, a corrected count rate to flux conversion and a different cosmology were used.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rosnepoid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rosnepoid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rosnepoid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rosnepoid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROSATNEPID [3]</TD>
            <TD>ROSAT North Ecliptic Pole Survey Optical Identifications</TD>
            <TD>This table contains the ROSAT North Ecliptic Pole (NEP) Survey list of optical identifications. The X-ray data around the NEP from the ROSAT All-Sky Survey (RASS) were used to construct a contiguous area survey which consisted of a sample of 445 individual X-ray sources with fluxes more than ~2x10^-14 erg/cm^2/s in the 0.5 - 2.0 keV energy band. The NEP survey is centered at RA= 18hr 00min Dec= +66deg 33', and covers a region of 80.7 square degrees at a moderate Galactic latitude b= 29.8 degrees. Hence, the NEP survey is as deep as and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. The authors identified 99.6% of the sources and determined redshifts for the extragalactic objects. This table contains the optical identifications for the NEP catalog of X-ray sources, including basic X-ray data and properties of the sources. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGN) (~49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (~34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. The data on AGN in this catalog are essentially superceded by the data in the more recent catalog of Mullis et al. (2004, ApJ, 617, 192), available in HEASARC Browse as the ROSNEPOID table (q.v.), in which, inter alia, a corrected count rate to flux conversion and a different cosmology were used.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rosnepoid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rosnepoid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rosnepoid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rosnepoid.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ACTEGSRCAT [1]</TD>
            <TD>Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog</TD>
            <TD>This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (&gt;50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha&lt;sub&gt;5-20&lt;/sub&gt; = -0.07 +/- 0.06, alpha&lt;sub&gt;20-148&lt;/sub&gt; = -0.39 +/- 0.04, and alpha&lt;sub&gt;5-148&lt;/sub&gt; = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C&lt;sub&gt;Sync&lt;/sub&gt; = (2.8 +/- 0.3) x 10&lt;sup&gt;-6&lt;/sup&gt; microKelvin&lt;sup&gt;2&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/actegsrcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/actegsrcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=actegsrcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/actegsrcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ACTEGSRCAT [2]</TD>
            <TD>Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog</TD>
            <TD>This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (&gt;50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha&lt;sub&gt;5-20&lt;/sub&gt; = -0.07 +/- 0.06, alpha&lt;sub&gt;20-148&lt;/sub&gt; = -0.39 +/- 0.04, and alpha&lt;sub&gt;5-148&lt;/sub&gt; = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C&lt;sub&gt;Sync&lt;/sub&gt; = (2.8 +/- 0.3) x 10&lt;sup&gt;-6&lt;/sup&gt; microKelvin&lt;sup&gt;2&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/actegsrcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/actegsrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=actegsrcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/actegsrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ACTEGSRCAT [3]</TD>
            <TD>Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog</TD>
            <TD>This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (&gt;50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha&lt;sub&gt;5-20&lt;/sub&gt; = -0.07 +/- 0.06, alpha&lt;sub&gt;20-148&lt;/sub&gt; = -0.39 +/- 0.04, and alpha&lt;sub&gt;5-148&lt;/sub&gt; = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C&lt;sub&gt;Sync&lt;/sub&gt; = (2.8 +/- 0.3) x 10&lt;sup&gt;-6&lt;/sup&gt; microKelvin&lt;sup&gt;2&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/actegsrcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/actegsrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_actegsrcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/actegsrcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROSATNEPID [1]</TD>
            <TD>ROSAT North Ecliptic Pole Survey Optical Identifications</TD>
            <TD>This table contains the ROSAT North Ecliptic Pole (NEP) Survey list of optical identifications. The X-ray data around the NEP from the ROSAT All-Sky Survey (RASS) were used to construct a contiguous area survey which consisted of a sample of 445 individual X-ray sources with fluxes more than ~2x10^-14 erg/cm^2/s in the 0.5 - 2.0 keV energy band. The NEP survey is centered at RA= 18hr 00min Dec= +66deg 33', and covers a region of 80.7 square degrees at a moderate Galactic latitude b= 29.8 degrees. Hence, the NEP survey is as deep as and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. The authors identified 99.6% of the sources and determined redshifts for the extragalactic objects. This table contains the optical identifications for the NEP catalog of X-ray sources, including basic X-ray data and properties of the sources. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGN) (~49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (~34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. The data on AGN in this catalog are essentially superceded by the data in the more recent catalog of Mullis et al. (2004, ApJ, 617, 192), available in HEASARC Browse as the ROSNEPOID table (q.v.), in which, inter alia, a corrected count rate to flux conversion and a different cosmology were used.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rosnepoid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rosnepoid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rosnepoid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rosnepoid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROSATNEPID [2]</TD>
            <TD>ROSAT North Ecliptic Pole Survey Optical Identifications</TD>
            <TD>This table contains the ROSAT North Ecliptic Pole (NEP) Survey list of optical identifications. The X-ray data around the NEP from the ROSAT All-Sky Survey (RASS) were used to construct a contiguous area survey which consisted of a sample of 445 individual X-ray sources with fluxes more than ~2x10^-14 erg/cm^2/s in the 0.5 - 2.0 keV energy band. The NEP survey is centered at RA= 18hr 00min Dec= +66deg 33', and covers a region of 80.7 square degrees at a moderate Galactic latitude b= 29.8 degrees. Hence, the NEP survey is as deep as and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. The authors identified 99.6% of the sources and determined redshifts for the extragalactic objects. This table contains the optical identifications for the NEP catalog of X-ray sources, including basic X-ray data and properties of the sources. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGN) (~49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (~34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. The data on AGN in this catalog are essentially superceded by the data in the more recent catalog of Mullis et al. (2004, ApJ, 617, 192), available in HEASARC Browse as the ROSNEPOID table (q.v.), in which, inter alia, a corrected count rate to flux conversion and a different cosmology were used.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rosnepoid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rosnepoid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rosnepoid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rosnepoid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROSATNEPID [3]</TD>
            <TD>ROSAT North Ecliptic Pole Survey Optical Identifications</TD>
            <TD>This table contains the ROSAT North Ecliptic Pole (NEP) Survey list of optical identifications. The X-ray data around the NEP from the ROSAT All-Sky Survey (RASS) were used to construct a contiguous area survey which consisted of a sample of 445 individual X-ray sources with fluxes more than ~2x10^-14 erg/cm^2/s in the 0.5 - 2.0 keV energy band. The NEP survey is centered at RA= 18hr 00min Dec= +66deg 33', and covers a region of 80.7 square degrees at a moderate Galactic latitude b= 29.8 degrees. Hence, the NEP survey is as deep as and covers a comparable solid angle to the ROSAT serendipitous surveys but is also contiguous. The authors identified 99.6% of the sources and determined redshifts for the extragalactic objects. This table contains the optical identifications for the NEP catalog of X-ray sources, including basic X-ray data and properties of the sources. The classification of the optical counterparts to the NEP sources is very similar to that of previous surveys, in particular the Einstein Extended Medium Sensitivity Survey (EMSS). The main constituents of the catalog are active galactic nuclei (AGN) (~49%), either type 1 or type 2 according to the broadness of their permitted emission lines. Stellar counterparts are the second most common identification class (~34%). Clusters and groups of galaxies comprise 14%, and BL Lacertae objects 2%. One non-AGN galaxy and one planetary nebula have also been found. The NEP catalog of X-ray sources is a homogeneous sample of astronomical objects featuring complete optical identification. The data on AGN in this catalog are essentially superceded by the data in the more recent catalog of Mullis et al. (2004, ApJ, 617, 192), available in HEASARC Browse as the ROSNEPOID table (q.v.), in which, inter alia, a corrected count rate to flux conversion and a different cosmology were used.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rosnepoid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Optical Counterpart#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rosnepoid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rosnepoid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rosnepoid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/1 [1]</TD>
            <TD>Radio continuum spectra in Virgo cluster region (Vollmer+, 2004)</TD>
            <TD>We extend the galaxy sample of Niklas et al. (1995A&amp;A...293...56N) by adding observations at 8.6GHz and enlarging the sample to 81 galaxies, which were observed at 10.55, 8.6, 4.85GHz with the Effelsberg 100-m telescope in December 2000, January 2001, and in August September November 2002. Our data is complemented by 1.4GHz flux densities from the NVSS where advantage is taken of the NVSS images to check for source confusion and to estimate the correct source flux. In addition 0.6GHz and FIR (IRAS)data are given. The 1.4 and 0.6GHz and FIR data are taken from the Goldmine database, which is operated by the University of Milano-Bicocca (Gavazzi et al., 2003A&amp;A...400..451G). Radio spectra are derived for galaxies, for which detections at at least 3 different frequencies are available. The spectral index is given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1#1</TD>
            <TD>2012-11-13T13:42:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/1 [2]</TD>
            <TD>Radio continuum spectra in Virgo cluster region (Vollmer+, 2004)</TD>
            <TD>We extend the galaxy sample of Niklas et al. (1995A&amp;A...293...56N) by adding observations at 8.6GHz and enlarging the sample to 81 galaxies, which were observed at 10.55, 8.6, 4.85GHz with the Effelsberg 100-m telescope in December 2000, January 2001, and in August September November 2002. Our data is complemented by 1.4GHz flux densities from the NVSS where advantage is taken of the NVSS images to check for source confusion and to estimate the correct source flux. In addition 0.6GHz and FIR (IRAS)data are given. The 1.4 and 0.6GHz and FIR data are taken from the Goldmine database, which is operated by the University of Milano-Bicocca (Gavazzi et al., 2003A&amp;A...400..451G). Radio spectra are derived for galaxies, for which detections at at least 3 different frequencies are available. The spectral index is given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1#2</TD>
            <TD>2012-11-13T13:42:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/418/1 [table3]</TD>
            <TD>Radio continuum spectra in Virgo cluster region (Vollmer+, 2004)</TD>
            <TD>We extend the galaxy sample of Niklas et al. (1995A&amp;A...293...56N) by adding observations at 8.6GHz and enlarging the sample to 81 galaxies, which were observed at 10.55, 8.6, 4.85GHz with the Effelsberg 100-m telescope in December 2000, January 2001, and in August September November 2002. Our data is complemented by 1.4GHz flux densities from the NVSS where advantage is taken of the NVSS images to check for source confusion and to estimate the correct source flux. In addition 0.6GHz and FIR (IRAS)data are given. The 1.4 and 0.6GHz and FIR data are taken from the Goldmine database, which is operated by the University of Milano-Bicocca (Gavazzi et al., 2003A&amp;A...400..451G). Radio spectra are derived for galaxies, for which detections at at least 3 different frequencies are available. The spectral index is given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1#table3</TD>
            <TD>2012-11-13T13:42:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/418/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROSAT/WARPS [1]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)</TD>
            <TD>The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=warps&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROSAT/WARPS [2]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)</TD>
            <TD>The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=warps&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROSAT/WARPS [3]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)</TD>
            <TD>The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_warps&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ACTEGSRCAT [1]</TD>
            <TD>Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog</TD>
            <TD>This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (&gt;50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha&lt;sub&gt;5-20&lt;/sub&gt; = -0.07 +/- 0.06, alpha&lt;sub&gt;20-148&lt;/sub&gt; = -0.39 +/- 0.04, and alpha&lt;sub&gt;5-148&lt;/sub&gt; = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C&lt;sub&gt;Sync&lt;/sub&gt; = (2.8 +/- 0.3) x 10&lt;sup&gt;-6&lt;/sup&gt; microKelvin&lt;sup&gt;2&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/actegsrcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/actegsrcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=actegsrcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/actegsrcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ACTEGSRCAT [2]</TD>
            <TD>Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog</TD>
            <TD>This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (&gt;50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha&lt;sub&gt;5-20&lt;/sub&gt; = -0.07 +/- 0.06, alpha&lt;sub&gt;20-148&lt;/sub&gt; = -0.39 +/- 0.04, and alpha&lt;sub&gt;5-148&lt;/sub&gt; = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C&lt;sub&gt;Sync&lt;/sub&gt; = (2.8 +/- 0.3) x 10&lt;sup&gt;-6&lt;/sup&gt; microKelvin&lt;sup&gt;2&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/actegsrcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/actegsrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=actegsrcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/actegsrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ACTEGSRCAT [3]</TD>
            <TD>Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog</TD>
            <TD>This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (&gt;50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha&lt;sub&gt;5-20&lt;/sub&gt; = -0.07 +/- 0.06, alpha&lt;sub&gt;20-148&lt;/sub&gt; = -0.39 +/- 0.04, and alpha&lt;sub&gt;5-148&lt;/sub&gt; = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C&lt;sub&gt;Sync&lt;/sub&gt; = (2.8 +/- 0.3) x 10&lt;sup&gt;-6&lt;/sup&gt; microKelvin&lt;sup&gt;2&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/actegsrcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/actegsrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_actegsrcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/actegsrcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROSAT/WARPS [1]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)</TD>
            <TD>The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=warps&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROSAT/WARPS [2]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)</TD>
            <TD>The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=warps&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROSAT/WARPS [3]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)</TD>
            <TD>The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_warps&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/1 [1]</TD>
            <TD>Radio continuum spectra in Virgo cluster region (Vollmer+, 2004)</TD>
            <TD>We extend the galaxy sample of Niklas et al. (1995A&amp;A...293...56N) by adding observations at 8.6GHz and enlarging the sample to 81 galaxies, which were observed at 10.55, 8.6, 4.85GHz with the Effelsberg 100-m telescope in December 2000, January 2001, and in August September November 2002. Our data is complemented by 1.4GHz flux densities from the NVSS where advantage is taken of the NVSS images to check for source confusion and to estimate the correct source flux. In addition 0.6GHz and FIR (IRAS)data are given. The 1.4 and 0.6GHz and FIR data are taken from the Goldmine database, which is operated by the University of Milano-Bicocca (Gavazzi et al., 2003A&amp;A...400..451G). Radio spectra are derived for galaxies, for which detections at at least 3 different frequencies are available. The spectral index is given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1#1</TD>
            <TD>2012-11-13T13:42:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/1 [2]</TD>
            <TD>Radio continuum spectra in Virgo cluster region (Vollmer+, 2004)</TD>
            <TD>We extend the galaxy sample of Niklas et al. (1995A&amp;A...293...56N) by adding observations at 8.6GHz and enlarging the sample to 81 galaxies, which were observed at 10.55, 8.6, 4.85GHz with the Effelsberg 100-m telescope in December 2000, January 2001, and in August September November 2002. Our data is complemented by 1.4GHz flux densities from the NVSS where advantage is taken of the NVSS images to check for source confusion and to estimate the correct source flux. In addition 0.6GHz and FIR (IRAS)data are given. The 1.4 and 0.6GHz and FIR data are taken from the Goldmine database, which is operated by the University of Milano-Bicocca (Gavazzi et al., 2003A&amp;A...400..451G). Radio spectra are derived for galaxies, for which detections at at least 3 different frequencies are available. The spectral index is given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1#2</TD>
            <TD>2012-11-13T13:42:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/418/1 [table3]</TD>
            <TD>Radio continuum spectra in Virgo cluster region (Vollmer+, 2004)</TD>
            <TD>We extend the galaxy sample of Niklas et al. (1995A&amp;A...293...56N) by adding observations at 8.6GHz and enlarging the sample to 81 galaxies, which were observed at 10.55, 8.6, 4.85GHz with the Effelsberg 100-m telescope in December 2000, January 2001, and in August September November 2002. Our data is complemented by 1.4GHz flux densities from the NVSS where advantage is taken of the NVSS images to check for source confusion and to estimate the correct source flux. In addition 0.6GHz and FIR (IRAS)data are given. The 1.4 and 0.6GHz and FIR data are taken from the Goldmine database, which is operated by the University of Milano-Bicocca (Gavazzi et al., 2003A&amp;A...400..451G). Radio spectra are derived for galaxies, for which detections at at least 3 different frequencies are available. The spectral index is given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1#table3</TD>
            <TD>2012-11-13T13:42:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/418/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ACTEGSRCAT [1]</TD>
            <TD>Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog</TD>
            <TD>This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (&gt;50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha&lt;sub&gt;5-20&lt;/sub&gt; = -0.07 +/- 0.06, alpha&lt;sub&gt;20-148&lt;/sub&gt; = -0.39 +/- 0.04, and alpha&lt;sub&gt;5-148&lt;/sub&gt; = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C&lt;sub&gt;Sync&lt;/sub&gt; = (2.8 +/- 0.3) x 10&lt;sup&gt;-6&lt;/sup&gt; microKelvin&lt;sup&gt;2&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/actegsrcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/actegsrcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=actegsrcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/actegsrcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ACTEGSRCAT [2]</TD>
            <TD>Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog</TD>
            <TD>This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (&gt;50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha&lt;sub&gt;5-20&lt;/sub&gt; = -0.07 +/- 0.06, alpha&lt;sub&gt;20-148&lt;/sub&gt; = -0.39 +/- 0.04, and alpha&lt;sub&gt;5-148&lt;/sub&gt; = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C&lt;sub&gt;Sync&lt;/sub&gt; = (2.8 +/- 0.3) x 10&lt;sup&gt;-6&lt;/sup&gt; microKelvin&lt;sup&gt;2&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/actegsrcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/actegsrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=actegsrcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/actegsrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ACTEGSRCAT [3]</TD>
            <TD>Atacama Cosmology Telescope 2008 Survey 148-GHz Extragalactic Source Catalog</TD>
            <TD>This table contains a list of extragalactic radio sources detected in a 455 square-degree map of the southern sky made at a frequency of 148 GHz from the Atacama Cosmology Telescope (ACT) 2008 observing season. This catalog has 157 sources with flux densities spanning two orders of magnitude from 15 to 1500 mJy. Comparison to other catalogs shows that 98% of the ACT detections correspond to sources detected at lower radio frequencies. Three of the sources appear to be associated with the brightest cluster galaxies of low redshift X-ray selected galaxy clusters. Estimates of the radio to mm-wave spectral indices and differential counts of the sources further bolster the hypothesis that they are nearly all radio sources, and that their emission is not dominated by re-emission from warm dust. In a bright (&gt;50 mJy) 148 GHz-selected sample with complete cross-identifications from the Australia Telescope 20-GHz survey, the authors of the study observe an average steepening of the spectra between 5, 20, and 148 GHz with median spectral indices of alpha&lt;sub&gt;5-20&lt;/sub&gt; = -0.07 +/- 0.06, alpha&lt;sub&gt;20-148&lt;/sub&gt; = -0.39 +/- 0.04, and alpha&lt;sub&gt;5-148&lt;/sub&gt; = -0.20 +/- 0.03. When the measured spectral indices are taken into account, the 148-GHz differential source counts are consistent with previous measurements at 30 GHz in the context of a source count model dominated by flat spectrum radio sources. Extrapolating with an appropriately rescaled model for the radio source counts, the Poisson contribution to the spatial power spectrum from synchrotron-dominated sources with flux density less than 20 mJy is C&lt;sub&gt;Sync&lt;/sub&gt; = (2.8 +/- 0.3) x 10&lt;sup&gt;-6&lt;/sup&gt; microKelvin&lt;sup&gt;2&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/actegsrcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/actegsrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_actegsrcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/actegsrcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROSAT/WARPS [1]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)</TD>
            <TD>The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=warps&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROSAT/WARPS [2]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)</TD>
            <TD>The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=warps&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROSAT/WARPS [3]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I)</TD>
            <TD>The Wide Angle ROSAT Pointed Survey, First Phase (WARPS-I) table is a catalog which contains optical identifications for objects found in a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and to extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. The X-ray source screening and optical identification process for WARPS-I yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5-2.0keV) = 6.5x10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_warps&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/1 [1]</TD>
            <TD>Radio continuum spectra in Virgo cluster region (Vollmer+, 2004)</TD>
            <TD>We extend the galaxy sample of Niklas et al. (1995A&amp;A...293...56N) by adding observations at 8.6GHz and enlarging the sample to 81 galaxies, which were observed at 10.55, 8.6, 4.85GHz with the Effelsberg 100-m telescope in December 2000, January 2001, and in August September November 2002. Our data is complemented by 1.4GHz flux densities from the NVSS where advantage is taken of the NVSS images to check for source confusion and to estimate the correct source flux. In addition 0.6GHz and FIR (IRAS)data are given. The 1.4 and 0.6GHz and FIR data are taken from the Goldmine database, which is operated by the University of Milano-Bicocca (Gavazzi et al., 2003A&amp;A...400..451G). Radio spectra are derived for galaxies, for which detections at at least 3 different frequencies are available. The spectral index is given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1#1</TD>
            <TD>2012-11-13T13:42:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/1 [2]</TD>
            <TD>Radio continuum spectra in Virgo cluster region (Vollmer+, 2004)</TD>
            <TD>We extend the galaxy sample of Niklas et al. (1995A&amp;A...293...56N) by adding observations at 8.6GHz and enlarging the sample to 81 galaxies, which were observed at 10.55, 8.6, 4.85GHz with the Effelsberg 100-m telescope in December 2000, January 2001, and in August September November 2002. Our data is complemented by 1.4GHz flux densities from the NVSS where advantage is taken of the NVSS images to check for source confusion and to estimate the correct source flux. In addition 0.6GHz and FIR (IRAS)data are given. The 1.4 and 0.6GHz and FIR data are taken from the Goldmine database, which is operated by the University of Milano-Bicocca (Gavazzi et al., 2003A&amp;A...400..451G). Radio spectra are derived for galaxies, for which detections at at least 3 different frequencies are available. The spectral index is given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1#2</TD>
            <TD>2012-11-13T13:42:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/418/1 [table3]</TD>
            <TD>Radio continuum spectra in Virgo cluster region (Vollmer+, 2004)</TD>
            <TD>We extend the galaxy sample of Niklas et al. (1995A&amp;A...293...56N) by adding observations at 8.6GHz and enlarging the sample to 81 galaxies, which were observed at 10.55, 8.6, 4.85GHz with the Effelsberg 100-m telescope in December 2000, January 2001, and in August September November 2002. Our data is complemented by 1.4GHz flux densities from the NVSS where advantage is taken of the NVSS images to check for source confusion and to estimate the correct source flux. In addition 0.6GHz and FIR (IRAS)data are given. The 1.4 and 0.6GHz and FIR data are taken from the Goldmine database, which is operated by the University of Milano-Bicocca (Gavazzi et al., 2003A&amp;A...400..451G). Radio spectra are derived for galaxies, for which detections at at least 3 different frequencies are available. The spectral index is given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1#table3</TD>
            <TD>2012-11-13T13:42:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/418/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHANDFS4MS [1]</TD>
            <TD>Chandra Deep Field South 4-Megasecond Catalog</TD>
            <TD>This table contains the main Chandra source catalog for the 4 megasecond (Ms) Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin&lt;sup&gt;2&lt;/sup&gt;. It contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt; in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P &lt; 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog (the HEASARC CHANDFS2MS table) sources. The authors determined X-ray source positions using centroid and matched-filter techniques and obtained a median positional uncertainty of ~0.42 arcseconds. In their paper, they also provided a supplementary catalog (not included in this HEASARC table), which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt;, satisfy the condition of 0.004 &lt; P &lt; 0.1, and have an optical counterpart with R &lt; 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (~97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (~94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that &gt;75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3'), the observed AGN and galaxy source densities have reached 9800 (+1300,-1100) deg&lt;sup&gt;-2&lt;/sup&gt; and 6900 (+1100,-900) deg&lt;sup&gt;-2&lt;/sup&gt;, respectively. Simulations show that the main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms&lt;sup&gt;-1&lt;/sup&gt; pixel&lt;sup&gt;-1&lt;/sup&gt; (for a pixel size of 0.492 arcseconds) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ~3.2 x 10&lt;sup&gt;-17&lt;/sup&gt;, 9.1 x 10&lt;sup&gt;-18&lt;/sup&gt;, and 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ~2-2.5 would provide further significant gains and probe key unexplored discovery space. This HEASARC table comprises Table 3 from the reference paper, the Main Chandra Source Catalog of 740 X-ray sources. The 36 optically bright Chandra sources that were listed in Table 6 of the reference paper are thus not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chandfs4ms#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chandfs4ms</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chandfs4ms&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chandfs4ms.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHANDFS4MS [2]</TD>
            <TD>Chandra Deep Field South 4-Megasecond Catalog</TD>
            <TD>This table contains the main Chandra source catalog for the 4 megasecond (Ms) Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin&lt;sup&gt;2&lt;/sup&gt;. It contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt; in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P &lt; 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog (the HEASARC CHANDFS2MS table) sources. The authors determined X-ray source positions using centroid and matched-filter techniques and obtained a median positional uncertainty of ~0.42 arcseconds. In their paper, they also provided a supplementary catalog (not included in this HEASARC table), which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt;, satisfy the condition of 0.004 &lt; P &lt; 0.1, and have an optical counterpart with R &lt; 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (~97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (~94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that &gt;75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3'), the observed AGN and galaxy source densities have reached 9800 (+1300,-1100) deg&lt;sup&gt;-2&lt;/sup&gt; and 6900 (+1100,-900) deg&lt;sup&gt;-2&lt;/sup&gt;, respectively. Simulations show that the main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms&lt;sup&gt;-1&lt;/sup&gt; pixel&lt;sup&gt;-1&lt;/sup&gt; (for a pixel size of 0.492 arcseconds) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ~3.2 x 10&lt;sup&gt;-17&lt;/sup&gt;, 9.1 x 10&lt;sup&gt;-18&lt;/sup&gt;, and 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ~2-2.5 would provide further significant gains and probe key unexplored discovery space. This HEASARC table comprises Table 3 from the reference paper, the Main Chandra Source Catalog of 740 X-ray sources. The 36 optically bright Chandra sources that were listed in Table 6 of the reference paper are thus not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chandfs4ms#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chandfs4ms</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chandfs4ms&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chandfs4ms.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHANDFS4MS [3]</TD>
            <TD>Chandra Deep Field South 4-Megasecond Catalog</TD>
            <TD>This table contains the main Chandra source catalog for the 4 megasecond (Ms) Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin&lt;sup&gt;2&lt;/sup&gt;. It contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt; in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P &lt; 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog (the HEASARC CHANDFS2MS table) sources. The authors determined X-ray source positions using centroid and matched-filter techniques and obtained a median positional uncertainty of ~0.42 arcseconds. In their paper, they also provided a supplementary catalog (not included in this HEASARC table), which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt;, satisfy the condition of 0.004 &lt; P &lt; 0.1, and have an optical counterpart with R &lt; 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (~97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (~94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that &gt;75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3'), the observed AGN and galaxy source densities have reached 9800 (+1300,-1100) deg&lt;sup&gt;-2&lt;/sup&gt; and 6900 (+1100,-900) deg&lt;sup&gt;-2&lt;/sup&gt;, respectively. Simulations show that the main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms&lt;sup&gt;-1&lt;/sup&gt; pixel&lt;sup&gt;-1&lt;/sup&gt; (for a pixel size of 0.492 arcseconds) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ~3.2 x 10&lt;sup&gt;-17&lt;/sup&gt;, 9.1 x 10&lt;sup&gt;-18&lt;/sup&gt;, and 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ~2-2.5 would provide further significant gains and probe key unexplored discovery space. This HEASARC table comprises Table 3 from the reference paper, the Main Chandra Source Catalog of 740 X-ray sources. The 36 optically bright Chandra sources that were listed in Table 6 of the reference paper are thus not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chandfs4ms#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chandfs4ms</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chandfs4ms&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chandfs4ms.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHNGPSCLIU [1]</TD>
            <TD>Chandra ACIS Survey of Nearby Galaxies X-Ray Point Source Catalog</TD>
            <TD>The Chandra data archive is a treasure trove for various studies, and in this study the author exploits this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axes above 1 arcminute had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures were applied to the 626 ACIS observations and led to the detection of 28,099 point sources, which belong to 17,559 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8,519 sources within the D&lt;sub&gt;25&lt;/sub&gt; isophotes of 351 galaxies, 3,305 sources between the D&lt;sub&gt;25&lt;/sub&gt; and 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 309 galaxies, and an additional 5,735 sources outside the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of the sources within the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes above 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 71% of the sources above 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 63% of the sources above 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, and 56% of all sources are truly associated with the galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L&lt;sub&gt;X&lt;/sub&gt; in the 0.3-8 keV band &gt;= 2 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; within the D&lt;sub&gt;25&lt;/sub&gt; isophotes, 179 ULXs between the D&lt;sub&gt;25&lt;/sub&gt; and the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with the host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L&lt;sub&gt;X&lt;/sub&gt; (0.3-8 keV) &gt;= 2 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. This table contains the list of 17,559 'independent' X-ray point sources that was contained in table 4 of the reference paper. As the author notes in Section 5 of this paper, there are 341 sources projected within 2 galaxies with overlapping domains which are listed for both galaxies. The 5,735 sources lieing outside the 2* D&lt;sub&gt;25&lt;/sub&gt; isophotes of the galaxies are also included in this table. For these sources, the X-ray luminosities are computed as if they were in a galaxy of that group, which may or may not be the case; thus, they may not be their 'true' luminosities, but are listed for the purposes of comparison.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chngpscliu#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chngpscliu</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chngpscliu&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chngpscliu.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHNGPSCLIU [2]</TD>
            <TD>Chandra ACIS Survey of Nearby Galaxies X-Ray Point Source Catalog</TD>
            <TD>The Chandra data archive is a treasure trove for various studies, and in this study the author exploits this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axes above 1 arcminute had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures were applied to the 626 ACIS observations and led to the detection of 28,099 point sources, which belong to 17,559 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8,519 sources within the D&lt;sub&gt;25&lt;/sub&gt; isophotes of 351 galaxies, 3,305 sources between the D&lt;sub&gt;25&lt;/sub&gt; and 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 309 galaxies, and an additional 5,735 sources outside the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of the sources within the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes above 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 71% of the sources above 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 63% of the sources above 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, and 56% of all sources are truly associated with the galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L&lt;sub&gt;X&lt;/sub&gt; in the 0.3-8 keV band &gt;= 2 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; within the D&lt;sub&gt;25&lt;/sub&gt; isophotes, 179 ULXs between the D&lt;sub&gt;25&lt;/sub&gt; and the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with the host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L&lt;sub&gt;X&lt;/sub&gt; (0.3-8 keV) &gt;= 2 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. This table contains the list of 17,559 'independent' X-ray point sources that was contained in table 4 of the reference paper. As the author notes in Section 5 of this paper, there are 341 sources projected within 2 galaxies with overlapping domains which are listed for both galaxies. The 5,735 sources lieing outside the 2* D&lt;sub&gt;25&lt;/sub&gt; isophotes of the galaxies are also included in this table. For these sources, the X-ray luminosities are computed as if they were in a galaxy of that group, which may or may not be the case; thus, they may not be their 'true' luminosities, but are listed for the purposes of comparison.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chngpscliu#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chngpscliu</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chngpscliu&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chngpscliu.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHNGPSCLIU [3]</TD>
            <TD>Chandra ACIS Survey of Nearby Galaxies X-Ray Point Source Catalog</TD>
            <TD>The Chandra data archive is a treasure trove for various studies, and in this study the author exploits this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axes above 1 arcminute had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures were applied to the 626 ACIS observations and led to the detection of 28,099 point sources, which belong to 17,559 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8,519 sources within the D&lt;sub&gt;25&lt;/sub&gt; isophotes of 351 galaxies, 3,305 sources between the D&lt;sub&gt;25&lt;/sub&gt; and 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 309 galaxies, and an additional 5,735 sources outside the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of the sources within the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes above 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 71% of the sources above 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 63% of the sources above 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, and 56% of all sources are truly associated with the galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L&lt;sub&gt;X&lt;/sub&gt; in the 0.3-8 keV band &gt;= 2 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; within the D&lt;sub&gt;25&lt;/sub&gt; isophotes, 179 ULXs between the D&lt;sub&gt;25&lt;/sub&gt; and the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with the host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L&lt;sub&gt;X&lt;/sub&gt; (0.3-8 keV) &gt;= 2 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. This table contains the list of 17,559 'independent' X-ray point sources that was contained in table 4 of the reference paper. As the author notes in Section 5 of this paper, there are 341 sources projected within 2 galaxies with overlapping domains which are listed for both galaxies. The 5,735 sources lieing outside the 2* D&lt;sub&gt;25&lt;/sub&gt; isophotes of the galaxies are also included in this table. For these sources, the X-ray luminosities are computed as if they were in a galaxy of that group, which may or may not be the case; thus, they may not be their 'true' luminosities, but are listed for the purposes of comparison.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chngpscliu&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chngpscliu.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/99/1079 [1]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/99/1079 [2]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#2</TD>
            <TD>2012-11-13T13:59:09Z</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/99/1079 [table3]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#table3</TD>
            <TD>2012-11-13T13:59:09Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1079 [table2]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#table2</TD>
            <TD>2012-11-13T13:59:09Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>17-Jan-2005</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>CHANDFS4MS [1]</TD>
            <TD>Chandra Deep Field South 4-Megasecond Catalog</TD>
            <TD>This table contains the main Chandra source catalog for the 4 megasecond (Ms) Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin&lt;sup&gt;2&lt;/sup&gt;. It contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt; in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P &lt; 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog (the HEASARC CHANDFS2MS table) sources. The authors determined X-ray source positions using centroid and matched-filter techniques and obtained a median positional uncertainty of ~0.42 arcseconds. In their paper, they also provided a supplementary catalog (not included in this HEASARC table), which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt;, satisfy the condition of 0.004 &lt; P &lt; 0.1, and have an optical counterpart with R &lt; 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (~97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (~94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that &gt;75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3'), the observed AGN and galaxy source densities have reached 9800 (+1300,-1100) deg&lt;sup&gt;-2&lt;/sup&gt; and 6900 (+1100,-900) deg&lt;sup&gt;-2&lt;/sup&gt;, respectively. Simulations show that the main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms&lt;sup&gt;-1&lt;/sup&gt; pixel&lt;sup&gt;-1&lt;/sup&gt; (for a pixel size of 0.492 arcseconds) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ~3.2 x 10&lt;sup&gt;-17&lt;/sup&gt;, 9.1 x 10&lt;sup&gt;-18&lt;/sup&gt;, and 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ~2-2.5 would provide further significant gains and probe key unexplored discovery space. This HEASARC table comprises Table 3 from the reference paper, the Main Chandra Source Catalog of 740 X-ray sources. The 36 optically bright Chandra sources that were listed in Table 6 of the reference paper are thus not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chandfs4ms#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>CHANDFS4MS [2]</TD>
            <TD>Chandra Deep Field South 4-Megasecond Catalog</TD>
            <TD>This table contains the main Chandra source catalog for the 4 megasecond (Ms) Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin&lt;sup&gt;2&lt;/sup&gt;. It contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt; in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P &lt; 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog (the HEASARC CHANDFS2MS table) sources. The authors determined X-ray source positions using centroid and matched-filter techniques and obtained a median positional uncertainty of ~0.42 arcseconds. In their paper, they also provided a supplementary catalog (not included in this HEASARC table), which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt;, satisfy the condition of 0.004 &lt; P &lt; 0.1, and have an optical counterpart with R &lt; 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (~97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (~94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that &gt;75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3'), the observed AGN and galaxy source densities have reached 9800 (+1300,-1100) deg&lt;sup&gt;-2&lt;/sup&gt; and 6900 (+1100,-900) deg&lt;sup&gt;-2&lt;/sup&gt;, respectively. Simulations show that the main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms&lt;sup&gt;-1&lt;/sup&gt; pixel&lt;sup&gt;-1&lt;/sup&gt; (for a pixel size of 0.492 arcseconds) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ~3.2 x 10&lt;sup&gt;-17&lt;/sup&gt;, 9.1 x 10&lt;sup&gt;-18&lt;/sup&gt;, and 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ~2-2.5 would provide further significant gains and probe key unexplored discovery space. This HEASARC table comprises Table 3 from the reference paper, the Main Chandra Source Catalog of 740 X-ray sources. The 36 optically bright Chandra sources that were listed in Table 6 of the reference paper are thus not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>ivo://nasa.heasarc/chandfs4ms#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>CHANDFS4MS [3]</TD>
            <TD>Chandra Deep Field South 4-Megasecond Catalog</TD>
            <TD>This table contains the main Chandra source catalog for the 4 megasecond (Ms) Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin&lt;sup&gt;2&lt;/sup&gt;. It contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt; in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P &lt; 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog (the HEASARC CHANDFS2MS table) sources. The authors determined X-ray source positions using centroid and matched-filter techniques and obtained a median positional uncertainty of ~0.42 arcseconds. In their paper, they also provided a supplementary catalog (not included in this HEASARC table), which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt;, satisfy the condition of 0.004 &lt; P &lt; 0.1, and have an optical counterpart with R &lt; 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (~97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (~94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that &gt;75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3'), the observed AGN and galaxy source densities have reached 9800 (+1300,-1100) deg&lt;sup&gt;-2&lt;/sup&gt; and 6900 (+1100,-900) deg&lt;sup&gt;-2&lt;/sup&gt;, respectively. Simulations show that the main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms&lt;sup&gt;-1&lt;/sup&gt; pixel&lt;sup&gt;-1&lt;/sup&gt; (for a pixel size of 0.492 arcseconds) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ~3.2 x 10&lt;sup&gt;-17&lt;/sup&gt;, 9.1 x 10&lt;sup&gt;-18&lt;/sup&gt;, and 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ~2-2.5 would provide further significant gains and probe key unexplored discovery space. This HEASARC table comprises Table 3 from the reference paper, the Main Chandra Source Catalog of 740 X-ray sources. The 36 optically bright Chandra sources that were listed in Table 6 of the reference paper are thus not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chandfs4ms#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD />
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          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHNGPSCLIU [1]</TD>
            <TD>Chandra ACIS Survey of Nearby Galaxies X-Ray Point Source Catalog</TD>
            <TD>The Chandra data archive is a treasure trove for various studies, and in this study the author exploits this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axes above 1 arcminute had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures were applied to the 626 ACIS observations and led to the detection of 28,099 point sources, which belong to 17,559 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8,519 sources within the D&lt;sub&gt;25&lt;/sub&gt; isophotes of 351 galaxies, 3,305 sources between the D&lt;sub&gt;25&lt;/sub&gt; and 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 309 galaxies, and an additional 5,735 sources outside the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of the sources within the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes above 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 71% of the sources above 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 63% of the sources above 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, and 56% of all sources are truly associated with the galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L&lt;sub&gt;X&lt;/sub&gt; in the 0.3-8 keV band &gt;= 2 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; within the D&lt;sub&gt;25&lt;/sub&gt; isophotes, 179 ULXs between the D&lt;sub&gt;25&lt;/sub&gt; and the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with the host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L&lt;sub&gt;X&lt;/sub&gt; (0.3-8 keV) &gt;= 2 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. This table contains the list of 17,559 'independent' X-ray point sources that was contained in table 4 of the reference paper. As the author notes in Section 5 of this paper, there are 341 sources projected within 2 galaxies with overlapping domains which are listed for both galaxies. The 5,735 sources lieing outside the 2* D&lt;sub&gt;25&lt;/sub&gt; isophotes of the galaxies are also included in this table. For these sources, the X-ray luminosities are computed as if they were in a galaxy of that group, which may or may not be the case; thus, they may not be their 'true' luminosities, but are listed for the purposes of comparison.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chngpscliu#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chngpscliu</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chngpscliu&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chngpscliu.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHNGPSCLIU [2]</TD>
            <TD>Chandra ACIS Survey of Nearby Galaxies X-Ray Point Source Catalog</TD>
            <TD>The Chandra data archive is a treasure trove for various studies, and in this study the author exploits this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axes above 1 arcminute had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures were applied to the 626 ACIS observations and led to the detection of 28,099 point sources, which belong to 17,559 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8,519 sources within the D&lt;sub&gt;25&lt;/sub&gt; isophotes of 351 galaxies, 3,305 sources between the D&lt;sub&gt;25&lt;/sub&gt; and 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 309 galaxies, and an additional 5,735 sources outside the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of the sources within the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes above 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 71% of the sources above 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 63% of the sources above 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, and 56% of all sources are truly associated with the galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L&lt;sub&gt;X&lt;/sub&gt; in the 0.3-8 keV band &gt;= 2 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; within the D&lt;sub&gt;25&lt;/sub&gt; isophotes, 179 ULXs between the D&lt;sub&gt;25&lt;/sub&gt; and the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with the host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L&lt;sub&gt;X&lt;/sub&gt; (0.3-8 keV) &gt;= 2 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. This table contains the list of 17,559 'independent' X-ray point sources that was contained in table 4 of the reference paper. As the author notes in Section 5 of this paper, there are 341 sources projected within 2 galaxies with overlapping domains which are listed for both galaxies. The 5,735 sources lieing outside the 2* D&lt;sub&gt;25&lt;/sub&gt; isophotes of the galaxies are also included in this table. For these sources, the X-ray luminosities are computed as if they were in a galaxy of that group, which may or may not be the case; thus, they may not be their 'true' luminosities, but are listed for the purposes of comparison.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chngpscliu#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
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            <TD>ivo://nasa.heasarc/chngpscliu</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chngpscliu&amp;</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chngpscliu.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHNGPSCLIU [3]</TD>
            <TD>Chandra ACIS Survey of Nearby Galaxies X-Ray Point Source Catalog</TD>
            <TD>The Chandra data archive is a treasure trove for various studies, and in this study the author exploits this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axes above 1 arcminute had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures were applied to the 626 ACIS observations and led to the detection of 28,099 point sources, which belong to 17,559 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8,519 sources within the D&lt;sub&gt;25&lt;/sub&gt; isophotes of 351 galaxies, 3,305 sources between the D&lt;sub&gt;25&lt;/sub&gt; and 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 309 galaxies, and an additional 5,735 sources outside the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of the sources within the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes above 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 71% of the sources above 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 63% of the sources above 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, and 56% of all sources are truly associated with the galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L&lt;sub&gt;X&lt;/sub&gt; in the 0.3-8 keV band &gt;= 2 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; within the D&lt;sub&gt;25&lt;/sub&gt; isophotes, 179 ULXs between the D&lt;sub&gt;25&lt;/sub&gt; and the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with the host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L&lt;sub&gt;X&lt;/sub&gt; (0.3-8 keV) &gt;= 2 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. This table contains the list of 17,559 'independent' X-ray point sources that was contained in table 4 of the reference paper. As the author notes in Section 5 of this paper, there are 341 sources projected within 2 galaxies with overlapping domains which are listed for both galaxies. The 5,735 sources lieing outside the 2* D&lt;sub&gt;25&lt;/sub&gt; isophotes of the galaxies are also included in this table. For these sources, the X-ray luminosities are computed as if they were in a galaxy of that group, which may or may not be the case; thus, they may not be their 'true' luminosities, but are listed for the purposes of comparison.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
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            <TD>ivo://nasa.heasarc/chngpscliu</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chngpscliu&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chngpscliu.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/99/1079 [1]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#1</TD>
            <TD>2012-11-13T13:59:09Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/99/1079</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/99/1079 [2]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#2</TD>
            <TD>2012-11-13T13:59:09Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079</TD>
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            <TD>ParamHTTP</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1079 [table3]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#table3</TD>
            <TD>2012-11-13T13:59:09Z</TD>
            <TD>#Novae#</TD>
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            <TD>#Research#</TD>
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            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1079&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1079 [table2]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#table2</TD>
            <TD>2012-11-13T13:59:09Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1079&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>CHNGPSCLIU [1]</TD>
            <TD>Chandra ACIS Survey of Nearby Galaxies X-Ray Point Source Catalog</TD>
            <TD>The Chandra data archive is a treasure trove for various studies, and in this study the author exploits this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axes above 1 arcminute had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures were applied to the 626 ACIS observations and led to the detection of 28,099 point sources, which belong to 17,559 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8,519 sources within the D&lt;sub&gt;25&lt;/sub&gt; isophotes of 351 galaxies, 3,305 sources between the D&lt;sub&gt;25&lt;/sub&gt; and 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 309 galaxies, and an additional 5,735 sources outside the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of the sources within the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes above 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 71% of the sources above 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 63% of the sources above 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, and 56% of all sources are truly associated with the galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L&lt;sub&gt;X&lt;/sub&gt; in the 0.3-8 keV band &gt;= 2 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; within the D&lt;sub&gt;25&lt;/sub&gt; isophotes, 179 ULXs between the D&lt;sub&gt;25&lt;/sub&gt; and the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with the host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L&lt;sub&gt;X&lt;/sub&gt; (0.3-8 keV) &gt;= 2 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. This table contains the list of 17,559 'independent' X-ray point sources that was contained in table 4 of the reference paper. As the author notes in Section 5 of this paper, there are 341 sources projected within 2 galaxies with overlapping domains which are listed for both galaxies. The 5,735 sources lieing outside the 2* D&lt;sub&gt;25&lt;/sub&gt; isophotes of the galaxies are also included in this table. For these sources, the X-ray luminosities are computed as if they were in a galaxy of that group, which may or may not be the case; thus, they may not be their 'true' luminosities, but are listed for the purposes of comparison.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chngpscliu#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chngpscliu</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chngpscliu&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chngpscliu.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHNGPSCLIU [2]</TD>
            <TD>Chandra ACIS Survey of Nearby Galaxies X-Ray Point Source Catalog</TD>
            <TD>The Chandra data archive is a treasure trove for various studies, and in this study the author exploits this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axes above 1 arcminute had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures were applied to the 626 ACIS observations and led to the detection of 28,099 point sources, which belong to 17,559 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8,519 sources within the D&lt;sub&gt;25&lt;/sub&gt; isophotes of 351 galaxies, 3,305 sources between the D&lt;sub&gt;25&lt;/sub&gt; and 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 309 galaxies, and an additional 5,735 sources outside the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of the sources within the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes above 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 71% of the sources above 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 63% of the sources above 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, and 56% of all sources are truly associated with the galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L&lt;sub&gt;X&lt;/sub&gt; in the 0.3-8 keV band &gt;= 2 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; within the D&lt;sub&gt;25&lt;/sub&gt; isophotes, 179 ULXs between the D&lt;sub&gt;25&lt;/sub&gt; and the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with the host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L&lt;sub&gt;X&lt;/sub&gt; (0.3-8 keV) &gt;= 2 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. This table contains the list of 17,559 'independent' X-ray point sources that was contained in table 4 of the reference paper. As the author notes in Section 5 of this paper, there are 341 sources projected within 2 galaxies with overlapping domains which are listed for both galaxies. The 5,735 sources lieing outside the 2* D&lt;sub&gt;25&lt;/sub&gt; isophotes of the galaxies are also included in this table. For these sources, the X-ray luminosities are computed as if they were in a galaxy of that group, which may or may not be the case; thus, they may not be their 'true' luminosities, but are listed for the purposes of comparison.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chngpscliu#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chngpscliu</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chngpscliu&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chngpscliu.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHNGPSCLIU [3]</TD>
            <TD>Chandra ACIS Survey of Nearby Galaxies X-Ray Point Source Catalog</TD>
            <TD>The Chandra data archive is a treasure trove for various studies, and in this study the author exploits this valuable resource to study the X-ray point source populations in nearby galaxies. By 2007 December 14, 383 galaxies within 40 Mpc with isophotal major axes above 1 arcminute had been observed by 626 public ACIS observations, most of which were for the first time analyzed by this survey to study the X-ray point sources. Uniform data analysis procedures were applied to the 626 ACIS observations and led to the detection of 28,099 point sources, which belong to 17,559 independent sources. These include 8700 sources observed twice or more and 1000 sources observed 10 times or more, providing a wealth of data to study the long-term variability of these X-ray sources. Cross-correlation of these sources with galaxy isophotes led to 8,519 sources within the D&lt;sub&gt;25&lt;/sub&gt; isophotes of 351 galaxies, 3,305 sources between the D&lt;sub&gt;25&lt;/sub&gt; and 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 309 galaxies, and an additional 5,735 sources outside the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of galaxies. This survey has produced a uniform catalog, by far the largest, of 11,824 X-ray point sources within 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes of 380 galaxies. Contamination analysis using the log N-log S relation shows that 74% of the sources within the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes above 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 71% of the sources above 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, 63% of the sources above 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, and 56% of all sources are truly associated with the galaxies. Meticulous efforts have identified 234 X-ray sources with galactic nuclei of nearby galaxies. This archival survey leads to 300 ultraluminous X-ray sources (ULXs) with L&lt;sub&gt;X&lt;/sub&gt; in the 0.3-8 keV band &gt;= 2 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; within the D&lt;sub&gt;25&lt;/sub&gt; isophotes, 179 ULXs between the D&lt;sub&gt;25&lt;/sub&gt; and the 2 * D&lt;sub&gt;25&lt;/sub&gt; isophotes, and a total of 479 ULXs within 188 host galaxies, with about 324 ULXs truly associated with the host galaxies based on the contamination analysis. About 4% of the sources exhibited at least one supersoft phase, and 70 sources are classified as ultraluminous supersoft sources with L&lt;sub&gt;X&lt;/sub&gt; (0.3-8 keV) &gt;= 2 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With a uniform data set and good statistics, this survey enables future works on various topics, such as X-ray luminosity functions for the ordinary X-ray binary populations in different types of galaxies, and X-ray properties of galactic nuclei. This table contains the list of 17,559 'independent' X-ray point sources that was contained in table 4 of the reference paper. As the author notes in Section 5 of this paper, there are 341 sources projected within 2 galaxies with overlapping domains which are listed for both galaxies. The 5,735 sources lieing outside the 2* D&lt;sub&gt;25&lt;/sub&gt; isophotes of the galaxies are also included in this table. For these sources, the X-ray luminosities are computed as if they were in a galaxy of that group, which may or may not be the case; thus, they may not be their 'true' luminosities, but are listed for the purposes of comparison.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chngpscliu#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chngpscliu</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chngpscliu&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chngpscliu.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHANDFS4MS [1]</TD>
            <TD>Chandra Deep Field South 4-Megasecond Catalog</TD>
            <TD>This table contains the main Chandra source catalog for the 4 megasecond (Ms) Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin&lt;sup&gt;2&lt;/sup&gt;. It contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt; in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P &lt; 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog (the HEASARC CHANDFS2MS table) sources. The authors determined X-ray source positions using centroid and matched-filter techniques and obtained a median positional uncertainty of ~0.42 arcseconds. In their paper, they also provided a supplementary catalog (not included in this HEASARC table), which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt;, satisfy the condition of 0.004 &lt; P &lt; 0.1, and have an optical counterpart with R &lt; 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (~97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (~94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that &gt;75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3'), the observed AGN and galaxy source densities have reached 9800 (+1300,-1100) deg&lt;sup&gt;-2&lt;/sup&gt; and 6900 (+1100,-900) deg&lt;sup&gt;-2&lt;/sup&gt;, respectively. Simulations show that the main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms&lt;sup&gt;-1&lt;/sup&gt; pixel&lt;sup&gt;-1&lt;/sup&gt; (for a pixel size of 0.492 arcseconds) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ~3.2 x 10&lt;sup&gt;-17&lt;/sup&gt;, 9.1 x 10&lt;sup&gt;-18&lt;/sup&gt;, and 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ~2-2.5 would provide further significant gains and probe key unexplored discovery space. This HEASARC table comprises Table 3 from the reference paper, the Main Chandra Source Catalog of 740 X-ray sources. The 36 optically bright Chandra sources that were listed in Table 6 of the reference paper are thus not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chandfs4ms#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chandfs4ms</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chandfs4ms&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chandfs4ms.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHANDFS4MS [2]</TD>
            <TD>Chandra Deep Field South 4-Megasecond Catalog</TD>
            <TD>This table contains the main Chandra source catalog for the 4 megasecond (Ms) Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin&lt;sup&gt;2&lt;/sup&gt;. It contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt; in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P &lt; 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog (the HEASARC CHANDFS2MS table) sources. The authors determined X-ray source positions using centroid and matched-filter techniques and obtained a median positional uncertainty of ~0.42 arcseconds. In their paper, they also provided a supplementary catalog (not included in this HEASARC table), which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt;, satisfy the condition of 0.004 &lt; P &lt; 0.1, and have an optical counterpart with R &lt; 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (~97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (~94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that &gt;75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3'), the observed AGN and galaxy source densities have reached 9800 (+1300,-1100) deg&lt;sup&gt;-2&lt;/sup&gt; and 6900 (+1100,-900) deg&lt;sup&gt;-2&lt;/sup&gt;, respectively. Simulations show that the main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms&lt;sup&gt;-1&lt;/sup&gt; pixel&lt;sup&gt;-1&lt;/sup&gt; (for a pixel size of 0.492 arcseconds) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ~3.2 x 10&lt;sup&gt;-17&lt;/sup&gt;, 9.1 x 10&lt;sup&gt;-18&lt;/sup&gt;, and 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ~2-2.5 would provide further significant gains and probe key unexplored discovery space. This HEASARC table comprises Table 3 from the reference paper, the Main Chandra Source Catalog of 740 X-ray sources. The 36 optically bright Chandra sources that were listed in Table 6 of the reference paper are thus not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chandfs4ms#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chandfs4ms</TD>
            <TD />
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chandfs4ms&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chandfs4ms.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHANDFS4MS [3]</TD>
            <TD>Chandra Deep Field South 4-Megasecond Catalog</TD>
            <TD>This table contains the main Chandra source catalog for the 4 megasecond (Ms) Chandra Deep Field-South (CDF-S), which is the deepest Chandra survey to date and covers an area of 464.5 arcmin&lt;sup&gt;2&lt;/sup&gt;. It contains 740 X-ray sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt; in at least one of three X-ray bands (0.5-8 keV, full band; 0.5-2 keV, soft band; and 2-8 keV, hard band) and also satisfy a binomial-probability source-selection criterion of P &lt; 0.004 (i.e., the probability of sources not being real is less than 0.004); this approach is designed to maximize the number of reliable sources detected. A total of 300 main-catalog sources are new compared to the previous 2 Ms CDF-S main-catalog (the HEASARC CHANDFS2MS table) sources. The authors determined X-ray source positions using centroid and matched-filter techniques and obtained a median positional uncertainty of ~0.42 arcseconds. In their paper, they also provided a supplementary catalog (not included in this HEASARC table), which consists of 36 sources that are detected with wavdetect at a false-positive probability threshold of 10&lt;sup&gt;-5&lt;/sup&gt;, satisfy the condition of 0.004 &lt; P &lt; 0.1, and have an optical counterpart with R &lt; 24. Multiwavelength identifications, basic optical/infrared/radio photometry, and spectroscopic/photometric redshifts are provided for the X-ray sources in the main and supplementary catalogs. Seven hundred sixteen (~97%) of the 740 main-catalog sources have multiwavelength counterparts, with 673 (~94% of 716) having either spectroscopic or photometric redshifts. The 740 main-catalog sources span broad ranges of full-band flux and 0.5-8 keV luminosity; the 300 new main-catalog sources span similar ranges although they tend to be systematically lower. Basic analyses of the X-ray and multiwavelength properties of the sources indicate that &gt;75% of the main-catalog sources are active galactic nuclei (AGNs); of the 300 new main-catalog sources, about 35% are likely normal and starburst galaxies, reflecting the rise of normal and starburst galaxies at the very faint flux levels uniquely accessible to the 4 Ms CDF-S. Near the center of the 4 Ms CDF-S (i.e., within an off-axis angle of 3'), the observed AGN and galaxy source densities have reached 9800 (+1300,-1100) deg&lt;sup&gt;-2&lt;/sup&gt; and 6900 (+1100,-900) deg&lt;sup&gt;-2&lt;/sup&gt;, respectively. Simulations show that the main catalog is highly reliable and is reasonably complete. The mean backgrounds (corrected for vignetting and exposure-time variations) are 0.063 and 0.178 counts Ms&lt;sup&gt;-1&lt;/sup&gt; pixel&lt;sup&gt;-1&lt;/sup&gt; (for a pixel size of 0.492 arcseconds) for the soft and hard bands, respectively; the majority of the pixels have zero background counts. The 4 Ms CDF-S reaches on-axis flux limits of ~3.2 x 10&lt;sup&gt;-17&lt;/sup&gt;, 9.1 x 10&lt;sup&gt;-18&lt;/sup&gt;, and 5.5 x 10&lt;sup&gt;-17&lt;/sup&gt; erg cm&lt;sup&gt;-2&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt; for the full, soft, and hard bands, respectively. An increase in the CDF-S exposure time by a factor of ~2-2.5 would provide further significant gains and probe key unexplored discovery space. This HEASARC table comprises Table 3 from the reference paper, the Main Chandra Source Catalog of 740 X-ray sources. The 36 optically bright Chandra sources that were listed in Table 6 of the reference paper are thus not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chandfs4ms#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chandfs4ms</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chandfs4ms&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chandfs4ms.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/99/1079 [1]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#1</TD>
            <TD>2012-11-13T13:59:09Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/99/1079</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/99/1079 [2]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#2</TD>
            <TD>2012-11-13T13:59:09Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079</TD>
            <TD />
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/99/1079&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1079 [table3]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#table3</TD>
            <TD>2012-11-13T13:59:09Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1079&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/99/1079 [table2]</TD>
            <TD>Nova rate in NGC 5128 (Ciardullo+, 1990)</TD>
            <TD>We present the results of a five year nova survey of NGC 5128 performed with an H{alpha} filter at the prime focus of the CTIO 4m telescope. In all, 16 novae were detected, of which 12 are members of a statistically complete and homogeneous sample unaffected by the absorption lane of the galaxy. When normalized to B luminosity, the nova rate in the elliptical component of NGC 5128 is 2.7+/-1.0 times less than that observed in the bulge of M 31. However, when normalized in the infrared K bandpass, the two nova rates are identical, and comparable to that measured in the Large Magellanic Cloud. These data suggest that (1) the percentage of binary stars is approximately constant over a large range of star-forming environments, (2) the nova rate in our own galaxy is between 11 and 46yr^-1^ , and (3) nova rates are not strongly affected by tidal captures in bright globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079#table2</TD>
            <TD>2012-11-13T13:59:09Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/99/1079</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/99/1079&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/99/1079</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMMCTY2AGN [1]</TD>
            <TD>XMM-COSMOS X-Ray Selected Type-2 AGN</TD>
            <TD>This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10&lt;sup&gt;10&lt;/sup&gt; solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcty2agn#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcty2agn</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xmmcty2agn&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcty2agn.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMMCTY2AGN [2]</TD>
            <TD>XMM-COSMOS X-Ray Selected Type-2 AGN</TD>
            <TD>This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10&lt;sup&gt;10&lt;/sup&gt; solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcty2agn#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcty2agn</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xmmcty2agn&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcty2agn.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMMCTY2AGN [3]</TD>
            <TD>XMM-COSMOS X-Ray Selected Type-2 AGN</TD>
            <TD>This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10&lt;sup&gt;10&lt;/sup&gt; solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcty2agn#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcty2agn</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xmmcty2agn&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcty2agn.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAMPDBLOG [1]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1 1990 and September 30, 2011, inclusive. (The observation log for the 30-m telescope is available as the HEASARC database table &lt;a href="iram30mlog.html"&gt;IRAM30MLOG&lt;/a&gt;.) No observations were done by the PDBI in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/irampdblog#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/irampdblog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=irampdblog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/irampdblog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRAMPDBLOG [2]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1 1990 and September 30, 2011, inclusive. (The observation log for the 30-m telescope is available as the HEASARC database table &lt;a href="iram30mlog.html"&gt;IRAM30MLOG&lt;/a&gt;.) No observations were done by the PDBI in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/irampdblog#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/irampdblog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=irampdblog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/irampdblog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRAMPDBLOG [3]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1 1990 and September 30, 2011, inclusive. (The observation log for the 30-m telescope is available as the HEASARC database table &lt;a href="iram30mlog.html"&gt;IRAM30MLOG&lt;/a&gt;.) No observations were done by the PDBI in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/irampdblog#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/irampdblog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_irampdblog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/irampdblog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/253/485 [1]</TD>
            <TD>QMW IRAS galaxy catalogue (Rowan-Robinson+, 1991)</TD>
            <TD>This study presents a highly complete and reliable IRAS 60-micron galaxy catalog covering 82 percent of the sky. IRAS color conditions are used to exclude galactic sources, including the remaining cirrus sources. All sources flagged as extended, confused, or having a poor correlation coefficient with a point-source template are examined with the raw IRAS data and accurate fluxes determined using mapping routines. The completeness, reliability, and flux accuracy of the catalog are discussed. Identifications are made with existing optical galaxy catalogs and with galaxy redshift surveys in the literature. It is estimated that redshifts are available for 79 percent of the galaxies in the catalog with V less than 5000km/s, and the 3D distribution of such galaxies is displayed. The dipole component of the surface-brightness distribution of galaxies in the catalog is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485#1</TD>
            <TD>2012-11-13T14:09:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/253/485</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/253/485</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/253/485 [2]</TD>
            <TD>QMW IRAS galaxy catalogue (Rowan-Robinson+, 1991)</TD>
            <TD>This study presents a highly complete and reliable IRAS 60-micron galaxy catalog covering 82 percent of the sky. IRAS color conditions are used to exclude galactic sources, including the remaining cirrus sources. All sources flagged as extended, confused, or having a poor correlation coefficient with a point-source template are examined with the raw IRAS data and accurate fluxes determined using mapping routines. The completeness, reliability, and flux accuracy of the catalog are discussed. Identifications are made with existing optical galaxy catalogs and with galaxy redshift surveys in the literature. It is estimated that redshifts are available for 79 percent of the galaxies in the catalog with V less than 5000km/s, and the 3D distribution of such galaxies is displayed. The dipole component of the surface-brightness distribution of galaxies in the catalog is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485#2</TD>
            <TD>2012-11-13T14:09:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/253/485&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/253/485</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/253/485 [qigc]</TD>
            <TD>QMW IRAS galaxy catalogue (Rowan-Robinson+, 1991)</TD>
            <TD>This study presents a highly complete and reliable IRAS 60-micron galaxy catalog covering 82 percent of the sky. IRAS color conditions are used to exclude galactic sources, including the remaining cirrus sources. All sources flagged as extended, confused, or having a poor correlation coefficient with a point-source template are examined with the raw IRAS data and accurate fluxes determined using mapping routines. The completeness, reliability, and flux accuracy of the catalog are discussed. Identifications are made with existing optical galaxy catalogs and with galaxy redshift surveys in the literature. It is estimated that redshifts are available for 79 percent of the galaxies in the catalog with V less than 5000km/s, and the 3D distribution of such galaxies is displayed. The dipole component of the surface-brightness distribution of galaxies in the catalog is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485#qigc</TD>
            <TD>2012-11-13T14:09:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/253/485&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/253/485</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAMPDBLOG [1]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1 1990 and September 30, 2011, inclusive. (The observation log for the 30-m telescope is available as the HEASARC database table &lt;a href="iram30mlog.html"&gt;IRAM30MLOG&lt;/a&gt;.) No observations were done by the PDBI in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/irampdblog#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/irampdblog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=irampdblog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/irampdblog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRAMPDBLOG [2]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1 1990 and September 30, 2011, inclusive. (The observation log for the 30-m telescope is available as the HEASARC database table &lt;a href="iram30mlog.html"&gt;IRAM30MLOG&lt;/a&gt;.) No observations were done by the PDBI in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/irampdblog#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/irampdblog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=irampdblog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/irampdblog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRAMPDBLOG [3]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1 1990 and September 30, 2011, inclusive. (The observation log for the 30-m telescope is available as the HEASARC database table &lt;a href="iram30mlog.html"&gt;IRAM30MLOG&lt;/a&gt;.) No observations were done by the PDBI in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/irampdblog#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/irampdblog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_irampdblog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/irampdblog.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMMCTY2AGN [1]</TD>
            <TD>XMM-COSMOS X-Ray Selected Type-2 AGN</TD>
            <TD>This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10&lt;sup&gt;10&lt;/sup&gt; solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcty2agn#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcty2agn</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xmmcty2agn&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcty2agn.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMMCTY2AGN [2]</TD>
            <TD>XMM-COSMOS X-Ray Selected Type-2 AGN</TD>
            <TD>This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10&lt;sup&gt;10&lt;/sup&gt; solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcty2agn#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcty2agn</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xmmcty2agn&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcty2agn.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMMCTY2AGN [3]</TD>
            <TD>XMM-COSMOS X-Ray Selected Type-2 AGN</TD>
            <TD>This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10&lt;sup&gt;10&lt;/sup&gt; solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcty2agn#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcty2agn</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xmmcty2agn&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcty2agn.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAMPDBLOG [1]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1 1990 and September 30, 2011, inclusive. (The observation log for the 30-m telescope is available as the HEASARC database table &lt;a href="iram30mlog.html"&gt;IRAM30MLOG&lt;/a&gt;.) No observations were done by the PDBI in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/irampdblog#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/irampdblog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=irampdblog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/irampdblog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRAMPDBLOG [2]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1 1990 and September 30, 2011, inclusive. (The observation log for the 30-m telescope is available as the HEASARC database table &lt;a href="iram30mlog.html"&gt;IRAM30MLOG&lt;/a&gt;.) No observations were done by the PDBI in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/irampdblog#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/irampdblog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=irampdblog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/irampdblog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRAMPDBLOG [3]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1 1990 and September 30, 2011, inclusive. (The observation log for the 30-m telescope is available as the HEASARC database table &lt;a href="iram30mlog.html"&gt;IRAM30MLOG&lt;/a&gt;.) No observations were done by the PDBI in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/irampdblog#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/irampdblog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_irampdblog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/irampdblog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/253/485 [1]</TD>
            <TD>QMW IRAS galaxy catalogue (Rowan-Robinson+, 1991)</TD>
            <TD>This study presents a highly complete and reliable IRAS 60-micron galaxy catalog covering 82 percent of the sky. IRAS color conditions are used to exclude galactic sources, including the remaining cirrus sources. All sources flagged as extended, confused, or having a poor correlation coefficient with a point-source template are examined with the raw IRAS data and accurate fluxes determined using mapping routines. The completeness, reliability, and flux accuracy of the catalog are discussed. Identifications are made with existing optical galaxy catalogs and with galaxy redshift surveys in the literature. It is estimated that redshifts are available for 79 percent of the galaxies in the catalog with V less than 5000km/s, and the 3D distribution of such galaxies is displayed. The dipole component of the surface-brightness distribution of galaxies in the catalog is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485#1</TD>
            <TD>2012-11-13T14:09:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/253/485</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/253/485</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/253/485 [2]</TD>
            <TD>QMW IRAS galaxy catalogue (Rowan-Robinson+, 1991)</TD>
            <TD>This study presents a highly complete and reliable IRAS 60-micron galaxy catalog covering 82 percent of the sky. IRAS color conditions are used to exclude galactic sources, including the remaining cirrus sources. All sources flagged as extended, confused, or having a poor correlation coefficient with a point-source template are examined with the raw IRAS data and accurate fluxes determined using mapping routines. The completeness, reliability, and flux accuracy of the catalog are discussed. Identifications are made with existing optical galaxy catalogs and with galaxy redshift surveys in the literature. It is estimated that redshifts are available for 79 percent of the galaxies in the catalog with V less than 5000km/s, and the 3D distribution of such galaxies is displayed. The dipole component of the surface-brightness distribution of galaxies in the catalog is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485#2</TD>
            <TD>2012-11-13T14:09:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/253/485&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/253/485</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/253/485 [qigc]</TD>
            <TD>QMW IRAS galaxy catalogue (Rowan-Robinson+, 1991)</TD>
            <TD>This study presents a highly complete and reliable IRAS 60-micron galaxy catalog covering 82 percent of the sky. IRAS color conditions are used to exclude galactic sources, including the remaining cirrus sources. All sources flagged as extended, confused, or having a poor correlation coefficient with a point-source template are examined with the raw IRAS data and accurate fluxes determined using mapping routines. The completeness, reliability, and flux accuracy of the catalog are discussed. Identifications are made with existing optical galaxy catalogs and with galaxy redshift surveys in the literature. It is estimated that redshifts are available for 79 percent of the galaxies in the catalog with V less than 5000km/s, and the 3D distribution of such galaxies is displayed. The dipole component of the surface-brightness distribution of galaxies in the catalog is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485#qigc</TD>
            <TD>2012-11-13T14:09:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/253/485&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/253/485</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IC10XMMCXO [1]</TD>
            <TD>IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 CDS Catalog II/246) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ic10xmmcxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ic10xmmcxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ic10xmmcxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ic10xmmcxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IC10XMMCXO [2]</TD>
            <TD>IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 CDS Catalog II/246) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ic10xmmcxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ic10xmmcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ic10xmmcxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ic10xmmcxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IC10XMMCXO [3]</TD>
            <TD>IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 CDS Catalog II/246) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ic10xmmcxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ic10xmmcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ic10xmmcxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ic10xmmcxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMMCTY2AGN [1]</TD>
            <TD>XMM-COSMOS X-Ray Selected Type-2 AGN</TD>
            <TD>This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10&lt;sup&gt;10&lt;/sup&gt; solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcty2agn#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcty2agn</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xmmcty2agn&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcty2agn.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMMCTY2AGN [2]</TD>
            <TD>XMM-COSMOS X-Ray Selected Type-2 AGN</TD>
            <TD>This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10&lt;sup&gt;10&lt;/sup&gt; solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcty2agn#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcty2agn</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xmmcty2agn&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcty2agn.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMMCTY2AGN [3]</TD>
            <TD>XMM-COSMOS X-Ray Selected Type-2 AGN</TD>
            <TD>This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10&lt;sup&gt;10&lt;/sup&gt; solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M&lt;sub&gt;U&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;V&lt;/sub&gt;, absolute magnitude M&lt;sub&gt;J&lt;/sub&gt; (Johnson-Kron-Cousin system), and the morphological class.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcty2agn#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcty2agn</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xmmcty2agn&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcty2agn.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IC10XMMCXO [1]</TD>
            <TD>IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 CDS Catalog II/246) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ic10xmmcxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ic10xmmcxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ic10xmmcxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ic10xmmcxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IC10XMMCXO [2]</TD>
            <TD>IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 CDS Catalog II/246) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ic10xmmcxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ic10xmmcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ic10xmmcxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ic10xmmcxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IC10XMMCXO [3]</TD>
            <TD>IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 CDS Catalog II/246) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ic10xmmcxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ic10xmmcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ic10xmmcxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ic10xmmcxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/253/485 [1]</TD>
            <TD>QMW IRAS galaxy catalogue (Rowan-Robinson+, 1991)</TD>
            <TD>This study presents a highly complete and reliable IRAS 60-micron galaxy catalog covering 82 percent of the sky. IRAS color conditions are used to exclude galactic sources, including the remaining cirrus sources. All sources flagged as extended, confused, or having a poor correlation coefficient with a point-source template are examined with the raw IRAS data and accurate fluxes determined using mapping routines. The completeness, reliability, and flux accuracy of the catalog are discussed. Identifications are made with existing optical galaxy catalogs and with galaxy redshift surveys in the literature. It is estimated that redshifts are available for 79 percent of the galaxies in the catalog with V less than 5000km/s, and the 3D distribution of such galaxies is displayed. The dipole component of the surface-brightness distribution of galaxies in the catalog is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485#1</TD>
            <TD>2012-11-13T14:09:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/253/485</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/253/485</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/253/485 [2]</TD>
            <TD>QMW IRAS galaxy catalogue (Rowan-Robinson+, 1991)</TD>
            <TD>This study presents a highly complete and reliable IRAS 60-micron galaxy catalog covering 82 percent of the sky. IRAS color conditions are used to exclude galactic sources, including the remaining cirrus sources. All sources flagged as extended, confused, or having a poor correlation coefficient with a point-source template are examined with the raw IRAS data and accurate fluxes determined using mapping routines. The completeness, reliability, and flux accuracy of the catalog are discussed. Identifications are made with existing optical galaxy catalogs and with galaxy redshift surveys in the literature. It is estimated that redshifts are available for 79 percent of the galaxies in the catalog with V less than 5000km/s, and the 3D distribution of such galaxies is displayed. The dipole component of the surface-brightness distribution of galaxies in the catalog is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485#2</TD>
            <TD>2012-11-13T14:09:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/253/485&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/253/485</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/253/485 [qigc]</TD>
            <TD>QMW IRAS galaxy catalogue (Rowan-Robinson+, 1991)</TD>
            <TD>This study presents a highly complete and reliable IRAS 60-micron galaxy catalog covering 82 percent of the sky. IRAS color conditions are used to exclude galactic sources, including the remaining cirrus sources. All sources flagged as extended, confused, or having a poor correlation coefficient with a point-source template are examined with the raw IRAS data and accurate fluxes determined using mapping routines. The completeness, reliability, and flux accuracy of the catalog are discussed. Identifications are made with existing optical galaxy catalogs and with galaxy redshift surveys in the literature. It is estimated that redshifts are available for 79 percent of the galaxies in the catalog with V less than 5000km/s, and the 3D distribution of such galaxies is displayed. The dipole component of the surface-brightness distribution of galaxies in the catalog is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485#qigc</TD>
            <TD>2012-11-13T14:09:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/253/485</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/253/485&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/253/485</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IC10XMMCXO [1]</TD>
            <TD>IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 CDS Catalog II/246) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ic10xmmcxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ic10xmmcxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ic10xmmcxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ic10xmmcxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IC10XMMCXO [2]</TD>
            <TD>IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 CDS Catalog II/246) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ic10xmmcxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ic10xmmcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ic10xmmcxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ic10xmmcxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IC10XMMCXO [3]</TD>
            <TD>IC 10 XMM-Newton and Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from an X-ray study of our nearest starburst galaxy IC 10, based on XMM-Newton and Chandra observations. It contains a list of 73 XMM-Newton and 28 Chandra detections of point-like X-ray sources in the field of this galaxy; a substantial fraction of them are likely to be stellar objects in the Milky Way due to the low Galactic latitude location of IC 10. The brightest source in the IC 10 field, X-1, has a mean 0.3-8.0 keV luminosity of ~1.2E38 erg s&lt;sup&gt;-1&lt;/sup&gt; and shows a large variation by a factor of up to ~6 on timescales of ~10&lt;sup&gt;4&lt;/sup&gt; s during the XMM-Newton observation. The XMM-Newton observations were taken on 2003 July 3 with a total exposure time of ~45 ks for the EPIC-MOS cameras and ~42 ks for the European Photon Imaging Camera (EPIC) PN camera. The authors use only the data from the PN camera (with a thin optical blocking filter) because of its high sensitivity to soft X-rays in the study of diffuse emission and include the data from the MOS cameras in the analysis of X-1. The Chandra observation, taken on 2003 March 12 with an exposure of 29 ks and already described by Bauer and Brandt (2004, ApJ, 601, 67), was reprocessed by the authors using the then-latest CIAO software (version 3.2.1) and calibration database (version 3.0.0). The authors used the Two-Micron All Sky Survey (2MASS) All-Sky Catalog of Point Sources (Cutri et al. 2003 CDS Catalog II/246) to search for potential counterparts. They cross-correlated the spatial positions of the objects in this catalog with their X-ray source positions, using a matching radius of 4 arcsec for XMM-Newton PN sources and 2 arcsec for Chandra ACIS sources. The radius was chosen to be greater than the 1-sigma statistical position uncertainty of almost all the sources.In no case is there a match with multiple 2MASS objects. The 3-sigma limiting sensitivities of the 2MASS Catalog are 17.1, 16.4 and 15.3 mag in the three bands, J, H, and K&lt;sub&gt;S&lt;/sub&gt;, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ic10xmmcxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ic10xmmcxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ic10xmmcxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ic10xmmcxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMMSDSSGCS [1]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey</TD>
            <TD>This catalog of X-ray selected galaxy clusters and groups, the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprises 175 clusters of galaxies. Among them, 139 objects are new X-ray discoveries, while the others were previously known as X-ray sources. This survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates, and study the correlation of the X-ray and optical properties. In their paper, the authors describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalog (2XMMi-DR3). Cross-correlation of the initial catalog with recently published optically selected SDSS galaxy cluster catalogs yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). The authors developed an automated method to reprocess the XMM-Newton X-ray observations, determine the optimum source extraction radius, generate source and background spectra, and derive the temperatures and luminosities of the optically confirmed clusters. Here the X-ray properties of the first cluster sample comprising 175 clusters are presented. For each cluster, the catalog provides: two identifiers, coordinates, temperature, flux [0.5-2keV, luminosity [0.5-2] keV extracted from an optimum aperture, bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, radius R&lt;sub&gt;500&lt;/sub&gt;, and the optical properties of the counterpart. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L&lt;sub&gt;500&lt;/sub&gt; = 1.9 x 10&lt;sup&gt;42&lt;/sup&gt; - 1.2 x 10&lt;sup&gt;45&lt;/sup&gt; erg/s, and masses M&lt;sub&gt;500&lt;/sub&gt; = 2.3 x 10&lt;sup&gt;13&lt;/sup&gt; - 4.9 x 10&lt;sup&gt;14&lt;/sup&gt;M&lt;sub&gt;sun&lt;/sub&gt;. The authors extend the relation between the X-ray bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt; and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. The cluster catalog with the X-ray/optical overlay and fitted spectra for each cluster is also available at the authors' web site: &lt;a href="http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html"&gt;http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmsdssgcs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmsdssgcs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xmmsdssgcs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmsdssgcs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMMSDSSGCS [2]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey</TD>
            <TD>This catalog of X-ray selected galaxy clusters and groups, the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprises 175 clusters of galaxies. Among them, 139 objects are new X-ray discoveries, while the others were previously known as X-ray sources. This survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates, and study the correlation of the X-ray and optical properties. In their paper, the authors describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalog (2XMMi-DR3). Cross-correlation of the initial catalog with recently published optically selected SDSS galaxy cluster catalogs yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). The authors developed an automated method to reprocess the XMM-Newton X-ray observations, determine the optimum source extraction radius, generate source and background spectra, and derive the temperatures and luminosities of the optically confirmed clusters. Here the X-ray properties of the first cluster sample comprising 175 clusters are presented. For each cluster, the catalog provides: two identifiers, coordinates, temperature, flux [0.5-2keV, luminosity [0.5-2] keV extracted from an optimum aperture, bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, radius R&lt;sub&gt;500&lt;/sub&gt;, and the optical properties of the counterpart. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L&lt;sub&gt;500&lt;/sub&gt; = 1.9 x 10&lt;sup&gt;42&lt;/sup&gt; - 1.2 x 10&lt;sup&gt;45&lt;/sup&gt; erg/s, and masses M&lt;sub&gt;500&lt;/sub&gt; = 2.3 x 10&lt;sup&gt;13&lt;/sup&gt; - 4.9 x 10&lt;sup&gt;14&lt;/sup&gt;M&lt;sub&gt;sun&lt;/sub&gt;. The authors extend the relation between the X-ray bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt; and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. The cluster catalog with the X-ray/optical overlay and fitted spectra for each cluster is also available at the authors' web site: &lt;a href="http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html"&gt;http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmsdssgcs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmsdssgcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xmmsdssgcs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmsdssgcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMMSDSSGCS [3]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey</TD>
            <TD>This catalog of X-ray selected galaxy clusters and groups, the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprises 175 clusters of galaxies. Among them, 139 objects are new X-ray discoveries, while the others were previously known as X-ray sources. This survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates, and study the correlation of the X-ray and optical properties. In their paper, the authors describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalog (2XMMi-DR3). Cross-correlation of the initial catalog with recently published optically selected SDSS galaxy cluster catalogs yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). The authors developed an automated method to reprocess the XMM-Newton X-ray observations, determine the optimum source extraction radius, generate source and background spectra, and derive the temperatures and luminosities of the optically confirmed clusters. Here the X-ray properties of the first cluster sample comprising 175 clusters are presented. For each cluster, the catalog provides: two identifiers, coordinates, temperature, flux [0.5-2keV, luminosity [0.5-2] keV extracted from an optimum aperture, bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, radius R&lt;sub&gt;500&lt;/sub&gt;, and the optical properties of the counterpart. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L&lt;sub&gt;500&lt;/sub&gt; = 1.9 x 10&lt;sup&gt;42&lt;/sup&gt; - 1.2 x 10&lt;sup&gt;45&lt;/sup&gt; erg/s, and masses M&lt;sub&gt;500&lt;/sub&gt; = 2.3 x 10&lt;sup&gt;13&lt;/sup&gt; - 4.9 x 10&lt;sup&gt;14&lt;/sup&gt;M&lt;sub&gt;sun&lt;/sub&gt;. The authors extend the relation between the X-ray bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt; and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. The cluster catalog with the X-ray/optical overlay and fitted spectra for each cluster is also available at the authors' web site: &lt;a href="http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html"&gt;http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmsdssgcs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmsdssgcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xmmsdssgcs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmsdssgcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1982 [1]</TD>
            <TD>HST UBVI photometry of NGC 3081 inner regions (Buta+, 2004)</TD>
            <TD>The Hubble Space Telescope (HST) observations of NGC 3081 were secured on 2000 June 25 with the Wide Field Planetary Camera 2 (WFPC2). The center of the galaxy was placed near the overlap section between WFPC2 sections WF3 and WF4. Five broadband filters were used to observe the galaxy: F255W, F336W, F439W, F555W, and F814W. The latter four filters are intended to approximate Johnson U, B, V, and Cousins I photometric systems, respectively, while F255W is a mid-ultraviolet filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982#1</TD>
            <TD>2011-09-14T19:47:18Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1982</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1982</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1982 [2]</TD>
            <TD>HST UBVI photometry of NGC 3081 inner regions (Buta+, 2004)</TD>
            <TD>The Hubble Space Telescope (HST) observations of NGC 3081 were secured on 2000 June 25 with the Wide Field Planetary Camera 2 (WFPC2). The center of the galaxy was placed near the overlap section between WFPC2 sections WF3 and WF4. Five broadband filters were used to observe the galaxy: F255W, F336W, F439W, F555W, and F814W. The latter four filters are intended to approximate Johnson U, B, V, and Cousins I photometric systems, respectively, while F255W is a mid-ultraviolet filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982#2</TD>
            <TD>2011-09-14T19:47:18Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1982&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1982</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/1982 [table3]</TD>
            <TD>HST UBVI photometry of NGC 3081 inner regions (Buta+, 2004)</TD>
            <TD>The Hubble Space Telescope (HST) observations of NGC 3081 were secured on 2000 June 25 with the Wide Field Planetary Camera 2 (WFPC2). The center of the galaxy was placed near the overlap section between WFPC2 sections WF3 and WF4. Five broadband filters were used to observe the galaxy: F255W, F336W, F439W, F555W, and F814W. The latter four filters are intended to approximate Johnson U, B, V, and Cousins I photometric systems, respectively, while F255W is a mid-ultraviolet filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982#table3</TD>
            <TD>2011-09-14T19:47:18Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/1982&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1982</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMMSDSSGCS [1]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey</TD>
            <TD>This catalog of X-ray selected galaxy clusters and groups, the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprises 175 clusters of galaxies. Among them, 139 objects are new X-ray discoveries, while the others were previously known as X-ray sources. This survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates, and study the correlation of the X-ray and optical properties. In their paper, the authors describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalog (2XMMi-DR3). Cross-correlation of the initial catalog with recently published optically selected SDSS galaxy cluster catalogs yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). The authors developed an automated method to reprocess the XMM-Newton X-ray observations, determine the optimum source extraction radius, generate source and background spectra, and derive the temperatures and luminosities of the optically confirmed clusters. Here the X-ray properties of the first cluster sample comprising 175 clusters are presented. For each cluster, the catalog provides: two identifiers, coordinates, temperature, flux [0.5-2keV, luminosity [0.5-2] keV extracted from an optimum aperture, bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, radius R&lt;sub&gt;500&lt;/sub&gt;, and the optical properties of the counterpart. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L&lt;sub&gt;500&lt;/sub&gt; = 1.9 x 10&lt;sup&gt;42&lt;/sup&gt; - 1.2 x 10&lt;sup&gt;45&lt;/sup&gt; erg/s, and masses M&lt;sub&gt;500&lt;/sub&gt; = 2.3 x 10&lt;sup&gt;13&lt;/sup&gt; - 4.9 x 10&lt;sup&gt;14&lt;/sup&gt;M&lt;sub&gt;sun&lt;/sub&gt;. The authors extend the relation between the X-ray bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt; and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. The cluster catalog with the X-ray/optical overlay and fitted spectra for each cluster is also available at the authors' web site: &lt;a href="http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html"&gt;http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmsdssgcs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmsdssgcs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xmmsdssgcs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmsdssgcs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMMSDSSGCS [2]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey</TD>
            <TD>This catalog of X-ray selected galaxy clusters and groups, the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprises 175 clusters of galaxies. Among them, 139 objects are new X-ray discoveries, while the others were previously known as X-ray sources. This survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates, and study the correlation of the X-ray and optical properties. In their paper, the authors describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalog (2XMMi-DR3). Cross-correlation of the initial catalog with recently published optically selected SDSS galaxy cluster catalogs yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). The authors developed an automated method to reprocess the XMM-Newton X-ray observations, determine the optimum source extraction radius, generate source and background spectra, and derive the temperatures and luminosities of the optically confirmed clusters. Here the X-ray properties of the first cluster sample comprising 175 clusters are presented. For each cluster, the catalog provides: two identifiers, coordinates, temperature, flux [0.5-2keV, luminosity [0.5-2] keV extracted from an optimum aperture, bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, radius R&lt;sub&gt;500&lt;/sub&gt;, and the optical properties of the counterpart. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L&lt;sub&gt;500&lt;/sub&gt; = 1.9 x 10&lt;sup&gt;42&lt;/sup&gt; - 1.2 x 10&lt;sup&gt;45&lt;/sup&gt; erg/s, and masses M&lt;sub&gt;500&lt;/sub&gt; = 2.3 x 10&lt;sup&gt;13&lt;/sup&gt; - 4.9 x 10&lt;sup&gt;14&lt;/sup&gt;M&lt;sub&gt;sun&lt;/sub&gt;. The authors extend the relation between the X-ray bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt; and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. The cluster catalog with the X-ray/optical overlay and fitted spectra for each cluster is also available at the authors' web site: &lt;a href="http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html"&gt;http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmsdssgcs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmsdssgcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xmmsdssgcs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmsdssgcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMMSDSSGCS [3]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey</TD>
            <TD>This catalog of X-ray selected galaxy clusters and groups, the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprises 175 clusters of galaxies. Among them, 139 objects are new X-ray discoveries, while the others were previously known as X-ray sources. This survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates, and study the correlation of the X-ray and optical properties. In their paper, the authors describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalog (2XMMi-DR3). Cross-correlation of the initial catalog with recently published optically selected SDSS galaxy cluster catalogs yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). The authors developed an automated method to reprocess the XMM-Newton X-ray observations, determine the optimum source extraction radius, generate source and background spectra, and derive the temperatures and luminosities of the optically confirmed clusters. Here the X-ray properties of the first cluster sample comprising 175 clusters are presented. For each cluster, the catalog provides: two identifiers, coordinates, temperature, flux [0.5-2keV, luminosity [0.5-2] keV extracted from an optimum aperture, bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, radius R&lt;sub&gt;500&lt;/sub&gt;, and the optical properties of the counterpart. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L&lt;sub&gt;500&lt;/sub&gt; = 1.9 x 10&lt;sup&gt;42&lt;/sup&gt; - 1.2 x 10&lt;sup&gt;45&lt;/sup&gt; erg/s, and masses M&lt;sub&gt;500&lt;/sub&gt; = 2.3 x 10&lt;sup&gt;13&lt;/sup&gt; - 4.9 x 10&lt;sup&gt;14&lt;/sup&gt;M&lt;sub&gt;sun&lt;/sub&gt;. The authors extend the relation between the X-ray bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt; and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. The cluster catalog with the X-ray/optical overlay and fitted spectra for each cluster is also available at the authors' web site: &lt;a href="http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html"&gt;http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmsdssgcs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmsdssgcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xmmsdssgcs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmsdssgcs.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MCXC [1]</TD>
            <TD>MCXC Meta-Catalog of X-Ray Detected Clusters of Galaxies</TD>
            <TD>The MCXC is the Meta-Catalog of the compiled properties of X-ray detected Clusters of galaxies. This very large catalog is based on publicly available ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogs. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogs have been carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster, the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, and radius R&lt;sub&gt;500&lt;/sub&gt;, where the 500 suffix means that the quantity has been calculated up to a standard characteristic radius R&lt;sub&gt;500&lt;/sub&gt;, the radius within which the mean overdensity of the cluster is 500 times the critical density at the cluster redshift . The meta-catalog additionally furnishes information on overlaps between the input catalogs and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is made available so as to provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other multiwavelength studies. The catalogs and sub-catalogs included in this meta-catalog are listed in Table 1 of the reference paper, and come from the following references: &lt;pre&gt; Catalog Sub- Reference Title Catalog or CDS Cat. (Author) RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS) (Voges+, 1999) BCS BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I. (Ebeling+, 1998) eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) CIZA X-ray clusters behind the Milky Way CIZAI ApJ, 580, 774 (Ebeling+, 2002) CIZAII J/APJ/662/224 (Kocevski+, 2007) EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey (Gioia+, 1990) EMSS_1994 ApJS, 94, 583 (Gioia &amp; Luppino, 1994) EMSS_2004 ApJ, 608, 603 (Henry 2004) MACS ApJ, 553, 668 Massive Cluster Survey (Ebeling+, 2001) MACS_MJFV ApJS, 174, 117 (Maughan+, 2008) MACS_BRIGHT MNRAS, 407, 83 (Ebeling+, 2010) MACS_DIST ApJ, 661, L33 (Ebeling+, 2007) NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog (Henry+, 2006) NORAS/ REFLEX NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I. (Boehringer+, 2000) REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat (Boehringer+, 2004) SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP (Cruddace+, 2002) SHARC SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog (Romer+, 2000) SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog (Burke+, 2003) WARPS WARPSI J/ApJS/140/265 WARPS survey. VI. (Perlman+, 2002) WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII. (Horner+, 2008) 160SD 160SD J/ApJ/594/154 160 square degree ROSAT Survey (Mullis+, 2003) 400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey (Burenin+, 2007) 400SD_SER Serendipitous clusters 400SD_NONSER Not entirely serendipitous clusters &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/mcxc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcxc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=mcxc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/mcxc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MCXC [2]</TD>
            <TD>MCXC Meta-Catalog of X-Ray Detected Clusters of Galaxies</TD>
            <TD>The MCXC is the Meta-Catalog of the compiled properties of X-ray detected Clusters of galaxies. This very large catalog is based on publicly available ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogs. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogs have been carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster, the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, and radius R&lt;sub&gt;500&lt;/sub&gt;, where the 500 suffix means that the quantity has been calculated up to a standard characteristic radius R&lt;sub&gt;500&lt;/sub&gt;, the radius within which the mean overdensity of the cluster is 500 times the critical density at the cluster redshift . The meta-catalog additionally furnishes information on overlaps between the input catalogs and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is made available so as to provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other multiwavelength studies. The catalogs and sub-catalogs included in this meta-catalog are listed in Table 1 of the reference paper, and come from the following references: &lt;pre&gt; Catalog Sub- Reference Title Catalog or CDS Cat. (Author) RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS) (Voges+, 1999) BCS BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I. (Ebeling+, 1998) eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) CIZA X-ray clusters behind the Milky Way CIZAI ApJ, 580, 774 (Ebeling+, 2002) CIZAII J/APJ/662/224 (Kocevski+, 2007) EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey (Gioia+, 1990) EMSS_1994 ApJS, 94, 583 (Gioia &amp; Luppino, 1994) EMSS_2004 ApJ, 608, 603 (Henry 2004) MACS ApJ, 553, 668 Massive Cluster Survey (Ebeling+, 2001) MACS_MJFV ApJS, 174, 117 (Maughan+, 2008) MACS_BRIGHT MNRAS, 407, 83 (Ebeling+, 2010) MACS_DIST ApJ, 661, L33 (Ebeling+, 2007) NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog (Henry+, 2006) NORAS/ REFLEX NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I. (Boehringer+, 2000) REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat (Boehringer+, 2004) SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP (Cruddace+, 2002) SHARC SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog (Romer+, 2000) SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog (Burke+, 2003) WARPS WARPSI J/ApJS/140/265 WARPS survey. VI. (Perlman+, 2002) WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII. (Horner+, 2008) 160SD 160SD J/ApJ/594/154 160 square degree ROSAT Survey (Mullis+, 2003) 400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey (Burenin+, 2007) 400SD_SER Serendipitous clusters 400SD_NONSER Not entirely serendipitous clusters &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/mcxc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcxc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=mcxc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/mcxc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MCXC [3]</TD>
            <TD>MCXC Meta-Catalog of X-Ray Detected Clusters of Galaxies</TD>
            <TD>The MCXC is the Meta-Catalog of the compiled properties of X-ray detected Clusters of galaxies. This very large catalog is based on publicly available ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogs. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogs have been carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster, the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, and radius R&lt;sub&gt;500&lt;/sub&gt;, where the 500 suffix means that the quantity has been calculated up to a standard characteristic radius R&lt;sub&gt;500&lt;/sub&gt;, the radius within which the mean overdensity of the cluster is 500 times the critical density at the cluster redshift . The meta-catalog additionally furnishes information on overlaps between the input catalogs and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is made available so as to provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other multiwavelength studies. The catalogs and sub-catalogs included in this meta-catalog are listed in Table 1 of the reference paper, and come from the following references: &lt;pre&gt; Catalog Sub- Reference Title Catalog or CDS Cat. (Author) RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS) (Voges+, 1999) BCS BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I. (Ebeling+, 1998) eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) CIZA X-ray clusters behind the Milky Way CIZAI ApJ, 580, 774 (Ebeling+, 2002) CIZAII J/APJ/662/224 (Kocevski+, 2007) EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey (Gioia+, 1990) EMSS_1994 ApJS, 94, 583 (Gioia &amp; Luppino, 1994) EMSS_2004 ApJ, 608, 603 (Henry 2004) MACS ApJ, 553, 668 Massive Cluster Survey (Ebeling+, 2001) MACS_MJFV ApJS, 174, 117 (Maughan+, 2008) MACS_BRIGHT MNRAS, 407, 83 (Ebeling+, 2010) MACS_DIST ApJ, 661, L33 (Ebeling+, 2007) NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog (Henry+, 2006) NORAS/ REFLEX NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I. (Boehringer+, 2000) REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat (Boehringer+, 2004) SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP (Cruddace+, 2002) SHARC SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog (Romer+, 2000) SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog (Burke+, 2003) WARPS WARPSI J/ApJS/140/265 WARPS survey. VI. (Perlman+, 2002) WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII. (Horner+, 2008) 160SD 160SD J/ApJ/594/154 160 square degree ROSAT Survey (Mullis+, 2003) 400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey (Burenin+, 2007) 400SD_SER Serendipitous clusters 400SD_NONSER Not entirely serendipitous clusters &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/mcxc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcxc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_mcxc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/mcxc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMMSDSSGCS [1]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey</TD>
            <TD>This catalog of X-ray selected galaxy clusters and groups, the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprises 175 clusters of galaxies. Among them, 139 objects are new X-ray discoveries, while the others were previously known as X-ray sources. This survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates, and study the correlation of the X-ray and optical properties. In their paper, the authors describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalog (2XMMi-DR3). Cross-correlation of the initial catalog with recently published optically selected SDSS galaxy cluster catalogs yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). The authors developed an automated method to reprocess the XMM-Newton X-ray observations, determine the optimum source extraction radius, generate source and background spectra, and derive the temperatures and luminosities of the optically confirmed clusters. Here the X-ray properties of the first cluster sample comprising 175 clusters are presented. For each cluster, the catalog provides: two identifiers, coordinates, temperature, flux [0.5-2keV, luminosity [0.5-2] keV extracted from an optimum aperture, bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, radius R&lt;sub&gt;500&lt;/sub&gt;, and the optical properties of the counterpart. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L&lt;sub&gt;500&lt;/sub&gt; = 1.9 x 10&lt;sup&gt;42&lt;/sup&gt; - 1.2 x 10&lt;sup&gt;45&lt;/sup&gt; erg/s, and masses M&lt;sub&gt;500&lt;/sub&gt; = 2.3 x 10&lt;sup&gt;13&lt;/sup&gt; - 4.9 x 10&lt;sup&gt;14&lt;/sup&gt;M&lt;sub&gt;sun&lt;/sub&gt;. The authors extend the relation between the X-ray bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt; and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. The cluster catalog with the X-ray/optical overlay and fitted spectra for each cluster is also available at the authors' web site: &lt;a href="http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html"&gt;http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmsdssgcs#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmsdssgcs</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xmmsdssgcs&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmsdssgcs.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMMSDSSGCS [2]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey</TD>
            <TD>This catalog of X-ray selected galaxy clusters and groups, the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprises 175 clusters of galaxies. Among them, 139 objects are new X-ray discoveries, while the others were previously known as X-ray sources. This survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates, and study the correlation of the X-ray and optical properties. In their paper, the authors describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalog (2XMMi-DR3). Cross-correlation of the initial catalog with recently published optically selected SDSS galaxy cluster catalogs yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). The authors developed an automated method to reprocess the XMM-Newton X-ray observations, determine the optimum source extraction radius, generate source and background spectra, and derive the temperatures and luminosities of the optically confirmed clusters. Here the X-ray properties of the first cluster sample comprising 175 clusters are presented. For each cluster, the catalog provides: two identifiers, coordinates, temperature, flux [0.5-2keV, luminosity [0.5-2] keV extracted from an optimum aperture, bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, radius R&lt;sub&gt;500&lt;/sub&gt;, and the optical properties of the counterpart. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L&lt;sub&gt;500&lt;/sub&gt; = 1.9 x 10&lt;sup&gt;42&lt;/sup&gt; - 1.2 x 10&lt;sup&gt;45&lt;/sup&gt; erg/s, and masses M&lt;sub&gt;500&lt;/sub&gt; = 2.3 x 10&lt;sup&gt;13&lt;/sup&gt; - 4.9 x 10&lt;sup&gt;14&lt;/sup&gt;M&lt;sub&gt;sun&lt;/sub&gt;. The authors extend the relation between the X-ray bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt; and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. The cluster catalog with the X-ray/optical overlay and fitted spectra for each cluster is also available at the authors' web site: &lt;a href="http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html"&gt;http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmsdssgcs#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmsdssgcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xmmsdssgcs&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmsdssgcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMMSDSSGCS [3]</TD>
            <TD>2XMMi/SDSS Galaxy Cluster Survey</TD>
            <TD>This catalog of X-ray selected galaxy clusters and groups, the first release of the 2XMMi/SDSS Galaxy Cluster Survey, comprises 175 clusters of galaxies. Among them, 139 objects are new X-ray discoveries, while the others were previously known as X-ray sources. This survey is a search for galaxy clusters detected serendipitously in observations with XMM-Newton in the footprint of the Sloan Digital Sky Survey (SDSS). The main aims of the survey are to identify new X-ray galaxy clusters, investigate their X-ray scaling relations, identify distant cluster candidates, and study the correlation of the X-ray and optical properties. In their paper, the authors describe the basic strategy to identify and characterize the X-ray cluster candidates that currently comprise 1180 objects selected from the second XMM-Newton serendipitous source catalog (2XMMi-DR3). Cross-correlation of the initial catalog with recently published optically selected SDSS galaxy cluster catalogs yields photometric redshifts for 275 objects. Of these, 182 clusters have at least one member with a spectroscopic redshift from existing public data (SDSS-DR8). The authors developed an automated method to reprocess the XMM-Newton X-ray observations, determine the optimum source extraction radius, generate source and background spectra, and derive the temperatures and luminosities of the optically confirmed clusters. Here the X-ray properties of the first cluster sample comprising 175 clusters are presented. For each cluster, the catalog provides: two identifiers, coordinates, temperature, flux [0.5-2keV, luminosity [0.5-2] keV extracted from an optimum aperture, bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, radius R&lt;sub&gt;500&lt;/sub&gt;, and the optical properties of the counterpart. The first cluster sample from the survey covers a wide range of redshifts from 0.09 to 0.61, bolometric luminosities L&lt;sub&gt;500&lt;/sub&gt; = 1.9 x 10&lt;sup&gt;42&lt;/sup&gt; - 1.2 x 10&lt;sup&gt;45&lt;/sup&gt; erg/s, and masses M&lt;sub&gt;500&lt;/sub&gt; = 2.3 x 10&lt;sup&gt;13&lt;/sup&gt; - 4.9 x 10&lt;sup&gt;14&lt;/sup&gt;M&lt;sub&gt;sun&lt;/sub&gt;. The authors extend the relation between the X-ray bolometric luminosity L&lt;sub&gt;500&lt;/sub&gt; and the X-ray temperature towards significantly lower T and L and still find that the slope of the linear L-T relation is consistent with values published for high luminosities. The cluster catalog with the X-ray/optical overlay and fitted spectra for each cluster is also available at the authors' web site: &lt;a href="http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html"&gt;http://www.aip.de/groups/xray/XMM_SDSS_CLUSTERS.html&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmsdssgcs#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmsdssgcs</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xmmsdssgcs&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmsdssgcs.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1982 [1]</TD>
            <TD>HST UBVI photometry of NGC 3081 inner regions (Buta+, 2004)</TD>
            <TD>The Hubble Space Telescope (HST) observations of NGC 3081 were secured on 2000 June 25 with the Wide Field Planetary Camera 2 (WFPC2). The center of the galaxy was placed near the overlap section between WFPC2 sections WF3 and WF4. Five broadband filters were used to observe the galaxy: F255W, F336W, F439W, F555W, and F814W. The latter four filters are intended to approximate Johnson U, B, V, and Cousins I photometric systems, respectively, while F255W is a mid-ultraviolet filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982#1</TD>
            <TD>2011-09-14T19:47:18Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1982</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1982</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1982 [2]</TD>
            <TD>HST UBVI photometry of NGC 3081 inner regions (Buta+, 2004)</TD>
            <TD>The Hubble Space Telescope (HST) observations of NGC 3081 were secured on 2000 June 25 with the Wide Field Planetary Camera 2 (WFPC2). The center of the galaxy was placed near the overlap section between WFPC2 sections WF3 and WF4. Five broadband filters were used to observe the galaxy: F255W, F336W, F439W, F555W, and F814W. The latter four filters are intended to approximate Johnson U, B, V, and Cousins I photometric systems, respectively, while F255W is a mid-ultraviolet filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982#2</TD>
            <TD>2011-09-14T19:47:18Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1982&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1982</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/1982 [table3]</TD>
            <TD>HST UBVI photometry of NGC 3081 inner regions (Buta+, 2004)</TD>
            <TD>The Hubble Space Telescope (HST) observations of NGC 3081 were secured on 2000 June 25 with the Wide Field Planetary Camera 2 (WFPC2). The center of the galaxy was placed near the overlap section between WFPC2 sections WF3 and WF4. Five broadband filters were used to observe the galaxy: F255W, F336W, F439W, F555W, and F814W. The latter four filters are intended to approximate Johnson U, B, V, and Cousins I photometric systems, respectively, while F255W is a mid-ultraviolet filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982#table3</TD>
            <TD>2011-09-14T19:47:18Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1982</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/1982&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1982</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MCXC [1]</TD>
            <TD>MCXC Meta-Catalog of X-Ray Detected Clusters of Galaxies</TD>
            <TD>The MCXC is the Meta-Catalog of the compiled properties of X-ray detected Clusters of galaxies. This very large catalog is based on publicly available ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogs. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogs have been carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster, the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, and radius R&lt;sub&gt;500&lt;/sub&gt;, where the 500 suffix means that the quantity has been calculated up to a standard characteristic radius R&lt;sub&gt;500&lt;/sub&gt;, the radius within which the mean overdensity of the cluster is 500 times the critical density at the cluster redshift . The meta-catalog additionally furnishes information on overlaps between the input catalogs and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is made available so as to provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other multiwavelength studies. The catalogs and sub-catalogs included in this meta-catalog are listed in Table 1 of the reference paper, and come from the following references: &lt;pre&gt; Catalog Sub- Reference Title Catalog or CDS Cat. (Author) RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS) (Voges+, 1999) BCS BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I. (Ebeling+, 1998) eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) CIZA X-ray clusters behind the Milky Way CIZAI ApJ, 580, 774 (Ebeling+, 2002) CIZAII J/APJ/662/224 (Kocevski+, 2007) EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey (Gioia+, 1990) EMSS_1994 ApJS, 94, 583 (Gioia &amp; Luppino, 1994) EMSS_2004 ApJ, 608, 603 (Henry 2004) MACS ApJ, 553, 668 Massive Cluster Survey (Ebeling+, 2001) MACS_MJFV ApJS, 174, 117 (Maughan+, 2008) MACS_BRIGHT MNRAS, 407, 83 (Ebeling+, 2010) MACS_DIST ApJ, 661, L33 (Ebeling+, 2007) NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog (Henry+, 2006) NORAS/ REFLEX NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I. (Boehringer+, 2000) REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat (Boehringer+, 2004) SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP (Cruddace+, 2002) SHARC SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog (Romer+, 2000) SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog (Burke+, 2003) WARPS WARPSI J/ApJS/140/265 WARPS survey. VI. (Perlman+, 2002) WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII. (Horner+, 2008) 160SD 160SD J/ApJ/594/154 160 square degree ROSAT Survey (Mullis+, 2003) 400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey (Burenin+, 2007) 400SD_SER Serendipitous clusters 400SD_NONSER Not entirely serendipitous clusters &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/mcxc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcxc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=mcxc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/mcxc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MCXC [2]</TD>
            <TD>MCXC Meta-Catalog of X-Ray Detected Clusters of Galaxies</TD>
            <TD>The MCXC is the Meta-Catalog of the compiled properties of X-ray detected Clusters of galaxies. This very large catalog is based on publicly available ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogs. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogs have been carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster, the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, and radius R&lt;sub&gt;500&lt;/sub&gt;, where the 500 suffix means that the quantity has been calculated up to a standard characteristic radius R&lt;sub&gt;500&lt;/sub&gt;, the radius within which the mean overdensity of the cluster is 500 times the critical density at the cluster redshift . The meta-catalog additionally furnishes information on overlaps between the input catalogs and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is made available so as to provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other multiwavelength studies. The catalogs and sub-catalogs included in this meta-catalog are listed in Table 1 of the reference paper, and come from the following references: &lt;pre&gt; Catalog Sub- Reference Title Catalog or CDS Cat. (Author) RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS) (Voges+, 1999) BCS BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I. (Ebeling+, 1998) eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) CIZA X-ray clusters behind the Milky Way CIZAI ApJ, 580, 774 (Ebeling+, 2002) CIZAII J/APJ/662/224 (Kocevski+, 2007) EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey (Gioia+, 1990) EMSS_1994 ApJS, 94, 583 (Gioia &amp; Luppino, 1994) EMSS_2004 ApJ, 608, 603 (Henry 2004) MACS ApJ, 553, 668 Massive Cluster Survey (Ebeling+, 2001) MACS_MJFV ApJS, 174, 117 (Maughan+, 2008) MACS_BRIGHT MNRAS, 407, 83 (Ebeling+, 2010) MACS_DIST ApJ, 661, L33 (Ebeling+, 2007) NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog (Henry+, 2006) NORAS/ REFLEX NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I. (Boehringer+, 2000) REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat (Boehringer+, 2004) SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP (Cruddace+, 2002) SHARC SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog (Romer+, 2000) SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog (Burke+, 2003) WARPS WARPSI J/ApJS/140/265 WARPS survey. VI. (Perlman+, 2002) WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII. (Horner+, 2008) 160SD 160SD J/ApJ/594/154 160 square degree ROSAT Survey (Mullis+, 2003) 400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey (Burenin+, 2007) 400SD_SER Serendipitous clusters 400SD_NONSER Not entirely serendipitous clusters &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/mcxc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcxc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=mcxc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/mcxc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MCXC [3]</TD>
            <TD>MCXC Meta-Catalog of X-Ray Detected Clusters of Galaxies</TD>
            <TD>The MCXC is the Meta-Catalog of the compiled properties of X-ray detected Clusters of galaxies. This very large catalog is based on publicly available ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogs. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogs have been carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster, the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, and radius R&lt;sub&gt;500&lt;/sub&gt;, where the 500 suffix means that the quantity has been calculated up to a standard characteristic radius R&lt;sub&gt;500&lt;/sub&gt;, the radius within which the mean overdensity of the cluster is 500 times the critical density at the cluster redshift . The meta-catalog additionally furnishes information on overlaps between the input catalogs and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is made available so as to provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other multiwavelength studies. The catalogs and sub-catalogs included in this meta-catalog are listed in Table 1 of the reference paper, and come from the following references: &lt;pre&gt; Catalog Sub- Reference Title Catalog or CDS Cat. (Author) RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS) (Voges+, 1999) BCS BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I. (Ebeling+, 1998) eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) CIZA X-ray clusters behind the Milky Way CIZAI ApJ, 580, 774 (Ebeling+, 2002) CIZAII J/APJ/662/224 (Kocevski+, 2007) EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey (Gioia+, 1990) EMSS_1994 ApJS, 94, 583 (Gioia &amp; Luppino, 1994) EMSS_2004 ApJ, 608, 603 (Henry 2004) MACS ApJ, 553, 668 Massive Cluster Survey (Ebeling+, 2001) MACS_MJFV ApJS, 174, 117 (Maughan+, 2008) MACS_BRIGHT MNRAS, 407, 83 (Ebeling+, 2010) MACS_DIST ApJ, 661, L33 (Ebeling+, 2007) NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog (Henry+, 2006) NORAS/ REFLEX NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I. (Boehringer+, 2000) REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat (Boehringer+, 2004) SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP (Cruddace+, 2002) SHARC SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog (Romer+, 2000) SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog (Burke+, 2003) WARPS WARPSI J/ApJS/140/265 WARPS survey. VI. (Perlman+, 2002) WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII. (Horner+, 2008) 160SD 160SD J/ApJ/594/154 160 square degree ROSAT Survey (Mullis+, 2003) 400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey (Burenin+, 2007) 400SD_SER Serendipitous clusters 400SD_NONSER Not entirely serendipitous clusters &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/mcxc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcxc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_mcxc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/mcxc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ULXNGCAT [1]</TD>
            <TD>Ultraluminous X-Ray Sources in Nearby Galaxies Catalog</TD>
            <TD>One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 &lt; log (M/M&lt;sub&gt;sun&lt;/sub&gt;) &lt; 11.4, and in star formation rate, 0.0002 &lt; SFR(M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;) &lt;= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, one per ~0.5 M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; star formation rate, and one per 57 Mpc&lt;sup&gt;3&lt;/sup&gt; corresponding to a luminosity density of ~2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, requiring a new population class to explain these extreme objects.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ulxngcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ulxngcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ulxngcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ulxngcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ULXNGCAT [2]</TD>
            <TD>Ultraluminous X-Ray Sources in Nearby Galaxies Catalog</TD>
            <TD>One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 &lt; log (M/M&lt;sub&gt;sun&lt;/sub&gt;) &lt; 11.4, and in star formation rate, 0.0002 &lt; SFR(M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;) &lt;= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, one per ~0.5 M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; star formation rate, and one per 57 Mpc&lt;sup&gt;3&lt;/sup&gt; corresponding to a luminosity density of ~2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, requiring a new population class to explain these extreme objects.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ulxngcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ulxngcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ulxngcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ulxngcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ULXNGCAT [3]</TD>
            <TD>Ultraluminous X-Ray Sources in Nearby Galaxies Catalog</TD>
            <TD>One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 &lt; log (M/M&lt;sub&gt;sun&lt;/sub&gt;) &lt; 11.4, and in star formation rate, 0.0002 &lt; SFR(M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;) &lt;= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, one per ~0.5 M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; star formation rate, and one per 57 Mpc&lt;sup&gt;3&lt;/sup&gt; corresponding to a luminosity density of ~2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, requiring a new population class to explain these extreme objects.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ulxngcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ulxngcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ulxngcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ulxngcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MCXC [1]</TD>
            <TD>MCXC Meta-Catalog of X-Ray Detected Clusters of Galaxies</TD>
            <TD>The MCXC is the Meta-Catalog of the compiled properties of X-ray detected Clusters of galaxies. This very large catalog is based on publicly available ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogs. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogs have been carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster, the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, and radius R&lt;sub&gt;500&lt;/sub&gt;, where the 500 suffix means that the quantity has been calculated up to a standard characteristic radius R&lt;sub&gt;500&lt;/sub&gt;, the radius within which the mean overdensity of the cluster is 500 times the critical density at the cluster redshift . The meta-catalog additionally furnishes information on overlaps between the input catalogs and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is made available so as to provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other multiwavelength studies. The catalogs and sub-catalogs included in this meta-catalog are listed in Table 1 of the reference paper, and come from the following references: &lt;pre&gt; Catalog Sub- Reference Title Catalog or CDS Cat. (Author) RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS) (Voges+, 1999) BCS BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I. (Ebeling+, 1998) eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) CIZA X-ray clusters behind the Milky Way CIZAI ApJ, 580, 774 (Ebeling+, 2002) CIZAII J/APJ/662/224 (Kocevski+, 2007) EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey (Gioia+, 1990) EMSS_1994 ApJS, 94, 583 (Gioia &amp; Luppino, 1994) EMSS_2004 ApJ, 608, 603 (Henry 2004) MACS ApJ, 553, 668 Massive Cluster Survey (Ebeling+, 2001) MACS_MJFV ApJS, 174, 117 (Maughan+, 2008) MACS_BRIGHT MNRAS, 407, 83 (Ebeling+, 2010) MACS_DIST ApJ, 661, L33 (Ebeling+, 2007) NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog (Henry+, 2006) NORAS/ REFLEX NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I. (Boehringer+, 2000) REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat (Boehringer+, 2004) SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP (Cruddace+, 2002) SHARC SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog (Romer+, 2000) SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog (Burke+, 2003) WARPS WARPSI J/ApJS/140/265 WARPS survey. VI. (Perlman+, 2002) WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII. (Horner+, 2008) 160SD 160SD J/ApJ/594/154 160 square degree ROSAT Survey (Mullis+, 2003) 400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey (Burenin+, 2007) 400SD_SER Serendipitous clusters 400SD_NONSER Not entirely serendipitous clusters &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/mcxc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcxc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=mcxc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/mcxc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MCXC [2]</TD>
            <TD>MCXC Meta-Catalog of X-Ray Detected Clusters of Galaxies</TD>
            <TD>The MCXC is the Meta-Catalog of the compiled properties of X-ray detected Clusters of galaxies. This very large catalog is based on publicly available ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogs. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogs have been carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster, the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, and radius R&lt;sub&gt;500&lt;/sub&gt;, where the 500 suffix means that the quantity has been calculated up to a standard characteristic radius R&lt;sub&gt;500&lt;/sub&gt;, the radius within which the mean overdensity of the cluster is 500 times the critical density at the cluster redshift . The meta-catalog additionally furnishes information on overlaps between the input catalogs and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is made available so as to provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other multiwavelength studies. The catalogs and sub-catalogs included in this meta-catalog are listed in Table 1 of the reference paper, and come from the following references: &lt;pre&gt; Catalog Sub- Reference Title Catalog or CDS Cat. (Author) RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS) (Voges+, 1999) BCS BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I. (Ebeling+, 1998) eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) CIZA X-ray clusters behind the Milky Way CIZAI ApJ, 580, 774 (Ebeling+, 2002) CIZAII J/APJ/662/224 (Kocevski+, 2007) EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey (Gioia+, 1990) EMSS_1994 ApJS, 94, 583 (Gioia &amp; Luppino, 1994) EMSS_2004 ApJ, 608, 603 (Henry 2004) MACS ApJ, 553, 668 Massive Cluster Survey (Ebeling+, 2001) MACS_MJFV ApJS, 174, 117 (Maughan+, 2008) MACS_BRIGHT MNRAS, 407, 83 (Ebeling+, 2010) MACS_DIST ApJ, 661, L33 (Ebeling+, 2007) NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog (Henry+, 2006) NORAS/ REFLEX NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I. (Boehringer+, 2000) REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat (Boehringer+, 2004) SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP (Cruddace+, 2002) SHARC SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog (Romer+, 2000) SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog (Burke+, 2003) WARPS WARPSI J/ApJS/140/265 WARPS survey. VI. (Perlman+, 2002) WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII. (Horner+, 2008) 160SD 160SD J/ApJ/594/154 160 square degree ROSAT Survey (Mullis+, 2003) 400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey (Burenin+, 2007) 400SD_SER Serendipitous clusters 400SD_NONSER Not entirely serendipitous clusters &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/mcxc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcxc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=mcxc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/mcxc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MCXC [3]</TD>
            <TD>MCXC Meta-Catalog of X-Ray Detected Clusters of Galaxies</TD>
            <TD>The MCXC is the Meta-Catalog of the compiled properties of X-ray detected Clusters of galaxies. This very large catalog is based on publicly available ROSAT All Sky Survey (RASS)-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and ROSAT serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogs. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogs have been carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster, the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalog, and standardised 0.1 - 2.4 keV band luminosity Lx&lt;sub&gt;500&lt;/sub&gt;, total mass M&lt;sub&gt;500&lt;/sub&gt;, and radius R&lt;sub&gt;500&lt;/sub&gt;, where the 500 suffix means that the quantity has been calculated up to a standard characteristic radius R&lt;sub&gt;500&lt;/sub&gt;, the radius within which the mean overdensity of the cluster is 500 times the critical density at the cluster redshift . The meta-catalog additionally furnishes information on overlaps between the input catalogs and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects. The MCXC is made available so as to provide maximum usefulness for X-ray, Sunyaev-Zel'dovich (SZ) and other multiwavelength studies. The catalogs and sub-catalogs included in this meta-catalog are listed in Table 1 of the reference paper, and come from the following references: &lt;pre&gt; Catalog Sub- Reference Title Catalog or CDS Cat. (Author) RASS IX/10 ROSAT All-Sky Bright Source Catalog (1RXS) (Voges+, 1999) BCS BCS J/MNRAS/301/881 ROSAT brightest cluster sample - I. (Ebeling+, 1998) eBCS J/MNRAS/318/333 Extended ROSAT Bright Cluster Sample (Ebeling+ 2000) CIZA X-ray clusters behind the Milky Way CIZAI ApJ, 580, 774 (Ebeling+, 2002) CIZAII J/APJ/662/224 (Kocevski+, 2007) EMSS ApJS, 72, 567 Einstein Extended Medium Sensitivity Survey (Gioia+, 1990) EMSS_1994 ApJS, 94, 583 (Gioia &amp; Luppino, 1994) EMSS_2004 ApJ, 608, 603 (Henry 2004) MACS ApJ, 553, 668 Massive Cluster Survey (Ebeling+, 2001) MACS_MJFV ApJS, 174, 117 (Maughan+, 2008) MACS_BRIGHT MNRAS, 407, 83 (Ebeling+, 2010) MACS_DIST ApJ, 661, L33 (Ebeling+, 2007) NEP NEP J/ApJS/162/304 ROSAT NEP X-ray source catalog (Henry+, 2006) NORAS/ REFLEX NORAS J/ApJS/129/435 NORAS galaxy cluster survey. I. (Boehringer+, 2000) REFLEX J/A+A/425/367 REFLEX Galaxy Cluster Survey Cat (Boehringer+, 2004) SGP SGP J/ApJS/140/239 Clusters of galaxies around SGP (Cruddace+, 2002) SHARC SHARC_BRIGHT J/ApJS/126/209 Bright SHARC survey cluster catalog (Romer+, 2000) SHARC_SOUTH J/MNRAS/341/1093 The Southern SHARC catalog (Burke+, 2003) WARPS WARPSI J/ApJS/140/265 WARPS survey. VI. (Perlman+, 2002) WARPSII J/ApJS/176/374 WARPS-II Cluster catalog. VII. (Horner+, 2008) 160SD 160SD J/ApJ/594/154 160 square degree ROSAT Survey (Mullis+, 2003) 400SD J/ApJS/172/561 400 square degree ROSAT Cluster Survey (Burenin+, 2007) 400SD_SER Serendipitous clusters 400SD_NONSER Not entirely serendipitous clusters &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/mcxc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mcxc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_mcxc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/mcxc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/496 [1]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#1</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/496</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/496 [2]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#2</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/496&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/496 [table4]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#table4</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/496&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/496 [KISSr]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#KISSr</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/496&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ULXNGCAT [1]</TD>
            <TD>Ultraluminous X-Ray Sources in Nearby Galaxies Catalog</TD>
            <TD>One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 &lt; log (M/M&lt;sub&gt;sun&lt;/sub&gt;) &lt; 11.4, and in star formation rate, 0.0002 &lt; SFR(M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;) &lt;= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, one per ~0.5 M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; star formation rate, and one per 57 Mpc&lt;sup&gt;3&lt;/sup&gt; corresponding to a luminosity density of ~2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, requiring a new population class to explain these extreme objects.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ulxngcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ulxngcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ulxngcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ulxngcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ULXNGCAT [2]</TD>
            <TD>Ultraluminous X-Ray Sources in Nearby Galaxies Catalog</TD>
            <TD>One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 &lt; log (M/M&lt;sub&gt;sun&lt;/sub&gt;) &lt; 11.4, and in star formation rate, 0.0002 &lt; SFR(M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;) &lt;= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, one per ~0.5 M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; star formation rate, and one per 57 Mpc&lt;sup&gt;3&lt;/sup&gt; corresponding to a luminosity density of ~2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, requiring a new population class to explain these extreme objects.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ulxngcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ulxngcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ulxngcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ulxngcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ULXNGCAT [3]</TD>
            <TD>Ultraluminous X-Ray Sources in Nearby Galaxies Catalog</TD>
            <TD>One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 &lt; log (M/M&lt;sub&gt;sun&lt;/sub&gt;) &lt; 11.4, and in star formation rate, 0.0002 &lt; SFR(M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;) &lt;= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, one per ~0.5 M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; star formation rate, and one per 57 Mpc&lt;sup&gt;3&lt;/sup&gt; corresponding to a luminosity density of ~2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, requiring a new population class to explain these extreme objects.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ulxngcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ulxngcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ulxngcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ulxngcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ATLASCSID [1]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascsid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascsid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=atlascsid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascsid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ATLASCSID [2]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascsid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascsid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=atlascsid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascsid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ATLASCSID [3]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascsid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascsid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_atlascsid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascsid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/496 [1]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#1</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/496</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/496 [2]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#2</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/496&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/496 [table4]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#table4</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/496&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/496 [KISSr]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#KISSr</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/496&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ULXNGCAT [1]</TD>
            <TD>Ultraluminous X-Ray Sources in Nearby Galaxies Catalog</TD>
            <TD>One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 &lt; log (M/M&lt;sub&gt;sun&lt;/sub&gt;) &lt; 11.4, and in star formation rate, 0.0002 &lt; SFR(M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;) &lt;= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, one per ~0.5 M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; star formation rate, and one per 57 Mpc&lt;sup&gt;3&lt;/sup&gt; corresponding to a luminosity density of ~2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, requiring a new population class to explain these extreme objects.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ulxngcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ulxngcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ulxngcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ulxngcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ULXNGCAT [2]</TD>
            <TD>Ultraluminous X-Ray Sources in Nearby Galaxies Catalog</TD>
            <TD>One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 &lt; log (M/M&lt;sub&gt;sun&lt;/sub&gt;) &lt; 11.4, and in star formation rate, 0.0002 &lt; SFR(M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;) &lt;= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, one per ~0.5 M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; star formation rate, and one per 57 Mpc&lt;sup&gt;3&lt;/sup&gt; corresponding to a luminosity density of ~2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, requiring a new population class to explain these extreme objects.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ulxngcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ulxngcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ulxngcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ulxngcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ULXNGCAT [3]</TD>
            <TD>Ultraluminous X-Ray Sources in Nearby Galaxies Catalog</TD>
            <TD>One hundred and seven ultraluminous X-ray sources (ULXs) with 0.3-10.0 keV luminosities in excess of 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; are identified in a complete sample of 127 nearby galaxies. The sample includes all galaxies within 14.5 Mpc above the completeness limits of both the Uppsala Galaxy Catalogue and the Infrared Astronomical Satellite survey. The galaxy sample spans all Hubble types, a four-decade range in mass, 7.5 &lt; log (M/M&lt;sub&gt;sun&lt;/sub&gt;) &lt; 11.4, and in star formation rate, 0.0002 &lt; SFR(M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt;) &lt;= 3.6. ULXs are detected in this sample at rates of one per 3.2 x 10&lt;sup&gt;10&lt;/sup&gt; M&lt;sub&gt;sun&lt;/sub&gt;, one per ~0.5 M&lt;sub&gt;sun&lt;/sub&gt; yr&lt;sup&gt;-1&lt;/sup&gt; star formation rate, and one per 57 Mpc&lt;sup&gt;3&lt;/sup&gt; corresponding to a luminosity density of ~2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-3&lt;/sup&gt;. At these rates, the authors estimate as many as 19 additional ULXs remain undetected in fainter dwarf galaxies within the survey volume. An estimated 14 objects, or 13%, of the 107 ULX candidates are expected to be background sources. The differential ULX luminosity function shows a power-law slope alpha ~ -0.8 to -2.0 with an exponential cutoff at ~20 x 10&lt;sup&gt;39&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; with precise values depending on the model and on whether the ULX luminosities are estimated from their observed numbers of counts or, for a subset of candidates, from their spectral shapes. Extrapolating the observed luminosity function predicts at most one very luminous ULX, L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, within a distance as small as 100 Mpc. The luminosity distribution of ULXs within the local universe cannot account for the recent claims of luminosities in excess of 2 x 10&lt;sup&gt;41&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, requiring a new population class to explain these extreme objects.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ulxngcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ulxngcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ulxngcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ulxngcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/496 [1]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#1</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/496</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/496 [2]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#2</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/496&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/496 [table4]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#table4</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/496&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/496 [KISSr]</TD>
            <TD>KISS emission-line galaxy candidates (Jangren+, 2005)</TD>
            <TD>We obtained spectra for 315 KISS objects at the MDM 2.4m telescope over the course of three observing runs in 2002 April, 2003 April, and 2004 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496#KISSr</TD>
            <TD>2011-09-14T19:48:56Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/496</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/496&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/496</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ATLASCSID [1]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascsid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascsid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=atlascsid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascsid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ATLASCSID [2]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascsid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascsid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=atlascsid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascsid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ATLASCSID [3]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascsid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascsid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_atlascsid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascsid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/147/1 [1]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#1</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/147/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/147/1 [2]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#2</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table4]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table4</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table1]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table1</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table3]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table3</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table2]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table2</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table5]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table5</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/312/442 [1]</TD>
            <TD>UV-selected galaxy redshift survey. II. (Sullivan+, 2000)</TD>
            <TD>We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000{AA} from the FOCA balloon-borne imaging camera of Milliard et al. (1992A&amp;A...257...24M). This work represents an extension of the initial study by Treyer et al. (Cat. &lt;J/MNRAS/300/303&gt;). Our enlarged catalogue contains 433 sources (~3 times as many as in our earlier study) across two FOCA fields. 273 of these are galaxies, nearly all with redshifts z~0-0.4. Nebular emission-line measurements are available for 216 galaxies, allowing us to address issues of excitation, reddening and metallicity. The UV and H{alpha} luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0&lt;z&lt;0.4. Our data are more consistent with a modest evolutionary trend, as suggested by recent redshift survey results. Investigating the emission-line properties, we find no evidence for a significant number of AGN in our sample; most UV-selected sources to z~0.4 are intense star-forming galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442#1</TD>
            <TD>2012-11-13T14:10:02Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/312/442</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/442</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/312/442 [2]</TD>
            <TD>UV-selected galaxy redshift survey. II. (Sullivan+, 2000)</TD>
            <TD>We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000{AA} from the FOCA balloon-borne imaging camera of Milliard et al. (1992A&amp;A...257...24M). This work represents an extension of the initial study by Treyer et al. (Cat. &lt;J/MNRAS/300/303&gt;). Our enlarged catalogue contains 433 sources (~3 times as many as in our earlier study) across two FOCA fields. 273 of these are galaxies, nearly all with redshifts z~0-0.4. Nebular emission-line measurements are available for 216 galaxies, allowing us to address issues of excitation, reddening and metallicity. The UV and H{alpha} luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0&lt;z&lt;0.4. Our data are more consistent with a modest evolutionary trend, as suggested by recent redshift survey results. Investigating the emission-line properties, we find no evidence for a significant number of AGN in our sample; most UV-selected sources to z~0.4 are intense star-forming galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442#2</TD>
            <TD>2012-11-13T14:10:02Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/312/442&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/442</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/312/442 [table7]</TD>
            <TD>UV-selected galaxy redshift survey. II. (Sullivan+, 2000)</TD>
            <TD>We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000{AA} from the FOCA balloon-borne imaging camera of Milliard et al. (1992A&amp;A...257...24M). This work represents an extension of the initial study by Treyer et al. (Cat. &lt;J/MNRAS/300/303&gt;). Our enlarged catalogue contains 433 sources (~3 times as many as in our earlier study) across two FOCA fields. 273 of these are galaxies, nearly all with redshifts z~0-0.4. Nebular emission-line measurements are available for 216 galaxies, allowing us to address issues of excitation, reddening and metallicity. The UV and H{alpha} luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0&lt;z&lt;0.4. Our data are more consistent with a modest evolutionary trend, as suggested by recent redshift survey results. Investigating the emission-line properties, we find no evidence for a significant number of AGN in our sample; most UV-selected sources to z~0.4 are intense star-forming galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442#table7</TD>
            <TD>2012-11-13T14:10:02Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/312/442&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/442</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/147/1 [1]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#1</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/147/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/147/1 [2]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#2</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table4]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table4</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table1]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table1</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table3]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table3</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table2]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table2</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table5]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table5</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ATLASCSID [1]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascsid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascsid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=atlascsid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascsid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ATLASCSID [2]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascsid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascsid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=atlascsid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascsid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ATLASCSID [3]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE ID and Classification Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified (see the companion table ATLASCSCPT), corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 726 radio sources and their cross-identifications at optical and infrared wavelengths which were given in Table 6 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascsid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascsid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_atlascsid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascsid.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ATESP1P4GH [1]</TD>
            <TD>Australia Telescope ESO Slice Project 1.4-GHz Source Catalog</TD>
            <TD>The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&amp;A, 325, 954) galaxy redshift survey. This 26-degree&lt;sup&gt;2&lt;/sup&gt; region is centered at Declination -40 degrees, and ranges in RA from 22&lt;sup&gt;h&lt;/sup&gt; 30&lt;sup&gt;m&lt;/sup&gt; to 01&lt;sup&gt;h&lt;/sup&gt; 15&lt;sup&gt;m&lt;/sup&gt;. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atesp1p4gh#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atesp1p4gh</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=atesp1p4gh&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atesp1p4gh.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ATESP1P4GH [2]</TD>
            <TD>Australia Telescope ESO Slice Project 1.4-GHz Source Catalog</TD>
            <TD>The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&amp;A, 325, 954) galaxy redshift survey. This 26-degree&lt;sup&gt;2&lt;/sup&gt; region is centered at Declination -40 degrees, and ranges in RA from 22&lt;sup&gt;h&lt;/sup&gt; 30&lt;sup&gt;m&lt;/sup&gt; to 01&lt;sup&gt;h&lt;/sup&gt; 15&lt;sup&gt;m&lt;/sup&gt;. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atesp1p4gh#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atesp1p4gh</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=atesp1p4gh&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atesp1p4gh.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ATESP1P4GH [3]</TD>
            <TD>Australia Telescope ESO Slice Project 1.4-GHz Source Catalog</TD>
            <TD>The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&amp;A, 325, 954) galaxy redshift survey. This 26-degree&lt;sup&gt;2&lt;/sup&gt; region is centered at Declination -40 degrees, and ranges in RA from 22&lt;sup&gt;h&lt;/sup&gt; 30&lt;sup&gt;m&lt;/sup&gt; to 01&lt;sup&gt;h&lt;/sup&gt; 15&lt;sup&gt;m&lt;/sup&gt;. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atesp1p4gh#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atesp1p4gh</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_atesp1p4gh&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atesp1p4gh.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/147/1 [1]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#1</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/147/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/147/1 [2]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#2</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table4]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table4</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table1]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table1</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table3]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table3</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table2]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table2</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/147/1 [table5]</TD>
            <TD>Classification of nearby galaxies (Conselice+, 2003)</TD>
            <TD>A major problem in extragalactic astronomy is the inability to distinguish in a robust, physical, and model-independent way how galaxy populations are physically related to each other and to their formation histories. A similar, but distinct, and also long-standing question is whether the structural appearances of galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation modes and can be used as a robust classification system. These parameters quantitatively measure: the concentration (C), asymmetry (A), and clumpiness (S) of a galaxy's stellar light distribution. When combined into a three-dimensional "CAS" volume all major classes of galaxies in various phases of evolution are cleanly distinguished. We argue that these three parameters correlate with important modes of galaxy evolution: star formation and major merging activity. This is argued through the strong correlation of H{alpha} equivalent width and broadband colors with the clumpiness parameter S, the uniquely large asymmetries of 66 galaxies undergoing mergers, and the correlation of bulge to total light ratios, and stellar masses, with the concentration index. As an obvious goal is to use this system at high redshifts to trace evolution, we demonstrate that these parameters can be measured, within a reasonable and quantifiable uncertainty with available data out to z~3 using the Hubble Space Telescope GOODS ACS and Hubble Deep Field images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1#table5</TD>
            <TD>2011-09-14T19:49:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/147/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/147/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/147/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GCPTSRCCXO [1]</TD>
            <TD>Chandra Point Sources in 18 Distant Galaxy Clusters</TD>
            <TD>With the superb angular resolution of the Chandra Observatory, it is now possible to detect X-ray point sources, either embedded in galaxy clusters or along the cluster line of sight, which could not be resolved by previous instruments. This now allows studies of source counts in distant cluster fields. The authors want to analyze the inner region of clusters of galaxies to check for the presence of any over-density of X-ray point sources embedded in the gas diffuse emission. These point sources are possible AGN belonging to the clusters and could contaminate the cluster emission. The authors used a sample of 18 distant (0.25 &lt; z &lt; 1.01) galaxy clusters from the Chandra archive to construct the log N - log S relation, in both the soft and hard energy bands, for the X-ray point sources detected in the central cluster region to be compared with the counts of point sources detected in similarly deep fields without clusters. The authors find a ~2-sigma excess of cluster region sources at the bright end of the log N - log S distributon. The radial distribution of the brightest X-ray point sources confirms this excess and indicates that it is confined to the inner 0.5 Mpc of the cluster region. The results suggest the possible existence of X-ray sources belonging to the cluster (most probably AGN, given their 0.5-10 keV luminosity ranging from 10&lt;sup&gt;43&lt;/sup&gt; to 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;): on average one every three clusters. Unlike previous studies, which have mainly investigated the point-source population in the vicinity of the galaxy clusters, the present study analyzes the content of point sources within the 1 Mpc region covered by the cluster extent. This work confirms the findings of other investigators who analyzed the central 1 Mpc region of more massive clusters and/or groups in a similar redshift range. The X-ray source excess found here is much smaller than the excess of radio galaxies found recently in high-z X-ray selected clusters, possibly due to the better sensitivity of the radio observations. The properties of the clusters and of the Chandra exposures in which they were observed are given in Table 1 of the reference paper, and are reproduced below: &lt;pre&gt; Cluster Namne z RA (J2000) Dec ObsID ACIS Mode Exp N_H L_sb L_hb h m s d ' " ks [units are below] Abell 2125 0.246 15 41 12 +66 16 01 2207 I VF 79.7 2.77 0.13 0.56 ZW CL 1454.8+2233 0.258 14 57 15 +22 20 33 4192 I VF 91.4 3.22 0.23 0.74 MS 1008.1-1224 0.302 10 10 32 -12 39 23 926 I VF 44.2 6.74 0.44 1.57 ZW CL 0024.0+1652 0.394 00 26 35 +17 09 39 929 S VF 36.7 4.19 0.34 2.22 MS 1621.5+2640 0.426 16 23 36 +26 34 21 546 I F 30.0 3.59 0.81 3.41 RXJ 1701.3+6414 0.453 17 01 24 +64 14 10 547 I VF 49.5 2.59 0.64 2.67 CL 1641+4001 0.464 16 41 53 +40 01 46 3575 I VF 44.0 1.02 0.67 2.62 V 1524.6+0957 0.516 15 24 40 +09 57 48 1664 I VF 49.9 2.92 0.89 3.29 MS 0451.6-0305 0.539 04 54 12 -03 00 53 902 S F 41.5 5.18 0.73 4.12 V 1121+2327 0.562 11 20 57 +23 26 27 1660 I VF 66.9 1.30 0.73 3.00 MS 2053.7-0449 0.583 20 56 21 -04 37 51 1667 I VF 43.5 4.96 1.32 4.91 V 1221+4918 0.700 12 21 26 +49 18 30 1662 I VF 79.4 1.44 1.18 4.62 MS 1137.5+6625 0.782 11 40 22 +66 08 18 536 I VF 117.5 1.18 0.81 4.04 RDCSJ 1317+2911 0.805 13 17 21 +29 11 19 2228 I VF 111.3 1.04 0.85 3.59 RDCSJ 1350+6007 0.805 13 50 48 +60 06 54 2229 I VF 58.3 1.76 1.77 7.26 RXJ 1716.4+6708 0.813 17 16 49 +67 08 26 548 I F 51.5 3.71 2.17 9.45 MS 1054.4-0321 0.830 10 56 59 -03 37 37 512 S F 67.5 3.67 1.07 6.61 WARPJ 1415.1+3612 1.013 14 15 11 +36 12 00 4163 I VF 89.2 1.10 1.93 7.54 &lt;/pre&gt; where Exp is the Chandra exposure time in ks corresponding to the nominal exposure filtered to exclude time periods of high background, N_H is the Galactic hydrogen column density in the direction of the cluster of galaxies, in units of 10&lt;sup&gt;20&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;, and L_sb and L_hb are the limiting luminosities in units of 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for point sources in the clusters in the 0.5-2.0 kev and 2-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/gcptsrccxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gcptsrccxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=gcptsrccxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/gcptsrccxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GCPTSRCCXO [2]</TD>
            <TD>Chandra Point Sources in 18 Distant Galaxy Clusters</TD>
            <TD>With the superb angular resolution of the Chandra Observatory, it is now possible to detect X-ray point sources, either embedded in galaxy clusters or along the cluster line of sight, which could not be resolved by previous instruments. This now allows studies of source counts in distant cluster fields. The authors want to analyze the inner region of clusters of galaxies to check for the presence of any over-density of X-ray point sources embedded in the gas diffuse emission. These point sources are possible AGN belonging to the clusters and could contaminate the cluster emission. The authors used a sample of 18 distant (0.25 &lt; z &lt; 1.01) galaxy clusters from the Chandra archive to construct the log N - log S relation, in both the soft and hard energy bands, for the X-ray point sources detected in the central cluster region to be compared with the counts of point sources detected in similarly deep fields without clusters. The authors find a ~2-sigma excess of cluster region sources at the bright end of the log N - log S distributon. The radial distribution of the brightest X-ray point sources confirms this excess and indicates that it is confined to the inner 0.5 Mpc of the cluster region. The results suggest the possible existence of X-ray sources belonging to the cluster (most probably AGN, given their 0.5-10 keV luminosity ranging from 10&lt;sup&gt;43&lt;/sup&gt; to 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;): on average one every three clusters. Unlike previous studies, which have mainly investigated the point-source population in the vicinity of the galaxy clusters, the present study analyzes the content of point sources within the 1 Mpc region covered by the cluster extent. This work confirms the findings of other investigators who analyzed the central 1 Mpc region of more massive clusters and/or groups in a similar redshift range. The X-ray source excess found here is much smaller than the excess of radio galaxies found recently in high-z X-ray selected clusters, possibly due to the better sensitivity of the radio observations. The properties of the clusters and of the Chandra exposures in which they were observed are given in Table 1 of the reference paper, and are reproduced below: &lt;pre&gt; Cluster Namne z RA (J2000) Dec ObsID ACIS Mode Exp N_H L_sb L_hb h m s d ' " ks [units are below] Abell 2125 0.246 15 41 12 +66 16 01 2207 I VF 79.7 2.77 0.13 0.56 ZW CL 1454.8+2233 0.258 14 57 15 +22 20 33 4192 I VF 91.4 3.22 0.23 0.74 MS 1008.1-1224 0.302 10 10 32 -12 39 23 926 I VF 44.2 6.74 0.44 1.57 ZW CL 0024.0+1652 0.394 00 26 35 +17 09 39 929 S VF 36.7 4.19 0.34 2.22 MS 1621.5+2640 0.426 16 23 36 +26 34 21 546 I F 30.0 3.59 0.81 3.41 RXJ 1701.3+6414 0.453 17 01 24 +64 14 10 547 I VF 49.5 2.59 0.64 2.67 CL 1641+4001 0.464 16 41 53 +40 01 46 3575 I VF 44.0 1.02 0.67 2.62 V 1524.6+0957 0.516 15 24 40 +09 57 48 1664 I VF 49.9 2.92 0.89 3.29 MS 0451.6-0305 0.539 04 54 12 -03 00 53 902 S F 41.5 5.18 0.73 4.12 V 1121+2327 0.562 11 20 57 +23 26 27 1660 I VF 66.9 1.30 0.73 3.00 MS 2053.7-0449 0.583 20 56 21 -04 37 51 1667 I VF 43.5 4.96 1.32 4.91 V 1221+4918 0.700 12 21 26 +49 18 30 1662 I VF 79.4 1.44 1.18 4.62 MS 1137.5+6625 0.782 11 40 22 +66 08 18 536 I VF 117.5 1.18 0.81 4.04 RDCSJ 1317+2911 0.805 13 17 21 +29 11 19 2228 I VF 111.3 1.04 0.85 3.59 RDCSJ 1350+6007 0.805 13 50 48 +60 06 54 2229 I VF 58.3 1.76 1.77 7.26 RXJ 1716.4+6708 0.813 17 16 49 +67 08 26 548 I F 51.5 3.71 2.17 9.45 MS 1054.4-0321 0.830 10 56 59 -03 37 37 512 S F 67.5 3.67 1.07 6.61 WARPJ 1415.1+3612 1.013 14 15 11 +36 12 00 4163 I VF 89.2 1.10 1.93 7.54 &lt;/pre&gt; where Exp is the Chandra exposure time in ks corresponding to the nominal exposure filtered to exclude time periods of high background, N_H is the Galactic hydrogen column density in the direction of the cluster of galaxies, in units of 10&lt;sup&gt;20&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;, and L_sb and L_hb are the limiting luminosities in units of 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for point sources in the clusters in the 0.5-2.0 kev and 2-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/gcptsrccxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gcptsrccxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=gcptsrccxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/gcptsrccxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GCPTSRCCXO [3]</TD>
            <TD>Chandra Point Sources in 18 Distant Galaxy Clusters</TD>
            <TD>With the superb angular resolution of the Chandra Observatory, it is now possible to detect X-ray point sources, either embedded in galaxy clusters or along the cluster line of sight, which could not be resolved by previous instruments. This now allows studies of source counts in distant cluster fields. The authors want to analyze the inner region of clusters of galaxies to check for the presence of any over-density of X-ray point sources embedded in the gas diffuse emission. These point sources are possible AGN belonging to the clusters and could contaminate the cluster emission. The authors used a sample of 18 distant (0.25 &lt; z &lt; 1.01) galaxy clusters from the Chandra archive to construct the log N - log S relation, in both the soft and hard energy bands, for the X-ray point sources detected in the central cluster region to be compared with the counts of point sources detected in similarly deep fields without clusters. The authors find a ~2-sigma excess of cluster region sources at the bright end of the log N - log S distributon. The radial distribution of the brightest X-ray point sources confirms this excess and indicates that it is confined to the inner 0.5 Mpc of the cluster region. The results suggest the possible existence of X-ray sources belonging to the cluster (most probably AGN, given their 0.5-10 keV luminosity ranging from 10&lt;sup&gt;43&lt;/sup&gt; to 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;): on average one every three clusters. Unlike previous studies, which have mainly investigated the point-source population in the vicinity of the galaxy clusters, the present study analyzes the content of point sources within the 1 Mpc region covered by the cluster extent. This work confirms the findings of other investigators who analyzed the central 1 Mpc region of more massive clusters and/or groups in a similar redshift range. The X-ray source excess found here is much smaller than the excess of radio galaxies found recently in high-z X-ray selected clusters, possibly due to the better sensitivity of the radio observations. The properties of the clusters and of the Chandra exposures in which they were observed are given in Table 1 of the reference paper, and are reproduced below: &lt;pre&gt; Cluster Namne z RA (J2000) Dec ObsID ACIS Mode Exp N_H L_sb L_hb h m s d ' " ks [units are below] Abell 2125 0.246 15 41 12 +66 16 01 2207 I VF 79.7 2.77 0.13 0.56 ZW CL 1454.8+2233 0.258 14 57 15 +22 20 33 4192 I VF 91.4 3.22 0.23 0.74 MS 1008.1-1224 0.302 10 10 32 -12 39 23 926 I VF 44.2 6.74 0.44 1.57 ZW CL 0024.0+1652 0.394 00 26 35 +17 09 39 929 S VF 36.7 4.19 0.34 2.22 MS 1621.5+2640 0.426 16 23 36 +26 34 21 546 I F 30.0 3.59 0.81 3.41 RXJ 1701.3+6414 0.453 17 01 24 +64 14 10 547 I VF 49.5 2.59 0.64 2.67 CL 1641+4001 0.464 16 41 53 +40 01 46 3575 I VF 44.0 1.02 0.67 2.62 V 1524.6+0957 0.516 15 24 40 +09 57 48 1664 I VF 49.9 2.92 0.89 3.29 MS 0451.6-0305 0.539 04 54 12 -03 00 53 902 S F 41.5 5.18 0.73 4.12 V 1121+2327 0.562 11 20 57 +23 26 27 1660 I VF 66.9 1.30 0.73 3.00 MS 2053.7-0449 0.583 20 56 21 -04 37 51 1667 I VF 43.5 4.96 1.32 4.91 V 1221+4918 0.700 12 21 26 +49 18 30 1662 I VF 79.4 1.44 1.18 4.62 MS 1137.5+6625 0.782 11 40 22 +66 08 18 536 I VF 117.5 1.18 0.81 4.04 RDCSJ 1317+2911 0.805 13 17 21 +29 11 19 2228 I VF 111.3 1.04 0.85 3.59 RDCSJ 1350+6007 0.805 13 50 48 +60 06 54 2229 I VF 58.3 1.76 1.77 7.26 RXJ 1716.4+6708 0.813 17 16 49 +67 08 26 548 I F 51.5 3.71 2.17 9.45 MS 1054.4-0321 0.830 10 56 59 -03 37 37 512 S F 67.5 3.67 1.07 6.61 WARPJ 1415.1+3612 1.013 14 15 11 +36 12 00 4163 I VF 89.2 1.10 1.93 7.54 &lt;/pre&gt; where Exp is the Chandra exposure time in ks corresponding to the nominal exposure filtered to exclude time periods of high background, N_H is the Galactic hydrogen column density in the direction of the cluster of galaxies, in units of 10&lt;sup&gt;20&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;, and L_sb and L_hb are the limiting luminosities in units of 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for point sources in the clusters in the 0.5-2.0 kev and 2-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/gcptsrccxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gcptsrccxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_gcptsrccxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/gcptsrccxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/1017 [1]</TD>
            <TD>Northern Optical Cluster Survey. IV. (Lopes+, 2005)</TD>
            <TD>This paper presents a galaxy cluster catalog that is an extension of those presented in Papers II (Gal et al., 2003, Cat. &lt;J/AJ/125/2064&gt;) and III (Gal et al., 2005, in prep.). It covers 2700{deg}^2^ of digitized Second Palomar Observatory Sky Survey (DPOSS) data and is expected to be complete for rich clusters out to z~0.3, with clusters still detected to z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017#1</TD>
            <TD>2011-09-14T19:53:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/1017</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1017</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/1017 [2]</TD>
            <TD>Northern Optical Cluster Survey. IV. (Lopes+, 2005)</TD>
            <TD>This paper presents a galaxy cluster catalog that is an extension of those presented in Papers II (Gal et al., 2003, Cat. &lt;J/AJ/125/2064&gt;) and III (Gal et al., 2005, in prep.). It covers 2700{deg}^2^ of digitized Second Palomar Observatory Sky Survey (DPOSS) data and is expected to be complete for rich clusters out to z~0.3, with clusters still detected to z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017#2</TD>
            <TD>2011-09-14T19:53:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/1017&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1017</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/1017 [table1]</TD>
            <TD>Northern Optical Cluster Survey. IV. (Lopes+, 2005)</TD>
            <TD>This paper presents a galaxy cluster catalog that is an extension of those presented in Papers II (Gal et al., 2003, Cat. &lt;J/AJ/125/2064&gt;) and III (Gal et al., 2005, in prep.). It covers 2700{deg}^2^ of digitized Second Palomar Observatory Sky Survey (DPOSS) data and is expected to be complete for rich clusters out to z~0.3, with clusters still detected to z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017#table1</TD>
            <TD>2011-09-14T19:53:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/1017&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1017</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ATESP1P4GH [1]</TD>
            <TD>Australia Telescope ESO Slice Project 1.4-GHz Source Catalog</TD>
            <TD>The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&amp;A, 325, 954) galaxy redshift survey. This 26-degree&lt;sup&gt;2&lt;/sup&gt; region is centered at Declination -40 degrees, and ranges in RA from 22&lt;sup&gt;h&lt;/sup&gt; 30&lt;sup&gt;m&lt;/sup&gt; to 01&lt;sup&gt;h&lt;/sup&gt; 15&lt;sup&gt;m&lt;/sup&gt;. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atesp1p4gh#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atesp1p4gh</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=atesp1p4gh&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atesp1p4gh.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ATESP1P4GH [2]</TD>
            <TD>Australia Telescope ESO Slice Project 1.4-GHz Source Catalog</TD>
            <TD>The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&amp;A, 325, 954) galaxy redshift survey. This 26-degree&lt;sup&gt;2&lt;/sup&gt; region is centered at Declination -40 degrees, and ranges in RA from 22&lt;sup&gt;h&lt;/sup&gt; 30&lt;sup&gt;m&lt;/sup&gt; to 01&lt;sup&gt;h&lt;/sup&gt; 15&lt;sup&gt;m&lt;/sup&gt;. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atesp1p4gh#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atesp1p4gh</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=atesp1p4gh&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atesp1p4gh.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ATESP1P4GH [3]</TD>
            <TD>Australia Telescope ESO Slice Project 1.4-GHz Source Catalog</TD>
            <TD>The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&amp;A, 325, 954) galaxy redshift survey. This 26-degree&lt;sup&gt;2&lt;/sup&gt; region is centered at Declination -40 degrees, and ranges in RA from 22&lt;sup&gt;h&lt;/sup&gt; 30&lt;sup&gt;m&lt;/sup&gt; to 01&lt;sup&gt;h&lt;/sup&gt; 15&lt;sup&gt;m&lt;/sup&gt;. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atesp1p4gh#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atesp1p4gh</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_atesp1p4gh&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atesp1p4gh.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GCPTSRCCXO [1]</TD>
            <TD>Chandra Point Sources in 18 Distant Galaxy Clusters</TD>
            <TD>With the superb angular resolution of the Chandra Observatory, it is now possible to detect X-ray point sources, either embedded in galaxy clusters or along the cluster line of sight, which could not be resolved by previous instruments. This now allows studies of source counts in distant cluster fields. The authors want to analyze the inner region of clusters of galaxies to check for the presence of any over-density of X-ray point sources embedded in the gas diffuse emission. These point sources are possible AGN belonging to the clusters and could contaminate the cluster emission. The authors used a sample of 18 distant (0.25 &lt; z &lt; 1.01) galaxy clusters from the Chandra archive to construct the log N - log S relation, in both the soft and hard energy bands, for the X-ray point sources detected in the central cluster region to be compared with the counts of point sources detected in similarly deep fields without clusters. The authors find a ~2-sigma excess of cluster region sources at the bright end of the log N - log S distributon. The radial distribution of the brightest X-ray point sources confirms this excess and indicates that it is confined to the inner 0.5 Mpc of the cluster region. The results suggest the possible existence of X-ray sources belonging to the cluster (most probably AGN, given their 0.5-10 keV luminosity ranging from 10&lt;sup&gt;43&lt;/sup&gt; to 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;): on average one every three clusters. Unlike previous studies, which have mainly investigated the point-source population in the vicinity of the galaxy clusters, the present study analyzes the content of point sources within the 1 Mpc region covered by the cluster extent. This work confirms the findings of other investigators who analyzed the central 1 Mpc region of more massive clusters and/or groups in a similar redshift range. The X-ray source excess found here is much smaller than the excess of radio galaxies found recently in high-z X-ray selected clusters, possibly due to the better sensitivity of the radio observations. The properties of the clusters and of the Chandra exposures in which they were observed are given in Table 1 of the reference paper, and are reproduced below: &lt;pre&gt; Cluster Namne z RA (J2000) Dec ObsID ACIS Mode Exp N_H L_sb L_hb h m s d ' " ks [units are below] Abell 2125 0.246 15 41 12 +66 16 01 2207 I VF 79.7 2.77 0.13 0.56 ZW CL 1454.8+2233 0.258 14 57 15 +22 20 33 4192 I VF 91.4 3.22 0.23 0.74 MS 1008.1-1224 0.302 10 10 32 -12 39 23 926 I VF 44.2 6.74 0.44 1.57 ZW CL 0024.0+1652 0.394 00 26 35 +17 09 39 929 S VF 36.7 4.19 0.34 2.22 MS 1621.5+2640 0.426 16 23 36 +26 34 21 546 I F 30.0 3.59 0.81 3.41 RXJ 1701.3+6414 0.453 17 01 24 +64 14 10 547 I VF 49.5 2.59 0.64 2.67 CL 1641+4001 0.464 16 41 53 +40 01 46 3575 I VF 44.0 1.02 0.67 2.62 V 1524.6+0957 0.516 15 24 40 +09 57 48 1664 I VF 49.9 2.92 0.89 3.29 MS 0451.6-0305 0.539 04 54 12 -03 00 53 902 S F 41.5 5.18 0.73 4.12 V 1121+2327 0.562 11 20 57 +23 26 27 1660 I VF 66.9 1.30 0.73 3.00 MS 2053.7-0449 0.583 20 56 21 -04 37 51 1667 I VF 43.5 4.96 1.32 4.91 V 1221+4918 0.700 12 21 26 +49 18 30 1662 I VF 79.4 1.44 1.18 4.62 MS 1137.5+6625 0.782 11 40 22 +66 08 18 536 I VF 117.5 1.18 0.81 4.04 RDCSJ 1317+2911 0.805 13 17 21 +29 11 19 2228 I VF 111.3 1.04 0.85 3.59 RDCSJ 1350+6007 0.805 13 50 48 +60 06 54 2229 I VF 58.3 1.76 1.77 7.26 RXJ 1716.4+6708 0.813 17 16 49 +67 08 26 548 I F 51.5 3.71 2.17 9.45 MS 1054.4-0321 0.830 10 56 59 -03 37 37 512 S F 67.5 3.67 1.07 6.61 WARPJ 1415.1+3612 1.013 14 15 11 +36 12 00 4163 I VF 89.2 1.10 1.93 7.54 &lt;/pre&gt; where Exp is the Chandra exposure time in ks corresponding to the nominal exposure filtered to exclude time periods of high background, N_H is the Galactic hydrogen column density in the direction of the cluster of galaxies, in units of 10&lt;sup&gt;20&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;, and L_sb and L_hb are the limiting luminosities in units of 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for point sources in the clusters in the 0.5-2.0 kev and 2-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/gcptsrccxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gcptsrccxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=gcptsrccxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/gcptsrccxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GCPTSRCCXO [2]</TD>
            <TD>Chandra Point Sources in 18 Distant Galaxy Clusters</TD>
            <TD>With the superb angular resolution of the Chandra Observatory, it is now possible to detect X-ray point sources, either embedded in galaxy clusters or along the cluster line of sight, which could not be resolved by previous instruments. This now allows studies of source counts in distant cluster fields. The authors want to analyze the inner region of clusters of galaxies to check for the presence of any over-density of X-ray point sources embedded in the gas diffuse emission. These point sources are possible AGN belonging to the clusters and could contaminate the cluster emission. The authors used a sample of 18 distant (0.25 &lt; z &lt; 1.01) galaxy clusters from the Chandra archive to construct the log N - log S relation, in both the soft and hard energy bands, for the X-ray point sources detected in the central cluster region to be compared with the counts of point sources detected in similarly deep fields without clusters. The authors find a ~2-sigma excess of cluster region sources at the bright end of the log N - log S distributon. The radial distribution of the brightest X-ray point sources confirms this excess and indicates that it is confined to the inner 0.5 Mpc of the cluster region. The results suggest the possible existence of X-ray sources belonging to the cluster (most probably AGN, given their 0.5-10 keV luminosity ranging from 10&lt;sup&gt;43&lt;/sup&gt; to 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;): on average one every three clusters. Unlike previous studies, which have mainly investigated the point-source population in the vicinity of the galaxy clusters, the present study analyzes the content of point sources within the 1 Mpc region covered by the cluster extent. This work confirms the findings of other investigators who analyzed the central 1 Mpc region of more massive clusters and/or groups in a similar redshift range. The X-ray source excess found here is much smaller than the excess of radio galaxies found recently in high-z X-ray selected clusters, possibly due to the better sensitivity of the radio observations. The properties of the clusters and of the Chandra exposures in which they were observed are given in Table 1 of the reference paper, and are reproduced below: &lt;pre&gt; Cluster Namne z RA (J2000) Dec ObsID ACIS Mode Exp N_H L_sb L_hb h m s d ' " ks [units are below] Abell 2125 0.246 15 41 12 +66 16 01 2207 I VF 79.7 2.77 0.13 0.56 ZW CL 1454.8+2233 0.258 14 57 15 +22 20 33 4192 I VF 91.4 3.22 0.23 0.74 MS 1008.1-1224 0.302 10 10 32 -12 39 23 926 I VF 44.2 6.74 0.44 1.57 ZW CL 0024.0+1652 0.394 00 26 35 +17 09 39 929 S VF 36.7 4.19 0.34 2.22 MS 1621.5+2640 0.426 16 23 36 +26 34 21 546 I F 30.0 3.59 0.81 3.41 RXJ 1701.3+6414 0.453 17 01 24 +64 14 10 547 I VF 49.5 2.59 0.64 2.67 CL 1641+4001 0.464 16 41 53 +40 01 46 3575 I VF 44.0 1.02 0.67 2.62 V 1524.6+0957 0.516 15 24 40 +09 57 48 1664 I VF 49.9 2.92 0.89 3.29 MS 0451.6-0305 0.539 04 54 12 -03 00 53 902 S F 41.5 5.18 0.73 4.12 V 1121+2327 0.562 11 20 57 +23 26 27 1660 I VF 66.9 1.30 0.73 3.00 MS 2053.7-0449 0.583 20 56 21 -04 37 51 1667 I VF 43.5 4.96 1.32 4.91 V 1221+4918 0.700 12 21 26 +49 18 30 1662 I VF 79.4 1.44 1.18 4.62 MS 1137.5+6625 0.782 11 40 22 +66 08 18 536 I VF 117.5 1.18 0.81 4.04 RDCSJ 1317+2911 0.805 13 17 21 +29 11 19 2228 I VF 111.3 1.04 0.85 3.59 RDCSJ 1350+6007 0.805 13 50 48 +60 06 54 2229 I VF 58.3 1.76 1.77 7.26 RXJ 1716.4+6708 0.813 17 16 49 +67 08 26 548 I F 51.5 3.71 2.17 9.45 MS 1054.4-0321 0.830 10 56 59 -03 37 37 512 S F 67.5 3.67 1.07 6.61 WARPJ 1415.1+3612 1.013 14 15 11 +36 12 00 4163 I VF 89.2 1.10 1.93 7.54 &lt;/pre&gt; where Exp is the Chandra exposure time in ks corresponding to the nominal exposure filtered to exclude time periods of high background, N_H is the Galactic hydrogen column density in the direction of the cluster of galaxies, in units of 10&lt;sup&gt;20&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;, and L_sb and L_hb are the limiting luminosities in units of 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for point sources in the clusters in the 0.5-2.0 kev and 2-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/gcptsrccxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gcptsrccxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=gcptsrccxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/gcptsrccxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GCPTSRCCXO [3]</TD>
            <TD>Chandra Point Sources in 18 Distant Galaxy Clusters</TD>
            <TD>With the superb angular resolution of the Chandra Observatory, it is now possible to detect X-ray point sources, either embedded in galaxy clusters or along the cluster line of sight, which could not be resolved by previous instruments. This now allows studies of source counts in distant cluster fields. The authors want to analyze the inner region of clusters of galaxies to check for the presence of any over-density of X-ray point sources embedded in the gas diffuse emission. These point sources are possible AGN belonging to the clusters and could contaminate the cluster emission. The authors used a sample of 18 distant (0.25 &lt; z &lt; 1.01) galaxy clusters from the Chandra archive to construct the log N - log S relation, in both the soft and hard energy bands, for the X-ray point sources detected in the central cluster region to be compared with the counts of point sources detected in similarly deep fields without clusters. The authors find a ~2-sigma excess of cluster region sources at the bright end of the log N - log S distributon. The radial distribution of the brightest X-ray point sources confirms this excess and indicates that it is confined to the inner 0.5 Mpc of the cluster region. The results suggest the possible existence of X-ray sources belonging to the cluster (most probably AGN, given their 0.5-10 keV luminosity ranging from 10&lt;sup&gt;43&lt;/sup&gt; to 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;): on average one every three clusters. Unlike previous studies, which have mainly investigated the point-source population in the vicinity of the galaxy clusters, the present study analyzes the content of point sources within the 1 Mpc region covered by the cluster extent. This work confirms the findings of other investigators who analyzed the central 1 Mpc region of more massive clusters and/or groups in a similar redshift range. The X-ray source excess found here is much smaller than the excess of radio galaxies found recently in high-z X-ray selected clusters, possibly due to the better sensitivity of the radio observations. The properties of the clusters and of the Chandra exposures in which they were observed are given in Table 1 of the reference paper, and are reproduced below: &lt;pre&gt; Cluster Namne z RA (J2000) Dec ObsID ACIS Mode Exp N_H L_sb L_hb h m s d ' " ks [units are below] Abell 2125 0.246 15 41 12 +66 16 01 2207 I VF 79.7 2.77 0.13 0.56 ZW CL 1454.8+2233 0.258 14 57 15 +22 20 33 4192 I VF 91.4 3.22 0.23 0.74 MS 1008.1-1224 0.302 10 10 32 -12 39 23 926 I VF 44.2 6.74 0.44 1.57 ZW CL 0024.0+1652 0.394 00 26 35 +17 09 39 929 S VF 36.7 4.19 0.34 2.22 MS 1621.5+2640 0.426 16 23 36 +26 34 21 546 I F 30.0 3.59 0.81 3.41 RXJ 1701.3+6414 0.453 17 01 24 +64 14 10 547 I VF 49.5 2.59 0.64 2.67 CL 1641+4001 0.464 16 41 53 +40 01 46 3575 I VF 44.0 1.02 0.67 2.62 V 1524.6+0957 0.516 15 24 40 +09 57 48 1664 I VF 49.9 2.92 0.89 3.29 MS 0451.6-0305 0.539 04 54 12 -03 00 53 902 S F 41.5 5.18 0.73 4.12 V 1121+2327 0.562 11 20 57 +23 26 27 1660 I VF 66.9 1.30 0.73 3.00 MS 2053.7-0449 0.583 20 56 21 -04 37 51 1667 I VF 43.5 4.96 1.32 4.91 V 1221+4918 0.700 12 21 26 +49 18 30 1662 I VF 79.4 1.44 1.18 4.62 MS 1137.5+6625 0.782 11 40 22 +66 08 18 536 I VF 117.5 1.18 0.81 4.04 RDCSJ 1317+2911 0.805 13 17 21 +29 11 19 2228 I VF 111.3 1.04 0.85 3.59 RDCSJ 1350+6007 0.805 13 50 48 +60 06 54 2229 I VF 58.3 1.76 1.77 7.26 RXJ 1716.4+6708 0.813 17 16 49 +67 08 26 548 I F 51.5 3.71 2.17 9.45 MS 1054.4-0321 0.830 10 56 59 -03 37 37 512 S F 67.5 3.67 1.07 6.61 WARPJ 1415.1+3612 1.013 14 15 11 +36 12 00 4163 I VF 89.2 1.10 1.93 7.54 &lt;/pre&gt; where Exp is the Chandra exposure time in ks corresponding to the nominal exposure filtered to exclude time periods of high background, N_H is the Galactic hydrogen column density in the direction of the cluster of galaxies, in units of 10&lt;sup&gt;20&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;, and L_sb and L_hb are the limiting luminosities in units of 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for point sources in the clusters in the 0.5-2.0 kev and 2-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/gcptsrccxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gcptsrccxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_gcptsrccxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/gcptsrccxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/1017 [1]</TD>
            <TD>Northern Optical Cluster Survey. IV. (Lopes+, 2005)</TD>
            <TD>This paper presents a galaxy cluster catalog that is an extension of those presented in Papers II (Gal et al., 2003, Cat. &lt;J/AJ/125/2064&gt;) and III (Gal et al., 2005, in prep.). It covers 2700{deg}^2^ of digitized Second Palomar Observatory Sky Survey (DPOSS) data and is expected to be complete for rich clusters out to z~0.3, with clusters still detected to z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017#1</TD>
            <TD>2011-09-14T19:53:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/1017</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1017</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/1017 [2]</TD>
            <TD>Northern Optical Cluster Survey. IV. (Lopes+, 2005)</TD>
            <TD>This paper presents a galaxy cluster catalog that is an extension of those presented in Papers II (Gal et al., 2003, Cat. &lt;J/AJ/125/2064&gt;) and III (Gal et al., 2005, in prep.). It covers 2700{deg}^2^ of digitized Second Palomar Observatory Sky Survey (DPOSS) data and is expected to be complete for rich clusters out to z~0.3, with clusters still detected to z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017#2</TD>
            <TD>2011-09-14T19:53:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/1017&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1017</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/1017 [table1]</TD>
            <TD>Northern Optical Cluster Survey. IV. (Lopes+, 2005)</TD>
            <TD>This paper presents a galaxy cluster catalog that is an extension of those presented in Papers II (Gal et al., 2003, Cat. &lt;J/AJ/125/2064&gt;) and III (Gal et al., 2005, in prep.). It covers 2700{deg}^2^ of digitized Second Palomar Observatory Sky Survey (DPOSS) data and is expected to be complete for rich clusters out to z~0.3, with clusters still detected to z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017#table1</TD>
            <TD>2011-09-14T19:53:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/1017&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1017</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ATESP1P4GH [1]</TD>
            <TD>Australia Telescope ESO Slice Project 1.4-GHz Source Catalog</TD>
            <TD>The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&amp;A, 325, 954) galaxy redshift survey. This 26-degree&lt;sup&gt;2&lt;/sup&gt; region is centered at Declination -40 degrees, and ranges in RA from 22&lt;sup&gt;h&lt;/sup&gt; 30&lt;sup&gt;m&lt;/sup&gt; to 01&lt;sup&gt;h&lt;/sup&gt; 15&lt;sup&gt;m&lt;/sup&gt;. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atesp1p4gh#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atesp1p4gh</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=atesp1p4gh&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atesp1p4gh.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ATESP1P4GH [2]</TD>
            <TD>Australia Telescope ESO Slice Project 1.4-GHz Source Catalog</TD>
            <TD>The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&amp;A, 325, 954) galaxy redshift survey. This 26-degree&lt;sup&gt;2&lt;/sup&gt; region is centered at Declination -40 degrees, and ranges in RA from 22&lt;sup&gt;h&lt;/sup&gt; 30&lt;sup&gt;m&lt;/sup&gt; to 01&lt;sup&gt;h&lt;/sup&gt; 15&lt;sup&gt;m&lt;/sup&gt;. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atesp1p4gh#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atesp1p4gh</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=atesp1p4gh&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atesp1p4gh.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ATESP1P4GH [3]</TD>
            <TD>Australia Telescope ESO Slice Project 1.4-GHz Source Catalog</TD>
            <TD>The Australia Telescope ESO Slice Project (ATESP) survey is a radio survey which was accomplished with the Australia Telescope Compact Array (ATCA) at 1.4 GHz over the region covered by the ESO Slice Project (ESP: Vettolani et al. 1997, A&amp;A, 325, 954) galaxy redshift survey. This 26-degree&lt;sup&gt;2&lt;/sup&gt; region is centered at Declination -40 degrees, and ranges in RA from 22&lt;sup&gt;h&lt;/sup&gt; 30&lt;sup&gt;m&lt;/sup&gt; to 01&lt;sup&gt;h&lt;/sup&gt; 15&lt;sup&gt;m&lt;/sup&gt;. The ATESP survey consisted of 16 radio mosaics with 8 x 14 arcseconds resolution and uniform sensitivity (1 sigma noise level of ~ 79 microJansky) over the whole area of the ESP redshift survey. According to the reference paper, the final 6-sigma ATESP catalog contained 2960 sources down to a detection limit of ~ 0.5 mJy (6 sigma), 1402 of which are sub-mJy sources, and 189 of which are multiple sources (168 doubles, 19 triples and 2 quadruples). This table contains the list of 6-sigma or more sources detected in the ATESP survey. For composite sources with multiple components, the individual components each have entries in this table, and there is also an entry for the entire source. Based on the numbers quoted above, this would imply that there should be (2960 + 2*168 + 3*19 + 4*2) = 3361 entries in this table. The HEASARC notes that there are actually 3370 entries in the CDS version of this table that the present table is based on, 169 of which are doubles, 19 triples and 2 quadruples, implying that this version has 2967 sources, slightly more than the number quoted in the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atesp1p4gh#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atesp1p4gh</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_atesp1p4gh&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atesp1p4gh.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GCPTSRCCXO [1]</TD>
            <TD>Chandra Point Sources in 18 Distant Galaxy Clusters</TD>
            <TD>With the superb angular resolution of the Chandra Observatory, it is now possible to detect X-ray point sources, either embedded in galaxy clusters or along the cluster line of sight, which could not be resolved by previous instruments. This now allows studies of source counts in distant cluster fields. The authors want to analyze the inner region of clusters of galaxies to check for the presence of any over-density of X-ray point sources embedded in the gas diffuse emission. These point sources are possible AGN belonging to the clusters and could contaminate the cluster emission. The authors used a sample of 18 distant (0.25 &lt; z &lt; 1.01) galaxy clusters from the Chandra archive to construct the log N - log S relation, in both the soft and hard energy bands, for the X-ray point sources detected in the central cluster region to be compared with the counts of point sources detected in similarly deep fields without clusters. The authors find a ~2-sigma excess of cluster region sources at the bright end of the log N - log S distributon. The radial distribution of the brightest X-ray point sources confirms this excess and indicates that it is confined to the inner 0.5 Mpc of the cluster region. The results suggest the possible existence of X-ray sources belonging to the cluster (most probably AGN, given their 0.5-10 keV luminosity ranging from 10&lt;sup&gt;43&lt;/sup&gt; to 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;): on average one every three clusters. Unlike previous studies, which have mainly investigated the point-source population in the vicinity of the galaxy clusters, the present study analyzes the content of point sources within the 1 Mpc region covered by the cluster extent. This work confirms the findings of other investigators who analyzed the central 1 Mpc region of more massive clusters and/or groups in a similar redshift range. The X-ray source excess found here is much smaller than the excess of radio galaxies found recently in high-z X-ray selected clusters, possibly due to the better sensitivity of the radio observations. The properties of the clusters and of the Chandra exposures in which they were observed are given in Table 1 of the reference paper, and are reproduced below: &lt;pre&gt; Cluster Namne z RA (J2000) Dec ObsID ACIS Mode Exp N_H L_sb L_hb h m s d ' " ks [units are below] Abell 2125 0.246 15 41 12 +66 16 01 2207 I VF 79.7 2.77 0.13 0.56 ZW CL 1454.8+2233 0.258 14 57 15 +22 20 33 4192 I VF 91.4 3.22 0.23 0.74 MS 1008.1-1224 0.302 10 10 32 -12 39 23 926 I VF 44.2 6.74 0.44 1.57 ZW CL 0024.0+1652 0.394 00 26 35 +17 09 39 929 S VF 36.7 4.19 0.34 2.22 MS 1621.5+2640 0.426 16 23 36 +26 34 21 546 I F 30.0 3.59 0.81 3.41 RXJ 1701.3+6414 0.453 17 01 24 +64 14 10 547 I VF 49.5 2.59 0.64 2.67 CL 1641+4001 0.464 16 41 53 +40 01 46 3575 I VF 44.0 1.02 0.67 2.62 V 1524.6+0957 0.516 15 24 40 +09 57 48 1664 I VF 49.9 2.92 0.89 3.29 MS 0451.6-0305 0.539 04 54 12 -03 00 53 902 S F 41.5 5.18 0.73 4.12 V 1121+2327 0.562 11 20 57 +23 26 27 1660 I VF 66.9 1.30 0.73 3.00 MS 2053.7-0449 0.583 20 56 21 -04 37 51 1667 I VF 43.5 4.96 1.32 4.91 V 1221+4918 0.700 12 21 26 +49 18 30 1662 I VF 79.4 1.44 1.18 4.62 MS 1137.5+6625 0.782 11 40 22 +66 08 18 536 I VF 117.5 1.18 0.81 4.04 RDCSJ 1317+2911 0.805 13 17 21 +29 11 19 2228 I VF 111.3 1.04 0.85 3.59 RDCSJ 1350+6007 0.805 13 50 48 +60 06 54 2229 I VF 58.3 1.76 1.77 7.26 RXJ 1716.4+6708 0.813 17 16 49 +67 08 26 548 I F 51.5 3.71 2.17 9.45 MS 1054.4-0321 0.830 10 56 59 -03 37 37 512 S F 67.5 3.67 1.07 6.61 WARPJ 1415.1+3612 1.013 14 15 11 +36 12 00 4163 I VF 89.2 1.10 1.93 7.54 &lt;/pre&gt; where Exp is the Chandra exposure time in ks corresponding to the nominal exposure filtered to exclude time periods of high background, N_H is the Galactic hydrogen column density in the direction of the cluster of galaxies, in units of 10&lt;sup&gt;20&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;, and L_sb and L_hb are the limiting luminosities in units of 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for point sources in the clusters in the 0.5-2.0 kev and 2-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/gcptsrccxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gcptsrccxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=gcptsrccxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/gcptsrccxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GCPTSRCCXO [2]</TD>
            <TD>Chandra Point Sources in 18 Distant Galaxy Clusters</TD>
            <TD>With the superb angular resolution of the Chandra Observatory, it is now possible to detect X-ray point sources, either embedded in galaxy clusters or along the cluster line of sight, which could not be resolved by previous instruments. This now allows studies of source counts in distant cluster fields. The authors want to analyze the inner region of clusters of galaxies to check for the presence of any over-density of X-ray point sources embedded in the gas diffuse emission. These point sources are possible AGN belonging to the clusters and could contaminate the cluster emission. The authors used a sample of 18 distant (0.25 &lt; z &lt; 1.01) galaxy clusters from the Chandra archive to construct the log N - log S relation, in both the soft and hard energy bands, for the X-ray point sources detected in the central cluster region to be compared with the counts of point sources detected in similarly deep fields without clusters. The authors find a ~2-sigma excess of cluster region sources at the bright end of the log N - log S distributon. The radial distribution of the brightest X-ray point sources confirms this excess and indicates that it is confined to the inner 0.5 Mpc of the cluster region. The results suggest the possible existence of X-ray sources belonging to the cluster (most probably AGN, given their 0.5-10 keV luminosity ranging from 10&lt;sup&gt;43&lt;/sup&gt; to 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;): on average one every three clusters. Unlike previous studies, which have mainly investigated the point-source population in the vicinity of the galaxy clusters, the present study analyzes the content of point sources within the 1 Mpc region covered by the cluster extent. This work confirms the findings of other investigators who analyzed the central 1 Mpc region of more massive clusters and/or groups in a similar redshift range. The X-ray source excess found here is much smaller than the excess of radio galaxies found recently in high-z X-ray selected clusters, possibly due to the better sensitivity of the radio observations. The properties of the clusters and of the Chandra exposures in which they were observed are given in Table 1 of the reference paper, and are reproduced below: &lt;pre&gt; Cluster Namne z RA (J2000) Dec ObsID ACIS Mode Exp N_H L_sb L_hb h m s d ' " ks [units are below] Abell 2125 0.246 15 41 12 +66 16 01 2207 I VF 79.7 2.77 0.13 0.56 ZW CL 1454.8+2233 0.258 14 57 15 +22 20 33 4192 I VF 91.4 3.22 0.23 0.74 MS 1008.1-1224 0.302 10 10 32 -12 39 23 926 I VF 44.2 6.74 0.44 1.57 ZW CL 0024.0+1652 0.394 00 26 35 +17 09 39 929 S VF 36.7 4.19 0.34 2.22 MS 1621.5+2640 0.426 16 23 36 +26 34 21 546 I F 30.0 3.59 0.81 3.41 RXJ 1701.3+6414 0.453 17 01 24 +64 14 10 547 I VF 49.5 2.59 0.64 2.67 CL 1641+4001 0.464 16 41 53 +40 01 46 3575 I VF 44.0 1.02 0.67 2.62 V 1524.6+0957 0.516 15 24 40 +09 57 48 1664 I VF 49.9 2.92 0.89 3.29 MS 0451.6-0305 0.539 04 54 12 -03 00 53 902 S F 41.5 5.18 0.73 4.12 V 1121+2327 0.562 11 20 57 +23 26 27 1660 I VF 66.9 1.30 0.73 3.00 MS 2053.7-0449 0.583 20 56 21 -04 37 51 1667 I VF 43.5 4.96 1.32 4.91 V 1221+4918 0.700 12 21 26 +49 18 30 1662 I VF 79.4 1.44 1.18 4.62 MS 1137.5+6625 0.782 11 40 22 +66 08 18 536 I VF 117.5 1.18 0.81 4.04 RDCSJ 1317+2911 0.805 13 17 21 +29 11 19 2228 I VF 111.3 1.04 0.85 3.59 RDCSJ 1350+6007 0.805 13 50 48 +60 06 54 2229 I VF 58.3 1.76 1.77 7.26 RXJ 1716.4+6708 0.813 17 16 49 +67 08 26 548 I F 51.5 3.71 2.17 9.45 MS 1054.4-0321 0.830 10 56 59 -03 37 37 512 S F 67.5 3.67 1.07 6.61 WARPJ 1415.1+3612 1.013 14 15 11 +36 12 00 4163 I VF 89.2 1.10 1.93 7.54 &lt;/pre&gt; where Exp is the Chandra exposure time in ks corresponding to the nominal exposure filtered to exclude time periods of high background, N_H is the Galactic hydrogen column density in the direction of the cluster of galaxies, in units of 10&lt;sup&gt;20&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;, and L_sb and L_hb are the limiting luminosities in units of 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for point sources in the clusters in the 0.5-2.0 kev and 2-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/gcptsrccxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
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            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=gcptsrccxo&amp;</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/gcptsrccxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GCPTSRCCXO [3]</TD>
            <TD>Chandra Point Sources in 18 Distant Galaxy Clusters</TD>
            <TD>With the superb angular resolution of the Chandra Observatory, it is now possible to detect X-ray point sources, either embedded in galaxy clusters or along the cluster line of sight, which could not be resolved by previous instruments. This now allows studies of source counts in distant cluster fields. The authors want to analyze the inner region of clusters of galaxies to check for the presence of any over-density of X-ray point sources embedded in the gas diffuse emission. These point sources are possible AGN belonging to the clusters and could contaminate the cluster emission. The authors used a sample of 18 distant (0.25 &lt; z &lt; 1.01) galaxy clusters from the Chandra archive to construct the log N - log S relation, in both the soft and hard energy bands, for the X-ray point sources detected in the central cluster region to be compared with the counts of point sources detected in similarly deep fields without clusters. The authors find a ~2-sigma excess of cluster region sources at the bright end of the log N - log S distributon. The radial distribution of the brightest X-ray point sources confirms this excess and indicates that it is confined to the inner 0.5 Mpc of the cluster region. The results suggest the possible existence of X-ray sources belonging to the cluster (most probably AGN, given their 0.5-10 keV luminosity ranging from 10&lt;sup&gt;43&lt;/sup&gt; to 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;): on average one every three clusters. Unlike previous studies, which have mainly investigated the point-source population in the vicinity of the galaxy clusters, the present study analyzes the content of point sources within the 1 Mpc region covered by the cluster extent. This work confirms the findings of other investigators who analyzed the central 1 Mpc region of more massive clusters and/or groups in a similar redshift range. The X-ray source excess found here is much smaller than the excess of radio galaxies found recently in high-z X-ray selected clusters, possibly due to the better sensitivity of the radio observations. The properties of the clusters and of the Chandra exposures in which they were observed are given in Table 1 of the reference paper, and are reproduced below: &lt;pre&gt; Cluster Namne z RA (J2000) Dec ObsID ACIS Mode Exp N_H L_sb L_hb h m s d ' " ks [units are below] Abell 2125 0.246 15 41 12 +66 16 01 2207 I VF 79.7 2.77 0.13 0.56 ZW CL 1454.8+2233 0.258 14 57 15 +22 20 33 4192 I VF 91.4 3.22 0.23 0.74 MS 1008.1-1224 0.302 10 10 32 -12 39 23 926 I VF 44.2 6.74 0.44 1.57 ZW CL 0024.0+1652 0.394 00 26 35 +17 09 39 929 S VF 36.7 4.19 0.34 2.22 MS 1621.5+2640 0.426 16 23 36 +26 34 21 546 I F 30.0 3.59 0.81 3.41 RXJ 1701.3+6414 0.453 17 01 24 +64 14 10 547 I VF 49.5 2.59 0.64 2.67 CL 1641+4001 0.464 16 41 53 +40 01 46 3575 I VF 44.0 1.02 0.67 2.62 V 1524.6+0957 0.516 15 24 40 +09 57 48 1664 I VF 49.9 2.92 0.89 3.29 MS 0451.6-0305 0.539 04 54 12 -03 00 53 902 S F 41.5 5.18 0.73 4.12 V 1121+2327 0.562 11 20 57 +23 26 27 1660 I VF 66.9 1.30 0.73 3.00 MS 2053.7-0449 0.583 20 56 21 -04 37 51 1667 I VF 43.5 4.96 1.32 4.91 V 1221+4918 0.700 12 21 26 +49 18 30 1662 I VF 79.4 1.44 1.18 4.62 MS 1137.5+6625 0.782 11 40 22 +66 08 18 536 I VF 117.5 1.18 0.81 4.04 RDCSJ 1317+2911 0.805 13 17 21 +29 11 19 2228 I VF 111.3 1.04 0.85 3.59 RDCSJ 1350+6007 0.805 13 50 48 +60 06 54 2229 I VF 58.3 1.76 1.77 7.26 RXJ 1716.4+6708 0.813 17 16 49 +67 08 26 548 I F 51.5 3.71 2.17 9.45 MS 1054.4-0321 0.830 10 56 59 -03 37 37 512 S F 67.5 3.67 1.07 6.61 WARPJ 1415.1+3612 1.013 14 15 11 +36 12 00 4163 I VF 89.2 1.10 1.93 7.54 &lt;/pre&gt; where Exp is the Chandra exposure time in ks corresponding to the nominal exposure filtered to exclude time periods of high background, N_H is the Galactic hydrogen column density in the direction of the cluster of galaxies, in units of 10&lt;sup&gt;20&lt;/sup&gt; cm&lt;sup&gt;-2&lt;/sup&gt;, and L_sb and L_hb are the limiting luminosities in units of 10&lt;sup&gt;42&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for point sources in the clusters in the 0.5-2.0 kev and 2-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/gcptsrccxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
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            <TD />
            <TD>ivo://nasa.heasarc/gcptsrccxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_gcptsrccxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/gcptsrccxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ECDFSOID2 [1]</TD>
            <TD>Extended Chandra Deep Field-South Optical and Near-IR Counterparts</TD>
            <TD>This table contains the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since their new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, the authors provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. The authors demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from their data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L&lt;sub&gt;0.5-8keV&lt;/sub&gt; ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) at 1.5 &lt;~ z &lt;~ 3, including those with and without broad emission lines. This redshift catalog includes 17 type-2 QSOs at 1 &lt;~ z &lt;~ 3.5 that significantly increases (doubles) such samples. Based on thei deepest (9 hr) VLT/VIMOS observation, the authors identify "elusive" optically faint galaxies (R&lt;sub&gt;mag&lt;/sub&gt; ~ 25) at z ~ 2 - 3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); in their paper, they highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, they determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ecdfsoid2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>0.0166666666666666667</TD>
            <TD />
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ecdfsoid2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ECDFSOID2 [2]</TD>
            <TD>Extended Chandra Deep Field-South Optical and Near-IR Counterparts</TD>
            <TD>This table contains the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since their new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, the authors provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. The authors demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from their data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L&lt;sub&gt;0.5-8keV&lt;/sub&gt; ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) at 1.5 &lt;~ z &lt;~ 3, including those with and without broad emission lines. This redshift catalog includes 17 type-2 QSOs at 1 &lt;~ z &lt;~ 3.5 that significantly increases (doubles) such samples. Based on thei deepest (9 hr) VLT/VIMOS observation, the authors identify "elusive" optically faint galaxies (R&lt;sub&gt;mag&lt;/sub&gt; ~ 25) at z ~ 2 - 3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); in their paper, they highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, they determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ecdfsoid2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ecdfsoid2&amp;</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ecdfsoid2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ECDFSOID2 [3]</TD>
            <TD>Extended Chandra Deep Field-South Optical and Near-IR Counterparts</TD>
            <TD>This table contains the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since their new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, the authors provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. The authors demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from their data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L&lt;sub&gt;0.5-8keV&lt;/sub&gt; ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) at 1.5 &lt;~ z &lt;~ 3, including those with and without broad emission lines. This redshift catalog includes 17 type-2 QSOs at 1 &lt;~ z &lt;~ 3.5 that significantly increases (doubles) such samples. Based on thei deepest (9 hr) VLT/VIMOS observation, the authors identify "elusive" optically faint galaxies (R&lt;sub&gt;mag&lt;/sub&gt; ~ 25) at z ~ 2 - 3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); in their paper, they highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, they determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ecdfsoid2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD />
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            <TD>WebBrowser</TD>
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            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ecdfsoid2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ecdfsoid2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/1017 [1]</TD>
            <TD>Northern Optical Cluster Survey. IV. (Lopes+, 2005)</TD>
            <TD>This paper presents a galaxy cluster catalog that is an extension of those presented in Papers II (Gal et al., 2003, Cat. &lt;J/AJ/125/2064&gt;) and III (Gal et al., 2005, in prep.). It covers 2700{deg}^2^ of digitized Second Palomar Observatory Sky Survey (DPOSS) data and is expected to be complete for rich clusters out to z~0.3, with clusters still detected to z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017#1</TD>
            <TD>2011-09-14T19:53:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/1017</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1017</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/1017 [2]</TD>
            <TD>Northern Optical Cluster Survey. IV. (Lopes+, 2005)</TD>
            <TD>This paper presents a galaxy cluster catalog that is an extension of those presented in Papers II (Gal et al., 2003, Cat. &lt;J/AJ/125/2064&gt;) and III (Gal et al., 2005, in prep.). It covers 2700{deg}^2^ of digitized Second Palomar Observatory Sky Survey (DPOSS) data and is expected to be complete for rich clusters out to z~0.3, with clusters still detected to z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017#2</TD>
            <TD>2011-09-14T19:53:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/1017&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1017</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/1017 [table1]</TD>
            <TD>Northern Optical Cluster Survey. IV. (Lopes+, 2005)</TD>
            <TD>This paper presents a galaxy cluster catalog that is an extension of those presented in Papers II (Gal et al., 2003, Cat. &lt;J/AJ/125/2064&gt;) and III (Gal et al., 2005, in prep.). It covers 2700{deg}^2^ of digitized Second Palomar Observatory Sky Survey (DPOSS) data and is expected to be complete for rich clusters out to z~0.3, with clusters still detected to z~0.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017#table1</TD>
            <TD>2011-09-14T19:53:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1017</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/1017&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1017</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NEARGALCAT [1]</TD>
            <TD>Neighboring Galaxies Catalog</TD>
            <TD>This table contains an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D &lt;~ 10 Mpc or a radial velocity with respect to the Local Group (LG) centroid V&lt;sub&gt;LG&lt;/sub&gt; &lt; 550 km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. The authors expect the catalog completeness to be roughly 70% - 80% within 8 Mpc.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/neargalcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/neargalcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=neargalcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/neargalcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NEARGALCAT [2]</TD>
            <TD>Neighboring Galaxies Catalog</TD>
            <TD>This table contains an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D &lt;~ 10 Mpc or a radial velocity with respect to the Local Group (LG) centroid V&lt;sub&gt;LG&lt;/sub&gt; &lt; 550 km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. The authors expect the catalog completeness to be roughly 70% - 80% within 8 Mpc.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/neargalcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/neargalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=neargalcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/neargalcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NEARGALCAT [3]</TD>
            <TD>Neighboring Galaxies Catalog</TD>
            <TD>This table contains an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D &lt;~ 10 Mpc or a radial velocity with respect to the Local Group (LG) centroid V&lt;sub&gt;LG&lt;/sub&gt; &lt; 550 km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. The authors expect the catalog completeness to be roughly 70% - 80% within 8 Mpc.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/neargalcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/neargalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_neargalcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/neargalcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ECDFSOID2 [1]</TD>
            <TD>Extended Chandra Deep Field-South Optical and Near-IR Counterparts</TD>
            <TD>This table contains the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since their new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, the authors provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. The authors demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from their data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L&lt;sub&gt;0.5-8keV&lt;/sub&gt; ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) at 1.5 &lt;~ z &lt;~ 3, including those with and without broad emission lines. This redshift catalog includes 17 type-2 QSOs at 1 &lt;~ z &lt;~ 3.5 that significantly increases (doubles) such samples. Based on thei deepest (9 hr) VLT/VIMOS observation, the authors identify "elusive" optically faint galaxies (R&lt;sub&gt;mag&lt;/sub&gt; ~ 25) at z ~ 2 - 3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); in their paper, they highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, they determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ecdfsoid2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ecdfsoid2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ecdfsoid2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ecdfsoid2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ECDFSOID2 [2]</TD>
            <TD>Extended Chandra Deep Field-South Optical and Near-IR Counterparts</TD>
            <TD>This table contains the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since their new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, the authors provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. The authors demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from their data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L&lt;sub&gt;0.5-8keV&lt;/sub&gt; ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) at 1.5 &lt;~ z &lt;~ 3, including those with and without broad emission lines. This redshift catalog includes 17 type-2 QSOs at 1 &lt;~ z &lt;~ 3.5 that significantly increases (doubles) such samples. Based on thei deepest (9 hr) VLT/VIMOS observation, the authors identify "elusive" optically faint galaxies (R&lt;sub&gt;mag&lt;/sub&gt; ~ 25) at z ~ 2 - 3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); in their paper, they highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, they determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ecdfsoid2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ecdfsoid2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ecdfsoid2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ecdfsoid2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ECDFSOID2 [3]</TD>
            <TD>Extended Chandra Deep Field-South Optical and Near-IR Counterparts</TD>
            <TD>This table contains the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since their new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, the authors provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. The authors demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from their data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L&lt;sub&gt;0.5-8keV&lt;/sub&gt; ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) at 1.5 &lt;~ z &lt;~ 3, including those with and without broad emission lines. This redshift catalog includes 17 type-2 QSOs at 1 &lt;~ z &lt;~ 3.5 that significantly increases (doubles) such samples. Based on thei deepest (9 hr) VLT/VIMOS observation, the authors identify "elusive" optically faint galaxies (R&lt;sub&gt;mag&lt;/sub&gt; ~ 25) at z ~ 2 - 3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); in their paper, they highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, they determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ecdfsoid2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ecdfsoid2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ecdfsoid2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ecdfsoid2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/328/1181 [1]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#1</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/328/1181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/328/1181 [2]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#2</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/1181 [table1]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#table1</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/1181 [table3]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#table3</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/1181 [table2]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#table2</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NEARGALCAT [1]</TD>
            <TD>Neighboring Galaxies Catalog</TD>
            <TD>This table contains an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D &lt;~ 10 Mpc or a radial velocity with respect to the Local Group (LG) centroid V&lt;sub&gt;LG&lt;/sub&gt; &lt; 550 km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. The authors expect the catalog completeness to be roughly 70% - 80% within 8 Mpc.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/neargalcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/neargalcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=neargalcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/neargalcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NEARGALCAT [2]</TD>
            <TD>Neighboring Galaxies Catalog</TD>
            <TD>This table contains an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D &lt;~ 10 Mpc or a radial velocity with respect to the Local Group (LG) centroid V&lt;sub&gt;LG&lt;/sub&gt; &lt; 550 km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. The authors expect the catalog completeness to be roughly 70% - 80% within 8 Mpc.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/neargalcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/neargalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=neargalcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/neargalcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NEARGALCAT [3]</TD>
            <TD>Neighboring Galaxies Catalog</TD>
            <TD>This table contains an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D &lt;~ 10 Mpc or a radial velocity with respect to the Local Group (LG) centroid V&lt;sub&gt;LG&lt;/sub&gt; &lt; 550 km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. The authors expect the catalog completeness to be roughly 70% - 80% within 8 Mpc.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/neargalcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/neargalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_neargalcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/neargalcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ECDFSOID2 [1]</TD>
            <TD>Extended Chandra Deep Field-South Optical and Near-IR Counterparts</TD>
            <TD>This table contains the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since their new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, the authors provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. The authors demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from their data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L&lt;sub&gt;0.5-8keV&lt;/sub&gt; ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) at 1.5 &lt;~ z &lt;~ 3, including those with and without broad emission lines. This redshift catalog includes 17 type-2 QSOs at 1 &lt;~ z &lt;~ 3.5 that significantly increases (doubles) such samples. Based on thei deepest (9 hr) VLT/VIMOS observation, the authors identify "elusive" optically faint galaxies (R&lt;sub&gt;mag&lt;/sub&gt; ~ 25) at z ~ 2 - 3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); in their paper, they highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, they determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ecdfsoid2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ecdfsoid2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ecdfsoid2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ecdfsoid2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ECDFSOID2 [2]</TD>
            <TD>Extended Chandra Deep Field-South Optical and Near-IR Counterparts</TD>
            <TD>This table contains the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since their new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, the authors provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. The authors demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from their data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L&lt;sub&gt;0.5-8keV&lt;/sub&gt; ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) at 1.5 &lt;~ z &lt;~ 3, including those with and without broad emission lines. This redshift catalog includes 17 type-2 QSOs at 1 &lt;~ z &lt;~ 3.5 that significantly increases (doubles) such samples. Based on thei deepest (9 hr) VLT/VIMOS observation, the authors identify "elusive" optically faint galaxies (R&lt;sub&gt;mag&lt;/sub&gt; ~ 25) at z ~ 2 - 3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); in their paper, they highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, they determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ecdfsoid2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ecdfsoid2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ecdfsoid2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ecdfsoid2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ECDFSOID2 [3]</TD>
            <TD>Extended Chandra Deep Field-South Optical and Near-IR Counterparts</TD>
            <TD>This table contains the results of a program to acquire high-quality optical spectra of X-ray sources detected in the Extended-Chandra Deep Field-South (E-CDF-S) and its central 2 Ms area. New spectroscopic redshifts, up to z = 4, are measured for 283 counterparts to Chandra sources with deep exposures (t ~ 2-9 hr per pointing) using multi-slit facilities on both VLT (VIMOS) and Keck (DEIMOS), thus bringing the total number of spectroscopically identified X-ray sources to over 500 in this survey field. Since their new spectroscopic identifications are mainly associated with X-ray sources in the shallower 250 ks coverage, the authors provide a comprehensive catalog of X-ray sources detected in the E-CDF-S including the optical and near-infrared counterparts, determined by a likelihood routine, and redshifts (both spectroscopic and photometric), that incorporate published spectroscopic catalogs, thus resulting in a final sample with a high fraction (80%) of X-ray sources having secure identifications. The authors demonstrate the remarkable coverage of the luminosity-redshift plane now accessible from their data while emphasizing the detection of active galactic nuclei (AGNs) that contribute to the faint end of the luminosity function (L&lt;sub&gt;0.5-8keV&lt;/sub&gt; ~ 10&lt;sup&gt;43&lt;/sup&gt; - 10&lt;sup&gt;44&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) at 1.5 &lt;~ z &lt;~ 3, including those with and without broad emission lines. This redshift catalog includes 17 type-2 QSOs at 1 &lt;~ z &lt;~ 3.5 that significantly increases (doubles) such samples. Based on thei deepest (9 hr) VLT/VIMOS observation, the authors identify "elusive" optically faint galaxies (R&lt;sub&gt;mag&lt;/sub&gt; ~ 25) at z ~ 2 - 3 based upon the detection of interstellar absorption lines (e.g., O II+Si IV, C II], C IV); in their paper, they highlight one such case, an absorption-line galaxy at z = 3.208 having no obvious signs of an AGN in its optical spectrum. In addition, they determine accurate distances to eight galaxy groups with extended X-ray emission detected both by Chandra and XMM-Newton.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ecdfsoid2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ecdfsoid2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ecdfsoid2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ecdfsoid2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/328/1181 [1]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#1</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/328/1181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/328/1181 [2]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#2</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/1181 [table1]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#table1</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/1181 [table3]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#table3</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/1181 [table2]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#table2</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NEARGALCAT [1]</TD>
            <TD>Neighboring Galaxies Catalog</TD>
            <TD>This table contains an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D &lt;~ 10 Mpc or a radial velocity with respect to the Local Group (LG) centroid V&lt;sub&gt;LG&lt;/sub&gt; &lt; 550 km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. The authors expect the catalog completeness to be roughly 70% - 80% within 8 Mpc.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/neargalcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/neargalcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=neargalcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/neargalcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NEARGALCAT [2]</TD>
            <TD>Neighboring Galaxies Catalog</TD>
            <TD>This table contains an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D &lt;~ 10 Mpc or a radial velocity with respect to the Local Group (LG) centroid V&lt;sub&gt;LG&lt;/sub&gt; &lt; 550 km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. The authors expect the catalog completeness to be roughly 70% - 80% within 8 Mpc.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/neargalcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/neargalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=neargalcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/neargalcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NEARGALCAT [3]</TD>
            <TD>Neighboring Galaxies Catalog</TD>
            <TD>This table contains an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D &lt;~ 10 Mpc or a radial velocity with respect to the Local Group (LG) centroid V&lt;sub&gt;LG&lt;/sub&gt; &lt; 550 km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. The authors expect the catalog completeness to be roughly 70% - 80% within 8 Mpc.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/neargalcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/neargalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_neargalcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/neargalcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ETGALXRAY [1]</TD>
            <TD>Early-Type Galaxies X-Ray Luminosities Catalog</TD>
            <TD>This table contains a catalog of X-ray luminosities for 401 early-type galaxies (and 24 other galaxies which were listed in previuous studies as early but which have LEDA T-types &gt;= -1.5), of which 136 are based on newly analysed ROSAT PSPC pointed observations. The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. In their paper, the authors use this sample to fit the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation for early-type galaxies and find a best-fit slope for the catalog of ~ 2.2. The authors demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modeled by a single power-law fit. They also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L&lt;sub&gt;(discrete-source-contribution)&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; ~ 29.5 erg s&lt;sup&gt;-1&lt;/sup&gt;/L&lt;sub&gt;Bsun&lt;/sub&gt;. The authors compare this result with luminosities from their catalog. Lastly, they examine the influence of environment on galaxy X-ray luminosity and on the form of the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation. They conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations. The sample of early-type galaxies was selected from the Lyon-Meudon Extragalactic Data Archive (LEDA). This catalog at that time contained information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and morphological data. Galaxies were selected using the following criteria: (i) Morphological Type T &lt; -1.5 (i.e. E, E-S0 and S0 galaxies). (ii) Virgo-corrected recession velocity V &lt;= 9,000 km s&lt;sup&gt;-1&lt;/sup&gt;. (iii) Apparent Magnitude B&lt;sub&gt;T&lt;/sub&gt; &lt;= 13.5. The redshift and apparent magnitude restrictions were chosen in order to minimize the effects of incompleteness on their sample. The LEDA catalogue is known to be 90 per cent complete at B&lt;sub&gt;T&lt;/sub&gt; = 14.5, so the selection should be close to statistical completeness. The selection process produced ~ 700 objects. The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. All of the X-ray luminosities have been converted to a common format based on a reliable distance scale (assuming H&lt;sub&gt;0&lt;/sub&gt; = 75 km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;), and correcting for differences in spectral fitting techniques and waveband.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=etgalxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/etgalxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ETGALXRAY [2]</TD>
            <TD>Early-Type Galaxies X-Ray Luminosities Catalog</TD>
            <TD>This table contains a catalog of X-ray luminosities for 401 early-type galaxies (and 24 other galaxies which were listed in previuous studies as early but which have LEDA T-types &gt;= -1.5), of which 136 are based on newly analysed ROSAT PSPC pointed observations. The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. In their paper, the authors use this sample to fit the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation for early-type galaxies and find a best-fit slope for the catalog of ~ 2.2. The authors demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modeled by a single power-law fit. They also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L&lt;sub&gt;(discrete-source-contribution)&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; ~ 29.5 erg s&lt;sup&gt;-1&lt;/sup&gt;/L&lt;sub&gt;Bsun&lt;/sub&gt;. The authors compare this result with luminosities from their catalog. Lastly, they examine the influence of environment on galaxy X-ray luminosity and on the form of the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation. They conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations. The sample of early-type galaxies was selected from the Lyon-Meudon Extragalactic Data Archive (LEDA). This catalog at that time contained information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and morphological data. Galaxies were selected using the following criteria: (i) Morphological Type T &lt; -1.5 (i.e. E, E-S0 and S0 galaxies). (ii) Virgo-corrected recession velocity V &lt;= 9,000 km s&lt;sup&gt;-1&lt;/sup&gt;. (iii) Apparent Magnitude B&lt;sub&gt;T&lt;/sub&gt; &lt;= 13.5. The redshift and apparent magnitude restrictions were chosen in order to minimize the effects of incompleteness on their sample. The LEDA catalogue is known to be 90 per cent complete at B&lt;sub&gt;T&lt;/sub&gt; = 14.5, so the selection should be close to statistical completeness. The selection process produced ~ 700 objects. The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. All of the X-ray luminosities have been converted to a common format based on a reliable distance scale (assuming H&lt;sub&gt;0&lt;/sub&gt; = 75 km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;), and correcting for differences in spectral fitting techniques and waveband.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=etgalxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/etgalxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ETGALXRAY [3]</TD>
            <TD>Early-Type Galaxies X-Ray Luminosities Catalog</TD>
            <TD>This table contains a catalog of X-ray luminosities for 401 early-type galaxies (and 24 other galaxies which were listed in previuous studies as early but which have LEDA T-types &gt;= -1.5), of which 136 are based on newly analysed ROSAT PSPC pointed observations. The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. In their paper, the authors use this sample to fit the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation for early-type galaxies and find a best-fit slope for the catalog of ~ 2.2. The authors demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modeled by a single power-law fit. They also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L&lt;sub&gt;(discrete-source-contribution)&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; ~ 29.5 erg s&lt;sup&gt;-1&lt;/sup&gt;/L&lt;sub&gt;Bsun&lt;/sub&gt;. The authors compare this result with luminosities from their catalog. Lastly, they examine the influence of environment on galaxy X-ray luminosity and on the form of the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation. They conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations. The sample of early-type galaxies was selected from the Lyon-Meudon Extragalactic Data Archive (LEDA). This catalog at that time contained information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and morphological data. Galaxies were selected using the following criteria: (i) Morphological Type T &lt; -1.5 (i.e. E, E-S0 and S0 galaxies). (ii) Virgo-corrected recession velocity V &lt;= 9,000 km s&lt;sup&gt;-1&lt;/sup&gt;. (iii) Apparent Magnitude B&lt;sub&gt;T&lt;/sub&gt; &lt;= 13.5. The redshift and apparent magnitude restrictions were chosen in order to minimize the effects of incompleteness on their sample. The LEDA catalogue is known to be 90 per cent complete at B&lt;sub&gt;T&lt;/sub&gt; = 14.5, so the selection should be close to statistical completeness. The selection process produced ~ 700 objects. The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. All of the X-ray luminosities have been converted to a common format based on a reliable distance scale (assuming H&lt;sub&gt;0&lt;/sub&gt; = 75 km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;), and correcting for differences in spectral fitting techniques and waveband.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_etgalxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/etgalxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/328/1181 [1]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#1</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/328/1181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/328/1181 [2]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#2</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/1181 [table1]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#table1</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/1181 [table3]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#table3</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/328/1181 [table2]</TD>
            <TD>Extragalactic supernovae (Navasardyan+, 2001)</TD>
            <TD>In order to investigate the influence of environment on supernova (SN) production, we have performed a statistical investigation of the SNe discovered in isolated galaxies, in pairs and in groups of galaxies. 22 SNe in 18 isolated galaxies, 48 SNe in 40 galaxy members of 37 pairs and 211 SNe in 170 galaxy members of 116 groups have been selected and studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181#table2</TD>
            <TD>2011-09-14T19:53:22Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/328/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/328/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/328/1181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/312/442 [1]</TD>
            <TD>UV-selected galaxy redshift survey. II. (Sullivan+, 2000)</TD>
            <TD>We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000{AA} from the FOCA balloon-borne imaging camera of Milliard et al. (1992A&amp;A...257...24M). This work represents an extension of the initial study by Treyer et al. (Cat. &lt;J/MNRAS/300/303&gt;). Our enlarged catalogue contains 433 sources (~3 times as many as in our earlier study) across two FOCA fields. 273 of these are galaxies, nearly all with redshifts z~0-0.4. Nebular emission-line measurements are available for 216 galaxies, allowing us to address issues of excitation, reddening and metallicity. The UV and H{alpha} luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0&lt;z&lt;0.4. Our data are more consistent with a modest evolutionary trend, as suggested by recent redshift survey results. Investigating the emission-line properties, we find no evidence for a significant number of AGN in our sample; most UV-selected sources to z~0.4 are intense star-forming galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442#1</TD>
            <TD>2012-11-13T14:10:02Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/312/442</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/442</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/312/442 [2]</TD>
            <TD>UV-selected galaxy redshift survey. II. (Sullivan+, 2000)</TD>
            <TD>We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000{AA} from the FOCA balloon-borne imaging camera of Milliard et al. (1992A&amp;A...257...24M). This work represents an extension of the initial study by Treyer et al. (Cat. &lt;J/MNRAS/300/303&gt;). Our enlarged catalogue contains 433 sources (~3 times as many as in our earlier study) across two FOCA fields. 273 of these are galaxies, nearly all with redshifts z~0-0.4. Nebular emission-line measurements are available for 216 galaxies, allowing us to address issues of excitation, reddening and metallicity. The UV and H{alpha} luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0&lt;z&lt;0.4. Our data are more consistent with a modest evolutionary trend, as suggested by recent redshift survey results. Investigating the emission-line properties, we find no evidence for a significant number of AGN in our sample; most UV-selected sources to z~0.4 are intense star-forming galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442#2</TD>
            <TD>2012-11-13T14:10:02Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/312/442&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/442</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/312/442 [table7]</TD>
            <TD>UV-selected galaxy redshift survey. II. (Sullivan+, 2000)</TD>
            <TD>We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000{AA} from the FOCA balloon-borne imaging camera of Milliard et al. (1992A&amp;A...257...24M). This work represents an extension of the initial study by Treyer et al. (Cat. &lt;J/MNRAS/300/303&gt;). Our enlarged catalogue contains 433 sources (~3 times as many as in our earlier study) across two FOCA fields. 273 of these are galaxies, nearly all with redshifts z~0-0.4. Nebular emission-line measurements are available for 216 galaxies, allowing us to address issues of excitation, reddening and metallicity. The UV and H{alpha} luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0&lt;z&lt;0.4. Our data are more consistent with a modest evolutionary trend, as suggested by recent redshift survey results. Investigating the emission-line properties, we find no evidence for a significant number of AGN in our sample; most UV-selected sources to z~0.4 are intense star-forming galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442#table7</TD>
            <TD>2012-11-13T14:10:02Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/312/442&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/442</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ETGALXRAY [1]</TD>
            <TD>Early-Type Galaxies X-Ray Luminosities Catalog</TD>
            <TD>This table contains a catalog of X-ray luminosities for 401 early-type galaxies (and 24 other galaxies which were listed in previuous studies as early but which have LEDA T-types &gt;= -1.5), of which 136 are based on newly analysed ROSAT PSPC pointed observations. The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. In their paper, the authors use this sample to fit the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation for early-type galaxies and find a best-fit slope for the catalog of ~ 2.2. The authors demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modeled by a single power-law fit. They also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L&lt;sub&gt;(discrete-source-contribution)&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; ~ 29.5 erg s&lt;sup&gt;-1&lt;/sup&gt;/L&lt;sub&gt;Bsun&lt;/sub&gt;. The authors compare this result with luminosities from their catalog. Lastly, they examine the influence of environment on galaxy X-ray luminosity and on the form of the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation. They conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations. The sample of early-type galaxies was selected from the Lyon-Meudon Extragalactic Data Archive (LEDA). This catalog at that time contained information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and morphological data. Galaxies were selected using the following criteria: (i) Morphological Type T &lt; -1.5 (i.e. E, E-S0 and S0 galaxies). (ii) Virgo-corrected recession velocity V &lt;= 9,000 km s&lt;sup&gt;-1&lt;/sup&gt;. (iii) Apparent Magnitude B&lt;sub&gt;T&lt;/sub&gt; &lt;= 13.5. The redshift and apparent magnitude restrictions were chosen in order to minimize the effects of incompleteness on their sample. The LEDA catalogue is known to be 90 per cent complete at B&lt;sub&gt;T&lt;/sub&gt; = 14.5, so the selection should be close to statistical completeness. The selection process produced ~ 700 objects. The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. All of the X-ray luminosities have been converted to a common format based on a reliable distance scale (assuming H&lt;sub&gt;0&lt;/sub&gt; = 75 km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;), and correcting for differences in spectral fitting techniques and waveband.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=etgalxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/etgalxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ETGALXRAY [2]</TD>
            <TD>Early-Type Galaxies X-Ray Luminosities Catalog</TD>
            <TD>This table contains a catalog of X-ray luminosities for 401 early-type galaxies (and 24 other galaxies which were listed in previuous studies as early but which have LEDA T-types &gt;= -1.5), of which 136 are based on newly analysed ROSAT PSPC pointed observations. The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. In their paper, the authors use this sample to fit the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation for early-type galaxies and find a best-fit slope for the catalog of ~ 2.2. The authors demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modeled by a single power-law fit. They also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L&lt;sub&gt;(discrete-source-contribution)&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; ~ 29.5 erg s&lt;sup&gt;-1&lt;/sup&gt;/L&lt;sub&gt;Bsun&lt;/sub&gt;. The authors compare this result with luminosities from their catalog. Lastly, they examine the influence of environment on galaxy X-ray luminosity and on the form of the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation. They conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations. The sample of early-type galaxies was selected from the Lyon-Meudon Extragalactic Data Archive (LEDA). This catalog at that time contained information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and morphological data. Galaxies were selected using the following criteria: (i) Morphological Type T &lt; -1.5 (i.e. E, E-S0 and S0 galaxies). (ii) Virgo-corrected recession velocity V &lt;= 9,000 km s&lt;sup&gt;-1&lt;/sup&gt;. (iii) Apparent Magnitude B&lt;sub&gt;T&lt;/sub&gt; &lt;= 13.5. The redshift and apparent magnitude restrictions were chosen in order to minimize the effects of incompleteness on their sample. The LEDA catalogue is known to be 90 per cent complete at B&lt;sub&gt;T&lt;/sub&gt; = 14.5, so the selection should be close to statistical completeness. The selection process produced ~ 700 objects. The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. All of the X-ray luminosities have been converted to a common format based on a reliable distance scale (assuming H&lt;sub&gt;0&lt;/sub&gt; = 75 km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;), and correcting for differences in spectral fitting techniques and waveband.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=etgalxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/etgalxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ETGALXRAY [3]</TD>
            <TD>Early-Type Galaxies X-Ray Luminosities Catalog</TD>
            <TD>This table contains a catalog of X-ray luminosities for 401 early-type galaxies (and 24 other galaxies which were listed in previuous studies as early but which have LEDA T-types &gt;= -1.5), of which 136 are based on newly analysed ROSAT PSPC pointed observations. The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. In their paper, the authors use this sample to fit the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation for early-type galaxies and find a best-fit slope for the catalog of ~ 2.2. The authors demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modeled by a single power-law fit. They also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L&lt;sub&gt;(discrete-source-contribution)&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; ~ 29.5 erg s&lt;sup&gt;-1&lt;/sup&gt;/L&lt;sub&gt;Bsun&lt;/sub&gt;. The authors compare this result with luminosities from their catalog. Lastly, they examine the influence of environment on galaxy X-ray luminosity and on the form of the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation. They conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations. The sample of early-type galaxies was selected from the Lyon-Meudon Extragalactic Data Archive (LEDA). This catalog at that time contained information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and morphological data. Galaxies were selected using the following criteria: (i) Morphological Type T &lt; -1.5 (i.e. E, E-S0 and S0 galaxies). (ii) Virgo-corrected recession velocity V &lt;= 9,000 km s&lt;sup&gt;-1&lt;/sup&gt;. (iii) Apparent Magnitude B&lt;sub&gt;T&lt;/sub&gt; &lt;= 13.5. The redshift and apparent magnitude restrictions were chosen in order to minimize the effects of incompleteness on their sample. The LEDA catalogue is known to be 90 per cent complete at B&lt;sub&gt;T&lt;/sub&gt; = 14.5, so the selection should be close to statistical completeness. The selection process produced ~ 700 objects. The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. All of the X-ray luminosities have been converted to a common format based on a reliable distance scale (assuming H&lt;sub&gt;0&lt;/sub&gt; = 75 km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;), and correcting for differences in spectral fitting techniques and waveband.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_etgalxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/etgalxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/163 [1]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#1</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/163</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/163 [2]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#2</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/163&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table3]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table3</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table2]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table2</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table5]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table5</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table7]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table7</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/312/442 [1]</TD>
            <TD>UV-selected galaxy redshift survey. II. (Sullivan+, 2000)</TD>
            <TD>We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000{AA} from the FOCA balloon-borne imaging camera of Milliard et al. (1992A&amp;A...257...24M). This work represents an extension of the initial study by Treyer et al. (Cat. &lt;J/MNRAS/300/303&gt;). Our enlarged catalogue contains 433 sources (~3 times as many as in our earlier study) across two FOCA fields. 273 of these are galaxies, nearly all with redshifts z~0-0.4. Nebular emission-line measurements are available for 216 galaxies, allowing us to address issues of excitation, reddening and metallicity. The UV and H{alpha} luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0&lt;z&lt;0.4. Our data are more consistent with a modest evolutionary trend, as suggested by recent redshift survey results. Investigating the emission-line properties, we find no evidence for a significant number of AGN in our sample; most UV-selected sources to z~0.4 are intense star-forming galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442#1</TD>
            <TD>2012-11-13T14:10:02Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/312/442</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/442</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/312/442 [2]</TD>
            <TD>UV-selected galaxy redshift survey. II. (Sullivan+, 2000)</TD>
            <TD>We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000{AA} from the FOCA balloon-borne imaging camera of Milliard et al. (1992A&amp;A...257...24M). This work represents an extension of the initial study by Treyer et al. (Cat. &lt;J/MNRAS/300/303&gt;). Our enlarged catalogue contains 433 sources (~3 times as many as in our earlier study) across two FOCA fields. 273 of these are galaxies, nearly all with redshifts z~0-0.4. Nebular emission-line measurements are available for 216 galaxies, allowing us to address issues of excitation, reddening and metallicity. The UV and H{alpha} luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0&lt;z&lt;0.4. Our data are more consistent with a modest evolutionary trend, as suggested by recent redshift survey results. Investigating the emission-line properties, we find no evidence for a significant number of AGN in our sample; most UV-selected sources to z~0.4 are intense star-forming galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442#2</TD>
            <TD>2012-11-13T14:10:02Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/312/442&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/442</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/312/442 [table7]</TD>
            <TD>UV-selected galaxy redshift survey. II. (Sullivan+, 2000)</TD>
            <TD>We present further spectroscopic observations for a sample of galaxies selected in the vacuum ultraviolet (UV) at 2000{AA} from the FOCA balloon-borne imaging camera of Milliard et al. (1992A&amp;A...257...24M). This work represents an extension of the initial study by Treyer et al. (Cat. &lt;J/MNRAS/300/303&gt;). Our enlarged catalogue contains 433 sources (~3 times as many as in our earlier study) across two FOCA fields. 273 of these are galaxies, nearly all with redshifts z~0-0.4. Nebular emission-line measurements are available for 216 galaxies, allowing us to address issues of excitation, reddening and metallicity. The UV and H{alpha} luminosity functions strengthen our earlier assertions that the local volume-averaged star formation rate is higher than indicated from earlier surveys. Moreover, internally within our sample, we do not find a steep rise in the UV luminosity density with redshift over 0&lt;z&lt;0.4. Our data are more consistent with a modest evolutionary trend, as suggested by recent redshift survey results. Investigating the emission-line properties, we find no evidence for a significant number of AGN in our sample; most UV-selected sources to z~0.4 are intense star-forming galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442#table7</TD>
            <TD>2012-11-13T14:10:02Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/442</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/312/442&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/442</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/163 [1]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#1</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/163</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/163 [2]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#2</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/163&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table3]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table3</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table2]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table2</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table5]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table5</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table7]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table7</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ETGALXRAY [1]</TD>
            <TD>Early-Type Galaxies X-Ray Luminosities Catalog</TD>
            <TD>This table contains a catalog of X-ray luminosities for 401 early-type galaxies (and 24 other galaxies which were listed in previuous studies as early but which have LEDA T-types &gt;= -1.5), of which 136 are based on newly analysed ROSAT PSPC pointed observations. The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. In their paper, the authors use this sample to fit the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation for early-type galaxies and find a best-fit slope for the catalog of ~ 2.2. The authors demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modeled by a single power-law fit. They also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L&lt;sub&gt;(discrete-source-contribution)&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; ~ 29.5 erg s&lt;sup&gt;-1&lt;/sup&gt;/L&lt;sub&gt;Bsun&lt;/sub&gt;. The authors compare this result with luminosities from their catalog. Lastly, they examine the influence of environment on galaxy X-ray luminosity and on the form of the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation. They conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations. The sample of early-type galaxies was selected from the Lyon-Meudon Extragalactic Data Archive (LEDA). This catalog at that time contained information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and morphological data. Galaxies were selected using the following criteria: (i) Morphological Type T &lt; -1.5 (i.e. E, E-S0 and S0 galaxies). (ii) Virgo-corrected recession velocity V &lt;= 9,000 km s&lt;sup&gt;-1&lt;/sup&gt;. (iii) Apparent Magnitude B&lt;sub&gt;T&lt;/sub&gt; &lt;= 13.5. The redshift and apparent magnitude restrictions were chosen in order to minimize the effects of incompleteness on their sample. The LEDA catalogue is known to be 90 per cent complete at B&lt;sub&gt;T&lt;/sub&gt; = 14.5, so the selection should be close to statistical completeness. The selection process produced ~ 700 objects. The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. All of the X-ray luminosities have been converted to a common format based on a reliable distance scale (assuming H&lt;sub&gt;0&lt;/sub&gt; = 75 km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;), and correcting for differences in spectral fitting techniques and waveband.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalxray#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalxray</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=etgalxray&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/etgalxray.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ETGALXRAY [2]</TD>
            <TD>Early-Type Galaxies X-Ray Luminosities Catalog</TD>
            <TD>This table contains a catalog of X-ray luminosities for 401 early-type galaxies (and 24 other galaxies which were listed in previuous studies as early but which have LEDA T-types &gt;= -1.5), of which 136 are based on newly analysed ROSAT PSPC pointed observations. The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. In their paper, the authors use this sample to fit the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation for early-type galaxies and find a best-fit slope for the catalog of ~ 2.2. The authors demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modeled by a single power-law fit. They also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L&lt;sub&gt;(discrete-source-contribution)&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; ~ 29.5 erg s&lt;sup&gt;-1&lt;/sup&gt;/L&lt;sub&gt;Bsun&lt;/sub&gt;. The authors compare this result with luminosities from their catalog. Lastly, they examine the influence of environment on galaxy X-ray luminosity and on the form of the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation. They conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations. The sample of early-type galaxies was selected from the Lyon-Meudon Extragalactic Data Archive (LEDA). This catalog at that time contained information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and morphological data. Galaxies were selected using the following criteria: (i) Morphological Type T &lt; -1.5 (i.e. E, E-S0 and S0 galaxies). (ii) Virgo-corrected recession velocity V &lt;= 9,000 km s&lt;sup&gt;-1&lt;/sup&gt;. (iii) Apparent Magnitude B&lt;sub&gt;T&lt;/sub&gt; &lt;= 13.5. The redshift and apparent magnitude restrictions were chosen in order to minimize the effects of incompleteness on their sample. The LEDA catalogue is known to be 90 per cent complete at B&lt;sub&gt;T&lt;/sub&gt; = 14.5, so the selection should be close to statistical completeness. The selection process produced ~ 700 objects. The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. All of the X-ray luminosities have been converted to a common format based on a reliable distance scale (assuming H&lt;sub&gt;0&lt;/sub&gt; = 75 km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;), and correcting for differences in spectral fitting techniques and waveband.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalxray#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=etgalxray&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/etgalxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ETGALXRAY [3]</TD>
            <TD>Early-Type Galaxies X-Ray Luminosities Catalog</TD>
            <TD>This table contains a catalog of X-ray luminosities for 401 early-type galaxies (and 24 other galaxies which were listed in previuous studies as early but which have LEDA T-types &gt;= -1.5), of which 136 are based on newly analysed ROSAT PSPC pointed observations. The remaining luminosities are taken from the literature and converted to a common energy band, spectral model and distance scale. In their paper, the authors use this sample to fit the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation for early-type galaxies and find a best-fit slope for the catalog of ~ 2.2. The authors demonstrate the influence of group-dominant galaxies on the fit and present evidence that the relation is not well modeled by a single power-law fit. They also derive estimates of the contribution to galaxy X-ray luminosities from discrete-sources and conclude that they provide L&lt;sub&gt;(discrete-source-contribution)&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; ~ 29.5 erg s&lt;sup&gt;-1&lt;/sup&gt;/L&lt;sub&gt;Bsun&lt;/sub&gt;. The authors compare this result with luminosities from their catalog. Lastly, they examine the influence of environment on galaxy X-ray luminosity and on the form of the L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;B&lt;/sub&gt; relation. They conclude that although environment undoubtedly affects the X-ray properties of individual galaxies, particularly those in the centres of groups and clusters, it does not change the nature of whole populations. The sample of early-type galaxies was selected from the Lyon-Meudon Extragalactic Data Archive (LEDA). This catalog at that time contained information on ~ 100,000 galaxies, of which ~ 40,000 had redshift and morphological data. Galaxies were selected using the following criteria: (i) Morphological Type T &lt; -1.5 (i.e. E, E-S0 and S0 galaxies). (ii) Virgo-corrected recession velocity V &lt;= 9,000 km s&lt;sup&gt;-1&lt;/sup&gt;. (iii) Apparent Magnitude B&lt;sub&gt;T&lt;/sub&gt; &lt;= 13.5. The redshift and apparent magnitude restrictions were chosen in order to minimize the effects of incompleteness on their sample. The LEDA catalogue is known to be 90 per cent complete at B&lt;sub&gt;T&lt;/sub&gt; = 14.5, so the selection should be close to statistical completeness. The selection process produced ~ 700 objects. The authors then cross-correlated this list with a list of public ROSAT PSPC pointings. Only pointings within 30 arcminutes of the target were accepted, as, further off-axis, the PSPC point-spread function becomes large enough to make analysis problematic. This left 209 galaxies with X-ray data available. The authors also added data from previously published catalogs, ROSAT PSPC All-Sky Survey values from Beuing et al. (1999, MNRAS, 302, 209), and Einstein IPC values from Fabbiano et al. (1992, ApJS, 80, 531) and Roberts et al. (1991, ApJS, 75, 751). These other references use a range of models to fit the data, different wavebands, distances and blue luminosities. O'Sullivan et al. corrected for these differences by converting the catalogs to a common set of values, as used for their own results. All of the X-ray luminosities have been converted to a common format based on a reliable distance scale (assuming H&lt;sub&gt;0&lt;/sub&gt; = 75 km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt;), and correcting for differences in spectral fitting techniques and waveband.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/etgalxray#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/etgalxray</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_etgalxray&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/etgalxray.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/163 [1]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#1</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/163</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/163 [2]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#2</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/163&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table3]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table3</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table2]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table2</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table5]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table5</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/163 [table7]</TD>
            <TD>Galaxy morphological classification (Lotz+, 2004)</TD>
            <TD>We present two new nonparametric methods for quantifying galaxy morphology: the relative distribution of the galaxy pixel flux values (the Gini coefficient or G) and the second-order moment of the brightest 20% of the galaxy's flux (M_20_). We test the robustness of G and M_20_ to decreasing signal-to-noise ratio (S/N) and spatial resolution and find that both measures are reliable to within 10% for images with average S/N per pixel greater than 2 and resolutions better than 1000 and 500pc, respectively. We have measured G and M_20_, as well as concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame near-ultraviolet/optical wavelengths for 148 bright local "normal" Hubble-type galaxies (E-Sd) galaxies, 22 dwarf irregulars, and 73 0.05&lt;z&lt;0.25 ultraluminous infrared galaxies (ULIRGs).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163#table7</TD>
            <TD>2011-09-14T19:54:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/163</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/27/170 [1]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#1</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/27/170</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/27/170 [2]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#2</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/27/170&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/27/170 [table2]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#table2</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/27/170&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/27/170 [table1]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#table1</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/27/170&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/491/93 [1]</TD>
            <TD>JHK photometry of 9 gamma-ray burst fields (Larson+ 1997)</TD>
            <TD>Results of a deep, near-infrared survey of a predetermined, consistent sample of gamma-ray burst localizations are presented. This systematic study, conducted from 1994 to 1996, is the first to be designed specifically to examine the extragalactic content of these regions of sky. JHK images of nine of the smallest error boxes from the third Interplanetary Network together with 70arcmin^2^ of control fields were obtained reaching levels up to 200 times fainter than those reached by previous infrared studies of burst locations. Photometric measurements and star/galaxy separation measurements of more than 3000 detected objects were made. An overabundance of brighter galaxies exists in the gamma-ray burst images at the 98% confidence level, which indicates that the bursts are cosmological. Both the level of this enhancement and the galaxy brightness, where it appears, match what is expected for host galaxies. As a group, the brightest galaxy within each error box is slightly brighter than normal but is still consistent with a random population of galaxies. Their positions within the boxes are also consistent with a random distribution, with no preference toward the center. The bright galaxy excess in these regions of sky, combined with a seemingly random population of brightest error box galaxies, suggest that either the true host galaxies are fainter or the error boxes do not point accurately to the hosts.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93#1</TD>
            <TD>2011-09-14T19:54:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/491/93</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/93</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/491/93 [2]</TD>
            <TD>JHK photometry of 9 gamma-ray burst fields (Larson+ 1997)</TD>
            <TD>Results of a deep, near-infrared survey of a predetermined, consistent sample of gamma-ray burst localizations are presented. This systematic study, conducted from 1994 to 1996, is the first to be designed specifically to examine the extragalactic content of these regions of sky. JHK images of nine of the smallest error boxes from the third Interplanetary Network together with 70arcmin^2^ of control fields were obtained reaching levels up to 200 times fainter than those reached by previous infrared studies of burst locations. Photometric measurements and star/galaxy separation measurements of more than 3000 detected objects were made. An overabundance of brighter galaxies exists in the gamma-ray burst images at the 98% confidence level, which indicates that the bursts are cosmological. Both the level of this enhancement and the galaxy brightness, where it appears, match what is expected for host galaxies. As a group, the brightest galaxy within each error box is slightly brighter than normal but is still consistent with a random population of galaxies. Their positions within the boxes are also consistent with a random distribution, with no preference toward the center. The bright galaxy excess in these regions of sky, combined with a seemingly random population of brightest error box galaxies, suggest that either the true host galaxies are fainter or the error boxes do not point accurately to the hosts.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93#2</TD>
            <TD>2011-09-14T19:54:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/491/93&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/93</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/491/93 [grbcat]</TD>
            <TD>JHK photometry of 9 gamma-ray burst fields (Larson+ 1997)</TD>
            <TD>Results of a deep, near-infrared survey of a predetermined, consistent sample of gamma-ray burst localizations are presented. This systematic study, conducted from 1994 to 1996, is the first to be designed specifically to examine the extragalactic content of these regions of sky. JHK images of nine of the smallest error boxes from the third Interplanetary Network together with 70arcmin^2^ of control fields were obtained reaching levels up to 200 times fainter than those reached by previous infrared studies of burst locations. Photometric measurements and star/galaxy separation measurements of more than 3000 detected objects were made. An overabundance of brighter galaxies exists in the gamma-ray burst images at the 98% confidence level, which indicates that the bursts are cosmological. Both the level of this enhancement and the galaxy brightness, where it appears, match what is expected for host galaxies. As a group, the brightest galaxy within each error box is slightly brighter than normal but is still consistent with a random population of galaxies. Their positions within the boxes are also consistent with a random distribution, with no preference toward the center. The bright galaxy excess in these regions of sky, combined with a seemingly random population of brightest error box galaxies, suggest that either the true host galaxies are fainter or the error boxes do not point accurately to the hosts.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93#grbcat</TD>
            <TD>2011-09-14T19:54:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>13-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/491/93&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/93</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC1291CXO [1]</TD>
            <TD>NGC 1291 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from a study of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. Utilizing the four available Chandra observations totaling an effective exposure of 179 ks, the authors detect 169 X-ray point sources in the galaxy in the full band (0.3 - 8.0 keV) with a false-positive probability threshold of 10&lt;sup&gt;-6&lt;/sup&gt; (implying approximately 2 false detections given the size of the image). Of these sources, 75 are in the bulge and 71 are in the ring. The authors report photometric properties of these sources in a point-source catalog. There are ~ 40% of the bulge sources and ~ 25% of the ring sources showing &gt; 3-sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (~ 75%) and ring (~ 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. The authors construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. They reach 90% completeness limits of ~ 1.5 x 10&lt;sup&gt;37&lt;/sup&gt; and ~ 2.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. In the paper, the authors perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. They compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1291cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1291cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc1291cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1291cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC1291CXO [2]</TD>
            <TD>NGC 1291 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from a study of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. Utilizing the four available Chandra observations totaling an effective exposure of 179 ks, the authors detect 169 X-ray point sources in the galaxy in the full band (0.3 - 8.0 keV) with a false-positive probability threshold of 10&lt;sup&gt;-6&lt;/sup&gt; (implying approximately 2 false detections given the size of the image). Of these sources, 75 are in the bulge and 71 are in the ring. The authors report photometric properties of these sources in a point-source catalog. There are ~ 40% of the bulge sources and ~ 25% of the ring sources showing &gt; 3-sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (~ 75%) and ring (~ 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. The authors construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. They reach 90% completeness limits of ~ 1.5 x 10&lt;sup&gt;37&lt;/sup&gt; and ~ 2.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. In the paper, the authors perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. They compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1291cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1291cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc1291cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1291cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC1291CXO [3]</TD>
            <TD>NGC 1291 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from a study of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. Utilizing the four available Chandra observations totaling an effective exposure of 179 ks, the authors detect 169 X-ray point sources in the galaxy in the full band (0.3 - 8.0 keV) with a false-positive probability threshold of 10&lt;sup&gt;-6&lt;/sup&gt; (implying approximately 2 false detections given the size of the image). Of these sources, 75 are in the bulge and 71 are in the ring. The authors report photometric properties of these sources in a point-source catalog. There are ~ 40% of the bulge sources and ~ 25% of the ring sources showing &gt; 3-sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (~ 75%) and ring (~ 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. The authors construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. They reach 90% completeness limits of ~ 1.5 x 10&lt;sup&gt;37&lt;/sup&gt; and ~ 2.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. In the paper, the authors perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. They compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1291cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1291cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc1291cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1291cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/491/93 [1]</TD>
            <TD>JHK photometry of 9 gamma-ray burst fields (Larson+ 1997)</TD>
            <TD>Results of a deep, near-infrared survey of a predetermined, consistent sample of gamma-ray burst localizations are presented. This systematic study, conducted from 1994 to 1996, is the first to be designed specifically to examine the extragalactic content of these regions of sky. JHK images of nine of the smallest error boxes from the third Interplanetary Network together with 70arcmin^2^ of control fields were obtained reaching levels up to 200 times fainter than those reached by previous infrared studies of burst locations. Photometric measurements and star/galaxy separation measurements of more than 3000 detected objects were made. An overabundance of brighter galaxies exists in the gamma-ray burst images at the 98% confidence level, which indicates that the bursts are cosmological. Both the level of this enhancement and the galaxy brightness, where it appears, match what is expected for host galaxies. As a group, the brightest galaxy within each error box is slightly brighter than normal but is still consistent with a random population of galaxies. Their positions within the boxes are also consistent with a random distribution, with no preference toward the center. The bright galaxy excess in these regions of sky, combined with a seemingly random population of brightest error box galaxies, suggest that either the true host galaxies are fainter or the error boxes do not point accurately to the hosts.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93#1</TD>
            <TD>2011-09-14T19:54:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/491/93</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/93</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/491/93 [2]</TD>
            <TD>JHK photometry of 9 gamma-ray burst fields (Larson+ 1997)</TD>
            <TD>Results of a deep, near-infrared survey of a predetermined, consistent sample of gamma-ray burst localizations are presented. This systematic study, conducted from 1994 to 1996, is the first to be designed specifically to examine the extragalactic content of these regions of sky. JHK images of nine of the smallest error boxes from the third Interplanetary Network together with 70arcmin^2^ of control fields were obtained reaching levels up to 200 times fainter than those reached by previous infrared studies of burst locations. Photometric measurements and star/galaxy separation measurements of more than 3000 detected objects were made. An overabundance of brighter galaxies exists in the gamma-ray burst images at the 98% confidence level, which indicates that the bursts are cosmological. Both the level of this enhancement and the galaxy brightness, where it appears, match what is expected for host galaxies. As a group, the brightest galaxy within each error box is slightly brighter than normal but is still consistent with a random population of galaxies. Their positions within the boxes are also consistent with a random distribution, with no preference toward the center. The bright galaxy excess in these regions of sky, combined with a seemingly random population of brightest error box galaxies, suggest that either the true host galaxies are fainter or the error boxes do not point accurately to the hosts.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93#2</TD>
            <TD>2011-09-14T19:54:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/491/93&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/93</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/491/93 [grbcat]</TD>
            <TD>JHK photometry of 9 gamma-ray burst fields (Larson+ 1997)</TD>
            <TD>Results of a deep, near-infrared survey of a predetermined, consistent sample of gamma-ray burst localizations are presented. This systematic study, conducted from 1994 to 1996, is the first to be designed specifically to examine the extragalactic content of these regions of sky. JHK images of nine of the smallest error boxes from the third Interplanetary Network together with 70arcmin^2^ of control fields were obtained reaching levels up to 200 times fainter than those reached by previous infrared studies of burst locations. Photometric measurements and star/galaxy separation measurements of more than 3000 detected objects were made. An overabundance of brighter galaxies exists in the gamma-ray burst images at the 98% confidence level, which indicates that the bursts are cosmological. Both the level of this enhancement and the galaxy brightness, where it appears, match what is expected for host galaxies. As a group, the brightest galaxy within each error box is slightly brighter than normal but is still consistent with a random population of galaxies. Their positions within the boxes are also consistent with a random distribution, with no preference toward the center. The bright galaxy excess in these regions of sky, combined with a seemingly random population of brightest error box galaxies, suggest that either the true host galaxies are fainter or the error boxes do not point accurately to the hosts.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93#grbcat</TD>
            <TD>2011-09-14T19:54:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/491/93&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/93</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/27/170 [1]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#1</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/27/170</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/27/170 [2]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#2</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/27/170&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/27/170 [table2]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#table2</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/27/170&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/27/170 [table1]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#table1</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/27/170&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/491/93 [1]</TD>
            <TD>JHK photometry of 9 gamma-ray burst fields (Larson+ 1997)</TD>
            <TD>Results of a deep, near-infrared survey of a predetermined, consistent sample of gamma-ray burst localizations are presented. This systematic study, conducted from 1994 to 1996, is the first to be designed specifically to examine the extragalactic content of these regions of sky. JHK images of nine of the smallest error boxes from the third Interplanetary Network together with 70arcmin^2^ of control fields were obtained reaching levels up to 200 times fainter than those reached by previous infrared studies of burst locations. Photometric measurements and star/galaxy separation measurements of more than 3000 detected objects were made. An overabundance of brighter galaxies exists in the gamma-ray burst images at the 98% confidence level, which indicates that the bursts are cosmological. Both the level of this enhancement and the galaxy brightness, where it appears, match what is expected for host galaxies. As a group, the brightest galaxy within each error box is slightly brighter than normal but is still consistent with a random population of galaxies. Their positions within the boxes are also consistent with a random distribution, with no preference toward the center. The bright galaxy excess in these regions of sky, combined with a seemingly random population of brightest error box galaxies, suggest that either the true host galaxies are fainter or the error boxes do not point accurately to the hosts.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93#1</TD>
            <TD>2011-09-14T19:54:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/491/93</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/93</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/491/93 [2]</TD>
            <TD>JHK photometry of 9 gamma-ray burst fields (Larson+ 1997)</TD>
            <TD>Results of a deep, near-infrared survey of a predetermined, consistent sample of gamma-ray burst localizations are presented. This systematic study, conducted from 1994 to 1996, is the first to be designed specifically to examine the extragalactic content of these regions of sky. JHK images of nine of the smallest error boxes from the third Interplanetary Network together with 70arcmin^2^ of control fields were obtained reaching levels up to 200 times fainter than those reached by previous infrared studies of burst locations. Photometric measurements and star/galaxy separation measurements of more than 3000 detected objects were made. An overabundance of brighter galaxies exists in the gamma-ray burst images at the 98% confidence level, which indicates that the bursts are cosmological. Both the level of this enhancement and the galaxy brightness, where it appears, match what is expected for host galaxies. As a group, the brightest galaxy within each error box is slightly brighter than normal but is still consistent with a random population of galaxies. Their positions within the boxes are also consistent with a random distribution, with no preference toward the center. The bright galaxy excess in these regions of sky, combined with a seemingly random population of brightest error box galaxies, suggest that either the true host galaxies are fainter or the error boxes do not point accurately to the hosts.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93#2</TD>
            <TD>2011-09-14T19:54:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/491/93&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/93</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/491/93 [grbcat]</TD>
            <TD>JHK photometry of 9 gamma-ray burst fields (Larson+ 1997)</TD>
            <TD>Results of a deep, near-infrared survey of a predetermined, consistent sample of gamma-ray burst localizations are presented. This systematic study, conducted from 1994 to 1996, is the first to be designed specifically to examine the extragalactic content of these regions of sky. JHK images of nine of the smallest error boxes from the third Interplanetary Network together with 70arcmin^2^ of control fields were obtained reaching levels up to 200 times fainter than those reached by previous infrared studies of burst locations. Photometric measurements and star/galaxy separation measurements of more than 3000 detected objects were made. An overabundance of brighter galaxies exists in the gamma-ray burst images at the 98% confidence level, which indicates that the bursts are cosmological. Both the level of this enhancement and the galaxy brightness, where it appears, match what is expected for host galaxies. As a group, the brightest galaxy within each error box is slightly brighter than normal but is still consistent with a random population of galaxies. Their positions within the boxes are also consistent with a random distribution, with no preference toward the center. The bright galaxy excess in these regions of sky, combined with a seemingly random population of brightest error box galaxies, suggest that either the true host galaxies are fainter or the error boxes do not point accurately to the hosts.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93#grbcat</TD>
            <TD>2011-09-14T19:54:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/491/93</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/491/93&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/491/93</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC1291CXO [1]</TD>
            <TD>NGC 1291 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from a study of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. Utilizing the four available Chandra observations totaling an effective exposure of 179 ks, the authors detect 169 X-ray point sources in the galaxy in the full band (0.3 - 8.0 keV) with a false-positive probability threshold of 10&lt;sup&gt;-6&lt;/sup&gt; (implying approximately 2 false detections given the size of the image). Of these sources, 75 are in the bulge and 71 are in the ring. The authors report photometric properties of these sources in a point-source catalog. There are ~ 40% of the bulge sources and ~ 25% of the ring sources showing &gt; 3-sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (~ 75%) and ring (~ 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. The authors construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. They reach 90% completeness limits of ~ 1.5 x 10&lt;sup&gt;37&lt;/sup&gt; and ~ 2.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. In the paper, the authors perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. They compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1291cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1291cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc1291cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1291cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC1291CXO [2]</TD>
            <TD>NGC 1291 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from a study of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. Utilizing the four available Chandra observations totaling an effective exposure of 179 ks, the authors detect 169 X-ray point sources in the galaxy in the full band (0.3 - 8.0 keV) with a false-positive probability threshold of 10&lt;sup&gt;-6&lt;/sup&gt; (implying approximately 2 false detections given the size of the image). Of these sources, 75 are in the bulge and 71 are in the ring. The authors report photometric properties of these sources in a point-source catalog. There are ~ 40% of the bulge sources and ~ 25% of the ring sources showing &gt; 3-sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (~ 75%) and ring (~ 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. The authors construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. They reach 90% completeness limits of ~ 1.5 x 10&lt;sup&gt;37&lt;/sup&gt; and ~ 2.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. In the paper, the authors perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. They compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1291cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1291cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc1291cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1291cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC1291CXO [3]</TD>
            <TD>NGC 1291 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from a study of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. Utilizing the four available Chandra observations totaling an effective exposure of 179 ks, the authors detect 169 X-ray point sources in the galaxy in the full band (0.3 - 8.0 keV) with a false-positive probability threshold of 10&lt;sup&gt;-6&lt;/sup&gt; (implying approximately 2 false detections given the size of the image). Of these sources, 75 are in the bulge and 71 are in the ring. The authors report photometric properties of these sources in a point-source catalog. There are ~ 40% of the bulge sources and ~ 25% of the ring sources showing &gt; 3-sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (~ 75%) and ring (~ 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. The authors construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. They reach 90% completeness limits of ~ 1.5 x 10&lt;sup&gt;37&lt;/sup&gt; and ~ 2.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. In the paper, the authors perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. They compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1291cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1291cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc1291cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1291cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/27/170 [1]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#1</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/27/170</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/27/170 [2]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#2</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/27/170&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/27/170 [table2]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#table2</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/27/170&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/27/170 [table1]</TD>
            <TD>BR photometry of the UMa galaxy supercluster (Kopylov+, 2001)</TD>
            <TD>A catalogue of 1192 galaxies in the central regions (30' x 30') of 11 clusters in the Ursa Major supercluster is presented. For each galaxy equatorial and relative coordinates and total B and R_c_ magnitudes and B-R_c_ colour are given. Plates taken with the 2-m Tautenburg Observatory telescope and CCD images obtained with the 6-m and 1-m SAO telescopes are used.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170#table1</TD>
            <TD>2012-11-13T14:14:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-March-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/170</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/27/170&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/170</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/305 [1]</TD>
            <TD>SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</TD>
            <TD>The SAGE project is a Cycle 2 legacy program on the Spitzer Space Telescope, entitled, "Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)", with Margaret Meixner (STScI) as the PI. The project overview and initial results are described in a paper by Meixner et al. (2006AJ....132.2268M). The Catalog is a highly reliable list of 6.4 million sources. Faint limits for SAGE are 18.1, 17.5, 15.3, and 14.2 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. The SAGE-SMC project is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, "SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud", with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2011AJ....142..102G). The Catalog is a highly reliable list of 2.0 million sources. Faint limits for SAGE-SMC are 18.3, 17.7, 15.7, and 14.5 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. IRAC Single Frame + Mosaic Photometry Catalog: a combination of mosaic photometry source list extracted from the combined Epoch 1 and Epoch 2 12 second frametime mosaics with all-epochs single frame source list, bandmerged with 2MASS or 2MASS6X. Detailed documentations are available from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE/doc/ as SAGEDataProductsDescription_Sep09.pdf and from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE-SMC/docs/ as sage-smc_delivery_apr11.pdf</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/305#1</TD>
            <TD>2012-03-09T12:22:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/II/305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/305 [2]</TD>
            <TD>SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</TD>
            <TD>The SAGE project is a Cycle 2 legacy program on the Spitzer Space Telescope, entitled, "Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)", with Margaret Meixner (STScI) as the PI. The project overview and initial results are described in a paper by Meixner et al. (2006AJ....132.2268M). The Catalog is a highly reliable list of 6.4 million sources. Faint limits for SAGE are 18.1, 17.5, 15.3, and 14.2 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. The SAGE-SMC project is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, "SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud", with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2011AJ....142..102G). The Catalog is a highly reliable list of 2.0 million sources. Faint limits for SAGE-SMC are 18.3, 17.7, 15.7, and 14.5 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. IRAC Single Frame + Mosaic Photometry Catalog: a combination of mosaic photometry source list extracted from the combined Epoch 1 and Epoch 2 12 second frametime mosaics with all-epochs single frame source list, bandmerged with 2MASS or 2MASS6X. Detailed documentations are available from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE/doc/ as SAGEDataProductsDescription_Sep09.pdf and from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE-SMC/docs/ as sage-smc_delivery_apr11.pdf</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/305#2</TD>
            <TD>2012-03-09T12:22:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/II/305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/305 [sage]</TD>
            <TD>SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</TD>
            <TD>The SAGE project is a Cycle 2 legacy program on the Spitzer Space Telescope, entitled, "Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)", with Margaret Meixner (STScI) as the PI. The project overview and initial results are described in a paper by Meixner et al. (2006AJ....132.2268M). The Catalog is a highly reliable list of 6.4 million sources. Faint limits for SAGE are 18.1, 17.5, 15.3, and 14.2 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. The SAGE-SMC project is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, "SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud", with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2011AJ....142..102G). The Catalog is a highly reliable list of 2.0 million sources. Faint limits for SAGE-SMC are 18.3, 17.7, 15.7, and 14.5 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. IRAC Single Frame + Mosaic Photometry Catalog: a combination of mosaic photometry source list extracted from the combined Epoch 1 and Epoch 2 12 second frametime mosaics with all-epochs single frame source list, bandmerged with 2MASS or 2MASS6X. Detailed documentations are available from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE/doc/ as SAGEDataProductsDescription_Sep09.pdf and from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE-SMC/docs/ as sage-smc_delivery_apr11.pdf</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/305#sage</TD>
            <TD>2012-03-09T12:22:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/II/305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PDS1P4GHZ [1]</TD>
            <TD>Phoenix Deep Survey 1.4-GHz Catalog</TD>
            <TD>The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 &lt; z &lt; 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 14&lt;sup&gt;m&lt;/sup&gt; 12.16&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 11&lt;sup&gt;m&lt;/sup&gt; 13.0&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; and reaches to a measured level of 12 microJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/pds1p4ghz#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pds1p4ghz</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=pds1p4ghz&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/pds1p4ghz.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PDS1P4GHZ [2]</TD>
            <TD>Phoenix Deep Survey 1.4-GHz Catalog</TD>
            <TD>The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 &lt; z &lt; 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 14&lt;sup&gt;m&lt;/sup&gt; 12.16&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 11&lt;sup&gt;m&lt;/sup&gt; 13.0&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; and reaches to a measured level of 12 microJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/pds1p4ghz#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pds1p4ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=pds1p4ghz&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/pds1p4ghz.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PDS1P4GHZ [3]</TD>
            <TD>Phoenix Deep Survey 1.4-GHz Catalog</TD>
            <TD>The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 &lt; z &lt; 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 14&lt;sup&gt;m&lt;/sup&gt; 12.16&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 11&lt;sup&gt;m&lt;/sup&gt; 13.0&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; and reaches to a measured level of 12 microJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/pds1p4ghz#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pds1p4ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_pds1p4ghz&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/pds1p4ghz.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/51/791 [1]</TD>
            <TD>Molecular clouds in southern HII regions (Yamaguchi+ 1999)</TD>
            <TD>We have carried out extensive ^13^CO(J=1-0) observations toward 23 southern H II regions associated with bright-rimmed clouds. In total, 95 molecular clouds have been identified to be associated with the H II regions. Among the 95, 57 clouds are found to be associated with 204 IRAS point sources which are candidates for young stellar objects. There is a significant increase of star-formation efficiency on the side facing to the H II regions; the luminosity-to-mass ratio, defined as the ratio of the stellar luminosity to the molecular cloud mass, is higher by an order of magnitude on the near side of the H II regions than that on the. far side. This indicates that molecular gas facing to the H II regions is more actively forming massive stars whose luminosity is ~&gt;10^3^L_{sun}_. In addition, the number density of the IRAS point sources increases by a factor of 2 on the near side of the H II regions compared with on the far side. These results strongly suggest that the active formation of massive stars on the near side of the H II regions is due to the effects of the H II regions, such as the compression of molecular material by the ionization/shock fronts. For the whole Galaxy, we estimate that the present star-formation rate under such effects is at least 0.2-0.4M_{sun}_/yr, corresponding to a few 10% by mass.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791#1</TD>
            <TD>2012-11-13T14:14:49Z</TD>
            <TD>#Nebulae#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/51/791</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/51/791</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/51/791 [2]</TD>
            <TD>Molecular clouds in southern HII regions (Yamaguchi+ 1999)</TD>
            <TD>We have carried out extensive ^13^CO(J=1-0) observations toward 23 southern H II regions associated with bright-rimmed clouds. In total, 95 molecular clouds have been identified to be associated with the H II regions. Among the 95, 57 clouds are found to be associated with 204 IRAS point sources which are candidates for young stellar objects. There is a significant increase of star-formation efficiency on the side facing to the H II regions; the luminosity-to-mass ratio, defined as the ratio of the stellar luminosity to the molecular cloud mass, is higher by an order of magnitude on the near side of the H II regions than that on the. far side. This indicates that molecular gas facing to the H II regions is more actively forming massive stars whose luminosity is ~&gt;10^3^L_{sun}_. In addition, the number density of the IRAS point sources increases by a factor of 2 on the near side of the H II regions compared with on the far side. These results strongly suggest that the active formation of massive stars on the near side of the H II regions is due to the effects of the H II regions, such as the compression of molecular material by the ionization/shock fronts. For the whole Galaxy, we estimate that the present star-formation rate under such effects is at least 0.2-0.4M_{sun}_/yr, corresponding to a few 10% by mass.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791#2</TD>
            <TD>2012-11-13T14:14:49Z</TD>
            <TD>#Nebulae#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/51/791&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/51/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/51/791 [clouds]</TD>
            <TD>Molecular clouds in southern HII regions (Yamaguchi+ 1999)</TD>
            <TD>We have carried out extensive ^13^CO(J=1-0) observations toward 23 southern H II regions associated with bright-rimmed clouds. In total, 95 molecular clouds have been identified to be associated with the H II regions. Among the 95, 57 clouds are found to be associated with 204 IRAS point sources which are candidates for young stellar objects. There is a significant increase of star-formation efficiency on the side facing to the H II regions; the luminosity-to-mass ratio, defined as the ratio of the stellar luminosity to the molecular cloud mass, is higher by an order of magnitude on the near side of the H II regions than that on the. far side. This indicates that molecular gas facing to the H II regions is more actively forming massive stars whose luminosity is ~&gt;10^3^L_{sun}_. In addition, the number density of the IRAS point sources increases by a factor of 2 on the near side of the H II regions compared with on the far side. These results strongly suggest that the active formation of massive stars on the near side of the H II regions is due to the effects of the H II regions, such as the compression of molecular material by the ionization/shock fronts. For the whole Galaxy, we estimate that the present star-formation rate under such effects is at least 0.2-0.4M_{sun}_/yr, corresponding to a few 10% by mass.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791#clouds</TD>
            <TD>2012-11-13T14:14:49Z</TD>
            <TD>#Nebulae#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/51/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/51/791</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/51/791 [1]</TD>
            <TD>Molecular clouds in southern HII regions (Yamaguchi+ 1999)</TD>
            <TD>We have carried out extensive ^13^CO(J=1-0) observations toward 23 southern H II regions associated with bright-rimmed clouds. In total, 95 molecular clouds have been identified to be associated with the H II regions. Among the 95, 57 clouds are found to be associated with 204 IRAS point sources which are candidates for young stellar objects. There is a significant increase of star-formation efficiency on the side facing to the H II regions; the luminosity-to-mass ratio, defined as the ratio of the stellar luminosity to the molecular cloud mass, is higher by an order of magnitude on the near side of the H II regions than that on the. far side. This indicates that molecular gas facing to the H II regions is more actively forming massive stars whose luminosity is ~&gt;10^3^L_{sun}_. In addition, the number density of the IRAS point sources increases by a factor of 2 on the near side of the H II regions compared with on the far side. These results strongly suggest that the active formation of massive stars on the near side of the H II regions is due to the effects of the H II regions, such as the compression of molecular material by the ionization/shock fronts. For the whole Galaxy, we estimate that the present star-formation rate under such effects is at least 0.2-0.4M_{sun}_/yr, corresponding to a few 10% by mass.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791#1</TD>
            <TD>2012-11-13T14:14:49Z</TD>
            <TD>#Nebulae#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/51/791</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/51/791</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/51/791 [2]</TD>
            <TD>Molecular clouds in southern HII regions (Yamaguchi+ 1999)</TD>
            <TD>We have carried out extensive ^13^CO(J=1-0) observations toward 23 southern H II regions associated with bright-rimmed clouds. In total, 95 molecular clouds have been identified to be associated with the H II regions. Among the 95, 57 clouds are found to be associated with 204 IRAS point sources which are candidates for young stellar objects. There is a significant increase of star-formation efficiency on the side facing to the H II regions; the luminosity-to-mass ratio, defined as the ratio of the stellar luminosity to the molecular cloud mass, is higher by an order of magnitude on the near side of the H II regions than that on the. far side. This indicates that molecular gas facing to the H II regions is more actively forming massive stars whose luminosity is ~&gt;10^3^L_{sun}_. In addition, the number density of the IRAS point sources increases by a factor of 2 on the near side of the H II regions compared with on the far side. These results strongly suggest that the active formation of massive stars on the near side of the H II regions is due to the effects of the H II regions, such as the compression of molecular material by the ionization/shock fronts. For the whole Galaxy, we estimate that the present star-formation rate under such effects is at least 0.2-0.4M_{sun}_/yr, corresponding to a few 10% by mass.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791#2</TD>
            <TD>2012-11-13T14:14:49Z</TD>
            <TD>#Nebulae#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/51/791&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/51/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/51/791 [clouds]</TD>
            <TD>Molecular clouds in southern HII regions (Yamaguchi+ 1999)</TD>
            <TD>We have carried out extensive ^13^CO(J=1-0) observations toward 23 southern H II regions associated with bright-rimmed clouds. In total, 95 molecular clouds have been identified to be associated with the H II regions. Among the 95, 57 clouds are found to be associated with 204 IRAS point sources which are candidates for young stellar objects. There is a significant increase of star-formation efficiency on the side facing to the H II regions; the luminosity-to-mass ratio, defined as the ratio of the stellar luminosity to the molecular cloud mass, is higher by an order of magnitude on the near side of the H II regions than that on the. far side. This indicates that molecular gas facing to the H II regions is more actively forming massive stars whose luminosity is ~&gt;10^3^L_{sun}_. In addition, the number density of the IRAS point sources increases by a factor of 2 on the near side of the H II regions compared with on the far side. These results strongly suggest that the active formation of massive stars on the near side of the H II regions is due to the effects of the H II regions, such as the compression of molecular material by the ionization/shock fronts. For the whole Galaxy, we estimate that the present star-formation rate under such effects is at least 0.2-0.4M_{sun}_/yr, corresponding to a few 10% by mass.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791#clouds</TD>
            <TD>2012-11-13T14:14:49Z</TD>
            <TD>#Nebulae#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/51/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/51/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC1291CXO [1]</TD>
            <TD>NGC 1291 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from a study of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. Utilizing the four available Chandra observations totaling an effective exposure of 179 ks, the authors detect 169 X-ray point sources in the galaxy in the full band (0.3 - 8.0 keV) with a false-positive probability threshold of 10&lt;sup&gt;-6&lt;/sup&gt; (implying approximately 2 false detections given the size of the image). Of these sources, 75 are in the bulge and 71 are in the ring. The authors report photometric properties of these sources in a point-source catalog. There are ~ 40% of the bulge sources and ~ 25% of the ring sources showing &gt; 3-sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (~ 75%) and ring (~ 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. The authors construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. They reach 90% completeness limits of ~ 1.5 x 10&lt;sup&gt;37&lt;/sup&gt; and ~ 2.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. In the paper, the authors perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. They compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1291cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1291cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc1291cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1291cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC1291CXO [2]</TD>
            <TD>NGC 1291 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from a study of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. Utilizing the four available Chandra observations totaling an effective exposure of 179 ks, the authors detect 169 X-ray point sources in the galaxy in the full band (0.3 - 8.0 keV) with a false-positive probability threshold of 10&lt;sup&gt;-6&lt;/sup&gt; (implying approximately 2 false detections given the size of the image). Of these sources, 75 are in the bulge and 71 are in the ring. The authors report photometric properties of these sources in a point-source catalog. There are ~ 40% of the bulge sources and ~ 25% of the ring sources showing &gt; 3-sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (~ 75%) and ring (~ 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. The authors construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. They reach 90% completeness limits of ~ 1.5 x 10&lt;sup&gt;37&lt;/sup&gt; and ~ 2.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. In the paper, the authors perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. They compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1291cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1291cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc1291cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1291cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC1291CXO [3]</TD>
            <TD>NGC 1291 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains some of the results from a study of the X-ray binary (XRB) populations in the bulge and ring regions of the ring galaxy NGC 1291. Utilizing the four available Chandra observations totaling an effective exposure of 179 ks, the authors detect 169 X-ray point sources in the galaxy in the full band (0.3 - 8.0 keV) with a false-positive probability threshold of 10&lt;sup&gt;-6&lt;/sup&gt; (implying approximately 2 false detections given the size of the image). Of these sources, 75 are in the bulge and 71 are in the ring. The authors report photometric properties of these sources in a point-source catalog. There are ~ 40% of the bulge sources and ~ 25% of the ring sources showing &gt; 3-sigma long-term variability in their X-ray count rate. The X-ray colors suggest that a significant fraction of the bulge (~ 75%) and ring (~ 65%) sources are likely low-mass X-ray binaries (LMXBs). The spectra of the nuclear source indicate that it is a low-luminosity active galactic nucleus (AGN) with moderate obscuration; spectral variability is observed between individual observations. The authors construct 0.3-8.0 keV X-ray luminosity functions (XLFs) for the bulge and ring XRB populations, taking into account the detection incompleteness and background AGN contamination. They reach 90% completeness limits of ~ 1.5 x 10&lt;sup&gt;37&lt;/sup&gt; and ~ 2.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; for the bulge and ring populations, respectively. Both XLFs can be fit with a broken power-law model, and the shapes are consistent with those expected for populations dominated by LMXBs. In the paper, the authors perform detailed population synthesis modeling of the XRB populations in NGC 1291, which suggests that the observed combined XLF is dominated by an old LMXB population. They compare the bulge and ring XRB populations, and argue that the ring XRBs are associated with a younger stellar population than the bulge sources, based on the relative overdensity of X-ray sources in the ring, the generally harder X-ray color of the ring sources, the overabundance of luminous sources in the combined XLF, and the flatter shape of the ring XLF.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1291cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1291cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc1291cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1291cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/305 [1]</TD>
            <TD>SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</TD>
            <TD>The SAGE project is a Cycle 2 legacy program on the Spitzer Space Telescope, entitled, "Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)", with Margaret Meixner (STScI) as the PI. The project overview and initial results are described in a paper by Meixner et al. (2006AJ....132.2268M). The Catalog is a highly reliable list of 6.4 million sources. Faint limits for SAGE are 18.1, 17.5, 15.3, and 14.2 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. The SAGE-SMC project is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, "SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud", with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2011AJ....142..102G). The Catalog is a highly reliable list of 2.0 million sources. Faint limits for SAGE-SMC are 18.3, 17.7, 15.7, and 14.5 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. IRAC Single Frame + Mosaic Photometry Catalog: a combination of mosaic photometry source list extracted from the combined Epoch 1 and Epoch 2 12 second frametime mosaics with all-epochs single frame source list, bandmerged with 2MASS or 2MASS6X. Detailed documentations are available from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE/doc/ as SAGEDataProductsDescription_Sep09.pdf and from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE-SMC/docs/ as sage-smc_delivery_apr11.pdf</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/305#1</TD>
            <TD>2012-03-09T12:22:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/II/305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/305 [2]</TD>
            <TD>SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</TD>
            <TD>The SAGE project is a Cycle 2 legacy program on the Spitzer Space Telescope, entitled, "Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)", with Margaret Meixner (STScI) as the PI. The project overview and initial results are described in a paper by Meixner et al. (2006AJ....132.2268M). The Catalog is a highly reliable list of 6.4 million sources. Faint limits for SAGE are 18.1, 17.5, 15.3, and 14.2 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. The SAGE-SMC project is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, "SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud", with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2011AJ....142..102G). The Catalog is a highly reliable list of 2.0 million sources. Faint limits for SAGE-SMC are 18.3, 17.7, 15.7, and 14.5 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. IRAC Single Frame + Mosaic Photometry Catalog: a combination of mosaic photometry source list extracted from the combined Epoch 1 and Epoch 2 12 second frametime mosaics with all-epochs single frame source list, bandmerged with 2MASS or 2MASS6X. Detailed documentations are available from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE/doc/ as SAGEDataProductsDescription_Sep09.pdf and from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE-SMC/docs/ as sage-smc_delivery_apr11.pdf</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/305#2</TD>
            <TD>2012-03-09T12:22:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/II/305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/305 [sage]</TD>
            <TD>SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</TD>
            <TD>The SAGE project is a Cycle 2 legacy program on the Spitzer Space Telescope, entitled, "Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)", with Margaret Meixner (STScI) as the PI. The project overview and initial results are described in a paper by Meixner et al. (2006AJ....132.2268M). The Catalog is a highly reliable list of 6.4 million sources. Faint limits for SAGE are 18.1, 17.5, 15.3, and 14.2 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. The SAGE-SMC project is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, "SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud", with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2011AJ....142..102G). The Catalog is a highly reliable list of 2.0 million sources. Faint limits for SAGE-SMC are 18.3, 17.7, 15.7, and 14.5 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. IRAC Single Frame + Mosaic Photometry Catalog: a combination of mosaic photometry source list extracted from the combined Epoch 1 and Epoch 2 12 second frametime mosaics with all-epochs single frame source list, bandmerged with 2MASS or 2MASS6X. Detailed documentations are available from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE/doc/ as SAGEDataProductsDescription_Sep09.pdf and from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE-SMC/docs/ as sage-smc_delivery_apr11.pdf</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/305#sage</TD>
            <TD>2012-03-09T12:22:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/II/305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PDS1P4GHZ [1]</TD>
            <TD>Phoenix Deep Survey 1.4-GHz Catalog</TD>
            <TD>The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 &lt; z &lt; 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 14&lt;sup&gt;m&lt;/sup&gt; 12.16&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 11&lt;sup&gt;m&lt;/sup&gt; 13.0&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; and reaches to a measured level of 12 microJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/pds1p4ghz#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pds1p4ghz</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=pds1p4ghz&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/pds1p4ghz.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PDS1P4GHZ [2]</TD>
            <TD>Phoenix Deep Survey 1.4-GHz Catalog</TD>
            <TD>The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 &lt; z &lt; 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 14&lt;sup&gt;m&lt;/sup&gt; 12.16&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 11&lt;sup&gt;m&lt;/sup&gt; 13.0&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; and reaches to a measured level of 12 microJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/pds1p4ghz#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pds1p4ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=pds1p4ghz&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/pds1p4ghz.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PDS1P4GHZ [3]</TD>
            <TD>Phoenix Deep Survey 1.4-GHz Catalog</TD>
            <TD>The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 &lt; z &lt; 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 14&lt;sup&gt;m&lt;/sup&gt; 12.16&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 11&lt;sup&gt;m&lt;/sup&gt; 13.0&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; and reaches to a measured level of 12 microJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/pds1p4ghz#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pds1p4ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_pds1p4ghz&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/pds1p4ghz.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/305 [1]</TD>
            <TD>SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</TD>
            <TD>The SAGE project is a Cycle 2 legacy program on the Spitzer Space Telescope, entitled, "Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)", with Margaret Meixner (STScI) as the PI. The project overview and initial results are described in a paper by Meixner et al. (2006AJ....132.2268M). The Catalog is a highly reliable list of 6.4 million sources. Faint limits for SAGE are 18.1, 17.5, 15.3, and 14.2 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. The SAGE-SMC project is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, "SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud", with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2011AJ....142..102G). The Catalog is a highly reliable list of 2.0 million sources. Faint limits for SAGE-SMC are 18.3, 17.7, 15.7, and 14.5 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. IRAC Single Frame + Mosaic Photometry Catalog: a combination of mosaic photometry source list extracted from the combined Epoch 1 and Epoch 2 12 second frametime mosaics with all-epochs single frame source list, bandmerged with 2MASS or 2MASS6X. Detailed documentations are available from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE/doc/ as SAGEDataProductsDescription_Sep09.pdf and from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE-SMC/docs/ as sage-smc_delivery_apr11.pdf</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/305#1</TD>
            <TD>2012-03-09T12:22:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/II/305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/305 [2]</TD>
            <TD>SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</TD>
            <TD>The SAGE project is a Cycle 2 legacy program on the Spitzer Space Telescope, entitled, "Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)", with Margaret Meixner (STScI) as the PI. The project overview and initial results are described in a paper by Meixner et al. (2006AJ....132.2268M). The Catalog is a highly reliable list of 6.4 million sources. Faint limits for SAGE are 18.1, 17.5, 15.3, and 14.2 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. The SAGE-SMC project is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, "SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud", with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2011AJ....142..102G). The Catalog is a highly reliable list of 2.0 million sources. Faint limits for SAGE-SMC are 18.3, 17.7, 15.7, and 14.5 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. IRAC Single Frame + Mosaic Photometry Catalog: a combination of mosaic photometry source list extracted from the combined Epoch 1 and Epoch 2 12 second frametime mosaics with all-epochs single frame source list, bandmerged with 2MASS or 2MASS6X. Detailed documentations are available from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE/doc/ as SAGEDataProductsDescription_Sep09.pdf and from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE-SMC/docs/ as sage-smc_delivery_apr11.pdf</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/305#2</TD>
            <TD>2012-03-09T12:22:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/II/305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/305 [sage]</TD>
            <TD>SAGE LMC and SMC IRAC Source Catalog (IPAC 2009)</TD>
            <TD>The SAGE project is a Cycle 2 legacy program on the Spitzer Space Telescope, entitled, "Spitzer Survey of the Large Magellanic Cloud: Surveying the Agents of a Galaxy's Evolution (SAGE)", with Margaret Meixner (STScI) as the PI. The project overview and initial results are described in a paper by Meixner et al. (2006AJ....132.2268M). The Catalog is a highly reliable list of 6.4 million sources. Faint limits for SAGE are 18.1, 17.5, 15.3, and 14.2 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. The SAGE-SMC project is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, "SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud", with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2011AJ....142..102G). The Catalog is a highly reliable list of 2.0 million sources. Faint limits for SAGE-SMC are 18.3, 17.7, 15.7, and 14.5 for IRAC 3.6, 4.5, 5.8, 8.0 um, respectively. IRAC Single Frame + Mosaic Photometry Catalog: a combination of mosaic photometry source list extracted from the combined Epoch 1 and Epoch 2 12 second frametime mosaics with all-epochs single frame source list, bandmerged with 2MASS or 2MASS6X. Detailed documentations are available from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE/doc/ as SAGEDataProductsDescription_Sep09.pdf and from http://irsa.ipac.caltech.edu/data/SPITZER/SAGE-SMC/docs/ as sage-smc_delivery_apr11.pdf</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/305#sage</TD>
            <TD>2012-03-09T12:22:14Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/II/305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC1893CXO [1]</TD>
            <TD>NGC 1893 Chandra X-Ray Point Source Catalog</TD>
            <TD>The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius &gt;= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10&lt;sup&gt;29.5&lt;/sup&gt; - 10&lt;sup&gt;31.5&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1893cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1893cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc1893cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1893cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC1893CXO [2]</TD>
            <TD>NGC 1893 Chandra X-Ray Point Source Catalog</TD>
            <TD>The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius &gt;= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10&lt;sup&gt;29.5&lt;/sup&gt; - 10&lt;sup&gt;31.5&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1893cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1893cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc1893cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1893cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC1893CXO [3]</TD>
            <TD>NGC 1893 Chandra X-Ray Point Source Catalog</TD>
            <TD>The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius &gt;= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10&lt;sup&gt;29.5&lt;/sup&gt; - 10&lt;sup&gt;31.5&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1893cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1893cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc1893cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1893cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PDS1P4GHZ [1]</TD>
            <TD>Phoenix Deep Survey 1.4-GHz Catalog</TD>
            <TD>The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 &lt; z &lt; 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 14&lt;sup&gt;m&lt;/sup&gt; 12.16&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 11&lt;sup&gt;m&lt;/sup&gt; 13.0&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; and reaches to a measured level of 12 microJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/pds1p4ghz#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pds1p4ghz</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=pds1p4ghz&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/pds1p4ghz.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PDS1P4GHZ [2]</TD>
            <TD>Phoenix Deep Survey 1.4-GHz Catalog</TD>
            <TD>The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 &lt; z &lt; 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 14&lt;sup&gt;m&lt;/sup&gt; 12.16&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 11&lt;sup&gt;m&lt;/sup&gt; 13.0&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; and reaches to a measured level of 12 microJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/pds1p4ghz#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pds1p4ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=pds1p4ghz&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/pds1p4ghz.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PDS1P4GHZ [3]</TD>
            <TD>Phoenix Deep Survey 1.4-GHz Catalog</TD>
            <TD>The initial Phoenix Deep Survey (PDS) observations with the Australia Telescope Compact Array (ATCA) have been supplemented by additional 1.4 GHz observations over the past few years. Here we present details of the construction of a new mosaic image covering an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; referred to as the Phoenix Deep field (PDF), an investigation of the reliability of the source measurements, and the 1.4 GHz source counts for the compiled radio catalog. The mosaic achieves a 1-sigma rms noise of 12 microJy at its most sensitive, and a homogeneous radio-selected catalog of over 2000 sources reaching flux densities as faint as 60 microJy has been compiled. The source parameter measurements are found to be consistent with the expected uncertainties from the image noise levels and the Gaussian source fitting procedure. A radio-selected sample avoids the complications of obscuration associated with optically selected samples, and by utilizing complementary PDS observations, including multicolor optical, near-infrared, and spectroscopic data, this radio catalog will be used in a detailed investigation of the evolution in star formation spanning the redshift range 0 &lt; z &lt; 1. The homogeneity of the catalog ensures a consistent picture of galaxy evolution can be developed over the full cosmologically significant redshift range of interest. The PDF covers a high-latitude region that is of low optical obscuration and devoid of bright radio sources. ATCA 1.4 GHz observations were made in 1994, 1997, 1999, 2000, and 2001 in the 6A, 6B, and 6C array configurations, accumulating a total of 523 hr of observing time. The initial 1994 ATCA observations (Hopkins et al. 1998, MNRAS, 296, 839; Hopkins 1998, PhD thesis) consisted of 30 pointings on a hexagonal tessellation, resulting in a 2 degrees diameter field centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 14&lt;sup&gt;m&lt;/sup&gt; 12.16&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 44' 8.0" (J2000.0), with roughly uniform sensitivity of about 60 microJy rms. This survey was supplemented from 1997 to 2001 by extensive observations of a further 19 pointings situated on a more finely spaced hexagonal grid, centered on R.A. = 01&lt;sup&gt;h&lt;/sup&gt; 11&lt;sup&gt;m&lt;/sup&gt; 13.0&lt;sup&gt;s&lt;/sup&gt;, Dec = -45&lt;sup&gt;o&lt;/sup&gt; 45' 00" (J2000.0). The locations of all pointing centers are given in Table 1 of the reference paper. The final mosaic constructed from all 49 pointings was trimmed to remove the highest noise regions at the edges by masking out regions with an rms noise level greater than 0.25 mJy. The trimmed PDF mosaic image covers an area of 4.56 deg&lt;sup&gt;2&lt;/sup&gt; and reaches to a measured level of 12 microJy rms noise in the most sensitive regions. The table contained here is the final merged catalog of PDS surveys based on the union of the 10% false discovery rate (FDR) threshold catalog (PDS_atca_fdr10_full_vis.cat) for the trimmed mosaic, visually edited to remove objects clearly associated with artifacts close to bright sources, containing 2058 sources, and the 10% FDR threshold catalog (PDS_atca_fdr10_deep.cat) for the 33' x 33' region centered on the most sensitive portion of the mosaic, containing 491 sources. The merged catalog was constructed to contain all unique catalogued sources; where common sources were identified, only the entry from PDS_atca_fdr10_deep.cat was retained. There are a total of 2148 sources in the final merged catalog, of which up to 10% may be false.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/pds1p4ghz#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pds1p4ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_pds1p4ghz&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/pds1p4ghz.html</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>HST.angst</TD>
            <TD>Hubble Space Telescope ACS Nearby Galaxy Survey (ANGST)</TD>
            <TD>The ACS Nearby Galaxy Survey observed roughly 14 million stars in 69 galaxies. The survey explored a region called the "Local Volume," and the galaxy distances ranged from 6.5 million light-years to 13 million light-years from Earth. The Local Volume resides beyond the Local Group of galaxies, an even nearer collection of a few dozen galaxies within about 3 million light-years of our Milky Way Galaxy. The observations were made in November 2006 with Hubble's Advanced Camera for Surveysi (ACS).</TD>
            <TD>MAST</TD>
            <TD>#Optical#</TD>
            <TD>ivo://mast.stsci/siap/angst#1</TD>
            <TD>2012-03-08T20:41:01Z</TD>
            <TD>#Galaxies#Extra-galactic stars#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1.0</TD>
            <TD>ivo://mast.stsci/siap/angst</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://archive.stsci.edu/siap/search.php?id=angst&amp;</TD>
            <TD />
            <TD>203</TD>
            <TD />
            <TD>http://archive.stsci.edu/prepds/angst/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC1893CXO [1]</TD>
            <TD>NGC 1893 Chandra X-Ray Point Source Catalog</TD>
            <TD>The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius &gt;= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10&lt;sup&gt;29.5&lt;/sup&gt; - 10&lt;sup&gt;31.5&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1893cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1893cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc1893cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1893cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC1893CXO [2]</TD>
            <TD>NGC 1893 Chandra X-Ray Point Source Catalog</TD>
            <TD>The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius &gt;= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10&lt;sup&gt;29.5&lt;/sup&gt; - 10&lt;sup&gt;31.5&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1893cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1893cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc1893cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1893cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC1893CXO [3]</TD>
            <TD>NGC 1893 Chandra X-Ray Point Source Catalog</TD>
            <TD>The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius &gt;= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10&lt;sup&gt;29.5&lt;/sup&gt; - 10&lt;sup&gt;31.5&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1893cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1893cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc1893cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1893cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/51/791 [1]</TD>
            <TD>Molecular clouds in southern HII regions (Yamaguchi+ 1999)</TD>
            <TD>We have carried out extensive ^13^CO(J=1-0) observations toward 23 southern H II regions associated with bright-rimmed clouds. In total, 95 molecular clouds have been identified to be associated with the H II regions. Among the 95, 57 clouds are found to be associated with 204 IRAS point sources which are candidates for young stellar objects. There is a significant increase of star-formation efficiency on the side facing to the H II regions; the luminosity-to-mass ratio, defined as the ratio of the stellar luminosity to the molecular cloud mass, is higher by an order of magnitude on the near side of the H II regions than that on the. far side. This indicates that molecular gas facing to the H II regions is more actively forming massive stars whose luminosity is ~&gt;10^3^L_{sun}_. In addition, the number density of the IRAS point sources increases by a factor of 2 on the near side of the H II regions compared with on the far side. These results strongly suggest that the active formation of massive stars on the near side of the H II regions is due to the effects of the H II regions, such as the compression of molecular material by the ionization/shock fronts. For the whole Galaxy, we estimate that the present star-formation rate under such effects is at least 0.2-0.4M_{sun}_/yr, corresponding to a few 10% by mass.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791#1</TD>
            <TD>2012-11-13T14:14:49Z</TD>
            <TD>#Nebulae#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/51/791</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/51/791</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/51/791 [2]</TD>
            <TD>Molecular clouds in southern HII regions (Yamaguchi+ 1999)</TD>
            <TD>We have carried out extensive ^13^CO(J=1-0) observations toward 23 southern H II regions associated with bright-rimmed clouds. In total, 95 molecular clouds have been identified to be associated with the H II regions. Among the 95, 57 clouds are found to be associated with 204 IRAS point sources which are candidates for young stellar objects. There is a significant increase of star-formation efficiency on the side facing to the H II regions; the luminosity-to-mass ratio, defined as the ratio of the stellar luminosity to the molecular cloud mass, is higher by an order of magnitude on the near side of the H II regions than that on the. far side. This indicates that molecular gas facing to the H II regions is more actively forming massive stars whose luminosity is ~&gt;10^3^L_{sun}_. In addition, the number density of the IRAS point sources increases by a factor of 2 on the near side of the H II regions compared with on the far side. These results strongly suggest that the active formation of massive stars on the near side of the H II regions is due to the effects of the H II regions, such as the compression of molecular material by the ionization/shock fronts. For the whole Galaxy, we estimate that the present star-formation rate under such effects is at least 0.2-0.4M_{sun}_/yr, corresponding to a few 10% by mass.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791#2</TD>
            <TD>2012-11-13T14:14:49Z</TD>
            <TD>#Nebulae#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/51/791&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/51/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/51/791 [clouds]</TD>
            <TD>Molecular clouds in southern HII regions (Yamaguchi+ 1999)</TD>
            <TD>We have carried out extensive ^13^CO(J=1-0) observations toward 23 southern H II regions associated with bright-rimmed clouds. In total, 95 molecular clouds have been identified to be associated with the H II regions. Among the 95, 57 clouds are found to be associated with 204 IRAS point sources which are candidates for young stellar objects. There is a significant increase of star-formation efficiency on the side facing to the H II regions; the luminosity-to-mass ratio, defined as the ratio of the stellar luminosity to the molecular cloud mass, is higher by an order of magnitude on the near side of the H II regions than that on the. far side. This indicates that molecular gas facing to the H II regions is more actively forming massive stars whose luminosity is ~&gt;10^3^L_{sun}_. In addition, the number density of the IRAS point sources increases by a factor of 2 on the near side of the H II regions compared with on the far side. These results strongly suggest that the active formation of massive stars on the near side of the H II regions is due to the effects of the H II regions, such as the compression of molecular material by the ionization/shock fronts. For the whole Galaxy, we estimate that the present star-formation rate under such effects is at least 0.2-0.4M_{sun}_/yr, corresponding to a few 10% by mass.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791#clouds</TD>
            <TD>2012-11-13T14:14:49Z</TD>
            <TD>#Nebulae#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2005</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/51/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/51/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/51/791</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>HST.COMA</TD>
            <TD>HST ACS Coma cluster (Abell 1656) Treasury Survey (COMA)</TD>
            <TD>The HST ACS Coma cluster Treasury survey is a deep two-passband imaging survey of one of the nearest rich clusters of galaxies, the Coma cluster (Abell 1656).</TD>
            <TD>MAST</TD>
            <TD>#Optical#</TD>
            <TD>ivo://mast.stsci/siap/coma#1</TD>
            <TD>2012-03-08T20:42:36Z</TD>
            <TD>#Galaxy Evolution and Structure#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1.0</TD>
            <TD>ivo://mast.stsci/siap/coma</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://archive.stsci.edu/siap/search.php?id=coma&amp;</TD>
            <TD />
            <TD>46</TD>
            <TD />
            <TD>http://archive.stsci.edu/prepds/coma/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC1893CXO [1]</TD>
            <TD>NGC 1893 Chandra X-Ray Point Source Catalog</TD>
            <TD>The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius &gt;= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10&lt;sup&gt;29.5&lt;/sup&gt; - 10&lt;sup&gt;31.5&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1893cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1893cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc1893cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1893cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC1893CXO [2]</TD>
            <TD>NGC 1893 Chandra X-Ray Point Source Catalog</TD>
            <TD>The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius &gt;= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10&lt;sup&gt;29.5&lt;/sup&gt; - 10&lt;sup&gt;31.5&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1893cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1893cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc1893cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1893cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC1893CXO [3]</TD>
            <TD>NGC 1893 Chandra X-Ray Point Source Catalog</TD>
            <TD>The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius &gt;= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10&lt;sup&gt;29.5&lt;/sup&gt; - 10&lt;sup&gt;31.5&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc1893cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc1893cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc1893cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc1893cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/1206 [1]</TD>
            <TD>XMM survey of 12um selected galaxies (Brightman+, 2011)</TD>
            <TD>We present an X-ray spectral analysis of 126 galaxies of the 12um galaxy sample (Rush et al. 1993, Cat. VII/157). By studying this sample at X-ray wavelengths, we aim to determine the intrinsic power, continuum shape and obscuration level in these sources. We improve upon previous works by the use of superior data in the form of higher signal-to-noise ratio spectra, finer spectral resolution and a broader bandpass from XMM-Newton. We pay particular attention to Compton thick active galactic nucleus (AGN) with the help of new spectral fitting models that we have produced, which are based on Monte Carlo simulations of X-ray radiative transfer, using both a spherical and torus geometry, and taking into account Compton scattering and iron fluorescence.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206#1</TD>
            <TD>2012-02-10T15:59:17Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/1206</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1206</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/1206 [2]</TD>
            <TD>XMM survey of 12um selected galaxies (Brightman+, 2011)</TD>
            <TD>We present an X-ray spectral analysis of 126 galaxies of the 12um galaxy sample (Rush et al. 1993, Cat. VII/157). By studying this sample at X-ray wavelengths, we aim to determine the intrinsic power, continuum shape and obscuration level in these sources. We improve upon previous works by the use of superior data in the form of higher signal-to-noise ratio spectra, finer spectral resolution and a broader bandpass from XMM-Newton. We pay particular attention to Compton thick active galactic nucleus (AGN) with the help of new spectral fitting models that we have produced, which are based on Monte Carlo simulations of X-ray radiative transfer, using both a spherical and torus geometry, and taking into account Compton scattering and iron fluorescence.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206#2</TD>
            <TD>2012-02-10T15:59:17Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/1206&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/1206 [Xsources]</TD>
            <TD>XMM survey of 12um selected galaxies (Brightman+, 2011)</TD>
            <TD>We present an X-ray spectral analysis of 126 galaxies of the 12um galaxy sample (Rush et al. 1993, Cat. VII/157). By studying this sample at X-ray wavelengths, we aim to determine the intrinsic power, continuum shape and obscuration level in these sources. We improve upon previous works by the use of superior data in the form of higher signal-to-noise ratio spectra, finer spectral resolution and a broader bandpass from XMM-Newton. We pay particular attention to Compton thick active galactic nucleus (AGN) with the help of new spectral fitting models that we have produced, which are based on Monte Carlo simulations of X-ray radiative transfer, using both a spherical and torus geometry, and taking into account Compton scattering and iron fluorescence.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206#Xsources</TD>
            <TD>2012-02-10T15:59:17Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/1206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1206</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GHOSTS [1]</TD>
            <TD>Galaxy Halos, Outer disks, Substructure, Thick disks and Star clusters (GHOSTS)</TD>
            <TD>The GHOSTS survey is the largest study to date of the resolved stellar populations in the outskirts of disk galaxies. The sample consists of 14 disk galaxies within 17 Mpc, whose outer disks and halos are imaged with the Hubble Space Telescope Advanced Camera for Surveys (ACS).</TD>
            <TD>Space Telescope Science Institute Archive</TD>
            <TD>#Optical#</TD>
            <TD>ivo://archive.stsci.edu/ghosts#1</TD>
            <TD>2012-04-30T20:48:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://archive.stsci.edu/ghosts</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD>1.0</TD>
            <TD>STD</TD>
            <TD>http://archive.stsci.edu/siap/search.php?id=ghosts&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://archive.stsci.edu/stsci-arc</TD>
            <TD>http://archive.stsci.edu/prepds/ghosts</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GHOSTS [2]</TD>
            <TD>Galaxy Halos, Outer disks, Substructure, Thick disks and Star clusters (GHOSTS)</TD>
            <TD>The GHOSTS survey is the largest study to date of the resolved stellar populations in the outskirts of disk galaxies. The sample consists of 14 disk galaxies within 17 Mpc, whose outer disks and halos are imaged with the Hubble Space Telescope Advanced Camera for Surveys (ACS).</TD>
            <TD>Space Telescope Science Institute Archive</TD>
            <TD>#Optical#</TD>
            <TD>ivo://archive.stsci.edu/ghosts#2</TD>
            <TD>2012-04-30T20:48:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://archive.stsci.edu/ghosts</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://archive.stsci.edu/prepds/ghosts/display_page.html</TD>
            <TD />
            <TD />
            <TD>ivo://archive.stsci.edu/stsci-arc</TD>
            <TD>http://archive.stsci.edu/prepds/ghosts</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC2403CXO [1]</TD>
            <TD>NGC 2403 Central 3-kpc Region Chandra Source Catalog</TD>
            <TD>Archival Chandra observations are used to study the X-ray emission associated with star formation in the central region of the nearby (D = 3.2 Mpc, 1 arcminute = 1 kpc) SAB(s)cd galaxy NGC 2403. The distribution of X-ray emission is compared to the morphology visible at other wavelengths using complementary Spitzer, Galaxy Evolution Explorer, and ground-based H-alpha imagery. In general, the brightest X-ray emission is associated with H II regions and to other star-forming structures, but is more pervasive, existing also in regions devoid of strong H-alpha and UV emission. NGC 2403 was observed in full-frame mode with the Chandra ACIS-S on four occasions for a total of ~ 180 ks, on 2001 Apr 17, 2004 Aug 13, 2004 Oct 03 and 2004 Dec 22. The source-finding tool described by Tennant (2006, AJ, 132, 1372) was applied to all 4 individual data sets and to the merged data set in order to search for discrete X-ray sources. The search was limited to the cnetral 6' x 6' (6 kpc x 6 kpc) region and to events within the full Chandra energy range 0.3-8.0 keV. Fifty eight point sources were detected in the merged data set with a signal-to-noise ratio (S/N) above 2.8 and with a minimum of 5 sigma above background uncertainty (corresponding to a detection limit of 8-10 counts for a typical on-axis source). These sources were listed in Table 2 of the reference paper and and are contained in the present HEASARC table. They can be selected by specifying source_type = 'Point Source'. The X-ray data were also examined to see if there was emission from known SNRs and H II regions after masking out the afore-mentioned X-ray point sources (see Section 2.1 of the reference paper for full details). Events falling within the areas defined by 24 optically identified SNRs that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 1-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only 4 or 5 of these SNRs are likely to be 'truely' detected X-ray sources. The SNRs can be selected in the present HEASARC table by specifying source_type ='SNR'. A similar procedure was used to search the X-ray data for the presence of X-ray emission at the locations of 47 H II regions in NGC 2403. Events falling within the areas defined by 47 H II regiuons that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 2-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only the most X-ray-luminous H II regions are likely to be 'truely' detected X-ray sources. The H II regions can be selected in the present HEASARC table by specifying source_type ='HII Region'.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc2403cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC2403CXO [2]</TD>
            <TD>NGC 2403 Central 3-kpc Region Chandra Source Catalog</TD>
            <TD>Archival Chandra observations are used to study the X-ray emission associated with star formation in the central region of the nearby (D = 3.2 Mpc, 1 arcminute = 1 kpc) SAB(s)cd galaxy NGC 2403. The distribution of X-ray emission is compared to the morphology visible at other wavelengths using complementary Spitzer, Galaxy Evolution Explorer, and ground-based H-alpha imagery. In general, the brightest X-ray emission is associated with H II regions and to other star-forming structures, but is more pervasive, existing also in regions devoid of strong H-alpha and UV emission. NGC 2403 was observed in full-frame mode with the Chandra ACIS-S on four occasions for a total of ~ 180 ks, on 2001 Apr 17, 2004 Aug 13, 2004 Oct 03 and 2004 Dec 22. The source-finding tool described by Tennant (2006, AJ, 132, 1372) was applied to all 4 individual data sets and to the merged data set in order to search for discrete X-ray sources. The search was limited to the cnetral 6' x 6' (6 kpc x 6 kpc) region and to events within the full Chandra energy range 0.3-8.0 keV. Fifty eight point sources were detected in the merged data set with a signal-to-noise ratio (S/N) above 2.8 and with a minimum of 5 sigma above background uncertainty (corresponding to a detection limit of 8-10 counts for a typical on-axis source). These sources were listed in Table 2 of the reference paper and and are contained in the present HEASARC table. They can be selected by specifying source_type = 'Point Source'. The X-ray data were also examined to see if there was emission from known SNRs and H II regions after masking out the afore-mentioned X-ray point sources (see Section 2.1 of the reference paper for full details). Events falling within the areas defined by 24 optically identified SNRs that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 1-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only 4 or 5 of these SNRs are likely to be 'truely' detected X-ray sources. The SNRs can be selected in the present HEASARC table by specifying source_type ='SNR'. A similar procedure was used to search the X-ray data for the presence of X-ray emission at the locations of 47 H II regions in NGC 2403. Events falling within the areas defined by 47 H II regiuons that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 2-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only the most X-ray-luminous H II regions are likely to be 'truely' detected X-ray sources. The H II regions can be selected in the present HEASARC table by specifying source_type ='HII Region'.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc2403cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ParamHTTP</TD>
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          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC2403CXO [3]</TD>
            <TD>NGC 2403 Central 3-kpc Region Chandra Source Catalog</TD>
            <TD>Archival Chandra observations are used to study the X-ray emission associated with star formation in the central region of the nearby (D = 3.2 Mpc, 1 arcminute = 1 kpc) SAB(s)cd galaxy NGC 2403. The distribution of X-ray emission is compared to the morphology visible at other wavelengths using complementary Spitzer, Galaxy Evolution Explorer, and ground-based H-alpha imagery. In general, the brightest X-ray emission is associated with H II regions and to other star-forming structures, but is more pervasive, existing also in regions devoid of strong H-alpha and UV emission. NGC 2403 was observed in full-frame mode with the Chandra ACIS-S on four occasions for a total of ~ 180 ks, on 2001 Apr 17, 2004 Aug 13, 2004 Oct 03 and 2004 Dec 22. The source-finding tool described by Tennant (2006, AJ, 132, 1372) was applied to all 4 individual data sets and to the merged data set in order to search for discrete X-ray sources. The search was limited to the cnetral 6' x 6' (6 kpc x 6 kpc) region and to events within the full Chandra energy range 0.3-8.0 keV. Fifty eight point sources were detected in the merged data set with a signal-to-noise ratio (S/N) above 2.8 and with a minimum of 5 sigma above background uncertainty (corresponding to a detection limit of 8-10 counts for a typical on-axis source). These sources were listed in Table 2 of the reference paper and and are contained in the present HEASARC table. They can be selected by specifying source_type = 'Point Source'. The X-ray data were also examined to see if there was emission from known SNRs and H II regions after masking out the afore-mentioned X-ray point sources (see Section 2.1 of the reference paper for full details). Events falling within the areas defined by 24 optically identified SNRs that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 1-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only 4 or 5 of these SNRs are likely to be 'truely' detected X-ray sources. The SNRs can be selected in the present HEASARC table by specifying source_type ='SNR'. A similar procedure was used to search the X-ray data for the presence of X-ray emission at the locations of 47 H II regions in NGC 2403. Events falling within the areas defined by 47 H II regiuons that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 2-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only the most X-ray-luminous H II regions are likely to be 'truely' detected X-ray sources. The H II regions can be selected in the present HEASARC table by specifying source_type ='HII Region'.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc2403cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD />
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            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc2403cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc2403cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/1206 [1]</TD>
            <TD>XMM survey of 12um selected galaxies (Brightman+, 2011)</TD>
            <TD>We present an X-ray spectral analysis of 126 galaxies of the 12um galaxy sample (Rush et al. 1993, Cat. VII/157). By studying this sample at X-ray wavelengths, we aim to determine the intrinsic power, continuum shape and obscuration level in these sources. We improve upon previous works by the use of superior data in the form of higher signal-to-noise ratio spectra, finer spectral resolution and a broader bandpass from XMM-Newton. We pay particular attention to Compton thick active galactic nucleus (AGN) with the help of new spectral fitting models that we have produced, which are based on Monte Carlo simulations of X-ray radiative transfer, using both a spherical and torus geometry, and taking into account Compton scattering and iron fluorescence.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206#1</TD>
            <TD>2012-02-10T15:59:17Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
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            <TD>12-Dec-2011</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1206</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/1206 [2]</TD>
            <TD>XMM survey of 12um selected galaxies (Brightman+, 2011)</TD>
            <TD>We present an X-ray spectral analysis of 126 galaxies of the 12um galaxy sample (Rush et al. 1993, Cat. VII/157). By studying this sample at X-ray wavelengths, we aim to determine the intrinsic power, continuum shape and obscuration level in these sources. We improve upon previous works by the use of superior data in the form of higher signal-to-noise ratio spectra, finer spectral resolution and a broader bandpass from XMM-Newton. We pay particular attention to Compton thick active galactic nucleus (AGN) with the help of new spectral fitting models that we have produced, which are based on Monte Carlo simulations of X-ray radiative transfer, using both a spherical and torus geometry, and taking into account Compton scattering and iron fluorescence.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206#2</TD>
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            <TD>12-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/413/1206 [Xsources]</TD>
            <TD>XMM survey of 12um selected galaxies (Brightman+, 2011)</TD>
            <TD>We present an X-ray spectral analysis of 126 galaxies of the 12um galaxy sample (Rush et al. 1993, Cat. VII/157). By studying this sample at X-ray wavelengths, we aim to determine the intrinsic power, continuum shape and obscuration level in these sources. We improve upon previous works by the use of superior data in the form of higher signal-to-noise ratio spectra, finer spectral resolution and a broader bandpass from XMM-Newton. We pay particular attention to Compton thick active galactic nucleus (AGN) with the help of new spectral fitting models that we have produced, which are based on Monte Carlo simulations of X-ray radiative transfer, using both a spherical and torus geometry, and taking into account Compton scattering and iron fluorescence.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
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            <TD>12-Dec-2011</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/321 [1]</TD>
            <TD>Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)</TD>
            <TD>We present a study of the nuclear morphology of a sample of narrow- and broad-line Seyfert 1 galaxies (NLS1s and BLS1s, respectively) based on broadband images in the Hubble Space Telescope archives. In our previous study we found that large-scale stellar bars at &gt;1kpc from the nucleus are more common in NLS1s than BLS1s. In this paper we find that NLS1s preferentially have grand-design dust spirals within ~1kpc of their centers. We also find that NLS1s have a higher fraction of nuclear star-forming rings than BLS1s. We find that many of the morphological differences are due to the presence or absence of a large-scale stellar bar within the spiral host galaxy. In general, barred Seyfert 1 galaxies tend to have grand-design dust spirals at their centers, confirming the results of other researchers. The high fraction of grand-design nuclear dust spirals and stellar nuclear rings observed in NLS1s' host galaxies suggests a means for efficient fueling of their nuclei to support their high Eddington ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321#1</TD>
            <TD>2011-09-14T20:13:54Z</TD>
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            <TD />
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            <TD>ivo://CDS.VizieR/J/AJ/132/321</TD>
            <TD />
            <TD />
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/321</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/321</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/321 [2]</TD>
            <TD>Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)</TD>
            <TD>We present a study of the nuclear morphology of a sample of narrow- and broad-line Seyfert 1 galaxies (NLS1s and BLS1s, respectively) based on broadband images in the Hubble Space Telescope archives. In our previous study we found that large-scale stellar bars at &gt;1kpc from the nucleus are more common in NLS1s than BLS1s. In this paper we find that NLS1s preferentially have grand-design dust spirals within ~1kpc of their centers. We also find that NLS1s have a higher fraction of nuclear star-forming rings than BLS1s. We find that many of the morphological differences are due to the presence or absence of a large-scale stellar bar within the spiral host galaxy. In general, barred Seyfert 1 galaxies tend to have grand-design dust spirals at their centers, confirming the results of other researchers. The high fraction of grand-design nuclear dust spirals and stellar nuclear rings observed in NLS1s' host galaxies suggests a means for efficient fueling of their nuclei to support their high Eddington ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321#2</TD>
            <TD>2011-09-14T20:13:54Z</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/321 [table1]</TD>
            <TD>Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)</TD>
            <TD>We present a study of the nuclear morphology of a sample of narrow- and broad-line Seyfert 1 galaxies (NLS1s and BLS1s, respectively) based on broadband images in the Hubble Space Telescope archives. In our previous study we found that large-scale stellar bars at &gt;1kpc from the nucleus are more common in NLS1s than BLS1s. In this paper we find that NLS1s preferentially have grand-design dust spirals within ~1kpc of their centers. We also find that NLS1s have a higher fraction of nuclear star-forming rings than BLS1s. We find that many of the morphological differences are due to the presence or absence of a large-scale stellar bar within the spiral host galaxy. In general, barred Seyfert 1 galaxies tend to have grand-design dust spirals at their centers, confirming the results of other researchers. The high fraction of grand-design nuclear dust spirals and stellar nuclear rings observed in NLS1s' host galaxies suggests a means for efficient fueling of their nuclei to support their high Eddington ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321#table1</TD>
            <TD>2011-09-14T20:13:54Z</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/1206 [1]</TD>
            <TD>XMM survey of 12um selected galaxies (Brightman+, 2011)</TD>
            <TD>We present an X-ray spectral analysis of 126 galaxies of the 12um galaxy sample (Rush et al. 1993, Cat. VII/157). By studying this sample at X-ray wavelengths, we aim to determine the intrinsic power, continuum shape and obscuration level in these sources. We improve upon previous works by the use of superior data in the form of higher signal-to-noise ratio spectra, finer spectral resolution and a broader bandpass from XMM-Newton. We pay particular attention to Compton thick active galactic nucleus (AGN) with the help of new spectral fitting models that we have produced, which are based on Monte Carlo simulations of X-ray radiative transfer, using both a spherical and torus geometry, and taking into account Compton scattering and iron fluorescence.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206#1</TD>
            <TD>2012-02-10T15:59:17Z</TD>
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            <TD>12-Dec-2011</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/1206 [2]</TD>
            <TD>XMM survey of 12um selected galaxies (Brightman+, 2011)</TD>
            <TD>We present an X-ray spectral analysis of 126 galaxies of the 12um galaxy sample (Rush et al. 1993, Cat. VII/157). By studying this sample at X-ray wavelengths, we aim to determine the intrinsic power, continuum shape and obscuration level in these sources. We improve upon previous works by the use of superior data in the form of higher signal-to-noise ratio spectra, finer spectral resolution and a broader bandpass from XMM-Newton. We pay particular attention to Compton thick active galactic nucleus (AGN) with the help of new spectral fitting models that we have produced, which are based on Monte Carlo simulations of X-ray radiative transfer, using both a spherical and torus geometry, and taking into account Compton scattering and iron fluorescence.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206#2</TD>
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            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/413/1206 [Xsources]</TD>
            <TD>XMM survey of 12um selected galaxies (Brightman+, 2011)</TD>
            <TD>We present an X-ray spectral analysis of 126 galaxies of the 12um galaxy sample (Rush et al. 1993, Cat. VII/157). By studying this sample at X-ray wavelengths, we aim to determine the intrinsic power, continuum shape and obscuration level in these sources. We improve upon previous works by the use of superior data in the form of higher signal-to-noise ratio spectra, finer spectral resolution and a broader bandpass from XMM-Newton. We pay particular attention to Compton thick active galactic nucleus (AGN) with the help of new spectral fitting models that we have produced, which are based on Monte Carlo simulations of X-ray radiative transfer, using both a spherical and torus geometry, and taking into account Compton scattering and iron fluorescence.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206#Xsources</TD>
            <TD>2012-02-10T15:59:17Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/1206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/1206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/1206</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/321 [1]</TD>
            <TD>Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)</TD>
            <TD>We present a study of the nuclear morphology of a sample of narrow- and broad-line Seyfert 1 galaxies (NLS1s and BLS1s, respectively) based on broadband images in the Hubble Space Telescope archives. In our previous study we found that large-scale stellar bars at &gt;1kpc from the nucleus are more common in NLS1s than BLS1s. In this paper we find that NLS1s preferentially have grand-design dust spirals within ~1kpc of their centers. We also find that NLS1s have a higher fraction of nuclear star-forming rings than BLS1s. We find that many of the morphological differences are due to the presence or absence of a large-scale stellar bar within the spiral host galaxy. In general, barred Seyfert 1 galaxies tend to have grand-design dust spirals at their centers, confirming the results of other researchers. The high fraction of grand-design nuclear dust spirals and stellar nuclear rings observed in NLS1s' host galaxies suggests a means for efficient fueling of their nuclei to support their high Eddington ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321#1</TD>
            <TD>2011-09-14T20:13:54Z</TD>
            <TD>#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/321</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/321</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/321 [2]</TD>
            <TD>Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)</TD>
            <TD>We present a study of the nuclear morphology of a sample of narrow- and broad-line Seyfert 1 galaxies (NLS1s and BLS1s, respectively) based on broadband images in the Hubble Space Telescope archives. In our previous study we found that large-scale stellar bars at &gt;1kpc from the nucleus are more common in NLS1s than BLS1s. In this paper we find that NLS1s preferentially have grand-design dust spirals within ~1kpc of their centers. We also find that NLS1s have a higher fraction of nuclear star-forming rings than BLS1s. We find that many of the morphological differences are due to the presence or absence of a large-scale stellar bar within the spiral host galaxy. In general, barred Seyfert 1 galaxies tend to have grand-design dust spirals at their centers, confirming the results of other researchers. The high fraction of grand-design nuclear dust spirals and stellar nuclear rings observed in NLS1s' host galaxies suggests a means for efficient fueling of their nuclei to support their high Eddington ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321#2</TD>
            <TD>2011-09-14T20:13:54Z</TD>
            <TD>#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/321&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/321</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/321 [table1]</TD>
            <TD>Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)</TD>
            <TD>We present a study of the nuclear morphology of a sample of narrow- and broad-line Seyfert 1 galaxies (NLS1s and BLS1s, respectively) based on broadband images in the Hubble Space Telescope archives. In our previous study we found that large-scale stellar bars at &gt;1kpc from the nucleus are more common in NLS1s than BLS1s. In this paper we find that NLS1s preferentially have grand-design dust spirals within ~1kpc of their centers. We also find that NLS1s have a higher fraction of nuclear star-forming rings than BLS1s. We find that many of the morphological differences are due to the presence or absence of a large-scale stellar bar within the spiral host galaxy. In general, barred Seyfert 1 galaxies tend to have grand-design dust spirals at their centers, confirming the results of other researchers. The high fraction of grand-design nuclear dust spirals and stellar nuclear rings observed in NLS1s' host galaxies suggests a means for efficient fueling of their nuclei to support their high Eddington ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321#table1</TD>
            <TD>2011-09-14T20:13:54Z</TD>
            <TD>#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/321&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/321</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC2403CXO [1]</TD>
            <TD>NGC 2403 Central 3-kpc Region Chandra Source Catalog</TD>
            <TD>Archival Chandra observations are used to study the X-ray emission associated with star formation in the central region of the nearby (D = 3.2 Mpc, 1 arcminute = 1 kpc) SAB(s)cd galaxy NGC 2403. The distribution of X-ray emission is compared to the morphology visible at other wavelengths using complementary Spitzer, Galaxy Evolution Explorer, and ground-based H-alpha imagery. In general, the brightest X-ray emission is associated with H II regions and to other star-forming structures, but is more pervasive, existing also in regions devoid of strong H-alpha and UV emission. NGC 2403 was observed in full-frame mode with the Chandra ACIS-S on four occasions for a total of ~ 180 ks, on 2001 Apr 17, 2004 Aug 13, 2004 Oct 03 and 2004 Dec 22. The source-finding tool described by Tennant (2006, AJ, 132, 1372) was applied to all 4 individual data sets and to the merged data set in order to search for discrete X-ray sources. The search was limited to the cnetral 6' x 6' (6 kpc x 6 kpc) region and to events within the full Chandra energy range 0.3-8.0 keV. Fifty eight point sources were detected in the merged data set with a signal-to-noise ratio (S/N) above 2.8 and with a minimum of 5 sigma above background uncertainty (corresponding to a detection limit of 8-10 counts for a typical on-axis source). These sources were listed in Table 2 of the reference paper and and are contained in the present HEASARC table. They can be selected by specifying source_type = 'Point Source'. The X-ray data were also examined to see if there was emission from known SNRs and H II regions after masking out the afore-mentioned X-ray point sources (see Section 2.1 of the reference paper for full details). Events falling within the areas defined by 24 optically identified SNRs that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 1-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only 4 or 5 of these SNRs are likely to be 'truely' detected X-ray sources. The SNRs can be selected in the present HEASARC table by specifying source_type ='SNR'. A similar procedure was used to search the X-ray data for the presence of X-ray emission at the locations of 47 H II regions in NGC 2403. Events falling within the areas defined by 47 H II regiuons that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 2-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only the most X-ray-luminous H II regions are likely to be 'truely' detected X-ray sources. The H II regions can be selected in the present HEASARC table by specifying source_type ='HII Region'.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc2403cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2403cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc2403cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc2403cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC2403CXO [2]</TD>
            <TD>NGC 2403 Central 3-kpc Region Chandra Source Catalog</TD>
            <TD>Archival Chandra observations are used to study the X-ray emission associated with star formation in the central region of the nearby (D = 3.2 Mpc, 1 arcminute = 1 kpc) SAB(s)cd galaxy NGC 2403. The distribution of X-ray emission is compared to the morphology visible at other wavelengths using complementary Spitzer, Galaxy Evolution Explorer, and ground-based H-alpha imagery. In general, the brightest X-ray emission is associated with H II regions and to other star-forming structures, but is more pervasive, existing also in regions devoid of strong H-alpha and UV emission. NGC 2403 was observed in full-frame mode with the Chandra ACIS-S on four occasions for a total of ~ 180 ks, on 2001 Apr 17, 2004 Aug 13, 2004 Oct 03 and 2004 Dec 22. The source-finding tool described by Tennant (2006, AJ, 132, 1372) was applied to all 4 individual data sets and to the merged data set in order to search for discrete X-ray sources. The search was limited to the cnetral 6' x 6' (6 kpc x 6 kpc) region and to events within the full Chandra energy range 0.3-8.0 keV. Fifty eight point sources were detected in the merged data set with a signal-to-noise ratio (S/N) above 2.8 and with a minimum of 5 sigma above background uncertainty (corresponding to a detection limit of 8-10 counts for a typical on-axis source). These sources were listed in Table 2 of the reference paper and and are contained in the present HEASARC table. They can be selected by specifying source_type = 'Point Source'. The X-ray data were also examined to see if there was emission from known SNRs and H II regions after masking out the afore-mentioned X-ray point sources (see Section 2.1 of the reference paper for full details). Events falling within the areas defined by 24 optically identified SNRs that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 1-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only 4 or 5 of these SNRs are likely to be 'truely' detected X-ray sources. The SNRs can be selected in the present HEASARC table by specifying source_type ='SNR'. A similar procedure was used to search the X-ray data for the presence of X-ray emission at the locations of 47 H II regions in NGC 2403. Events falling within the areas defined by 47 H II regiuons that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 2-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only the most X-ray-luminous H II regions are likely to be 'truely' detected X-ray sources. The H II regions can be selected in the present HEASARC table by specifying source_type ='HII Region'.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc2403cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2403cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc2403cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc2403cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC2403CXO [3]</TD>
            <TD>NGC 2403 Central 3-kpc Region Chandra Source Catalog</TD>
            <TD>Archival Chandra observations are used to study the X-ray emission associated with star formation in the central region of the nearby (D = 3.2 Mpc, 1 arcminute = 1 kpc) SAB(s)cd galaxy NGC 2403. The distribution of X-ray emission is compared to the morphology visible at other wavelengths using complementary Spitzer, Galaxy Evolution Explorer, and ground-based H-alpha imagery. In general, the brightest X-ray emission is associated with H II regions and to other star-forming structures, but is more pervasive, existing also in regions devoid of strong H-alpha and UV emission. NGC 2403 was observed in full-frame mode with the Chandra ACIS-S on four occasions for a total of ~ 180 ks, on 2001 Apr 17, 2004 Aug 13, 2004 Oct 03 and 2004 Dec 22. The source-finding tool described by Tennant (2006, AJ, 132, 1372) was applied to all 4 individual data sets and to the merged data set in order to search for discrete X-ray sources. The search was limited to the cnetral 6' x 6' (6 kpc x 6 kpc) region and to events within the full Chandra energy range 0.3-8.0 keV. Fifty eight point sources were detected in the merged data set with a signal-to-noise ratio (S/N) above 2.8 and with a minimum of 5 sigma above background uncertainty (corresponding to a detection limit of 8-10 counts for a typical on-axis source). These sources were listed in Table 2 of the reference paper and and are contained in the present HEASARC table. They can be selected by specifying source_type = 'Point Source'. The X-ray data were also examined to see if there was emission from known SNRs and H II regions after masking out the afore-mentioned X-ray point sources (see Section 2.1 of the reference paper for full details). Events falling within the areas defined by 24 optically identified SNRs that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 1-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only 4 or 5 of these SNRs are likely to be 'truely' detected X-ray sources. The SNRs can be selected in the present HEASARC table by specifying source_type ='SNR'. A similar procedure was used to search the X-ray data for the presence of X-ray emission at the locations of 47 H II regions in NGC 2403. Events falling within the areas defined by 47 H II regiuons that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 2-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only the most X-ray-luminous H II regions are likely to be 'truely' detected X-ray sources. The H II regions can be selected in the present HEASARC table by specifying source_type ='HII Region'.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc2403cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2403cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc2403cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc2403cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE143 [1]</TD>
            <TD>Planck Early Release 143-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 143-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke143#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke143&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke143.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE143 [2]</TD>
            <TD>Planck Early Release 143-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 143-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
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            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke143.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE143 [3]</TD>
            <TD>Planck Early Release 143-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 143-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke143&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke143.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/321 [1]</TD>
            <TD>Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)</TD>
            <TD>We present a study of the nuclear morphology of a sample of narrow- and broad-line Seyfert 1 galaxies (NLS1s and BLS1s, respectively) based on broadband images in the Hubble Space Telescope archives. In our previous study we found that large-scale stellar bars at &gt;1kpc from the nucleus are more common in NLS1s than BLS1s. In this paper we find that NLS1s preferentially have grand-design dust spirals within ~1kpc of their centers. We also find that NLS1s have a higher fraction of nuclear star-forming rings than BLS1s. We find that many of the morphological differences are due to the presence or absence of a large-scale stellar bar within the spiral host galaxy. In general, barred Seyfert 1 galaxies tend to have grand-design dust spirals at their centers, confirming the results of other researchers. The high fraction of grand-design nuclear dust spirals and stellar nuclear rings observed in NLS1s' host galaxies suggests a means for efficient fueling of their nuclei to support their high Eddington ratios.</TD>
            <TD>CDS</TD>
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            <TD>2011-09-14T20:13:54Z</TD>
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            <TD />
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            <TD>WebBrowser</TD>
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            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/321</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/321 [2]</TD>
            <TD>Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)</TD>
            <TD>We present a study of the nuclear morphology of a sample of narrow- and broad-line Seyfert 1 galaxies (NLS1s and BLS1s, respectively) based on broadband images in the Hubble Space Telescope archives. In our previous study we found that large-scale stellar bars at &gt;1kpc from the nucleus are more common in NLS1s than BLS1s. In this paper we find that NLS1s preferentially have grand-design dust spirals within ~1kpc of their centers. We also find that NLS1s have a higher fraction of nuclear star-forming rings than BLS1s. We find that many of the morphological differences are due to the presence or absence of a large-scale stellar bar within the spiral host galaxy. In general, barred Seyfert 1 galaxies tend to have grand-design dust spirals at their centers, confirming the results of other researchers. The high fraction of grand-design nuclear dust spirals and stellar nuclear rings observed in NLS1s' host galaxies suggests a means for efficient fueling of their nuclei to support their high Eddington ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321#2</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/321 [table1]</TD>
            <TD>Morphology of narrow-line Seyfert 1 galaxies (Deo+, 2006)</TD>
            <TD>We present a study of the nuclear morphology of a sample of narrow- and broad-line Seyfert 1 galaxies (NLS1s and BLS1s, respectively) based on broadband images in the Hubble Space Telescope archives. In our previous study we found that large-scale stellar bars at &gt;1kpc from the nucleus are more common in NLS1s than BLS1s. In this paper we find that NLS1s preferentially have grand-design dust spirals within ~1kpc of their centers. We also find that NLS1s have a higher fraction of nuclear star-forming rings than BLS1s. We find that many of the morphological differences are due to the presence or absence of a large-scale stellar bar within the spiral host galaxy. In general, barred Seyfert 1 galaxies tend to have grand-design dust spirals at their centers, confirming the results of other researchers. The high fraction of grand-design nuclear dust spirals and stellar nuclear rings observed in NLS1s' host galaxies suggests a means for efficient fueling of their nuclei to support their high Eddington ratios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321#table1</TD>
            <TD>2011-09-14T20:13:54Z</TD>
            <TD>#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/321</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/321</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>NGC2403CXO [1]</TD>
            <TD>NGC 2403 Central 3-kpc Region Chandra Source Catalog</TD>
            <TD>Archival Chandra observations are used to study the X-ray emission associated with star formation in the central region of the nearby (D = 3.2 Mpc, 1 arcminute = 1 kpc) SAB(s)cd galaxy NGC 2403. The distribution of X-ray emission is compared to the morphology visible at other wavelengths using complementary Spitzer, Galaxy Evolution Explorer, and ground-based H-alpha imagery. In general, the brightest X-ray emission is associated with H II regions and to other star-forming structures, but is more pervasive, existing also in regions devoid of strong H-alpha and UV emission. NGC 2403 was observed in full-frame mode with the Chandra ACIS-S on four occasions for a total of ~ 180 ks, on 2001 Apr 17, 2004 Aug 13, 2004 Oct 03 and 2004 Dec 22. The source-finding tool described by Tennant (2006, AJ, 132, 1372) was applied to all 4 individual data sets and to the merged data set in order to search for discrete X-ray sources. The search was limited to the cnetral 6' x 6' (6 kpc x 6 kpc) region and to events within the full Chandra energy range 0.3-8.0 keV. Fifty eight point sources were detected in the merged data set with a signal-to-noise ratio (S/N) above 2.8 and with a minimum of 5 sigma above background uncertainty (corresponding to a detection limit of 8-10 counts for a typical on-axis source). These sources were listed in Table 2 of the reference paper and and are contained in the present HEASARC table. They can be selected by specifying source_type = 'Point Source'. The X-ray data were also examined to see if there was emission from known SNRs and H II regions after masking out the afore-mentioned X-ray point sources (see Section 2.1 of the reference paper for full details). Events falling within the areas defined by 24 optically identified SNRs that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 1-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only 4 or 5 of these SNRs are likely to be 'truely' detected X-ray sources. The SNRs can be selected in the present HEASARC table by specifying source_type ='SNR'. A similar procedure was used to search the X-ray data for the presence of X-ray emission at the locations of 47 H II regions in NGC 2403. Events falling within the areas defined by 47 H II regiuons that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 2-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only the most X-ray-luminous H II regions are likely to be 'truely' detected X-ray sources. The H II regions can be selected in the present HEASARC table by specifying source_type ='HII Region'.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc2403cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc2403cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc2403cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc2403cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC2403CXO [2]</TD>
            <TD>NGC 2403 Central 3-kpc Region Chandra Source Catalog</TD>
            <TD>Archival Chandra observations are used to study the X-ray emission associated with star formation in the central region of the nearby (D = 3.2 Mpc, 1 arcminute = 1 kpc) SAB(s)cd galaxy NGC 2403. The distribution of X-ray emission is compared to the morphology visible at other wavelengths using complementary Spitzer, Galaxy Evolution Explorer, and ground-based H-alpha imagery. In general, the brightest X-ray emission is associated with H II regions and to other star-forming structures, but is more pervasive, existing also in regions devoid of strong H-alpha and UV emission. NGC 2403 was observed in full-frame mode with the Chandra ACIS-S on four occasions for a total of ~ 180 ks, on 2001 Apr 17, 2004 Aug 13, 2004 Oct 03 and 2004 Dec 22. The source-finding tool described by Tennant (2006, AJ, 132, 1372) was applied to all 4 individual data sets and to the merged data set in order to search for discrete X-ray sources. The search was limited to the cnetral 6' x 6' (6 kpc x 6 kpc) region and to events within the full Chandra energy range 0.3-8.0 keV. Fifty eight point sources were detected in the merged data set with a signal-to-noise ratio (S/N) above 2.8 and with a minimum of 5 sigma above background uncertainty (corresponding to a detection limit of 8-10 counts for a typical on-axis source). These sources were listed in Table 2 of the reference paper and and are contained in the present HEASARC table. They can be selected by specifying source_type = 'Point Source'. The X-ray data were also examined to see if there was emission from known SNRs and H II regions after masking out the afore-mentioned X-ray point sources (see Section 2.1 of the reference paper for full details). Events falling within the areas defined by 24 optically identified SNRs that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 1-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only 4 or 5 of these SNRs are likely to be 'truely' detected X-ray sources. The SNRs can be selected in the present HEASARC table by specifying source_type ='SNR'. A similar procedure was used to search the X-ray data for the presence of X-ray emission at the locations of 47 H II regions in NGC 2403. Events falling within the areas defined by 47 H II regiuons that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 2-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only the most X-ray-luminous H II regions are likely to be 'truely' detected X-ray sources. The H II regions can be selected in the present HEASARC table by specifying source_type ='HII Region'.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc2403cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD />
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            <TD />
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          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC2403CXO [3]</TD>
            <TD>NGC 2403 Central 3-kpc Region Chandra Source Catalog</TD>
            <TD>Archival Chandra observations are used to study the X-ray emission associated with star formation in the central region of the nearby (D = 3.2 Mpc, 1 arcminute = 1 kpc) SAB(s)cd galaxy NGC 2403. The distribution of X-ray emission is compared to the morphology visible at other wavelengths using complementary Spitzer, Galaxy Evolution Explorer, and ground-based H-alpha imagery. In general, the brightest X-ray emission is associated with H II regions and to other star-forming structures, but is more pervasive, existing also in regions devoid of strong H-alpha and UV emission. NGC 2403 was observed in full-frame mode with the Chandra ACIS-S on four occasions for a total of ~ 180 ks, on 2001 Apr 17, 2004 Aug 13, 2004 Oct 03 and 2004 Dec 22. The source-finding tool described by Tennant (2006, AJ, 132, 1372) was applied to all 4 individual data sets and to the merged data set in order to search for discrete X-ray sources. The search was limited to the cnetral 6' x 6' (6 kpc x 6 kpc) region and to events within the full Chandra energy range 0.3-8.0 keV. Fifty eight point sources were detected in the merged data set with a signal-to-noise ratio (S/N) above 2.8 and with a minimum of 5 sigma above background uncertainty (corresponding to a detection limit of 8-10 counts for a typical on-axis source). These sources were listed in Table 2 of the reference paper and and are contained in the present HEASARC table. They can be selected by specifying source_type = 'Point Source'. The X-ray data were also examined to see if there was emission from known SNRs and H II regions after masking out the afore-mentioned X-ray point sources (see Section 2.1 of the reference paper for full details). Events falling within the areas defined by 24 optically identified SNRs that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 1-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only 4 or 5 of these SNRs are likely to be 'truely' detected X-ray sources. The SNRs can be selected in the present HEASARC table by specifying source_type ='SNR'. A similar procedure was used to search the X-ray data for the presence of X-ray emission at the locations of 47 H II regions in NGC 2403. Events falling within the areas defined by 47 H II regiuons that were imaged on the S3 chip in the first three observations were used to construct a composite spectrum. This stacked spectrum was fit by an absorbed 2-T APEC model with the hydrogen column density as a free parameter in XSPEC which was then used to translate the observed net count rates into X-ray luminosities. Only the most X-ray-luminous H II regions are likely to be 'truely' detected X-ray sources. The H II regions can be selected in the present HEASARC table by specifying source_type ='HII Region'.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc2403cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
            <TD />
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            <TD />
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            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc2403cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc2403cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/561/189 [1]</TD>
            <TD>Chandra X-ray sources in M101 (Pence+, 2001)</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M101. From this rich data set we have created a catalog of the 110 sources from the S3 chip detected with a significance of greater than 3{sigma}. This detection threshold corresponds to a flux of ~10^-16^ergs/cm^2^/s and a luminosity of ~10^36^ergs/s for a distance to M101 of 7.2Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189#1</TD>
            <TD>2011-09-14T20:14:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/561/189</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/561/189</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/561/189 [2]</TD>
            <TD>Chandra X-ray sources in M101 (Pence+, 2001)</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M101. From this rich data set we have created a catalog of the 110 sources from the S3 chip detected with a significance of greater than 3{sigma}. This detection threshold corresponds to a flux of ~10^-16^ergs/cm^2^/s and a luminosity of ~10^36^ergs/s for a distance to M101 of 7.2Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189#2</TD>
            <TD>2011-09-14T20:14:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/561/189&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/561/189</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/561/189 [table1]</TD>
            <TD>Chandra X-ray sources in M101 (Pence+, 2001)</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M101. From this rich data set we have created a catalog of the 110 sources from the S3 chip detected with a significance of greater than 3{sigma}. This detection threshold corresponds to a flux of ~10^-16^ergs/cm^2^/s and a luminosity of ~10^36^ergs/s for a distance to M101 of 7.2Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189#table1</TD>
            <TD>2011-09-14T20:14:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/561/189&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/561/189</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE857 [1]</TD>
            <TD>Planck Early Release 857-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 857-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke857#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke857&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke857.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE857 [2]</TD>
            <TD>Planck Early Release 857-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 857-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke857#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke857.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE857 [3]</TD>
            <TD>Planck Early Release 857-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 857-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke857#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke857&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke857.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/561/189 [1]</TD>
            <TD>Chandra X-ray sources in M101 (Pence+, 2001)</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M101. From this rich data set we have created a catalog of the 110 sources from the S3 chip detected with a significance of greater than 3{sigma}. This detection threshold corresponds to a flux of ~10^-16^ergs/cm^2^/s and a luminosity of ~10^36^ergs/s for a distance to M101 of 7.2Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189#1</TD>
            <TD>2011-09-14T20:14:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/561/189</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/561/189</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/561/189 [2]</TD>
            <TD>Chandra X-ray sources in M101 (Pence+, 2001)</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M101. From this rich data set we have created a catalog of the 110 sources from the S3 chip detected with a significance of greater than 3{sigma}. This detection threshold corresponds to a flux of ~10^-16^ergs/cm^2^/s and a luminosity of ~10^36^ergs/s for a distance to M101 of 7.2Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189#2</TD>
            <TD>2011-09-14T20:14:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/561/189&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/561/189</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/561/189 [table1]</TD>
            <TD>Chandra X-ray sources in M101 (Pence+, 2001)</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M101. From this rich data set we have created a catalog of the 110 sources from the S3 chip detected with a significance of greater than 3{sigma}. This detection threshold corresponds to a flux of ~10^-16^ergs/cm^2^/s and a luminosity of ~10^36^ergs/s for a distance to M101 of 7.2Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189#table1</TD>
            <TD>2011-09-14T20:14:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/561/189&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/561/189</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE857 [1]</TD>
            <TD>Planck Early Release 857-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 857-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
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            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>180</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE857 [2]</TD>
            <TD>Planck Early Release 857-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 857-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke857#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke857.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE857 [3]</TD>
            <TD>Planck Early Release 857-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 857-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke857#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD />
            <TD>ivo://nasa.heasarc/plancke857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke857&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke857.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/561/189 [1]</TD>
            <TD>Chandra X-ray sources in M101 (Pence+, 2001)</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M101. From this rich data set we have created a catalog of the 110 sources from the S3 chip detected with a significance of greater than 3{sigma}. This detection threshold corresponds to a flux of ~10^-16^ergs/cm^2^/s and a luminosity of ~10^36^ergs/s for a distance to M101 of 7.2Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189#1</TD>
            <TD>2011-09-14T20:14:11Z</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/561/189</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/561/189</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/561/189 [2]</TD>
            <TD>Chandra X-ray sources in M101 (Pence+, 2001)</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M101. From this rich data set we have created a catalog of the 110 sources from the S3 chip detected with a significance of greater than 3{sigma}. This detection threshold corresponds to a flux of ~10^-16^ergs/cm^2^/s and a luminosity of ~10^36^ergs/s for a distance to M101 of 7.2Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189#2</TD>
            <TD>2011-09-14T20:14:11Z</TD>
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            <TD />
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/561/189</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJ/561/189 [table1]</TD>
            <TD>Chandra X-ray sources in M101 (Pence+, 2001)</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M101. From this rich data set we have created a catalog of the 110 sources from the S3 chip detected with a significance of greater than 3{sigma}. This detection threshold corresponds to a flux of ~10^-16^ergs/cm^2^/s and a luminosity of ~10^36^ergs/s for a distance to M101 of 7.2Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/561/189#table1</TD>
            <TD>2011-09-14T20:14:11Z</TD>
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            <TD>#Research#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE857 [1]</TD>
            <TD>Planck Early Release 857-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 857-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke857#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke857&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke857.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE857 [2]</TD>
            <TD>Planck Early Release 857-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 857-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke857#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke857.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE857 [3]</TD>
            <TD>Planck Early Release 857-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 857-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke857#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke857&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke857.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/162/346 [1]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#1</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/162/346</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/162/346 [2]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#2</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/162/346&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/162/346 [table4]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#table4</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/162/346&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/162/346 [table6]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#table6</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/162/346&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASSBSCPGC [1]</TD>
            <TD>ROSAT All-Sky Survey Bright Source Catalog/Catalog of Principal Galaxies Matches</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog (RASS-BSC, CDS Cat. &lt;XI/10&gt;, the HEASARC table RASSBSC) with the Catalogue of Principal Galaxies (PGC, CDS Cat. &lt;VII/119&gt;, the HEASARC table PGC2003), 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100 arcseconds. A visual screening process was applied to classify the reliability of the correlations. 547 correlations have been quoted as reliable identifications. From these, 349 sources are known to be active galaxies. Although for the other sources no hints for activity were found in the literature, 69% of those for which we have distances show X-ray luminosities exceeding those of normal galaxies, a clear sign that these galaxies also own hitherto unreported X-ray active components. Some objects are located inside or in the direction of a known group or cluster of galaxies. Their X-ray flux may therefore be in part affected by hot gas emission. In the paper, luminosity and log N-log S distributions are used to characterize different subsamples. Nuclei that are both optically and X-ray active are found predominantly in spirals. Two special source samples are defined, one with candidates for X-ray emission from hitherto unknown groups or clusters of galaxies, and one with high X-ray luminosity sources, that are likely candidates to possess hitherto unreported active galactic nuclei. Besides a compilation of X-ray and optical parameters, X-ray overlays on optical images for all the objects are also supplied as part of this work. This table contains 1124 optical galaxy entries for the 904 relevant X-ray candidates/counterparts from the RASS. Besides a compilation of X-ray and optical parameters for each source, the results of an identification screening are also given. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement of the reliability of the associations.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassbscpgc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassbscpgc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rassbscpgc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassbscpgc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASSBSCPGC [2]</TD>
            <TD>ROSAT All-Sky Survey Bright Source Catalog/Catalog of Principal Galaxies Matches</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog (RASS-BSC, CDS Cat. &lt;XI/10&gt;, the HEASARC table RASSBSC) with the Catalogue of Principal Galaxies (PGC, CDS Cat. &lt;VII/119&gt;, the HEASARC table PGC2003), 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100 arcseconds. A visual screening process was applied to classify the reliability of the correlations. 547 correlations have been quoted as reliable identifications. From these, 349 sources are known to be active galaxies. Although for the other sources no hints for activity were found in the literature, 69% of those for which we have distances show X-ray luminosities exceeding those of normal galaxies, a clear sign that these galaxies also own hitherto unreported X-ray active components. Some objects are located inside or in the direction of a known group or cluster of galaxies. Their X-ray flux may therefore be in part affected by hot gas emission. In the paper, luminosity and log N-log S distributions are used to characterize different subsamples. Nuclei that are both optically and X-ray active are found predominantly in spirals. Two special source samples are defined, one with candidates for X-ray emission from hitherto unknown groups or clusters of galaxies, and one with high X-ray luminosity sources, that are likely candidates to possess hitherto unreported active galactic nuclei. Besides a compilation of X-ray and optical parameters, X-ray overlays on optical images for all the objects are also supplied as part of this work. This table contains 1124 optical galaxy entries for the 904 relevant X-ray candidates/counterparts from the RASS. Besides a compilation of X-ray and optical parameters for each source, the results of an identification screening are also given. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement of the reliability of the associations.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassbscpgc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassbscpgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rassbscpgc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassbscpgc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASSBSCPGC [3]</TD>
            <TD>ROSAT All-Sky Survey Bright Source Catalog/Catalog of Principal Galaxies Matches</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog (RASS-BSC, CDS Cat. &lt;XI/10&gt;, the HEASARC table RASSBSC) with the Catalogue of Principal Galaxies (PGC, CDS Cat. &lt;VII/119&gt;, the HEASARC table PGC2003), 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100 arcseconds. A visual screening process was applied to classify the reliability of the correlations. 547 correlations have been quoted as reliable identifications. From these, 349 sources are known to be active galaxies. Although for the other sources no hints for activity were found in the literature, 69% of those for which we have distances show X-ray luminosities exceeding those of normal galaxies, a clear sign that these galaxies also own hitherto unreported X-ray active components. Some objects are located inside or in the direction of a known group or cluster of galaxies. Their X-ray flux may therefore be in part affected by hot gas emission. In the paper, luminosity and log N-log S distributions are used to characterize different subsamples. Nuclei that are both optically and X-ray active are found predominantly in spirals. Two special source samples are defined, one with candidates for X-ray emission from hitherto unknown groups or clusters of galaxies, and one with high X-ray luminosity sources, that are likely candidates to possess hitherto unreported active galactic nuclei. Besides a compilation of X-ray and optical parameters, X-ray overlays on optical images for all the objects are also supplied as part of this work. This table contains 1124 optical galaxy entries for the 904 relevant X-ray candidates/counterparts from the RASS. Besides a compilation of X-ray and optical parameters for each source, the results of an identification screening are also given. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement of the reliability of the associations.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassbscpgc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassbscpgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rassbscpgc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassbscpgc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/162/346 [1]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#1</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/162/346</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/162/346 [2]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#2</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/162/346&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/162/346 [table4]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#table4</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/162/346&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/162/346 [table6]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#table6</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/162/346&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASSBSCPGC [1]</TD>
            <TD>ROSAT All-Sky Survey Bright Source Catalog/Catalog of Principal Galaxies Matches</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog (RASS-BSC, CDS Cat. &lt;XI/10&gt;, the HEASARC table RASSBSC) with the Catalogue of Principal Galaxies (PGC, CDS Cat. &lt;VII/119&gt;, the HEASARC table PGC2003), 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100 arcseconds. A visual screening process was applied to classify the reliability of the correlations. 547 correlations have been quoted as reliable identifications. From these, 349 sources are known to be active galaxies. Although for the other sources no hints for activity were found in the literature, 69% of those for which we have distances show X-ray luminosities exceeding those of normal galaxies, a clear sign that these galaxies also own hitherto unreported X-ray active components. Some objects are located inside or in the direction of a known group or cluster of galaxies. Their X-ray flux may therefore be in part affected by hot gas emission. In the paper, luminosity and log N-log S distributions are used to characterize different subsamples. Nuclei that are both optically and X-ray active are found predominantly in spirals. Two special source samples are defined, one with candidates for X-ray emission from hitherto unknown groups or clusters of galaxies, and one with high X-ray luminosity sources, that are likely candidates to possess hitherto unreported active galactic nuclei. Besides a compilation of X-ray and optical parameters, X-ray overlays on optical images for all the objects are also supplied as part of this work. This table contains 1124 optical galaxy entries for the 904 relevant X-ray candidates/counterparts from the RASS. Besides a compilation of X-ray and optical parameters for each source, the results of an identification screening are also given. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement of the reliability of the associations.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassbscpgc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassbscpgc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rassbscpgc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassbscpgc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASSBSCPGC [2]</TD>
            <TD>ROSAT All-Sky Survey Bright Source Catalog/Catalog of Principal Galaxies Matches</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog (RASS-BSC, CDS Cat. &lt;XI/10&gt;, the HEASARC table RASSBSC) with the Catalogue of Principal Galaxies (PGC, CDS Cat. &lt;VII/119&gt;, the HEASARC table PGC2003), 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100 arcseconds. A visual screening process was applied to classify the reliability of the correlations. 547 correlations have been quoted as reliable identifications. From these, 349 sources are known to be active galaxies. Although for the other sources no hints for activity were found in the literature, 69% of those for which we have distances show X-ray luminosities exceeding those of normal galaxies, a clear sign that these galaxies also own hitherto unreported X-ray active components. Some objects are located inside or in the direction of a known group or cluster of galaxies. Their X-ray flux may therefore be in part affected by hot gas emission. In the paper, luminosity and log N-log S distributions are used to characterize different subsamples. Nuclei that are both optically and X-ray active are found predominantly in spirals. Two special source samples are defined, one with candidates for X-ray emission from hitherto unknown groups or clusters of galaxies, and one with high X-ray luminosity sources, that are likely candidates to possess hitherto unreported active galactic nuclei. Besides a compilation of X-ray and optical parameters, X-ray overlays on optical images for all the objects are also supplied as part of this work. This table contains 1124 optical galaxy entries for the 904 relevant X-ray candidates/counterparts from the RASS. Besides a compilation of X-ray and optical parameters for each source, the results of an identification screening are also given. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement of the reliability of the associations.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassbscpgc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassbscpgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rassbscpgc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassbscpgc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASSBSCPGC [3]</TD>
            <TD>ROSAT All-Sky Survey Bright Source Catalog/Catalog of Principal Galaxies Matches</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog (RASS-BSC, CDS Cat. &lt;XI/10&gt;, the HEASARC table RASSBSC) with the Catalogue of Principal Galaxies (PGC, CDS Cat. &lt;VII/119&gt;, the HEASARC table PGC2003), 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100 arcseconds. A visual screening process was applied to classify the reliability of the correlations. 547 correlations have been quoted as reliable identifications. From these, 349 sources are known to be active galaxies. Although for the other sources no hints for activity were found in the literature, 69% of those for which we have distances show X-ray luminosities exceeding those of normal galaxies, a clear sign that these galaxies also own hitherto unreported X-ray active components. Some objects are located inside or in the direction of a known group or cluster of galaxies. Their X-ray flux may therefore be in part affected by hot gas emission. In the paper, luminosity and log N-log S distributions are used to characterize different subsamples. Nuclei that are both optically and X-ray active are found predominantly in spirals. Two special source samples are defined, one with candidates for X-ray emission from hitherto unknown groups or clusters of galaxies, and one with high X-ray luminosity sources, that are likely candidates to possess hitherto unreported active galactic nuclei. Besides a compilation of X-ray and optical parameters, X-ray overlays on optical images for all the objects are also supplied as part of this work. This table contains 1124 optical galaxy entries for the 904 relevant X-ray candidates/counterparts from the RASS. Besides a compilation of X-ray and optical parameters for each source, the results of an identification screening are also given. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement of the reliability of the associations.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassbscpgc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassbscpgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rassbscpgc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassbscpgc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/162/346 [1]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#1</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/162/346</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/162/346 [2]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#2</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/162/346&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/162/346 [table4]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#table4</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/162/346&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/162/346 [table6]</TD>
            <TD>Abundance gradients in the Galaxy (Rudolph+, 2006)</TD>
            <TD>The FIR observations of [SIII] (19{mu}m), [OIII] (52, 88{mu}m), and [NIII] (57{mu}m) were made with the 91cm telescope of the KAO using the facility Cryogenic Grating Spectrometer (CGS) on flights of 1995 August 6, 10, and 12.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346#table6</TD>
            <TD>2011-09-14T20:14:43Z</TD>
            <TD>#Abundances#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/346</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/162/346&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RASSBSCPGC [1]</TD>
            <TD>ROSAT All-Sky Survey Bright Source Catalog/Catalog of Principal Galaxies Matches</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog (RASS-BSC, CDS Cat. &lt;XI/10&gt;, the HEASARC table RASSBSC) with the Catalogue of Principal Galaxies (PGC, CDS Cat. &lt;VII/119&gt;, the HEASARC table PGC2003), 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100 arcseconds. A visual screening process was applied to classify the reliability of the correlations. 547 correlations have been quoted as reliable identifications. From these, 349 sources are known to be active galaxies. Although for the other sources no hints for activity were found in the literature, 69% of those for which we have distances show X-ray luminosities exceeding those of normal galaxies, a clear sign that these galaxies also own hitherto unreported X-ray active components. Some objects are located inside or in the direction of a known group or cluster of galaxies. Their X-ray flux may therefore be in part affected by hot gas emission. In the paper, luminosity and log N-log S distributions are used to characterize different subsamples. Nuclei that are both optically and X-ray active are found predominantly in spirals. Two special source samples are defined, one with candidates for X-ray emission from hitherto unknown groups or clusters of galaxies, and one with high X-ray luminosity sources, that are likely candidates to possess hitherto unreported active galactic nuclei. Besides a compilation of X-ray and optical parameters, X-ray overlays on optical images for all the objects are also supplied as part of this work. This table contains 1124 optical galaxy entries for the 904 relevant X-ray candidates/counterparts from the RASS. Besides a compilation of X-ray and optical parameters for each source, the results of an identification screening are also given. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement of the reliability of the associations.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassbscpgc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassbscpgc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rassbscpgc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassbscpgc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RASSBSCPGC [2]</TD>
            <TD>ROSAT All-Sky Survey Bright Source Catalog/Catalog of Principal Galaxies Matches</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog (RASS-BSC, CDS Cat. &lt;XI/10&gt;, the HEASARC table RASSBSC) with the Catalogue of Principal Galaxies (PGC, CDS Cat. &lt;VII/119&gt;, the HEASARC table PGC2003), 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100 arcseconds. A visual screening process was applied to classify the reliability of the correlations. 547 correlations have been quoted as reliable identifications. From these, 349 sources are known to be active galaxies. Although for the other sources no hints for activity were found in the literature, 69% of those for which we have distances show X-ray luminosities exceeding those of normal galaxies, a clear sign that these galaxies also own hitherto unreported X-ray active components. Some objects are located inside or in the direction of a known group or cluster of galaxies. Their X-ray flux may therefore be in part affected by hot gas emission. In the paper, luminosity and log N-log S distributions are used to characterize different subsamples. Nuclei that are both optically and X-ray active are found predominantly in spirals. Two special source samples are defined, one with candidates for X-ray emission from hitherto unknown groups or clusters of galaxies, and one with high X-ray luminosity sources, that are likely candidates to possess hitherto unreported active galactic nuclei. Besides a compilation of X-ray and optical parameters, X-ray overlays on optical images for all the objects are also supplied as part of this work. This table contains 1124 optical galaxy entries for the 904 relevant X-ray candidates/counterparts from the RASS. Besides a compilation of X-ray and optical parameters for each source, the results of an identification screening are also given. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement of the reliability of the associations.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassbscpgc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassbscpgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rassbscpgc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassbscpgc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RASSBSCPGC [3]</TD>
            <TD>ROSAT All-Sky Survey Bright Source Catalog/Catalog of Principal Galaxies Matches</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalog (RASS-BSC, CDS Cat. &lt;XI/10&gt;, the HEASARC table RASSBSC) with the Catalogue of Principal Galaxies (PGC, CDS Cat. &lt;VII/119&gt;, the HEASARC table PGC2003), 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100 arcseconds. A visual screening process was applied to classify the reliability of the correlations. 547 correlations have been quoted as reliable identifications. From these, 349 sources are known to be active galaxies. Although for the other sources no hints for activity were found in the literature, 69% of those for which we have distances show X-ray luminosities exceeding those of normal galaxies, a clear sign that these galaxies also own hitherto unreported X-ray active components. Some objects are located inside or in the direction of a known group or cluster of galaxies. Their X-ray flux may therefore be in part affected by hot gas emission. In the paper, luminosity and log N-log S distributions are used to characterize different subsamples. Nuclei that are both optically and X-ray active are found predominantly in spirals. Two special source samples are defined, one with candidates for X-ray emission from hitherto unknown groups or clusters of galaxies, and one with high X-ray luminosity sources, that are likely candidates to possess hitherto unreported active galactic nuclei. Besides a compilation of X-ray and optical parameters, X-ray overlays on optical images for all the objects are also supplied as part of this work. This table contains 1124 optical galaxy entries for the 904 relevant X-ray candidates/counterparts from the RASS. Besides a compilation of X-ray and optical parameters for each source, the results of an identification screening are also given. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement of the reliability of the associations.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/rassbscpgc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rassbscpgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rassbscpgc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/rassbscpgc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/117/37 [1]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#1</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/117/37</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/117/37 [2]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#2</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/117/37&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/37 [ngc2419]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#ngc2419</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/37 [pal14]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#pal14</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/37 [pal4]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#pal4</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/138/1203 [1]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#1</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/138/1203</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/138/1203 [2]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#2</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/138/1203&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1203 [table1]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#table1</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1203 [table3]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#table3</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/117/37 [1]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#1</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/117/37</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/117/37 [2]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#2</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/117/37&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/37 [ngc2419]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#ngc2419</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/37 [pal14]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#pal14</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/37 [pal4]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#pal4</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/456/467 [1]</TD>
            <TD>New sample of bright galaxy pairs in UZC (Focardi+, 2006)</TD>
            <TD>We present a new sample of bright galaxy pairs extracted applying an objective selection code to the UZC catalog. The sample is volume-limited to M_zw_=-18.9+5logh and contains 89 galaxy pairs. We analyze the kinematical, morphological, and photometrical properties of galaxies belonging to this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467#1</TD>
            <TD>2011-09-14T19:56:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/456/467</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/467</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/456/467 [2]</TD>
            <TD>New sample of bright galaxy pairs in UZC (Focardi+, 2006)</TD>
            <TD>We present a new sample of bright galaxy pairs extracted applying an objective selection code to the UZC catalog. The sample is volume-limited to M_zw_=-18.9+5logh and contains 89 galaxy pairs. We analyze the kinematical, morphological, and photometrical properties of galaxies belonging to this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467#2</TD>
            <TD>2011-09-14T19:56:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/456/467&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/467</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/456/467 [table1]</TD>
            <TD>New sample of bright galaxy pairs in UZC (Focardi+, 2006)</TD>
            <TD>We present a new sample of bright galaxy pairs extracted applying an objective selection code to the UZC catalog. The sample is volume-limited to M_zw_=-18.9+5logh and contains 89 galaxy pairs. We analyze the kinematical, morphological, and photometrical properties of galaxies belonging to this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467#table1</TD>
            <TD>2011-09-14T19:56:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/456/467&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/467</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/117/37 [1]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#1</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/117/37</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/117/37 [2]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#2</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/117/37&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/37 [ngc2419]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#ngc2419</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/37 [pal14]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#pal14</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/37 [pal4]</TD>
            <TD>BVRI photometry in NGC 2419, Pal 4, and Pal 14 (Saha+, 2005)</TD>
            <TD>Observations were made primarily with the WIYN 3.5m telescope at the Kitt Peak National Observatory. In addition, our target fields and standard stars were also observed at the WIYN 0.9m telescope at Kitt Peak. Observations of NGC 2419, Pal 4, and Pal 14, all of which are distant globular clusters in our galaxy and have the additional virtue of having been observed repeatedly with the WFPC2 camera of the HST, were made on nights that appeared to be cloudless.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37#pal4</TD>
            <TD>2011-09-14T20:14:44Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Feb-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/37</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/37&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/37</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/456/467 [1]</TD>
            <TD>New sample of bright galaxy pairs in UZC (Focardi+, 2006)</TD>
            <TD>We present a new sample of bright galaxy pairs extracted applying an objective selection code to the UZC catalog. The sample is volume-limited to M_zw_=-18.9+5logh and contains 89 galaxy pairs. We analyze the kinematical, morphological, and photometrical properties of galaxies belonging to this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467#1</TD>
            <TD>2011-09-14T19:56:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/456/467</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/467</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/456/467 [2]</TD>
            <TD>New sample of bright galaxy pairs in UZC (Focardi+, 2006)</TD>
            <TD>We present a new sample of bright galaxy pairs extracted applying an objective selection code to the UZC catalog. The sample is volume-limited to M_zw_=-18.9+5logh and contains 89 galaxy pairs. We analyze the kinematical, morphological, and photometrical properties of galaxies belonging to this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467#2</TD>
            <TD>2011-09-14T19:56:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/456/467&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/467</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/456/467 [table1]</TD>
            <TD>New sample of bright galaxy pairs in UZC (Focardi+, 2006)</TD>
            <TD>We present a new sample of bright galaxy pairs extracted applying an objective selection code to the UZC catalog. The sample is volume-limited to M_zw_=-18.9+5logh and contains 89 galaxy pairs. We analyze the kinematical, morphological, and photometrical properties of galaxies belonging to this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467#table1</TD>
            <TD>2011-09-14T19:56:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/456/467&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/467</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/372/1259 [1]</TD>
            <TD>Abundances of extragalactic globular clusters (Sharina+, 2006)</TD>
            <TD>We present measurements of ages, metallicities and [alpha/Fe] ratios for 16 globular clusters (GCs) in NGC 147, 185 and 205 and of the central regions of the diffuse galaxy light in NGC 185 and 205. Our results are based on spectra obtained with the SCORPIO multislit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality Hubble Space Telescope/WFPC2 photometry of individual stars in the studied GCs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. All our sample GCs appear to be old (T&gt;8Gyr) and metal-poor ([Z/H]&lt;1.1), except for the GCs Hubble V in NGC 205 (T=1.2+/-0.6Gyr, [Z/H]=0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2Gyr, [Z/H]=0.8+/-0.2) and FJJVII in NGC 185 (T=7+/-3Gyr, [Z/H]=0.8+/-0.2). The majority of our GCs sample has solar [alpha/Fe] enhancement in contrast to the halo population of GCs in M31 and the Milky Way. The HB morphologies for our sample GCs follow the same behaviour with metallicity as younger halo Galactic GCs. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Spectroscopic ages and metallicities of the central regions in NGC 205 and 185 coincide with those obtained from colour-magnitude diagrams. The central field stellar populations in these galaxies have approximately the same age as their most central GCs (Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the central GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1259#1</TD>
            <TD>2011-09-14T20:15:48Z</TD>
            <TD>#Abundances#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1259</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/372/1259</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1259</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/372/1259 [2]</TD>
            <TD>Abundances of extragalactic globular clusters (Sharina+, 2006)</TD>
            <TD>We present measurements of ages, metallicities and [alpha/Fe] ratios for 16 globular clusters (GCs) in NGC 147, 185 and 205 and of the central regions of the diffuse galaxy light in NGC 185 and 205. Our results are based on spectra obtained with the SCORPIO multislit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality Hubble Space Telescope/WFPC2 photometry of individual stars in the studied GCs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. All our sample GCs appear to be old (T&gt;8Gyr) and metal-poor ([Z/H]&lt;1.1), except for the GCs Hubble V in NGC 205 (T=1.2+/-0.6Gyr, [Z/H]=0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2Gyr, [Z/H]=0.8+/-0.2) and FJJVII in NGC 185 (T=7+/-3Gyr, [Z/H]=0.8+/-0.2). The majority of our GCs sample has solar [alpha/Fe] enhancement in contrast to the halo population of GCs in M31 and the Milky Way. The HB morphologies for our sample GCs follow the same behaviour with metallicity as younger halo Galactic GCs. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Spectroscopic ages and metallicities of the central regions in NGC 205 and 185 coincide with those obtained from colour-magnitude diagrams. The central field stellar populations in these galaxies have approximately the same age as their most central GCs (Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the central GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1259#2</TD>
            <TD>2011-09-14T20:15:48Z</TD>
            <TD>#Abundances#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1259</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/372/1259&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/372/1259 [objects]</TD>
            <TD>Abundances of extragalactic globular clusters (Sharina+, 2006)</TD>
            <TD>We present measurements of ages, metallicities and [alpha/Fe] ratios for 16 globular clusters (GCs) in NGC 147, 185 and 205 and of the central regions of the diffuse galaxy light in NGC 185 and 205. Our results are based on spectra obtained with the SCORPIO multislit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality Hubble Space Telescope/WFPC2 photometry of individual stars in the studied GCs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. All our sample GCs appear to be old (T&gt;8Gyr) and metal-poor ([Z/H]&lt;1.1), except for the GCs Hubble V in NGC 205 (T=1.2+/-0.6Gyr, [Z/H]=0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2Gyr, [Z/H]=0.8+/-0.2) and FJJVII in NGC 185 (T=7+/-3Gyr, [Z/H]=0.8+/-0.2). The majority of our GCs sample has solar [alpha/Fe] enhancement in contrast to the halo population of GCs in M31 and the Milky Way. The HB morphologies for our sample GCs follow the same behaviour with metallicity as younger halo Galactic GCs. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Spectroscopic ages and metallicities of the central regions in NGC 205 and 185 coincide with those obtained from colour-magnitude diagrams. The central field stellar populations in these galaxies have approximately the same age as their most central GCs (Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the central GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1259#objects</TD>
            <TD>2011-09-14T20:15:48Z</TD>
            <TD>#Abundances#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/372/1259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1259</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/456/467 [1]</TD>
            <TD>New sample of bright galaxy pairs in UZC (Focardi+, 2006)</TD>
            <TD>We present a new sample of bright galaxy pairs extracted applying an objective selection code to the UZC catalog. The sample is volume-limited to M_zw_=-18.9+5logh and contains 89 galaxy pairs. We analyze the kinematical, morphological, and photometrical properties of galaxies belonging to this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467#1</TD>
            <TD>2011-09-14T19:56:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/456/467</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/467</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/456/467 [2]</TD>
            <TD>New sample of bright galaxy pairs in UZC (Focardi+, 2006)</TD>
            <TD>We present a new sample of bright galaxy pairs extracted applying an objective selection code to the UZC catalog. The sample is volume-limited to M_zw_=-18.9+5logh and contains 89 galaxy pairs. We analyze the kinematical, morphological, and photometrical properties of galaxies belonging to this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467#2</TD>
            <TD>2011-09-14T19:56:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/456/467&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/467</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/456/467 [table1]</TD>
            <TD>New sample of bright galaxy pairs in UZC (Focardi+, 2006)</TD>
            <TD>We present a new sample of bright galaxy pairs extracted applying an objective selection code to the UZC catalog. The sample is volume-limited to M_zw_=-18.9+5logh and contains 89 galaxy pairs. We analyze the kinematical, morphological, and photometrical properties of galaxies belonging to this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467#table1</TD>
            <TD>2011-09-14T19:56:46Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/467</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/456/467&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/467</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/135/1917 [1]</TD>
            <TD>Photometric search for transients in galaxy clusters (Sand+, 2008)</TD>
            <TD>++++Lrecl of file 'table4.dat' (95) increased to 101 %B The observations were conducted with the prime focus imager, 90Prime, on the 2.3m Bok telescope on Kitt Peak.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917#1</TD>
            <TD>2011-09-14T21:14:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/135/1917</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1917</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/135/1917 [2]</TD>
            <TD>Photometric search for transients in galaxy clusters (Sand+, 2008)</TD>
            <TD>++++Lrecl of file 'table4.dat' (95) increased to 101 %B The observations were conducted with the prime focus imager, 90Prime, on the 2.3m Bok telescope on Kitt Peak.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917#2</TD>
            <TD>2011-09-14T21:14:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/135/1917&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1917</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/135/1917 [tables]</TD>
            <TD>Photometric search for transients in galaxy clusters (Sand+, 2008)</TD>
            <TD>++++Lrecl of file 'table4.dat' (95) increased to 101 %B The observations were conducted with the prime focus imager, 90Prime, on the 2.3m Bok telescope on Kitt Peak.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917#tables</TD>
            <TD>2011-09-14T21:14:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/135/1917&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1917</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/444/831 [1]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#1</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/444/831</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/444/831 [2]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#2</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/444/831&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/444/831 [clusters]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#clusters</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/444/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/444/831 [table2]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#table2</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/444/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/135/1917 [1]</TD>
            <TD>Photometric search for transients in galaxy clusters (Sand+, 2008)</TD>
            <TD>++++Lrecl of file 'table4.dat' (95) increased to 101 %B The observations were conducted with the prime focus imager, 90Prime, on the 2.3m Bok telescope on Kitt Peak.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917#1</TD>
            <TD>2011-09-14T21:14:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/135/1917</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1917</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/135/1917 [2]</TD>
            <TD>Photometric search for transients in galaxy clusters (Sand+, 2008)</TD>
            <TD>++++Lrecl of file 'table4.dat' (95) increased to 101 %B The observations were conducted with the prime focus imager, 90Prime, on the 2.3m Bok telescope on Kitt Peak.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917#2</TD>
            <TD>2011-09-14T21:14:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/135/1917&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1917</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/135/1917 [tables]</TD>
            <TD>Photometric search for transients in galaxy clusters (Sand+, 2008)</TD>
            <TD>++++Lrecl of file 'table4.dat' (95) increased to 101 %B The observations were conducted with the prime focus imager, 90Prime, on the 2.3m Bok telescope on Kitt Peak.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917#tables</TD>
            <TD>2011-09-14T21:14:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/135/1917&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1917</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/444/831 [1]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#1</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/444/831</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/444/831 [2]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#2</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/444/831&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/444/831 [clusters]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#clusters</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/444/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/444/831 [table2]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#table2</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/444/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/135/1917 [1]</TD>
            <TD>Photometric search for transients in galaxy clusters (Sand+, 2008)</TD>
            <TD>++++Lrecl of file 'table4.dat' (95) increased to 101 %B The observations were conducted with the prime focus imager, 90Prime, on the 2.3m Bok telescope on Kitt Peak.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917#1</TD>
            <TD>2011-09-14T21:14:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/135/1917</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1917</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/135/1917 [2]</TD>
            <TD>Photometric search for transients in galaxy clusters (Sand+, 2008)</TD>
            <TD>++++Lrecl of file 'table4.dat' (95) increased to 101 %B The observations were conducted with the prime focus imager, 90Prime, on the 2.3m Bok telescope on Kitt Peak.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917#2</TD>
            <TD>2011-09-14T21:14:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/135/1917&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1917</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/135/1917 [tables]</TD>
            <TD>Photometric search for transients in galaxy clusters (Sand+, 2008)</TD>
            <TD>++++Lrecl of file 'table4.dat' (95) increased to 101 %B The observations were conducted with the prime focus imager, 90Prime, on the 2.3m Bok telescope on Kitt Peak.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917#tables</TD>
            <TD>2011-09-14T21:14:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/135/1917</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/135/1917&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/135/1917</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/444/831 [1]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#1</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/444/831</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/444/831 [2]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#2</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/444/831&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/444/831 [clusters]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#clusters</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/444/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/444/831 [table2]</TD>
            <TD>New star clusters in M33 (Bedin+, 2005)</TD>
            <TD>In this work we present the detection of 33 star clusters and 51 candidates in one field of the near by galaxy M 33. This study is based on WFC/ACS images available from the HST archive. Thanks to the high resolving power, we were able to confirm that two candidates previously indicated by Christian &amp; Schommer (1982ApJS...49..405C) are indeed star clusters. We list the main properties for the star clusters (and candidates), along with some peculiar objects, such as background galaxies and possible HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831#table2</TD>
            <TD>2011-09-14T19:57:17Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/444/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/831</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/511/A18 [1]</TD>
            <TD>NIR observations of stars near SgrA* (Schoedel+, 2010)</TD>
            <TD>The table tablea2.dat contains photometry in the H, Ks, and L'-bands for stars within a projected distance of approximately 1pc from the Galaxy's central black hole, Sagittarius A*. The data are based on observations with the NACO adaptive optics assisted near-infrared camera at the ESO VLT. Approximate astrometry for the stars is given relative to Sagittarius A*, as derived from the approximate camera pixel scale used, 0.027"/pixel, and assuming a 0 degree rotator angle. We estimate that absolute uncertainties in the astrometric precision can be as large as 0.1". The J2000.0 position of Sagittarius A* is (17:45:40.0409, -29:00:28.118) according to Reid &amp; Brunthaler (2004ApJ...616..872R). The uncertainties of the H, Ks , and L'-magnitudes in the table are statistical uncertainties. The one sigma uncertainties of the zero points are not included. They are 0.06mag for the H and Ks filters and 0.15mag for the L'-filter. A value of 0.00 in either of the H, Ks, or L'-fields means that the star was not detected with the corresponding filter. The FITS file AKs_fg6.fit is the extinction map for the Ks-band that is shown in the upper left panel of Fig. 6 of the original paper. The value of each pixel in the FITS image corresponds to the extinction in the Ks-band in magnitudes at the corresponding position. The effective wavelength is 2.168 micrometer. North is up and east is to the left. The pixel scale is 0.027" and Sagittarius A* is located at pixel position (808,611). These values will provide astrometry with an accuracy of roughly 0.1", a factor about 10 better than the actual resolution of the extinction map, which is about 1".</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18#1</TD>
            <TD>2011-09-14T21:15:15Z</TD>
            <TD>#Stars#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/511/A18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/511/A18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/511/A18 [2]</TD>
            <TD>NIR observations of stars near SgrA* (Schoedel+, 2010)</TD>
            <TD>The table tablea2.dat contains photometry in the H, Ks, and L'-bands for stars within a projected distance of approximately 1pc from the Galaxy's central black hole, Sagittarius A*. The data are based on observations with the NACO adaptive optics assisted near-infrared camera at the ESO VLT. Approximate astrometry for the stars is given relative to Sagittarius A*, as derived from the approximate camera pixel scale used, 0.027"/pixel, and assuming a 0 degree rotator angle. We estimate that absolute uncertainties in the astrometric precision can be as large as 0.1". The J2000.0 position of Sagittarius A* is (17:45:40.0409, -29:00:28.118) according to Reid &amp; Brunthaler (2004ApJ...616..872R). The uncertainties of the H, Ks , and L'-magnitudes in the table are statistical uncertainties. The one sigma uncertainties of the zero points are not included. They are 0.06mag for the H and Ks filters and 0.15mag for the L'-filter. A value of 0.00 in either of the H, Ks, or L'-fields means that the star was not detected with the corresponding filter. The FITS file AKs_fg6.fit is the extinction map for the Ks-band that is shown in the upper left panel of Fig. 6 of the original paper. The value of each pixel in the FITS image corresponds to the extinction in the Ks-band in magnitudes at the corresponding position. The effective wavelength is 2.168 micrometer. North is up and east is to the left. The pixel scale is 0.027" and Sagittarius A* is located at pixel position (808,611). These values will provide astrometry with an accuracy of roughly 0.1", a factor about 10 better than the actual resolution of the extinction map, which is about 1".</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18#2</TD>
            <TD>2011-09-14T21:15:15Z</TD>
            <TD>#Stars#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/511/A18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/511/A18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/511/A18 [tablea2]</TD>
            <TD>NIR observations of stars near SgrA* (Schoedel+, 2010)</TD>
            <TD>The table tablea2.dat contains photometry in the H, Ks, and L'-bands for stars within a projected distance of approximately 1pc from the Galaxy's central black hole, Sagittarius A*. The data are based on observations with the NACO adaptive optics assisted near-infrared camera at the ESO VLT. Approximate astrometry for the stars is given relative to Sagittarius A*, as derived from the approximate camera pixel scale used, 0.027"/pixel, and assuming a 0 degree rotator angle. We estimate that absolute uncertainties in the astrometric precision can be as large as 0.1". The J2000.0 position of Sagittarius A* is (17:45:40.0409, -29:00:28.118) according to Reid &amp; Brunthaler (2004ApJ...616..872R). The uncertainties of the H, Ks , and L'-magnitudes in the table are statistical uncertainties. The one sigma uncertainties of the zero points are not included. They are 0.06mag for the H and Ks filters and 0.15mag for the L'-filter. A value of 0.00 in either of the H, Ks, or L'-fields means that the star was not detected with the corresponding filter. The FITS file AKs_fg6.fit is the extinction map for the Ks-band that is shown in the upper left panel of Fig. 6 of the original paper. The value of each pixel in the FITS image corresponds to the extinction in the Ks-band in magnitudes at the corresponding position. The effective wavelength is 2.168 micrometer. North is up and east is to the left. The pixel scale is 0.027" and Sagittarius A* is located at pixel position (808,611). These values will provide astrometry with an accuracy of roughly 0.1", a factor about 10 better than the actual resolution of the extinction map, which is about 1".</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18#tablea2</TD>
            <TD>2011-09-14T21:15:15Z</TD>
            <TD>#Stars#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/511/A18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/511/A18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/143/73 [1]</TD>
            <TD>Morphology of spiral galaxies (Eskridge+, 2002)</TD>
            <TD>We announce the initial release of data from the Ohio State University (OSU) Bright Spiral Galaxy Survey (OSUBSGS), a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T type earlier in the H band than in the B band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73#1</TD>
            <TD>2011-09-14T19:58:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/143/73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/143/73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/143/73 [2]</TD>
            <TD>Morphology of spiral galaxies (Eskridge+, 2002)</TD>
            <TD>We announce the initial release of data from the Ohio State University (OSU) Bright Spiral Galaxy Survey (OSUBSGS), a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T type earlier in the H band than in the B band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73#2</TD>
            <TD>2011-09-14T19:58:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/143/73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/143/73</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/143/73 [table1]</TD>
            <TD>Morphology of spiral galaxies (Eskridge+, 2002)</TD>
            <TD>We announce the initial release of data from the Ohio State University (OSU) Bright Spiral Galaxy Survey (OSUBSGS), a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T type earlier in the H band than in the B band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73#table1</TD>
            <TD>2011-09-14T19:58:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/143/73&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/143/73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/511/A18 [1]</TD>
            <TD>NIR observations of stars near SgrA* (Schoedel+, 2010)</TD>
            <TD>The table tablea2.dat contains photometry in the H, Ks, and L'-bands for stars within a projected distance of approximately 1pc from the Galaxy's central black hole, Sagittarius A*. The data are based on observations with the NACO adaptive optics assisted near-infrared camera at the ESO VLT. Approximate astrometry for the stars is given relative to Sagittarius A*, as derived from the approximate camera pixel scale used, 0.027"/pixel, and assuming a 0 degree rotator angle. We estimate that absolute uncertainties in the astrometric precision can be as large as 0.1". The J2000.0 position of Sagittarius A* is (17:45:40.0409, -29:00:28.118) according to Reid &amp; Brunthaler (2004ApJ...616..872R). The uncertainties of the H, Ks , and L'-magnitudes in the table are statistical uncertainties. The one sigma uncertainties of the zero points are not included. They are 0.06mag for the H and Ks filters and 0.15mag for the L'-filter. A value of 0.00 in either of the H, Ks, or L'-fields means that the star was not detected with the corresponding filter. The FITS file AKs_fg6.fit is the extinction map for the Ks-band that is shown in the upper left panel of Fig. 6 of the original paper. The value of each pixel in the FITS image corresponds to the extinction in the Ks-band in magnitudes at the corresponding position. The effective wavelength is 2.168 micrometer. North is up and east is to the left. The pixel scale is 0.027" and Sagittarius A* is located at pixel position (808,611). These values will provide astrometry with an accuracy of roughly 0.1", a factor about 10 better than the actual resolution of the extinction map, which is about 1".</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18#1</TD>
            <TD>2011-09-14T21:15:15Z</TD>
            <TD>#Stars#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/511/A18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/511/A18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/511/A18 [2]</TD>
            <TD>NIR observations of stars near SgrA* (Schoedel+, 2010)</TD>
            <TD>The table tablea2.dat contains photometry in the H, Ks, and L'-bands for stars within a projected distance of approximately 1pc from the Galaxy's central black hole, Sagittarius A*. The data are based on observations with the NACO adaptive optics assisted near-infrared camera at the ESO VLT. Approximate astrometry for the stars is given relative to Sagittarius A*, as derived from the approximate camera pixel scale used, 0.027"/pixel, and assuming a 0 degree rotator angle. We estimate that absolute uncertainties in the astrometric precision can be as large as 0.1". The J2000.0 position of Sagittarius A* is (17:45:40.0409, -29:00:28.118) according to Reid &amp; Brunthaler (2004ApJ...616..872R). The uncertainties of the H, Ks , and L'-magnitudes in the table are statistical uncertainties. The one sigma uncertainties of the zero points are not included. They are 0.06mag for the H and Ks filters and 0.15mag for the L'-filter. A value of 0.00 in either of the H, Ks, or L'-fields means that the star was not detected with the corresponding filter. The FITS file AKs_fg6.fit is the extinction map for the Ks-band that is shown in the upper left panel of Fig. 6 of the original paper. The value of each pixel in the FITS image corresponds to the extinction in the Ks-band in magnitudes at the corresponding position. The effective wavelength is 2.168 micrometer. North is up and east is to the left. The pixel scale is 0.027" and Sagittarius A* is located at pixel position (808,611). These values will provide astrometry with an accuracy of roughly 0.1", a factor about 10 better than the actual resolution of the extinction map, which is about 1".</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18#2</TD>
            <TD>2011-09-14T21:15:15Z</TD>
            <TD>#Stars#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/511/A18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/511/A18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/511/A18 [tablea2]</TD>
            <TD>NIR observations of stars near SgrA* (Schoedel+, 2010)</TD>
            <TD>The table tablea2.dat contains photometry in the H, Ks, and L'-bands for stars within a projected distance of approximately 1pc from the Galaxy's central black hole, Sagittarius A*. The data are based on observations with the NACO adaptive optics assisted near-infrared camera at the ESO VLT. Approximate astrometry for the stars is given relative to Sagittarius A*, as derived from the approximate camera pixel scale used, 0.027"/pixel, and assuming a 0 degree rotator angle. We estimate that absolute uncertainties in the astrometric precision can be as large as 0.1". The J2000.0 position of Sagittarius A* is (17:45:40.0409, -29:00:28.118) according to Reid &amp; Brunthaler (2004ApJ...616..872R). The uncertainties of the H, Ks , and L'-magnitudes in the table are statistical uncertainties. The one sigma uncertainties of the zero points are not included. They are 0.06mag for the H and Ks filters and 0.15mag for the L'-filter. A value of 0.00 in either of the H, Ks, or L'-fields means that the star was not detected with the corresponding filter. The FITS file AKs_fg6.fit is the extinction map for the Ks-band that is shown in the upper left panel of Fig. 6 of the original paper. The value of each pixel in the FITS image corresponds to the extinction in the Ks-band in magnitudes at the corresponding position. The effective wavelength is 2.168 micrometer. North is up and east is to the left. The pixel scale is 0.027" and Sagittarius A* is located at pixel position (808,611). These values will provide astrometry with an accuracy of roughly 0.1", a factor about 10 better than the actual resolution of the extinction map, which is about 1".</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18#tablea2</TD>
            <TD>2011-09-14T21:15:15Z</TD>
            <TD>#Stars#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/511/A18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/511/A18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/138/1203 [1]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#1</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/138/1203</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/138/1203 [2]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#2</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/138/1203&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1203 [table1]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#table1</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1203 [table3]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#table3</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/511/A18 [1]</TD>
            <TD>NIR observations of stars near SgrA* (Schoedel+, 2010)</TD>
            <TD>The table tablea2.dat contains photometry in the H, Ks, and L'-bands for stars within a projected distance of approximately 1pc from the Galaxy's central black hole, Sagittarius A*. The data are based on observations with the NACO adaptive optics assisted near-infrared camera at the ESO VLT. Approximate astrometry for the stars is given relative to Sagittarius A*, as derived from the approximate camera pixel scale used, 0.027"/pixel, and assuming a 0 degree rotator angle. We estimate that absolute uncertainties in the astrometric precision can be as large as 0.1". The J2000.0 position of Sagittarius A* is (17:45:40.0409, -29:00:28.118) according to Reid &amp; Brunthaler (2004ApJ...616..872R). The uncertainties of the H, Ks , and L'-magnitudes in the table are statistical uncertainties. The one sigma uncertainties of the zero points are not included. They are 0.06mag for the H and Ks filters and 0.15mag for the L'-filter. A value of 0.00 in either of the H, Ks, or L'-fields means that the star was not detected with the corresponding filter. The FITS file AKs_fg6.fit is the extinction map for the Ks-band that is shown in the upper left panel of Fig. 6 of the original paper. The value of each pixel in the FITS image corresponds to the extinction in the Ks-band in magnitudes at the corresponding position. The effective wavelength is 2.168 micrometer. North is up and east is to the left. The pixel scale is 0.027" and Sagittarius A* is located at pixel position (808,611). These values will provide astrometry with an accuracy of roughly 0.1", a factor about 10 better than the actual resolution of the extinction map, which is about 1".</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18#1</TD>
            <TD>2011-09-14T21:15:15Z</TD>
            <TD>#Stars#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/511/A18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/511/A18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/511/A18 [2]</TD>
            <TD>NIR observations of stars near SgrA* (Schoedel+, 2010)</TD>
            <TD>The table tablea2.dat contains photometry in the H, Ks, and L'-bands for stars within a projected distance of approximately 1pc from the Galaxy's central black hole, Sagittarius A*. The data are based on observations with the NACO adaptive optics assisted near-infrared camera at the ESO VLT. Approximate astrometry for the stars is given relative to Sagittarius A*, as derived from the approximate camera pixel scale used, 0.027"/pixel, and assuming a 0 degree rotator angle. We estimate that absolute uncertainties in the astrometric precision can be as large as 0.1". The J2000.0 position of Sagittarius A* is (17:45:40.0409, -29:00:28.118) according to Reid &amp; Brunthaler (2004ApJ...616..872R). The uncertainties of the H, Ks , and L'-magnitudes in the table are statistical uncertainties. The one sigma uncertainties of the zero points are not included. They are 0.06mag for the H and Ks filters and 0.15mag for the L'-filter. A value of 0.00 in either of the H, Ks, or L'-fields means that the star was not detected with the corresponding filter. The FITS file AKs_fg6.fit is the extinction map for the Ks-band that is shown in the upper left panel of Fig. 6 of the original paper. The value of each pixel in the FITS image corresponds to the extinction in the Ks-band in magnitudes at the corresponding position. The effective wavelength is 2.168 micrometer. North is up and east is to the left. The pixel scale is 0.027" and Sagittarius A* is located at pixel position (808,611). These values will provide astrometry with an accuracy of roughly 0.1", a factor about 10 better than the actual resolution of the extinction map, which is about 1".</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18#2</TD>
            <TD>2011-09-14T21:15:15Z</TD>
            <TD>#Stars#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/511/A18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/511/A18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/511/A18 [tablea2]</TD>
            <TD>NIR observations of stars near SgrA* (Schoedel+, 2010)</TD>
            <TD>The table tablea2.dat contains photometry in the H, Ks, and L'-bands for stars within a projected distance of approximately 1pc from the Galaxy's central black hole, Sagittarius A*. The data are based on observations with the NACO adaptive optics assisted near-infrared camera at the ESO VLT. Approximate astrometry for the stars is given relative to Sagittarius A*, as derived from the approximate camera pixel scale used, 0.027"/pixel, and assuming a 0 degree rotator angle. We estimate that absolute uncertainties in the astrometric precision can be as large as 0.1". The J2000.0 position of Sagittarius A* is (17:45:40.0409, -29:00:28.118) according to Reid &amp; Brunthaler (2004ApJ...616..872R). The uncertainties of the H, Ks , and L'-magnitudes in the table are statistical uncertainties. The one sigma uncertainties of the zero points are not included. They are 0.06mag for the H and Ks filters and 0.15mag for the L'-filter. A value of 0.00 in either of the H, Ks, or L'-fields means that the star was not detected with the corresponding filter. The FITS file AKs_fg6.fit is the extinction map for the Ks-band that is shown in the upper left panel of Fig. 6 of the original paper. The value of each pixel in the FITS image corresponds to the extinction in the Ks-band in magnitudes at the corresponding position. The effective wavelength is 2.168 micrometer. North is up and east is to the left. The pixel scale is 0.027" and Sagittarius A* is located at pixel position (808,611). These values will provide astrometry with an accuracy of roughly 0.1", a factor about 10 better than the actual resolution of the extinction map, which is about 1".</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18#tablea2</TD>
            <TD>2011-09-14T21:15:15Z</TD>
            <TD>#Stars#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/511/A18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/511/A18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/511/A18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/138/1203 [1]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#1</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/138/1203</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/138/1203 [2]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#2</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/138/1203&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1203 [table1]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#table1</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1203 [table3]</TD>
            <TD>Star formation regions in nearby dwarf galaxies (Melena+, 2009)</TD>
            <TD>In this paper, we compare the properties of individual star-forming regions in outer and inner disks of a sample of dwarf galaxies. The young regions are identified on Galaxy Evolution Explorer (GALEX) near-UV (NUV) images archives. We use far-UV (FUV) and NUV, UBV, and some JHK colors to model the masses and ages of the regions. Our investigation includes approximately 2000 separate star-forming regions. With these data we compare mass, age, and several other key properties of star-forming regions in inner and outer disks. GALEX images were taken simultaneously in two channels: FUV, with a bandpass of 1350-1750{AA}, an effective wavelength of 1516{AA}, and a resolution of 4.0" and NUV with a bandpass of 1750-2800{AA}, an effective wavelength of 2267{AA}, and a resolution of 5.6".</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203#table3</TD>
            <TD>2012-02-26T21:16:14Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1203</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/682/821 [1]</TD>
            <TD>Spectral fits of galaxy clusters in X-ray (Cavagnolo+, 2008)</TD>
            <TD>We explore the band dependence of the inferred X-ray temperature of the intracluster medium (ICM) for 192 well-observed galaxy clusters selected from the Chandra Data Archive. If the hot ICM is nearly isothermal in the projected region of interest, the X-ray temperature inferred from a broadband (0.7-7.0keV) spectrum should be identical to the X-ray temperature inferred from a hard-band (2.0-7.0keV) spectrum. However, if unresolved cool lumps of gas are contributing soft X-ray emission, the temperature of a best-fit single-component thermal model will be cooler for the broadband spectrum than for the hard-band spectrum. Using this difference as a diagnostic, the ratio of best-fitting hard-band and broadband temperatures may indicate the presence of cooler gas even when the X-ray spectrum itself may not have sufficient signal-to-noise ratio (S/N) to resolve multiple temperature components. To test this possible diagnostic, we extract X-ray spectra from core-excised annular regions for each cluster in our archival sample. We compare the X-ray temperatures inferred from single-temperature fits when the energy range of the fit is 0.7-7.0keV (broad) and when the energy range is 2.0/(1+z)-7.0keV (hard). We find that the hard-band temperature is significantly higher, on average, than the broadband temperature. On further exploration, we find this temperature ratio is enhanced preferentially for clusters which are known merging systems. In addition, cool-core clusters tend to have best-fit hard-band temperatures that are in closer agreement with their best-fit broadband temperatures. We show, using simulated spectra, that this diagnostic is sensitive to secondary cool components (T_X_=0.5-3.0keV) with emission measures &gt;=10-30% of the primary hot component.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821#1</TD>
            <TD>2011-09-14T21:15:29Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/682/821</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/821</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/682/821 [2]</TD>
            <TD>Spectral fits of galaxy clusters in X-ray (Cavagnolo+, 2008)</TD>
            <TD>We explore the band dependence of the inferred X-ray temperature of the intracluster medium (ICM) for 192 well-observed galaxy clusters selected from the Chandra Data Archive. If the hot ICM is nearly isothermal in the projected region of interest, the X-ray temperature inferred from a broadband (0.7-7.0keV) spectrum should be identical to the X-ray temperature inferred from a hard-band (2.0-7.0keV) spectrum. However, if unresolved cool lumps of gas are contributing soft X-ray emission, the temperature of a best-fit single-component thermal model will be cooler for the broadband spectrum than for the hard-band spectrum. Using this difference as a diagnostic, the ratio of best-fitting hard-band and broadband temperatures may indicate the presence of cooler gas even when the X-ray spectrum itself may not have sufficient signal-to-noise ratio (S/N) to resolve multiple temperature components. To test this possible diagnostic, we extract X-ray spectra from core-excised annular regions for each cluster in our archival sample. We compare the X-ray temperatures inferred from single-temperature fits when the energy range of the fit is 0.7-7.0keV (broad) and when the energy range is 2.0/(1+z)-7.0keV (hard). We find that the hard-band temperature is significantly higher, on average, than the broadband temperature. On further exploration, we find this temperature ratio is enhanced preferentially for clusters which are known merging systems. In addition, cool-core clusters tend to have best-fit hard-band temperatures that are in closer agreement with their best-fit broadband temperatures. We show, using simulated spectra, that this diagnostic is sensitive to secondary cool components (T_X_=0.5-3.0keV) with emission measures &gt;=10-30% of the primary hot component.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821#2</TD>
            <TD>2011-09-14T21:15:29Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/682/821&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/682/821 [table1]</TD>
            <TD>Spectral fits of galaxy clusters in X-ray (Cavagnolo+, 2008)</TD>
            <TD>We explore the band dependence of the inferred X-ray temperature of the intracluster medium (ICM) for 192 well-observed galaxy clusters selected from the Chandra Data Archive. If the hot ICM is nearly isothermal in the projected region of interest, the X-ray temperature inferred from a broadband (0.7-7.0keV) spectrum should be identical to the X-ray temperature inferred from a hard-band (2.0-7.0keV) spectrum. However, if unresolved cool lumps of gas are contributing soft X-ray emission, the temperature of a best-fit single-component thermal model will be cooler for the broadband spectrum than for the hard-band spectrum. Using this difference as a diagnostic, the ratio of best-fitting hard-band and broadband temperatures may indicate the presence of cooler gas even when the X-ray spectrum itself may not have sufficient signal-to-noise ratio (S/N) to resolve multiple temperature components. To test this possible diagnostic, we extract X-ray spectra from core-excised annular regions for each cluster in our archival sample. We compare the X-ray temperatures inferred from single-temperature fits when the energy range of the fit is 0.7-7.0keV (broad) and when the energy range is 2.0/(1+z)-7.0keV (hard). We find that the hard-band temperature is significantly higher, on average, than the broadband temperature. On further exploration, we find this temperature ratio is enhanced preferentially for clusters which are known merging systems. In addition, cool-core clusters tend to have best-fit hard-band temperatures that are in closer agreement with their best-fit broadband temperatures. We show, using simulated spectra, that this diagnostic is sensitive to secondary cool components (T_X_=0.5-3.0keV) with emission measures &gt;=10-30% of the primary hot component.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821#table1</TD>
            <TD>2011-09-14T21:15:29Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/682/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/821</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/711/284 [1]</TD>
            <TD>Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)</TD>
            <TD>We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby universe (z&lt;0.05) and to break down the active galactic nucleus (AGN) host galaxy population by color, stellar mass, and morphology. We find that the black hole growth at luminosities L[OIII]&gt;10^40^erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (10^10^-10^11^M_{sun}_), reside in the green valley of the color-mass diagram and their central black holes have median masses around 10^6.5^M_{sun}_. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while in late-type galaxies, it is preferentially the most massive black holes that are growing. At high-Eddington ratios (L/L_Edd_&gt;0.1), the only population with a substantial fraction of AGNs are the low-mass green valley early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284#1</TD>
            <TD>2012-05-16T12:56:27Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/711/284</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/284</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/711/284 [2]</TD>
            <TD>Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)</TD>
            <TD>We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby universe (z&lt;0.05) and to break down the active galactic nucleus (AGN) host galaxy population by color, stellar mass, and morphology. We find that the black hole growth at luminosities L[OIII]&gt;10^40^erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (10^10^-10^11^M_{sun}_), reside in the green valley of the color-mass diagram and their central black holes have median masses around 10^6.5^M_{sun}_. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while in late-type galaxies, it is preferentially the most massive black holes that are growing. At high-Eddington ratios (L/L_Edd_&gt;0.1), the only population with a substantial fraction of AGNs are the low-mass green valley early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284#2</TD>
            <TD>2012-05-16T12:56:27Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/711/284&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/284</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/284 [table3]</TD>
            <TD>Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)</TD>
            <TD>We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby universe (z&lt;0.05) and to break down the active galactic nucleus (AGN) host galaxy population by color, stellar mass, and morphology. We find that the black hole growth at luminosities L[OIII]&gt;10^40^erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (10^10^-10^11^M_{sun}_), reside in the green valley of the color-mass diagram and their central black holes have median masses around 10^6.5^M_{sun}_. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while in late-type galaxies, it is preferentially the most massive black holes that are growing. At high-Eddington ratios (L/L_Edd_&gt;0.1), the only population with a substantial fraction of AGNs are the low-mass green valley early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284#table3</TD>
            <TD>2012-05-16T12:56:27Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/284&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/284</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/682/821 [1]</TD>
            <TD>Spectral fits of galaxy clusters in X-ray (Cavagnolo+, 2008)</TD>
            <TD>We explore the band dependence of the inferred X-ray temperature of the intracluster medium (ICM) for 192 well-observed galaxy clusters selected from the Chandra Data Archive. If the hot ICM is nearly isothermal in the projected region of interest, the X-ray temperature inferred from a broadband (0.7-7.0keV) spectrum should be identical to the X-ray temperature inferred from a hard-band (2.0-7.0keV) spectrum. However, if unresolved cool lumps of gas are contributing soft X-ray emission, the temperature of a best-fit single-component thermal model will be cooler for the broadband spectrum than for the hard-band spectrum. Using this difference as a diagnostic, the ratio of best-fitting hard-band and broadband temperatures may indicate the presence of cooler gas even when the X-ray spectrum itself may not have sufficient signal-to-noise ratio (S/N) to resolve multiple temperature components. To test this possible diagnostic, we extract X-ray spectra from core-excised annular regions for each cluster in our archival sample. We compare the X-ray temperatures inferred from single-temperature fits when the energy range of the fit is 0.7-7.0keV (broad) and when the energy range is 2.0/(1+z)-7.0keV (hard). We find that the hard-band temperature is significantly higher, on average, than the broadband temperature. On further exploration, we find this temperature ratio is enhanced preferentially for clusters which are known merging systems. In addition, cool-core clusters tend to have best-fit hard-band temperatures that are in closer agreement with their best-fit broadband temperatures. We show, using simulated spectra, that this diagnostic is sensitive to secondary cool components (T_X_=0.5-3.0keV) with emission measures &gt;=10-30% of the primary hot component.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821#1</TD>
            <TD>2011-09-14T21:15:29Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/682/821</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/821</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/682/821 [2]</TD>
            <TD>Spectral fits of galaxy clusters in X-ray (Cavagnolo+, 2008)</TD>
            <TD>We explore the band dependence of the inferred X-ray temperature of the intracluster medium (ICM) for 192 well-observed galaxy clusters selected from the Chandra Data Archive. If the hot ICM is nearly isothermal in the projected region of interest, the X-ray temperature inferred from a broadband (0.7-7.0keV) spectrum should be identical to the X-ray temperature inferred from a hard-band (2.0-7.0keV) spectrum. However, if unresolved cool lumps of gas are contributing soft X-ray emission, the temperature of a best-fit single-component thermal model will be cooler for the broadband spectrum than for the hard-band spectrum. Using this difference as a diagnostic, the ratio of best-fitting hard-band and broadband temperatures may indicate the presence of cooler gas even when the X-ray spectrum itself may not have sufficient signal-to-noise ratio (S/N) to resolve multiple temperature components. To test this possible diagnostic, we extract X-ray spectra from core-excised annular regions for each cluster in our archival sample. We compare the X-ray temperatures inferred from single-temperature fits when the energy range of the fit is 0.7-7.0keV (broad) and when the energy range is 2.0/(1+z)-7.0keV (hard). We find that the hard-band temperature is significantly higher, on average, than the broadband temperature. On further exploration, we find this temperature ratio is enhanced preferentially for clusters which are known merging systems. In addition, cool-core clusters tend to have best-fit hard-band temperatures that are in closer agreement with their best-fit broadband temperatures. We show, using simulated spectra, that this diagnostic is sensitive to secondary cool components (T_X_=0.5-3.0keV) with emission measures &gt;=10-30% of the primary hot component.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821#2</TD>
            <TD>2011-09-14T21:15:29Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/682/821&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/682/821 [table1]</TD>
            <TD>Spectral fits of galaxy clusters in X-ray (Cavagnolo+, 2008)</TD>
            <TD>We explore the band dependence of the inferred X-ray temperature of the intracluster medium (ICM) for 192 well-observed galaxy clusters selected from the Chandra Data Archive. If the hot ICM is nearly isothermal in the projected region of interest, the X-ray temperature inferred from a broadband (0.7-7.0keV) spectrum should be identical to the X-ray temperature inferred from a hard-band (2.0-7.0keV) spectrum. However, if unresolved cool lumps of gas are contributing soft X-ray emission, the temperature of a best-fit single-component thermal model will be cooler for the broadband spectrum than for the hard-band spectrum. Using this difference as a diagnostic, the ratio of best-fitting hard-band and broadband temperatures may indicate the presence of cooler gas even when the X-ray spectrum itself may not have sufficient signal-to-noise ratio (S/N) to resolve multiple temperature components. To test this possible diagnostic, we extract X-ray spectra from core-excised annular regions for each cluster in our archival sample. We compare the X-ray temperatures inferred from single-temperature fits when the energy range of the fit is 0.7-7.0keV (broad) and when the energy range is 2.0/(1+z)-7.0keV (hard). We find that the hard-band temperature is significantly higher, on average, than the broadband temperature. On further exploration, we find this temperature ratio is enhanced preferentially for clusters which are known merging systems. In addition, cool-core clusters tend to have best-fit hard-band temperatures that are in closer agreement with their best-fit broadband temperatures. We show, using simulated spectra, that this diagnostic is sensitive to secondary cool components (T_X_=0.5-3.0keV) with emission measures &gt;=10-30% of the primary hot component.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821#table1</TD>
            <TD>2011-09-14T21:15:29Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/682/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/821</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/711/284 [1]</TD>
            <TD>Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)</TD>
            <TD>We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby universe (z&lt;0.05) and to break down the active galactic nucleus (AGN) host galaxy population by color, stellar mass, and morphology. We find that the black hole growth at luminosities L[OIII]&gt;10^40^erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (10^10^-10^11^M_{sun}_), reside in the green valley of the color-mass diagram and their central black holes have median masses around 10^6.5^M_{sun}_. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while in late-type galaxies, it is preferentially the most massive black holes that are growing. At high-Eddington ratios (L/L_Edd_&gt;0.1), the only population with a substantial fraction of AGNs are the low-mass green valley early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284#1</TD>
            <TD>2012-05-16T12:56:27Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/711/284</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/284</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/711/284 [2]</TD>
            <TD>Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)</TD>
            <TD>We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby universe (z&lt;0.05) and to break down the active galactic nucleus (AGN) host galaxy population by color, stellar mass, and morphology. We find that the black hole growth at luminosities L[OIII]&gt;10^40^erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (10^10^-10^11^M_{sun}_), reside in the green valley of the color-mass diagram and their central black holes have median masses around 10^6.5^M_{sun}_. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while in late-type galaxies, it is preferentially the most massive black holes that are growing. At high-Eddington ratios (L/L_Edd_&gt;0.1), the only population with a substantial fraction of AGNs are the low-mass green valley early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284#2</TD>
            <TD>2012-05-16T12:56:27Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/711/284&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/284</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/284 [table3]</TD>
            <TD>Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)</TD>
            <TD>We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby universe (z&lt;0.05) and to break down the active galactic nucleus (AGN) host galaxy population by color, stellar mass, and morphology. We find that the black hole growth at luminosities L[OIII]&gt;10^40^erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (10^10^-10^11^M_{sun}_), reside in the green valley of the color-mass diagram and their central black holes have median masses around 10^6.5^M_{sun}_. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while in late-type galaxies, it is preferentially the most massive black holes that are growing. At high-Eddington ratios (L/L_Edd_&gt;0.1), the only population with a substantial fraction of AGNs are the low-mass green valley early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284#table3</TD>
            <TD>2012-05-16T12:56:27Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/284&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/284</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/682/821 [1]</TD>
            <TD>Spectral fits of galaxy clusters in X-ray (Cavagnolo+, 2008)</TD>
            <TD>We explore the band dependence of the inferred X-ray temperature of the intracluster medium (ICM) for 192 well-observed galaxy clusters selected from the Chandra Data Archive. If the hot ICM is nearly isothermal in the projected region of interest, the X-ray temperature inferred from a broadband (0.7-7.0keV) spectrum should be identical to the X-ray temperature inferred from a hard-band (2.0-7.0keV) spectrum. However, if unresolved cool lumps of gas are contributing soft X-ray emission, the temperature of a best-fit single-component thermal model will be cooler for the broadband spectrum than for the hard-band spectrum. Using this difference as a diagnostic, the ratio of best-fitting hard-band and broadband temperatures may indicate the presence of cooler gas even when the X-ray spectrum itself may not have sufficient signal-to-noise ratio (S/N) to resolve multiple temperature components. To test this possible diagnostic, we extract X-ray spectra from core-excised annular regions for each cluster in our archival sample. We compare the X-ray temperatures inferred from single-temperature fits when the energy range of the fit is 0.7-7.0keV (broad) and when the energy range is 2.0/(1+z)-7.0keV (hard). We find that the hard-band temperature is significantly higher, on average, than the broadband temperature. On further exploration, we find this temperature ratio is enhanced preferentially for clusters which are known merging systems. In addition, cool-core clusters tend to have best-fit hard-band temperatures that are in closer agreement with their best-fit broadband temperatures. We show, using simulated spectra, that this diagnostic is sensitive to secondary cool components (T_X_=0.5-3.0keV) with emission measures &gt;=10-30% of the primary hot component.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821#1</TD>
            <TD>2011-09-14T21:15:29Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/682/821</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/821</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/682/821 [2]</TD>
            <TD>Spectral fits of galaxy clusters in X-ray (Cavagnolo+, 2008)</TD>
            <TD>We explore the band dependence of the inferred X-ray temperature of the intracluster medium (ICM) for 192 well-observed galaxy clusters selected from the Chandra Data Archive. If the hot ICM is nearly isothermal in the projected region of interest, the X-ray temperature inferred from a broadband (0.7-7.0keV) spectrum should be identical to the X-ray temperature inferred from a hard-band (2.0-7.0keV) spectrum. However, if unresolved cool lumps of gas are contributing soft X-ray emission, the temperature of a best-fit single-component thermal model will be cooler for the broadband spectrum than for the hard-band spectrum. Using this difference as a diagnostic, the ratio of best-fitting hard-band and broadband temperatures may indicate the presence of cooler gas even when the X-ray spectrum itself may not have sufficient signal-to-noise ratio (S/N) to resolve multiple temperature components. To test this possible diagnostic, we extract X-ray spectra from core-excised annular regions for each cluster in our archival sample. We compare the X-ray temperatures inferred from single-temperature fits when the energy range of the fit is 0.7-7.0keV (broad) and when the energy range is 2.0/(1+z)-7.0keV (hard). We find that the hard-band temperature is significantly higher, on average, than the broadband temperature. On further exploration, we find this temperature ratio is enhanced preferentially for clusters which are known merging systems. In addition, cool-core clusters tend to have best-fit hard-band temperatures that are in closer agreement with their best-fit broadband temperatures. We show, using simulated spectra, that this diagnostic is sensitive to secondary cool components (T_X_=0.5-3.0keV) with emission measures &gt;=10-30% of the primary hot component.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821#2</TD>
            <TD>2011-09-14T21:15:29Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/682/821&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/682/821 [table1]</TD>
            <TD>Spectral fits of galaxy clusters in X-ray (Cavagnolo+, 2008)</TD>
            <TD>We explore the band dependence of the inferred X-ray temperature of the intracluster medium (ICM) for 192 well-observed galaxy clusters selected from the Chandra Data Archive. If the hot ICM is nearly isothermal in the projected region of interest, the X-ray temperature inferred from a broadband (0.7-7.0keV) spectrum should be identical to the X-ray temperature inferred from a hard-band (2.0-7.0keV) spectrum. However, if unresolved cool lumps of gas are contributing soft X-ray emission, the temperature of a best-fit single-component thermal model will be cooler for the broadband spectrum than for the hard-band spectrum. Using this difference as a diagnostic, the ratio of best-fitting hard-band and broadband temperatures may indicate the presence of cooler gas even when the X-ray spectrum itself may not have sufficient signal-to-noise ratio (S/N) to resolve multiple temperature components. To test this possible diagnostic, we extract X-ray spectra from core-excised annular regions for each cluster in our archival sample. We compare the X-ray temperatures inferred from single-temperature fits when the energy range of the fit is 0.7-7.0keV (broad) and when the energy range is 2.0/(1+z)-7.0keV (hard). We find that the hard-band temperature is significantly higher, on average, than the broadband temperature. On further exploration, we find this temperature ratio is enhanced preferentially for clusters which are known merging systems. In addition, cool-core clusters tend to have best-fit hard-band temperatures that are in closer agreement with their best-fit broadband temperatures. We show, using simulated spectra, that this diagnostic is sensitive to secondary cool components (T_X_=0.5-3.0keV) with emission measures &gt;=10-30% of the primary hot component.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821#table1</TD>
            <TD>2011-09-14T21:15:29Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/682/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/821</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/711/284 [1]</TD>
            <TD>Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)</TD>
            <TD>We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby universe (z&lt;0.05) and to break down the active galactic nucleus (AGN) host galaxy population by color, stellar mass, and morphology. We find that the black hole growth at luminosities L[OIII]&gt;10^40^erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (10^10^-10^11^M_{sun}_), reside in the green valley of the color-mass diagram and their central black holes have median masses around 10^6.5^M_{sun}_. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while in late-type galaxies, it is preferentially the most massive black holes that are growing. At high-Eddington ratios (L/L_Edd_&gt;0.1), the only population with a substantial fraction of AGNs are the low-mass green valley early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284#1</TD>
            <TD>2012-05-16T12:56:27Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/711/284</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/284</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/711/284 [2]</TD>
            <TD>Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)</TD>
            <TD>We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby universe (z&lt;0.05) and to break down the active galactic nucleus (AGN) host galaxy population by color, stellar mass, and morphology. We find that the black hole growth at luminosities L[OIII]&gt;10^40^erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (10^10^-10^11^M_{sun}_), reside in the green valley of the color-mass diagram and their central black holes have median masses around 10^6.5^M_{sun}_. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while in late-type galaxies, it is preferentially the most massive black holes that are growing. At high-Eddington ratios (L/L_Edd_&gt;0.1), the only population with a substantial fraction of AGNs are the low-mass green valley early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284#2</TD>
            <TD>2012-05-16T12:56:27Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/711/284&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/284</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/711/284 [table3]</TD>
            <TD>Galaxy Zoo: AGN host galaxies (Schawinski+, 2010)</TD>
            <TD>We use data from the Sloan Digital Sky Survey and visual classifications of morphology from the Galaxy Zoo project to study black hole growth in the nearby universe (z&lt;0.05) and to break down the active galactic nucleus (AGN) host galaxy population by color, stellar mass, and morphology. We find that the black hole growth at luminosities L[OIII]&gt;10^40^erg/s in early- and late-type galaxies is fundamentally different. AGN host galaxies as a population have a broad range of stellar masses (10^10^-10^11^M_{sun}_), reside in the green valley of the color-mass diagram and their central black holes have median masses around 10^6.5^M_{sun}_. However, by comparing early- and late-type AGN host galaxies to their non-active counterparts, we find several key differences: in early-type galaxies, it is preferentially the galaxies with the least massive black holes that are growing, while in late-type galaxies, it is preferentially the most massive black holes that are growing. At high-Eddington ratios (L/L_Edd_&gt;0.1), the only population with a substantial fraction of AGNs are the low-mass green valley early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284#table3</TD>
            <TD>2012-05-16T12:56:27Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/711/284</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/711/284&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/711/284</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/389/1924 [1]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#1</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/389/1924</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/389/1924 [2]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#2</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1924 [table1]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#table1</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1924 [table3]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#table3</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1924 [table2]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#table2</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/714/1256 [1]</TD>
            <TD>Far-IR star formation rate indicators (Calzetti+, 2010)</TD>
            <TD>We combine data from two Spitzer Legacy surveys, Local Volume Legacy (LVL; Dale et al. 2009, Cat. J/ApJ/703/517; J. C. Lee et al. 2010AAS...21520205L) and Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al. 2003PASP..115..928K), with the local starburst galaxy sample of the Spitzer MIPS-GTO programs (Engelbracht et al. 2008ApJ...685..678E) and the luminous infrared galaxies (LIRGs) sample of Alonso-Herrero et al. (2006ApJ...650..835A).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256#1</TD>
            <TD>2012-06-10T16:35:12Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/714/1256</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1256</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/714/1256 [2]</TD>
            <TD>Far-IR star formation rate indicators (Calzetti+, 2010)</TD>
            <TD>We combine data from two Spitzer Legacy surveys, Local Volume Legacy (LVL; Dale et al. 2009, Cat. J/ApJ/703/517; J. C. Lee et al. 2010AAS...21520205L) and Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al. 2003PASP..115..928K), with the local starburst galaxy sample of the Spitzer MIPS-GTO programs (Engelbracht et al. 2008ApJ...685..678E) and the luminous infrared galaxies (LIRGs) sample of Alonso-Herrero et al. (2006ApJ...650..835A).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256#2</TD>
            <TD>2012-06-10T16:35:12Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/714/1256&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1256</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/714/1256 [table1]</TD>
            <TD>Far-IR star formation rate indicators (Calzetti+, 2010)</TD>
            <TD>We combine data from two Spitzer Legacy surveys, Local Volume Legacy (LVL; Dale et al. 2009, Cat. J/ApJ/703/517; J. C. Lee et al. 2010AAS...21520205L) and Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al. 2003PASP..115..928K), with the local starburst galaxy sample of the Spitzer MIPS-GTO programs (Engelbracht et al. 2008ApJ...685..678E) and the luminous infrared galaxies (LIRGs) sample of Alonso-Herrero et al. (2006ApJ...650..835A).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256#table1</TD>
            <TD>2012-06-10T16:35:12Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/714/1256&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1256</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/714/1256 [1]</TD>
            <TD>Far-IR star formation rate indicators (Calzetti+, 2010)</TD>
            <TD>We combine data from two Spitzer Legacy surveys, Local Volume Legacy (LVL; Dale et al. 2009, Cat. J/ApJ/703/517; J. C. Lee et al. 2010AAS...21520205L) and Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al. 2003PASP..115..928K), with the local starburst galaxy sample of the Spitzer MIPS-GTO programs (Engelbracht et al. 2008ApJ...685..678E) and the luminous infrared galaxies (LIRGs) sample of Alonso-Herrero et al. (2006ApJ...650..835A).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256#1</TD>
            <TD>2012-06-10T16:35:12Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/714/1256</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1256</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/714/1256 [2]</TD>
            <TD>Far-IR star formation rate indicators (Calzetti+, 2010)</TD>
            <TD>We combine data from two Spitzer Legacy surveys, Local Volume Legacy (LVL; Dale et al. 2009, Cat. J/ApJ/703/517; J. C. Lee et al. 2010AAS...21520205L) and Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al. 2003PASP..115..928K), with the local starburst galaxy sample of the Spitzer MIPS-GTO programs (Engelbracht et al. 2008ApJ...685..678E) and the luminous infrared galaxies (LIRGs) sample of Alonso-Herrero et al. (2006ApJ...650..835A).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256#2</TD>
            <TD>2012-06-10T16:35:12Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/714/1256&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1256</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/714/1256 [table1]</TD>
            <TD>Far-IR star formation rate indicators (Calzetti+, 2010)</TD>
            <TD>We combine data from two Spitzer Legacy surveys, Local Volume Legacy (LVL; Dale et al. 2009, Cat. J/ApJ/703/517; J. C. Lee et al. 2010AAS...21520205L) and Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al. 2003PASP..115..928K), with the local starburst galaxy sample of the Spitzer MIPS-GTO programs (Engelbracht et al. 2008ApJ...685..678E) and the luminous infrared galaxies (LIRGs) sample of Alonso-Herrero et al. (2006ApJ...650..835A).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256#table1</TD>
            <TD>2012-06-10T16:35:12Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/714/1256&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1256</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/143/73 [1]</TD>
            <TD>Morphology of spiral galaxies (Eskridge+, 2002)</TD>
            <TD>We announce the initial release of data from the Ohio State University (OSU) Bright Spiral Galaxy Survey (OSUBSGS), a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T type earlier in the H band than in the B band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73#1</TD>
            <TD>2011-09-14T19:58:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/143/73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/143/73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/143/73 [2]</TD>
            <TD>Morphology of spiral galaxies (Eskridge+, 2002)</TD>
            <TD>We announce the initial release of data from the Ohio State University (OSU) Bright Spiral Galaxy Survey (OSUBSGS), a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T type earlier in the H band than in the B band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73#2</TD>
            <TD>2011-09-14T19:58:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/143/73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/143/73</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/143/73 [table1]</TD>
            <TD>Morphology of spiral galaxies (Eskridge+, 2002)</TD>
            <TD>We announce the initial release of data from the Ohio State University (OSU) Bright Spiral Galaxy Survey (OSUBSGS), a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T type earlier in the H band than in the B band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73#table1</TD>
            <TD>2011-09-14T19:58:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/143/73&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/143/73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/389/1924 [1]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#1</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/389/1924</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/389/1924 [2]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#2</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1924 [table1]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#table1</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1924 [table3]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#table3</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1924 [table2]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#table2</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/143/73 [1]</TD>
            <TD>Morphology of spiral galaxies (Eskridge+, 2002)</TD>
            <TD>We announce the initial release of data from the Ohio State University (OSU) Bright Spiral Galaxy Survey (OSUBSGS), a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T type earlier in the H band than in the B band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73#1</TD>
            <TD>2011-09-14T19:58:08Z</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/143/73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/143/73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/143/73 [2]</TD>
            <TD>Morphology of spiral galaxies (Eskridge+, 2002)</TD>
            <TD>We announce the initial release of data from the Ohio State University (OSU) Bright Spiral Galaxy Survey (OSUBSGS), a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T type earlier in the H band than in the B band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73#2</TD>
            <TD>2011-09-14T19:58:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/143/73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/143/73</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/143/73 [table1]</TD>
            <TD>Morphology of spiral galaxies (Eskridge+, 2002)</TD>
            <TD>We announce the initial release of data from the Ohio State University (OSU) Bright Spiral Galaxy Survey (OSUBSGS), a BVRJHK imaging survey of a well-defined sample of 205 bright, nearby spiral galaxies. We present H-band morphological classification on the Hubble sequence for the OSU Survey sample. We compare the H-band classification to B-band classification from our own images and from standard galaxy catalogs. Our B-band classifications match well with those of the standard catalogs. On average, galaxies with optical classifications from Sa through Scd appear about one T type earlier in the H band than in the B band, but with large scatter. This result does not support recent claims made in the literature that the optical and near-IR morphologies of spiral galaxies are uncorrelated. We present detailed descriptions of the H-band morphologies of our entire sample, as well as B- and H-band images for a set of 17 galaxies chosen as type examples and BRH color-composite images of six galaxies chosen to demonstrate the range in morphological variation as a function of wavelength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73#table1</TD>
            <TD>2011-09-14T19:58:08Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/143/73</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/143/73&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/143/73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/389/1924 [1]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#1</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/389/1924</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/389/1924 [2]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#2</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1924 [table1]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#table1</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1924 [table3]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#table3</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1924 [table2]</TD>
            <TD>Old stellar systems (globulars to ellipticals) (Forbes+, 2008)</TD>
            <TD>Elliptical galaxies and globular clusters (GCs) have traditionally been regarded as physically distinct entities due to their discontinuous distribution in key scaling diagrams involving size, luminosity and velocity dispersion. Recently this distinctness has been challenged by the discovery of stellar systems with mass intermediate between those of GCs and dwarf ellipticals (such as ultracompact dwarfs and dwarf galaxy transition objects). Here we examine the relationship between the virial and stellar mass for a range of old stellar systems, from GCs to giant ellipticals, and including such intermediate-mass objects (IMOs). Improvements on previous work in this area include the use of (i) near-infrared magnitudes from the Two Micron All Sky Survey (2MASS), (ii) aperture corrections to velocity dispersions, (iii) homogeneous half-light radii and (iv) accounting for the effects of non-homology in galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924#table2</TD>
            <TD>2011-09-14T21:15:30Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1924</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1924&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1924</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/840 [1]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#1</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/840 [2]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#2</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/840 [table4]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#table4</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/840 [table3]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#table3</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/840 [table2]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#table2</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/688/237 [1]</TD>
            <TD>Disk corrugations in IC 2233 (Matthews+, 2008)</TD>
            <TD>We recently reported the discovery of a regular corrugation pattern in the HI disk of the isolated, edge-on spiral galaxy IC 2233. Here we present measurements of the vertical structure of this galaxy at several additional wavelengths, ranging from the far-ultraviolet to the far-infrared. We find that undular patterns with amplitude &lt;~5"(&lt;~250pc) are visible in a variety of Population I tracers in IC 2233, including the young to intermediate-age stars, the HII regions, and the dust. However, the vertical excursions become less pronounced in the older stellar populations traced by the mid-infrared light. This suggests that the process leading to the vertical displacements may be linked with the regulation of star formation in the galaxy. We have also identified a relationship between the locations of the density corrugations and small-amplitude (&lt;~5km/s) velocity undulations in the HI rotation curve. We are able to exclude several possible mechanisms for the origin of the observed corrugations, including tidal interaction from a companion, Parker instabilities, or a galactic bore. Global gravitational instabilities appear to be the most likely explanation, although local perturbations may also be important.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/688/237#1</TD>
            <TD>2011-09-14T21:16:02Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/688/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/688/237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/688/237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/688/237 [2]</TD>
            <TD>Disk corrugations in IC 2233 (Matthews+, 2008)</TD>
            <TD>We recently reported the discovery of a regular corrugation pattern in the HI disk of the isolated, edge-on spiral galaxy IC 2233. Here we present measurements of the vertical structure of this galaxy at several additional wavelengths, ranging from the far-ultraviolet to the far-infrared. We find that undular patterns with amplitude &lt;~5"(&lt;~250pc) are visible in a variety of Population I tracers in IC 2233, including the young to intermediate-age stars, the HII regions, and the dust. However, the vertical excursions become less pronounced in the older stellar populations traced by the mid-infrared light. This suggests that the process leading to the vertical displacements may be linked with the regulation of star formation in the galaxy. We have also identified a relationship between the locations of the density corrugations and small-amplitude (&lt;~5km/s) velocity undulations in the HI rotation curve. We are able to exclude several possible mechanisms for the origin of the observed corrugations, including tidal interaction from a companion, Parker instabilities, or a galactic bore. Global gravitational instabilities appear to be the most likely explanation, although local perturbations may also be important.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/688/237#2</TD>
            <TD>2011-09-14T21:16:02Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/688/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/688/237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/688/237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/840 [1]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#1</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/840 [2]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#2</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/840 [table4]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#table4</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/840 [table3]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#table3</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/840 [table2]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#table2</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/688/237 [1]</TD>
            <TD>Disk corrugations in IC 2233 (Matthews+, 2008)</TD>
            <TD>We recently reported the discovery of a regular corrugation pattern in the HI disk of the isolated, edge-on spiral galaxy IC 2233. Here we present measurements of the vertical structure of this galaxy at several additional wavelengths, ranging from the far-ultraviolet to the far-infrared. We find that undular patterns with amplitude &lt;~5"(&lt;~250pc) are visible in a variety of Population I tracers in IC 2233, including the young to intermediate-age stars, the HII regions, and the dust. However, the vertical excursions become less pronounced in the older stellar populations traced by the mid-infrared light. This suggests that the process leading to the vertical displacements may be linked with the regulation of star formation in the galaxy. We have also identified a relationship between the locations of the density corrugations and small-amplitude (&lt;~5km/s) velocity undulations in the HI rotation curve. We are able to exclude several possible mechanisms for the origin of the observed corrugations, including tidal interaction from a companion, Parker instabilities, or a galactic bore. Global gravitational instabilities appear to be the most likely explanation, although local perturbations may also be important.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/688/237#1</TD>
            <TD>2011-09-14T21:16:02Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/688/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/688/237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/688/237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/688/237 [2]</TD>
            <TD>Disk corrugations in IC 2233 (Matthews+, 2008)</TD>
            <TD>We recently reported the discovery of a regular corrugation pattern in the HI disk of the isolated, edge-on spiral galaxy IC 2233. Here we present measurements of the vertical structure of this galaxy at several additional wavelengths, ranging from the far-ultraviolet to the far-infrared. We find that undular patterns with amplitude &lt;~5"(&lt;~250pc) are visible in a variety of Population I tracers in IC 2233, including the young to intermediate-age stars, the HII regions, and the dust. However, the vertical excursions become less pronounced in the older stellar populations traced by the mid-infrared light. This suggests that the process leading to the vertical displacements may be linked with the regulation of star formation in the galaxy. We have also identified a relationship between the locations of the density corrugations and small-amplitude (&lt;~5km/s) velocity undulations in the HI rotation curve. We are able to exclude several possible mechanisms for the origin of the observed corrugations, including tidal interaction from a companion, Parker instabilities, or a galactic bore. Global gravitational instabilities appear to be the most likely explanation, although local perturbations may also be important.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/688/237#2</TD>
            <TD>2011-09-14T21:16:02Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/688/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/688/237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/688/237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/840 [1]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#1</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/840 [2]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#2</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/840 [table4]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#table4</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/840 [table3]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#table3</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/840 [table2]</TD>
            <TD>VI photometry of variable stars in Fornax (Bersier+, 2002)</TD>
            <TD>We present a search for variable stars in the Fornax dwarf galaxy covering an area of half a square degree. We have ~30 epochs of VI data. We found and determined periods for more than 500 RR Lyrae, 17 anomalous Cepheids, and six Population II Cepheids. In addition we have 85 candidate long-period variables, the majority of which were previously unknown. We estimate that the average metal abundance of RR Lyrae stars is [Fe/H]~=-1.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840#table2</TD>
            <TD>2011-09-14T19:58:38Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/675/1002 [1]</TD>
            <TD>Proximate damped Ly{alpha} systems in SDSS-DR5 (Prochaska+, 2008)</TD>
            <TD>Using the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5), we survey proximate damped Ly{alpha} systems (PDLAs): absorption-line systems with HI column density N_H_&gt;=2x10^20^cm^-2^ at velocity separation {delta}v&lt;2999km/s from their background quasar. Many of these absorbers may be physically associated with their background quasars, and their statistics allow us to study quasar environments out to z~5. However, the large ionizing flux emitted by a quasar can ionize the neutral gas in a nearby galaxy, possibly giving rise to a "proximity effect", analogous to the similar effect observed in the Ly{alpha} forest. From a sample of 108 PDLAs, we measure the HI frequency distribution f(N_H_,X) incidence, and gas mass density of the PDLAs near luminous quasars over the redshift interval z=2.2-5. The incidence and mass density of PDLAs at z~3 is approximately twice that of intervening DLAs, while at z&lt;2.5 and &gt;3.5 the f(N_H_X) distribution is enhanced but statistically consistent with the intervening population. We interpret the observed enhancement of PDLAs around quasars in terms of quasar-galaxy clustering and compare the strength of the clustering signal to the expectation from independent measures of the respective clustering strengths of DLAs and quasars, as well as a complementary analysis of the clustering of absorbers around quasars in the transverse direction. We find that there are a factor of 5-10 fewer PDLAs around quasars than expected and interpret this result as evidence for the hypothesis that the ionizing flux from the quasars photoevaporates HI in nearby DLA galaxies, thus reducing their cross section for DLA absorption. This constitutes the first detection of a "proximity effect" for DLAs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002#1</TD>
            <TD>2011-09-14T21:16:19Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/675/1002</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1002</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/675/1002 [2]</TD>
            <TD>Proximate damped Ly{alpha} systems in SDSS-DR5 (Prochaska+, 2008)</TD>
            <TD>Using the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5), we survey proximate damped Ly{alpha} systems (PDLAs): absorption-line systems with HI column density N_H_&gt;=2x10^20^cm^-2^ at velocity separation {delta}v&lt;2999km/s from their background quasar. Many of these absorbers may be physically associated with their background quasars, and their statistics allow us to study quasar environments out to z~5. However, the large ionizing flux emitted by a quasar can ionize the neutral gas in a nearby galaxy, possibly giving rise to a "proximity effect", analogous to the similar effect observed in the Ly{alpha} forest. From a sample of 108 PDLAs, we measure the HI frequency distribution f(N_H_,X) incidence, and gas mass density of the PDLAs near luminous quasars over the redshift interval z=2.2-5. The incidence and mass density of PDLAs at z~3 is approximately twice that of intervening DLAs, while at z&lt;2.5 and &gt;3.5 the f(N_H_X) distribution is enhanced but statistically consistent with the intervening population. We interpret the observed enhancement of PDLAs around quasars in terms of quasar-galaxy clustering and compare the strength of the clustering signal to the expectation from independent measures of the respective clustering strengths of DLAs and quasars, as well as a complementary analysis of the clustering of absorbers around quasars in the transverse direction. We find that there are a factor of 5-10 fewer PDLAs around quasars than expected and interpret this result as evidence for the hypothesis that the ionizing flux from the quasars photoevaporates HI in nearby DLA galaxies, thus reducing their cross section for DLA absorption. This constitutes the first detection of a "proximity effect" for DLAs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002#2</TD>
            <TD>2011-09-14T21:16:19Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/675/1002&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1002</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/675/1002 [table1]</TD>
            <TD>Proximate damped Ly{alpha} systems in SDSS-DR5 (Prochaska+, 2008)</TD>
            <TD>Using the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5), we survey proximate damped Ly{alpha} systems (PDLAs): absorption-line systems with HI column density N_H_&gt;=2x10^20^cm^-2^ at velocity separation {delta}v&lt;2999km/s from their background quasar. Many of these absorbers may be physically associated with their background quasars, and their statistics allow us to study quasar environments out to z~5. However, the large ionizing flux emitted by a quasar can ionize the neutral gas in a nearby galaxy, possibly giving rise to a "proximity effect", analogous to the similar effect observed in the Ly{alpha} forest. From a sample of 108 PDLAs, we measure the HI frequency distribution f(N_H_,X) incidence, and gas mass density of the PDLAs near luminous quasars over the redshift interval z=2.2-5. The incidence and mass density of PDLAs at z~3 is approximately twice that of intervening DLAs, while at z&lt;2.5 and &gt;3.5 the f(N_H_X) distribution is enhanced but statistically consistent with the intervening population. We interpret the observed enhancement of PDLAs around quasars in terms of quasar-galaxy clustering and compare the strength of the clustering signal to the expectation from independent measures of the respective clustering strengths of DLAs and quasars, as well as a complementary analysis of the clustering of absorbers around quasars in the transverse direction. We find that there are a factor of 5-10 fewer PDLAs around quasars than expected and interpret this result as evidence for the hypothesis that the ionizing flux from the quasars photoevaporates HI in nearby DLA galaxies, thus reducing their cross section for DLA absorption. This constitutes the first detection of a "proximity effect" for DLAs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002#table1</TD>
            <TD>2011-09-14T21:16:19Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/675/1002&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1002</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/675/1002 [1]</TD>
            <TD>Proximate damped Ly{alpha} systems in SDSS-DR5 (Prochaska+, 2008)</TD>
            <TD>Using the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5), we survey proximate damped Ly{alpha} systems (PDLAs): absorption-line systems with HI column density N_H_&gt;=2x10^20^cm^-2^ at velocity separation {delta}v&lt;2999km/s from their background quasar. Many of these absorbers may be physically associated with their background quasars, and their statistics allow us to study quasar environments out to z~5. However, the large ionizing flux emitted by a quasar can ionize the neutral gas in a nearby galaxy, possibly giving rise to a "proximity effect", analogous to the similar effect observed in the Ly{alpha} forest. From a sample of 108 PDLAs, we measure the HI frequency distribution f(N_H_,X) incidence, and gas mass density of the PDLAs near luminous quasars over the redshift interval z=2.2-5. The incidence and mass density of PDLAs at z~3 is approximately twice that of intervening DLAs, while at z&lt;2.5 and &gt;3.5 the f(N_H_X) distribution is enhanced but statistically consistent with the intervening population. We interpret the observed enhancement of PDLAs around quasars in terms of quasar-galaxy clustering and compare the strength of the clustering signal to the expectation from independent measures of the respective clustering strengths of DLAs and quasars, as well as a complementary analysis of the clustering of absorbers around quasars in the transverse direction. We find that there are a factor of 5-10 fewer PDLAs around quasars than expected and interpret this result as evidence for the hypothesis that the ionizing flux from the quasars photoevaporates HI in nearby DLA galaxies, thus reducing their cross section for DLA absorption. This constitutes the first detection of a "proximity effect" for DLAs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002#1</TD>
            <TD>2011-09-14T21:16:19Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/675/1002</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1002</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/675/1002 [2]</TD>
            <TD>Proximate damped Ly{alpha} systems in SDSS-DR5 (Prochaska+, 2008)</TD>
            <TD>Using the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5), we survey proximate damped Ly{alpha} systems (PDLAs): absorption-line systems with HI column density N_H_&gt;=2x10^20^cm^-2^ at velocity separation {delta}v&lt;2999km/s from their background quasar. Many of these absorbers may be physically associated with their background quasars, and their statistics allow us to study quasar environments out to z~5. However, the large ionizing flux emitted by a quasar can ionize the neutral gas in a nearby galaxy, possibly giving rise to a "proximity effect", analogous to the similar effect observed in the Ly{alpha} forest. From a sample of 108 PDLAs, we measure the HI frequency distribution f(N_H_,X) incidence, and gas mass density of the PDLAs near luminous quasars over the redshift interval z=2.2-5. The incidence and mass density of PDLAs at z~3 is approximately twice that of intervening DLAs, while at z&lt;2.5 and &gt;3.5 the f(N_H_X) distribution is enhanced but statistically consistent with the intervening population. We interpret the observed enhancement of PDLAs around quasars in terms of quasar-galaxy clustering and compare the strength of the clustering signal to the expectation from independent measures of the respective clustering strengths of DLAs and quasars, as well as a complementary analysis of the clustering of absorbers around quasars in the transverse direction. We find that there are a factor of 5-10 fewer PDLAs around quasars than expected and interpret this result as evidence for the hypothesis that the ionizing flux from the quasars photoevaporates HI in nearby DLA galaxies, thus reducing their cross section for DLA absorption. This constitutes the first detection of a "proximity effect" for DLAs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002#2</TD>
            <TD>2011-09-14T21:16:19Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/675/1002&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1002</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/675/1002 [table1]</TD>
            <TD>Proximate damped Ly{alpha} systems in SDSS-DR5 (Prochaska+, 2008)</TD>
            <TD>Using the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5), we survey proximate damped Ly{alpha} systems (PDLAs): absorption-line systems with HI column density N_H_&gt;=2x10^20^cm^-2^ at velocity separation {delta}v&lt;2999km/s from their background quasar. Many of these absorbers may be physically associated with their background quasars, and their statistics allow us to study quasar environments out to z~5. However, the large ionizing flux emitted by a quasar can ionize the neutral gas in a nearby galaxy, possibly giving rise to a "proximity effect", analogous to the similar effect observed in the Ly{alpha} forest. From a sample of 108 PDLAs, we measure the HI frequency distribution f(N_H_,X) incidence, and gas mass density of the PDLAs near luminous quasars over the redshift interval z=2.2-5. The incidence and mass density of PDLAs at z~3 is approximately twice that of intervening DLAs, while at z&lt;2.5 and &gt;3.5 the f(N_H_X) distribution is enhanced but statistically consistent with the intervening population. We interpret the observed enhancement of PDLAs around quasars in terms of quasar-galaxy clustering and compare the strength of the clustering signal to the expectation from independent measures of the respective clustering strengths of DLAs and quasars, as well as a complementary analysis of the clustering of absorbers around quasars in the transverse direction. We find that there are a factor of 5-10 fewer PDLAs around quasars than expected and interpret this result as evidence for the hypothesis that the ionizing flux from the quasars photoevaporates HI in nearby DLA galaxies, thus reducing their cross section for DLA absorption. This constitutes the first detection of a "proximity effect" for DLAs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002#table1</TD>
            <TD>2011-09-14T21:16:19Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/675/1002&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1002</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/442/841 [1]</TD>
            <TD>High-redshift galaxy clusters (Olsen+, 2005)</TD>
            <TD>The observations were carried out in the nights September 21-25, 2000, using FORS1 mounted at the VLT-ANTU telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841#1</TD>
            <TD>2011-09-14T19:58:54Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/442/841</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/841</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/442/841 [2]</TD>
            <TD>High-redshift galaxy clusters (Olsen+, 2005)</TD>
            <TD>The observations were carried out in the nights September 21-25, 2000, using FORS1 mounted at the VLT-ANTU telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841#2</TD>
            <TD>2011-09-14T19:58:54Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/442/841&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/841</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/442/841 [tablea]</TD>
            <TD>High-redshift galaxy clusters (Olsen+, 2005)</TD>
            <TD>The observations were carried out in the nights September 21-25, 2000, using FORS1 mounted at the VLT-ANTU telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841#tablea</TD>
            <TD>2011-09-14T19:58:54Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/442/841&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/841</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/675/1002 [1]</TD>
            <TD>Proximate damped Ly{alpha} systems in SDSS-DR5 (Prochaska+, 2008)</TD>
            <TD>Using the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5), we survey proximate damped Ly{alpha} systems (PDLAs): absorption-line systems with HI column density N_H_&gt;=2x10^20^cm^-2^ at velocity separation {delta}v&lt;2999km/s from their background quasar. Many of these absorbers may be physically associated with their background quasars, and their statistics allow us to study quasar environments out to z~5. However, the large ionizing flux emitted by a quasar can ionize the neutral gas in a nearby galaxy, possibly giving rise to a "proximity effect", analogous to the similar effect observed in the Ly{alpha} forest. From a sample of 108 PDLAs, we measure the HI frequency distribution f(N_H_,X) incidence, and gas mass density of the PDLAs near luminous quasars over the redshift interval z=2.2-5. The incidence and mass density of PDLAs at z~3 is approximately twice that of intervening DLAs, while at z&lt;2.5 and &gt;3.5 the f(N_H_X) distribution is enhanced but statistically consistent with the intervening population. We interpret the observed enhancement of PDLAs around quasars in terms of quasar-galaxy clustering and compare the strength of the clustering signal to the expectation from independent measures of the respective clustering strengths of DLAs and quasars, as well as a complementary analysis of the clustering of absorbers around quasars in the transverse direction. We find that there are a factor of 5-10 fewer PDLAs around quasars than expected and interpret this result as evidence for the hypothesis that the ionizing flux from the quasars photoevaporates HI in nearby DLA galaxies, thus reducing their cross section for DLA absorption. This constitutes the first detection of a "proximity effect" for DLAs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002#1</TD>
            <TD>2011-09-14T21:16:19Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/675/1002</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1002</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/675/1002 [2]</TD>
            <TD>Proximate damped Ly{alpha} systems in SDSS-DR5 (Prochaska+, 2008)</TD>
            <TD>Using the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5), we survey proximate damped Ly{alpha} systems (PDLAs): absorption-line systems with HI column density N_H_&gt;=2x10^20^cm^-2^ at velocity separation {delta}v&lt;2999km/s from their background quasar. Many of these absorbers may be physically associated with their background quasars, and their statistics allow us to study quasar environments out to z~5. However, the large ionizing flux emitted by a quasar can ionize the neutral gas in a nearby galaxy, possibly giving rise to a "proximity effect", analogous to the similar effect observed in the Ly{alpha} forest. From a sample of 108 PDLAs, we measure the HI frequency distribution f(N_H_,X) incidence, and gas mass density of the PDLAs near luminous quasars over the redshift interval z=2.2-5. The incidence and mass density of PDLAs at z~3 is approximately twice that of intervening DLAs, while at z&lt;2.5 and &gt;3.5 the f(N_H_X) distribution is enhanced but statistically consistent with the intervening population. We interpret the observed enhancement of PDLAs around quasars in terms of quasar-galaxy clustering and compare the strength of the clustering signal to the expectation from independent measures of the respective clustering strengths of DLAs and quasars, as well as a complementary analysis of the clustering of absorbers around quasars in the transverse direction. We find that there are a factor of 5-10 fewer PDLAs around quasars than expected and interpret this result as evidence for the hypothesis that the ionizing flux from the quasars photoevaporates HI in nearby DLA galaxies, thus reducing their cross section for DLA absorption. This constitutes the first detection of a "proximity effect" for DLAs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002#2</TD>
            <TD>2011-09-14T21:16:19Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/675/1002&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1002</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/675/1002 [table1]</TD>
            <TD>Proximate damped Ly{alpha} systems in SDSS-DR5 (Prochaska+, 2008)</TD>
            <TD>Using the Sloan Digital Sky Survey Data Release 5 (SDSS-DR5), we survey proximate damped Ly{alpha} systems (PDLAs): absorption-line systems with HI column density N_H_&gt;=2x10^20^cm^-2^ at velocity separation {delta}v&lt;2999km/s from their background quasar. Many of these absorbers may be physically associated with their background quasars, and their statistics allow us to study quasar environments out to z~5. However, the large ionizing flux emitted by a quasar can ionize the neutral gas in a nearby galaxy, possibly giving rise to a "proximity effect", analogous to the similar effect observed in the Ly{alpha} forest. From a sample of 108 PDLAs, we measure the HI frequency distribution f(N_H_,X) incidence, and gas mass density of the PDLAs near luminous quasars over the redshift interval z=2.2-5. The incidence and mass density of PDLAs at z~3 is approximately twice that of intervening DLAs, while at z&lt;2.5 and &gt;3.5 the f(N_H_X) distribution is enhanced but statistically consistent with the intervening population. We interpret the observed enhancement of PDLAs around quasars in terms of quasar-galaxy clustering and compare the strength of the clustering signal to the expectation from independent measures of the respective clustering strengths of DLAs and quasars, as well as a complementary analysis of the clustering of absorbers around quasars in the transverse direction. We find that there are a factor of 5-10 fewer PDLAs around quasars than expected and interpret this result as evidence for the hypothesis that the ionizing flux from the quasars photoevaporates HI in nearby DLA galaxies, thus reducing their cross section for DLA absorption. This constitutes the first detection of a "proximity effect" for DLAs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002#table1</TD>
            <TD>2011-09-14T21:16:19Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1002</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/675/1002&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1002</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/714/1256 [1]</TD>
            <TD>Far-IR star formation rate indicators (Calzetti+, 2010)</TD>
            <TD>We combine data from two Spitzer Legacy surveys, Local Volume Legacy (LVL; Dale et al. 2009, Cat. J/ApJ/703/517; J. C. Lee et al. 2010AAS...21520205L) and Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al. 2003PASP..115..928K), with the local starburst galaxy sample of the Spitzer MIPS-GTO programs (Engelbracht et al. 2008ApJ...685..678E) and the luminous infrared galaxies (LIRGs) sample of Alonso-Herrero et al. (2006ApJ...650..835A).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256#1</TD>
            <TD>2012-06-10T16:35:12Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/714/1256</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1256</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/714/1256 [2]</TD>
            <TD>Far-IR star formation rate indicators (Calzetti+, 2010)</TD>
            <TD>We combine data from two Spitzer Legacy surveys, Local Volume Legacy (LVL; Dale et al. 2009, Cat. J/ApJ/703/517; J. C. Lee et al. 2010AAS...21520205L) and Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al. 2003PASP..115..928K), with the local starburst galaxy sample of the Spitzer MIPS-GTO programs (Engelbracht et al. 2008ApJ...685..678E) and the luminous infrared galaxies (LIRGs) sample of Alonso-Herrero et al. (2006ApJ...650..835A).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256#2</TD>
            <TD>2012-06-10T16:35:12Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/714/1256&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1256</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/714/1256 [table1]</TD>
            <TD>Far-IR star formation rate indicators (Calzetti+, 2010)</TD>
            <TD>We combine data from two Spitzer Legacy surveys, Local Volume Legacy (LVL; Dale et al. 2009, Cat. J/ApJ/703/517; J. C. Lee et al. 2010AAS...21520205L) and Spitzer Infrared Nearby Galaxies Survey (SINGS; Kennicutt et al. 2003PASP..115..928K), with the local starburst galaxy sample of the Spitzer MIPS-GTO programs (Engelbracht et al. 2008ApJ...685..678E) and the luminous infrared galaxies (LIRGs) sample of Alonso-Herrero et al. (2006ApJ...650..835A).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256#table1</TD>
            <TD>2012-06-10T16:35:12Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/1256</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/714/1256&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/1256</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/257 [1]</TD>
            <TD>2MASS-selected Isolated Galaxies (2MIG) (Karachentseva+, 2010)</TD>
            <TD>We undertook searches for isolated galaxies based on automatic selection of infrared sources from the Two Micron All-Sky Survey (2MASS, Cat. II/246) followed by a visual inspection of their surrounding. Using a modified criterion by Karachentseva (1973SoSAO...8....3K), we compiled a catalog of 3227 isolated galaxies (2MIG) containing 6% of 2MASS Extended Sources (2MASX, Cat. VII/233) brighter than K_s_=12mag with angular diameters a_K_&lt;=30". The most isolated 2493 galaxies among them enter in the 2MASS Very Isolated Galaxy Catalog, 2MVIG. Being situated in the regions of extremely low mass density, the 2MVIG galaxies can serve as a reference sample for investigation the influence of environment on structure and evolution of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/257#1</TD>
            <TD>2011-09-14T21:16:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/VII/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/257</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/257</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/257 [2]</TD>
            <TD>2MASS-selected Isolated Galaxies (2MIG) (Karachentseva+, 2010)</TD>
            <TD>We undertook searches for isolated galaxies based on automatic selection of infrared sources from the Two Micron All-Sky Survey (2MASS, Cat. II/246) followed by a visual inspection of their surrounding. Using a modified criterion by Karachentseva (1973SoSAO...8....3K), we compiled a catalog of 3227 isolated galaxies (2MIG) containing 6% of 2MASS Extended Sources (2MASX, Cat. VII/233) brighter than K_s_=12mag with angular diameters a_K_&lt;=30". The most isolated 2493 galaxies among them enter in the 2MASS Very Isolated Galaxy Catalog, 2MVIG. Being situated in the regions of extremely low mass density, the 2MVIG galaxies can serve as a reference sample for investigation the influence of environment on structure and evolution of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/257#2</TD>
            <TD>2011-09-14T21:16:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/VII/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/257&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/257</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/257 [2mig]</TD>
            <TD>2MASS-selected Isolated Galaxies (2MIG) (Karachentseva+, 2010)</TD>
            <TD>We undertook searches for isolated galaxies based on automatic selection of infrared sources from the Two Micron All-Sky Survey (2MASS, Cat. II/246) followed by a visual inspection of their surrounding. Using a modified criterion by Karachentseva (1973SoSAO...8....3K), we compiled a catalog of 3227 isolated galaxies (2MIG) containing 6% of 2MASS Extended Sources (2MASX, Cat. VII/233) brighter than K_s_=12mag with angular diameters a_K_&lt;=30". The most isolated 2493 galaxies among them enter in the 2MASS Very Isolated Galaxy Catalog, 2MVIG. Being situated in the regions of extremely low mass density, the 2MVIG galaxies can serve as a reference sample for investigation the influence of environment on structure and evolution of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/257#2mig</TD>
            <TD>2011-09-14T21:16:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/VII/257</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/257&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/257</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/257 [1]</TD>
            <TD>2MASS-selected Isolated Galaxies (2MIG) (Karachentseva+, 2010)</TD>
            <TD>We undertook searches for isolated galaxies based on automatic selection of infrared sources from the Two Micron All-Sky Survey (2MASS, Cat. II/246) followed by a visual inspection of their surrounding. Using a modified criterion by Karachentseva (1973SoSAO...8....3K), we compiled a catalog of 3227 isolated galaxies (2MIG) containing 6% of 2MASS Extended Sources (2MASX, Cat. VII/233) brighter than K_s_=12mag with angular diameters a_K_&lt;=30". The most isolated 2493 galaxies among them enter in the 2MASS Very Isolated Galaxy Catalog, 2MVIG. Being situated in the regions of extremely low mass density, the 2MVIG galaxies can serve as a reference sample for investigation the influence of environment on structure and evolution of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/257#1</TD>
            <TD>2011-09-14T21:16:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/VII/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/257</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/257</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/257 [2]</TD>
            <TD>2MASS-selected Isolated Galaxies (2MIG) (Karachentseva+, 2010)</TD>
            <TD>We undertook searches for isolated galaxies based on automatic selection of infrared sources from the Two Micron All-Sky Survey (2MASS, Cat. II/246) followed by a visual inspection of their surrounding. Using a modified criterion by Karachentseva (1973SoSAO...8....3K), we compiled a catalog of 3227 isolated galaxies (2MIG) containing 6% of 2MASS Extended Sources (2MASX, Cat. VII/233) brighter than K_s_=12mag with angular diameters a_K_&lt;=30". The most isolated 2493 galaxies among them enter in the 2MASS Very Isolated Galaxy Catalog, 2MVIG. Being situated in the regions of extremely low mass density, the 2MVIG galaxies can serve as a reference sample for investigation the influence of environment on structure and evolution of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/257#2</TD>
            <TD>2011-09-14T21:16:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/VII/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/257&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/257</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/257 [2mig]</TD>
            <TD>2MASS-selected Isolated Galaxies (2MIG) (Karachentseva+, 2010)</TD>
            <TD>We undertook searches for isolated galaxies based on automatic selection of infrared sources from the Two Micron All-Sky Survey (2MASS, Cat. II/246) followed by a visual inspection of their surrounding. Using a modified criterion by Karachentseva (1973SoSAO...8....3K), we compiled a catalog of 3227 isolated galaxies (2MIG) containing 6% of 2MASS Extended Sources (2MASX, Cat. VII/233) brighter than K_s_=12mag with angular diameters a_K_&lt;=30". The most isolated 2493 galaxies among them enter in the 2MASS Very Isolated Galaxy Catalog, 2MVIG. Being situated in the regions of extremely low mass density, the 2MVIG galaxies can serve as a reference sample for investigation the influence of environment on structure and evolution of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/257#2mig</TD>
            <TD>2011-09-14T21:16:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/VII/257</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/257&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/257</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE143 [1]</TD>
            <TD>Planck Early Release 143-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 143-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke143#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke143&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke143.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE143 [2]</TD>
            <TD>Planck Early Release 143-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 143-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke143#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke143.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE143 [3]</TD>
            <TD>Planck Early Release 143-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 143-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke143#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke143&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke143.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/257 [1]</TD>
            <TD>2MASS-selected Isolated Galaxies (2MIG) (Karachentseva+, 2010)</TD>
            <TD>We undertook searches for isolated galaxies based on automatic selection of infrared sources from the Two Micron All-Sky Survey (2MASS, Cat. II/246) followed by a visual inspection of their surrounding. Using a modified criterion by Karachentseva (1973SoSAO...8....3K), we compiled a catalog of 3227 isolated galaxies (2MIG) containing 6% of 2MASS Extended Sources (2MASX, Cat. VII/233) brighter than K_s_=12mag with angular diameters a_K_&lt;=30". The most isolated 2493 galaxies among them enter in the 2MASS Very Isolated Galaxy Catalog, 2MVIG. Being situated in the regions of extremely low mass density, the 2MVIG galaxies can serve as a reference sample for investigation the influence of environment on structure and evolution of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/257#1</TD>
            <TD>2011-09-14T21:16:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/VII/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/257</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/257</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/257 [2]</TD>
            <TD>2MASS-selected Isolated Galaxies (2MIG) (Karachentseva+, 2010)</TD>
            <TD>We undertook searches for isolated galaxies based on automatic selection of infrared sources from the Two Micron All-Sky Survey (2MASS, Cat. II/246) followed by a visual inspection of their surrounding. Using a modified criterion by Karachentseva (1973SoSAO...8....3K), we compiled a catalog of 3227 isolated galaxies (2MIG) containing 6% of 2MASS Extended Sources (2MASX, Cat. VII/233) brighter than K_s_=12mag with angular diameters a_K_&lt;=30". The most isolated 2493 galaxies among them enter in the 2MASS Very Isolated Galaxy Catalog, 2MVIG. Being situated in the regions of extremely low mass density, the 2MVIG galaxies can serve as a reference sample for investigation the influence of environment on structure and evolution of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/257#2</TD>
            <TD>2011-09-14T21:16:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/VII/257</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/257&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/257</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/257 [2mig]</TD>
            <TD>2MASS-selected Isolated Galaxies (2MIG) (Karachentseva+, 2010)</TD>
            <TD>We undertook searches for isolated galaxies based on automatic selection of infrared sources from the Two Micron All-Sky Survey (2MASS, Cat. II/246) followed by a visual inspection of their surrounding. Using a modified criterion by Karachentseva (1973SoSAO...8....3K), we compiled a catalog of 3227 isolated galaxies (2MIG) containing 6% of 2MASS Extended Sources (2MASX, Cat. VII/233) brighter than K_s_=12mag with angular diameters a_K_&lt;=30". The most isolated 2493 galaxies among them enter in the 2MASS Very Isolated Galaxy Catalog, 2MVIG. Being situated in the regions of extremely low mass density, the 2MVIG galaxies can serve as a reference sample for investigation the influence of environment on structure and evolution of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/257#2mig</TD>
            <TD>2011-09-14T21:16:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/VII/257</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/257&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/257</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChandraGC150 [1]</TD>
            <TD>Chandra Galactic Central 150 Parsecs Source Catalog</TD>
            <TD>The Chandra Catalog of X-Ray Sources in the Central 150 Parsecs of the Galaxy lists X-ray sources detected in a shallow Chandra survey of the inner 2 by 0.8 degrees of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (N_H &gt;~ 4 x 10^22 cm^-2) and are therefore likely to lie near the Galactic center (D ~ 8 kpc), and 549 less absorbed sources that lie within &lt;~ 6 kpc of Earth, except that two bright, previously known LMXBs, 1E 1740.7-2942 and 2E 1743.1-2842, have been omitted because they were badly saturated in these survey images, and their positions and properties have been reported elsewhere (Marti et al. 2000, A&amp;A, 363, 184; Porquet et al. 2003, A&amp;A, 406, 299). On the basis of the inferred luminosities of the X-ray sources and the expected numbers of various classes of objects, the authors suggest that the sources with L_X &lt;~ 10^33 ergs s^-1 that comprise ~ 90% of the catalog are cataclysmic variables, and that the ~ 100 brighter objects are accreting neutron stars and black holes, young isolated pulsars, and Wolf-Rayet and O (WR/O) stars in colliding-wind binaries. They find that the spatial distribution of X-ray sources matches that of the old stellar population observed in the infrared, which supports their suggestion that most of the X-ray sources are old cataclysmic variables. However, they find that there is an apparent excess of ~ 10 bright sources in the Radio Arches region. That region is already known to be the site of recent star formation, so they suggest that the bright sources in this region are young high-mass X-ray binaries, pulsars, or WR/O star binaries.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanc150pc#1</TD>
            <TD>2008-12-24T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanc150pc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chanc150pc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanc150pc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChandraGC150 [2]</TD>
            <TD>Chandra Galactic Central 150 Parsecs Source Catalog</TD>
            <TD>The Chandra Catalog of X-Ray Sources in the Central 150 Parsecs of the Galaxy lists X-ray sources detected in a shallow Chandra survey of the inner 2 by 0.8 degrees of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (N_H &gt;~ 4 x 10^22 cm^-2) and are therefore likely to lie near the Galactic center (D ~ 8 kpc), and 549 less absorbed sources that lie within &lt;~ 6 kpc of Earth, except that two bright, previously known LMXBs, 1E 1740.7-2942 and 2E 1743.1-2842, have been omitted because they were badly saturated in these survey images, and their positions and properties have been reported elsewhere (Marti et al. 2000, A&amp;A, 363, 184; Porquet et al. 2003, A&amp;A, 406, 299). On the basis of the inferred luminosities of the X-ray sources and the expected numbers of various classes of objects, the authors suggest that the sources with L_X &lt;~ 10^33 ergs s^-1 that comprise ~ 90% of the catalog are cataclysmic variables, and that the ~ 100 brighter objects are accreting neutron stars and black holes, young isolated pulsars, and Wolf-Rayet and O (WR/O) stars in colliding-wind binaries. They find that the spatial distribution of X-ray sources matches that of the old stellar population observed in the infrared, which supports their suggestion that most of the X-ray sources are old cataclysmic variables. However, they find that there is an apparent excess of ~ 10 bright sources in the Radio Arches region. That region is already known to be the site of recent star formation, so they suggest that the bright sources in this region are young high-mass X-ray binaries, pulsars, or WR/O star binaries.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanc150pc#2</TD>
            <TD>2008-12-24T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanc150pc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chanc150pc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanc150pc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChandraGC150 [3]</TD>
            <TD>Chandra Galactic Central 150 Parsecs Source Catalog</TD>
            <TD>The Chandra Catalog of X-Ray Sources in the Central 150 Parsecs of the Galaxy lists X-ray sources detected in a shallow Chandra survey of the inner 2 by 0.8 degrees of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (N_H &gt;~ 4 x 10^22 cm^-2) and are therefore likely to lie near the Galactic center (D ~ 8 kpc), and 549 less absorbed sources that lie within &lt;~ 6 kpc of Earth, except that two bright, previously known LMXBs, 1E 1740.7-2942 and 2E 1743.1-2842, have been omitted because they were badly saturated in these survey images, and their positions and properties have been reported elsewhere (Marti et al. 2000, A&amp;A, 363, 184; Porquet et al. 2003, A&amp;A, 406, 299). On the basis of the inferred luminosities of the X-ray sources and the expected numbers of various classes of objects, the authors suggest that the sources with L_X &lt;~ 10^33 ergs s^-1 that comprise ~ 90% of the catalog are cataclysmic variables, and that the ~ 100 brighter objects are accreting neutron stars and black holes, young isolated pulsars, and Wolf-Rayet and O (WR/O) stars in colliding-wind binaries. They find that the spatial distribution of X-ray sources matches that of the old stellar population observed in the infrared, which supports their suggestion that most of the X-ray sources are old cataclysmic variables. However, they find that there is an apparent excess of ~ 10 bright sources in the Radio Arches region. That region is already known to be the site of recent star formation, so they suggest that the bright sources in this region are young high-mass X-ray binaries, pulsars, or WR/O star binaries.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanc150pc#3</TD>
            <TD>2008-12-24T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanc150pc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chanc150pc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanc150pc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>HDFN</TD>
            <TD>The Hubble Deep Field North</TD>
            <TD>Hubble Deep Field North Open SkyNode. The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image a typical field at high galactic latitude in four wavelength passbands as deeply as reasonably possible. In order to optimize observing in the time available, a field in the northern continuous viewing zone (CVZ) was selected and images were taken for 10 consecutive days, or approximately 150 orbits. Shorter 1-orbit images were also obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground-based telescopes. The observations were carried out from 18-30 December 1995, and the data are available to the community for study.</TD>
            <TD>STScI</TD>
            <TD>#Optical#</TD>
            <TD>ivo://archive.stsci.edu/hdfn/SKYNODE#1</TD>
            <TD>2011-09-14T18:11:58Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#Hubble#</TD>
            <TD />
            <TD />
            <TD />
            <TD>V1.0</TD>
            <TD>ivo://archive.stsci.edu/hdfn/SKYNODE</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://galex.stsci.edu/skynode/ohdfn/nodeb.asmx</TD>
            <TD />
            <TD>0</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChandraGC150 [1]</TD>
            <TD>Chandra Galactic Central 150 Parsecs Source Catalog</TD>
            <TD>The Chandra Catalog of X-Ray Sources in the Central 150 Parsecs of the Galaxy lists X-ray sources detected in a shallow Chandra survey of the inner 2 by 0.8 degrees of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (N_H &gt;~ 4 x 10^22 cm^-2) and are therefore likely to lie near the Galactic center (D ~ 8 kpc), and 549 less absorbed sources that lie within &lt;~ 6 kpc of Earth, except that two bright, previously known LMXBs, 1E 1740.7-2942 and 2E 1743.1-2842, have been omitted because they were badly saturated in these survey images, and their positions and properties have been reported elsewhere (Marti et al. 2000, A&amp;A, 363, 184; Porquet et al. 2003, A&amp;A, 406, 299). On the basis of the inferred luminosities of the X-ray sources and the expected numbers of various classes of objects, the authors suggest that the sources with L_X &lt;~ 10^33 ergs s^-1 that comprise ~ 90% of the catalog are cataclysmic variables, and that the ~ 100 brighter objects are accreting neutron stars and black holes, young isolated pulsars, and Wolf-Rayet and O (WR/O) stars in colliding-wind binaries. They find that the spatial distribution of X-ray sources matches that of the old stellar population observed in the infrared, which supports their suggestion that most of the X-ray sources are old cataclysmic variables. However, they find that there is an apparent excess of ~ 10 bright sources in the Radio Arches region. That region is already known to be the site of recent star formation, so they suggest that the bright sources in this region are young high-mass X-ray binaries, pulsars, or WR/O star binaries.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanc150pc#1</TD>
            <TD>2008-12-24T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanc150pc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chanc150pc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanc150pc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChandraGC150 [2]</TD>
            <TD>Chandra Galactic Central 150 Parsecs Source Catalog</TD>
            <TD>The Chandra Catalog of X-Ray Sources in the Central 150 Parsecs of the Galaxy lists X-ray sources detected in a shallow Chandra survey of the inner 2 by 0.8 degrees of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (N_H &gt;~ 4 x 10^22 cm^-2) and are therefore likely to lie near the Galactic center (D ~ 8 kpc), and 549 less absorbed sources that lie within &lt;~ 6 kpc of Earth, except that two bright, previously known LMXBs, 1E 1740.7-2942 and 2E 1743.1-2842, have been omitted because they were badly saturated in these survey images, and their positions and properties have been reported elsewhere (Marti et al. 2000, A&amp;A, 363, 184; Porquet et al. 2003, A&amp;A, 406, 299). On the basis of the inferred luminosities of the X-ray sources and the expected numbers of various classes of objects, the authors suggest that the sources with L_X &lt;~ 10^33 ergs s^-1 that comprise ~ 90% of the catalog are cataclysmic variables, and that the ~ 100 brighter objects are accreting neutron stars and black holes, young isolated pulsars, and Wolf-Rayet and O (WR/O) stars in colliding-wind binaries. They find that the spatial distribution of X-ray sources matches that of the old stellar population observed in the infrared, which supports their suggestion that most of the X-ray sources are old cataclysmic variables. However, they find that there is an apparent excess of ~ 10 bright sources in the Radio Arches region. That region is already known to be the site of recent star formation, so they suggest that the bright sources in this region are young high-mass X-ray binaries, pulsars, or WR/O star binaries.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanc150pc#2</TD>
            <TD>2008-12-24T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanc150pc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chanc150pc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanc150pc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChandraGC150 [3]</TD>
            <TD>Chandra Galactic Central 150 Parsecs Source Catalog</TD>
            <TD>The Chandra Catalog of X-Ray Sources in the Central 150 Parsecs of the Galaxy lists X-ray sources detected in a shallow Chandra survey of the inner 2 by 0.8 degrees of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (N_H &gt;~ 4 x 10^22 cm^-2) and are therefore likely to lie near the Galactic center (D ~ 8 kpc), and 549 less absorbed sources that lie within &lt;~ 6 kpc of Earth, except that two bright, previously known LMXBs, 1E 1740.7-2942 and 2E 1743.1-2842, have been omitted because they were badly saturated in these survey images, and their positions and properties have been reported elsewhere (Marti et al. 2000, A&amp;A, 363, 184; Porquet et al. 2003, A&amp;A, 406, 299). On the basis of the inferred luminosities of the X-ray sources and the expected numbers of various classes of objects, the authors suggest that the sources with L_X &lt;~ 10^33 ergs s^-1 that comprise ~ 90% of the catalog are cataclysmic variables, and that the ~ 100 brighter objects are accreting neutron stars and black holes, young isolated pulsars, and Wolf-Rayet and O (WR/O) stars in colliding-wind binaries. They find that the spatial distribution of X-ray sources matches that of the old stellar population observed in the infrared, which supports their suggestion that most of the X-ray sources are old cataclysmic variables. However, they find that there is an apparent excess of ~ 10 bright sources in the Radio Arches region. That region is already known to be the site of recent star formation, so they suggest that the bright sources in this region are young high-mass X-ray binaries, pulsars, or WR/O star binaries.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanc150pc#3</TD>
            <TD>2008-12-24T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanc150pc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chanc150pc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanc150pc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/348/866 [1]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#1</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/348/866</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/348/866 [2]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfsgpgr]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfsgpgr</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfngpga]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfngpga</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfngpgr]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfngpgr</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfsgpga]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfsgpga</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/442/841 [1]</TD>
            <TD>High-redshift galaxy clusters (Olsen+, 2005)</TD>
            <TD>The observations were carried out in the nights September 21-25, 2000, using FORS1 mounted at the VLT-ANTU telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841#1</TD>
            <TD>2011-09-14T19:58:54Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/442/841</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/841</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/442/841 [2]</TD>
            <TD>High-redshift galaxy clusters (Olsen+, 2005)</TD>
            <TD>The observations were carried out in the nights September 21-25, 2000, using FORS1 mounted at the VLT-ANTU telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841#2</TD>
            <TD>2011-09-14T19:58:54Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/442/841&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/841</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/442/841 [tablea]</TD>
            <TD>High-redshift galaxy clusters (Olsen+, 2005)</TD>
            <TD>The observations were carried out in the nights September 21-25, 2000, using FORS1 mounted at the VLT-ANTU telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841#tablea</TD>
            <TD>2011-09-14T19:58:54Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/442/841&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/841</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>USNOB</TD>
            <TD>US Naval Observatory B</TD>
            <TD>The USNO-B1.0 Catalogue presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,175,762 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalogue is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects</TD>
            <TD>US Naval Observatory</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/usnob#1</TD>
            <TD>2011-09-14T18:11:58Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD>1.0</TD>
            <TD>ivo://sdss.jhu/openskynode/usnob</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/usnob/nodeb.asmx</TD>
            <TD />
            <TD>0</TD>
            <TD />
            <TD>http://www.usno.navy.mil/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ChandraGC150 [1]</TD>
            <TD>Chandra Galactic Central 150 Parsecs Source Catalog</TD>
            <TD>The Chandra Catalog of X-Ray Sources in the Central 150 Parsecs of the Galaxy lists X-ray sources detected in a shallow Chandra survey of the inner 2 by 0.8 degrees of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (N_H &gt;~ 4 x 10^22 cm^-2) and are therefore likely to lie near the Galactic center (D ~ 8 kpc), and 549 less absorbed sources that lie within &lt;~ 6 kpc of Earth, except that two bright, previously known LMXBs, 1E 1740.7-2942 and 2E 1743.1-2842, have been omitted because they were badly saturated in these survey images, and their positions and properties have been reported elsewhere (Marti et al. 2000, A&amp;A, 363, 184; Porquet et al. 2003, A&amp;A, 406, 299). On the basis of the inferred luminosities of the X-ray sources and the expected numbers of various classes of objects, the authors suggest that the sources with L_X &lt;~ 10^33 ergs s^-1 that comprise ~ 90% of the catalog are cataclysmic variables, and that the ~ 100 brighter objects are accreting neutron stars and black holes, young isolated pulsars, and Wolf-Rayet and O (WR/O) stars in colliding-wind binaries. They find that the spatial distribution of X-ray sources matches that of the old stellar population observed in the infrared, which supports their suggestion that most of the X-ray sources are old cataclysmic variables. However, they find that there is an apparent excess of ~ 10 bright sources in the Radio Arches region. That region is already known to be the site of recent star formation, so they suggest that the bright sources in this region are young high-mass X-ray binaries, pulsars, or WR/O star binaries.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanc150pc#1</TD>
            <TD>2008-12-24T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanc150pc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chanc150pc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanc150pc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ChandraGC150 [2]</TD>
            <TD>Chandra Galactic Central 150 Parsecs Source Catalog</TD>
            <TD>The Chandra Catalog of X-Ray Sources in the Central 150 Parsecs of the Galaxy lists X-ray sources detected in a shallow Chandra survey of the inner 2 by 0.8 degrees of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (N_H &gt;~ 4 x 10^22 cm^-2) and are therefore likely to lie near the Galactic center (D ~ 8 kpc), and 549 less absorbed sources that lie within &lt;~ 6 kpc of Earth, except that two bright, previously known LMXBs, 1E 1740.7-2942 and 2E 1743.1-2842, have been omitted because they were badly saturated in these survey images, and their positions and properties have been reported elsewhere (Marti et al. 2000, A&amp;A, 363, 184; Porquet et al. 2003, A&amp;A, 406, 299). On the basis of the inferred luminosities of the X-ray sources and the expected numbers of various classes of objects, the authors suggest that the sources with L_X &lt;~ 10^33 ergs s^-1 that comprise ~ 90% of the catalog are cataclysmic variables, and that the ~ 100 brighter objects are accreting neutron stars and black holes, young isolated pulsars, and Wolf-Rayet and O (WR/O) stars in colliding-wind binaries. They find that the spatial distribution of X-ray sources matches that of the old stellar population observed in the infrared, which supports their suggestion that most of the X-ray sources are old cataclysmic variables. However, they find that there is an apparent excess of ~ 10 bright sources in the Radio Arches region. That region is already known to be the site of recent star formation, so they suggest that the bright sources in this region are young high-mass X-ray binaries, pulsars, or WR/O star binaries.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanc150pc#2</TD>
            <TD>2008-12-24T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanc150pc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chanc150pc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanc150pc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ChandraGC150 [3]</TD>
            <TD>Chandra Galactic Central 150 Parsecs Source Catalog</TD>
            <TD>The Chandra Catalog of X-Ray Sources in the Central 150 Parsecs of the Galaxy lists X-ray sources detected in a shallow Chandra survey of the inner 2 by 0.8 degrees of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (N_H &gt;~ 4 x 10^22 cm^-2) and are therefore likely to lie near the Galactic center (D ~ 8 kpc), and 549 less absorbed sources that lie within &lt;~ 6 kpc of Earth, except that two bright, previously known LMXBs, 1E 1740.7-2942 and 2E 1743.1-2842, have been omitted because they were badly saturated in these survey images, and their positions and properties have been reported elsewhere (Marti et al. 2000, A&amp;A, 363, 184; Porquet et al. 2003, A&amp;A, 406, 299). On the basis of the inferred luminosities of the X-ray sources and the expected numbers of various classes of objects, the authors suggest that the sources with L_X &lt;~ 10^33 ergs s^-1 that comprise ~ 90% of the catalog are cataclysmic variables, and that the ~ 100 brighter objects are accreting neutron stars and black holes, young isolated pulsars, and Wolf-Rayet and O (WR/O) stars in colliding-wind binaries. They find that the spatial distribution of X-ray sources matches that of the old stellar population observed in the infrared, which supports their suggestion that most of the X-ray sources are old cataclysmic variables. However, they find that there is an apparent excess of ~ 10 bright sources in the Radio Arches region. That region is already known to be the site of recent star formation, so they suggest that the bright sources in this region are young high-mass X-ray binaries, pulsars, or WR/O star binaries.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanc150pc#3</TD>
            <TD>2008-12-24T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanc150pc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chanc150pc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanc150pc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>DLS</TD>
            <TD>Deep Lens Survey</TD>
            <TD>The Deep Lens Survey is an ultra-deep multi-band optical survey of seven 4 square degree fields. Mosaic CCD imagers at NOAO's Blanco and Mayall telescopes are being used. The deep fields will take five years to complete, in four bands: B,V,R,z'.</TD>
            <TD>JHU</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/DLS#1</TD>
            <TD>2011-09-14T18:11:59Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD />
            <TD>0.25</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/DLS</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/DLS/nodeb.asmx</TD>
            <TD />
            <TD>0</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/442/841 [1]</TD>
            <TD>High-redshift galaxy clusters (Olsen+, 2005)</TD>
            <TD>The observations were carried out in the nights September 21-25, 2000, using FORS1 mounted at the VLT-ANTU telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841#1</TD>
            <TD>2011-09-14T19:58:54Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/442/841</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/841</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/442/841 [2]</TD>
            <TD>High-redshift galaxy clusters (Olsen+, 2005)</TD>
            <TD>The observations were carried out in the nights September 21-25, 2000, using FORS1 mounted at the VLT-ANTU telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841#2</TD>
            <TD>2011-09-14T19:58:54Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/442/841&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/841</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/442/841 [tablea]</TD>
            <TD>High-redshift galaxy clusters (Olsen+, 2005)</TD>
            <TD>The observations were carried out in the nights September 21-25, 2000, using FORS1 mounted at the VLT-ANTU telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841#tablea</TD>
            <TD>2011-09-14T19:58:54Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/841</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/442/841&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/841</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>FIRST</TD>
            <TD>Faint Images of the Radio Sky at Twenty-centimeter</TD>
            <TD>FIRST -- Faint Images of the Radio Sky at Twenty-cm -- is a project designed to produce the radio equivalent of the Palomar Observatory Sky Survey over 10,000 square degrees of the North and South Galactic Caps. Using the NRAO Very Large Array (VLA) and an automated mapping pipeline, we produce images with 1.8" pixels, a typical rms of 0.15 mJy, and a resolution of 5". At the 1 mJy source detection threshold, there are ~90 sources per square degree, ~35% of which have resolved structure on scales from 2-30"</TD>
            <TD>JHU</TD>
            <TD>#Radio#</TD>
            <TD>ivo://sdss.jhu/OpneSkyNode/First#1</TD>
            <TD>2011-09-14T18:12:00Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#Radio#</TD>
            <TD />
            <TD />
            <TD>0.25</TD>
            <TD />
            <TD>ivo://sdss.jhu/OpneSkyNode/First</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes/FIRST/nodeb.asmx</TD>
            <TD />
            <TD>0</TD>
            <TD />
            <TD />
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/381 [1]</TD>
            <TD>Blueshifted [O III] emission (Boroson+, 2005)</TD>
            <TD>The [OIII]{lambda}5007 line is commonly used as an indicator of the systemic redshift of active galactic nuclei (AGNs). Also, recent studies have used the width of this emission line as a proxy for the stellar velocity dispersion in the host galaxy. This paper calls both of these assumptions into question by analyzing a sample of approximately 400 AGN spectra from the first data release of the Sloan Digital Sky Survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381#1</TD>
            <TD>2011-09-14T19:59:09Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/381</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/381</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/381 [2]</TD>
            <TD>Blueshifted [O III] emission (Boroson+, 2005)</TD>
            <TD>The [OIII]{lambda}5007 line is commonly used as an indicator of the systemic redshift of active galactic nuclei (AGNs). Also, recent studies have used the width of this emission line as a proxy for the stellar velocity dispersion in the host galaxy. This paper calls both of these assumptions into question by analyzing a sample of approximately 400 AGN spectra from the first data release of the Sloan Digital Sky Survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381#2</TD>
            <TD>2011-09-14T19:59:09Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/381&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/381</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/381 [table1]</TD>
            <TD>Blueshifted [O III] emission (Boroson+, 2005)</TD>
            <TD>The [OIII]{lambda}5007 line is commonly used as an indicator of the systemic redshift of active galactic nuclei (AGNs). Also, recent studies have used the width of this emission line as a proxy for the stellar velocity dispersion in the host galaxy. This paper calls both of these assumptions into question by analyzing a sample of approximately 400 AGN spectra from the first data release of the Sloan Digital Sky Survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381#table1</TD>
            <TD>2011-09-14T19:59:09Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/381&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/381</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/381 [1]</TD>
            <TD>Blueshifted [O III] emission (Boroson+, 2005)</TD>
            <TD>The [OIII]{lambda}5007 line is commonly used as an indicator of the systemic redshift of active galactic nuclei (AGNs). Also, recent studies have used the width of this emission line as a proxy for the stellar velocity dispersion in the host galaxy. This paper calls both of these assumptions into question by analyzing a sample of approximately 400 AGN spectra from the first data release of the Sloan Digital Sky Survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381#1</TD>
            <TD>2011-09-14T19:59:09Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/381</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/381</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/381 [2]</TD>
            <TD>Blueshifted [O III] emission (Boroson+, 2005)</TD>
            <TD>The [OIII]{lambda}5007 line is commonly used as an indicator of the systemic redshift of active galactic nuclei (AGNs). Also, recent studies have used the width of this emission line as a proxy for the stellar velocity dispersion in the host galaxy. This paper calls both of these assumptions into question by analyzing a sample of approximately 400 AGN spectra from the first data release of the Sloan Digital Sky Survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381#2</TD>
            <TD>2011-09-14T19:59:09Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/381&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/381</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/381 [table1]</TD>
            <TD>Blueshifted [O III] emission (Boroson+, 2005)</TD>
            <TD>The [OIII]{lambda}5007 line is commonly used as an indicator of the systemic redshift of active galactic nuclei (AGNs). Also, recent studies have used the width of this emission line as a proxy for the stellar velocity dispersion in the host galaxy. This paper calls both of these assumptions into question by analyzing a sample of approximately 400 AGN spectra from the first data release of the Sloan Digital Sky Survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381#table1</TD>
            <TD>2011-09-14T19:59:09Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/381&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/381</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/465/375 [1]</TD>
            <TD>X-ray monitoring of optical novae in M31 (Pietsch+, 2007)</TD>
            <TD>Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380d after outburst. One nova is detected to turn on 50d, another 200d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (&gt;30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375#1</TD>
            <TD>2011-09-14T20:02:56Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/465/375</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/375</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/465/375 [2]</TD>
            <TD>X-ray monitoring of optical novae in M31 (Pietsch+, 2007)</TD>
            <TD>Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380d after outburst. One nova is detected to turn on 50d, another 200d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (&gt;30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375#2</TD>
            <TD>2011-09-14T20:02:56Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/465/375&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/375</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/465/375 [tablea1]</TD>
            <TD>X-ray monitoring of optical novae in M31 (Pietsch+, 2007)</TD>
            <TD>Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380d after outburst. One nova is detected to turn on 50d, another 200d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (&gt;30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375#tablea1</TD>
            <TD>2011-09-14T20:02:56Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/465/375&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/375</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/381 [1]</TD>
            <TD>Blueshifted [O III] emission (Boroson+, 2005)</TD>
            <TD>The [OIII]{lambda}5007 line is commonly used as an indicator of the systemic redshift of active galactic nuclei (AGNs). Also, recent studies have used the width of this emission line as a proxy for the stellar velocity dispersion in the host galaxy. This paper calls both of these assumptions into question by analyzing a sample of approximately 400 AGN spectra from the first data release of the Sloan Digital Sky Survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381#1</TD>
            <TD>2011-09-14T19:59:09Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/381</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/381</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/381 [2]</TD>
            <TD>Blueshifted [O III] emission (Boroson+, 2005)</TD>
            <TD>The [OIII]{lambda}5007 line is commonly used as an indicator of the systemic redshift of active galactic nuclei (AGNs). Also, recent studies have used the width of this emission line as a proxy for the stellar velocity dispersion in the host galaxy. This paper calls both of these assumptions into question by analyzing a sample of approximately 400 AGN spectra from the first data release of the Sloan Digital Sky Survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381#2</TD>
            <TD>2011-09-14T19:59:09Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/381&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/381</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/381 [table1]</TD>
            <TD>Blueshifted [O III] emission (Boroson+, 2005)</TD>
            <TD>The [OIII]{lambda}5007 line is commonly used as an indicator of the systemic redshift of active galactic nuclei (AGNs). Also, recent studies have used the width of this emission line as a proxy for the stellar velocity dispersion in the host galaxy. This paper calls both of these assumptions into question by analyzing a sample of approximately 400 AGN spectra from the first data release of the Sloan Digital Sky Survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381#table1</TD>
            <TD>2011-09-14T19:59:09Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/381</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/381&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/381</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/348/866 [1]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#1</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/348/866</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/348/866 [2]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfsgpgr]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfsgpgr</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfngpga]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfngpga</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfngpgr]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfngpgr</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfsgpga]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfsgpga</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/465/375 [1]</TD>
            <TD>X-ray monitoring of optical novae in M31 (Pietsch+, 2007)</TD>
            <TD>Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380d after outburst. One nova is detected to turn on 50d, another 200d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (&gt;30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375#1</TD>
            <TD>2011-09-14T20:02:56Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/465/375</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/375</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/465/375 [2]</TD>
            <TD>X-ray monitoring of optical novae in M31 (Pietsch+, 2007)</TD>
            <TD>Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380d after outburst. One nova is detected to turn on 50d, another 200d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (&gt;30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375#2</TD>
            <TD>2011-09-14T20:02:56Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/465/375&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/375</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/465/375 [tablea1]</TD>
            <TD>X-ray monitoring of optical novae in M31 (Pietsch+, 2007)</TD>
            <TD>Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380d after outburst. One nova is detected to turn on 50d, another 200d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (&gt;30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375#tablea1</TD>
            <TD>2011-09-14T20:02:56Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/465/375&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/375</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/633/871 [1]</TD>
            <TD>Positions and photometry of HII knots in M51 (Calzetti+, 2005)</TD>
            <TD>Far-ultraviolet to far-infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Telescope) and ground-based data, are used to investigate local and global star formation and the impact of dust extinction. The Spitzer data provide unprecedented spatial detail in the infrared, down to sizes 500 pc at the distance of NGC 5194. The multiwavelength set is used to trace the relatively young stellar populations, the ionized gas, and the dust absorption and emission in HII-emitting knots, over 3 orders of magnitude in wavelength range.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871#1</TD>
            <TD>2011-09-14T19:59:10Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/633/871</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/633/871</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/633/871 [2]</TD>
            <TD>Positions and photometry of HII knots in M51 (Calzetti+, 2005)</TD>
            <TD>Far-ultraviolet to far-infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Telescope) and ground-based data, are used to investigate local and global star formation and the impact of dust extinction. The Spitzer data provide unprecedented spatial detail in the infrared, down to sizes 500 pc at the distance of NGC 5194. The multiwavelength set is used to trace the relatively young stellar populations, the ionized gas, and the dust absorption and emission in HII-emitting knots, over 3 orders of magnitude in wavelength range.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871#2</TD>
            <TD>2011-09-14T19:59:10Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/633/871&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/633/871</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/633/871 [table1]</TD>
            <TD>Positions and photometry of HII knots in M51 (Calzetti+, 2005)</TD>
            <TD>Far-ultraviolet to far-infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Telescope) and ground-based data, are used to investigate local and global star formation and the impact of dust extinction. The Spitzer data provide unprecedented spatial detail in the infrared, down to sizes 500 pc at the distance of NGC 5194. The multiwavelength set is used to trace the relatively young stellar populations, the ionized gas, and the dust absorption and emission in HII-emitting knots, over 3 orders of magnitude in wavelength range.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871#table1</TD>
            <TD>2011-09-14T19:59:10Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/633/871&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/633/871</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/633/871 [1]</TD>
            <TD>Positions and photometry of HII knots in M51 (Calzetti+, 2005)</TD>
            <TD>Far-ultraviolet to far-infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Telescope) and ground-based data, are used to investigate local and global star formation and the impact of dust extinction. The Spitzer data provide unprecedented spatial detail in the infrared, down to sizes 500 pc at the distance of NGC 5194. The multiwavelength set is used to trace the relatively young stellar populations, the ionized gas, and the dust absorption and emission in HII-emitting knots, over 3 orders of magnitude in wavelength range.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871#1</TD>
            <TD>2011-09-14T19:59:10Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/633/871</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/633/871</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/633/871 [2]</TD>
            <TD>Positions and photometry of HII knots in M51 (Calzetti+, 2005)</TD>
            <TD>Far-ultraviolet to far-infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Telescope) and ground-based data, are used to investigate local and global star formation and the impact of dust extinction. The Spitzer data provide unprecedented spatial detail in the infrared, down to sizes 500 pc at the distance of NGC 5194. The multiwavelength set is used to trace the relatively young stellar populations, the ionized gas, and the dust absorption and emission in HII-emitting knots, over 3 orders of magnitude in wavelength range.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871#2</TD>
            <TD>2011-09-14T19:59:10Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/633/871&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/633/871</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/633/871 [table1]</TD>
            <TD>Positions and photometry of HII knots in M51 (Calzetti+, 2005)</TD>
            <TD>Far-ultraviolet to far-infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Telescope) and ground-based data, are used to investigate local and global star formation and the impact of dust extinction. The Spitzer data provide unprecedented spatial detail in the infrared, down to sizes 500 pc at the distance of NGC 5194. The multiwavelength set is used to trace the relatively young stellar populations, the ionized gas, and the dust absorption and emission in HII-emitting knots, over 3 orders of magnitude in wavelength range.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871#table1</TD>
            <TD>2011-09-14T19:59:10Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/633/871&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/633/871</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/348/866 [1]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#1</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/348/866</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/348/866 [2]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfsgpgr]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfsgpgr</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfngpga]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfngpga</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfngpgr]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfngpgr</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/866 [2dfsgpga]</TD>
            <TD>2dFGRS Percolation-Inferred Galaxy Group (2PIGG) (Eke+, 2004)</TD>
            <TD>The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the ~190000 galaxies considered are placed into groups containing at least two members of which ~29000 are found. Of these, ~7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260km/s. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866#2dfsgpga</TD>
            <TD>2012-09-04T09:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/866</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/866&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/866</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4636CXO [1]</TD>
            <TD>NGC 4636 Chandra X-Ray Point Source Catalog</TD>
            <TD>This catalog lists the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling ~193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, the authors detected 318 individual point sources. For their analysis, they used a subset of 277 detections with &gt;= net 10 counts (a limiting luminosity of approximately 1.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV band, outside the central 1.5 arcminutes bright galaxy core). This table contains this subset of 277 X-ray sources. The authors discuss the radial distribution of the point sources. Between 1.5 and 6 arcminutes from the center, 25% of the sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% to be low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6 arcminutes, background sources (AGN) will dominate the point sources. The authors explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, ~10% of the sources in each observation show significant short-term variability. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope Alpha = 1.14 +/- 0.03. The authors do not detect, but estimate an upper limit of ~4.5 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the current X-ray luminosity of, the historical supernova SN1939A. They find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1.5 to 6 arcminutes of the galaxy center, 48 of the 129 X-ray point sources (37%) with &gt;=10 net counts are matched with GC candidates. Since they expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, the authors find that ~70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. The authors do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;= L_x &lt;= 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4636cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4636cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4636cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4636cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4636CXO [2]</TD>
            <TD>NGC 4636 Chandra X-Ray Point Source Catalog</TD>
            <TD>This catalog lists the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling ~193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, the authors detected 318 individual point sources. For their analysis, they used a subset of 277 detections with &gt;= net 10 counts (a limiting luminosity of approximately 1.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV band, outside the central 1.5 arcminutes bright galaxy core). This table contains this subset of 277 X-ray sources. The authors discuss the radial distribution of the point sources. Between 1.5 and 6 arcminutes from the center, 25% of the sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% to be low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6 arcminutes, background sources (AGN) will dominate the point sources. The authors explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, ~10% of the sources in each observation show significant short-term variability. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope Alpha = 1.14 +/- 0.03. The authors do not detect, but estimate an upper limit of ~4.5 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the current X-ray luminosity of, the historical supernova SN1939A. They find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1.5 to 6 arcminutes of the galaxy center, 48 of the 129 X-ray point sources (37%) with &gt;=10 net counts are matched with GC candidates. Since they expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, the authors find that ~70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. The authors do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;= L_x &lt;= 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4636cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4636cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4636cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4636cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4636CXO [3]</TD>
            <TD>NGC 4636 Chandra X-Ray Point Source Catalog</TD>
            <TD>This catalog lists the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling ~193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, the authors detected 318 individual point sources. For their analysis, they used a subset of 277 detections with &gt;= net 10 counts (a limiting luminosity of approximately 1.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV band, outside the central 1.5 arcminutes bright galaxy core). This table contains this subset of 277 X-ray sources. The authors discuss the radial distribution of the point sources. Between 1.5 and 6 arcminutes from the center, 25% of the sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% to be low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6 arcminutes, background sources (AGN) will dominate the point sources. The authors explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, ~10% of the sources in each observation show significant short-term variability. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope Alpha = 1.14 +/- 0.03. The authors do not detect, but estimate an upper limit of ~4.5 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the current X-ray luminosity of, the historical supernova SN1939A. They find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1.5 to 6 arcminutes of the galaxy center, 48 of the 129 X-ray point sources (37%) with &gt;=10 net counts are matched with GC candidates. Since they expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, the authors find that ~70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. The authors do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;= L_x &lt;= 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4636cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4636cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4636cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4636cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/465/375 [1]</TD>
            <TD>X-ray monitoring of optical novae in M31 (Pietsch+, 2007)</TD>
            <TD>Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380d after outburst. One nova is detected to turn on 50d, another 200d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (&gt;30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375#1</TD>
            <TD>2011-09-14T20:02:56Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/465/375</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/375</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/465/375 [2]</TD>
            <TD>X-ray monitoring of optical novae in M31 (Pietsch+, 2007)</TD>
            <TD>Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380d after outburst. One nova is detected to turn on 50d, another 200d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (&gt;30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375#2</TD>
            <TD>2011-09-14T20:02:56Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/465/375&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/375</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/465/375 [tablea1]</TD>
            <TD>X-ray monitoring of optical novae in M31 (Pietsch+, 2007)</TD>
            <TD>Optical novae have recently been identified as the major class of supersoft X-ray sources in M 31 based on ROSAT and early XMM-Newton and Chandra observations. This paper reports on a search for X-ray counterparts of optical novae in M 31 based on archival Chandra HRC-I and ACIS-I as well as XMM-Newton observations of the galaxy center region obtained from July 2004 to February 2005. We systematically determine X-ray brightness or upper limit for counterparts of all known optical novae with outbursts between November 2003 to the end of the X-ray coverage. In addition, we determine the X-ray brightnesses for counterparts of four novae with earlier outbursts. For comparison with the X-ray data we created a catalogue of optical novae in M 31 based on our own nova search programs and on all novae reported in the literature. We collected all known properties and named the novae consistently following the CBAT scheme. We detect eleven out of 34 novae within a year after the optical outburst in X-rays. While for eleven novae we detect the end of the supersoft source phase, seven novae are still bright more than 1200, 1600, 1950, 2650, 3100, 3370 and 3380d after outburst. One nova is detected to turn on 50d, another 200d after outburst. Three novae unexpectedly showed short X-ray outbursts starting within 50d after the optical outburst and lasting only two to three months. The X-ray emission of several of the novae can be characterized as supersoft from hardness ratios and/or X-ray spectra or by comparing HRC-I count rates with ACIS-I count rates or upper limits. The number of detected optical novae at supersoft X-rays is much higher than previously estimated (&gt;30%). We use the X-ray light curves to estimate the burned masses of the White Dwarf and of the ejecta.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375#tablea1</TD>
            <TD>2011-09-14T20:02:56Z</TD>
            <TD>#Novae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/375</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/465/375&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/375</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4636CXO [1]</TD>
            <TD>NGC 4636 Chandra X-Ray Point Source Catalog</TD>
            <TD>This catalog lists the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling ~193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, the authors detected 318 individual point sources. For their analysis, they used a subset of 277 detections with &gt;= net 10 counts (a limiting luminosity of approximately 1.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV band, outside the central 1.5 arcminutes bright galaxy core). This table contains this subset of 277 X-ray sources. The authors discuss the radial distribution of the point sources. Between 1.5 and 6 arcminutes from the center, 25% of the sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% to be low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6 arcminutes, background sources (AGN) will dominate the point sources. The authors explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, ~10% of the sources in each observation show significant short-term variability. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope Alpha = 1.14 +/- 0.03. The authors do not detect, but estimate an upper limit of ~4.5 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the current X-ray luminosity of, the historical supernova SN1939A. They find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1.5 to 6 arcminutes of the galaxy center, 48 of the 129 X-ray point sources (37%) with &gt;=10 net counts are matched with GC candidates. Since they expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, the authors find that ~70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. The authors do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;= L_x &lt;= 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4636cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4636cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4636cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4636cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4636CXO [2]</TD>
            <TD>NGC 4636 Chandra X-Ray Point Source Catalog</TD>
            <TD>This catalog lists the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling ~193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, the authors detected 318 individual point sources. For their analysis, they used a subset of 277 detections with &gt;= net 10 counts (a limiting luminosity of approximately 1.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV band, outside the central 1.5 arcminutes bright galaxy core). This table contains this subset of 277 X-ray sources. The authors discuss the radial distribution of the point sources. Between 1.5 and 6 arcminutes from the center, 25% of the sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% to be low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6 arcminutes, background sources (AGN) will dominate the point sources. The authors explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, ~10% of the sources in each observation show significant short-term variability. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope Alpha = 1.14 +/- 0.03. The authors do not detect, but estimate an upper limit of ~4.5 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the current X-ray luminosity of, the historical supernova SN1939A. They find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1.5 to 6 arcminutes of the galaxy center, 48 of the 129 X-ray point sources (37%) with &gt;=10 net counts are matched with GC candidates. Since they expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, the authors find that ~70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. The authors do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;= L_x &lt;= 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4636cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4636cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4636cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4636cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4636CXO [3]</TD>
            <TD>NGC 4636 Chandra X-Ray Point Source Catalog</TD>
            <TD>This catalog lists the X-ray point-source population in the nearby Virgo elliptical galaxy NGC 4636 from three Chandra X-ray observations. These observations, totaling ~193 ks after time filtering, were taken with the Advanced CCD Imaging Camera (ACIS) over a three-year period. Using a wavelet decomposition detection algorithm, the authors detected 318 individual point sources. For their analysis, they used a subset of 277 detections with &gt;= net 10 counts (a limiting luminosity of approximately 1.2 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5-2 keV band, outside the central 1.5 arcminutes bright galaxy core). This table contains this subset of 277 X-ray sources. The authors discuss the radial distribution of the point sources. Between 1.5 and 6 arcminutes from the center, 25% of the sources are likely to be background sources (active galactic nuclei (AGNs)) and 75% to be low-mass X-ray binaries (LMXBs) within the galaxy, while at radial distances greater than 6 arcminutes, background sources (AGN) will dominate the point sources. The authors explore short and long-term variability (over timescales of 1 day to three years) for X-ray point sources in this elliptical galaxy. 54 sources (24%) in the common ACIS fields of view show significant variability between observations. Of these, 37 are detected with at least 10 net counts in only one observation and thus may be "transient." In addition, ~10% of the sources in each observation show significant short-term variability. The cumulative luminosity function (LF) for the point sources in NGC 4636 can be represented as a power law of slope Alpha = 1.14 +/- 0.03. The authors do not detect, but estimate an upper limit of ~4.5 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; to the current X-ray luminosity of, the historical supernova SN1939A. They find 77 matches between X-ray point sources and globular cluster (GC) candidates found in deep optical images of NGC 4636. In the annulus from 1.5 to 6 arcminutes of the galaxy center, 48 of the 129 X-ray point sources (37%) with &gt;=10 net counts are matched with GC candidates. Since they expect 25% of these sources to be background AGN, the percentage matched with GCs could be as high as 50%. Of these matched sources, the authors find that ~70% are associated with the redder GC candidates, those that are thought to have near-solar metal abundance. The fraction of GC candidates with an X-ray point source match decreases with decreasing GC luminosity. The authors do not find a correlation between the X-ray luminosities of the matched point sources and the luminosity or color of the host GC candidates. The LFs of the X-ray point sources matched with GCs and those that are unmatched have similar slopes over 1.8 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; &lt;= L_x &lt;= 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4636cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4636cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4636cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4636cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/633/871 [1]</TD>
            <TD>Positions and photometry of HII knots in M51 (Calzetti+, 2005)</TD>
            <TD>Far-ultraviolet to far-infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Telescope) and ground-based data, are used to investigate local and global star formation and the impact of dust extinction. The Spitzer data provide unprecedented spatial detail in the infrared, down to sizes 500 pc at the distance of NGC 5194. The multiwavelength set is used to trace the relatively young stellar populations, the ionized gas, and the dust absorption and emission in HII-emitting knots, over 3 orders of magnitude in wavelength range.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871#1</TD>
            <TD>2011-09-14T19:59:10Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/633/871</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/633/871</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/633/871 [2]</TD>
            <TD>Positions and photometry of HII knots in M51 (Calzetti+, 2005)</TD>
            <TD>Far-ultraviolet to far-infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Telescope) and ground-based data, are used to investigate local and global star formation and the impact of dust extinction. The Spitzer data provide unprecedented spatial detail in the infrared, down to sizes 500 pc at the distance of NGC 5194. The multiwavelength set is used to trace the relatively young stellar populations, the ionized gas, and the dust absorption and emission in HII-emitting knots, over 3 orders of magnitude in wavelength range.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871#2</TD>
            <TD>2011-09-14T19:59:10Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/633/871&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/633/871</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/633/871 [table1]</TD>
            <TD>Positions and photometry of HII knots in M51 (Calzetti+, 2005)</TD>
            <TD>Far-ultraviolet to far-infrared images of the nearby galaxy NGC 5194 (M51a), from a combination of space-based (Spitzer, GALEX, and Hubble Space Telescope) and ground-based data, are used to investigate local and global star formation and the impact of dust extinction. The Spitzer data provide unprecedented spatial detail in the infrared, down to sizes 500 pc at the distance of NGC 5194. The multiwavelength set is used to trace the relatively young stellar populations, the ionized gas, and the dust absorption and emission in HII-emitting knots, over 3 orders of magnitude in wavelength range.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871#table1</TD>
            <TD>2011-09-14T19:59:10Z</TD>
            <TD>#Galaxies#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/633/871</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/633/871&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/633/871</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/369/1880 [1]</TD>
            <TD>Photometry of SN 2003cg (Elias-Rosa+, 2006)</TD>
            <TD>SN 2003cg was discovered in 2003 March 21.51 UT by Itagati and Arbour (IAUC 8097) at 14"E and 5"N from the centre of the nearby spiral galaxy NGC 3169 .</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1880#1</TD>
            <TD>2011-09-14T20:03:26Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1880</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/369/1880</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1880</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/369/1880 [2]</TD>
            <TD>Photometry of SN 2003cg (Elias-Rosa+, 2006)</TD>
            <TD>SN 2003cg was discovered in 2003 March 21.51 UT by Itagati and Arbour (IAUC 8097) at 14"E and 5"N from the centre of the nearby spiral galaxy NGC 3169 .</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1880#2</TD>
            <TD>2011-09-14T20:03:26Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1880</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/369/1880&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1880</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/458/113 [1]</TD>
            <TD>BVRIc photometry towards inner Galactic Bulge (Santiago+, 2006)</TD>
            <TD>4 files containing photometric data on 4 directions located within the central 3.5{deg} of the Galaxy, where extinction is lower than usual. Equatorial coordinates (J2000.0) and optical BVRI magnitudes obtained at Pico dos Dias, Laboratorio Nacional de Astrofisica, Brasil, are combined with near infra-red data from the 2 Micron All Sky Survey, providing a long spectral baseline for over 100.000 stars in these low-extinction windows. The file names indicate the galactic longitude and latitude of each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113#1</TD>
            <TD>2011-09-14T19:59:12Z</TD>
            <TD>#Extinction#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/458/113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/458/113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/458/113 [2]</TD>
            <TD>BVRIc photometry towards inner Galactic Bulge (Santiago+, 2006)</TD>
            <TD>4 files containing photometric data on 4 directions located within the central 3.5{deg} of the Galaxy, where extinction is lower than usual. Equatorial coordinates (J2000.0) and optical BVRI magnitudes obtained at Pico dos Dias, Laboratorio Nacional de Astrofisica, Brasil, are combined with near infra-red data from the 2 Micron All Sky Survey, providing a long spectral baseline for over 100.000 stars in these low-extinction windows. The file names indicate the galactic longitude and latitude of each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113#2</TD>
            <TD>2011-09-14T19:59:12Z</TD>
            <TD>#Extinction#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/458/113&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/458/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/458/113 [catalog]</TD>
            <TD>BVRIc photometry towards inner Galactic Bulge (Santiago+, 2006)</TD>
            <TD>4 files containing photometric data on 4 directions located within the central 3.5{deg} of the Galaxy, where extinction is lower than usual. Equatorial coordinates (J2000.0) and optical BVRI magnitudes obtained at Pico dos Dias, Laboratorio Nacional de Astrofisica, Brasil, are combined with near infra-red data from the 2 Micron All Sky Survey, providing a long spectral baseline for over 100.000 stars in these low-extinction windows. The file names indicate the galactic longitude and latitude of each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113#catalog</TD>
            <TD>2011-09-14T19:59:12Z</TD>
            <TD>#Extinction#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/458/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/458/113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/369/1880 [1]</TD>
            <TD>Photometry of SN 2003cg (Elias-Rosa+, 2006)</TD>
            <TD>SN 2003cg was discovered in 2003 March 21.51 UT by Itagati and Arbour (IAUC 8097) at 14"E and 5"N from the centre of the nearby spiral galaxy NGC 3169 .</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1880#1</TD>
            <TD>2011-09-14T20:03:26Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1880</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/369/1880</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1880</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/369/1880 [2]</TD>
            <TD>Photometry of SN 2003cg (Elias-Rosa+, 2006)</TD>
            <TD>SN 2003cg was discovered in 2003 March 21.51 UT by Itagati and Arbour (IAUC 8097) at 14"E and 5"N from the centre of the nearby spiral galaxy NGC 3169 .</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1880#2</TD>
            <TD>2011-09-14T20:03:26Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/369/1880</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/369/1880&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/369/1880</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/458/113 [1]</TD>
            <TD>BVRIc photometry towards inner Galactic Bulge (Santiago+, 2006)</TD>
            <TD>4 files containing photometric data on 4 directions located within the central 3.5{deg} of the Galaxy, where extinction is lower than usual. Equatorial coordinates (J2000.0) and optical BVRI magnitudes obtained at Pico dos Dias, Laboratorio Nacional de Astrofisica, Brasil, are combined with near infra-red data from the 2 Micron All Sky Survey, providing a long spectral baseline for over 100.000 stars in these low-extinction windows. The file names indicate the galactic longitude and latitude of each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113#1</TD>
            <TD>2011-09-14T19:59:12Z</TD>
            <TD>#Extinction#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/458/113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/458/113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/458/113 [2]</TD>
            <TD>BVRIc photometry towards inner Galactic Bulge (Santiago+, 2006)</TD>
            <TD>4 files containing photometric data on 4 directions located within the central 3.5{deg} of the Galaxy, where extinction is lower than usual. Equatorial coordinates (J2000.0) and optical BVRI magnitudes obtained at Pico dos Dias, Laboratorio Nacional de Astrofisica, Brasil, are combined with near infra-red data from the 2 Micron All Sky Survey, providing a long spectral baseline for over 100.000 stars in these low-extinction windows. The file names indicate the galactic longitude and latitude of each region.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113#2</TD>
            <TD>2011-09-14T19:59:12Z</TD>
            <TD>#Extinction#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/458/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/458/113&amp;</TD>
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            <TD>J/AJ/123/2223 [1]</TD>
            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
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            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
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            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
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            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
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            <TD>BVRIc photometry towards inner Galactic Bulge (Santiago+, 2006)</TD>
            <TD>4 files containing photometric data on 4 directions located within the central 3.5{deg} of the Galaxy, where extinction is lower than usual. Equatorial coordinates (J2000.0) and optical BVRI magnitudes obtained at Pico dos Dias, Laboratorio Nacional de Astrofisica, Brasil, are combined with near infra-red data from the 2 Micron All Sky Survey, providing a long spectral baseline for over 100.000 stars in these low-extinction windows. The file names indicate the galactic longitude and latitude of each region.</TD>
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            <TD>J/AJ/123/2223 [1]</TD>
            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
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            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
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            <TD>J/AJ/123/2223 [table2]</TD>
            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2223#table2</TD>
            <TD>2011-09-14T20:04:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
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            <TD>30-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2223</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2223 [table1]</TD>
            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2223#table1</TD>
            <TD>2011-09-14T20:04:00Z</TD>
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            <TD>30-May-2002</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/445/819 [1]</TD>
            <TD>Systems of galaxies in Shapley supercluster (Ragone+, 2006)</TD>
            <TD>Based on the largest compilation of galaxies with redshift in the region of the Shapley Supercluster (Proust et al., 2004 in prep., 2006A&amp;A...447..133P), we identified 122 galaxy systems, 60 of which are new systems. Using the SuperCOSMOS catalogue, we have assigned b_j_ magnitudes to each galaxy in our compilation. The sample of galaxy systems was used to estimate the mass function of systems in the range 10^13^ to 10^15^M_{sun}/h^-1^. We computed a lower value to the total mass in the region of the Shapley Supercluster with this mass function. Using 15 mock catalogues we derived the mean mass that these kinds of systems have before comparing it with that obtained from the real data.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/445/819#1</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/445/819</TD>
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/445/819 [2]</TD>
            <TD>Systems of galaxies in Shapley supercluster (Ragone+, 2006)</TD>
            <TD>Based on the largest compilation of galaxies with redshift in the region of the Shapley Supercluster (Proust et al., 2004 in prep., 2006A&amp;A...447..133P), we identified 122 galaxy systems, 60 of which are new systems. Using the SuperCOSMOS catalogue, we have assigned b_j_ magnitudes to each galaxy in our compilation. The sample of galaxy systems was used to estimate the mass function of systems in the range 10^13^ to 10^15^M_{sun}/h^-1^. We computed a lower value to the total mass in the region of the Shapley Supercluster with this mass function. Using 15 mock catalogues we derived the mean mass that these kinds of systems have before comparing it with that obtained from the real data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819#2</TD>
            <TD>2011-09-14T20:00:49Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
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            <TD>#Research#</TD>
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            <TD>14-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/445/819&amp;</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/445/819 [table1]</TD>
            <TD>Systems of galaxies in Shapley supercluster (Ragone+, 2006)</TD>
            <TD>Based on the largest compilation of galaxies with redshift in the region of the Shapley Supercluster (Proust et al., 2004 in prep., 2006A&amp;A...447..133P), we identified 122 galaxy systems, 60 of which are new systems. Using the SuperCOSMOS catalogue, we have assigned b_j_ magnitudes to each galaxy in our compilation. The sample of galaxy systems was used to estimate the mass function of systems in the range 10^13^ to 10^15^M_{sun}/h^-1^. We computed a lower value to the total mass in the region of the Shapley Supercluster with this mass function. Using 15 mock catalogues we derived the mean mass that these kinds of systems have before comparing it with that obtained from the real data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819#table1</TD>
            <TD>2011-09-14T20:00:49Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
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            <TD>14-Nov-2006</TD>
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            <TD>ConeSearch</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2223 [1]</TD>
            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2223 [2]</TD>
            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2223#2</TD>
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            <TD>J/AJ/123/2223 [table2]</TD>
            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2223 [table1]</TD>
            <TD>SPICES II: CHANDRA observations of Lynx (Stern+, 2002)</TD>
            <TD>We present our first results on field X-ray sources detected in a deep, 184.7ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (RA=08h48min, DE=+44{deg}54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z=0.57, 1.26, and 1.27. Not including the known clusters, in the 17'x17' ACIS-I field we detect 132 sources in the 0.5-2keV (soft) X-ray band down to a limiting flux of ~1.7x10^-16^ergs/cm^2^/s and 11 sources in the 2-10keV (hard) X-ray band down to a limiting flux of ~1.3x10^-15^ergs/cm^2^/s. The combined catalog contains a total of 153 sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, we find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox." From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I=24, and 71% of the X-ray sources have near-infrared counterparts to Ks=20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I-Ks&gt;=4). We have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which we have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. We briefly review non-active galactic nucleus mechanisms to produce X-ray emission and discuss properties of the Lynx Chandra sample in relation to other samples of X-ray and non-X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2223#table1</TD>
            <TD>2011-09-14T20:04:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
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            <TD>30-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2223</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC752XMM [1]</TD>
            <TD>NGC 752 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table provides a list of X-ray sources detected in a ~50 ks XMM-Newton X-ray observation of the open cluster NGC 752. For the sources with 2MASS counterparts, the values of their magnitudes in the J, H and K bands are also given. Additionally, for the sources with a Chandra counterpart (within a search radius of 5 arcsec), the values of their Chandra source number (as given in the related Browse table NGC752CXO) are also given. Very little is known about the evolution of stellar activity between the ages of the Hyades (0.8 Gyr) and the Sun (4.6 Gyr). To gain information on the typical level of coronal activity at a star's intermediate age, the authors have studied the X-ray emission from stars in the 1.9 Gyr-old open cluster NGC 752. They analysed a ~ 140 ks Chandra observation of NGC 752 and a ~50 ks XMM-Newton observation of the same cluster. They detected 262 X-ray sources in the Chandra data and 145 sources in the XMM-Newton observation. Around 90% of the catalogued cluster members within Chandra's field of view are detected in the X-ray observation. The X-ray luminosity of all observed cluster members (28 stars) and of 11 cluster member candidates was derived. These data indicate that, at an age of 1.9 Gyr, the typical X-ray luminosity L_x of the cluster members with masses of 0.8 to 1.2 solar masses is 1.3 x 10&lt;sup&gt;28&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, which is approximately a factor of 6 times less intense than that observed in the younger Hyades. Given that L_x is proportional to the square of a star's rotational rate, the median L_x of NGC 752 is consistent, for t &gt;= 1 Gyr, with a decaying rate in rotational velocities v_rot ~ t&lt;sup&gt;-alpha&lt;/sup&gt; with alpha ~ 0.75, steeper than the Skumanich relation (alpha ~ 0.5) and significantly steeper than that observed between the Pleiades and the Hyades (where alpha &lt;0.3), suggesting that a change in the rotational regimes of the stellar interiors is taking place at an age of ~ 1 Gyr. NGC 752 was observed for 49 ks by the XMM-Newton EPIC camera on February 5, 2003 starting at 23:29:25 UT, and the nominal pointing was towards J2000.0 RA and Declination of (01:57:38, +37:47:60), thus the XMM-Newton field-of-view (FOV) includes the Chandra FOV. For the source detection, the authors used the PWXDETECT code developed at Palermo Observatory and derived from the analogous Chandra PWDETECT code based on wavelet transform analysis. This allows the three EPIC exposures (PN, MOS1 and MOS2) to be combined in order to gain a deeper sensitivity with respect to the source detection based on single images. THere were 145 point sources detected in the energy band 0.5 - 2.0 keV. An extended source (not listed in this present table), very likely a galaxy cluster, is also visible in the EPIC data. The authors searched for 2MASS counterparts to the XMM-Newton sources using a search radius of 5 arcsec and found a counterpart for 38 sources. As for the Chandra data, all sources with a visible counterpart from DLM94 have also a 2MASS counterpart, so this leaves 15 XMM-Newton sources with a 2MASS counterpart and no counterpart in Daniel et al. (1994, PASP, 106, 281); of these, 3 were also detected by Chandra; of the other 12, 10 are outside the Chandra FOV, while two are within it (XMM-Newton sources 58 and 65). Source 65 was caught by XMM-Newton during the decay phase of a flare, which explains why it is not detected in the Chandra data. For source 58 there is no immediate explanation for this, since the light curve does not show evidence of a flare. No additional near-IR counterpart to the XMM-Newton sources was found within the Point Source Reject Table of the 2MASS Extended Mission.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC752XMM [2]</TD>
            <TD>NGC 752 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table provides a list of X-ray sources detected in a ~50 ks XMM-Newton X-ray observation of the open cluster NGC 752. For the sources with 2MASS counterparts, the values of their magnitudes in the J, H and K bands are also given. Additionally, for the sources with a Chandra counterpart (within a search radius of 5 arcsec), the values of their Chandra source number (as given in the related Browse table NGC752CXO) are also given. Very little is known about the evolution of stellar activity between the ages of the Hyades (0.8 Gyr) and the Sun (4.6 Gyr). To gain information on the typical level of coronal activity at a star's intermediate age, the authors have studied the X-ray emission from stars in the 1.9 Gyr-old open cluster NGC 752. They analysed a ~ 140 ks Chandra observation of NGC 752 and a ~50 ks XMM-Newton observation of the same cluster. They detected 262 X-ray sources in the Chandra data and 145 sources in the XMM-Newton observation. Around 90% of the catalogued cluster members within Chandra's field of view are detected in the X-ray observation. The X-ray luminosity of all observed cluster members (28 stars) and of 11 cluster member candidates was derived. These data indicate that, at an age of 1.9 Gyr, the typical X-ray luminosity L_x of the cluster members with masses of 0.8 to 1.2 solar masses is 1.3 x 10&lt;sup&gt;28&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, which is approximately a factor of 6 times less intense than that observed in the younger Hyades. Given that L_x is proportional to the square of a star's rotational rate, the median L_x of NGC 752 is consistent, for t &gt;= 1 Gyr, with a decaying rate in rotational velocities v_rot ~ t&lt;sup&gt;-alpha&lt;/sup&gt; with alpha ~ 0.75, steeper than the Skumanich relation (alpha ~ 0.5) and significantly steeper than that observed between the Pleiades and the Hyades (where alpha &lt;0.3), suggesting that a change in the rotational regimes of the stellar interiors is taking place at an age of ~ 1 Gyr. NGC 752 was observed for 49 ks by the XMM-Newton EPIC camera on February 5, 2003 starting at 23:29:25 UT, and the nominal pointing was towards J2000.0 RA and Declination of (01:57:38, +37:47:60), thus the XMM-Newton field-of-view (FOV) includes the Chandra FOV. For the source detection, the authors used the PWXDETECT code developed at Palermo Observatory and derived from the analogous Chandra PWDETECT code based on wavelet transform analysis. This allows the three EPIC exposures (PN, MOS1 and MOS2) to be combined in order to gain a deeper sensitivity with respect to the source detection based on single images. THere were 145 point sources detected in the energy band 0.5 - 2.0 keV. An extended source (not listed in this present table), very likely a galaxy cluster, is also visible in the EPIC data. The authors searched for 2MASS counterparts to the XMM-Newton sources using a search radius of 5 arcsec and found a counterpart for 38 sources. As for the Chandra data, all sources with a visible counterpart from DLM94 have also a 2MASS counterpart, so this leaves 15 XMM-Newton sources with a 2MASS counterpart and no counterpart in Daniel et al. (1994, PASP, 106, 281); of these, 3 were also detected by Chandra; of the other 12, 10 are outside the Chandra FOV, while two are within it (XMM-Newton sources 58 and 65). Source 65 was caught by XMM-Newton during the decay phase of a flare, which explains why it is not detected in the Chandra data. For source 58 there is no immediate explanation for this, since the light curve does not show evidence of a flare. No additional near-IR counterpart to the XMM-Newton sources was found within the Point Source Reject Table of the 2MASS Extended Mission.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc752xmm#2</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc752xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC752XMM [3]</TD>
            <TD>NGC 752 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table provides a list of X-ray sources detected in a ~50 ks XMM-Newton X-ray observation of the open cluster NGC 752. For the sources with 2MASS counterparts, the values of their magnitudes in the J, H and K bands are also given. Additionally, for the sources with a Chandra counterpart (within a search radius of 5 arcsec), the values of their Chandra source number (as given in the related Browse table NGC752CXO) are also given. Very little is known about the evolution of stellar activity between the ages of the Hyades (0.8 Gyr) and the Sun (4.6 Gyr). To gain information on the typical level of coronal activity at a star's intermediate age, the authors have studied the X-ray emission from stars in the 1.9 Gyr-old open cluster NGC 752. They analysed a ~ 140 ks Chandra observation of NGC 752 and a ~50 ks XMM-Newton observation of the same cluster. They detected 262 X-ray sources in the Chandra data and 145 sources in the XMM-Newton observation. Around 90% of the catalogued cluster members within Chandra's field of view are detected in the X-ray observation. The X-ray luminosity of all observed cluster members (28 stars) and of 11 cluster member candidates was derived. These data indicate that, at an age of 1.9 Gyr, the typical X-ray luminosity L_x of the cluster members with masses of 0.8 to 1.2 solar masses is 1.3 x 10&lt;sup&gt;28&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, which is approximately a factor of 6 times less intense than that observed in the younger Hyades. Given that L_x is proportional to the square of a star's rotational rate, the median L_x of NGC 752 is consistent, for t &gt;= 1 Gyr, with a decaying rate in rotational velocities v_rot ~ t&lt;sup&gt;-alpha&lt;/sup&gt; with alpha ~ 0.75, steeper than the Skumanich relation (alpha ~ 0.5) and significantly steeper than that observed between the Pleiades and the Hyades (where alpha &lt;0.3), suggesting that a change in the rotational regimes of the stellar interiors is taking place at an age of ~ 1 Gyr. NGC 752 was observed for 49 ks by the XMM-Newton EPIC camera on February 5, 2003 starting at 23:29:25 UT, and the nominal pointing was towards J2000.0 RA and Declination of (01:57:38, +37:47:60), thus the XMM-Newton field-of-view (FOV) includes the Chandra FOV. For the source detection, the authors used the PWXDETECT code developed at Palermo Observatory and derived from the analogous Chandra PWDETECT code based on wavelet transform analysis. This allows the three EPIC exposures (PN, MOS1 and MOS2) to be combined in order to gain a deeper sensitivity with respect to the source detection based on single images. THere were 145 point sources detected in the energy band 0.5 - 2.0 keV. An extended source (not listed in this present table), very likely a galaxy cluster, is also visible in the EPIC data. The authors searched for 2MASS counterparts to the XMM-Newton sources using a search radius of 5 arcsec and found a counterpart for 38 sources. As for the Chandra data, all sources with a visible counterpart from DLM94 have also a 2MASS counterpart, so this leaves 15 XMM-Newton sources with a 2MASS counterpart and no counterpart in Daniel et al. (1994, PASP, 106, 281); of these, 3 were also detected by Chandra; of the other 12, 10 are outside the Chandra FOV, while two are within it (XMM-Newton sources 58 and 65). Source 65 was caught by XMM-Newton during the decay phase of a flare, which explains why it is not detected in the Chandra data. For source 58 there is no immediate explanation for this, since the light curve does not show evidence of a flare. No additional near-IR counterpart to the XMM-Newton sources was found within the Point Source Reject Table of the 2MASS Extended Mission.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/99/551 [1]</TD>
            <TD>BVI photometry of massive stars in M33 and M31 (Hunter+ 1995)</TD>
            <TD>We present BVI photometry of the massive stars in and around five Halpha shells in M33 and two in M31. These data can be used to statistically compare the stellar population with ionization and formation requirements of the gas shell. We have counted the numbers of massive stars encircled by the shells and embedded within the gaseous structures and corrected these numbers statistically for background and foreground interlopers. We find that the stellar production exceeds the ionization requirements of the nebulae by factors of 4-10. Thus, it is reasonable that the shells are photoionized and that a large fraction of the ionizing photons escape into the rest of the galaxy. We have also compared the number of massive stars counted and extrapolated to 7M_{sun}_ with the number required to form the shells according to a simple formation model. With one exception, we find that the number of stars estimated to be present exceeds the number required by the model for our assumptions of age and ambient gas density. This comparison and the morphology evident in Halpha images suggests that the modification of the interstellar medium by the massive stars in these regions has been far more complicated than is currently considered in formation models. There is evidence for multiple, and to some extent discreet, events in the production of the gas structures. A more detailed modeling will be necessary to adequately account for the stellar populations and Halpha morphology.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>02-Feb-1996</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/99/551</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/99/551 [2]</TD>
            <TD>BVI photometry of massive stars in M33 and M31 (Hunter+ 1995)</TD>
            <TD>We present BVI photometry of the massive stars in and around five Halpha shells in M33 and two in M31. These data can be used to statistically compare the stellar population with ionization and formation requirements of the gas shell. We have counted the numbers of massive stars encircled by the shells and embedded within the gaseous structures and corrected these numbers statistically for background and foreground interlopers. We find that the stellar production exceeds the ionization requirements of the nebulae by factors of 4-10. Thus, it is reasonable that the shells are photoionized and that a large fraction of the ionizing photons escape into the rest of the galaxy. We have also compared the number of massive stars counted and extrapolated to 7M_{sun}_ with the number required to form the shells according to a simple formation model. With one exception, we find that the number of stars estimated to be present exceeds the number required by the model for our assumptions of age and ambient gas density. This comparison and the morphology evident in Halpha images suggests that the modification of the interstellar medium by the massive stars in these regions has been far more complicated than is currently considered in formation models. There is evidence for multiple, and to some extent discreet, events in the production of the gas structures. A more detailed modeling will be necessary to adequately account for the stellar populations and Halpha morphology.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/551#2</TD>
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          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/464/201 [1]</TD>
            <TD>RGB stars in Sagittarius streams (Monaco+, 2007)</TD>
            <TD>Spectra were secured using different high resolution facilities: UVES@VLT, HARPS@3.6m, and SARG@TNG. Radial velocities are obtained through cross correlation with a template spectra. Concerning chemical analysis, for the various elements, selected line equivalent widths were measured and abundances computed using the WIDTH code and ATLAS model atmospheres. A total of 13 stars were observed between August 30, 2004, and January 24, 2005, using the SARG spectrograph mounted on the Telescopio Nazionale Galileo (TNG) telescope at La Palma. We present iron (Fe) and alpha-element (Mg, Ca) abundances for 12 red giant branch stars belonging to the Sagittarius dwarf spheroidal galaxy tidal streams. Spectra were obtained with the SARG spectrograph mounted at the Telescopio Nazionale Galileo (La Palma, Spain). We used the 1.6" slit, which provides a resolution of R=29000. For each star we report the equivalent widths (EWs) measured for a selected sample of Fe, Mg, and Ca lines along with the abundances derived for each line from the measured EWs and the adopted atomic parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T20:04:17Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
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            <TD>07-Apr-2007</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/464/201 [2]</TD>
            <TD>RGB stars in Sagittarius streams (Monaco+, 2007)</TD>
            <TD>Spectra were secured using different high resolution facilities: UVES@VLT, HARPS@3.6m, and SARG@TNG. Radial velocities are obtained through cross correlation with a template spectra. Concerning chemical analysis, for the various elements, selected line equivalent widths were measured and abundances computed using the WIDTH code and ATLAS model atmospheres. A total of 13 stars were observed between August 30, 2004, and January 24, 2005, using the SARG spectrograph mounted on the Telescopio Nazionale Galileo (TNG) telescope at La Palma. We present iron (Fe) and alpha-element (Mg, Ca) abundances for 12 red giant branch stars belonging to the Sagittarius dwarf spheroidal galaxy tidal streams. Spectra were obtained with the SARG spectrograph mounted at the Telescopio Nazionale Galileo (La Palma, Spain). We used the 1.6" slit, which provides a resolution of R=29000. For each star we report the equivalent widths (EWs) measured for a selected sample of Fe, Mg, and Ca lines along with the abundances derived for each line from the measured EWs and the adopted atomic parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201#2</TD>
            <TD>2011-09-14T20:04:17Z</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/201 [table1]</TD>
            <TD>RGB stars in Sagittarius streams (Monaco+, 2007)</TD>
            <TD>Spectra were secured using different high resolution facilities: UVES@VLT, HARPS@3.6m, and SARG@TNG. Radial velocities are obtained through cross correlation with a template spectra. Concerning chemical analysis, for the various elements, selected line equivalent widths were measured and abundances computed using the WIDTH code and ATLAS model atmospheres. A total of 13 stars were observed between August 30, 2004, and January 24, 2005, using the SARG spectrograph mounted on the Telescopio Nazionale Galileo (TNG) telescope at La Palma. We present iron (Fe) and alpha-element (Mg, Ca) abundances for 12 red giant branch stars belonging to the Sagittarius dwarf spheroidal galaxy tidal streams. Spectra were obtained with the SARG spectrograph mounted at the Telescopio Nazionale Galileo (La Palma, Spain). We used the 1.6" slit, which provides a resolution of R=29000. For each star we report the equivalent widths (EWs) measured for a selected sample of Fe, Mg, and Ca lines along with the abundances derived for each line from the measured EWs and the adopted atomic parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201#table1</TD>
            <TD>2011-09-14T20:04:17Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
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          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/464/201 [1]</TD>
            <TD>RGB stars in Sagittarius streams (Monaco+, 2007)</TD>
            <TD>Spectra were secured using different high resolution facilities: UVES@VLT, HARPS@3.6m, and SARG@TNG. Radial velocities are obtained through cross correlation with a template spectra. Concerning chemical analysis, for the various elements, selected line equivalent widths were measured and abundances computed using the WIDTH code and ATLAS model atmospheres. A total of 13 stars were observed between August 30, 2004, and January 24, 2005, using the SARG spectrograph mounted on the Telescopio Nazionale Galileo (TNG) telescope at La Palma. We present iron (Fe) and alpha-element (Mg, Ca) abundances for 12 red giant branch stars belonging to the Sagittarius dwarf spheroidal galaxy tidal streams. Spectra were obtained with the SARG spectrograph mounted at the Telescopio Nazionale Galileo (La Palma, Spain). We used the 1.6" slit, which provides a resolution of R=29000. For each star we report the equivalent widths (EWs) measured for a selected sample of Fe, Mg, and Ca lines along with the abundances derived for each line from the measured EWs and the adopted atomic parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T20:04:17Z</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/201</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/464/201 [2]</TD>
            <TD>RGB stars in Sagittarius streams (Monaco+, 2007)</TD>
            <TD>Spectra were secured using different high resolution facilities: UVES@VLT, HARPS@3.6m, and SARG@TNG. Radial velocities are obtained through cross correlation with a template spectra. Concerning chemical analysis, for the various elements, selected line equivalent widths were measured and abundances computed using the WIDTH code and ATLAS model atmospheres. A total of 13 stars were observed between August 30, 2004, and January 24, 2005, using the SARG spectrograph mounted on the Telescopio Nazionale Galileo (TNG) telescope at La Palma. We present iron (Fe) and alpha-element (Mg, Ca) abundances for 12 red giant branch stars belonging to the Sagittarius dwarf spheroidal galaxy tidal streams. Spectra were obtained with the SARG spectrograph mounted at the Telescopio Nazionale Galileo (La Palma, Spain). We used the 1.6" slit, which provides a resolution of R=29000. For each star we report the equivalent widths (EWs) measured for a selected sample of Fe, Mg, and Ca lines along with the abundances derived for each line from the measured EWs and the adopted atomic parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201#2</TD>
            <TD>2011-09-14T20:04:17Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/464/201&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/201 [table1]</TD>
            <TD>RGB stars in Sagittarius streams (Monaco+, 2007)</TD>
            <TD>Spectra were secured using different high resolution facilities: UVES@VLT, HARPS@3.6m, and SARG@TNG. Radial velocities are obtained through cross correlation with a template spectra. Concerning chemical analysis, for the various elements, selected line equivalent widths were measured and abundances computed using the WIDTH code and ATLAS model atmospheres. A total of 13 stars were observed between August 30, 2004, and January 24, 2005, using the SARG spectrograph mounted on the Telescopio Nazionale Galileo (TNG) telescope at La Palma. We present iron (Fe) and alpha-element (Mg, Ca) abundances for 12 red giant branch stars belonging to the Sagittarius dwarf spheroidal galaxy tidal streams. Spectra were obtained with the SARG spectrograph mounted at the Telescopio Nazionale Galileo (La Palma, Spain). We used the 1.6" slit, which provides a resolution of R=29000. For each star we report the equivalent widths (EWs) measured for a selected sample of Fe, Mg, and Ca lines along with the abundances derived for each line from the measured EWs and the adopted atomic parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201#table1</TD>
            <TD>2011-09-14T20:04:17Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/201</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/99/551 [1]</TD>
            <TD>BVI photometry of massive stars in M33 and M31 (Hunter+ 1995)</TD>
            <TD>We present BVI photometry of the massive stars in and around five Halpha shells in M33 and two in M31. These data can be used to statistically compare the stellar population with ionization and formation requirements of the gas shell. We have counted the numbers of massive stars encircled by the shells and embedded within the gaseous structures and corrected these numbers statistically for background and foreground interlopers. We find that the stellar production exceeds the ionization requirements of the nebulae by factors of 4-10. Thus, it is reasonable that the shells are photoionized and that a large fraction of the ionizing photons escape into the rest of the galaxy. We have also compared the number of massive stars counted and extrapolated to 7M_{sun}_ with the number required to form the shells according to a simple formation model. With one exception, we find that the number of stars estimated to be present exceeds the number required by the model for our assumptions of age and ambient gas density. This comparison and the morphology evident in Halpha images suggests that the modification of the interstellar medium by the massive stars in these regions has been far more complicated than is currently considered in formation models. There is evidence for multiple, and to some extent discreet, events in the production of the gas structures. A more detailed modeling will be necessary to adequately account for the stellar populations and Halpha morphology.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/551#1</TD>
            <TD>2011-09-14T18:37:36Z</TD>
            <TD>#Photometry#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/551</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/99/551</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/99/551</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/99/551 [2]</TD>
            <TD>BVI photometry of massive stars in M33 and M31 (Hunter+ 1995)</TD>
            <TD>We present BVI photometry of the massive stars in and around five Halpha shells in M33 and two in M31. These data can be used to statistically compare the stellar population with ionization and formation requirements of the gas shell. We have counted the numbers of massive stars encircled by the shells and embedded within the gaseous structures and corrected these numbers statistically for background and foreground interlopers. We find that the stellar production exceeds the ionization requirements of the nebulae by factors of 4-10. Thus, it is reasonable that the shells are photoionized and that a large fraction of the ionizing photons escape into the rest of the galaxy. We have also compared the number of massive stars counted and extrapolated to 7M_{sun}_ with the number required to form the shells according to a simple formation model. With one exception, we find that the number of stars estimated to be present exceeds the number required by the model for our assumptions of age and ambient gas density. This comparison and the morphology evident in Halpha images suggests that the modification of the interstellar medium by the massive stars in these regions has been far more complicated than is currently considered in formation models. There is evidence for multiple, and to some extent discreet, events in the production of the gas structures. A more detailed modeling will be necessary to adequately account for the stellar populations and Halpha morphology.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/551#2</TD>
            <TD>2011-09-14T18:37:36Z</TD>
            <TD>#Photometry#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/551</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/99/551&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/99/551</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/464/201 [1]</TD>
            <TD>RGB stars in Sagittarius streams (Monaco+, 2007)</TD>
            <TD>Spectra were secured using different high resolution facilities: UVES@VLT, HARPS@3.6m, and SARG@TNG. Radial velocities are obtained through cross correlation with a template spectra. Concerning chemical analysis, for the various elements, selected line equivalent widths were measured and abundances computed using the WIDTH code and ATLAS model atmospheres. A total of 13 stars were observed between August 30, 2004, and January 24, 2005, using the SARG spectrograph mounted on the Telescopio Nazionale Galileo (TNG) telescope at La Palma. We present iron (Fe) and alpha-element (Mg, Ca) abundances for 12 red giant branch stars belonging to the Sagittarius dwarf spheroidal galaxy tidal streams. Spectra were obtained with the SARG spectrograph mounted at the Telescopio Nazionale Galileo (La Palma, Spain). We used the 1.6" slit, which provides a resolution of R=29000. For each star we report the equivalent widths (EWs) measured for a selected sample of Fe, Mg, and Ca lines along with the abundances derived for each line from the measured EWs and the adopted atomic parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201#1</TD>
            <TD>2011-09-14T20:04:17Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/464/201</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/201</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/464/201 [2]</TD>
            <TD>RGB stars in Sagittarius streams (Monaco+, 2007)</TD>
            <TD>Spectra were secured using different high resolution facilities: UVES@VLT, HARPS@3.6m, and SARG@TNG. Radial velocities are obtained through cross correlation with a template spectra. Concerning chemical analysis, for the various elements, selected line equivalent widths were measured and abundances computed using the WIDTH code and ATLAS model atmospheres. A total of 13 stars were observed between August 30, 2004, and January 24, 2005, using the SARG spectrograph mounted on the Telescopio Nazionale Galileo (TNG) telescope at La Palma. We present iron (Fe) and alpha-element (Mg, Ca) abundances for 12 red giant branch stars belonging to the Sagittarius dwarf spheroidal galaxy tidal streams. Spectra were obtained with the SARG spectrograph mounted at the Telescopio Nazionale Galileo (La Palma, Spain). We used the 1.6" slit, which provides a resolution of R=29000. For each star we report the equivalent widths (EWs) measured for a selected sample of Fe, Mg, and Ca lines along with the abundances derived for each line from the measured EWs and the adopted atomic parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201#2</TD>
            <TD>2011-09-14T20:04:17Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/464/201&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/201 [table1]</TD>
            <TD>RGB stars in Sagittarius streams (Monaco+, 2007)</TD>
            <TD>Spectra were secured using different high resolution facilities: UVES@VLT, HARPS@3.6m, and SARG@TNG. Radial velocities are obtained through cross correlation with a template spectra. Concerning chemical analysis, for the various elements, selected line equivalent widths were measured and abundances computed using the WIDTH code and ATLAS model atmospheres. A total of 13 stars were observed between August 30, 2004, and January 24, 2005, using the SARG spectrograph mounted on the Telescopio Nazionale Galileo (TNG) telescope at La Palma. We present iron (Fe) and alpha-element (Mg, Ca) abundances for 12 red giant branch stars belonging to the Sagittarius dwarf spheroidal galaxy tidal streams. Spectra were obtained with the SARG spectrograph mounted at the Telescopio Nazionale Galileo (La Palma, Spain). We used the 1.6" slit, which provides a resolution of R=29000. For each star we report the equivalent widths (EWs) measured for a selected sample of Fe, Mg, and Ca lines along with the abundances derived for each line from the measured EWs and the adopted atomic parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201#table1</TD>
            <TD>2011-09-14T20:04:17Z</TD>
            <TD>#Abundances#Stars#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/201</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/905 [1]</TD>
            <TD>HII regions in NGC 628 (Fathi+, 2007)</TD>
            <TD>Complete list of the 376 photometrically calibrated individual HII regions in the spiral galaxy NGC 628.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905#1</TD>
            <TD>2011-09-14T20:04:38Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/905 [2]</TD>
            <TD>HII regions in NGC 628 (Fathi+, 2007)</TD>
            <TD>Complete list of the 376 photometrically calibrated individual HII regions in the spiral galaxy NGC 628.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905#2</TD>
            <TD>2011-09-14T20:04:38Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/905 [table]</TD>
            <TD>HII regions in NGC 628 (Fathi+, 2007)</TD>
            <TD>Complete list of the 376 photometrically calibrated individual HII regions in the spiral galaxy NGC 628.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905#table</TD>
            <TD>2011-09-14T20:04:38Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/211/637 [1]</TD>
            <TD>Abell 85 CCD observations (Murphy 1984)</TD>
            <TD>A CCD camera survey has been conducted of the X-ray emitting regions of a sample of clusters of galaxies. This sample includes at least one cluster from each of the classes in the new Forman-Jones classification scheme (Forman &amp; Jones 1982ARA&amp;A..20..547F). In this paper, the techniques used to obtain, reduce and analyse the data are presented, along with results for the cluster Abell 85. For the central X-ray emitting region of this cluster, a core radius of between 1.2 and 1.6Mpc is estimated from the galaxy radial number density distribution. The properties of the galaxies in the core of this cluster are significantly different from those of the galaxies in the outer regions of the area covered in the survey, in terms of luminosity function and colour distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/211/637#1</TD>
            <TD>2011-09-14T18:37:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/211/637</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/211/637</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/211/637</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/211/637 [2]</TD>
            <TD>Abell 85 CCD observations (Murphy 1984)</TD>
            <TD>A CCD camera survey has been conducted of the X-ray emitting regions of a sample of clusters of galaxies. This sample includes at least one cluster from each of the classes in the new Forman-Jones classification scheme (Forman &amp; Jones 1982ARA&amp;A..20..547F). In this paper, the techniques used to obtain, reduce and analyse the data are presented, along with results for the cluster Abell 85. For the central X-ray emitting region of this cluster, a core radius of between 1.2 and 1.6Mpc is estimated from the galaxy radial number density distribution. The properties of the galaxies in the core of this cluster are significantly different from those of the galaxies in the outer regions of the area covered in the survey, in terms of luminosity function and colour distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/211/637#2</TD>
            <TD>2011-09-14T18:37:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/211/637</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/211/637&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/211/637</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/905 [1]</TD>
            <TD>HII regions in NGC 628 (Fathi+, 2007)</TD>
            <TD>Complete list of the 376 photometrically calibrated individual HII regions in the spiral galaxy NGC 628.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905#1</TD>
            <TD>2011-09-14T20:04:38Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/905 [2]</TD>
            <TD>HII regions in NGC 628 (Fathi+, 2007)</TD>
            <TD>Complete list of the 376 photometrically calibrated individual HII regions in the spiral galaxy NGC 628.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905#2</TD>
            <TD>2011-09-14T20:04:38Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/905 [table]</TD>
            <TD>HII regions in NGC 628 (Fathi+, 2007)</TD>
            <TD>Complete list of the 376 photometrically calibrated individual HII regions in the spiral galaxy NGC 628.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905#table</TD>
            <TD>2011-09-14T20:04:38Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/211/637 [1]</TD>
            <TD>Abell 85 CCD observations (Murphy 1984)</TD>
            <TD>A CCD camera survey has been conducted of the X-ray emitting regions of a sample of clusters of galaxies. This sample includes at least one cluster from each of the classes in the new Forman-Jones classification scheme (Forman &amp; Jones 1982ARA&amp;A..20..547F). In this paper, the techniques used to obtain, reduce and analyse the data are presented, along with results for the cluster Abell 85. For the central X-ray emitting region of this cluster, a core radius of between 1.2 and 1.6Mpc is estimated from the galaxy radial number density distribution. The properties of the galaxies in the core of this cluster are significantly different from those of the galaxies in the outer regions of the area covered in the survey, in terms of luminosity function and colour distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/211/637#1</TD>
            <TD>2011-09-14T18:37:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/211/637</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/211/637</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/211/637</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/211/637 [2]</TD>
            <TD>Abell 85 CCD observations (Murphy 1984)</TD>
            <TD>A CCD camera survey has been conducted of the X-ray emitting regions of a sample of clusters of galaxies. This sample includes at least one cluster from each of the classes in the new Forman-Jones classification scheme (Forman &amp; Jones 1982ARA&amp;A..20..547F). In this paper, the techniques used to obtain, reduce and analyse the data are presented, along with results for the cluster Abell 85. For the central X-ray emitting region of this cluster, a core radius of between 1.2 and 1.6Mpc is estimated from the galaxy radial number density distribution. The properties of the galaxies in the core of this cluster are significantly different from those of the galaxies in the outer regions of the area covered in the survey, in terms of luminosity function and colour distribution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/211/637#2</TD>
            <TD>2011-09-14T18:37:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/211/637</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/211/637&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/211/637</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/905 [1]</TD>
            <TD>HII regions in NGC 628 (Fathi+, 2007)</TD>
            <TD>Complete list of the 376 photometrically calibrated individual HII regions in the spiral galaxy NGC 628.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905#1</TD>
            <TD>2011-09-14T20:04:38Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/905 [2]</TD>
            <TD>HII regions in NGC 628 (Fathi+, 2007)</TD>
            <TD>Complete list of the 376 photometrically calibrated individual HII regions in the spiral galaxy NGC 628.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905#2</TD>
            <TD>2011-09-14T20:04:38Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/905 [table]</TD>
            <TD>HII regions in NGC 628 (Fathi+, 2007)</TD>
            <TD>Complete list of the 376 photometrically calibrated individual HII regions in the spiral galaxy NGC 628.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905#table</TD>
            <TD>2011-09-14T20:04:38Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/445/819 [1]</TD>
            <TD>Systems of galaxies in Shapley supercluster (Ragone+, 2006)</TD>
            <TD>Based on the largest compilation of galaxies with redshift in the region of the Shapley Supercluster (Proust et al., 2004 in prep., 2006A&amp;A...447..133P), we identified 122 galaxy systems, 60 of which are new systems. Using the SuperCOSMOS catalogue, we have assigned b_j_ magnitudes to each galaxy in our compilation. The sample of galaxy systems was used to estimate the mass function of systems in the range 10^13^ to 10^15^M_{sun}/h^-1^. We computed a lower value to the total mass in the region of the Shapley Supercluster with this mass function. Using 15 mock catalogues we derived the mean mass that these kinds of systems have before comparing it with that obtained from the real data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819#1</TD>
            <TD>2011-09-14T20:00:49Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/445/819</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/819</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/445/819 [2]</TD>
            <TD>Systems of galaxies in Shapley supercluster (Ragone+, 2006)</TD>
            <TD>Based on the largest compilation of galaxies with redshift in the region of the Shapley Supercluster (Proust et al., 2004 in prep., 2006A&amp;A...447..133P), we identified 122 galaxy systems, 60 of which are new systems. Using the SuperCOSMOS catalogue, we have assigned b_j_ magnitudes to each galaxy in our compilation. The sample of galaxy systems was used to estimate the mass function of systems in the range 10^13^ to 10^15^M_{sun}/h^-1^. We computed a lower value to the total mass in the region of the Shapley Supercluster with this mass function. Using 15 mock catalogues we derived the mean mass that these kinds of systems have before comparing it with that obtained from the real data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819#2</TD>
            <TD>2011-09-14T20:00:49Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/445/819&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/819</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/445/819 [table1]</TD>
            <TD>Systems of galaxies in Shapley supercluster (Ragone+, 2006)</TD>
            <TD>Based on the largest compilation of galaxies with redshift in the region of the Shapley Supercluster (Proust et al., 2004 in prep., 2006A&amp;A...447..133P), we identified 122 galaxy systems, 60 of which are new systems. Using the SuperCOSMOS catalogue, we have assigned b_j_ magnitudes to each galaxy in our compilation. The sample of galaxy systems was used to estimate the mass function of systems in the range 10^13^ to 10^15^M_{sun}/h^-1^. We computed a lower value to the total mass in the region of the Shapley Supercluster with this mass function. Using 15 mock catalogues we derived the mean mass that these kinds of systems have before comparing it with that obtained from the real data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819#table1</TD>
            <TD>2011-09-14T20:00:49Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/445/819&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/819</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC752XMM [1]</TD>
            <TD>NGC 752 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table provides a list of X-ray sources detected in a ~50 ks XMM-Newton X-ray observation of the open cluster NGC 752. For the sources with 2MASS counterparts, the values of their magnitudes in the J, H and K bands are also given. Additionally, for the sources with a Chandra counterpart (within a search radius of 5 arcsec), the values of their Chandra source number (as given in the related Browse table NGC752CXO) are also given. Very little is known about the evolution of stellar activity between the ages of the Hyades (0.8 Gyr) and the Sun (4.6 Gyr). To gain information on the typical level of coronal activity at a star's intermediate age, the authors have studied the X-ray emission from stars in the 1.9 Gyr-old open cluster NGC 752. They analysed a ~ 140 ks Chandra observation of NGC 752 and a ~50 ks XMM-Newton observation of the same cluster. They detected 262 X-ray sources in the Chandra data and 145 sources in the XMM-Newton observation. Around 90% of the catalogued cluster members within Chandra's field of view are detected in the X-ray observation. The X-ray luminosity of all observed cluster members (28 stars) and of 11 cluster member candidates was derived. These data indicate that, at an age of 1.9 Gyr, the typical X-ray luminosity L_x of the cluster members with masses of 0.8 to 1.2 solar masses is 1.3 x 10&lt;sup&gt;28&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, which is approximately a factor of 6 times less intense than that observed in the younger Hyades. Given that L_x is proportional to the square of a star's rotational rate, the median L_x of NGC 752 is consistent, for t &gt;= 1 Gyr, with a decaying rate in rotational velocities v_rot ~ t&lt;sup&gt;-alpha&lt;/sup&gt; with alpha ~ 0.75, steeper than the Skumanich relation (alpha ~ 0.5) and significantly steeper than that observed between the Pleiades and the Hyades (where alpha &lt;0.3), suggesting that a change in the rotational regimes of the stellar interiors is taking place at an age of ~ 1 Gyr. NGC 752 was observed for 49 ks by the XMM-Newton EPIC camera on February 5, 2003 starting at 23:29:25 UT, and the nominal pointing was towards J2000.0 RA and Declination of (01:57:38, +37:47:60), thus the XMM-Newton field-of-view (FOV) includes the Chandra FOV. For the source detection, the authors used the PWXDETECT code developed at Palermo Observatory and derived from the analogous Chandra PWDETECT code based on wavelet transform analysis. This allows the three EPIC exposures (PN, MOS1 and MOS2) to be combined in order to gain a deeper sensitivity with respect to the source detection based on single images. THere were 145 point sources detected in the energy band 0.5 - 2.0 keV. An extended source (not listed in this present table), very likely a galaxy cluster, is also visible in the EPIC data. The authors searched for 2MASS counterparts to the XMM-Newton sources using a search radius of 5 arcsec and found a counterpart for 38 sources. As for the Chandra data, all sources with a visible counterpart from DLM94 have also a 2MASS counterpart, so this leaves 15 XMM-Newton sources with a 2MASS counterpart and no counterpart in Daniel et al. (1994, PASP, 106, 281); of these, 3 were also detected by Chandra; of the other 12, 10 are outside the Chandra FOV, while two are within it (XMM-Newton sources 58 and 65). Source 65 was caught by XMM-Newton during the decay phase of a flare, which explains why it is not detected in the Chandra data. For source 58 there is no immediate explanation for this, since the light curve does not show evidence of a flare. No additional near-IR counterpart to the XMM-Newton sources was found within the Point Source Reject Table of the 2MASS Extended Mission.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc752xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc752xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc752xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc752xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC752XMM [2]</TD>
            <TD>NGC 752 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table provides a list of X-ray sources detected in a ~50 ks XMM-Newton X-ray observation of the open cluster NGC 752. For the sources with 2MASS counterparts, the values of their magnitudes in the J, H and K bands are also given. Additionally, for the sources with a Chandra counterpart (within a search radius of 5 arcsec), the values of their Chandra source number (as given in the related Browse table NGC752CXO) are also given. Very little is known about the evolution of stellar activity between the ages of the Hyades (0.8 Gyr) and the Sun (4.6 Gyr). To gain information on the typical level of coronal activity at a star's intermediate age, the authors have studied the X-ray emission from stars in the 1.9 Gyr-old open cluster NGC 752. They analysed a ~ 140 ks Chandra observation of NGC 752 and a ~50 ks XMM-Newton observation of the same cluster. They detected 262 X-ray sources in the Chandra data and 145 sources in the XMM-Newton observation. Around 90% of the catalogued cluster members within Chandra's field of view are detected in the X-ray observation. The X-ray luminosity of all observed cluster members (28 stars) and of 11 cluster member candidates was derived. These data indicate that, at an age of 1.9 Gyr, the typical X-ray luminosity L_x of the cluster members with masses of 0.8 to 1.2 solar masses is 1.3 x 10&lt;sup&gt;28&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, which is approximately a factor of 6 times less intense than that observed in the younger Hyades. Given that L_x is proportional to the square of a star's rotational rate, the median L_x of NGC 752 is consistent, for t &gt;= 1 Gyr, with a decaying rate in rotational velocities v_rot ~ t&lt;sup&gt;-alpha&lt;/sup&gt; with alpha ~ 0.75, steeper than the Skumanich relation (alpha ~ 0.5) and significantly steeper than that observed between the Pleiades and the Hyades (where alpha &lt;0.3), suggesting that a change in the rotational regimes of the stellar interiors is taking place at an age of ~ 1 Gyr. NGC 752 was observed for 49 ks by the XMM-Newton EPIC camera on February 5, 2003 starting at 23:29:25 UT, and the nominal pointing was towards J2000.0 RA and Declination of (01:57:38, +37:47:60), thus the XMM-Newton field-of-view (FOV) includes the Chandra FOV. For the source detection, the authors used the PWXDETECT code developed at Palermo Observatory and derived from the analogous Chandra PWDETECT code based on wavelet transform analysis. This allows the three EPIC exposures (PN, MOS1 and MOS2) to be combined in order to gain a deeper sensitivity with respect to the source detection based on single images. THere were 145 point sources detected in the energy band 0.5 - 2.0 keV. An extended source (not listed in this present table), very likely a galaxy cluster, is also visible in the EPIC data. The authors searched for 2MASS counterparts to the XMM-Newton sources using a search radius of 5 arcsec and found a counterpart for 38 sources. As for the Chandra data, all sources with a visible counterpart from DLM94 have also a 2MASS counterpart, so this leaves 15 XMM-Newton sources with a 2MASS counterpart and no counterpart in Daniel et al. (1994, PASP, 106, 281); of these, 3 were also detected by Chandra; of the other 12, 10 are outside the Chandra FOV, while two are within it (XMM-Newton sources 58 and 65). Source 65 was caught by XMM-Newton during the decay phase of a flare, which explains why it is not detected in the Chandra data. For source 58 there is no immediate explanation for this, since the light curve does not show evidence of a flare. No additional near-IR counterpart to the XMM-Newton sources was found within the Point Source Reject Table of the 2MASS Extended Mission.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc752xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc752xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc752xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc752xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC752XMM [3]</TD>
            <TD>NGC 752 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table provides a list of X-ray sources detected in a ~50 ks XMM-Newton X-ray observation of the open cluster NGC 752. For the sources with 2MASS counterparts, the values of their magnitudes in the J, H and K bands are also given. Additionally, for the sources with a Chandra counterpart (within a search radius of 5 arcsec), the values of their Chandra source number (as given in the related Browse table NGC752CXO) are also given. Very little is known about the evolution of stellar activity between the ages of the Hyades (0.8 Gyr) and the Sun (4.6 Gyr). To gain information on the typical level of coronal activity at a star's intermediate age, the authors have studied the X-ray emission from stars in the 1.9 Gyr-old open cluster NGC 752. They analysed a ~ 140 ks Chandra observation of NGC 752 and a ~50 ks XMM-Newton observation of the same cluster. They detected 262 X-ray sources in the Chandra data and 145 sources in the XMM-Newton observation. Around 90% of the catalogued cluster members within Chandra's field of view are detected in the X-ray observation. The X-ray luminosity of all observed cluster members (28 stars) and of 11 cluster member candidates was derived. These data indicate that, at an age of 1.9 Gyr, the typical X-ray luminosity L_x of the cluster members with masses of 0.8 to 1.2 solar masses is 1.3 x 10&lt;sup&gt;28&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, which is approximately a factor of 6 times less intense than that observed in the younger Hyades. Given that L_x is proportional to the square of a star's rotational rate, the median L_x of NGC 752 is consistent, for t &gt;= 1 Gyr, with a decaying rate in rotational velocities v_rot ~ t&lt;sup&gt;-alpha&lt;/sup&gt; with alpha ~ 0.75, steeper than the Skumanich relation (alpha ~ 0.5) and significantly steeper than that observed between the Pleiades and the Hyades (where alpha &lt;0.3), suggesting that a change in the rotational regimes of the stellar interiors is taking place at an age of ~ 1 Gyr. NGC 752 was observed for 49 ks by the XMM-Newton EPIC camera on February 5, 2003 starting at 23:29:25 UT, and the nominal pointing was towards J2000.0 RA and Declination of (01:57:38, +37:47:60), thus the XMM-Newton field-of-view (FOV) includes the Chandra FOV. For the source detection, the authors used the PWXDETECT code developed at Palermo Observatory and derived from the analogous Chandra PWDETECT code based on wavelet transform analysis. This allows the three EPIC exposures (PN, MOS1 and MOS2) to be combined in order to gain a deeper sensitivity with respect to the source detection based on single images. THere were 145 point sources detected in the energy band 0.5 - 2.0 keV. An extended source (not listed in this present table), very likely a galaxy cluster, is also visible in the EPIC data. The authors searched for 2MASS counterparts to the XMM-Newton sources using a search radius of 5 arcsec and found a counterpart for 38 sources. As for the Chandra data, all sources with a visible counterpart from DLM94 have also a 2MASS counterpart, so this leaves 15 XMM-Newton sources with a 2MASS counterpart and no counterpart in Daniel et al. (1994, PASP, 106, 281); of these, 3 were also detected by Chandra; of the other 12, 10 are outside the Chandra FOV, while two are within it (XMM-Newton sources 58 and 65). Source 65 was caught by XMM-Newton during the decay phase of a flare, which explains why it is not detected in the Chandra data. For source 58 there is no immediate explanation for this, since the light curve does not show evidence of a flare. No additional near-IR counterpart to the XMM-Newton sources was found within the Point Source Reject Table of the 2MASS Extended Mission.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc752xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc752xmm</TD>
            <TD />
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            <TD>J/A+A/434/483 [1]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
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            <TD />
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/434/483</TD>
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            <TD>HTTP Request</TD>
            <TD>J/A+A/434/483 [2]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
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            <TD>J/A+A/434/483 [table2]</TD>
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            <TD>CDS</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>ParamHTTP</TD>
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            <TD>J/A+A/434/483 [table1]</TD>
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            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>ParamHTTP</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/434/483 [1]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
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            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/434/483</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/434/483</TD>
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            <TD>HTTP Request</TD>
            <TD>J/A+A/434/483 [2]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
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            <TD>ParamHTTP</TD>
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            <TD>J/A+A/434/483 [table2]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>Catalog</TD>
            <TD>J/A+A/434/483 [table1]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>J/A+A/445/819 [1]</TD>
            <TD>Systems of galaxies in Shapley supercluster (Ragone+, 2006)</TD>
            <TD>Based on the largest compilation of galaxies with redshift in the region of the Shapley Supercluster (Proust et al., 2004 in prep., 2006A&amp;A...447..133P), we identified 122 galaxy systems, 60 of which are new systems. Using the SuperCOSMOS catalogue, we have assigned b_j_ magnitudes to each galaxy in our compilation. The sample of galaxy systems was used to estimate the mass function of systems in the range 10^13^ to 10^15^M_{sun}/h^-1^. We computed a lower value to the total mass in the region of the Shapley Supercluster with this mass function. Using 15 mock catalogues we derived the mean mass that these kinds of systems have before comparing it with that obtained from the real data.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/445/819</TD>
            <TD />
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/445/819</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/819</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/445/819 [2]</TD>
            <TD>Systems of galaxies in Shapley supercluster (Ragone+, 2006)</TD>
            <TD>Based on the largest compilation of galaxies with redshift in the region of the Shapley Supercluster (Proust et al., 2004 in prep., 2006A&amp;A...447..133P), we identified 122 galaxy systems, 60 of which are new systems. Using the SuperCOSMOS catalogue, we have assigned b_j_ magnitudes to each galaxy in our compilation. The sample of galaxy systems was used to estimate the mass function of systems in the range 10^13^ to 10^15^M_{sun}/h^-1^. We computed a lower value to the total mass in the region of the Shapley Supercluster with this mass function. Using 15 mock catalogues we derived the mean mass that these kinds of systems have before comparing it with that obtained from the real data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819#2</TD>
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            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/445/819&amp;</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/445/819 [table1]</TD>
            <TD>Systems of galaxies in Shapley supercluster (Ragone+, 2006)</TD>
            <TD>Based on the largest compilation of galaxies with redshift in the region of the Shapley Supercluster (Proust et al., 2004 in prep., 2006A&amp;A...447..133P), we identified 122 galaxy systems, 60 of which are new systems. Using the SuperCOSMOS catalogue, we have assigned b_j_ magnitudes to each galaxy in our compilation. The sample of galaxy systems was used to estimate the mass function of systems in the range 10^13^ to 10^15^M_{sun}/h^-1^. We computed a lower value to the total mass in the region of the Shapley Supercluster with this mass function. Using 15 mock catalogues we derived the mean mass that these kinds of systems have before comparing it with that obtained from the real data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819#table1</TD>
            <TD>2011-09-14T20:00:49Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
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            <TD>14-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/819</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/819</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC752XMM [1]</TD>
            <TD>NGC 752 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table provides a list of X-ray sources detected in a ~50 ks XMM-Newton X-ray observation of the open cluster NGC 752. For the sources with 2MASS counterparts, the values of their magnitudes in the J, H and K bands are also given. Additionally, for the sources with a Chandra counterpart (within a search radius of 5 arcsec), the values of their Chandra source number (as given in the related Browse table NGC752CXO) are also given. Very little is known about the evolution of stellar activity between the ages of the Hyades (0.8 Gyr) and the Sun (4.6 Gyr). To gain information on the typical level of coronal activity at a star's intermediate age, the authors have studied the X-ray emission from stars in the 1.9 Gyr-old open cluster NGC 752. They analysed a ~ 140 ks Chandra observation of NGC 752 and a ~50 ks XMM-Newton observation of the same cluster. They detected 262 X-ray sources in the Chandra data and 145 sources in the XMM-Newton observation. Around 90% of the catalogued cluster members within Chandra's field of view are detected in the X-ray observation. The X-ray luminosity of all observed cluster members (28 stars) and of 11 cluster member candidates was derived. These data indicate that, at an age of 1.9 Gyr, the typical X-ray luminosity L_x of the cluster members with masses of 0.8 to 1.2 solar masses is 1.3 x 10&lt;sup&gt;28&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, which is approximately a factor of 6 times less intense than that observed in the younger Hyades. Given that L_x is proportional to the square of a star's rotational rate, the median L_x of NGC 752 is consistent, for t &gt;= 1 Gyr, with a decaying rate in rotational velocities v_rot ~ t&lt;sup&gt;-alpha&lt;/sup&gt; with alpha ~ 0.75, steeper than the Skumanich relation (alpha ~ 0.5) and significantly steeper than that observed between the Pleiades and the Hyades (where alpha &lt;0.3), suggesting that a change in the rotational regimes of the stellar interiors is taking place at an age of ~ 1 Gyr. NGC 752 was observed for 49 ks by the XMM-Newton EPIC camera on February 5, 2003 starting at 23:29:25 UT, and the nominal pointing was towards J2000.0 RA and Declination of (01:57:38, +37:47:60), thus the XMM-Newton field-of-view (FOV) includes the Chandra FOV. For the source detection, the authors used the PWXDETECT code developed at Palermo Observatory and derived from the analogous Chandra PWDETECT code based on wavelet transform analysis. This allows the three EPIC exposures (PN, MOS1 and MOS2) to be combined in order to gain a deeper sensitivity with respect to the source detection based on single images. THere were 145 point sources detected in the energy band 0.5 - 2.0 keV. An extended source (not listed in this present table), very likely a galaxy cluster, is also visible in the EPIC data. The authors searched for 2MASS counterparts to the XMM-Newton sources using a search radius of 5 arcsec and found a counterpart for 38 sources. As for the Chandra data, all sources with a visible counterpart from DLM94 have also a 2MASS counterpart, so this leaves 15 XMM-Newton sources with a 2MASS counterpart and no counterpart in Daniel et al. (1994, PASP, 106, 281); of these, 3 were also detected by Chandra; of the other 12, 10 are outside the Chandra FOV, while two are within it (XMM-Newton sources 58 and 65). Source 65 was caught by XMM-Newton during the decay phase of a flare, which explains why it is not detected in the Chandra data. For source 58 there is no immediate explanation for this, since the light curve does not show evidence of a flare. No additional near-IR counterpart to the XMM-Newton sources was found within the Point Source Reject Table of the 2MASS Extended Mission.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc752xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ConeSearch</TD>
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            <TD>ParamHTTP</TD>
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            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc752xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC752XMM [2]</TD>
            <TD>NGC 752 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table provides a list of X-ray sources detected in a ~50 ks XMM-Newton X-ray observation of the open cluster NGC 752. For the sources with 2MASS counterparts, the values of their magnitudes in the J, H and K bands are also given. Additionally, for the sources with a Chandra counterpart (within a search radius of 5 arcsec), the values of their Chandra source number (as given in the related Browse table NGC752CXO) are also given. Very little is known about the evolution of stellar activity between the ages of the Hyades (0.8 Gyr) and the Sun (4.6 Gyr). To gain information on the typical level of coronal activity at a star's intermediate age, the authors have studied the X-ray emission from stars in the 1.9 Gyr-old open cluster NGC 752. They analysed a ~ 140 ks Chandra observation of NGC 752 and a ~50 ks XMM-Newton observation of the same cluster. They detected 262 X-ray sources in the Chandra data and 145 sources in the XMM-Newton observation. Around 90% of the catalogued cluster members within Chandra's field of view are detected in the X-ray observation. The X-ray luminosity of all observed cluster members (28 stars) and of 11 cluster member candidates was derived. These data indicate that, at an age of 1.9 Gyr, the typical X-ray luminosity L_x of the cluster members with masses of 0.8 to 1.2 solar masses is 1.3 x 10&lt;sup&gt;28&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, which is approximately a factor of 6 times less intense than that observed in the younger Hyades. Given that L_x is proportional to the square of a star's rotational rate, the median L_x of NGC 752 is consistent, for t &gt;= 1 Gyr, with a decaying rate in rotational velocities v_rot ~ t&lt;sup&gt;-alpha&lt;/sup&gt; with alpha ~ 0.75, steeper than the Skumanich relation (alpha ~ 0.5) and significantly steeper than that observed between the Pleiades and the Hyades (where alpha &lt;0.3), suggesting that a change in the rotational regimes of the stellar interiors is taking place at an age of ~ 1 Gyr. NGC 752 was observed for 49 ks by the XMM-Newton EPIC camera on February 5, 2003 starting at 23:29:25 UT, and the nominal pointing was towards J2000.0 RA and Declination of (01:57:38, +37:47:60), thus the XMM-Newton field-of-view (FOV) includes the Chandra FOV. For the source detection, the authors used the PWXDETECT code developed at Palermo Observatory and derived from the analogous Chandra PWDETECT code based on wavelet transform analysis. This allows the three EPIC exposures (PN, MOS1 and MOS2) to be combined in order to gain a deeper sensitivity with respect to the source detection based on single images. THere were 145 point sources detected in the energy band 0.5 - 2.0 keV. An extended source (not listed in this present table), very likely a galaxy cluster, is also visible in the EPIC data. The authors searched for 2MASS counterparts to the XMM-Newton sources using a search radius of 5 arcsec and found a counterpart for 38 sources. As for the Chandra data, all sources with a visible counterpart from DLM94 have also a 2MASS counterpart, so this leaves 15 XMM-Newton sources with a 2MASS counterpart and no counterpart in Daniel et al. (1994, PASP, 106, 281); of these, 3 were also detected by Chandra; of the other 12, 10 are outside the Chandra FOV, while two are within it (XMM-Newton sources 58 and 65). Source 65 was caught by XMM-Newton during the decay phase of a flare, which explains why it is not detected in the Chandra data. For source 58 there is no immediate explanation for this, since the light curve does not show evidence of a flare. No additional near-IR counterpart to the XMM-Newton sources was found within the Point Source Reject Table of the 2MASS Extended Mission.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc752xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc752xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC752XMM [3]</TD>
            <TD>NGC 752 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table provides a list of X-ray sources detected in a ~50 ks XMM-Newton X-ray observation of the open cluster NGC 752. For the sources with 2MASS counterparts, the values of their magnitudes in the J, H and K bands are also given. Additionally, for the sources with a Chandra counterpart (within a search radius of 5 arcsec), the values of their Chandra source number (as given in the related Browse table NGC752CXO) are also given. Very little is known about the evolution of stellar activity between the ages of the Hyades (0.8 Gyr) and the Sun (4.6 Gyr). To gain information on the typical level of coronal activity at a star's intermediate age, the authors have studied the X-ray emission from stars in the 1.9 Gyr-old open cluster NGC 752. They analysed a ~ 140 ks Chandra observation of NGC 752 and a ~50 ks XMM-Newton observation of the same cluster. They detected 262 X-ray sources in the Chandra data and 145 sources in the XMM-Newton observation. Around 90% of the catalogued cluster members within Chandra's field of view are detected in the X-ray observation. The X-ray luminosity of all observed cluster members (28 stars) and of 11 cluster member candidates was derived. These data indicate that, at an age of 1.9 Gyr, the typical X-ray luminosity L_x of the cluster members with masses of 0.8 to 1.2 solar masses is 1.3 x 10&lt;sup&gt;28&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, which is approximately a factor of 6 times less intense than that observed in the younger Hyades. Given that L_x is proportional to the square of a star's rotational rate, the median L_x of NGC 752 is consistent, for t &gt;= 1 Gyr, with a decaying rate in rotational velocities v_rot ~ t&lt;sup&gt;-alpha&lt;/sup&gt; with alpha ~ 0.75, steeper than the Skumanich relation (alpha ~ 0.5) and significantly steeper than that observed between the Pleiades and the Hyades (where alpha &lt;0.3), suggesting that a change in the rotational regimes of the stellar interiors is taking place at an age of ~ 1 Gyr. NGC 752 was observed for 49 ks by the XMM-Newton EPIC camera on February 5, 2003 starting at 23:29:25 UT, and the nominal pointing was towards J2000.0 RA and Declination of (01:57:38, +37:47:60), thus the XMM-Newton field-of-view (FOV) includes the Chandra FOV. For the source detection, the authors used the PWXDETECT code developed at Palermo Observatory and derived from the analogous Chandra PWDETECT code based on wavelet transform analysis. This allows the three EPIC exposures (PN, MOS1 and MOS2) to be combined in order to gain a deeper sensitivity with respect to the source detection based on single images. THere were 145 point sources detected in the energy band 0.5 - 2.0 keV. An extended source (not listed in this present table), very likely a galaxy cluster, is also visible in the EPIC data. The authors searched for 2MASS counterparts to the XMM-Newton sources using a search radius of 5 arcsec and found a counterpart for 38 sources. As for the Chandra data, all sources with a visible counterpart from DLM94 have also a 2MASS counterpart, so this leaves 15 XMM-Newton sources with a 2MASS counterpart and no counterpart in Daniel et al. (1994, PASP, 106, 281); of these, 3 were also detected by Chandra; of the other 12, 10 are outside the Chandra FOV, while two are within it (XMM-Newton sources 58 and 65). Source 65 was caught by XMM-Newton during the decay phase of a flare, which explains why it is not detected in the Chandra data. For source 58 there is no immediate explanation for this, since the light curve does not show evidence of a flare. No additional near-IR counterpart to the XMM-Newton sources was found within the Point Source Reject Table of the 2MASS Extended Mission.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc752xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/ngc752xmm</TD>
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc752xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc752xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/434/483 [1]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
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            <TD>2011-09-14T20:05:34Z</TD>
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            <TD>17-Dec-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/434/483</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/434/483</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/434/483</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/434/483 [2]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/434/483#2</TD>
            <TD>2011-09-14T20:05:34Z</TD>
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          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/434/483 [table2]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/434/483#table2</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/434/483 [table1]</TD>
            <TD>An XMM-Newton survey of M 31 (Pietsch+, 2005)</TD>
            <TD>In an analysis of XMM archival observations of the bright Local Group spiral galaxy M 31 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 4.4x10^34^erg/s. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 856 sources in an area of 1.24 square degrees. We correlate our sources with earlier M 31 X-ray catalogues and use information from optical, infra-red and radio wavelengths. As sources within M 31 we detect 21 supernova remnants (SNR) and 23 SNR candidates, 18 supersoft source (SSS) candidates, 7 X-ray binaries (XRBs) and 9 XRB candidates, as well as 27 globular cluster sources (GlC) and 10 GlC candidates, which most likely are low mass XRBs within the GlC. Comparison to earlier X-ray surveys reveal transients not detected with XMM-Newton, which add to the number of M 31 XRBs. There are 567 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 31 or background AGN. The number of 44 SNRs and candidates more than doubles the X-ray-detected SNRs. 22 sources are new SNR candidates in M 31 based on X-ray selection criteria. Another SNR candidate may be the first plerion detected outside the Galaxy and the Magellanic Clouds. On the other hand, six sources are foreground stars and 90 foreground star candidates, one is a BL Lac-type active galactic nucleus (AGN) and 36 are AGN candidates, one source coincides with the Local Group galaxy M 32, one with a background galaxy cluster (GCl) and another is a GCl candidate, all sources not connected to M31.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/434/483#table1</TD>
            <TD>2011-09-14T20:05:34Z</TD>
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            <TD>17-Dec-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/434/483</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/459/423 [1]</TD>
            <TD>VI and [Fe/H] of Fornax dSph RGB stars (Battaglia+, 2006)</TD>
            <TD>We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for the targets with a S/N per Angstrom &gt;10 and an error in velocity &lt;5km/s, because we found this to be the minimum for an accurate determination of velocity and equivalent width. We checked the sample to weed out any spurious object (e.g., broken fibres, background galaxies, foreground stars, spectra not consistent with RGBs). We use a 2.5sigma cut from the system velocity to derive which stars are probable velocity members of the Fornax dSph. We transform the equivalent width of the CaT lines of probable velocity members into metallicity ([Fe/H]) using the relation derived by Rutledge et al. (1997PASP..109..907R) and combining the CaT lines as in Tolstoy et al. (2001MNRAS.327..918T). The errors in [Fe/H] are based on S/N computations and adjusted to agree with repeated measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423#1</TD>
            <TD>2011-09-14T20:00:50Z</TD>
            <TD>#Abundances#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/459/423</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/423</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/459/423 [2]</TD>
            <TD>VI and [Fe/H] of Fornax dSph RGB stars (Battaglia+, 2006)</TD>
            <TD>We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for the targets with a S/N per Angstrom &gt;10 and an error in velocity &lt;5km/s, because we found this to be the minimum for an accurate determination of velocity and equivalent width. We checked the sample to weed out any spurious object (e.g., broken fibres, background galaxies, foreground stars, spectra not consistent with RGBs). We use a 2.5sigma cut from the system velocity to derive which stars are probable velocity members of the Fornax dSph. We transform the equivalent width of the CaT lines of probable velocity members into metallicity ([Fe/H]) using the relation derived by Rutledge et al. (1997PASP..109..907R) and combining the CaT lines as in Tolstoy et al. (2001MNRAS.327..918T). The errors in [Fe/H] are based on S/N computations and adjusted to agree with repeated measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423#2</TD>
            <TD>2011-09-14T20:00:50Z</TD>
            <TD>#Abundances#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/459/423&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/459/423 [table4]</TD>
            <TD>VI and [Fe/H] of Fornax dSph RGB stars (Battaglia+, 2006)</TD>
            <TD>We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for the targets with a S/N per Angstrom &gt;10 and an error in velocity &lt;5km/s, because we found this to be the minimum for an accurate determination of velocity and equivalent width. We checked the sample to weed out any spurious object (e.g., broken fibres, background galaxies, foreground stars, spectra not consistent with RGBs). We use a 2.5sigma cut from the system velocity to derive which stars are probable velocity members of the Fornax dSph. We transform the equivalent width of the CaT lines of probable velocity members into metallicity ([Fe/H]) using the relation derived by Rutledge et al. (1997PASP..109..907R) and combining the CaT lines as in Tolstoy et al. (2001MNRAS.327..918T). The errors in [Fe/H] are based on S/N computations and adjusted to agree with repeated measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423#table4</TD>
            <TD>2011-09-14T20:00:50Z</TD>
            <TD>#Abundances#Photometry#Stars#Galaxies#</TD>
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            <TD>28-Nov-2006</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/423</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>OMEGCENXMM [1]</TD>
            <TD>Omega Centauri XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Omega Centauri (NGC 5139) is one of the best studied objects in our galaxy. It is the most massive globular cluster (5.1 x 10&lt;sup&gt;6&lt;/sup&gt; solar masses), and is characterized by large core and half mass radii (154.88 and 250.8 arcseconds, respectively (Harris 1996, AJ, 112, 1487). The authors observed Omega Cen with XMM-Newton on August 13th, 2001. The observation lasted 37 ks and was performed with the medium filter. The authors detected 11 and 27 faint X-ray sources in the core and half mass radii, respectively, searching down to a luminosity of 1.3 x 10&lt;sup&gt;31&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5 - 5 keV range (for an assumed distance to Omega Cen of 5.3 kpc). Most sources have bolometric X-ray luminosities between ~ 10&lt;sup&gt;31&lt;/sup&gt; - 10&lt;sup&gt;32&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. The bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. The authors also analyzed a publicly available Chandra ACIS-I observation performed on January 24 - 25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra). This table lists all 146 X-ray sources detected in the XMM-Newton observation above a maximum likelihood threshold in the 0.5 - 5 keV band of 12, including the 27 sources within the half-mass radius (listed in Table 1 of the reference paper), and the 119 sources outside the half-mass radius (listed in Table 2 of the reference paper). About 9 of the 27 sources within the half-mass radius are expected to be background sources, as are ~ 65 of the sources within 12.5 arcminutes of the cluster center, i.e., a significant fraction of the 146 total observed X-ray sources. For each XMM-Newton source, its position, count rate, correlation with previous X-ray observation, and their associated errors are given. The detailed spectral information given in Table 5 of the reference paper for 17 selected X-ray sources is however not included in this HEASARC table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/omegcenxmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=omegcenxmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/omegcenxmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>OMEGCENXMM [2]</TD>
            <TD>Omega Centauri XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Omega Centauri (NGC 5139) is one of the best studied objects in our galaxy. It is the most massive globular cluster (5.1 x 10&lt;sup&gt;6&lt;/sup&gt; solar masses), and is characterized by large core and half mass radii (154.88 and 250.8 arcseconds, respectively (Harris 1996, AJ, 112, 1487). The authors observed Omega Cen with XMM-Newton on August 13th, 2001. The observation lasted 37 ks and was performed with the medium filter. The authors detected 11 and 27 faint X-ray sources in the core and half mass radii, respectively, searching down to a luminosity of 1.3 x 10&lt;sup&gt;31&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5 - 5 keV range (for an assumed distance to Omega Cen of 5.3 kpc). Most sources have bolometric X-ray luminosities between ~ 10&lt;sup&gt;31&lt;/sup&gt; - 10&lt;sup&gt;32&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. The bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. The authors also analyzed a publicly available Chandra ACIS-I observation performed on January 24 - 25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra). This table lists all 146 X-ray sources detected in the XMM-Newton observation above a maximum likelihood threshold in the 0.5 - 5 keV band of 12, including the 27 sources within the half-mass radius (listed in Table 1 of the reference paper), and the 119 sources outside the half-mass radius (listed in Table 2 of the reference paper). About 9 of the 27 sources within the half-mass radius are expected to be background sources, as are ~ 65 of the sources within 12.5 arcminutes of the cluster center, i.e., a significant fraction of the 146 total observed X-ray sources. For each XMM-Newton source, its position, count rate, correlation with previous X-ray observation, and their associated errors are given. The detailed spectral information given in Table 5 of the reference paper for 17 selected X-ray sources is however not included in this HEASARC table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/omegcenxmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/omegcenxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>OMEGCENXMM [3]</TD>
            <TD>Omega Centauri XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Omega Centauri (NGC 5139) is one of the best studied objects in our galaxy. It is the most massive globular cluster (5.1 x 10&lt;sup&gt;6&lt;/sup&gt; solar masses), and is characterized by large core and half mass radii (154.88 and 250.8 arcseconds, respectively (Harris 1996, AJ, 112, 1487). The authors observed Omega Cen with XMM-Newton on August 13th, 2001. The observation lasted 37 ks and was performed with the medium filter. The authors detected 11 and 27 faint X-ray sources in the core and half mass radii, respectively, searching down to a luminosity of 1.3 x 10&lt;sup&gt;31&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5 - 5 keV range (for an assumed distance to Omega Cen of 5.3 kpc). Most sources have bolometric X-ray luminosities between ~ 10&lt;sup&gt;31&lt;/sup&gt; - 10&lt;sup&gt;32&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. The bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. The authors also analyzed a publicly available Chandra ACIS-I observation performed on January 24 - 25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra). This table lists all 146 X-ray sources detected in the XMM-Newton observation above a maximum likelihood threshold in the 0.5 - 5 keV band of 12, including the 27 sources within the half-mass radius (listed in Table 1 of the reference paper), and the 119 sources outside the half-mass radius (listed in Table 2 of the reference paper). About 9 of the 27 sources within the half-mass radius are expected to be background sources, as are ~ 65 of the sources within 12.5 arcminutes of the cluster center, i.e., a significant fraction of the 146 total observed X-ray sources. For each XMM-Newton source, its position, count rate, correlation with previous X-ray observation, and their associated errors are given. The detailed spectral information given in Table 5 of the reference paper for 17 selected X-ray sources is however not included in this HEASARC table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/omegcenxmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/omegcenxmm</TD>
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_omegcenxmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/omegcenxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/459/423 [1]</TD>
            <TD>VI and [Fe/H] of Fornax dSph RGB stars (Battaglia+, 2006)</TD>
            <TD>We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for the targets with a S/N per Angstrom &gt;10 and an error in velocity &lt;5km/s, because we found this to be the minimum for an accurate determination of velocity and equivalent width. We checked the sample to weed out any spurious object (e.g., broken fibres, background galaxies, foreground stars, spectra not consistent with RGBs). We use a 2.5sigma cut from the system velocity to derive which stars are probable velocity members of the Fornax dSph. We transform the equivalent width of the CaT lines of probable velocity members into metallicity ([Fe/H]) using the relation derived by Rutledge et al. (1997PASP..109..907R) and combining the CaT lines as in Tolstoy et al. (2001MNRAS.327..918T). The errors in [Fe/H] are based on S/N computations and adjusted to agree with repeated measurements.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/459/423#1</TD>
            <TD>2011-09-14T20:00:50Z</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/459/423</TD>
            <TD />
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/459/423</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/423</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/459/423 [2]</TD>
            <TD>VI and [Fe/H] of Fornax dSph RGB stars (Battaglia+, 2006)</TD>
            <TD>We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for the targets with a S/N per Angstrom &gt;10 and an error in velocity &lt;5km/s, because we found this to be the minimum for an accurate determination of velocity and equivalent width. We checked the sample to weed out any spurious object (e.g., broken fibres, background galaxies, foreground stars, spectra not consistent with RGBs). We use a 2.5sigma cut from the system velocity to derive which stars are probable velocity members of the Fornax dSph. We transform the equivalent width of the CaT lines of probable velocity members into metallicity ([Fe/H]) using the relation derived by Rutledge et al. (1997PASP..109..907R) and combining the CaT lines as in Tolstoy et al. (2001MNRAS.327..918T). The errors in [Fe/H] are based on S/N computations and adjusted to agree with repeated measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423#2</TD>
            <TD>2011-09-14T20:00:50Z</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/459/423&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/423</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/459/423 [table4]</TD>
            <TD>VI and [Fe/H] of Fornax dSph RGB stars (Battaglia+, 2006)</TD>
            <TD>We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for the targets with a S/N per Angstrom &gt;10 and an error in velocity &lt;5km/s, because we found this to be the minimum for an accurate determination of velocity and equivalent width. We checked the sample to weed out any spurious object (e.g., broken fibres, background galaxies, foreground stars, spectra not consistent with RGBs). We use a 2.5sigma cut from the system velocity to derive which stars are probable velocity members of the Fornax dSph. We transform the equivalent width of the CaT lines of probable velocity members into metallicity ([Fe/H]) using the relation derived by Rutledge et al. (1997PASP..109..907R) and combining the CaT lines as in Tolstoy et al. (2001MNRAS.327..918T). The errors in [Fe/H] are based on S/N computations and adjusted to agree with repeated measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423#table4</TD>
            <TD>2011-09-14T20:00:50Z</TD>
            <TD>#Abundances#Photometry#Stars#Galaxies#</TD>
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            <TD>28-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/459/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/423</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/371/1405 [1]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#1</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/371/1405</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/371/1405 [2]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#2</TD>
            <TD>2011-09-14T20:06:22Z</TD>
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            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/371/1405&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1405 [table24]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#table24</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
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            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1405&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1405 [table56]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#table56</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1405&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/459/423 [1]</TD>
            <TD>VI and [Fe/H] of Fornax dSph RGB stars (Battaglia+, 2006)</TD>
            <TD>We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for the targets with a S/N per Angstrom &gt;10 and an error in velocity &lt;5km/s, because we found this to be the minimum for an accurate determination of velocity and equivalent width. We checked the sample to weed out any spurious object (e.g., broken fibres, background galaxies, foreground stars, spectra not consistent with RGBs). We use a 2.5sigma cut from the system velocity to derive which stars are probable velocity members of the Fornax dSph. We transform the equivalent width of the CaT lines of probable velocity members into metallicity ([Fe/H]) using the relation derived by Rutledge et al. (1997PASP..109..907R) and combining the CaT lines as in Tolstoy et al. (2001MNRAS.327..918T). The errors in [Fe/H] are based on S/N computations and adjusted to agree with repeated measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423#1</TD>
            <TD>2011-09-14T20:00:50Z</TD>
            <TD>#Abundances#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/459/423</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/423</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/459/423 [2]</TD>
            <TD>VI and [Fe/H] of Fornax dSph RGB stars (Battaglia+, 2006)</TD>
            <TD>We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for the targets with a S/N per Angstrom &gt;10 and an error in velocity &lt;5km/s, because we found this to be the minimum for an accurate determination of velocity and equivalent width. We checked the sample to weed out any spurious object (e.g., broken fibres, background galaxies, foreground stars, spectra not consistent with RGBs). We use a 2.5sigma cut from the system velocity to derive which stars are probable velocity members of the Fornax dSph. We transform the equivalent width of the CaT lines of probable velocity members into metallicity ([Fe/H]) using the relation derived by Rutledge et al. (1997PASP..109..907R) and combining the CaT lines as in Tolstoy et al. (2001MNRAS.327..918T). The errors in [Fe/H] are based on S/N computations and adjusted to agree with repeated measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423#2</TD>
            <TD>2011-09-14T20:00:50Z</TD>
            <TD>#Abundances#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/459/423&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/459/423 [table4]</TD>
            <TD>VI and [Fe/H] of Fornax dSph RGB stars (Battaglia+, 2006)</TD>
            <TD>We present the results of the DART imaging and CaII triplet (CaT) survey of the Fornax dwarf spheroidal galaxy (dSph) at ESO. We collected hundreds of low resolution spectra of Red Giant Branch (RGB) stars in the CaT region, using VLT/FLAMES in Medusa mode, with the GIRAFFE spectrograph (grating LR8, resolving power R~6500). We list the results for the targets with a S/N per Angstrom &gt;10 and an error in velocity &lt;5km/s, because we found this to be the minimum for an accurate determination of velocity and equivalent width. We checked the sample to weed out any spurious object (e.g., broken fibres, background galaxies, foreground stars, spectra not consistent with RGBs). We use a 2.5sigma cut from the system velocity to derive which stars are probable velocity members of the Fornax dSph. We transform the equivalent width of the CaT lines of probable velocity members into metallicity ([Fe/H]) using the relation derived by Rutledge et al. (1997PASP..109..907R) and combining the CaT lines as in Tolstoy et al. (2001MNRAS.327..918T). The errors in [Fe/H] are based on S/N computations and adjusted to agree with repeated measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423#table4</TD>
            <TD>2011-09-14T20:00:50Z</TD>
            <TD>#Abundances#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/459/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/423</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/371/1405 [1]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#1</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/371/1405</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/371/1405 [2]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#2</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/371/1405&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1405 [table24]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#table24</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1405&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1405 [table56]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#table56</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1405&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/371/1405 [1]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#1</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/371/1405</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/371/1405 [2]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#2</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/371/1405&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1405 [table24]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#table24</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1405&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1405 [table56]</TD>
            <TD>Variables in M33 (Hartman+, 2006)</TD>
            <TD>The data were obtained using the Queue Service Observing mode at the CFHT on 27 separate nights between 2003 August and 2005 January. We used the g', r' and i' Sloan filters, obtaining 36 images centred on the galaxy with each filter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405#table56</TD>
            <TD>2011-09-14T20:06:22Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1405</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1405&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1405</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/ARA+A/43 [1]</TD>
            <TD>L and T dwarf stars (Kirkpatrick, 2005)</TD>
            <TD>The establishment of new spectral classes cooler than type M has had a brief, yet already rich, history. Prototypes of the new "L dwarf" and "T dwarf" classes were first found in the late 1980s to mid-1990s, with a flood of new discoveries occurring in the late 1990s with the advent of deep, large-area, digital sky surveys. Over four hundred and fifty L and T dwarfs are now catalogued. This review concentrates on the spectroscopic properties of these objects, beginning with the establishment of classification schemes rooted in the MK Process. The resulting grid of spectral types is then used as a tool to ferret out the underlying physics. The temperature ranges covered by these spectral types, the complex chemical processes responsible for the shape of their emergent spectra, their nature as either true stars or brown dwarfs, and their number density in the Galaxy are discussed. Two promising avenues for future research are also explored: the extension of the classification system to three dimensions to account for gravity- and metallicity-dependent features, and the capability of newer large-area surveys to uncover brown dwarfs cooler than those now recognized.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195#1</TD>
            <TD>2011-09-14T20:01:04Z</TD>
            <TD>#Stars#Spectral_Classification#Parallaxes#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/ARA+A/43.195</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ARA+A/43.195</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/ARA+A/43 [2]</TD>
            <TD>L and T dwarf stars (Kirkpatrick, 2005)</TD>
            <TD>The establishment of new spectral classes cooler than type M has had a brief, yet already rich, history. Prototypes of the new "L dwarf" and "T dwarf" classes were first found in the late 1980s to mid-1990s, with a flood of new discoveries occurring in the late 1990s with the advent of deep, large-area, digital sky surveys. Over four hundred and fifty L and T dwarfs are now catalogued. This review concentrates on the spectroscopic properties of these objects, beginning with the establishment of classification schemes rooted in the MK Process. The resulting grid of spectral types is then used as a tool to ferret out the underlying physics. The temperature ranges covered by these spectral types, the complex chemical processes responsible for the shape of their emergent spectra, their nature as either true stars or brown dwarfs, and their number density in the Galaxy are discussed. Two promising avenues for future research are also explored: the extension of the classification system to three dimensions to account for gravity- and metallicity-dependent features, and the capability of newer large-area surveys to uncover brown dwarfs cooler than those now recognized.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195#2</TD>
            <TD>2011-09-14T20:01:04Z</TD>
            <TD>#Stars#Spectral_Classification#Parallaxes#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/ARA+A/43.195&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ARA+A/43.195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/ARA+A/43 [table3]</TD>
            <TD>L and T dwarf stars (Kirkpatrick, 2005)</TD>
            <TD>The establishment of new spectral classes cooler than type M has had a brief, yet already rich, history. Prototypes of the new "L dwarf" and "T dwarf" classes were first found in the late 1980s to mid-1990s, with a flood of new discoveries occurring in the late 1990s with the advent of deep, large-area, digital sky surveys. Over four hundred and fifty L and T dwarfs are now catalogued. This review concentrates on the spectroscopic properties of these objects, beginning with the establishment of classification schemes rooted in the MK Process. The resulting grid of spectral types is then used as a tool to ferret out the underlying physics. The temperature ranges covered by these spectral types, the complex chemical processes responsible for the shape of their emergent spectra, their nature as either true stars or brown dwarfs, and their number density in the Galaxy are discussed. Two promising avenues for future research are also explored: the extension of the classification system to three dimensions to account for gravity- and metallicity-dependent features, and the capability of newer large-area surveys to uncover brown dwarfs cooler than those now recognized.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195#table3</TD>
            <TD>2011-09-14T20:01:04Z</TD>
            <TD>#Stars#Spectral_Classification#Parallaxes#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/ARA+A/43.195&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ARA+A/43.195</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/371/38 [1]</TD>
            <TD>X-ray observations of the Galaxy center (Wang+, 2006)</TD>
            <TD>Our deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>CDS</TD>
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            <TD />
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/371/38</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/38</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/371/38 [2]</TD>
            <TD>X-ray observations of the Galaxy center (Wang+, 2006)</TD>
            <TD>Our deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/38#2</TD>
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            <TD>15-May-2007</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/371/38&amp;</TD>
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            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/38</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/38 [table1]</TD>
            <TD>X-ray observations of the Galaxy center (Wang+, 2006)</TD>
            <TD>Our deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/38#table1</TD>
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            <TD>Catalog</TD>
            <TD>OMEGCENXMM [1]</TD>
            <TD>Omega Centauri XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Omega Centauri (NGC 5139) is one of the best studied objects in our galaxy. It is the most massive globular cluster (5.1 x 10&lt;sup&gt;6&lt;/sup&gt; solar masses), and is characterized by large core and half mass radii (154.88 and 250.8 arcseconds, respectively (Harris 1996, AJ, 112, 1487). The authors observed Omega Cen with XMM-Newton on August 13th, 2001. The observation lasted 37 ks and was performed with the medium filter. The authors detected 11 and 27 faint X-ray sources in the core and half mass radii, respectively, searching down to a luminosity of 1.3 x 10&lt;sup&gt;31&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5 - 5 keV range (for an assumed distance to Omega Cen of 5.3 kpc). Most sources have bolometric X-ray luminosities between ~ 10&lt;sup&gt;31&lt;/sup&gt; - 10&lt;sup&gt;32&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. The bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. The authors also analyzed a publicly available Chandra ACIS-I observation performed on January 24 - 25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra). This table lists all 146 X-ray sources detected in the XMM-Newton observation above a maximum likelihood threshold in the 0.5 - 5 keV band of 12, including the 27 sources within the half-mass radius (listed in Table 1 of the reference paper), and the 119 sources outside the half-mass radius (listed in Table 2 of the reference paper). About 9 of the 27 sources within the half-mass radius are expected to be background sources, as are ~ 65 of the sources within 12.5 arcminutes of the cluster center, i.e., a significant fraction of the 146 total observed X-ray sources. For each XMM-Newton source, its position, count rate, correlation with previous X-ray observation, and their associated errors are given. The detailed spectral information given in Table 5 of the reference paper for 17 selected X-ray sources is however not included in this HEASARC table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/omegcenxmm#1</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/omegcenxmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>OMEGCENXMM [2]</TD>
            <TD>Omega Centauri XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Omega Centauri (NGC 5139) is one of the best studied objects in our galaxy. It is the most massive globular cluster (5.1 x 10&lt;sup&gt;6&lt;/sup&gt; solar masses), and is characterized by large core and half mass radii (154.88 and 250.8 arcseconds, respectively (Harris 1996, AJ, 112, 1487). The authors observed Omega Cen with XMM-Newton on August 13th, 2001. The observation lasted 37 ks and was performed with the medium filter. The authors detected 11 and 27 faint X-ray sources in the core and half mass radii, respectively, searching down to a luminosity of 1.3 x 10&lt;sup&gt;31&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5 - 5 keV range (for an assumed distance to Omega Cen of 5.3 kpc). Most sources have bolometric X-ray luminosities between ~ 10&lt;sup&gt;31&lt;/sup&gt; - 10&lt;sup&gt;32&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. The bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. The authors also analyzed a publicly available Chandra ACIS-I observation performed on January 24 - 25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra). This table lists all 146 X-ray sources detected in the XMM-Newton observation above a maximum likelihood threshold in the 0.5 - 5 keV band of 12, including the 27 sources within the half-mass radius (listed in Table 1 of the reference paper), and the 119 sources outside the half-mass radius (listed in Table 2 of the reference paper). About 9 of the 27 sources within the half-mass radius are expected to be background sources, as are ~ 65 of the sources within 12.5 arcminutes of the cluster center, i.e., a significant fraction of the 146 total observed X-ray sources. For each XMM-Newton source, its position, count rate, correlation with previous X-ray observation, and their associated errors are given. The detailed spectral information given in Table 5 of the reference paper for 17 selected X-ray sources is however not included in this HEASARC table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>OMEGCENXMM [3]</TD>
            <TD>Omega Centauri XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Omega Centauri (NGC 5139) is one of the best studied objects in our galaxy. It is the most massive globular cluster (5.1 x 10&lt;sup&gt;6&lt;/sup&gt; solar masses), and is characterized by large core and half mass radii (154.88 and 250.8 arcseconds, respectively (Harris 1996, AJ, 112, 1487). The authors observed Omega Cen with XMM-Newton on August 13th, 2001. The observation lasted 37 ks and was performed with the medium filter. The authors detected 11 and 27 faint X-ray sources in the core and half mass radii, respectively, searching down to a luminosity of 1.3 x 10&lt;sup&gt;31&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5 - 5 keV range (for an assumed distance to Omega Cen of 5.3 kpc). Most sources have bolometric X-ray luminosities between ~ 10&lt;sup&gt;31&lt;/sup&gt; - 10&lt;sup&gt;32&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. The bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. The authors also analyzed a publicly available Chandra ACIS-I observation performed on January 24 - 25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra). This table lists all 146 X-ray sources detected in the XMM-Newton observation above a maximum likelihood threshold in the 0.5 - 5 keV band of 12, including the 27 sources within the half-mass radius (listed in Table 1 of the reference paper), and the 119 sources outside the half-mass radius (listed in Table 2 of the reference paper). About 9 of the 27 sources within the half-mass radius are expected to be background sources, as are ~ 65 of the sources within 12.5 arcminutes of the cluster center, i.e., a significant fraction of the 146 total observed X-ray sources. For each XMM-Newton source, its position, count rate, correlation with previous X-ray observation, and their associated errors are given. The detailed spectral information given in Table 5 of the reference paper for 17 selected X-ray sources is however not included in this HEASARC table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_omegcenxmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/omegcenxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/371/38 [1]</TD>
            <TD>X-ray observations of the Galaxy center (Wang+, 2006)</TD>
            <TD>Our deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/371/38</TD>
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            <TD>HTTP Request</TD>
            <TD>J/MNRAS/371/38 [2]</TD>
            <TD>X-ray observations of the Galaxy center (Wang+, 2006)</TD>
            <TD>Our deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/38</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/371/38 [table1]</TD>
            <TD>X-ray observations of the Galaxy center (Wang+, 2006)</TD>
            <TD>Our deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>CDS</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/38</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>OMEGCENXMM [1]</TD>
            <TD>Omega Centauri XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Omega Centauri (NGC 5139) is one of the best studied objects in our galaxy. It is the most massive globular cluster (5.1 x 10&lt;sup&gt;6&lt;/sup&gt; solar masses), and is characterized by large core and half mass radii (154.88 and 250.8 arcseconds, respectively (Harris 1996, AJ, 112, 1487). The authors observed Omega Cen with XMM-Newton on August 13th, 2001. The observation lasted 37 ks and was performed with the medium filter. The authors detected 11 and 27 faint X-ray sources in the core and half mass radii, respectively, searching down to a luminosity of 1.3 x 10&lt;sup&gt;31&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5 - 5 keV range (for an assumed distance to Omega Cen of 5.3 kpc). Most sources have bolometric X-ray luminosities between ~ 10&lt;sup&gt;31&lt;/sup&gt; - 10&lt;sup&gt;32&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. The bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. The authors also analyzed a publicly available Chandra ACIS-I observation performed on January 24 - 25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra). This table lists all 146 X-ray sources detected in the XMM-Newton observation above a maximum likelihood threshold in the 0.5 - 5 keV band of 12, including the 27 sources within the half-mass radius (listed in Table 1 of the reference paper), and the 119 sources outside the half-mass radius (listed in Table 2 of the reference paper). About 9 of the 27 sources within the half-mass radius are expected to be background sources, as are ~ 65 of the sources within 12.5 arcminutes of the cluster center, i.e., a significant fraction of the 146 total observed X-ray sources. For each XMM-Newton source, its position, count rate, correlation with previous X-ray observation, and their associated errors are given. The detailed spectral information given in Table 5 of the reference paper for 17 selected X-ray sources is however not included in this HEASARC table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>OMEGCENXMM [2]</TD>
            <TD>Omega Centauri XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Omega Centauri (NGC 5139) is one of the best studied objects in our galaxy. It is the most massive globular cluster (5.1 x 10&lt;sup&gt;6&lt;/sup&gt; solar masses), and is characterized by large core and half mass radii (154.88 and 250.8 arcseconds, respectively (Harris 1996, AJ, 112, 1487). The authors observed Omega Cen with XMM-Newton on August 13th, 2001. The observation lasted 37 ks and was performed with the medium filter. The authors detected 11 and 27 faint X-ray sources in the core and half mass radii, respectively, searching down to a luminosity of 1.3 x 10&lt;sup&gt;31&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5 - 5 keV range (for an assumed distance to Omega Cen of 5.3 kpc). Most sources have bolometric X-ray luminosities between ~ 10&lt;sup&gt;31&lt;/sup&gt; - 10&lt;sup&gt;32&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. The bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. The authors also analyzed a publicly available Chandra ACIS-I observation performed on January 24 - 25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra). This table lists all 146 X-ray sources detected in the XMM-Newton observation above a maximum likelihood threshold in the 0.5 - 5 keV band of 12, including the 27 sources within the half-mass radius (listed in Table 1 of the reference paper), and the 119 sources outside the half-mass radius (listed in Table 2 of the reference paper). About 9 of the 27 sources within the half-mass radius are expected to be background sources, as are ~ 65 of the sources within 12.5 arcminutes of the cluster center, i.e., a significant fraction of the 146 total observed X-ray sources. For each XMM-Newton source, its position, count rate, correlation with previous X-ray observation, and their associated errors are given. The detailed spectral information given in Table 5 of the reference paper for 17 selected X-ray sources is however not included in this HEASARC table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/omegcenxmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/omegcenxmm</TD>
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            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=omegcenxmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/omegcenxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>OMEGCENXMM [3]</TD>
            <TD>Omega Centauri XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Omega Centauri (NGC 5139) is one of the best studied objects in our galaxy. It is the most massive globular cluster (5.1 x 10&lt;sup&gt;6&lt;/sup&gt; solar masses), and is characterized by large core and half mass radii (154.88 and 250.8 arcseconds, respectively (Harris 1996, AJ, 112, 1487). The authors observed Omega Cen with XMM-Newton on August 13th, 2001. The observation lasted 37 ks and was performed with the medium filter. The authors detected 11 and 27 faint X-ray sources in the core and half mass radii, respectively, searching down to a luminosity of 1.3 x 10&lt;sup&gt;31&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt; in the 0.5 - 5 keV range (for an assumed distance to Omega Cen of 5.3 kpc). Most sources have bolometric X-ray luminosities between ~ 10&lt;sup&gt;31&lt;/sup&gt; - 10&lt;sup&gt;32&lt;/sup&gt; ergs s&lt;sup&gt;-1&lt;/sup&gt;. The bulk of sources are hard and spectrally similar to CVs. The lack of soft faint sources might be related to the absence of millisecond pulsars in the cluster. The XMM-Newton observations reveal the presence of an excess of sources well outside the core of the cluster where several RS CVn binaries have already been found. The authors also analyzed a publicly available Chandra ACIS-I observation performed on January 24 - 25th, 2000, to improve the XMM-Newton source positions and to search for source intensity variations between the two data sets. 63 XMM-Newton sources have a Chandra counterpart, and 15 sources within the half-mass radius have shown time variability. Overall, the general properties of the faint X-ray sources in omega Cen suggest that they are predominantly CVs and active binaries (RS CVn or BY Dra). This table lists all 146 X-ray sources detected in the XMM-Newton observation above a maximum likelihood threshold in the 0.5 - 5 keV band of 12, including the 27 sources within the half-mass radius (listed in Table 1 of the reference paper), and the 119 sources outside the half-mass radius (listed in Table 2 of the reference paper). About 9 of the 27 sources within the half-mass radius are expected to be background sources, as are ~ 65 of the sources within 12.5 arcminutes of the cluster center, i.e., a significant fraction of the 146 total observed X-ray sources. For each XMM-Newton source, its position, count rate, correlation with previous X-ray observation, and their associated errors are given. The detailed spectral information given in Table 5 of the reference paper for 17 selected X-ray sources is however not included in this HEASARC table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/omegcenxmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/omegcenxmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_omegcenxmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/omegcenxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/371/38 [1]</TD>
            <TD>X-ray observations of the Galaxy center (Wang+, 2006)</TD>
            <TD>Our deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/38#1</TD>
            <TD>2011-09-14T20:06:30Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/38</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/371/38</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/38</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/371/38 [2]</TD>
            <TD>X-ray observations of the Galaxy center (Wang+, 2006)</TD>
            <TD>Our deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/38#2</TD>
            <TD>2011-09-14T20:06:30Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/38</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/371/38&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/38</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/38 [table1]</TD>
            <TD>X-ray observations of the Galaxy center (Wang+, 2006)</TD>
            <TD>Our deep Chandra ACIS-I observation (Obs. ID: 4500) was carried out on 2004 June 9. The Arches cluster was placed about 1-arcmin away from the aim point to minimize the effect of the CCD gaps on mapping the extended X-ray emission around the cluster.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/38#table1</TD>
            <TD>2011-09-14T20:06:30Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/38</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/38&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/38</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROSAT/ESOClus. [1]</TD>
            <TD>ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey</TD>
            <TD>This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey Catalog. The REFLEX Cluster Survey provides information on the X-ray properties, redshifts, and some identification details of clusters in the REFLEX sample. The catalog describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3x10^-12 erg/s/cm^2 (0.1 to 2.4 keV) in an area of 4.24 steradian in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. The X-ray luminosities and other distance-dependent cluster parameters are calculated for a Lambda cosmology with a Hubble Constant H_0 of 70 km/s/Mpc, Omega_m of 0.3, and Omega_Lambda of 0.7. The CDS version of this catalog contains an additional table (reflex50.dat) with these parameters calculated for an Einstein-de Sitter universe with H_0 = 50 km/s/Mpc, Omega_m = 1.0, and Omega_Lambda = 0.0.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/reflex#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/reflex</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=reflex&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/reflex.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROSAT/ESOClus. [2]</TD>
            <TD>ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey</TD>
            <TD>This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey Catalog. The REFLEX Cluster Survey provides information on the X-ray properties, redshifts, and some identification details of clusters in the REFLEX sample. The catalog describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3x10^-12 erg/s/cm^2 (0.1 to 2.4 keV) in an area of 4.24 steradian in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. The X-ray luminosities and other distance-dependent cluster parameters are calculated for a Lambda cosmology with a Hubble Constant H_0 of 70 km/s/Mpc, Omega_m of 0.3, and Omega_Lambda of 0.7. The CDS version of this catalog contains an additional table (reflex50.dat) with these parameters calculated for an Einstein-de Sitter universe with H_0 = 50 km/s/Mpc, Omega_m = 1.0, and Omega_Lambda = 0.0.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/reflex#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/reflex</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=reflex&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/reflex.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROSAT/ESOClus. [3]</TD>
            <TD>ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey</TD>
            <TD>This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey Catalog. The REFLEX Cluster Survey provides information on the X-ray properties, redshifts, and some identification details of clusters in the REFLEX sample. The catalog describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3x10^-12 erg/s/cm^2 (0.1 to 2.4 keV) in an area of 4.24 steradian in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. The X-ray luminosities and other distance-dependent cluster parameters are calculated for a Lambda cosmology with a Hubble Constant H_0 of 70 km/s/Mpc, Omega_m of 0.3, and Omega_Lambda of 0.7. The CDS version of this catalog contains an additional table (reflex50.dat) with these parameters calculated for an Einstein-de Sitter universe with H_0 = 50 km/s/Mpc, Omega_m = 1.0, and Omega_Lambda = 0.0.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/reflex#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/reflex</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_reflex&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/reflex.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/2728 [1]</TD>
            <TD>I photometry of early-type galaxies (Scodeggio+, 1998)</TD>
            <TD>As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2728#1</TD>
            <TD>2011-09-14T20:31:35Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2728</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/2728</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2728</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/2728 [2]</TD>
            <TD>I photometry of early-type galaxies (Scodeggio+, 1998)</TD>
            <TD>As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2728#2</TD>
            <TD>2011-09-14T20:31:35Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2728</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/2728&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2728</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/2728 [table3]</TD>
            <TD>I photometry of early-type galaxies (Scodeggio+, 1998)</TD>
            <TD>As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2728#table3</TD>
            <TD>2011-09-14T20:31:35Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2728</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/2728&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2728</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ROSAT/ESOClus. [1]</TD>
            <TD>ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey</TD>
            <TD>This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey Catalog. The REFLEX Cluster Survey provides information on the X-ray properties, redshifts, and some identification details of clusters in the REFLEX sample. The catalog describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3x10^-12 erg/s/cm^2 (0.1 to 2.4 keV) in an area of 4.24 steradian in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. The X-ray luminosities and other distance-dependent cluster parameters are calculated for a Lambda cosmology with a Hubble Constant H_0 of 70 km/s/Mpc, Omega_m of 0.3, and Omega_Lambda of 0.7. The CDS version of this catalog contains an additional table (reflex50.dat) with these parameters calculated for an Einstein-de Sitter universe with H_0 = 50 km/s/Mpc, Omega_m = 1.0, and Omega_Lambda = 0.0.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/reflex#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/reflex</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=reflex&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/reflex.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ROSAT/ESOClus. [2]</TD>
            <TD>ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey</TD>
            <TD>This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey Catalog. The REFLEX Cluster Survey provides information on the X-ray properties, redshifts, and some identification details of clusters in the REFLEX sample. The catalog describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3x10^-12 erg/s/cm^2 (0.1 to 2.4 keV) in an area of 4.24 steradian in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. The X-ray luminosities and other distance-dependent cluster parameters are calculated for a Lambda cosmology with a Hubble Constant H_0 of 70 km/s/Mpc, Omega_m of 0.3, and Omega_Lambda of 0.7. The CDS version of this catalog contains an additional table (reflex50.dat) with these parameters calculated for an Einstein-de Sitter universe with H_0 = 50 km/s/Mpc, Omega_m = 1.0, and Omega_Lambda = 0.0.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/reflex#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.05</TD>
            <TD />
            <TD>ivo://nasa.heasarc/reflex</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=reflex&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/reflex.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ROSAT/ESOClus. [3]</TD>
            <TD>ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey</TD>
            <TD>This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey Catalog. The REFLEX Cluster Survey provides information on the X-ray properties, redshifts, and some identification details of clusters in the REFLEX sample. The catalog describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3x10^-12 erg/s/cm^2 (0.1 to 2.4 keV) in an area of 4.24 steradian in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. The X-ray luminosities and other distance-dependent cluster parameters are calculated for a Lambda cosmology with a Hubble Constant H_0 of 70 km/s/Mpc, Omega_m of 0.3, and Omega_Lambda of 0.7. The CDS version of this catalog contains an additional table (reflex50.dat) with these parameters calculated for an Einstein-de Sitter universe with H_0 = 50 km/s/Mpc, Omega_m = 1.0, and Omega_Lambda = 0.0.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD />
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/2728 [1]</TD>
            <TD>I photometry of early-type galaxies (Scodeggio+, 1998)</TD>
            <TD>As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.</TD>
            <TD>CDS</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/2728 [2]</TD>
            <TD>I photometry of early-type galaxies (Scodeggio+, 1998)</TD>
            <TD>As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.</TD>
            <TD>CDS</TD>
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            <TD>J/AJ/116/2728 [table3]</TD>
            <TD>I photometry of early-type galaxies (Scodeggio+, 1998)</TD>
            <TD>As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.</TD>
            <TD>CDS</TD>
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            <TD>Catalog</TD>
            <TD>ROSAT/ESOClus. [1]</TD>
            <TD>ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey</TD>
            <TD>This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey Catalog. The REFLEX Cluster Survey provides information on the X-ray properties, redshifts, and some identification details of clusters in the REFLEX sample. The catalog describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3x10^-12 erg/s/cm^2 (0.1 to 2.4 keV) in an area of 4.24 steradian in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. The X-ray luminosities and other distance-dependent cluster parameters are calculated for a Lambda cosmology with a Hubble Constant H_0 of 70 km/s/Mpc, Omega_m of 0.3, and Omega_Lambda of 0.7. The CDS version of this catalog contains an additional table (reflex50.dat) with these parameters calculated for an Einstein-de Sitter universe with H_0 = 50 km/s/Mpc, Omega_m = 1.0, and Omega_Lambda = 0.0.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>ROSAT/ESOClus. [2]</TD>
            <TD>ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey</TD>
            <TD>This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey Catalog. The REFLEX Cluster Survey provides information on the X-ray properties, redshifts, and some identification details of clusters in the REFLEX sample. The catalog describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3x10^-12 erg/s/cm^2 (0.1 to 2.4 keV) in an area of 4.24 steradian in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. The X-ray luminosities and other distance-dependent cluster parameters are calculated for a Lambda cosmology with a Hubble Constant H_0 of 70 km/s/Mpc, Omega_m of 0.3, and Omega_Lambda of 0.7. The CDS version of this catalog contains an additional table (reflex50.dat) with these parameters calculated for an Einstein-de Sitter universe with H_0 = 50 km/s/Mpc, Omega_m = 1.0, and Omega_Lambda = 0.0.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/reflex.html</TD>
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            <TD>Web Page</TD>
            <TD>ROSAT/ESOClus. [3]</TD>
            <TD>ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey</TD>
            <TD>This table is the ROSAT-ESO Flux-Limited X-Ray (REFLEX) Galaxy Cluster Survey Catalog. The REFLEX Cluster Survey provides information on the X-ray properties, redshifts, and some identification details of clusters in the REFLEX sample. The catalog describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3x10^-12 erg/s/cm^2 (0.1 to 2.4 keV) in an area of 4.24 steradian in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. The X-ray luminosities and other distance-dependent cluster parameters are calculated for a Lambda cosmology with a Hubble Constant H_0 of 70 km/s/Mpc, Omega_m of 0.3, and Omega_Lambda of 0.7. The CDS version of this catalog contains an additional table (reflex50.dat) with these parameters calculated for an Einstein-de Sitter universe with H_0 = 50 km/s/Mpc, Omega_m = 1.0, and Omega_Lambda = 0.0.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD />
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            <TD>J/AJ/116/2728 [1]</TD>
            <TD>I photometry of early-type galaxies (Scodeggio+, 1998)</TD>
            <TD>As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2728#1</TD>
            <TD>2011-09-14T20:31:35Z</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/2728 [2]</TD>
            <TD>I photometry of early-type galaxies (Scodeggio+, 1998)</TD>
            <TD>As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2728#2</TD>
            <TD>2011-09-14T20:31:35Z</TD>
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            <TD>J/AJ/116/2728 [table3]</TD>
            <TD>I photometry of early-type galaxies (Scodeggio+, 1998)</TD>
            <TD>As part of a project to compare the fundamental plane and Tully-Fisher distance scales, we present here I-band CCD photometry for 636 early-type galaxies in eight clusters and groups of galaxies. These are the A262, A1367, Coma (A1656), A2634, Cancer and Pegasus Clusters, and the NGC 383 and NGC 507 Groups. Sample selection, cluster properties, and cluster membership assignment criteria are discussed. We present photometric parameters that are used in the fundamental plane relation, the effective radius r_e_, and the effective surface brightness {mu}_e_, as derived from a r^1/4^ fit to the observed radial photometric profile of each galaxy. A comparison with similar data found in the literature for the Coma Cluster shows that large systematic uncertainties can be introduced in the measurement of r_e_ and {mu}_e_ by the particular method used to derive those parameters. However, the particular combination of these two parameters that enters in the fundamental plane relation is a quantity that can be measured with high accuracy.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/116/2728#table3</TD>
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            <TD>SA57XMM [1]</TD>
            <TD>Selected Area 57 XMM-Newton X-Ray Source Catalog</TD>
            <TD>The maximum number density of Active Galactic Nuclei (AGNs), as deduced from X-ray studies, occurs at z &gt;= 1, with lower luminosity objects peaking at smaller redshifts. Optical studies lead to a different evolutionary behaviour, with a number density peaking at z ~ 2 independently of the intrinsic luminosity, but this result is limited to active nuclei brighter than the host galaxy. A selection based on optical variability can detect low luminosity AGNs (LLAGNs), where the host galaxy light prevents the identification by non-stellar colours. The authors collected X-ray data in a field where there existed an optically-selected sample of "variable galaxies", i.e. variable objects with diffuse appearance, in order to investigate the X-ray and optical properties of the population of AGNs, particularly of low luminosity ones, where the host galaxy is visible. They observed a field of ~ 0.2 deg^2 in the Selected Area 57, for 67 ks with XMM-Newton. They correlated the list of detected X-ray sources with a photographic survey of SA 57, complete to B_J ~ 23 and with the available spectroscopic data. They obtained a catalog of 140 X-ray sources to limiting fluxes of 5 x 10^-16 and 2 x 10^-15 erg/cm^2/s in the 0.5 - 2 keV and 2 - 10 keV bands, respectively, 98 of which are identified in the optical bands. The X-ray detection of part of the variability-selected candidates confirms their AGN nature. Diffuse variable objects populate the low luminosity side of the sample. Only 25/44 optically-selected QSOs are detected in X-rays. 15% of all QSOs in the field have X/O &lt; 0.1. Additional information on the likely optical counterparts of 98 of the X-ray sources is available in the reference paper, e.g., in Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>180</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>SA57XMM [2]</TD>
            <TD>Selected Area 57 XMM-Newton X-Ray Source Catalog</TD>
            <TD>The maximum number density of Active Galactic Nuclei (AGNs), as deduced from X-ray studies, occurs at z &gt;= 1, with lower luminosity objects peaking at smaller redshifts. Optical studies lead to a different evolutionary behaviour, with a number density peaking at z ~ 2 independently of the intrinsic luminosity, but this result is limited to active nuclei brighter than the host galaxy. A selection based on optical variability can detect low luminosity AGNs (LLAGNs), where the host galaxy light prevents the identification by non-stellar colours. The authors collected X-ray data in a field where there existed an optically-selected sample of "variable galaxies", i.e. variable objects with diffuse appearance, in order to investigate the X-ray and optical properties of the population of AGNs, particularly of low luminosity ones, where the host galaxy is visible. They observed a field of ~ 0.2 deg^2 in the Selected Area 57, for 67 ks with XMM-Newton. They correlated the list of detected X-ray sources with a photographic survey of SA 57, complete to B_J ~ 23 and with the available spectroscopic data. They obtained a catalog of 140 X-ray sources to limiting fluxes of 5 x 10^-16 and 2 x 10^-15 erg/cm^2/s in the 0.5 - 2 keV and 2 - 10 keV bands, respectively, 98 of which are identified in the optical bands. The X-ray detection of part of the variability-selected candidates confirms their AGN nature. Diffuse variable objects populate the low luminosity side of the sample. Only 25/44 optically-selected QSOs are detected in X-rays. 15% of all QSOs in the field have X/O &lt; 0.1. Additional information on the likely optical counterparts of 98 of the X-ray sources is available in the reference paper, e.g., in Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sa57xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
            <TD>We report R- and V-band photometry derived from CCD imaging for objects in nine fields in and around the Draco dwarf spheroidal galaxy. The most distant fields are about 1.3{deg} from the center. We use these data to search for Draco stars outside of its measured tidal boundary. The search involves three methods: (1) plotting color-magnitude diagrams for individual fields, for sections of fields, and for combined fields and sections - a colour-magnitude diagram can reveal a population of Draco stars by the presence of the expected principal sequences; (2) measuring field-to-field fluctuations in the surface density of objects located near the Draco principal sequences in the color-magnitude diagram; (3) measuring intrafield fluctuations in the surface density of those objects. We find evidence for the presence of Draco stars immediately beyond the measured tidal boundary of Draco and place an upper limit on the number of such stars in more distant fields that lie close to the extension of its major axis. The best evidence is the presence of the Draco principal sequences in the color-magnitude diagram for some combined fields and sections of fields. The measurements of the field-to-field fluctuations in the stellar surface density confirm this result.</TD>
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            <TD>J/AJ/121/841 [2]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
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            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
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            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
            <TD>We report R- and V-band photometry derived from CCD imaging for objects in nine fields in and around the Draco dwarf spheroidal galaxy. The most distant fields are about 1.3{deg} from the center. We use these data to search for Draco stars outside of its measured tidal boundary. The search involves three methods: (1) plotting color-magnitude diagrams for individual fields, for sections of fields, and for combined fields and sections - a colour-magnitude diagram can reveal a population of Draco stars by the presence of the expected principal sequences; (2) measuring field-to-field fluctuations in the surface density of objects located near the Draco principal sequences in the color-magnitude diagram; (3) measuring intrafield fluctuations in the surface density of those objects. We find evidence for the presence of Draco stars immediately beyond the measured tidal boundary of Draco and place an upper limit on the number of such stars in more distant fields that lie close to the extension of its major axis. The best evidence is the presence of the Draco principal sequences in the color-magnitude diagram for some combined fields and sections of fields. The measurements of the field-to-field fluctuations in the stellar surface density confirm this result.</TD>
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            <TD>Selected Area 57 XMM-Newton X-Ray Source Catalog</TD>
            <TD>The maximum number density of Active Galactic Nuclei (AGNs), as deduced from X-ray studies, occurs at z &gt;= 1, with lower luminosity objects peaking at smaller redshifts. Optical studies lead to a different evolutionary behaviour, with a number density peaking at z ~ 2 independently of the intrinsic luminosity, but this result is limited to active nuclei brighter than the host galaxy. A selection based on optical variability can detect low luminosity AGNs (LLAGNs), where the host galaxy light prevents the identification by non-stellar colours. The authors collected X-ray data in a field where there existed an optically-selected sample of "variable galaxies", i.e. variable objects with diffuse appearance, in order to investigate the X-ray and optical properties of the population of AGNs, particularly of low luminosity ones, where the host galaxy is visible. They observed a field of ~ 0.2 deg^2 in the Selected Area 57, for 67 ks with XMM-Newton. They correlated the list of detected X-ray sources with a photographic survey of SA 57, complete to B_J ~ 23 and with the available spectroscopic data. They obtained a catalog of 140 X-ray sources to limiting fluxes of 5 x 10^-16 and 2 x 10^-15 erg/cm^2/s in the 0.5 - 2 keV and 2 - 10 keV bands, respectively, 98 of which are identified in the optical bands. The X-ray detection of part of the variability-selected candidates confirms their AGN nature. Diffuse variable objects populate the low luminosity side of the sample. Only 25/44 optically-selected QSOs are detected in X-rays. 15% of all QSOs in the field have X/O &lt; 0.1. Additional information on the likely optical counterparts of 98 of the X-ray sources is available in the reference paper, e.g., in Table 3.</TD>
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            <TD>Selected Area 57 XMM-Newton X-Ray Source Catalog</TD>
            <TD>The maximum number density of Active Galactic Nuclei (AGNs), as deduced from X-ray studies, occurs at z &gt;= 1, with lower luminosity objects peaking at smaller redshifts. Optical studies lead to a different evolutionary behaviour, with a number density peaking at z ~ 2 independently of the intrinsic luminosity, but this result is limited to active nuclei brighter than the host galaxy. A selection based on optical variability can detect low luminosity AGNs (LLAGNs), where the host galaxy light prevents the identification by non-stellar colours. The authors collected X-ray data in a field where there existed an optically-selected sample of "variable galaxies", i.e. variable objects with diffuse appearance, in order to investigate the X-ray and optical properties of the population of AGNs, particularly of low luminosity ones, where the host galaxy is visible. They observed a field of ~ 0.2 deg^2 in the Selected Area 57, for 67 ks with XMM-Newton. They correlated the list of detected X-ray sources with a photographic survey of SA 57, complete to B_J ~ 23 and with the available spectroscopic data. They obtained a catalog of 140 X-ray sources to limiting fluxes of 5 x 10^-16 and 2 x 10^-15 erg/cm^2/s in the 0.5 - 2 keV and 2 - 10 keV bands, respectively, 98 of which are identified in the optical bands. The X-ray detection of part of the variability-selected candidates confirms their AGN nature. Diffuse variable objects populate the low luminosity side of the sample. Only 25/44 optically-selected QSOs are detected in X-rays. 15% of all QSOs in the field have X/O &lt; 0.1. Additional information on the likely optical counterparts of 98 of the X-ray sources is available in the reference paper, e.g., in Table 3.</TD>
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            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
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            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
            <TD>We report R- and V-band photometry derived from CCD imaging for objects in nine fields in and around the Draco dwarf spheroidal galaxy. The most distant fields are about 1.3{deg} from the center. We use these data to search for Draco stars outside of its measured tidal boundary. The search involves three methods: (1) plotting color-magnitude diagrams for individual fields, for sections of fields, and for combined fields and sections - a colour-magnitude diagram can reveal a population of Draco stars by the presence of the expected principal sequences; (2) measuring field-to-field fluctuations in the surface density of objects located near the Draco principal sequences in the color-magnitude diagram; (3) measuring intrafield fluctuations in the surface density of those objects. We find evidence for the presence of Draco stars immediately beyond the measured tidal boundary of Draco and place an upper limit on the number of such stars in more distant fields that lie close to the extension of its major axis. The best evidence is the presence of the Draco principal sequences in the color-magnitude diagram for some combined fields and sections of fields. The measurements of the field-to-field fluctuations in the stellar surface density confirm this result.</TD>
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            <TD>J/AJ/121/841 [table4]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
            <TD>We report R- and V-band photometry derived from CCD imaging for objects in nine fields in and around the Draco dwarf spheroidal galaxy. The most distant fields are about 1.3{deg} from the center. We use these data to search for Draco stars outside of its measured tidal boundary. The search involves three methods: (1) plotting color-magnitude diagrams for individual fields, for sections of fields, and for combined fields and sections - a colour-magnitude diagram can reveal a population of Draco stars by the presence of the expected principal sequences; (2) measuring field-to-field fluctuations in the surface density of objects located near the Draco principal sequences in the color-magnitude diagram; (3) measuring intrafield fluctuations in the surface density of those objects. We find evidence for the presence of Draco stars immediately beyond the measured tidal boundary of Draco and place an upper limit on the number of such stars in more distant fields that lie close to the extension of its major axis. The best evidence is the presence of the Draco principal sequences in the color-magnitude diagram for some combined fields and sections of fields. The measurements of the field-to-field fluctuations in the stellar surface density confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/841#table4</TD>
            <TD>2011-09-14T20:33:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/841</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/841</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SA57XMM [1]</TD>
            <TD>Selected Area 57 XMM-Newton X-Ray Source Catalog</TD>
            <TD>The maximum number density of Active Galactic Nuclei (AGNs), as deduced from X-ray studies, occurs at z &gt;= 1, with lower luminosity objects peaking at smaller redshifts. Optical studies lead to a different evolutionary behaviour, with a number density peaking at z ~ 2 independently of the intrinsic luminosity, but this result is limited to active nuclei brighter than the host galaxy. A selection based on optical variability can detect low luminosity AGNs (LLAGNs), where the host galaxy light prevents the identification by non-stellar colours. The authors collected X-ray data in a field where there existed an optically-selected sample of "variable galaxies", i.e. variable objects with diffuse appearance, in order to investigate the X-ray and optical properties of the population of AGNs, particularly of low luminosity ones, where the host galaxy is visible. They observed a field of ~ 0.2 deg^2 in the Selected Area 57, for 67 ks with XMM-Newton. They correlated the list of detected X-ray sources with a photographic survey of SA 57, complete to B_J ~ 23 and with the available spectroscopic data. They obtained a catalog of 140 X-ray sources to limiting fluxes of 5 x 10^-16 and 2 x 10^-15 erg/cm^2/s in the 0.5 - 2 keV and 2 - 10 keV bands, respectively, 98 of which are identified in the optical bands. The X-ray detection of part of the variability-selected candidates confirms their AGN nature. Diffuse variable objects populate the low luminosity side of the sample. Only 25/44 optically-selected QSOs are detected in X-rays. 15% of all QSOs in the field have X/O &lt; 0.1. Additional information on the likely optical counterparts of 98 of the X-ray sources is available in the reference paper, e.g., in Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sa57xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sa57xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sa57xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/sa57xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SA57XMM [2]</TD>
            <TD>Selected Area 57 XMM-Newton X-Ray Source Catalog</TD>
            <TD>The maximum number density of Active Galactic Nuclei (AGNs), as deduced from X-ray studies, occurs at z &gt;= 1, with lower luminosity objects peaking at smaller redshifts. Optical studies lead to a different evolutionary behaviour, with a number density peaking at z ~ 2 independently of the intrinsic luminosity, but this result is limited to active nuclei brighter than the host galaxy. A selection based on optical variability can detect low luminosity AGNs (LLAGNs), where the host galaxy light prevents the identification by non-stellar colours. The authors collected X-ray data in a field where there existed an optically-selected sample of "variable galaxies", i.e. variable objects with diffuse appearance, in order to investigate the X-ray and optical properties of the population of AGNs, particularly of low luminosity ones, where the host galaxy is visible. They observed a field of ~ 0.2 deg^2 in the Selected Area 57, for 67 ks with XMM-Newton. They correlated the list of detected X-ray sources with a photographic survey of SA 57, complete to B_J ~ 23 and with the available spectroscopic data. They obtained a catalog of 140 X-ray sources to limiting fluxes of 5 x 10^-16 and 2 x 10^-15 erg/cm^2/s in the 0.5 - 2 keV and 2 - 10 keV bands, respectively, 98 of which are identified in the optical bands. The X-ray detection of part of the variability-selected candidates confirms their AGN nature. Diffuse variable objects populate the low luminosity side of the sample. Only 25/44 optically-selected QSOs are detected in X-rays. 15% of all QSOs in the field have X/O &lt; 0.1. Additional information on the likely optical counterparts of 98 of the X-ray sources is available in the reference paper, e.g., in Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sa57xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/sa57xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sa57xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/sa57xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SA57XMM [3]</TD>
            <TD>Selected Area 57 XMM-Newton X-Ray Source Catalog</TD>
            <TD>The maximum number density of Active Galactic Nuclei (AGNs), as deduced from X-ray studies, occurs at z &gt;= 1, with lower luminosity objects peaking at smaller redshifts. Optical studies lead to a different evolutionary behaviour, with a number density peaking at z ~ 2 independently of the intrinsic luminosity, but this result is limited to active nuclei brighter than the host galaxy. A selection based on optical variability can detect low luminosity AGNs (LLAGNs), where the host galaxy light prevents the identification by non-stellar colours. The authors collected X-ray data in a field where there existed an optically-selected sample of "variable galaxies", i.e. variable objects with diffuse appearance, in order to investigate the X-ray and optical properties of the population of AGNs, particularly of low luminosity ones, where the host galaxy is visible. They observed a field of ~ 0.2 deg^2 in the Selected Area 57, for 67 ks with XMM-Newton. They correlated the list of detected X-ray sources with a photographic survey of SA 57, complete to B_J ~ 23 and with the available spectroscopic data. They obtained a catalog of 140 X-ray sources to limiting fluxes of 5 x 10^-16 and 2 x 10^-15 erg/cm^2/s in the 0.5 - 2 keV and 2 - 10 keV bands, respectively, 98 of which are identified in the optical bands. The X-ray detection of part of the variability-selected candidates confirms their AGN nature. Diffuse variable objects populate the low luminosity side of the sample. Only 25/44 optically-selected QSOs are detected in X-rays. 15% of all QSOs in the field have X/O &lt; 0.1. Additional information on the likely optical counterparts of 98 of the X-ray sources is available in the reference paper, e.g., in Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sa57xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sa57xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sa57xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/sa57xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/841 [1]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
            <TD>We report R- and V-band photometry derived from CCD imaging for objects in nine fields in and around the Draco dwarf spheroidal galaxy. The most distant fields are about 1.3{deg} from the center. We use these data to search for Draco stars outside of its measured tidal boundary. The search involves three methods: (1) plotting color-magnitude diagrams for individual fields, for sections of fields, and for combined fields and sections - a colour-magnitude diagram can reveal a population of Draco stars by the presence of the expected principal sequences; (2) measuring field-to-field fluctuations in the surface density of objects located near the Draco principal sequences in the color-magnitude diagram; (3) measuring intrafield fluctuations in the surface density of those objects. We find evidence for the presence of Draco stars immediately beyond the measured tidal boundary of Draco and place an upper limit on the number of such stars in more distant fields that lie close to the extension of its major axis. The best evidence is the presence of the Draco principal sequences in the color-magnitude diagram for some combined fields and sections of fields. The measurements of the field-to-field fluctuations in the stellar surface density confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/841#1</TD>
            <TD>2011-09-14T20:33:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/121/841</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/841</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/841</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/841 [2]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
            <TD>We report R- and V-band photometry derived from CCD imaging for objects in nine fields in and around the Draco dwarf spheroidal galaxy. The most distant fields are about 1.3{deg} from the center. We use these data to search for Draco stars outside of its measured tidal boundary. The search involves three methods: (1) plotting color-magnitude diagrams for individual fields, for sections of fields, and for combined fields and sections - a colour-magnitude diagram can reveal a population of Draco stars by the presence of the expected principal sequences; (2) measuring field-to-field fluctuations in the surface density of objects located near the Draco principal sequences in the color-magnitude diagram; (3) measuring intrafield fluctuations in the surface density of those objects. We find evidence for the presence of Draco stars immediately beyond the measured tidal boundary of Draco and place an upper limit on the number of such stars in more distant fields that lie close to the extension of its major axis. The best evidence is the presence of the Draco principal sequences in the color-magnitude diagram for some combined fields and sections of fields. The measurements of the field-to-field fluctuations in the stellar surface density confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/841#2</TD>
            <TD>2011-09-14T20:33:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/841</TD>
            <TD />
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/841&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/841</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/841 [table1]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
            <TD>We report R- and V-band photometry derived from CCD imaging for objects in nine fields in and around the Draco dwarf spheroidal galaxy. The most distant fields are about 1.3{deg} from the center. We use these data to search for Draco stars outside of its measured tidal boundary. The search involves three methods: (1) plotting color-magnitude diagrams for individual fields, for sections of fields, and for combined fields and sections - a colour-magnitude diagram can reveal a population of Draco stars by the presence of the expected principal sequences; (2) measuring field-to-field fluctuations in the surface density of objects located near the Draco principal sequences in the color-magnitude diagram; (3) measuring intrafield fluctuations in the surface density of those objects. We find evidence for the presence of Draco stars immediately beyond the measured tidal boundary of Draco and place an upper limit on the number of such stars in more distant fields that lie close to the extension of its major axis. The best evidence is the presence of the Draco principal sequences in the color-magnitude diagram for some combined fields and sections of fields. The measurements of the field-to-field fluctuations in the stellar surface density confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/841#table1</TD>
            <TD>2011-09-14T20:33:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/841</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/841&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/841</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/841 [table4]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2001)</TD>
            <TD>We report R- and V-band photometry derived from CCD imaging for objects in nine fields in and around the Draco dwarf spheroidal galaxy. The most distant fields are about 1.3{deg} from the center. We use these data to search for Draco stars outside of its measured tidal boundary. The search involves three methods: (1) plotting color-magnitude diagrams for individual fields, for sections of fields, and for combined fields and sections - a colour-magnitude diagram can reveal a population of Draco stars by the presence of the expected principal sequences; (2) measuring field-to-field fluctuations in the surface density of objects located near the Draco principal sequences in the color-magnitude diagram; (3) measuring intrafield fluctuations in the surface density of those objects. We find evidence for the presence of Draco stars immediately beyond the measured tidal boundary of Draco and place an upper limit on the number of such stars in more distant fields that lie close to the extension of its major axis. The best evidence is the presence of the Draco principal sequences in the color-magnitude diagram for some combined fields and sections of fields. The measurements of the field-to-field fluctuations in the stellar surface density confirm this result.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/841#table4</TD>
            <TD>2011-09-14T20:33:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/841</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/841&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/841</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Shk.(Group) [1]</TD>
            <TD>Shakbazian Compact Groups of Galaxies</TD>
            <TD>This catalog is a compilation of ten lists of compact groups of compact galaxies found on the Palomar Sky Survey red charts and published in the period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog contains 377 groups of compact galaxies and includes identifications, equatorial coordinates, numbers of constituent galaxies, magnitudes of the brightest member, sizes of the groups as a whole, and coefficients of relative compactness. The HEASARC has a related database table, SHKGALAXY, which contains data on the individual galaxies in the Shakhbazian Compact Groups.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shk#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shk</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=shk&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shk.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Shk.(Group) [2]</TD>
            <TD>Shakbazian Compact Groups of Galaxies</TD>
            <TD>This catalog is a compilation of ten lists of compact groups of compact galaxies found on the Palomar Sky Survey red charts and published in the period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog contains 377 groups of compact galaxies and includes identifications, equatorial coordinates, numbers of constituent galaxies, magnitudes of the brightest member, sizes of the groups as a whole, and coefficients of relative compactness. The HEASARC has a related database table, SHKGALAXY, which contains data on the individual galaxies in the Shakhbazian Compact Groups.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shk#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shk</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=shk&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shk.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Shk.(Group) [3]</TD>
            <TD>Shakbazian Compact Groups of Galaxies</TD>
            <TD>This catalog is a compilation of ten lists of compact groups of compact galaxies found on the Palomar Sky Survey red charts and published in the period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog contains 377 groups of compact galaxies and includes identifications, equatorial coordinates, numbers of constituent galaxies, magnitudes of the brightest member, sizes of the groups as a whole, and coefficients of relative compactness. The HEASARC has a related database table, SHKGALAXY, which contains data on the individual galaxies in the Shakhbazian Compact Groups.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shk#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shk</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_shk&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shk.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/98/1305 [1]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#1</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/98/1305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/98/1305 [2]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#2</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/98/1305 [posmk]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#posmk</TD>
            <TD>2011-09-14T20:33:47Z</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/98/1305 [table2]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#table2</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/98/1305 [table7]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#table7</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>Shk.(Group) [1]</TD>
            <TD>Shakbazian Compact Groups of Galaxies</TD>
            <TD>This catalog is a compilation of ten lists of compact groups of compact galaxies found on the Palomar Sky Survey red charts and published in the period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog contains 377 groups of compact galaxies and includes identifications, equatorial coordinates, numbers of constituent galaxies, magnitudes of the brightest member, sizes of the groups as a whole, and coefficients of relative compactness. The HEASARC has a related database table, SHKGALAXY, which contains data on the individual galaxies in the Shakhbazian Compact Groups.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shk#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shk</TD>
            <TD>ConeSearch</TD>
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            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shk.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Shk.(Group) [2]</TD>
            <TD>Shakbazian Compact Groups of Galaxies</TD>
            <TD>This catalog is a compilation of ten lists of compact groups of compact galaxies found on the Palomar Sky Survey red charts and published in the period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog contains 377 groups of compact galaxies and includes identifications, equatorial coordinates, numbers of constituent galaxies, magnitudes of the brightest member, sizes of the groups as a whole, and coefficients of relative compactness. The HEASARC has a related database table, SHKGALAXY, which contains data on the individual galaxies in the Shakhbazian Compact Groups.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shk#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=shk&amp;</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shk.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Shk.(Group) [3]</TD>
            <TD>Shakbazian Compact Groups of Galaxies</TD>
            <TD>This catalog is a compilation of ten lists of compact groups of compact galaxies found on the Palomar Sky Survey red charts and published in the period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog contains 377 groups of compact galaxies and includes identifications, equatorial coordinates, numbers of constituent galaxies, magnitudes of the brightest member, sizes of the groups as a whole, and coefficients of relative compactness. The HEASARC has a related database table, SHKGALAXY, which contains data on the individual galaxies in the Shakhbazian Compact Groups.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shk#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shk</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_shk&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/98/1305 [1]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#1</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/98/1305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/98/1305 [2]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#2</TD>
            <TD>2011-09-14T20:33:47Z</TD>
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            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD />
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/98/1305 [posmk]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#posmk</TD>
            <TD>2011-09-14T20:33:47Z</TD>
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            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/98/1305 [table2]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#table2</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/98/1305 [table7]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#table7</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Shk.(Group) [1]</TD>
            <TD>Shakbazian Compact Groups of Galaxies</TD>
            <TD>This catalog is a compilation of ten lists of compact groups of compact galaxies found on the Palomar Sky Survey red charts and published in the period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog contains 377 groups of compact galaxies and includes identifications, equatorial coordinates, numbers of constituent galaxies, magnitudes of the brightest member, sizes of the groups as a whole, and coefficients of relative compactness. The HEASARC has a related database table, SHKGALAXY, which contains data on the individual galaxies in the Shakhbazian Compact Groups.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shk#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shk</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=shk&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shk.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Shk.(Group) [2]</TD>
            <TD>Shakbazian Compact Groups of Galaxies</TD>
            <TD>This catalog is a compilation of ten lists of compact groups of compact galaxies found on the Palomar Sky Survey red charts and published in the period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog contains 377 groups of compact galaxies and includes identifications, equatorial coordinates, numbers of constituent galaxies, magnitudes of the brightest member, sizes of the groups as a whole, and coefficients of relative compactness. The HEASARC has a related database table, SHKGALAXY, which contains data on the individual galaxies in the Shakhbazian Compact Groups.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shk#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shk</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=shk&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shk.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Shk.(Group) [3]</TD>
            <TD>Shakbazian Compact Groups of Galaxies</TD>
            <TD>This catalog is a compilation of ten lists of compact groups of compact galaxies found on the Palomar Sky Survey red charts and published in the period 1973 to 1979 by Shakhbazian, Petrosian, and collaborators. The catalog contains 377 groups of compact galaxies and includes identifications, equatorial coordinates, numbers of constituent galaxies, magnitudes of the brightest member, sizes of the groups as a whole, and coefficients of relative compactness. The HEASARC has a related database table, SHKGALAXY, which contains data on the individual galaxies in the Shakhbazian Compact Groups.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shk#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shk</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_shk&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shk.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/98/1305 [1]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#1</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/98/1305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/98/1305 [2]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#2</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/98/1305 [posmk]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#posmk</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/98/1305 [table2]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#table2</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/98/1305 [table7]</TD>
            <TD>Stellar content of NGC 346 (Massey+, 1989)</TD>
            <TD>Using CCD UBV photometry and spectroscopy, we have investigated the stellar content of NGC 346, the brightest H II region in the SMC. Spectra of 42 stars confirm that 33 are of O type, of which 11 are of type O6.5 or earlier; this is as many early-type O stars as is known in the rest of the SMC. From the spectroscopy and photometry we are able to construct an H-R diagram which is essentially complete down to ~10M_{sun}_. We find an initial mass-function slope {GAMMA}=-1.9, similar to that found for massive stars near the Sun and in the LMC: the presence of six stars in the mass range 40-85M_{sun}_ suggests that the upper-mass limit of the IMF is also not appreciably lower in the SMC than it is in the Galaxy. Our photometry has identified five probable red supergiants of which one was previously known. These stars, plus two B supergiants, are evolved stars of considerably lower mass (15M_{sun}_) than many of the unevolved cluster members. Most of these lower-mass, evolved stars form a spatially distinct subgroup; we believe that NGC 346 thus provides an example of sequential star formation in the SMC. We also have identified a background field population of 5M_{sun}_ stars. We find that the ionizing flux from the hot stars is consistent with the previously known Half nebular luminosity. Finally, we discuss the enigmatic W-R binary HD 5980, which our point-spread-function fitting has identified as a close visual double.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305#table7</TD>
            <TD>2011-09-14T20:33:47Z</TD>
            <TD>#Photometry#Nebulae#HII_regions#Spectrophotometry#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/98/1305</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/98/1305&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/98/1305</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SPICESCXO [1]</TD>
            <TD>SPICES Lynx Field Chandra X-Ray Source Catalog</TD>
            <TD>This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10^-16 erg/cm^2/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10^-15 erg/cm^2/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K_s = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K_s &gt;= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s^-1 per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin^2. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N_H = 2 x 10^20 cm^-2. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H_0 = 50 h_50 km s^-1 Mpc^-1, Omega_M = 1, and Omega_Lambda = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H_0 = 65 km s^-1 Mpc^-1, Omega_M = 0.35, and Omega_Lambda = 0.65).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/spicescxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/spicescxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=spicescxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/spicescxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SPICESCXO [2]</TD>
            <TD>SPICES Lynx Field Chandra X-Ray Source Catalog</TD>
            <TD>This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10^-16 erg/cm^2/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10^-15 erg/cm^2/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K_s = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K_s &gt;= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s^-1 per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin^2. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N_H = 2 x 10^20 cm^-2. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H_0 = 50 h_50 km s^-1 Mpc^-1, Omega_M = 1, and Omega_Lambda = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H_0 = 65 km s^-1 Mpc^-1, Omega_M = 0.35, and Omega_Lambda = 0.65).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/spicescxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/spicescxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=spicescxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/spicescxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SPICESCXO [3]</TD>
            <TD>SPICES Lynx Field Chandra X-Ray Source Catalog</TD>
            <TD>This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10^-16 erg/cm^2/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10^-15 erg/cm^2/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K_s = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K_s &gt;= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s^-1 per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin^2. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N_H = 2 x 10^20 cm^-2. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H_0 = 50 h_50 km s^-1 Mpc^-1, Omega_M = 1, and Omega_Lambda = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H_0 = 65 km s^-1 Mpc^-1, Omega_M = 0.35, and Omega_Lambda = 0.65).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/spicescxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/spicescxo</TD>
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_spicescxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/spicescxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/398/1129 [1]</TD>
            <TD>Central galaxies in groups and clusters (Guo+, 2009)</TD>
            <TD>#+++ 3 non-ascii chars (line 63) %B Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129#1</TD>
            <TD>2011-09-14T20:55:04Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/398/1129</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/1129</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/398/1129 [2]</TD>
            <TD>Central galaxies in groups and clusters (Guo+, 2009)</TD>
            <TD>#+++ 3 non-ascii chars (line 63) %B Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129#2</TD>
            <TD>2011-09-14T20:55:04Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/398/1129&amp;</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/398/1129 [samples]</TD>
            <TD>Central galaxies in groups and clusters (Guo+, 2009)</TD>
            <TD>#+++ 3 non-ascii chars (line 63) %B Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129#samples</TD>
            <TD>2011-09-14T20:55:04Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/398/1129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/1129</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>SPICESCXO [1]</TD>
            <TD>SPICES Lynx Field Chandra X-Ray Source Catalog</TD>
            <TD>This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10^-16 erg/cm^2/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10^-15 erg/cm^2/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K_s = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K_s &gt;= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s^-1 per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin^2. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N_H = 2 x 10^20 cm^-2. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H_0 = 50 h_50 km s^-1 Mpc^-1, Omega_M = 1, and Omega_Lambda = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H_0 = 65 km s^-1 Mpc^-1, Omega_M = 0.35, and Omega_Lambda = 0.65).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/spicescxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/spicescxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=spicescxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/spicescxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SPICESCXO [2]</TD>
            <TD>SPICES Lynx Field Chandra X-Ray Source Catalog</TD>
            <TD>This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10^-16 erg/cm^2/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10^-15 erg/cm^2/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K_s = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K_s &gt;= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s^-1 per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin^2. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N_H = 2 x 10^20 cm^-2. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H_0 = 50 h_50 km s^-1 Mpc^-1, Omega_M = 1, and Omega_Lambda = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H_0 = 65 km s^-1 Mpc^-1, Omega_M = 0.35, and Omega_Lambda = 0.65).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/spicescxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ParamHTTP</TD>
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            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/spicescxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SPICESCXO [3]</TD>
            <TD>SPICES Lynx Field Chandra X-Ray Source Catalog</TD>
            <TD>This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10^-16 erg/cm^2/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10^-15 erg/cm^2/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K_s = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K_s &gt;= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s^-1 per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin^2. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N_H = 2 x 10^20 cm^-2. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H_0 = 50 h_50 km s^-1 Mpc^-1, Omega_M = 1, and Omega_Lambda = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H_0 = 65 km s^-1 Mpc^-1, Omega_M = 0.35, and Omega_Lambda = 0.65).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/spicescxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD />
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            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_spicescxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/spicescxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/398/1129 [1]</TD>
            <TD>Central galaxies in groups and clusters (Guo+, 2009)</TD>
            <TD>#+++ 3 non-ascii chars (line 63) %B Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129#1</TD>
            <TD>2011-09-14T20:55:04Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/398/1129</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/1129</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/398/1129 [2]</TD>
            <TD>Central galaxies in groups and clusters (Guo+, 2009)</TD>
            <TD>#+++ 3 non-ascii chars (line 63) %B Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129#2</TD>
            <TD>2011-09-14T20:55:04Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/398/1129&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/1129</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/398/1129 [samples]</TD>
            <TD>Central galaxies in groups and clusters (Guo+, 2009)</TD>
            <TD>#+++ 3 non-ascii chars (line 63) %B Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129#samples</TD>
            <TD>2011-09-14T20:55:04Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/398/1129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/1129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SPICESCXO [1]</TD>
            <TD>SPICES Lynx Field Chandra X-Ray Source Catalog</TD>
            <TD>This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10^-16 erg/cm^2/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10^-15 erg/cm^2/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K_s = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K_s &gt;= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s^-1 per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin^2. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N_H = 2 x 10^20 cm^-2. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H_0 = 50 h_50 km s^-1 Mpc^-1, Omega_M = 1, and Omega_Lambda = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H_0 = 65 km s^-1 Mpc^-1, Omega_M = 0.35, and Omega_Lambda = 0.65).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/spicescxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/spicescxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=spicescxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/spicescxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SPICESCXO [2]</TD>
            <TD>SPICES Lynx Field Chandra X-Ray Source Catalog</TD>
            <TD>This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10^-16 erg/cm^2/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10^-15 erg/cm^2/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K_s = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K_s &gt;= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s^-1 per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin^2. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N_H = 2 x 10^20 cm^-2. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H_0 = 50 h_50 km s^-1 Mpc^-1, Omega_M = 1, and Omega_Lambda = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H_0 = 65 km s^-1 Mpc^-1, Omega_M = 0.35, and Omega_Lambda = 0.65).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/spicescxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/spicescxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=spicescxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/spicescxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SPICESCXO [3]</TD>
            <TD>SPICES Lynx Field Chandra X-Ray Source Catalog</TD>
            <TD>This table contains the first results on field X-ray sources detected in a deep, 184.7 ks observation with the Advanced CCD Imaging Spectrometer (ACIS-I) on the Chandra X-Ray Observatory. The observations target the Lynx field (J2000.0 RA = 08h 48m and Dec = +44d 54') of SPICES, the Spectroscopic Photometric Infrared-Chosen Extragalactic Survey, which contains three known X-ray-emitting clusters at redshifts of z = 0.57, 1.26, and 1.27. Not including the known clusters, in the 17' x 17' ACIS-I field the authors detect 132 sources in the 0.5 - 2 keV (soft) X-ray band down to a 2.1-sigma limiting flux of ~ 1.7 x 10^-16 erg/cm^2/s and 11 sources in the 2 - 10 keV (hard) X-ray band down to a 2.1-sigma limiting flux of ~ 1.3 x 10^-15 erg/cm^2/s. The combined catalog contains a total of 153 X-ray sources, of which 42 are detected only in the soft band and 21 are detected only in the hard band. Confirming previous Chandra results, the authors find that the fainter sources have harder X-ray spectra, providing a consistent solution to the long-standing "spectral paradox". From deep optical and near-infrared follow-up data, 77% of the X-ray sources have optical counterparts to I = 24, and 71% of the X-ray sources have near-infrared counterparts to K_s = 20. Four of the 24 sources in the near-IR field are associated with extremely red objects (EROs; I - K_s &gt;= 4). The authors have obtained spectroscopic redshifts with the Keck telescopes of 18 of the Lynx Chandra sources. These sources comprise a mix of broad-lined active galaxies, apparently normal galaxies, and two late-type Galactic dwarfs. Intriguingly, one Galactic source (number 72) is identified with an M7 dwarf exhibiting nontransient, hard X-ray emission. Thirteen of the Chandra sources are located within regions for which the authors have Hubble Space Telescope imaging. Nine of the sources are detected, showing a range of morphologies: several show compact cores embedded within diffuse emission, while others are spatially extended showing typical galaxy morphologies. Two of the Chandra sources in this subsample appear to be associated with mergers. ACIS-I observations of the Lynx field were obtained on 2000 May 3 (65 ks; OBS-ID 1708) and 2000 May 4 (125 ks; OBS-ID 927). Time intervals with background rates larger than 3 sigma over the quiescent value of ~ 0.30 counts s^-1 per chip in the 0.3 - 10 keV band were removed. This procedure gave 60.7 ks of effective exposure out of the first observation and 124 ks out of the second, for a total of 184.7 ks. The two observations are almost coincident on the sky, so that the total coverage is 298 arcmin^2. The aim point for the observations was RA = 08h 48m 54.79s, Dec = +44d 54' 32.9" (J2000.0), and both exposures were obtained in the faint mode when ACIS was at a temperature of -120 C. The Galactic absorbing column for this field is N_H = 2 x 10^20 cm^-2. The position angle of the observations was 258.45 degrees. Cosmology-dependent parameters are calculated for two models: an Einstein-de Sitter (EdS) universe consistent with previous work in this field (H_0 = 50 h_50 km s^-1 Mpc^-1, Omega_M = 1, and Omega_Lambda = 0) and the dark energy cosmology (DEC) universe favored by recent work on high-redshift supernovae and fluctuations in the cosmic microwave background (H_0 = 65 km s^-1 Mpc^-1, Omega_M = 0.35, and Omega_Lambda = 0.65).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/spicescxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/spicescxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_spicescxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/spicescxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/398/1129 [1]</TD>
            <TD>Central galaxies in groups and clusters (Guo+, 2009)</TD>
            <TD>#+++ 3 non-ascii chars (line 63) %B Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129#1</TD>
            <TD>2011-09-14T20:55:04Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/398/1129</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/1129</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/398/1129 [2]</TD>
            <TD>Central galaxies in groups and clusters (Guo+, 2009)</TD>
            <TD>#+++ 3 non-ascii chars (line 63) %B Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129#2</TD>
            <TD>2011-09-14T20:55:04Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/398/1129&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/1129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/398/1129 [samples]</TD>
            <TD>Central galaxies in groups and clusters (Guo+, 2009)</TD>
            <TD>#+++ 3 non-ascii chars (line 63) %B Using a statistically representative sample of 911 central galaxies (CENs) from the Sloan Digital Sky Survey (SDSS) Data Release 4 group catalogue, we study how the structure (shape and size) of the first rank (by stellar mass) group and cluster members depends on (1) galaxy stellar mass (M_star_), (2) the global environment defined by the dark matter halo mass (M_halo_) of the host group and (3) the local environment defined by their special halocentric position. We quantify the structure of SDSS galaxies with a galfit-based pipeline that fits two-dimensional Sersic models to the r-band image data. Through tests with simulated and real galaxy images, we demonstrate that our pipeline can recover Sersic parameters without significant bias. Moreover, to test the impact of local environment on CENs, we compare the structure of CENs with that satellite galaxies (SATs) of comparable M_star_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129#samples</TD>
            <TD>2011-09-14T20:55:04Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/1129</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/398/1129&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/1129</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UZC [1]</TD>
            <TD>Updated Zwicky Catalog</TD>
            <TD>The Zwicky Catalog of Galaxies, with a magnitude limit m_Zw &lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~&lt;2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m_Zw &lt;=15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr &gt;= RA(1950) &lt;= 4 hr and 8 hr &lt;= RA(1950) &lt;= 17 hr and the declination range -2.5 degrees &lt;= Dec(1950) &lt;= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/uzc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/uzc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=uzc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/uzc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UZC [2]</TD>
            <TD>Updated Zwicky Catalog</TD>
            <TD>The Zwicky Catalog of Galaxies, with a magnitude limit m_Zw &lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~&lt;2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m_Zw &lt;=15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr &gt;= RA(1950) &lt;= 4 hr and 8 hr &lt;= RA(1950) &lt;= 17 hr and the declination range -2.5 degrees &lt;= Dec(1950) &lt;= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/uzc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/uzc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=uzc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/uzc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>UZC [3]</TD>
            <TD>Updated Zwicky Catalog</TD>
            <TD>The Zwicky Catalog of Galaxies, with a magnitude limit m_Zw &lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~&lt;2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m_Zw &lt;=15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr &gt;= RA(1950) &lt;= 4 hr and 8 hr &lt;= RA(1950) &lt;= 17 hr and the declination range -2.5 degrees &lt;= Dec(1950) &lt;= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/uzc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/uzc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_uzc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/uzc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UZC [1]</TD>
            <TD>Updated Zwicky Catalog</TD>
            <TD>The Zwicky Catalog of Galaxies, with a magnitude limit m_Zw &lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~&lt;2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m_Zw &lt;=15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr &gt;= RA(1950) &lt;= 4 hr and 8 hr &lt;= RA(1950) &lt;= 17 hr and the declination range -2.5 degrees &lt;= Dec(1950) &lt;= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/uzc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/uzc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=uzc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/uzc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UZC [2]</TD>
            <TD>Updated Zwicky Catalog</TD>
            <TD>The Zwicky Catalog of Galaxies, with a magnitude limit m_Zw &lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~&lt;2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m_Zw &lt;=15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr &gt;= RA(1950) &lt;= 4 hr and 8 hr &lt;= RA(1950) &lt;= 17 hr and the declination range -2.5 degrees &lt;= Dec(1950) &lt;= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/uzc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/uzc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=uzc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/uzc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>UZC [3]</TD>
            <TD>Updated Zwicky Catalog</TD>
            <TD>The Zwicky Catalog of Galaxies, with a magnitude limit m_Zw &lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~&lt;2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m_Zw &lt;=15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr &gt;= RA(1950) &lt;= 4 hr and 8 hr &lt;= RA(1950) &lt;= 17 hr and the declination range -2.5 degrees &lt;= Dec(1950) &lt;= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/uzc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/uzc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_uzc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/uzc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/2398 [1]</TD>
            <TD>Stellar SEDs in SDSS and 2MASS filters (Covey+, 2007)</TD>
            <TD>The Sloan Digital Sky Survey (SDSS) and Two Micron All Sky Survey (2MASS) are rich resources for studying stellar astrophysics and the structure and formation history of the Galaxy. As new surveys and instruments adopt similar filter sets, it is increasingly important to understand the properties of the ugrizJHKs stellar locus, both to inform studies of "normal" main-sequence stars and enable robust searches for point sources with unusual colors. Using a sample of ~600000 point sources detected by SDSS and 2MASS, we tabulate the position and width of the ugrizJHKs stellar locus as a function of g-i color, and provide accurate polynomial fits. We map the Morgan-Keenan spectral type sequence to the median stellar locus by using synthetic photometry of spectral standards and by analyzing 3000 SDSS stellar spectra with a custom spectral typing pipeline, described in the Appendix to this paper. We develop an algorithm to calculate a point source's minimum separation from the stellar locus in a seven-dimensional color space, and use it to robustly identify objects with unusual colors, as well as spurious SDSS/2MASS matches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2398#1</TD>
            <TD>2011-09-14T20:55:11Z</TD>
            <TD>#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2398</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/2398</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2398</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/2398 [2]</TD>
            <TD>Stellar SEDs in SDSS and 2MASS filters (Covey+, 2007)</TD>
            <TD>The Sloan Digital Sky Survey (SDSS) and Two Micron All Sky Survey (2MASS) are rich resources for studying stellar astrophysics and the structure and formation history of the Galaxy. As new surveys and instruments adopt similar filter sets, it is increasingly important to understand the properties of the ugrizJHKs stellar locus, both to inform studies of "normal" main-sequence stars and enable robust searches for point sources with unusual colors. Using a sample of ~600000 point sources detected by SDSS and 2MASS, we tabulate the position and width of the ugrizJHKs stellar locus as a function of g-i color, and provide accurate polynomial fits. We map the Morgan-Keenan spectral type sequence to the median stellar locus by using synthetic photometry of spectral standards and by analyzing 3000 SDSS stellar spectra with a custom spectral typing pipeline, described in the Appendix to this paper. We develop an algorithm to calculate a point source's minimum separation from the stellar locus in a seven-dimensional color space, and use it to robustly identify objects with unusual colors, as well as spurious SDSS/2MASS matches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2398#2</TD>
            <TD>2011-09-14T20:55:11Z</TD>
            <TD>#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2398</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/2398&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2398</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UZC [1]</TD>
            <TD>Updated Zwicky Catalog</TD>
            <TD>The Zwicky Catalog of Galaxies, with a magnitude limit m_Zw &lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~&lt;2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m_Zw &lt;=15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr &gt;= RA(1950) &lt;= 4 hr and 8 hr &lt;= RA(1950) &lt;= 17 hr and the declination range -2.5 degrees &lt;= Dec(1950) &lt;= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/uzc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/uzc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=uzc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/uzc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UZC [2]</TD>
            <TD>Updated Zwicky Catalog</TD>
            <TD>The Zwicky Catalog of Galaxies, with a magnitude limit m_Zw &lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~&lt;2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m_Zw &lt;=15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr &gt;= RA(1950) &lt;= 4 hr and 8 hr &lt;= RA(1950) &lt;= 17 hr and the declination range -2.5 degrees &lt;= Dec(1950) &lt;= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/uzc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/uzc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=uzc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/uzc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>UZC [3]</TD>
            <TD>Updated Zwicky Catalog</TD>
            <TD>The Zwicky Catalog of Galaxies, with a magnitude limit m_Zw &lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the Zwicky Catalog and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. In this Updated Zwicky Catalog (UZC), some of the inadequacies of previous catalogs are corrected by providing (1) coordinates with ~&lt;2 arcsecond errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts cz (radial velocities) for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum are included. Redshifts (radial velocities) are provided for the 7257 galaxies in the CfA2 redshift survey that were not previously published; for another 5625 CfA redshifts (radial velocities), the remeasured or uniformly rereduced values are listed. Among the new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete. These multiplets provide new candidates for examination of tidal interaction among galaxies. All of the new redshifts (radial velocities) correspond to UZC galaxies with properties recorded in the CfA redshift compilation known as ZCAT. The redshift catalog included in the UZC is ~96% complete to m_Zw &lt;=15.5 and ~98% complete (12,925 galaxies out of a total of 13,150) for the right ascension ranges 20 hr &gt;= RA(1950) &lt;= 4 hr and 8 hr &lt;= RA(1950) &lt;= 17 hr and the declination range -2.5 degrees &lt;= Dec(1950) &lt;= 50 degrees. This more complete region includes all of the CfA2 survey as analyzed to the date of the publication of the UZC (1999).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/uzc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.25</TD>
            <TD />
            <TD>ivo://nasa.heasarc/uzc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_uzc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/uzc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/2398 [1]</TD>
            <TD>Stellar SEDs in SDSS and 2MASS filters (Covey+, 2007)</TD>
            <TD>The Sloan Digital Sky Survey (SDSS) and Two Micron All Sky Survey (2MASS) are rich resources for studying stellar astrophysics and the structure and formation history of the Galaxy. As new surveys and instruments adopt similar filter sets, it is increasingly important to understand the properties of the ugrizJHKs stellar locus, both to inform studies of "normal" main-sequence stars and enable robust searches for point sources with unusual colors. Using a sample of ~600000 point sources detected by SDSS and 2MASS, we tabulate the position and width of the ugrizJHKs stellar locus as a function of g-i color, and provide accurate polynomial fits. We map the Morgan-Keenan spectral type sequence to the median stellar locus by using synthetic photometry of spectral standards and by analyzing 3000 SDSS stellar spectra with a custom spectral typing pipeline, described in the Appendix to this paper. We develop an algorithm to calculate a point source's minimum separation from the stellar locus in a seven-dimensional color space, and use it to robustly identify objects with unusual colors, as well as spurious SDSS/2MASS matches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2398#1</TD>
            <TD>2011-09-14T20:55:11Z</TD>
            <TD>#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2398</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/2398</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2398</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/2398 [2]</TD>
            <TD>Stellar SEDs in SDSS and 2MASS filters (Covey+, 2007)</TD>
            <TD>The Sloan Digital Sky Survey (SDSS) and Two Micron All Sky Survey (2MASS) are rich resources for studying stellar astrophysics and the structure and formation history of the Galaxy. As new surveys and instruments adopt similar filter sets, it is increasingly important to understand the properties of the ugrizJHKs stellar locus, both to inform studies of "normal" main-sequence stars and enable robust searches for point sources with unusual colors. Using a sample of ~600000 point sources detected by SDSS and 2MASS, we tabulate the position and width of the ugrizJHKs stellar locus as a function of g-i color, and provide accurate polynomial fits. We map the Morgan-Keenan spectral type sequence to the median stellar locus by using synthetic photometry of spectral standards and by analyzing 3000 SDSS stellar spectra with a custom spectral typing pipeline, described in the Appendix to this paper. We develop an algorithm to calculate a point source's minimum separation from the stellar locus in a seven-dimensional color space, and use it to robustly identify objects with unusual colors, as well as spurious SDSS/2MASS matches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2398#2</TD>
            <TD>2011-09-14T20:55:11Z</TD>
            <TD>#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2398</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/2398&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2398</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMMCOSMOS [1]</TD>
            <TD>XMM-Newton COSMOS X-Ray Point Source Catalog</TD>
            <TD>This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg&lt;sup&gt;2&lt;/sup&gt;. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml &gt; 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s, ~9.3 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s and ~1.3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s over 90% of the area (1.92 deg&lt;sup&gt;2&lt;/sup&gt;) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcosmos#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcosmos</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xmmcosmos&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcosmos.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMMCOSMOS [2]</TD>
            <TD>XMM-Newton COSMOS X-Ray Point Source Catalog</TD>
            <TD>This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg&lt;sup&gt;2&lt;/sup&gt;. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml &gt; 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s, ~9.3 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s and ~1.3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s over 90% of the area (1.92 deg&lt;sup&gt;2&lt;/sup&gt;) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcosmos#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xmmcosmos&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcosmos.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMMCOSMOS [3]</TD>
            <TD>XMM-Newton COSMOS X-Ray Point Source Catalog</TD>
            <TD>This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg&lt;sup&gt;2&lt;/sup&gt;. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml &gt; 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s, ~9.3 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s and ~1.3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s over 90% of the area (1.92 deg&lt;sup&gt;2&lt;/sup&gt;) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcosmos#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xmmcosmos&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcosmos.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/259 [1]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#1</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/259</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/259 [2]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#2</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/259&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/259 [6dfgs]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#6dfgs</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/259 [spectra]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#spectra</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMMCOSMOS [1]</TD>
            <TD>XMM-Newton COSMOS X-Ray Point Source Catalog</TD>
            <TD>This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg&lt;sup&gt;2&lt;/sup&gt;. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml &gt; 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s, ~9.3 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s and ~1.3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s over 90% of the area (1.92 deg&lt;sup&gt;2&lt;/sup&gt;) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcosmos#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcosmos</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xmmcosmos&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcosmos.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMMCOSMOS [2]</TD>
            <TD>XMM-Newton COSMOS X-Ray Point Source Catalog</TD>
            <TD>This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg&lt;sup&gt;2&lt;/sup&gt;. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml &gt; 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s, ~9.3 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s and ~1.3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s over 90% of the area (1.92 deg&lt;sup&gt;2&lt;/sup&gt;) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcosmos#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xmmcosmos&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcosmos.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMMCOSMOS [3]</TD>
            <TD>XMM-Newton COSMOS X-Ray Point Source Catalog</TD>
            <TD>This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg&lt;sup&gt;2&lt;/sup&gt;. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml &gt; 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s, ~9.3 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s and ~1.3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s over 90% of the area (1.92 deg&lt;sup&gt;2&lt;/sup&gt;) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcosmos#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xmmcosmos&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcosmos.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/259 [1]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#1</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/259</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/259 [2]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#2</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/259&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/259 [6dfgs]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#6dfgs</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/259 [spectra]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#spectra</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XMMCOSMOS [1]</TD>
            <TD>XMM-Newton COSMOS X-Ray Point Source Catalog</TD>
            <TD>This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg&lt;sup&gt;2&lt;/sup&gt;. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml &gt; 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s, ~9.3 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s and ~1.3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s over 90% of the area (1.92 deg&lt;sup&gt;2&lt;/sup&gt;) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcosmos#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcosmos</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xmmcosmos&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcosmos.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XMMCOSMOS [2]</TD>
            <TD>XMM-Newton COSMOS X-Ray Point Source Catalog</TD>
            <TD>This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg&lt;sup&gt;2&lt;/sup&gt;. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml &gt; 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s, ~9.3 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s and ~1.3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s over 90% of the area (1.92 deg&lt;sup&gt;2&lt;/sup&gt;) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcosmos#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xmmcosmos&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcosmos.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XMMCOSMOS [3]</TD>
            <TD>XMM-Newton COSMOS X-Ray Point Source Catalog</TD>
            <TD>This table contains the XMM-Newton EPIC COSMOS X-ray point-like source catalog (XMM-COSMOS). The COSMOS survey is a multiwavelength survey aimed to study the evolution of galaxies, AGN and large scale structures. Within this survey, XMM-COSMOS is a powerful tool for detecting AGN and galaxy clusters. The XMM-COSMOS is a deep X-ray survey over the full 2 deg&lt;sup&gt;2&lt;/sup&gt; of the COSMOS area. It consists of 55 XMM-Newton pointings for a total exposure of ~1.5 Ms with an average vignetting-corrected depth of 40 ks across the field of view and a sky coverage of 2.13 deg&lt;sup&gt;2&lt;/sup&gt;. The analysis was performed using the XMM-SAS data analysis package in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands. Source detection has been performed using a maximum likelihood technique especially designed for raster scan surveys. The completeness of the catalog as well as log N-log S and source density maps have been calibrated using Monte Carlo simulations. This is the catalogue of point-like X-ray sources detected with the EPIC CCD cameras. The catalogs contains a total of 1887 unique sources detected in at least one band with likelihood parameter det_ml &gt; 10. The survey, which shows unprecedented homogeneity, has a flux limit of ~1.7 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s, ~9.3 x 10&lt;sup&gt;-15&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s and ~1.3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s over 90% of the area (1.92 deg&lt;sup&gt;2&lt;/sup&gt;) in the 0.5-2 keV, 2-10 keV and 5-10 keV energy bands, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xmmcosmos#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xmmcosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xmmcosmos&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/xmmcosmos.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/259 [1]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#1</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/259</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/259 [2]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#2</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/259&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/259 [6dfgs]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#6dfgs</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/259 [spectra]</TD>
            <TD>6dF galaxy survey final redshift release (Jones+, 2009)</TD>
            <TD>The final redshift release of the 6dF Galaxy Survey (6dFGS) is a combined redshift and peculiar velocity survey over the southern sky (|b|&gt;10{deg}). Its 136304 spectra have yielded 110256 new extragalactic redshifts and a new catalogue of 125071 galaxies making near-complete samples with limits in (K, H, J, rF, bJ) (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. The catalog includes basic data for the galaxies in the 6dFGS with redshifts, using the best 6dFGS redshifts (Q=3 or 4) plus available redshifts from SDSS, 2dFGRS and ZCAT (124647 entries in all). It supersedes the previous DR2 version (Cat. VII/249). The URL of the 6dFGS data base is: http://www-wfau.roe.ac.uk/6dFGS</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/259#spectra</TD>
            <TD>2011-09-14T20:56:15Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/VII/259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GLXSDSSQS2 [1]</TD>
            <TD>GALEX/SDSS z=0.5-1.5 QSO Candidates Catalog</TD>
            <TD>A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. In their paper, they discuss the distributions of redshift, luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be present in their final sample of 19,812 point sources. This latter catalog is available in the present table. This paper is based on archival data from the Galaxy Evolution Explorer (GALEX) which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034, and on data from the SDSS.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqs2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqs2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=glxsdssqs2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqs2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GLXSDSSQS2 [2]</TD>
            <TD>GALEX/SDSS z=0.5-1.5 QSO Candidates Catalog</TD>
            <TD>A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. In their paper, they discuss the distributions of redshift, luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be present in their final sample of 19,812 point sources. This latter catalog is available in the present table. This paper is based on archival data from the Galaxy Evolution Explorer (GALEX) which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034, and on data from the SDSS.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqs2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqs2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=glxsdssqs2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqs2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GLXSDSSQS2 [3]</TD>
            <TD>GALEX/SDSS z=0.5-1.5 QSO Candidates Catalog</TD>
            <TD>A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. In their paper, they discuss the distributions of redshift, luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be present in their final sample of 19,812 point sources. This latter catalog is available in the present table. This paper is based on archival data from the Galaxy Evolution Explorer (GALEX) which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034, and on data from the SDSS.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqs2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqs2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_glxsdssqs2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqs2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/ARA+A/43 [1]</TD>
            <TD>L and T dwarf stars (Kirkpatrick, 2005)</TD>
            <TD>The establishment of new spectral classes cooler than type M has had a brief, yet already rich, history. Prototypes of the new "L dwarf" and "T dwarf" classes were first found in the late 1980s to mid-1990s, with a flood of new discoveries occurring in the late 1990s with the advent of deep, large-area, digital sky surveys. Over four hundred and fifty L and T dwarfs are now catalogued. This review concentrates on the spectroscopic properties of these objects, beginning with the establishment of classification schemes rooted in the MK Process. The resulting grid of spectral types is then used as a tool to ferret out the underlying physics. The temperature ranges covered by these spectral types, the complex chemical processes responsible for the shape of their emergent spectra, their nature as either true stars or brown dwarfs, and their number density in the Galaxy are discussed. Two promising avenues for future research are also explored: the extension of the classification system to three dimensions to account for gravity- and metallicity-dependent features, and the capability of newer large-area surveys to uncover brown dwarfs cooler than those now recognized.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195#1</TD>
            <TD>2011-09-14T20:01:04Z</TD>
            <TD>#Stars#Spectral_Classification#Parallaxes#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/ARA+A/43.195</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ARA+A/43.195</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/ARA+A/43 [2]</TD>
            <TD>L and T dwarf stars (Kirkpatrick, 2005)</TD>
            <TD>The establishment of new spectral classes cooler than type M has had a brief, yet already rich, history. Prototypes of the new "L dwarf" and "T dwarf" classes were first found in the late 1980s to mid-1990s, with a flood of new discoveries occurring in the late 1990s with the advent of deep, large-area, digital sky surveys. Over four hundred and fifty L and T dwarfs are now catalogued. This review concentrates on the spectroscopic properties of these objects, beginning with the establishment of classification schemes rooted in the MK Process. The resulting grid of spectral types is then used as a tool to ferret out the underlying physics. The temperature ranges covered by these spectral types, the complex chemical processes responsible for the shape of their emergent spectra, their nature as either true stars or brown dwarfs, and their number density in the Galaxy are discussed. Two promising avenues for future research are also explored: the extension of the classification system to three dimensions to account for gravity- and metallicity-dependent features, and the capability of newer large-area surveys to uncover brown dwarfs cooler than those now recognized.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195#2</TD>
            <TD>2011-09-14T20:01:04Z</TD>
            <TD>#Stars#Spectral_Classification#Parallaxes#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/ARA+A/43.195&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ARA+A/43.195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/ARA+A/43 [table3]</TD>
            <TD>L and T dwarf stars (Kirkpatrick, 2005)</TD>
            <TD>The establishment of new spectral classes cooler than type M has had a brief, yet already rich, history. Prototypes of the new "L dwarf" and "T dwarf" classes were first found in the late 1980s to mid-1990s, with a flood of new discoveries occurring in the late 1990s with the advent of deep, large-area, digital sky surveys. Over four hundred and fifty L and T dwarfs are now catalogued. This review concentrates on the spectroscopic properties of these objects, beginning with the establishment of classification schemes rooted in the MK Process. The resulting grid of spectral types is then used as a tool to ferret out the underlying physics. The temperature ranges covered by these spectral types, the complex chemical processes responsible for the shape of their emergent spectra, their nature as either true stars or brown dwarfs, and their number density in the Galaxy are discussed. Two promising avenues for future research are also explored: the extension of the classification system to three dimensions to account for gravity- and metallicity-dependent features, and the capability of newer large-area surveys to uncover brown dwarfs cooler than those now recognized.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195#table3</TD>
            <TD>2011-09-14T20:01:04Z</TD>
            <TD>#Stars#Spectral_Classification#Parallaxes#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/ARA+A/43.195&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ARA+A/43.195</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/ARA+A/43 [1]</TD>
            <TD>L and T dwarf stars (Kirkpatrick, 2005)</TD>
            <TD>The establishment of new spectral classes cooler than type M has had a brief, yet already rich, history. Prototypes of the new "L dwarf" and "T dwarf" classes were first found in the late 1980s to mid-1990s, with a flood of new discoveries occurring in the late 1990s with the advent of deep, large-area, digital sky surveys. Over four hundred and fifty L and T dwarfs are now catalogued. This review concentrates on the spectroscopic properties of these objects, beginning with the establishment of classification schemes rooted in the MK Process. The resulting grid of spectral types is then used as a tool to ferret out the underlying physics. The temperature ranges covered by these spectral types, the complex chemical processes responsible for the shape of their emergent spectra, their nature as either true stars or brown dwarfs, and their number density in the Galaxy are discussed. Two promising avenues for future research are also explored: the extension of the classification system to three dimensions to account for gravity- and metallicity-dependent features, and the capability of newer large-area surveys to uncover brown dwarfs cooler than those now recognized.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195#1</TD>
            <TD>2011-09-14T20:01:04Z</TD>
            <TD>#Stars#Spectral_Classification#Parallaxes#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/ARA+A/43.195</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ARA+A/43.195</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/ARA+A/43 [2]</TD>
            <TD>L and T dwarf stars (Kirkpatrick, 2005)</TD>
            <TD>The establishment of new spectral classes cooler than type M has had a brief, yet already rich, history. Prototypes of the new "L dwarf" and "T dwarf" classes were first found in the late 1980s to mid-1990s, with a flood of new discoveries occurring in the late 1990s with the advent of deep, large-area, digital sky surveys. Over four hundred and fifty L and T dwarfs are now catalogued. This review concentrates on the spectroscopic properties of these objects, beginning with the establishment of classification schemes rooted in the MK Process. The resulting grid of spectral types is then used as a tool to ferret out the underlying physics. The temperature ranges covered by these spectral types, the complex chemical processes responsible for the shape of their emergent spectra, their nature as either true stars or brown dwarfs, and their number density in the Galaxy are discussed. Two promising avenues for future research are also explored: the extension of the classification system to three dimensions to account for gravity- and metallicity-dependent features, and the capability of newer large-area surveys to uncover brown dwarfs cooler than those now recognized.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195#2</TD>
            <TD>2011-09-14T20:01:04Z</TD>
            <TD>#Stars#Spectral_Classification#Parallaxes#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/ARA+A/43.195&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ARA+A/43.195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/ARA+A/43 [table3]</TD>
            <TD>L and T dwarf stars (Kirkpatrick, 2005)</TD>
            <TD>The establishment of new spectral classes cooler than type M has had a brief, yet already rich, history. Prototypes of the new "L dwarf" and "T dwarf" classes were first found in the late 1980s to mid-1990s, with a flood of new discoveries occurring in the late 1990s with the advent of deep, large-area, digital sky surveys. Over four hundred and fifty L and T dwarfs are now catalogued. This review concentrates on the spectroscopic properties of these objects, beginning with the establishment of classification schemes rooted in the MK Process. The resulting grid of spectral types is then used as a tool to ferret out the underlying physics. The temperature ranges covered by these spectral types, the complex chemical processes responsible for the shape of their emergent spectra, their nature as either true stars or brown dwarfs, and their number density in the Galaxy are discussed. Two promising avenues for future research are also explored: the extension of the classification system to three dimensions to account for gravity- and metallicity-dependent features, and the capability of newer large-area surveys to uncover brown dwarfs cooler than those now recognized.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195#table3</TD>
            <TD>2011-09-14T20:01:04Z</TD>
            <TD>#Stars#Spectral_Classification#Parallaxes#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/other/ARA+A/43.195</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/ARA+A/43.195&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ARA+A/43.195</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/1680 [1]</TD>
            <TD>ATLAS3D project. VII. (Cappellari+, 2011)</TD>
            <TD>In Paper I of this series we introduced a volume-limited parent sample of 871 galaxies from which we extracted the ATLAS3D sample of 260 early-type galaxies (ETGs). In Papers II and III we classified the ETGs using their stellar kinematics, in a way that is nearly insensitive to the projection effects, and we separated them into fast and slow rotators. Here we look at galaxy morphology and note that the edge-on fast rotators generally are lenticular galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680#1</TD>
            <TD>2012-06-11T20:02:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/1680</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/1680</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/1680 [2]</TD>
            <TD>ATLAS3D project. VII. (Cappellari+, 2011)</TD>
            <TD>In Paper I of this series we introduced a volume-limited parent sample of 871 galaxies from which we extracted the ATLAS3D sample of 260 early-type galaxies (ETGs). In Papers II and III we classified the ETGs using their stellar kinematics, in a way that is nearly insensitive to the projection effects, and we separated them into fast and slow rotators. Here we look at galaxy morphology and note that the edge-on fast rotators generally are lenticular galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680#2</TD>
            <TD>2012-06-11T20:02:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/1680&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/1680</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/1680 [atlas3d]</TD>
            <TD>ATLAS3D project. VII. (Cappellari+, 2011)</TD>
            <TD>In Paper I of this series we introduced a volume-limited parent sample of 871 galaxies from which we extracted the ATLAS3D sample of 260 early-type galaxies (ETGs). In Papers II and III we classified the ETGs using their stellar kinematics, in a way that is nearly insensitive to the projection effects, and we separated them into fast and slow rotators. Here we look at galaxy morphology and note that the edge-on fast rotators generally are lenticular galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680#atlas3d</TD>
            <TD>2012-06-11T20:02:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/1680&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/1680</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GLXSDSSQS2 [1]</TD>
            <TD>GALEX/SDSS z=0.5-1.5 QSO Candidates Catalog</TD>
            <TD>A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. In their paper, they discuss the distributions of redshift, luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be present in their final sample of 19,812 point sources. This latter catalog is available in the present table. This paper is based on archival data from the Galaxy Evolution Explorer (GALEX) which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034, and on data from the SDSS.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqs2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqs2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=glxsdssqs2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqs2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GLXSDSSQS2 [2]</TD>
            <TD>GALEX/SDSS z=0.5-1.5 QSO Candidates Catalog</TD>
            <TD>A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. In their paper, they discuss the distributions of redshift, luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be present in their final sample of 19,812 point sources. This latter catalog is available in the present table. This paper is based on archival data from the Galaxy Evolution Explorer (GALEX) which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034, and on data from the SDSS.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqs2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqs2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=glxsdssqs2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqs2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GLXSDSSQS2 [3]</TD>
            <TD>GALEX/SDSS z=0.5-1.5 QSO Candidates Catalog</TD>
            <TD>A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. In their paper, they discuss the distributions of redshift, luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be present in their final sample of 19,812 point sources. This latter catalog is available in the present table. This paper is based on archival data from the Galaxy Evolution Explorer (GALEX) which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034, and on data from the SDSS.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqs2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqs2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_glxsdssqs2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqs2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/1680 [1]</TD>
            <TD>ATLAS3D project. VII. (Cappellari+, 2011)</TD>
            <TD>In Paper I of this series we introduced a volume-limited parent sample of 871 galaxies from which we extracted the ATLAS3D sample of 260 early-type galaxies (ETGs). In Papers II and III we classified the ETGs using their stellar kinematics, in a way that is nearly insensitive to the projection effects, and we separated them into fast and slow rotators. Here we look at galaxy morphology and note that the edge-on fast rotators generally are lenticular galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680#1</TD>
            <TD>2012-06-11T20:02:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/1680</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/1680</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/1680 [2]</TD>
            <TD>ATLAS3D project. VII. (Cappellari+, 2011)</TD>
            <TD>In Paper I of this series we introduced a volume-limited parent sample of 871 galaxies from which we extracted the ATLAS3D sample of 260 early-type galaxies (ETGs). In Papers II and III we classified the ETGs using their stellar kinematics, in a way that is nearly insensitive to the projection effects, and we separated them into fast and slow rotators. Here we look at galaxy morphology and note that the edge-on fast rotators generally are lenticular galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680#2</TD>
            <TD>2012-06-11T20:02:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/1680&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/1680</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/1680 [atlas3d]</TD>
            <TD>ATLAS3D project. VII. (Cappellari+, 2011)</TD>
            <TD>In Paper I of this series we introduced a volume-limited parent sample of 871 galaxies from which we extracted the ATLAS3D sample of 260 early-type galaxies (ETGs). In Papers II and III we classified the ETGs using their stellar kinematics, in a way that is nearly insensitive to the projection effects, and we separated them into fast and slow rotators. Here we look at galaxy morphology and note that the edge-on fast rotators generally are lenticular galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680#atlas3d</TD>
            <TD>2012-06-11T20:02:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/1680&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/1680</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GLXSDSSQS2 [1]</TD>
            <TD>GALEX/SDSS z=0.5-1.5 QSO Candidates Catalog</TD>
            <TD>A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. In their paper, they discuss the distributions of redshift, luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be present in their final sample of 19,812 point sources. This latter catalog is available in the present table. This paper is based on archival data from the Galaxy Evolution Explorer (GALEX) which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034, and on data from the SDSS.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqs2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqs2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=glxsdssqs2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqs2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GLXSDSSQS2 [2]</TD>
            <TD>GALEX/SDSS z=0.5-1.5 QSO Candidates Catalog</TD>
            <TD>A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. In their paper, they discuss the distributions of redshift, luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be present in their final sample of 19,812 point sources. This latter catalog is available in the present table. This paper is based on archival data from the Galaxy Evolution Explorer (GALEX) which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034, and on data from the SDSS.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqs2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqs2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=glxsdssqs2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqs2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GLXSDSSQS2 [3]</TD>
            <TD>GALEX/SDSS z=0.5-1.5 QSO Candidates Catalog</TD>
            <TD>A sample of ~60,000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5 to 1.5 is discussed. The authors use SDSS spectra of a subsample of ~ 4,500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. In their paper, they discuss the distributions of redshift, luminosity, and reddening of the 19,100 QSOs (~96%) that they estimate to be present in their final sample of 19,812 point sources. This latter catalog is available in the present table. This paper is based on archival data from the Galaxy Evolution Explorer (GALEX) which is operated for NASA by the California Institute of Technology under NASA contract NAS5-98034, and on data from the SDSS.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#UV#</TD>
            <TD>ivo://nasa.heasarc/glxsdssqs2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/glxsdssqs2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_glxsdssqs2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/glxsdssqs2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/1680 [1]</TD>
            <TD>ATLAS3D project. VII. (Cappellari+, 2011)</TD>
            <TD>In Paper I of this series we introduced a volume-limited parent sample of 871 galaxies from which we extracted the ATLAS3D sample of 260 early-type galaxies (ETGs). In Papers II and III we classified the ETGs using their stellar kinematics, in a way that is nearly insensitive to the projection effects, and we separated them into fast and slow rotators. Here we look at galaxy morphology and note that the edge-on fast rotators generally are lenticular galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680#1</TD>
            <TD>2012-06-11T20:02:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/1680</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/1680</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/1680 [2]</TD>
            <TD>ATLAS3D project. VII. (Cappellari+, 2011)</TD>
            <TD>In Paper I of this series we introduced a volume-limited parent sample of 871 galaxies from which we extracted the ATLAS3D sample of 260 early-type galaxies (ETGs). In Papers II and III we classified the ETGs using their stellar kinematics, in a way that is nearly insensitive to the projection effects, and we separated them into fast and slow rotators. Here we look at galaxy morphology and note that the edge-on fast rotators generally are lenticular galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680#2</TD>
            <TD>2012-06-11T20:02:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/1680&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/1680</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/1680 [atlas3d]</TD>
            <TD>ATLAS3D project. VII. (Cappellari+, 2011)</TD>
            <TD>In Paper I of this series we introduced a volume-limited parent sample of 871 galaxies from which we extracted the ATLAS3D sample of 260 early-type galaxies (ETGs). In Papers II and III we classified the ETGs using their stellar kinematics, in a way that is nearly insensitive to the projection effects, and we separated them into fast and slow rotators. Here we look at galaxy morphology and note that the edge-on fast rotators generally are lenticular galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680#atlas3d</TD>
            <TD>2012-06-11T20:02:13Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/1680</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/1680&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/1680</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAM30MLOG [1]</TD>
            <TD>IRAM 30-m Single-Dish Telescope Observation Log</TD>
            <TD>This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there between January 1, 2009, and December 31, 2010, inclusive. (The observation log for the Plateau de Bure Interferometer (PdBI) is available as the HEASARC database table &lt;a href="irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;.) For more information on IRAM, see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iram30mlog#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iram30mlog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=iram30mlog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iram30mlog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRAM30MLOG [2]</TD>
            <TD>IRAM 30-m Single-Dish Telescope Observation Log</TD>
            <TD>This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there between January 1, 2009, and December 31, 2010, inclusive. (The observation log for the Plateau de Bure Interferometer (PdBI) is available as the HEASARC database table &lt;a href="irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;.) For more information on IRAM, see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iram30mlog#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iram30mlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=iram30mlog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iram30mlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRAM30MLOG [3]</TD>
            <TD>IRAM 30-m Single-Dish Telescope Observation Log</TD>
            <TD>This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there between January 1, 2009, and December 31, 2010, inclusive. (The observation log for the Plateau de Bure Interferometer (PdBI) is available as the HEASARC database table &lt;a href="irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;.) For more information on IRAM, see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iram30mlog#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iram30mlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_iram30mlog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iram30mlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/161/240 [1]</TD>
            <TD>High-ionization emission in metal-deficient BCDs (Thuan+, 2005)</TD>
            <TD>We have obtained new high signal-to-noise ratio spectrophotometric observations for 26 HII regions in 18 BCDs and for one supergiant HII region in the spiral galaxy M101 with the 6.5m MMT on the nights of 2004 February 1920 and 2005 February 4. Three BCDs were observed by Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;) with the Kitt Peak 4m telescope and five others were selected from the DR3 of the SDSS (Abazajian et al. 2005, Cat. &lt;II/259&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240#1</TD>
            <TD>2012-06-03T22:25:10Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/161/240</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/240</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/161/240 [2]</TD>
            <TD>High-ionization emission in metal-deficient BCDs (Thuan+, 2005)</TD>
            <TD>We have obtained new high signal-to-noise ratio spectrophotometric observations for 26 HII regions in 18 BCDs and for one supergiant HII region in the spiral galaxy M101 with the 6.5m MMT on the nights of 2004 February 1920 and 2005 February 4. Three BCDs were observed by Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;) with the Kitt Peak 4m telescope and five others were selected from the DR3 of the SDSS (Abazajian et al. 2005, Cat. &lt;II/259&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240#2</TD>
            <TD>2012-06-03T22:25:10Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/161/240&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/240 [table1]</TD>
            <TD>High-ionization emission in metal-deficient BCDs (Thuan+, 2005)</TD>
            <TD>We have obtained new high signal-to-noise ratio spectrophotometric observations for 26 HII regions in 18 BCDs and for one supergiant HII region in the spiral galaxy M101 with the 6.5m MMT on the nights of 2004 February 1920 and 2005 February 4. Three BCDs were observed by Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;) with the Kitt Peak 4m telescope and five others were selected from the DR3 of the SDSS (Abazajian et al. 2005, Cat. &lt;II/259&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240#table1</TD>
            <TD>2012-06-03T22:25:10Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/240&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAM30MLOG [1]</TD>
            <TD>IRAM 30-m Single-Dish Telescope Observation Log</TD>
            <TD>This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there between January 1, 2009, and December 31, 2010, inclusive. (The observation log for the Plateau de Bure Interferometer (PdBI) is available as the HEASARC database table &lt;a href="irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;.) For more information on IRAM, see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iram30mlog#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iram30mlog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=iram30mlog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iram30mlog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRAM30MLOG [2]</TD>
            <TD>IRAM 30-m Single-Dish Telescope Observation Log</TD>
            <TD>This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there between January 1, 2009, and December 31, 2010, inclusive. (The observation log for the Plateau de Bure Interferometer (PdBI) is available as the HEASARC database table &lt;a href="irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;.) For more information on IRAM, see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iram30mlog#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iram30mlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=iram30mlog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iram30mlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRAM30MLOG [3]</TD>
            <TD>IRAM 30-m Single-Dish Telescope Observation Log</TD>
            <TD>This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there between January 1, 2009, and December 31, 2010, inclusive. (The observation log for the Plateau de Bure Interferometer (PdBI) is available as the HEASARC database table &lt;a href="irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;.) For more information on IRAM, see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iram30mlog#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iram30mlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_iram30mlog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iram30mlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/161/240 [1]</TD>
            <TD>High-ionization emission in metal-deficient BCDs (Thuan+, 2005)</TD>
            <TD>We have obtained new high signal-to-noise ratio spectrophotometric observations for 26 HII regions in 18 BCDs and for one supergiant HII region in the spiral galaxy M101 with the 6.5m MMT on the nights of 2004 February 1920 and 2005 February 4. Three BCDs were observed by Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;) with the Kitt Peak 4m telescope and five others were selected from the DR3 of the SDSS (Abazajian et al. 2005, Cat. &lt;II/259&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240#1</TD>
            <TD>2012-06-03T22:25:10Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/161/240</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/240</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/161/240 [2]</TD>
            <TD>High-ionization emission in metal-deficient BCDs (Thuan+, 2005)</TD>
            <TD>We have obtained new high signal-to-noise ratio spectrophotometric observations for 26 HII regions in 18 BCDs and for one supergiant HII region in the spiral galaxy M101 with the 6.5m MMT on the nights of 2004 February 1920 and 2005 February 4. Three BCDs were observed by Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;) with the Kitt Peak 4m telescope and five others were selected from the DR3 of the SDSS (Abazajian et al. 2005, Cat. &lt;II/259&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240#2</TD>
            <TD>2012-06-03T22:25:10Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/161/240&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/240 [table1]</TD>
            <TD>High-ionization emission in metal-deficient BCDs (Thuan+, 2005)</TD>
            <TD>We have obtained new high signal-to-noise ratio spectrophotometric observations for 26 HII regions in 18 BCDs and for one supergiant HII region in the spiral galaxy M101 with the 6.5m MMT on the nights of 2004 February 1920 and 2005 February 4. Three BCDs were observed by Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;) with the Kitt Peak 4m telescope and five others were selected from the DR3 of the SDSS (Abazajian et al. 2005, Cat. &lt;II/259&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240#table1</TD>
            <TD>2012-06-03T22:25:10Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/240&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAM30MLOG [1]</TD>
            <TD>IRAM 30-m Single-Dish Telescope Observation Log</TD>
            <TD>This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there between January 1, 2009, and December 31, 2010, inclusive. (The observation log for the Plateau de Bure Interferometer (PdBI) is available as the HEASARC database table &lt;a href="irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;.) For more information on IRAM, see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iram30mlog#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iram30mlog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=iram30mlog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iram30mlog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRAM30MLOG [2]</TD>
            <TD>IRAM 30-m Single-Dish Telescope Observation Log</TD>
            <TD>This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there between January 1, 2009, and December 31, 2010, inclusive. (The observation log for the Plateau de Bure Interferometer (PdBI) is available as the HEASARC database table &lt;a href="irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;.) For more information on IRAM, see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iram30mlog#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iram30mlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=iram30mlog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iram30mlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRAM30MLOG [3]</TD>
            <TD>IRAM 30-m Single-Dish Telescope Observation Log</TD>
            <TD>This table contains the IRAM 30-m single-dish telescope observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the 30-m single-dish telescope, and summarizes the observations made there between January 1, 2009, and December 31, 2010, inclusive. (The observation log for the Plateau de Bure Interferometer (PdBI) is available as the HEASARC database table &lt;a href="irampdblog.html"&gt;IRAMPDBLOG&lt;/a&gt;.) For more information on IRAM, see &lt;a href="http://www.iram.fr/"&gt;the IRAM home page&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iram30mlog#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iram30mlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_iram30mlog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iram30mlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/161/240 [1]</TD>
            <TD>High-ionization emission in metal-deficient BCDs (Thuan+, 2005)</TD>
            <TD>We have obtained new high signal-to-noise ratio spectrophotometric observations for 26 HII regions in 18 BCDs and for one supergiant HII region in the spiral galaxy M101 with the 6.5m MMT on the nights of 2004 February 1920 and 2005 February 4. Three BCDs were observed by Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;) with the Kitt Peak 4m telescope and five others were selected from the DR3 of the SDSS (Abazajian et al. 2005, Cat. &lt;II/259&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240#1</TD>
            <TD>2012-06-03T22:25:10Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/161/240</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/240</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/161/240 [2]</TD>
            <TD>High-ionization emission in metal-deficient BCDs (Thuan+, 2005)</TD>
            <TD>We have obtained new high signal-to-noise ratio spectrophotometric observations for 26 HII regions in 18 BCDs and for one supergiant HII region in the spiral galaxy M101 with the 6.5m MMT on the nights of 2004 February 1920 and 2005 February 4. Three BCDs were observed by Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;) with the Kitt Peak 4m telescope and five others were selected from the DR3 of the SDSS (Abazajian et al. 2005, Cat. &lt;II/259&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240#2</TD>
            <TD>2012-06-03T22:25:10Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/161/240&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/161/240 [table1]</TD>
            <TD>High-ionization emission in metal-deficient BCDs (Thuan+, 2005)</TD>
            <TD>We have obtained new high signal-to-noise ratio spectrophotometric observations for 26 HII regions in 18 BCDs and for one supergiant HII region in the spiral galaxy M101 with the 6.5m MMT on the nights of 2004 February 1920 and 2005 February 4. Three BCDs were observed by Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;) with the Kitt Peak 4m telescope and five others were selected from the DR3 of the SDSS (Abazajian et al. 2005, Cat. &lt;II/259&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240#table1</TD>
            <TD>2012-06-03T22:25:10Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/161/240</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/161/240&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/161/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M81CXO2 [1]</TD>
            <TD>M 81 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the source table from an analysis of 15 Chandra ACIS observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With these observations and one previous deeper Chandra observation (the properties of which are described in Table 1 and Section 2 of the reference paper), the authors have compiled a master source list of 265 point sources, extracted and fitted their spectra, and differentiated basic populations of sources through their colors. They also carried out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. They find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. They also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way. This table contains the 265 point sources at or above the 99.9% probability level of being real according to AE's PROB_NO_SOURCE statistic (the "master" source list), and 11 additional "borderline" sources which have 99.0-99.9% probability of being real according to AE's PROB_NO_SOURCE statistic, for a total of 276 sources whose properties were described in Tables 3 and 4 of the reference paper. The 265 "master" sources have source numbers from 1 to 265 while the 11 "borderline" sources have source numbers beginning with 'B', e.g., they have source numbers 'B1' to 'B11'. Note that only coordinates are listed for 3 sources in the master source list (source numbers 234, 241 and 262) and 2 sources in the borderline source list (B8 and B9) because they were only in the field of view (on chip) of one observation (ObsID 735). Six additional sources near the center of M81 which were found using maximum likelihood image reconstruction are not included in either the master or borderline source lists contained herein but their positions are listed in table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m81cxo2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M81CXO2 [2]</TD>
            <TD>M 81 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the source table from an analysis of 15 Chandra ACIS observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With these observations and one previous deeper Chandra observation (the properties of which are described in Table 1 and Section 2 of the reference paper), the authors have compiled a master source list of 265 point sources, extracted and fitted their spectra, and differentiated basic populations of sources through their colors. They also carried out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. They find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. They also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way. This table contains the 265 point sources at or above the 99.9% probability level of being real according to AE's PROB_NO_SOURCE statistic (the "master" source list), and 11 additional "borderline" sources which have 99.0-99.9% probability of being real according to AE's PROB_NO_SOURCE statistic, for a total of 276 sources whose properties were described in Tables 3 and 4 of the reference paper. The 265 "master" sources have source numbers from 1 to 265 while the 11 "borderline" sources have source numbers beginning with 'B', e.g., they have source numbers 'B1' to 'B11'. Note that only coordinates are listed for 3 sources in the master source list (source numbers 234, 241 and 262) and 2 sources in the borderline source list (B8 and B9) because they were only in the field of view (on chip) of one observation (ObsID 735). Six additional sources near the center of M81 which were found using maximum likelihood image reconstruction are not included in either the master or borderline source lists contained herein but their positions are listed in table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m81cxo2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M81CXO2 [3]</TD>
            <TD>M 81 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the source table from an analysis of 15 Chandra ACIS observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With these observations and one previous deeper Chandra observation (the properties of which are described in Table 1 and Section 2 of the reference paper), the authors have compiled a master source list of 265 point sources, extracted and fitted their spectra, and differentiated basic populations of sources through their colors. They also carried out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. They find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. They also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way. This table contains the 265 point sources at or above the 99.9% probability level of being real according to AE's PROB_NO_SOURCE statistic (the "master" source list), and 11 additional "borderline" sources which have 99.0-99.9% probability of being real according to AE's PROB_NO_SOURCE statistic, for a total of 276 sources whose properties were described in Tables 3 and 4 of the reference paper. The 265 "master" sources have source numbers from 1 to 265 while the 11 "borderline" sources have source numbers beginning with 'B', e.g., they have source numbers 'B1' to 'B11'. Note that only coordinates are listed for 3 sources in the master source list (source numbers 234, 241 and 262) and 2 sources in the borderline source list (B8 and B9) because they were only in the field of view (on chip) of one observation (ObsID 735). Six additional sources near the center of M81 which were found using maximum likelihood image reconstruction are not included in either the master or borderline source lists contained herein but their positions are listed in table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m81cxo2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/33/403 [1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#1</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/33/403</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/33/403 [2]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#2</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/33/403&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/33/403 [table1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#table1</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/33/403&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/33/403 [table2]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#table2</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/33/403&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M81CXO2 [1]</TD>
            <TD>M 81 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the source table from an analysis of 15 Chandra ACIS observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With these observations and one previous deeper Chandra observation (the properties of which are described in Table 1 and Section 2 of the reference paper), the authors have compiled a master source list of 265 point sources, extracted and fitted their spectra, and differentiated basic populations of sources through their colors. They also carried out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. They find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. They also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way. This table contains the 265 point sources at or above the 99.9% probability level of being real according to AE's PROB_NO_SOURCE statistic (the "master" source list), and 11 additional "borderline" sources which have 99.0-99.9% probability of being real according to AE's PROB_NO_SOURCE statistic, for a total of 276 sources whose properties were described in Tables 3 and 4 of the reference paper. The 265 "master" sources have source numbers from 1 to 265 while the 11 "borderline" sources have source numbers beginning with 'B', e.g., they have source numbers 'B1' to 'B11'. Note that only coordinates are listed for 3 sources in the master source list (source numbers 234, 241 and 262) and 2 sources in the borderline source list (B8 and B9) because they were only in the field of view (on chip) of one observation (ObsID 735). Six additional sources near the center of M81 which were found using maximum likelihood image reconstruction are not included in either the master or borderline source lists contained herein but their positions are listed in table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m81cxo2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M81CXO2 [2]</TD>
            <TD>M 81 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the source table from an analysis of 15 Chandra ACIS observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With these observations and one previous deeper Chandra observation (the properties of which are described in Table 1 and Section 2 of the reference paper), the authors have compiled a master source list of 265 point sources, extracted and fitted their spectra, and differentiated basic populations of sources through their colors. They also carried out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. They find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. They also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way. This table contains the 265 point sources at or above the 99.9% probability level of being real according to AE's PROB_NO_SOURCE statistic (the "master" source list), and 11 additional "borderline" sources which have 99.0-99.9% probability of being real according to AE's PROB_NO_SOURCE statistic, for a total of 276 sources whose properties were described in Tables 3 and 4 of the reference paper. The 265 "master" sources have source numbers from 1 to 265 while the 11 "borderline" sources have source numbers beginning with 'B', e.g., they have source numbers 'B1' to 'B11'. Note that only coordinates are listed for 3 sources in the master source list (source numbers 234, 241 and 262) and 2 sources in the borderline source list (B8 and B9) because they were only in the field of view (on chip) of one observation (ObsID 735). Six additional sources near the center of M81 which were found using maximum likelihood image reconstruction are not included in either the master or borderline source lists contained herein but their positions are listed in table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m81cxo2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M81CXO2 [3]</TD>
            <TD>M 81 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the source table from an analysis of 15 Chandra ACIS observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With these observations and one previous deeper Chandra observation (the properties of which are described in Table 1 and Section 2 of the reference paper), the authors have compiled a master source list of 265 point sources, extracted and fitted their spectra, and differentiated basic populations of sources through their colors. They also carried out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. They find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. They also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way. This table contains the 265 point sources at or above the 99.9% probability level of being real according to AE's PROB_NO_SOURCE statistic (the "master" source list), and 11 additional "borderline" sources which have 99.0-99.9% probability of being real according to AE's PROB_NO_SOURCE statistic, for a total of 276 sources whose properties were described in Tables 3 and 4 of the reference paper. The 265 "master" sources have source numbers from 1 to 265 while the 11 "borderline" sources have source numbers beginning with 'B', e.g., they have source numbers 'B1' to 'B11'. Note that only coordinates are listed for 3 sources in the master source list (source numbers 234, 241 and 262) and 2 sources in the borderline source list (B8 and B9) because they were only in the field of view (on chip) of one observation (ObsID 735). Six additional sources near the center of M81 which were found using maximum likelihood image reconstruction are not included in either the master or borderline source lists contained herein but their positions are listed in table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m81cxo2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/33/403 [1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#1</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/33/403</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/33/403 [2]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#2</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/33/403&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/33/403 [table1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#table1</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/33/403&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/33/403 [table2]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#table2</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/33/403&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/393/1531 [1]</TD>
            <TD>BUDDA structural properties of galaxies (Gadotti+, 2009)</TD>
            <TD>++++Lrecl of file 'budda_g.dat' (192) increased to 198 ++++Lrecl of file 'budda_i.dat' (192) increased to 198 %B BUDDA on SDSS : Bulge/Disk/Bar Image Decomposition of ~1000 galaxies @ z~0.05 in g, r and i. The tables with the structural parameters resulting from the fits are separated in three groups. The first group gives the parameters as obtained directly from the fits in each band. The second group provides colors obtained from fits in different bands for each galaxy component, and in the third group one finds integrated colors and magnitudes for each component. Also provided is a table with the stellar mass-to-light ratio and mass of each component, as well as the lists of galaxies classified as ellipticals, disk galaxies with classical bulges, disk galaxies with pseudo-bulges, barred and unbarred galaxies, and bulgeless galaxies. A description of the columns in each table is also given below. Surface brightness is given in magnitudes per square arcsecond, scale lengths in kpc (H_0=75km/s/Mpc), colors in magnitudes, and masses in solar units.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531#1</TD>
            <TD>2011-09-14T21:03:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/393/1531</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/393/1531</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/393/1531 [2]</TD>
            <TD>BUDDA structural properties of galaxies (Gadotti+, 2009)</TD>
            <TD>++++Lrecl of file 'budda_g.dat' (192) increased to 198 ++++Lrecl of file 'budda_i.dat' (192) increased to 198 %B BUDDA on SDSS : Bulge/Disk/Bar Image Decomposition of ~1000 galaxies @ z~0.05 in g, r and i. The tables with the structural parameters resulting from the fits are separated in three groups. The first group gives the parameters as obtained directly from the fits in each band. The second group provides colors obtained from fits in different bands for each galaxy component, and in the third group one finds integrated colors and magnitudes for each component. Also provided is a table with the stellar mass-to-light ratio and mass of each component, as well as the lists of galaxies classified as ellipticals, disk galaxies with classical bulges, disk galaxies with pseudo-bulges, barred and unbarred galaxies, and bulgeless galaxies. A description of the columns in each table is also given below. Surface brightness is given in magnitudes per square arcsecond, scale lengths in kpc (H_0=75km/s/Mpc), colors in magnitudes, and masses in solar units.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531#2</TD>
            <TD>2011-09-14T21:03:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/393/1531&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/393/1531</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/393/1531 [galaxies]</TD>
            <TD>BUDDA structural properties of galaxies (Gadotti+, 2009)</TD>
            <TD>++++Lrecl of file 'budda_g.dat' (192) increased to 198 ++++Lrecl of file 'budda_i.dat' (192) increased to 198 %B BUDDA on SDSS : Bulge/Disk/Bar Image Decomposition of ~1000 galaxies @ z~0.05 in g, r and i. The tables with the structural parameters resulting from the fits are separated in three groups. The first group gives the parameters as obtained directly from the fits in each band. The second group provides colors obtained from fits in different bands for each galaxy component, and in the third group one finds integrated colors and magnitudes for each component. Also provided is a table with the stellar mass-to-light ratio and mass of each component, as well as the lists of galaxies classified as ellipticals, disk galaxies with classical bulges, disk galaxies with pseudo-bulges, barred and unbarred galaxies, and bulgeless galaxies. A description of the columns in each table is also given below. Surface brightness is given in magnitudes per square arcsecond, scale lengths in kpc (H_0=75km/s/Mpc), colors in magnitudes, and masses in solar units.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531#galaxies</TD>
            <TD>2011-09-14T21:03:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/393/1531&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/393/1531</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M81CXO2 [1]</TD>
            <TD>M 81 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the source table from an analysis of 15 Chandra ACIS observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With these observations and one previous deeper Chandra observation (the properties of which are described in Table 1 and Section 2 of the reference paper), the authors have compiled a master source list of 265 point sources, extracted and fitted their spectra, and differentiated basic populations of sources through their colors. They also carried out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. They find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. They also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way. This table contains the 265 point sources at or above the 99.9% probability level of being real according to AE's PROB_NO_SOURCE statistic (the "master" source list), and 11 additional "borderline" sources which have 99.0-99.9% probability of being real according to AE's PROB_NO_SOURCE statistic, for a total of 276 sources whose properties were described in Tables 3 and 4 of the reference paper. The 265 "master" sources have source numbers from 1 to 265 while the 11 "borderline" sources have source numbers beginning with 'B', e.g., they have source numbers 'B1' to 'B11'. Note that only coordinates are listed for 3 sources in the master source list (source numbers 234, 241 and 262) and 2 sources in the borderline source list (B8 and B9) because they were only in the field of view (on chip) of one observation (ObsID 735). Six additional sources near the center of M81 which were found using maximum likelihood image reconstruction are not included in either the master or borderline source lists contained herein but their positions are listed in table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m81cxo2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M81CXO2 [2]</TD>
            <TD>M 81 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the source table from an analysis of 15 Chandra ACIS observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With these observations and one previous deeper Chandra observation (the properties of which are described in Table 1 and Section 2 of the reference paper), the authors have compiled a master source list of 265 point sources, extracted and fitted their spectra, and differentiated basic populations of sources through their colors. They also carried out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. They find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. They also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way. This table contains the 265 point sources at or above the 99.9% probability level of being real according to AE's PROB_NO_SOURCE statistic (the "master" source list), and 11 additional "borderline" sources which have 99.0-99.9% probability of being real according to AE's PROB_NO_SOURCE statistic, for a total of 276 sources whose properties were described in Tables 3 and 4 of the reference paper. The 265 "master" sources have source numbers from 1 to 265 while the 11 "borderline" sources have source numbers beginning with 'B', e.g., they have source numbers 'B1' to 'B11'. Note that only coordinates are listed for 3 sources in the master source list (source numbers 234, 241 and 262) and 2 sources in the borderline source list (B8 and B9) because they were only in the field of view (on chip) of one observation (ObsID 735). Six additional sources near the center of M81 which were found using maximum likelihood image reconstruction are not included in either the master or borderline source lists contained herein but their positions are listed in table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m81cxo2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M81CXO2 [3]</TD>
            <TD>M 81 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table contains the source table from an analysis of 15 Chandra ACIS observations of the nearby spiral galaxy M81 taken over the course of six weeks in 2005 May-July. Each observation reaches a sensitivity of ~10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. With these observations and one previous deeper Chandra observation (the properties of which are described in Table 1 and Section 2 of the reference paper), the authors have compiled a master source list of 265 point sources, extracted and fitted their spectra, and differentiated basic populations of sources through their colors. They also carried out variability analyses of individual point sources and of X-ray luminosity functions (XLFs) in multiple regions of M81 on timescales of days, months, and years. They find that, despite measuring significant variability in a considerable fraction of sources, snapshot observations provide a consistent determination of the XLF of M81. They also fit the XLFs for multiple regions of M81 and, using common parameterizations, compare these luminosity functions to those of two other spiral galaxies, M31 and the Milky Way. This table contains the 265 point sources at or above the 99.9% probability level of being real according to AE's PROB_NO_SOURCE statistic (the "master" source list), and 11 additional "borderline" sources which have 99.0-99.9% probability of being real according to AE's PROB_NO_SOURCE statistic, for a total of 276 sources whose properties were described in Tables 3 and 4 of the reference paper. The 265 "master" sources have source numbers from 1 to 265 while the 11 "borderline" sources have source numbers beginning with 'B', e.g., they have source numbers 'B1' to 'B11'. Note that only coordinates are listed for 3 sources in the master source list (source numbers 234, 241 and 262) and 2 sources in the borderline source list (B8 and B9) because they were only in the field of view (on chip) of one observation (ObsID 735). Six additional sources near the center of M81 which were found using maximum likelihood image reconstruction are not included in either the master or borderline source lists contained herein but their positions are listed in table 2 of the reference paper.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m81cxo2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m81cxo2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m81cxo2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m81cxo2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/33/403 [1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#1</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/33/403</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/33/403 [2]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#2</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/33/403&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/33/403 [table1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#table1</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/33/403&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/33/403 [table2]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova+, 2007)</TD>
            <TD>Based on the SDSS catalog, we have found new close quasar-galaxy pairs. We analyze the radial distribution of quasars from pairs around galaxies of different types. We show that the quasars from pairs follow the density profile of halo globular clusters. This is new observational evidence that the quasars projected onto the halos of galaxies are magnified by gravitational lensing by halo globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403#table2</TD>
            <TD>2011-09-14T20:17:02Z</TD>
            <TD>#Globular_Clusters#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/33/403</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/33/403&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/33/403</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSS</TD>
            <TD>Sloan Digital Sky Survey</TD>
            <TD>This SkyNode points to the latest public SDSS catalog data release available at http://cas.sdss.org/ The Sloan Digital Sky Survey is the most ambitious astronomical survey ever undertaken. The survey will map one-quarter of the entire sky in detail, determining the positions and absolute brightnesses of hundreds of millions of celestial objects. It will also measure the distances to more than a million galaxies and quasars. The SDSS addresses fascinating, fundamental questions about the universe. With the survey, astronomers will be able to see the large-scale patterns of galaxies: sheets and voids through the whole universe. Scientists have many ideas about how the universe evolved, and different patterns of large-scale structure point to different theories. The Sloan Digital Sky Survey will tell us which theories are right - or whether we will have to come up with entirely new ideas.</TD>
            <TD>JHU</TD>
            <TD>#Optical#</TD>
            <TD>ivo://sdss.jhu/openskynode/sdss#1</TD>
            <TD>2011-09-14T18:12:23Z</TD>
            <TD>#OpenSkyNode#Galaxy#Star#</TD>
            <TD />
            <TD />
            <TD>0.800000011920929</TD>
            <TD />
            <TD>ivo://sdss.jhu/openskynode/sdss</TD>
            <TD>OpenSkyNode</TD>
            <TD>ivo://ivoa.net/std/OpenSkyNode</TD>
            <TD>2</TD>
            <TD>WebService</TD>
            <TD />
            <TD>std</TD>
            <TD>http://openskyquery.net/nodes//SDSS/nodeb.asmx</TD>
            <TD />
            <TD>5000</TD>
            <TD />
            <TD>http://cas.sdss.org/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/375/931 [1]</TD>
            <TD>Radio sources in the 6dFGS (Mauch+, 2007)</TD>
            <TD>We have identified 7824 radio sources from the 1.4GHz NRAO VLA Sky Survey (NVSS, Cat. &lt;VIII/65&gt;) with galaxies brighter than K=12.75mag in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2, Cat. &lt;VII/249&gt;). The resulting sample of redshifts and optical spectra for radio sources over an effective sky area of 7076deg^2^ (about 17 per cent of the celestial sphere) is the largest of its kind ever obtained. NVSS radio sources associated with galaxies in the 6dFGS span a redshift range 0.003&lt;z&lt;0.3 and have median z{bar}=0.043. Through visual examination of 6dF spectra we have identified the dominant mechanism for radio emission from each galaxy. 60 per cent are fuelled by star formation and 40 per cent are fuelled by an active galactic nucleus (AGN) powered by a supermassive black hole. We have accurately determined the local radio luminosity function (RLF) at 1.4GHz for both classes of radio source and have found it to agree well with other recent determinations. From the RLF of star-forming galaxies we derive a local star formation density of 0.022+/-0.001M_{sun}_/yr/Mpc^3^, in broad agreement with recent determinations at radio and other wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931#1</TD>
            <TD>2011-09-14T20:17:20Z</TD>
            <TD>#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/375/931</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/931</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/375/931 [2]</TD>
            <TD>Radio sources in the 6dFGS (Mauch+, 2007)</TD>
            <TD>We have identified 7824 radio sources from the 1.4GHz NRAO VLA Sky Survey (NVSS, Cat. &lt;VIII/65&gt;) with galaxies brighter than K=12.75mag in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2, Cat. &lt;VII/249&gt;). The resulting sample of redshifts and optical spectra for radio sources over an effective sky area of 7076deg^2^ (about 17 per cent of the celestial sphere) is the largest of its kind ever obtained. NVSS radio sources associated with galaxies in the 6dFGS span a redshift range 0.003&lt;z&lt;0.3 and have median z{bar}=0.043. Through visual examination of 6dF spectra we have identified the dominant mechanism for radio emission from each galaxy. 60 per cent are fuelled by star formation and 40 per cent are fuelled by an active galactic nucleus (AGN) powered by a supermassive black hole. We have accurately determined the local radio luminosity function (RLF) at 1.4GHz for both classes of radio source and have found it to agree well with other recent determinations. From the RLF of star-forming galaxies we derive a local star formation density of 0.022+/-0.001M_{sun}_/yr/Mpc^3^, in broad agreement with recent determinations at radio and other wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931#2</TD>
            <TD>2011-09-14T20:17:20Z</TD>
            <TD>#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/375/931&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/931</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/931 [table3]</TD>
            <TD>Radio sources in the 6dFGS (Mauch+, 2007)</TD>
            <TD>We have identified 7824 radio sources from the 1.4GHz NRAO VLA Sky Survey (NVSS, Cat. &lt;VIII/65&gt;) with galaxies brighter than K=12.75mag in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2, Cat. &lt;VII/249&gt;). The resulting sample of redshifts and optical spectra for radio sources over an effective sky area of 7076deg^2^ (about 17 per cent of the celestial sphere) is the largest of its kind ever obtained. NVSS radio sources associated with galaxies in the 6dFGS span a redshift range 0.003&lt;z&lt;0.3 and have median z{bar}=0.043. Through visual examination of 6dF spectra we have identified the dominant mechanism for radio emission from each galaxy. 60 per cent are fuelled by star formation and 40 per cent are fuelled by an active galactic nucleus (AGN) powered by a supermassive black hole. We have accurately determined the local radio luminosity function (RLF) at 1.4GHz for both classes of radio source and have found it to agree well with other recent determinations. From the RLF of star-forming galaxies we derive a local star formation density of 0.022+/-0.001M_{sun}_/yr/Mpc^3^, in broad agreement with recent determinations at radio and other wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931#table3</TD>
            <TD>2011-09-14T20:17:20Z</TD>
            <TD>#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/931&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/931</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/393/1531 [1]</TD>
            <TD>BUDDA structural properties of galaxies (Gadotti+, 2009)</TD>
            <TD>++++Lrecl of file 'budda_g.dat' (192) increased to 198 ++++Lrecl of file 'budda_i.dat' (192) increased to 198 %B BUDDA on SDSS : Bulge/Disk/Bar Image Decomposition of ~1000 galaxies @ z~0.05 in g, r and i. The tables with the structural parameters resulting from the fits are separated in three groups. The first group gives the parameters as obtained directly from the fits in each band. The second group provides colors obtained from fits in different bands for each galaxy component, and in the third group one finds integrated colors and magnitudes for each component. Also provided is a table with the stellar mass-to-light ratio and mass of each component, as well as the lists of galaxies classified as ellipticals, disk galaxies with classical bulges, disk galaxies with pseudo-bulges, barred and unbarred galaxies, and bulgeless galaxies. A description of the columns in each table is also given below. Surface brightness is given in magnitudes per square arcsecond, scale lengths in kpc (H_0=75km/s/Mpc), colors in magnitudes, and masses in solar units.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531#1</TD>
            <TD>2011-09-14T21:03:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/393/1531</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/393/1531</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/393/1531 [2]</TD>
            <TD>BUDDA structural properties of galaxies (Gadotti+, 2009)</TD>
            <TD>++++Lrecl of file 'budda_g.dat' (192) increased to 198 ++++Lrecl of file 'budda_i.dat' (192) increased to 198 %B BUDDA on SDSS : Bulge/Disk/Bar Image Decomposition of ~1000 galaxies @ z~0.05 in g, r and i. The tables with the structural parameters resulting from the fits are separated in three groups. The first group gives the parameters as obtained directly from the fits in each band. The second group provides colors obtained from fits in different bands for each galaxy component, and in the third group one finds integrated colors and magnitudes for each component. Also provided is a table with the stellar mass-to-light ratio and mass of each component, as well as the lists of galaxies classified as ellipticals, disk galaxies with classical bulges, disk galaxies with pseudo-bulges, barred and unbarred galaxies, and bulgeless galaxies. A description of the columns in each table is also given below. Surface brightness is given in magnitudes per square arcsecond, scale lengths in kpc (H_0=75km/s/Mpc), colors in magnitudes, and masses in solar units.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531#2</TD>
            <TD>2011-09-14T21:03:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/393/1531&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/393/1531</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/393/1531 [galaxies]</TD>
            <TD>BUDDA structural properties of galaxies (Gadotti+, 2009)</TD>
            <TD>++++Lrecl of file 'budda_g.dat' (192) increased to 198 ++++Lrecl of file 'budda_i.dat' (192) increased to 198 %B BUDDA on SDSS : Bulge/Disk/Bar Image Decomposition of ~1000 galaxies @ z~0.05 in g, r and i. The tables with the structural parameters resulting from the fits are separated in three groups. The first group gives the parameters as obtained directly from the fits in each band. The second group provides colors obtained from fits in different bands for each galaxy component, and in the third group one finds integrated colors and magnitudes for each component. Also provided is a table with the stellar mass-to-light ratio and mass of each component, as well as the lists of galaxies classified as ellipticals, disk galaxies with classical bulges, disk galaxies with pseudo-bulges, barred and unbarred galaxies, and bulgeless galaxies. A description of the columns in each table is also given below. Surface brightness is given in magnitudes per square arcsecond, scale lengths in kpc (H_0=75km/s/Mpc), colors in magnitudes, and masses in solar units.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531#galaxies</TD>
            <TD>2011-09-14T21:03:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/393/1531&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/393/1531</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/375/931 [1]</TD>
            <TD>Radio sources in the 6dFGS (Mauch+, 2007)</TD>
            <TD>We have identified 7824 radio sources from the 1.4GHz NRAO VLA Sky Survey (NVSS, Cat. &lt;VIII/65&gt;) with galaxies brighter than K=12.75mag in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2, Cat. &lt;VII/249&gt;). The resulting sample of redshifts and optical spectra for radio sources over an effective sky area of 7076deg^2^ (about 17 per cent of the celestial sphere) is the largest of its kind ever obtained. NVSS radio sources associated with galaxies in the 6dFGS span a redshift range 0.003&lt;z&lt;0.3 and have median z{bar}=0.043. Through visual examination of 6dF spectra we have identified the dominant mechanism for radio emission from each galaxy. 60 per cent are fuelled by star formation and 40 per cent are fuelled by an active galactic nucleus (AGN) powered by a supermassive black hole. We have accurately determined the local radio luminosity function (RLF) at 1.4GHz for both classes of radio source and have found it to agree well with other recent determinations. From the RLF of star-forming galaxies we derive a local star formation density of 0.022+/-0.001M_{sun}_/yr/Mpc^3^, in broad agreement with recent determinations at radio and other wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931#1</TD>
            <TD>2011-09-14T20:17:20Z</TD>
            <TD>#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/375/931</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/931</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/375/931 [2]</TD>
            <TD>Radio sources in the 6dFGS (Mauch+, 2007)</TD>
            <TD>We have identified 7824 radio sources from the 1.4GHz NRAO VLA Sky Survey (NVSS, Cat. &lt;VIII/65&gt;) with galaxies brighter than K=12.75mag in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2, Cat. &lt;VII/249&gt;). The resulting sample of redshifts and optical spectra for radio sources over an effective sky area of 7076deg^2^ (about 17 per cent of the celestial sphere) is the largest of its kind ever obtained. NVSS radio sources associated with galaxies in the 6dFGS span a redshift range 0.003&lt;z&lt;0.3 and have median z{bar}=0.043. Through visual examination of 6dF spectra we have identified the dominant mechanism for radio emission from each galaxy. 60 per cent are fuelled by star formation and 40 per cent are fuelled by an active galactic nucleus (AGN) powered by a supermassive black hole. We have accurately determined the local radio luminosity function (RLF) at 1.4GHz for both classes of radio source and have found it to agree well with other recent determinations. From the RLF of star-forming galaxies we derive a local star formation density of 0.022+/-0.001M_{sun}_/yr/Mpc^3^, in broad agreement with recent determinations at radio and other wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931#2</TD>
            <TD>2011-09-14T20:17:20Z</TD>
            <TD>#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/375/931&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/931</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/931 [table3]</TD>
            <TD>Radio sources in the 6dFGS (Mauch+, 2007)</TD>
            <TD>We have identified 7824 radio sources from the 1.4GHz NRAO VLA Sky Survey (NVSS, Cat. &lt;VIII/65&gt;) with galaxies brighter than K=12.75mag in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2, Cat. &lt;VII/249&gt;). The resulting sample of redshifts and optical spectra for radio sources over an effective sky area of 7076deg^2^ (about 17 per cent of the celestial sphere) is the largest of its kind ever obtained. NVSS radio sources associated with galaxies in the 6dFGS span a redshift range 0.003&lt;z&lt;0.3 and have median z{bar}=0.043. Through visual examination of 6dF spectra we have identified the dominant mechanism for radio emission from each galaxy. 60 per cent are fuelled by star formation and 40 per cent are fuelled by an active galactic nucleus (AGN) powered by a supermassive black hole. We have accurately determined the local radio luminosity function (RLF) at 1.4GHz for both classes of radio source and have found it to agree well with other recent determinations. From the RLF of star-forming galaxies we derive a local star formation density of 0.022+/-0.001M_{sun}_/yr/Mpc^3^, in broad agreement with recent determinations at radio and other wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931#table3</TD>
            <TD>2011-09-14T20:17:20Z</TD>
            <TD>#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/931&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/931</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M31DEEPXMM [1]</TD>
            <TD>M 31 Deep XMM-Newton Survey X-Ray Source Catalog</TD>
            <TD>The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~10&lt;sup&gt;35&lt;/sup&gt;erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D&lt;sub&gt;25&lt;/sub&gt; ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31deepxmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31deepxmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m31deepxmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31deepxmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M31DEEPXMM [2]</TD>
            <TD>M 31 Deep XMM-Newton Survey X-Ray Source Catalog</TD>
            <TD>The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~10&lt;sup&gt;35&lt;/sup&gt;erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D&lt;sub&gt;25&lt;/sub&gt; ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31deepxmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31deepxmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m31deepxmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31deepxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M31DEEPXMM [3]</TD>
            <TD>M 31 Deep XMM-Newton Survey X-Ray Source Catalog</TD>
            <TD>The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~10&lt;sup&gt;35&lt;/sup&gt;erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D&lt;sub&gt;25&lt;/sub&gt; ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31deepxmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31deepxmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m31deepxmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31deepxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/393/1531 [1]</TD>
            <TD>BUDDA structural properties of galaxies (Gadotti+, 2009)</TD>
            <TD>++++Lrecl of file 'budda_g.dat' (192) increased to 198 ++++Lrecl of file 'budda_i.dat' (192) increased to 198 %B BUDDA on SDSS : Bulge/Disk/Bar Image Decomposition of ~1000 galaxies @ z~0.05 in g, r and i. The tables with the structural parameters resulting from the fits are separated in three groups. The first group gives the parameters as obtained directly from the fits in each band. The second group provides colors obtained from fits in different bands for each galaxy component, and in the third group one finds integrated colors and magnitudes for each component. Also provided is a table with the stellar mass-to-light ratio and mass of each component, as well as the lists of galaxies classified as ellipticals, disk galaxies with classical bulges, disk galaxies with pseudo-bulges, barred and unbarred galaxies, and bulgeless galaxies. A description of the columns in each table is also given below. Surface brightness is given in magnitudes per square arcsecond, scale lengths in kpc (H_0=75km/s/Mpc), colors in magnitudes, and masses in solar units.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531#1</TD>
            <TD>2011-09-14T21:03:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/393/1531</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/393/1531</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/393/1531 [2]</TD>
            <TD>BUDDA structural properties of galaxies (Gadotti+, 2009)</TD>
            <TD>++++Lrecl of file 'budda_g.dat' (192) increased to 198 ++++Lrecl of file 'budda_i.dat' (192) increased to 198 %B BUDDA on SDSS : Bulge/Disk/Bar Image Decomposition of ~1000 galaxies @ z~0.05 in g, r and i. The tables with the structural parameters resulting from the fits are separated in three groups. The first group gives the parameters as obtained directly from the fits in each band. The second group provides colors obtained from fits in different bands for each galaxy component, and in the third group one finds integrated colors and magnitudes for each component. Also provided is a table with the stellar mass-to-light ratio and mass of each component, as well as the lists of galaxies classified as ellipticals, disk galaxies with classical bulges, disk galaxies with pseudo-bulges, barred and unbarred galaxies, and bulgeless galaxies. A description of the columns in each table is also given below. Surface brightness is given in magnitudes per square arcsecond, scale lengths in kpc (H_0=75km/s/Mpc), colors in magnitudes, and masses in solar units.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531#2</TD>
            <TD>2011-09-14T21:03:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/393/1531&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/393/1531</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/393/1531 [galaxies]</TD>
            <TD>BUDDA structural properties of galaxies (Gadotti+, 2009)</TD>
            <TD>++++Lrecl of file 'budda_g.dat' (192) increased to 198 ++++Lrecl of file 'budda_i.dat' (192) increased to 198 %B BUDDA on SDSS : Bulge/Disk/Bar Image Decomposition of ~1000 galaxies @ z~0.05 in g, r and i. The tables with the structural parameters resulting from the fits are separated in three groups. The first group gives the parameters as obtained directly from the fits in each band. The second group provides colors obtained from fits in different bands for each galaxy component, and in the third group one finds integrated colors and magnitudes for each component. Also provided is a table with the stellar mass-to-light ratio and mass of each component, as well as the lists of galaxies classified as ellipticals, disk galaxies with classical bulges, disk galaxies with pseudo-bulges, barred and unbarred galaxies, and bulgeless galaxies. A description of the columns in each table is also given below. Surface brightness is given in magnitudes per square arcsecond, scale lengths in kpc (H_0=75km/s/Mpc), colors in magnitudes, and masses in solar units.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531#galaxies</TD>
            <TD>2011-09-14T21:03:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/393/1531</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/393/1531&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/393/1531</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M31DEEPXMM [1]</TD>
            <TD>M 31 Deep XMM-Newton Survey X-Ray Source Catalog</TD>
            <TD>The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~10&lt;sup&gt;35&lt;/sup&gt;erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D&lt;sub&gt;25&lt;/sub&gt; ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31deepxmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31deepxmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m31deepxmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31deepxmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M31DEEPXMM [2]</TD>
            <TD>M 31 Deep XMM-Newton Survey X-Ray Source Catalog</TD>
            <TD>The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~10&lt;sup&gt;35&lt;/sup&gt;erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D&lt;sub&gt;25&lt;/sub&gt; ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31deepxmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31deepxmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m31deepxmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31deepxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M31DEEPXMM [3]</TD>
            <TD>M 31 Deep XMM-Newton Survey X-Ray Source Catalog</TD>
            <TD>The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~10&lt;sup&gt;35&lt;/sup&gt;erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D&lt;sub&gt;25&lt;/sub&gt; ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31deepxmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31deepxmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m31deepxmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31deepxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/375/931 [1]</TD>
            <TD>Radio sources in the 6dFGS (Mauch+, 2007)</TD>
            <TD>We have identified 7824 radio sources from the 1.4GHz NRAO VLA Sky Survey (NVSS, Cat. &lt;VIII/65&gt;) with galaxies brighter than K=12.75mag in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2, Cat. &lt;VII/249&gt;). The resulting sample of redshifts and optical spectra for radio sources over an effective sky area of 7076deg^2^ (about 17 per cent of the celestial sphere) is the largest of its kind ever obtained. NVSS radio sources associated with galaxies in the 6dFGS span a redshift range 0.003&lt;z&lt;0.3 and have median z{bar}=0.043. Through visual examination of 6dF spectra we have identified the dominant mechanism for radio emission from each galaxy. 60 per cent are fuelled by star formation and 40 per cent are fuelled by an active galactic nucleus (AGN) powered by a supermassive black hole. We have accurately determined the local radio luminosity function (RLF) at 1.4GHz for both classes of radio source and have found it to agree well with other recent determinations. From the RLF of star-forming galaxies we derive a local star formation density of 0.022+/-0.001M_{sun}_/yr/Mpc^3^, in broad agreement with recent determinations at radio and other wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931#1</TD>
            <TD>2011-09-14T20:17:20Z</TD>
            <TD>#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/375/931</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/931</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/375/931 [2]</TD>
            <TD>Radio sources in the 6dFGS (Mauch+, 2007)</TD>
            <TD>We have identified 7824 radio sources from the 1.4GHz NRAO VLA Sky Survey (NVSS, Cat. &lt;VIII/65&gt;) with galaxies brighter than K=12.75mag in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2, Cat. &lt;VII/249&gt;). The resulting sample of redshifts and optical spectra for radio sources over an effective sky area of 7076deg^2^ (about 17 per cent of the celestial sphere) is the largest of its kind ever obtained. NVSS radio sources associated with galaxies in the 6dFGS span a redshift range 0.003&lt;z&lt;0.3 and have median z{bar}=0.043. Through visual examination of 6dF spectra we have identified the dominant mechanism for radio emission from each galaxy. 60 per cent are fuelled by star formation and 40 per cent are fuelled by an active galactic nucleus (AGN) powered by a supermassive black hole. We have accurately determined the local radio luminosity function (RLF) at 1.4GHz for both classes of radio source and have found it to agree well with other recent determinations. From the RLF of star-forming galaxies we derive a local star formation density of 0.022+/-0.001M_{sun}_/yr/Mpc^3^, in broad agreement with recent determinations at radio and other wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931#2</TD>
            <TD>2011-09-14T20:17:20Z</TD>
            <TD>#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/375/931&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/931</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/931 [table3]</TD>
            <TD>Radio sources in the 6dFGS (Mauch+, 2007)</TD>
            <TD>We have identified 7824 radio sources from the 1.4GHz NRAO VLA Sky Survey (NVSS, Cat. &lt;VIII/65&gt;) with galaxies brighter than K=12.75mag in the Second Incremental Data Release of the 6 degree Field Galaxy Survey (6dFGS DR2, Cat. &lt;VII/249&gt;). The resulting sample of redshifts and optical spectra for radio sources over an effective sky area of 7076deg^2^ (about 17 per cent of the celestial sphere) is the largest of its kind ever obtained. NVSS radio sources associated with galaxies in the 6dFGS span a redshift range 0.003&lt;z&lt;0.3 and have median z{bar}=0.043. Through visual examination of 6dF spectra we have identified the dominant mechanism for radio emission from each galaxy. 60 per cent are fuelled by star formation and 40 per cent are fuelled by an active galactic nucleus (AGN) powered by a supermassive black hole. We have accurately determined the local radio luminosity function (RLF) at 1.4GHz for both classes of radio source and have found it to agree well with other recent determinations. From the RLF of star-forming galaxies we derive a local star formation density of 0.022+/-0.001M_{sun}_/yr/Mpc^3^, in broad agreement with recent determinations at radio and other wavelengths.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931#table3</TD>
            <TD>2011-09-14T20:17:20Z</TD>
            <TD>#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/931</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/931&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/931</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/675/1459 [1]</TD>
            <TD>Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)</TD>
            <TD>The CBCG catalog is compiled from information provided in the following four astronomical catalogs: (1) the Hubble Space Telescope (HST) Key Project catalog used to measure the Hubble constant (Freedman et al. 2001ApJ...553...47F), (2) Mateo's dwarf galaxies of the local group catalog (Mateo, 2001ApJ...553...47F), (3) the HyperLeda (LEDA) database of galaxies (Paturel et al. 2003A&amp;A...412...45P, Cat. VII/237) and (4) an updated version of the Tully Nearby Galaxy Catalog (B. Tully 2006, private communication).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459#1</TD>
            <TD>2011-09-14T21:03:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/675/1459</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1459</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/675/1459 [2]</TD>
            <TD>Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)</TD>
            <TD>The CBCG catalog is compiled from information provided in the following four astronomical catalogs: (1) the Hubble Space Telescope (HST) Key Project catalog used to measure the Hubble constant (Freedman et al. 2001ApJ...553...47F), (2) Mateo's dwarf galaxies of the local group catalog (Mateo, 2001ApJ...553...47F), (3) the HyperLeda (LEDA) database of galaxies (Paturel et al. 2003A&amp;A...412...45P, Cat. VII/237) and (4) an updated version of the Tully Nearby Galaxy Catalog (B. Tully 2006, private communication).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459#2</TD>
            <TD>2011-09-14T21:03:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/675/1459&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1459</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/675/1459 [table1]</TD>
            <TD>Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)</TD>
            <TD>The CBCG catalog is compiled from information provided in the following four astronomical catalogs: (1) the Hubble Space Telescope (HST) Key Project catalog used to measure the Hubble constant (Freedman et al. 2001ApJ...553...47F), (2) Mateo's dwarf galaxies of the local group catalog (Mateo, 2001ApJ...553...47F), (3) the HyperLeda (LEDA) database of galaxies (Paturel et al. 2003A&amp;A...412...45P, Cat. VII/237) and (4) an updated version of the Tully Nearby Galaxy Catalog (B. Tully 2006, private communication).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459#table1</TD>
            <TD>2011-09-14T21:03:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/675/1459&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1459</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M31DEEPXMM [1]</TD>
            <TD>M 31 Deep XMM-Newton Survey X-Ray Source Catalog</TD>
            <TD>The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~10&lt;sup&gt;35&lt;/sup&gt;erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D&lt;sub&gt;25&lt;/sub&gt; ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31deepxmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31deepxmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m31deepxmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31deepxmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M31DEEPXMM [2]</TD>
            <TD>M 31 Deep XMM-Newton Survey X-Ray Source Catalog</TD>
            <TD>The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~10&lt;sup&gt;35&lt;/sup&gt;erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D&lt;sub&gt;25&lt;/sub&gt; ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31deepxmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31deepxmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m31deepxmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31deepxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M31DEEPXMM [3]</TD>
            <TD>M 31 Deep XMM-Newton Survey X-Ray Source Catalog</TD>
            <TD>The largest Local Group spiral galaxy, M 31, has been completely imaged for the first time, with an obtained luminosity lower limit ~10&lt;sup&gt;35&lt;/sup&gt;erg/s in the 0.2 - 4.5 keV band. This XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D&lt;sub&gt;25&lt;/sub&gt; ellipse. The main goal of the present paper was to study the X-ray source populations of M31. An X-ray catalog of 1897 sources was created ('the XMM LP-total catalog'), with 914 sources detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extents of the sources, and cross correlation with catalogs in the X-ray, optical, infrared and radio wavelengths. The authors also analysed the long-term variability of the X-ray sources and this variability allowed them to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed the authors to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. Fourteen of the 30 supersoft source (SSS) candidates represent supersoft emission of optical novae. Many of the 25 supernova remnants (SNRs) and 31 SNR candidates lie within the 10 kpc dust ring and other star-forming regions in M 31. This connection between SNRs and star-forming regions implies that most of the remnants originate in type II supernovae. The brightest sources in X-rays in M 31 belong to the class of X-ray binaries (XRBs). Ten low-mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition, 36 LMXBs and 17 LMXB candidates were identified owing to correlations with globular clusters and globular cluster candidates. From optical and X-ray colour-colour diagrams, possible high-mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as expected for an HMXB containing a neutron star primary. While this survey has greatly improved our understanding of the X-ray source populations in M 31, at this point 65% of the sources can still only be classified as "hard" sources; i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31 or X-ray sources in the background. Deeper observations in X-ray and at other wavelengths would help to classify these sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m31deepxmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31deepxmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m31deepxmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m31deepxmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/675/1459 [1]</TD>
            <TD>Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)</TD>
            <TD>The CBCG catalog is compiled from information provided in the following four astronomical catalogs: (1) the Hubble Space Telescope (HST) Key Project catalog used to measure the Hubble constant (Freedman et al. 2001ApJ...553...47F), (2) Mateo's dwarf galaxies of the local group catalog (Mateo, 2001ApJ...553...47F), (3) the HyperLeda (LEDA) database of galaxies (Paturel et al. 2003A&amp;A...412...45P, Cat. VII/237) and (4) an updated version of the Tully Nearby Galaxy Catalog (B. Tully 2006, private communication).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459#1</TD>
            <TD>2011-09-14T21:03:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/675/1459</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1459</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/675/1459 [2]</TD>
            <TD>Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)</TD>
            <TD>The CBCG catalog is compiled from information provided in the following four astronomical catalogs: (1) the Hubble Space Telescope (HST) Key Project catalog used to measure the Hubble constant (Freedman et al. 2001ApJ...553...47F), (2) Mateo's dwarf galaxies of the local group catalog (Mateo, 2001ApJ...553...47F), (3) the HyperLeda (LEDA) database of galaxies (Paturel et al. 2003A&amp;A...412...45P, Cat. VII/237) and (4) an updated version of the Tully Nearby Galaxy Catalog (B. Tully 2006, private communication).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459#2</TD>
            <TD>2011-09-14T21:03:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/675/1459&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1459</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/675/1459 [table1]</TD>
            <TD>Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)</TD>
            <TD>The CBCG catalog is compiled from information provided in the following four astronomical catalogs: (1) the Hubble Space Telescope (HST) Key Project catalog used to measure the Hubble constant (Freedman et al. 2001ApJ...553...47F), (2) Mateo's dwarf galaxies of the local group catalog (Mateo, 2001ApJ...553...47F), (3) the HyperLeda (LEDA) database of galaxies (Paturel et al. 2003A&amp;A...412...45P, Cat. VII/237) and (4) an updated version of the Tully Nearby Galaxy Catalog (B. Tully 2006, private communication).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459#table1</TD>
            <TD>2011-09-14T21:03:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/675/1459&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1459</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/475/791 [1]</TD>
            <TD>12um ISOCAM survey of the ESO-Sculptor field (Seymour+, 2007)</TD>
            <TD>We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al., 1997A&amp;AS..124..163A). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5{sigma}), is presented above an integrated flux density of 0.31mJy. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12um flux density is derived by fitting optical colours from a multi-band {chi}^2^ to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007A&amp;A...475..801R) where the 12um faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PEGASE.3.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791#1</TD>
            <TD>2011-09-14T20:17:34Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/475/791</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/475/791</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/475/791 [2]</TD>
            <TD>12um ISOCAM survey of the ESO-Sculptor field (Seymour+, 2007)</TD>
            <TD>We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al., 1997A&amp;AS..124..163A). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5{sigma}), is presented above an integrated flux density of 0.31mJy. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12um flux density is derived by fitting optical colours from a multi-band {chi}^2^ to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007A&amp;A...475..801R) where the 12um faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PEGASE.3.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791#2</TD>
            <TD>2011-09-14T20:17:34Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/475/791&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/475/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/475/791 [catalog]</TD>
            <TD>12um ISOCAM survey of the ESO-Sculptor field (Seymour+, 2007)</TD>
            <TD>We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al., 1997A&amp;AS..124..163A). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5{sigma}), is presented above an integrated flux density of 0.31mJy. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12um flux density is derived by fitting optical colours from a multi-band {chi}^2^ to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007A&amp;A...475..801R) where the 12um faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PEGASE.3.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791#catalog</TD>
            <TD>2011-09-14T20:17:34Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/475/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/475/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ACCEPTCAT [1]</TD>
            <TD>Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog</TD>
            <TD>This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K&lt;sub&gt;0&lt;/sub&gt; + K&lt;sub&gt;100&lt;/sub&gt; (r/100 kpc)&lt;sup&gt;alpha&lt;/sup&gt;, where K&lt;sub&gt;0&lt;/sub&gt; quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K&lt;sub&gt;0&lt;/sub&gt; distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K&lt;sub&gt;0&lt;/sub&gt; ~ 30 - 50 keV cm&lt;sup&gt;2&lt;/sup&gt; and population peaks at K&lt;sub&gt;0&lt;/sub&gt; ~ 15 keV cm&lt;sup&gt;2&lt;/sup&gt; and K&lt;sub&gt;0&lt;/sub&gt; ~ 150 keV cm&lt;sup&gt;2&lt;/sup&gt;. The effects of point-spread function smearing and angular resolution on best-fit K&lt;sub&gt;0&lt;/sub&gt; values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K&lt;sub&gt;0&lt;/sub&gt; is also considered, and they find no indication that K&lt;sub&gt;0&lt;/sub&gt; is significantly impacted by either. All data and results associated with this work are publicly available via the project web site &lt;a href="http://www.pa.msu.edu/astro/MC2/accept/"&gt;http://www.pa.msu.edu/astro/MC2/accept/&lt;/a&gt;. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/acceptcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/acceptcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=acceptcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/acceptcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ACCEPTCAT [2]</TD>
            <TD>Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog</TD>
            <TD>This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K&lt;sub&gt;0&lt;/sub&gt; + K&lt;sub&gt;100&lt;/sub&gt; (r/100 kpc)&lt;sup&gt;alpha&lt;/sup&gt;, where K&lt;sub&gt;0&lt;/sub&gt; quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K&lt;sub&gt;0&lt;/sub&gt; distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K&lt;sub&gt;0&lt;/sub&gt; ~ 30 - 50 keV cm&lt;sup&gt;2&lt;/sup&gt; and population peaks at K&lt;sub&gt;0&lt;/sub&gt; ~ 15 keV cm&lt;sup&gt;2&lt;/sup&gt; and K&lt;sub&gt;0&lt;/sub&gt; ~ 150 keV cm&lt;sup&gt;2&lt;/sup&gt;. The effects of point-spread function smearing and angular resolution on best-fit K&lt;sub&gt;0&lt;/sub&gt; values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K&lt;sub&gt;0&lt;/sub&gt; is also considered, and they find no indication that K&lt;sub&gt;0&lt;/sub&gt; is significantly impacted by either. All data and results associated with this work are publicly available via the project web site &lt;a href="http://www.pa.msu.edu/astro/MC2/accept/"&gt;http://www.pa.msu.edu/astro/MC2/accept/&lt;/a&gt;. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/acceptcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/acceptcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=acceptcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/acceptcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ACCEPTCAT [3]</TD>
            <TD>Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog</TD>
            <TD>This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K&lt;sub&gt;0&lt;/sub&gt; + K&lt;sub&gt;100&lt;/sub&gt; (r/100 kpc)&lt;sup&gt;alpha&lt;/sup&gt;, where K&lt;sub&gt;0&lt;/sub&gt; quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K&lt;sub&gt;0&lt;/sub&gt; distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K&lt;sub&gt;0&lt;/sub&gt; ~ 30 - 50 keV cm&lt;sup&gt;2&lt;/sup&gt; and population peaks at K&lt;sub&gt;0&lt;/sub&gt; ~ 15 keV cm&lt;sup&gt;2&lt;/sup&gt; and K&lt;sub&gt;0&lt;/sub&gt; ~ 150 keV cm&lt;sup&gt;2&lt;/sup&gt;. The effects of point-spread function smearing and angular resolution on best-fit K&lt;sub&gt;0&lt;/sub&gt; values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K&lt;sub&gt;0&lt;/sub&gt; is also considered, and they find no indication that K&lt;sub&gt;0&lt;/sub&gt; is significantly impacted by either. All data and results associated with this work are publicly available via the project web site &lt;a href="http://www.pa.msu.edu/astro/MC2/accept/"&gt;http://www.pa.msu.edu/astro/MC2/accept/&lt;/a&gt;. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/acceptcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/acceptcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_acceptcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/acceptcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/675/1459 [1]</TD>
            <TD>Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)</TD>
            <TD>The CBCG catalog is compiled from information provided in the following four astronomical catalogs: (1) the Hubble Space Telescope (HST) Key Project catalog used to measure the Hubble constant (Freedman et al. 2001ApJ...553...47F), (2) Mateo's dwarf galaxies of the local group catalog (Mateo, 2001ApJ...553...47F), (3) the HyperLeda (LEDA) database of galaxies (Paturel et al. 2003A&amp;A...412...45P, Cat. VII/237) and (4) an updated version of the Tully Nearby Galaxy Catalog (B. Tully 2006, private communication).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459#1</TD>
            <TD>2011-09-14T21:03:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/675/1459</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1459</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/675/1459 [2]</TD>
            <TD>Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)</TD>
            <TD>The CBCG catalog is compiled from information provided in the following four astronomical catalogs: (1) the Hubble Space Telescope (HST) Key Project catalog used to measure the Hubble constant (Freedman et al. 2001ApJ...553...47F), (2) Mateo's dwarf galaxies of the local group catalog (Mateo, 2001ApJ...553...47F), (3) the HyperLeda (LEDA) database of galaxies (Paturel et al. 2003A&amp;A...412...45P, Cat. VII/237) and (4) an updated version of the Tully Nearby Galaxy Catalog (B. Tully 2006, private communication).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459#2</TD>
            <TD>2011-09-14T21:03:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/675/1459&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1459</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/675/1459 [table1]</TD>
            <TD>Compact Binary Coalescence Galaxy Catalog (Kopparapu+, 2008)</TD>
            <TD>The CBCG catalog is compiled from information provided in the following four astronomical catalogs: (1) the Hubble Space Telescope (HST) Key Project catalog used to measure the Hubble constant (Freedman et al. 2001ApJ...553...47F), (2) Mateo's dwarf galaxies of the local group catalog (Mateo, 2001ApJ...553...47F), (3) the HyperLeda (LEDA) database of galaxies (Paturel et al. 2003A&amp;A...412...45P, Cat. VII/237) and (4) an updated version of the Tully Nearby Galaxy Catalog (B. Tully 2006, private communication).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459#table1</TD>
            <TD>2011-09-14T21:03:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/675/1459</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/675/1459&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/675/1459</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/475/791 [1]</TD>
            <TD>12um ISOCAM survey of the ESO-Sculptor field (Seymour+, 2007)</TD>
            <TD>We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al., 1997A&amp;AS..124..163A). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5{sigma}), is presented above an integrated flux density of 0.31mJy. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12um flux density is derived by fitting optical colours from a multi-band {chi}^2^ to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007A&amp;A...475..801R) where the 12um faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PEGASE.3.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791#1</TD>
            <TD>2011-09-14T20:17:34Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/475/791</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/475/791</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/475/791 [2]</TD>
            <TD>12um ISOCAM survey of the ESO-Sculptor field (Seymour+, 2007)</TD>
            <TD>We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al., 1997A&amp;AS..124..163A). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5{sigma}), is presented above an integrated flux density of 0.31mJy. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12um flux density is derived by fitting optical colours from a multi-band {chi}^2^ to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007A&amp;A...475..801R) where the 12um faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PEGASE.3.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791#2</TD>
            <TD>2011-09-14T20:17:34Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/475/791&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/475/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/475/791 [catalog]</TD>
            <TD>12um ISOCAM survey of the ESO-Sculptor field (Seymour+, 2007)</TD>
            <TD>We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al., 1997A&amp;AS..124..163A). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5{sigma}), is presented above an integrated flux density of 0.31mJy. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12um flux density is derived by fitting optical colours from a multi-band {chi}^2^ to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007A&amp;A...475..801R) where the 12um faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PEGASE.3.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791#catalog</TD>
            <TD>2011-09-14T20:17:34Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/475/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/475/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ACCEPTCAT [1]</TD>
            <TD>Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog</TD>
            <TD>This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K&lt;sub&gt;0&lt;/sub&gt; + K&lt;sub&gt;100&lt;/sub&gt; (r/100 kpc)&lt;sup&gt;alpha&lt;/sup&gt;, where K&lt;sub&gt;0&lt;/sub&gt; quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K&lt;sub&gt;0&lt;/sub&gt; distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K&lt;sub&gt;0&lt;/sub&gt; ~ 30 - 50 keV cm&lt;sup&gt;2&lt;/sup&gt; and population peaks at K&lt;sub&gt;0&lt;/sub&gt; ~ 15 keV cm&lt;sup&gt;2&lt;/sup&gt; and K&lt;sub&gt;0&lt;/sub&gt; ~ 150 keV cm&lt;sup&gt;2&lt;/sup&gt;. The effects of point-spread function smearing and angular resolution on best-fit K&lt;sub&gt;0&lt;/sub&gt; values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K&lt;sub&gt;0&lt;/sub&gt; is also considered, and they find no indication that K&lt;sub&gt;0&lt;/sub&gt; is significantly impacted by either. All data and results associated with this work are publicly available via the project web site &lt;a href="http://www.pa.msu.edu/astro/MC2/accept/"&gt;http://www.pa.msu.edu/astro/MC2/accept/&lt;/a&gt;. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/acceptcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/acceptcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=acceptcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/acceptcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ACCEPTCAT [2]</TD>
            <TD>Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog</TD>
            <TD>This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K&lt;sub&gt;0&lt;/sub&gt; + K&lt;sub&gt;100&lt;/sub&gt; (r/100 kpc)&lt;sup&gt;alpha&lt;/sup&gt;, where K&lt;sub&gt;0&lt;/sub&gt; quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K&lt;sub&gt;0&lt;/sub&gt; distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K&lt;sub&gt;0&lt;/sub&gt; ~ 30 - 50 keV cm&lt;sup&gt;2&lt;/sup&gt; and population peaks at K&lt;sub&gt;0&lt;/sub&gt; ~ 15 keV cm&lt;sup&gt;2&lt;/sup&gt; and K&lt;sub&gt;0&lt;/sub&gt; ~ 150 keV cm&lt;sup&gt;2&lt;/sup&gt;. The effects of point-spread function smearing and angular resolution on best-fit K&lt;sub&gt;0&lt;/sub&gt; values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K&lt;sub&gt;0&lt;/sub&gt; is also considered, and they find no indication that K&lt;sub&gt;0&lt;/sub&gt; is significantly impacted by either. All data and results associated with this work are publicly available via the project web site &lt;a href="http://www.pa.msu.edu/astro/MC2/accept/"&gt;http://www.pa.msu.edu/astro/MC2/accept/&lt;/a&gt;. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/acceptcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/acceptcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=acceptcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/acceptcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ACCEPTCAT [3]</TD>
            <TD>Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog</TD>
            <TD>This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K&lt;sub&gt;0&lt;/sub&gt; + K&lt;sub&gt;100&lt;/sub&gt; (r/100 kpc)&lt;sup&gt;alpha&lt;/sup&gt;, where K&lt;sub&gt;0&lt;/sub&gt; quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K&lt;sub&gt;0&lt;/sub&gt; distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K&lt;sub&gt;0&lt;/sub&gt; ~ 30 - 50 keV cm&lt;sup&gt;2&lt;/sup&gt; and population peaks at K&lt;sub&gt;0&lt;/sub&gt; ~ 15 keV cm&lt;sup&gt;2&lt;/sup&gt; and K&lt;sub&gt;0&lt;/sub&gt; ~ 150 keV cm&lt;sup&gt;2&lt;/sup&gt;. The effects of point-spread function smearing and angular resolution on best-fit K&lt;sub&gt;0&lt;/sub&gt; values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K&lt;sub&gt;0&lt;/sub&gt; is also considered, and they find no indication that K&lt;sub&gt;0&lt;/sub&gt; is significantly impacted by either. All data and results associated with this work are publicly available via the project web site &lt;a href="http://www.pa.msu.edu/astro/MC2/accept/"&gt;http://www.pa.msu.edu/astro/MC2/accept/&lt;/a&gt;. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/acceptcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/acceptcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_acceptcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/acceptcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/410/1837 [1]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#1</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/410/1837</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/410/1837 [2]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#2</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/410/1837&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/410/1837 [table1]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#table1</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/410/1837&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/410/1837 [tablea1]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#tablea1</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/410/1837&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/475/791 [1]</TD>
            <TD>12um ISOCAM survey of the ESO-Sculptor field (Seymour+, 2007)</TD>
            <TD>We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al., 1997A&amp;AS..124..163A). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5{sigma}), is presented above an integrated flux density of 0.31mJy. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12um flux density is derived by fitting optical colours from a multi-band {chi}^2^ to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007A&amp;A...475..801R) where the 12um faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PEGASE.3.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791#1</TD>
            <TD>2011-09-14T20:17:34Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/475/791</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/475/791</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/475/791 [2]</TD>
            <TD>12um ISOCAM survey of the ESO-Sculptor field (Seymour+, 2007)</TD>
            <TD>We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al., 1997A&amp;AS..124..163A). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5{sigma}), is presented above an integrated flux density of 0.31mJy. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12um flux density is derived by fitting optical colours from a multi-band {chi}^2^ to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007A&amp;A...475..801R) where the 12um faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PEGASE.3.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791#2</TD>
            <TD>2011-09-14T20:17:34Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/475/791&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/475/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/475/791 [catalog]</TD>
            <TD>12um ISOCAM survey of the ESO-Sculptor field (Seymour+, 2007)</TD>
            <TD>We present a detailed reduction of a mid-infrared 12um (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al., 1997A&amp;AS..124..163A). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5{sigma}), is presented above an integrated flux density of 0.31mJy. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1mJy and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12um flux density is derived by fitting optical colours from a multi-band {chi}^2^ to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007A&amp;A...475..801R) where the 12um faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PEGASE.3.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791#catalog</TD>
            <TD>2011-09-14T20:17:34Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/475/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/475/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/475/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ACCEPTCAT [1]</TD>
            <TD>Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog</TD>
            <TD>This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K&lt;sub&gt;0&lt;/sub&gt; + K&lt;sub&gt;100&lt;/sub&gt; (r/100 kpc)&lt;sup&gt;alpha&lt;/sup&gt;, where K&lt;sub&gt;0&lt;/sub&gt; quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K&lt;sub&gt;0&lt;/sub&gt; distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K&lt;sub&gt;0&lt;/sub&gt; ~ 30 - 50 keV cm&lt;sup&gt;2&lt;/sup&gt; and population peaks at K&lt;sub&gt;0&lt;/sub&gt; ~ 15 keV cm&lt;sup&gt;2&lt;/sup&gt; and K&lt;sub&gt;0&lt;/sub&gt; ~ 150 keV cm&lt;sup&gt;2&lt;/sup&gt;. The effects of point-spread function smearing and angular resolution on best-fit K&lt;sub&gt;0&lt;/sub&gt; values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K&lt;sub&gt;0&lt;/sub&gt; is also considered, and they find no indication that K&lt;sub&gt;0&lt;/sub&gt; is significantly impacted by either. All data and results associated with this work are publicly available via the project web site &lt;a href="http://www.pa.msu.edu/astro/MC2/accept/"&gt;http://www.pa.msu.edu/astro/MC2/accept/&lt;/a&gt;. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/acceptcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/acceptcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=acceptcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/acceptcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ACCEPTCAT [2]</TD>
            <TD>Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog</TD>
            <TD>This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K&lt;sub&gt;0&lt;/sub&gt; + K&lt;sub&gt;100&lt;/sub&gt; (r/100 kpc)&lt;sup&gt;alpha&lt;/sup&gt;, where K&lt;sub&gt;0&lt;/sub&gt; quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K&lt;sub&gt;0&lt;/sub&gt; distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K&lt;sub&gt;0&lt;/sub&gt; ~ 30 - 50 keV cm&lt;sup&gt;2&lt;/sup&gt; and population peaks at K&lt;sub&gt;0&lt;/sub&gt; ~ 15 keV cm&lt;sup&gt;2&lt;/sup&gt; and K&lt;sub&gt;0&lt;/sub&gt; ~ 150 keV cm&lt;sup&gt;2&lt;/sup&gt;. The effects of point-spread function smearing and angular resolution on best-fit K&lt;sub&gt;0&lt;/sub&gt; values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K&lt;sub&gt;0&lt;/sub&gt; is also considered, and they find no indication that K&lt;sub&gt;0&lt;/sub&gt; is significantly impacted by either. All data and results associated with this work are publicly available via the project web site &lt;a href="http://www.pa.msu.edu/astro/MC2/accept/"&gt;http://www.pa.msu.edu/astro/MC2/accept/&lt;/a&gt;. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/acceptcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/acceptcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=acceptcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/acceptcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ACCEPTCAT [3]</TD>
            <TD>Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog</TD>
            <TD>This table, the Archive of Chandra Cluster Entropy Profile Tables (ACCEPT) Catalog, contains the radial entropy profiles of the intracluster medium (ICM) for a collection of 239 clusters taken from the Chandra X-ray Observatory's Data Archive. Entropy is of great interest because it controls ICM global properties and records the thermal history of a cluster. The authors find that most ICM entropy profiles are well fitted by a model which is a power law at large radii and approaches a constant value at small radii: K(r) = K&lt;sub&gt;0&lt;/sub&gt; + K&lt;sub&gt;100&lt;/sub&gt; (r/100 kpc)&lt;sup&gt;alpha&lt;/sup&gt;, where K&lt;sub&gt;0&lt;/sub&gt; quantifies the typical excess of core entropy above the best-fitting power law found at larger radii. The authors also show that the K&lt;sub&gt;0&lt;/sub&gt; distributions of both the full archival sample and the primary Highest X-Ray Flux Galaxy Cluster Sample of Reiprich (2001, Ph.D. thesis) are bimodal with a distinct gap between K&lt;sub&gt;0&lt;/sub&gt; ~ 30 - 50 keV cm&lt;sup&gt;2&lt;/sup&gt; and population peaks at K&lt;sub&gt;0&lt;/sub&gt; ~ 15 keV cm&lt;sup&gt;2&lt;/sup&gt; and K&lt;sub&gt;0&lt;/sub&gt; ~ 150 keV cm&lt;sup&gt;2&lt;/sup&gt;. The effects of point-spread function smearing and angular resolution on best-fit K&lt;sub&gt;0&lt;/sub&gt; values are investigated using mock Chandra observations and degraded entropy profiles, respectively. The authors find that neither of these effects is sufficient to explain the entropy-profile flattening they measure at small radii. The influence of profile curvature and the number of radial bins on the best-fit K&lt;sub&gt;0&lt;/sub&gt; is also considered, and they find no indication that K&lt;sub&gt;0&lt;/sub&gt; is significantly impacted by either. All data and results associated with this work are publicly available via the project web site &lt;a href="http://www.pa.msu.edu/astro/MC2/accept/"&gt;http://www.pa.msu.edu/astro/MC2/accept/&lt;/a&gt;. The sample is collected from observations taken with the Chandra X-ray Observatory and which were publicly available in the CDA (Chandra Data Archive) as of 2008 August.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/acceptcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/acceptcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_acceptcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/acceptcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/410/1837 [1]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#1</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/410/1837</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/410/1837 [2]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#2</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/410/1837&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/410/1837 [table1]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#table1</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/410/1837&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/410/1837 [tablea1]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#tablea1</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/410/1837&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/427/397 [1]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#1</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/427/397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/427/397 [2]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#2</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/427/397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl1216]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl1216</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl1040]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl1040</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl105412]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl105412</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl105411]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl105411</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl1232]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl1232</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ATLASCSCPT [1]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascscpt#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascscpt</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=atlascscpt&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascscpt.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ATLASCSCPT [2]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascscpt#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascscpt</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=atlascscpt&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascscpt.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ATLASCSCPT [3]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascscpt#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascscpt</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_atlascscpt&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascscpt.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/410/1837 [1]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#1</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/410/1837</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/410/1837 [2]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#2</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/410/1837&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/410/1837 [table1]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#table1</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/410/1837&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/410/1837 [tablea1]</TD>
            <TD>Architecture of A1386 and the Sloan Great Wall (Pimbblet+ 2011)</TD>
            <TD>We present new radial velocities for 307 galaxies (bJ&lt;19.5) in the region of the rich cluster Abell 1386. 72 of these galaxies did not have any redshift published before. For each galaxy equatorial coordinates, total R magnitudes and all previously published redshifts are listed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837#tablea1</TD>
            <TD>2011-09-14T21:14:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/410/1837</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/410/1837&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/410/1837</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/427/397 [1]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#1</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/427/397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/427/397 [2]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#2</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/427/397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl1216]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl1216</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl1040]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl1040</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl105412]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl105412</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl105411]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl105411</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl1232]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl1232</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ATLASCSCPT [1]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascscpt#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascscpt</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=atlascscpt&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascscpt.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ATLASCSCPT [2]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascscpt#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascscpt</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=atlascscpt&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascscpt.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ATLASCSCPT [3]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascscpt#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascscpt</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_atlascscpt&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascscpt.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/Ser/179. [1]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87#1</TD>
            <TD>2011-09-14T21:22:14Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/Ser/179.87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/Ser/179.87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/Ser/179. [2]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87#2</TD>
            <TD>2011-09-14T21:22:14Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/Ser/179.87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/Ser/179.87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/Ser/179. [table5]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87#table5</TD>
            <TD>2011-09-14T21:22:14Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/Ser/179.87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/Ser/179.87</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/427/397 [1]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#1</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/427/397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/427/397 [2]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#2</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/427/397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl1216]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl1216</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl1040]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl1040</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl105412]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl105412</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl105411]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl105411</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/427/397 [cl1232]</TD>
            <TD>Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)</TD>
            <TD>Spectroscopic observations are presented for objects in the fields of 4 galaxy clusters at z=0.7-0.8 (Cl 1040.7-1155 (Cl 1040), Cl 1054.4-1146 (Cl 1054-11), Cl 1054.7-1245 (Cl 1054-12), and Cl 1216.8-1201 (Cl 1216)) and in one cluster at z~0.5 (Cl 1232.5-1250 (Cl 1232)) of the ESO Distant Cluster Survey (EDisCS). We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1 arcsecond, spectroscopic redshifts for objects in the fields of our 5 clusters, and membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397#cl1232</TD>
            <TD>2011-09-14T20:19:12Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/427/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/427/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/427/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ATLASCSCPT [1]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascscpt#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascscpt</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=atlascscpt&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascscpt.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ATLASCSCPT [2]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascscpt#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascscpt</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=atlascscpt&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascscpt.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ATLASCSCPT [3]</TD>
            <TD>AT Large Area Survey (ATLAS) CDF-S/SWIRE 1.4-GHz Components Catalog</TD>
            <TD>This table contains some of the first results from the Australia Telescope Large Area Survey (ATLAS), which consists of deep 1.4-GHz radio observations of a 3.7 deg&lt;sup&gt;2&lt;/sup&gt; field surrounding the Chandra Deep Field-South (CDF-S), largely coincident with the infrared Spitzer Wide-Area Infrared Extragalactic (SWIRE) Survey. A total of 784 radio components are identified, corresponding to 726 distinct radio sources, nearly all of which are identified with SWIRE sources in the companion table ATLASCSID. Of the radio sources with measured redshifts, most lie in the redshift range 0.5 to 2 and include both star-forming galaxies and active galactic nuclei. The authors identify a rare population of infrared-faint radio sources that are bright at radio wavelengths but are not seen in the available optical, infrared, or X-ray data. Such rare classes of sources can only be discovered in wide, deep surveys such as this. The radio observations where made on 2002 Apr 4-27, Aug 24-29 and 2004 Jan 7-12, Feb 1-5, Jun 6-12 and Nov 24-30, with the Australia Telescope Compact Array (ATCA). The observations in 2002 were made in a mosaic of 7 overlapping fields, for a total of 149 hours of integration time, or 21.3 hours per pointing. The observations in 2004 were taken in the AT mosaic mode, in which the array was cycled around 21 pointing centers They total 173 hours of integration time, or 8.2 hours per pointing. All observations were made with two 128-MHz bands, centered on frequencies of 1344 and 1472 MHz. This table contains the list of 784 radio components given in Table 4 of the reference paper. The authors define a radio 'component' as a region of radio emission identified in the source extraction process. They define a radio 'source' as one or more radio components that appear to be physically connected and that probably correspond to one galaxy. Thus, the authors count a classical triple radio-loud source as being a radio source consisting of three radio components, but count a pair of interacting starburst galaxies as being two sources, each with one radio component.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/atlascscpt#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/atlascscpt</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_atlascscpt&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/atlascscpt.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/Ser/179. [1]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87#1</TD>
            <TD>2011-09-14T21:22:14Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/Ser/179.87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/Ser/179.87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/Ser/179. [2]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87#2</TD>
            <TD>2011-09-14T21:22:14Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/Ser/179.87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/Ser/179.87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/Ser/179. [table5]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87#table5</TD>
            <TD>2011-09-14T21:22:14Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/Ser/179.87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/Ser/179.87</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>I/284 [1]</TD>
            <TD>The USNO-B1.0 Catalog (Monet+ 2003)</TD>
            <TD>The USNO-B1.0 is a catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,913,669 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalog is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/284#1</TD>
            <TD>2011-09-14T20:20:20Z</TD>
            <TD>#Positional_Data#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/I/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=I/284</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/284</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>I/284 [2]</TD>
            <TD>The USNO-B1.0 Catalog (Monet+ 2003)</TD>
            <TD>The USNO-B1.0 is a catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,913,669 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalog is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/284#2</TD>
            <TD>2011-09-14T20:20:20Z</TD>
            <TD>#Positional_Data#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/I/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=I/284&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/284</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>I/284 [out]</TD>
            <TD>The USNO-B1.0 Catalog (Monet+ 2003)</TD>
            <TD>The USNO-B1.0 is a catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,913,669 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalog is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/284#out</TD>
            <TD>2011-09-14T20:20:20Z</TD>
            <TD>#Positional_Data#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/I/284</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=I/284&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/284</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>INTIBISGAL [1]</TD>
            <TD>INTEGRAL IBIS 9-Year Galactic Hard X-Ray Survey Catalog</TD>
            <TD>The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. The authors aimed to perform a Galactic survey that could be used as the basis of Galactic source population studies, and performed mapping of the Milky Way in hard X-rays over the maximum exposure available at Galactic latitudes |b| &lt; 17.5 degrees. They used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. In their paper. they presented sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17 - 60, 17 - 35, and 35 - 80 keV in the Galactic plane at |b| &lt; 17.5 degrees. The total number of sources in the reference 17 - 60 keV band includes 402 objects exceeding a 4.7-sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei and 3 galaxy clusters. The sample of Galactic sources with S/N &gt; 4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients. This table contains the catalog of 402 INTEGRAL sources exceeding the detection threshold in the 17 - 60 keV energy band.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/intibisgal#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisgal</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=intibisgal&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisgal.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>INTIBISGAL [2]</TD>
            <TD>INTEGRAL IBIS 9-Year Galactic Hard X-Ray Survey Catalog</TD>
            <TD>The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. The authors aimed to perform a Galactic survey that could be used as the basis of Galactic source population studies, and performed mapping of the Milky Way in hard X-rays over the maximum exposure available at Galactic latitudes |b| &lt; 17.5 degrees. They used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. In their paper. they presented sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17 - 60, 17 - 35, and 35 - 80 keV in the Galactic plane at |b| &lt; 17.5 degrees. The total number of sources in the reference 17 - 60 keV band includes 402 objects exceeding a 4.7-sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei and 3 galaxy clusters. The sample of Galactic sources with S/N &gt; 4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients. This table contains the catalog of 402 INTEGRAL sources exceeding the detection threshold in the 17 - 60 keV energy band.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/intibisgal#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=intibisgal&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisgal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>INTIBISGAL [3]</TD>
            <TD>INTEGRAL IBIS 9-Year Galactic Hard X-Ray Survey Catalog</TD>
            <TD>The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. The authors aimed to perform a Galactic survey that could be used as the basis of Galactic source population studies, and performed mapping of the Milky Way in hard X-rays over the maximum exposure available at Galactic latitudes |b| &lt; 17.5 degrees. They used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. In their paper. they presented sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17 - 60, 17 - 35, and 35 - 80 keV in the Galactic plane at |b| &lt; 17.5 degrees. The total number of sources in the reference 17 - 60 keV band includes 402 objects exceeding a 4.7-sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei and 3 galaxy clusters. The sample of Galactic sources with S/N &gt; 4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients. This table contains the catalog of 402 INTEGRAL sources exceeding the detection threshold in the 17 - 60 keV energy band.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/intibisgal#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_intibisgal&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisgal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/Ser/179. [1]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87#1</TD>
            <TD>2011-09-14T21:22:14Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/Ser/179.87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/Ser/179.87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/Ser/179. [2]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87#2</TD>
            <TD>2011-09-14T21:22:14Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/Ser/179.87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/Ser/179.87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/Ser/179. [table5]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87#table5</TD>
            <TD>2011-09-14T21:22:14Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/Ser/179.87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/Ser/179.87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/Ser/179.87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>INTIBISGAL [1]</TD>
            <TD>INTEGRAL IBIS 9-Year Galactic Hard X-Ray Survey Catalog</TD>
            <TD>The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. The authors aimed to perform a Galactic survey that could be used as the basis of Galactic source population studies, and performed mapping of the Milky Way in hard X-rays over the maximum exposure available at Galactic latitudes |b| &lt; 17.5 degrees. They used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. In their paper. they presented sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17 - 60, 17 - 35, and 35 - 80 keV in the Galactic plane at |b| &lt; 17.5 degrees. The total number of sources in the reference 17 - 60 keV band includes 402 objects exceeding a 4.7-sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei and 3 galaxy clusters. The sample of Galactic sources with S/N &gt; 4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients. This table contains the catalog of 402 INTEGRAL sources exceeding the detection threshold in the 17 - 60 keV energy band.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/intibisgal#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisgal</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=intibisgal&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisgal.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>INTIBISGAL [2]</TD>
            <TD>INTEGRAL IBIS 9-Year Galactic Hard X-Ray Survey Catalog</TD>
            <TD>The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. The authors aimed to perform a Galactic survey that could be used as the basis of Galactic source population studies, and performed mapping of the Milky Way in hard X-rays over the maximum exposure available at Galactic latitudes |b| &lt; 17.5 degrees. They used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. In their paper. they presented sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17 - 60, 17 - 35, and 35 - 80 keV in the Galactic plane at |b| &lt; 17.5 degrees. The total number of sources in the reference 17 - 60 keV band includes 402 objects exceeding a 4.7-sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei and 3 galaxy clusters. The sample of Galactic sources with S/N &gt; 4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients. This table contains the catalog of 402 INTEGRAL sources exceeding the detection threshold in the 17 - 60 keV energy band.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/intibisgal#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=intibisgal&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisgal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>INTIBISGAL [3]</TD>
            <TD>INTEGRAL IBIS 9-Year Galactic Hard X-Ray Survey Catalog</TD>
            <TD>The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. The authors aimed to perform a Galactic survey that could be used as the basis of Galactic source population studies, and performed mapping of the Milky Way in hard X-rays over the maximum exposure available at Galactic latitudes |b| &lt; 17.5 degrees. They used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. In their paper. they presented sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17 - 60, 17 - 35, and 35 - 80 keV in the Galactic plane at |b| &lt; 17.5 degrees. The total number of sources in the reference 17 - 60 keV band includes 402 objects exceeding a 4.7-sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei and 3 galaxy clusters. The sample of Galactic sources with S/N &gt; 4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients. This table contains the catalog of 402 INTEGRAL sources exceeding the detection threshold in the 17 - 60 keV energy band.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/intibisgal#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_intibisgal&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisgal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>I/284 [1]</TD>
            <TD>The USNO-B1.0 Catalog (Monet+ 2003)</TD>
            <TD>The USNO-B1.0 is a catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,913,669 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalog is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/284#1</TD>
            <TD>2011-09-14T20:20:20Z</TD>
            <TD>#Positional_Data#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/I/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=I/284</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/284</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>I/284 [2]</TD>
            <TD>The USNO-B1.0 Catalog (Monet+ 2003)</TD>
            <TD>The USNO-B1.0 is a catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,913,669 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalog is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/284#2</TD>
            <TD>2011-09-14T20:20:20Z</TD>
            <TD>#Positional_Data#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/I/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=I/284&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/284</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>I/284 [out]</TD>
            <TD>The USNO-B1.0 Catalog (Monet+ 2003)</TD>
            <TD>The USNO-B1.0 is a catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,913,669 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalog is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/284#out</TD>
            <TD>2011-09-14T20:20:20Z</TD>
            <TD>#Positional_Data#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/I/284</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=I/284&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/284</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/192/10 [1]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#1</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/192/10</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/192/10 [2]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#2</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [ulx]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#ulx</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [table4]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#table4</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [table1]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#table1</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [table3]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#table3</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>INTIBISGAL [1]</TD>
            <TD>INTEGRAL IBIS 9-Year Galactic Hard X-Ray Survey Catalog</TD>
            <TD>The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. The authors aimed to perform a Galactic survey that could be used as the basis of Galactic source population studies, and performed mapping of the Milky Way in hard X-rays over the maximum exposure available at Galactic latitudes |b| &lt; 17.5 degrees. They used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. In their paper. they presented sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17 - 60, 17 - 35, and 35 - 80 keV in the Galactic plane at |b| &lt; 17.5 degrees. The total number of sources in the reference 17 - 60 keV band includes 402 objects exceeding a 4.7-sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei and 3 galaxy clusters. The sample of Galactic sources with S/N &gt; 4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients. This table contains the catalog of 402 INTEGRAL sources exceeding the detection threshold in the 17 - 60 keV energy band.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/intibisgal#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisgal</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=intibisgal&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisgal.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>INTIBISGAL [2]</TD>
            <TD>INTEGRAL IBIS 9-Year Galactic Hard X-Ray Survey Catalog</TD>
            <TD>The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. The authors aimed to perform a Galactic survey that could be used as the basis of Galactic source population studies, and performed mapping of the Milky Way in hard X-rays over the maximum exposure available at Galactic latitudes |b| &lt; 17.5 degrees. They used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. In their paper. they presented sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17 - 60, 17 - 35, and 35 - 80 keV in the Galactic plane at |b| &lt; 17.5 degrees. The total number of sources in the reference 17 - 60 keV band includes 402 objects exceeding a 4.7-sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei and 3 galaxy clusters. The sample of Galactic sources with S/N &gt; 4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients. This table contains the catalog of 402 INTEGRAL sources exceeding the detection threshold in the 17 - 60 keV energy band.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/intibisgal#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=intibisgal&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisgal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>INTIBISGAL [3]</TD>
            <TD>INTEGRAL IBIS 9-Year Galactic Hard X-Ray Survey Catalog</TD>
            <TD>The INTEGRAL observatory operating in a hard X-ray/gamma domain has gathered a large observational data set over nine years starting in 2003. Most of the observing time was dedicated to the Galactic source population study, making possible the deepest Galactic survey in hard X-rays ever compiled. The authors aimed to perform a Galactic survey that could be used as the basis of Galactic source population studies, and performed mapping of the Milky Way in hard X-rays over the maximum exposure available at Galactic latitudes |b| &lt; 17.5 degrees. They used sky reconstruction algorithms especially developed for the high quality imaging of INTEGRAL/IBIS data. In their paper. they presented sky images, sensitivity maps, and catalogs of detected sources in the three energy bands 17 - 60, 17 - 35, and 35 - 80 keV in the Galactic plane at |b| &lt; 17.5 degrees. The total number of sources in the reference 17 - 60 keV band includes 402 objects exceeding a 4.7-sigma detection threshold on the nine-year time-averaged map. Among the identified sources with known and tentatively identified natures, 253 are Galactic objects (108 low-mass X-ray binaries, 82 high-mass X-ray binaries, 36 cataclysmic variables, and 27 are of other types), and 115 are extragalactic objects, including 112 active galactic nuclei and 3 galaxy clusters. The sample of Galactic sources with S/N &gt; 4.7 sigma has an identification completeness of ~92%, which is valuable for population studies. Since the survey is based on the nine-year sky maps, it is optimized for persistent sources and may be biased against finding transients. This table contains the catalog of 402 INTEGRAL sources exceeding the detection threshold in the 17 - 60 keV energy band.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/intibisgal#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/intibisgal</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_intibisgal&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/integral/intibisgal.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>I/284 [1]</TD>
            <TD>The USNO-B1.0 Catalog (Monet+ 2003)</TD>
            <TD>The USNO-B1.0 is a catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,913,669 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalog is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/284#1</TD>
            <TD>2011-09-14T20:20:20Z</TD>
            <TD>#Positional_Data#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/I/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=I/284</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/284</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>I/284 [2]</TD>
            <TD>The USNO-B1.0 Catalog (Monet+ 2003)</TD>
            <TD>The USNO-B1.0 is a catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,913,669 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalog is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/284#2</TD>
            <TD>2011-09-14T20:20:20Z</TD>
            <TD>#Positional_Data#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/I/284</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=I/284&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/284</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>I/284 [out]</TD>
            <TD>The USNO-B1.0 Catalog (Monet+ 2003)</TD>
            <TD>The USNO-B1.0 is a catalog that presents positions, proper motions, magnitudes in various optical passbands, and star/galaxy estimators for 1,045,913,669 objects derived from 3,648,832,040 separate observations. The data were taken from scans of 7,435 Schmidt plates taken from various sky surveys during the last 50 years. The catalog is expected to be complete down to V=21; the estimated accuracies are 0.2arcsec for the positions at J2000, 0.3mag in up to 5 colors, and 85% accuracy for distinguishing stars from non-stellar objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/I/284#out</TD>
            <TD>2011-09-14T20:20:20Z</TD>
            <TD>#Positional_Data#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/I/284</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=I/284&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?I/284</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/192/10 [1]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#1</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/192/10</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/192/10 [2]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#2</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [ulx]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#ulx</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [table4]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#table4</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [table1]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#table1</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [table3]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#table3</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MAXIGSCHGL [1]</TD>
            <TD>First MAXI/GSC High Galactic-Latitude Source Catalog</TD>
            <TD>This table contains the first unbiased source catalog of the Japanese Monitor of All-sky X-ray Image (MAXI) mission at high Galactic latitudes positions (|b| &gt; 10 degrees), produced from the first 7 months of data (2009 September 1 to 2010 March 31) of the Gas Slit Camera (GSC) in the 4-10 keV band. The authors have developed an analysis procedure to detect faint sources from the MAXI data, utilizing a maximum likelihood image fitting method, where the image response, background, and detailed observational conditions are taken into account. The catalog consists of 143 X-ray sources above the 7-sigma significance level with a limiting sensitivity of ~ 1.5 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s (1.2 milliCrab) in the 4-10 keV band. Among them, the authors have identified 38 Galactic/LMC/SMC objects, 48 galaxy clusters, 39 Seyfert galaxies, 12 blazars, and 1 galaxy. Four other sources are confused with multiple objects, and one remains unidentified. The log N - log S relation of extragalactic objects is in good agreement with the HEAO-1 A-2 result, although the list of the brightest AGNs in the entire sky has significantly changed since that produced 30 years ago.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/maxigschgl#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/maxigschgl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=maxigschgl&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/maxi/maxigschgl.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MAXIGSCHGL [2]</TD>
            <TD>First MAXI/GSC High Galactic-Latitude Source Catalog</TD>
            <TD>This table contains the first unbiased source catalog of the Japanese Monitor of All-sky X-ray Image (MAXI) mission at high Galactic latitudes positions (|b| &gt; 10 degrees), produced from the first 7 months of data (2009 September 1 to 2010 March 31) of the Gas Slit Camera (GSC) in the 4-10 keV band. The authors have developed an analysis procedure to detect faint sources from the MAXI data, utilizing a maximum likelihood image fitting method, where the image response, background, and detailed observational conditions are taken into account. The catalog consists of 143 X-ray sources above the 7-sigma significance level with a limiting sensitivity of ~ 1.5 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s (1.2 milliCrab) in the 4-10 keV band. Among them, the authors have identified 38 Galactic/LMC/SMC objects, 48 galaxy clusters, 39 Seyfert galaxies, 12 blazars, and 1 galaxy. Four other sources are confused with multiple objects, and one remains unidentified. The log N - log S relation of extragalactic objects is in good agreement with the HEAO-1 A-2 result, although the list of the brightest AGNs in the entire sky has significantly changed since that produced 30 years ago.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/maxigschgl#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/maxigschgl</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=maxigschgl&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/maxi/maxigschgl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MAXIGSCHGL [3]</TD>
            <TD>First MAXI/GSC High Galactic-Latitude Source Catalog</TD>
            <TD>This table contains the first unbiased source catalog of the Japanese Monitor of All-sky X-ray Image (MAXI) mission at high Galactic latitudes positions (|b| &gt; 10 degrees), produced from the first 7 months of data (2009 September 1 to 2010 March 31) of the Gas Slit Camera (GSC) in the 4-10 keV band. The authors have developed an analysis procedure to detect faint sources from the MAXI data, utilizing a maximum likelihood image fitting method, where the image response, background, and detailed observational conditions are taken into account. The catalog consists of 143 X-ray sources above the 7-sigma significance level with a limiting sensitivity of ~ 1.5 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s (1.2 milliCrab) in the 4-10 keV band. Among them, the authors have identified 38 Galactic/LMC/SMC objects, 48 galaxy clusters, 39 Seyfert galaxies, 12 blazars, and 1 galaxy. Four other sources are confused with multiple objects, and one remains unidentified. The log N - log S relation of extragalactic objects is in good agreement with the HEAO-1 A-2 result, although the list of the brightest AGNs in the entire sky has significantly changed since that produced 30 years ago.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/maxigschgl#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/maxigschgl</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_maxigschgl&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/maxi/maxigschgl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/514 [1]</TD>
            <TD>Galaxies of RX J1416.4+2315 cluster (Cypriano+, 2006)</TD>
            <TD>The imaging and multislit spectroscopic observations of the galaxy group RX J1416.4+2315 were done with the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini North telescope on 2005 February 22 and 2005 March 67, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514#1</TD>
            <TD>2011-09-14T20:20:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/514</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/514</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/514 [2]</TD>
            <TD>Galaxies of RX J1416.4+2315 cluster (Cypriano+, 2006)</TD>
            <TD>The imaging and multislit spectroscopic observations of the galaxy group RX J1416.4+2315 were done with the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini North telescope on 2005 February 22 and 2005 March 67, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514#2</TD>
            <TD>2011-09-14T20:20:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/514&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/514 [table1]</TD>
            <TD>Galaxies of RX J1416.4+2315 cluster (Cypriano+, 2006)</TD>
            <TD>The imaging and multislit spectroscopic observations of the galaxy group RX J1416.4+2315 were done with the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini North telescope on 2005 February 22 and 2005 March 67, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514#table1</TD>
            <TD>2011-09-14T20:20:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/514&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/514</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/192/10 [1]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#1</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/192/10</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/192/10 [2]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#2</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [ulx]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#ulx</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [table4]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#table4</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [table1]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#table1</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/192/10 [table3]</TD>
            <TD>Chandra ACIS survey in 383 nearby galaxies. I. (Liu, 2011)</TD>
            <TD>The nearby galaxy sample is extracted from the Third Reference Catalog of Galaxies (RC3; de Vaucouleurs et al. 1991, Cat. VII/155). The 626 ACIS observations selected for this survey include 83 ACIS-I observations and 543 ACIS-S observations. We have placed the 626 ACIS observations into 320 groups based on the proximity of the pointings. Observations are listed in table 2.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10#table3</TD>
            <TD>2011-09-14T21:22:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/192/10</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/192/10&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/192/10</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MAXIGSCHGL [1]</TD>
            <TD>First MAXI/GSC High Galactic-Latitude Source Catalog</TD>
            <TD>This table contains the first unbiased source catalog of the Japanese Monitor of All-sky X-ray Image (MAXI) mission at high Galactic latitudes positions (|b| &gt; 10 degrees), produced from the first 7 months of data (2009 September 1 to 2010 March 31) of the Gas Slit Camera (GSC) in the 4-10 keV band. The authors have developed an analysis procedure to detect faint sources from the MAXI data, utilizing a maximum likelihood image fitting method, where the image response, background, and detailed observational conditions are taken into account. The catalog consists of 143 X-ray sources above the 7-sigma significance level with a limiting sensitivity of ~ 1.5 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s (1.2 milliCrab) in the 4-10 keV band. Among them, the authors have identified 38 Galactic/LMC/SMC objects, 48 galaxy clusters, 39 Seyfert galaxies, 12 blazars, and 1 galaxy. Four other sources are confused with multiple objects, and one remains unidentified. The log N - log S relation of extragalactic objects is in good agreement with the HEAO-1 A-2 result, although the list of the brightest AGNs in the entire sky has significantly changed since that produced 30 years ago.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/maxigschgl#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/maxigschgl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=maxigschgl&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/maxi/maxigschgl.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MAXIGSCHGL [2]</TD>
            <TD>First MAXI/GSC High Galactic-Latitude Source Catalog</TD>
            <TD>This table contains the first unbiased source catalog of the Japanese Monitor of All-sky X-ray Image (MAXI) mission at high Galactic latitudes positions (|b| &gt; 10 degrees), produced from the first 7 months of data (2009 September 1 to 2010 March 31) of the Gas Slit Camera (GSC) in the 4-10 keV band. The authors have developed an analysis procedure to detect faint sources from the MAXI data, utilizing a maximum likelihood image fitting method, where the image response, background, and detailed observational conditions are taken into account. The catalog consists of 143 X-ray sources above the 7-sigma significance level with a limiting sensitivity of ~ 1.5 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s (1.2 milliCrab) in the 4-10 keV band. Among them, the authors have identified 38 Galactic/LMC/SMC objects, 48 galaxy clusters, 39 Seyfert galaxies, 12 blazars, and 1 galaxy. Four other sources are confused with multiple objects, and one remains unidentified. The log N - log S relation of extragalactic objects is in good agreement with the HEAO-1 A-2 result, although the list of the brightest AGNs in the entire sky has significantly changed since that produced 30 years ago.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/maxigschgl#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/maxigschgl</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=maxigschgl&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/maxi/maxigschgl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MAXIGSCHGL [3]</TD>
            <TD>First MAXI/GSC High Galactic-Latitude Source Catalog</TD>
            <TD>This table contains the first unbiased source catalog of the Japanese Monitor of All-sky X-ray Image (MAXI) mission at high Galactic latitudes positions (|b| &gt; 10 degrees), produced from the first 7 months of data (2009 September 1 to 2010 March 31) of the Gas Slit Camera (GSC) in the 4-10 keV band. The authors have developed an analysis procedure to detect faint sources from the MAXI data, utilizing a maximum likelihood image fitting method, where the image response, background, and detailed observational conditions are taken into account. The catalog consists of 143 X-ray sources above the 7-sigma significance level with a limiting sensitivity of ~ 1.5 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s (1.2 milliCrab) in the 4-10 keV band. Among them, the authors have identified 38 Galactic/LMC/SMC objects, 48 galaxy clusters, 39 Seyfert galaxies, 12 blazars, and 1 galaxy. Four other sources are confused with multiple objects, and one remains unidentified. The log N - log S relation of extragalactic objects is in good agreement with the HEAO-1 A-2 result, although the list of the brightest AGNs in the entire sky has significantly changed since that produced 30 years ago.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/maxigschgl#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/maxigschgl</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_maxigschgl&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/maxi/maxigschgl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/514 [1]</TD>
            <TD>Galaxies of RX J1416.4+2315 cluster (Cypriano+, 2006)</TD>
            <TD>The imaging and multislit spectroscopic observations of the galaxy group RX J1416.4+2315 were done with the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini North telescope on 2005 February 22 and 2005 March 67, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514#1</TD>
            <TD>2011-09-14T20:20:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/514</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/514</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/514 [2]</TD>
            <TD>Galaxies of RX J1416.4+2315 cluster (Cypriano+, 2006)</TD>
            <TD>The imaging and multislit spectroscopic observations of the galaxy group RX J1416.4+2315 were done with the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini North telescope on 2005 February 22 and 2005 March 67, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514#2</TD>
            <TD>2011-09-14T20:20:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/514&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/514 [table1]</TD>
            <TD>Galaxies of RX J1416.4+2315 cluster (Cypriano+, 2006)</TD>
            <TD>The imaging and multislit spectroscopic observations of the galaxy group RX J1416.4+2315 were done with the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini North telescope on 2005 February 22 and 2005 March 67, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514#table1</TD>
            <TD>2011-09-14T20:20:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/514&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/514</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/692/556 [1]</TD>
            <TD>Star forming galaxy templates (Rieke+, 2009)</TD>
            <TD>We assembled SED templates for 11 local luminous and ultraluminous purely star forming infrared galaxies (LIRGs and ULIRGs). Our sample is IRAS 12112+0305, IRAS 14348-1447, IRAS 22491-1808, and Arp 220, all of which were studied by Armus et al. (2007ApJ...656..148A) and thus with high quality Infrared Spectrograph (IRS) spectra, plus IRAS 17208-0014 where a usable spectrum is available from the ISO (Rigopoulou et al. 1999AJ....118.2625R). We selected LIRGs from a sample originally selected for Pa{alpha} imaging with NICMOS (and hence over a restricted range of redshift) and to represent a full range of SED properties. They are NGC 1614, NGC 2369, NGC 3256, ESO 0320-g030, and Zw 049.057 (Alonso-Herrero et al. 2006ApJ...650..835A), plus NGC 4194.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/556#1</TD>
            <TD>2011-09-14T21:22:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/556</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/692/556</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/556</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/692/556 [2]</TD>
            <TD>Star forming galaxy templates (Rieke+, 2009)</TD>
            <TD>We assembled SED templates for 11 local luminous and ultraluminous purely star forming infrared galaxies (LIRGs and ULIRGs). Our sample is IRAS 12112+0305, IRAS 14348-1447, IRAS 22491-1808, and Arp 220, all of which were studied by Armus et al. (2007ApJ...656..148A) and thus with high quality Infrared Spectrograph (IRS) spectra, plus IRAS 17208-0014 where a usable spectrum is available from the ISO (Rigopoulou et al. 1999AJ....118.2625R). We selected LIRGs from a sample originally selected for Pa{alpha} imaging with NICMOS (and hence over a restricted range of redshift) and to represent a full range of SED properties. They are NGC 1614, NGC 2369, NGC 3256, ESO 0320-g030, and Zw 049.057 (Alonso-Herrero et al. 2006ApJ...650..835A), plus NGC 4194.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/556#2</TD>
            <TD>2011-09-14T21:22:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/556</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/692/556&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/556</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MAXIGSCHGL [1]</TD>
            <TD>First MAXI/GSC High Galactic-Latitude Source Catalog</TD>
            <TD>This table contains the first unbiased source catalog of the Japanese Monitor of All-sky X-ray Image (MAXI) mission at high Galactic latitudes positions (|b| &gt; 10 degrees), produced from the first 7 months of data (2009 September 1 to 2010 March 31) of the Gas Slit Camera (GSC) in the 4-10 keV band. The authors have developed an analysis procedure to detect faint sources from the MAXI data, utilizing a maximum likelihood image fitting method, where the image response, background, and detailed observational conditions are taken into account. The catalog consists of 143 X-ray sources above the 7-sigma significance level with a limiting sensitivity of ~ 1.5 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s (1.2 milliCrab) in the 4-10 keV band. Among them, the authors have identified 38 Galactic/LMC/SMC objects, 48 galaxy clusters, 39 Seyfert galaxies, 12 blazars, and 1 galaxy. Four other sources are confused with multiple objects, and one remains unidentified. The log N - log S relation of extragalactic objects is in good agreement with the HEAO-1 A-2 result, although the list of the brightest AGNs in the entire sky has significantly changed since that produced 30 years ago.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/maxigschgl#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/maxigschgl</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=maxigschgl&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/maxi/maxigschgl.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MAXIGSCHGL [2]</TD>
            <TD>First MAXI/GSC High Galactic-Latitude Source Catalog</TD>
            <TD>This table contains the first unbiased source catalog of the Japanese Monitor of All-sky X-ray Image (MAXI) mission at high Galactic latitudes positions (|b| &gt; 10 degrees), produced from the first 7 months of data (2009 September 1 to 2010 March 31) of the Gas Slit Camera (GSC) in the 4-10 keV band. The authors have developed an analysis procedure to detect faint sources from the MAXI data, utilizing a maximum likelihood image fitting method, where the image response, background, and detailed observational conditions are taken into account. The catalog consists of 143 X-ray sources above the 7-sigma significance level with a limiting sensitivity of ~ 1.5 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s (1.2 milliCrab) in the 4-10 keV band. Among them, the authors have identified 38 Galactic/LMC/SMC objects, 48 galaxy clusters, 39 Seyfert galaxies, 12 blazars, and 1 galaxy. Four other sources are confused with multiple objects, and one remains unidentified. The log N - log S relation of extragalactic objects is in good agreement with the HEAO-1 A-2 result, although the list of the brightest AGNs in the entire sky has significantly changed since that produced 30 years ago.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/maxigschgl#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/maxigschgl</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=maxigschgl&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/maxi/maxigschgl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MAXIGSCHGL [3]</TD>
            <TD>First MAXI/GSC High Galactic-Latitude Source Catalog</TD>
            <TD>This table contains the first unbiased source catalog of the Japanese Monitor of All-sky X-ray Image (MAXI) mission at high Galactic latitudes positions (|b| &gt; 10 degrees), produced from the first 7 months of data (2009 September 1 to 2010 March 31) of the Gas Slit Camera (GSC) in the 4-10 keV band. The authors have developed an analysis procedure to detect faint sources from the MAXI data, utilizing a maximum likelihood image fitting method, where the image response, background, and detailed observational conditions are taken into account. The catalog consists of 143 X-ray sources above the 7-sigma significance level with a limiting sensitivity of ~ 1.5 x 10&lt;sup&gt;-11&lt;/sup&gt; erg/cm&lt;sup&gt;2&lt;/sup&gt;/s (1.2 milliCrab) in the 4-10 keV band. Among them, the authors have identified 38 Galactic/LMC/SMC objects, 48 galaxy clusters, 39 Seyfert galaxies, 12 blazars, and 1 galaxy. Four other sources are confused with multiple objects, and one remains unidentified. The log N - log S relation of extragalactic objects is in good agreement with the HEAO-1 A-2 result, although the list of the brightest AGNs in the entire sky has significantly changed since that produced 30 years ago.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/maxigschgl#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/maxigschgl</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_maxigschgl&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/maxi/maxigschgl.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/692/556 [1]</TD>
            <TD>Star forming galaxy templates (Rieke+, 2009)</TD>
            <TD>We assembled SED templates for 11 local luminous and ultraluminous purely star forming infrared galaxies (LIRGs and ULIRGs). Our sample is IRAS 12112+0305, IRAS 14348-1447, IRAS 22491-1808, and Arp 220, all of which were studied by Armus et al. (2007ApJ...656..148A) and thus with high quality Infrared Spectrograph (IRS) spectra, plus IRAS 17208-0014 where a usable spectrum is available from the ISO (Rigopoulou et al. 1999AJ....118.2625R). We selected LIRGs from a sample originally selected for Pa{alpha} imaging with NICMOS (and hence over a restricted range of redshift) and to represent a full range of SED properties. They are NGC 1614, NGC 2369, NGC 3256, ESO 0320-g030, and Zw 049.057 (Alonso-Herrero et al. 2006ApJ...650..835A), plus NGC 4194.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/556#1</TD>
            <TD>2011-09-14T21:22:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/556</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/692/556</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/556</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/692/556 [2]</TD>
            <TD>Star forming galaxy templates (Rieke+, 2009)</TD>
            <TD>We assembled SED templates for 11 local luminous and ultraluminous purely star forming infrared galaxies (LIRGs and ULIRGs). Our sample is IRAS 12112+0305, IRAS 14348-1447, IRAS 22491-1808, and Arp 220, all of which were studied by Armus et al. (2007ApJ...656..148A) and thus with high quality Infrared Spectrograph (IRS) spectra, plus IRAS 17208-0014 where a usable spectrum is available from the ISO (Rigopoulou et al. 1999AJ....118.2625R). We selected LIRGs from a sample originally selected for Pa{alpha} imaging with NICMOS (and hence over a restricted range of redshift) and to represent a full range of SED properties. They are NGC 1614, NGC 2369, NGC 3256, ESO 0320-g030, and Zw 049.057 (Alonso-Herrero et al. 2006ApJ...650..835A), plus NGC 4194.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/556#2</TD>
            <TD>2011-09-14T21:22:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/692/556</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/692/556&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/692/556</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/514 [1]</TD>
            <TD>Galaxies of RX J1416.4+2315 cluster (Cypriano+, 2006)</TD>
            <TD>The imaging and multislit spectroscopic observations of the galaxy group RX J1416.4+2315 were done with the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini North telescope on 2005 February 22 and 2005 March 67, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514#1</TD>
            <TD>2011-09-14T20:20:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/514</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/514</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/514 [2]</TD>
            <TD>Galaxies of RX J1416.4+2315 cluster (Cypriano+, 2006)</TD>
            <TD>The imaging and multislit spectroscopic observations of the galaxy group RX J1416.4+2315 were done with the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini North telescope on 2005 February 22 and 2005 March 67, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514#2</TD>
            <TD>2011-09-14T20:20:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/514&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/514 [table1]</TD>
            <TD>Galaxies of RX J1416.4+2315 cluster (Cypriano+, 2006)</TD>
            <TD>The imaging and multislit spectroscopic observations of the galaxy group RX J1416.4+2315 were done with the Gemini Multi-Object Spectrograph (GMOS) mounted on the Gemini North telescope on 2005 February 22 and 2005 March 67, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514#table1</TD>
            <TD>2011-09-14T20:20:52Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/514</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/514&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE217 [1]</TD>
            <TD>Planck Early Release 217-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 217-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke217#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke217</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke217&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke217.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE217 [2]</TD>
            <TD>Planck Early Release 217-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 217-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke217#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke217</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke217&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke217.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE217 [3]</TD>
            <TD>Planck Early Release 217-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 217-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke217#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke217</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke217&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke217.html</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>SHASSA [1]</TD>
            <TD>The Southern H-Alpha Sky Survey Atlas: Continuum</TD>
            <TD>The Southern H-Alpha Sky Survey Atlas is the product of a wide-angle digital imaging survey of the H-alpha emission from the warm ionized interstellar gas of our Galaxy. This atlas covers the southern hemisphere sky (declinations less than +15 degrees). The observations were taken with a robotic camera operating at Cerro Tololo Inter-American Observatory (CTIO) in Chile. The atlas consists of 2168 images covering 542 fields. There are four images available for each field: &lt;b&gt;H-alpha&lt;/b&gt;, &lt;b&gt;Continuum&lt;/b&gt;, &lt;b&gt;Continuum-Corrected&lt;/b&gt; (the difference of the H-alpha and Continuum images), and &lt;b&gt;Smoothed&lt;/b&gt; (median filtered to 5 pixel, or 4.0 arcminute, resolution to remove star residuals better). The &lt;a href="http://amundsen.swarthmore.edu/SHASSA"&gt;SHASSA web site&lt;/a&gt; has more details of the data and the status of this and related projects. Images can also be obtained from the &lt;a href="http://amundsen.astro.swarthmore.edu/SHASSA/#Images"&gt;Download Images&lt;/a&gt; section at the SHASSA site.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/skyview/shassa#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/shassa</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=shassa&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SHASSA [2]</TD>
            <TD>The Southern H-Alpha Sky Survey Atlas: Continuum</TD>
            <TD>The Southern H-Alpha Sky Survey Atlas is the product of a wide-angle digital imaging survey of the H-alpha emission from the warm ionized interstellar gas of our Galaxy. This atlas covers the southern hemisphere sky (declinations less than +15 degrees). The observations were taken with a robotic camera operating at Cerro Tololo Inter-American Observatory (CTIO) in Chile. The atlas consists of 2168 images covering 542 fields. There are four images available for each field: &lt;b&gt;H-alpha&lt;/b&gt;, &lt;b&gt;Continuum&lt;/b&gt;, &lt;b&gt;Continuum-Corrected&lt;/b&gt; (the difference of the H-alpha and Continuum images), and &lt;b&gt;Smoothed&lt;/b&gt; (median filtered to 5 pixel, or 4.0 arcminute, resolution to remove star residuals better). The &lt;a href="http://amundsen.swarthmore.edu/SHASSA"&gt;SHASSA web site&lt;/a&gt; has more details of the data and the status of this and related projects. Images can also be obtained from the &lt;a href="http://amundsen.astro.swarthmore.edu/SHASSA/#Images"&gt;Download Images&lt;/a&gt; section at the SHASSA site.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/skyview/shassa#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/shassa</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/119/7 [1]</TD>
            <TD>HST WFPC2 star clusters in M31 (Krienke+, 2007)</TD>
            <TD>As a followup to the automated cluster search carried out by Williams &amp; Hodge (2001ApJ...548..190W), we have examined 39 Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) pointings to locate and study a comprehensive collection of disk clusters. The Williams technique was effective in finding young clusters, but not intermediate-age or old clusters. Our searches have shown that M31 has large numbers of these intermediate and older open clusters, most of them undetected by both the Williams survey and other ground-based searches. We present a catalog of 343 clusters detected on the WFPC2 images. Extrapolation from our data indicates that the entire disk of M31 contains approximately 80000 star clusters. We have carried out integrated multicolor photometry of these clusters to ascertain their properties and to compare their properties with cluster systems of other galaxies. We show the cluster luminosity function, the color-magnitude diagram, the formation function, and the size distribution. Cluster densities and colors show trends with disk position. An age distribution is derived and, although the ages are very uncertain for the fainter clusters, there is evidence for cluster dynamical destruction at about the same rate as in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7#1</TD>
            <TD>2011-09-14T20:21:24Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/119/7</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/119/7</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/119/7 [2]</TD>
            <TD>HST WFPC2 star clusters in M31 (Krienke+, 2007)</TD>
            <TD>As a followup to the automated cluster search carried out by Williams &amp; Hodge (2001ApJ...548..190W), we have examined 39 Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) pointings to locate and study a comprehensive collection of disk clusters. The Williams technique was effective in finding young clusters, but not intermediate-age or old clusters. Our searches have shown that M31 has large numbers of these intermediate and older open clusters, most of them undetected by both the Williams survey and other ground-based searches. We present a catalog of 343 clusters detected on the WFPC2 images. Extrapolation from our data indicates that the entire disk of M31 contains approximately 80000 star clusters. We have carried out integrated multicolor photometry of these clusters to ascertain their properties and to compare their properties with cluster systems of other galaxies. We show the cluster luminosity function, the color-magnitude diagram, the formation function, and the size distribution. Cluster densities and colors show trends with disk position. An age distribution is derived and, although the ages are very uncertain for the fainter clusters, there is evidence for cluster dynamical destruction at about the same rate as in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7#2</TD>
            <TD>2011-09-14T20:21:24Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/119/7&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/119/7</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/119/7 [table2]</TD>
            <TD>HST WFPC2 star clusters in M31 (Krienke+, 2007)</TD>
            <TD>As a followup to the automated cluster search carried out by Williams &amp; Hodge (2001ApJ...548..190W), we have examined 39 Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) pointings to locate and study a comprehensive collection of disk clusters. The Williams technique was effective in finding young clusters, but not intermediate-age or old clusters. Our searches have shown that M31 has large numbers of these intermediate and older open clusters, most of them undetected by both the Williams survey and other ground-based searches. We present a catalog of 343 clusters detected on the WFPC2 images. Extrapolation from our data indicates that the entire disk of M31 contains approximately 80000 star clusters. We have carried out integrated multicolor photometry of these clusters to ascertain their properties and to compare their properties with cluster systems of other galaxies. We show the cluster luminosity function, the color-magnitude diagram, the formation function, and the size distribution. Cluster densities and colors show trends with disk position. An age distribution is derived and, although the ages are very uncertain for the fainter clusters, there is evidence for cluster dynamical destruction at about the same rate as in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7#table2</TD>
            <TD>2011-09-14T20:21:24Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/119/7&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/119/7</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE217 [1]</TD>
            <TD>Planck Early Release 217-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 217-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke217#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke217</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke217&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke217.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE217 [2]</TD>
            <TD>Planck Early Release 217-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 217-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke217#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke217</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke217&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke217.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE217 [3]</TD>
            <TD>Planck Early Release 217-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 217-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke217#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke217</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke217&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke217.html</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>SHASSA [1]</TD>
            <TD>The Southern H-Alpha Sky Survey Atlas: Continuum</TD>
            <TD>The Southern H-Alpha Sky Survey Atlas is the product of a wide-angle digital imaging survey of the H-alpha emission from the warm ionized interstellar gas of our Galaxy. This atlas covers the southern hemisphere sky (declinations less than +15 degrees). The observations were taken with a robotic camera operating at Cerro Tololo Inter-American Observatory (CTIO) in Chile. The atlas consists of 2168 images covering 542 fields. There are four images available for each field: &lt;b&gt;H-alpha&lt;/b&gt;, &lt;b&gt;Continuum&lt;/b&gt;, &lt;b&gt;Continuum-Corrected&lt;/b&gt; (the difference of the H-alpha and Continuum images), and &lt;b&gt;Smoothed&lt;/b&gt; (median filtered to 5 pixel, or 4.0 arcminute, resolution to remove star residuals better). The &lt;a href="http://amundsen.swarthmore.edu/SHASSA"&gt;SHASSA web site&lt;/a&gt; has more details of the data and the status of this and related projects. Images can also be obtained from the &lt;a href="http://amundsen.astro.swarthmore.edu/SHASSA/#Images"&gt;Download Images&lt;/a&gt; section at the SHASSA site.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/skyview/shassa#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/shassa</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=shassa&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SHASSA [2]</TD>
            <TD>The Southern H-Alpha Sky Survey Atlas: Continuum</TD>
            <TD>The Southern H-Alpha Sky Survey Atlas is the product of a wide-angle digital imaging survey of the H-alpha emission from the warm ionized interstellar gas of our Galaxy. This atlas covers the southern hemisphere sky (declinations less than +15 degrees). The observations were taken with a robotic camera operating at Cerro Tololo Inter-American Observatory (CTIO) in Chile. The atlas consists of 2168 images covering 542 fields. There are four images available for each field: &lt;b&gt;H-alpha&lt;/b&gt;, &lt;b&gt;Continuum&lt;/b&gt;, &lt;b&gt;Continuum-Corrected&lt;/b&gt; (the difference of the H-alpha and Continuum images), and &lt;b&gt;Smoothed&lt;/b&gt; (median filtered to 5 pixel, or 4.0 arcminute, resolution to remove star residuals better). The &lt;a href="http://amundsen.swarthmore.edu/SHASSA"&gt;SHASSA web site&lt;/a&gt; has more details of the data and the status of this and related projects. Images can also be obtained from the &lt;a href="http://amundsen.astro.swarthmore.edu/SHASSA/#Images"&gt;Download Images&lt;/a&gt; section at the SHASSA site.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/skyview/shassa#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/shassa</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/119/7 [1]</TD>
            <TD>HST WFPC2 star clusters in M31 (Krienke+, 2007)</TD>
            <TD>As a followup to the automated cluster search carried out by Williams &amp; Hodge (2001ApJ...548..190W), we have examined 39 Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) pointings to locate and study a comprehensive collection of disk clusters. The Williams technique was effective in finding young clusters, but not intermediate-age or old clusters. Our searches have shown that M31 has large numbers of these intermediate and older open clusters, most of them undetected by both the Williams survey and other ground-based searches. We present a catalog of 343 clusters detected on the WFPC2 images. Extrapolation from our data indicates that the entire disk of M31 contains approximately 80000 star clusters. We have carried out integrated multicolor photometry of these clusters to ascertain their properties and to compare their properties with cluster systems of other galaxies. We show the cluster luminosity function, the color-magnitude diagram, the formation function, and the size distribution. Cluster densities and colors show trends with disk position. An age distribution is derived and, although the ages are very uncertain for the fainter clusters, there is evidence for cluster dynamical destruction at about the same rate as in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7#1</TD>
            <TD>2011-09-14T20:21:24Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/119/7</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/119/7</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/119/7 [2]</TD>
            <TD>HST WFPC2 star clusters in M31 (Krienke+, 2007)</TD>
            <TD>As a followup to the automated cluster search carried out by Williams &amp; Hodge (2001ApJ...548..190W), we have examined 39 Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) pointings to locate and study a comprehensive collection of disk clusters. The Williams technique was effective in finding young clusters, but not intermediate-age or old clusters. Our searches have shown that M31 has large numbers of these intermediate and older open clusters, most of them undetected by both the Williams survey and other ground-based searches. We present a catalog of 343 clusters detected on the WFPC2 images. Extrapolation from our data indicates that the entire disk of M31 contains approximately 80000 star clusters. We have carried out integrated multicolor photometry of these clusters to ascertain their properties and to compare their properties with cluster systems of other galaxies. We show the cluster luminosity function, the color-magnitude diagram, the formation function, and the size distribution. Cluster densities and colors show trends with disk position. An age distribution is derived and, although the ages are very uncertain for the fainter clusters, there is evidence for cluster dynamical destruction at about the same rate as in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7#2</TD>
            <TD>2011-09-14T20:21:24Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/119/7&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/119/7</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/119/7 [table2]</TD>
            <TD>HST WFPC2 star clusters in M31 (Krienke+, 2007)</TD>
            <TD>As a followup to the automated cluster search carried out by Williams &amp; Hodge (2001ApJ...548..190W), we have examined 39 Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) pointings to locate and study a comprehensive collection of disk clusters. The Williams technique was effective in finding young clusters, but not intermediate-age or old clusters. Our searches have shown that M31 has large numbers of these intermediate and older open clusters, most of them undetected by both the Williams survey and other ground-based searches. We present a catalog of 343 clusters detected on the WFPC2 images. Extrapolation from our data indicates that the entire disk of M31 contains approximately 80000 star clusters. We have carried out integrated multicolor photometry of these clusters to ascertain their properties and to compare their properties with cluster systems of other galaxies. We show the cluster luminosity function, the color-magnitude diagram, the formation function, and the size distribution. Cluster densities and colors show trends with disk position. An age distribution is derived and, although the ages are very uncertain for the fainter clusters, there is evidence for cluster dynamical destruction at about the same rate as in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7#table2</TD>
            <TD>2011-09-14T20:21:24Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/119/7&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/119/7</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/1921 [1]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#1</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/1921</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/1921 [2]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#2</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table9]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table9</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table5]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table5</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table8]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table8</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table10]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table10</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/1921 [1]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#1</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/1921</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/1921 [2]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#2</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table9]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table9</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table5]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table5</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table8]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table8</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table10]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table10</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/1921 [1]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#1</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/1921</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/1921 [2]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#2</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table9]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table9</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table5]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table5</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table8]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table8</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/1921 [table10]</TD>
            <TD>Variable stars of Draco dSph (Kinemuchi+, 2008)</TD>
            <TD>Our survey of the Draco dSph galaxy was conducted at two telescopes: the 1.0m at the US Naval Observatory (USNO) in Flagstaff, AZ, and the 2.3m telescope at the Wyoming Infrared Observatory (WIRO), at Mt. Jelm, Wyoming. Combined, the two data sets cover a time interval of four years (1993-1996).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921#table10</TD>
            <TD>2011-10-04T11:09:49Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/1921</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/1921&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/1921</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/119/7 [1]</TD>
            <TD>HST WFPC2 star clusters in M31 (Krienke+, 2007)</TD>
            <TD>As a followup to the automated cluster search carried out by Williams &amp; Hodge (2001ApJ...548..190W), we have examined 39 Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) pointings to locate and study a comprehensive collection of disk clusters. The Williams technique was effective in finding young clusters, but not intermediate-age or old clusters. Our searches have shown that M31 has large numbers of these intermediate and older open clusters, most of them undetected by both the Williams survey and other ground-based searches. We present a catalog of 343 clusters detected on the WFPC2 images. Extrapolation from our data indicates that the entire disk of M31 contains approximately 80000 star clusters. We have carried out integrated multicolor photometry of these clusters to ascertain their properties and to compare their properties with cluster systems of other galaxies. We show the cluster luminosity function, the color-magnitude diagram, the formation function, and the size distribution. Cluster densities and colors show trends with disk position. An age distribution is derived and, although the ages are very uncertain for the fainter clusters, there is evidence for cluster dynamical destruction at about the same rate as in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7#1</TD>
            <TD>2011-09-14T20:21:24Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/119/7</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/119/7</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/119/7 [2]</TD>
            <TD>HST WFPC2 star clusters in M31 (Krienke+, 2007)</TD>
            <TD>As a followup to the automated cluster search carried out by Williams &amp; Hodge (2001ApJ...548..190W), we have examined 39 Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) pointings to locate and study a comprehensive collection of disk clusters. The Williams technique was effective in finding young clusters, but not intermediate-age or old clusters. Our searches have shown that M31 has large numbers of these intermediate and older open clusters, most of them undetected by both the Williams survey and other ground-based searches. We present a catalog of 343 clusters detected on the WFPC2 images. Extrapolation from our data indicates that the entire disk of M31 contains approximately 80000 star clusters. We have carried out integrated multicolor photometry of these clusters to ascertain their properties and to compare their properties with cluster systems of other galaxies. We show the cluster luminosity function, the color-magnitude diagram, the formation function, and the size distribution. Cluster densities and colors show trends with disk position. An age distribution is derived and, although the ages are very uncertain for the fainter clusters, there is evidence for cluster dynamical destruction at about the same rate as in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7#2</TD>
            <TD>2011-09-14T20:21:24Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/119/7&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/119/7</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/119/7 [table2]</TD>
            <TD>HST WFPC2 star clusters in M31 (Krienke+, 2007)</TD>
            <TD>As a followup to the automated cluster search carried out by Williams &amp; Hodge (2001ApJ...548..190W), we have examined 39 Hubble Space Telescope Wide Field Planetary Camera 2 (WFPC2) pointings to locate and study a comprehensive collection of disk clusters. The Williams technique was effective in finding young clusters, but not intermediate-age or old clusters. Our searches have shown that M31 has large numbers of these intermediate and older open clusters, most of them undetected by both the Williams survey and other ground-based searches. We present a catalog of 343 clusters detected on the WFPC2 images. Extrapolation from our data indicates that the entire disk of M31 contains approximately 80000 star clusters. We have carried out integrated multicolor photometry of these clusters to ascertain their properties and to compare their properties with cluster systems of other galaxies. We show the cluster luminosity function, the color-magnitude diagram, the formation function, and the size distribution. Cluster densities and colors show trends with disk position. An age distribution is derived and, although the ages are very uncertain for the fainter clusters, there is evidence for cluster dynamical destruction at about the same rate as in our Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7#table2</TD>
            <TD>2011-09-14T20:21:24Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/PASP/119/7</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/119/7&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/119/7</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/478/321 [1]</TD>
            <TD>QSO Type1/Type2 dichotomy (Borguet+, 2008)</TD>
            <TD>This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321#1</TD>
            <TD>2011-09-14T20:21:39Z</TD>
            <TD>#Polarization#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/478/321</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/321</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/478/321 [2]</TD>
            <TD>QSO Type1/Type2 dichotomy (Borguet+, 2008)</TD>
            <TD>This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321#2</TD>
            <TD>2011-09-14T20:21:39Z</TD>
            <TD>#Polarization#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/478/321&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/321</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/478/321 [table6]</TD>
            <TD>QSO Type1/Type2 dichotomy (Borguet+, 2008)</TD>
            <TD>This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321#table6</TD>
            <TD>2011-09-14T20:21:39Z</TD>
            <TD>#Polarization#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/478/321&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/321</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A134 [1]</TD>
            <TD>Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)</TD>
            <TD>In the XMM-Newton archival data, we selected the 28 brightest clusters of galaxies with z&lt;0.08 and total exposures above 7ks after filtering out background flares.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134#1</TD>
            <TD>2011-09-18T10:27:32Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A134</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A134</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A134 [2]</TD>
            <TD>Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)</TD>
            <TD>In the XMM-Newton archival data, we selected the 28 brightest clusters of galaxies with z&lt;0.08 and total exposures above 7ks after filtering out background flares.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134#2</TD>
            <TD>2011-09-18T10:27:32Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A134&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A134</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A134 [clusters]</TD>
            <TD>Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)</TD>
            <TD>In the XMM-Newton archival data, we selected the 28 brightest clusters of galaxies with z&lt;0.08 and total exposures above 7ks after filtering out background flares.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134#clusters</TD>
            <TD>2011-09-18T10:27:32Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A134&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A134</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE217 [1]</TD>
            <TD>Planck Early Release 217-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 217-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke217#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke217</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke217&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke217.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE217 [2]</TD>
            <TD>Planck Early Release 217-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 217-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke217#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke217</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke217&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke217.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE217 [3]</TD>
            <TD>Planck Early Release 217-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 217-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke217#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke217</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke217&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke217.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/478/321 [1]</TD>
            <TD>QSO Type1/Type2 dichotomy (Borguet+, 2008)</TD>
            <TD>This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321#1</TD>
            <TD>2011-09-14T20:21:39Z</TD>
            <TD>#Polarization#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/478/321</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/321</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/478/321 [2]</TD>
            <TD>QSO Type1/Type2 dichotomy (Borguet+, 2008)</TD>
            <TD>This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321#2</TD>
            <TD>2011-09-14T20:21:39Z</TD>
            <TD>#Polarization#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/478/321&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/321</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/478/321 [table6]</TD>
            <TD>QSO Type1/Type2 dichotomy (Borguet+, 2008)</TD>
            <TD>This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321#table6</TD>
            <TD>2011-09-14T20:21:39Z</TD>
            <TD>#Polarization#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/478/321&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/321</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A134 [1]</TD>
            <TD>Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)</TD>
            <TD>In the XMM-Newton archival data, we selected the 28 brightest clusters of galaxies with z&lt;0.08 and total exposures above 7ks after filtering out background flares.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134#1</TD>
            <TD>2011-09-18T10:27:32Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A134</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A134</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A134 [2]</TD>
            <TD>Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)</TD>
            <TD>In the XMM-Newton archival data, we selected the 28 brightest clusters of galaxies with z&lt;0.08 and total exposures above 7ks after filtering out background flares.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134#2</TD>
            <TD>2011-09-18T10:27:32Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A134&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A134</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A134 [clusters]</TD>
            <TD>Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)</TD>
            <TD>In the XMM-Newton archival data, we selected the 28 brightest clusters of galaxies with z&lt;0.08 and total exposures above 7ks after filtering out background flares.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134#clusters</TD>
            <TD>2011-09-18T10:27:32Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A134&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A134</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE545 [1]</TD>
            <TD>Planck Early Release 545-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 545-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke545#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke545</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke545&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke545.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE545 [2]</TD>
            <TD>Planck Early Release 545-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 545-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke545#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke545</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke545&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke545.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE545 [3]</TD>
            <TD>Planck Early Release 545-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 545-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke545#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke545</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke545&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke545.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/478/321 [1]</TD>
            <TD>QSO Type1/Type2 dichotomy (Borguet+, 2008)</TD>
            <TD>This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321#1</TD>
            <TD>2011-09-14T20:21:39Z</TD>
            <TD>#Polarization#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/478/321</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/321</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/478/321 [2]</TD>
            <TD>QSO Type1/Type2 dichotomy (Borguet+, 2008)</TD>
            <TD>This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321#2</TD>
            <TD>2011-09-14T20:21:39Z</TD>
            <TD>#Polarization#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/478/321&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/321</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/478/321 [table6]</TD>
            <TD>QSO Type1/Type2 dichotomy (Borguet+, 2008)</TD>
            <TD>This table contains the measurements/compilation of host galaxy/ extended emission position angle in the visible and near-IR domain, polarimetric data, and radio axis orientation for the 135 quasars of our sample. The angles are given in degrees east of north. The table gives the spectral and the radio-loud/radio-quiet classification of each object according to the references.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321#table6</TD>
            <TD>2011-09-14T20:21:39Z</TD>
            <TD>#Polarization#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/321</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/478/321&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/321</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE545 [1]</TD>
            <TD>Planck Early Release 545-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 545-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke545#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke545</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke545&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke545.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE545 [2]</TD>
            <TD>Planck Early Release 545-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 545-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke545#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke545</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke545&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke545.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE545 [3]</TD>
            <TD>Planck Early Release 545-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 545-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke545#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke545</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke545&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke545.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A134 [1]</TD>
            <TD>Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)</TD>
            <TD>In the XMM-Newton archival data, we selected the 28 brightest clusters of galaxies with z&lt;0.08 and total exposures above 7ks after filtering out background flares.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134#1</TD>
            <TD>2011-09-18T10:27:32Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A134</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A134</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A134 [2]</TD>
            <TD>Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)</TD>
            <TD>In the XMM-Newton archival data, we selected the 28 brightest clusters of galaxies with z&lt;0.08 and total exposures above 7ks after filtering out background flares.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134#2</TD>
            <TD>2011-09-18T10:27:32Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A134&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A134</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A134 [clusters]</TD>
            <TD>Fe abundances for 28 XMM galaxy clusters (Matsushita, 2011)</TD>
            <TD>In the XMM-Newton archival data, we selected the 28 brightest clusters of galaxies with z&lt;0.08 and total exposures above 7ks after filtering out background flares.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134#clusters</TD>
            <TD>2011-09-18T10:27:32Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A134</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A134&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A134</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE545 [1]</TD>
            <TD>Planck Early Release 545-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 545-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke545#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke545</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke545&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke545.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE545 [2]</TD>
            <TD>Planck Early Release 545-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 545-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke545#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke545</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke545&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke545.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE545 [3]</TD>
            <TD>Planck Early Release 545-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 545-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke545#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke545</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke545&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke545.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/482/419 [1]</TD>
            <TD>ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)</TD>
            <TD>Spectroscopic observations obtained using VLT/FORS2 are presented for objects in 14 survey fields of the ESO Distant Cluster Survey (EDisCS). The fields contain galaxy clusters at z=0.40-0.96. The objects in the catalogues are either galaxies (which can be cluster members or fields galaxies), foreground stars, or objects for which no redshift could be determined. For a 15th field (1122.9-1136) which is part of the paper, no data are published, since very little data was obtained. We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1", spectroscopic redshifts for objects in the 14 fields, and cluster membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively. The 'main' table contains one entry per unique object, and this is the table people normally should use. The 'supp' table contains possible extra redshifts obtained. If an object was observed N times, the best redshift (decided from a number of rules) is put in 'main' and the remaining N-1 redshifts are put in 'supp'. Cl 1238.5-1144 has no data in supp.dat file. The data tables have been prepared so that they can be read both using tools that expect data columns separated by white space (e.g. the UNIX tool awk) and tools that expect things to be at fixed character/byte locations in the file (e.g. the UNIX tool cut). The contents of the data tables are fully described in Sect. 4.3 of the paper (including the sample data in Table 4 in the paper). Some of the salient features are repeated as Notes. Finally, note that spectroscopic observations for 5 other EDisCS fields (1040.7-1155, 1054.4-1146, 1054.7-1245, 1216.8-1201 and 1232.5-1250 ) were presented in a previous paper (Halliday et al., 2004, Cat. J/A+A/427/397) but note that the format of the published data tables for that paper is not fully identical to the format used for this paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419#1</TD>
            <TD>2011-09-14T20:22:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>24-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419</TD>
            <TD />
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            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/482/419</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/419</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/482/419 [2]</TD>
            <TD>ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)</TD>
            <TD>Spectroscopic observations obtained using VLT/FORS2 are presented for objects in 14 survey fields of the ESO Distant Cluster Survey (EDisCS). The fields contain galaxy clusters at z=0.40-0.96. The objects in the catalogues are either galaxies (which can be cluster members or fields galaxies), foreground stars, or objects for which no redshift could be determined. For a 15th field (1122.9-1136) which is part of the paper, no data are published, since very little data was obtained. We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1", spectroscopic redshifts for objects in the 14 fields, and cluster membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively. The 'main' table contains one entry per unique object, and this is the table people normally should use. The 'supp' table contains possible extra redshifts obtained. If an object was observed N times, the best redshift (decided from a number of rules) is put in 'main' and the remaining N-1 redshifts are put in 'supp'. Cl 1238.5-1144 has no data in supp.dat file. The data tables have been prepared so that they can be read both using tools that expect data columns separated by white space (e.g. the UNIX tool awk) and tools that expect things to be at fixed character/byte locations in the file (e.g. the UNIX tool cut). The contents of the data tables are fully described in Sect. 4.3 of the paper (including the sample data in Table 4 in the paper). Some of the salient features are repeated as Notes. Finally, note that spectroscopic observations for 5 other EDisCS fields (1040.7-1155, 1054.4-1146, 1054.7-1245, 1216.8-1201 and 1232.5-1250 ) were presented in a previous paper (Halliday et al., 2004, Cat. J/A+A/427/397) but note that the format of the published data tables for that paper is not fully identical to the format used for this paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T20:22:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>24-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/482/419&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/419</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/482/419 [data]</TD>
            <TD>ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)</TD>
            <TD>Spectroscopic observations obtained using VLT/FORS2 are presented for objects in 14 survey fields of the ESO Distant Cluster Survey (EDisCS). The fields contain galaxy clusters at z=0.40-0.96. The objects in the catalogues are either galaxies (which can be cluster members or fields galaxies), foreground stars, or objects for which no redshift could be determined. For a 15th field (1122.9-1136) which is part of the paper, no data are published, since very little data was obtained. We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1", spectroscopic redshifts for objects in the 14 fields, and cluster membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively. The 'main' table contains one entry per unique object, and this is the table people normally should use. The 'supp' table contains possible extra redshifts obtained. If an object was observed N times, the best redshift (decided from a number of rules) is put in 'main' and the remaining N-1 redshifts are put in 'supp'. Cl 1238.5-1144 has no data in supp.dat file. The data tables have been prepared so that they can be read both using tools that expect data columns separated by white space (e.g. the UNIX tool awk) and tools that expect things to be at fixed character/byte locations in the file (e.g. the UNIX tool cut). The contents of the data tables are fully described in Sect. 4.3 of the paper (including the sample data in Table 4 in the paper). Some of the salient features are repeated as Notes. Finally, note that spectroscopic observations for 5 other EDisCS fields (1040.7-1155, 1054.4-1146, 1054.7-1245, 1216.8-1201 and 1232.5-1250 ) were presented in a previous paper (Halliday et al., 2004, Cat. J/A+A/427/397) but note that the format of the published data tables for that paper is not fully identical to the format used for this paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419#data</TD>
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            <TD>#Catalog#</TD>
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            <TD>24-Apr-2008</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/482/419&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/419</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/482/419 [1]</TD>
            <TD>ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)</TD>
            <TD>Spectroscopic observations obtained using VLT/FORS2 are presented for objects in 14 survey fields of the ESO Distant Cluster Survey (EDisCS). The fields contain galaxy clusters at z=0.40-0.96. The objects in the catalogues are either galaxies (which can be cluster members or fields galaxies), foreground stars, or objects for which no redshift could be determined. For a 15th field (1122.9-1136) which is part of the paper, no data are published, since very little data was obtained. We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1", spectroscopic redshifts for objects in the 14 fields, and cluster membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively. The 'main' table contains one entry per unique object, and this is the table people normally should use. The 'supp' table contains possible extra redshifts obtained. If an object was observed N times, the best redshift (decided from a number of rules) is put in 'main' and the remaining N-1 redshifts are put in 'supp'. Cl 1238.5-1144 has no data in supp.dat file. The data tables have been prepared so that they can be read both using tools that expect data columns separated by white space (e.g. the UNIX tool awk) and tools that expect things to be at fixed character/byte locations in the file (e.g. the UNIX tool cut). The contents of the data tables are fully described in Sect. 4.3 of the paper (including the sample data in Table 4 in the paper). Some of the salient features are repeated as Notes. Finally, note that spectroscopic observations for 5 other EDisCS fields (1040.7-1155, 1054.4-1146, 1054.7-1245, 1216.8-1201 and 1232.5-1250 ) were presented in a previous paper (Halliday et al., 2004, Cat. J/A+A/427/397) but note that the format of the published data tables for that paper is not fully identical to the format used for this paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419#1</TD>
            <TD>2011-09-14T20:22:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>24-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/482/419</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/419</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/482/419 [2]</TD>
            <TD>ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)</TD>
            <TD>Spectroscopic observations obtained using VLT/FORS2 are presented for objects in 14 survey fields of the ESO Distant Cluster Survey (EDisCS). The fields contain galaxy clusters at z=0.40-0.96. The objects in the catalogues are either galaxies (which can be cluster members or fields galaxies), foreground stars, or objects for which no redshift could be determined. For a 15th field (1122.9-1136) which is part of the paper, no data are published, since very little data was obtained. We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1", spectroscopic redshifts for objects in the 14 fields, and cluster membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively. The 'main' table contains one entry per unique object, and this is the table people normally should use. The 'supp' table contains possible extra redshifts obtained. If an object was observed N times, the best redshift (decided from a number of rules) is put in 'main' and the remaining N-1 redshifts are put in 'supp'. Cl 1238.5-1144 has no data in supp.dat file. The data tables have been prepared so that they can be read both using tools that expect data columns separated by white space (e.g. the UNIX tool awk) and tools that expect things to be at fixed character/byte locations in the file (e.g. the UNIX tool cut). The contents of the data tables are fully described in Sect. 4.3 of the paper (including the sample data in Table 4 in the paper). Some of the salient features are repeated as Notes. Finally, note that spectroscopic observations for 5 other EDisCS fields (1040.7-1155, 1054.4-1146, 1054.7-1245, 1216.8-1201 and 1232.5-1250 ) were presented in a previous paper (Halliday et al., 2004, Cat. J/A+A/427/397) but note that the format of the published data tables for that paper is not fully identical to the format used for this paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419#2</TD>
            <TD>2011-09-14T20:22:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>24-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/482/419&amp;</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/419</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/482/419 [data]</TD>
            <TD>ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)</TD>
            <TD>Spectroscopic observations obtained using VLT/FORS2 are presented for objects in 14 survey fields of the ESO Distant Cluster Survey (EDisCS). The fields contain galaxy clusters at z=0.40-0.96. The objects in the catalogues are either galaxies (which can be cluster members or fields galaxies), foreground stars, or objects for which no redshift could be determined. For a 15th field (1122.9-1136) which is part of the paper, no data are published, since very little data was obtained. We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1", spectroscopic redshifts for objects in the 14 fields, and cluster membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively. The 'main' table contains one entry per unique object, and this is the table people normally should use. The 'supp' table contains possible extra redshifts obtained. If an object was observed N times, the best redshift (decided from a number of rules) is put in 'main' and the remaining N-1 redshifts are put in 'supp'. Cl 1238.5-1144 has no data in supp.dat file. The data tables have been prepared so that they can be read both using tools that expect data columns separated by white space (e.g. the UNIX tool awk) and tools that expect things to be at fixed character/byte locations in the file (e.g. the UNIX tool cut). The contents of the data tables are fully described in Sect. 4.3 of the paper (including the sample data in Table 4 in the paper). Some of the salient features are repeated as Notes. Finally, note that spectroscopic observations for 5 other EDisCS fields (1040.7-1155, 1054.4-1146, 1054.7-1245, 1216.8-1201 and 1232.5-1250 ) were presented in a previous paper (Halliday et al., 2004, Cat. J/A+A/427/397) but note that the format of the published data tables for that paper is not fully identical to the format used for this paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419#data</TD>
            <TD>2011-09-14T20:22:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
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            <TD>24-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/482/419&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/419</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A143 [1]</TD>
            <TD>RX J105453.3+552102 cluster SDSS photometry (Aguerri+, 2011)</TD>
            <TD>Optical imaging of RX J105453.3+552102 was carried out at the 2.5m NOT telescope in March 2008. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143#1</TD>
            <TD>2011-09-18T11:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/527/A143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A143</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A143</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A143 [2]</TD>
            <TD>RX J105453.3+552102 cluster SDSS photometry (Aguerri+, 2011)</TD>
            <TD>Optical imaging of RX J105453.3+552102 was carried out at the 2.5m NOT telescope in March 2008. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143#2</TD>
            <TD>2011-09-18T11:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/527/A143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A143&amp;</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/527/A143 [table1]</TD>
            <TD>RX J105453.3+552102 cluster SDSS photometry (Aguerri+, 2011)</TD>
            <TD>Optical imaging of RX J105453.3+552102 was carried out at the 2.5m NOT telescope in March 2008. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143#table1</TD>
            <TD>2011-09-18T11:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/527/A143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/482/419 [1]</TD>
            <TD>ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)</TD>
            <TD>Spectroscopic observations obtained using VLT/FORS2 are presented for objects in 14 survey fields of the ESO Distant Cluster Survey (EDisCS). The fields contain galaxy clusters at z=0.40-0.96. The objects in the catalogues are either galaxies (which can be cluster members or fields galaxies), foreground stars, or objects for which no redshift could be determined. For a 15th field (1122.9-1136) which is part of the paper, no data are published, since very little data was obtained. We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1", spectroscopic redshifts for objects in the 14 fields, and cluster membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively. The 'main' table contains one entry per unique object, and this is the table people normally should use. The 'supp' table contains possible extra redshifts obtained. If an object was observed N times, the best redshift (decided from a number of rules) is put in 'main' and the remaining N-1 redshifts are put in 'supp'. Cl 1238.5-1144 has no data in supp.dat file. The data tables have been prepared so that they can be read both using tools that expect data columns separated by white space (e.g. the UNIX tool awk) and tools that expect things to be at fixed character/byte locations in the file (e.g. the UNIX tool cut). The contents of the data tables are fully described in Sect. 4.3 of the paper (including the sample data in Table 4 in the paper). Some of the salient features are repeated as Notes. Finally, note that spectroscopic observations for 5 other EDisCS fields (1040.7-1155, 1054.4-1146, 1054.7-1245, 1216.8-1201 and 1232.5-1250 ) were presented in a previous paper (Halliday et al., 2004, Cat. J/A+A/427/397) but note that the format of the published data tables for that paper is not fully identical to the format used for this paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419#1</TD>
            <TD>2011-09-14T20:22:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/482/419</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/419</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/482/419 [2]</TD>
            <TD>ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)</TD>
            <TD>Spectroscopic observations obtained using VLT/FORS2 are presented for objects in 14 survey fields of the ESO Distant Cluster Survey (EDisCS). The fields contain galaxy clusters at z=0.40-0.96. The objects in the catalogues are either galaxies (which can be cluster members or fields galaxies), foreground stars, or objects for which no redshift could be determined. For a 15th field (1122.9-1136) which is part of the paper, no data are published, since very little data was obtained. We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1", spectroscopic redshifts for objects in the 14 fields, and cluster membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively. The 'main' table contains one entry per unique object, and this is the table people normally should use. The 'supp' table contains possible extra redshifts obtained. If an object was observed N times, the best redshift (decided from a number of rules) is put in 'main' and the remaining N-1 redshifts are put in 'supp'. Cl 1238.5-1144 has no data in supp.dat file. The data tables have been prepared so that they can be read both using tools that expect data columns separated by white space (e.g. the UNIX tool awk) and tools that expect things to be at fixed character/byte locations in the file (e.g. the UNIX tool cut). The contents of the data tables are fully described in Sect. 4.3 of the paper (including the sample data in Table 4 in the paper). Some of the salient features are repeated as Notes. Finally, note that spectroscopic observations for 5 other EDisCS fields (1040.7-1155, 1054.4-1146, 1054.7-1245, 1216.8-1201 and 1232.5-1250 ) were presented in a previous paper (Halliday et al., 2004, Cat. J/A+A/427/397) but note that the format of the published data tables for that paper is not fully identical to the format used for this paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419#2</TD>
            <TD>2011-09-14T20:22:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/482/419&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/419</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/482/419 [data]</TD>
            <TD>ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)</TD>
            <TD>Spectroscopic observations obtained using VLT/FORS2 are presented for objects in 14 survey fields of the ESO Distant Cluster Survey (EDisCS). The fields contain galaxy clusters at z=0.40-0.96. The objects in the catalogues are either galaxies (which can be cluster members or fields galaxies), foreground stars, or objects for which no redshift could be determined. For a 15th field (1122.9-1136) which is part of the paper, no data are published, since very little data was obtained. We present tables of RA and DE positions for an equinox of 2000 (J2000, epoch 2001), I-band magnitudes for an aperture of radius 1", spectroscopic redshifts for objects in the 14 fields, and cluster membership and targeting flags to indicate whether the object is a cluster member and/or was targeted to be a cluster member respectively. The 'main' table contains one entry per unique object, and this is the table people normally should use. The 'supp' table contains possible extra redshifts obtained. If an object was observed N times, the best redshift (decided from a number of rules) is put in 'main' and the remaining N-1 redshifts are put in 'supp'. Cl 1238.5-1144 has no data in supp.dat file. The data tables have been prepared so that they can be read both using tools that expect data columns separated by white space (e.g. the UNIX tool awk) and tools that expect things to be at fixed character/byte locations in the file (e.g. the UNIX tool cut). The contents of the data tables are fully described in Sect. 4.3 of the paper (including the sample data in Table 4 in the paper). Some of the salient features are repeated as Notes. Finally, note that spectroscopic observations for 5 other EDisCS fields (1040.7-1155, 1054.4-1146, 1054.7-1245, 1216.8-1201 and 1232.5-1250 ) were presented in a previous paper (Halliday et al., 2004, Cat. J/A+A/427/397) but note that the format of the published data tables for that paper is not fully identical to the format used for this paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419#data</TD>
            <TD>2011-09-14T20:22:29Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/419</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/482/419&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/419</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A143 [1]</TD>
            <TD>RX J105453.3+552102 cluster SDSS photometry (Aguerri+, 2011)</TD>
            <TD>Optical imaging of RX J105453.3+552102 was carried out at the 2.5m NOT telescope in March 2008. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143#1</TD>
            <TD>2011-09-18T11:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A143</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A143</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A143 [2]</TD>
            <TD>RX J105453.3+552102 cluster SDSS photometry (Aguerri+, 2011)</TD>
            <TD>Optical imaging of RX J105453.3+552102 was carried out at the 2.5m NOT telescope in March 2008. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143#2</TD>
            <TD>2011-09-18T11:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A143 [table1]</TD>
            <TD>RX J105453.3+552102 cluster SDSS photometry (Aguerri+, 2011)</TD>
            <TD>Optical imaging of RX J105453.3+552102 was carried out at the 2.5m NOT telescope in March 2008. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143#table1</TD>
            <TD>2011-09-18T11:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A143</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1275 [1]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#1</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1275</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1275 [2]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#2</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1275&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1275 [table3]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#table3</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1275 [table1]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#table1</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A143 [1]</TD>
            <TD>RX J105453.3+552102 cluster SDSS photometry (Aguerri+, 2011)</TD>
            <TD>Optical imaging of RX J105453.3+552102 was carried out at the 2.5m NOT telescope in March 2008. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143#1</TD>
            <TD>2011-09-18T11:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A143</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A143</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A143 [2]</TD>
            <TD>RX J105453.3+552102 cluster SDSS photometry (Aguerri+, 2011)</TD>
            <TD>Optical imaging of RX J105453.3+552102 was carried out at the 2.5m NOT telescope in March 2008. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143#2</TD>
            <TD>2011-09-18T11:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A143 [table1]</TD>
            <TD>RX J105453.3+552102 cluster SDSS photometry (Aguerri+, 2011)</TD>
            <TD>Optical imaging of RX J105453.3+552102 was carried out at the 2.5m NOT telescope in March 2008. Optical deep images were used for studying the properties of the brightest group galaxy and for computing the photometric luminosity function of the group. We have also performed a detail dynamical analysis of the system based on redshift data for 116 galaxies. Combining galaxy velocities and positions we selected 78 group members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143#table1</TD>
            <TD>2011-09-18T11:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A143</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1275 [1]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#1</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1275</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1275 [2]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#2</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1275&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1275 [table3]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#table3</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1275 [table1]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#table1</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/266 [1]</TD>
            <TD>Atlas of Virgo galaxies (McDonald+ 2011)</TD>
            <TD>This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/266#1</TD>
            <TD>2011-10-23T07:25:31Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/VII/266</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/266</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/266</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/266 [2]</TD>
            <TD>Atlas of Virgo galaxies (McDonald+ 2011)</TD>
            <TD>This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/266#2</TD>
            <TD>2011-10-23T07:25:31Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/VII/266</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/266&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/266</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/266 [vcc]</TD>
            <TD>Atlas of Virgo galaxies (McDonald+ 2011)</TD>
            <TD>This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/266#vcc</TD>
            <TD>2011-10-23T07:25:31Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/VII/266</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/266&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/266</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1275 [1]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#1</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1275</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1275 [2]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#2</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1275&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1275 [table3]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#table3</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1275 [table1]</TD>
            <TD>CIRS (Cluster Infall Regions in the SDSS). I. (Rines+, 2006)</TD>
            <TD>We use the Fourth Data Release of the Sloan Digital Sky Survey (SDSS) to test the ubiquity of infall patterns around galaxy clusters and measure cluster mass profiles to large radii. The Cluster and Infall Region Nearby Survey (CAIRNS) found infall patterns in nine clusters, but the cluster sample was incomplete. Here we match X-ray cluster catalogs with SDSS, search for infall patterns, and compute mass profiles for a complete sample of X-ray-selected clusters. Very clean infall patterns are apparent in most of the clusters, with the fraction decreasing with increasing redshift due to shallower sampling. All 72 clusters in a well-defined sample limited by redshift (ensuring good sampling) and X-ray flux (excluding superpositions) show infall patterns sufficient to apply the caustic technique. This sample is by far the largest sample of cluster mass profiles extending to large radii to date. Similar to CAIRNS, cluster infall patterns are better defined in observations than in simulations. Further work is needed to determine the source of this difference. We use the infall patterns to compute mass profiles for 72 clusters and compare them to model profiles. Cluster scaling relations using caustic masses agree well with those using X-ray or virial mass estimates, confirming the reliability of the caustic technique. We confirm the conclusion of CAIRNS that cluster infall regions are well fitted by Navarro-Frenk-White (NFW) and Hernquist profiles and poorly fitted by singular isothermal spheres. This much larger sample enables new comparisons of cluster properties with those in simulations. The shapes (specifically NFW concentrations) of the mass profiles agree well with the predictions of simulations. The mass in the infall region is typically comparable to or larger than that in the virial region. Specifically, the mass inside the turnaround radius is on average 2.19+/-0.18 times that within the virial radius. This ratio agrees well with recent predictions from simulations of the final masses of dark matter halos.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275#table1</TD>
            <TD>2011-09-14T20:24:08Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1275</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/266 [1]</TD>
            <TD>Atlas of Virgo galaxies (McDonald+ 2011)</TD>
            <TD>This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/266#1</TD>
            <TD>2011-10-23T07:25:31Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/VII/266</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/266</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/266</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/266 [2]</TD>
            <TD>Atlas of Virgo galaxies (McDonald+ 2011)</TD>
            <TD>This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/266#2</TD>
            <TD>2011-10-23T07:25:31Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/VII/266</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/266&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/266</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/266 [vcc]</TD>
            <TD>Atlas of Virgo galaxies (McDonald+ 2011)</TD>
            <TD>This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/266#vcc</TD>
            <TD>2011-10-23T07:25:31Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/VII/266</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/266&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/266</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/165/307 [1]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#1</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/165/307</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/165/307 [2]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#2</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/165/307&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/165/307 [sr1]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#sr1</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/165/307&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/165/307 [table2]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#table2</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/165/307&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SFGALHMXB [1]</TD>
            <TD>Star-Forming Galaxies High-Mass X-Ray Binaries Catalog</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L&lt;sub&gt;X&lt;/sub&gt; ~ 2.6 x 10&lt;sup&gt;39&lt;/sup&gt; x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L&lt;sub&gt;X&lt;/sub&gt;) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;40&lt;/sup&gt; erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f&lt;sub&gt;X&lt;/sub&gt; ~ 0.2 x (0.1 Myr/tau&lt;sub&gt;x&lt;/sub&gt;), where tau&lt;sub&gt;x&lt;/sub&gt; is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (&lt;~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sfgalhmxb#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sfgalhmxb</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sfgalhmxb&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/sfgalhmxb.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SFGALHMXB [2]</TD>
            <TD>Star-Forming Galaxies High-Mass X-Ray Binaries Catalog</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L&lt;sub&gt;X&lt;/sub&gt; ~ 2.6 x 10&lt;sup&gt;39&lt;/sup&gt; x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L&lt;sub&gt;X&lt;/sub&gt;) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;40&lt;/sup&gt; erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f&lt;sub&gt;X&lt;/sub&gt; ~ 0.2 x (0.1 Myr/tau&lt;sub&gt;x&lt;/sub&gt;), where tau&lt;sub&gt;x&lt;/sub&gt; is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (&lt;~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sfgalhmxb#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sfgalhmxb</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sfgalhmxb&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/sfgalhmxb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SFGALHMXB [3]</TD>
            <TD>Star-Forming Galaxies High-Mass X-Ray Binaries Catalog</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L&lt;sub&gt;X&lt;/sub&gt; ~ 2.6 x 10&lt;sup&gt;39&lt;/sup&gt; x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L&lt;sub&gt;X&lt;/sub&gt;) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;40&lt;/sup&gt; erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f&lt;sub&gt;X&lt;/sub&gt; ~ 0.2 x (0.1 Myr/tau&lt;sub&gt;x&lt;/sub&gt;), where tau&lt;sub&gt;x&lt;/sub&gt; is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (&lt;~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sfgalhmxb#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sfgalhmxb</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sfgalhmxb&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/sfgalhmxb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/266 [1]</TD>
            <TD>Atlas of Virgo galaxies (McDonald+ 2011)</TD>
            <TD>This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/266#1</TD>
            <TD>2011-10-23T07:25:31Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/VII/266</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/266</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/266</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/266 [2]</TD>
            <TD>Atlas of Virgo galaxies (McDonald+ 2011)</TD>
            <TD>This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/266#2</TD>
            <TD>2011-10-23T07:25:31Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/VII/266</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/266&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/266</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/266 [vcc]</TD>
            <TD>Atlas of Virgo galaxies (McDonald+ 2011)</TD>
            <TD>This database contains surface brightness profiles in the optical g, r, i, z bands and near-IR H-band for 286 Virgo cluster galaxies. This morphologically-complete sample spans a huge range in galaxy size, luminosity, surface brightness and stellar populations. These data have been used to study the luminosity and surface brightness distribution of Virgo cluster galaxies, in McDonald et al. (2009MNRAS.394.2022M). We find compelling evidence for bimodal populations in surface brightness, with both early- and late-type galaxies having a dearth of intermediate surface brightness galaxies. Most convincing is our confirmation of the result by Tully and Verheijen that the surface brightness of galaxy disks are strongly bimodal (1997ApJ...484..145T) The near-IR H-band data have been obtained from a variety of telescopes. We downloaded archival images for 31/286 and 84/286 bright galaxies from the 2MASS and GOLDMine online databases, respectively. The remaining 171 galaxies have new observations from the UH 2.2-m (130/286), CFHT (20/286) and UKIRT (21/286) telescopes. These data were all reduced in a homogeneous way, as outlined in our data paper. The optical g, r, i, z data were all obtained from the SDSS archives. Surface brightness profiles were extracted homogeneously from the optical and near-IR data following similar procedures, as outlined in our paper (2011MNRAS.414.2055M) The parametric and non-parametric parameters from bulge-disk decompositions of 285 optical griz and near-IR H-band surface brightness (SB) profiles are given in the bdd_* files in this directory. The profiles are stored in the "prof_g", "prof_r", "prof_i", "prof_z" and "prof_h" subdirectories, one for each color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/266#vcc</TD>
            <TD>2011-10-23T07:25:31Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/VII/266</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/266&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/266</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/165/307 [1]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#1</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/165/307</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/165/307 [2]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#2</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/165/307&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/165/307 [sr1]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#sr1</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/165/307&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/165/307 [table2]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#table2</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/165/307&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SFGALHMXB [1]</TD>
            <TD>Star-Forming Galaxies High-Mass X-Ray Binaries Catalog</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L&lt;sub&gt;X&lt;/sub&gt; ~ 2.6 x 10&lt;sup&gt;39&lt;/sup&gt; x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L&lt;sub&gt;X&lt;/sub&gt;) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;40&lt;/sup&gt; erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f&lt;sub&gt;X&lt;/sub&gt; ~ 0.2 x (0.1 Myr/tau&lt;sub&gt;x&lt;/sub&gt;), where tau&lt;sub&gt;x&lt;/sub&gt; is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (&lt;~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sfgalhmxb#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sfgalhmxb</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sfgalhmxb&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/sfgalhmxb.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SFGALHMXB [2]</TD>
            <TD>Star-Forming Galaxies High-Mass X-Ray Binaries Catalog</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L&lt;sub&gt;X&lt;/sub&gt; ~ 2.6 x 10&lt;sup&gt;39&lt;/sup&gt; x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L&lt;sub&gt;X&lt;/sub&gt;) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;40&lt;/sup&gt; erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f&lt;sub&gt;X&lt;/sub&gt; ~ 0.2 x (0.1 Myr/tau&lt;sub&gt;x&lt;/sub&gt;), where tau&lt;sub&gt;x&lt;/sub&gt; is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (&lt;~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sfgalhmxb#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sfgalhmxb</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sfgalhmxb&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/sfgalhmxb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SFGALHMXB [3]</TD>
            <TD>Star-Forming Galaxies High-Mass X-Ray Binaries Catalog</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L&lt;sub&gt;X&lt;/sub&gt; ~ 2.6 x 10&lt;sup&gt;39&lt;/sup&gt; x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L&lt;sub&gt;X&lt;/sub&gt;) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;40&lt;/sup&gt; erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f&lt;sub&gt;X&lt;/sub&gt; ~ 0.2 x (0.1 Myr/tau&lt;sub&gt;x&lt;/sub&gt;), where tau&lt;sub&gt;x&lt;/sub&gt; is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (&lt;~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sfgalhmxb#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sfgalhmxb</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sfgalhmxb&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/sfgalhmxb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/165/307 [1]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#1</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/165/307</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/165/307 [2]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#2</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/165/307&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/165/307 [sr1]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#sr1</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/165/307&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/165/307 [table2]</TD>
            <TD>Survey for ionization in neutral gas galaxies. I. (Meurer+, 2006)</TD>
            <TD>We introduce the Survey for Ionization in Neutral Gas Galaxies (SINGG), a census of star formation in HI-selected galaxies. The survey consists of H{alpha} and R-band imaging of a sample of 468 galaxies selected from the HI Parkes All Sky Survey (HIPASS). The sample spans three decades in HI mass and is free of many of the biases that affect other star-forming galaxy samples. We present the criteria for sample selection, list the entire sample, discuss our observational techniques, and describe the data reduction and calibration methods. This paper focuses on 93 SINGG targets whose observations have been fully reduced and analyzed to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307#table2</TD>
            <TD>2011-09-14T20:24:09Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/307</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/165/307&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/307</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SFGALHMXB [1]</TD>
            <TD>Star-Forming Galaxies High-Mass X-Ray Binaries Catalog</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L&lt;sub&gt;X&lt;/sub&gt; ~ 2.6 x 10&lt;sup&gt;39&lt;/sup&gt; x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L&lt;sub&gt;X&lt;/sub&gt;) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;40&lt;/sup&gt; erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f&lt;sub&gt;X&lt;/sub&gt; ~ 0.2 x (0.1 Myr/tau&lt;sub&gt;x&lt;/sub&gt;), where tau&lt;sub&gt;x&lt;/sub&gt; is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (&lt;~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sfgalhmxb#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sfgalhmxb</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sfgalhmxb&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/sfgalhmxb.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SFGALHMXB [2]</TD>
            <TD>Star-Forming Galaxies High-Mass X-Ray Binaries Catalog</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L&lt;sub&gt;X&lt;/sub&gt; ~ 2.6 x 10&lt;sup&gt;39&lt;/sup&gt; x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L&lt;sub&gt;X&lt;/sub&gt;) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;40&lt;/sup&gt; erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f&lt;sub&gt;X&lt;/sub&gt; ~ 0.2 x (0.1 Myr/tau&lt;sub&gt;x&lt;/sub&gt;), where tau&lt;sub&gt;x&lt;/sub&gt; is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (&lt;~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sfgalhmxb#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sfgalhmxb</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sfgalhmxb&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/sfgalhmxb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SFGALHMXB [3]</TD>
            <TD>Star-Forming Galaxies High-Mass X-Ray Binaries Catalog</TD>
            <TD>Based on a homogeneous set of X-ray, infrared and ultraviolet observations from Chandra, Spitzer, GALEX and 2MASS archives, the authors studied populations of high-mass X-ray binaries (HMXBs) in a sample of 29 nearby star-forming galaxies and their relation with the star formation rate (SFR). In agreement with previous results, the authors find that HMXBs are a good tracer of the recent star formation activity in the host galaxy and their collective luminosity and number scale with the SFR, in particular, L&lt;sub&gt;X&lt;/sub&gt; ~ 2.6 x 10&lt;sup&gt;39&lt;/sup&gt; x SFR. However, the scaling relations still bear a rather large dispersion of rms ~ 0.4 dex, which the authors believe is of a physical origin. This table contains the catalog of 1055 compact X-ray sources detected within the D25 ellipse for galaxies of this sample which the authors used to construct the average X-ray luminosity function (XLF) of HMXBs with substantially improved statistical accuracy and better control of systematic effects than achieved in previous studies. The XLF follows a power law with slope of 1.6 in the log(L&lt;sub&gt;X&lt;/sub&gt;) ~ 35 - 40 luminosity range with a moderately significant evidence for a break or cut-off at L&lt;sub&gt;X&lt;/sub&gt; ~ 10&lt;sup&gt;40&lt;/sup&gt; erg/s. As before, the authors did not find any features at the Eddington limit for a neutron star or a stellar mass black hole. In their paper, the authors discuss the implications of their results for the theory of binary evolution. In particular, they estimate the fraction of compact objects that once during their lifetime experienced an X-ray active phase powered by accretion from a high mass companion and obtain a rather large number, f&lt;sub&gt;X&lt;/sub&gt; ~ 0.2 x (0.1 Myr/tau&lt;sub&gt;x&lt;/sub&gt;), where tau&lt;sub&gt;x&lt;/sub&gt; is the life time of the X-ray active phase. This is about 4 orders of magnitude more frequent than in low-mass X-ray binaries (LMXBs). The authors also derive constrains on the mass distribution of the secondary star in HMXBs. Note that, in their paper, the authors estimate that ~ 300 of the 1055 sources are likely to be background AGNs (cosmic X-ray background or CXB sources) and that the majority (&lt;~ 700) of the remaining ~ 750 sources are young HMXB systems associated with star formation in their host galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sfgalhmxb#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sfgalhmxb</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sfgalhmxb&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/sfgalhmxb.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/37/281 [1]</TD>
            <TD>Galactic rotation curve from selected maser (Stepanishechev+ 2011)</TD>
            <TD>Based on currently available observations of 28 maser sources in 25 star-forming regions with measured trigonometric parallaxes, proper motions, and radial velocities, we have constructed the rotation curve of the Galaxy. Taking different distances to the Galactic center R_0_, we have estimated the peculiar velocity of the Sun, the angular velocity of Galactic rotation, and its three derivatives.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281#1</TD>
            <TD>2011-05-27T11:08:21Z</TD>
            <TD>#Galaxies#HII_regions#Masers#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/37/281</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/37/281</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/37/281 [2]</TD>
            <TD>Galactic rotation curve from selected maser (Stepanishechev+ 2011)</TD>
            <TD>Based on currently available observations of 28 maser sources in 25 star-forming regions with measured trigonometric parallaxes, proper motions, and radial velocities, we have constructed the rotation curve of the Galaxy. Taking different distances to the Galactic center R_0_, we have estimated the peculiar velocity of the Sun, the angular velocity of Galactic rotation, and its three derivatives.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281#2</TD>
            <TD>2011-05-27T11:08:21Z</TD>
            <TD>#Galaxies#HII_regions#Masers#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/37/281&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/37/281</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/37/281 [masers]</TD>
            <TD>Galactic rotation curve from selected maser (Stepanishechev+ 2011)</TD>
            <TD>Based on currently available observations of 28 maser sources in 25 star-forming regions with measured trigonometric parallaxes, proper motions, and radial velocities, we have constructed the rotation curve of the Galaxy. Taking different distances to the Galactic center R_0_, we have estimated the peculiar velocity of the Sun, the angular velocity of Galactic rotation, and its three derivatives.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281#masers</TD>
            <TD>2011-05-27T11:08:21Z</TD>
            <TD>#Galaxies#HII_regions#Masers#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/37/281&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/37/281</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/384/943 [1]</TD>
            <TD>Velocities of NGC 1023 planetary nebulae (Noordermeer+, 2008)</TD>
            <TD>We investigate the manner in which lenticular galaxies are formed by studying their stellar kinematics: an S0 formed from a fading spiral galaxy should display similar cold outer disc kinematics to its progenitor, while an S0 formed in a minor merger should be more dominated by random motions. In a pilot study to attempt to distinguish between these scenarios, we have measured the planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the Planetary Nebula Spectrograph, we have detected and measured the line-of-sight velocities of 204 candidate PNe in the field of this galaxy. Out to intermediate radii, the system displays the kinematics of a normal rotationally-supported disc system. After correction of its rotational velocities for asymmetric drift, the galaxy lies just below the spiral galaxy Tully-Fisher relation, as one would expect for a fading system. However, at larger radii the kinematics undergo a gradual but major transition to random motion with little rotation. This transition does not seem to reflect a change in the viewing geometry or the presence of a distinct halo component, since the number counts of PNe follow the same simple exponential decline as the stellar continuum with the same projected disc ellipticity out to large radii. The galaxy's small companion, NGC 1023A, does not seem to be large enough to have caused the observed modification either. This combination of properties would seem to indicate a complex evolutionary history in either the transition to form an S0 or in the past life of the spiral galaxy from which the S0 formed. More data sets of this type from both spirals and S0s are needed in order to definitively determine the relationship between these types of system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943#1</TD>
            <TD>2011-09-14T20:26:32Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/384/943</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/943</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/384/943 [2]</TD>
            <TD>Velocities of NGC 1023 planetary nebulae (Noordermeer+, 2008)</TD>
            <TD>We investigate the manner in which lenticular galaxies are formed by studying their stellar kinematics: an S0 formed from a fading spiral galaxy should display similar cold outer disc kinematics to its progenitor, while an S0 formed in a minor merger should be more dominated by random motions. In a pilot study to attempt to distinguish between these scenarios, we have measured the planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the Planetary Nebula Spectrograph, we have detected and measured the line-of-sight velocities of 204 candidate PNe in the field of this galaxy. Out to intermediate radii, the system displays the kinematics of a normal rotationally-supported disc system. After correction of its rotational velocities for asymmetric drift, the galaxy lies just below the spiral galaxy Tully-Fisher relation, as one would expect for a fading system. However, at larger radii the kinematics undergo a gradual but major transition to random motion with little rotation. This transition does not seem to reflect a change in the viewing geometry or the presence of a distinct halo component, since the number counts of PNe follow the same simple exponential decline as the stellar continuum with the same projected disc ellipticity out to large radii. The galaxy's small companion, NGC 1023A, does not seem to be large enough to have caused the observed modification either. This combination of properties would seem to indicate a complex evolutionary history in either the transition to form an S0 or in the past life of the spiral galaxy from which the S0 formed. More data sets of this type from both spirals and S0s are needed in order to definitively determine the relationship between these types of system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943#2</TD>
            <TD>2011-09-14T20:26:32Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/384/943&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/943</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/384/943 [table2]</TD>
            <TD>Velocities of NGC 1023 planetary nebulae (Noordermeer+, 2008)</TD>
            <TD>We investigate the manner in which lenticular galaxies are formed by studying their stellar kinematics: an S0 formed from a fading spiral galaxy should display similar cold outer disc kinematics to its progenitor, while an S0 formed in a minor merger should be more dominated by random motions. In a pilot study to attempt to distinguish between these scenarios, we have measured the planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the Planetary Nebula Spectrograph, we have detected and measured the line-of-sight velocities of 204 candidate PNe in the field of this galaxy. Out to intermediate radii, the system displays the kinematics of a normal rotationally-supported disc system. After correction of its rotational velocities for asymmetric drift, the galaxy lies just below the spiral galaxy Tully-Fisher relation, as one would expect for a fading system. However, at larger radii the kinematics undergo a gradual but major transition to random motion with little rotation. This transition does not seem to reflect a change in the viewing geometry or the presence of a distinct halo component, since the number counts of PNe follow the same simple exponential decline as the stellar continuum with the same projected disc ellipticity out to large radii. The galaxy's small companion, NGC 1023A, does not seem to be large enough to have caused the observed modification either. This combination of properties would seem to indicate a complex evolutionary history in either the transition to form an S0 or in the past life of the spiral galaxy from which the S0 formed. More data sets of this type from both spirals and S0s are needed in order to definitively determine the relationship between these types of system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943#table2</TD>
            <TD>2011-09-14T20:26:32Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/384/943&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/943</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>TWOMASSRSC [1]</TD>
            <TD>2MASS Redshift Survey (2MRS) Catalog</TD>
            <TD>This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and |b| &gt;= 5 degrees (&gt;= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.25 mag and |b| &gt;= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: &lt;pre&gt; K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and detected at H, E(B - V) &lt;= 1 mag, |b| &gt;= 5 degrees for 30 degrees &lt; l &lt; 330 degrees, |b| &gt;= 8 degrees otherwise. &lt;/pre&gt; They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/twomassrsc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/twomassrsc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=twomassrsc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/twomassrsc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>TWOMASSRSC [2]</TD>
            <TD>2MASS Redshift Survey (2MRS) Catalog</TD>
            <TD>This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and |b| &gt;= 5 degrees (&gt;= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.25 mag and |b| &gt;= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: &lt;pre&gt; K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and detected at H, E(B - V) &lt;= 1 mag, |b| &gt;= 5 degrees for 30 degrees &lt; l &lt; 330 degrees, |b| &gt;= 8 degrees otherwise. &lt;/pre&gt; They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/twomassrsc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/twomassrsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=twomassrsc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/twomassrsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>TWOMASSRSC [3]</TD>
            <TD>2MASS Redshift Survey (2MRS) Catalog</TD>
            <TD>This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and |b| &gt;= 5 degrees (&gt;= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.25 mag and |b| &gt;= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: &lt;pre&gt; K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and detected at H, E(B - V) &lt;= 1 mag, |b| &gt;= 5 degrees for 30 degrees &lt; l &lt; 330 degrees, |b| &gt;= 8 degrees otherwise. &lt;/pre&gt; They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/twomassrsc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/twomassrsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_twomassrsc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/twomassrsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/37/281 [1]</TD>
            <TD>Galactic rotation curve from selected maser (Stepanishechev+ 2011)</TD>
            <TD>Based on currently available observations of 28 maser sources in 25 star-forming regions with measured trigonometric parallaxes, proper motions, and radial velocities, we have constructed the rotation curve of the Galaxy. Taking different distances to the Galactic center R_0_, we have estimated the peculiar velocity of the Sun, the angular velocity of Galactic rotation, and its three derivatives.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281#1</TD>
            <TD>2011-05-27T11:08:21Z</TD>
            <TD>#Galaxies#HII_regions#Masers#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/37/281</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/37/281</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/37/281 [2]</TD>
            <TD>Galactic rotation curve from selected maser (Stepanishechev+ 2011)</TD>
            <TD>Based on currently available observations of 28 maser sources in 25 star-forming regions with measured trigonometric parallaxes, proper motions, and radial velocities, we have constructed the rotation curve of the Galaxy. Taking different distances to the Galactic center R_0_, we have estimated the peculiar velocity of the Sun, the angular velocity of Galactic rotation, and its three derivatives.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281#2</TD>
            <TD>2011-05-27T11:08:21Z</TD>
            <TD>#Galaxies#HII_regions#Masers#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/37/281&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/37/281</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/37/281 [masers]</TD>
            <TD>Galactic rotation curve from selected maser (Stepanishechev+ 2011)</TD>
            <TD>Based on currently available observations of 28 maser sources in 25 star-forming regions with measured trigonometric parallaxes, proper motions, and radial velocities, we have constructed the rotation curve of the Galaxy. Taking different distances to the Galactic center R_0_, we have estimated the peculiar velocity of the Sun, the angular velocity of Galactic rotation, and its three derivatives.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281#masers</TD>
            <TD>2011-05-27T11:08:21Z</TD>
            <TD>#Galaxies#HII_regions#Masers#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/37/281&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/37/281</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/384/943 [1]</TD>
            <TD>Velocities of NGC 1023 planetary nebulae (Noordermeer+, 2008)</TD>
            <TD>We investigate the manner in which lenticular galaxies are formed by studying their stellar kinematics: an S0 formed from a fading spiral galaxy should display similar cold outer disc kinematics to its progenitor, while an S0 formed in a minor merger should be more dominated by random motions. In a pilot study to attempt to distinguish between these scenarios, we have measured the planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the Planetary Nebula Spectrograph, we have detected and measured the line-of-sight velocities of 204 candidate PNe in the field of this galaxy. Out to intermediate radii, the system displays the kinematics of a normal rotationally-supported disc system. After correction of its rotational velocities for asymmetric drift, the galaxy lies just below the spiral galaxy Tully-Fisher relation, as one would expect for a fading system. However, at larger radii the kinematics undergo a gradual but major transition to random motion with little rotation. This transition does not seem to reflect a change in the viewing geometry or the presence of a distinct halo component, since the number counts of PNe follow the same simple exponential decline as the stellar continuum with the same projected disc ellipticity out to large radii. The galaxy's small companion, NGC 1023A, does not seem to be large enough to have caused the observed modification either. This combination of properties would seem to indicate a complex evolutionary history in either the transition to form an S0 or in the past life of the spiral galaxy from which the S0 formed. More data sets of this type from both spirals and S0s are needed in order to definitively determine the relationship between these types of system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943#1</TD>
            <TD>2011-09-14T20:26:32Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/384/943</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/943</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/384/943 [2]</TD>
            <TD>Velocities of NGC 1023 planetary nebulae (Noordermeer+, 2008)</TD>
            <TD>We investigate the manner in which lenticular galaxies are formed by studying their stellar kinematics: an S0 formed from a fading spiral galaxy should display similar cold outer disc kinematics to its progenitor, while an S0 formed in a minor merger should be more dominated by random motions. In a pilot study to attempt to distinguish between these scenarios, we have measured the planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the Planetary Nebula Spectrograph, we have detected and measured the line-of-sight velocities of 204 candidate PNe in the field of this galaxy. Out to intermediate radii, the system displays the kinematics of a normal rotationally-supported disc system. After correction of its rotational velocities for asymmetric drift, the galaxy lies just below the spiral galaxy Tully-Fisher relation, as one would expect for a fading system. However, at larger radii the kinematics undergo a gradual but major transition to random motion with little rotation. This transition does not seem to reflect a change in the viewing geometry or the presence of a distinct halo component, since the number counts of PNe follow the same simple exponential decline as the stellar continuum with the same projected disc ellipticity out to large radii. The galaxy's small companion, NGC 1023A, does not seem to be large enough to have caused the observed modification either. This combination of properties would seem to indicate a complex evolutionary history in either the transition to form an S0 or in the past life of the spiral galaxy from which the S0 formed. More data sets of this type from both spirals and S0s are needed in order to definitively determine the relationship between these types of system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943#2</TD>
            <TD>2011-09-14T20:26:32Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/384/943&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/943</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/384/943 [table2]</TD>
            <TD>Velocities of NGC 1023 planetary nebulae (Noordermeer+, 2008)</TD>
            <TD>We investigate the manner in which lenticular galaxies are formed by studying their stellar kinematics: an S0 formed from a fading spiral galaxy should display similar cold outer disc kinematics to its progenitor, while an S0 formed in a minor merger should be more dominated by random motions. In a pilot study to attempt to distinguish between these scenarios, we have measured the planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the Planetary Nebula Spectrograph, we have detected and measured the line-of-sight velocities of 204 candidate PNe in the field of this galaxy. Out to intermediate radii, the system displays the kinematics of a normal rotationally-supported disc system. After correction of its rotational velocities for asymmetric drift, the galaxy lies just below the spiral galaxy Tully-Fisher relation, as one would expect for a fading system. However, at larger radii the kinematics undergo a gradual but major transition to random motion with little rotation. This transition does not seem to reflect a change in the viewing geometry or the presence of a distinct halo component, since the number counts of PNe follow the same simple exponential decline as the stellar continuum with the same projected disc ellipticity out to large radii. The galaxy's small companion, NGC 1023A, does not seem to be large enough to have caused the observed modification either. This combination of properties would seem to indicate a complex evolutionary history in either the transition to form an S0 or in the past life of the spiral galaxy from which the S0 formed. More data sets of this type from both spirals and S0s are needed in order to definitively determine the relationship between these types of system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943#table2</TD>
            <TD>2011-09-14T20:26:32Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/384/943&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/943</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>TWOMASSRSC [1]</TD>
            <TD>2MASS Redshift Survey (2MRS) Catalog</TD>
            <TD>This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and |b| &gt;= 5 degrees (&gt;= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.25 mag and |b| &gt;= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: &lt;pre&gt; K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and detected at H, E(B - V) &lt;= 1 mag, |b| &gt;= 5 degrees for 30 degrees &lt; l &lt; 330 degrees, |b| &gt;= 8 degrees otherwise. &lt;/pre&gt; They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/twomassrsc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/twomassrsc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=twomassrsc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/twomassrsc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>TWOMASSRSC [2]</TD>
            <TD>2MASS Redshift Survey (2MRS) Catalog</TD>
            <TD>This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and |b| &gt;= 5 degrees (&gt;= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.25 mag and |b| &gt;= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: &lt;pre&gt; K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and detected at H, E(B - V) &lt;= 1 mag, |b| &gt;= 5 degrees for 30 degrees &lt; l &lt; 330 degrees, |b| &gt;= 8 degrees otherwise. &lt;/pre&gt; They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/twomassrsc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/twomassrsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=twomassrsc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/twomassrsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>TWOMASSRSC [3]</TD>
            <TD>2MASS Redshift Survey (2MRS) Catalog</TD>
            <TD>This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and |b| &gt;= 5 degrees (&gt;= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.25 mag and |b| &gt;= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: &lt;pre&gt; K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and detected at H, E(B - V) &lt;= 1 mag, |b| &gt;= 5 degrees for 30 degrees &lt; l &lt; 330 degrees, |b| &gt;= 8 degrees otherwise. &lt;/pre&gt; They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/twomassrsc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/twomassrsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_twomassrsc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/twomassrsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/384/943 [1]</TD>
            <TD>Velocities of NGC 1023 planetary nebulae (Noordermeer+, 2008)</TD>
            <TD>We investigate the manner in which lenticular galaxies are formed by studying their stellar kinematics: an S0 formed from a fading spiral galaxy should display similar cold outer disc kinematics to its progenitor, while an S0 formed in a minor merger should be more dominated by random motions. In a pilot study to attempt to distinguish between these scenarios, we have measured the planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the Planetary Nebula Spectrograph, we have detected and measured the line-of-sight velocities of 204 candidate PNe in the field of this galaxy. Out to intermediate radii, the system displays the kinematics of a normal rotationally-supported disc system. After correction of its rotational velocities for asymmetric drift, the galaxy lies just below the spiral galaxy Tully-Fisher relation, as one would expect for a fading system. However, at larger radii the kinematics undergo a gradual but major transition to random motion with little rotation. This transition does not seem to reflect a change in the viewing geometry or the presence of a distinct halo component, since the number counts of PNe follow the same simple exponential decline as the stellar continuum with the same projected disc ellipticity out to large radii. The galaxy's small companion, NGC 1023A, does not seem to be large enough to have caused the observed modification either. This combination of properties would seem to indicate a complex evolutionary history in either the transition to form an S0 or in the past life of the spiral galaxy from which the S0 formed. More data sets of this type from both spirals and S0s are needed in order to definitively determine the relationship between these types of system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943#1</TD>
            <TD>2011-09-14T20:26:32Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/384/943</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/943</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/384/943 [2]</TD>
            <TD>Velocities of NGC 1023 planetary nebulae (Noordermeer+, 2008)</TD>
            <TD>We investigate the manner in which lenticular galaxies are formed by studying their stellar kinematics: an S0 formed from a fading spiral galaxy should display similar cold outer disc kinematics to its progenitor, while an S0 formed in a minor merger should be more dominated by random motions. In a pilot study to attempt to distinguish between these scenarios, we have measured the planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the Planetary Nebula Spectrograph, we have detected and measured the line-of-sight velocities of 204 candidate PNe in the field of this galaxy. Out to intermediate radii, the system displays the kinematics of a normal rotationally-supported disc system. After correction of its rotational velocities for asymmetric drift, the galaxy lies just below the spiral galaxy Tully-Fisher relation, as one would expect for a fading system. However, at larger radii the kinematics undergo a gradual but major transition to random motion with little rotation. This transition does not seem to reflect a change in the viewing geometry or the presence of a distinct halo component, since the number counts of PNe follow the same simple exponential decline as the stellar continuum with the same projected disc ellipticity out to large radii. The galaxy's small companion, NGC 1023A, does not seem to be large enough to have caused the observed modification either. This combination of properties would seem to indicate a complex evolutionary history in either the transition to form an S0 or in the past life of the spiral galaxy from which the S0 formed. More data sets of this type from both spirals and S0s are needed in order to definitively determine the relationship between these types of system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943#2</TD>
            <TD>2011-09-14T20:26:32Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/384/943&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/943</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/384/943 [table2]</TD>
            <TD>Velocities of NGC 1023 planetary nebulae (Noordermeer+, 2008)</TD>
            <TD>We investigate the manner in which lenticular galaxies are formed by studying their stellar kinematics: an S0 formed from a fading spiral galaxy should display similar cold outer disc kinematics to its progenitor, while an S0 formed in a minor merger should be more dominated by random motions. In a pilot study to attempt to distinguish between these scenarios, we have measured the planetary nebula (PN) kinematics of the nearby S0 system NGC 1023. Using the Planetary Nebula Spectrograph, we have detected and measured the line-of-sight velocities of 204 candidate PNe in the field of this galaxy. Out to intermediate radii, the system displays the kinematics of a normal rotationally-supported disc system. After correction of its rotational velocities for asymmetric drift, the galaxy lies just below the spiral galaxy Tully-Fisher relation, as one would expect for a fading system. However, at larger radii the kinematics undergo a gradual but major transition to random motion with little rotation. This transition does not seem to reflect a change in the viewing geometry or the presence of a distinct halo component, since the number counts of PNe follow the same simple exponential decline as the stellar continuum with the same projected disc ellipticity out to large radii. The galaxy's small companion, NGC 1023A, does not seem to be large enough to have caused the observed modification either. This combination of properties would seem to indicate a complex evolutionary history in either the transition to form an S0 or in the past life of the spiral galaxy from which the S0 formed. More data sets of this type from both spirals and S0s are needed in order to definitively determine the relationship between these types of system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943#table2</TD>
            <TD>2011-09-14T20:26:32Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/384/943</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/384/943&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/384/943</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/37/281 [1]</TD>
            <TD>Galactic rotation curve from selected maser (Stepanishechev+ 2011)</TD>
            <TD>Based on currently available observations of 28 maser sources in 25 star-forming regions with measured trigonometric parallaxes, proper motions, and radial velocities, we have constructed the rotation curve of the Galaxy. Taking different distances to the Galactic center R_0_, we have estimated the peculiar velocity of the Sun, the angular velocity of Galactic rotation, and its three derivatives.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281#1</TD>
            <TD>2011-05-27T11:08:21Z</TD>
            <TD>#Galaxies#HII_regions#Masers#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/37/281</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/37/281</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/37/281 [2]</TD>
            <TD>Galactic rotation curve from selected maser (Stepanishechev+ 2011)</TD>
            <TD>Based on currently available observations of 28 maser sources in 25 star-forming regions with measured trigonometric parallaxes, proper motions, and radial velocities, we have constructed the rotation curve of the Galaxy. Taking different distances to the Galactic center R_0_, we have estimated the peculiar velocity of the Sun, the angular velocity of Galactic rotation, and its three derivatives.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281#2</TD>
            <TD>2011-05-27T11:08:21Z</TD>
            <TD>#Galaxies#HII_regions#Masers#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/37/281&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/37/281</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/37/281 [masers]</TD>
            <TD>Galactic rotation curve from selected maser (Stepanishechev+ 2011)</TD>
            <TD>Based on currently available observations of 28 maser sources in 25 star-forming regions with measured trigonometric parallaxes, proper motions, and radial velocities, we have constructed the rotation curve of the Galaxy. Taking different distances to the Galactic center R_0_, we have estimated the peculiar velocity of the Sun, the angular velocity of Galactic rotation, and its three derivatives.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281#masers</TD>
            <TD>2011-05-27T11:08:21Z</TD>
            <TD>#Galaxies#HII_regions#Masers#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/37/281</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/37/281&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/37/281</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/451/881 [1]</TD>
            <TD>ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)</TD>
            <TD>The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881#1</TD>
            <TD>2011-09-14T20:27:23Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/451/881</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/451/881</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/451/881 [2]</TD>
            <TD>ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)</TD>
            <TD>The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881#2</TD>
            <TD>2011-09-14T20:27:23Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/451/881&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/451/881</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/451/881 [esisbvr]</TD>
            <TD>ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)</TD>
            <TD>The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881#esisbvr</TD>
            <TD>2011-09-14T20:27:23Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/451/881&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/451/881</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/407/2399 [1]</TD>
            <TD>AGN activity and black hole mass (McKernan+, 2010)</TD>
            <TD>We investigate the role of host galaxy classification and black hole mass (MBH) in a heterogeneous sample of 276 mostly nearby (z&lt;0.1) X-ray and IR-selected active galactic nuclei (AGN).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399#1</TD>
            <TD>2011-05-29T17:47:45Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/407/2399</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/407/2399 [2]</TD>
            <TD>AGN activity and black hole mass (McKernan+, 2010)</TD>
            <TD>We investigate the role of host galaxy classification and black hole mass (MBH) in a heterogeneous sample of 276 mostly nearby (z&lt;0.1) X-ray and IR-selected active galactic nuclei (AGN).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399#2</TD>
            <TD>2011-05-29T17:47:45Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/407/2399&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/407/2399 [table1]</TD>
            <TD>AGN activity and black hole mass (McKernan+, 2010)</TD>
            <TD>We investigate the role of host galaxy classification and black hole mass (MBH) in a heterogeneous sample of 276 mostly nearby (z&lt;0.1) X-ray and IR-selected active galactic nuclei (AGN).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399#table1</TD>
            <TD>2011-05-29T17:47:45Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/407/2399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2399</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/451/881 [1]</TD>
            <TD>ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)</TD>
            <TD>The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881#1</TD>
            <TD>2011-09-14T20:27:23Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/451/881</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/451/881</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/451/881 [2]</TD>
            <TD>ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)</TD>
            <TD>The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881#2</TD>
            <TD>2011-09-14T20:27:23Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/451/881&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/451/881</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/451/881 [esisbvr]</TD>
            <TD>ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)</TD>
            <TD>The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881#esisbvr</TD>
            <TD>2011-09-14T20:27:23Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/451/881&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/451/881</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/407/2399 [1]</TD>
            <TD>AGN activity and black hole mass (McKernan+, 2010)</TD>
            <TD>We investigate the role of host galaxy classification and black hole mass (MBH) in a heterogeneous sample of 276 mostly nearby (z&lt;0.1) X-ray and IR-selected active galactic nuclei (AGN).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399#1</TD>
            <TD>2011-05-29T17:47:45Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/407/2399</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/407/2399 [2]</TD>
            <TD>AGN activity and black hole mass (McKernan+, 2010)</TD>
            <TD>We investigate the role of host galaxy classification and black hole mass (MBH) in a heterogeneous sample of 276 mostly nearby (z&lt;0.1) X-ray and IR-selected active galactic nuclei (AGN).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399#2</TD>
            <TD>2011-05-29T17:47:45Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/407/2399&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/407/2399 [table1]</TD>
            <TD>AGN activity and black hole mass (McKernan+, 2010)</TD>
            <TD>We investigate the role of host galaxy classification and black hole mass (MBH) in a heterogeneous sample of 276 mostly nearby (z&lt;0.1) X-ray and IR-selected active galactic nuclei (AGN).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399#table1</TD>
            <TD>2011-05-29T17:47:45Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/407/2399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2399</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/451/881 [1]</TD>
            <TD>ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)</TD>
            <TD>The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881#1</TD>
            <TD>2011-09-14T20:27:23Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/451/881</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/451/881</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/451/881 [2]</TD>
            <TD>ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)</TD>
            <TD>The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881#2</TD>
            <TD>2011-09-14T20:27:23Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/451/881&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/451/881</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/451/881 [esisbvr]</TD>
            <TD>ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)</TD>
            <TD>The ESO-Spitzer extragalactic Imaging Survey (ESIS) is the optical follow up of the Spitzer Wide-Area InfraRed Extragalactic (SWIRE) survey in the ELAIS-S1 area. The multiwavelength study of galaxy emission is the key to understand the interplay of the various components of galaxies and to trace their role in cosmic evolution. ESIS provides optical identification and colors of Spitzer IR galaxies and builds the bases for photometric redshift estimates. This paper presents B, V, R Wide Field Imager observations of the first 1.5 square degree of the ESIS survey. Data reduction includes astrometric calibration, illumination and color corrections. Synthetic sources are simulated in scientific and super-sky-flat images, with the purpose of estimating completeness and photometric accuracy for the survey. Number counts and color distributions are compared to literature observational and theoretical data, including non-evolutionary, PLE, evolutionary and semi-analytic Lambda-CDM galaxy models, as well as Milky Way stellar predictions. Object coordinates are defined with an accuracy as good as ~0.15" rms with respect to GSC 2.2; flux uncertainties are ~2, 10, 20% at mag. 20, 23, 24 respectively (Vega); we reach 95% completeness at B, V~25 and R~24.5. ESIS galaxy number counts are in good agreement with previous works and are best reproduced by evolutionary and hierarchical Lambda-CDM scenarios.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881#esisbvr</TD>
            <TD>2011-09-14T20:27:23Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/451/881</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/451/881&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/451/881</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/407/2399 [1]</TD>
            <TD>AGN activity and black hole mass (McKernan+, 2010)</TD>
            <TD>We investigate the role of host galaxy classification and black hole mass (MBH) in a heterogeneous sample of 276 mostly nearby (z&lt;0.1) X-ray and IR-selected active galactic nuclei (AGN).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399#1</TD>
            <TD>2011-05-29T17:47:45Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/407/2399</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/407/2399 [2]</TD>
            <TD>AGN activity and black hole mass (McKernan+, 2010)</TD>
            <TD>We investigate the role of host galaxy classification and black hole mass (MBH) in a heterogeneous sample of 276 mostly nearby (z&lt;0.1) X-ray and IR-selected active galactic nuclei (AGN).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399#2</TD>
            <TD>2011-05-29T17:47:45Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/407/2399&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/407/2399 [table1]</TD>
            <TD>AGN activity and black hole mass (McKernan+, 2010)</TD>
            <TD>We investigate the role of host galaxy classification and black hole mass (MBH) in a heterogeneous sample of 276 mostly nearby (z&lt;0.1) X-ray and IR-selected active galactic nuclei (AGN).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399#table1</TD>
            <TD>2011-05-29T17:47:45Z</TD>
            <TD>#AGN#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/407/2399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2399</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/489/533 [1]</TD>
            <TD>M83 volume densities of giant molecular clouds (Heiner+, 2008)</TD>
            <TD>Using observed GALEX far-ultraviolet (FUV) fluxes and VLA images of the 21-cm HIcolumn densities, along with estimates of the local dust abundances, we measure the volume densities of a sample of actively star-forming giant molecular clouds (GMCs) in the nearby spiral galaxy M83 on a typical resolution scale of 170 pc. Our approach is based on an equilibrium model for the cycle of molecular hydrogen formation on dust grains and photodissociation under the influence of the FUV radiation on the cloud surfaces of GMCs. We find a range of total volume densities on the surface of GMCs in M83, namely 0.1-400cm^-3^ inside R_25_, 0.5-50cm^-3^ outside R_25_. Our data include a number of GMCs in the HI-ring surrounding this galaxy. Finally, we discuss the effects of observational selection, which may bias our results.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533#1</TD>
            <TD>2011-09-14T20:29:42Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/489/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/489/533 [2]</TD>
            <TD>M83 volume densities of giant molecular clouds (Heiner+, 2008)</TD>
            <TD>Using observed GALEX far-ultraviolet (FUV) fluxes and VLA images of the 21-cm HIcolumn densities, along with estimates of the local dust abundances, we measure the volume densities of a sample of actively star-forming giant molecular clouds (GMCs) in the nearby spiral galaxy M83 on a typical resolution scale of 170 pc. Our approach is based on an equilibrium model for the cycle of molecular hydrogen formation on dust grains and photodissociation under the influence of the FUV radiation on the cloud surfaces of GMCs. We find a range of total volume densities on the surface of GMCs in M83, namely 0.1-400cm^-3^ inside R_25_, 0.5-50cm^-3^ outside R_25_. Our data include a number of GMCs in the HI-ring surrounding this galaxy. Finally, we discuss the effects of observational selection, which may bias our results.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533#2</TD>
            <TD>2011-09-14T20:29:42Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/489/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/489/533 [table1]</TD>
            <TD>M83 volume densities of giant molecular clouds (Heiner+, 2008)</TD>
            <TD>Using observed GALEX far-ultraviolet (FUV) fluxes and VLA images of the 21-cm HIcolumn densities, along with estimates of the local dust abundances, we measure the volume densities of a sample of actively star-forming giant molecular clouds (GMCs) in the nearby spiral galaxy M83 on a typical resolution scale of 170 pc. Our approach is based on an equilibrium model for the cycle of molecular hydrogen formation on dust grains and photodissociation under the influence of the FUV radiation on the cloud surfaces of GMCs. We find a range of total volume densities on the surface of GMCs in M83, namely 0.1-400cm^-3^ inside R_25_, 0.5-50cm^-3^ outside R_25_. Our data include a number of GMCs in the HI-ring surrounding this galaxy. Finally, we discuss the effects of observational selection, which may bias our results.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533#table1</TD>
            <TD>2011-09-14T20:29:42Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/489/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/2563 [1]</TD>
            <TD>HI Nearby Galaxy Survey, THINGS (Walter+, 2008)</TD>
            <TD>We present "The HI Nearby Galaxy Survey (THINGS)," a high spectral (&lt;=5.2km/s) and spatial (~6") resolution survey of HI emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA). The overarching scientific goal of THINGS is to investigate fundamental characteristics of the interstellar medium (ISM) related to galaxy morphology, star formation, and mass distribution across the Hubble sequence. Unique characteristics of the THINGS database are the homogeneous sensitivity as well as spatial and velocity resolution of the HI data, which is at the limit of what can be achieved with the VLA for a significant number of galaxies. A sample of 34 objects at distances 2&lt;~D&gt;~15Mpc (resulting in linear resolutions of ~100 to 500pc) are targeted in THINGS, covering a wide range of star formation rates (~10^-3^ to 6M_{sun}_/yr), total HI masses MHI (0.01 to 14x10^9^M_{sun}_), absolute luminosities MB (-11.5 to -21.7mag), and metallicities (7.5 to 9.2 in units of 12+log[O/H]). We describe the setup of the VLA observations, the data reduction procedures, and the creation of the final THINGS data products. We present an atlas of the integrated HI maps, the velocity fields, the second moment (velocity dispersion) maps and individual channel maps of each THINGS galaxy. The THINGS data products are made publicly available through a dedicated webpage (http://www.mpia.de/THINGS). Accompanying THINGS papers (in this issue of the Astronomical Journal) address issues such as the small-scale structure of the ISM, the (dark) matter distribution in THINGS galaxies, and the processes leading to star formation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563#1</TD>
            <TD>2011-09-12T11:19:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/2563</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2563</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/2563 [2]</TD>
            <TD>HI Nearby Galaxy Survey, THINGS (Walter+, 2008)</TD>
            <TD>We present "The HI Nearby Galaxy Survey (THINGS)," a high spectral (&lt;=5.2km/s) and spatial (~6") resolution survey of HI emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA). The overarching scientific goal of THINGS is to investigate fundamental characteristics of the interstellar medium (ISM) related to galaxy morphology, star formation, and mass distribution across the Hubble sequence. Unique characteristics of the THINGS database are the homogeneous sensitivity as well as spatial and velocity resolution of the HI data, which is at the limit of what can be achieved with the VLA for a significant number of galaxies. A sample of 34 objects at distances 2&lt;~D&gt;~15Mpc (resulting in linear resolutions of ~100 to 500pc) are targeted in THINGS, covering a wide range of star formation rates (~10^-3^ to 6M_{sun}_/yr), total HI masses MHI (0.01 to 14x10^9^M_{sun}_), absolute luminosities MB (-11.5 to -21.7mag), and metallicities (7.5 to 9.2 in units of 12+log[O/H]). We describe the setup of the VLA observations, the data reduction procedures, and the creation of the final THINGS data products. We present an atlas of the integrated HI maps, the velocity fields, the second moment (velocity dispersion) maps and individual channel maps of each THINGS galaxy. The THINGS data products are made publicly available through a dedicated webpage (http://www.mpia.de/THINGS). Accompanying THINGS papers (in this issue of the Astronomical Journal) address issues such as the small-scale structure of the ISM, the (dark) matter distribution in THINGS galaxies, and the processes leading to star formation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563#2</TD>
            <TD>2011-09-12T11:19:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/2563&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2563</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/2563 [table1]</TD>
            <TD>HI Nearby Galaxy Survey, THINGS (Walter+, 2008)</TD>
            <TD>We present "The HI Nearby Galaxy Survey (THINGS)," a high spectral (&lt;=5.2km/s) and spatial (~6") resolution survey of HI emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA). The overarching scientific goal of THINGS is to investigate fundamental characteristics of the interstellar medium (ISM) related to galaxy morphology, star formation, and mass distribution across the Hubble sequence. Unique characteristics of the THINGS database are the homogeneous sensitivity as well as spatial and velocity resolution of the HI data, which is at the limit of what can be achieved with the VLA for a significant number of galaxies. A sample of 34 objects at distances 2&lt;~D&gt;~15Mpc (resulting in linear resolutions of ~100 to 500pc) are targeted in THINGS, covering a wide range of star formation rates (~10^-3^ to 6M_{sun}_/yr), total HI masses MHI (0.01 to 14x10^9^M_{sun}_), absolute luminosities MB (-11.5 to -21.7mag), and metallicities (7.5 to 9.2 in units of 12+log[O/H]). We describe the setup of the VLA observations, the data reduction procedures, and the creation of the final THINGS data products. We present an atlas of the integrated HI maps, the velocity fields, the second moment (velocity dispersion) maps and individual channel maps of each THINGS galaxy. The THINGS data products are made publicly available through a dedicated webpage (http://www.mpia.de/THINGS). Accompanying THINGS papers (in this issue of the Astronomical Journal) address issues such as the small-scale structure of the ISM, the (dark) matter distribution in THINGS galaxies, and the processes leading to star formation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563#table1</TD>
            <TD>2011-09-12T11:19:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/2563&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2563</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/489/533 [1]</TD>
            <TD>M83 volume densities of giant molecular clouds (Heiner+, 2008)</TD>
            <TD>Using observed GALEX far-ultraviolet (FUV) fluxes and VLA images of the 21-cm HIcolumn densities, along with estimates of the local dust abundances, we measure the volume densities of a sample of actively star-forming giant molecular clouds (GMCs) in the nearby spiral galaxy M83 on a typical resolution scale of 170 pc. Our approach is based on an equilibrium model for the cycle of molecular hydrogen formation on dust grains and photodissociation under the influence of the FUV radiation on the cloud surfaces of GMCs. We find a range of total volume densities on the surface of GMCs in M83, namely 0.1-400cm^-3^ inside R_25_, 0.5-50cm^-3^ outside R_25_. Our data include a number of GMCs in the HI-ring surrounding this galaxy. Finally, we discuss the effects of observational selection, which may bias our results.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533#1</TD>
            <TD>2011-09-14T20:29:42Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/489/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/489/533 [2]</TD>
            <TD>M83 volume densities of giant molecular clouds (Heiner+, 2008)</TD>
            <TD>Using observed GALEX far-ultraviolet (FUV) fluxes and VLA images of the 21-cm HIcolumn densities, along with estimates of the local dust abundances, we measure the volume densities of a sample of actively star-forming giant molecular clouds (GMCs) in the nearby spiral galaxy M83 on a typical resolution scale of 170 pc. Our approach is based on an equilibrium model for the cycle of molecular hydrogen formation on dust grains and photodissociation under the influence of the FUV radiation on the cloud surfaces of GMCs. We find a range of total volume densities on the surface of GMCs in M83, namely 0.1-400cm^-3^ inside R_25_, 0.5-50cm^-3^ outside R_25_. Our data include a number of GMCs in the HI-ring surrounding this galaxy. Finally, we discuss the effects of observational selection, which may bias our results.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533#2</TD>
            <TD>2011-09-14T20:29:42Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/489/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/489/533 [table1]</TD>
            <TD>M83 volume densities of giant molecular clouds (Heiner+, 2008)</TD>
            <TD>Using observed GALEX far-ultraviolet (FUV) fluxes and VLA images of the 21-cm HIcolumn densities, along with estimates of the local dust abundances, we measure the volume densities of a sample of actively star-forming giant molecular clouds (GMCs) in the nearby spiral galaxy M83 on a typical resolution scale of 170 pc. Our approach is based on an equilibrium model for the cycle of molecular hydrogen formation on dust grains and photodissociation under the influence of the FUV radiation on the cloud surfaces of GMCs. We find a range of total volume densities on the surface of GMCs in M83, namely 0.1-400cm^-3^ inside R_25_, 0.5-50cm^-3^ outside R_25_. Our data include a number of GMCs in the HI-ring surrounding this galaxy. Finally, we discuss the effects of observational selection, which may bias our results.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533#table1</TD>
            <TD>2011-09-14T20:29:42Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/489/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/2563 [1]</TD>
            <TD>HI Nearby Galaxy Survey, THINGS (Walter+, 2008)</TD>
            <TD>We present "The HI Nearby Galaxy Survey (THINGS)," a high spectral (&lt;=5.2km/s) and spatial (~6") resolution survey of HI emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA). The overarching scientific goal of THINGS is to investigate fundamental characteristics of the interstellar medium (ISM) related to galaxy morphology, star formation, and mass distribution across the Hubble sequence. Unique characteristics of the THINGS database are the homogeneous sensitivity as well as spatial and velocity resolution of the HI data, which is at the limit of what can be achieved with the VLA for a significant number of galaxies. A sample of 34 objects at distances 2&lt;~D&gt;~15Mpc (resulting in linear resolutions of ~100 to 500pc) are targeted in THINGS, covering a wide range of star formation rates (~10^-3^ to 6M_{sun}_/yr), total HI masses MHI (0.01 to 14x10^9^M_{sun}_), absolute luminosities MB (-11.5 to -21.7mag), and metallicities (7.5 to 9.2 in units of 12+log[O/H]). We describe the setup of the VLA observations, the data reduction procedures, and the creation of the final THINGS data products. We present an atlas of the integrated HI maps, the velocity fields, the second moment (velocity dispersion) maps and individual channel maps of each THINGS galaxy. The THINGS data products are made publicly available through a dedicated webpage (http://www.mpia.de/THINGS). Accompanying THINGS papers (in this issue of the Astronomical Journal) address issues such as the small-scale structure of the ISM, the (dark) matter distribution in THINGS galaxies, and the processes leading to star formation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563#1</TD>
            <TD>2011-09-12T11:19:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/2563</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2563</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/2563 [2]</TD>
            <TD>HI Nearby Galaxy Survey, THINGS (Walter+, 2008)</TD>
            <TD>We present "The HI Nearby Galaxy Survey (THINGS)," a high spectral (&lt;=5.2km/s) and spatial (~6") resolution survey of HI emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA). The overarching scientific goal of THINGS is to investigate fundamental characteristics of the interstellar medium (ISM) related to galaxy morphology, star formation, and mass distribution across the Hubble sequence. Unique characteristics of the THINGS database are the homogeneous sensitivity as well as spatial and velocity resolution of the HI data, which is at the limit of what can be achieved with the VLA for a significant number of galaxies. A sample of 34 objects at distances 2&lt;~D&gt;~15Mpc (resulting in linear resolutions of ~100 to 500pc) are targeted in THINGS, covering a wide range of star formation rates (~10^-3^ to 6M_{sun}_/yr), total HI masses MHI (0.01 to 14x10^9^M_{sun}_), absolute luminosities MB (-11.5 to -21.7mag), and metallicities (7.5 to 9.2 in units of 12+log[O/H]). We describe the setup of the VLA observations, the data reduction procedures, and the creation of the final THINGS data products. We present an atlas of the integrated HI maps, the velocity fields, the second moment (velocity dispersion) maps and individual channel maps of each THINGS galaxy. The THINGS data products are made publicly available through a dedicated webpage (http://www.mpia.de/THINGS). Accompanying THINGS papers (in this issue of the Astronomical Journal) address issues such as the small-scale structure of the ISM, the (dark) matter distribution in THINGS galaxies, and the processes leading to star formation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563#2</TD>
            <TD>2011-09-12T11:19:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/2563&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2563</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/2563 [table1]</TD>
            <TD>HI Nearby Galaxy Survey, THINGS (Walter+, 2008)</TD>
            <TD>We present "The HI Nearby Galaxy Survey (THINGS)," a high spectral (&lt;=5.2km/s) and spatial (~6") resolution survey of HI emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA). The overarching scientific goal of THINGS is to investigate fundamental characteristics of the interstellar medium (ISM) related to galaxy morphology, star formation, and mass distribution across the Hubble sequence. Unique characteristics of the THINGS database are the homogeneous sensitivity as well as spatial and velocity resolution of the HI data, which is at the limit of what can be achieved with the VLA for a significant number of galaxies. A sample of 34 objects at distances 2&lt;~D&gt;~15Mpc (resulting in linear resolutions of ~100 to 500pc) are targeted in THINGS, covering a wide range of star formation rates (~10^-3^ to 6M_{sun}_/yr), total HI masses MHI (0.01 to 14x10^9^M_{sun}_), absolute luminosities MB (-11.5 to -21.7mag), and metallicities (7.5 to 9.2 in units of 12+log[O/H]). We describe the setup of the VLA observations, the data reduction procedures, and the creation of the final THINGS data products. We present an atlas of the integrated HI maps, the velocity fields, the second moment (velocity dispersion) maps and individual channel maps of each THINGS galaxy. The THINGS data products are made publicly available through a dedicated webpage (http://www.mpia.de/THINGS). Accompanying THINGS papers (in this issue of the Astronomical Journal) address issues such as the small-scale structure of the ISM, the (dark) matter distribution in THINGS galaxies, and the processes leading to star formation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563#table1</TD>
            <TD>2011-09-12T11:19:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/2563&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2563</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/2563 [1]</TD>
            <TD>HI Nearby Galaxy Survey, THINGS (Walter+, 2008)</TD>
            <TD>We present "The HI Nearby Galaxy Survey (THINGS)," a high spectral (&lt;=5.2km/s) and spatial (~6") resolution survey of HI emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA). The overarching scientific goal of THINGS is to investigate fundamental characteristics of the interstellar medium (ISM) related to galaxy morphology, star formation, and mass distribution across the Hubble sequence. Unique characteristics of the THINGS database are the homogeneous sensitivity as well as spatial and velocity resolution of the HI data, which is at the limit of what can be achieved with the VLA for a significant number of galaxies. A sample of 34 objects at distances 2&lt;~D&gt;~15Mpc (resulting in linear resolutions of ~100 to 500pc) are targeted in THINGS, covering a wide range of star formation rates (~10^-3^ to 6M_{sun}_/yr), total HI masses MHI (0.01 to 14x10^9^M_{sun}_), absolute luminosities MB (-11.5 to -21.7mag), and metallicities (7.5 to 9.2 in units of 12+log[O/H]). We describe the setup of the VLA observations, the data reduction procedures, and the creation of the final THINGS data products. We present an atlas of the integrated HI maps, the velocity fields, the second moment (velocity dispersion) maps and individual channel maps of each THINGS galaxy. The THINGS data products are made publicly available through a dedicated webpage (http://www.mpia.de/THINGS). Accompanying THINGS papers (in this issue of the Astronomical Journal) address issues such as the small-scale structure of the ISM, the (dark) matter distribution in THINGS galaxies, and the processes leading to star formation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563#1</TD>
            <TD>2011-09-12T11:19:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/2563</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2563</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/2563 [2]</TD>
            <TD>HI Nearby Galaxy Survey, THINGS (Walter+, 2008)</TD>
            <TD>We present "The HI Nearby Galaxy Survey (THINGS)," a high spectral (&lt;=5.2km/s) and spatial (~6") resolution survey of HI emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA). The overarching scientific goal of THINGS is to investigate fundamental characteristics of the interstellar medium (ISM) related to galaxy morphology, star formation, and mass distribution across the Hubble sequence. Unique characteristics of the THINGS database are the homogeneous sensitivity as well as spatial and velocity resolution of the HI data, which is at the limit of what can be achieved with the VLA for a significant number of galaxies. A sample of 34 objects at distances 2&lt;~D&gt;~15Mpc (resulting in linear resolutions of ~100 to 500pc) are targeted in THINGS, covering a wide range of star formation rates (~10^-3^ to 6M_{sun}_/yr), total HI masses MHI (0.01 to 14x10^9^M_{sun}_), absolute luminosities MB (-11.5 to -21.7mag), and metallicities (7.5 to 9.2 in units of 12+log[O/H]). We describe the setup of the VLA observations, the data reduction procedures, and the creation of the final THINGS data products. We present an atlas of the integrated HI maps, the velocity fields, the second moment (velocity dispersion) maps and individual channel maps of each THINGS galaxy. The THINGS data products are made publicly available through a dedicated webpage (http://www.mpia.de/THINGS). Accompanying THINGS papers (in this issue of the Astronomical Journal) address issues such as the small-scale structure of the ISM, the (dark) matter distribution in THINGS galaxies, and the processes leading to star formation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563#2</TD>
            <TD>2011-09-12T11:19:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/2563&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2563</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/2563 [table1]</TD>
            <TD>HI Nearby Galaxy Survey, THINGS (Walter+, 2008)</TD>
            <TD>We present "The HI Nearby Galaxy Survey (THINGS)," a high spectral (&lt;=5.2km/s) and spatial (~6") resolution survey of HI emission in 34 nearby galaxies obtained using the NRAO Very Large Array (VLA). The overarching scientific goal of THINGS is to investigate fundamental characteristics of the interstellar medium (ISM) related to galaxy morphology, star formation, and mass distribution across the Hubble sequence. Unique characteristics of the THINGS database are the homogeneous sensitivity as well as spatial and velocity resolution of the HI data, which is at the limit of what can be achieved with the VLA for a significant number of galaxies. A sample of 34 objects at distances 2&lt;~D&gt;~15Mpc (resulting in linear resolutions of ~100 to 500pc) are targeted in THINGS, covering a wide range of star formation rates (~10^-3^ to 6M_{sun}_/yr), total HI masses MHI (0.01 to 14x10^9^M_{sun}_), absolute luminosities MB (-11.5 to -21.7mag), and metallicities (7.5 to 9.2 in units of 12+log[O/H]). We describe the setup of the VLA observations, the data reduction procedures, and the creation of the final THINGS data products. We present an atlas of the integrated HI maps, the velocity fields, the second moment (velocity dispersion) maps and individual channel maps of each THINGS galaxy. The THINGS data products are made publicly available through a dedicated webpage (http://www.mpia.de/THINGS). Accompanying THINGS papers (in this issue of the Astronomical Journal) address issues such as the small-scale structure of the ISM, the (dark) matter distribution in THINGS galaxies, and the processes leading to star formation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563#table1</TD>
            <TD>2011-09-12T11:19:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2563</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/2563&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2563</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/535/A65 [1]</TD>
            <TD>Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)</TD>
            <TD>We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&amp;A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg^2^, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1&lt;=z&lt;=1.15, with estimated mean masses between 1.3x10^14^ and 12.6x10^14^M_{sun}_. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65#1</TD>
            <TD>2011-11-08T07:43:34Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/535/A65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/535/A65 [2]</TD>
            <TD>Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)</TD>
            <TD>We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&amp;A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg^2^, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1&lt;=z&lt;=1.15, with estimated mean masses between 1.3x10^14^ and 12.6x10^14^M_{sun}_. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65#2</TD>
            <TD>2011-11-08T07:43:34Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/535/A65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/535/A65 [wide1234]</TD>
            <TD>Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)</TD>
            <TD>We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&amp;A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg^2^, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1&lt;=z&lt;=1.15, with estimated mean masses between 1.3x10^14^ and 12.6x10^14^M_{sun}_. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65#wide1234</TD>
            <TD>2011-11-08T07:43:34Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/535/A65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/489/533 [1]</TD>
            <TD>M83 volume densities of giant molecular clouds (Heiner+, 2008)</TD>
            <TD>Using observed GALEX far-ultraviolet (FUV) fluxes and VLA images of the 21-cm HIcolumn densities, along with estimates of the local dust abundances, we measure the volume densities of a sample of actively star-forming giant molecular clouds (GMCs) in the nearby spiral galaxy M83 on a typical resolution scale of 170 pc. Our approach is based on an equilibrium model for the cycle of molecular hydrogen formation on dust grains and photodissociation under the influence of the FUV radiation on the cloud surfaces of GMCs. We find a range of total volume densities on the surface of GMCs in M83, namely 0.1-400cm^-3^ inside R_25_, 0.5-50cm^-3^ outside R_25_. Our data include a number of GMCs in the HI-ring surrounding this galaxy. Finally, we discuss the effects of observational selection, which may bias our results.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533#1</TD>
            <TD>2011-09-14T20:29:42Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/489/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/489/533 [2]</TD>
            <TD>M83 volume densities of giant molecular clouds (Heiner+, 2008)</TD>
            <TD>Using observed GALEX far-ultraviolet (FUV) fluxes and VLA images of the 21-cm HIcolumn densities, along with estimates of the local dust abundances, we measure the volume densities of a sample of actively star-forming giant molecular clouds (GMCs) in the nearby spiral galaxy M83 on a typical resolution scale of 170 pc. Our approach is based on an equilibrium model for the cycle of molecular hydrogen formation on dust grains and photodissociation under the influence of the FUV radiation on the cloud surfaces of GMCs. We find a range of total volume densities on the surface of GMCs in M83, namely 0.1-400cm^-3^ inside R_25_, 0.5-50cm^-3^ outside R_25_. Our data include a number of GMCs in the HI-ring surrounding this galaxy. Finally, we discuss the effects of observational selection, which may bias our results.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533#2</TD>
            <TD>2011-09-14T20:29:42Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/489/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/489/533 [table1]</TD>
            <TD>M83 volume densities of giant molecular clouds (Heiner+, 2008)</TD>
            <TD>Using observed GALEX far-ultraviolet (FUV) fluxes and VLA images of the 21-cm HIcolumn densities, along with estimates of the local dust abundances, we measure the volume densities of a sample of actively star-forming giant molecular clouds (GMCs) in the nearby spiral galaxy M83 on a typical resolution scale of 170 pc. Our approach is based on an equilibrium model for the cycle of molecular hydrogen formation on dust grains and photodissociation under the influence of the FUV radiation on the cloud surfaces of GMCs. We find a range of total volume densities on the surface of GMCs in M83, namely 0.1-400cm^-3^ inside R_25_, 0.5-50cm^-3^ outside R_25_. Our data include a number of GMCs in the HI-ring surrounding this galaxy. Finally, we discuss the effects of observational selection, which may bias our results.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533#table1</TD>
            <TD>2011-09-14T20:29:42Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/489/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/535/A65 [1]</TD>
            <TD>Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)</TD>
            <TD>We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&amp;A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg^2^, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1&lt;=z&lt;=1.15, with estimated mean masses between 1.3x10^14^ and 12.6x10^14^M_{sun}_. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65#1</TD>
            <TD>2011-11-08T07:43:34Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/535/A65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/535/A65 [2]</TD>
            <TD>Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)</TD>
            <TD>We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&amp;A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg^2^, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1&lt;=z&lt;=1.15, with estimated mean masses between 1.3x10^14^ and 12.6x10^14^M_{sun}_. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65#2</TD>
            <TD>2011-11-08T07:43:34Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/535/A65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/535/A65 [wide1234]</TD>
            <TD>Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)</TD>
            <TD>We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&amp;A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg^2^, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1&lt;=z&lt;=1.15, with estimated mean masses between 1.3x10^14^ and 12.6x10^14^M_{sun}_. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65#wide1234</TD>
            <TD>2011-11-08T07:43:34Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/535/A65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/645/228 [1]</TD>
            <TD>Velocities of satellites of external disk galaxies (Azzaro+ 2006)</TD>
            <TD>We analyze the angular distribution and the orbital rotation directions of a sample of carefully selected satellite galaxies about disk galaxy primaries extracted from the Sloan Digital Sky Survey (SDSS). We complement this analysis with a theoretical study of these statistics in an N-body simulation of cosmological structure formation set within the {Delta}CDM paradigm under various assumptions for the orientations of disk angular momenta.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228#1</TD>
            <TD>2011-09-14T20:29:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/645/228</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/228</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/645/228 [2]</TD>
            <TD>Velocities of satellites of external disk galaxies (Azzaro+ 2006)</TD>
            <TD>We analyze the angular distribution and the orbital rotation directions of a sample of carefully selected satellite galaxies about disk galaxy primaries extracted from the Sloan Digital Sky Survey (SDSS). We complement this analysis with a theoretical study of these statistics in an N-body simulation of cosmological structure formation set within the {Delta}CDM paradigm under various assumptions for the orientations of disk angular momenta.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228#2</TD>
            <TD>2011-09-14T20:29:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/645/228&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/228</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/645/228 [table3]</TD>
            <TD>Velocities of satellites of external disk galaxies (Azzaro+ 2006)</TD>
            <TD>We analyze the angular distribution and the orbital rotation directions of a sample of carefully selected satellite galaxies about disk galaxy primaries extracted from the Sloan Digital Sky Survey (SDSS). We complement this analysis with a theoretical study of these statistics in an N-body simulation of cosmological structure formation set within the {Delta}CDM paradigm under various assumptions for the orientations of disk angular momenta.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228#table3</TD>
            <TD>2011-09-14T20:29:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/645/228&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/228</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/535/A65 [1]</TD>
            <TD>Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)</TD>
            <TD>We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&amp;A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg^2^, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1&lt;=z&lt;=1.15, with estimated mean masses between 1.3x10^14^ and 12.6x10^14^M_{sun}_. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65#1</TD>
            <TD>2011-11-08T07:43:34Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/535/A65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/535/A65 [2]</TD>
            <TD>Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)</TD>
            <TD>We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&amp;A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg^2^, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1&lt;=z&lt;=1.15, with estimated mean masses between 1.3x10^14^ and 12.6x10^14^M_{sun}_. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65#2</TD>
            <TD>2011-11-08T07:43:34Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/535/A65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/535/A65 [wide1234]</TD>
            <TD>Galaxy clusters in the 4 CFHTLS Wide fields (Durret+, 2011)</TD>
            <TD>We have developed a method for detecting clusters in large imaging surveys, based on the detection of structures in galaxy density maps made in slices of photometric redshifts. This method was first applied to the Canada France Hawaii Telescope Legacy Survey (CFHTLS) Deep 1 field by Mazure et al. (2007A&amp;A...467...49M), then to all the Deep and Wide CFHTLS fields available in the T0004 data release by Adami et al. (2010, Cat. J/A+A/509/81). The validity of the cluster detection rate was estimated by applying the same procedure to galaxies from the Millennium simulation. Here we analyse with the same method the full CFHTLS Wide survey, based on the T0006 data release. In a total area of 154deg^2^, we have detected 4061 candidate clusters at 3sigma or above (6802 at 2sigma and above), in the redshift range 0.1&lt;=z&lt;=1.15, with estimated mean masses between 1.3x10^14^ and 12.6x10^14^M_{sun}_. We compare our detections with those made in various CFHTLS analyses with other methods. By stacking a subsample of clusters, we show that this subsample has typical cluster characteristics (colour-magnitude relation, galaxy luminosity function). We also confirm that the cluster-cluster correlation function is comparable to that obtained for other cluster surveys and analyze large scale filamentary galaxy distributions. We have increased the number of known optical high redshift cluster candidates by a large factor, an important step towards obtaining reliable cluster counts to measure cosmological parameters. The clusters that we detect behave as expected for a sample of clusters fed by filaments at the intersection of which they are located.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65#wide1234</TD>
            <TD>2011-11-08T07:43:34Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/535/A65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/535/A65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/535/A65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/645/228 [1]</TD>
            <TD>Velocities of satellites of external disk galaxies (Azzaro+ 2006)</TD>
            <TD>We analyze the angular distribution and the orbital rotation directions of a sample of carefully selected satellite galaxies about disk galaxy primaries extracted from the Sloan Digital Sky Survey (SDSS). We complement this analysis with a theoretical study of these statistics in an N-body simulation of cosmological structure formation set within the {Delta}CDM paradigm under various assumptions for the orientations of disk angular momenta.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228#1</TD>
            <TD>2011-09-14T20:29:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/645/228</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/228</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/645/228 [2]</TD>
            <TD>Velocities of satellites of external disk galaxies (Azzaro+ 2006)</TD>
            <TD>We analyze the angular distribution and the orbital rotation directions of a sample of carefully selected satellite galaxies about disk galaxy primaries extracted from the Sloan Digital Sky Survey (SDSS). We complement this analysis with a theoretical study of these statistics in an N-body simulation of cosmological structure formation set within the {Delta}CDM paradigm under various assumptions for the orientations of disk angular momenta.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228#2</TD>
            <TD>2011-09-14T20:29:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/645/228&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/228</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/645/228 [table3]</TD>
            <TD>Velocities of satellites of external disk galaxies (Azzaro+ 2006)</TD>
            <TD>We analyze the angular distribution and the orbital rotation directions of a sample of carefully selected satellite galaxies about disk galaxy primaries extracted from the Sloan Digital Sky Survey (SDSS). We complement this analysis with a theoretical study of these statistics in an N-body simulation of cosmological structure formation set within the {Delta}CDM paradigm under various assumptions for the orientations of disk angular momenta.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228#table3</TD>
            <TD>2011-09-14T20:29:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/645/228&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/228</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A109 [1]</TD>
            <TD>MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)</TD>
            <TD>We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L_500_, total mass M_500_, and radius R_500_. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109#1</TD>
            <TD>2011-11-12T15:59:57Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A109 [2]</TD>
            <TD>MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)</TD>
            <TD>We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L_500_, total mass M_500_, and radius R_500_. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109#2</TD>
            <TD>2011-11-12T15:59:57Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A109</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A109 [mcxc]</TD>
            <TD>MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)</TD>
            <TD>We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L_500_, total mass M_500_, and radius R_500_. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109#mcxc</TD>
            <TD>2011-11-12T15:59:57Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A109&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/645/228 [1]</TD>
            <TD>Velocities of satellites of external disk galaxies (Azzaro+ 2006)</TD>
            <TD>We analyze the angular distribution and the orbital rotation directions of a sample of carefully selected satellite galaxies about disk galaxy primaries extracted from the Sloan Digital Sky Survey (SDSS). We complement this analysis with a theoretical study of these statistics in an N-body simulation of cosmological structure formation set within the {Delta}CDM paradigm under various assumptions for the orientations of disk angular momenta.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228#1</TD>
            <TD>2011-09-14T20:29:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/645/228</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/228</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/645/228 [2]</TD>
            <TD>Velocities of satellites of external disk galaxies (Azzaro+ 2006)</TD>
            <TD>We analyze the angular distribution and the orbital rotation directions of a sample of carefully selected satellite galaxies about disk galaxy primaries extracted from the Sloan Digital Sky Survey (SDSS). We complement this analysis with a theoretical study of these statistics in an N-body simulation of cosmological structure formation set within the {Delta}CDM paradigm under various assumptions for the orientations of disk angular momenta.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228#2</TD>
            <TD>2011-09-14T20:29:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/645/228&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/228</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/645/228 [table3]</TD>
            <TD>Velocities of satellites of external disk galaxies (Azzaro+ 2006)</TD>
            <TD>We analyze the angular distribution and the orbital rotation directions of a sample of carefully selected satellite galaxies about disk galaxy primaries extracted from the Sloan Digital Sky Survey (SDSS). We complement this analysis with a theoretical study of these statistics in an N-body simulation of cosmological structure formation set within the {Delta}CDM paradigm under various assumptions for the orientations of disk angular momenta.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228#table3</TD>
            <TD>2011-09-14T20:29:57Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/228</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/645/228&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/228</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A109 [1]</TD>
            <TD>MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)</TD>
            <TD>We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L_500_, total mass M_500_, and radius R_500_. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109#1</TD>
            <TD>2011-11-12T15:59:57Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A109 [2]</TD>
            <TD>MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)</TD>
            <TD>We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L_500_, total mass M_500_, and radius R_500_. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109#2</TD>
            <TD>2011-11-12T15:59:57Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A109</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A109 [mcxc]</TD>
            <TD>MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)</TD>
            <TD>We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L_500_, total mass M_500_, and radius R_500_. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109#mcxc</TD>
            <TD>2011-11-12T15:59:57Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A109&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/968 [1]</TD>
            <TD>SDSS-C4 cluster catalog (Miller+, 2005)</TD>
            <TD>We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2, 2004AJ....128..502A) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers ~2600deg^2^ of sky and ranges in redshift from z=0.02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r=17.7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L_r_), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the {Lambda}CDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968#1</TD>
            <TD>2011-09-14T20:29:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/968</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/968</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/968 [2]</TD>
            <TD>SDSS-C4 cluster catalog (Miller+, 2005)</TD>
            <TD>We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2, 2004AJ....128..502A) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers ~2600deg^2^ of sky and ranges in redshift from z=0.02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r=17.7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L_r_), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the {Lambda}CDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968#2</TD>
            <TD>2011-09-14T20:29:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/968&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/968</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/968 [table2]</TD>
            <TD>SDSS-C4 cluster catalog (Miller+, 2005)</TD>
            <TD>We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2, 2004AJ....128..502A) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers ~2600deg^2^ of sky and ranges in redshift from z=0.02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r=17.7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L_r_), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the {Lambda}CDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968#table2</TD>
            <TD>2011-09-14T20:29:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/968&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/968</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A109 [1]</TD>
            <TD>MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)</TD>
            <TD>We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L_500_, total mass M_500_, and radius R_500_. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109#1</TD>
            <TD>2011-11-12T15:59:57Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A109 [2]</TD>
            <TD>MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)</TD>
            <TD>We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L_500_, total mass M_500_, and radius R_500_. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109#2</TD>
            <TD>2011-11-12T15:59:57Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A109</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A109 [mcxc]</TD>
            <TD>MCXC Meta-Catalogue X-ray galaxy Clusters (Piffaretti+, 2011)</TD>
            <TD>We present the compilation and properties of a meta-catalogue of X-ray detected clusters of galaxies, the MCXC. This very large catalogue is based on publicly available ROSAT All Sky Survey-based (NORAS, REFLEX, BCS, SGP, NEP, MACS, and CIZA) and serendipitous (160SD, 400SD, SHARC, WARPS, and EMSS) cluster catalogues. Data have been systematically homogenised to an overdensity of 500, and duplicate entries from overlaps between the survey areas of the individual input catalogues are carefully handled. The MCXC comprises 1743 clusters with virtually no duplicate entries. For each cluster the MCXC provides three identifiers, a redshift, coordinates, membership in the original catalogue, and standardised 0.1-2.4keV band luminosity L_500_, total mass M_500_, and radius R_500_. The meta-catalogue additionally furnishes information on overlaps between the input catalogues and the luminosity ratios when measurements from different surveys are available, and gives notes on individual objects.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109#mcxc</TD>
            <TD>2011-11-12T15:59:57Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A109</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A109&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1959 [1]</TD>
            <TD>1.4GHz emission of KISS emission-line galaxies (Van Duyne+, 2004)</TD>
            <TD>We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) and the NRAO VLA Sky Survey (NVSS, &lt;VIII/65&gt;) 1.4GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (~10%) in the first two H{alpha}-selected survey lists (Cats &lt;J/AJ/121/66&gt;, &lt;J/AJ/127/1943&gt;) were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z&lt;0.1). Because of the selection technique used for KISS, our radio ELGs represent a quasivolume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959#1</TD>
            <TD>2011-11-20T19:57:38Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1959</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1959</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1959 [2]</TD>
            <TD>1.4GHz emission of KISS emission-line galaxies (Van Duyne+, 2004)</TD>
            <TD>We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) and the NRAO VLA Sky Survey (NVSS, &lt;VIII/65&gt;) 1.4GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (~10%) in the first two H{alpha}-selected survey lists (Cats &lt;J/AJ/121/66&gt;, &lt;J/AJ/127/1943&gt;) were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z&lt;0.1). Because of the selection technique used for KISS, our radio ELGs represent a quasivolume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959#2</TD>
            <TD>2011-11-20T19:57:38Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1959&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1959</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/1959 [table3]</TD>
            <TD>1.4GHz emission of KISS emission-line galaxies (Van Duyne+, 2004)</TD>
            <TD>We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) and the NRAO VLA Sky Survey (NVSS, &lt;VIII/65&gt;) 1.4GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (~10%) in the first two H{alpha}-selected survey lists (Cats &lt;J/AJ/121/66&gt;, &lt;J/AJ/127/1943&gt;) were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z&lt;0.1). Because of the selection technique used for KISS, our radio ELGs represent a quasivolume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959#table3</TD>
            <TD>2011-11-20T19:57:38Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/1959&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1959</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/968 [1]</TD>
            <TD>SDSS-C4 cluster catalog (Miller+, 2005)</TD>
            <TD>We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2, 2004AJ....128..502A) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers ~2600deg^2^ of sky and ranges in redshift from z=0.02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r=17.7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L_r_), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the {Lambda}CDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968#1</TD>
            <TD>2011-09-14T20:29:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/968</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/968</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/968 [2]</TD>
            <TD>SDSS-C4 cluster catalog (Miller+, 2005)</TD>
            <TD>We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2, 2004AJ....128..502A) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers ~2600deg^2^ of sky and ranges in redshift from z=0.02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r=17.7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L_r_), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the {Lambda}CDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968#2</TD>
            <TD>2011-09-14T20:29:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/968&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/968</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/968 [table2]</TD>
            <TD>SDSS-C4 cluster catalog (Miller+, 2005)</TD>
            <TD>We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2, 2004AJ....128..502A) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers ~2600deg^2^ of sky and ranges in redshift from z=0.02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r=17.7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L_r_), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the {Lambda}CDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968#table2</TD>
            <TD>2011-09-14T20:29:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/968&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/968</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1959 [1]</TD>
            <TD>1.4GHz emission of KISS emission-line galaxies (Van Duyne+, 2004)</TD>
            <TD>We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) and the NRAO VLA Sky Survey (NVSS, &lt;VIII/65&gt;) 1.4GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (~10%) in the first two H{alpha}-selected survey lists (Cats &lt;J/AJ/121/66&gt;, &lt;J/AJ/127/1943&gt;) were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z&lt;0.1). Because of the selection technique used for KISS, our radio ELGs represent a quasivolume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959#1</TD>
            <TD>2011-11-20T19:57:38Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1959</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1959</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1959 [2]</TD>
            <TD>1.4GHz emission of KISS emission-line galaxies (Van Duyne+, 2004)</TD>
            <TD>We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) and the NRAO VLA Sky Survey (NVSS, &lt;VIII/65&gt;) 1.4GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (~10%) in the first two H{alpha}-selected survey lists (Cats &lt;J/AJ/121/66&gt;, &lt;J/AJ/127/1943&gt;) were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z&lt;0.1). Because of the selection technique used for KISS, our radio ELGs represent a quasivolume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959#2</TD>
            <TD>2011-11-20T19:57:38Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1959&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1959</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/1959 [table3]</TD>
            <TD>1.4GHz emission of KISS emission-line galaxies (Van Duyne+, 2004)</TD>
            <TD>We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) and the NRAO VLA Sky Survey (NVSS, &lt;VIII/65&gt;) 1.4GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (~10%) in the first two H{alpha}-selected survey lists (Cats &lt;J/AJ/121/66&gt;, &lt;J/AJ/127/1943&gt;) were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z&lt;0.1). Because of the selection technique used for KISS, our radio ELGs represent a quasivolume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959#table3</TD>
            <TD>2011-11-20T19:57:38Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/1959&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1959</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/968 [1]</TD>
            <TD>SDSS-C4 cluster catalog (Miller+, 2005)</TD>
            <TD>We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2, 2004AJ....128..502A) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers ~2600deg^2^ of sky and ranges in redshift from z=0.02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r=17.7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L_r_), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the {Lambda}CDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968#1</TD>
            <TD>2011-09-14T20:29:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/968</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/968</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/968 [2]</TD>
            <TD>SDSS-C4 cluster catalog (Miller+, 2005)</TD>
            <TD>We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2, 2004AJ....128..502A) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers ~2600deg^2^ of sky and ranges in redshift from z=0.02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r=17.7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L_r_), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the {Lambda}CDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968#2</TD>
            <TD>2011-09-14T20:29:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/968&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/968</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/968 [table2]</TD>
            <TD>SDSS-C4 cluster catalog (Miller+, 2005)</TD>
            <TD>We present the C4 Cluster Catalog, a new sample of 748 clusters of galaxies identified in the spectroscopic sample of the Second Data Release (DR2, 2004AJ....128..502A) of the Sloan Digital Sky Survey (SDSS). The C4 cluster-finding algorithm identifies clusters as overdensities in a seven-dimensional position and color space, thus minimizing projection effects that have plagued previous optical cluster selection. The present C4 catalog covers ~2600deg^2^ of sky and ranges in redshift from z=0.02 to 0.17. The mean cluster membership is 36 galaxies (with measured redshifts) brighter than r=17.7, but the catalog includes a range of systems, from groups containing 10 members to massive clusters with over 200 cluster members with measured redshifts. The catalog provides a large number of measured cluster properties including sky location, mean redshift, galaxy membership, summed r-band optical luminosity (L_r_), and velocity dispersion, as well as quantitative measures of substructure and the surrounding large-scale environment. We use new, multicolor mock SDSS galaxy catalogs, empirically constructed from the {Lambda}CDM Hubble Volume (HV) Sky Survey output, to investigate the sensitivity of the C4 catalog to the various algorithm parameters (detection threshold, choice of passbands, and search aperture), as well as to quantify the purity and completeness of the C4 cluster catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968#table2</TD>
            <TD>2011-09-14T20:29:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/968</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/968&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/968</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1959 [1]</TD>
            <TD>1.4GHz emission of KISS emission-line galaxies (Van Duyne+, 2004)</TD>
            <TD>We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) and the NRAO VLA Sky Survey (NVSS, &lt;VIII/65&gt;) 1.4GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (~10%) in the first two H{alpha}-selected survey lists (Cats &lt;J/AJ/121/66&gt;, &lt;J/AJ/127/1943&gt;) were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z&lt;0.1). Because of the selection technique used for KISS, our radio ELGs represent a quasivolume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959#1</TD>
            <TD>2011-11-20T19:57:38Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1959</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1959</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1959 [2]</TD>
            <TD>1.4GHz emission of KISS emission-line galaxies (Van Duyne+, 2004)</TD>
            <TD>We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) and the NRAO VLA Sky Survey (NVSS, &lt;VIII/65&gt;) 1.4GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (~10%) in the first two H{alpha}-selected survey lists (Cats &lt;J/AJ/121/66&gt;, &lt;J/AJ/127/1943&gt;) were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z&lt;0.1). Because of the selection technique used for KISS, our radio ELGs represent a quasivolume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959#2</TD>
            <TD>2011-11-20T19:57:38Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1959&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1959</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/1959 [table3]</TD>
            <TD>1.4GHz emission of KISS emission-line galaxies (Van Duyne+, 2004)</TD>
            <TD>We have searched the Faint Images of the Radio Sky at Twenty centimeters (FIRST, &lt;VIII/71&gt;) and the NRAO VLA Sky Survey (NVSS, &lt;VIII/65&gt;) 1.4GHz radio surveys for sources that are coincident with emission-line galaxy (ELG) candidates from the KPNO International Spectroscopic Survey (KISS). A total of 207 of the 2157 KISS ELGs (~10%) in the first two H{alpha}-selected survey lists (Cats &lt;J/AJ/121/66&gt;, &lt;J/AJ/127/1943&gt;) were found to possess radio detections in FIRST, NVSS, or both. Follow-up spectra exist for all of the radio detections, allowing us to determine the activity type (star-forming vs. active nucleus) for the entire sample. We explore the properties of the radio-detected KISS galaxies in order to gain a better insight into the nature of radio-emitting galaxies in the local universe (z&lt;0.1). Because of the selection technique used for KISS, our radio ELGs represent a quasivolume-limited sample, which allows us to develop a clearer picture of the radio galaxy population at low redshift. Nearly two-thirds of the KISS radio galaxies are starburst or star-forming galaxies, which is in stark contrast to the results of flux-limited radio surveys, which are dominated by active galactic nuclei (AGNs) and elliptical galaxies (i.e., classical radio galaxies).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959#table3</TD>
            <TD>2011-11-20T19:57:38Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1959</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/1959&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1959</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/531/A4 [1]</TD>
            <TD>Ultra compact dwarfs and globulars in Hya I (Misgeld+, 2011)</TD>
            <TD>VIMOS allows simultaneous observation of four quadrants in one telescope pointing. Each quadrant is of dimension 7'x8', with a gap of about 2' between the quadrants. For the UCD survey, we placed four multi-object spectroscopy (MOS) pointings around NGC 3311, the central cD galaxy of the Hydra I cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4#1</TD>
            <TD>2011-11-24T08:02:25Z</TD>
            <TD>#Clusters_of_galaxies#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/531/A4</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A4</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/531/A4 [2]</TD>
            <TD>Ultra compact dwarfs and globulars in Hya I (Misgeld+, 2011)</TD>
            <TD>VIMOS allows simultaneous observation of four quadrants in one telescope pointing. Each quadrant is of dimension 7'x8', with a gap of about 2' between the quadrants. For the UCD survey, we placed four multi-object spectroscopy (MOS) pointings around NGC 3311, the central cD galaxy of the Hydra I cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4#2</TD>
            <TD>2011-11-24T08:02:25Z</TD>
            <TD>#Clusters_of_galaxies#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/531/A4&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A4</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A4 [tablea1]</TD>
            <TD>Ultra compact dwarfs and globulars in Hya I (Misgeld+, 2011)</TD>
            <TD>VIMOS allows simultaneous observation of four quadrants in one telescope pointing. Each quadrant is of dimension 7'x8', with a gap of about 2' between the quadrants. For the UCD survey, we placed four multi-object spectroscopy (MOS) pointings around NGC 3311, the central cD galaxy of the Hydra I cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4#tablea1</TD>
            <TD>2011-11-24T08:02:25Z</TD>
            <TD>#Clusters_of_galaxies#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A4&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A4</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/379/1571 [1]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. IV (Aretxaga+, 2007)</TD>
            <TD>We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio-mm-far-infrared (FIR) colours of 120 robustly detected 850um sources in the Lockman Hole East (LH) and Subaru XMM-Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radiosub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571#1</TD>
            <TD>2011-09-14T20:30:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/379/1571</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/1571</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/379/1571 [2]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. IV (Aretxaga+, 2007)</TD>
            <TD>We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio-mm-far-infrared (FIR) colours of 120 robustly detected 850um sources in the Lockman Hole East (LH) and Subaru XMM-Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radiosub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571#2</TD>
            <TD>2011-09-14T20:30:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/379/1571&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/1571</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/379/1571 [data]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. IV (Aretxaga+, 2007)</TD>
            <TD>We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio-mm-far-infrared (FIR) colours of 120 robustly detected 850um sources in the Lockman Hole East (LH) and Subaru XMM-Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radiosub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571#data</TD>
            <TD>2011-09-14T20:30:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/379/1571&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/1571</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/531/A4 [1]</TD>
            <TD>Ultra compact dwarfs and globulars in Hya I (Misgeld+, 2011)</TD>
            <TD>VIMOS allows simultaneous observation of four quadrants in one telescope pointing. Each quadrant is of dimension 7'x8', with a gap of about 2' between the quadrants. For the UCD survey, we placed four multi-object spectroscopy (MOS) pointings around NGC 3311, the central cD galaxy of the Hydra I cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4#1</TD>
            <TD>2011-11-24T08:02:25Z</TD>
            <TD>#Clusters_of_galaxies#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/531/A4</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A4</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/531/A4 [2]</TD>
            <TD>Ultra compact dwarfs and globulars in Hya I (Misgeld+, 2011)</TD>
            <TD>VIMOS allows simultaneous observation of four quadrants in one telescope pointing. Each quadrant is of dimension 7'x8', with a gap of about 2' between the quadrants. For the UCD survey, we placed four multi-object spectroscopy (MOS) pointings around NGC 3311, the central cD galaxy of the Hydra I cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4#2</TD>
            <TD>2011-11-24T08:02:25Z</TD>
            <TD>#Clusters_of_galaxies#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/531/A4&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A4</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A4 [tablea1]</TD>
            <TD>Ultra compact dwarfs and globulars in Hya I (Misgeld+, 2011)</TD>
            <TD>VIMOS allows simultaneous observation of four quadrants in one telescope pointing. Each quadrant is of dimension 7'x8', with a gap of about 2' between the quadrants. For the UCD survey, we placed four multi-object spectroscopy (MOS) pointings around NGC 3311, the central cD galaxy of the Hydra I cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4#tablea1</TD>
            <TD>2011-11-24T08:02:25Z</TD>
            <TD>#Clusters_of_galaxies#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A4&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A4</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/531/A4 [1]</TD>
            <TD>Ultra compact dwarfs and globulars in Hya I (Misgeld+, 2011)</TD>
            <TD>VIMOS allows simultaneous observation of four quadrants in one telescope pointing. Each quadrant is of dimension 7'x8', with a gap of about 2' between the quadrants. For the UCD survey, we placed four multi-object spectroscopy (MOS) pointings around NGC 3311, the central cD galaxy of the Hydra I cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4#1</TD>
            <TD>2011-11-24T08:02:25Z</TD>
            <TD>#Clusters_of_galaxies#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/531/A4</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A4</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/531/A4 [2]</TD>
            <TD>Ultra compact dwarfs and globulars in Hya I (Misgeld+, 2011)</TD>
            <TD>VIMOS allows simultaneous observation of four quadrants in one telescope pointing. Each quadrant is of dimension 7'x8', with a gap of about 2' between the quadrants. For the UCD survey, we placed four multi-object spectroscopy (MOS) pointings around NGC 3311, the central cD galaxy of the Hydra I cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4#2</TD>
            <TD>2011-11-24T08:02:25Z</TD>
            <TD>#Clusters_of_galaxies#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/531/A4&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A4</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A4 [tablea1]</TD>
            <TD>Ultra compact dwarfs and globulars in Hya I (Misgeld+, 2011)</TD>
            <TD>VIMOS allows simultaneous observation of four quadrants in one telescope pointing. Each quadrant is of dimension 7'x8', with a gap of about 2' between the quadrants. For the UCD survey, we placed four multi-object spectroscopy (MOS) pointings around NGC 3311, the central cD galaxy of the Hydra I cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4#tablea1</TD>
            <TD>2011-11-24T08:02:25Z</TD>
            <TD>#Clusters_of_galaxies#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A4</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A4&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A4</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/379/1571 [1]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. IV (Aretxaga+, 2007)</TD>
            <TD>We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio-mm-far-infrared (FIR) colours of 120 robustly detected 850um sources in the Lockman Hole East (LH) and Subaru XMM-Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radiosub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571#1</TD>
            <TD>2011-09-14T20:30:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/379/1571</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/1571</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/379/1571 [2]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. IV (Aretxaga+, 2007)</TD>
            <TD>We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio-mm-far-infrared (FIR) colours of 120 robustly detected 850um sources in the Lockman Hole East (LH) and Subaru XMM-Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radiosub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571#2</TD>
            <TD>2011-09-14T20:30:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/379/1571&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/1571</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/379/1571 [data]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. IV (Aretxaga+, 2007)</TD>
            <TD>We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio-mm-far-infrared (FIR) colours of 120 robustly detected 850um sources in the Lockman Hole East (LH) and Subaru XMM-Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radiosub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571#data</TD>
            <TD>2011-09-14T20:30:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/379/1571&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/1571</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A55 [1]</TD>
            <TD>Deep XMM-Newton Survey of M31 (Stiele+, 2011)</TD>
            <TD>The largest Local Group spiral galaxy, M31, has been completely imaged for the first time, obtaining a luminosity lower limit about 10^35^erg/s in the 0.2-4.5keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D_25_ ellipse. The main goal of the paper is to study X-ray source populations of M31. An X-ray catalogue of 1897(*) sources was created with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. (*) the final catalog of table5 icludes 1948 sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55#1</TD>
            <TD>2011-12-04T13:50:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A55</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A55</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A55 [2]</TD>
            <TD>Deep XMM-Newton Survey of M31 (Stiele+, 2011)</TD>
            <TD>The largest Local Group spiral galaxy, M31, has been completely imaged for the first time, obtaining a luminosity lower limit about 10^35^erg/s in the 0.2-4.5keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D_25_ ellipse. The main goal of the paper is to study X-ray source populations of M31. An X-ray catalogue of 1897(*) sources was created with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. (*) the final catalog of table5 icludes 1948 sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55#2</TD>
            <TD>2011-12-04T13:50:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A55&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A55</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A55 [table5]</TD>
            <TD>Deep XMM-Newton Survey of M31 (Stiele+, 2011)</TD>
            <TD>The largest Local Group spiral galaxy, M31, has been completely imaged for the first time, obtaining a luminosity lower limit about 10^35^erg/s in the 0.2-4.5keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D_25_ ellipse. The main goal of the paper is to study X-ray source populations of M31. An X-ray catalogue of 1897(*) sources was created with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. (*) the final catalog of table5 icludes 1948 sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55#table5</TD>
            <TD>2011-12-04T13:50:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A55&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A55</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A55 [1]</TD>
            <TD>Deep XMM-Newton Survey of M31 (Stiele+, 2011)</TD>
            <TD>The largest Local Group spiral galaxy, M31, has been completely imaged for the first time, obtaining a luminosity lower limit about 10^35^erg/s in the 0.2-4.5keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D_25_ ellipse. The main goal of the paper is to study X-ray source populations of M31. An X-ray catalogue of 1897(*) sources was created with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. (*) the final catalog of table5 icludes 1948 sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55#1</TD>
            <TD>2011-12-04T13:50:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A55</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A55</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A55 [2]</TD>
            <TD>Deep XMM-Newton Survey of M31 (Stiele+, 2011)</TD>
            <TD>The largest Local Group spiral galaxy, M31, has been completely imaged for the first time, obtaining a luminosity lower limit about 10^35^erg/s in the 0.2-4.5keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D_25_ ellipse. The main goal of the paper is to study X-ray source populations of M31. An X-ray catalogue of 1897(*) sources was created with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. (*) the final catalog of table5 icludes 1948 sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55#2</TD>
            <TD>2011-12-04T13:50:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A55&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A55</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A55 [table5]</TD>
            <TD>Deep XMM-Newton Survey of M31 (Stiele+, 2011)</TD>
            <TD>The largest Local Group spiral galaxy, M31, has been completely imaged for the first time, obtaining a luminosity lower limit about 10^35^erg/s in the 0.2-4.5keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D_25_ ellipse. The main goal of the paper is to study X-ray source populations of M31. An X-ray catalogue of 1897(*) sources was created with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. (*) the final catalog of table5 icludes 1948 sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55#table5</TD>
            <TD>2011-12-04T13:50:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A55&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A55</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/379/1571 [1]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. IV (Aretxaga+, 2007)</TD>
            <TD>We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio-mm-far-infrared (FIR) colours of 120 robustly detected 850um sources in the Lockman Hole East (LH) and Subaru XMM-Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radiosub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571#1</TD>
            <TD>2011-09-14T20:30:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/379/1571</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/1571</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/379/1571 [2]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. IV (Aretxaga+, 2007)</TD>
            <TD>We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio-mm-far-infrared (FIR) colours of 120 robustly detected 850um sources in the Lockman Hole East (LH) and Subaru XMM-Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radiosub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571#2</TD>
            <TD>2011-09-14T20:30:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/379/1571&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/1571</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/379/1571 [data]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. IV (Aretxaga+, 2007)</TD>
            <TD>We present the redshift distribution of the Submillimetre Common-User Bolometer Array (SCUBA) Half Degree Survey (SHADES) galaxy population based on the rest-frame radio-mm-far-infrared (FIR) colours of 120 robustly detected 850um sources in the Lockman Hole East (LH) and Subaru XMM-Newton Deep Field (SXDF). The redshift distribution derived from the full spectral energy distribution (SED) information is shown to be narrower than that determined from the radiosub-mm spectral index, as more photometric bands contribute to a higher redshift accuracy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571#data</TD>
            <TD>2011-09-14T20:30:12Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/1571</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/379/1571&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/1571</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/534/A55 [1]</TD>
            <TD>Deep XMM-Newton Survey of M31 (Stiele+, 2011)</TD>
            <TD>The largest Local Group spiral galaxy, M31, has been completely imaged for the first time, obtaining a luminosity lower limit about 10^35^erg/s in the 0.2-4.5keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D_25_ ellipse. The main goal of the paper is to study X-ray source populations of M31. An X-ray catalogue of 1897(*) sources was created with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. (*) the final catalog of table5 icludes 1948 sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55#1</TD>
            <TD>2011-12-04T13:50:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/534/A55</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A55</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/534/A55 [2]</TD>
            <TD>Deep XMM-Newton Survey of M31 (Stiele+, 2011)</TD>
            <TD>The largest Local Group spiral galaxy, M31, has been completely imaged for the first time, obtaining a luminosity lower limit about 10^35^erg/s in the 0.2-4.5keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D_25_ ellipse. The main goal of the paper is to study X-ray source populations of M31. An X-ray catalogue of 1897(*) sources was created with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. (*) the final catalog of table5 icludes 1948 sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55#2</TD>
            <TD>2011-12-04T13:50:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/534/A55&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A55</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/534/A55 [table5]</TD>
            <TD>Deep XMM-Newton Survey of M31 (Stiele+, 2011)</TD>
            <TD>The largest Local Group spiral galaxy, M31, has been completely imaged for the first time, obtaining a luminosity lower limit about 10^35^erg/s in the 0.2-4.5keV band. Our XMM-Newton EPIC survey combines archival observations along the major axis, from June 2000 to July 2004, with observations taken between June 2006 and February 2008 that cover the remainder of the D_25_ ellipse. The main goal of the paper is to study X-ray source populations of M31. An X-ray catalogue of 1897(*) sources was created with 914 detected for the first time. Source classification and identification were based on X-ray hardness ratios, spatial extent of the sources, and cross correlation with catalogues in the X-ray, optical, infrared and radio wavelengths. We also analysed the long-term variability of the X-ray sources and this variability allows us to distinguish between X-ray binaries and active galactic nuclei (AGN). Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed us to detect additional transient or at least highly variable sources, which are good candidate X-ray binaries. (*) the final catalog of table5 icludes 1948 sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55#table5</TD>
            <TD>2011-12-04T13:50:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/534/A55</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/534/A55&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/534/A55</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1796 [1]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#1</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1796</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1796 [2]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#2</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1796&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1796 [table1]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#table1</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1796&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1796 [table4]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#table4</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1796&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/701/1219 [1]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#1</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/701/1219</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/701/1219 [2]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#2</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1219 [table4]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#table4</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1219 [table6]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#table6</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1219 [table5]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#table5</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1796 [1]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#1</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1796</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1796 [2]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#2</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1796&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1796 [table1]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#table1</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1796&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1796 [table4]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#table4</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1796&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/701/1219 [1]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#1</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/701/1219</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/701/1219 [2]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#2</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1219 [table4]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#table4</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1219 [table6]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#table6</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1219 [table5]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#table5</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1796 [1]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#1</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1796</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1796 [2]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#2</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1796&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1796 [table1]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#table1</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1796&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1796 [table4]</TD>
            <TD>Spectroscpy in nearby group cores (Carrasco+, 2006)</TD>
            <TD>The four groups studied were selected from the catalog of Garcia (1993, Cat.&lt;J/A+AS/100/47&gt;). The groups vary in richness and density, with galaxy populations that differ widely in morphological fractions. Some of their characteristics are described below.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796#table4</TD>
            <TD>2011-09-14T20:30:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1796</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1796&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1796</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/701/1219 [1]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#1</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/701/1219</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/701/1219 [2]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#2</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1219 [table4]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#table4</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1219 [table6]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#table6</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/701/1219 [table5]</TD>
            <TD>Galaxy survey in 3 QSO fields (Chen+, 2009)</TD>
            <TD>The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219#table5</TD>
            <TD>2011-12-13T14:05:31Z</TD>
            <TD>#Galaxies:spectra#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/701/1219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/701/1219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/701/1219</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/412/1419 [1]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#1</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/412/1419</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/412/1419 [2]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#2</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/412/1419&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/412/1419 [table2]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#table2</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/412/1419&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/412/1419 [table4]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#table4</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/412/1419&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/412/1419 [1]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#1</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/412/1419</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/412/1419 [2]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#2</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/412/1419&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/412/1419 [table2]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#table2</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/412/1419&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/412/1419 [table4]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#table4</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/412/1419&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/489/849 [1]</TD>
            <TD>Revised catalogue of EGRET gamma-ray sources (Casandjian+, 2008)</TD>
            <TD>We present a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. We used the entire gamma-ray dataset of reprocessed photons at energies above 100MeV and new Galactic interstellar emission models based on CO, HI, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. We applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue. The revised catalogue lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalogue. We do not detect 107 sources discovered previously because additional structure is present in the interstellar background.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849#1</TD>
            <TD>2011-09-14T20:31:33Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/489/849</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/849</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/489/849 [2]</TD>
            <TD>Revised catalogue of EGRET gamma-ray sources (Casandjian+, 2008)</TD>
            <TD>We present a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. We used the entire gamma-ray dataset of reprocessed photons at energies above 100MeV and new Galactic interstellar emission models based on CO, HI, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. We applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue. The revised catalogue lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalogue. We do not detect 107 sources discovered previously because additional structure is present in the interstellar background.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849#2</TD>
            <TD>2011-09-14T20:31:33Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/489/849&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/849</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/489/849 [egr]</TD>
            <TD>Revised catalogue of EGRET gamma-ray sources (Casandjian+, 2008)</TD>
            <TD>We present a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. We used the entire gamma-ray dataset of reprocessed photons at energies above 100MeV and new Galactic interstellar emission models based on CO, HI, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. We applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue. The revised catalogue lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalogue. We do not detect 107 sources discovered previously because additional structure is present in the interstellar background.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849#egr</TD>
            <TD>2011-09-14T20:31:33Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/489/849&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/849</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/489/849 [1]</TD>
            <TD>Revised catalogue of EGRET gamma-ray sources (Casandjian+, 2008)</TD>
            <TD>We present a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. We used the entire gamma-ray dataset of reprocessed photons at energies above 100MeV and new Galactic interstellar emission models based on CO, HI, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. We applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue. The revised catalogue lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalogue. We do not detect 107 sources discovered previously because additional structure is present in the interstellar background.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849#1</TD>
            <TD>2011-09-14T20:31:33Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/489/849</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/849</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/489/849 [2]</TD>
            <TD>Revised catalogue of EGRET gamma-ray sources (Casandjian+, 2008)</TD>
            <TD>We present a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. We used the entire gamma-ray dataset of reprocessed photons at energies above 100MeV and new Galactic interstellar emission models based on CO, HI, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. We applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue. The revised catalogue lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalogue. We do not detect 107 sources discovered previously because additional structure is present in the interstellar background.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849#2</TD>
            <TD>2011-09-14T20:31:33Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/489/849&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/849</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/489/849 [egr]</TD>
            <TD>Revised catalogue of EGRET gamma-ray sources (Casandjian+, 2008)</TD>
            <TD>We present a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. We used the entire gamma-ray dataset of reprocessed photons at energies above 100MeV and new Galactic interstellar emission models based on CO, HI, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. We applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue. The revised catalogue lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalogue. We do not detect 107 sources discovered previously because additional structure is present in the interstellar background.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849#egr</TD>
            <TD>2011-09-14T20:31:33Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/489/849&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/849</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/412/1419 [1]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#1</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/412/1419</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/412/1419 [2]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#2</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/412/1419&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/412/1419 [table2]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#table2</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/412/1419&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/412/1419 [table4]</TD>
            <TD>Nearby supernova rates (Leaman+, 2011)</TD>
            <TD>The requirement to have the Hubble type and photometry results in further cuts to our galaxy sample, and our final sample has 14882 galaxies (hereinafter the "full" galaxy sample). All of the galaxies in this sample have Hubble-type information, 98.6 per cent have B-band photometry and 91.8 per cent have K-band photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419#table4</TD>
            <TD>2011-12-19T10:28:46Z</TD>
            <TD>#Photometry#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/412/1419</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/412/1419&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/412/1419</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/489/849 [1]</TD>
            <TD>Revised catalogue of EGRET gamma-ray sources (Casandjian+, 2008)</TD>
            <TD>We present a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. We used the entire gamma-ray dataset of reprocessed photons at energies above 100MeV and new Galactic interstellar emission models based on CO, HI, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. We applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue. The revised catalogue lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalogue. We do not detect 107 sources discovered previously because additional structure is present in the interstellar background.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849#1</TD>
            <TD>2011-09-14T20:31:33Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/489/849</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/849</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/489/849 [2]</TD>
            <TD>Revised catalogue of EGRET gamma-ray sources (Casandjian+, 2008)</TD>
            <TD>We present a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. We used the entire gamma-ray dataset of reprocessed photons at energies above 100MeV and new Galactic interstellar emission models based on CO, HI, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. We applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue. The revised catalogue lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalogue. We do not detect 107 sources discovered previously because additional structure is present in the interstellar background.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849#2</TD>
            <TD>2011-09-14T20:31:33Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/489/849&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/849</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/489/849 [egr]</TD>
            <TD>Revised catalogue of EGRET gamma-ray sources (Casandjian+, 2008)</TD>
            <TD>We present a catalog of point gamma-ray sources detected by the EGRET detector on the Compton Gamma Ray Observatory. We used the entire gamma-ray dataset of reprocessed photons at energies above 100MeV and new Galactic interstellar emission models based on CO, HI, dark gas, and interstellar radiation field data. Two different assumptions are used to describe the cosmic-ray distribution in the Galaxy to analyse the systematic uncertainties in source detection and characterization. We applied a 2-dimensional maximum-likelihood detection method similar to that used to analyze the 3rd EGRET catalogue. The revised catalogue lists 188 sources, 14 of which are marked as confused, in contrast to the 271 entries of the 3rd EGRET (3EG) catalogue. We do not detect 107 sources discovered previously because additional structure is present in the interstellar background.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849#egr</TD>
            <TD>2011-09-14T20:31:33Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/849</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/489/849&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/849</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/399/2146 [1]</TD>
            <TD>Orbits of open clusters in the Galaxy (Wu+, 2009)</TD>
            <TD>We present and analyse the kinematics and orbits for a sample of 488 open clusters (OCs) in the Galaxy. The velocity ellipsoid for our present sample is derived as ({sigma}(U),{sigma}(V),{sigma}(W)) = (28.7, 15.8, 11.0)km/s which represents a young thin-disc population. We also confirm that the velocity dispersions increase with the age of a cluster subsample. The orbits of OCs are calculated with three Galactic gravitational potential models. The errors of orbital parameters are also calculated considering the intrinsic variation of the orbital parameters and the effects of observational uncertainties. The observational uncertainties dominate the errors of derived orbital parameters. The vertical motions of clusters calculated using different Galactic disc models are rather different. The observed radial metallicity gradient of clusters is derived with a slope of b=-0.070+/-0.011dex/kpc. The radial metallicity gradient of clusters based on their apogalactic distances is also derived with a slope of b=-0.082+/-0.014dex/kpc. The distribution of derived orbital eccentricities for OCs is very similar to that derived for the field population of dwarfs and giants in the thin disc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146#1</TD>
            <TD>2012-01-12T08:14:26Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/399/2146</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/399/2146</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/399/2146 [2]</TD>
            <TD>Orbits of open clusters in the Galaxy (Wu+, 2009)</TD>
            <TD>We present and analyse the kinematics and orbits for a sample of 488 open clusters (OCs) in the Galaxy. The velocity ellipsoid for our present sample is derived as ({sigma}(U),{sigma}(V),{sigma}(W)) = (28.7, 15.8, 11.0)km/s which represents a young thin-disc population. We also confirm that the velocity dispersions increase with the age of a cluster subsample. The orbits of OCs are calculated with three Galactic gravitational potential models. The errors of orbital parameters are also calculated considering the intrinsic variation of the orbital parameters and the effects of observational uncertainties. The observational uncertainties dominate the errors of derived orbital parameters. The vertical motions of clusters calculated using different Galactic disc models are rather different. The observed radial metallicity gradient of clusters is derived with a slope of b=-0.070+/-0.011dex/kpc. The radial metallicity gradient of clusters based on their apogalactic distances is also derived with a slope of b=-0.082+/-0.014dex/kpc. The distribution of derived orbital eccentricities for OCs is very similar to that derived for the field population of dwarfs and giants in the thin disc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146#2</TD>
            <TD>2012-01-12T08:14:26Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/399/2146&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/399/2146</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/399/2146 [clusters]</TD>
            <TD>Orbits of open clusters in the Galaxy (Wu+, 2009)</TD>
            <TD>We present and analyse the kinematics and orbits for a sample of 488 open clusters (OCs) in the Galaxy. The velocity ellipsoid for our present sample is derived as ({sigma}(U),{sigma}(V),{sigma}(W)) = (28.7, 15.8, 11.0)km/s which represents a young thin-disc population. We also confirm that the velocity dispersions increase with the age of a cluster subsample. The orbits of OCs are calculated with three Galactic gravitational potential models. The errors of orbital parameters are also calculated considering the intrinsic variation of the orbital parameters and the effects of observational uncertainties. The observational uncertainties dominate the errors of derived orbital parameters. The vertical motions of clusters calculated using different Galactic disc models are rather different. The observed radial metallicity gradient of clusters is derived with a slope of b=-0.070+/-0.011dex/kpc. The radial metallicity gradient of clusters based on their apogalactic distances is also derived with a slope of b=-0.082+/-0.014dex/kpc. The distribution of derived orbital eccentricities for OCs is very similar to that derived for the field population of dwarfs and giants in the thin disc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146#clusters</TD>
            <TD>2012-01-12T08:14:26Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/399/2146&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/399/2146</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/510/A39 [1]</TD>
            <TD>CoRoT light curves of V1127 Aql (Chadid+, 2010)</TD>
            <TD>Frequencies, Fourier amplitudes, phases, spectral significances and identification of the frequencies of the CoRoT light curve of the RR Lyrae star V1127 Aql - CoRoT ID:0100689962 - during 143 days in the First Long Run Center of Milky Way. The CoRoT data used in this study are the calibrated light curves, N2-level, that have been measured by the CoRoT Exoplanet CCDs during the first long run in the centre direction of Galaxy. The total time span is 143days. The time sampling of the light curves is 32s, an average is taken on board over 16 such measurements and resulting in a nominal sampling time of 512s. We used here the resulting "white" flux.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A39#1</TD>
            <TD>2011-09-14T21:08:05Z</TD>
            <TD>#Spectroscopy#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A39</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/510/A39</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A39</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/510/A39 [2]</TD>
            <TD>CoRoT light curves of V1127 Aql (Chadid+, 2010)</TD>
            <TD>Frequencies, Fourier amplitudes, phases, spectral significances and identification of the frequencies of the CoRoT light curve of the RR Lyrae star V1127 Aql - CoRoT ID:0100689962 - during 143 days in the First Long Run Center of Milky Way. The CoRoT data used in this study are the calibrated light curves, N2-level, that have been measured by the CoRoT Exoplanet CCDs during the first long run in the centre direction of Galaxy. The total time span is 143days. The time sampling of the light curves is 32s, an average is taken on board over 16 such measurements and resulting in a nominal sampling time of 512s. We used here the resulting "white" flux.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A39#2</TD>
            <TD>2011-09-14T21:08:05Z</TD>
            <TD>#Spectroscopy#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A39</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/510/A39&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A39</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/399/2146 [1]</TD>
            <TD>Orbits of open clusters in the Galaxy (Wu+, 2009)</TD>
            <TD>We present and analyse the kinematics and orbits for a sample of 488 open clusters (OCs) in the Galaxy. The velocity ellipsoid for our present sample is derived as ({sigma}(U),{sigma}(V),{sigma}(W)) = (28.7, 15.8, 11.0)km/s which represents a young thin-disc population. We also confirm that the velocity dispersions increase with the age of a cluster subsample. The orbits of OCs are calculated with three Galactic gravitational potential models. The errors of orbital parameters are also calculated considering the intrinsic variation of the orbital parameters and the effects of observational uncertainties. The observational uncertainties dominate the errors of derived orbital parameters. The vertical motions of clusters calculated using different Galactic disc models are rather different. The observed radial metallicity gradient of clusters is derived with a slope of b=-0.070+/-0.011dex/kpc. The radial metallicity gradient of clusters based on their apogalactic distances is also derived with a slope of b=-0.082+/-0.014dex/kpc. The distribution of derived orbital eccentricities for OCs is very similar to that derived for the field population of dwarfs and giants in the thin disc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146#1</TD>
            <TD>2012-01-12T08:14:26Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/399/2146</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/399/2146</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/399/2146 [2]</TD>
            <TD>Orbits of open clusters in the Galaxy (Wu+, 2009)</TD>
            <TD>We present and analyse the kinematics and orbits for a sample of 488 open clusters (OCs) in the Galaxy. The velocity ellipsoid for our present sample is derived as ({sigma}(U),{sigma}(V),{sigma}(W)) = (28.7, 15.8, 11.0)km/s which represents a young thin-disc population. We also confirm that the velocity dispersions increase with the age of a cluster subsample. The orbits of OCs are calculated with three Galactic gravitational potential models. The errors of orbital parameters are also calculated considering the intrinsic variation of the orbital parameters and the effects of observational uncertainties. The observational uncertainties dominate the errors of derived orbital parameters. The vertical motions of clusters calculated using different Galactic disc models are rather different. The observed radial metallicity gradient of clusters is derived with a slope of b=-0.070+/-0.011dex/kpc. The radial metallicity gradient of clusters based on their apogalactic distances is also derived with a slope of b=-0.082+/-0.014dex/kpc. The distribution of derived orbital eccentricities for OCs is very similar to that derived for the field population of dwarfs and giants in the thin disc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146#2</TD>
            <TD>2012-01-12T08:14:26Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/399/2146&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/399/2146</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/399/2146 [clusters]</TD>
            <TD>Orbits of open clusters in the Galaxy (Wu+, 2009)</TD>
            <TD>We present and analyse the kinematics and orbits for a sample of 488 open clusters (OCs) in the Galaxy. The velocity ellipsoid for our present sample is derived as ({sigma}(U),{sigma}(V),{sigma}(W)) = (28.7, 15.8, 11.0)km/s which represents a young thin-disc population. We also confirm that the velocity dispersions increase with the age of a cluster subsample. The orbits of OCs are calculated with three Galactic gravitational potential models. The errors of orbital parameters are also calculated considering the intrinsic variation of the orbital parameters and the effects of observational uncertainties. The observational uncertainties dominate the errors of derived orbital parameters. The vertical motions of clusters calculated using different Galactic disc models are rather different. The observed radial metallicity gradient of clusters is derived with a slope of b=-0.070+/-0.011dex/kpc. The radial metallicity gradient of clusters based on their apogalactic distances is also derived with a slope of b=-0.082+/-0.014dex/kpc. The distribution of derived orbital eccentricities for OCs is very similar to that derived for the field population of dwarfs and giants in the thin disc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146#clusters</TD>
            <TD>2012-01-12T08:14:26Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/399/2146&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/399/2146</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>TWOMASSRSC [1]</TD>
            <TD>2MASS Redshift Survey (2MRS) Catalog</TD>
            <TD>This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and |b| &gt;= 5 degrees (&gt;= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.25 mag and |b| &gt;= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: &lt;pre&gt; K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and detected at H, E(B - V) &lt;= 1 mag, |b| &gt;= 5 degrees for 30 degrees &lt; l &lt; 330 degrees, |b| &gt;= 8 degrees otherwise. &lt;/pre&gt; They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/twomassrsc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/twomassrsc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=twomassrsc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/twomassrsc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>TWOMASSRSC [2]</TD>
            <TD>2MASS Redshift Survey (2MRS) Catalog</TD>
            <TD>This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and |b| &gt;= 5 degrees (&gt;= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.25 mag and |b| &gt;= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: &lt;pre&gt; K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and detected at H, E(B - V) &lt;= 1 mag, |b| &gt;= 5 degrees for 30 degrees &lt; l &lt; 330 degrees, |b| &gt;= 8 degrees otherwise. &lt;/pre&gt; They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/twomassrsc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/twomassrsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=twomassrsc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/twomassrsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>TWOMASSRSC [3]</TD>
            <TD>2MASS Redshift Survey (2MRS) Catalog</TD>
            <TD>This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and |b| &gt;= 5 degrees (&gt;= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h&lt;sup&gt;-1&lt;/sup&gt; Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.25 mag and |b| &gt;= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: &lt;pre&gt; K&lt;sub&gt;s&lt;/sub&gt; &lt;= 11.75 mag and detected at H, E(B - V) &lt;= 1 mag, |b| &gt;= 5 degrees for 30 degrees &lt; l &lt; 330 degrees, |b| &gt;= 8 degrees otherwise. &lt;/pre&gt; They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/twomassrsc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/twomassrsc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_twomassrsc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/twomassrsc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/510/A39 [1]</TD>
            <TD>CoRoT light curves of V1127 Aql (Chadid+, 2010)</TD>
            <TD>Frequencies, Fourier amplitudes, phases, spectral significances and identification of the frequencies of the CoRoT light curve of the RR Lyrae star V1127 Aql - CoRoT ID:0100689962 - during 143 days in the First Long Run Center of Milky Way. The CoRoT data used in this study are the calibrated light curves, N2-level, that have been measured by the CoRoT Exoplanet CCDs during the first long run in the centre direction of Galaxy. The total time span is 143days. The time sampling of the light curves is 32s, an average is taken on board over 16 such measurements and resulting in a nominal sampling time of 512s. We used here the resulting "white" flux.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A39#1</TD>
            <TD>2011-09-14T21:08:05Z</TD>
            <TD>#Spectroscopy#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A39</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/510/A39</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A39</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/510/A39 [2]</TD>
            <TD>CoRoT light curves of V1127 Aql (Chadid+, 2010)</TD>
            <TD>Frequencies, Fourier amplitudes, phases, spectral significances and identification of the frequencies of the CoRoT light curve of the RR Lyrae star V1127 Aql - CoRoT ID:0100689962 - during 143 days in the First Long Run Center of Milky Way. The CoRoT data used in this study are the calibrated light curves, N2-level, that have been measured by the CoRoT Exoplanet CCDs during the first long run in the centre direction of Galaxy. The total time span is 143days. The time sampling of the light curves is 32s, an average is taken on board over 16 such measurements and resulting in a nominal sampling time of 512s. We used here the resulting "white" flux.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A39#2</TD>
            <TD>2011-09-14T21:08:05Z</TD>
            <TD>#Spectroscopy#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/510/A39</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/510/A39&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/510/A39</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/399/2146 [1]</TD>
            <TD>Orbits of open clusters in the Galaxy (Wu+, 2009)</TD>
            <TD>We present and analyse the kinematics and orbits for a sample of 488 open clusters (OCs) in the Galaxy. The velocity ellipsoid for our present sample is derived as ({sigma}(U),{sigma}(V),{sigma}(W)) = (28.7, 15.8, 11.0)km/s which represents a young thin-disc population. We also confirm that the velocity dispersions increase with the age of a cluster subsample. The orbits of OCs are calculated with three Galactic gravitational potential models. The errors of orbital parameters are also calculated considering the intrinsic variation of the orbital parameters and the effects of observational uncertainties. The observational uncertainties dominate the errors of derived orbital parameters. The vertical motions of clusters calculated using different Galactic disc models are rather different. The observed radial metallicity gradient of clusters is derived with a slope of b=-0.070+/-0.011dex/kpc. The radial metallicity gradient of clusters based on their apogalactic distances is also derived with a slope of b=-0.082+/-0.014dex/kpc. The distribution of derived orbital eccentricities for OCs is very similar to that derived for the field population of dwarfs and giants in the thin disc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146#1</TD>
            <TD>2012-01-12T08:14:26Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/399/2146</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/399/2146</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/399/2146 [2]</TD>
            <TD>Orbits of open clusters in the Galaxy (Wu+, 2009)</TD>
            <TD>We present and analyse the kinematics and orbits for a sample of 488 open clusters (OCs) in the Galaxy. The velocity ellipsoid for our present sample is derived as ({sigma}(U),{sigma}(V),{sigma}(W)) = (28.7, 15.8, 11.0)km/s which represents a young thin-disc population. We also confirm that the velocity dispersions increase with the age of a cluster subsample. The orbits of OCs are calculated with three Galactic gravitational potential models. The errors of orbital parameters are also calculated considering the intrinsic variation of the orbital parameters and the effects of observational uncertainties. The observational uncertainties dominate the errors of derived orbital parameters. The vertical motions of clusters calculated using different Galactic disc models are rather different. The observed radial metallicity gradient of clusters is derived with a slope of b=-0.070+/-0.011dex/kpc. The radial metallicity gradient of clusters based on their apogalactic distances is also derived with a slope of b=-0.082+/-0.014dex/kpc. The distribution of derived orbital eccentricities for OCs is very similar to that derived for the field population of dwarfs and giants in the thin disc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146#2</TD>
            <TD>2012-01-12T08:14:26Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/399/2146&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/399/2146</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/399/2146 [clusters]</TD>
            <TD>Orbits of open clusters in the Galaxy (Wu+, 2009)</TD>
            <TD>We present and analyse the kinematics and orbits for a sample of 488 open clusters (OCs) in the Galaxy. The velocity ellipsoid for our present sample is derived as ({sigma}(U),{sigma}(V),{sigma}(W)) = (28.7, 15.8, 11.0)km/s which represents a young thin-disc population. We also confirm that the velocity dispersions increase with the age of a cluster subsample. The orbits of OCs are calculated with three Galactic gravitational potential models. The errors of orbital parameters are also calculated considering the intrinsic variation of the orbital parameters and the effects of observational uncertainties. The observational uncertainties dominate the errors of derived orbital parameters. The vertical motions of clusters calculated using different Galactic disc models are rather different. The observed radial metallicity gradient of clusters is derived with a slope of b=-0.070+/-0.011dex/kpc. The radial metallicity gradient of clusters based on their apogalactic distances is also derived with a slope of b=-0.082+/-0.014dex/kpc. The distribution of derived orbital eccentricities for OCs is very similar to that derived for the field population of dwarfs and giants in the thin disc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146#clusters</TD>
            <TD>2012-01-12T08:14:26Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/399/2146</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/399/2146&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/399/2146</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WSRTGP [1]</TD>
            <TD>WSRT Galactic Plane Compact 327-MHz Source Catalog</TD>
            <TD>The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| &lt; 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parameterized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity &gt; 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis &lt; 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct nonthermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at &lt;a href="http://www.ras.ucalgary.ca/wsrt_survey.html"&gt;http://www.ras.ucalgary.ca/wsrt_survey.html&lt;/a&gt; for the WSRTGP images (JPEG, Postscript and and FITS formats).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/wsrtgp#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wsrtgp</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=wsrtgp&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/wsrtgp.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WSRTGP [2]</TD>
            <TD>WSRT Galactic Plane Compact 327-MHz Source Catalog</TD>
            <TD>The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| &lt; 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parameterized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity &gt; 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis &lt; 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct nonthermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at &lt;a href="http://www.ras.ucalgary.ca/wsrt_survey.html"&gt;http://www.ras.ucalgary.ca/wsrt_survey.html&lt;/a&gt; for the WSRTGP images (JPEG, Postscript and and FITS formats).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/wsrtgp#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wsrtgp</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=wsrtgp&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/wsrtgp.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WSRTGP [3]</TD>
            <TD>WSRT Galactic Plane Compact 327-MHz Source Catalog</TD>
            <TD>The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| &lt; 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parameterized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity &gt; 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis &lt; 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct nonthermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at &lt;a href="http://www.ras.ucalgary.ca/wsrt_survey.html"&gt;http://www.ras.ucalgary.ca/wsrt_survey.html&lt;/a&gt; for the WSRTGP images (JPEG, Postscript and and FITS formats).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/wsrtgp#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wsrtgp</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_wsrtgp&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/wsrtgp.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/507/131 [1]</TD>
            <TD>BzJK observations around radio galaxies (Galametz+, 2009)</TD>
            <TD>We imaged the two targets using the Bessel B-band filter of the Large Format Camera (LFC) on the Palomar 5m Hale Telescope. We imaged the radio galaxy fields using the z-band filter of Palomar/LFC. In February 2005, we observed 7C 1751+6809 for 60-min under photometric conditions. In August 2005, we observed 7C 1756+6520 for 135-min but in non-photometric conditions. The tables provide the B, z, J and Ks magnitudes and coordinates of the pBzK* galaxies (red passively evolving candidates selected by BzK=(z-K)-(B-z)&lt;-0.2 and (z-K)&gt;2.2) for both fields. The B and z bands were obtained using the Large Format Camera (LFC) on the Palomar 5m Hale Telescope, and the J and Ks bands using Wide-field Infrared Camera (WIRCAM) of the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131#1</TD>
            <TD>2011-09-14T21:08:20Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/507/131</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/131</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/507/131 [2]</TD>
            <TD>BzJK observations around radio galaxies (Galametz+, 2009)</TD>
            <TD>We imaged the two targets using the Bessel B-band filter of the Large Format Camera (LFC) on the Palomar 5m Hale Telescope. We imaged the radio galaxy fields using the z-band filter of Palomar/LFC. In February 2005, we observed 7C 1751+6809 for 60-min under photometric conditions. In August 2005, we observed 7C 1756+6520 for 135-min but in non-photometric conditions. The tables provide the B, z, J and Ks magnitudes and coordinates of the pBzK* galaxies (red passively evolving candidates selected by BzK=(z-K)-(B-z)&lt;-0.2 and (z-K)&gt;2.2) for both fields. The B and z bands were obtained using the Large Format Camera (LFC) on the Palomar 5m Hale Telescope, and the J and Ks bands using Wide-field Infrared Camera (WIRCAM) of the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131#2</TD>
            <TD>2011-09-14T21:08:20Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/507/131&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/507/131 [pBzKs]</TD>
            <TD>BzJK observations around radio galaxies (Galametz+, 2009)</TD>
            <TD>We imaged the two targets using the Bessel B-band filter of the Large Format Camera (LFC) on the Palomar 5m Hale Telescope. We imaged the radio galaxy fields using the z-band filter of Palomar/LFC. In February 2005, we observed 7C 1751+6809 for 60-min under photometric conditions. In August 2005, we observed 7C 1756+6520 for 135-min but in non-photometric conditions. The tables provide the B, z, J and Ks magnitudes and coordinates of the pBzK* galaxies (red passively evolving candidates selected by BzK=(z-K)-(B-z)&lt;-0.2 and (z-K)&gt;2.2) for both fields. The B and z bands were obtained using the Large Format Camera (LFC) on the Palomar 5m Hale Telescope, and the J and Ks bands using Wide-field Infrared Camera (WIRCAM) of the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131#pBzKs</TD>
            <TD>2011-09-14T21:08:20Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/507/131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/131</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/420/926 [1]</TD>
            <TD>Morphology of galaxies in WINGS clusters (Fasano+, 2012)</TD>
            <TD>Morphological types for 39923 galaxies in 76 clusters of the WINGS survey are presented. The morphology has been mostly estimated using the automatic tool MORPHOT, while for ~3000 galaxies visual estimates are also provided. For each galaxy we give a Maximum Likelihood, a Neural Network and a final estimate of the morphological type, together with the corresponding confidence intervals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926#1</TD>
            <TD>2012-01-31T10:24:36Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/420/926</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/926</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/420/926 [2]</TD>
            <TD>Morphology of galaxies in WINGS clusters (Fasano+, 2012)</TD>
            <TD>Morphological types for 39923 galaxies in 76 clusters of the WINGS survey are presented. The morphology has been mostly estimated using the automatic tool MORPHOT, while for ~3000 galaxies visual estimates are also provided. For each galaxy we give a Maximum Likelihood, a Neural Network and a final estimate of the morphological type, together with the corresponding confidence intervals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926#2</TD>
            <TD>2012-01-31T10:24:36Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/420/926&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/926</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/420/926 [morphot]</TD>
            <TD>Morphology of galaxies in WINGS clusters (Fasano+, 2012)</TD>
            <TD>Morphological types for 39923 galaxies in 76 clusters of the WINGS survey are presented. The morphology has been mostly estimated using the automatic tool MORPHOT, while for ~3000 galaxies visual estimates are also provided. For each galaxy we give a Maximum Likelihood, a Neural Network and a final estimate of the morphological type, together with the corresponding confidence intervals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926#morphot</TD>
            <TD>2012-01-31T10:24:36Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/420/926&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/926</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WSRTGP [1]</TD>
            <TD>WSRT Galactic Plane Compact 327-MHz Source Catalog</TD>
            <TD>The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| &lt; 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parameterized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity &gt; 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis &lt; 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct nonthermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at &lt;a href="http://www.ras.ucalgary.ca/wsrt_survey.html"&gt;http://www.ras.ucalgary.ca/wsrt_survey.html&lt;/a&gt; for the WSRTGP images (JPEG, Postscript and and FITS formats).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/wsrtgp#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wsrtgp</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=wsrtgp&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/wsrtgp.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WSRTGP [2]</TD>
            <TD>WSRT Galactic Plane Compact 327-MHz Source Catalog</TD>
            <TD>The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| &lt; 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parameterized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity &gt; 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis &lt; 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct nonthermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at &lt;a href="http://www.ras.ucalgary.ca/wsrt_survey.html"&gt;http://www.ras.ucalgary.ca/wsrt_survey.html&lt;/a&gt; for the WSRTGP images (JPEG, Postscript and and FITS formats).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/wsrtgp#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wsrtgp</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=wsrtgp&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/wsrtgp.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WSRTGP [3]</TD>
            <TD>WSRT Galactic Plane Compact 327-MHz Source Catalog</TD>
            <TD>The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| &lt; 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parameterized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity &gt; 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis &lt; 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct nonthermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at &lt;a href="http://www.ras.ucalgary.ca/wsrt_survey.html"&gt;http://www.ras.ucalgary.ca/wsrt_survey.html&lt;/a&gt; for the WSRTGP images (JPEG, Postscript and and FITS formats).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/wsrtgp#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wsrtgp</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_wsrtgp&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/wsrtgp.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/420/926 [1]</TD>
            <TD>Morphology of galaxies in WINGS clusters (Fasano+, 2012)</TD>
            <TD>Morphological types for 39923 galaxies in 76 clusters of the WINGS survey are presented. The morphology has been mostly estimated using the automatic tool MORPHOT, while for ~3000 galaxies visual estimates are also provided. For each galaxy we give a Maximum Likelihood, a Neural Network and a final estimate of the morphological type, together with the corresponding confidence intervals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926#1</TD>
            <TD>2012-01-31T10:24:36Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/420/926</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/926</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/420/926 [2]</TD>
            <TD>Morphology of galaxies in WINGS clusters (Fasano+, 2012)</TD>
            <TD>Morphological types for 39923 galaxies in 76 clusters of the WINGS survey are presented. The morphology has been mostly estimated using the automatic tool MORPHOT, while for ~3000 galaxies visual estimates are also provided. For each galaxy we give a Maximum Likelihood, a Neural Network and a final estimate of the morphological type, together with the corresponding confidence intervals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926#2</TD>
            <TD>2012-01-31T10:24:36Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/420/926&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/926</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/420/926 [morphot]</TD>
            <TD>Morphology of galaxies in WINGS clusters (Fasano+, 2012)</TD>
            <TD>Morphological types for 39923 galaxies in 76 clusters of the WINGS survey are presented. The morphology has been mostly estimated using the automatic tool MORPHOT, while for ~3000 galaxies visual estimates are also provided. For each galaxy we give a Maximum Likelihood, a Neural Network and a final estimate of the morphological type, together with the corresponding confidence intervals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926#morphot</TD>
            <TD>2012-01-31T10:24:36Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/420/926&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/926</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/420/926 [1]</TD>
            <TD>Morphology of galaxies in WINGS clusters (Fasano+, 2012)</TD>
            <TD>Morphological types for 39923 galaxies in 76 clusters of the WINGS survey are presented. The morphology has been mostly estimated using the automatic tool MORPHOT, while for ~3000 galaxies visual estimates are also provided. For each galaxy we give a Maximum Likelihood, a Neural Network and a final estimate of the morphological type, together with the corresponding confidence intervals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926#1</TD>
            <TD>2012-01-31T10:24:36Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/420/926</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/926</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/420/926 [2]</TD>
            <TD>Morphology of galaxies in WINGS clusters (Fasano+, 2012)</TD>
            <TD>Morphological types for 39923 galaxies in 76 clusters of the WINGS survey are presented. The morphology has been mostly estimated using the automatic tool MORPHOT, while for ~3000 galaxies visual estimates are also provided. For each galaxy we give a Maximum Likelihood, a Neural Network and a final estimate of the morphological type, together with the corresponding confidence intervals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926#2</TD>
            <TD>2012-01-31T10:24:36Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/420/926&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/926</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/420/926 [morphot]</TD>
            <TD>Morphology of galaxies in WINGS clusters (Fasano+, 2012)</TD>
            <TD>Morphological types for 39923 galaxies in 76 clusters of the WINGS survey are presented. The morphology has been mostly estimated using the automatic tool MORPHOT, while for ~3000 galaxies visual estimates are also provided. For each galaxy we give a Maximum Likelihood, a Neural Network and a final estimate of the morphological type, together with the corresponding confidence intervals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926#morphot</TD>
            <TD>2012-01-31T10:24:36Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/926</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/420/926&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/926</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/174 [1]</TD>
            <TD>Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980)</TD>
            <TD>Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/174#1</TD>
            <TD>2012-11-13T06:49:07Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/174</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/174</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/174</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/174 [2]</TD>
            <TD>Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980)</TD>
            <TD>Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/174#2</TD>
            <TD>2012-11-13T06:49:07Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/174</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/174&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/174</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/174 [table2]</TD>
            <TD>Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980)</TD>
            <TD>Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/174#table2</TD>
            <TD>2012-11-13T06:49:07Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/174</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/174&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/174</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/121 [1]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#1</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/121</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/121 [2]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#2</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/121&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/121 [sa189]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#sa189</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/121 [sa141]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#sa141</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/121 [sa127]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#sa127</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/174 [1]</TD>
            <TD>Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980)</TD>
            <TD>Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/174#1</TD>
            <TD>2012-11-13T06:49:07Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/174</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/174</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/174</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/174 [2]</TD>
            <TD>Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980)</TD>
            <TD>Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/174#2</TD>
            <TD>2012-11-13T06:49:07Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/174</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/174&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/174</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/174 [table2]</TD>
            <TD>Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980)</TD>
            <TD>Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/174#table2</TD>
            <TD>2012-11-13T06:49:07Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/174</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/174&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/174</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/174 [1]</TD>
            <TD>Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980)</TD>
            <TD>Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/174#1</TD>
            <TD>2012-11-13T06:49:07Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/174</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/174</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/174</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/174 [2]</TD>
            <TD>Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980)</TD>
            <TD>Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/174#2</TD>
            <TD>2012-11-13T06:49:07Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/174</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/174&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/174</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/174 [table2]</TD>
            <TD>Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980)</TD>
            <TD>Data are presented from a study of 55 rich clusters of galaxies. The data include positions, morphological types, estimated total magnitudes, bulge sizes, and ellipticities for ~6000 galaxies, as determined from high scale photographic plates. data reduction procedures are described, and a brief analysis of cluster richness, which indicates that Abell richness classes are only rough indicators of total cluster membership, is included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/174#table2</TD>
            <TD>2012-11-13T06:49:07Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/174</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/174&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/174</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/507/131 [1]</TD>
            <TD>BzJK observations around radio galaxies (Galametz+, 2009)</TD>
            <TD>We imaged the two targets using the Bessel B-band filter of the Large Format Camera (LFC) on the Palomar 5m Hale Telescope. We imaged the radio galaxy fields using the z-band filter of Palomar/LFC. In February 2005, we observed 7C 1751+6809 for 60-min under photometric conditions. In August 2005, we observed 7C 1756+6520 for 135-min but in non-photometric conditions. The tables provide the B, z, J and Ks magnitudes and coordinates of the pBzK* galaxies (red passively evolving candidates selected by BzK=(z-K)-(B-z)&lt;-0.2 and (z-K)&gt;2.2) for both fields. The B and z bands were obtained using the Large Format Camera (LFC) on the Palomar 5m Hale Telescope, and the J and Ks bands using Wide-field Infrared Camera (WIRCAM) of the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131#1</TD>
            <TD>2011-09-14T21:08:20Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/507/131</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/131</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/507/131 [2]</TD>
            <TD>BzJK observations around radio galaxies (Galametz+, 2009)</TD>
            <TD>We imaged the two targets using the Bessel B-band filter of the Large Format Camera (LFC) on the Palomar 5m Hale Telescope. We imaged the radio galaxy fields using the z-band filter of Palomar/LFC. In February 2005, we observed 7C 1751+6809 for 60-min under photometric conditions. In August 2005, we observed 7C 1756+6520 for 135-min but in non-photometric conditions. The tables provide the B, z, J and Ks magnitudes and coordinates of the pBzK* galaxies (red passively evolving candidates selected by BzK=(z-K)-(B-z)&lt;-0.2 and (z-K)&gt;2.2) for both fields. The B and z bands were obtained using the Large Format Camera (LFC) on the Palomar 5m Hale Telescope, and the J and Ks bands using Wide-field Infrared Camera (WIRCAM) of the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131#2</TD>
            <TD>2011-09-14T21:08:20Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/507/131&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/507/131 [pBzKs]</TD>
            <TD>BzJK observations around radio galaxies (Galametz+, 2009)</TD>
            <TD>We imaged the two targets using the Bessel B-band filter of the Large Format Camera (LFC) on the Palomar 5m Hale Telescope. We imaged the radio galaxy fields using the z-band filter of Palomar/LFC. In February 2005, we observed 7C 1751+6809 for 60-min under photometric conditions. In August 2005, we observed 7C 1756+6520 for 135-min but in non-photometric conditions. The tables provide the B, z, J and Ks magnitudes and coordinates of the pBzK* galaxies (red passively evolving candidates selected by BzK=(z-K)-(B-z)&lt;-0.2 and (z-K)&gt;2.2) for both fields. The B and z bands were obtained using the Large Format Camera (LFC) on the Palomar 5m Hale Telescope, and the J and Ks bands using Wide-field Infrared Camera (WIRCAM) of the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131#pBzKs</TD>
            <TD>2011-09-14T21:08:20Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/507/131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/131</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/121 [1]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#1</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/121</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/121 [2]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#2</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/121&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/121 [sa189]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#sa189</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/121 [sa141]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#sa141</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/121 [sa127]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#sa127</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/226 [1]</TD>
            <TD>The 2dF Galaxy Redshift Survey 100k Data Release (2dFGRS Team, 2001)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2 degree diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than bJ=19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80x15degrees around the South Galactic Pole, and the other in the Northern Galactic hemisphere spanning 75x10degrees along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 square degrees and has a median depth of z=0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. The 100k release contains the 102426 objects observed up to 31 January 2001. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. This catalog was extracted from the 2dF Galaxy Redshift Survey 100k release CD-ROMs using the included mSQL database. This catalog comprises the basic spectroscopic information from the best spectrum of each object, that is contained in the extnum=0 rows of the mSQL database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/226#1</TD>
            <TD>2012-11-13T06:50:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/VII/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/226</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/226</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/226 [2]</TD>
            <TD>The 2dF Galaxy Redshift Survey 100k Data Release (2dFGRS Team, 2001)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2 degree diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than bJ=19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80x15degrees around the South Galactic Pole, and the other in the Northern Galactic hemisphere spanning 75x10degrees along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 square degrees and has a median depth of z=0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. The 100k release contains the 102426 objects observed up to 31 January 2001. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. This catalog was extracted from the 2dF Galaxy Redshift Survey 100k release CD-ROMs using the included mSQL database. This catalog comprises the basic spectroscopic information from the best spectrum of each object, that is contained in the extnum=0 rows of the mSQL database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/226#2</TD>
            <TD>2012-11-13T06:50:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/VII/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/226&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/226</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/226 [2df_100k]</TD>
            <TD>The 2dF Galaxy Redshift Survey 100k Data Release (2dFGRS Team, 2001)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2 degree diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than bJ=19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80x15degrees around the South Galactic Pole, and the other in the Northern Galactic hemisphere spanning 75x10degrees along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 square degrees and has a median depth of z=0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. The 100k release contains the 102426 objects observed up to 31 January 2001. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. This catalog was extracted from the 2dF Galaxy Redshift Survey 100k release CD-ROMs using the included mSQL database. This catalog comprises the basic spectroscopic information from the best spectrum of each object, that is contained in the extnum=0 rows of the mSQL database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/226#2df_100k</TD>
            <TD>2012-11-13T06:50:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/VII/226</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/226&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/226</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/121 [1]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#1</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/121</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/121 [2]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#2</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/121&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/121 [sa189]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#sa189</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/121 [sa141]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#sa141</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/121 [sa127]</TD>
            <TD>Stellar Distribution Near SA 127, SA 141, SA 189 (Ratnatunga 1983)</TD>
            <TD>Photographic photometry and 1950 coordinates were determined using Automated Image location on 50 micron aperture PDS scans of the regions on UKSTU Schmidt plates. Galaxy contamination, which is small at these relatively bright apparent magnitudes, has not been removed from the images located. The image locating algorithm does not locate faint stars within 9 seconds of arc of an image of a brighter star on the plate. Assuming uniform random distributions, the estimated incompleteness is 0.5% at magnitude 15 and 2.2% at 17.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/121#sa127</TD>
            <TD>2011-09-14T18:13:10Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-1995</TD>
            <TD>ivo://CDS.VizieR/II/121</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/121&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/121</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/226 [1]</TD>
            <TD>The 2dF Galaxy Redshift Survey 100k Data Release (2dFGRS Team, 2001)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2 degree diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than bJ=19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80x15degrees around the South Galactic Pole, and the other in the Northern Galactic hemisphere spanning 75x10degrees along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 square degrees and has a median depth of z=0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. The 100k release contains the 102426 objects observed up to 31 January 2001. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. This catalog was extracted from the 2dF Galaxy Redshift Survey 100k release CD-ROMs using the included mSQL database. This catalog comprises the basic spectroscopic information from the best spectrum of each object, that is contained in the extnum=0 rows of the mSQL database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/226#1</TD>
            <TD>2012-11-13T06:50:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/VII/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/226</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/226</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/226 [2]</TD>
            <TD>The 2dF Galaxy Redshift Survey 100k Data Release (2dFGRS Team, 2001)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2 degree diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than bJ=19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80x15degrees around the South Galactic Pole, and the other in the Northern Galactic hemisphere spanning 75x10degrees along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 square degrees and has a median depth of z=0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. The 100k release contains the 102426 objects observed up to 31 January 2001. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. This catalog was extracted from the 2dF Galaxy Redshift Survey 100k release CD-ROMs using the included mSQL database. This catalog comprises the basic spectroscopic information from the best spectrum of each object, that is contained in the extnum=0 rows of the mSQL database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/226#2</TD>
            <TD>2012-11-13T06:50:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/VII/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/226&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/226</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/226 [2df_100k]</TD>
            <TD>The 2dF Galaxy Redshift Survey 100k Data Release (2dFGRS Team, 2001)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2 degree diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than bJ=19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80x15degrees around the South Galactic Pole, and the other in the Northern Galactic hemisphere spanning 75x10degrees along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 square degrees and has a median depth of z=0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. The 100k release contains the 102426 objects observed up to 31 January 2001. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. This catalog was extracted from the 2dF Galaxy Redshift Survey 100k release CD-ROMs using the included mSQL database. This catalog comprises the basic spectroscopic information from the best spectrum of each object, that is contained in the extnum=0 rows of the mSQL database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/226#2df_100k</TD>
            <TD>2012-11-13T06:50:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/VII/226</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/226&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/226</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/311/361 [1]</TD>
            <TD>Evolution models of elliptical galaxies. II. (Tantalo+, 1996)</TD>
            <TD>In this paper we present new chemo-spectro-photometric models of elliptical galaxies in which infall of primordial gas is allowed to occur. They aim to simulate the collapse of a galaxy made of two components, i.e. luminous material and dark matter. The mass of the dark component is assumed to be constant in time, whereas that of the luminous material is supposed to accrete at a suitable rate. They also include the effect of galactic winds powered by supernova explosions and stellar winds from massive, early-type stars. The models are constrained to match a number of properties of elliptical galaxies, i.e. the slope and mean colours of the colour-magnitude relation (CMR), V versus (V-K), the UV excess as measured by the colour (1550-V) together with the overall shape of the integrated spectral energy distribution (ISED) in the ultraviolet, the relation between the Mg_2_ index and (1550-V), the mass to blue luminosity ratio M/L_B_ as a function of the B luminosity, and finally the broad-band colours (U-B), (B-V), (V-I), (V-K), etc. The CMR is interpreted as a mass-metallicity sequence of old, nearly coeval objects, whose mean age is 15Gyr. Assuming the law of star formation to be proportional to M_g_^k^(t) with k=1, the rate of star formation as function of time starts small, grows to a maximum, and then declines thus easily avoiding the excess of metal-poor stars found by BCF with the closed-box scheme (the analog of the G-Dwarf Problem in the solar vicinity). Owing to their stellar content, infall models can easily reproduce all the basic data of the galaxies under examination. As far as the UV excess is concerned, the same sources proposed by BCF are found to hold also with the infall scheme. H-HB and AGB manque stars of high metallicity play the dominant role, and provide a robust explanation of the correlation between the (1550-V) colour and the luminosity, mass and metallicity of the galaxies. Furthermore, these models confirm the potential of the (1550-V) colour as an age indicator in cosmology as already suggested by BCF. In the rest frame of a massive and metal-rich elliptical galaxy, this colour suffers from one major variation: at the onset of the so-called H-HB and AGB-manque stars (age about 5.6Gyr). This transition occurs at reasonably small red-shifts and therefore could be detected with the present-day instrumentation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/361#1</TD>
            <TD>2011-09-14T18:15:14Z</TD>
            <TD>#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/311/361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/311/361</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/311/361 [2]</TD>
            <TD>Evolution models of elliptical galaxies. II. (Tantalo+, 1996)</TD>
            <TD>In this paper we present new chemo-spectro-photometric models of elliptical galaxies in which infall of primordial gas is allowed to occur. They aim to simulate the collapse of a galaxy made of two components, i.e. luminous material and dark matter. The mass of the dark component is assumed to be constant in time, whereas that of the luminous material is supposed to accrete at a suitable rate. They also include the effect of galactic winds powered by supernova explosions and stellar winds from massive, early-type stars. The models are constrained to match a number of properties of elliptical galaxies, i.e. the slope and mean colours of the colour-magnitude relation (CMR), V versus (V-K), the UV excess as measured by the colour (1550-V) together with the overall shape of the integrated spectral energy distribution (ISED) in the ultraviolet, the relation between the Mg_2_ index and (1550-V), the mass to blue luminosity ratio M/L_B_ as a function of the B luminosity, and finally the broad-band colours (U-B), (B-V), (V-I), (V-K), etc. The CMR is interpreted as a mass-metallicity sequence of old, nearly coeval objects, whose mean age is 15Gyr. Assuming the law of star formation to be proportional to M_g_^k^(t) with k=1, the rate of star formation as function of time starts small, grows to a maximum, and then declines thus easily avoiding the excess of metal-poor stars found by BCF with the closed-box scheme (the analog of the G-Dwarf Problem in the solar vicinity). Owing to their stellar content, infall models can easily reproduce all the basic data of the galaxies under examination. As far as the UV excess is concerned, the same sources proposed by BCF are found to hold also with the infall scheme. H-HB and AGB manque stars of high metallicity play the dominant role, and provide a robust explanation of the correlation between the (1550-V) colour and the luminosity, mass and metallicity of the galaxies. Furthermore, these models confirm the potential of the (1550-V) colour as an age indicator in cosmology as already suggested by BCF. In the rest frame of a massive and metal-rich elliptical galaxy, this colour suffers from one major variation: at the onset of the so-called H-HB and AGB-manque stars (age about 5.6Gyr). This transition occurs at reasonably small red-shifts and therefore could be detected with the present-day instrumentation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/361#2</TD>
            <TD>2011-09-14T18:15:14Z</TD>
            <TD>#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/311/361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/311/361</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WSRTGP [1]</TD>
            <TD>WSRT Galactic Plane Compact 327-MHz Source Catalog</TD>
            <TD>The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| &lt; 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parameterized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity &gt; 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis &lt; 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct nonthermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at &lt;a href="http://www.ras.ucalgary.ca/wsrt_survey.html"&gt;http://www.ras.ucalgary.ca/wsrt_survey.html&lt;/a&gt; for the WSRTGP images (JPEG, Postscript and and FITS formats).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/wsrtgp#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wsrtgp</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=wsrtgp&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/wsrtgp.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WSRTGP [2]</TD>
            <TD>WSRT Galactic Plane Compact 327-MHz Source Catalog</TD>
            <TD>The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| &lt; 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parameterized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity &gt; 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis &lt; 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct nonthermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at &lt;a href="http://www.ras.ucalgary.ca/wsrt_survey.html"&gt;http://www.ras.ucalgary.ca/wsrt_survey.html&lt;/a&gt; for the WSRTGP images (JPEG, Postscript and and FITS formats).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/wsrtgp#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wsrtgp</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=wsrtgp&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/wsrtgp.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WSRTGP [3]</TD>
            <TD>WSRT Galactic Plane Compact 327-MHz Source Catalog</TD>
            <TD>The Westerbork Synthesis Radio Telescope (WSRT) in the Netherlands has been used to survey the section of the galactic plane from +42 to +92 degrees Galactic Longitude l at a radio frequency of 327 MHz. Twenty-three overlapping synthesis fields were observed in the Galactic Latitude b band of |b| &lt; 1.6 degrees. Each field was observed at two epochs, several years apart, to identify variable sources. Intensity data from the separate epochs were combined, and the resulting images mosaicked to produce a single image of the entire survey region. The sensitivity of the mosaic is typically a few mJy, corresponding to a detection level as low as 10 mJy/beam. The spatial resolution is 1' by 1' * cosec(Dec). The survey image provided the first high resolution view of the Galaxy at low radio frequencies, and included sections of the Sagittarius and Cygnus arms. These sections contain numerous extended features, among them supernova remnants, H II regions, "bubbles" of thermal emission, and large patches of amorphous galactic thermal emission. The inter-arm region is characterized by lower densities of extended features, but numerous discrete compact radio sources, most of which are background objects such as quasars and other types of active galactic nuclei. However, the resolution, sensitivity and low frequency of this survey make it ideal for detecting weak, non-thermal compact galactic sources, e.g. compact, low surface brightness SNRs and radio stars. Inspection of the survey image has produced a catalog of nearly 4000 discrete sources with sizes of less than about 3'. Gaussian model parameters for each compact source in the mosaicked images were obtained using the AIPS routine IMFIT. The background-removed intensity distribution of each source was fitted by a 2-dimensional Gaussian, parameterized by the source position, peak intensity, major and minor axes, and the position angle of the major axis. The catalog contains all sources having peak intensity &gt; 5 times the rms noise level measured in the surrounding area of the image, and lists RA, Dec, flux density, and, if the source is resolved, the deconvolved major and minor axis and the position angle of the source. Sources were identified based on visual inspection of the images. In practice, a source had to have dimensions of less than a few arcminutes to be classified as a compact source. Most (85%) of the sources are either unresolved or only slightly resolved (major axis &lt; 60"), but some sources have dimensions as large as 6'. A source was considered resolved if the area of its Gaussian model was greater than the area of the beam by more than 4 times its uncertainty. Approximately 15% of the sources are resolved, with dimensions of 1'- 3'. The spatial distribution of resolved sources shows concentrations toward the spiral arms and follows the warping of the Galactic disk over the length of the survey region, indicating that a sizable fraction is Galactic. In the reference paper, spectral indices are calculated for 1313 sources detected in other radio surveys at frequencies greater than 408 MHz. The resolved sources exhibit a bimodal spectral index distribution, with distinct nonthermal and thermal populations. Comparison with the IRAS Point Source Catalogue results in 118 identifications between WSRT and IRAS sources, which are listed in Table 1 of the reference paper. Most of these are thermal radio sources associated with compact Galactic objects such as H II regions and planetary nebulae. A search for variability among 2148 of the compact sources has resulted in 29 candidate low-frequency variable sources, which are listed in Table 2 of the reference paper. See the project website at &lt;a href="http://www.ras.ucalgary.ca/wsrt_survey.html"&gt;http://www.ras.ucalgary.ca/wsrt_survey.html&lt;/a&gt; for the WSRTGP images (JPEG, Postscript and and FITS formats).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/wsrtgp#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/wsrtgp</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_wsrtgp&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/wsrtgp.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/226 [1]</TD>
            <TD>The 2dF Galaxy Redshift Survey 100k Data Release (2dFGRS Team, 2001)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2 degree diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than bJ=19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80x15degrees around the South Galactic Pole, and the other in the Northern Galactic hemisphere spanning 75x10degrees along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 square degrees and has a median depth of z=0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. The 100k release contains the 102426 objects observed up to 31 January 2001. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. This catalog was extracted from the 2dF Galaxy Redshift Survey 100k release CD-ROMs using the included mSQL database. This catalog comprises the basic spectroscopic information from the best spectrum of each object, that is contained in the extnum=0 rows of the mSQL database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/226#1</TD>
            <TD>2012-11-13T06:50:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/VII/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/226</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/226</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/226 [2]</TD>
            <TD>The 2dF Galaxy Redshift Survey 100k Data Release (2dFGRS Team, 2001)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2 degree diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than bJ=19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80x15degrees around the South Galactic Pole, and the other in the Northern Galactic hemisphere spanning 75x10degrees along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 square degrees and has a median depth of z=0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. The 100k release contains the 102426 objects observed up to 31 January 2001. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. This catalog was extracted from the 2dF Galaxy Redshift Survey 100k release CD-ROMs using the included mSQL database. This catalog comprises the basic spectroscopic information from the best spectrum of each object, that is contained in the extnum=0 rows of the mSQL database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/226#2</TD>
            <TD>2012-11-13T06:50:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/VII/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/226&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/226</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/226 [2df_100k]</TD>
            <TD>The 2dF Galaxy Redshift Survey 100k Data Release (2dFGRS Team, 2001)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is designed to measure redshifts for approximately 250000 galaxies. The 2dFGRS uses the 2dF multifibre spectrograph on the Anglo-Australian Telescope, which is capable of observing 400 objects simultaneously over a 2 degree diameter field. The source catalogue for the survey is a revised and extended version of the APM galaxy catalogue, and the targets are galaxies with extinction-corrected magnitudes brighter than bJ=19.45. The main survey regions are two declination strips, one in the southern Galactic hemisphere spanning 80x15degrees around the South Galactic Pole, and the other in the Northern Galactic hemisphere spanning 75x10degrees along the celestial equator; in addition, there are 99 fields spread over the southern Galactic cap. The survey covers 2000 square degrees and has a median depth of z=0.11. Adaptive tiling is used to give a highly uniform sampling rate of 93% over the whole survey region. The 100k release contains the 102426 objects observed up to 31 January 2001. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS. This catalog was extracted from the 2dF Galaxy Redshift Survey 100k release CD-ROMs using the included mSQL database. This catalog comprises the basic spectroscopic information from the best spectrum of each object, that is contained in the extnum=0 rows of the mSQL database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/226#2df_100k</TD>
            <TD>2012-11-13T06:50:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/VII/226</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/226&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/226</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/311/361 [1]</TD>
            <TD>Evolution models of elliptical galaxies. II. (Tantalo+, 1996)</TD>
            <TD>In this paper we present new chemo-spectro-photometric models of elliptical galaxies in which infall of primordial gas is allowed to occur. They aim to simulate the collapse of a galaxy made of two components, i.e. luminous material and dark matter. The mass of the dark component is assumed to be constant in time, whereas that of the luminous material is supposed to accrete at a suitable rate. They also include the effect of galactic winds powered by supernova explosions and stellar winds from massive, early-type stars. The models are constrained to match a number of properties of elliptical galaxies, i.e. the slope and mean colours of the colour-magnitude relation (CMR), V versus (V-K), the UV excess as measured by the colour (1550-V) together with the overall shape of the integrated spectral energy distribution (ISED) in the ultraviolet, the relation between the Mg_2_ index and (1550-V), the mass to blue luminosity ratio M/L_B_ as a function of the B luminosity, and finally the broad-band colours (U-B), (B-V), (V-I), (V-K), etc. The CMR is interpreted as a mass-metallicity sequence of old, nearly coeval objects, whose mean age is 15Gyr. Assuming the law of star formation to be proportional to M_g_^k^(t) with k=1, the rate of star formation as function of time starts small, grows to a maximum, and then declines thus easily avoiding the excess of metal-poor stars found by BCF with the closed-box scheme (the analog of the G-Dwarf Problem in the solar vicinity). Owing to their stellar content, infall models can easily reproduce all the basic data of the galaxies under examination. As far as the UV excess is concerned, the same sources proposed by BCF are found to hold also with the infall scheme. H-HB and AGB manque stars of high metallicity play the dominant role, and provide a robust explanation of the correlation between the (1550-V) colour and the luminosity, mass and metallicity of the galaxies. Furthermore, these models confirm the potential of the (1550-V) colour as an age indicator in cosmology as already suggested by BCF. In the rest frame of a massive and metal-rich elliptical galaxy, this colour suffers from one major variation: at the onset of the so-called H-HB and AGB-manque stars (age about 5.6Gyr). This transition occurs at reasonably small red-shifts and therefore could be detected with the present-day instrumentation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/361#1</TD>
            <TD>2011-09-14T18:15:14Z</TD>
            <TD>#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/311/361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/311/361</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/311/361 [2]</TD>
            <TD>Evolution models of elliptical galaxies. II. (Tantalo+, 1996)</TD>
            <TD>In this paper we present new chemo-spectro-photometric models of elliptical galaxies in which infall of primordial gas is allowed to occur. They aim to simulate the collapse of a galaxy made of two components, i.e. luminous material and dark matter. The mass of the dark component is assumed to be constant in time, whereas that of the luminous material is supposed to accrete at a suitable rate. They also include the effect of galactic winds powered by supernova explosions and stellar winds from massive, early-type stars. The models are constrained to match a number of properties of elliptical galaxies, i.e. the slope and mean colours of the colour-magnitude relation (CMR), V versus (V-K), the UV excess as measured by the colour (1550-V) together with the overall shape of the integrated spectral energy distribution (ISED) in the ultraviolet, the relation between the Mg_2_ index and (1550-V), the mass to blue luminosity ratio M/L_B_ as a function of the B luminosity, and finally the broad-band colours (U-B), (B-V), (V-I), (V-K), etc. The CMR is interpreted as a mass-metallicity sequence of old, nearly coeval objects, whose mean age is 15Gyr. Assuming the law of star formation to be proportional to M_g_^k^(t) with k=1, the rate of star formation as function of time starts small, grows to a maximum, and then declines thus easily avoiding the excess of metal-poor stars found by BCF with the closed-box scheme (the analog of the G-Dwarf Problem in the solar vicinity). Owing to their stellar content, infall models can easily reproduce all the basic data of the galaxies under examination. As far as the UV excess is concerned, the same sources proposed by BCF are found to hold also with the infall scheme. H-HB and AGB manque stars of high metallicity play the dominant role, and provide a robust explanation of the correlation between the (1550-V) colour and the luminosity, mass and metallicity of the galaxies. Furthermore, these models confirm the potential of the (1550-V) colour as an age indicator in cosmology as already suggested by BCF. In the rest frame of a massive and metal-rich elliptical galaxy, this colour suffers from one major variation: at the onset of the so-called H-HB and AGB-manque stars (age about 5.6Gyr). This transition occurs at reasonably small red-shifts and therefore could be detected with the present-day instrumentation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/361#2</TD>
            <TD>2011-09-14T18:15:14Z</TD>
            <TD>#Models#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/311/361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/311/361</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/507/131 [1]</TD>
            <TD>BzJK observations around radio galaxies (Galametz+, 2009)</TD>
            <TD>We imaged the two targets using the Bessel B-band filter of the Large Format Camera (LFC) on the Palomar 5m Hale Telescope. We imaged the radio galaxy fields using the z-band filter of Palomar/LFC. In February 2005, we observed 7C 1751+6809 for 60-min under photometric conditions. In August 2005, we observed 7C 1756+6520 for 135-min but in non-photometric conditions. The tables provide the B, z, J and Ks magnitudes and coordinates of the pBzK* galaxies (red passively evolving candidates selected by BzK=(z-K)-(B-z)&lt;-0.2 and (z-K)&gt;2.2) for both fields. The B and z bands were obtained using the Large Format Camera (LFC) on the Palomar 5m Hale Telescope, and the J and Ks bands using Wide-field Infrared Camera (WIRCAM) of the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131#1</TD>
            <TD>2011-09-14T21:08:20Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/507/131</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/131</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/507/131 [2]</TD>
            <TD>BzJK observations around radio galaxies (Galametz+, 2009)</TD>
            <TD>We imaged the two targets using the Bessel B-band filter of the Large Format Camera (LFC) on the Palomar 5m Hale Telescope. We imaged the radio galaxy fields using the z-band filter of Palomar/LFC. In February 2005, we observed 7C 1751+6809 for 60-min under photometric conditions. In August 2005, we observed 7C 1756+6520 for 135-min but in non-photometric conditions. The tables provide the B, z, J and Ks magnitudes and coordinates of the pBzK* galaxies (red passively evolving candidates selected by BzK=(z-K)-(B-z)&lt;-0.2 and (z-K)&gt;2.2) for both fields. The B and z bands were obtained using the Large Format Camera (LFC) on the Palomar 5m Hale Telescope, and the J and Ks bands using Wide-field Infrared Camera (WIRCAM) of the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131#2</TD>
            <TD>2011-09-14T21:08:20Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/507/131&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/507/131 [pBzKs]</TD>
            <TD>BzJK observations around radio galaxies (Galametz+, 2009)</TD>
            <TD>We imaged the two targets using the Bessel B-band filter of the Large Format Camera (LFC) on the Palomar 5m Hale Telescope. We imaged the radio galaxy fields using the z-band filter of Palomar/LFC. In February 2005, we observed 7C 1751+6809 for 60-min under photometric conditions. In August 2005, we observed 7C 1756+6520 for 135-min but in non-photometric conditions. The tables provide the B, z, J and Ks magnitudes and coordinates of the pBzK* galaxies (red passively evolving candidates selected by BzK=(z-K)-(B-z)&lt;-0.2 and (z-K)&gt;2.2) for both fields. The B and z bands were obtained using the Large Format Camera (LFC) on the Palomar 5m Hale Telescope, and the J and Ks bands using Wide-field Infrared Camera (WIRCAM) of the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131#pBzKs</TD>
            <TD>2011-09-14T21:08:20Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/507/131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/131</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/344/715 [1]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#1</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/344/715</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/344/715 [2]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#2</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/344/715&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/715 [table5]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#table5</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/715 [tab2-4]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#tab2-4</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/311/484 [1]</TD>
            <TD>CH Cyg 1991-1995 UBV-JHKLM photometry (Munari+, 1996)</TD>
            <TD>We present new UBV-JHKLM photoelectric photometry of the symbiotic binary CH Cyg covering the period 1991-1995, which extend our monitoring started in 1978. The large and highly homogeneous set of data that we have accumulated in the last eighteen years is reviewed and discussed. By July 1995 the outbursting component has returned to the same conditions which characterized the previous minimum in 1988-1989. In J, H, K CH Cyg shows a long term modulation that can be fitted with a sinusoid of 32 year period. It may be a dust obscuration event similar to those known to undergo in symbiotic Miras. The cool giant exhibits in the infrared a variability of large amplitude, best described as chaotic-like. The only detectable periodicity is 1980 days. The photometric properties of the cool giant denounce a clear partnership with the spheroidal component of the Galaxy. This lowers the estimated distance to ~120pc and the cool giant mass to ~1.0M_{sun}_. Several episodes of dust condensation in the wind of the giant are identified. One is in full progress at the time of writing. The dust condensation temperature is found to be ~1,000K. The condensed dust grains absorb selectively in the infrared but are large enough to absorb neutrally in the UBV wavelength region. There is no evidence for dust condensing in an hypothetical wind or ejected material from the outbursting white dwarf. The recently proposed triple-star model for CH Cyg is confronted with photometric observations. Several serious discrepancies are outlined and individually discussed. We believe that, without additional evidences and careful modelling, the triple star model cannot survive the comparison with the photometric observations. The low amplitude (2.6km/s) and periodic (756 days) radial velocity variations apparently do not trace an orbital motion. They may be due to one of the many superimposed pulsation modes of the highly variable M giant.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/484#1</TD>
            <TD>2011-09-14T18:15:15Z</TD>
            <TD>#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/484</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/311/484</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/311/484</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/311/484 [2]</TD>
            <TD>CH Cyg 1991-1995 UBV-JHKLM photometry (Munari+, 1996)</TD>
            <TD>We present new UBV-JHKLM photoelectric photometry of the symbiotic binary CH Cyg covering the period 1991-1995, which extend our monitoring started in 1978. The large and highly homogeneous set of data that we have accumulated in the last eighteen years is reviewed and discussed. By July 1995 the outbursting component has returned to the same conditions which characterized the previous minimum in 1988-1989. In J, H, K CH Cyg shows a long term modulation that can be fitted with a sinusoid of 32 year period. It may be a dust obscuration event similar to those known to undergo in symbiotic Miras. The cool giant exhibits in the infrared a variability of large amplitude, best described as chaotic-like. The only detectable periodicity is 1980 days. The photometric properties of the cool giant denounce a clear partnership with the spheroidal component of the Galaxy. This lowers the estimated distance to ~120pc and the cool giant mass to ~1.0M_{sun}_. Several episodes of dust condensation in the wind of the giant are identified. One is in full progress at the time of writing. The dust condensation temperature is found to be ~1,000K. The condensed dust grains absorb selectively in the infrared but are large enough to absorb neutrally in the UBV wavelength region. There is no evidence for dust condensing in an hypothetical wind or ejected material from the outbursting white dwarf. The recently proposed triple-star model for CH Cyg is confronted with photometric observations. Several serious discrepancies are outlined and individually discussed. We believe that, without additional evidences and careful modelling, the triple star model cannot survive the comparison with the photometric observations. The low amplitude (2.6km/s) and periodic (756 days) radial velocity variations apparently do not trace an orbital motion. They may be due to one of the many superimposed pulsation modes of the highly variable M giant.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/484#2</TD>
            <TD>2011-09-14T18:15:15Z</TD>
            <TD>#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/484</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/311/484&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/311/484</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/344/715 [1]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#1</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/344/715</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/344/715 [2]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#2</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/344/715&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/715 [table5]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#table5</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/715 [tab2-4]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#tab2-4</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/716/1514 [1]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#1</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/716/1514</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/716/1514 [2]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#2</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/716/1514&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/716/1514 [table1]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#table1</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/716/1514&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/716/1514 [table2]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#table2</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/716/1514&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/311/484 [1]</TD>
            <TD>CH Cyg 1991-1995 UBV-JHKLM photometry (Munari+, 1996)</TD>
            <TD>We present new UBV-JHKLM photoelectric photometry of the symbiotic binary CH Cyg covering the period 1991-1995, which extend our monitoring started in 1978. The large and highly homogeneous set of data that we have accumulated in the last eighteen years is reviewed and discussed. By July 1995 the outbursting component has returned to the same conditions which characterized the previous minimum in 1988-1989. In J, H, K CH Cyg shows a long term modulation that can be fitted with a sinusoid of 32 year period. It may be a dust obscuration event similar to those known to undergo in symbiotic Miras. The cool giant exhibits in the infrared a variability of large amplitude, best described as chaotic-like. The only detectable periodicity is 1980 days. The photometric properties of the cool giant denounce a clear partnership with the spheroidal component of the Galaxy. This lowers the estimated distance to ~120pc and the cool giant mass to ~1.0M_{sun}_. Several episodes of dust condensation in the wind of the giant are identified. One is in full progress at the time of writing. The dust condensation temperature is found to be ~1,000K. The condensed dust grains absorb selectively in the infrared but are large enough to absorb neutrally in the UBV wavelength region. There is no evidence for dust condensing in an hypothetical wind or ejected material from the outbursting white dwarf. The recently proposed triple-star model for CH Cyg is confronted with photometric observations. Several serious discrepancies are outlined and individually discussed. We believe that, without additional evidences and careful modelling, the triple star model cannot survive the comparison with the photometric observations. The low amplitude (2.6km/s) and periodic (756 days) radial velocity variations apparently do not trace an orbital motion. They may be due to one of the many superimposed pulsation modes of the highly variable M giant.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/484#1</TD>
            <TD>2011-09-14T18:15:15Z</TD>
            <TD>#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/484</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/311/484</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/311/484</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/311/484 [2]</TD>
            <TD>CH Cyg 1991-1995 UBV-JHKLM photometry (Munari+, 1996)</TD>
            <TD>We present new UBV-JHKLM photoelectric photometry of the symbiotic binary CH Cyg covering the period 1991-1995, which extend our monitoring started in 1978. The large and highly homogeneous set of data that we have accumulated in the last eighteen years is reviewed and discussed. By July 1995 the outbursting component has returned to the same conditions which characterized the previous minimum in 1988-1989. In J, H, K CH Cyg shows a long term modulation that can be fitted with a sinusoid of 32 year period. It may be a dust obscuration event similar to those known to undergo in symbiotic Miras. The cool giant exhibits in the infrared a variability of large amplitude, best described as chaotic-like. The only detectable periodicity is 1980 days. The photometric properties of the cool giant denounce a clear partnership with the spheroidal component of the Galaxy. This lowers the estimated distance to ~120pc and the cool giant mass to ~1.0M_{sun}_. Several episodes of dust condensation in the wind of the giant are identified. One is in full progress at the time of writing. The dust condensation temperature is found to be ~1,000K. The condensed dust grains absorb selectively in the infrared but are large enough to absorb neutrally in the UBV wavelength region. There is no evidence for dust condensing in an hypothetical wind or ejected material from the outbursting white dwarf. The recently proposed triple-star model for CH Cyg is confronted with photometric observations. Several serious discrepancies are outlined and individually discussed. We believe that, without additional evidences and careful modelling, the triple star model cannot survive the comparison with the photometric observations. The low amplitude (2.6km/s) and periodic (756 days) radial velocity variations apparently do not trace an orbital motion. They may be due to one of the many superimposed pulsation modes of the highly variable M giant.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/484#2</TD>
            <TD>2011-09-14T18:15:15Z</TD>
            <TD>#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/311/484</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/311/484&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/311/484</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/344/715 [1]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#1</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/344/715</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/344/715 [2]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#2</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/344/715&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/715 [table5]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#table5</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/715 [tab2-4]</TD>
            <TD>Planetary nebulae as standard candles. IV. (Ciardullo+, 1989)</TD>
            <TD>We present the results of a planetary nebula survey of galaxies in the Leo I group performed with the Kitt Peak and Cerro Tololo 4m telescopes and on-band off-band {lambda}5007 interference filters. In all, we detected 249 PN candidates populating the top 1.5mag of the planetary nebula luminosity function (PNLF), including 93 in the E0 galaxy NGC 3379, 54 in the E6 galaxy NGC 3377, and 102 in the S0 spiral NGC 3384.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715#tab2-4</TD>
            <TD>2012-11-13T07:12:17Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/715</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/715&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/715</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/106/451 [1]</TD>
            <TD>Face-on disk galaxies photometry. I. (de Jong+, 1994)</TD>
            <TD>We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451#1</TD>
            <TD>2011-09-14T18:17:06Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/106/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/106/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/106/451 [2]</TD>
            <TD>Face-on disk galaxies photometry. I. (de Jong+, 1994)</TD>
            <TD>We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451#2</TD>
            <TD>2011-09-14T18:17:06Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/106/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/106/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/106/451 [table3]</TD>
            <TD>Face-on disk galaxies photometry. I. (de Jong+, 1994)</TD>
            <TD>We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451#table3</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/106/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/106/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/414/454 [1]</TD>
            <TD>NGC 3379 planetary nebulae radial velocities (Ciardullo+, 1993)</TD>
            <TD>We present the results of a radial velocity survey of planetary nebulae (PNs) in the normal elliptical galaxy NGC 3379 performed with the Kitt Peak 4m telescope and the NESSIE multifiber spectrograph. In two half-nights, we measured 29 PNs with projected galactocentric distances between 0.4 and 3.8 effective radii (1&lt;R&lt;10kpc) with an observational uncertainty of ~7km/s. These data extend 3 times further into the halo than any previous absorption-line velocity study. The velocity dispersion and photometric profile of the galaxy agrees extremely well with that expected from a constant mass-to-light ratio, isotropic orbit Jaffe model with M/L_B_~7; the best-fitting anisotropic models from a quadratic programming algorithm also give M/L_B_~7. The data are consistent with models that contain no dark matter within 3.5 effective radii of the galaxy's nucleus.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454#1</TD>
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            <TD>ivo://CDS.VizieR/J/ApJ/414/454</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/414/454</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/454</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/414/454 [2]</TD>
            <TD>NGC 3379 planetary nebulae radial velocities (Ciardullo+, 1993)</TD>
            <TD>We present the results of a radial velocity survey of planetary nebulae (PNs) in the normal elliptical galaxy NGC 3379 performed with the Kitt Peak 4m telescope and the NESSIE multifiber spectrograph. In two half-nights, we measured 29 PNs with projected galactocentric distances between 0.4 and 3.8 effective radii (1&lt;R&lt;10kpc) with an observational uncertainty of ~7km/s. These data extend 3 times further into the halo than any previous absorption-line velocity study. The velocity dispersion and photometric profile of the galaxy agrees extremely well with that expected from a constant mass-to-light ratio, isotropic orbit Jaffe model with M/L_B_~7; the best-fitting anisotropic models from a quadratic programming algorithm also give M/L_B_~7. The data are consistent with models that contain no dark matter within 3.5 effective radii of the galaxy's nucleus.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454#2</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/414/454&amp;</TD>
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            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJ/414/454 [table1]</TD>
            <TD>NGC 3379 planetary nebulae radial velocities (Ciardullo+, 1993)</TD>
            <TD>We present the results of a radial velocity survey of planetary nebulae (PNs) in the normal elliptical galaxy NGC 3379 performed with the Kitt Peak 4m telescope and the NESSIE multifiber spectrograph. In two half-nights, we measured 29 PNs with projected galactocentric distances between 0.4 and 3.8 effective radii (1&lt;R&lt;10kpc) with an observational uncertainty of ~7km/s. These data extend 3 times further into the halo than any previous absorption-line velocity study. The velocity dispersion and photometric profile of the galaxy agrees extremely well with that expected from a constant mass-to-light ratio, isotropic orbit Jaffe model with M/L_B_~7; the best-fitting anisotropic models from a quadratic programming algorithm also give M/L_B_~7. The data are consistent with models that contain no dark matter within 3.5 effective radii of the galaxy's nucleus.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454#table1</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/454</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/106/451 [1]</TD>
            <TD>Face-on disk galaxies photometry. I. (de Jong+, 1994)</TD>
            <TD>We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451#1</TD>
            <TD>2011-09-14T18:17:06Z</TD>
            <TD>#Photometry:surface#</TD>
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            <TD>24-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451</TD>
            <TD />
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            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/106/451</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/106/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/106/451 [2]</TD>
            <TD>Face-on disk galaxies photometry. I. (de Jong+, 1994)</TD>
            <TD>We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451#2</TD>
            <TD>2011-09-14T18:17:06Z</TD>
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            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/106/451&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/106/451</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/106/451 [table3]</TD>
            <TD>Face-on disk galaxies photometry. I. (de Jong+, 1994)</TD>
            <TD>We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451#table3</TD>
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            <TD>24-Jul-1995</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/106/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/106/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/414/454 [1]</TD>
            <TD>NGC 3379 planetary nebulae radial velocities (Ciardullo+, 1993)</TD>
            <TD>We present the results of a radial velocity survey of planetary nebulae (PNs) in the normal elliptical galaxy NGC 3379 performed with the Kitt Peak 4m telescope and the NESSIE multifiber spectrograph. In two half-nights, we measured 29 PNs with projected galactocentric distances between 0.4 and 3.8 effective radii (1&lt;R&lt;10kpc) with an observational uncertainty of ~7km/s. These data extend 3 times further into the halo than any previous absorption-line velocity study. The velocity dispersion and photometric profile of the galaxy agrees extremely well with that expected from a constant mass-to-light ratio, isotropic orbit Jaffe model with M/L_B_~7; the best-fitting anisotropic models from a quadratic programming algorithm also give M/L_B_~7. The data are consistent with models that contain no dark matter within 3.5 effective radii of the galaxy's nucleus.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454#1</TD>
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            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/414/454</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/454</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/414/454 [2]</TD>
            <TD>NGC 3379 planetary nebulae radial velocities (Ciardullo+, 1993)</TD>
            <TD>We present the results of a radial velocity survey of planetary nebulae (PNs) in the normal elliptical galaxy NGC 3379 performed with the Kitt Peak 4m telescope and the NESSIE multifiber spectrograph. In two half-nights, we measured 29 PNs with projected galactocentric distances between 0.4 and 3.8 effective radii (1&lt;R&lt;10kpc) with an observational uncertainty of ~7km/s. These data extend 3 times further into the halo than any previous absorption-line velocity study. The velocity dispersion and photometric profile of the galaxy agrees extremely well with that expected from a constant mass-to-light ratio, isotropic orbit Jaffe model with M/L_B_~7; the best-fitting anisotropic models from a quadratic programming algorithm also give M/L_B_~7. The data are consistent with models that contain no dark matter within 3.5 effective radii of the galaxy's nucleus.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454#2</TD>
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            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/414/454&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/454</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/414/454 [table1]</TD>
            <TD>NGC 3379 planetary nebulae radial velocities (Ciardullo+, 1993)</TD>
            <TD>We present the results of a radial velocity survey of planetary nebulae (PNs) in the normal elliptical galaxy NGC 3379 performed with the Kitt Peak 4m telescope and the NESSIE multifiber spectrograph. In two half-nights, we measured 29 PNs with projected galactocentric distances between 0.4 and 3.8 effective radii (1&lt;R&lt;10kpc) with an observational uncertainty of ~7km/s. These data extend 3 times further into the halo than any previous absorption-line velocity study. The velocity dispersion and photometric profile of the galaxy agrees extremely well with that expected from a constant mass-to-light ratio, isotropic orbit Jaffe model with M/L_B_~7; the best-fitting anisotropic models from a quadratic programming algorithm also give M/L_B_~7. The data are consistent with models that contain no dark matter within 3.5 effective radii of the galaxy's nucleus.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454#table1</TD>
            <TD>2012-11-13T07:12:24Z</TD>
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            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/414/454&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/454</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/414/454 [1]</TD>
            <TD>NGC 3379 planetary nebulae radial velocities (Ciardullo+, 1993)</TD>
            <TD>We present the results of a radial velocity survey of planetary nebulae (PNs) in the normal elliptical galaxy NGC 3379 performed with the Kitt Peak 4m telescope and the NESSIE multifiber spectrograph. In two half-nights, we measured 29 PNs with projected galactocentric distances between 0.4 and 3.8 effective radii (1&lt;R&lt;10kpc) with an observational uncertainty of ~7km/s. These data extend 3 times further into the halo than any previous absorption-line velocity study. The velocity dispersion and photometric profile of the galaxy agrees extremely well with that expected from a constant mass-to-light ratio, isotropic orbit Jaffe model with M/L_B_~7; the best-fitting anisotropic models from a quadratic programming algorithm also give M/L_B_~7. The data are consistent with models that contain no dark matter within 3.5 effective radii of the galaxy's nucleus.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454#1</TD>
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            <TD>#Planetary_Nebulae#Velocities#</TD>
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            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/414/454</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/454</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/414/454 [2]</TD>
            <TD>NGC 3379 planetary nebulae radial velocities (Ciardullo+, 1993)</TD>
            <TD>We present the results of a radial velocity survey of planetary nebulae (PNs) in the normal elliptical galaxy NGC 3379 performed with the Kitt Peak 4m telescope and the NESSIE multifiber spectrograph. In two half-nights, we measured 29 PNs with projected galactocentric distances between 0.4 and 3.8 effective radii (1&lt;R&lt;10kpc) with an observational uncertainty of ~7km/s. These data extend 3 times further into the halo than any previous absorption-line velocity study. The velocity dispersion and photometric profile of the galaxy agrees extremely well with that expected from a constant mass-to-light ratio, isotropic orbit Jaffe model with M/L_B_~7; the best-fitting anisotropic models from a quadratic programming algorithm also give M/L_B_~7. The data are consistent with models that contain no dark matter within 3.5 effective radii of the galaxy's nucleus.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454#2</TD>
            <TD>2012-11-13T07:12:24Z</TD>
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            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/414/454&amp;</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/414/454 [table1]</TD>
            <TD>NGC 3379 planetary nebulae radial velocities (Ciardullo+, 1993)</TD>
            <TD>We present the results of a radial velocity survey of planetary nebulae (PNs) in the normal elliptical galaxy NGC 3379 performed with the Kitt Peak 4m telescope and the NESSIE multifiber spectrograph. In two half-nights, we measured 29 PNs with projected galactocentric distances between 0.4 and 3.8 effective radii (1&lt;R&lt;10kpc) with an observational uncertainty of ~7km/s. These data extend 3 times further into the halo than any previous absorption-line velocity study. The velocity dispersion and photometric profile of the galaxy agrees extremely well with that expected from a constant mass-to-light ratio, isotropic orbit Jaffe model with M/L_B_~7; the best-fitting anisotropic models from a quadratic programming algorithm also give M/L_B_~7. The data are consistent with models that contain no dark matter within 3.5 effective radii of the galaxy's nucleus.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454#table1</TD>
            <TD>2012-11-13T07:12:24Z</TD>
            <TD>#Planetary_Nebulae#Velocities#</TD>
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            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/454</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/414/454&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/454</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/317 [1]</TD>
            <TD>BR photometry of UGC 685 (Hopp, 1999)</TD>
            <TD>B and R CCD images and J NICMOS3 frames taken with the Calar Alto 3.5m telescope of the dwarf irregular galaxy UGC 685 are presented. The brightest part of the stellar population is resolved in B and R, very few also in J. The stellar color-magnitude diagram is discussed. An estimate of the distance to UGC 685 of 5. 5Mpc is derived based on the brightest blue supergiant stars. Most of the resolved bright stars show colors in the range -0.1&lt;=B-R&lt;=+0.7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317#1</TD>
            <TD>2011-09-14T21:10:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/317</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/317</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/317 [2]</TD>
            <TD>BR photometry of UGC 685 (Hopp, 1999)</TD>
            <TD>B and R CCD images and J NICMOS3 frames taken with the Calar Alto 3.5m telescope of the dwarf irregular galaxy UGC 685 are presented. The brightest part of the stellar population is resolved in B and R, very few also in J. The stellar color-magnitude diagram is discussed. An estimate of the distance to UGC 685 of 5. 5Mpc is derived based on the brightest blue supergiant stars. Most of the resolved bright stars show colors in the range -0.1&lt;=B-R&lt;=+0.7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317#2</TD>
            <TD>2011-09-14T21:10:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/317&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/317</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/317 [table3]</TD>
            <TD>BR photometry of UGC 685 (Hopp, 1999)</TD>
            <TD>B and R CCD images and J NICMOS3 frames taken with the Calar Alto 3.5m telescope of the dwarf irregular galaxy UGC 685 are presented. The brightest part of the stellar population is resolved in B and R, very few also in J. The stellar color-magnitude diagram is discussed. An estimate of the distance to UGC 685 of 5. 5Mpc is derived based on the brightest blue supergiant stars. Most of the resolved bright stars show colors in the range -0.1&lt;=B-R&lt;=+0.7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317#table3</TD>
            <TD>2011-09-14T21:10:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/317&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/317</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/626/887 [1]</TD>
            <TD>HI clouds in Southern Galactic Plane Survey (Kavars+, 2005)</TD>
            <TD>The SGPS is one of three large sky surveys that image HI line emission and 21cm continuum in the plane of the Galaxy. The other two surveys are the CGPS and the VGPS. Together, the three make up the International Galactic Plane Survey (IGPS). The SGPS combines interferometer data from the Australia Telescope Compact Array (ATCA) and single-dish data from the Parkes 64m telescope. It maps the region of 253{deg}&lt;=l&lt;=358{deg} and -1.3{deg}&lt;=b&lt;=+1.3{deg} with an angular resolution of 2';, a channel spacing of 0.82km/s, and an rms brightness sensitivity per channel of 24K, depending on the brightness of the HI emission (McClure-Griffiths, 2001, Ph.D. thesis, Univ. Minnesota). The SGPS data are divided into cubes of 5{deg}x2.6{deg} centered on b=0{deg} and longitudes that are multiples of 5{deg}. A further description of the data is detailed in McClure-Griffiths et al. (2005ApJS..158..178M). SGPS HI images are available at http://www.atnf.csiro.au/research/HI/sgps/queryForm.html .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887#1</TD>
            <TD>2012-11-13T07:13:43Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/626/887</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/887</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/626/887 [2]</TD>
            <TD>HI clouds in Southern Galactic Plane Survey (Kavars+, 2005)</TD>
            <TD>The SGPS is one of three large sky surveys that image HI line emission and 21cm continuum in the plane of the Galaxy. The other two surveys are the CGPS and the VGPS. Together, the three make up the International Galactic Plane Survey (IGPS). The SGPS combines interferometer data from the Australia Telescope Compact Array (ATCA) and single-dish data from the Parkes 64m telescope. It maps the region of 253{deg}&lt;=l&lt;=358{deg} and -1.3{deg}&lt;=b&lt;=+1.3{deg} with an angular resolution of 2';, a channel spacing of 0.82km/s, and an rms brightness sensitivity per channel of 24K, depending on the brightness of the HI emission (McClure-Griffiths, 2001, Ph.D. thesis, Univ. Minnesota). The SGPS data are divided into cubes of 5{deg}x2.6{deg} centered on b=0{deg} and longitudes that are multiples of 5{deg}. A further description of the data is detailed in McClure-Griffiths et al. (2005ApJS..158..178M). SGPS HI images are available at http://www.atnf.csiro.au/research/HI/sgps/queryForm.html .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887#2</TD>
            <TD>2012-11-13T07:13:43Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/626/887&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/887</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/626/887 [table2]</TD>
            <TD>HI clouds in Southern Galactic Plane Survey (Kavars+, 2005)</TD>
            <TD>The SGPS is one of three large sky surveys that image HI line emission and 21cm continuum in the plane of the Galaxy. The other two surveys are the CGPS and the VGPS. Together, the three make up the International Galactic Plane Survey (IGPS). The SGPS combines interferometer data from the Australia Telescope Compact Array (ATCA) and single-dish data from the Parkes 64m telescope. It maps the region of 253{deg}&lt;=l&lt;=358{deg} and -1.3{deg}&lt;=b&lt;=+1.3{deg} with an angular resolution of 2';, a channel spacing of 0.82km/s, and an rms brightness sensitivity per channel of 24K, depending on the brightness of the HI emission (McClure-Griffiths, 2001, Ph.D. thesis, Univ. Minnesota). The SGPS data are divided into cubes of 5{deg}x2.6{deg} centered on b=0{deg} and longitudes that are multiples of 5{deg}. A further description of the data is detailed in McClure-Griffiths et al. (2005ApJS..158..178M). SGPS HI images are available at http://www.atnf.csiro.au/research/HI/sgps/queryForm.html .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887#table2</TD>
            <TD>2012-11-13T07:13:43Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/626/887&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/887</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/626/887 [1]</TD>
            <TD>HI clouds in Southern Galactic Plane Survey (Kavars+, 2005)</TD>
            <TD>The SGPS is one of three large sky surveys that image HI line emission and 21cm continuum in the plane of the Galaxy. The other two surveys are the CGPS and the VGPS. Together, the three make up the International Galactic Plane Survey (IGPS). The SGPS combines interferometer data from the Australia Telescope Compact Array (ATCA) and single-dish data from the Parkes 64m telescope. It maps the region of 253{deg}&lt;=l&lt;=358{deg} and -1.3{deg}&lt;=b&lt;=+1.3{deg} with an angular resolution of 2';, a channel spacing of 0.82km/s, and an rms brightness sensitivity per channel of 24K, depending on the brightness of the HI emission (McClure-Griffiths, 2001, Ph.D. thesis, Univ. Minnesota). The SGPS data are divided into cubes of 5{deg}x2.6{deg} centered on b=0{deg} and longitudes that are multiples of 5{deg}. A further description of the data is detailed in McClure-Griffiths et al. (2005ApJS..158..178M). SGPS HI images are available at http://www.atnf.csiro.au/research/HI/sgps/queryForm.html .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887#1</TD>
            <TD>2012-11-13T07:13:43Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/626/887</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/887</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/626/887 [2]</TD>
            <TD>HI clouds in Southern Galactic Plane Survey (Kavars+, 2005)</TD>
            <TD>The SGPS is one of three large sky surveys that image HI line emission and 21cm continuum in the plane of the Galaxy. The other two surveys are the CGPS and the VGPS. Together, the three make up the International Galactic Plane Survey (IGPS). The SGPS combines interferometer data from the Australia Telescope Compact Array (ATCA) and single-dish data from the Parkes 64m telescope. It maps the region of 253{deg}&lt;=l&lt;=358{deg} and -1.3{deg}&lt;=b&lt;=+1.3{deg} with an angular resolution of 2';, a channel spacing of 0.82km/s, and an rms brightness sensitivity per channel of 24K, depending on the brightness of the HI emission (McClure-Griffiths, 2001, Ph.D. thesis, Univ. Minnesota). The SGPS data are divided into cubes of 5{deg}x2.6{deg} centered on b=0{deg} and longitudes that are multiples of 5{deg}. A further description of the data is detailed in McClure-Griffiths et al. (2005ApJS..158..178M). SGPS HI images are available at http://www.atnf.csiro.au/research/HI/sgps/queryForm.html .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887#2</TD>
            <TD>2012-11-13T07:13:43Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
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            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/626/887&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/887</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/626/887 [table2]</TD>
            <TD>HI clouds in Southern Galactic Plane Survey (Kavars+, 2005)</TD>
            <TD>The SGPS is one of three large sky surveys that image HI line emission and 21cm continuum in the plane of the Galaxy. The other two surveys are the CGPS and the VGPS. Together, the three make up the International Galactic Plane Survey (IGPS). The SGPS combines interferometer data from the Australia Telescope Compact Array (ATCA) and single-dish data from the Parkes 64m telescope. It maps the region of 253{deg}&lt;=l&lt;=358{deg} and -1.3{deg}&lt;=b&lt;=+1.3{deg} with an angular resolution of 2';, a channel spacing of 0.82km/s, and an rms brightness sensitivity per channel of 24K, depending on the brightness of the HI emission (McClure-Griffiths, 2001, Ph.D. thesis, Univ. Minnesota). The SGPS data are divided into cubes of 5{deg}x2.6{deg} centered on b=0{deg} and longitudes that are multiples of 5{deg}. A further description of the data is detailed in McClure-Griffiths et al. (2005ApJS..158..178M). SGPS HI images are available at http://www.atnf.csiro.au/research/HI/sgps/queryForm.html .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887#table2</TD>
            <TD>2012-11-13T07:13:43Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/626/887&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/887</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/716/1514 [1]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#1</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/716/1514</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/716/1514 [2]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#2</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/716/1514&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/716/1514 [table1]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#table1</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/716/1514&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/716/1514 [table2]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#table2</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/716/1514&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/626/887 [1]</TD>
            <TD>HI clouds in Southern Galactic Plane Survey (Kavars+, 2005)</TD>
            <TD>The SGPS is one of three large sky surveys that image HI line emission and 21cm continuum in the plane of the Galaxy. The other two surveys are the CGPS and the VGPS. Together, the three make up the International Galactic Plane Survey (IGPS). The SGPS combines interferometer data from the Australia Telescope Compact Array (ATCA) and single-dish data from the Parkes 64m telescope. It maps the region of 253{deg}&lt;=l&lt;=358{deg} and -1.3{deg}&lt;=b&lt;=+1.3{deg} with an angular resolution of 2';, a channel spacing of 0.82km/s, and an rms brightness sensitivity per channel of 24K, depending on the brightness of the HI emission (McClure-Griffiths, 2001, Ph.D. thesis, Univ. Minnesota). The SGPS data are divided into cubes of 5{deg}x2.6{deg} centered on b=0{deg} and longitudes that are multiples of 5{deg}. A further description of the data is detailed in McClure-Griffiths et al. (2005ApJS..158..178M). SGPS HI images are available at http://www.atnf.csiro.au/research/HI/sgps/queryForm.html .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887#1</TD>
            <TD>2012-11-13T07:13:43Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/626/887</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/887</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/626/887 [2]</TD>
            <TD>HI clouds in Southern Galactic Plane Survey (Kavars+, 2005)</TD>
            <TD>The SGPS is one of three large sky surveys that image HI line emission and 21cm continuum in the plane of the Galaxy. The other two surveys are the CGPS and the VGPS. Together, the three make up the International Galactic Plane Survey (IGPS). The SGPS combines interferometer data from the Australia Telescope Compact Array (ATCA) and single-dish data from the Parkes 64m telescope. It maps the region of 253{deg}&lt;=l&lt;=358{deg} and -1.3{deg}&lt;=b&lt;=+1.3{deg} with an angular resolution of 2';, a channel spacing of 0.82km/s, and an rms brightness sensitivity per channel of 24K, depending on the brightness of the HI emission (McClure-Griffiths, 2001, Ph.D. thesis, Univ. Minnesota). The SGPS data are divided into cubes of 5{deg}x2.6{deg} centered on b=0{deg} and longitudes that are multiples of 5{deg}. A further description of the data is detailed in McClure-Griffiths et al. (2005ApJS..158..178M). SGPS HI images are available at http://www.atnf.csiro.au/research/HI/sgps/queryForm.html .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887#2</TD>
            <TD>2012-11-13T07:13:43Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/626/887&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/887</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/626/887 [table2]</TD>
            <TD>HI clouds in Southern Galactic Plane Survey (Kavars+, 2005)</TD>
            <TD>The SGPS is one of three large sky surveys that image HI line emission and 21cm continuum in the plane of the Galaxy. The other two surveys are the CGPS and the VGPS. Together, the three make up the International Galactic Plane Survey (IGPS). The SGPS combines interferometer data from the Australia Telescope Compact Array (ATCA) and single-dish data from the Parkes 64m telescope. It maps the region of 253{deg}&lt;=l&lt;=358{deg} and -1.3{deg}&lt;=b&lt;=+1.3{deg} with an angular resolution of 2';, a channel spacing of 0.82km/s, and an rms brightness sensitivity per channel of 24K, depending on the brightness of the HI emission (McClure-Griffiths, 2001, Ph.D. thesis, Univ. Minnesota). The SGPS data are divided into cubes of 5{deg}x2.6{deg} centered on b=0{deg} and longitudes that are multiples of 5{deg}. A further description of the data is detailed in McClure-Griffiths et al. (2005ApJS..158..178M). SGPS HI images are available at http://www.atnf.csiro.au/research/HI/sgps/queryForm.html .</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887#table2</TD>
            <TD>2012-11-13T07:13:43Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/626/887</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/626/887&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/626/887</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/63/821 [1]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#1</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/63/821</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/63/821 [2]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#2</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/63/821&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/63/821 [table2]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#table2</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/63/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/63/821 [table1]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#table1</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/63/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/63/821 [1]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#1</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/63/821</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/63/821 [2]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#2</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/63/821&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/63/821 [table2]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#table2</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/63/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/63/821 [table1]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#table1</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/63/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/63/821 [1]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#1</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/63/821</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/63/821 [2]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#2</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/63/821&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/63/821 [table2]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#table2</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/63/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/63/821 [table1]</TD>
            <TD>Inner Galaxy Molecular clouds and cloud cores (Scoville+, 1987)</TD>
            <TD>A compilation of CO emission regions and their measured parameters is presented which represents a nearly complete accounting of the molecular clouds in the first quadrant of the Galaxy. Emission regions associated with radio H II regions have systematically brighter CO peaks that are a factor of two to three times larger and have twice the mean velocity dispersion as the general cloud population. Both the H II region clouds and the hot core regions have a Galactic distribution characteristic of a spiral arm population, whereas the colder clouds are much less confined in Galactic azimuthal angle. Virial masses are obtained for the large sample of clouds with assigned kinematic distances. The mean H2 density for a GMC of diameter 40 pc is 180cm^-3^. For these clouds, a linear relationship is found between the H2 column density and the integrated CO emission. The variation in the Z-dispersion of clouds as a function of cloud mass suggests that more massive GMCs have smaller random velocities.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821#table1</TD>
            <TD>2012-11-13T07:16:40Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/63/821</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/63/821&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/63/821</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/716/1514 [1]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#1</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/716/1514</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/716/1514 [2]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#2</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/716/1514&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/716/1514 [table1]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#table1</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/716/1514&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/716/1514 [table2]</TD>
            <TD>Galaxies as tracers of the circumgalactic gas (Yao+, 2010)</TD>
            <TD>The circumgalactic medium (CGM) around galaxies is believed to record various forms of galaxy feedback and contain a significant portion of the "missing baryons" of individual dark matter halos. However, clear observational evidence for the existence of the hot CGM is still absent. We use intervening galaxies along 12 background active galactic nuclei (AGNs) as tracers to search for X-ray absorption lines produced in the corresponding CGM. Stacking Chandra grating observations with respect to galaxy groups and different luminosities of these intervening galaxies, we obtain spectra with signal-to-noise ratios of 46-72 per 20m{AA} spectral bin at the expected OVIIK{alpha} line. We find no detectable absorption lines of CVI, NVII, OVII, OVIII, or NeIX. The high spectral quality allows us to tightly constrain upper limits to the corresponding ionic column densities (in particular log[N_OVII_(cm^-2^)]&lt;=14.2-14.8). These nondetections are inconsistent with the Local Group hypothesis of the X-ray absorption lines at z~0 commonly observed in the spectra of AGNs. These results indicate that the putative CGM in the temperature range of 10^5.5^-10^6.3^K may not be able to account for the missing baryons unless the metallicity is less than 10% solar.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514#table2</TD>
            <TD>2012-12-03T13:53:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/1514</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/716/1514&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/1514</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/327/325 [1]</TD>
            <TD>Distances of molecular cloud (May+, 1997)</TD>
            <TD>We have used a deep CO survey (at 115GHz) of the third galactic quadrant (May et al., 1993A&amp;AS...99..105M) to derive the physical properties of molecular clouds in the outer Galaxy. Within the range of this survey, from 194{deg} to 270{deg} in galactic longitude, 177 molecular clouds have been identified beyond 2 kpc from the Sun. Distances have been determined kinematically using the rotation curve of Brand (1986, Ph.D. Thesis, University of Leiden) with R_{sun}_=8.5kpc and {Theta}_{sun}_=220km/s.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325#1</TD>
            <TD>2012-11-13T13:38:52Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/327/325</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/325</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/327/325 [2]</TD>
            <TD>Distances of molecular cloud (May+, 1997)</TD>
            <TD>We have used a deep CO survey (at 115GHz) of the third galactic quadrant (May et al., 1993A&amp;AS...99..105M) to derive the physical properties of molecular clouds in the outer Galaxy. Within the range of this survey, from 194{deg} to 270{deg} in galactic longitude, 177 molecular clouds have been identified beyond 2 kpc from the Sun. Distances have been determined kinematically using the rotation curve of Brand (1986, Ph.D. Thesis, University of Leiden) with R_{sun}_=8.5kpc and {Theta}_{sun}_=220km/s.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325#2</TD>
            <TD>2012-11-13T13:38:52Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/327/325&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/325</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/325 [table2]</TD>
            <TD>Distances of molecular cloud (May+, 1997)</TD>
            <TD>We have used a deep CO survey (at 115GHz) of the third galactic quadrant (May et al., 1993A&amp;AS...99..105M) to derive the physical properties of molecular clouds in the outer Galaxy. Within the range of this survey, from 194{deg} to 270{deg} in galactic longitude, 177 molecular clouds have been identified beyond 2 kpc from the Sun. Distances have been determined kinematically using the rotation curve of Brand (1986, Ph.D. Thesis, University of Leiden) with R_{sun}_=8.5kpc and {Theta}_{sun}_=220km/s.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325#table2</TD>
            <TD>2012-11-13T13:38:52Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/325&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/325</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/317 [1]</TD>
            <TD>BR photometry of UGC 685 (Hopp, 1999)</TD>
            <TD>B and R CCD images and J NICMOS3 frames taken with the Calar Alto 3.5m telescope of the dwarf irregular galaxy UGC 685 are presented. The brightest part of the stellar population is resolved in B and R, very few also in J. The stellar color-magnitude diagram is discussed. An estimate of the distance to UGC 685 of 5. 5Mpc is derived based on the brightest blue supergiant stars. Most of the resolved bright stars show colors in the range -0.1&lt;=B-R&lt;=+0.7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317#1</TD>
            <TD>2011-09-14T21:10:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/317</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/317</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/317 [2]</TD>
            <TD>BR photometry of UGC 685 (Hopp, 1999)</TD>
            <TD>B and R CCD images and J NICMOS3 frames taken with the Calar Alto 3.5m telescope of the dwarf irregular galaxy UGC 685 are presented. The brightest part of the stellar population is resolved in B and R, very few also in J. The stellar color-magnitude diagram is discussed. An estimate of the distance to UGC 685 of 5. 5Mpc is derived based on the brightest blue supergiant stars. Most of the resolved bright stars show colors in the range -0.1&lt;=B-R&lt;=+0.7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317#2</TD>
            <TD>2011-09-14T21:10:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/317&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/317</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/317 [table3]</TD>
            <TD>BR photometry of UGC 685 (Hopp, 1999)</TD>
            <TD>B and R CCD images and J NICMOS3 frames taken with the Calar Alto 3.5m telescope of the dwarf irregular galaxy UGC 685 are presented. The brightest part of the stellar population is resolved in B and R, very few also in J. The stellar color-magnitude diagram is discussed. An estimate of the distance to UGC 685 of 5. 5Mpc is derived based on the brightest blue supergiant stars. Most of the resolved bright stars show colors in the range -0.1&lt;=B-R&lt;=+0.7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317#table3</TD>
            <TD>2011-09-14T21:10:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/317&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/317</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/327/325 [1]</TD>
            <TD>Distances of molecular cloud (May+, 1997)</TD>
            <TD>We have used a deep CO survey (at 115GHz) of the third galactic quadrant (May et al., 1993A&amp;AS...99..105M) to derive the physical properties of molecular clouds in the outer Galaxy. Within the range of this survey, from 194{deg} to 270{deg} in galactic longitude, 177 molecular clouds have been identified beyond 2 kpc from the Sun. Distances have been determined kinematically using the rotation curve of Brand (1986, Ph.D. Thesis, University of Leiden) with R_{sun}_=8.5kpc and {Theta}_{sun}_=220km/s.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325#1</TD>
            <TD>2012-11-13T13:38:52Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/327/325</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/325</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/327/325 [2]</TD>
            <TD>Distances of molecular cloud (May+, 1997)</TD>
            <TD>We have used a deep CO survey (at 115GHz) of the third galactic quadrant (May et al., 1993A&amp;AS...99..105M) to derive the physical properties of molecular clouds in the outer Galaxy. Within the range of this survey, from 194{deg} to 270{deg} in galactic longitude, 177 molecular clouds have been identified beyond 2 kpc from the Sun. Distances have been determined kinematically using the rotation curve of Brand (1986, Ph.D. Thesis, University of Leiden) with R_{sun}_=8.5kpc and {Theta}_{sun}_=220km/s.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325#2</TD>
            <TD>2012-11-13T13:38:52Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/327/325&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/325</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/325 [table2]</TD>
            <TD>Distances of molecular cloud (May+, 1997)</TD>
            <TD>We have used a deep CO survey (at 115GHz) of the third galactic quadrant (May et al., 1993A&amp;AS...99..105M) to derive the physical properties of molecular clouds in the outer Galaxy. Within the range of this survey, from 194{deg} to 270{deg} in galactic longitude, 177 molecular clouds have been identified beyond 2 kpc from the Sun. Distances have been determined kinematically using the rotation curve of Brand (1986, Ph.D. Thesis, University of Leiden) with R_{sun}_=8.5kpc and {Theta}_{sun}_=220km/s.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325#table2</TD>
            <TD>2012-11-13T13:38:52Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/325&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/325</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/38/571 [1]</TD>
            <TD>Astrophysical parameters for 593 open clusters (Gozha+, 2012)</TD>
            <TD>Based on published data, we have compiled a catalogue of fundamental astrophysical parameters for 593 open clusters of the Galaxy. In particular, the catalogue provides the Galactic orbital elements for 500 clusters, the masses, central concentrations, and ellipticities for 424 clusters, the metallicities for 264 clusters, and the relative magnesium abundances for 56 clusters. We describe the sources of initial data and estimate the errors in the investigated parameters. The selection effects are discussed. The chemical and kinematical properties of the open clusters and field thin-disk stars are shown to differ. We provide evidence for the heterogeneity of the population of open star clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571#1</TD>
            <TD>2012-12-08T14:23:03Z</TD>
            <TD>#Abundances#Open_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/38/571</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/38/571</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/38/571 [2]</TD>
            <TD>Astrophysical parameters for 593 open clusters (Gozha+, 2012)</TD>
            <TD>Based on published data, we have compiled a catalogue of fundamental astrophysical parameters for 593 open clusters of the Galaxy. In particular, the catalogue provides the Galactic orbital elements for 500 clusters, the masses, central concentrations, and ellipticities for 424 clusters, the metallicities for 264 clusters, and the relative magnesium abundances for 56 clusters. We describe the sources of initial data and estimate the errors in the investigated parameters. The selection effects are discussed. The chemical and kinematical properties of the open clusters and field thin-disk stars are shown to differ. We provide evidence for the heterogeneity of the population of open star clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571#2</TD>
            <TD>2012-12-08T14:23:03Z</TD>
            <TD>#Abundances#Open_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/38/571&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/38/571</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/38/571 [catalog]</TD>
            <TD>Astrophysical parameters for 593 open clusters (Gozha+, 2012)</TD>
            <TD>Based on published data, we have compiled a catalogue of fundamental astrophysical parameters for 593 open clusters of the Galaxy. In particular, the catalogue provides the Galactic orbital elements for 500 clusters, the masses, central concentrations, and ellipticities for 424 clusters, the metallicities for 264 clusters, and the relative magnesium abundances for 56 clusters. We describe the sources of initial data and estimate the errors in the investigated parameters. The selection effects are discussed. The chemical and kinematical properties of the open clusters and field thin-disk stars are shown to differ. We provide evidence for the heterogeneity of the population of open star clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571#catalog</TD>
            <TD>2012-12-08T14:23:03Z</TD>
            <TD>#Abundances#Open_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/38/571&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/38/571</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/317 [1]</TD>
            <TD>BR photometry of UGC 685 (Hopp, 1999)</TD>
            <TD>B and R CCD images and J NICMOS3 frames taken with the Calar Alto 3.5m telescope of the dwarf irregular galaxy UGC 685 are presented. The brightest part of the stellar population is resolved in B and R, very few also in J. The stellar color-magnitude diagram is discussed. An estimate of the distance to UGC 685 of 5. 5Mpc is derived based on the brightest blue supergiant stars. Most of the resolved bright stars show colors in the range -0.1&lt;=B-R&lt;=+0.7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317#1</TD>
            <TD>2011-09-14T21:10:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/317</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/317</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/317 [2]</TD>
            <TD>BR photometry of UGC 685 (Hopp, 1999)</TD>
            <TD>B and R CCD images and J NICMOS3 frames taken with the Calar Alto 3.5m telescope of the dwarf irregular galaxy UGC 685 are presented. The brightest part of the stellar population is resolved in B and R, very few also in J. The stellar color-magnitude diagram is discussed. An estimate of the distance to UGC 685 of 5. 5Mpc is derived based on the brightest blue supergiant stars. Most of the resolved bright stars show colors in the range -0.1&lt;=B-R&lt;=+0.7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317#2</TD>
            <TD>2011-09-14T21:10:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/317&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/317</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/317 [table3]</TD>
            <TD>BR photometry of UGC 685 (Hopp, 1999)</TD>
            <TD>B and R CCD images and J NICMOS3 frames taken with the Calar Alto 3.5m telescope of the dwarf irregular galaxy UGC 685 are presented. The brightest part of the stellar population is resolved in B and R, very few also in J. The stellar color-magnitude diagram is discussed. An estimate of the distance to UGC 685 of 5. 5Mpc is derived based on the brightest blue supergiant stars. Most of the resolved bright stars show colors in the range -0.1&lt;=B-R&lt;=+0.7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317#table3</TD>
            <TD>2011-09-14T21:10:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/317</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/317&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/317</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/327/325 [1]</TD>
            <TD>Distances of molecular cloud (May+, 1997)</TD>
            <TD>We have used a deep CO survey (at 115GHz) of the third galactic quadrant (May et al., 1993A&amp;AS...99..105M) to derive the physical properties of molecular clouds in the outer Galaxy. Within the range of this survey, from 194{deg} to 270{deg} in galactic longitude, 177 molecular clouds have been identified beyond 2 kpc from the Sun. Distances have been determined kinematically using the rotation curve of Brand (1986, Ph.D. Thesis, University of Leiden) with R_{sun}_=8.5kpc and {Theta}_{sun}_=220km/s.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325#1</TD>
            <TD>2012-11-13T13:38:52Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/327/325</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/325</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/327/325 [2]</TD>
            <TD>Distances of molecular cloud (May+, 1997)</TD>
            <TD>We have used a deep CO survey (at 115GHz) of the third galactic quadrant (May et al., 1993A&amp;AS...99..105M) to derive the physical properties of molecular clouds in the outer Galaxy. Within the range of this survey, from 194{deg} to 270{deg} in galactic longitude, 177 molecular clouds have been identified beyond 2 kpc from the Sun. Distances have been determined kinematically using the rotation curve of Brand (1986, Ph.D. Thesis, University of Leiden) with R_{sun}_=8.5kpc and {Theta}_{sun}_=220km/s.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325#2</TD>
            <TD>2012-11-13T13:38:52Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/327/325&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/325</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/327/325 [table2]</TD>
            <TD>Distances of molecular cloud (May+, 1997)</TD>
            <TD>We have used a deep CO survey (at 115GHz) of the third galactic quadrant (May et al., 1993A&amp;AS...99..105M) to derive the physical properties of molecular clouds in the outer Galaxy. Within the range of this survey, from 194{deg} to 270{deg} in galactic longitude, 177 molecular clouds have been identified beyond 2 kpc from the Sun. Distances have been determined kinematically using the rotation curve of Brand (1986, Ph.D. Thesis, University of Leiden) with R_{sun}_=8.5kpc and {Theta}_{sun}_=220km/s.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325#table2</TD>
            <TD>2012-11-13T13:38:52Z</TD>
            <TD>#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/327/325</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/327/325&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/327/325</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/38/571 [1]</TD>
            <TD>Astrophysical parameters for 593 open clusters (Gozha+, 2012)</TD>
            <TD>Based on published data, we have compiled a catalogue of fundamental astrophysical parameters for 593 open clusters of the Galaxy. In particular, the catalogue provides the Galactic orbital elements for 500 clusters, the masses, central concentrations, and ellipticities for 424 clusters, the metallicities for 264 clusters, and the relative magnesium abundances for 56 clusters. We describe the sources of initial data and estimate the errors in the investigated parameters. The selection effects are discussed. The chemical and kinematical properties of the open clusters and field thin-disk stars are shown to differ. We provide evidence for the heterogeneity of the population of open star clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571#1</TD>
            <TD>2012-12-08T14:23:03Z</TD>
            <TD>#Abundances#Open_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/38/571</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/38/571</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/38/571 [2]</TD>
            <TD>Astrophysical parameters for 593 open clusters (Gozha+, 2012)</TD>
            <TD>Based on published data, we have compiled a catalogue of fundamental astrophysical parameters for 593 open clusters of the Galaxy. In particular, the catalogue provides the Galactic orbital elements for 500 clusters, the masses, central concentrations, and ellipticities for 424 clusters, the metallicities for 264 clusters, and the relative magnesium abundances for 56 clusters. We describe the sources of initial data and estimate the errors in the investigated parameters. The selection effects are discussed. The chemical and kinematical properties of the open clusters and field thin-disk stars are shown to differ. We provide evidence for the heterogeneity of the population of open star clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571#2</TD>
            <TD>2012-12-08T14:23:03Z</TD>
            <TD>#Abundances#Open_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/38/571&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/38/571</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/38/571 [catalog]</TD>
            <TD>Astrophysical parameters for 593 open clusters (Gozha+, 2012)</TD>
            <TD>Based on published data, we have compiled a catalogue of fundamental astrophysical parameters for 593 open clusters of the Galaxy. In particular, the catalogue provides the Galactic orbital elements for 500 clusters, the masses, central concentrations, and ellipticities for 424 clusters, the metallicities for 264 clusters, and the relative magnesium abundances for 56 clusters. We describe the sources of initial data and estimate the errors in the investigated parameters. The selection effects are discussed. The chemical and kinematical properties of the open clusters and field thin-disk stars are shown to differ. We provide evidence for the heterogeneity of the population of open star clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571#catalog</TD>
            <TD>2012-12-08T14:23:03Z</TD>
            <TD>#Abundances#Open_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/38/571&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/38/571</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/526/A45 [1]</TD>
            <TD>WINGS-SPE II catalog (Fritz+, 2011)</TD>
            <TD>Total stellar mass, stellar mass as a function of age, luminosity- and mass-weighted ages, and dust extinction values are presented for 5299 galaxies in 48 nearby galaxy clusters. Galaxies in the following clusters have been observed: A1069, A119, A151, A160, A193, A1291, A1631a, A1644, A1795, A1831, A1983, A1991, A2107, A2124, A2169, A2382, A2399, A2415, A2457, A2572a, A2589, A2593, A2622, A2626, A3128, A3158, A3266, A3376, A3395, A3490, A3497, A3556, A3560, A376, A3809, A500, A671, A754, A957x, A970, IIZw108, MKW3s,RX0058, RX1022, RX1740, Z2844, Z8338, and Z8852. Together with the afore mentioned parameters, we also provide model-derived observed and absolute magnitudes in Johnson and SLOAN photometric systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45#1</TD>
            <TD>2011-09-14T21:11:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/526/A45</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A45</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/526/A45 [2]</TD>
            <TD>WINGS-SPE II catalog (Fritz+, 2011)</TD>
            <TD>Total stellar mass, stellar mass as a function of age, luminosity- and mass-weighted ages, and dust extinction values are presented for 5299 galaxies in 48 nearby galaxy clusters. Galaxies in the following clusters have been observed: A1069, A119, A151, A160, A193, A1291, A1631a, A1644, A1795, A1831, A1983, A1991, A2107, A2124, A2169, A2382, A2399, A2415, A2457, A2572a, A2589, A2593, A2622, A2626, A3128, A3158, A3266, A3376, A3395, A3490, A3497, A3556, A3560, A376, A3809, A500, A671, A754, A957x, A970, IIZw108, MKW3s,RX0058, RX1022, RX1740, Z2844, Z8338, and Z8852. Together with the afore mentioned parameters, we also provide model-derived observed and absolute magnitudes in Johnson and SLOAN photometric systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45#2</TD>
            <TD>2011-09-14T21:11:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/526/A45&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/526/A45 [sfhist]</TD>
            <TD>WINGS-SPE II catalog (Fritz+, 2011)</TD>
            <TD>Total stellar mass, stellar mass as a function of age, luminosity- and mass-weighted ages, and dust extinction values are presented for 5299 galaxies in 48 nearby galaxy clusters. Galaxies in the following clusters have been observed: A1069, A119, A151, A160, A193, A1291, A1631a, A1644, A1795, A1831, A1983, A1991, A2107, A2124, A2169, A2382, A2399, A2415, A2457, A2572a, A2589, A2593, A2622, A2626, A3128, A3158, A3266, A3376, A3395, A3490, A3497, A3556, A3560, A376, A3809, A500, A671, A754, A957x, A970, IIZw108, MKW3s,RX0058, RX1022, RX1740, Z2844, Z8338, and Z8852. Together with the afore mentioned parameters, we also provide model-derived observed and absolute magnitudes in Johnson and SLOAN photometric systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45#sfhist</TD>
            <TD>2011-09-14T21:11:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/526/A45&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A45</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/450/105 [1]</TD>
            <TD>Properties of 153 Galactic globular clusters (Bica+, 2006)</TD>
            <TD>Parameters of the 153 presently known globular clusters in the Galaxy are listed in Table 1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105#1</TD>
            <TD>2012-11-13T13:44:00Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/450/105</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/450/105</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/450/105 [2]</TD>
            <TD>Properties of 153 Galactic globular clusters (Bica+, 2006)</TD>
            <TD>Parameters of the 153 presently known globular clusters in the Galaxy are listed in Table 1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105#2</TD>
            <TD>2012-11-13T13:44:00Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/450/105&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/450/105</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/450/105 [table1]</TD>
            <TD>Properties of 153 Galactic globular clusters (Bica+, 2006)</TD>
            <TD>Parameters of the 153 presently known globular clusters in the Galaxy are listed in Table 1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105#table1</TD>
            <TD>2012-11-13T13:44:00Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/450/105&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/450/105</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/38/571 [1]</TD>
            <TD>Astrophysical parameters for 593 open clusters (Gozha+, 2012)</TD>
            <TD>Based on published data, we have compiled a catalogue of fundamental astrophysical parameters for 593 open clusters of the Galaxy. In particular, the catalogue provides the Galactic orbital elements for 500 clusters, the masses, central concentrations, and ellipticities for 424 clusters, the metallicities for 264 clusters, and the relative magnesium abundances for 56 clusters. We describe the sources of initial data and estimate the errors in the investigated parameters. The selection effects are discussed. The chemical and kinematical properties of the open clusters and field thin-disk stars are shown to differ. We provide evidence for the heterogeneity of the population of open star clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571#1</TD>
            <TD>2012-12-08T14:23:03Z</TD>
            <TD>#Abundances#Open_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/38/571</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/38/571</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/38/571 [2]</TD>
            <TD>Astrophysical parameters for 593 open clusters (Gozha+, 2012)</TD>
            <TD>Based on published data, we have compiled a catalogue of fundamental astrophysical parameters for 593 open clusters of the Galaxy. In particular, the catalogue provides the Galactic orbital elements for 500 clusters, the masses, central concentrations, and ellipticities for 424 clusters, the metallicities for 264 clusters, and the relative magnesium abundances for 56 clusters. We describe the sources of initial data and estimate the errors in the investigated parameters. The selection effects are discussed. The chemical and kinematical properties of the open clusters and field thin-disk stars are shown to differ. We provide evidence for the heterogeneity of the population of open star clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571#2</TD>
            <TD>2012-12-08T14:23:03Z</TD>
            <TD>#Abundances#Open_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/38/571&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/38/571</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/38/571 [catalog]</TD>
            <TD>Astrophysical parameters for 593 open clusters (Gozha+, 2012)</TD>
            <TD>Based on published data, we have compiled a catalogue of fundamental astrophysical parameters for 593 open clusters of the Galaxy. In particular, the catalogue provides the Galactic orbital elements for 500 clusters, the masses, central concentrations, and ellipticities for 424 clusters, the metallicities for 264 clusters, and the relative magnesium abundances for 56 clusters. We describe the sources of initial data and estimate the errors in the investigated parameters. The selection effects are discussed. The chemical and kinematical properties of the open clusters and field thin-disk stars are shown to differ. We provide evidence for the heterogeneity of the population of open star clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571#catalog</TD>
            <TD>2012-12-08T14:23:03Z</TD>
            <TD>#Abundances#Open_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/38/571</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/38/571&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/38/571</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/450/105 [1]</TD>
            <TD>Properties of 153 Galactic globular clusters (Bica+, 2006)</TD>
            <TD>Parameters of the 153 presently known globular clusters in the Galaxy are listed in Table 1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105#1</TD>
            <TD>2012-11-13T13:44:00Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/450/105</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/450/105</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/450/105 [2]</TD>
            <TD>Properties of 153 Galactic globular clusters (Bica+, 2006)</TD>
            <TD>Parameters of the 153 presently known globular clusters in the Galaxy are listed in Table 1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105#2</TD>
            <TD>2012-11-13T13:44:00Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/450/105&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/450/105</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/450/105 [table1]</TD>
            <TD>Properties of 153 Galactic globular clusters (Bica+, 2006)</TD>
            <TD>Parameters of the 153 presently known globular clusters in the Galaxy are listed in Table 1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105#table1</TD>
            <TD>2012-11-13T13:44:00Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/450/105&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/450/105</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/526/A45 [1]</TD>
            <TD>WINGS-SPE II catalog (Fritz+, 2011)</TD>
            <TD>Total stellar mass, stellar mass as a function of age, luminosity- and mass-weighted ages, and dust extinction values are presented for 5299 galaxies in 48 nearby galaxy clusters. Galaxies in the following clusters have been observed: A1069, A119, A151, A160, A193, A1291, A1631a, A1644, A1795, A1831, A1983, A1991, A2107, A2124, A2169, A2382, A2399, A2415, A2457, A2572a, A2589, A2593, A2622, A2626, A3128, A3158, A3266, A3376, A3395, A3490, A3497, A3556, A3560, A376, A3809, A500, A671, A754, A957x, A970, IIZw108, MKW3s,RX0058, RX1022, RX1740, Z2844, Z8338, and Z8852. Together with the afore mentioned parameters, we also provide model-derived observed and absolute magnitudes in Johnson and SLOAN photometric systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45#1</TD>
            <TD>2011-09-14T21:11:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/526/A45</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A45</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/526/A45 [2]</TD>
            <TD>WINGS-SPE II catalog (Fritz+, 2011)</TD>
            <TD>Total stellar mass, stellar mass as a function of age, luminosity- and mass-weighted ages, and dust extinction values are presented for 5299 galaxies in 48 nearby galaxy clusters. Galaxies in the following clusters have been observed: A1069, A119, A151, A160, A193, A1291, A1631a, A1644, A1795, A1831, A1983, A1991, A2107, A2124, A2169, A2382, A2399, A2415, A2457, A2572a, A2589, A2593, A2622, A2626, A3128, A3158, A3266, A3376, A3395, A3490, A3497, A3556, A3560, A376, A3809, A500, A671, A754, A957x, A970, IIZw108, MKW3s,RX0058, RX1022, RX1740, Z2844, Z8338, and Z8852. Together with the afore mentioned parameters, we also provide model-derived observed and absolute magnitudes in Johnson and SLOAN photometric systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45#2</TD>
            <TD>2011-09-14T21:11:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/526/A45&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/526/A45 [sfhist]</TD>
            <TD>WINGS-SPE II catalog (Fritz+, 2011)</TD>
            <TD>Total stellar mass, stellar mass as a function of age, luminosity- and mass-weighted ages, and dust extinction values are presented for 5299 galaxies in 48 nearby galaxy clusters. Galaxies in the following clusters have been observed: A1069, A119, A151, A160, A193, A1291, A1631a, A1644, A1795, A1831, A1983, A1991, A2107, A2124, A2169, A2382, A2399, A2415, A2457, A2572a, A2589, A2593, A2622, A2626, A3128, A3158, A3266, A3376, A3395, A3490, A3497, A3556, A3560, A376, A3809, A500, A671, A754, A957x, A970, IIZw108, MKW3s,RX0058, RX1022, RX1740, Z2844, Z8338, and Z8852. Together with the afore mentioned parameters, we also provide model-derived observed and absolute magnitudes in Johnson and SLOAN photometric systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45#sfhist</TD>
            <TD>2011-09-14T21:11:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/526/A45&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAM [1]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1990 and March 2009 inclusive. No observation was done in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;http://www.iram.fr/&lt;/a&gt; (the IRAM Home Page).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iramlog#1</TD>
            <TD>2010-04-20T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iramlog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=iramlog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iramlog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRAM [2]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1990 and March 2009 inclusive. No observation was done in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;http://www.iram.fr/&lt;/a&gt; (the IRAM Home Page).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iramlog#2</TD>
            <TD>2010-04-20T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iramlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=iramlog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iramlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRAM [3]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1990 and March 2009 inclusive. No observation was done in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;http://www.iram.fr/&lt;/a&gt; (the IRAM Home Page).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iramlog#3</TD>
            <TD>2010-04-20T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iramlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_iramlog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iramlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/526/A45 [1]</TD>
            <TD>WINGS-SPE II catalog (Fritz+, 2011)</TD>
            <TD>Total stellar mass, stellar mass as a function of age, luminosity- and mass-weighted ages, and dust extinction values are presented for 5299 galaxies in 48 nearby galaxy clusters. Galaxies in the following clusters have been observed: A1069, A119, A151, A160, A193, A1291, A1631a, A1644, A1795, A1831, A1983, A1991, A2107, A2124, A2169, A2382, A2399, A2415, A2457, A2572a, A2589, A2593, A2622, A2626, A3128, A3158, A3266, A3376, A3395, A3490, A3497, A3556, A3560, A376, A3809, A500, A671, A754, A957x, A970, IIZw108, MKW3s,RX0058, RX1022, RX1740, Z2844, Z8338, and Z8852. Together with the afore mentioned parameters, we also provide model-derived observed and absolute magnitudes in Johnson and SLOAN photometric systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45#1</TD>
            <TD>2011-09-14T21:11:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/526/A45</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A45</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/526/A45 [2]</TD>
            <TD>WINGS-SPE II catalog (Fritz+, 2011)</TD>
            <TD>Total stellar mass, stellar mass as a function of age, luminosity- and mass-weighted ages, and dust extinction values are presented for 5299 galaxies in 48 nearby galaxy clusters. Galaxies in the following clusters have been observed: A1069, A119, A151, A160, A193, A1291, A1631a, A1644, A1795, A1831, A1983, A1991, A2107, A2124, A2169, A2382, A2399, A2415, A2457, A2572a, A2589, A2593, A2622, A2626, A3128, A3158, A3266, A3376, A3395, A3490, A3497, A3556, A3560, A376, A3809, A500, A671, A754, A957x, A970, IIZw108, MKW3s,RX0058, RX1022, RX1740, Z2844, Z8338, and Z8852. Together with the afore mentioned parameters, we also provide model-derived observed and absolute magnitudes in Johnson and SLOAN photometric systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45#2</TD>
            <TD>2011-09-14T21:11:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/526/A45&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/526/A45 [sfhist]</TD>
            <TD>WINGS-SPE II catalog (Fritz+, 2011)</TD>
            <TD>Total stellar mass, stellar mass as a function of age, luminosity- and mass-weighted ages, and dust extinction values are presented for 5299 galaxies in 48 nearby galaxy clusters. Galaxies in the following clusters have been observed: A1069, A119, A151, A160, A193, A1291, A1631a, A1644, A1795, A1831, A1983, A1991, A2107, A2124, A2169, A2382, A2399, A2415, A2457, A2572a, A2589, A2593, A2622, A2626, A3128, A3158, A3266, A3376, A3395, A3490, A3497, A3556, A3560, A376, A3809, A500, A671, A754, A957x, A970, IIZw108, MKW3s,RX0058, RX1022, RX1740, Z2844, Z8338, and Z8852. Together with the afore mentioned parameters, we also provide model-derived observed and absolute magnitudes in Johnson and SLOAN photometric systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45#sfhist</TD>
            <TD>2011-09-14T21:11:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A45</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/526/A45&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A45</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/450/105 [1]</TD>
            <TD>Properties of 153 Galactic globular clusters (Bica+, 2006)</TD>
            <TD>Parameters of the 153 presently known globular clusters in the Galaxy are listed in Table 1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105#1</TD>
            <TD>2012-11-13T13:44:00Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/450/105</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/450/105</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/450/105 [2]</TD>
            <TD>Properties of 153 Galactic globular clusters (Bica+, 2006)</TD>
            <TD>Parameters of the 153 presently known globular clusters in the Galaxy are listed in Table 1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105#2</TD>
            <TD>2012-11-13T13:44:00Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/450/105&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/450/105</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/450/105 [table1]</TD>
            <TD>Properties of 153 Galactic globular clusters (Bica+, 2006)</TD>
            <TD>Parameters of the 153 presently known globular clusters in the Galaxy are listed in Table 1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105#table1</TD>
            <TD>2012-11-13T13:44:00Z</TD>
            <TD>#Abundances#Globular_Clusters#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/450/105</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/450/105&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/450/105</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/861 [1]</TD>
            <TD>RR Lyrae in Draco dSph (Bonanos+, 2004)</TD>
            <TD>++++Lrecl of file 'table1.dat' (86) increased to 98 %B We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2m telescope on Mount Hopkins, Arizona, between 1998 August 19 and 1999 June 20, over 22 nights, over a period of 10 months, covering a 22'x22' field centered at {alpha}=17h19m57.5s, {delta}=57{deg}50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould &amp; Popowski (1998ApJ...508..844G) and 94 RRab stars from our field, we obtain a distance modulus of (m-M)_0_=19.40+/-0.02(stat)+/-0.15(syst)mag for Draco, corresponding to a distance of 75.8+/-0.7(stat)+/-5.4(syst)kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861#1</TD>
            <TD>2011-09-14T21:12:43Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/861</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/861</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/861 [2]</TD>
            <TD>RR Lyrae in Draco dSph (Bonanos+, 2004)</TD>
            <TD>++++Lrecl of file 'table1.dat' (86) increased to 98 %B We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2m telescope on Mount Hopkins, Arizona, between 1998 August 19 and 1999 June 20, over 22 nights, over a period of 10 months, covering a 22'x22' field centered at {alpha}=17h19m57.5s, {delta}=57{deg}50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould &amp; Popowski (1998ApJ...508..844G) and 94 RRab stars from our field, we obtain a distance modulus of (m-M)_0_=19.40+/-0.02(stat)+/-0.15(syst)mag for Draco, corresponding to a distance of 75.8+/-0.7(stat)+/-5.4(syst)kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861#2</TD>
            <TD>2011-09-14T21:12:43Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/861&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/861 [table1]</TD>
            <TD>RR Lyrae in Draco dSph (Bonanos+, 2004)</TD>
            <TD>++++Lrecl of file 'table1.dat' (86) increased to 98 %B We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2m telescope on Mount Hopkins, Arizona, between 1998 August 19 and 1999 June 20, over 22 nights, over a period of 10 months, covering a 22'x22' field centered at {alpha}=17h19m57.5s, {delta}=57{deg}50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould &amp; Popowski (1998ApJ...508..844G) and 94 RRab stars from our field, we obtain a distance modulus of (m-M)_0_=19.40+/-0.02(stat)+/-0.15(syst)mag for Draco, corresponding to a distance of 75.8+/-0.7(stat)+/-5.4(syst)kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861#table1</TD>
            <TD>2011-09-14T21:12:43Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/861&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAM [1]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1990 and March 2009 inclusive. No observation was done in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;http://www.iram.fr/&lt;/a&gt; (the IRAM Home Page).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iramlog#1</TD>
            <TD>2010-04-20T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iramlog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=iramlog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iramlog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRAM [2]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1990 and March 2009 inclusive. No observation was done in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;http://www.iram.fr/&lt;/a&gt; (the IRAM Home Page).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iramlog#2</TD>
            <TD>2010-04-20T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iramlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=iramlog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iramlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRAM [3]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1990 and March 2009 inclusive. No observation was done in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;http://www.iram.fr/&lt;/a&gt; (the IRAM Home Page).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iramlog#3</TD>
            <TD>2010-04-20T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iramlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_iramlog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iramlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/463 [1]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#1</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/463</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/463 [2]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#2</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table4]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table4</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table1]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table1</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table3]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table3</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table2]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table2</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/861 [1]</TD>
            <TD>RR Lyrae in Draco dSph (Bonanos+, 2004)</TD>
            <TD>++++Lrecl of file 'table1.dat' (86) increased to 98 %B We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2m telescope on Mount Hopkins, Arizona, between 1998 August 19 and 1999 June 20, over 22 nights, over a period of 10 months, covering a 22'x22' field centered at {alpha}=17h19m57.5s, {delta}=57{deg}50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould &amp; Popowski (1998ApJ...508..844G) and 94 RRab stars from our field, we obtain a distance modulus of (m-M)_0_=19.40+/-0.02(stat)+/-0.15(syst)mag for Draco, corresponding to a distance of 75.8+/-0.7(stat)+/-5.4(syst)kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861#1</TD>
            <TD>2011-09-14T21:12:43Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/861</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/861</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/861 [2]</TD>
            <TD>RR Lyrae in Draco dSph (Bonanos+, 2004)</TD>
            <TD>++++Lrecl of file 'table1.dat' (86) increased to 98 %B We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2m telescope on Mount Hopkins, Arizona, between 1998 August 19 and 1999 June 20, over 22 nights, over a period of 10 months, covering a 22'x22' field centered at {alpha}=17h19m57.5s, {delta}=57{deg}50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould &amp; Popowski (1998ApJ...508..844G) and 94 RRab stars from our field, we obtain a distance modulus of (m-M)_0_=19.40+/-0.02(stat)+/-0.15(syst)mag for Draco, corresponding to a distance of 75.8+/-0.7(stat)+/-5.4(syst)kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861#2</TD>
            <TD>2011-09-14T21:12:43Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/861&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/861 [table1]</TD>
            <TD>RR Lyrae in Draco dSph (Bonanos+, 2004)</TD>
            <TD>++++Lrecl of file 'table1.dat' (86) increased to 98 %B We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2m telescope on Mount Hopkins, Arizona, between 1998 August 19 and 1999 June 20, over 22 nights, over a period of 10 months, covering a 22'x22' field centered at {alpha}=17h19m57.5s, {delta}=57{deg}50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould &amp; Popowski (1998ApJ...508..844G) and 94 RRab stars from our field, we obtain a distance modulus of (m-M)_0_=19.40+/-0.02(stat)+/-0.15(syst)mag for Draco, corresponding to a distance of 75.8+/-0.7(stat)+/-5.4(syst)kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861#table1</TD>
            <TD>2011-09-14T21:12:43Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/861&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/861</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/861 [1]</TD>
            <TD>RR Lyrae in Draco dSph (Bonanos+, 2004)</TD>
            <TD>++++Lrecl of file 'table1.dat' (86) increased to 98 %B We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2m telescope on Mount Hopkins, Arizona, between 1998 August 19 and 1999 June 20, over 22 nights, over a period of 10 months, covering a 22'x22' field centered at {alpha}=17h19m57.5s, {delta}=57{deg}50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould &amp; Popowski (1998ApJ...508..844G) and 94 RRab stars from our field, we obtain a distance modulus of (m-M)_0_=19.40+/-0.02(stat)+/-0.15(syst)mag for Draco, corresponding to a distance of 75.8+/-0.7(stat)+/-5.4(syst)kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861#1</TD>
            <TD>2011-09-14T21:12:43Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/861</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/861</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/861 [2]</TD>
            <TD>RR Lyrae in Draco dSph (Bonanos+, 2004)</TD>
            <TD>++++Lrecl of file 'table1.dat' (86) increased to 98 %B We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2m telescope on Mount Hopkins, Arizona, between 1998 August 19 and 1999 June 20, over 22 nights, over a period of 10 months, covering a 22'x22' field centered at {alpha}=17h19m57.5s, {delta}=57{deg}50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould &amp; Popowski (1998ApJ...508..844G) and 94 RRab stars from our field, we obtain a distance modulus of (m-M)_0_=19.40+/-0.02(stat)+/-0.15(syst)mag for Draco, corresponding to a distance of 75.8+/-0.7(stat)+/-5.4(syst)kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861#2</TD>
            <TD>2011-09-14T21:12:43Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/861&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/861 [table1]</TD>
            <TD>RR Lyrae in Draco dSph (Bonanos+, 2004)</TD>
            <TD>++++Lrecl of file 'table1.dat' (86) increased to 98 %B We present the first CCD variability study of the Draco dwarf spheroidal galaxy. The data were obtained with the Fred Lawrence Whipple Observatory 1.2m telescope on Mount Hopkins, Arizona, between 1998 August 19 and 1999 June 20, over 22 nights, over a period of 10 months, covering a 22'x22' field centered at {alpha}=17h19m57.5s, {delta}=57{deg}50'05" (J2000.0). The analysis of the BVI images produced 163 variable stars, 146 of which were RR Lyrae: 123 RRab, 16 RRc, 6 RRd, and one RR12. The other variables include a SX Phe star, four anomalous Cepheids, and a field eclipsing binary. Using the short distance scale statistical parallax calibration of Gould &amp; Popowski (1998ApJ...508..844G) and 94 RRab stars from our field, we obtain a distance modulus of (m-M)_0_=19.40+/-0.02(stat)+/-0.15(syst)mag for Draco, corresponding to a distance of 75.8+/-0.7(stat)+/-5.4(syst)kpc. By comparing the spread in magnitudes of RRab stars in B, V, and I, we find no evidence for internal dust in the Draco dwarf spheroidal galaxy. The catalog of all variables, as well as their photometry and finding charts, is available electronically via anonymous ftp and the World Wide Web. The complete set of the CCD frames is available upon request.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861#table1</TD>
            <TD>2011-09-14T21:12:43Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/861</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/861&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/861</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>IRAM [1]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1990 and March 2009 inclusive. No observation was done in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;http://www.iram.fr/&lt;/a&gt; (the IRAM Home Page).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iramlog#1</TD>
            <TD>2010-04-20T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iramlog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=iramlog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iramlog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>IRAM [2]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1990 and March 2009 inclusive. No observation was done in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;http://www.iram.fr/&lt;/a&gt; (the IRAM Home Page).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iramlog#2</TD>
            <TD>2010-04-20T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iramlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=iramlog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iramlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>IRAM [3]</TD>
            <TD>IRAM Plateau de Bure Interferometer Observation Log</TD>
            <TD>This table contains the IRAM Plateau de Bure Interferometer observation log. The Institut de Radio Astronomie Millimetrique (IRAM) was founded in 1979 and is operated as a French-German-Spanish collaboration. Its partner institutes are the CNRS (Centre National de la Recherche Scientifique, France), the MPG (Max Planck Gesellschaft, Germany), and the IGN (Instituto Geografico Nacional, Spain). The principal activity of IRAM is the study of cold matter (molecular gas and dust) in the solar system, in our Galaxy, and out to cosmological distances, in order to determine its composition, density, mass, temperature, and kinematics. IRAM operates two observatories at millimeter wavelengths which are open to the international astronomical community: the 30-m single-dish telescope on Pico Veleta (2850m), Spain, and the six-antenna interferometer on the Plateau de Bure (2550m) in France. Both sites are at high altitude to reduce the absorption by water vapor. The observatories are supported by the IRAM offices and laboratories in Granada and Grenoble. The observation log included here concerns the Plateau de Bure Interferometer (PDBI), and summarizes the observations made there between December 1990 and March 2009 inclusive. No observation was done in the periods of 1999-Sep-30 to 2000-Dec-03, and of 2006-Sep-25 to 2007-Jan-18 (installation of the new receiver), notice. For more information on IRAM see &lt;a href="http://www.iram.fr/"&gt;http://www.iram.fr/&lt;/a&gt; (the IRAM Home Page).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/iramlog#3</TD>
            <TD>2010-04-20T00:00:00Z</TD>
            <TD>#Observation#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/iramlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_iramlog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/ground-based/iramlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/463 [1]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#1</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/463</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/463 [2]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#2</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table4]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table4</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table1]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table1</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table3]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table3</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table2]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table2</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/405/783 [1]</TD>
            <TD>Passive red spirals in Galaxy Zoo (Masters+, 2010)</TD>
            <TD>The sample of visually classified spiral galaxies used in this paper is drawn from the Galaxy Zoo (GZ1) clean catalogue (Lintott et al. 2008MNRAS.389.1179L) which, by an order of magnitude, is the largest morphologically classified sample of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783#1</TD>
            <TD>2011-09-14T21:25:51Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/405/783</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/783</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/405/783 [2]</TD>
            <TD>Passive red spirals in Galaxy Zoo (Masters+, 2010)</TD>
            <TD>The sample of visually classified spiral galaxies used in this paper is drawn from the Galaxy Zoo (GZ1) clean catalogue (Lintott et al. 2008MNRAS.389.1179L) which, by an order of magnitude, is the largest morphologically classified sample of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783#2</TD>
            <TD>2011-09-14T21:25:51Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/405/783&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/405/783 [spirals]</TD>
            <TD>Passive red spirals in Galaxy Zoo (Masters+, 2010)</TD>
            <TD>The sample of visually classified spiral galaxies used in this paper is drawn from the Galaxy Zoo (GZ1) clean catalogue (Lintott et al. 2008MNRAS.389.1179L) which, by an order of magnitude, is the largest morphologically classified sample of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783#spirals</TD>
            <TD>2011-09-14T21:25:51Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/405/783&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/783</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/440/783 [1]</TD>
            <TD>OB associations in NGC 7793 (Pietrzynski+, 2005)</TD>
            <TD>The observations were performed during two photometric nights in July 2001 with the ESO VLT and FORS1 instrument (see ESO website for details) in imaging mode. The FORS1 field of view is approximately 6.8x6.8arcmin, and the pixel scale of the FORS1 detector is 0.2arcsec/pix. We obtained images in B, V, I, and Halpha filters for two fields, which together cover almost the entire galaxy. The data were obtained under 1-arcsec seeing conditions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783#1</TD>
            <TD>2011-09-14T19:57:07Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/440/783</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/783</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/440/783 [2]</TD>
            <TD>OB associations in NGC 7793 (Pietrzynski+, 2005)</TD>
            <TD>The observations were performed during two photometric nights in July 2001 with the ESO VLT and FORS1 instrument (see ESO website for details) in imaging mode. The FORS1 field of view is approximately 6.8x6.8arcmin, and the pixel scale of the FORS1 detector is 0.2arcsec/pix. We obtained images in B, V, I, and Halpha filters for two fields, which together cover almost the entire galaxy. The data were obtained under 1-arcsec seeing conditions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783#2</TD>
            <TD>2011-09-14T19:57:07Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/440/783&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/440/783 [table1]</TD>
            <TD>OB associations in NGC 7793 (Pietrzynski+, 2005)</TD>
            <TD>The observations were performed during two photometric nights in July 2001 with the ESO VLT and FORS1 instrument (see ESO website for details) in imaging mode. The FORS1 field of view is approximately 6.8x6.8arcmin, and the pixel scale of the FORS1 detector is 0.2arcsec/pix. We obtained images in B, V, I, and Halpha filters for two fields, which together cover almost the entire galaxy. The data were obtained under 1-arcsec seeing conditions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783#table1</TD>
            <TD>2011-09-14T19:57:07Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/440/783&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/783</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/463 [1]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#1</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/463</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/463 [2]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#2</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table4]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table4</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table1]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table1</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table3]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table3</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/463 [table2]</TD>
            <TD>Crux region redshifts (Fairall+ 1998)</TD>
            <TD>In our systematic optical galaxy search behind the southern Milky Way, 3760 (mostly unknown) galaxies with diameters D&gt;0.2' were identified in the Crux region (287{deg}&lt;~l&lt;~318{deg}, |b|&lt;~10{deg}, Woudt &amp; Kraan-Korteweg 1998, in press). Prior to this investigation, only 65 of these galaxies had known redshifts. In order to map the galaxy distribution in redshift space we obtained spectra for 226 bright (B_J_&lt;~18.0mag) objects with the 1.9m telescope of the South African Astronomical Observatory (SAAO). Redshifts could be determined for 209 objects, of which 173 have good signal-to-noise ratios. Of the 36 tentative redshifts, four are confirmed through independent values in the literature. The redshifts of three objects indicate them to be galactic in origin. One of these confirms a suspected Planetary Nebula. For 17 of the galaxies, no redshift could be determined due to poor signal-to-noise ratios. In addition, 26 redshifts have have been measured in the Hydra-Antlia region investigated earlier (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;), of which one is a tentative estimate. Two main structures crossing the Galactic Plane in the Crux region have now become clear. A narrow, nearby filament from (l, b)=(340{deg}, -25{deg}) to the Centaurus cluster can be traced. This filament runs almost parallel to the extension of the Hydra-Antlia clusters found earlier and is part of what we have earlier termed the ``Centaurus Wall'' extending in redshift-space between 0&lt;=v&lt;=6000km/s (Fairall &amp; Paverd 1995, in Wide-Field Spedctroscopy and the Distant Universe, p. 121). The main outcome of this survey however, is the recognition of another massive extended structure between 4000&lt;=v&lt;=8000km/s. This broad structure, dubbed the Norma Supercluster (Woudt et al. 1997, in press), runs nearly parallel to the Galactic Plane from Vela to ACO 3627 (its centre) from where it continues to the Pavo cluster. This massive structure is believed to be associated with the Great Attractor. The survey has furthermore revealed a set of cellular structures, similar to those seen in redshift space at higher galactic latitudes, but never before seen so clearly behind the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463#table2</TD>
            <TD>2012-11-13T13:52:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/463</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/405/783 [1]</TD>
            <TD>Passive red spirals in Galaxy Zoo (Masters+, 2010)</TD>
            <TD>The sample of visually classified spiral galaxies used in this paper is drawn from the Galaxy Zoo (GZ1) clean catalogue (Lintott et al. 2008MNRAS.389.1179L) which, by an order of magnitude, is the largest morphologically classified sample of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783#1</TD>
            <TD>2011-09-14T21:25:51Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/405/783</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/783</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/405/783 [2]</TD>
            <TD>Passive red spirals in Galaxy Zoo (Masters+, 2010)</TD>
            <TD>The sample of visually classified spiral galaxies used in this paper is drawn from the Galaxy Zoo (GZ1) clean catalogue (Lintott et al. 2008MNRAS.389.1179L) which, by an order of magnitude, is the largest morphologically classified sample of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783#2</TD>
            <TD>2011-09-14T21:25:51Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/405/783&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/405/783 [spirals]</TD>
            <TD>Passive red spirals in Galaxy Zoo (Masters+, 2010)</TD>
            <TD>The sample of visually classified spiral galaxies used in this paper is drawn from the Galaxy Zoo (GZ1) clean catalogue (Lintott et al. 2008MNRAS.389.1179L) which, by an order of magnitude, is the largest morphologically classified sample of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783#spirals</TD>
            <TD>2011-09-14T21:25:51Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/405/783&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/783</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/440/783 [1]</TD>
            <TD>OB associations in NGC 7793 (Pietrzynski+, 2005)</TD>
            <TD>The observations were performed during two photometric nights in July 2001 with the ESO VLT and FORS1 instrument (see ESO website for details) in imaging mode. The FORS1 field of view is approximately 6.8x6.8arcmin, and the pixel scale of the FORS1 detector is 0.2arcsec/pix. We obtained images in B, V, I, and Halpha filters for two fields, which together cover almost the entire galaxy. The data were obtained under 1-arcsec seeing conditions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783#1</TD>
            <TD>2011-09-14T19:57:07Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/440/783</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/783</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/440/783 [2]</TD>
            <TD>OB associations in NGC 7793 (Pietrzynski+, 2005)</TD>
            <TD>The observations were performed during two photometric nights in July 2001 with the ESO VLT and FORS1 instrument (see ESO website for details) in imaging mode. The FORS1 field of view is approximately 6.8x6.8arcmin, and the pixel scale of the FORS1 detector is 0.2arcsec/pix. We obtained images in B, V, I, and Halpha filters for two fields, which together cover almost the entire galaxy. The data were obtained under 1-arcsec seeing conditions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783#2</TD>
            <TD>2011-09-14T19:57:07Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/440/783&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/440/783 [table1]</TD>
            <TD>OB associations in NGC 7793 (Pietrzynski+, 2005)</TD>
            <TD>The observations were performed during two photometric nights in July 2001 with the ESO VLT and FORS1 instrument (see ESO website for details) in imaging mode. The FORS1 field of view is approximately 6.8x6.8arcmin, and the pixel scale of the FORS1 detector is 0.2arcsec/pix. We obtained images in B, V, I, and Halpha filters for two fields, which together cover almost the entire galaxy. The data were obtained under 1-arcsec seeing conditions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783#table1</TD>
            <TD>2011-09-14T19:57:07Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/440/783&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/783</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/90/1681 [1]</TD>
            <TD>The Virgo Cluster Catalog (VCC) (Binggeli+, 1985)</TD>
            <TD>The present catalog of 2096 galaxies within an area of about 140{deg}^2^ approximately centered on the Virgo cluster should be an essentially complete listing of all certain and possible cluster members, independent of morphological type. Cluster membership is essentially decided by galaxy morphology; for giants and the rare class of high surface brightness dwarfs, membership rests on velocity data. While 1277 of the catalog entries are considered members of the Virgo cluster, 574 are possible members and 245 appear to be background Zwicky galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681#1</TD>
            <TD>2012-11-13T13:58:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/90/1681</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/1681</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/90/1681 [2]</TD>
            <TD>The Virgo Cluster Catalog (VCC) (Binggeli+, 1985)</TD>
            <TD>The present catalog of 2096 galaxies within an area of about 140{deg}^2^ approximately centered on the Virgo cluster should be an essentially complete listing of all certain and possible cluster members, independent of morphological type. Cluster membership is essentially decided by galaxy morphology; for giants and the rare class of high surface brightness dwarfs, membership rests on velocity data. While 1277 of the catalog entries are considered members of the Virgo cluster, 574 are possible members and 245 appear to be background Zwicky galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681#2</TD>
            <TD>2012-11-13T13:58:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/90/1681&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/1681</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/90/1681 [vcc]</TD>
            <TD>The Virgo Cluster Catalog (VCC) (Binggeli+, 1985)</TD>
            <TD>The present catalog of 2096 galaxies within an area of about 140{deg}^2^ approximately centered on the Virgo cluster should be an essentially complete listing of all certain and possible cluster members, independent of morphological type. Cluster membership is essentially decided by galaxy morphology; for giants and the rare class of high surface brightness dwarfs, membership rests on velocity data. While 1277 of the catalog entries are considered members of the Virgo cluster, 574 are possible members and 245 appear to be background Zwicky galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681#vcc</TD>
            <TD>2012-11-13T13:58:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/90/1681&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/1681</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/405/783 [1]</TD>
            <TD>Passive red spirals in Galaxy Zoo (Masters+, 2010)</TD>
            <TD>The sample of visually classified spiral galaxies used in this paper is drawn from the Galaxy Zoo (GZ1) clean catalogue (Lintott et al. 2008MNRAS.389.1179L) which, by an order of magnitude, is the largest morphologically classified sample of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783#1</TD>
            <TD>2011-09-14T21:25:51Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/405/783</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/783</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/405/783 [2]</TD>
            <TD>Passive red spirals in Galaxy Zoo (Masters+, 2010)</TD>
            <TD>The sample of visually classified spiral galaxies used in this paper is drawn from the Galaxy Zoo (GZ1) clean catalogue (Lintott et al. 2008MNRAS.389.1179L) which, by an order of magnitude, is the largest morphologically classified sample of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783#2</TD>
            <TD>2011-09-14T21:25:51Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/405/783&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/405/783 [spirals]</TD>
            <TD>Passive red spirals in Galaxy Zoo (Masters+, 2010)</TD>
            <TD>The sample of visually classified spiral galaxies used in this paper is drawn from the Galaxy Zoo (GZ1) clean catalogue (Lintott et al. 2008MNRAS.389.1179L) which, by an order of magnitude, is the largest morphologically classified sample of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783#spirals</TD>
            <TD>2011-09-14T21:25:51Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/783</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/405/783&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/783</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/440/783 [1]</TD>
            <TD>OB associations in NGC 7793 (Pietrzynski+, 2005)</TD>
            <TD>The observations were performed during two photometric nights in July 2001 with the ESO VLT and FORS1 instrument (see ESO website for details) in imaging mode. The FORS1 field of view is approximately 6.8x6.8arcmin, and the pixel scale of the FORS1 detector is 0.2arcsec/pix. We obtained images in B, V, I, and Halpha filters for two fields, which together cover almost the entire galaxy. The data were obtained under 1-arcsec seeing conditions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783#1</TD>
            <TD>2011-09-14T19:57:07Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/440/783</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/783</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/440/783 [2]</TD>
            <TD>OB associations in NGC 7793 (Pietrzynski+, 2005)</TD>
            <TD>The observations were performed during two photometric nights in July 2001 with the ESO VLT and FORS1 instrument (see ESO website for details) in imaging mode. The FORS1 field of view is approximately 6.8x6.8arcmin, and the pixel scale of the FORS1 detector is 0.2arcsec/pix. We obtained images in B, V, I, and Halpha filters for two fields, which together cover almost the entire galaxy. The data were obtained under 1-arcsec seeing conditions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783#2</TD>
            <TD>2011-09-14T19:57:07Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/440/783&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/440/783 [table1]</TD>
            <TD>OB associations in NGC 7793 (Pietrzynski+, 2005)</TD>
            <TD>The observations were performed during two photometric nights in July 2001 with the ESO VLT and FORS1 instrument (see ESO website for details) in imaging mode. The FORS1 field of view is approximately 6.8x6.8arcmin, and the pixel scale of the FORS1 detector is 0.2arcsec/pix. We obtained images in B, V, I, and Halpha filters for two fields, which together cover almost the entire galaxy. The data were obtained under 1-arcsec seeing conditions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783#table1</TD>
            <TD>2011-09-14T19:57:07Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/783</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/440/783&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/783</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/90/1681 [1]</TD>
            <TD>The Virgo Cluster Catalog (VCC) (Binggeli+, 1985)</TD>
            <TD>The present catalog of 2096 galaxies within an area of about 140{deg}^2^ approximately centered on the Virgo cluster should be an essentially complete listing of all certain and possible cluster members, independent of morphological type. Cluster membership is essentially decided by galaxy morphology; for giants and the rare class of high surface brightness dwarfs, membership rests on velocity data. While 1277 of the catalog entries are considered members of the Virgo cluster, 574 are possible members and 245 appear to be background Zwicky galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681#1</TD>
            <TD>2012-11-13T13:58:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/90/1681</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/1681</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/90/1681 [2]</TD>
            <TD>The Virgo Cluster Catalog (VCC) (Binggeli+, 1985)</TD>
            <TD>The present catalog of 2096 galaxies within an area of about 140{deg}^2^ approximately centered on the Virgo cluster should be an essentially complete listing of all certain and possible cluster members, independent of morphological type. Cluster membership is essentially decided by galaxy morphology; for giants and the rare class of high surface brightness dwarfs, membership rests on velocity data. While 1277 of the catalog entries are considered members of the Virgo cluster, 574 are possible members and 245 appear to be background Zwicky galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681#2</TD>
            <TD>2012-11-13T13:58:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/90/1681&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/1681</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/90/1681 [vcc]</TD>
            <TD>The Virgo Cluster Catalog (VCC) (Binggeli+, 1985)</TD>
            <TD>The present catalog of 2096 galaxies within an area of about 140{deg}^2^ approximately centered on the Virgo cluster should be an essentially complete listing of all certain and possible cluster members, independent of morphological type. Cluster membership is essentially decided by galaxy morphology; for giants and the rare class of high surface brightness dwarfs, membership rests on velocity data. While 1277 of the catalog entries are considered members of the Virgo cluster, 574 are possible members and 245 appear to be background Zwicky galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681#vcc</TD>
            <TD>2012-11-13T13:58:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/90/1681&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/1681</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/486 [1]</TD>
            <TD>HDF-S: STIS imaging (Gardner+, 2000)</TD>
            <TD>We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486#1</TD>
            <TD>2011-09-14T19:59:26Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/486</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/486</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/486 [2]</TD>
            <TD>HDF-S: STIS imaging (Gardner+, 2000)</TD>
            <TD>We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486#2</TD>
            <TD>2011-09-14T19:59:26Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/486&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/486</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/119/486 [table2]</TD>
            <TD>HDF-S: STIS imaging (Gardner+, 2000)</TD>
            <TD>We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486#table2</TD>
            <TD>2011-09-14T19:59:26Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/119/486&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/486</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A101 [1]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#1</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A101 [2]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#2</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A101 [table8]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#table8</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A101 [table9]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#table9</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/90/1681 [1]</TD>
            <TD>The Virgo Cluster Catalog (VCC) (Binggeli+, 1985)</TD>
            <TD>The present catalog of 2096 galaxies within an area of about 140{deg}^2^ approximately centered on the Virgo cluster should be an essentially complete listing of all certain and possible cluster members, independent of morphological type. Cluster membership is essentially decided by galaxy morphology; for giants and the rare class of high surface brightness dwarfs, membership rests on velocity data. While 1277 of the catalog entries are considered members of the Virgo cluster, 574 are possible members and 245 appear to be background Zwicky galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681#1</TD>
            <TD>2012-11-13T13:58:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/90/1681</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/1681</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/90/1681 [2]</TD>
            <TD>The Virgo Cluster Catalog (VCC) (Binggeli+, 1985)</TD>
            <TD>The present catalog of 2096 galaxies within an area of about 140{deg}^2^ approximately centered on the Virgo cluster should be an essentially complete listing of all certain and possible cluster members, independent of morphological type. Cluster membership is essentially decided by galaxy morphology; for giants and the rare class of high surface brightness dwarfs, membership rests on velocity data. While 1277 of the catalog entries are considered members of the Virgo cluster, 574 are possible members and 245 appear to be background Zwicky galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681#2</TD>
            <TD>2012-11-13T13:58:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/90/1681&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/1681</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/90/1681 [vcc]</TD>
            <TD>The Virgo Cluster Catalog (VCC) (Binggeli+, 1985)</TD>
            <TD>The present catalog of 2096 galaxies within an area of about 140{deg}^2^ approximately centered on the Virgo cluster should be an essentially complete listing of all certain and possible cluster members, independent of morphological type. Cluster membership is essentially decided by galaxy morphology; for giants and the rare class of high surface brightness dwarfs, membership rests on velocity data. While 1277 of the catalog entries are considered members of the Virgo cluster, 574 are possible members and 245 appear to be background Zwicky galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681#vcc</TD>
            <TD>2012-11-13T13:58:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/1681</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/90/1681&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/1681</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/486 [1]</TD>
            <TD>HDF-S: STIS imaging (Gardner+, 2000)</TD>
            <TD>We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486#1</TD>
            <TD>2011-09-14T19:59:26Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/486</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/486</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/486 [2]</TD>
            <TD>HDF-S: STIS imaging (Gardner+, 2000)</TD>
            <TD>We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486#2</TD>
            <TD>2011-09-14T19:59:26Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/486&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/486</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/119/486 [table2]</TD>
            <TD>HDF-S: STIS imaging (Gardner+, 2000)</TD>
            <TD>We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486#table2</TD>
            <TD>2011-09-14T19:59:26Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/119/486&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/486</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A101 [1]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#1</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A101 [2]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#2</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A101 [table8]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#table8</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A101 [table9]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#table9</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/14 [1]</TD>
            <TD>Optical spectroscopy of Abell clusters. I. (Owen+ 1995)</TD>
            <TD>We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14#1</TD>
            <TD>2012-11-13T14:02:32Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/14</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/14</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/14 [2]</TD>
            <TD>Optical spectroscopy of Abell clusters. I. (Owen+ 1995)</TD>
            <TD>We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14#2</TD>
            <TD>2012-11-13T14:02:32Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/14&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/14</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/14 [galaxies]</TD>
            <TD>Optical spectroscopy of Abell clusters. I. (Owen+ 1995)</TD>
            <TD>We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14#galaxies</TD>
            <TD>2012-11-13T14:02:32Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/14&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/14</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/486 [1]</TD>
            <TD>HDF-S: STIS imaging (Gardner+, 2000)</TD>
            <TD>We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486#1</TD>
            <TD>2011-09-14T19:59:26Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/486</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/486</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/486 [2]</TD>
            <TD>HDF-S: STIS imaging (Gardner+, 2000)</TD>
            <TD>We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486#2</TD>
            <TD>2011-09-14T19:59:26Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/486&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/486</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/119/486 [table2]</TD>
            <TD>HDF-S: STIS imaging (Gardner+, 2000)</TD>
            <TD>We present the imaging observations made with the Space Telescope Imaging Spectrograph (STIS) of the Hubble Deep Field South. The field was imaged in four bandpasses: a clear CCD bandpass for 156ks, a long-pass filter for 22-25ks/pix typical exposure, a near-UV bandpass for 23ks, and a far-UV bandpass for 52ks. The clear, visible image is the deepest observation ever made in the UV-optical wavelength region, reaching a 10{sigma}AB magnitude of 29.4 for an object of area 0.2arcsec^2^. The field contains QSO J2233-606, the target of the STIS spectroscopy, and extends 50"x50" for the visible images, and 25"x25" for the ultraviolet images. We present the images, catalog of objects, and galaxy counts obtained in the field.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486#table2</TD>
            <TD>2011-09-14T19:59:26Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/486</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/119/486&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/486</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/14 [1]</TD>
            <TD>Optical spectroscopy of Abell clusters. I. (Owen+ 1995)</TD>
            <TD>We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14#1</TD>
            <TD>2012-11-13T14:02:32Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/14</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/14</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/14 [2]</TD>
            <TD>Optical spectroscopy of Abell clusters. I. (Owen+ 1995)</TD>
            <TD>We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14#2</TD>
            <TD>2012-11-13T14:02:32Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/14&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/14</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/14 [galaxies]</TD>
            <TD>Optical spectroscopy of Abell clusters. I. (Owen+ 1995)</TD>
            <TD>We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14#galaxies</TD>
            <TD>2012-11-13T14:02:32Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/14&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/14</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/527/A101 [1]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#1</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/527/A101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/527/A101 [2]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#2</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/527/A101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A101 [table8]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#table8</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/527/A101 [table9]</TD>
            <TD>Galaxy population of Abell 1367 (Kriwattanawong+, 2011)</TD>
            <TD>Spectroscopic and photometric data of the galaxy population of the galaxy cluster Abell 1367, over a field of 34'x90', covering the cluster centre out to a radius of ~2.2Mpc, are presented as the first stage of a study of their stellar population and star formation properties. Spectroscopic catalogue contains new detection data of emission and/or absorption lines for 84 galaxies in our survey regions. Photometric data give optical and near-infrared isophotal magnitudes for 303 galaxies, determined within R_24_ isophotal diameters. H{alpha} emission catalogue reports equivalent widths and fluxes of 72 galaxies, confirmed as cluster members of Abell 1367.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101#table9</TD>
            <TD>2011-09-14T21:27:32Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/527/A101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/527/A101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/527/A101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/444/685 [1]</TD>
            <TD>VGCF detection of galaxy systems (Barrena+, 2005)</TD>
            <TD>We select 4 pointings for the Wide Field Camera (WFC) mounted at the prime focus of the 2.5m Isaac Newton Telescope (INT), located at the Roque de Los Muchachos Observatory, La Palma. We carried out observations from October 12 to October 14, 1999.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685#1</TD>
            <TD>2011-09-14T20:00:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/444/685</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/685</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/444/685 [2]</TD>
            <TD>VGCF detection of galaxy systems (Barrena+, 2005)</TD>
            <TD>We select 4 pointings for the Wide Field Camera (WFC) mounted at the prime focus of the 2.5m Isaac Newton Telescope (INT), located at the Roque de Los Muchachos Observatory, La Palma. We carried out observations from October 12 to October 14, 1999.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685#2</TD>
            <TD>2011-09-14T20:00:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/444/685&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/685</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/444/685 [table5]</TD>
            <TD>VGCF detection of galaxy systems (Barrena+, 2005)</TD>
            <TD>We select 4 pointings for the Wide Field Camera (WFC) mounted at the prime focus of the 2.5m Isaac Newton Telescope (INT), located at the Roque de Los Muchachos Observatory, La Palma. We carried out observations from October 12 to October 14, 1999.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685#table5</TD>
            <TD>2011-09-14T20:00:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/444/685&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/685</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/14 [1]</TD>
            <TD>Optical spectroscopy of Abell clusters. I. (Owen+ 1995)</TD>
            <TD>We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14#1</TD>
            <TD>2012-11-13T14:02:32Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/14</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/14</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/14 [2]</TD>
            <TD>Optical spectroscopy of Abell clusters. I. (Owen+ 1995)</TD>
            <TD>We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14#2</TD>
            <TD>2012-11-13T14:02:32Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/14&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/14</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/14 [galaxies]</TD>
            <TD>Optical spectroscopy of Abell clusters. I. (Owen+ 1995)</TD>
            <TD>We present results of a program of optical spectroscopy of radio galaxies in rich clusters. Redshifts are reported for 268 radio galaxies or close companions in Abell clusters and 36 objects which turned out to be foreground or background objects. Absolute line strengths are also reported for the 3727{AA} [OII] line and the [NII]/H{alpha} complex. We find no evidence that the radio activity in our sample of mostly FR I radio galaxies is associated with emission-line luminosities above those found in "normal" galaxies of the same absolute magnitude and optical type. We also find that the radial velocity differences between radio galaxies and the cluster mean seem mainly to be a function of galaxy absolute magnitude rather than radio properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14#galaxies</TD>
            <TD>2012-11-13T14:02:32Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/14</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/14&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/14</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/697/1138 [1]</TD>
            <TD>Discovery of PNe in M82 (Johnson+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (64) increased to 76 %B Observations of M 82 were made using the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the 8.2m Subaru Telescope located atop Mauna Kea, Hawaii on three nights, 2004 November 6-9. To complete our set of observations, we used a Hubble Space Telescope six-point mosaic H{alpha} image of the galaxy, observed using the Advanced Camera for Surveys (ACS) wide-field imager. These observations were made available via the Multimission Archive at STScI.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138#1</TD>
            <TD>2011-09-14T21:28:03Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/697/1138</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/1138</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/697/1138 [2]</TD>
            <TD>Discovery of PNe in M82 (Johnson+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (64) increased to 76 %B Observations of M 82 were made using the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the 8.2m Subaru Telescope located atop Mauna Kea, Hawaii on three nights, 2004 November 6-9. To complete our set of observations, we used a Hubble Space Telescope six-point mosaic H{alpha} image of the galaxy, observed using the Advanced Camera for Surveys (ACS) wide-field imager. These observations were made available via the Multimission Archive at STScI.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138#2</TD>
            <TD>2011-09-14T21:28:03Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/697/1138&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/1138</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/697/1138 [pne]</TD>
            <TD>Discovery of PNe in M82 (Johnson+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (64) increased to 76 %B Observations of M 82 were made using the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the 8.2m Subaru Telescope located atop Mauna Kea, Hawaii on three nights, 2004 November 6-9. To complete our set of observations, we used a Hubble Space Telescope six-point mosaic H{alpha} image of the galaxy, observed using the Advanced Camera for Surveys (ACS) wide-field imager. These observations were made available via the Multimission Archive at STScI.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138#pne</TD>
            <TD>2011-09-14T21:28:03Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/697/1138&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/1138</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/444/685 [1]</TD>
            <TD>VGCF detection of galaxy systems (Barrena+, 2005)</TD>
            <TD>We select 4 pointings for the Wide Field Camera (WFC) mounted at the prime focus of the 2.5m Isaac Newton Telescope (INT), located at the Roque de Los Muchachos Observatory, La Palma. We carried out observations from October 12 to October 14, 1999.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685#1</TD>
            <TD>2011-09-14T20:00:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/444/685</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/685</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/444/685 [2]</TD>
            <TD>VGCF detection of galaxy systems (Barrena+, 2005)</TD>
            <TD>We select 4 pointings for the Wide Field Camera (WFC) mounted at the prime focus of the 2.5m Isaac Newton Telescope (INT), located at the Roque de Los Muchachos Observatory, La Palma. We carried out observations from October 12 to October 14, 1999.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685#2</TD>
            <TD>2011-09-14T20:00:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/444/685&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/685</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/444/685 [table5]</TD>
            <TD>VGCF detection of galaxy systems (Barrena+, 2005)</TD>
            <TD>We select 4 pointings for the Wide Field Camera (WFC) mounted at the prime focus of the 2.5m Isaac Newton Telescope (INT), located at the Roque de Los Muchachos Observatory, La Palma. We carried out observations from October 12 to October 14, 1999.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685#table5</TD>
            <TD>2011-09-14T20:00:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/444/685&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/685</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1 [1]</TD>
            <TD>Southern Sky Redshift Survey (Da Costa+, 1998)</TD>
            <TD>We report redshifts, magnitudes, and morphological classifications for 5369 galaxies with m_B_&lt;=15.5 and for 57 galaxies fainter than this limit, in two regions covering a total of 1.70 sr in the southern celestial hemisphere. The galaxy catalog is drawn primarily from the list of nonstellar objects identified in the Hubble Space Telescope Guide Star Catalog (GSC). The galaxies have positions accurate to ~1" and magnitudes with an rms scatter of ~0.3mag. We compute magnitudes (m_SSRS2_) from the relation between instrumental GSC magnitudes and the photometry by Lauberts &amp; Valentijn. From a comparison with CCD photometry, we find that our system is homogeneous across the sky and corresponds to magnitudes measured at the isophotal level ~26mag/arcsec^2^. The precision of the radial velocities is ~40km/s, and the redshift survey is more than 99% complete to the m_SSRS2_=15.5mag limit. This sample is in the direction opposite that of the CfA2; in combination the two surveys provide an important database for studies of the properties of galaxies and their large-scale distribution in the nearby universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1#1</TD>
            <TD>2012-11-13T14:04:10Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1 [2]</TD>
            <TD>Southern Sky Redshift Survey (Da Costa+, 1998)</TD>
            <TD>We report redshifts, magnitudes, and morphological classifications for 5369 galaxies with m_B_&lt;=15.5 and for 57 galaxies fainter than this limit, in two regions covering a total of 1.70 sr in the southern celestial hemisphere. The galaxy catalog is drawn primarily from the list of nonstellar objects identified in the Hubble Space Telescope Guide Star Catalog (GSC). The galaxies have positions accurate to ~1" and magnitudes with an rms scatter of ~0.3mag. We compute magnitudes (m_SSRS2_) from the relation between instrumental GSC magnitudes and the photometry by Lauberts &amp; Valentijn. From a comparison with CCD photometry, we find that our system is homogeneous across the sky and corresponds to magnitudes measured at the isophotal level ~26mag/arcsec^2^. The precision of the radial velocities is ~40km/s, and the redshift survey is more than 99% complete to the m_SSRS2_=15.5mag limit. This sample is in the direction opposite that of the CfA2; in combination the two surveys provide an important database for studies of the properties of galaxies and their large-scale distribution in the nearby universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1#2</TD>
            <TD>2012-11-13T14:04:10Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1 [galaxies]</TD>
            <TD>Southern Sky Redshift Survey (Da Costa+, 1998)</TD>
            <TD>We report redshifts, magnitudes, and morphological classifications for 5369 galaxies with m_B_&lt;=15.5 and for 57 galaxies fainter than this limit, in two regions covering a total of 1.70 sr in the southern celestial hemisphere. The galaxy catalog is drawn primarily from the list of nonstellar objects identified in the Hubble Space Telescope Guide Star Catalog (GSC). The galaxies have positions accurate to ~1" and magnitudes with an rms scatter of ~0.3mag. We compute magnitudes (m_SSRS2_) from the relation between instrumental GSC magnitudes and the photometry by Lauberts &amp; Valentijn. From a comparison with CCD photometry, we find that our system is homogeneous across the sky and corresponds to magnitudes measured at the isophotal level ~26mag/arcsec^2^. The precision of the radial velocities is ~40km/s, and the redshift survey is more than 99% complete to the m_SSRS2_=15.5mag limit. This sample is in the direction opposite that of the CfA2; in combination the two surveys provide an important database for studies of the properties of galaxies and their large-scale distribution in the nearby universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1#galaxies</TD>
            <TD>2012-11-13T14:04:10Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/697/1138 [1]</TD>
            <TD>Discovery of PNe in M82 (Johnson+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (64) increased to 76 %B Observations of M 82 were made using the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the 8.2m Subaru Telescope located atop Mauna Kea, Hawaii on three nights, 2004 November 6-9. To complete our set of observations, we used a Hubble Space Telescope six-point mosaic H{alpha} image of the galaxy, observed using the Advanced Camera for Surveys (ACS) wide-field imager. These observations were made available via the Multimission Archive at STScI.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138#1</TD>
            <TD>2011-09-14T21:28:03Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/697/1138</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/1138</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/697/1138 [2]</TD>
            <TD>Discovery of PNe in M82 (Johnson+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (64) increased to 76 %B Observations of M 82 were made using the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the 8.2m Subaru Telescope located atop Mauna Kea, Hawaii on three nights, 2004 November 6-9. To complete our set of observations, we used a Hubble Space Telescope six-point mosaic H{alpha} image of the galaxy, observed using the Advanced Camera for Surveys (ACS) wide-field imager. These observations were made available via the Multimission Archive at STScI.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138#2</TD>
            <TD>2011-09-14T21:28:03Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/697/1138&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/1138</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/697/1138 [pne]</TD>
            <TD>Discovery of PNe in M82 (Johnson+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (64) increased to 76 %B Observations of M 82 were made using the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the 8.2m Subaru Telescope located atop Mauna Kea, Hawaii on three nights, 2004 November 6-9. To complete our set of observations, we used a Hubble Space Telescope six-point mosaic H{alpha} image of the galaxy, observed using the Advanced Camera for Surveys (ACS) wide-field imager. These observations were made available via the Multimission Archive at STScI.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138#pne</TD>
            <TD>2011-09-14T21:28:03Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/697/1138&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/1138</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/444/685 [1]</TD>
            <TD>VGCF detection of galaxy systems (Barrena+, 2005)</TD>
            <TD>We select 4 pointings for the Wide Field Camera (WFC) mounted at the prime focus of the 2.5m Isaac Newton Telescope (INT), located at the Roque de Los Muchachos Observatory, La Palma. We carried out observations from October 12 to October 14, 1999.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685#1</TD>
            <TD>2011-09-14T20:00:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/444/685</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/685</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/444/685 [2]</TD>
            <TD>VGCF detection of galaxy systems (Barrena+, 2005)</TD>
            <TD>We select 4 pointings for the Wide Field Camera (WFC) mounted at the prime focus of the 2.5m Isaac Newton Telescope (INT), located at the Roque de Los Muchachos Observatory, La Palma. We carried out observations from October 12 to October 14, 1999.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685#2</TD>
            <TD>2011-09-14T20:00:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/444/685&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/685</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/444/685 [table5]</TD>
            <TD>VGCF detection of galaxy systems (Barrena+, 2005)</TD>
            <TD>We select 4 pointings for the Wide Field Camera (WFC) mounted at the prime focus of the 2.5m Isaac Newton Telescope (INT), located at the Roque de Los Muchachos Observatory, La Palma. We carried out observations from October 12 to October 14, 1999.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685#table5</TD>
            <TD>2011-09-14T20:00:19Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/444/685</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/444/685&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/444/685</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1 [1]</TD>
            <TD>Southern Sky Redshift Survey (Da Costa+, 1998)</TD>
            <TD>We report redshifts, magnitudes, and morphological classifications for 5369 galaxies with m_B_&lt;=15.5 and for 57 galaxies fainter than this limit, in two regions covering a total of 1.70 sr in the southern celestial hemisphere. The galaxy catalog is drawn primarily from the list of nonstellar objects identified in the Hubble Space Telescope Guide Star Catalog (GSC). The galaxies have positions accurate to ~1" and magnitudes with an rms scatter of ~0.3mag. We compute magnitudes (m_SSRS2_) from the relation between instrumental GSC magnitudes and the photometry by Lauberts &amp; Valentijn. From a comparison with CCD photometry, we find that our system is homogeneous across the sky and corresponds to magnitudes measured at the isophotal level ~26mag/arcsec^2^. The precision of the radial velocities is ~40km/s, and the redshift survey is more than 99% complete to the m_SSRS2_=15.5mag limit. This sample is in the direction opposite that of the CfA2; in combination the two surveys provide an important database for studies of the properties of galaxies and their large-scale distribution in the nearby universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1#1</TD>
            <TD>2012-11-13T14:04:10Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1 [2]</TD>
            <TD>Southern Sky Redshift Survey (Da Costa+, 1998)</TD>
            <TD>We report redshifts, magnitudes, and morphological classifications for 5369 galaxies with m_B_&lt;=15.5 and for 57 galaxies fainter than this limit, in two regions covering a total of 1.70 sr in the southern celestial hemisphere. The galaxy catalog is drawn primarily from the list of nonstellar objects identified in the Hubble Space Telescope Guide Star Catalog (GSC). The galaxies have positions accurate to ~1" and magnitudes with an rms scatter of ~0.3mag. We compute magnitudes (m_SSRS2_) from the relation between instrumental GSC magnitudes and the photometry by Lauberts &amp; Valentijn. From a comparison with CCD photometry, we find that our system is homogeneous across the sky and corresponds to magnitudes measured at the isophotal level ~26mag/arcsec^2^. The precision of the radial velocities is ~40km/s, and the redshift survey is more than 99% complete to the m_SSRS2_=15.5mag limit. This sample is in the direction opposite that of the CfA2; in combination the two surveys provide an important database for studies of the properties of galaxies and their large-scale distribution in the nearby universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1#2</TD>
            <TD>2012-11-13T14:04:10Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1 [galaxies]</TD>
            <TD>Southern Sky Redshift Survey (Da Costa+, 1998)</TD>
            <TD>We report redshifts, magnitudes, and morphological classifications for 5369 galaxies with m_B_&lt;=15.5 and for 57 galaxies fainter than this limit, in two regions covering a total of 1.70 sr in the southern celestial hemisphere. The galaxy catalog is drawn primarily from the list of nonstellar objects identified in the Hubble Space Telescope Guide Star Catalog (GSC). The galaxies have positions accurate to ~1" and magnitudes with an rms scatter of ~0.3mag. We compute magnitudes (m_SSRS2_) from the relation between instrumental GSC magnitudes and the photometry by Lauberts &amp; Valentijn. From a comparison with CCD photometry, we find that our system is homogeneous across the sky and corresponds to magnitudes measured at the isophotal level ~26mag/arcsec^2^. The precision of the radial velocities is ~40km/s, and the redshift survey is more than 99% complete to the m_SSRS2_=15.5mag limit. This sample is in the direction opposite that of the CfA2; in combination the two surveys provide an important database for studies of the properties of galaxies and their large-scale distribution in the nearby universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1#galaxies</TD>
            <TD>2012-11-13T14:04:10Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/697/1138 [1]</TD>
            <TD>Discovery of PNe in M82 (Johnson+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (64) increased to 76 %B Observations of M 82 were made using the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the 8.2m Subaru Telescope located atop Mauna Kea, Hawaii on three nights, 2004 November 6-9. To complete our set of observations, we used a Hubble Space Telescope six-point mosaic H{alpha} image of the galaxy, observed using the Advanced Camera for Surveys (ACS) wide-field imager. These observations were made available via the Multimission Archive at STScI.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138#1</TD>
            <TD>2011-09-14T21:28:03Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/697/1138</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/1138</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/697/1138 [2]</TD>
            <TD>Discovery of PNe in M82 (Johnson+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (64) increased to 76 %B Observations of M 82 were made using the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the 8.2m Subaru Telescope located atop Mauna Kea, Hawaii on three nights, 2004 November 6-9. To complete our set of observations, we used a Hubble Space Telescope six-point mosaic H{alpha} image of the galaxy, observed using the Advanced Camera for Surveys (ACS) wide-field imager. These observations were made available via the Multimission Archive at STScI.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138#2</TD>
            <TD>2011-09-14T21:28:03Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/697/1138&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/1138</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/697/1138 [pne]</TD>
            <TD>Discovery of PNe in M82 (Johnson+, 2009)</TD>
            <TD>++++Lrecl of file 'table3.dat' (64) increased to 76 %B Observations of M 82 were made using the Faint Object Camera and Spectrograph (FOCAS) at the Cassegrain focus of the 8.2m Subaru Telescope located atop Mauna Kea, Hawaii on three nights, 2004 November 6-9. To complete our set of observations, we used a Hubble Space Telescope six-point mosaic H{alpha} image of the galaxy, observed using the Advanced Camera for Surveys (ACS) wide-field imager. These observations were made available via the Multimission Archive at STScI.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138#pne</TD>
            <TD>2011-09-14T21:28:03Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/697/1138</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/697/1138&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/697/1138</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/453/493 [1]</TD>
            <TD>Line-strength indices in IC 4200 (Serra+, 2006)</TD>
            <TD>Optical spectroscopy, imaging and radio observations of the galaxy IC 4200 are analysed in order to determine the formation history of the galaxy. The two tables available contain informations extracted from the long-slit spectra of IC 4200. The spectra were taken with ESO/NTT/EMMI mounted on the NTT on 12 July 2004, as described in Sec. 3.2 and in Table 4 of the paper. tablec1.dat contains informations on the stellar and ionised-gas kinematics along the optical major and minor axis of the galaxy. The stellar kinematics was determined by fitting Bruzual &amp; Charlot (2003MNRAS.344.1000B) stellar populations synthesis models to the low-S/N 1D bins extracted from the 2D spectrum of IC 4200 (Sec. 3.2.1). The kinematics of the ionised gas was determined by fitting single Gaussians to the Halpha emission line; for this purpose we used IRAF.NOAO.ONEDSPEC.SPLOT. tablec2.dat contains the values of the Lick/IDS indices measured along the optical major and minor axis of IC 4200. The values given are corrected for the effect of velocity dispersion and shifted to the Lick/IDS system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/453/493#1</TD>
            <TD>2011-09-14T20:00:27Z</TD>
            <TD>#Abundances#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/453/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/453/493</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/453/493</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/453/493 [2]</TD>
            <TD>Line-strength indices in IC 4200 (Serra+, 2006)</TD>
            <TD>Optical spectroscopy, imaging and radio observations of the galaxy IC 4200 are analysed in order to determine the formation history of the galaxy. The two tables available contain informations extracted from the long-slit spectra of IC 4200. The spectra were taken with ESO/NTT/EMMI mounted on the NTT on 12 July 2004, as described in Sec. 3.2 and in Table 4 of the paper. tablec1.dat contains informations on the stellar and ionised-gas kinematics along the optical major and minor axis of the galaxy. The stellar kinematics was determined by fitting Bruzual &amp; Charlot (2003MNRAS.344.1000B) stellar populations synthesis models to the low-S/N 1D bins extracted from the 2D spectrum of IC 4200 (Sec. 3.2.1). The kinematics of the ionised gas was determined by fitting single Gaussians to the Halpha emission line; for this purpose we used IRAF.NOAO.ONEDSPEC.SPLOT. tablec2.dat contains the values of the Lick/IDS indices measured along the optical major and minor axis of IC 4200. The values given are corrected for the effect of velocity dispersion and shifted to the Lick/IDS system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/453/493#2</TD>
            <TD>2011-09-14T20:00:27Z</TD>
            <TD>#Abundances#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/453/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/453/493&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/453/493</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1 [1]</TD>
            <TD>Southern Sky Redshift Survey (Da Costa+, 1998)</TD>
            <TD>We report redshifts, magnitudes, and morphological classifications for 5369 galaxies with m_B_&lt;=15.5 and for 57 galaxies fainter than this limit, in two regions covering a total of 1.70 sr in the southern celestial hemisphere. The galaxy catalog is drawn primarily from the list of nonstellar objects identified in the Hubble Space Telescope Guide Star Catalog (GSC). The galaxies have positions accurate to ~1" and magnitudes with an rms scatter of ~0.3mag. We compute magnitudes (m_SSRS2_) from the relation between instrumental GSC magnitudes and the photometry by Lauberts &amp; Valentijn. From a comparison with CCD photometry, we find that our system is homogeneous across the sky and corresponds to magnitudes measured at the isophotal level ~26mag/arcsec^2^. The precision of the radial velocities is ~40km/s, and the redshift survey is more than 99% complete to the m_SSRS2_=15.5mag limit. This sample is in the direction opposite that of the CfA2; in combination the two surveys provide an important database for studies of the properties of galaxies and their large-scale distribution in the nearby universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1#1</TD>
            <TD>2012-11-13T14:04:10Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1 [2]</TD>
            <TD>Southern Sky Redshift Survey (Da Costa+, 1998)</TD>
            <TD>We report redshifts, magnitudes, and morphological classifications for 5369 galaxies with m_B_&lt;=15.5 and for 57 galaxies fainter than this limit, in two regions covering a total of 1.70 sr in the southern celestial hemisphere. The galaxy catalog is drawn primarily from the list of nonstellar objects identified in the Hubble Space Telescope Guide Star Catalog (GSC). The galaxies have positions accurate to ~1" and magnitudes with an rms scatter of ~0.3mag. We compute magnitudes (m_SSRS2_) from the relation between instrumental GSC magnitudes and the photometry by Lauberts &amp; Valentijn. From a comparison with CCD photometry, we find that our system is homogeneous across the sky and corresponds to magnitudes measured at the isophotal level ~26mag/arcsec^2^. The precision of the radial velocities is ~40km/s, and the redshift survey is more than 99% complete to the m_SSRS2_=15.5mag limit. This sample is in the direction opposite that of the CfA2; in combination the two surveys provide an important database for studies of the properties of galaxies and their large-scale distribution in the nearby universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1#2</TD>
            <TD>2012-11-13T14:04:10Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1 [galaxies]</TD>
            <TD>Southern Sky Redshift Survey (Da Costa+, 1998)</TD>
            <TD>We report redshifts, magnitudes, and morphological classifications for 5369 galaxies with m_B_&lt;=15.5 and for 57 galaxies fainter than this limit, in two regions covering a total of 1.70 sr in the southern celestial hemisphere. The galaxy catalog is drawn primarily from the list of nonstellar objects identified in the Hubble Space Telescope Guide Star Catalog (GSC). The galaxies have positions accurate to ~1" and magnitudes with an rms scatter of ~0.3mag. We compute magnitudes (m_SSRS2_) from the relation between instrumental GSC magnitudes and the photometry by Lauberts &amp; Valentijn. From a comparison with CCD photometry, we find that our system is homogeneous across the sky and corresponds to magnitudes measured at the isophotal level ~26mag/arcsec^2^. The precision of the radial velocities is ~40km/s, and the redshift survey is more than 99% complete to the m_SSRS2_=15.5mag limit. This sample is in the direction opposite that of the CfA2; in combination the two surveys provide an important database for studies of the properties of galaxies and their large-scale distribution in the nearby universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1#galaxies</TD>
            <TD>2012-11-13T14:04:10Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/453/493 [1]</TD>
            <TD>Line-strength indices in IC 4200 (Serra+, 2006)</TD>
            <TD>Optical spectroscopy, imaging and radio observations of the galaxy IC 4200 are analysed in order to determine the formation history of the galaxy. The two tables available contain informations extracted from the long-slit spectra of IC 4200. The spectra were taken with ESO/NTT/EMMI mounted on the NTT on 12 July 2004, as described in Sec. 3.2 and in Table 4 of the paper. tablec1.dat contains informations on the stellar and ionised-gas kinematics along the optical major and minor axis of the galaxy. The stellar kinematics was determined by fitting Bruzual &amp; Charlot (2003MNRAS.344.1000B) stellar populations synthesis models to the low-S/N 1D bins extracted from the 2D spectrum of IC 4200 (Sec. 3.2.1). The kinematics of the ionised gas was determined by fitting single Gaussians to the Halpha emission line; for this purpose we used IRAF.NOAO.ONEDSPEC.SPLOT. tablec2.dat contains the values of the Lick/IDS indices measured along the optical major and minor axis of IC 4200. The values given are corrected for the effect of velocity dispersion and shifted to the Lick/IDS system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/453/493#1</TD>
            <TD>2011-09-14T20:00:27Z</TD>
            <TD>#Abundances#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/453/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/453/493</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/453/493</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/453/493 [2]</TD>
            <TD>Line-strength indices in IC 4200 (Serra+, 2006)</TD>
            <TD>Optical spectroscopy, imaging and radio observations of the galaxy IC 4200 are analysed in order to determine the formation history of the galaxy. The two tables available contain informations extracted from the long-slit spectra of IC 4200. The spectra were taken with ESO/NTT/EMMI mounted on the NTT on 12 July 2004, as described in Sec. 3.2 and in Table 4 of the paper. tablec1.dat contains informations on the stellar and ionised-gas kinematics along the optical major and minor axis of the galaxy. The stellar kinematics was determined by fitting Bruzual &amp; Charlot (2003MNRAS.344.1000B) stellar populations synthesis models to the low-S/N 1D bins extracted from the 2D spectrum of IC 4200 (Sec. 3.2.1). The kinematics of the ionised gas was determined by fitting single Gaussians to the Halpha emission line; for this purpose we used IRAF.NOAO.ONEDSPEC.SPLOT. tablec2.dat contains the values of the Lick/IDS indices measured along the optical major and minor axis of IC 4200. The values given are corrected for the effect of velocity dispersion and shifted to the Lick/IDS system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/453/493#2</TD>
            <TD>2011-09-14T20:00:27Z</TD>
            <TD>#Abundances#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/453/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/453/493&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/453/493</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/300/303 [1]</TD>
            <TD>UV-selected galaxy redshift survey (Treyer+, 1998)</TD>
            <TD>The table contains the first results of a spectroscopic survey of galaxies constructed from a flux-limited sample of stars, galaxies and QSOs imaged at 2000{AA} with the FOCA balloon-borne imaging camera (see Milliard et al., 1992A&amp;A...257...24M) The galaxies were selected in the rest frame ultraviolet (UV), in Selected Area 57. Accurate positions for the UV sources have been obtained by matching with optical counterparts using APM scans of the Palomar Sky Survey limited at B=20.5. The results presented here are derived from optical spectroscopy conducted with the WIYN telescope and the WHT for 142 faint sources. The redshift distribution for this UV- selected sample extends over 0&lt;z&lt;0.5, and a high fraction of the sources show intense nebular emission lines and UV-optical colours bluer than normal Hubble sequence galaxies. Updated results for these galaxies were published later (see Sullivan et al. 2000, Cat. &lt;J/MNRAS/312/442&gt;)</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303#1</TD>
            <TD>2012-11-13T14:09:49Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/300/303</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/303</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/300/303 [2]</TD>
            <TD>UV-selected galaxy redshift survey (Treyer+, 1998)</TD>
            <TD>The table contains the first results of a spectroscopic survey of galaxies constructed from a flux-limited sample of stars, galaxies and QSOs imaged at 2000{AA} with the FOCA balloon-borne imaging camera (see Milliard et al., 1992A&amp;A...257...24M) The galaxies were selected in the rest frame ultraviolet (UV), in Selected Area 57. Accurate positions for the UV sources have been obtained by matching with optical counterparts using APM scans of the Palomar Sky Survey limited at B=20.5. The results presented here are derived from optical spectroscopy conducted with the WIYN telescope and the WHT for 142 faint sources. The redshift distribution for this UV- selected sample extends over 0&lt;z&lt;0.5, and a high fraction of the sources show intense nebular emission lines and UV-optical colours bluer than normal Hubble sequence galaxies. Updated results for these galaxies were published later (see Sullivan et al. 2000, Cat. &lt;J/MNRAS/312/442&gt;)</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303#2</TD>
            <TD>2012-11-13T14:09:49Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/300/303&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/303</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/300/303 [table1]</TD>
            <TD>UV-selected galaxy redshift survey (Treyer+, 1998)</TD>
            <TD>The table contains the first results of a spectroscopic survey of galaxies constructed from a flux-limited sample of stars, galaxies and QSOs imaged at 2000{AA} with the FOCA balloon-borne imaging camera (see Milliard et al., 1992A&amp;A...257...24M) The galaxies were selected in the rest frame ultraviolet (UV), in Selected Area 57. Accurate positions for the UV sources have been obtained by matching with optical counterparts using APM scans of the Palomar Sky Survey limited at B=20.5. The results presented here are derived from optical spectroscopy conducted with the WIYN telescope and the WHT for 142 faint sources. The redshift distribution for this UV- selected sample extends over 0&lt;z&lt;0.5, and a high fraction of the sources show intense nebular emission lines and UV-optical colours bluer than normal Hubble sequence galaxies. Updated results for these galaxies were published later (see Sullivan et al. 2000, Cat. &lt;J/MNRAS/312/442&gt;)</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303#table1</TD>
            <TD>2012-11-13T14:09:49Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/300/303&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/303</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/531/A26 [1]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#1</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/531/A26</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/531/A26 [2]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#2</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A26 [table1]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#table1</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A26 [list]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#list</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A26 [table2]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#table2</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/531/A26 [1]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#1</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/531/A26</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/531/A26 [2]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#2</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A26 [table1]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#table1</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A26 [list]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#list</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A26 [table2]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#table2</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/371/1777 [1]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#1</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/371/1777</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/371/1777 [2]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#2</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1777 [table12]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#table12</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1777 [tablea]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#tablea</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1777 [tableb]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#tableb</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/300/303 [1]</TD>
            <TD>UV-selected galaxy redshift survey (Treyer+, 1998)</TD>
            <TD>The table contains the first results of a spectroscopic survey of galaxies constructed from a flux-limited sample of stars, galaxies and QSOs imaged at 2000{AA} with the FOCA balloon-borne imaging camera (see Milliard et al., 1992A&amp;A...257...24M) The galaxies were selected in the rest frame ultraviolet (UV), in Selected Area 57. Accurate positions for the UV sources have been obtained by matching with optical counterparts using APM scans of the Palomar Sky Survey limited at B=20.5. The results presented here are derived from optical spectroscopy conducted with the WIYN telescope and the WHT for 142 faint sources. The redshift distribution for this UV- selected sample extends over 0&lt;z&lt;0.5, and a high fraction of the sources show intense nebular emission lines and UV-optical colours bluer than normal Hubble sequence galaxies. Updated results for these galaxies were published later (see Sullivan et al. 2000, Cat. &lt;J/MNRAS/312/442&gt;)</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303#1</TD>
            <TD>2012-11-13T14:09:49Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/300/303</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/303</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/300/303 [2]</TD>
            <TD>UV-selected galaxy redshift survey (Treyer+, 1998)</TD>
            <TD>The table contains the first results of a spectroscopic survey of galaxies constructed from a flux-limited sample of stars, galaxies and QSOs imaged at 2000{AA} with the FOCA balloon-borne imaging camera (see Milliard et al., 1992A&amp;A...257...24M) The galaxies were selected in the rest frame ultraviolet (UV), in Selected Area 57. Accurate positions for the UV sources have been obtained by matching with optical counterparts using APM scans of the Palomar Sky Survey limited at B=20.5. The results presented here are derived from optical spectroscopy conducted with the WIYN telescope and the WHT for 142 faint sources. The redshift distribution for this UV- selected sample extends over 0&lt;z&lt;0.5, and a high fraction of the sources show intense nebular emission lines and UV-optical colours bluer than normal Hubble sequence galaxies. Updated results for these galaxies were published later (see Sullivan et al. 2000, Cat. &lt;J/MNRAS/312/442&gt;)</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303#2</TD>
            <TD>2012-11-13T14:09:49Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/300/303&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/303</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/300/303 [table1]</TD>
            <TD>UV-selected galaxy redshift survey (Treyer+, 1998)</TD>
            <TD>The table contains the first results of a spectroscopic survey of galaxies constructed from a flux-limited sample of stars, galaxies and QSOs imaged at 2000{AA} with the FOCA balloon-borne imaging camera (see Milliard et al., 1992A&amp;A...257...24M) The galaxies were selected in the rest frame ultraviolet (UV), in Selected Area 57. Accurate positions for the UV sources have been obtained by matching with optical counterparts using APM scans of the Palomar Sky Survey limited at B=20.5. The results presented here are derived from optical spectroscopy conducted with the WIYN telescope and the WHT for 142 faint sources. The redshift distribution for this UV- selected sample extends over 0&lt;z&lt;0.5, and a high fraction of the sources show intense nebular emission lines and UV-optical colours bluer than normal Hubble sequence galaxies. Updated results for these galaxies were published later (see Sullivan et al. 2000, Cat. &lt;J/MNRAS/312/442&gt;)</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303#table1</TD>
            <TD>2012-11-13T14:09:49Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/300/303&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/303</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/531/A26 [1]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#1</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/531/A26</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/531/A26 [2]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#2</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A26 [table1]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#table1</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A26 [list]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#list</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/531/A26 [table2]</TD>
            <TD>Clumps in W31 from CO and 875um observations (Beuther+, 2011)</TD>
            <TD>The C^18^O(2-1) and ^13^CO(2-1) data at 219.560GHz and 220.399GHz were observed simultaneously with the Atacama Pathfinder Experiment (APEX1) in July 2009 in the 1mm band over the entire W31 complex in the on-the-fly mode. The 875um images are from the ATLASGAL survey of the Galaxy (Schuller et al. 2009A&amp;A...504..415S)</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26#table2</TD>
            <TD>2011-09-14T21:29:31Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/531/A26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/531/A26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/531/A26</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/371/1777 [1]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#1</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/371/1777</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/371/1777 [2]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#2</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1777 [table12]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#table12</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1777 [tablea]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#tablea</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1777 [tableb]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#tableb</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/300/303 [1]</TD>
            <TD>UV-selected galaxy redshift survey (Treyer+, 1998)</TD>
            <TD>The table contains the first results of a spectroscopic survey of galaxies constructed from a flux-limited sample of stars, galaxies and QSOs imaged at 2000{AA} with the FOCA balloon-borne imaging camera (see Milliard et al., 1992A&amp;A...257...24M) The galaxies were selected in the rest frame ultraviolet (UV), in Selected Area 57. Accurate positions for the UV sources have been obtained by matching with optical counterparts using APM scans of the Palomar Sky Survey limited at B=20.5. The results presented here are derived from optical spectroscopy conducted with the WIYN telescope and the WHT for 142 faint sources. The redshift distribution for this UV- selected sample extends over 0&lt;z&lt;0.5, and a high fraction of the sources show intense nebular emission lines and UV-optical colours bluer than normal Hubble sequence galaxies. Updated results for these galaxies were published later (see Sullivan et al. 2000, Cat. &lt;J/MNRAS/312/442&gt;)</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303#1</TD>
            <TD>2012-11-13T14:09:49Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/300/303</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/303</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/300/303 [2]</TD>
            <TD>UV-selected galaxy redshift survey (Treyer+, 1998)</TD>
            <TD>The table contains the first results of a spectroscopic survey of galaxies constructed from a flux-limited sample of stars, galaxies and QSOs imaged at 2000{AA} with the FOCA balloon-borne imaging camera (see Milliard et al., 1992A&amp;A...257...24M) The galaxies were selected in the rest frame ultraviolet (UV), in Selected Area 57. Accurate positions for the UV sources have been obtained by matching with optical counterparts using APM scans of the Palomar Sky Survey limited at B=20.5. The results presented here are derived from optical spectroscopy conducted with the WIYN telescope and the WHT for 142 faint sources. The redshift distribution for this UV- selected sample extends over 0&lt;z&lt;0.5, and a high fraction of the sources show intense nebular emission lines and UV-optical colours bluer than normal Hubble sequence galaxies. Updated results for these galaxies were published later (see Sullivan et al. 2000, Cat. &lt;J/MNRAS/312/442&gt;)</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303#2</TD>
            <TD>2012-11-13T14:09:49Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/300/303&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/303</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/300/303 [table1]</TD>
            <TD>UV-selected galaxy redshift survey (Treyer+, 1998)</TD>
            <TD>The table contains the first results of a spectroscopic survey of galaxies constructed from a flux-limited sample of stars, galaxies and QSOs imaged at 2000{AA} with the FOCA balloon-borne imaging camera (see Milliard et al., 1992A&amp;A...257...24M) The galaxies were selected in the rest frame ultraviolet (UV), in Selected Area 57. Accurate positions for the UV sources have been obtained by matching with optical counterparts using APM scans of the Palomar Sky Survey limited at B=20.5. The results presented here are derived from optical spectroscopy conducted with the WIYN telescope and the WHT for 142 faint sources. The redshift distribution for this UV- selected sample extends over 0&lt;z&lt;0.5, and a high fraction of the sources show intense nebular emission lines and UV-optical colours bluer than normal Hubble sequence galaxies. Updated results for these galaxies were published later (see Sullivan et al. 2000, Cat. &lt;J/MNRAS/312/442&gt;)</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303#table1</TD>
            <TD>2012-11-13T14:09:49Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/303</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/300/303&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/303</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/106/451 [1]</TD>
            <TD>Face-on disk galaxies photometry. I. (de Jong+, 1994)</TD>
            <TD>We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451#1</TD>
            <TD>2011-09-14T18:17:06Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/106/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/106/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/106/451 [2]</TD>
            <TD>Face-on disk galaxies photometry. I. (de Jong+, 1994)</TD>
            <TD>We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451#2</TD>
            <TD>2011-09-14T18:17:06Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/106/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/106/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/106/451 [table3]</TD>
            <TD>Face-on disk galaxies photometry. I. (de Jong+, 1994)</TD>
            <TD>We present accurate surface photometry in the B, V, R, I, H and K passbands of 86 spiral galaxies. The galaxies in this statistically complete sample of undisturbed spirals were selected from the UGC to have minimum diameters of 2' and minor over major axis ratios larger than 0.625. This sample has been selected in such a way that it can be used to represent a volume limited sample. The observation and reduction techniques are described in detail, especially the not often used driftscan technique for CCDs and the relatively new techniques using near-infrared (near-IR) arrays. For each galaxy we present radial profiles of surface brightness. Using these profiles we calculated the integrated magnitudes of the galaxies in the different passbands. We performed internal and external consistency checks for the magnitudes as well as the luminosity profiles. The internal consistency is well within the estimated errors. Comparisons with other authors indicate that measurements from photographic plates can show large deviations in the zero-point magnitude. Our surface brightness profiles agree within the errors with other CCD measurements. The comparison of integrated magnitudes shows a large scatter, but a consistent zero-point. These measurements will be used in a series of forthcoming papers to discuss central surface brightnesses, scalelengths, colors and color gradients of disks of spiral galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451#table3</TD>
            <TD>2011-09-14T18:17:06Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/106/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/106/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/106/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/371/1777 [1]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#1</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/371/1777</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/371/1777 [2]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#2</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1777 [table12]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#table12</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1777 [tablea]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#tablea</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/371/1777 [tableb]</TD>
            <TD>X-ray properties of 3 EDisCS galaxy clusters (Johnson+, 2006)</TD>
            <TD>Catalogs of X-ray and optical properties of X-ray point sources in three cluster fields observed with XMM-Newton in support of the European Southern Observatory Distant Cluster Survey (EDisCS): Cl1216-1201, Cl1054-1145, and Cl040-1155. Tables give X-ray properties (X-ray position, source counts, fluxes, hardness ratio) and optical properties of possible optical counterparts (optical position, likelihood of association, VRI photometry) for all sources in the XMM FOV.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777#tableb</TD>
            <TD>2011-09-14T20:00:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/371/1777</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/371/1777&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/371/1777</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/543/A61 [1]</TD>
            <TD>SINFONI data cube of NGC 7552 (Brandl+, 2012)</TD>
            <TD>Approximately 20% of all spiral galaxies display starburst activity in nuclear rings of a few hundred parsecs in diameter. It is our main aim to investigate how the starburst ignites and propagates within the ring, leading to the formation of massive stellar clusters. We observed the ring galaxy NGC 7552 with the mid-infrared (MIR) instrument VISIR at an angular resolution of 0.3"-0.4" and with the near-infrared (NIR) integral-field spectrograph SINFONI on the VLT, and complement these observations with data from ISO and Spitzer. The starburst ring is clearly detected at MIR wavelengths at the location of the dust-extincted, dark ring seen in HST observations. This "ring", however, is a rather complex annular region of more than 100 parsec width. We find a large fraction of diffuse [NeII] and PAH emission in the central region that is not associated with the MIR peaks on spatial scales of ~30pc. We do not detect MIR emission from the nucleus of NGC 7552, which is very prominent at optical and NIR continuum wavelengths. However, we have identified nine unresolved MIR peaks within the ring. The average extinction of these peaks is A_V_=7.4 and their total infrared luminosity is L_IR_=2.1x10^10^L_{sun}_. The properties of these peaks are typical for MIR-selected massive clusters found in other galaxies. The ages of the MIR-selected clusters are in the range of 5.9+/-0.3Myr. The age spread among the clusters of 0.8Myr is small compared to the travel time of ~5.6Myr for half an orbit within the starburst ring. We find no strong evidence for a scenario where the continuous inflow of gas leads to the ongoing formation of massive clusters at the contact points between galactic bar and starburst ring. Instead, it appears more likely that the gas density build up more gradually over larger ring segments, and that the local physical conditions govern cluster formation. We note that the fundamental limitation on the accurate derivation of cluster age, mass and initial mass function slope is the lack of higher angular resolution. Resolving the highly embedded, massive clusters requires milli-arcsecond resolution at infrared wavelengths, which will be provided by the next generation of instruments on extremely large telescopes (ELTs).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61#1</TD>
            <TD>2012-11-15T12:54:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/543/A61</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A61</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/543/A61 [2]</TD>
            <TD>SINFONI data cube of NGC 7552 (Brandl+, 2012)</TD>
            <TD>Approximately 20% of all spiral galaxies display starburst activity in nuclear rings of a few hundred parsecs in diameter. It is our main aim to investigate how the starburst ignites and propagates within the ring, leading to the formation of massive stellar clusters. We observed the ring galaxy NGC 7552 with the mid-infrared (MIR) instrument VISIR at an angular resolution of 0.3"-0.4" and with the near-infrared (NIR) integral-field spectrograph SINFONI on the VLT, and complement these observations with data from ISO and Spitzer. The starburst ring is clearly detected at MIR wavelengths at the location of the dust-extincted, dark ring seen in HST observations. This "ring", however, is a rather complex annular region of more than 100 parsec width. We find a large fraction of diffuse [NeII] and PAH emission in the central region that is not associated with the MIR peaks on spatial scales of ~30pc. We do not detect MIR emission from the nucleus of NGC 7552, which is very prominent at optical and NIR continuum wavelengths. However, we have identified nine unresolved MIR peaks within the ring. The average extinction of these peaks is A_V_=7.4 and their total infrared luminosity is L_IR_=2.1x10^10^L_{sun}_. The properties of these peaks are typical for MIR-selected massive clusters found in other galaxies. The ages of the MIR-selected clusters are in the range of 5.9+/-0.3Myr. The age spread among the clusters of 0.8Myr is small compared to the travel time of ~5.6Myr for half an orbit within the starburst ring. We find no strong evidence for a scenario where the continuous inflow of gas leads to the ongoing formation of massive clusters at the contact points between galactic bar and starburst ring. Instead, it appears more likely that the gas density build up more gradually over larger ring segments, and that the local physical conditions govern cluster formation. We note that the fundamental limitation on the accurate derivation of cluster age, mass and initial mass function slope is the lack of higher angular resolution. Resolving the highly embedded, massive clusters requires milli-arcsecond resolution at infrared wavelengths, which will be provided by the next generation of instruments on extremely large telescopes (ELTs).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61#2</TD>
            <TD>2012-11-15T12:54:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/543/A61&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A61</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/543/A61 [list]</TD>
            <TD>SINFONI data cube of NGC 7552 (Brandl+, 2012)</TD>
            <TD>Approximately 20% of all spiral galaxies display starburst activity in nuclear rings of a few hundred parsecs in diameter. It is our main aim to investigate how the starburst ignites and propagates within the ring, leading to the formation of massive stellar clusters. We observed the ring galaxy NGC 7552 with the mid-infrared (MIR) instrument VISIR at an angular resolution of 0.3"-0.4" and with the near-infrared (NIR) integral-field spectrograph SINFONI on the VLT, and complement these observations with data from ISO and Spitzer. The starburst ring is clearly detected at MIR wavelengths at the location of the dust-extincted, dark ring seen in HST observations. This "ring", however, is a rather complex annular region of more than 100 parsec width. We find a large fraction of diffuse [NeII] and PAH emission in the central region that is not associated with the MIR peaks on spatial scales of ~30pc. We do not detect MIR emission from the nucleus of NGC 7552, which is very prominent at optical and NIR continuum wavelengths. However, we have identified nine unresolved MIR peaks within the ring. The average extinction of these peaks is A_V_=7.4 and their total infrared luminosity is L_IR_=2.1x10^10^L_{sun}_. The properties of these peaks are typical for MIR-selected massive clusters found in other galaxies. The ages of the MIR-selected clusters are in the range of 5.9+/-0.3Myr. The age spread among the clusters of 0.8Myr is small compared to the travel time of ~5.6Myr for half an orbit within the starburst ring. We find no strong evidence for a scenario where the continuous inflow of gas leads to the ongoing formation of massive clusters at the contact points between galactic bar and starburst ring. Instead, it appears more likely that the gas density build up more gradually over larger ring segments, and that the local physical conditions govern cluster formation. We note that the fundamental limitation on the accurate derivation of cluster age, mass and initial mass function slope is the lack of higher angular resolution. Resolving the highly embedded, massive clusters requires milli-arcsecond resolution at infrared wavelengths, which will be provided by the next generation of instruments on extremely large telescopes (ELTs).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61#list</TD>
            <TD>2012-11-15T12:54:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/543/A61&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A61</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/117/1 [1]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#1</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/117/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/117/1 [2]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#2</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/117/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/1 [table2]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#table2</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/1 [table3]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#table3</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/543/A61 [1]</TD>
            <TD>SINFONI data cube of NGC 7552 (Brandl+, 2012)</TD>
            <TD>Approximately 20% of all spiral galaxies display starburst activity in nuclear rings of a few hundred parsecs in diameter. It is our main aim to investigate how the starburst ignites and propagates within the ring, leading to the formation of massive stellar clusters. We observed the ring galaxy NGC 7552 with the mid-infrared (MIR) instrument VISIR at an angular resolution of 0.3"-0.4" and with the near-infrared (NIR) integral-field spectrograph SINFONI on the VLT, and complement these observations with data from ISO and Spitzer. The starburst ring is clearly detected at MIR wavelengths at the location of the dust-extincted, dark ring seen in HST observations. This "ring", however, is a rather complex annular region of more than 100 parsec width. We find a large fraction of diffuse [NeII] and PAH emission in the central region that is not associated with the MIR peaks on spatial scales of ~30pc. We do not detect MIR emission from the nucleus of NGC 7552, which is very prominent at optical and NIR continuum wavelengths. However, we have identified nine unresolved MIR peaks within the ring. The average extinction of these peaks is A_V_=7.4 and their total infrared luminosity is L_IR_=2.1x10^10^L_{sun}_. The properties of these peaks are typical for MIR-selected massive clusters found in other galaxies. The ages of the MIR-selected clusters are in the range of 5.9+/-0.3Myr. The age spread among the clusters of 0.8Myr is small compared to the travel time of ~5.6Myr for half an orbit within the starburst ring. We find no strong evidence for a scenario where the continuous inflow of gas leads to the ongoing formation of massive clusters at the contact points between galactic bar and starburst ring. Instead, it appears more likely that the gas density build up more gradually over larger ring segments, and that the local physical conditions govern cluster formation. We note that the fundamental limitation on the accurate derivation of cluster age, mass and initial mass function slope is the lack of higher angular resolution. Resolving the highly embedded, massive clusters requires milli-arcsecond resolution at infrared wavelengths, which will be provided by the next generation of instruments on extremely large telescopes (ELTs).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61#1</TD>
            <TD>2012-11-15T12:54:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/543/A61</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A61</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/543/A61 [2]</TD>
            <TD>SINFONI data cube of NGC 7552 (Brandl+, 2012)</TD>
            <TD>Approximately 20% of all spiral galaxies display starburst activity in nuclear rings of a few hundred parsecs in diameter. It is our main aim to investigate how the starburst ignites and propagates within the ring, leading to the formation of massive stellar clusters. We observed the ring galaxy NGC 7552 with the mid-infrared (MIR) instrument VISIR at an angular resolution of 0.3"-0.4" and with the near-infrared (NIR) integral-field spectrograph SINFONI on the VLT, and complement these observations with data from ISO and Spitzer. The starburst ring is clearly detected at MIR wavelengths at the location of the dust-extincted, dark ring seen in HST observations. This "ring", however, is a rather complex annular region of more than 100 parsec width. We find a large fraction of diffuse [NeII] and PAH emission in the central region that is not associated with the MIR peaks on spatial scales of ~30pc. We do not detect MIR emission from the nucleus of NGC 7552, which is very prominent at optical and NIR continuum wavelengths. However, we have identified nine unresolved MIR peaks within the ring. The average extinction of these peaks is A_V_=7.4 and their total infrared luminosity is L_IR_=2.1x10^10^L_{sun}_. The properties of these peaks are typical for MIR-selected massive clusters found in other galaxies. The ages of the MIR-selected clusters are in the range of 5.9+/-0.3Myr. The age spread among the clusters of 0.8Myr is small compared to the travel time of ~5.6Myr for half an orbit within the starburst ring. We find no strong evidence for a scenario where the continuous inflow of gas leads to the ongoing formation of massive clusters at the contact points between galactic bar and starburst ring. Instead, it appears more likely that the gas density build up more gradually over larger ring segments, and that the local physical conditions govern cluster formation. We note that the fundamental limitation on the accurate derivation of cluster age, mass and initial mass function slope is the lack of higher angular resolution. Resolving the highly embedded, massive clusters requires milli-arcsecond resolution at infrared wavelengths, which will be provided by the next generation of instruments on extremely large telescopes (ELTs).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61#2</TD>
            <TD>2012-11-15T12:54:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/543/A61&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A61</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/543/A61 [list]</TD>
            <TD>SINFONI data cube of NGC 7552 (Brandl+, 2012)</TD>
            <TD>Approximately 20% of all spiral galaxies display starburst activity in nuclear rings of a few hundred parsecs in diameter. It is our main aim to investigate how the starburst ignites and propagates within the ring, leading to the formation of massive stellar clusters. We observed the ring galaxy NGC 7552 with the mid-infrared (MIR) instrument VISIR at an angular resolution of 0.3"-0.4" and with the near-infrared (NIR) integral-field spectrograph SINFONI on the VLT, and complement these observations with data from ISO and Spitzer. The starburst ring is clearly detected at MIR wavelengths at the location of the dust-extincted, dark ring seen in HST observations. This "ring", however, is a rather complex annular region of more than 100 parsec width. We find a large fraction of diffuse [NeII] and PAH emission in the central region that is not associated with the MIR peaks on spatial scales of ~30pc. We do not detect MIR emission from the nucleus of NGC 7552, which is very prominent at optical and NIR continuum wavelengths. However, we have identified nine unresolved MIR peaks within the ring. The average extinction of these peaks is A_V_=7.4 and their total infrared luminosity is L_IR_=2.1x10^10^L_{sun}_. The properties of these peaks are typical for MIR-selected massive clusters found in other galaxies. The ages of the MIR-selected clusters are in the range of 5.9+/-0.3Myr. The age spread among the clusters of 0.8Myr is small compared to the travel time of ~5.6Myr for half an orbit within the starburst ring. We find no strong evidence for a scenario where the continuous inflow of gas leads to the ongoing formation of massive clusters at the contact points between galactic bar and starburst ring. Instead, it appears more likely that the gas density build up more gradually over larger ring segments, and that the local physical conditions govern cluster formation. We note that the fundamental limitation on the accurate derivation of cluster age, mass and initial mass function slope is the lack of higher angular resolution. Resolving the highly embedded, massive clusters requires milli-arcsecond resolution at infrared wavelengths, which will be provided by the next generation of instruments on extremely large telescopes (ELTs).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61#list</TD>
            <TD>2012-11-15T12:54:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/543/A61&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A61</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/543/A61 [1]</TD>
            <TD>SINFONI data cube of NGC 7552 (Brandl+, 2012)</TD>
            <TD>Approximately 20% of all spiral galaxies display starburst activity in nuclear rings of a few hundred parsecs in diameter. It is our main aim to investigate how the starburst ignites and propagates within the ring, leading to the formation of massive stellar clusters. We observed the ring galaxy NGC 7552 with the mid-infrared (MIR) instrument VISIR at an angular resolution of 0.3"-0.4" and with the near-infrared (NIR) integral-field spectrograph SINFONI on the VLT, and complement these observations with data from ISO and Spitzer. The starburst ring is clearly detected at MIR wavelengths at the location of the dust-extincted, dark ring seen in HST observations. This "ring", however, is a rather complex annular region of more than 100 parsec width. We find a large fraction of diffuse [NeII] and PAH emission in the central region that is not associated with the MIR peaks on spatial scales of ~30pc. We do not detect MIR emission from the nucleus of NGC 7552, which is very prominent at optical and NIR continuum wavelengths. However, we have identified nine unresolved MIR peaks within the ring. The average extinction of these peaks is A_V_=7.4 and their total infrared luminosity is L_IR_=2.1x10^10^L_{sun}_. The properties of these peaks are typical for MIR-selected massive clusters found in other galaxies. The ages of the MIR-selected clusters are in the range of 5.9+/-0.3Myr. The age spread among the clusters of 0.8Myr is small compared to the travel time of ~5.6Myr for half an orbit within the starburst ring. We find no strong evidence for a scenario where the continuous inflow of gas leads to the ongoing formation of massive clusters at the contact points between galactic bar and starburst ring. Instead, it appears more likely that the gas density build up more gradually over larger ring segments, and that the local physical conditions govern cluster formation. We note that the fundamental limitation on the accurate derivation of cluster age, mass and initial mass function slope is the lack of higher angular resolution. Resolving the highly embedded, massive clusters requires milli-arcsecond resolution at infrared wavelengths, which will be provided by the next generation of instruments on extremely large telescopes (ELTs).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61#1</TD>
            <TD>2012-11-15T12:54:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/543/A61</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A61</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/543/A61 [2]</TD>
            <TD>SINFONI data cube of NGC 7552 (Brandl+, 2012)</TD>
            <TD>Approximately 20% of all spiral galaxies display starburst activity in nuclear rings of a few hundred parsecs in diameter. It is our main aim to investigate how the starburst ignites and propagates within the ring, leading to the formation of massive stellar clusters. We observed the ring galaxy NGC 7552 with the mid-infrared (MIR) instrument VISIR at an angular resolution of 0.3"-0.4" and with the near-infrared (NIR) integral-field spectrograph SINFONI on the VLT, and complement these observations with data from ISO and Spitzer. The starburst ring is clearly detected at MIR wavelengths at the location of the dust-extincted, dark ring seen in HST observations. This "ring", however, is a rather complex annular region of more than 100 parsec width. We find a large fraction of diffuse [NeII] and PAH emission in the central region that is not associated with the MIR peaks on spatial scales of ~30pc. We do not detect MIR emission from the nucleus of NGC 7552, which is very prominent at optical and NIR continuum wavelengths. However, we have identified nine unresolved MIR peaks within the ring. The average extinction of these peaks is A_V_=7.4 and their total infrared luminosity is L_IR_=2.1x10^10^L_{sun}_. The properties of these peaks are typical for MIR-selected massive clusters found in other galaxies. The ages of the MIR-selected clusters are in the range of 5.9+/-0.3Myr. The age spread among the clusters of 0.8Myr is small compared to the travel time of ~5.6Myr for half an orbit within the starburst ring. We find no strong evidence for a scenario where the continuous inflow of gas leads to the ongoing formation of massive clusters at the contact points between galactic bar and starburst ring. Instead, it appears more likely that the gas density build up more gradually over larger ring segments, and that the local physical conditions govern cluster formation. We note that the fundamental limitation on the accurate derivation of cluster age, mass and initial mass function slope is the lack of higher angular resolution. Resolving the highly embedded, massive clusters requires milli-arcsecond resolution at infrared wavelengths, which will be provided by the next generation of instruments on extremely large telescopes (ELTs).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61#2</TD>
            <TD>2012-11-15T12:54:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/543/A61&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A61</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/543/A61 [list]</TD>
            <TD>SINFONI data cube of NGC 7552 (Brandl+, 2012)</TD>
            <TD>Approximately 20% of all spiral galaxies display starburst activity in nuclear rings of a few hundred parsecs in diameter. It is our main aim to investigate how the starburst ignites and propagates within the ring, leading to the formation of massive stellar clusters. We observed the ring galaxy NGC 7552 with the mid-infrared (MIR) instrument VISIR at an angular resolution of 0.3"-0.4" and with the near-infrared (NIR) integral-field spectrograph SINFONI on the VLT, and complement these observations with data from ISO and Spitzer. The starburst ring is clearly detected at MIR wavelengths at the location of the dust-extincted, dark ring seen in HST observations. This "ring", however, is a rather complex annular region of more than 100 parsec width. We find a large fraction of diffuse [NeII] and PAH emission in the central region that is not associated with the MIR peaks on spatial scales of ~30pc. We do not detect MIR emission from the nucleus of NGC 7552, which is very prominent at optical and NIR continuum wavelengths. However, we have identified nine unresolved MIR peaks within the ring. The average extinction of these peaks is A_V_=7.4 and their total infrared luminosity is L_IR_=2.1x10^10^L_{sun}_. The properties of these peaks are typical for MIR-selected massive clusters found in other galaxies. The ages of the MIR-selected clusters are in the range of 5.9+/-0.3Myr. The age spread among the clusters of 0.8Myr is small compared to the travel time of ~5.6Myr for half an orbit within the starburst ring. We find no strong evidence for a scenario where the continuous inflow of gas leads to the ongoing formation of massive clusters at the contact points between galactic bar and starburst ring. Instead, it appears more likely that the gas density build up more gradually over larger ring segments, and that the local physical conditions govern cluster formation. We note that the fundamental limitation on the accurate derivation of cluster age, mass and initial mass function slope is the lack of higher angular resolution. Resolving the highly embedded, massive clusters requires milli-arcsecond resolution at infrared wavelengths, which will be provided by the next generation of instruments on extremely large telescopes (ELTs).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61#list</TD>
            <TD>2012-11-15T12:54:53Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/543/A61</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/543/A61&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/543/A61</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/117/1 [1]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#1</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/117/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/117/1 [2]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#2</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/117/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/1 [table2]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#table2</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/1 [table3]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#table3</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/407/2109 [1]</TD>
            <TD>Kinematic study of open clusters (Vande Putte+, 2010)</TD>
            <TD>The Galactic population of open clusters provides an insight into star formation in the Galaxy. The open cluster catalogue by Dias et al. (Cat. B/ocl) is a rich source of data, including kinematic information. This large sample made it possible to carry out a systematic analysis of 481 open cluster orbits, using parameters based on orbit eccentricity and separation from the Galactic plane. These two parameters may be indicative of origin, and we find them to be correlated. We also find them to be correlated with metallicity, another parameter suggested elsewhere to be a marker for origin in that high values of any of these two parameters generally indicate a low metallicity ([Fe/H]solar&lt;-0.2dex). The resulting analysis points to four open clusters in the catalogue being of extragalactic origin by impact of high-velocity cloud on the disc: Berkeley 21, 32, 99 and Melotte 66, with a possible further four due to this origin (NGC 2158, 2420, 7789 and IC 1311). A further three may be due to Galactic globular cluster impact on the disc, i.e. of internal Galactic origin (NGC 6791, 1817 and 7044).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109#1</TD>
            <TD>2011-05-04T22:53:33Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/407/2109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/407/2109 [2]</TD>
            <TD>Kinematic study of open clusters (Vande Putte+, 2010)</TD>
            <TD>The Galactic population of open clusters provides an insight into star formation in the Galaxy. The open cluster catalogue by Dias et al. (Cat. B/ocl) is a rich source of data, including kinematic information. This large sample made it possible to carry out a systematic analysis of 481 open cluster orbits, using parameters based on orbit eccentricity and separation from the Galactic plane. These two parameters may be indicative of origin, and we find them to be correlated. We also find them to be correlated with metallicity, another parameter suggested elsewhere to be a marker for origin in that high values of any of these two parameters generally indicate a low metallicity ([Fe/H]solar&lt;-0.2dex). The resulting analysis points to four open clusters in the catalogue being of extragalactic origin by impact of high-velocity cloud on the disc: Berkeley 21, 32, 99 and Melotte 66, with a possible further four due to this origin (NGC 2158, 2420, 7789 and IC 1311). A further three may be due to Galactic globular cluster impact on the disc, i.e. of internal Galactic origin (NGC 6791, 1817 and 7044).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109#2</TD>
            <TD>2011-05-04T22:53:33Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/407/2109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2109</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/407/2109 [clusters]</TD>
            <TD>Kinematic study of open clusters (Vande Putte+, 2010)</TD>
            <TD>The Galactic population of open clusters provides an insight into star formation in the Galaxy. The open cluster catalogue by Dias et al. (Cat. B/ocl) is a rich source of data, including kinematic information. This large sample made it possible to carry out a systematic analysis of 481 open cluster orbits, using parameters based on orbit eccentricity and separation from the Galactic plane. These two parameters may be indicative of origin, and we find them to be correlated. We also find them to be correlated with metallicity, another parameter suggested elsewhere to be a marker for origin in that high values of any of these two parameters generally indicate a low metallicity ([Fe/H]solar&lt;-0.2dex). The resulting analysis points to four open clusters in the catalogue being of extragalactic origin by impact of high-velocity cloud on the disc: Berkeley 21, 32, 99 and Melotte 66, with a possible further four due to this origin (NGC 2158, 2420, 7789 and IC 1311). A further three may be due to Galactic globular cluster impact on the disc, i.e. of internal Galactic origin (NGC 6791, 1817 and 7044).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109#clusters</TD>
            <TD>2011-05-04T22:53:33Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/407/2109&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/117/1 [1]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#1</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/117/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/117/1 [2]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#2</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/117/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/1 [table2]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#table2</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/1 [table3]</TD>
            <TD>Galaxies in the "zone of avoidance". II. (Seeberger+, 1996)</TD>
            <TD>We have carried out a systematic search for galaxies in the galactic plane in a ten degree wide strip (-5deg&lt;=b&lt;=+5deg). In an area of 300 square degrees between l=180deg and l=210deg, 755 galaxies have been detected on Palomar red- sensitive prints. The smallest galaxies show diameters of 0.1mm corresponding to 6.7". We extended our survey to {delta}=-27deg i.e. l=~247deg to check our catalogue for completeness by comparing it with the Saito et al. (1990, 1991) catalogues of galaxies and present 334 new galaxy candidates at l&gt;=210deg. An asymmetry with respect to the galactic equator is obvious. By assuming the 60{mu} and 100{mu} sky flux density to be a rough measure of the total interstellar galactic extinction, and comparing them with the surface densities of the galaxies, we detected one possible galaxy cluster candidate at (l,b)=~(181.5deg+3.5deg), a concentration of galaxies at (l,b)=~(195deg+4.5deg), and confirmed three other galaxy concentrations. Finally, we argue that the red-sensitive surveys (ESO R; POSS II-R, POSS II-IR) are the best suitable material for galaxy searches in the zone of avoidance.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1#table3</TD>
            <TD>2011-09-14T18:18:57Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/407/2109 [1]</TD>
            <TD>Kinematic study of open clusters (Vande Putte+, 2010)</TD>
            <TD>The Galactic population of open clusters provides an insight into star formation in the Galaxy. The open cluster catalogue by Dias et al. (Cat. B/ocl) is a rich source of data, including kinematic information. This large sample made it possible to carry out a systematic analysis of 481 open cluster orbits, using parameters based on orbit eccentricity and separation from the Galactic plane. These two parameters may be indicative of origin, and we find them to be correlated. We also find them to be correlated with metallicity, another parameter suggested elsewhere to be a marker for origin in that high values of any of these two parameters generally indicate a low metallicity ([Fe/H]solar&lt;-0.2dex). The resulting analysis points to four open clusters in the catalogue being of extragalactic origin by impact of high-velocity cloud on the disc: Berkeley 21, 32, 99 and Melotte 66, with a possible further four due to this origin (NGC 2158, 2420, 7789 and IC 1311). A further three may be due to Galactic globular cluster impact on the disc, i.e. of internal Galactic origin (NGC 6791, 1817 and 7044).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109#1</TD>
            <TD>2011-05-04T22:53:33Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/407/2109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/407/2109 [2]</TD>
            <TD>Kinematic study of open clusters (Vande Putte+, 2010)</TD>
            <TD>The Galactic population of open clusters provides an insight into star formation in the Galaxy. The open cluster catalogue by Dias et al. (Cat. B/ocl) is a rich source of data, including kinematic information. This large sample made it possible to carry out a systematic analysis of 481 open cluster orbits, using parameters based on orbit eccentricity and separation from the Galactic plane. These two parameters may be indicative of origin, and we find them to be correlated. We also find them to be correlated with metallicity, another parameter suggested elsewhere to be a marker for origin in that high values of any of these two parameters generally indicate a low metallicity ([Fe/H]solar&lt;-0.2dex). The resulting analysis points to four open clusters in the catalogue being of extragalactic origin by impact of high-velocity cloud on the disc: Berkeley 21, 32, 99 and Melotte 66, with a possible further four due to this origin (NGC 2158, 2420, 7789 and IC 1311). A further three may be due to Galactic globular cluster impact on the disc, i.e. of internal Galactic origin (NGC 6791, 1817 and 7044).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109#2</TD>
            <TD>2011-05-04T22:53:33Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/407/2109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2109</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/407/2109 [clusters]</TD>
            <TD>Kinematic study of open clusters (Vande Putte+, 2010)</TD>
            <TD>The Galactic population of open clusters provides an insight into star formation in the Galaxy. The open cluster catalogue by Dias et al. (Cat. B/ocl) is a rich source of data, including kinematic information. This large sample made it possible to carry out a systematic analysis of 481 open cluster orbits, using parameters based on orbit eccentricity and separation from the Galactic plane. These two parameters may be indicative of origin, and we find them to be correlated. We also find them to be correlated with metallicity, another parameter suggested elsewhere to be a marker for origin in that high values of any of these two parameters generally indicate a low metallicity ([Fe/H]solar&lt;-0.2dex). The resulting analysis points to four open clusters in the catalogue being of extragalactic origin by impact of high-velocity cloud on the disc: Berkeley 21, 32, 99 and Melotte 66, with a possible further four due to this origin (NGC 2158, 2420, 7789 and IC 1311). A further three may be due to Galactic globular cluster impact on the disc, i.e. of internal Galactic origin (NGC 6791, 1817 and 7044).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109#clusters</TD>
            <TD>2011-05-04T22:53:33Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/407/2109&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/407/2109 [1]</TD>
            <TD>Kinematic study of open clusters (Vande Putte+, 2010)</TD>
            <TD>The Galactic population of open clusters provides an insight into star formation in the Galaxy. The open cluster catalogue by Dias et al. (Cat. B/ocl) is a rich source of data, including kinematic information. This large sample made it possible to carry out a systematic analysis of 481 open cluster orbits, using parameters based on orbit eccentricity and separation from the Galactic plane. These two parameters may be indicative of origin, and we find them to be correlated. We also find them to be correlated with metallicity, another parameter suggested elsewhere to be a marker for origin in that high values of any of these two parameters generally indicate a low metallicity ([Fe/H]solar&lt;-0.2dex). The resulting analysis points to four open clusters in the catalogue being of extragalactic origin by impact of high-velocity cloud on the disc: Berkeley 21, 32, 99 and Melotte 66, with a possible further four due to this origin (NGC 2158, 2420, 7789 and IC 1311). A further three may be due to Galactic globular cluster impact on the disc, i.e. of internal Galactic origin (NGC 6791, 1817 and 7044).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109#1</TD>
            <TD>2011-05-04T22:53:33Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/407/2109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/407/2109 [2]</TD>
            <TD>Kinematic study of open clusters (Vande Putte+, 2010)</TD>
            <TD>The Galactic population of open clusters provides an insight into star formation in the Galaxy. The open cluster catalogue by Dias et al. (Cat. B/ocl) is a rich source of data, including kinematic information. This large sample made it possible to carry out a systematic analysis of 481 open cluster orbits, using parameters based on orbit eccentricity and separation from the Galactic plane. These two parameters may be indicative of origin, and we find them to be correlated. We also find them to be correlated with metallicity, another parameter suggested elsewhere to be a marker for origin in that high values of any of these two parameters generally indicate a low metallicity ([Fe/H]solar&lt;-0.2dex). The resulting analysis points to four open clusters in the catalogue being of extragalactic origin by impact of high-velocity cloud on the disc: Berkeley 21, 32, 99 and Melotte 66, with a possible further four due to this origin (NGC 2158, 2420, 7789 and IC 1311). A further three may be due to Galactic globular cluster impact on the disc, i.e. of internal Galactic origin (NGC 6791, 1817 and 7044).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109#2</TD>
            <TD>2011-05-04T22:53:33Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/407/2109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2109</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/407/2109 [clusters]</TD>
            <TD>Kinematic study of open clusters (Vande Putte+, 2010)</TD>
            <TD>The Galactic population of open clusters provides an insight into star formation in the Galaxy. The open cluster catalogue by Dias et al. (Cat. B/ocl) is a rich source of data, including kinematic information. This large sample made it possible to carry out a systematic analysis of 481 open cluster orbits, using parameters based on orbit eccentricity and separation from the Galactic plane. These two parameters may be indicative of origin, and we find them to be correlated. We also find them to be correlated with metallicity, another parameter suggested elsewhere to be a marker for origin in that high values of any of these two parameters generally indicate a low metallicity ([Fe/H]solar&lt;-0.2dex). The resulting analysis points to four open clusters in the catalogue being of extragalactic origin by impact of high-velocity cloud on the disc: Berkeley 21, 32, 99 and Melotte 66, with a possible further four due to this origin (NGC 2158, 2420, 7789 and IC 1311). A further three may be due to Galactic globular cluster impact on the disc, i.e. of internal Galactic origin (NGC 6791, 1817 and 7044).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109#clusters</TD>
            <TD>2011-05-04T22:53:33Z</TD>
            <TD>#Open_Clusters#Proper_Motions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/407/2109</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/407/2109&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/407/2109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/370/1223 [1]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#1</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/370/1223</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/370/1223 [2]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#2</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/370/1223&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/370/1223 [table3]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#table3</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/370/1223&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/370/1223 [tablea1]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#tablea1</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/370/1223&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/2140 [1]</TD>
            <TD>Abundances and velocities in globular clusters (Pritzl+, 2005)</TD>
            <TD>We have compiled a sample of globular clusters with high-quality stellar abundances from the literature to compare to the chemistries of stars in the Galaxy and in dwarf spheroidal galaxies. Of the 45 globular clusters examined, 29 also have kinematic information. Most of the globular clusters belong to the Galactic halo; however, a significant number have disk kinematics or belong to the bulge.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140#1</TD>
            <TD>2012-01-01T18:20:03Z</TD>
            <TD>#Abundances#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/2140</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2140</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/2140 [2]</TD>
            <TD>Abundances and velocities in globular clusters (Pritzl+, 2005)</TD>
            <TD>We have compiled a sample of globular clusters with high-quality stellar abundances from the literature to compare to the chemistries of stars in the Galaxy and in dwarf spheroidal galaxies. Of the 45 globular clusters examined, 29 also have kinematic information. Most of the globular clusters belong to the Galactic halo; however, a significant number have disk kinematics or belong to the bulge.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140#2</TD>
            <TD>2012-01-01T18:20:03Z</TD>
            <TD>#Abundances#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/2140&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/2140 [table3]</TD>
            <TD>Abundances and velocities in globular clusters (Pritzl+, 2005)</TD>
            <TD>We have compiled a sample of globular clusters with high-quality stellar abundances from the literature to compare to the chemistries of stars in the Galaxy and in dwarf spheroidal galaxies. Of the 45 globular clusters examined, 29 also have kinematic information. Most of the globular clusters belong to the Galactic halo; however, a significant number have disk kinematics or belong to the bulge.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140#table3</TD>
            <TD>2012-01-01T18:20:03Z</TD>
            <TD>#Abundances#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/2140&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2140</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/2140 [1]</TD>
            <TD>Abundances and velocities in globular clusters (Pritzl+, 2005)</TD>
            <TD>We have compiled a sample of globular clusters with high-quality stellar abundances from the literature to compare to the chemistries of stars in the Galaxy and in dwarf spheroidal galaxies. Of the 45 globular clusters examined, 29 also have kinematic information. Most of the globular clusters belong to the Galactic halo; however, a significant number have disk kinematics or belong to the bulge.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140#1</TD>
            <TD>2012-01-01T18:20:03Z</TD>
            <TD>#Abundances#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/2140</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2140</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/2140 [2]</TD>
            <TD>Abundances and velocities in globular clusters (Pritzl+, 2005)</TD>
            <TD>We have compiled a sample of globular clusters with high-quality stellar abundances from the literature to compare to the chemistries of stars in the Galaxy and in dwarf spheroidal galaxies. Of the 45 globular clusters examined, 29 also have kinematic information. Most of the globular clusters belong to the Galactic halo; however, a significant number have disk kinematics or belong to the bulge.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140#2</TD>
            <TD>2012-01-01T18:20:03Z</TD>
            <TD>#Abundances#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/2140&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/2140 [table3]</TD>
            <TD>Abundances and velocities in globular clusters (Pritzl+, 2005)</TD>
            <TD>We have compiled a sample of globular clusters with high-quality stellar abundances from the literature to compare to the chemistries of stars in the Galaxy and in dwarf spheroidal galaxies. Of the 45 globular clusters examined, 29 also have kinematic information. Most of the globular clusters belong to the Galactic halo; however, a significant number have disk kinematics or belong to the bulge.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140#table3</TD>
            <TD>2012-01-01T18:20:03Z</TD>
            <TD>#Abundances#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/2140&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2140</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/117/261 [1]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#1</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/117/261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/117/261 [2]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#2</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/117/261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/261 [table5]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#table5</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/261 [table6]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#table6</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/2140 [1]</TD>
            <TD>Abundances and velocities in globular clusters (Pritzl+, 2005)</TD>
            <TD>We have compiled a sample of globular clusters with high-quality stellar abundances from the literature to compare to the chemistries of stars in the Galaxy and in dwarf spheroidal galaxies. Of the 45 globular clusters examined, 29 also have kinematic information. Most of the globular clusters belong to the Galactic halo; however, a significant number have disk kinematics or belong to the bulge.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140#1</TD>
            <TD>2012-01-01T18:20:03Z</TD>
            <TD>#Abundances#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/2140</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2140</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/2140 [2]</TD>
            <TD>Abundances and velocities in globular clusters (Pritzl+, 2005)</TD>
            <TD>We have compiled a sample of globular clusters with high-quality stellar abundances from the literature to compare to the chemistries of stars in the Galaxy and in dwarf spheroidal galaxies. Of the 45 globular clusters examined, 29 also have kinematic information. Most of the globular clusters belong to the Galactic halo; however, a significant number have disk kinematics or belong to the bulge.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140#2</TD>
            <TD>2012-01-01T18:20:03Z</TD>
            <TD>#Abundances#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/2140&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/2140 [table3]</TD>
            <TD>Abundances and velocities in globular clusters (Pritzl+, 2005)</TD>
            <TD>We have compiled a sample of globular clusters with high-quality stellar abundances from the literature to compare to the chemistries of stars in the Galaxy and in dwarf spheroidal galaxies. Of the 45 globular clusters examined, 29 also have kinematic information. Most of the globular clusters belong to the Galactic halo; however, a significant number have disk kinematics or belong to the bulge.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140#table3</TD>
            <TD>2012-01-01T18:20:03Z</TD>
            <TD>#Abundances#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2140</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/2140&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2140</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/736/21 [1]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#1</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/736/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/736/21 [2]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#2</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/736/21 [gc_cat]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#gc_cat</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/736/21 [mg]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#mg</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/736/21 [bgccat]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#bgccat</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/117/261 [1]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#1</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/117/261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/117/261 [2]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#2</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/117/261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/261 [table5]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#table5</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/261 [table6]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#table6</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/370/1223 [1]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#1</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/370/1223</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/370/1223 [2]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#2</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/370/1223&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/370/1223 [table3]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#table3</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/370/1223&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/370/1223 [tablea1]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#tablea1</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/370/1223&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/705/1533 [1]</TD>
            <TD>NGC 5128 globular clusters (Chattopadhyay+, 2009)</TD>
            <TD>In the present study, we have first used a modified technique of principal component analysis (PCA; Salibian-Barrera et al. 2006, J. Am. Stat. Assoc., 101, 1198) to search for the optimum set of parameters which gives the maximum variation for the GCs in NGC 5128. Then we have classified the GCs on the basis of these significant parameters using a model-based method of cluster analysis (CA; Qui, D. &amp; Tamhane, A. C. 2007, J. Stat. Plan. Inference, 137, 3722) which finds the structure of the optimum groups of GCs instead of choosing groups in an ad hoc manner on the basis of a single parameter. Our analysis is based on the sample of GCs of the early-type central giant elliptical galaxy in the Centaurus group, NGC 5128, whose structural parameters have been derived by fitting King and Wilson models to the surface brightness profiles based on HST/ACS imaging in the F606W bandpass (McLaughlin et al. 2008MNRAS.384..563M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533#1</TD>
            <TD>2012-01-25T17:38:55Z</TD>
            <TD>#Globular_Clusters#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/705/1533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/1533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/705/1533 [2]</TD>
            <TD>NGC 5128 globular clusters (Chattopadhyay+, 2009)</TD>
            <TD>In the present study, we have first used a modified technique of principal component analysis (PCA; Salibian-Barrera et al. 2006, J. Am. Stat. Assoc., 101, 1198) to search for the optimum set of parameters which gives the maximum variation for the GCs in NGC 5128. Then we have classified the GCs on the basis of these significant parameters using a model-based method of cluster analysis (CA; Qui, D. &amp; Tamhane, A. C. 2007, J. Stat. Plan. Inference, 137, 3722) which finds the structure of the optimum groups of GCs instead of choosing groups in an ad hoc manner on the basis of a single parameter. Our analysis is based on the sample of GCs of the early-type central giant elliptical galaxy in the Centaurus group, NGC 5128, whose structural parameters have been derived by fitting King and Wilson models to the surface brightness profiles based on HST/ACS imaging in the F606W bandpass (McLaughlin et al. 2008MNRAS.384..563M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533#2</TD>
            <TD>2012-01-25T17:38:55Z</TD>
            <TD>#Globular_Clusters#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/705/1533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/1533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/1533 [glcl]</TD>
            <TD>NGC 5128 globular clusters (Chattopadhyay+, 2009)</TD>
            <TD>In the present study, we have first used a modified technique of principal component analysis (PCA; Salibian-Barrera et al. 2006, J. Am. Stat. Assoc., 101, 1198) to search for the optimum set of parameters which gives the maximum variation for the GCs in NGC 5128. Then we have classified the GCs on the basis of these significant parameters using a model-based method of cluster analysis (CA; Qui, D. &amp; Tamhane, A. C. 2007, J. Stat. Plan. Inference, 137, 3722) which finds the structure of the optimum groups of GCs instead of choosing groups in an ad hoc manner on the basis of a single parameter. Our analysis is based on the sample of GCs of the early-type central giant elliptical galaxy in the Centaurus group, NGC 5128, whose structural parameters have been derived by fitting King and Wilson models to the surface brightness profiles based on HST/ACS imaging in the F606W bandpass (McLaughlin et al. 2008MNRAS.384..563M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533#glcl</TD>
            <TD>2012-01-25T17:38:55Z</TD>
            <TD>#Globular_Clusters#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/1533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/1533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/117/261 [1]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#1</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/117/261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/117/261 [2]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#2</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/117/261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/261 [table5]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#table5</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/117/261 [table6]</TD>
            <TD>BR photometry of galaxies in low density regions (Vennik+, 1996)</TD>
            <TD>We perform detailed surface photometry, based on B- and/or R-band CCD images of 92 faint galaxies. They are a subsample of those galaxies which were studied by Hopp et al. (1994) in the direction of three nearby voids. We derive integral photometric parameters and radial surface brightness profiles and compare them to those of several faint galaxy samples, located in different environments, and of a bright field galaxy sample. According to the obtained photometric characteristics, our sample is a mixture of intrinsically bright and faint galaxies, about 60% of them belonging to the bright subsample (M_B_&lt;-19.0). These bright ones show mean characteristics of typical Freeman's disks and are mainly located in the background of the observed voids. The faint subsample (M_B_&gt;=-19.0) has parameters typical for the low-surface-brightness (LSB) galaxies. There are a few well isolated galaxies both among the bright and faint subsamples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261#table6</TD>
            <TD>2011-09-14T18:18:58Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/117/261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/117/261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/117/261</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/705/1533 [1]</TD>
            <TD>NGC 5128 globular clusters (Chattopadhyay+, 2009)</TD>
            <TD>In the present study, we have first used a modified technique of principal component analysis (PCA; Salibian-Barrera et al. 2006, J. Am. Stat. Assoc., 101, 1198) to search for the optimum set of parameters which gives the maximum variation for the GCs in NGC 5128. Then we have classified the GCs on the basis of these significant parameters using a model-based method of cluster analysis (CA; Qui, D. &amp; Tamhane, A. C. 2007, J. Stat. Plan. Inference, 137, 3722) which finds the structure of the optimum groups of GCs instead of choosing groups in an ad hoc manner on the basis of a single parameter. Our analysis is based on the sample of GCs of the early-type central giant elliptical galaxy in the Centaurus group, NGC 5128, whose structural parameters have been derived by fitting King and Wilson models to the surface brightness profiles based on HST/ACS imaging in the F606W bandpass (McLaughlin et al. 2008MNRAS.384..563M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533#1</TD>
            <TD>2012-01-25T17:38:55Z</TD>
            <TD>#Globular_Clusters#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/705/1533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/1533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/705/1533 [2]</TD>
            <TD>NGC 5128 globular clusters (Chattopadhyay+, 2009)</TD>
            <TD>In the present study, we have first used a modified technique of principal component analysis (PCA; Salibian-Barrera et al. 2006, J. Am. Stat. Assoc., 101, 1198) to search for the optimum set of parameters which gives the maximum variation for the GCs in NGC 5128. Then we have classified the GCs on the basis of these significant parameters using a model-based method of cluster analysis (CA; Qui, D. &amp; Tamhane, A. C. 2007, J. Stat. Plan. Inference, 137, 3722) which finds the structure of the optimum groups of GCs instead of choosing groups in an ad hoc manner on the basis of a single parameter. Our analysis is based on the sample of GCs of the early-type central giant elliptical galaxy in the Centaurus group, NGC 5128, whose structural parameters have been derived by fitting King and Wilson models to the surface brightness profiles based on HST/ACS imaging in the F606W bandpass (McLaughlin et al. 2008MNRAS.384..563M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533#2</TD>
            <TD>2012-01-25T17:38:55Z</TD>
            <TD>#Globular_Clusters#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/705/1533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/1533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/1533 [glcl]</TD>
            <TD>NGC 5128 globular clusters (Chattopadhyay+, 2009)</TD>
            <TD>In the present study, we have first used a modified technique of principal component analysis (PCA; Salibian-Barrera et al. 2006, J. Am. Stat. Assoc., 101, 1198) to search for the optimum set of parameters which gives the maximum variation for the GCs in NGC 5128. Then we have classified the GCs on the basis of these significant parameters using a model-based method of cluster analysis (CA; Qui, D. &amp; Tamhane, A. C. 2007, J. Stat. Plan. Inference, 137, 3722) which finds the structure of the optimum groups of GCs instead of choosing groups in an ad hoc manner on the basis of a single parameter. Our analysis is based on the sample of GCs of the early-type central giant elliptical galaxy in the Centaurus group, NGC 5128, whose structural parameters have been derived by fitting King and Wilson models to the surface brightness profiles based on HST/ACS imaging in the F606W bandpass (McLaughlin et al. 2008MNRAS.384..563M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533#glcl</TD>
            <TD>2012-01-25T17:38:55Z</TD>
            <TD>#Globular_Clusters#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/1533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/1533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/370/1223 [1]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#1</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/370/1223</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/370/1223 [2]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#2</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/370/1223&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/370/1223 [table3]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#table3</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/370/1223&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/370/1223 [tablea1]</TD>
            <TD>Dynamical properties of 15 nearby galaxy groups (Brough+, 2006)</TD>
            <TD>Here, we present an investigation of the properties of 15 nearby galaxy groups and their constituent galaxies. The groups are selected from the Group Evolution Multiwavelength Study (GEMS) and all have X-ray as well as wide-field neutral hydrogen (HI) observations. Group membership is determined using a friends-of-friends algorithm on the positions and velocities from the 6-degree Field Galaxy Survey and NASA/IPAC Extragalactic Database. For each group we derive their physical properties using this membership, including: velocity dispersions (sigma_v_), virial masses (M_V_), total K-band luminosities [L_K_(Tot)] and early-type fractions (f_early_) and present these data for the individual groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223#tablea1</TD>
            <TD>2011-09-14T20:00:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Nov-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/370/1223</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/370/1223&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/370/1223</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/120/323 [1]</TD>
            <TD>Long-slit spectroscopy of UCM galaxies (Gallego+ 1996)</TD>
            <TD>Spectroscopic observations for the full sample of H{alpha} emission-line galaxy candidates (ELGs) from the Universidad Complutense de Madrid objective-prism survey Lists 1 and 2 have been obtained in order to investigate fully the properties of the survey constituents as well as the selection characteristics and completeness limits of the survey itself. The spectroscopic data include redshifts, line fluxes, equivalent widths, emission-line ratios, optical reddening estimates and synthesized color indexes. We find that 74% of the objects in this sample do exhibit emission lines. We compare our observational data with parameters given in the published survey lists in order to assess the usefulness of the latter. The different emission-line galaxies have been classified according to their spectra in several groups. Gray-scale images of the CCD spectra near the main emission lines, spatial profiles at the continuum and the line for [OIII]{lambda}5007 and H{alpha} lines, as well as plots of the coadded spectra of selected galaxies are presented, and a number of peculiar objects are described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/323#1</TD>
            <TD>2011-09-14T18:19:31Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/120/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/120/323 [2]</TD>
            <TD>Long-slit spectroscopy of UCM galaxies (Gallego+ 1996)</TD>
            <TD>Spectroscopic observations for the full sample of H{alpha} emission-line galaxy candidates (ELGs) from the Universidad Complutense de Madrid objective-prism survey Lists 1 and 2 have been obtained in order to investigate fully the properties of the survey constituents as well as the selection characteristics and completeness limits of the survey itself. The spectroscopic data include redshifts, line fluxes, equivalent widths, emission-line ratios, optical reddening estimates and synthesized color indexes. We find that 74% of the objects in this sample do exhibit emission lines. We compare our observational data with parameters given in the published survey lists in order to assess the usefulness of the latter. The different emission-line galaxies have been classified according to their spectra in several groups. Gray-scale images of the CCD spectra near the main emission lines, spatial profiles at the continuum and the line for [OIII]{lambda}5007 and H{alpha} lines, as well as plots of the coadded spectra of selected galaxies are presented, and a number of peculiar objects are described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/323#2</TD>
            <TD>2011-09-14T18:19:31Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/120/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/705/1533 [1]</TD>
            <TD>NGC 5128 globular clusters (Chattopadhyay+, 2009)</TD>
            <TD>In the present study, we have first used a modified technique of principal component analysis (PCA; Salibian-Barrera et al. 2006, J. Am. Stat. Assoc., 101, 1198) to search for the optimum set of parameters which gives the maximum variation for the GCs in NGC 5128. Then we have classified the GCs on the basis of these significant parameters using a model-based method of cluster analysis (CA; Qui, D. &amp; Tamhane, A. C. 2007, J. Stat. Plan. Inference, 137, 3722) which finds the structure of the optimum groups of GCs instead of choosing groups in an ad hoc manner on the basis of a single parameter. Our analysis is based on the sample of GCs of the early-type central giant elliptical galaxy in the Centaurus group, NGC 5128, whose structural parameters have been derived by fitting King and Wilson models to the surface brightness profiles based on HST/ACS imaging in the F606W bandpass (McLaughlin et al. 2008MNRAS.384..563M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533#1</TD>
            <TD>2012-01-25T17:38:55Z</TD>
            <TD>#Globular_Clusters#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/705/1533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/1533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/705/1533 [2]</TD>
            <TD>NGC 5128 globular clusters (Chattopadhyay+, 2009)</TD>
            <TD>In the present study, we have first used a modified technique of principal component analysis (PCA; Salibian-Barrera et al. 2006, J. Am. Stat. Assoc., 101, 1198) to search for the optimum set of parameters which gives the maximum variation for the GCs in NGC 5128. Then we have classified the GCs on the basis of these significant parameters using a model-based method of cluster analysis (CA; Qui, D. &amp; Tamhane, A. C. 2007, J. Stat. Plan. Inference, 137, 3722) which finds the structure of the optimum groups of GCs instead of choosing groups in an ad hoc manner on the basis of a single parameter. Our analysis is based on the sample of GCs of the early-type central giant elliptical galaxy in the Centaurus group, NGC 5128, whose structural parameters have been derived by fitting King and Wilson models to the surface brightness profiles based on HST/ACS imaging in the F606W bandpass (McLaughlin et al. 2008MNRAS.384..563M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533#2</TD>
            <TD>2012-01-25T17:38:55Z</TD>
            <TD>#Globular_Clusters#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/705/1533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/1533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/1533 [glcl]</TD>
            <TD>NGC 5128 globular clusters (Chattopadhyay+, 2009)</TD>
            <TD>In the present study, we have first used a modified technique of principal component analysis (PCA; Salibian-Barrera et al. 2006, J. Am. Stat. Assoc., 101, 1198) to search for the optimum set of parameters which gives the maximum variation for the GCs in NGC 5128. Then we have classified the GCs on the basis of these significant parameters using a model-based method of cluster analysis (CA; Qui, D. &amp; Tamhane, A. C. 2007, J. Stat. Plan. Inference, 137, 3722) which finds the structure of the optimum groups of GCs instead of choosing groups in an ad hoc manner on the basis of a single parameter. Our analysis is based on the sample of GCs of the early-type central giant elliptical galaxy in the Centaurus group, NGC 5128, whose structural parameters have been derived by fitting King and Wilson models to the surface brightness profiles based on HST/ACS imaging in the F606W bandpass (McLaughlin et al. 2008MNRAS.384..563M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533#glcl</TD>
            <TD>2012-01-25T17:38:55Z</TD>
            <TD>#Globular_Clusters#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/1533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/1533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/1533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/513/733 [1]</TD>
            <TD>Globular cluster system in M87 (Kundu+, 1999)</TD>
            <TD>We have identified 1057 globular cluster candidates in a WFPC2 image of the inner region of M87. The globular cluster luminosity function (GCLF) can be well fitted by a Gaussian profile with a mean value of m^0^_V_=23.67+/-0.07mag and {sigma}=1.39+/-0.06mag. The GCLF in five radial bins is found to be statistically the same at all points, showing no clear evidence of dynamical destruction processes based on the luminosity function (LF). Similarly, there is no obvious trend between the half-light radius of the clusters and the galactocentric distance. The core radius of the globular cluster density distribution is R_c_=56", considerably larger than the core of the stellar component (R_c_=6.8"). The mean color of the cluster candidates is V-I=1.09mag, which corresponds to an average metallicity of Fe/H=-0.74dex. The color distribution is bimodal everywhere, with a blue peak at V-I=0.95mag and a red peak at V-I=1.20mag. The red population is only 0.1mag bluer than the underlying galaxy, indicating that these clusters formed late in the metal-enrichment history of the galaxy and were possibly created in a burst of star/cluster formation 3-6Gyr after the blue population. We also find that both the red and the blue cluster distributions have a more elliptical shape (Hubble type E3.5) than the nearly spherical galaxy. The average half-light radius of the clusters is ~2.5pc, which is comparable to the 3pc average effective radius of the Milky Way clusters, although the red clusters are ~20% smaller than the blue ones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733#1</TD>
            <TD>2011-09-14T20:01:08Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/513/733</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/513/733</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/513/733 [2]</TD>
            <TD>Globular cluster system in M87 (Kundu+, 1999)</TD>
            <TD>We have identified 1057 globular cluster candidates in a WFPC2 image of the inner region of M87. The globular cluster luminosity function (GCLF) can be well fitted by a Gaussian profile with a mean value of m^0^_V_=23.67+/-0.07mag and {sigma}=1.39+/-0.06mag. The GCLF in five radial bins is found to be statistically the same at all points, showing no clear evidence of dynamical destruction processes based on the luminosity function (LF). Similarly, there is no obvious trend between the half-light radius of the clusters and the galactocentric distance. The core radius of the globular cluster density distribution is R_c_=56", considerably larger than the core of the stellar component (R_c_=6.8"). The mean color of the cluster candidates is V-I=1.09mag, which corresponds to an average metallicity of Fe/H=-0.74dex. The color distribution is bimodal everywhere, with a blue peak at V-I=0.95mag and a red peak at V-I=1.20mag. The red population is only 0.1mag bluer than the underlying galaxy, indicating that these clusters formed late in the metal-enrichment history of the galaxy and were possibly created in a burst of star/cluster formation 3-6Gyr after the blue population. We also find that both the red and the blue cluster distributions have a more elliptical shape (Hubble type E3.5) than the nearly spherical galaxy. The average half-light radius of the clusters is ~2.5pc, which is comparable to the 3pc average effective radius of the Milky Way clusters, although the red clusters are ~20% smaller than the blue ones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733#2</TD>
            <TD>2011-09-14T20:01:08Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/513/733&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/513/733</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/513/733 [table2]</TD>
            <TD>Globular cluster system in M87 (Kundu+, 1999)</TD>
            <TD>We have identified 1057 globular cluster candidates in a WFPC2 image of the inner region of M87. The globular cluster luminosity function (GCLF) can be well fitted by a Gaussian profile with a mean value of m^0^_V_=23.67+/-0.07mag and {sigma}=1.39+/-0.06mag. The GCLF in five radial bins is found to be statistically the same at all points, showing no clear evidence of dynamical destruction processes based on the luminosity function (LF). Similarly, there is no obvious trend between the half-light radius of the clusters and the galactocentric distance. The core radius of the globular cluster density distribution is R_c_=56", considerably larger than the core of the stellar component (R_c_=6.8"). The mean color of the cluster candidates is V-I=1.09mag, which corresponds to an average metallicity of Fe/H=-0.74dex. The color distribution is bimodal everywhere, with a blue peak at V-I=0.95mag and a red peak at V-I=1.20mag. The red population is only 0.1mag bluer than the underlying galaxy, indicating that these clusters formed late in the metal-enrichment history of the galaxy and were possibly created in a burst of star/cluster formation 3-6Gyr after the blue population. We also find that both the red and the blue cluster distributions have a more elliptical shape (Hubble type E3.5) than the nearly spherical galaxy. The average half-light radius of the clusters is ~2.5pc, which is comparable to the 3pc average effective radius of the Milky Way clusters, although the red clusters are ~20% smaller than the blue ones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733#table2</TD>
            <TD>2011-09-14T20:01:08Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/513/733&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/513/733</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/120/323 [1]</TD>
            <TD>Long-slit spectroscopy of UCM galaxies (Gallego+ 1996)</TD>
            <TD>Spectroscopic observations for the full sample of H{alpha} emission-line galaxy candidates (ELGs) from the Universidad Complutense de Madrid objective-prism survey Lists 1 and 2 have been obtained in order to investigate fully the properties of the survey constituents as well as the selection characteristics and completeness limits of the survey itself. The spectroscopic data include redshifts, line fluxes, equivalent widths, emission-line ratios, optical reddening estimates and synthesized color indexes. We find that 74% of the objects in this sample do exhibit emission lines. We compare our observational data with parameters given in the published survey lists in order to assess the usefulness of the latter. The different emission-line galaxies have been classified according to their spectra in several groups. Gray-scale images of the CCD spectra near the main emission lines, spatial profiles at the continuum and the line for [OIII]{lambda}5007 and H{alpha} lines, as well as plots of the coadded spectra of selected galaxies are presented, and a number of peculiar objects are described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/323#1</TD>
            <TD>2011-09-14T18:19:31Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/120/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/120/323 [2]</TD>
            <TD>Long-slit spectroscopy of UCM galaxies (Gallego+ 1996)</TD>
            <TD>Spectroscopic observations for the full sample of H{alpha} emission-line galaxy candidates (ELGs) from the Universidad Complutense de Madrid objective-prism survey Lists 1 and 2 have been obtained in order to investigate fully the properties of the survey constituents as well as the selection characteristics and completeness limits of the survey itself. The spectroscopic data include redshifts, line fluxes, equivalent widths, emission-line ratios, optical reddening estimates and synthesized color indexes. We find that 74% of the objects in this sample do exhibit emission lines. We compare our observational data with parameters given in the published survey lists in order to assess the usefulness of the latter. The different emission-line galaxies have been classified according to their spectra in several groups. Gray-scale images of the CCD spectra near the main emission lines, spatial profiles at the continuum and the line for [OIII]{lambda}5007 and H{alpha} lines, as well as plots of the coadded spectra of selected galaxies are presented, and a number of peculiar objects are described.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/323#2</TD>
            <TD>2011-09-14T18:19:31Z</TD>
            <TD>#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/120/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/3059 [1]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#1</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/3059</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/3059 [2]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#2</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/3059&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/3059 [clusters]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#clusters</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/3059&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/3059 [qsos]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#qsos</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/3059&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/513/733 [1]</TD>
            <TD>Globular cluster system in M87 (Kundu+, 1999)</TD>
            <TD>We have identified 1057 globular cluster candidates in a WFPC2 image of the inner region of M87. The globular cluster luminosity function (GCLF) can be well fitted by a Gaussian profile with a mean value of m^0^_V_=23.67+/-0.07mag and {sigma}=1.39+/-0.06mag. The GCLF in five radial bins is found to be statistically the same at all points, showing no clear evidence of dynamical destruction processes based on the luminosity function (LF). Similarly, there is no obvious trend between the half-light radius of the clusters and the galactocentric distance. The core radius of the globular cluster density distribution is R_c_=56", considerably larger than the core of the stellar component (R_c_=6.8"). The mean color of the cluster candidates is V-I=1.09mag, which corresponds to an average metallicity of Fe/H=-0.74dex. The color distribution is bimodal everywhere, with a blue peak at V-I=0.95mag and a red peak at V-I=1.20mag. The red population is only 0.1mag bluer than the underlying galaxy, indicating that these clusters formed late in the metal-enrichment history of the galaxy and were possibly created in a burst of star/cluster formation 3-6Gyr after the blue population. We also find that both the red and the blue cluster distributions have a more elliptical shape (Hubble type E3.5) than the nearly spherical galaxy. The average half-light radius of the clusters is ~2.5pc, which is comparable to the 3pc average effective radius of the Milky Way clusters, although the red clusters are ~20% smaller than the blue ones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733#1</TD>
            <TD>2011-09-14T20:01:08Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/513/733</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/513/733</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/513/733 [2]</TD>
            <TD>Globular cluster system in M87 (Kundu+, 1999)</TD>
            <TD>We have identified 1057 globular cluster candidates in a WFPC2 image of the inner region of M87. The globular cluster luminosity function (GCLF) can be well fitted by a Gaussian profile with a mean value of m^0^_V_=23.67+/-0.07mag and {sigma}=1.39+/-0.06mag. The GCLF in five radial bins is found to be statistically the same at all points, showing no clear evidence of dynamical destruction processes based on the luminosity function (LF). Similarly, there is no obvious trend between the half-light radius of the clusters and the galactocentric distance. The core radius of the globular cluster density distribution is R_c_=56", considerably larger than the core of the stellar component (R_c_=6.8"). The mean color of the cluster candidates is V-I=1.09mag, which corresponds to an average metallicity of Fe/H=-0.74dex. The color distribution is bimodal everywhere, with a blue peak at V-I=0.95mag and a red peak at V-I=1.20mag. The red population is only 0.1mag bluer than the underlying galaxy, indicating that these clusters formed late in the metal-enrichment history of the galaxy and were possibly created in a burst of star/cluster formation 3-6Gyr after the blue population. We also find that both the red and the blue cluster distributions have a more elliptical shape (Hubble type E3.5) than the nearly spherical galaxy. The average half-light radius of the clusters is ~2.5pc, which is comparable to the 3pc average effective radius of the Milky Way clusters, although the red clusters are ~20% smaller than the blue ones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733#2</TD>
            <TD>2011-09-14T20:01:08Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/513/733&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/513/733</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/513/733 [table2]</TD>
            <TD>Globular cluster system in M87 (Kundu+, 1999)</TD>
            <TD>We have identified 1057 globular cluster candidates in a WFPC2 image of the inner region of M87. The globular cluster luminosity function (GCLF) can be well fitted by a Gaussian profile with a mean value of m^0^_V_=23.67+/-0.07mag and {sigma}=1.39+/-0.06mag. The GCLF in five radial bins is found to be statistically the same at all points, showing no clear evidence of dynamical destruction processes based on the luminosity function (LF). Similarly, there is no obvious trend between the half-light radius of the clusters and the galactocentric distance. The core radius of the globular cluster density distribution is R_c_=56", considerably larger than the core of the stellar component (R_c_=6.8"). The mean color of the cluster candidates is V-I=1.09mag, which corresponds to an average metallicity of Fe/H=-0.74dex. The color distribution is bimodal everywhere, with a blue peak at V-I=0.95mag and a red peak at V-I=1.20mag. The red population is only 0.1mag bluer than the underlying galaxy, indicating that these clusters formed late in the metal-enrichment history of the galaxy and were possibly created in a burst of star/cluster formation 3-6Gyr after the blue population. We also find that both the red and the blue cluster distributions have a more elliptical shape (Hubble type E3.5) than the nearly spherical galaxy. The average half-light radius of the clusters is ~2.5pc, which is comparable to the 3pc average effective radius of the Milky Way clusters, although the red clusters are ~20% smaller than the blue ones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733#table2</TD>
            <TD>2011-09-14T20:01:08Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/513/733&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/513/733</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/121/461 [1]</TD>
            <TD>UV variability of Fairall-9 (Recondo-Gonzalez+, 1997)</TD>
            <TD>This is a study of the UV variability of the galaxy Fairall-9 between 1978 and 1991. Table 1 shows the UV continuum fluxes measured in three "line-free" windows centered at 1171, 1400 and 1910 A (observed wavelengths), and corrected for E(B-V)=0.035 extinction. The IUE Fine Error Sensor (FES) counts (optical photometry) are also given in this table, corrected for the same extinction. Tables 10, 11, 12 and 13 show the variability of the components for the main UV lines (Ly{alpha}+NV, SiIV, CIV and MgII). Line profile variability has been used to isolate four gaussian line components, which are sufficient to describe all lines at all levels of brightness in a consistent way: one narrow (i.e. unresolved at the IUE resolution) and three broad components: a central (velocity same as the narrow line), a redshifted (v=3300 km/s) and a blue shifted one (v=-3600 km/s). The Ly{alpha}-NV blend is fitted together in the Ly{alpha} region (Table 10), to account the NV presence (one narrow and one red component). The results for SiIV are shown in Table 11. In CIV (Table 12) have been included a very weak component bluer than the blue component, most likely associated with NIV] 1486. Table 13 shows MgII results.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/121/461#1</TD>
            <TD>2011-09-14T18:19:44Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/121/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/121/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/121/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/121/461 [2]</TD>
            <TD>UV variability of Fairall-9 (Recondo-Gonzalez+, 1997)</TD>
            <TD>This is a study of the UV variability of the galaxy Fairall-9 between 1978 and 1991. Table 1 shows the UV continuum fluxes measured in three "line-free" windows centered at 1171, 1400 and 1910 A (observed wavelengths), and corrected for E(B-V)=0.035 extinction. The IUE Fine Error Sensor (FES) counts (optical photometry) are also given in this table, corrected for the same extinction. Tables 10, 11, 12 and 13 show the variability of the components for the main UV lines (Ly{alpha}+NV, SiIV, CIV and MgII). Line profile variability has been used to isolate four gaussian line components, which are sufficient to describe all lines at all levels of brightness in a consistent way: one narrow (i.e. unresolved at the IUE resolution) and three broad components: a central (velocity same as the narrow line), a redshifted (v=3300 km/s) and a blue shifted one (v=-3600 km/s). The Ly{alpha}-NV blend is fitted together in the Ly{alpha} region (Table 10), to account the NV presence (one narrow and one red component). The results for SiIV are shown in Table 11. In CIV (Table 12) have been included a very weak component bluer than the blue component, most likely associated with NIV] 1486. Table 13 shows MgII results.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/121/461#2</TD>
            <TD>2011-09-14T18:19:44Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/121/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/121/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/121/461</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/3059 [1]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#1</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/3059</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/3059 [2]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#2</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/3059&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/3059 [clusters]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#clusters</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/3059&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/3059 [qsos]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#qsos</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/3059&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/513/733 [1]</TD>
            <TD>Globular cluster system in M87 (Kundu+, 1999)</TD>
            <TD>We have identified 1057 globular cluster candidates in a WFPC2 image of the inner region of M87. The globular cluster luminosity function (GCLF) can be well fitted by a Gaussian profile with a mean value of m^0^_V_=23.67+/-0.07mag and {sigma}=1.39+/-0.06mag. The GCLF in five radial bins is found to be statistically the same at all points, showing no clear evidence of dynamical destruction processes based on the luminosity function (LF). Similarly, there is no obvious trend between the half-light radius of the clusters and the galactocentric distance. The core radius of the globular cluster density distribution is R_c_=56", considerably larger than the core of the stellar component (R_c_=6.8"). The mean color of the cluster candidates is V-I=1.09mag, which corresponds to an average metallicity of Fe/H=-0.74dex. The color distribution is bimodal everywhere, with a blue peak at V-I=0.95mag and a red peak at V-I=1.20mag. The red population is only 0.1mag bluer than the underlying galaxy, indicating that these clusters formed late in the metal-enrichment history of the galaxy and were possibly created in a burst of star/cluster formation 3-6Gyr after the blue population. We also find that both the red and the blue cluster distributions have a more elliptical shape (Hubble type E3.5) than the nearly spherical galaxy. The average half-light radius of the clusters is ~2.5pc, which is comparable to the 3pc average effective radius of the Milky Way clusters, although the red clusters are ~20% smaller than the blue ones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733#1</TD>
            <TD>2011-09-14T20:01:08Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/513/733</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/513/733</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/513/733 [2]</TD>
            <TD>Globular cluster system in M87 (Kundu+, 1999)</TD>
            <TD>We have identified 1057 globular cluster candidates in a WFPC2 image of the inner region of M87. The globular cluster luminosity function (GCLF) can be well fitted by a Gaussian profile with a mean value of m^0^_V_=23.67+/-0.07mag and {sigma}=1.39+/-0.06mag. The GCLF in five radial bins is found to be statistically the same at all points, showing no clear evidence of dynamical destruction processes based on the luminosity function (LF). Similarly, there is no obvious trend between the half-light radius of the clusters and the galactocentric distance. The core radius of the globular cluster density distribution is R_c_=56", considerably larger than the core of the stellar component (R_c_=6.8"). The mean color of the cluster candidates is V-I=1.09mag, which corresponds to an average metallicity of Fe/H=-0.74dex. The color distribution is bimodal everywhere, with a blue peak at V-I=0.95mag and a red peak at V-I=1.20mag. The red population is only 0.1mag bluer than the underlying galaxy, indicating that these clusters formed late in the metal-enrichment history of the galaxy and were possibly created in a burst of star/cluster formation 3-6Gyr after the blue population. We also find that both the red and the blue cluster distributions have a more elliptical shape (Hubble type E3.5) than the nearly spherical galaxy. The average half-light radius of the clusters is ~2.5pc, which is comparable to the 3pc average effective radius of the Milky Way clusters, although the red clusters are ~20% smaller than the blue ones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733#2</TD>
            <TD>2011-09-14T20:01:08Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/513/733&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/513/733</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/513/733 [table2]</TD>
            <TD>Globular cluster system in M87 (Kundu+, 1999)</TD>
            <TD>We have identified 1057 globular cluster candidates in a WFPC2 image of the inner region of M87. The globular cluster luminosity function (GCLF) can be well fitted by a Gaussian profile with a mean value of m^0^_V_=23.67+/-0.07mag and {sigma}=1.39+/-0.06mag. The GCLF in five radial bins is found to be statistically the same at all points, showing no clear evidence of dynamical destruction processes based on the luminosity function (LF). Similarly, there is no obvious trend between the half-light radius of the clusters and the galactocentric distance. The core radius of the globular cluster density distribution is R_c_=56", considerably larger than the core of the stellar component (R_c_=6.8"). The mean color of the cluster candidates is V-I=1.09mag, which corresponds to an average metallicity of Fe/H=-0.74dex. The color distribution is bimodal everywhere, with a blue peak at V-I=0.95mag and a red peak at V-I=1.20mag. The red population is only 0.1mag bluer than the underlying galaxy, indicating that these clusters formed late in the metal-enrichment history of the galaxy and were possibly created in a burst of star/cluster formation 3-6Gyr after the blue population. We also find that both the red and the blue cluster distributions have a more elliptical shape (Hubble type E3.5) than the nearly spherical galaxy. The average half-light radius of the clusters is ~2.5pc, which is comparable to the 3pc average effective radius of the Milky Way clusters, although the red clusters are ~20% smaller than the blue ones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733#table2</TD>
            <TD>2011-09-14T20:01:08Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/513/733</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/513/733&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/513/733</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/3059 [1]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#1</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/3059</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/3059 [2]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#2</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/3059&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/3059 [clusters]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#clusters</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/3059&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/3059 [qsos]</TD>
            <TD>4098 galaxy clusters in SDSS Stripe 82 (Geach+, 2011)</TD>
            <TD>We have chosen to distribute the full catalogue in Hierarchical Data Format (HDF, version 5). This format provides a natural way for us to release both the 'top level' cluster properties (coordinate, redshift, etc.) and a wide range of other information, including various richness classifications, and information for each of the constituent galaxies. However, for simple access, we also provide a "supplementary QSO sightline catalogue".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059#qsos</TD>
            <TD>2012-02-15T22:43:07Z</TD>
            <TD>#Clusters_of_galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/3059</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/3059&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/3059</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/707/1449 [1]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#1</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/707/1449</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/707/1449 [2]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#2</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/707/1449&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/707/1449 [table1]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#table1</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/707/1449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/707/1449 [table2]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#table2</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/707/1449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/707/1449 [1]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#1</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/707/1449</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/707/1449 [2]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#2</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/707/1449&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/707/1449 [table1]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#table1</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/707/1449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/707/1449 [table2]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#table2</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/707/1449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/707/1449 [1]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#1</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/707/1449</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/707/1449 [2]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#2</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/707/1449&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/707/1449 [table1]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#table1</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/707/1449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/707/1449 [table2]</TD>
            <TD>Local hosts of SNe Ia (Neill+, 2009)</TD>
            <TD>We use multi-wavelength, matched aperture, integrated photometry from the Galaxy Evolution Explorer (GALEX), the Sloan Digital Sky Survey, and the RC3 to estimate the physical properties of 166 nearby galaxies hosting 168 well-observed Type Ia supernovae (SNe Ia). The ultraviolet (UV) imaging of local SN Ia hosts from GALEX allows a direct comparison with higher-redshift hosts measured at optical wavelengths that correspond to the rest-frame UV. Our data corroborate well-known features that have been seen in other SN Ia samples. Specifically, hosts with active star formation produce brighter and slower SNe Ia on average, and hosts with luminosity-weighted ages older than 1Gyr produce on average more faint, fast, and fewer bright, slow SNe Ia than younger hosts. New results include that in our sample, the faintest and fastest SNe Ia occur only in galaxies exceeding a stellar mass threshold of ~10^10^M_{sun}_, leading us to conclude that their progenitors must arise in populations that are older and/or more metal rich than the general SN Ia population.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449#table2</TD>
            <TD>2012-02-17T21:54:41Z</TD>
            <TD>#Galaxies#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/707/1449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/707/1449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/707/1449</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/138/1037 [1]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#1</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/138/1037</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/138/1037 [2]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#2</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/138/1037&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1037 [digal]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#digal</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1037&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1037 [table3]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#table3</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1037&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/138/1037 [1]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#1</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/138/1037</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/138/1037 [2]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#2</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
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            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/138/1037&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1037 [digal]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#digal</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1037&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1037 [table3]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#table3</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1037&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/138/1037 [1]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#1</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/138/1037</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/138/1037 [2]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#2</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/138/1037&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1037 [digal]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#digal</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1037&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/138/1037 [table3]</TD>
            <TD>Star formation in Centaurus A Group dwarfs (Cote+ 2009)</TD>
            <TD>We observed all of the 19 dwarf irregular (dI) galaxy members of the Centaurus A Group listed in Cote et al. (1997AJ....114.1313C). Of these, 17 were detected and are listed in Table 1. The H{alpha} images, were obtained with the Cerro Tololo Inter-American Observatory (CTIO) 0.9m telescope over 8 nights in 1999 April. The observations usually consisted of 3x1200s through a narrow-band H{alpha} filter centered at 6559{AA} and with a FWHM of 64{AA}, followed by a 2x1200s for continuum off-band images through a filter centered at 6115{AA} and with a FWHM of 140{AA}. R-band images were also acquired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037#table3</TD>
            <TD>2012-02-26T18:11:23Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/138/1037</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/138/1037&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/138/1037</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/403/2063 [1]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#1</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/403/2063</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/403/2063 [2]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#2</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/2063 [table1]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#table1</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/2063 [table3]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#table3</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/2063 [table2]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#table2</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/403/2063 [1]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#1</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/403/2063</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/403/2063 [2]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#2</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/2063 [table1]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#table1</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/2063 [table3]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#table3</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/2063 [table2]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#table2</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/403/2063 [1]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#1</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/403/2063</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/403/2063 [2]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#2</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/2063 [table1]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#table1</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/2063 [table3]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#table3</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/2063 [table2]</TD>
            <TD>SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)</TD>
            <TD>We present the results of a search for galaxy clusters in the Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster flux in the 0.5-2keV band of 2x10^-15^erg/cm^2^/s over one of the widest XMM-Newton contiguous raster surveys, covering an area of 1.3deg^2^. Cluster candidates are identified through a wavelet detection of extended X-ray emission. The red-sequence technique allows us to identify 57 cluster candidates. We report on the progress with the cluster spectroscopic follow-up and derive their properties based on the X-ray luminosity and cluster scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063#table2</TD>
            <TD>2012-04-02T16:09:31Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/2063</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/2063&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/2063</TD>
          </TR>
          <TR>
            <TD>Spectra</TD>
            <TD>6dF Spectra</TD>
            <TD>6dF DR3 Simple Spectra Access</TD>
            <TD>The 6dF Galaxy Survey (6dFGS) aims to measure the redshifts of around 150 000 galaxies, and the peculiar velocities of a 15 000-member subsample, over almost the entire southern sky. The table called Spectra contains the redshifts and qualities of all the observations. When complete, it will be the largest redshift survey of the nearby Universe, reaching out to about z ~ 0.15, and more than an order of magnitude larger than any peculiar velocity survey to date. The targets are all galaxies brighter than K tot = 12.75 in the 2MASS Extended Source Catalog (XSC), supplemented by 2MASS and SuperCOSMOS galaxies that complete the sample to limits of (H, J , r F, bJ) = (13.05, 13.75, 15.6, 16.75). This is the Data Release 3 version.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Optical#</TD>
            <TD>ivo://wfau.roe.ac.uk/6dF-ssap#1</TD>
            <TD>2011-03-22T15:26:11Z</TD>
            <TD>#6dF Data Release 3 Spectra#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk/6dF-ssap</TD>
            <TD>SimpleSpectralAccess</TD>
            <TD>ivo://ivoa.net/std/SSA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/6dF-ssap/?</TD>
            <TD>360.0</TD>
            <TD>10000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www-wfau.roe.ac.uk/6dfgs/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/736/21 [1]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#1</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/736/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/736/21 [2]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#2</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/736/21 [gc_cat]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#gc_cat</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/736/21 [mg]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#mg</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/736/21 [bgccat]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#bgccat</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/714/25 [1]</TD>
            <TD>AMUSE-Virgo survey. II. (Gallo+, 2010)</TD>
            <TD>In Cycle 8 we proposed and were awarded a large Chandra/Spitzer program to observe 100 (84 new + 16 archival) spheroidal galaxies in the Virgo Cluster (AMUSE-Virgo; PI: Treu, 454ks). The targeted sample is that of the Hubble Virgo Cluster Survey (VCS; Cote et al. 2004, Cat. J/ApJS/153/223). For each galaxy, the high-resolution g- and z-band images enable us to resolve, when present, the nuclear star cluster, infer its enclosed mass, and thus estimate the chance contamination from a low-mass X-ray binary (LMXB) as bright/brighter than the detected X-ray core based on the shape and normalization of the LMXB luminosity function in external galaxies. As a part of the AMUSE-Virgo survey, each VCS galaxy was observed with Chandra/ACIS for a minimum of 5.4ks. The Chandra results from the first 32 targets (16 new + 16, typically more massive, archival observations) have been presented by Gallo et al. (Paper I; 2008ApJ...680..154G). In Paper II, we complete the X-ray analysis of the whole AMUSE-Virgo sample.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25#1</TD>
            <TD>2012-06-09T21:26:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/714/25</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/25</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/714/25 [2]</TD>
            <TD>AMUSE-Virgo survey. II. (Gallo+, 2010)</TD>
            <TD>In Cycle 8 we proposed and were awarded a large Chandra/Spitzer program to observe 100 (84 new + 16 archival) spheroidal galaxies in the Virgo Cluster (AMUSE-Virgo; PI: Treu, 454ks). The targeted sample is that of the Hubble Virgo Cluster Survey (VCS; Cote et al. 2004, Cat. J/ApJS/153/223). For each galaxy, the high-resolution g- and z-band images enable us to resolve, when present, the nuclear star cluster, infer its enclosed mass, and thus estimate the chance contamination from a low-mass X-ray binary (LMXB) as bright/brighter than the detected X-ray core based on the shape and normalization of the LMXB luminosity function in external galaxies. As a part of the AMUSE-Virgo survey, each VCS galaxy was observed with Chandra/ACIS for a minimum of 5.4ks. The Chandra results from the first 32 targets (16 new + 16, typically more massive, archival observations) have been presented by Gallo et al. (Paper I; 2008ApJ...680..154G). In Paper II, we complete the X-ray analysis of the whole AMUSE-Virgo sample.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25#2</TD>
            <TD>2012-06-09T21:26:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/714/25&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/714/25 [table1]</TD>
            <TD>AMUSE-Virgo survey. II. (Gallo+, 2010)</TD>
            <TD>In Cycle 8 we proposed and were awarded a large Chandra/Spitzer program to observe 100 (84 new + 16 archival) spheroidal galaxies in the Virgo Cluster (AMUSE-Virgo; PI: Treu, 454ks). The targeted sample is that of the Hubble Virgo Cluster Survey (VCS; Cote et al. 2004, Cat. J/ApJS/153/223). For each galaxy, the high-resolution g- and z-band images enable us to resolve, when present, the nuclear star cluster, infer its enclosed mass, and thus estimate the chance contamination from a low-mass X-ray binary (LMXB) as bright/brighter than the detected X-ray core based on the shape and normalization of the LMXB luminosity function in external galaxies. As a part of the AMUSE-Virgo survey, each VCS galaxy was observed with Chandra/ACIS for a minimum of 5.4ks. The Chandra results from the first 32 targets (16 new + 16, typically more massive, archival observations) have been presented by Gallo et al. (Paper I; 2008ApJ...680..154G). In Paper II, we complete the X-ray analysis of the whole AMUSE-Virgo sample.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25#table1</TD>
            <TD>2012-06-09T21:26:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/714/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/25</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/540/A106 [1]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#1</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/540/A106</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/540/A106 [2]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#2</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/540/A106&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A106 [dr8gal]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#dr8gal</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A106&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A106 [dr8gr]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#dr8gr</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A106&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/714/25 [1]</TD>
            <TD>AMUSE-Virgo survey. II. (Gallo+, 2010)</TD>
            <TD>In Cycle 8 we proposed and were awarded a large Chandra/Spitzer program to observe 100 (84 new + 16 archival) spheroidal galaxies in the Virgo Cluster (AMUSE-Virgo; PI: Treu, 454ks). The targeted sample is that of the Hubble Virgo Cluster Survey (VCS; Cote et al. 2004, Cat. J/ApJS/153/223). For each galaxy, the high-resolution g- and z-band images enable us to resolve, when present, the nuclear star cluster, infer its enclosed mass, and thus estimate the chance contamination from a low-mass X-ray binary (LMXB) as bright/brighter than the detected X-ray core based on the shape and normalization of the LMXB luminosity function in external galaxies. As a part of the AMUSE-Virgo survey, each VCS galaxy was observed with Chandra/ACIS for a minimum of 5.4ks. The Chandra results from the first 32 targets (16 new + 16, typically more massive, archival observations) have been presented by Gallo et al. (Paper I; 2008ApJ...680..154G). In Paper II, we complete the X-ray analysis of the whole AMUSE-Virgo sample.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25#1</TD>
            <TD>2012-06-09T21:26:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/714/25</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/25</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/714/25 [2]</TD>
            <TD>AMUSE-Virgo survey. II. (Gallo+, 2010)</TD>
            <TD>In Cycle 8 we proposed and were awarded a large Chandra/Spitzer program to observe 100 (84 new + 16 archival) spheroidal galaxies in the Virgo Cluster (AMUSE-Virgo; PI: Treu, 454ks). The targeted sample is that of the Hubble Virgo Cluster Survey (VCS; Cote et al. 2004, Cat. J/ApJS/153/223). For each galaxy, the high-resolution g- and z-band images enable us to resolve, when present, the nuclear star cluster, infer its enclosed mass, and thus estimate the chance contamination from a low-mass X-ray binary (LMXB) as bright/brighter than the detected X-ray core based on the shape and normalization of the LMXB luminosity function in external galaxies. As a part of the AMUSE-Virgo survey, each VCS galaxy was observed with Chandra/ACIS for a minimum of 5.4ks. The Chandra results from the first 32 targets (16 new + 16, typically more massive, archival observations) have been presented by Gallo et al. (Paper I; 2008ApJ...680..154G). In Paper II, we complete the X-ray analysis of the whole AMUSE-Virgo sample.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25#2</TD>
            <TD>2012-06-09T21:26:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/714/25&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/714/25 [table1]</TD>
            <TD>AMUSE-Virgo survey. II. (Gallo+, 2010)</TD>
            <TD>In Cycle 8 we proposed and were awarded a large Chandra/Spitzer program to observe 100 (84 new + 16 archival) spheroidal galaxies in the Virgo Cluster (AMUSE-Virgo; PI: Treu, 454ks). The targeted sample is that of the Hubble Virgo Cluster Survey (VCS; Cote et al. 2004, Cat. J/ApJS/153/223). For each galaxy, the high-resolution g- and z-band images enable us to resolve, when present, the nuclear star cluster, infer its enclosed mass, and thus estimate the chance contamination from a low-mass X-ray binary (LMXB) as bright/brighter than the detected X-ray core based on the shape and normalization of the LMXB luminosity function in external galaxies. As a part of the AMUSE-Virgo survey, each VCS galaxy was observed with Chandra/ACIS for a minimum of 5.4ks. The Chandra results from the first 32 targets (16 new + 16, typically more massive, archival observations) have been presented by Gallo et al. (Paper I; 2008ApJ...680..154G). In Paper II, we complete the X-ray analysis of the whole AMUSE-Virgo sample.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25#table1</TD>
            <TD>2012-06-09T21:26:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/714/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/25</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/714/25 [1]</TD>
            <TD>AMUSE-Virgo survey. II. (Gallo+, 2010)</TD>
            <TD>In Cycle 8 we proposed and were awarded a large Chandra/Spitzer program to observe 100 (84 new + 16 archival) spheroidal galaxies in the Virgo Cluster (AMUSE-Virgo; PI: Treu, 454ks). The targeted sample is that of the Hubble Virgo Cluster Survey (VCS; Cote et al. 2004, Cat. J/ApJS/153/223). For each galaxy, the high-resolution g- and z-band images enable us to resolve, when present, the nuclear star cluster, infer its enclosed mass, and thus estimate the chance contamination from a low-mass X-ray binary (LMXB) as bright/brighter than the detected X-ray core based on the shape and normalization of the LMXB luminosity function in external galaxies. As a part of the AMUSE-Virgo survey, each VCS galaxy was observed with Chandra/ACIS for a minimum of 5.4ks. The Chandra results from the first 32 targets (16 new + 16, typically more massive, archival observations) have been presented by Gallo et al. (Paper I; 2008ApJ...680..154G). In Paper II, we complete the X-ray analysis of the whole AMUSE-Virgo sample.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25#1</TD>
            <TD>2012-06-09T21:26:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/714/25</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/25</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/714/25 [2]</TD>
            <TD>AMUSE-Virgo survey. II. (Gallo+, 2010)</TD>
            <TD>In Cycle 8 we proposed and were awarded a large Chandra/Spitzer program to observe 100 (84 new + 16 archival) spheroidal galaxies in the Virgo Cluster (AMUSE-Virgo; PI: Treu, 454ks). The targeted sample is that of the Hubble Virgo Cluster Survey (VCS; Cote et al. 2004, Cat. J/ApJS/153/223). For each galaxy, the high-resolution g- and z-band images enable us to resolve, when present, the nuclear star cluster, infer its enclosed mass, and thus estimate the chance contamination from a low-mass X-ray binary (LMXB) as bright/brighter than the detected X-ray core based on the shape and normalization of the LMXB luminosity function in external galaxies. As a part of the AMUSE-Virgo survey, each VCS galaxy was observed with Chandra/ACIS for a minimum of 5.4ks. The Chandra results from the first 32 targets (16 new + 16, typically more massive, archival observations) have been presented by Gallo et al. (Paper I; 2008ApJ...680..154G). In Paper II, we complete the X-ray analysis of the whole AMUSE-Virgo sample.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25#2</TD>
            <TD>2012-06-09T21:26:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/714/25&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/714/25 [table1]</TD>
            <TD>AMUSE-Virgo survey. II. (Gallo+, 2010)</TD>
            <TD>In Cycle 8 we proposed and were awarded a large Chandra/Spitzer program to observe 100 (84 new + 16 archival) spheroidal galaxies in the Virgo Cluster (AMUSE-Virgo; PI: Treu, 454ks). The targeted sample is that of the Hubble Virgo Cluster Survey (VCS; Cote et al. 2004, Cat. J/ApJS/153/223). For each galaxy, the high-resolution g- and z-band images enable us to resolve, when present, the nuclear star cluster, infer its enclosed mass, and thus estimate the chance contamination from a low-mass X-ray binary (LMXB) as bright/brighter than the detected X-ray core based on the shape and normalization of the LMXB luminosity function in external galaxies. As a part of the AMUSE-Virgo survey, each VCS galaxy was observed with Chandra/ACIS for a minimum of 5.4ks. The Chandra results from the first 32 targets (16 new + 16, typically more massive, archival observations) have been presented by Gallo et al. (Paper I; 2008ApJ...680..154G). In Paper II, we complete the X-ray analysis of the whole AMUSE-Virgo sample.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25#table1</TD>
            <TD>2012-06-09T21:26:30Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/714/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/714/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/714/25</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/736/21 [1]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#1</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/736/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/736/21 [2]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#2</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/736/21 [gc_cat]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#gc_cat</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/736/21 [mg]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#mg</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/736/21 [bgccat]</TD>
            <TD>Galaxy clusters optical catalog from AMF on SDSS DR6 (Szabo+ 2011)</TD>
            <TD>We present a new cluster catalog extracted from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6) using an adaptive matched filter (AMF) cluster finder. We identify 69,173 galaxy clusters in the redshift range 0.045&lt;=z&lt;0.78 in 8420deg^2^ of the sky. We provide angular position, redshift, richness, core, and virial radii estimates for these clusters, as well as an error analysis for each of these quantities. We also provide a catalog of more than 205,000 galaxies representing the three brightest galaxies in the r band which are possible brightest cluster galaxy (BCG) candidates. We show basic properties of the BCG candidates and study how their luminosity scales in redshift and cluster richness. We compare our catalog with the maxBCG and GMBCG catalogs, as well as with that of Wen et al. We match between 30% and 50% of clusters between catalogs over all overlapping redshift ranges. We find that the percentage of matches increases with the richness for all catalogs. We cross match the AMF catalog with available X-ray data in the same area of the sky and find 539 matches, 119 of which with temperature measurements. We present scaling relations between optical and X-ray properties and cluster center comparison.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21#bgccat</TD>
            <TD>2011-09-14T21:30:05Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/736/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/736/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/736/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/390 [1]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#1</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/390</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/390 [2]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#2</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/390&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/390 [Rloud]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#Rloud</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/390&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/390 [Rquiet]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#Rquiet</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/390&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/540/A106 [1]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#1</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/540/A106</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/540/A106 [2]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#2</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/540/A106&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A106 [dr8gal]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#dr8gal</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A106&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A106 [dr8gr]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#dr8gr</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A106&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/533/A25 [1]</TD>
            <TD>VLT/X-shooter observations of PHL293B (Izotov+ 2011)</TD>
            <TD>Fig1.dat - the flux-calibrated and redshift-corrected VLT/X-shooter UV and optical spectrum of the low-metallicity blue compact dwarf galaxy PHL 293B. Fig2.dat - the flux-calibrated and redshift-corrected VLT/X-shooter near-infrared spectrum of the low-metallicity blue compact dwarf galaxy PHL 293B.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A25#1</TD>
            <TD>2011-09-14T21:30:06Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A25</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/533/A25</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A25</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/533/A25 [2]</TD>
            <TD>VLT/X-shooter observations of PHL293B (Izotov+ 2011)</TD>
            <TD>Fig1.dat - the flux-calibrated and redshift-corrected VLT/X-shooter UV and optical spectrum of the low-metallicity blue compact dwarf galaxy PHL 293B. Fig2.dat - the flux-calibrated and redshift-corrected VLT/X-shooter near-infrared spectrum of the low-metallicity blue compact dwarf galaxy PHL 293B.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A25#2</TD>
            <TD>2011-09-14T21:30:06Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A25</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/533/A25&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A25</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/390 [1]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#1</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/390</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/390 [2]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#2</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/390&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/390 [Rloud]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#Rloud</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/390&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/390 [Rquiet]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#Rquiet</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/390&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/540/A106 [1]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#1</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/540/A106</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/540/A106 [2]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#2</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/540/A106&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A106 [dr8gal]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#dr8gal</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A106&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A106 [dr8gr]</TD>
            <TD>SDSS-DR8 groups and clusters of galaxies (Tempel+, 2012)</TD>
            <TD>Galaxy and group/cluster catalogues based on SDSS DR8 data are presented. The tables are also available at http://www.aai.ee/~elmo/dr8groups</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106#dr8gr</TD>
            <TD>2012-06-12T15:51:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A106</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A106&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A106</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/390 [1]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#1</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/390</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/390 [2]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#2</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/390&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/390 [Rloud]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#Rloud</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/390&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/390 [Rquiet]</TD>
            <TD>Optically selected BL Lac objects from SDSS-DR7 (Plotkin+, 2010)</TD>
            <TD>We present a sample of 723 optically selected BL Lac candidates from the Sloan Digital Sky Survey Data Release 7 (SDSS DR7) spectroscopic database encompassing 8250deg^2^ of sky; our sample constitutes one of the largest uniform BL Lac samples yet derived. Each BL Lac candidate has a high-quality SDSS spectrum from which we determine spectroscopic redshifts for ~60% of the objects. Redshift lower limits are estimated for the remaining objects utilizing the lack of host galaxy flux contamination in their optical spectra; we find that objects lacking spectroscopic redshifts are likely at systematically higher redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390#Rquiet</TD>
            <TD>2012-06-12T13:14:25Z</TD>
            <TD>#AGN#BL_Lac_objects#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/390</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/390&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/390</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/533/A25 [1]</TD>
            <TD>VLT/X-shooter observations of PHL293B (Izotov+ 2011)</TD>
            <TD>Fig1.dat - the flux-calibrated and redshift-corrected VLT/X-shooter UV and optical spectrum of the low-metallicity blue compact dwarf galaxy PHL 293B. Fig2.dat - the flux-calibrated and redshift-corrected VLT/X-shooter near-infrared spectrum of the low-metallicity blue compact dwarf galaxy PHL 293B.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A25#1</TD>
            <TD>2011-09-14T21:30:06Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A25</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/533/A25</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A25</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/533/A25 [2]</TD>
            <TD>VLT/X-shooter observations of PHL293B (Izotov+ 2011)</TD>
            <TD>Fig1.dat - the flux-calibrated and redshift-corrected VLT/X-shooter UV and optical spectrum of the low-metallicity blue compact dwarf galaxy PHL 293B. Fig2.dat - the flux-calibrated and redshift-corrected VLT/X-shooter near-infrared spectrum of the low-metallicity blue compact dwarf galaxy PHL 293B.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A25#2</TD>
            <TD>2011-09-14T21:30:06Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/533/A25</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/533/A25&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/533/A25</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/625/6 [1]</TD>
            <TD>Galaxy groups in the DEEP2 Galaxy Redshift Survey (Gerke+, 2005)</TD>
            <TD>The survey consists of four fields on the sky, chosen to lie in zones of low Galactic dust extinction. Three-band (BRI) photometry has been obtained for each of these fields using the CFH12K camera on the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6#1</TD>
            <TD>2011-09-14T20:16:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/625/6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/625/6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/625/6 [2]</TD>
            <TD>Galaxy groups in the DEEP2 Galaxy Redshift Survey (Gerke+, 2005)</TD>
            <TD>The survey consists of four fields on the sky, chosen to lie in zones of low Galactic dust extinction. Three-band (BRI) photometry has been obtained for each of these fields using the CFH12K camera on the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6#2</TD>
            <TD>2011-09-14T20:16:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/625/6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/625/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/625/6 [table3]</TD>
            <TD>Galaxy groups in the DEEP2 Galaxy Redshift Survey (Gerke+, 2005)</TD>
            <TD>The survey consists of four fields on the sky, chosen to lie in zones of low Galactic dust extinction. Three-band (BRI) photometry has been obtained for each of these fields using the CFH12K camera on the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6#table3</TD>
            <TD>2011-09-14T20:16:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/625/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/625/6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/715/572 [1]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#1</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/715/572</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/715/572 [2]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#2</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/715/572&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/715/572 [systems]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#systems</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/715/572&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/715/572 [galaxies]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#galaxies</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/715/572&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/625/6 [1]</TD>
            <TD>Galaxy groups in the DEEP2 Galaxy Redshift Survey (Gerke+, 2005)</TD>
            <TD>The survey consists of four fields on the sky, chosen to lie in zones of low Galactic dust extinction. Three-band (BRI) photometry has been obtained for each of these fields using the CFH12K camera on the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6#1</TD>
            <TD>2011-09-14T20:16:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/625/6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/625/6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/625/6 [2]</TD>
            <TD>Galaxy groups in the DEEP2 Galaxy Redshift Survey (Gerke+, 2005)</TD>
            <TD>The survey consists of four fields on the sky, chosen to lie in zones of low Galactic dust extinction. Three-band (BRI) photometry has been obtained for each of these fields using the CFH12K camera on the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6#2</TD>
            <TD>2011-09-14T20:16:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/625/6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/625/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/625/6 [table3]</TD>
            <TD>Galaxy groups in the DEEP2 Galaxy Redshift Survey (Gerke+, 2005)</TD>
            <TD>The survey consists of four fields on the sky, chosen to lie in zones of low Galactic dust extinction. Three-band (BRI) photometry has been obtained for each of these fields using the CFH12K camera on the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6#table3</TD>
            <TD>2011-09-14T20:16:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/625/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/625/6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/2 [1]</TD>
            <TD>Photodissociation regions in M33 (Heiner+, 2011)</TD>
            <TD>We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-ultraviolet (FUV) photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess FUV emission that reaches the GMC from the OB association and of the excess 21-cm radio HI emission produced after these FUV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs and is especially sensitive to a range of densities well below the critical density for CO(1-0) emission.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2#1</TD>
            <TD>2012-07-14T09:40:34Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/2</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/2 [2]</TD>
            <TD>Photodissociation regions in M33 (Heiner+, 2011)</TD>
            <TD>We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-ultraviolet (FUV) photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess FUV emission that reaches the GMC from the OB association and of the excess 21-cm radio HI emission produced after these FUV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs and is especially sensitive to a range of densities well below the critical density for CO(1-0) emission.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2#2</TD>
            <TD>2012-07-14T09:40:34Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/2 [table5]</TD>
            <TD>Photodissociation regions in M33 (Heiner+, 2011)</TD>
            <TD>We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-ultraviolet (FUV) photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess FUV emission that reaches the GMC from the OB association and of the excess 21-cm radio HI emission produced after these FUV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs and is especially sensitive to a range of densities well below the critical density for CO(1-0) emission.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2#table5</TD>
            <TD>2012-07-14T09:40:34Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/2&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/715/572 [1]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#1</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/715/572</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/715/572 [2]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#2</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/715/572&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/715/572 [systems]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#systems</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/715/572&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/715/572 [galaxies]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#galaxies</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/715/572&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/715/572 [1]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#1</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/715/572</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/715/572 [2]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#2</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/715/572&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/715/572 [systems]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#systems</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/715/572&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/715/572 [galaxies]</TD>
            <TD>GOALS UV and FIR properties (Howell+, 2010)</TD>
            <TD>The GOALS GALEX sample consists of 135 systems observed as part of GALEX Cycle 1 program No. 13 (PI: Mazzarella), GALEX Cycle 5 program No. 38 (PI: Howell), the Nearby Galaxy Survey (NGS), and the All Sky Survey (AIS). All systems have been observed in both the FUV ({lambda}_eff_=1528{AA}) and NUV ({lambda}_eff_=2271{AA}).</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572#galaxies</TD>
            <TD>2012-06-23T17:44:04Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/715/572</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/715/572&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/715/572</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/121/461 [1]</TD>
            <TD>UV variability of Fairall-9 (Recondo-Gonzalez+, 1997)</TD>
            <TD>This is a study of the UV variability of the galaxy Fairall-9 between 1978 and 1991. Table 1 shows the UV continuum fluxes measured in three "line-free" windows centered at 1171, 1400 and 1910 A (observed wavelengths), and corrected for E(B-V)=0.035 extinction. The IUE Fine Error Sensor (FES) counts (optical photometry) are also given in this table, corrected for the same extinction. Tables 10, 11, 12 and 13 show the variability of the components for the main UV lines (Ly{alpha}+NV, SiIV, CIV and MgII). Line profile variability has been used to isolate four gaussian line components, which are sufficient to describe all lines at all levels of brightness in a consistent way: one narrow (i.e. unresolved at the IUE resolution) and three broad components: a central (velocity same as the narrow line), a redshifted (v=3300 km/s) and a blue shifted one (v=-3600 km/s). The Ly{alpha}-NV blend is fitted together in the Ly{alpha} region (Table 10), to account the NV presence (one narrow and one red component). The results for SiIV are shown in Table 11. In CIV (Table 12) have been included a very weak component bluer than the blue component, most likely associated with NIV] 1486. Table 13 shows MgII results.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/121/461#1</TD>
            <TD>2011-09-14T18:19:44Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/121/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/121/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/121/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/121/461 [2]</TD>
            <TD>UV variability of Fairall-9 (Recondo-Gonzalez+, 1997)</TD>
            <TD>This is a study of the UV variability of the galaxy Fairall-9 between 1978 and 1991. Table 1 shows the UV continuum fluxes measured in three "line-free" windows centered at 1171, 1400 and 1910 A (observed wavelengths), and corrected for E(B-V)=0.035 extinction. The IUE Fine Error Sensor (FES) counts (optical photometry) are also given in this table, corrected for the same extinction. Tables 10, 11, 12 and 13 show the variability of the components for the main UV lines (Ly{alpha}+NV, SiIV, CIV and MgII). Line profile variability has been used to isolate four gaussian line components, which are sufficient to describe all lines at all levels of brightness in a consistent way: one narrow (i.e. unresolved at the IUE resolution) and three broad components: a central (velocity same as the narrow line), a redshifted (v=3300 km/s) and a blue shifted one (v=-3600 km/s). The Ly{alpha}-NV blend is fitted together in the Ly{alpha} region (Table 10), to account the NV presence (one narrow and one red component). The results for SiIV are shown in Table 11. In CIV (Table 12) have been included a very weak component bluer than the blue component, most likely associated with NIV] 1486. Table 13 shows MgII results.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/121/461#2</TD>
            <TD>2011-09-14T18:19:44Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/121/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/121/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/121/461</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE143 [1]</TD>
            <TD>Planck Early Release 143-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 143-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke143#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/plancke143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke143&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke143.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE143 [2]</TD>
            <TD>Planck Early Release 143-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 143-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke143#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke143.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE143 [3]</TD>
            <TD>Planck Early Release 143-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 143-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke143#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
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            <TD />
            <TD>ivo://nasa.heasarc/plancke143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke143&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke143.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/104/1349 [1]</TD>
            <TD>Infrared-luminous giants in M32 (Freedman, 1992)</TD>
            <TD>A previously unknown population of very luminous, red, asymptotic-giant-branch stars has been identified as a result of near-infrared (JHK) imaging in the dwarf elliptical galaxy M32. Situated above the tip of the normal first red giant branch, these stars are intrinsically brighter than the most luminous normal giants in old Galactic globular clusters by approximately 2 bolometric magnitudes. Moreover, they are a full bolometric magnitude brighter than the brightest giants observed in our own Galactic bulge. Several possible explanations for this population are examined, including old long-period variables, binary mergers, supermetallicity, and intermediate-age stars. It is suggested that the simplest explanation at present, is that M32 had a star formation episode less than about 5 billion years ago. These stars would then be the evolved extended asymptotic giant branch population resulting from that event (similar to those stars observed in the intermediate-age clusters in the Magellanic Clouds). This population may be similar to that in the M31 bulge, recently observed by Rich and Mould. The detection of a young component in M32 is of particular interest because historically, M32 has been a fiducial galaxy for population synthesis techniques. An understanding of M32 remains crucial for our understanding of distant and more luminous elliptical galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/1349#1</TD>
            <TD>2011-09-14T18:21:02Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/1349</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/104/1349</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/1349</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/104/1349 [2]</TD>
            <TD>Infrared-luminous giants in M32 (Freedman, 1992)</TD>
            <TD>A previously unknown population of very luminous, red, asymptotic-giant-branch stars has been identified as a result of near-infrared (JHK) imaging in the dwarf elliptical galaxy M32. Situated above the tip of the normal first red giant branch, these stars are intrinsically brighter than the most luminous normal giants in old Galactic globular clusters by approximately 2 bolometric magnitudes. Moreover, they are a full bolometric magnitude brighter than the brightest giants observed in our own Galactic bulge. Several possible explanations for this population are examined, including old long-period variables, binary mergers, supermetallicity, and intermediate-age stars. It is suggested that the simplest explanation at present, is that M32 had a star formation episode less than about 5 billion years ago. These stars would then be the evolved extended asymptotic giant branch population resulting from that event (similar to those stars observed in the intermediate-age clusters in the Magellanic Clouds). This population may be similar to that in the M31 bulge, recently observed by Rich and Mould. The detection of a young component in M32 is of particular interest because historically, M32 has been a fiducial galaxy for population synthesis techniques. An understanding of M32 remains crucial for our understanding of distant and more luminous elliptical galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/1349#2</TD>
            <TD>2011-09-14T18:21:02Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/104/1349&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/1349</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE353 [1]</TD>
            <TD>Planck Early Release 353-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 353-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke353#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke353</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke353&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke353.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE353 [2]</TD>
            <TD>Planck Early Release 353-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 353-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke353#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/plancke353</TD>
            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke353&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke353.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE353 [3]</TD>
            <TD>Planck Early Release 353-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 353-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke353#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke353</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke353&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke353.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/104/1349 [1]</TD>
            <TD>Infrared-luminous giants in M32 (Freedman, 1992)</TD>
            <TD>A previously unknown population of very luminous, red, asymptotic-giant-branch stars has been identified as a result of near-infrared (JHK) imaging in the dwarf elliptical galaxy M32. Situated above the tip of the normal first red giant branch, these stars are intrinsically brighter than the most luminous normal giants in old Galactic globular clusters by approximately 2 bolometric magnitudes. Moreover, they are a full bolometric magnitude brighter than the brightest giants observed in our own Galactic bulge. Several possible explanations for this population are examined, including old long-period variables, binary mergers, supermetallicity, and intermediate-age stars. It is suggested that the simplest explanation at present, is that M32 had a star formation episode less than about 5 billion years ago. These stars would then be the evolved extended asymptotic giant branch population resulting from that event (similar to those stars observed in the intermediate-age clusters in the Magellanic Clouds). This population may be similar to that in the M31 bulge, recently observed by Rich and Mould. The detection of a young component in M32 is of particular interest because historically, M32 has been a fiducial galaxy for population synthesis techniques. An understanding of M32 remains crucial for our understanding of distant and more luminous elliptical galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/1349#1</TD>
            <TD>2011-09-14T18:21:02Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/1349</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/104/1349</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/1349</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/104/1349 [2]</TD>
            <TD>Infrared-luminous giants in M32 (Freedman, 1992)</TD>
            <TD>A previously unknown population of very luminous, red, asymptotic-giant-branch stars has been identified as a result of near-infrared (JHK) imaging in the dwarf elliptical galaxy M32. Situated above the tip of the normal first red giant branch, these stars are intrinsically brighter than the most luminous normal giants in old Galactic globular clusters by approximately 2 bolometric magnitudes. Moreover, they are a full bolometric magnitude brighter than the brightest giants observed in our own Galactic bulge. Several possible explanations for this population are examined, including old long-period variables, binary mergers, supermetallicity, and intermediate-age stars. It is suggested that the simplest explanation at present, is that M32 had a star formation episode less than about 5 billion years ago. These stars would then be the evolved extended asymptotic giant branch population resulting from that event (similar to those stars observed in the intermediate-age clusters in the Magellanic Clouds). This population may be similar to that in the M31 bulge, recently observed by Rich and Mould. The detection of a young component in M32 is of particular interest because historically, M32 has been a fiducial galaxy for population synthesis techniques. An understanding of M32 remains crucial for our understanding of distant and more luminous elliptical galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/1349#2</TD>
            <TD>2011-09-14T18:21:02Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
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            <TD>ivo://CDS.VizieR/J/AJ/104/1349</TD>
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/104/1349&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/1349</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/66 [1]</TD>
            <TD>NGC 1560 BVRI CCD photometry (Lee+ 1993)</TD>
            <TD>We present BVRI CCD photometry of ~600 stars in the central region of a resolved spiral galaxy NGC 1560 which is seen almost edge-on, apparently located in the IC 342 group. The V-(B-V) diagram shows a dominant group of significantly reddened blue plume stars consisting of young massive main-sequence and evolved blue supergiant stars. The tip of the blue plume is found to be at V~21 mag and (B-V)~0.4mag. The I-(R-I) diagram shows a large group of red supergiants the brightest of which are extending to I~19.5mag at (R-I)~1.1mag. The logarithmic slope of the V luminosity function of the blue plume stars is 0.69+/-0.10, similar to that for other nearby galaxies. The mean color of the blue plume stars is &lt;(B-V)&gt;=0.25+/-0.03mag. The total reddening, including both foreground and internal reddening, is estimated from the mean color of the blue plume stars, to be E(B-V)=0.40+/-0.10mag, whereas the foreground reddening based on the H I column density and faint galaxy counts is E(B-V)=0.16mag. Combining our results with those in the literature, we have obtained distance estimates using four methods: brightest blue stars [(m-M)_0_=27.11mag], brightest red stars [(m-M)_0_=27.02mag], B-band Tully-Fisher relation [(m-M)_0_=26.96mag], and H-band Tully-Fisher relation [(m-M)_0_=26.86mag]. These four estimates agree very well. Taking the average of these four estimates, we obtain a value for the true distance modulus to NGC 1560, (m-M)_0_=27.0+/-0.1mag, corresponding to a distance of 2.5+/-0.1Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/66#1</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
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            <TD />
            <TD>18-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/66</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/66</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/66</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/66 [2]</TD>
            <TD>NGC 1560 BVRI CCD photometry (Lee+ 1993)</TD>
            <TD>We present BVRI CCD photometry of ~600 stars in the central region of a resolved spiral galaxy NGC 1560 which is seen almost edge-on, apparently located in the IC 342 group. The V-(B-V) diagram shows a dominant group of significantly reddened blue plume stars consisting of young massive main-sequence and evolved blue supergiant stars. The tip of the blue plume is found to be at V~21 mag and (B-V)~0.4mag. The I-(R-I) diagram shows a large group of red supergiants the brightest of which are extending to I~19.5mag at (R-I)~1.1mag. The logarithmic slope of the V luminosity function of the blue plume stars is 0.69+/-0.10, similar to that for other nearby galaxies. The mean color of the blue plume stars is &lt;(B-V)&gt;=0.25+/-0.03mag. The total reddening, including both foreground and internal reddening, is estimated from the mean color of the blue plume stars, to be E(B-V)=0.40+/-0.10mag, whereas the foreground reddening based on the H I column density and faint galaxy counts is E(B-V)=0.16mag. Combining our results with those in the literature, we have obtained distance estimates using four methods: brightest blue stars [(m-M)_0_=27.11mag], brightest red stars [(m-M)_0_=27.02mag], B-band Tully-Fisher relation [(m-M)_0_=26.96mag], and H-band Tully-Fisher relation [(m-M)_0_=26.86mag]. These four estimates agree very well. Taking the average of these four estimates, we obtain a value for the true distance modulus to NGC 1560, (m-M)_0_=27.0+/-0.1mag, corresponding to a distance of 2.5+/-0.1Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/66#2</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/66</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/66&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE353 [1]</TD>
            <TD>Planck Early Release 353-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 353-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke353#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke353&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke353.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE353 [2]</TD>
            <TD>Planck Early Release 353-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 353-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke353#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke353</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke353&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke353.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE353 [3]</TD>
            <TD>Planck Early Release 353-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 353-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke353#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke353</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke353&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke353.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/66 [1]</TD>
            <TD>NGC 1560 BVRI CCD photometry (Lee+ 1993)</TD>
            <TD>We present BVRI CCD photometry of ~600 stars in the central region of a resolved spiral galaxy NGC 1560 which is seen almost edge-on, apparently located in the IC 342 group. The V-(B-V) diagram shows a dominant group of significantly reddened blue plume stars consisting of young massive main-sequence and evolved blue supergiant stars. The tip of the blue plume is found to be at V~21 mag and (B-V)~0.4mag. The I-(R-I) diagram shows a large group of red supergiants the brightest of which are extending to I~19.5mag at (R-I)~1.1mag. The logarithmic slope of the V luminosity function of the blue plume stars is 0.69+/-0.10, similar to that for other nearby galaxies. The mean color of the blue plume stars is &lt;(B-V)&gt;=0.25+/-0.03mag. The total reddening, including both foreground and internal reddening, is estimated from the mean color of the blue plume stars, to be E(B-V)=0.40+/-0.10mag, whereas the foreground reddening based on the H I column density and faint galaxy counts is E(B-V)=0.16mag. Combining our results with those in the literature, we have obtained distance estimates using four methods: brightest blue stars [(m-M)_0_=27.11mag], brightest red stars [(m-M)_0_=27.02mag], B-band Tully-Fisher relation [(m-M)_0_=26.96mag], and H-band Tully-Fisher relation [(m-M)_0_=26.86mag]. These four estimates agree very well. Taking the average of these four estimates, we obtain a value for the true distance modulus to NGC 1560, (m-M)_0_=27.0+/-0.1mag, corresponding to a distance of 2.5+/-0.1Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/66#1</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/66</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/66</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/66</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/66 [2]</TD>
            <TD>NGC 1560 BVRI CCD photometry (Lee+ 1993)</TD>
            <TD>We present BVRI CCD photometry of ~600 stars in the central region of a resolved spiral galaxy NGC 1560 which is seen almost edge-on, apparently located in the IC 342 group. The V-(B-V) diagram shows a dominant group of significantly reddened blue plume stars consisting of young massive main-sequence and evolved blue supergiant stars. The tip of the blue plume is found to be at V~21 mag and (B-V)~0.4mag. The I-(R-I) diagram shows a large group of red supergiants the brightest of which are extending to I~19.5mag at (R-I)~1.1mag. The logarithmic slope of the V luminosity function of the blue plume stars is 0.69+/-0.10, similar to that for other nearby galaxies. The mean color of the blue plume stars is &lt;(B-V)&gt;=0.25+/-0.03mag. The total reddening, including both foreground and internal reddening, is estimated from the mean color of the blue plume stars, to be E(B-V)=0.40+/-0.10mag, whereas the foreground reddening based on the H I column density and faint galaxy counts is E(B-V)=0.16mag. Combining our results with those in the literature, we have obtained distance estimates using four methods: brightest blue stars [(m-M)_0_=27.11mag], brightest red stars [(m-M)_0_=27.02mag], B-band Tully-Fisher relation [(m-M)_0_=26.96mag], and H-band Tully-Fisher relation [(m-M)_0_=26.86mag]. These four estimates agree very well. Taking the average of these four estimates, we obtain a value for the true distance modulus to NGC 1560, (m-M)_0_=27.0+/-0.1mag, corresponding to a distance of 2.5+/-0.1Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/66#2</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/66</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/66&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/66</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE353 [1]</TD>
            <TD>Planck Early Release 353-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 353-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke353#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke353</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke353&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke353.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE353 [2]</TD>
            <TD>Planck Early Release 353-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 353-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke353#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke353</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke353&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke353.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE353 [3]</TD>
            <TD>Planck Early Release 353-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 353-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke353#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke353</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke353&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke353.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/625/6 [1]</TD>
            <TD>Galaxy groups in the DEEP2 Galaxy Redshift Survey (Gerke+, 2005)</TD>
            <TD>The survey consists of four fields on the sky, chosen to lie in zones of low Galactic dust extinction. Three-band (BRI) photometry has been obtained for each of these fields using the CFH12K camera on the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6#1</TD>
            <TD>2011-09-14T20:16:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/625/6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/625/6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/625/6 [2]</TD>
            <TD>Galaxy groups in the DEEP2 Galaxy Redshift Survey (Gerke+, 2005)</TD>
            <TD>The survey consists of four fields on the sky, chosen to lie in zones of low Galactic dust extinction. Three-band (BRI) photometry has been obtained for each of these fields using the CFH12K camera on the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6#2</TD>
            <TD>2011-09-14T20:16:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/625/6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/625/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/625/6 [table3]</TD>
            <TD>Galaxy groups in the DEEP2 Galaxy Redshift Survey (Gerke+, 2005)</TD>
            <TD>The survey consists of four fields on the sky, chosen to lie in zones of low Galactic dust extinction. Three-band (BRI) photometry has been obtained for each of these fields using the CFH12K camera on the Canada-France-Hawaii Telescope (CFHT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6#table3</TD>
            <TD>2011-09-14T20:16:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/625/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/625/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/625/6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/831 [1]</TD>
            <TD>cD clusters of galaxies. I. (Hill+, 1993)</TD>
            <TD>We present the initial results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program is to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar velocity cD galaxies. In this paper we present redshifts for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124. We discuss our data reduction techniques, and compare our derived velocities with previously published values. We find a frequency of emission line galaxies of ~6% in clusters, a factor of 2-3 less than the field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831#1</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/831</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/831</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/831 [2]</TD>
            <TD>cD clusters of galaxies. I. (Hill+, 1993)</TD>
            <TD>We present the initial results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program is to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar velocity cD galaxies. In this paper we present redshifts for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124. We discuss our data reduction techniques, and compare our derived velocities with previously published values. We find a frequency of emission line galaxies of ~6% in clusters, a factor of 2-3 less than the field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831#2</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/831&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/106/831 [tables]</TD>
            <TD>cD clusters of galaxies. I. (Hill+, 1993)</TD>
            <TD>We present the initial results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program is to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar velocity cD galaxies. In this paper we present redshifts for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124. We discuss our data reduction techniques, and compare our derived velocities with previously published values. We find a frequency of emission line galaxies of ~6% in clusters, a factor of 2-3 less than the field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831#tables</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/106/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XDEEP2 [1]</TD>
            <TD>DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog</TD>
            <TD>This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg&lt;sup&gt;2&lt;/sup&gt; DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg&lt;sup&gt;2&lt;/sup&gt; fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (&lt;~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R&lt;sub&gt;AB&lt;/sub&gt; &lt; 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a &lt;~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xdeep2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xdeep2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xdeep2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/xdeep2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XDEEP2 [2]</TD>
            <TD>DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog</TD>
            <TD>This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg&lt;sup&gt;2&lt;/sup&gt; DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg&lt;sup&gt;2&lt;/sup&gt; fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (&lt;~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R&lt;sub&gt;AB&lt;/sub&gt; &lt; 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a &lt;~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xdeep2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xdeep2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xdeep2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/xdeep2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XDEEP2 [3]</TD>
            <TD>DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog</TD>
            <TD>This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg&lt;sup&gt;2&lt;/sup&gt; DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg&lt;sup&gt;2&lt;/sup&gt; fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (&lt;~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R&lt;sub&gt;AB&lt;/sub&gt; &lt; 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a &lt;~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xdeep2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xdeep2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xdeep2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/xdeep2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/2 [1]</TD>
            <TD>Photodissociation regions in M33 (Heiner+, 2011)</TD>
            <TD>We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-ultraviolet (FUV) photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess FUV emission that reaches the GMC from the OB association and of the excess 21-cm radio HI emission produced after these FUV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs and is especially sensitive to a range of densities well below the critical density for CO(1-0) emission.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2#1</TD>
            <TD>2012-07-14T09:40:34Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/2</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/2 [2]</TD>
            <TD>Photodissociation regions in M33 (Heiner+, 2011)</TD>
            <TD>We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-ultraviolet (FUV) photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess FUV emission that reaches the GMC from the OB association and of the excess 21-cm radio HI emission produced after these FUV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs and is especially sensitive to a range of densities well below the critical density for CO(1-0) emission.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2#2</TD>
            <TD>2012-07-14T09:40:34Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/2 [table5]</TD>
            <TD>Photodissociation regions in M33 (Heiner+, 2011)</TD>
            <TD>We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-ultraviolet (FUV) photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess FUV emission that reaches the GMC from the OB association and of the excess 21-cm radio HI emission produced after these FUV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs and is especially sensitive to a range of densities well below the critical density for CO(1-0) emission.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2#table5</TD>
            <TD>2012-07-14T09:40:34Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/2&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/474/783 [1]</TD>
            <TD>Main galaxy groups from SDSS-DR5 (Deng+, 2007)</TD>
            <TD>We investigate the correlations between galaxy properties and environment. From the main galaxy sample of the SDSS Data Release 5, we have extracted 11 163 groups at the linking length R_0_=0.2x({bar}n)^-1/3^=1.97Mpc (where {bar}n is the mean number density of galaxies) by the three-dimensional friends-of-friends (FOF) algorithm, where {bar}n is the mean galaxy density, and compare basic properties of member galaxies of main galaxy groups with those of the main galaxy sample and isolated galaxies in each redshift bin.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783#1</TD>
            <TD>2011-09-14T20:17:06Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/474/783</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/783</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/474/783 [2]</TD>
            <TD>Main galaxy groups from SDSS-DR5 (Deng+, 2007)</TD>
            <TD>We investigate the correlations between galaxy properties and environment. From the main galaxy sample of the SDSS Data Release 5, we have extracted 11 163 groups at the linking length R_0_=0.2x({bar}n)^-1/3^=1.97Mpc (where {bar}n is the mean number density of galaxies) by the three-dimensional friends-of-friends (FOF) algorithm, where {bar}n is the mean galaxy density, and compare basic properties of member galaxies of main galaxy groups with those of the main galaxy sample and isolated galaxies in each redshift bin.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783#2</TD>
            <TD>2011-09-14T20:17:06Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/474/783&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/474/783 [table2]</TD>
            <TD>Main galaxy groups from SDSS-DR5 (Deng+, 2007)</TD>
            <TD>We investigate the correlations between galaxy properties and environment. From the main galaxy sample of the SDSS Data Release 5, we have extracted 11 163 groups at the linking length R_0_=0.2x({bar}n)^-1/3^=1.97Mpc (where {bar}n is the mean number density of galaxies) by the three-dimensional friends-of-friends (FOF) algorithm, where {bar}n is the mean galaxy density, and compare basic properties of member galaxies of main galaxy groups with those of the main galaxy sample and isolated galaxies in each redshift bin.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783#table2</TD>
            <TD>2011-09-14T20:17:06Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/474/783&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XDEEP2 [1]</TD>
            <TD>DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog</TD>
            <TD>This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg&lt;sup&gt;2&lt;/sup&gt; DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg&lt;sup&gt;2&lt;/sup&gt; fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (&lt;~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R&lt;sub&gt;AB&lt;/sub&gt; &lt; 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a &lt;~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xdeep2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xdeep2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xdeep2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/xdeep2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XDEEP2 [2]</TD>
            <TD>DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog</TD>
            <TD>This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg&lt;sup&gt;2&lt;/sup&gt; DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg&lt;sup&gt;2&lt;/sup&gt; fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (&lt;~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R&lt;sub&gt;AB&lt;/sub&gt; &lt; 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a &lt;~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xdeep2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xdeep2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xdeep2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/xdeep2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XDEEP2 [3]</TD>
            <TD>DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog</TD>
            <TD>This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg&lt;sup&gt;2&lt;/sup&gt; DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg&lt;sup&gt;2&lt;/sup&gt; fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (&lt;~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R&lt;sub&gt;AB&lt;/sub&gt; &lt; 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a &lt;~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xdeep2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xdeep2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xdeep2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/xdeep2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/2 [1]</TD>
            <TD>Photodissociation regions in M33 (Heiner+, 2011)</TD>
            <TD>We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-ultraviolet (FUV) photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess FUV emission that reaches the GMC from the OB association and of the excess 21-cm radio HI emission produced after these FUV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs and is especially sensitive to a range of densities well below the critical density for CO(1-0) emission.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2#1</TD>
            <TD>2012-07-14T09:40:34Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/2</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/2 [2]</TD>
            <TD>Photodissociation regions in M33 (Heiner+, 2011)</TD>
            <TD>We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-ultraviolet (FUV) photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess FUV emission that reaches the GMC from the OB association and of the excess 21-cm radio HI emission produced after these FUV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs and is especially sensitive to a range of densities well below the critical density for CO(1-0) emission.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2#2</TD>
            <TD>2012-07-14T09:40:34Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/2 [table5]</TD>
            <TD>Photodissociation regions in M33 (Heiner+, 2011)</TD>
            <TD>We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-ultraviolet (FUV) photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess FUV emission that reaches the GMC from the OB association and of the excess 21-cm radio HI emission produced after these FUV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs and is especially sensitive to a range of densities well below the critical density for CO(1-0) emission.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2#table5</TD>
            <TD>2012-07-14T09:40:34Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/2&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/474/783 [1]</TD>
            <TD>Main galaxy groups from SDSS-DR5 (Deng+, 2007)</TD>
            <TD>We investigate the correlations between galaxy properties and environment. From the main galaxy sample of the SDSS Data Release 5, we have extracted 11 163 groups at the linking length R_0_=0.2x({bar}n)^-1/3^=1.97Mpc (where {bar}n is the mean number density of galaxies) by the three-dimensional friends-of-friends (FOF) algorithm, where {bar}n is the mean galaxy density, and compare basic properties of member galaxies of main galaxy groups with those of the main galaxy sample and isolated galaxies in each redshift bin.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783#1</TD>
            <TD>2011-09-14T20:17:06Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/474/783</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/783</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/474/783 [2]</TD>
            <TD>Main galaxy groups from SDSS-DR5 (Deng+, 2007)</TD>
            <TD>We investigate the correlations between galaxy properties and environment. From the main galaxy sample of the SDSS Data Release 5, we have extracted 11 163 groups at the linking length R_0_=0.2x({bar}n)^-1/3^=1.97Mpc (where {bar}n is the mean number density of galaxies) by the three-dimensional friends-of-friends (FOF) algorithm, where {bar}n is the mean galaxy density, and compare basic properties of member galaxies of main galaxy groups with those of the main galaxy sample and isolated galaxies in each redshift bin.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783#2</TD>
            <TD>2011-09-14T20:17:06Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/474/783&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/474/783 [table2]</TD>
            <TD>Main galaxy groups from SDSS-DR5 (Deng+, 2007)</TD>
            <TD>We investigate the correlations between galaxy properties and environment. From the main galaxy sample of the SDSS Data Release 5, we have extracted 11 163 groups at the linking length R_0_=0.2x({bar}n)^-1/3^=1.97Mpc (where {bar}n is the mean number density of galaxies) by the three-dimensional friends-of-friends (FOF) algorithm, where {bar}n is the mean galaxy density, and compare basic properties of member galaxies of main galaxy groups with those of the main galaxy sample and isolated galaxies in each redshift bin.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783#table2</TD>
            <TD>2011-09-14T20:17:06Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/474/783&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>XDEEP2 [1]</TD>
            <TD>DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog</TD>
            <TD>This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg&lt;sup&gt;2&lt;/sup&gt; DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg&lt;sup&gt;2&lt;/sup&gt; fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (&lt;~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R&lt;sub&gt;AB&lt;/sub&gt; &lt; 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a &lt;~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xdeep2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xdeep2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=xdeep2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/xdeep2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>XDEEP2 [2]</TD>
            <TD>DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog</TD>
            <TD>This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg&lt;sup&gt;2&lt;/sup&gt; DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg&lt;sup&gt;2&lt;/sup&gt; fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (&lt;~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R&lt;sub&gt;AB&lt;/sub&gt; &lt; 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a &lt;~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xdeep2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xdeep2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=xdeep2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/xdeep2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>XDEEP2 [3]</TD>
            <TD>DEEP2 Galaxy Redshift Survey Fields Chandra Point Source Catalog</TD>
            <TD>This table contains the X-ray point-source catalog produced from the Chandra Advanced CCD Imaging Spectrometer (ACIS-I) observations of the combined ~3.2 deg&lt;sup&gt;2&lt;/sup&gt; DEEP2 (XDEEP2) survey fields, which consist of four ~ 0.7 - 1.1 deg&lt;sup&gt;2&lt;/sup&gt; fields. The combined total exposures across all four XDEEP2 fields range from ~ 10 ks to 1.1 Ms. The authors detect X-ray point sources in both the individual ACIS-I observations and the overlapping regions in the merged (stacked) images. They find a total of 2976 unique X-ray sources within the survey area with an expected false-source contamination of ~ 30 sources (&lt;~ 1%). In their paper, the authors present the combined log N-log S distribution of sources detected across the XDEEP2 survey fields and find good agreement with the Extended Chandra Deep Field and Chandra-COSMOS fields to f_(X,0.5-2keV)_ ~ 2 x 10&lt;sup&gt;-16&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;. Given the large survey area of XDEEP2, they additionally place relatively strong constraints on the log N-log S distribution at high fluxes (f_(X,0.5-2keV) ~ 3 x 10&lt;sup&gt;-14&lt;/sup&gt; erg cm&lt;sup&gt;-1&lt;/sup&gt; s&lt;sup&gt;-1&lt;/sup&gt;), and find a small systematic offset (a factor ~ 1.5) toward lower source numbers in this regime, when compared to smaller area surveys. The number counts observed in XDEEP2 are in close agreement with those predicted by X-ray background synthesis models. Additionally, the authors present a Bayesian-style method for associating the X-ray sources with optical photometric counterparts in the DEEP2 catalog (complete to R&lt;sub&gt;AB&lt;/sub&gt; &lt; 25.2) and find that 2126 (~ 71.4% +/- 2.8%) of the 2976 X-ray sources presented here have a secure optical counterpart with a &lt;~ 6% contamination fraction. The present table provides the DEEP2 optical source properties (e.g., magnitude, redshift) as part of the X-ray-optical counterpart catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/xdeep2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/xdeep2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_xdeep2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/xdeep2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/370/468 [1]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#1</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/370/468</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/370/468 [2]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#2</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/370/468&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table7]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table7</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table1]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table1</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table5b]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table5b</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table5a]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table5a</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table6]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table6</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/474/783 [1]</TD>
            <TD>Main galaxy groups from SDSS-DR5 (Deng+, 2007)</TD>
            <TD>We investigate the correlations between galaxy properties and environment. From the main galaxy sample of the SDSS Data Release 5, we have extracted 11 163 groups at the linking length R_0_=0.2x({bar}n)^-1/3^=1.97Mpc (where {bar}n is the mean number density of galaxies) by the three-dimensional friends-of-friends (FOF) algorithm, where {bar}n is the mean galaxy density, and compare basic properties of member galaxies of main galaxy groups with those of the main galaxy sample and isolated galaxies in each redshift bin.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783#1</TD>
            <TD>2011-09-14T20:17:06Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/474/783</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/783</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/474/783 [2]</TD>
            <TD>Main galaxy groups from SDSS-DR5 (Deng+, 2007)</TD>
            <TD>We investigate the correlations between galaxy properties and environment. From the main galaxy sample of the SDSS Data Release 5, we have extracted 11 163 groups at the linking length R_0_=0.2x({bar}n)^-1/3^=1.97Mpc (where {bar}n is the mean number density of galaxies) by the three-dimensional friends-of-friends (FOF) algorithm, where {bar}n is the mean galaxy density, and compare basic properties of member galaxies of main galaxy groups with those of the main galaxy sample and isolated galaxies in each redshift bin.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783#2</TD>
            <TD>2011-09-14T20:17:06Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/474/783&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/783</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/474/783 [table2]</TD>
            <TD>Main galaxy groups from SDSS-DR5 (Deng+, 2007)</TD>
            <TD>We investigate the correlations between galaxy properties and environment. From the main galaxy sample of the SDSS Data Release 5, we have extracted 11 163 groups at the linking length R_0_=0.2x({bar}n)^-1/3^=1.97Mpc (where {bar}n is the mean number density of galaxies) by the three-dimensional friends-of-friends (FOF) algorithm, where {bar}n is the mean galaxy density, and compare basic properties of member galaxies of main galaxy groups with those of the main galaxy sample and isolated galaxies in each redshift bin.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783#table2</TD>
            <TD>2011-09-14T20:17:06Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/783</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/474/783&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/783</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/529/723 [1]</TD>
            <TD>VI photometry of Cepheids (Gibson+, 2000)</TD>
            <TD>Cepheid-based distances to seven Type Ia supernovae (SNe) host galaxies have been derived using the standard Hubble Space Telescope (HST) Key Project on the Extragalactic Distance Scale pipeline. For the first time, this allows for a transparent comparison of data accumulated as part of three different HST projects: the Key Project, the Sandage et al. Type Ia supernovae (SNe) program, and the Tanvir et al. Leo I Group study. Reanalyzing the Tanvir et al. galaxy and six Sandage et al. galaxies, we find a mean (weighted) offset in true distance moduli of 0.12+/-0.07mag; i.e., 6% in linear distance, in the sense of reducing the distance scale or increasing H_0_. Adopting the reddening-corrected Hubble relations of Suntzeff et al. tied to a zero point based on SNe 1990N, 1981B, 1998bu, 1989B, 1972E, and 1960F and the photometric calibration of Hill et al. leads to a Hubble constant of H_0_=68+/-2(random)+/-5(systematic)km/s/Mpc. Adopting the Kennicutt et al. Cepheid period-luminosity-metallicity dependency decreases the inferred H_0_ by 4%. The H0 result from Type Ia SNe is now in good agreement, to within their respective uncertainties, with that from the Tully-Fisher and surface brightness fluctuation relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/529/723#1</TD>
            <TD>2011-09-14T19:27:40Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/529/723</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/529/723</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/529/723</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/529/723 [2]</TD>
            <TD>VI photometry of Cepheids (Gibson+, 2000)</TD>
            <TD>Cepheid-based distances to seven Type Ia supernovae (SNe) host galaxies have been derived using the standard Hubble Space Telescope (HST) Key Project on the Extragalactic Distance Scale pipeline. For the first time, this allows for a transparent comparison of data accumulated as part of three different HST projects: the Key Project, the Sandage et al. Type Ia supernovae (SNe) program, and the Tanvir et al. Leo I Group study. Reanalyzing the Tanvir et al. galaxy and six Sandage et al. galaxies, we find a mean (weighted) offset in true distance moduli of 0.12+/-0.07mag; i.e., 6% in linear distance, in the sense of reducing the distance scale or increasing H_0_. Adopting the reddening-corrected Hubble relations of Suntzeff et al. tied to a zero point based on SNe 1990N, 1981B, 1998bu, 1989B, 1972E, and 1960F and the photometric calibration of Hill et al. leads to a Hubble constant of H_0_=68+/-2(random)+/-5(systematic)km/s/Mpc. Adopting the Kennicutt et al. Cepheid period-luminosity-metallicity dependency decreases the inferred H_0_ by 4%. The H0 result from Type Ia SNe is now in good agreement, to within their respective uncertainties, with that from the Tully-Fisher and surface brightness fluctuation relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/529/723#2</TD>
            <TD>2011-09-14T19:27:40Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/529/723</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/529/723&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/529/723</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/370/468 [1]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#1</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/370/468</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/370/468 [2]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#2</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/370/468&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table7]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table7</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table1]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table1</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table5b]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table5b</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table5a]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table5a</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table6]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table6</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/165/173 [1]</TD>
            <TD>Chandra sources in Galaxy central 150pc (Muno+, 2006)</TD>
            <TD>The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173#1</TD>
            <TD>2011-09-14T20:19:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/165/173</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/173</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/165/173 [2]</TD>
            <TD>Chandra sources in Galaxy central 150pc (Muno+, 2006)</TD>
            <TD>The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173#2</TD>
            <TD>2011-09-14T20:19:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/165/173&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/173</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/165/173 [table2]</TD>
            <TD>Chandra sources in Galaxy central 150pc (Muno+, 2006)</TD>
            <TD>The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173#table2</TD>
            <TD>2011-09-14T20:19:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/165/173&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/173</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/529/723 [1]</TD>
            <TD>VI photometry of Cepheids (Gibson+, 2000)</TD>
            <TD>Cepheid-based distances to seven Type Ia supernovae (SNe) host galaxies have been derived using the standard Hubble Space Telescope (HST) Key Project on the Extragalactic Distance Scale pipeline. For the first time, this allows for a transparent comparison of data accumulated as part of three different HST projects: the Key Project, the Sandage et al. Type Ia supernovae (SNe) program, and the Tanvir et al. Leo I Group study. Reanalyzing the Tanvir et al. galaxy and six Sandage et al. galaxies, we find a mean (weighted) offset in true distance moduli of 0.12+/-0.07mag; i.e., 6% in linear distance, in the sense of reducing the distance scale or increasing H_0_. Adopting the reddening-corrected Hubble relations of Suntzeff et al. tied to a zero point based on SNe 1990N, 1981B, 1998bu, 1989B, 1972E, and 1960F and the photometric calibration of Hill et al. leads to a Hubble constant of H_0_=68+/-2(random)+/-5(systematic)km/s/Mpc. Adopting the Kennicutt et al. Cepheid period-luminosity-metallicity dependency decreases the inferred H_0_ by 4%. The H0 result from Type Ia SNe is now in good agreement, to within their respective uncertainties, with that from the Tully-Fisher and surface brightness fluctuation relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/529/723#1</TD>
            <TD>2011-09-14T19:27:40Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/529/723</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/529/723</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/529/723</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/529/723 [2]</TD>
            <TD>VI photometry of Cepheids (Gibson+, 2000)</TD>
            <TD>Cepheid-based distances to seven Type Ia supernovae (SNe) host galaxies have been derived using the standard Hubble Space Telescope (HST) Key Project on the Extragalactic Distance Scale pipeline. For the first time, this allows for a transparent comparison of data accumulated as part of three different HST projects: the Key Project, the Sandage et al. Type Ia supernovae (SNe) program, and the Tanvir et al. Leo I Group study. Reanalyzing the Tanvir et al. galaxy and six Sandage et al. galaxies, we find a mean (weighted) offset in true distance moduli of 0.12+/-0.07mag; i.e., 6% in linear distance, in the sense of reducing the distance scale or increasing H_0_. Adopting the reddening-corrected Hubble relations of Suntzeff et al. tied to a zero point based on SNe 1990N, 1981B, 1998bu, 1989B, 1972E, and 1960F and the photometric calibration of Hill et al. leads to a Hubble constant of H_0_=68+/-2(random)+/-5(systematic)km/s/Mpc. Adopting the Kennicutt et al. Cepheid period-luminosity-metallicity dependency decreases the inferred H_0_ by 4%. The H0 result from Type Ia SNe is now in good agreement, to within their respective uncertainties, with that from the Tully-Fisher and surface brightness fluctuation relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/529/723#2</TD>
            <TD>2011-09-14T19:27:40Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/529/723</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/529/723&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/529/723</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/370/468 [1]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#1</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/370/468</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/370/468 [2]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#2</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/370/468&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table7]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table7</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table1]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table1</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table5b]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table5b</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table5a]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table5a</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/370/468 [table6]</TD>
            <TD>Variability of gamma-ray sources (Torres+, 2001)</TD>
            <TD>We present a study of 40 low-latitude unidentified 3EG gamma-ray sources which were found to be not positionally coincident with any known class of potential gamma-ray emitters in the Galaxy (Romero et al., 1999A&amp;A...348..868R). We have performed a variability analysis which reveals that many of these 40 sources are variable. These sources have, in addition, a steep mean value of the gamma-ray spectral index, &lt;{Gamma}&gt;=2.41+/-0.2, which, combined with the high level of variability, seems to rule out a pulsar origin. The positional coincidences with uncatalogued candidates to supernova remnants were also studied. Only 7 sources in the sample are spatially coincident with these candidates, a result that is shown to be consistent with the expected level of pure chance association. A complementary search for weak radio counterparts was also conducted and the results are presented as an extensive table containing all significant point-like radio sources within the 40 EGRET fields. We argue that in order to produce the high variability, steep gamma-ray spectra, and absence of strong radio counterparts observed in some of the gamma-ray sources of our sample, a new class of objects should be postulated, and we analyze a viable candidate.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468#table6</TD>
            <TD>2012-09-24T07:14:56Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/370/468</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/370/468&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/370/468</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/165/173 [1]</TD>
            <TD>Chandra sources in Galaxy central 150pc (Muno+, 2006)</TD>
            <TD>The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173#1</TD>
            <TD>2011-09-14T20:19:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/165/173</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/173</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/165/173 [2]</TD>
            <TD>Chandra sources in Galaxy central 150pc (Muno+, 2006)</TD>
            <TD>The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173#2</TD>
            <TD>2011-09-14T20:19:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/165/173&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/173</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/165/173 [table2]</TD>
            <TD>Chandra sources in Galaxy central 150pc (Muno+, 2006)</TD>
            <TD>The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173#table2</TD>
            <TD>2011-09-14T20:19:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/165/173&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/173</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/134/355 [1]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#1</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/134/355</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/134/355 [2]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#2</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/134/355&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/134/355 [table5]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#table5</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/134/355&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/134/355 [table6]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#table6</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/134/355&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/250 [1]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#1</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/250</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/250 [2]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#2</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/250&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/250 [parent]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#parent</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/250&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/250 [photo]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#photo</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/250&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/250 [2dfgrs]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#2dfgrs</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/250&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/165/173 [1]</TD>
            <TD>Chandra sources in Galaxy central 150pc (Muno+, 2006)</TD>
            <TD>The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173#1</TD>
            <TD>2011-09-14T20:19:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/165/173</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/173</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/165/173 [2]</TD>
            <TD>Chandra sources in Galaxy central 150pc (Muno+, 2006)</TD>
            <TD>The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173#2</TD>
            <TD>2011-09-14T20:19:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/165/173&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/173</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/165/173 [table2]</TD>
            <TD>Chandra sources in Galaxy central 150pc (Muno+, 2006)</TD>
            <TD>The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173#table2</TD>
            <TD>2011-09-14T20:19:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/165/173</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/165/173&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/165/173</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/134/355 [1]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#1</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/134/355</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/134/355 [2]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#2</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/134/355&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/134/355 [table5]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#table5</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/134/355&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/134/355 [table6]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#table6</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/134/355&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/831 [1]</TD>
            <TD>cD clusters of galaxies. I. (Hill+, 1993)</TD>
            <TD>We present the initial results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program is to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar velocity cD galaxies. In this paper we present redshifts for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124. We discuss our data reduction techniques, and compare our derived velocities with previously published values. We find a frequency of emission line galaxies of ~6% in clusters, a factor of 2-3 less than the field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831#1</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/831</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/831</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/831 [2]</TD>
            <TD>cD clusters of galaxies. I. (Hill+, 1993)</TD>
            <TD>We present the initial results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program is to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar velocity cD galaxies. In this paper we present redshifts for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124. We discuss our data reduction techniques, and compare our derived velocities with previously published values. We find a frequency of emission line galaxies of ~6% in clusters, a factor of 2-3 less than the field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831#2</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/831&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/106/831 [tables]</TD>
            <TD>cD clusters of galaxies. I. (Hill+, 1993)</TD>
            <TD>We present the initial results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program is to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar velocity cD galaxies. In this paper we present redshifts for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124. We discuss our data reduction techniques, and compare our derived velocities with previously published values. We find a frequency of emission line galaxies of ~6% in clusters, a factor of 2-3 less than the field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831#tables</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/106/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/831</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/134/355 [1]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#1</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/134/355</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/134/355 [2]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#2</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/134/355&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/134/355 [table5]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#table5</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/134/355&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/134/355 [table6]</TD>
            <TD>Radio galaxies in 18 nearby Abell clusters (Miller+, 2001)</TD>
            <TD>We report on the use of the NRAO VLA Sky Survey (NVSS) to identify radio galaxies in 18 nearby Abell clusters. The listings extend from the cores of the clusters out to radii of 3Mpc (H_0_=75km/s/Mpc), which corresponds to 1.5 Abell radii and approximately 4 orders of magnitude in galaxy density. To create a truly useful catalog, we have collected optical spectra for nearly all of the galaxies lacking public velocity measurements. Consequently, we are able to discriminate between those radio galaxies seen in projection on the cluster and those that are in actuality cluster members. The resulting catalog consists of 329 cluster radio galaxies plus 138 galaxies deemed foreground or background objects, and new velocity measurements are reported for 273 of these radio galaxies. The motivation for the catalog is the study of galaxy evolution in the cluster environment. The radio luminosity function is a powerful tool in the identification of active galaxies, as it is dominated by star-forming galaxies at intermediate luminosities and active galactic nuclei (AGNs) at higher luminosities. The flux limit of the NVSS allows us to identify AGNs and star-forming galaxies down to star formation rates less than 1M_{sun}_/yr. This sensitivity, coupled with the all-sky nature of the NVSS, allows us to produce a catalog of considerable depth and breadth. In addition to these data, we report detected infrared fluxes and upper limits obtained from IRAS data. It is hoped that this database will prove useful in a number of potential studies of the effect of environment on galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355#table6</TD>
            <TD>2011-09-14T19:56:44Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/134/355</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/134/355&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/134/355</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/831 [1]</TD>
            <TD>cD clusters of galaxies. I. (Hill+, 1993)</TD>
            <TD>We present the initial results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program is to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar velocity cD galaxies. In this paper we present redshifts for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124. We discuss our data reduction techniques, and compare our derived velocities with previously published values. We find a frequency of emission line galaxies of ~6% in clusters, a factor of 2-3 less than the field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831#1</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/831</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/831</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/831 [2]</TD>
            <TD>cD clusters of galaxies. I. (Hill+, 1993)</TD>
            <TD>We present the initial results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program is to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar velocity cD galaxies. In this paper we present redshifts for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124. We discuss our data reduction techniques, and compare our derived velocities with previously published values. We find a frequency of emission line galaxies of ~6% in clusters, a factor of 2-3 less than the field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831#2</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/831&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/106/831 [tables]</TD>
            <TD>cD clusters of galaxies. I. (Hill+, 1993)</TD>
            <TD>We present the initial results of a spectroscopic study of a sample of cD galaxy clusters. The goal of this program is to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar velocity cD galaxies. In this paper we present redshifts for 611 galaxies in the fields of the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124. We discuss our data reduction techniques, and compare our derived velocities with previously published values. We find a frequency of emission line galaxies of ~6% in clusters, a factor of 2-3 less than the field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831#tables</TD>
            <TD>2011-09-14T18:21:32Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Oct-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/106/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/831</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/476/151 [1]</TD>
            <TD>SWIRE ELAIS-S1 IR-peak galaxy IR fluxes (Berta+, 2007)</TD>
            <TD>Main data on the IR-peakers sample in the SWIRE ELAIS-S1 field. For each IR-peak galaxy, we report R band magnitude (AB units, from the ESIS survey, Berta et al., 2006A&amp;A...451..881B), Spitzer SWIRE fluxes (Lonsdale et al., 2003PASP..115..897L, 2004ApJS..154...54L), photometric redshift (based on Hyper-z fit, Bolzonella et al., 2000A&amp;A...363..476B), the stellar mass and its minimal-maximal range. The stellar mass estimate is based on mixed stellar population (MSP) synthesis (Berta et al., 2004A&amp;A...418..913B). The minimal and maximal stellar masses are obtained by exploring the SFH-extinction parameter space with the Adaptive Simulated Annealing algorithm (Ingber et al., 2001, http://www.ingber.com/asa01_lecture.pdf). See the paper associated to these data for more details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151#1</TD>
            <TD>2011-09-14T20:21:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/476/151</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/476/151</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/476/151 [2]</TD>
            <TD>SWIRE ELAIS-S1 IR-peak galaxy IR fluxes (Berta+, 2007)</TD>
            <TD>Main data on the IR-peakers sample in the SWIRE ELAIS-S1 field. For each IR-peak galaxy, we report R band magnitude (AB units, from the ESIS survey, Berta et al., 2006A&amp;A...451..881B), Spitzer SWIRE fluxes (Lonsdale et al., 2003PASP..115..897L, 2004ApJS..154...54L), photometric redshift (based on Hyper-z fit, Bolzonella et al., 2000A&amp;A...363..476B), the stellar mass and its minimal-maximal range. The stellar mass estimate is based on mixed stellar population (MSP) synthesis (Berta et al., 2004A&amp;A...418..913B). The minimal and maximal stellar masses are obtained by exploring the SFH-extinction parameter space with the Adaptive Simulated Annealing algorithm (Ingber et al., 2001, http://www.ingber.com/asa01_lecture.pdf). See the paper associated to these data for more details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151#2</TD>
            <TD>2011-09-14T20:21:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/476/151&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/476/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/476/151 [table]</TD>
            <TD>SWIRE ELAIS-S1 IR-peak galaxy IR fluxes (Berta+, 2007)</TD>
            <TD>Main data on the IR-peakers sample in the SWIRE ELAIS-S1 field. For each IR-peak galaxy, we report R band magnitude (AB units, from the ESIS survey, Berta et al., 2006A&amp;A...451..881B), Spitzer SWIRE fluxes (Lonsdale et al., 2003PASP..115..897L, 2004ApJS..154...54L), photometric redshift (based on Hyper-z fit, Bolzonella et al., 2000A&amp;A...363..476B), the stellar mass and its minimal-maximal range. The stellar mass estimate is based on mixed stellar population (MSP) synthesis (Berta et al., 2004A&amp;A...418..913B). The minimal and maximal stellar masses are obtained by exploring the SFH-extinction parameter space with the Adaptive Simulated Annealing algorithm (Ingber et al., 2001, http://www.ingber.com/asa01_lecture.pdf). See the paper associated to these data for more details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151#table</TD>
            <TD>2011-09-14T20:21:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/476/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/476/151</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/430/911 [1]</TD>
            <TD>Expansive components in HII regions (Relano+, 2005)</TD>
            <TD>The galaxies NGC 3359, NGC 6951 and NGC 1530 were observed with the TAURUS-II Fabry-Perot interferometer at the 4.2m William Herschel Telescope (WHT) on La Palma. The data reduction for each galaxy is described respectively in Rozas et al. (2000A&amp;A...354..823R, Cat. J/A+A/354/823&gt;) for NGC 3359, in Rozas et al. (2002A&amp;A...386...42R) for NGC 6951 and in Zurita et al. (2004A&amp;A...413...73Z) for NGC 1530.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/911#1</TD>
            <TD>2011-09-14T19:56:58Z</TD>
            <TD>#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/911</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/430/911</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/911</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/430/911 [2]</TD>
            <TD>Expansive components in HII regions (Relano+, 2005)</TD>
            <TD>The galaxies NGC 3359, NGC 6951 and NGC 1530 were observed with the TAURUS-II Fabry-Perot interferometer at the 4.2m William Herschel Telescope (WHT) on La Palma. The data reduction for each galaxy is described respectively in Rozas et al. (2000A&amp;A...354..823R, Cat. J/A+A/354/823&gt;) for NGC 3359, in Rozas et al. (2002A&amp;A...386...42R) for NGC 6951 and in Zurita et al. (2004A&amp;A...413...73Z) for NGC 1530.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/911#2</TD>
            <TD>2011-09-14T19:56:58Z</TD>
            <TD>#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/911</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/430/911&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/911</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/2087 [1]</TD>
            <TD>Globular Clusters in Ellipticals (Ajhar+ 1994)</TD>
            <TD>Tables 3-12 contain the positions, radial distances, magnitudes, and colors of objects located for each galaxy. Only objects brighter than R=22 and classified by DOPHOT as point sources in the V, R, and I images are included in the tables. The positions are in arcseconds and are relative to the center of the galaxy such that +x is to the west and +y is to the north. The magnitude and colors of each object have been corrected for reddening and absorption according to Equation (1) of the paper and following the values listed in Table 2 of the paper. Please use those values to recover the actual apparent magnitudes of these objects if desired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/2087#1</TD>
            <TD>2011-09-14T18:21:45Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/2087</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/2087</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/2087</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/2087 [2]</TD>
            <TD>Globular Clusters in Ellipticals (Ajhar+ 1994)</TD>
            <TD>Tables 3-12 contain the positions, radial distances, magnitudes, and colors of objects located for each galaxy. Only objects brighter than R=22 and classified by DOPHOT as point sources in the V, R, and I images are included in the tables. The positions are in arcseconds and are relative to the center of the galaxy such that +x is to the west and +y is to the north. The magnitude and colors of each object have been corrected for reddening and absorption according to Equation (1) of the paper and following the values listed in Table 2 of the paper. Please use those values to recover the actual apparent magnitudes of these objects if desired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/2087#2</TD>
            <TD>2011-09-14T18:21:45Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/2087</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/2087&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/2087</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/250 [1]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#1</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/250</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/250 [2]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#2</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/250&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/250 [parent]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#parent</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/250&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/250 [photo]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#photo</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/250&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/250 [2dfgrs]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#2dfgrs</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/250&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/430/911 [1]</TD>
            <TD>Expansive components in HII regions (Relano+, 2005)</TD>
            <TD>The galaxies NGC 3359, NGC 6951 and NGC 1530 were observed with the TAURUS-II Fabry-Perot interferometer at the 4.2m William Herschel Telescope (WHT) on La Palma. The data reduction for each galaxy is described respectively in Rozas et al. (2000A&amp;A...354..823R, Cat. J/A+A/354/823&gt;) for NGC 3359, in Rozas et al. (2002A&amp;A...386...42R) for NGC 6951 and in Zurita et al. (2004A&amp;A...413...73Z) for NGC 1530.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/911#1</TD>
            <TD>2011-09-14T19:56:58Z</TD>
            <TD>#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/911</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/430/911</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/911</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/430/911 [2]</TD>
            <TD>Expansive components in HII regions (Relano+, 2005)</TD>
            <TD>The galaxies NGC 3359, NGC 6951 and NGC 1530 were observed with the TAURUS-II Fabry-Perot interferometer at the 4.2m William Herschel Telescope (WHT) on La Palma. The data reduction for each galaxy is described respectively in Rozas et al. (2000A&amp;A...354..823R, Cat. J/A+A/354/823&gt;) for NGC 3359, in Rozas et al. (2002A&amp;A...386...42R) for NGC 6951 and in Zurita et al. (2004A&amp;A...413...73Z) for NGC 1530.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/911#2</TD>
            <TD>2011-09-14T19:56:58Z</TD>
            <TD>#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/911</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/430/911&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/911</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/2087 [1]</TD>
            <TD>Globular Clusters in Ellipticals (Ajhar+ 1994)</TD>
            <TD>Tables 3-12 contain the positions, radial distances, magnitudes, and colors of objects located for each galaxy. Only objects brighter than R=22 and classified by DOPHOT as point sources in the V, R, and I images are included in the tables. The positions are in arcseconds and are relative to the center of the galaxy such that +x is to the west and +y is to the north. The magnitude and colors of each object have been corrected for reddening and absorption according to Equation (1) of the paper and following the values listed in Table 2 of the paper. Please use those values to recover the actual apparent magnitudes of these objects if desired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/2087#1</TD>
            <TD>2011-09-14T18:21:45Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/2087</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/2087</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/2087</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/2087 [2]</TD>
            <TD>Globular Clusters in Ellipticals (Ajhar+ 1994)</TD>
            <TD>Tables 3-12 contain the positions, radial distances, magnitudes, and colors of objects located for each galaxy. Only objects brighter than R=22 and classified by DOPHOT as point sources in the V, R, and I images are included in the tables. The positions are in arcseconds and are relative to the center of the galaxy such that +x is to the west and +y is to the north. The magnitude and colors of each object have been corrected for reddening and absorption according to Equation (1) of the paper and following the values listed in Table 2 of the paper. Please use those values to recover the actual apparent magnitudes of these objects if desired.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/2087#2</TD>
            <TD>2011-09-14T18:21:45Z</TD>
            <TD>#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/2087</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/2087&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/2087</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/631/85 [1]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#1</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/631/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/631/85 [2]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#2</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/85 [tablea]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#tablea</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/85 [tablec]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#tablec</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/85 [tableb]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#tableb</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2166 [1]</TD>
            <TD>Variables in Sextans dSph galaxy (Mateo+ 1995)</TD>
            <TD>We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166#1</TD>
            <TD>2011-09-14T18:22:13Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2166</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2166</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2166 [2]</TD>
            <TD>Variables in Sextans dSph galaxy (Mateo+ 1995)</TD>
            <TD>We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166#2</TD>
            <TD>2011-09-14T18:22:13Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2166&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2166</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2166 [table10]</TD>
            <TD>Variables in Sextans dSph galaxy (Mateo+ 1995)</TD>
            <TD>We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166#table10</TD>
            <TD>2011-09-14T18:22:13Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2166&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2166</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/631/85 [1]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#1</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/631/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/631/85 [2]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#2</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/85 [tablea]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#tablea</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/85 [tablec]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#tablec</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/85 [tableb]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#tableb</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/476/151 [1]</TD>
            <TD>SWIRE ELAIS-S1 IR-peak galaxy IR fluxes (Berta+, 2007)</TD>
            <TD>Main data on the IR-peakers sample in the SWIRE ELAIS-S1 field. For each IR-peak galaxy, we report R band magnitude (AB units, from the ESIS survey, Berta et al., 2006A&amp;A...451..881B), Spitzer SWIRE fluxes (Lonsdale et al., 2003PASP..115..897L, 2004ApJS..154...54L), photometric redshift (based on Hyper-z fit, Bolzonella et al., 2000A&amp;A...363..476B), the stellar mass and its minimal-maximal range. The stellar mass estimate is based on mixed stellar population (MSP) synthesis (Berta et al., 2004A&amp;A...418..913B). The minimal and maximal stellar masses are obtained by exploring the SFH-extinction parameter space with the Adaptive Simulated Annealing algorithm (Ingber et al., 2001, http://www.ingber.com/asa01_lecture.pdf). See the paper associated to these data for more details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151#1</TD>
            <TD>2011-09-14T20:21:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/476/151</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/476/151</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/476/151 [2]</TD>
            <TD>SWIRE ELAIS-S1 IR-peak galaxy IR fluxes (Berta+, 2007)</TD>
            <TD>Main data on the IR-peakers sample in the SWIRE ELAIS-S1 field. For each IR-peak galaxy, we report R band magnitude (AB units, from the ESIS survey, Berta et al., 2006A&amp;A...451..881B), Spitzer SWIRE fluxes (Lonsdale et al., 2003PASP..115..897L, 2004ApJS..154...54L), photometric redshift (based on Hyper-z fit, Bolzonella et al., 2000A&amp;A...363..476B), the stellar mass and its minimal-maximal range. The stellar mass estimate is based on mixed stellar population (MSP) synthesis (Berta et al., 2004A&amp;A...418..913B). The minimal and maximal stellar masses are obtained by exploring the SFH-extinction parameter space with the Adaptive Simulated Annealing algorithm (Ingber et al., 2001, http://www.ingber.com/asa01_lecture.pdf). See the paper associated to these data for more details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151#2</TD>
            <TD>2011-09-14T20:21:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/476/151&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/476/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/476/151 [table]</TD>
            <TD>SWIRE ELAIS-S1 IR-peak galaxy IR fluxes (Berta+, 2007)</TD>
            <TD>Main data on the IR-peakers sample in the SWIRE ELAIS-S1 field. For each IR-peak galaxy, we report R band magnitude (AB units, from the ESIS survey, Berta et al., 2006A&amp;A...451..881B), Spitzer SWIRE fluxes (Lonsdale et al., 2003PASP..115..897L, 2004ApJS..154...54L), photometric redshift (based on Hyper-z fit, Bolzonella et al., 2000A&amp;A...363..476B), the stellar mass and its minimal-maximal range. The stellar mass estimate is based on mixed stellar population (MSP) synthesis (Berta et al., 2004A&amp;A...418..913B). The minimal and maximal stellar masses are obtained by exploring the SFH-extinction parameter space with the Adaptive Simulated Annealing algorithm (Ingber et al., 2001, http://www.ingber.com/asa01_lecture.pdf). See the paper associated to these data for more details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151#table</TD>
            <TD>2011-09-14T20:21:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/476/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/476/151</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/631/85 [1]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#1</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/631/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/631/85 [2]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#2</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/85 [tablea]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#tablea</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/85 [tablec]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#tablec</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/85 [tableb]</TD>
            <TD>Galaxy morphologies in the Hubble UDF (Elmegreen+, 2005)</TD>
            <TD>UDF images were obtained with the Hubble Space Telescope Advanced Camera for Surveys (HST ACS) by S. Beckwith and coworkers in 2004 and are available on the Space Telescope Science Institute (STScI) archive. The images are 10500x10500pix with a scale of 0.03"/pix (315"x315") in four filters: F435W (B band; 134880s exposure), F606W (V band; 135320s), F775W (i band; 347110s), and F850LP (z band_; 346620s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85#tableb</TD>
            <TD>2011-09-14T19:57:47Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/85</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/85&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/117/227 [1]</TD>
            <TD>Properties of 101 galaxies from the NFGS (Kewley+, 2005)</TD>
            <TD>We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M_{sun}_/yr, metallicities in the range 7.9&lt;~log(O/H)+12&lt;~9.0, and reddening of 0&lt;~A(V)&lt;~3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227#1</TD>
            <TD>2011-09-14T19:59:08Z</TD>
            <TD>#Abundances#Extinction#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/117/227</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/227</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/117/227 [2]</TD>
            <TD>Properties of 101 galaxies from the NFGS (Kewley+, 2005)</TD>
            <TD>We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M_{sun}_/yr, metallicities in the range 7.9&lt;~log(O/H)+12&lt;~9.0, and reddening of 0&lt;~A(V)&lt;~3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227#2</TD>
            <TD>2011-09-14T19:59:08Z</TD>
            <TD>#Abundances#Extinction#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/117/227&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/227 [table1]</TD>
            <TD>Properties of 101 galaxies from the NFGS (Kewley+, 2005)</TD>
            <TD>We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M_{sun}_/yr, metallicities in the range 7.9&lt;~log(O/H)+12&lt;~9.0, and reddening of 0&lt;~A(V)&lt;~3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227#table1</TD>
            <TD>2011-09-14T19:59:08Z</TD>
            <TD>#Abundances#Extinction#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/227</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/117/227 [1]</TD>
            <TD>Properties of 101 galaxies from the NFGS (Kewley+, 2005)</TD>
            <TD>We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M_{sun}_/yr, metallicities in the range 7.9&lt;~log(O/H)+12&lt;~9.0, and reddening of 0&lt;~A(V)&lt;~3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227#1</TD>
            <TD>2011-09-14T19:59:08Z</TD>
            <TD>#Abundances#Extinction#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/117/227</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/227</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/117/227 [2]</TD>
            <TD>Properties of 101 galaxies from the NFGS (Kewley+, 2005)</TD>
            <TD>We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M_{sun}_/yr, metallicities in the range 7.9&lt;~log(O/H)+12&lt;~9.0, and reddening of 0&lt;~A(V)&lt;~3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227#2</TD>
            <TD>2011-09-14T19:59:08Z</TD>
            <TD>#Abundances#Extinction#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/117/227&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/227 [table1]</TD>
            <TD>Properties of 101 galaxies from the NFGS (Kewley+, 2005)</TD>
            <TD>We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M_{sun}_/yr, metallicities in the range 7.9&lt;~log(O/H)+12&lt;~9.0, and reddening of 0&lt;~A(V)&lt;~3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227#table1</TD>
            <TD>2011-09-14T19:59:08Z</TD>
            <TD>#Abundances#Extinction#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/227</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/117/227 [1]</TD>
            <TD>Properties of 101 galaxies from the NFGS (Kewley+, 2005)</TD>
            <TD>We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M_{sun}_/yr, metallicities in the range 7.9&lt;~log(O/H)+12&lt;~9.0, and reddening of 0&lt;~A(V)&lt;~3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227#1</TD>
            <TD>2011-09-14T19:59:08Z</TD>
            <TD>#Abundances#Extinction#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/117/227</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/227</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/117/227 [2]</TD>
            <TD>Properties of 101 galaxies from the NFGS (Kewley+, 2005)</TD>
            <TD>We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M_{sun}_/yr, metallicities in the range 7.9&lt;~log(O/H)+12&lt;~9.0, and reddening of 0&lt;~A(V)&lt;~3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227#2</TD>
            <TD>2011-09-14T19:59:08Z</TD>
            <TD>#Abundances#Extinction#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/117/227&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/227</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/117/227 [table1]</TD>
            <TD>Properties of 101 galaxies from the NFGS (Kewley+, 2005)</TD>
            <TD>We use 101 galaxies selected from the Nearby Field Galaxy Survey to investigate the effect of aperture size on the star formation rate, metallicity, and reddening determinations for galaxies. Our sample includes galaxies of all Hubble types except ellipticals with global star formation rates (SFRs) ranging from 0.01 to 100M_{sun}_/yr, metallicities in the range 7.9&lt;~log(O/H)+12&lt;~9.0, and reddening of 0&lt;~A(V)&lt;~3.3. We compare the SFR, metallicity, and reddening derived from nuclear spectra to those derived from integrated spectra.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227#table1</TD>
            <TD>2011-09-14T19:59:08Z</TD>
            <TD>#Abundances#Extinction#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2006</TD>
            <TD>ivo://CDS.VizieR/J/PASP/117/227</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/117/227&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/117/227</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/430/19 [1]</TD>
            <TD>VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)</TD>
            <TD>The optical observations of Abell 3921 were carried out using the Wide Field Imager (WFI) mounted at the Cassegrain focus of the MPG/ESO 2.2m telescope at La Silla observatory. The data, including photometric calibration images, were obtained between August 20th and 23rd, 2001. Positions, V, R, I-band magnitudes (AB magnitude system), radial velocity measurements, and equivalent widths of [OII]3727{AA} and H{delta} lines of 239 objects in the central region of the galaxy cluster Abell 3921 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19#1</TD>
            <TD>2011-09-14T19:59:25Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/430/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/430/19 [2]</TD>
            <TD>VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)</TD>
            <TD>The optical observations of Abell 3921 were carried out using the Wide Field Imager (WFI) mounted at the Cassegrain focus of the MPG/ESO 2.2m telescope at La Silla observatory. The data, including photometric calibration images, were obtained between August 20th and 23rd, 2001. Positions, V, R, I-band magnitudes (AB magnitude system), radial velocity measurements, and equivalent widths of [OII]3727{AA} and H{delta} lines of 239 objects in the central region of the galaxy cluster Abell 3921 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19#2</TD>
            <TD>2011-09-14T19:59:25Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/430/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/430/19 [tablea]</TD>
            <TD>VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)</TD>
            <TD>The optical observations of Abell 3921 were carried out using the Wide Field Imager (WFI) mounted at the Cassegrain focus of the MPG/ESO 2.2m telescope at La Silla observatory. The data, including photometric calibration images, were obtained between August 20th and 23rd, 2001. Positions, V, R, I-band magnitudes (AB magnitude system), radial velocity measurements, and equivalent widths of [OII]3727{AA} and H{delta} lines of 239 objects in the central region of the galaxy cluster Abell 3921 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19#tablea</TD>
            <TD>2011-09-14T19:59:25Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/430/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/430/19 [1]</TD>
            <TD>VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)</TD>
            <TD>The optical observations of Abell 3921 were carried out using the Wide Field Imager (WFI) mounted at the Cassegrain focus of the MPG/ESO 2.2m telescope at La Silla observatory. The data, including photometric calibration images, were obtained between August 20th and 23rd, 2001. Positions, V, R, I-band magnitudes (AB magnitude system), radial velocity measurements, and equivalent widths of [OII]3727{AA} and H{delta} lines of 239 objects in the central region of the galaxy cluster Abell 3921 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19#1</TD>
            <TD>2011-09-14T19:59:25Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/430/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/430/19 [2]</TD>
            <TD>VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)</TD>
            <TD>The optical observations of Abell 3921 were carried out using the Wide Field Imager (WFI) mounted at the Cassegrain focus of the MPG/ESO 2.2m telescope at La Silla observatory. The data, including photometric calibration images, were obtained between August 20th and 23rd, 2001. Positions, V, R, I-band magnitudes (AB magnitude system), radial velocity measurements, and equivalent widths of [OII]3727{AA} and H{delta} lines of 239 objects in the central region of the galaxy cluster Abell 3921 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19#2</TD>
            <TD>2011-09-14T19:59:25Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/430/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/430/19 [tablea]</TD>
            <TD>VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)</TD>
            <TD>The optical observations of Abell 3921 were carried out using the Wide Field Imager (WFI) mounted at the Cassegrain focus of the MPG/ESO 2.2m telescope at La Silla observatory. The data, including photometric calibration images, were obtained between August 20th and 23rd, 2001. Positions, V, R, I-band magnitudes (AB magnitude system), radial velocity measurements, and equivalent widths of [OII]3727{AA} and H{delta} lines of 239 objects in the central region of the galaxy cluster Abell 3921 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19#tablea</TD>
            <TD>2011-09-14T19:59:25Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/430/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/430/19 [1]</TD>
            <TD>VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)</TD>
            <TD>The optical observations of Abell 3921 were carried out using the Wide Field Imager (WFI) mounted at the Cassegrain focus of the MPG/ESO 2.2m telescope at La Silla observatory. The data, including photometric calibration images, were obtained between August 20th and 23rd, 2001. Positions, V, R, I-band magnitudes (AB magnitude system), radial velocity measurements, and equivalent widths of [OII]3727{AA} and H{delta} lines of 239 objects in the central region of the galaxy cluster Abell 3921 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19#1</TD>
            <TD>2011-09-14T19:59:25Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/430/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/430/19 [2]</TD>
            <TD>VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)</TD>
            <TD>The optical observations of Abell 3921 were carried out using the Wide Field Imager (WFI) mounted at the Cassegrain focus of the MPG/ESO 2.2m telescope at La Silla observatory. The data, including photometric calibration images, were obtained between August 20th and 23rd, 2001. Positions, V, R, I-band magnitudes (AB magnitude system), radial velocity measurements, and equivalent widths of [OII]3727{AA} and H{delta} lines of 239 objects in the central region of the galaxy cluster Abell 3921 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19#2</TD>
            <TD>2011-09-14T19:59:25Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/430/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/430/19 [tablea]</TD>
            <TD>VRI photometry of Abell 3921 galaxies (Ferrari+, 2005)</TD>
            <TD>The optical observations of Abell 3921 were carried out using the Wide Field Imager (WFI) mounted at the Cassegrain focus of the MPG/ESO 2.2m telescope at La Silla observatory. The data, including photometric calibration images, were obtained between August 20th and 23rd, 2001. Positions, V, R, I-band magnitudes (AB magnitude system), radial velocity measurements, and equivalent widths of [OII]3727{AA} and H{delta} lines of 239 objects in the central region of the galaxy cluster Abell 3921 are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19#tablea</TD>
            <TD>2011-09-14T19:59:25Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/430/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/430/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/430/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/22 [1]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#1</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/22</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/22 [2]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#2</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/22&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/22 [table1]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#table1</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/22 [table3]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#table3</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/22 [1]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#1</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/22</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/22 [2]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#2</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/22&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/22 [table1]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#table1</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/22 [table3]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#table3</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/199/22 [1]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#1</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/199/22</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/199/22 [2]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#2</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/199/22&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/22 [table1]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#table1</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/199/22 [table3]</TD>
            <TD>UV to far-IR photometry of galaxies (Hernandez-Fernandez+, 2012)</TD>
            <TD>The cluster sample is observed in a sky area which is delimited by the intersection of observed sky areas of SDSS (DR6, Adelman-McCarthy et al. 2008, Cat. II/282) and Galaxy Evolution Explorer (GALEX; Martin et al. 2005ApJ...619L...1M) surveys. Both surveys are incomplete (at the moment of sample definition, 2008 March) and have smaller observed sky areas than the other ended surveys, Two Micron All Sky Survey (2MASS, Cat. II/246) and Infrared Astronomical Satellite (IRAS; Neugebauer et al. 1984ApJ...278L...1N; Cat. II/125 and II/156). In order to sample a broad range of environments, we select galaxy clusters observed by these surveys up to regions several virial radius beyond the virial region.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22#table3</TD>
            <TD>2012-06-03T22:24:23Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/199/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/199/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/199/22</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/380/1098 [1]</TD>
            <TD>UV-upturn of elliptical galaxies model (Han+, 2007)</TD>
            <TD>A long-standing problem in the study of elliptical galaxies is the far-ultraviolet (FUV) excess in their spectra (also known as UV-upturn, UV rising-branch, UV rising flux, or UVX). While it is now clear that this UV excess is caused by an old population of hot helium-burning stars without large hydrogen-rich envelopes. We have developed an evolutionary population synthesis (EPS) model for the FUV excess of elliptical galaxies based on the binary model of Han et al. (2002MNRAS.336..449H and 2003MNRAS.341..669H) for the formation of hot subdwarfs in our Galaxy. We give the colour evolution of a simple stellar population (SSP) (including binaries) of 10^10^M_{sun}_ for our standard simulation set. We have also compiled a file for the SED evolution, in which the SEDs without binary interactions are also supplied.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/1098#1</TD>
            <TD>2011-09-14T20:16:43Z</TD>
            <TD>#Photometry#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/1098</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/380/1098</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/1098</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/380/1098 [2]</TD>
            <TD>UV-upturn of elliptical galaxies model (Han+, 2007)</TD>
            <TD>A long-standing problem in the study of elliptical galaxies is the far-ultraviolet (FUV) excess in their spectra (also known as UV-upturn, UV rising-branch, UV rising flux, or UVX). While it is now clear that this UV excess is caused by an old population of hot helium-burning stars without large hydrogen-rich envelopes. We have developed an evolutionary population synthesis (EPS) model for the FUV excess of elliptical galaxies based on the binary model of Han et al. (2002MNRAS.336..449H and 2003MNRAS.341..669H) for the formation of hot subdwarfs in our Galaxy. We give the colour evolution of a simple stellar population (SSP) (including binaries) of 10^10^M_{sun}_ for our standard simulation set. We have also compiled a file for the SED evolution, in which the SEDs without binary interactions are also supplied.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/1098#2</TD>
            <TD>2011-09-14T20:16:43Z</TD>
            <TD>#Photometry#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/1098</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/380/1098&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/1098</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/380/1098 [1]</TD>
            <TD>UV-upturn of elliptical galaxies model (Han+, 2007)</TD>
            <TD>A long-standing problem in the study of elliptical galaxies is the far-ultraviolet (FUV) excess in their spectra (also known as UV-upturn, UV rising-branch, UV rising flux, or UVX). While it is now clear that this UV excess is caused by an old population of hot helium-burning stars without large hydrogen-rich envelopes. We have developed an evolutionary population synthesis (EPS) model for the FUV excess of elliptical galaxies based on the binary model of Han et al. (2002MNRAS.336..449H and 2003MNRAS.341..669H) for the formation of hot subdwarfs in our Galaxy. We give the colour evolution of a simple stellar population (SSP) (including binaries) of 10^10^M_{sun}_ for our standard simulation set. We have also compiled a file for the SED evolution, in which the SEDs without binary interactions are also supplied.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/1098#1</TD>
            <TD>2011-09-14T20:16:43Z</TD>
            <TD>#Photometry#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/1098</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/380/1098</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/1098</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/380/1098 [2]</TD>
            <TD>UV-upturn of elliptical galaxies model (Han+, 2007)</TD>
            <TD>A long-standing problem in the study of elliptical galaxies is the far-ultraviolet (FUV) excess in their spectra (also known as UV-upturn, UV rising-branch, UV rising flux, or UVX). While it is now clear that this UV excess is caused by an old population of hot helium-burning stars without large hydrogen-rich envelopes. We have developed an evolutionary population synthesis (EPS) model for the FUV excess of elliptical galaxies based on the binary model of Han et al. (2002MNRAS.336..449H and 2003MNRAS.341..669H) for the formation of hot subdwarfs in our Galaxy. We give the colour evolution of a simple stellar population (SSP) (including binaries) of 10^10^M_{sun}_ for our standard simulation set. We have also compiled a file for the SED evolution, in which the SEDs without binary interactions are also supplied.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/1098#2</TD>
            <TD>2011-09-14T20:16:43Z</TD>
            <TD>#Photometry#Galaxies#Models#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/1098</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/380/1098&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/1098</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/476/151 [1]</TD>
            <TD>SWIRE ELAIS-S1 IR-peak galaxy IR fluxes (Berta+, 2007)</TD>
            <TD>Main data on the IR-peakers sample in the SWIRE ELAIS-S1 field. For each IR-peak galaxy, we report R band magnitude (AB units, from the ESIS survey, Berta et al., 2006A&amp;A...451..881B), Spitzer SWIRE fluxes (Lonsdale et al., 2003PASP..115..897L, 2004ApJS..154...54L), photometric redshift (based on Hyper-z fit, Bolzonella et al., 2000A&amp;A...363..476B), the stellar mass and its minimal-maximal range. The stellar mass estimate is based on mixed stellar population (MSP) synthesis (Berta et al., 2004A&amp;A...418..913B). The minimal and maximal stellar masses are obtained by exploring the SFH-extinction parameter space with the Adaptive Simulated Annealing algorithm (Ingber et al., 2001, http://www.ingber.com/asa01_lecture.pdf). See the paper associated to these data for more details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151#1</TD>
            <TD>2011-09-14T20:21:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/476/151</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/476/151</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/476/151 [2]</TD>
            <TD>SWIRE ELAIS-S1 IR-peak galaxy IR fluxes (Berta+, 2007)</TD>
            <TD>Main data on the IR-peakers sample in the SWIRE ELAIS-S1 field. For each IR-peak galaxy, we report R band magnitude (AB units, from the ESIS survey, Berta et al., 2006A&amp;A...451..881B), Spitzer SWIRE fluxes (Lonsdale et al., 2003PASP..115..897L, 2004ApJS..154...54L), photometric redshift (based on Hyper-z fit, Bolzonella et al., 2000A&amp;A...363..476B), the stellar mass and its minimal-maximal range. The stellar mass estimate is based on mixed stellar population (MSP) synthesis (Berta et al., 2004A&amp;A...418..913B). The minimal and maximal stellar masses are obtained by exploring the SFH-extinction parameter space with the Adaptive Simulated Annealing algorithm (Ingber et al., 2001, http://www.ingber.com/asa01_lecture.pdf). See the paper associated to these data for more details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151#2</TD>
            <TD>2011-09-14T20:21:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/476/151&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/476/151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/476/151 [table]</TD>
            <TD>SWIRE ELAIS-S1 IR-peak galaxy IR fluxes (Berta+, 2007)</TD>
            <TD>Main data on the IR-peakers sample in the SWIRE ELAIS-S1 field. For each IR-peak galaxy, we report R band magnitude (AB units, from the ESIS survey, Berta et al., 2006A&amp;A...451..881B), Spitzer SWIRE fluxes (Lonsdale et al., 2003PASP..115..897L, 2004ApJS..154...54L), photometric redshift (based on Hyper-z fit, Bolzonella et al., 2000A&amp;A...363..476B), the stellar mass and its minimal-maximal range. The stellar mass estimate is based on mixed stellar population (MSP) synthesis (Berta et al., 2004A&amp;A...418..913B). The minimal and maximal stellar masses are obtained by exploring the SFH-extinction parameter space with the Adaptive Simulated Annealing algorithm (Ingber et al., 2001, http://www.ingber.com/asa01_lecture.pdf). See the paper associated to these data for more details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151#table</TD>
            <TD>2011-09-14T20:21:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/476/151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/476/151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/476/151</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/250 [1]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#1</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/250</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/250 [2]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#2</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/250&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/250 [parent]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#parent</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/250&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/250 [photo]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#photo</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/250&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/250 [2dfgrs]</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) (2dFGRS Team, 1998-2003)</TD>
            <TD>The 2dF Galaxy Redshift Survey (2dFGRS) is a major spectroscopic survey taking full advantage of the unique capabilities of the 2dF facility built by the Anglo-Australian Observatory. The 2dFGRS is integrated with the 2dF QSO survey (2QZ, Cat. VII/241). The 2dFGRS obtained spectra for 245591 objects, mainly galaxies, brighter than a nominal extinction-corrected magnitude limit of b_J_=19.45. Reliable (quality&gt;=3) redshifts were obtained for 221414 galaxies. The galaxies cover an area of approximately 1500 square degrees selected from the extended APM Galaxy Survey in three regions: a North Galactic Pole (NGP) strip, a South Galactic Pole (SGP) strip, and random fields scattered around the SGP strip. Redshifts are measured from spectra covering 3600-8000 Angstroms at a two-pixel resolution of 9.0 Angstrom and a median S/N of 13 per pixel. All redshift identifications are visually checked and assigned a quality parameter Q in the range 1-5; Q&gt;=3 redshifts are 98.4% reliable and have an rms uncertainty of 85 km/s. The overall redshift completeness for Q&gt;=3 redshifts is 91.8% but this varies with magnitude from 99% for the brightest galaxies to 90% for objects at the survey limit. The 2dFGRS data base is available on the World Wide Web at http://www.mso.anu.edu.au/2dFGRS/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/250#2dfgrs</TD>
            <TD>2012-09-24T07:21:19Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/VII/250</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/250&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/250</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/78/675 [1]</TD>
            <TD>Quasar-galaxy associations (Bukhmastova, 2001)</TD>
            <TD>A new catalog of 8382 close quasar-galaxy pairs is presented. The catalog was composed using published catalogued quasars and active galactic nuclei containing 11358 objects, as well as the LEDA catalog of galaxies, which contains on the order of 100000 objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675#1</TD>
            <TD>2011-09-14T20:17:14Z</TD>
            <TD>#AGN#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/78/675</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/78/675</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/78/675 [2]</TD>
            <TD>Quasar-galaxy associations (Bukhmastova, 2001)</TD>
            <TD>A new catalog of 8382 close quasar-galaxy pairs is presented. The catalog was composed using published catalogued quasars and active galactic nuclei containing 11358 objects, as well as the LEDA catalog of galaxies, which contains on the order of 100000 objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675#2</TD>
            <TD>2011-09-14T20:17:14Z</TD>
            <TD>#AGN#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/78/675&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/78/675</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AZh/78/675 [catalog]</TD>
            <TD>Quasar-galaxy associations (Bukhmastova, 2001)</TD>
            <TD>A new catalog of 8382 close quasar-galaxy pairs is presented. The catalog was composed using published catalogued quasars and active galactic nuclei containing 11358 objects, as well as the LEDA catalog of galaxies, which contains on the order of 100000 objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675#catalog</TD>
            <TD>2011-09-14T20:17:14Z</TD>
            <TD>#AGN#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AZh/78/675&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/78/675</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/705/L76 [1]</TD>
            <TD>AGNs with double-peaked [OIII] lines (Wang+, 2009)</TD>
            <TD>We start from the galaxy sample of SDSS DR7 and select active galaxies based on the widely used BPT diagram. Using the measured fluxes of narrow emission lines from the MPA/JHU catalog, we separate type 2 AGNs from other sources according to their line ratios. We select those objects with SDSS r-band magnitude r&lt;17.7, redshift z&lt;=0.15, and equivalent width of [OIII]5007&gt;5. In total, 6780 type 2 AGNs follow from this criterion. Finally, we are left with 87 sources having a flux ratio in the range of [0.3,3], 44 of which have high enough signal-to-noise ratio of the spectra to see similar double-peaked structures in other lines (e.g., [OIII]4959, H{beta}, H{alpha}, [NII], [SII]).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76#1</TD>
            <TD>2012-06-28T09:58:58Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/705/L76</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/L76</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/705/L76 [2]</TD>
            <TD>AGNs with double-peaked [OIII] lines (Wang+, 2009)</TD>
            <TD>We start from the galaxy sample of SDSS DR7 and select active galaxies based on the widely used BPT diagram. Using the measured fluxes of narrow emission lines from the MPA/JHU catalog, we separate type 2 AGNs from other sources according to their line ratios. We select those objects with SDSS r-band magnitude r&lt;17.7, redshift z&lt;=0.15, and equivalent width of [OIII]5007&gt;5. In total, 6780 type 2 AGNs follow from this criterion. Finally, we are left with 87 sources having a flux ratio in the range of [0.3,3], 44 of which have high enough signal-to-noise ratio of the spectra to see similar double-peaked structures in other lines (e.g., [OIII]4959, H{beta}, H{alpha}, [NII], [SII]).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76#2</TD>
            <TD>2012-06-28T09:58:58Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/705/L76&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/L76</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/L76 [table1]</TD>
            <TD>AGNs with double-peaked [OIII] lines (Wang+, 2009)</TD>
            <TD>We start from the galaxy sample of SDSS DR7 and select active galaxies based on the widely used BPT diagram. Using the measured fluxes of narrow emission lines from the MPA/JHU catalog, we separate type 2 AGNs from other sources according to their line ratios. We select those objects with SDSS r-band magnitude r&lt;17.7, redshift z&lt;=0.15, and equivalent width of [OIII]5007&gt;5. In total, 6780 type 2 AGNs follow from this criterion. Finally, we are left with 87 sources having a flux ratio in the range of [0.3,3], 44 of which have high enough signal-to-noise ratio of the spectra to see similar double-peaked structures in other lines (e.g., [OIII]4959, H{beta}, H{alpha}, [NII], [SII]).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76#table1</TD>
            <TD>2012-06-28T09:58:58Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/L76&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/L76</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/391/35 [1]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#1</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/391/35</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/391/35 [2]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#2</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/391/35&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/35 [table2]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#table2</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/35 [table1]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#table1</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/78/675 [1]</TD>
            <TD>Quasar-galaxy associations (Bukhmastova, 2001)</TD>
            <TD>A new catalog of 8382 close quasar-galaxy pairs is presented. The catalog was composed using published catalogued quasars and active galactic nuclei containing 11358 objects, as well as the LEDA catalog of galaxies, which contains on the order of 100000 objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675#1</TD>
            <TD>2011-09-14T20:17:14Z</TD>
            <TD>#AGN#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/78/675</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/78/675</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/78/675 [2]</TD>
            <TD>Quasar-galaxy associations (Bukhmastova, 2001)</TD>
            <TD>A new catalog of 8382 close quasar-galaxy pairs is presented. The catalog was composed using published catalogued quasars and active galactic nuclei containing 11358 objects, as well as the LEDA catalog of galaxies, which contains on the order of 100000 objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675#2</TD>
            <TD>2011-09-14T20:17:14Z</TD>
            <TD>#AGN#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/78/675&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/78/675</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AZh/78/675 [catalog]</TD>
            <TD>Quasar-galaxy associations (Bukhmastova, 2001)</TD>
            <TD>A new catalog of 8382 close quasar-galaxy pairs is presented. The catalog was composed using published catalogued quasars and active galactic nuclei containing 11358 objects, as well as the LEDA catalog of galaxies, which contains on the order of 100000 objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675#catalog</TD>
            <TD>2011-09-14T20:17:14Z</TD>
            <TD>#AGN#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AZh/78/675&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/78/675</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/705/L76 [1]</TD>
            <TD>AGNs with double-peaked [OIII] lines (Wang+, 2009)</TD>
            <TD>We start from the galaxy sample of SDSS DR7 and select active galaxies based on the widely used BPT diagram. Using the measured fluxes of narrow emission lines from the MPA/JHU catalog, we separate type 2 AGNs from other sources according to their line ratios. We select those objects with SDSS r-band magnitude r&lt;17.7, redshift z&lt;=0.15, and equivalent width of [OIII]5007&gt;5. In total, 6780 type 2 AGNs follow from this criterion. Finally, we are left with 87 sources having a flux ratio in the range of [0.3,3], 44 of which have high enough signal-to-noise ratio of the spectra to see similar double-peaked structures in other lines (e.g., [OIII]4959, H{beta}, H{alpha}, [NII], [SII]).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76#1</TD>
            <TD>2012-06-28T09:58:58Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/705/L76</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/L76</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/705/L76 [2]</TD>
            <TD>AGNs with double-peaked [OIII] lines (Wang+, 2009)</TD>
            <TD>We start from the galaxy sample of SDSS DR7 and select active galaxies based on the widely used BPT diagram. Using the measured fluxes of narrow emission lines from the MPA/JHU catalog, we separate type 2 AGNs from other sources according to their line ratios. We select those objects with SDSS r-band magnitude r&lt;17.7, redshift z&lt;=0.15, and equivalent width of [OIII]5007&gt;5. In total, 6780 type 2 AGNs follow from this criterion. Finally, we are left with 87 sources having a flux ratio in the range of [0.3,3], 44 of which have high enough signal-to-noise ratio of the spectra to see similar double-peaked structures in other lines (e.g., [OIII]4959, H{beta}, H{alpha}, [NII], [SII]).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76#2</TD>
            <TD>2012-06-28T09:58:58Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/705/L76&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/L76</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/L76 [table1]</TD>
            <TD>AGNs with double-peaked [OIII] lines (Wang+, 2009)</TD>
            <TD>We start from the galaxy sample of SDSS DR7 and select active galaxies based on the widely used BPT diagram. Using the measured fluxes of narrow emission lines from the MPA/JHU catalog, we separate type 2 AGNs from other sources according to their line ratios. We select those objects with SDSS r-band magnitude r&lt;17.7, redshift z&lt;=0.15, and equivalent width of [OIII]5007&gt;5. In total, 6780 type 2 AGNs follow from this criterion. Finally, we are left with 87 sources having a flux ratio in the range of [0.3,3], 44 of which have high enough signal-to-noise ratio of the spectra to see similar double-peaked structures in other lines (e.g., [OIII]4959, H{beta}, H{alpha}, [NII], [SII]).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76#table1</TD>
            <TD>2012-06-28T09:58:58Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/L76&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/L76</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/705/L76 [1]</TD>
            <TD>AGNs with double-peaked [OIII] lines (Wang+, 2009)</TD>
            <TD>We start from the galaxy sample of SDSS DR7 and select active galaxies based on the widely used BPT diagram. Using the measured fluxes of narrow emission lines from the MPA/JHU catalog, we separate type 2 AGNs from other sources according to their line ratios. We select those objects with SDSS r-band magnitude r&lt;17.7, redshift z&lt;=0.15, and equivalent width of [OIII]5007&gt;5. In total, 6780 type 2 AGNs follow from this criterion. Finally, we are left with 87 sources having a flux ratio in the range of [0.3,3], 44 of which have high enough signal-to-noise ratio of the spectra to see similar double-peaked structures in other lines (e.g., [OIII]4959, H{beta}, H{alpha}, [NII], [SII]).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76#1</TD>
            <TD>2012-06-28T09:58:58Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/705/L76</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/L76</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/705/L76 [2]</TD>
            <TD>AGNs with double-peaked [OIII] lines (Wang+, 2009)</TD>
            <TD>We start from the galaxy sample of SDSS DR7 and select active galaxies based on the widely used BPT diagram. Using the measured fluxes of narrow emission lines from the MPA/JHU catalog, we separate type 2 AGNs from other sources according to their line ratios. We select those objects with SDSS r-band magnitude r&lt;17.7, redshift z&lt;=0.15, and equivalent width of [OIII]5007&gt;5. In total, 6780 type 2 AGNs follow from this criterion. Finally, we are left with 87 sources having a flux ratio in the range of [0.3,3], 44 of which have high enough signal-to-noise ratio of the spectra to see similar double-peaked structures in other lines (e.g., [OIII]4959, H{beta}, H{alpha}, [NII], [SII]).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76#2</TD>
            <TD>2012-06-28T09:58:58Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/705/L76&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/L76</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/L76 [table1]</TD>
            <TD>AGNs with double-peaked [OIII] lines (Wang+, 2009)</TD>
            <TD>We start from the galaxy sample of SDSS DR7 and select active galaxies based on the widely used BPT diagram. Using the measured fluxes of narrow emission lines from the MPA/JHU catalog, we separate type 2 AGNs from other sources according to their line ratios. We select those objects with SDSS r-band magnitude r&lt;17.7, redshift z&lt;=0.15, and equivalent width of [OIII]5007&gt;5. In total, 6780 type 2 AGNs follow from this criterion. Finally, we are left with 87 sources having a flux ratio in the range of [0.3,3], 44 of which have high enough signal-to-noise ratio of the spectra to see similar double-peaked structures in other lines (e.g., [OIII]4959, H{beta}, H{alpha}, [NII], [SII]).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76#table1</TD>
            <TD>2012-06-28T09:58:58Z</TD>
            <TD>#AGN#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/L76</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/L76&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/L76</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/78/675 [1]</TD>
            <TD>Quasar-galaxy associations (Bukhmastova, 2001)</TD>
            <TD>A new catalog of 8382 close quasar-galaxy pairs is presented. The catalog was composed using published catalogued quasars and active galactic nuclei containing 11358 objects, as well as the LEDA catalog of galaxies, which contains on the order of 100000 objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675#1</TD>
            <TD>2011-09-14T20:17:14Z</TD>
            <TD>#AGN#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/78/675</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/78/675</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/78/675 [2]</TD>
            <TD>Quasar-galaxy associations (Bukhmastova, 2001)</TD>
            <TD>A new catalog of 8382 close quasar-galaxy pairs is presented. The catalog was composed using published catalogued quasars and active galactic nuclei containing 11358 objects, as well as the LEDA catalog of galaxies, which contains on the order of 100000 objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675#2</TD>
            <TD>2011-09-14T20:17:14Z</TD>
            <TD>#AGN#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/78/675&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/78/675</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AZh/78/675 [catalog]</TD>
            <TD>Quasar-galaxy associations (Bukhmastova, 2001)</TD>
            <TD>A new catalog of 8382 close quasar-galaxy pairs is presented. The catalog was composed using published catalogued quasars and active galactic nuclei containing 11358 objects, as well as the LEDA catalog of galaxies, which contains on the order of 100000 objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675#catalog</TD>
            <TD>2011-09-14T20:17:14Z</TD>
            <TD>#AGN#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AZh/78/675</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AZh/78/675&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/78/675</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/700/1299 [1]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#1</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/700/1299</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/700/1299 [2]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#2</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/700/1299&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/700/1299 [table6]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#table6</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/700/1299&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/700/1299 [table2]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#table2</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/700/1299&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/700/1299 [1]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#1</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/700/1299</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/700/1299 [2]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#2</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/700/1299&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/700/1299 [table6]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#table6</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/700/1299&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/700/1299 [table2]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#table2</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/700/1299&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/376/960 [1]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#1</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/376/960</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/376/960 [2]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#2</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/960 [table2]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#table2</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/960 [table4]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#table4</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/960 [table3]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#table3</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/700/1299 [1]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#1</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/700/1299</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/700/1299 [2]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#2</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/700/1299&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/700/1299 [table6]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#table6</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/700/1299&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/700/1299 [table2]</TD>
            <TD>Gas-phase element depletions in the ISM (Jenkins, 2009)</TD>
            <TD>A study of gas-phase element abundances reported in the literature for 17 different elements sampled over 243 sight lines in the local part of our Galaxy reveals that the depletions into solid form (dust grains) are extremely well characterized by trends that employ only three kinds of parameters. One is an index that describes the overall level of depletion applicable to the gas in any particular sight line, and the other two represent linear coefficients that describe how to derive each element's depletion from this sight-line parameter. The information from this study reveals the relative proportions of different elements that are incorporated into dust at different stages of grain growth.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299#table2</TD>
            <TD>2012-07-06T09:45:13Z</TD>
            <TD>#Abundances#Stars#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jul-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/1299</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/700/1299&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/1299</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/376/960 [1]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#1</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/376/960</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/376/960 [2]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#2</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/960 [table2]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#table2</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/960 [table4]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#table4</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/960 [table3]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#table3</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/376/960 [1]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#1</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/376/960</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/376/960 [2]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#2</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/960 [table2]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#table2</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/960 [table4]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#table4</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/376/960 [table3]</TD>
            <TD>X-ray emission from the Sombrero galaxy (NGC 4594) (Li+, 2007)</TD>
            <TD>The Chandra ACIS-S observation of Sombrero (Obs. ID. 1586) was taken on 2001 May 31 with an exposure of 18.8ks. The XMM-Newton EPIC observation of Sombrero (Obs. ID 0084030101) was taken on 2001 December 28, with the thin filter and with a total exposure of 43ks.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960#table3</TD>
            <TD>2011-09-14T20:18:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/376/960</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/376/960&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/376/960</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/380/986 [1]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#1</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/380/986</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/380/986 [2]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#2</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/380/986&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/380/986 [table3]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#table3</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/380/986&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/380/986 [table1]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#table1</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/380/986&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/380/986 [1]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#1</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/380/986</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/380/986 [2]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#2</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/380/986&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/380/986 [table3]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#table3</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/380/986&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/380/986 [table1]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#table1</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/380/986&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/391/35 [1]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#1</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/391/35</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/391/35 [2]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#2</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/391/35&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/35 [table2]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#table2</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/35 [table1]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#table1</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/380/986 [1]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#1</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/380/986</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/380/986 [2]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#2</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/380/986&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/380/986 [table3]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#table3</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/380/986&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/380/986 [table1]</TD>
            <TD>Lyman-break galaxies from GALEX (Burgarella+, 2007)</TD>
            <TD>Ultraviolet (UV) galaxies have been selected from the Galaxy Evolution Explorer deep imaging survey. The presence of a far-UV (FUV) drop-out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at z~1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR).</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986#table1</TD>
            <TD>2011-09-14T20:19:34Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/380/986</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/380/986&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/380/986</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AN/322/73 [1]</TD>
            <TD>BVIc photometry in NGC 2976 (Notni+, 2001)</TD>
            <TD>We present BVIc photometry of the brightest stars and compact star clusters in NGC 2976, a dwarf galaxy in the interacting M81/M82 group. Deep CCD images of the galaxy were obtained with the 6m-Telescope of the Special Astrophysical Observatory (Russia) at arcsec resolution. About 290 young stars and concentrated young clusters were measured. Supplementaxy data in the ultraviolet are taken from the literature. The extinction to the measured objects is comparatively low, E(B-V)~0.15-0.20mag. We estimate the ages of youngest resolved stars and concentrated star clusters to be ~5x10^6^years. This population is concentrated in a broad stripe facing M81. In the central disk the population is a bit older, about 8x10^6^years, this may be a hint to an outward spreading star formation process. The metallicity of the disk population is estimated as solar (z~0.02) from a fitting to Padova theoretical stellar isochrones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/322/73#1</TD>
            <TD>2011-09-14T20:27:08Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AN/322/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AN/322/73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/322/73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AN/322/73 [2]</TD>
            <TD>BVIc photometry in NGC 2976 (Notni+, 2001)</TD>
            <TD>We present BVIc photometry of the brightest stars and compact star clusters in NGC 2976, a dwarf galaxy in the interacting M81/M82 group. Deep CCD images of the galaxy were obtained with the 6m-Telescope of the Special Astrophysical Observatory (Russia) at arcsec resolution. About 290 young stars and concentrated young clusters were measured. Supplementaxy data in the ultraviolet are taken from the literature. The extinction to the measured objects is comparatively low, E(B-V)~0.15-0.20mag. We estimate the ages of youngest resolved stars and concentrated star clusters to be ~5x10^6^years. This population is concentrated in a broad stripe facing M81. In the central disk the population is a bit older, about 8x10^6^years, this may be a hint to an outward spreading star formation process. The metallicity of the disk population is estimated as solar (z~0.02) from a fitting to Padova theoretical stellar isochrones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/322/73#2</TD>
            <TD>2011-09-14T20:27:08Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AN/322/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AN/322/73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/322/73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/2426 [1]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#1</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/2426</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/2426 [2]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#2</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2426 [table3]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#table3</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2426 [table2]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#table2</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2426 [table1]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#table1</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/391/35 [1]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#1</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/391/35</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/391/35 [2]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#2</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/391/35&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/35 [table2]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#table2</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/35 [table1]</TD>
            <TD>Compact Groups in the UZC galaxy sample (Focardi+, 2002)</TD>
            <TD>Applying an automatic neighbour search algorithm to the 3D UZC galaxy catalogue (Falco et al., 1999, Cat. &lt;J/PASP/111/438&gt;) we have identified 291 compact groups (CGs) with radial velocity between 1000 and 10000km/s. The sample is analysed to investigate whether Triplets display kinematical and morphological characteristics similar to higher order CGs (Multiplets). It is found that Triplets constitute low velocity dispersion structures, have a gas-rich galaxy population and are typically retrieved in sparse environments. Conversely Multiplets show higher velocity dispersion, include few gas-rich members and are generally embedded structures. Evidence hence emerges indicating that Triplets and Multiplets, though sharing a common scale, correspond to different galaxy systems. Triplets are typically field structures whilst Multiplets are mainly subclumps (either temporarily projected or collapsing) within larger structures. Simulations show that selection effects can only partially account for differences, but significant contamination of Triplets by field galaxy interlopers could eventually induce the observed dependences on multiplicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35#table1</TD>
            <TD>2012-09-24T07:25:08Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/35</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AN/322/73 [1]</TD>
            <TD>BVIc photometry in NGC 2976 (Notni+, 2001)</TD>
            <TD>We present BVIc photometry of the brightest stars and compact star clusters in NGC 2976, a dwarf galaxy in the interacting M81/M82 group. Deep CCD images of the galaxy were obtained with the 6m-Telescope of the Special Astrophysical Observatory (Russia) at arcsec resolution. About 290 young stars and concentrated young clusters were measured. Supplementaxy data in the ultraviolet are taken from the literature. The extinction to the measured objects is comparatively low, E(B-V)~0.15-0.20mag. We estimate the ages of youngest resolved stars and concentrated star clusters to be ~5x10^6^years. This population is concentrated in a broad stripe facing M81. In the central disk the population is a bit older, about 8x10^6^years, this may be a hint to an outward spreading star formation process. The metallicity of the disk population is estimated as solar (z~0.02) from a fitting to Padova theoretical stellar isochrones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/322/73#1</TD>
            <TD>2011-09-14T20:27:08Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AN/322/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AN/322/73</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/322/73</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AN/322/73 [2]</TD>
            <TD>BVIc photometry in NGC 2976 (Notni+, 2001)</TD>
            <TD>We present BVIc photometry of the brightest stars and compact star clusters in NGC 2976, a dwarf galaxy in the interacting M81/M82 group. Deep CCD images of the galaxy were obtained with the 6m-Telescope of the Special Astrophysical Observatory (Russia) at arcsec resolution. About 290 young stars and concentrated young clusters were measured. Supplementaxy data in the ultraviolet are taken from the literature. The extinction to the measured objects is comparatively low, E(B-V)~0.15-0.20mag. We estimate the ages of youngest resolved stars and concentrated star clusters to be ~5x10^6^years. This population is concentrated in a broad stripe facing M81. In the central disk the population is a bit older, about 8x10^6^years, this may be a hint to an outward spreading star formation process. The metallicity of the disk population is estimated as solar (z~0.02) from a fitting to Padova theoretical stellar isochrones.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/322/73#2</TD>
            <TD>2011-09-14T20:27:08Z</TD>
            <TD>#Photometry#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/AN/322/73</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AN/322/73&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/322/73</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/2426 [1]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#1</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/2426</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/2426 [2]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#2</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2426 [table3]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#table3</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2426 [table2]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#table2</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2426 [table1]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#table1</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/113 [1]</TD>
            <TD>Catalogued Galaxies + QSOs observed in IRAS Survey, Vers.2 (IPAC 1989)</TD>
            <TD>The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (&lt;8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organisation of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/113#1</TD>
            <TD>2012-09-24T07:30:25Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/113 [2]</TD>
            <TD>Catalogued Galaxies + QSOs observed in IRAS Survey, Vers.2 (IPAC 1989)</TD>
            <TD>The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (&lt;8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organisation of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/113#2</TD>
            <TD>2012-09-24T07:30:25Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/113&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/113 [xcat]</TD>
            <TD>Catalogued Galaxies + QSOs observed in IRAS Survey, Vers.2 (IPAC 1989)</TD>
            <TD>The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (&lt;8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organisation of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/113#xcat</TD>
            <TD>2012-09-24T07:30:25Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/382/1552 [1]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#1</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/382/1552</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/382/1552 [2]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#2</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/382/1552&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/382/1552 [table1]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#table1</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/382/1552&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/382/1552 [table5]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#table5</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/382/1552&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/2426 [1]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#1</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/2426</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/2426 [2]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#2</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2426 [table3]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#table3</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2426 [table2]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#table2</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/2426 [table1]</TD>
            <TD>Optical and radio study of Abell 2111 (Miller+, 2006)</TD>
            <TD>Galaxy spectra within the field of A2111 were obtained using the Hydra multifiber spectrograph on the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5m telescope in 1996. Briefly, three fiber configurations were observed during 1996 May 20-22, with a fourth observed on 1996 June 10-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426#table1</TD>
            <TD>2011-09-14T20:21:11Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/2426</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/2426&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/2426</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/113 [1]</TD>
            <TD>Catalogued Galaxies + QSOs observed in IRAS Survey, Vers.2 (IPAC 1989)</TD>
            <TD>The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (&lt;8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organisation of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/113#1</TD>
            <TD>2012-09-24T07:30:25Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/113 [2]</TD>
            <TD>Catalogued Galaxies + QSOs observed in IRAS Survey, Vers.2 (IPAC 1989)</TD>
            <TD>The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (&lt;8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organisation of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/113#2</TD>
            <TD>2012-09-24T07:30:25Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/113&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/113 [xcat]</TD>
            <TD>Catalogued Galaxies + QSOs observed in IRAS Survey, Vers.2 (IPAC 1989)</TD>
            <TD>The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (&lt;8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organisation of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/113#xcat</TD>
            <TD>2012-09-24T07:30:25Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/382/1552 [1]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#1</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/382/1552</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/382/1552 [2]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#2</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/382/1552&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/382/1552 [table1]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#table1</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/382/1552&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/382/1552 [table5]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#table5</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/382/1552&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/477/125 [1]</TD>
            <TD>Microquasar candidates (Combi+, 2008)</TD>
            <TD>Microquasars are ideal natural laboratories for understanding accretion/ejection processes, studying the physics of relativistic jets, and testing gravitational phenomena. Nevertheless, these objects are difficult to find in our Galaxy. The main goal of this work is to increase the number of known systems of this kind, which should allow better testing of high-energy phenomena and more realistic statistical studies of this galactic population to be made. We have developed an improved search strategy based on positional cross-identification with very restrictive selection criteria to find new MQs, taking advantage of more sensitive modern X-ray data. To do this, we made combined use of the radio, infrared, and X-ray properties of the sources, using different available catalogs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125#1</TD>
            <TD>2011-09-14T20:21:27Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/477/125</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/477/125</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/477/125 [2]</TD>
            <TD>Microquasar candidates (Combi+, 2008)</TD>
            <TD>Microquasars are ideal natural laboratories for understanding accretion/ejection processes, studying the physics of relativistic jets, and testing gravitational phenomena. Nevertheless, these objects are difficult to find in our Galaxy. The main goal of this work is to increase the number of known systems of this kind, which should allow better testing of high-energy phenomena and more realistic statistical studies of this galactic population to be made. We have developed an improved search strategy based on positional cross-identification with very restrictive selection criteria to find new MQs, taking advantage of more sensitive modern X-ray data. To do this, we made combined use of the radio, infrared, and X-ray properties of the sources, using different available catalogs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125#2</TD>
            <TD>2011-09-14T20:21:27Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/477/125&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/477/125</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/477/125 [table1]</TD>
            <TD>Microquasar candidates (Combi+, 2008)</TD>
            <TD>Microquasars are ideal natural laboratories for understanding accretion/ejection processes, studying the physics of relativistic jets, and testing gravitational phenomena. Nevertheless, these objects are difficult to find in our Galaxy. The main goal of this work is to increase the number of known systems of this kind, which should allow better testing of high-energy phenomena and more realistic statistical studies of this galactic population to be made. We have developed an improved search strategy based on positional cross-identification with very restrictive selection criteria to find new MQs, taking advantage of more sensitive modern X-ray data. To do this, we made combined use of the radio, infrared, and X-ray properties of the sources, using different available catalogs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125#table1</TD>
            <TD>2011-09-14T20:21:27Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/477/125&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/477/125</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/477/125 [1]</TD>
            <TD>Microquasar candidates (Combi+, 2008)</TD>
            <TD>Microquasars are ideal natural laboratories for understanding accretion/ejection processes, studying the physics of relativistic jets, and testing gravitational phenomena. Nevertheless, these objects are difficult to find in our Galaxy. The main goal of this work is to increase the number of known systems of this kind, which should allow better testing of high-energy phenomena and more realistic statistical studies of this galactic population to be made. We have developed an improved search strategy based on positional cross-identification with very restrictive selection criteria to find new MQs, taking advantage of more sensitive modern X-ray data. To do this, we made combined use of the radio, infrared, and X-ray properties of the sources, using different available catalogs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125#1</TD>
            <TD>2011-09-14T20:21:27Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/477/125</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/477/125</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/477/125 [2]</TD>
            <TD>Microquasar candidates (Combi+, 2008)</TD>
            <TD>Microquasars are ideal natural laboratories for understanding accretion/ejection processes, studying the physics of relativistic jets, and testing gravitational phenomena. Nevertheless, these objects are difficult to find in our Galaxy. The main goal of this work is to increase the number of known systems of this kind, which should allow better testing of high-energy phenomena and more realistic statistical studies of this galactic population to be made. We have developed an improved search strategy based on positional cross-identification with very restrictive selection criteria to find new MQs, taking advantage of more sensitive modern X-ray data. To do this, we made combined use of the radio, infrared, and X-ray properties of the sources, using different available catalogs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125#2</TD>
            <TD>2011-09-14T20:21:27Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/477/125&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/477/125</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/477/125 [table1]</TD>
            <TD>Microquasar candidates (Combi+, 2008)</TD>
            <TD>Microquasars are ideal natural laboratories for understanding accretion/ejection processes, studying the physics of relativistic jets, and testing gravitational phenomena. Nevertheless, these objects are difficult to find in our Galaxy. The main goal of this work is to increase the number of known systems of this kind, which should allow better testing of high-energy phenomena and more realistic statistical studies of this galactic population to be made. We have developed an improved search strategy based on positional cross-identification with very restrictive selection criteria to find new MQs, taking advantage of more sensitive modern X-ray data. To do this, we made combined use of the radio, infrared, and X-ray properties of the sources, using different available catalogs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125#table1</TD>
            <TD>2011-09-14T20:21:27Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/477/125&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/477/125</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/477/125 [1]</TD>
            <TD>Microquasar candidates (Combi+, 2008)</TD>
            <TD>Microquasars are ideal natural laboratories for understanding accretion/ejection processes, studying the physics of relativistic jets, and testing gravitational phenomena. Nevertheless, these objects are difficult to find in our Galaxy. The main goal of this work is to increase the number of known systems of this kind, which should allow better testing of high-energy phenomena and more realistic statistical studies of this galactic population to be made. We have developed an improved search strategy based on positional cross-identification with very restrictive selection criteria to find new MQs, taking advantage of more sensitive modern X-ray data. To do this, we made combined use of the radio, infrared, and X-ray properties of the sources, using different available catalogs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125#1</TD>
            <TD>2011-09-14T20:21:27Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/477/125</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/477/125</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/477/125 [2]</TD>
            <TD>Microquasar candidates (Combi+, 2008)</TD>
            <TD>Microquasars are ideal natural laboratories for understanding accretion/ejection processes, studying the physics of relativistic jets, and testing gravitational phenomena. Nevertheless, these objects are difficult to find in our Galaxy. The main goal of this work is to increase the number of known systems of this kind, which should allow better testing of high-energy phenomena and more realistic statistical studies of this galactic population to be made. We have developed an improved search strategy based on positional cross-identification with very restrictive selection criteria to find new MQs, taking advantage of more sensitive modern X-ray data. To do this, we made combined use of the radio, infrared, and X-ray properties of the sources, using different available catalogs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125#2</TD>
            <TD>2011-09-14T20:21:27Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/477/125&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/477/125</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/477/125 [table1]</TD>
            <TD>Microquasar candidates (Combi+, 2008)</TD>
            <TD>Microquasars are ideal natural laboratories for understanding accretion/ejection processes, studying the physics of relativistic jets, and testing gravitational phenomena. Nevertheless, these objects are difficult to find in our Galaxy. The main goal of this work is to increase the number of known systems of this kind, which should allow better testing of high-energy phenomena and more realistic statistical studies of this galactic population to be made. We have developed an improved search strategy based on positional cross-identification with very restrictive selection criteria to find new MQs, taking advantage of more sensitive modern X-ray data. To do this, we made combined use of the radio, infrared, and X-ray properties of the sources, using different available catalogs.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125#table1</TD>
            <TD>2011-09-14T20:21:27Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/477/125</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/477/125&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/477/125</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/482/53 [1]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#1</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/482/53</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/482/53 [2]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#2</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/482/53&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/482/53 [table2]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#table2</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/482/53&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/482/53 [table1]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#table1</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/482/53&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/482/53 [1]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#1</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/482/53</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/482/53 [2]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#2</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/482/53&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/482/53 [table2]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#table2</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/482/53&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/482/53 [table1]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#table1</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/482/53&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/482/53 [1]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#1</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/482/53</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/482/53 [2]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#2</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/482/53&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/482/53 [table2]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#table2</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/482/53&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/482/53 [table1]</TD>
            <TD>Radial velocities of four LSB galaxies (Pizzella+, 2008)</TD>
            <TD>We present integral-field spectroscopy of the ionized gas in the central regions of four galaxies with a low surface brightness disk taken with the Visible Multi Object Spectrograph at the Very Large Telescope and aimed at testing the accuracy in the determination of the central logarithmic slope alpha of the mass density radial profile rho(r){prop.to}r^alpha^ in this class of objects. For all the sample galaxies we subtracted the best-fit model of gas in circular motions from the observed velocity field and derived the residuals. Only ESO-LV5340200 is characterized by a regular velocity field. We extracted the velocity curves of this galaxy along several position angles, in order to estimate the uncertainty in deriving the central gradient of the total mass density from long-slit spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53#table1</TD>
            <TD>2011-09-14T20:22:43Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/482/53</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/482/53&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/482/53</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/705/639 [1]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#1</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/705/639</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/705/639 [2]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#2</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/705/639&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/639 [table2]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#table2</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/639&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/639 [table3]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#table3</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/639&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/382/1552 [1]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#1</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/382/1552</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/382/1552 [2]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#2</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/382/1552&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/382/1552 [table1]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#table1</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/382/1552&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/382/1552 [table5]</TD>
            <TD>Multiwavelength study of nearby galaxy nuclei (Lira+, 2007)</TD>
            <TD>Broad-band optical images of the galaxies were obtained at the 1-m Jacobus Kapteyn Telescope in La Palma in 1994 February and August. The UBVRI images had a pixel scale of ~0.3arcsec and the total field of view (FOV) was of ~6arcmin. Near-infrared (NIR) images were taken at the 2.1-m telescope of the Observatorio Astronomico Nacional in Baja California in 1994 October and 1995 March and October. JHK images were obtained with a pixel scale of ~0.5arcsec and an FOV of ~2arcmin. Radio observations at 1.4GHz were taken with the Very Large Array (VLA) in B configuration in 1994 August.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552#table5</TD>
            <TD>2011-09-14T20:27:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/382/1552</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/382/1552&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/382/1552</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/705/639 [1]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#1</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/705/639</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/705/639 [2]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#2</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/705/639&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/639 [table2]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#table2</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/639&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/639 [table3]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#table3</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/639&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>VII/113 [1]</TD>
            <TD>Catalogued Galaxies + QSOs observed in IRAS Survey, Vers.2 (IPAC 1989)</TD>
            <TD>The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (&lt;8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organisation of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/113#1</TD>
            <TD>2012-09-24T07:30:25Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/113 [2]</TD>
            <TD>Catalogued Galaxies + QSOs observed in IRAS Survey, Vers.2 (IPAC 1989)</TD>
            <TD>The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (&lt;8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organisation of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/113#2</TD>
            <TD>2012-09-24T07:30:25Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/113&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/113 [xcat]</TD>
            <TD>Catalogued Galaxies + QSOs observed in IRAS Survey, Vers.2 (IPAC 1989)</TD>
            <TD>The Infrared Astronomical Satellite (IRAS) surveyed approximately 96% of the sky in four infrared wavelength bands centered at 12, 25, 60, and 100 um. The IRAS data are presented in catalogs of point sources and small extended sources (&lt;8') as well as in atlases of low resolution spectra and sky-brightness images. The Cataloged Galaxies and Quasars Observed in the IRAS Survey, hereafter referred to as the "Extragalactic Catalog", is the subset of those point source data pertaining to previously known galaxies and quasars. It is intended as a readily accessible compilation of IRAS data for objects appearing in the most widely-used extragalactic catalogs. The Extragalactic Catalog contains 11,444 IRAS point sources (IRAS Point Source Catalog, Version 2.0) that can be positionally associated with catalogued galaxies and quasars, including association information of point sources with sources from the IRAS Small Scale Structure Catalog. Section II summarizes important aspects of the IRAS mission and the data processing techniques. Section III describes the organisation of the Extragalactic Catalog and the way in which the associations were made with the various galaxy catalogs. Section IV describes the information given for each entry in the Extragalactic Catalog. Section V presents some preliminary statistics on the contents of the Extragalactic Catalog. Acknowledgments and References are given in Sections VI and VII. The catalog itself comprises Section VIII. Some notes and errata are given in Sections IX and X. A printed and a tape version of the Extragalactic Catalog are available.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/113#xcat</TD>
            <TD>2012-09-24T07:30:25Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
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            <TD>07-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/VII/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/705/639 [1]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#1</TD>
            <TD>2012-06-28T10:06:23Z</TD>
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            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD />
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            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/705/639</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/705/639 [2]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#2</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
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            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/705/639&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/639 [table2]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#table2</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/639&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/705/639 [table3]</TD>
            <TD>Sizes of Lyman alpha emitters at z=3.1 (Bond+, 2009)</TD>
            <TD>This paper complements the Gronwall et al. (2007, Cat. J/ApJ/667/79) and Gawiser et al. (2007ApJ...671..278G) studies of the MUSYC z=3.1 LAE sample by measuring the rest-UV size and component distributions using high-resolution V-band images, taken by the Advanced Camera for Surveys (ACS) and obtained as part of the Galaxy Evolution from Morphology and SEDs survey (GEMS; Rix et al. 2004ApJS..152..163R), Great Observatories Origins Deep Survey (GOODS; Giavalisco et al. 2004, Cat. II/261), and Hubble Ultradeep Field survey (HUDF; Beckwith et al. 2006, Cat. J/AJ/132/1729).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639#table3</TD>
            <TD>2012-06-28T10:06:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>02-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/705/639</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/705/639&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/705/639</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/378/1507 [1]</TD>
            <TD>Spectroscopic study of 6 galaxies (Brough+, 2007)</TD>
            <TD>The BGG and BCG galaxy samples were selected from the Group Evolution Multi-wavelength Study (GEMS; Osmond &amp; Ponman, 2004MNRAS.350.1511O; Forbes et al., 2006PASA...23...38F) and the BCG sample presented in Brough et al. (2005MNRAS.364.1354B). In both these samples the galaxy is selected as the brightest galaxy closest to the X-ray centroid, that is, closest to the centre of the potential well of these structures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507#1</TD>
            <TD>2011-09-14T20:28:03Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/378/1507</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/378/1507</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/378/1507 [2]</TD>
            <TD>Spectroscopic study of 6 galaxies (Brough+, 2007)</TD>
            <TD>The BGG and BCG galaxy samples were selected from the Group Evolution Multi-wavelength Study (GEMS; Osmond &amp; Ponman, 2004MNRAS.350.1511O; Forbes et al., 2006PASA...23...38F) and the BCG sample presented in Brough et al. (2005MNRAS.364.1354B). In both these samples the galaxy is selected as the brightest galaxy closest to the X-ray centroid, that is, closest to the centre of the potential well of these structures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507#2</TD>
            <TD>2011-09-14T20:28:03Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>16-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/378/1507&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/378/1507</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/378/1507 [galaxies]</TD>
            <TD>Spectroscopic study of 6 galaxies (Brough+, 2007)</TD>
            <TD>The BGG and BCG galaxy samples were selected from the Group Evolution Multi-wavelength Study (GEMS; Osmond &amp; Ponman, 2004MNRAS.350.1511O; Forbes et al., 2006PASA...23...38F) and the BCG sample presented in Brough et al. (2005MNRAS.364.1354B). In both these samples the galaxy is selected as the brightest galaxy closest to the X-ray centroid, that is, closest to the centre of the potential well of these structures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507#galaxies</TD>
            <TD>2011-09-14T20:28:03Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/378/1507&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/378/1507</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/716/521 [1]</TD>
            <TD>31GHz sky survey with the SZA (Muchovej+, 2010)</TD>
            <TD>The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8GHz wideband correlator and sensitive 26-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, we obtained high-sensitivity VLA observations at 5GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521#1</TD>
            <TD>2012-07-08T19:52:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/716/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/716/521 [2]</TD>
            <TD>31GHz sky survey with the SZA (Muchovej+, 2010)</TD>
            <TD>The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8GHz wideband correlator and sensitive 26-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, we obtained high-sensitivity VLA observations at 5GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521#2</TD>
            <TD>2012-07-08T19:52:24Z</TD>
            <TD>##</TD>
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            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/716/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/521</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/716/521 [table3]</TD>
            <TD>31GHz sky survey with the SZA (Muchovej+, 2010)</TD>
            <TD>The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8GHz wideband correlator and sensitive 26-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, we obtained high-sensitivity VLA observations at 5GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521#table3</TD>
            <TD>2012-07-08T19:52:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/716/521&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/366/771 [1]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#1</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/366/771</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/366/771 [2]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#2</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/366/771&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table5]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table5</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table6]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table6</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table3]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table3</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table7]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table7</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/378/1507 [1]</TD>
            <TD>Spectroscopic study of 6 galaxies (Brough+, 2007)</TD>
            <TD>The BGG and BCG galaxy samples were selected from the Group Evolution Multi-wavelength Study (GEMS; Osmond &amp; Ponman, 2004MNRAS.350.1511O; Forbes et al., 2006PASA...23...38F) and the BCG sample presented in Brough et al. (2005MNRAS.364.1354B). In both these samples the galaxy is selected as the brightest galaxy closest to the X-ray centroid, that is, closest to the centre of the potential well of these structures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507#1</TD>
            <TD>2011-09-14T20:28:03Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/378/1507</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/378/1507</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/378/1507 [2]</TD>
            <TD>Spectroscopic study of 6 galaxies (Brough+, 2007)</TD>
            <TD>The BGG and BCG galaxy samples were selected from the Group Evolution Multi-wavelength Study (GEMS; Osmond &amp; Ponman, 2004MNRAS.350.1511O; Forbes et al., 2006PASA...23...38F) and the BCG sample presented in Brough et al. (2005MNRAS.364.1354B). In both these samples the galaxy is selected as the brightest galaxy closest to the X-ray centroid, that is, closest to the centre of the potential well of these structures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507#2</TD>
            <TD>2011-09-14T20:28:03Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/378/1507&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/378/1507</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/378/1507 [galaxies]</TD>
            <TD>Spectroscopic study of 6 galaxies (Brough+, 2007)</TD>
            <TD>The BGG and BCG galaxy samples were selected from the Group Evolution Multi-wavelength Study (GEMS; Osmond &amp; Ponman, 2004MNRAS.350.1511O; Forbes et al., 2006PASA...23...38F) and the BCG sample presented in Brough et al. (2005MNRAS.364.1354B). In both these samples the galaxy is selected as the brightest galaxy closest to the X-ray centroid, that is, closest to the centre of the potential well of these structures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507#galaxies</TD>
            <TD>2011-09-14T20:28:03Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/378/1507&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/378/1507</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/716/521 [1]</TD>
            <TD>31GHz sky survey with the SZA (Muchovej+, 2010)</TD>
            <TD>The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8GHz wideband correlator and sensitive 26-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, we obtained high-sensitivity VLA observations at 5GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521#1</TD>
            <TD>2012-07-08T19:52:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/716/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/716/521 [2]</TD>
            <TD>31GHz sky survey with the SZA (Muchovej+, 2010)</TD>
            <TD>The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8GHz wideband correlator and sensitive 26-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, we obtained high-sensitivity VLA observations at 5GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521#2</TD>
            <TD>2012-07-08T19:52:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/716/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/521</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/716/521 [table3]</TD>
            <TD>31GHz sky survey with the SZA (Muchovej+, 2010)</TD>
            <TD>The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8GHz wideband correlator and sensitive 26-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, we obtained high-sensitivity VLA observations at 5GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521#table3</TD>
            <TD>2012-07-08T19:52:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/716/521&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/378/1507 [1]</TD>
            <TD>Spectroscopic study of 6 galaxies (Brough+, 2007)</TD>
            <TD>The BGG and BCG galaxy samples were selected from the Group Evolution Multi-wavelength Study (GEMS; Osmond &amp; Ponman, 2004MNRAS.350.1511O; Forbes et al., 2006PASA...23...38F) and the BCG sample presented in Brough et al. (2005MNRAS.364.1354B). In both these samples the galaxy is selected as the brightest galaxy closest to the X-ray centroid, that is, closest to the centre of the potential well of these structures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507#1</TD>
            <TD>2011-09-14T20:28:03Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/378/1507</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/378/1507</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/378/1507 [2]</TD>
            <TD>Spectroscopic study of 6 galaxies (Brough+, 2007)</TD>
            <TD>The BGG and BCG galaxy samples were selected from the Group Evolution Multi-wavelength Study (GEMS; Osmond &amp; Ponman, 2004MNRAS.350.1511O; Forbes et al., 2006PASA...23...38F) and the BCG sample presented in Brough et al. (2005MNRAS.364.1354B). In both these samples the galaxy is selected as the brightest galaxy closest to the X-ray centroid, that is, closest to the centre of the potential well of these structures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507#2</TD>
            <TD>2011-09-14T20:28:03Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/378/1507&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/378/1507</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/378/1507 [galaxies]</TD>
            <TD>Spectroscopic study of 6 galaxies (Brough+, 2007)</TD>
            <TD>The BGG and BCG galaxy samples were selected from the Group Evolution Multi-wavelength Study (GEMS; Osmond &amp; Ponman, 2004MNRAS.350.1511O; Forbes et al., 2006PASA...23...38F) and the BCG sample presented in Brough et al. (2005MNRAS.364.1354B). In both these samples the galaxy is selected as the brightest galaxy closest to the X-ray centroid, that is, closest to the centre of the potential well of these structures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507#galaxies</TD>
            <TD>2011-09-14T20:28:03Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/378/1507</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/378/1507&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/378/1507</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/366/771 [1]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#1</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/366/771</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/366/771 [2]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#2</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/366/771&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table5]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table5</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table6]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table6</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table3]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table3</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table7]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table7</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/716/521 [1]</TD>
            <TD>31GHz sky survey with the SZA (Muchovej+, 2010)</TD>
            <TD>The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8GHz wideband correlator and sensitive 26-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, we obtained high-sensitivity VLA observations at 5GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521#1</TD>
            <TD>2012-07-08T19:52:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/716/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/716/521 [2]</TD>
            <TD>31GHz sky survey with the SZA (Muchovej+, 2010)</TD>
            <TD>The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8GHz wideband correlator and sensitive 26-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, we obtained high-sensitivity VLA observations at 5GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521#2</TD>
            <TD>2012-07-08T19:52:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/716/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/521</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/716/521 [table3]</TD>
            <TD>31GHz sky survey with the SZA (Muchovej+, 2010)</TD>
            <TD>The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8GHz wideband correlator and sensitive 26-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, we obtained high-sensitivity VLA observations at 5GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521#table3</TD>
            <TD>2012-07-08T19:52:24Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/716/521</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/716/521&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/716/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/52/631 [1]</TD>
            <TD>Galactic plane VERA survey (Honma+, 2000)</TD>
            <TD>In order to search for new VLBI sources in the galactic plane that can be used as phase reference sources in differential VLBI, we conducted 22GHz observations of radio sources in the galactic plane using the Japanese VLBI Network (J-Net). We have observed 267 VLBI source candidates selected from existing radio surveys and have detected 93 sources at a signal-to-noise ratio larger than 5. While 42 of the 93 detected sources had already been detected with VLBI at relatively lower frequency (typically 2 to 8GHz), the remaining 51 are found to be new VLBI sources detected for the first time. These are located within |b|&lt;=5{deg}, and have a large number of galactic maser sources around them. Thus, they are potential candidates for phase reference sources for VLBI Exploration of Radio Astrometry (VERA), which is the first VLBI array dedicated to phase-referencing VLBI astrometry aimed at measuring the parallax and proper motion of maser sources in the whole Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631#1</TD>
            <TD>2011-09-14T20:29:13Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/52/631</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/52/631</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/52/631 [2]</TD>
            <TD>Galactic plane VERA survey (Honma+, 2000)</TD>
            <TD>In order to search for new VLBI sources in the galactic plane that can be used as phase reference sources in differential VLBI, we conducted 22GHz observations of radio sources in the galactic plane using the Japanese VLBI Network (J-Net). We have observed 267 VLBI source candidates selected from existing radio surveys and have detected 93 sources at a signal-to-noise ratio larger than 5. While 42 of the 93 detected sources had already been detected with VLBI at relatively lower frequency (typically 2 to 8GHz), the remaining 51 are found to be new VLBI sources detected for the first time. These are located within |b|&lt;=5{deg}, and have a large number of galactic maser sources around them. Thus, they are potential candidates for phase reference sources for VLBI Exploration of Radio Astrometry (VERA), which is the first VLBI array dedicated to phase-referencing VLBI astrometry aimed at measuring the parallax and proper motion of maser sources in the whole Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631#2</TD>
            <TD>2011-09-14T20:29:13Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/52/631&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/52/631</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/52/631 [table1]</TD>
            <TD>Galactic plane VERA survey (Honma+, 2000)</TD>
            <TD>In order to search for new VLBI sources in the galactic plane that can be used as phase reference sources in differential VLBI, we conducted 22GHz observations of radio sources in the galactic plane using the Japanese VLBI Network (J-Net). We have observed 267 VLBI source candidates selected from existing radio surveys and have detected 93 sources at a signal-to-noise ratio larger than 5. While 42 of the 93 detected sources had already been detected with VLBI at relatively lower frequency (typically 2 to 8GHz), the remaining 51 are found to be new VLBI sources detected for the first time. These are located within |b|&lt;=5{deg}, and have a large number of galactic maser sources around them. Thus, they are potential candidates for phase reference sources for VLBI Exploration of Radio Astrometry (VERA), which is the first VLBI array dedicated to phase-referencing VLBI astrometry aimed at measuring the parallax and proper motion of maser sources in the whole Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631#table1</TD>
            <TD>2011-09-14T20:29:13Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/52/631&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/52/631</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/366/771 [1]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#1</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/366/771</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/366/771 [2]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#2</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/366/771&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table5]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table5</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table6]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table6</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table3]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table3</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/771 [table7]</TD>
            <TD>The Hamburg/SAO Survey for ELGs. IV (Kniazev+, 2001)</TD>
            <TD>We present the fourth list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS hereafter, SAO -- Special Astrophysical Observatory, Russia). The main goal of the project is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact/HII galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. The main ELG candidate selection criteria applied are blue or flat enough continuum (near 4000{AA}) and the presence of strong or moderate emission lines close to 5000{AA} recognized on digitized prism spectra of galaxies with the survey estimated B-magnitudes in the range 16-19.5. No other criteria were applied. The list is a result of the follow-up spectroscopy conducted with the 6m SAO RAS telescope in 1998, 1999 and 2000. The data of this snap-shot spectroscopy survey confirmed 127 emission-line objects out of 176 observed candidates and allowed their quantitative spectral classification. We could classify 76 emission-line objects as BCG/HII galaxies or probable BCGs, 8 as QSOs, 2 as Seyfert galaxies, 2 as super-associations in a subluminous spiral and an irregular galaxy, and 37 as low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 2 ELGs. Furthermore, for 5 galaxies we did not detect any significant emission lines. For 91 emission-line galaxies, the redshifts and/or line intensities are determined for the first time. Of the remaining 28 previously known ELGs we give either improved data on the line intensities or some independent measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771#table7</TD>
            <TD>2012-09-24T08:14:28Z</TD>
            <TD>#Seyfert_Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/771</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/385/361 [1]</TD>
            <TD>BVRcIc photometry of NGC 821 globular clusters (Spitler+, 2008)</TD>
            <TD>We performed a photometric study of globular clusters around the isolated elliptical galaxy NGC 821. B, V and R-band photometry come from the Mini-Mosaic imager on the 3.5-m Wisconsin Indiana Yale NOAO (WIYN) telescope. Observations were conducted between November 30 - December 2, 2005. Average seeing conditions were ~0.7". Two Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC2) fields were analysed in the V and I-bands. Objects in this catalogue are the globular cluster candidates according to the selection criteria detailed in the journal article. Astrometric solution is from USNO-B stars. Note the center of NGC 821 on this system is located at 02:08:21.118 +10:59:42.21. Photometry has been corrected for Galactic extinction and we used a distance modulus of m-M=31.75 in our analysis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361#1</TD>
            <TD>2011-09-14T20:26:38Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/385/361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/361</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/385/361 [2]</TD>
            <TD>BVRcIc photometry of NGC 821 globular clusters (Spitler+, 2008)</TD>
            <TD>We performed a photometric study of globular clusters around the isolated elliptical galaxy NGC 821. B, V and R-band photometry come from the Mini-Mosaic imager on the 3.5-m Wisconsin Indiana Yale NOAO (WIYN) telescope. Observations were conducted between November 30 - December 2, 2005. Average seeing conditions were ~0.7". Two Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC2) fields were analysed in the V and I-bands. Objects in this catalogue are the globular cluster candidates according to the selection criteria detailed in the journal article. Astrometric solution is from USNO-B stars. Note the center of NGC 821 on this system is located at 02:08:21.118 +10:59:42.21. Photometry has been corrected for Galactic extinction and we used a distance modulus of m-M=31.75 in our analysis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361#2</TD>
            <TD>2011-09-14T20:26:38Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/385/361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/361</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/385/361 [table4]</TD>
            <TD>BVRcIc photometry of NGC 821 globular clusters (Spitler+, 2008)</TD>
            <TD>We performed a photometric study of globular clusters around the isolated elliptical galaxy NGC 821. B, V and R-band photometry come from the Mini-Mosaic imager on the 3.5-m Wisconsin Indiana Yale NOAO (WIYN) telescope. Observations were conducted between November 30 - December 2, 2005. Average seeing conditions were ~0.7". Two Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC2) fields were analysed in the V and I-bands. Objects in this catalogue are the globular cluster candidates according to the selection criteria detailed in the journal article. Astrometric solution is from USNO-B stars. Note the center of NGC 821 on this system is located at 02:08:21.118 +10:59:42.21. Photometry has been corrected for Galactic extinction and we used a distance modulus of m-M=31.75 in our analysis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361#table4</TD>
            <TD>2011-09-14T20:26:38Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/385/361&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/361</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/52/631 [1]</TD>
            <TD>Galactic plane VERA survey (Honma+, 2000)</TD>
            <TD>In order to search for new VLBI sources in the galactic plane that can be used as phase reference sources in differential VLBI, we conducted 22GHz observations of radio sources in the galactic plane using the Japanese VLBI Network (J-Net). We have observed 267 VLBI source candidates selected from existing radio surveys and have detected 93 sources at a signal-to-noise ratio larger than 5. While 42 of the 93 detected sources had already been detected with VLBI at relatively lower frequency (typically 2 to 8GHz), the remaining 51 are found to be new VLBI sources detected for the first time. These are located within |b|&lt;=5{deg}, and have a large number of galactic maser sources around them. Thus, they are potential candidates for phase reference sources for VLBI Exploration of Radio Astrometry (VERA), which is the first VLBI array dedicated to phase-referencing VLBI astrometry aimed at measuring the parallax and proper motion of maser sources in the whole Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631#1</TD>
            <TD>2011-09-14T20:29:13Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/52/631</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/52/631</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/52/631 [2]</TD>
            <TD>Galactic plane VERA survey (Honma+, 2000)</TD>
            <TD>In order to search for new VLBI sources in the galactic plane that can be used as phase reference sources in differential VLBI, we conducted 22GHz observations of radio sources in the galactic plane using the Japanese VLBI Network (J-Net). We have observed 267 VLBI source candidates selected from existing radio surveys and have detected 93 sources at a signal-to-noise ratio larger than 5. While 42 of the 93 detected sources had already been detected with VLBI at relatively lower frequency (typically 2 to 8GHz), the remaining 51 are found to be new VLBI sources detected for the first time. These are located within |b|&lt;=5{deg}, and have a large number of galactic maser sources around them. Thus, they are potential candidates for phase reference sources for VLBI Exploration of Radio Astrometry (VERA), which is the first VLBI array dedicated to phase-referencing VLBI astrometry aimed at measuring the parallax and proper motion of maser sources in the whole Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631#2</TD>
            <TD>2011-09-14T20:29:13Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/52/631&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/52/631</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/52/631 [table1]</TD>
            <TD>Galactic plane VERA survey (Honma+, 2000)</TD>
            <TD>In order to search for new VLBI sources in the galactic plane that can be used as phase reference sources in differential VLBI, we conducted 22GHz observations of radio sources in the galactic plane using the Japanese VLBI Network (J-Net). We have observed 267 VLBI source candidates selected from existing radio surveys and have detected 93 sources at a signal-to-noise ratio larger than 5. While 42 of the 93 detected sources had already been detected with VLBI at relatively lower frequency (typically 2 to 8GHz), the remaining 51 are found to be new VLBI sources detected for the first time. These are located within |b|&lt;=5{deg}, and have a large number of galactic maser sources around them. Thus, they are potential candidates for phase reference sources for VLBI Exploration of Radio Astrometry (VERA), which is the first VLBI array dedicated to phase-referencing VLBI astrometry aimed at measuring the parallax and proper motion of maser sources in the whole Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631#table1</TD>
            <TD>2011-09-14T20:29:13Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/52/631&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/52/631</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/105/209 [1]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#1</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/105/209</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/105/209 [2]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#2</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/105/209&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/105/209 [table3]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#table3</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/105/209&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/105/209 [catalog]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#catalog</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/105/209&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/385/361 [1]</TD>
            <TD>BVRcIc photometry of NGC 821 globular clusters (Spitler+, 2008)</TD>
            <TD>We performed a photometric study of globular clusters around the isolated elliptical galaxy NGC 821. B, V and R-band photometry come from the Mini-Mosaic imager on the 3.5-m Wisconsin Indiana Yale NOAO (WIYN) telescope. Observations were conducted between November 30 - December 2, 2005. Average seeing conditions were ~0.7". Two Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC2) fields were analysed in the V and I-bands. Objects in this catalogue are the globular cluster candidates according to the selection criteria detailed in the journal article. Astrometric solution is from USNO-B stars. Note the center of NGC 821 on this system is located at 02:08:21.118 +10:59:42.21. Photometry has been corrected for Galactic extinction and we used a distance modulus of m-M=31.75 in our analysis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361#1</TD>
            <TD>2011-09-14T20:26:38Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/385/361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/361</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/385/361 [2]</TD>
            <TD>BVRcIc photometry of NGC 821 globular clusters (Spitler+, 2008)</TD>
            <TD>We performed a photometric study of globular clusters around the isolated elliptical galaxy NGC 821. B, V and R-band photometry come from the Mini-Mosaic imager on the 3.5-m Wisconsin Indiana Yale NOAO (WIYN) telescope. Observations were conducted between November 30 - December 2, 2005. Average seeing conditions were ~0.7". Two Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC2) fields were analysed in the V and I-bands. Objects in this catalogue are the globular cluster candidates according to the selection criteria detailed in the journal article. Astrometric solution is from USNO-B stars. Note the center of NGC 821 on this system is located at 02:08:21.118 +10:59:42.21. Photometry has been corrected for Galactic extinction and we used a distance modulus of m-M=31.75 in our analysis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361#2</TD>
            <TD>2011-09-14T20:26:38Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/385/361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/361</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/385/361 [table4]</TD>
            <TD>BVRcIc photometry of NGC 821 globular clusters (Spitler+, 2008)</TD>
            <TD>We performed a photometric study of globular clusters around the isolated elliptical galaxy NGC 821. B, V and R-band photometry come from the Mini-Mosaic imager on the 3.5-m Wisconsin Indiana Yale NOAO (WIYN) telescope. Observations were conducted between November 30 - December 2, 2005. Average seeing conditions were ~0.7". Two Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC2) fields were analysed in the V and I-bands. Objects in this catalogue are the globular cluster candidates according to the selection criteria detailed in the journal article. Astrometric solution is from USNO-B stars. Note the center of NGC 821 on this system is located at 02:08:21.118 +10:59:42.21. Photometry has been corrected for Galactic extinction and we used a distance modulus of m-M=31.75 in our analysis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361#table4</TD>
            <TD>2011-09-14T20:26:38Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/385/361&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/361</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASJ/52/631 [1]</TD>
            <TD>Galactic plane VERA survey (Honma+, 2000)</TD>
            <TD>In order to search for new VLBI sources in the galactic plane that can be used as phase reference sources in differential VLBI, we conducted 22GHz observations of radio sources in the galactic plane using the Japanese VLBI Network (J-Net). We have observed 267 VLBI source candidates selected from existing radio surveys and have detected 93 sources at a signal-to-noise ratio larger than 5. While 42 of the 93 detected sources had already been detected with VLBI at relatively lower frequency (typically 2 to 8GHz), the remaining 51 are found to be new VLBI sources detected for the first time. These are located within |b|&lt;=5{deg}, and have a large number of galactic maser sources around them. Thus, they are potential candidates for phase reference sources for VLBI Exploration of Radio Astrometry (VERA), which is the first VLBI array dedicated to phase-referencing VLBI astrometry aimed at measuring the parallax and proper motion of maser sources in the whole Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631#1</TD>
            <TD>2011-09-14T20:29:13Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASJ/52/631</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/52/631</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASJ/52/631 [2]</TD>
            <TD>Galactic plane VERA survey (Honma+, 2000)</TD>
            <TD>In order to search for new VLBI sources in the galactic plane that can be used as phase reference sources in differential VLBI, we conducted 22GHz observations of radio sources in the galactic plane using the Japanese VLBI Network (J-Net). We have observed 267 VLBI source candidates selected from existing radio surveys and have detected 93 sources at a signal-to-noise ratio larger than 5. While 42 of the 93 detected sources had already been detected with VLBI at relatively lower frequency (typically 2 to 8GHz), the remaining 51 are found to be new VLBI sources detected for the first time. These are located within |b|&lt;=5{deg}, and have a large number of galactic maser sources around them. Thus, they are potential candidates for phase reference sources for VLBI Exploration of Radio Astrometry (VERA), which is the first VLBI array dedicated to phase-referencing VLBI astrometry aimed at measuring the parallax and proper motion of maser sources in the whole Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631#2</TD>
            <TD>2011-09-14T20:29:13Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASJ/52/631&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/52/631</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASJ/52/631 [table1]</TD>
            <TD>Galactic plane VERA survey (Honma+, 2000)</TD>
            <TD>In order to search for new VLBI sources in the galactic plane that can be used as phase reference sources in differential VLBI, we conducted 22GHz observations of radio sources in the galactic plane using the Japanese VLBI Network (J-Net). We have observed 267 VLBI source candidates selected from existing radio surveys and have detected 93 sources at a signal-to-noise ratio larger than 5. While 42 of the 93 detected sources had already been detected with VLBI at relatively lower frequency (typically 2 to 8GHz), the remaining 51 are found to be new VLBI sources detected for the first time. These are located within |b|&lt;=5{deg}, and have a large number of galactic maser sources around them. Thus, they are potential candidates for phase reference sources for VLBI Exploration of Radio Astrometry (VERA), which is the first VLBI array dedicated to phase-referencing VLBI astrometry aimed at measuring the parallax and proper motion of maser sources in the whole Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631#table1</TD>
            <TD>2011-09-14T20:29:13Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/PASJ/52/631</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASJ/52/631&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASJ/52/631</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/105/209 [1]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#1</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/105/209</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/105/209 [2]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#2</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/105/209&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/105/209 [table3]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#table3</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/105/209&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/105/209 [catalog]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#catalog</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/105/209&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/385/361 [1]</TD>
            <TD>BVRcIc photometry of NGC 821 globular clusters (Spitler+, 2008)</TD>
            <TD>We performed a photometric study of globular clusters around the isolated elliptical galaxy NGC 821. B, V and R-band photometry come from the Mini-Mosaic imager on the 3.5-m Wisconsin Indiana Yale NOAO (WIYN) telescope. Observations were conducted between November 30 - December 2, 2005. Average seeing conditions were ~0.7". Two Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC2) fields were analysed in the V and I-bands. Objects in this catalogue are the globular cluster candidates according to the selection criteria detailed in the journal article. Astrometric solution is from USNO-B stars. Note the center of NGC 821 on this system is located at 02:08:21.118 +10:59:42.21. Photometry has been corrected for Galactic extinction and we used a distance modulus of m-M=31.75 in our analysis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361#1</TD>
            <TD>2011-09-14T20:26:38Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/385/361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/361</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/385/361 [2]</TD>
            <TD>BVRcIc photometry of NGC 821 globular clusters (Spitler+, 2008)</TD>
            <TD>We performed a photometric study of globular clusters around the isolated elliptical galaxy NGC 821. B, V and R-band photometry come from the Mini-Mosaic imager on the 3.5-m Wisconsin Indiana Yale NOAO (WIYN) telescope. Observations were conducted between November 30 - December 2, 2005. Average seeing conditions were ~0.7". Two Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC2) fields were analysed in the V and I-bands. Objects in this catalogue are the globular cluster candidates according to the selection criteria detailed in the journal article. Astrometric solution is from USNO-B stars. Note the center of NGC 821 on this system is located at 02:08:21.118 +10:59:42.21. Photometry has been corrected for Galactic extinction and we used a distance modulus of m-M=31.75 in our analysis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361#2</TD>
            <TD>2011-09-14T20:26:38Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/385/361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/361</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/385/361 [table4]</TD>
            <TD>BVRcIc photometry of NGC 821 globular clusters (Spitler+, 2008)</TD>
            <TD>We performed a photometric study of globular clusters around the isolated elliptical galaxy NGC 821. B, V and R-band photometry come from the Mini-Mosaic imager on the 3.5-m Wisconsin Indiana Yale NOAO (WIYN) telescope. Observations were conducted between November 30 - December 2, 2005. Average seeing conditions were ~0.7". Two Hubble Space Telescope (HST) Wide-Field Planetary Camera 2 (WFPC2) fields were analysed in the V and I-bands. Objects in this catalogue are the globular cluster candidates according to the selection criteria detailed in the journal article. Astrometric solution is from USNO-B stars. Note the center of NGC 821 on this system is located at 02:08:21.118 +10:59:42.21. Photometry has been corrected for Galactic extinction and we used a distance modulus of m-M=31.75 in our analysis.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361#table4</TD>
            <TD>2011-09-14T20:26:38Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/385/361</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/385/361&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/385/361</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/1311 [1]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#1</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/1311</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/1311 [2]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#2</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/1311&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/1311 [table1]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#table1</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/1311&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/1311 [table2]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#table2</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/1311&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/105/209 [1]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#1</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/105/209</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/105/209 [2]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#2</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/105/209&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/105/209 [table3]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#table3</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/105/209&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/105/209 [catalog]</TD>
            <TD>Low surface brightness galaxies. I. The catalog (Impey+ 1996)</TD>
            <TD>Data are presented for 693 galaxies identified in a large new survey for low surface brightness galaxies in the nearby universe (z&lt;=0.1). The survey covers 786 square degrees centered on the equator, and it extends significantly the surface brightness range of galaxy surveys in which there are a substantial number of galaxies with redshifts. The data are derived from the Automated Plate Measuring machine scans of survey plates from the UK Schmidt Telescope and from follow-up observations at radio and optical wavelengths. Accurate positions, total B magnitudes, surface brightness parameters, and angular size are tabulated for each galaxy. Radial velocities, optical luminosities, and neutral hydrogen masses are listed for a subset of the sample. Finding charts are also presented for those objects having a large enough angular size that the scans from survey plates provide some morphological information. The selection function and the luminosity function that can be derived from the survey are discussed in two companion papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209#catalog</TD>
            <TD>2012-09-24T08:14:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/105/209</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/105/209&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/105/209</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/488/211 [1]</TD>
            <TD>Infrated photometry of NGC 1893 (Caramazza+, 2008)</TD>
            <TD>The independence of the star formation processes with respect to the environmental conditions is controversial. In particular it is not clear whether star formation in the outer Galaxy, where the environmental conditions are, theoretically, less conducive, occurs in the same way as in the inner Galaxy. We investigate the population of NGC 1893, a young cluster (~3-4Myr) in the outer part of the Galaxy (galactic radius &gt;11kpc) in order to explore the effects of environmental conditions on star forming regions. We present the infrared observations obtained with the IRAC camera on board of the Spitzer Space Telescope and analyze the color-color diagrams to establish the membership of stars with excesses. We also merge this information with that obtained from Chandra ACIS-I observations, in order to identify the Class III population. We find that the cluster is very rich, with 242 PMS Classical T-Tauri stars and 7 Class 0/I stars. Moreover we identify 110 Class III candidate cluster members in the ACIS-I field of view. We estimate a disk fraction for NGC 1893 of about 67%, similar to fraction calculated for nearby star forming regions of the same age. Although the environmental conditions are not favorable, star formation can clearly be very successful in the outer Galaxy, allowing creation of a very rich cluster like NGC 1893.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211#1</TD>
            <TD>2011-09-14T20:27:40Z</TD>
            <TD>#Open_Clusters#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/488/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/488/211 [2]</TD>
            <TD>Infrated photometry of NGC 1893 (Caramazza+, 2008)</TD>
            <TD>The independence of the star formation processes with respect to the environmental conditions is controversial. In particular it is not clear whether star formation in the outer Galaxy, where the environmental conditions are, theoretically, less conducive, occurs in the same way as in the inner Galaxy. We investigate the population of NGC 1893, a young cluster (~3-4Myr) in the outer part of the Galaxy (galactic radius &gt;11kpc) in order to explore the effects of environmental conditions on star forming regions. We present the infrared observations obtained with the IRAC camera on board of the Spitzer Space Telescope and analyze the color-color diagrams to establish the membership of stars with excesses. We also merge this information with that obtained from Chandra ACIS-I observations, in order to identify the Class III population. We find that the cluster is very rich, with 242 PMS Classical T-Tauri stars and 7 Class 0/I stars. Moreover we identify 110 Class III candidate cluster members in the ACIS-I field of view. We estimate a disk fraction for NGC 1893 of about 67%, similar to fraction calculated for nearby star forming regions of the same age. Although the environmental conditions are not favorable, star formation can clearly be very successful in the outer Galaxy, allowing creation of a very rich cluster like NGC 1893.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211#2</TD>
            <TD>2011-09-14T20:27:40Z</TD>
            <TD>#Open_Clusters#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/488/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/488/211 [table1]</TD>
            <TD>Infrated photometry of NGC 1893 (Caramazza+, 2008)</TD>
            <TD>The independence of the star formation processes with respect to the environmental conditions is controversial. In particular it is not clear whether star formation in the outer Galaxy, where the environmental conditions are, theoretically, less conducive, occurs in the same way as in the inner Galaxy. We investigate the population of NGC 1893, a young cluster (~3-4Myr) in the outer part of the Galaxy (galactic radius &gt;11kpc) in order to explore the effects of environmental conditions on star forming regions. We present the infrared observations obtained with the IRAC camera on board of the Spitzer Space Telescope and analyze the color-color diagrams to establish the membership of stars with excesses. We also merge this information with that obtained from Chandra ACIS-I observations, in order to identify the Class III population. We find that the cluster is very rich, with 242 PMS Classical T-Tauri stars and 7 Class 0/I stars. Moreover we identify 110 Class III candidate cluster members in the ACIS-I field of view. We estimate a disk fraction for NGC 1893 of about 67%, similar to fraction calculated for nearby star forming regions of the same age. Although the environmental conditions are not favorable, star formation can clearly be very successful in the outer Galaxy, allowing creation of a very rich cluster like NGC 1893.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211#table1</TD>
            <TD>2011-09-14T20:27:40Z</TD>
            <TD>#Open_Clusters#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/488/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/211</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/1311 [1]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#1</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/1311</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/1311 [2]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#2</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/1311&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/1311 [table1]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#table1</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/1311&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/1311 [table2]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#table2</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/1311&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/399/1083 [1]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#1</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/399/1083</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/399/1083 [2]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#2</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/399/1083&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/1083 [table1]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#table1</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/1083&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/1083 [table2]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#table2</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/1083&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/488/211 [1]</TD>
            <TD>Infrated photometry of NGC 1893 (Caramazza+, 2008)</TD>
            <TD>The independence of the star formation processes with respect to the environmental conditions is controversial. In particular it is not clear whether star formation in the outer Galaxy, where the environmental conditions are, theoretically, less conducive, occurs in the same way as in the inner Galaxy. We investigate the population of NGC 1893, a young cluster (~3-4Myr) in the outer part of the Galaxy (galactic radius &gt;11kpc) in order to explore the effects of environmental conditions on star forming regions. We present the infrared observations obtained with the IRAC camera on board of the Spitzer Space Telescope and analyze the color-color diagrams to establish the membership of stars with excesses. We also merge this information with that obtained from Chandra ACIS-I observations, in order to identify the Class III population. We find that the cluster is very rich, with 242 PMS Classical T-Tauri stars and 7 Class 0/I stars. Moreover we identify 110 Class III candidate cluster members in the ACIS-I field of view. We estimate a disk fraction for NGC 1893 of about 67%, similar to fraction calculated for nearby star forming regions of the same age. Although the environmental conditions are not favorable, star formation can clearly be very successful in the outer Galaxy, allowing creation of a very rich cluster like NGC 1893.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211#1</TD>
            <TD>2011-09-14T20:27:40Z</TD>
            <TD>#Open_Clusters#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/488/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/488/211 [2]</TD>
            <TD>Infrated photometry of NGC 1893 (Caramazza+, 2008)</TD>
            <TD>The independence of the star formation processes with respect to the environmental conditions is controversial. In particular it is not clear whether star formation in the outer Galaxy, where the environmental conditions are, theoretically, less conducive, occurs in the same way as in the inner Galaxy. We investigate the population of NGC 1893, a young cluster (~3-4Myr) in the outer part of the Galaxy (galactic radius &gt;11kpc) in order to explore the effects of environmental conditions on star forming regions. We present the infrared observations obtained with the IRAC camera on board of the Spitzer Space Telescope and analyze the color-color diagrams to establish the membership of stars with excesses. We also merge this information with that obtained from Chandra ACIS-I observations, in order to identify the Class III population. We find that the cluster is very rich, with 242 PMS Classical T-Tauri stars and 7 Class 0/I stars. Moreover we identify 110 Class III candidate cluster members in the ACIS-I field of view. We estimate a disk fraction for NGC 1893 of about 67%, similar to fraction calculated for nearby star forming regions of the same age. Although the environmental conditions are not favorable, star formation can clearly be very successful in the outer Galaxy, allowing creation of a very rich cluster like NGC 1893.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211#2</TD>
            <TD>2011-09-14T20:27:40Z</TD>
            <TD>#Open_Clusters#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/488/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/488/211 [table1]</TD>
            <TD>Infrated photometry of NGC 1893 (Caramazza+, 2008)</TD>
            <TD>The independence of the star formation processes with respect to the environmental conditions is controversial. In particular it is not clear whether star formation in the outer Galaxy, where the environmental conditions are, theoretically, less conducive, occurs in the same way as in the inner Galaxy. We investigate the population of NGC 1893, a young cluster (~3-4Myr) in the outer part of the Galaxy (galactic radius &gt;11kpc) in order to explore the effects of environmental conditions on star forming regions. We present the infrared observations obtained with the IRAC camera on board of the Spitzer Space Telescope and analyze the color-color diagrams to establish the membership of stars with excesses. We also merge this information with that obtained from Chandra ACIS-I observations, in order to identify the Class III population. We find that the cluster is very rich, with 242 PMS Classical T-Tauri stars and 7 Class 0/I stars. Moreover we identify 110 Class III candidate cluster members in the ACIS-I field of view. We estimate a disk fraction for NGC 1893 of about 67%, similar to fraction calculated for nearby star forming regions of the same age. Although the environmental conditions are not favorable, star formation can clearly be very successful in the outer Galaxy, allowing creation of a very rich cluster like NGC 1893.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211#table1</TD>
            <TD>2011-09-14T20:27:40Z</TD>
            <TD>#Open_Clusters#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/488/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/211</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/1311 [1]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#1</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/1311</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/1311 [2]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#2</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/1311&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/1311 [table1]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#table1</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/1311&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/1311 [table2]</TD>
            <TD>J-band photometry of ADBS Galaxies (Rosenberg+, 2005)</TD>
            <TD>We present the results of a J-band study of the H I-selected Arecibo Dual-Beam Survey (ADBS, Cat. J/ApJS/130/177) and Arecibo Slice Survey (AS, Cat. J/ApJS/119/159) galaxy samples using Two Micron All Sky Survey data.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311#table2</TD>
            <TD>2011-09-14T20:29:21Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1311</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/1311&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1311</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/399/1083 [1]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#1</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/399/1083</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/399/1083 [2]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#2</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/399/1083&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/1083 [table1]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#table1</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/1083&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/1083 [table2]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#table2</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/1083&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/488/211 [1]</TD>
            <TD>Infrated photometry of NGC 1893 (Caramazza+, 2008)</TD>
            <TD>The independence of the star formation processes with respect to the environmental conditions is controversial. In particular it is not clear whether star formation in the outer Galaxy, where the environmental conditions are, theoretically, less conducive, occurs in the same way as in the inner Galaxy. We investigate the population of NGC 1893, a young cluster (~3-4Myr) in the outer part of the Galaxy (galactic radius &gt;11kpc) in order to explore the effects of environmental conditions on star forming regions. We present the infrared observations obtained with the IRAC camera on board of the Spitzer Space Telescope and analyze the color-color diagrams to establish the membership of stars with excesses. We also merge this information with that obtained from Chandra ACIS-I observations, in order to identify the Class III population. We find that the cluster is very rich, with 242 PMS Classical T-Tauri stars and 7 Class 0/I stars. Moreover we identify 110 Class III candidate cluster members in the ACIS-I field of view. We estimate a disk fraction for NGC 1893 of about 67%, similar to fraction calculated for nearby star forming regions of the same age. Although the environmental conditions are not favorable, star formation can clearly be very successful in the outer Galaxy, allowing creation of a very rich cluster like NGC 1893.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211#1</TD>
            <TD>2011-09-14T20:27:40Z</TD>
            <TD>#Open_Clusters#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/488/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/488/211 [2]</TD>
            <TD>Infrated photometry of NGC 1893 (Caramazza+, 2008)</TD>
            <TD>The independence of the star formation processes with respect to the environmental conditions is controversial. In particular it is not clear whether star formation in the outer Galaxy, where the environmental conditions are, theoretically, less conducive, occurs in the same way as in the inner Galaxy. We investigate the population of NGC 1893, a young cluster (~3-4Myr) in the outer part of the Galaxy (galactic radius &gt;11kpc) in order to explore the effects of environmental conditions on star forming regions. We present the infrared observations obtained with the IRAC camera on board of the Spitzer Space Telescope and analyze the color-color diagrams to establish the membership of stars with excesses. We also merge this information with that obtained from Chandra ACIS-I observations, in order to identify the Class III population. We find that the cluster is very rich, with 242 PMS Classical T-Tauri stars and 7 Class 0/I stars. Moreover we identify 110 Class III candidate cluster members in the ACIS-I field of view. We estimate a disk fraction for NGC 1893 of about 67%, similar to fraction calculated for nearby star forming regions of the same age. Although the environmental conditions are not favorable, star formation can clearly be very successful in the outer Galaxy, allowing creation of a very rich cluster like NGC 1893.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211#2</TD>
            <TD>2011-09-14T20:27:40Z</TD>
            <TD>#Open_Clusters#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/488/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/488/211 [table1]</TD>
            <TD>Infrated photometry of NGC 1893 (Caramazza+, 2008)</TD>
            <TD>The independence of the star formation processes with respect to the environmental conditions is controversial. In particular it is not clear whether star formation in the outer Galaxy, where the environmental conditions are, theoretically, less conducive, occurs in the same way as in the inner Galaxy. We investigate the population of NGC 1893, a young cluster (~3-4Myr) in the outer part of the Galaxy (galactic radius &gt;11kpc) in order to explore the effects of environmental conditions on star forming regions. We present the infrared observations obtained with the IRAC camera on board of the Spitzer Space Telescope and analyze the color-color diagrams to establish the membership of stars with excesses. We also merge this information with that obtained from Chandra ACIS-I observations, in order to identify the Class III population. We find that the cluster is very rich, with 242 PMS Classical T-Tauri stars and 7 Class 0/I stars. Moreover we identify 110 Class III candidate cluster members in the ACIS-I field of view. We estimate a disk fraction for NGC 1893 of about 67%, similar to fraction calculated for nearby star forming regions of the same age. Although the environmental conditions are not favorable, star formation can clearly be very successful in the outer Galaxy, allowing creation of a very rich cluster like NGC 1893.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211#table1</TD>
            <TD>2011-09-14T20:27:40Z</TD>
            <TD>#Open_Clusters#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/488/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/211</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/178/1 [1]</TD>
            <TD>Distribution of HII regions in disk galaxies (Sanchez+, 2008)</TD>
            <TD>We have compiled literature data for positions of HII regions in external galaxies. Here we present the set of HII region catalogues for a sample of 101 disk galaxies (93 spirals and 8 irregulars). For each galaxy several properties are given including the calculated fractal (correlation) dimension of the distribution of HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1#1</TD>
            <TD>2011-09-14T20:29:36Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/178/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/178/1 [2]</TD>
            <TD>Distribution of HII regions in disk galaxies (Sanchez+, 2008)</TD>
            <TD>We have compiled literature data for positions of HII regions in external galaxies. Here we present the set of HII region catalogues for a sample of 101 disk galaxies (93 spirals and 8 irregulars). For each galaxy several properties are given including the calculated fractal (correlation) dimension of the distribution of HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1#2</TD>
            <TD>2011-09-14T20:29:36Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/178/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/1 [galaxies]</TD>
            <TD>Distribution of HII regions in disk galaxies (Sanchez+, 2008)</TD>
            <TD>We have compiled literature data for positions of HII regions in external galaxies. Here we present the set of HII region catalogues for a sample of 101 disk galaxies (93 spirals and 8 irregulars). For each galaxy several properties are given including the calculated fractal (correlation) dimension of the distribution of HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1#galaxies</TD>
            <TD>2011-09-14T20:29:36Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/399/1083 [1]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#1</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/399/1083</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/399/1083 [2]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#2</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/399/1083&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/1083 [table1]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#table1</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/1083&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/1083 [table2]</TD>
            <TD>Outer Galaxy IRAS sources and 12CO emission (Kerton+, 2003)</TD>
            <TD>We examined all of the IRAS sources within the Five College Radio Astronomy Observatory (FCRAO) Outer Galaxy Survey (OGS) region for associated ^12^CO emission (as accounted for in the Brunt, Kerton, and Pomerleau (2003, in press) catalogue of ^12^CO emission in the OGS). Table 1 provides a ranked listing of IRAS-CO associations and Table 2 provides a listing of those IRAS sources with no CO associations. In order to rank the various IRAS-CO associations we examined the association of random lines of sight with CO emission in the OGS. The resulting expectation numbers are provided to the reader in Table A1.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083#table2</TD>
            <TD>2012-09-24T08:33:52Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/1083</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/1083&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/1083</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/479/1 [1]</TD>
            <TD>Redshifts and morphology in A3667 (Johnston-Hollitt+, 2008)</TD>
            <TD>Spectroscopic redshifts for 143 galaxies found in the cluster A3667 and falling in the redshift range 0.044&lt;z&lt;0.068. For each galaxy we give the catalogue ID, Right ascension and Declination in J2000 coordinates, the blue magnitude, the redshift determined by absorption, the redshift determined by emission, the average redshift between absorption and emission features, any previously published spectroscopic redshift value and finally the morphological type determined by the best correlation to the spectral templates listed in Colless et al. (2001MNRAS.328.1039C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1#1</TD>
            <TD>2011-09-14T20:28:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/479/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/479/1 [2]</TD>
            <TD>Redshifts and morphology in A3667 (Johnston-Hollitt+, 2008)</TD>
            <TD>Spectroscopic redshifts for 143 galaxies found in the cluster A3667 and falling in the redshift range 0.044&lt;z&lt;0.068. For each galaxy we give the catalogue ID, Right ascension and Declination in J2000 coordinates, the blue magnitude, the redshift determined by absorption, the redshift determined by emission, the average redshift between absorption and emission features, any previously published spectroscopic redshift value and finally the morphological type determined by the best correlation to the spectral templates listed in Colless et al. (2001MNRAS.328.1039C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1#2</TD>
            <TD>2011-09-14T20:28:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/479/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/479/1 [table2]</TD>
            <TD>Redshifts and morphology in A3667 (Johnston-Hollitt+, 2008)</TD>
            <TD>Spectroscopic redshifts for 143 galaxies found in the cluster A3667 and falling in the redshift range 0.044&lt;z&lt;0.068. For each galaxy we give the catalogue ID, Right ascension and Declination in J2000 coordinates, the blue magnitude, the redshift determined by absorption, the redshift determined by emission, the average redshift between absorption and emission features, any previously published spectroscopic redshift value and finally the morphological type determined by the best correlation to the spectral templates listed in Colless et al. (2001MNRAS.328.1039C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1#table2</TD>
            <TD>2011-09-14T20:28:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/479/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/178/1 [1]</TD>
            <TD>Distribution of HII regions in disk galaxies (Sanchez+, 2008)</TD>
            <TD>We have compiled literature data for positions of HII regions in external galaxies. Here we present the set of HII region catalogues for a sample of 101 disk galaxies (93 spirals and 8 irregulars). For each galaxy several properties are given including the calculated fractal (correlation) dimension of the distribution of HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1#1</TD>
            <TD>2011-09-14T20:29:36Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/178/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/178/1 [2]</TD>
            <TD>Distribution of HII regions in disk galaxies (Sanchez+, 2008)</TD>
            <TD>We have compiled literature data for positions of HII regions in external galaxies. Here we present the set of HII region catalogues for a sample of 101 disk galaxies (93 spirals and 8 irregulars). For each galaxy several properties are given including the calculated fractal (correlation) dimension of the distribution of HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1#2</TD>
            <TD>2011-09-14T20:29:36Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/178/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/1 [galaxies]</TD>
            <TD>Distribution of HII regions in disk galaxies (Sanchez+, 2008)</TD>
            <TD>We have compiled literature data for positions of HII regions in external galaxies. Here we present the set of HII region catalogues for a sample of 101 disk galaxies (93 spirals and 8 irregulars). For each galaxy several properties are given including the calculated fractal (correlation) dimension of the distribution of HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1#galaxies</TD>
            <TD>2011-09-14T20:29:36Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/202 [1]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1997)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog &lt;VII/195&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/202#1</TD>
            <TD>2012-09-24T09:01:19Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1997</TD>
            <TD>ivo://CDS.VizieR/VII/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/202</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/202</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/202 [2]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1997)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog &lt;VII/195&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/202#2</TD>
            <TD>2012-09-24T09:01:19Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1997</TD>
            <TD>ivo://CDS.VizieR/VII/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/202&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/202</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/202 [catalog]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1997)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog &lt;VII/195&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/202#catalog</TD>
            <TD>2012-09-24T09:01:19Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1997</TD>
            <TD>ivo://CDS.VizieR/VII/202</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/202&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/202</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/479/1 [1]</TD>
            <TD>Redshifts and morphology in A3667 (Johnston-Hollitt+, 2008)</TD>
            <TD>Spectroscopic redshifts for 143 galaxies found in the cluster A3667 and falling in the redshift range 0.044&lt;z&lt;0.068. For each galaxy we give the catalogue ID, Right ascension and Declination in J2000 coordinates, the blue magnitude, the redshift determined by absorption, the redshift determined by emission, the average redshift between absorption and emission features, any previously published spectroscopic redshift value and finally the morphological type determined by the best correlation to the spectral templates listed in Colless et al. (2001MNRAS.328.1039C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1#1</TD>
            <TD>2011-09-14T20:28:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/479/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/479/1 [2]</TD>
            <TD>Redshifts and morphology in A3667 (Johnston-Hollitt+, 2008)</TD>
            <TD>Spectroscopic redshifts for 143 galaxies found in the cluster A3667 and falling in the redshift range 0.044&lt;z&lt;0.068. For each galaxy we give the catalogue ID, Right ascension and Declination in J2000 coordinates, the blue magnitude, the redshift determined by absorption, the redshift determined by emission, the average redshift between absorption and emission features, any previously published spectroscopic redshift value and finally the morphological type determined by the best correlation to the spectral templates listed in Colless et al. (2001MNRAS.328.1039C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1#2</TD>
            <TD>2011-09-14T20:28:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/479/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/479/1 [table2]</TD>
            <TD>Redshifts and morphology in A3667 (Johnston-Hollitt+, 2008)</TD>
            <TD>Spectroscopic redshifts for 143 galaxies found in the cluster A3667 and falling in the redshift range 0.044&lt;z&lt;0.068. For each galaxy we give the catalogue ID, Right ascension and Declination in J2000 coordinates, the blue magnitude, the redshift determined by absorption, the redshift determined by emission, the average redshift between absorption and emission features, any previously published spectroscopic redshift value and finally the morphological type determined by the best correlation to the spectral templates listed in Colless et al. (2001MNRAS.328.1039C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1#table2</TD>
            <TD>2011-09-14T20:28:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/479/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/178/1 [1]</TD>
            <TD>Distribution of HII regions in disk galaxies (Sanchez+, 2008)</TD>
            <TD>We have compiled literature data for positions of HII regions in external galaxies. Here we present the set of HII region catalogues for a sample of 101 disk galaxies (93 spirals and 8 irregulars). For each galaxy several properties are given including the calculated fractal (correlation) dimension of the distribution of HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1#1</TD>
            <TD>2011-09-14T20:29:36Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/178/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/178/1 [2]</TD>
            <TD>Distribution of HII regions in disk galaxies (Sanchez+, 2008)</TD>
            <TD>We have compiled literature data for positions of HII regions in external galaxies. Here we present the set of HII region catalogues for a sample of 101 disk galaxies (93 spirals and 8 irregulars). For each galaxy several properties are given including the calculated fractal (correlation) dimension of the distribution of HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1#2</TD>
            <TD>2011-09-14T20:29:36Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/178/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/1 [galaxies]</TD>
            <TD>Distribution of HII regions in disk galaxies (Sanchez+, 2008)</TD>
            <TD>We have compiled literature data for positions of HII regions in external galaxies. Here we present the set of HII region catalogues for a sample of 101 disk galaxies (93 spirals and 8 irregulars). For each galaxy several properties are given including the calculated fractal (correlation) dimension of the distribution of HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1#galaxies</TD>
            <TD>2011-09-14T20:29:36Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2166 [1]</TD>
            <TD>Variables in Sextans dSph galaxy (Mateo+ 1995)</TD>
            <TD>We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166#1</TD>
            <TD>2011-09-14T18:22:13Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2166</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2166</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2166 [2]</TD>
            <TD>Variables in Sextans dSph galaxy (Mateo+ 1995)</TD>
            <TD>We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166#2</TD>
            <TD>2011-09-14T18:22:13Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2166&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2166</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2166 [table10]</TD>
            <TD>Variables in Sextans dSph galaxy (Mateo+ 1995)</TD>
            <TD>We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166#table10</TD>
            <TD>2011-09-14T18:22:13Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2166&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2166</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/479/1 [1]</TD>
            <TD>Redshifts and morphology in A3667 (Johnston-Hollitt+, 2008)</TD>
            <TD>Spectroscopic redshifts for 143 galaxies found in the cluster A3667 and falling in the redshift range 0.044&lt;z&lt;0.068. For each galaxy we give the catalogue ID, Right ascension and Declination in J2000 coordinates, the blue magnitude, the redshift determined by absorption, the redshift determined by emission, the average redshift between absorption and emission features, any previously published spectroscopic redshift value and finally the morphological type determined by the best correlation to the spectral templates listed in Colless et al. (2001MNRAS.328.1039C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1#1</TD>
            <TD>2011-09-14T20:28:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/479/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/479/1 [2]</TD>
            <TD>Redshifts and morphology in A3667 (Johnston-Hollitt+, 2008)</TD>
            <TD>Spectroscopic redshifts for 143 galaxies found in the cluster A3667 and falling in the redshift range 0.044&lt;z&lt;0.068. For each galaxy we give the catalogue ID, Right ascension and Declination in J2000 coordinates, the blue magnitude, the redshift determined by absorption, the redshift determined by emission, the average redshift between absorption and emission features, any previously published spectroscopic redshift value and finally the morphological type determined by the best correlation to the spectral templates listed in Colless et al. (2001MNRAS.328.1039C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1#2</TD>
            <TD>2011-09-14T20:28:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/479/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/479/1 [table2]</TD>
            <TD>Redshifts and morphology in A3667 (Johnston-Hollitt+, 2008)</TD>
            <TD>Spectroscopic redshifts for 143 galaxies found in the cluster A3667 and falling in the redshift range 0.044&lt;z&lt;0.068. For each galaxy we give the catalogue ID, Right ascension and Declination in J2000 coordinates, the blue magnitude, the redshift determined by absorption, the redshift determined by emission, the average redshift between absorption and emission features, any previously published spectroscopic redshift value and finally the morphological type determined by the best correlation to the spectral templates listed in Colless et al. (2001MNRAS.328.1039C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1#table2</TD>
            <TD>2011-09-14T20:28:10Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Aug-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/479/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/490/945 [1]</TD>
            <TD>Redshifs of galaxies in 23 EIS fields (Grove+, 2008)</TD>
            <TD>We have carried out a spectroscopic survey of low-redshift galaxy systems identified by the matched-filter technique in a moderately deep I-band survey. We present new redshifts for 747 galaxies in 23 ESO Imaging Survey (EIS) cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space for identifying groups/clusters of galaxies corresponding to the original EIS matched-filter cluster candidates. In this way we spectroscopically confirm systems in 10 of the 23 cluster candidate fields with a matched-filter estimated redshift z_MF_=0.3-0.4 and with spectroscopic redshifts in the range from z=0.158 to z=0.534, with the observations favouring the confirmation of systems at the lower redshift end. After careful analysis of the redshift distribution, one system was split into two very close clumps in redshift space. We find that the systems identified in the present paper span a broad range of velocity dispersion and richness. The measured one-dimensional velocity dispersion range from 175km/s to 497km/s, consistent with the values obtained in previous papers using much larger samples for systems over the same redshift range. Both undersampling and contamination by substructures contribute to the uncertainty of these measurements. The richness range corresponds to clusters with an estimated total luminosity in the range 12L^*^-65L^*^, but these estimates are very uncertain as are their relation to the velocity dispersion (mass) of the systems. From the analysis of the colours of the galaxy populations we find that ~60% of the spectroscopically confirmed systems have a "significant" red sequence. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions. With this paper we complete our spectroscopic survey of the fields of 58 EIS cluster candidates with estimated redshifts z&lt;=0.4 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;, Olsen et al., 2005, Cat. &lt;J/A+A/435/781&gt;). We have measured a total of 1954 galaxy redshifts in the range z=0.0065 to z=0.6706. Of the 58 systems we confirm 42 (~75%) with redshifts between z=0.095 and z=0.534.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945#1</TD>
            <TD>2011-09-14T20:31:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/490/945</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/490/945</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/490/945 [2]</TD>
            <TD>Redshifs of galaxies in 23 EIS fields (Grove+, 2008)</TD>
            <TD>We have carried out a spectroscopic survey of low-redshift galaxy systems identified by the matched-filter technique in a moderately deep I-band survey. We present new redshifts for 747 galaxies in 23 ESO Imaging Survey (EIS) cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space for identifying groups/clusters of galaxies corresponding to the original EIS matched-filter cluster candidates. In this way we spectroscopically confirm systems in 10 of the 23 cluster candidate fields with a matched-filter estimated redshift z_MF_=0.3-0.4 and with spectroscopic redshifts in the range from z=0.158 to z=0.534, with the observations favouring the confirmation of systems at the lower redshift end. After careful analysis of the redshift distribution, one system was split into two very close clumps in redshift space. We find that the systems identified in the present paper span a broad range of velocity dispersion and richness. The measured one-dimensional velocity dispersion range from 175km/s to 497km/s, consistent with the values obtained in previous papers using much larger samples for systems over the same redshift range. Both undersampling and contamination by substructures contribute to the uncertainty of these measurements. The richness range corresponds to clusters with an estimated total luminosity in the range 12L^*^-65L^*^, but these estimates are very uncertain as are their relation to the velocity dispersion (mass) of the systems. From the analysis of the colours of the galaxy populations we find that ~60% of the spectroscopically confirmed systems have a "significant" red sequence. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions. With this paper we complete our spectroscopic survey of the fields of 58 EIS cluster candidates with estimated redshifts z&lt;=0.4 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;, Olsen et al., 2005, Cat. &lt;J/A+A/435/781&gt;). We have measured a total of 1954 galaxy redshifts in the range z=0.0065 to z=0.6706. Of the 58 systems we confirm 42 (~75%) with redshifts between z=0.095 and z=0.534.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945#2</TD>
            <TD>2011-09-14T20:31:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/490/945&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/490/945</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/490/945 [table3]</TD>
            <TD>Redshifs of galaxies in 23 EIS fields (Grove+, 2008)</TD>
            <TD>We have carried out a spectroscopic survey of low-redshift galaxy systems identified by the matched-filter technique in a moderately deep I-band survey. We present new redshifts for 747 galaxies in 23 ESO Imaging Survey (EIS) cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space for identifying groups/clusters of galaxies corresponding to the original EIS matched-filter cluster candidates. In this way we spectroscopically confirm systems in 10 of the 23 cluster candidate fields with a matched-filter estimated redshift z_MF_=0.3-0.4 and with spectroscopic redshifts in the range from z=0.158 to z=0.534, with the observations favouring the confirmation of systems at the lower redshift end. After careful analysis of the redshift distribution, one system was split into two very close clumps in redshift space. We find that the systems identified in the present paper span a broad range of velocity dispersion and richness. The measured one-dimensional velocity dispersion range from 175km/s to 497km/s, consistent with the values obtained in previous papers using much larger samples for systems over the same redshift range. Both undersampling and contamination by substructures contribute to the uncertainty of these measurements. The richness range corresponds to clusters with an estimated total luminosity in the range 12L^*^-65L^*^, but these estimates are very uncertain as are their relation to the velocity dispersion (mass) of the systems. From the analysis of the colours of the galaxy populations we find that ~60% of the spectroscopically confirmed systems have a "significant" red sequence. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions. With this paper we complete our spectroscopic survey of the fields of 58 EIS cluster candidates with estimated redshifts z&lt;=0.4 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;, Olsen et al., 2005, Cat. &lt;J/A+A/435/781&gt;). We have measured a total of 1954 galaxy redshifts in the range z=0.0065 to z=0.6706. Of the 58 systems we confirm 42 (~75%) with redshifts between z=0.095 and z=0.534.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945#table3</TD>
            <TD>2011-09-14T20:31:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/490/945&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/490/945</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/488/1167 [1]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#1</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/488/1167</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/1167</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/488/1167 [2]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#2</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/488/1167&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/1167</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/488/1167 [Bulge]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#Bulge</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/488/1167&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/1167</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/488/1167 [nonBulge]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#nonBulge</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/488/1167&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/1167</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/202 [1]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1997)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog &lt;VII/195&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/202#1</TD>
            <TD>2012-09-24T09:01:19Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1997</TD>
            <TD>ivo://CDS.VizieR/VII/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/202</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/202</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/202 [2]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1997)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog &lt;VII/195&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/202#2</TD>
            <TD>2012-09-24T09:01:19Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1997</TD>
            <TD>ivo://CDS.VizieR/VII/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/202&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/202</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/202 [catalog]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1997)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog &lt;VII/195&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/202#catalog</TD>
            <TD>2012-09-24T09:01:19Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1997</TD>
            <TD>ivo://CDS.VizieR/VII/202</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/202&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/202</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/490/945 [1]</TD>
            <TD>Redshifs of galaxies in 23 EIS fields (Grove+, 2008)</TD>
            <TD>We have carried out a spectroscopic survey of low-redshift galaxy systems identified by the matched-filter technique in a moderately deep I-band survey. We present new redshifts for 747 galaxies in 23 ESO Imaging Survey (EIS) cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space for identifying groups/clusters of galaxies corresponding to the original EIS matched-filter cluster candidates. In this way we spectroscopically confirm systems in 10 of the 23 cluster candidate fields with a matched-filter estimated redshift z_MF_=0.3-0.4 and with spectroscopic redshifts in the range from z=0.158 to z=0.534, with the observations favouring the confirmation of systems at the lower redshift end. After careful analysis of the redshift distribution, one system was split into two very close clumps in redshift space. We find that the systems identified in the present paper span a broad range of velocity dispersion and richness. The measured one-dimensional velocity dispersion range from 175km/s to 497km/s, consistent with the values obtained in previous papers using much larger samples for systems over the same redshift range. Both undersampling and contamination by substructures contribute to the uncertainty of these measurements. The richness range corresponds to clusters with an estimated total luminosity in the range 12L^*^-65L^*^, but these estimates are very uncertain as are their relation to the velocity dispersion (mass) of the systems. From the analysis of the colours of the galaxy populations we find that ~60% of the spectroscopically confirmed systems have a "significant" red sequence. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions. With this paper we complete our spectroscopic survey of the fields of 58 EIS cluster candidates with estimated redshifts z&lt;=0.4 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;, Olsen et al., 2005, Cat. &lt;J/A+A/435/781&gt;). We have measured a total of 1954 galaxy redshifts in the range z=0.0065 to z=0.6706. Of the 58 systems we confirm 42 (~75%) with redshifts between z=0.095 and z=0.534.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945#1</TD>
            <TD>2011-09-14T20:31:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/490/945</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/490/945</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/490/945 [2]</TD>
            <TD>Redshifs of galaxies in 23 EIS fields (Grove+, 2008)</TD>
            <TD>We have carried out a spectroscopic survey of low-redshift galaxy systems identified by the matched-filter technique in a moderately deep I-band survey. We present new redshifts for 747 galaxies in 23 ESO Imaging Survey (EIS) cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space for identifying groups/clusters of galaxies corresponding to the original EIS matched-filter cluster candidates. In this way we spectroscopically confirm systems in 10 of the 23 cluster candidate fields with a matched-filter estimated redshift z_MF_=0.3-0.4 and with spectroscopic redshifts in the range from z=0.158 to z=0.534, with the observations favouring the confirmation of systems at the lower redshift end. After careful analysis of the redshift distribution, one system was split into two very close clumps in redshift space. We find that the systems identified in the present paper span a broad range of velocity dispersion and richness. The measured one-dimensional velocity dispersion range from 175km/s to 497km/s, consistent with the values obtained in previous papers using much larger samples for systems over the same redshift range. Both undersampling and contamination by substructures contribute to the uncertainty of these measurements. The richness range corresponds to clusters with an estimated total luminosity in the range 12L^*^-65L^*^, but these estimates are very uncertain as are their relation to the velocity dispersion (mass) of the systems. From the analysis of the colours of the galaxy populations we find that ~60% of the spectroscopically confirmed systems have a "significant" red sequence. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions. With this paper we complete our spectroscopic survey of the fields of 58 EIS cluster candidates with estimated redshifts z&lt;=0.4 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;, Olsen et al., 2005, Cat. &lt;J/A+A/435/781&gt;). We have measured a total of 1954 galaxy redshifts in the range z=0.0065 to z=0.6706. Of the 58 systems we confirm 42 (~75%) with redshifts between z=0.095 and z=0.534.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945#2</TD>
            <TD>2011-09-14T20:31:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/490/945&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/490/945</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/490/945 [table3]</TD>
            <TD>Redshifs of galaxies in 23 EIS fields (Grove+, 2008)</TD>
            <TD>We have carried out a spectroscopic survey of low-redshift galaxy systems identified by the matched-filter technique in a moderately deep I-band survey. We present new redshifts for 747 galaxies in 23 ESO Imaging Survey (EIS) cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space for identifying groups/clusters of galaxies corresponding to the original EIS matched-filter cluster candidates. In this way we spectroscopically confirm systems in 10 of the 23 cluster candidate fields with a matched-filter estimated redshift z_MF_=0.3-0.4 and with spectroscopic redshifts in the range from z=0.158 to z=0.534, with the observations favouring the confirmation of systems at the lower redshift end. After careful analysis of the redshift distribution, one system was split into two very close clumps in redshift space. We find that the systems identified in the present paper span a broad range of velocity dispersion and richness. The measured one-dimensional velocity dispersion range from 175km/s to 497km/s, consistent with the values obtained in previous papers using much larger samples for systems over the same redshift range. Both undersampling and contamination by substructures contribute to the uncertainty of these measurements. The richness range corresponds to clusters with an estimated total luminosity in the range 12L^*^-65L^*^, but these estimates are very uncertain as are their relation to the velocity dispersion (mass) of the systems. From the analysis of the colours of the galaxy populations we find that ~60% of the spectroscopically confirmed systems have a "significant" red sequence. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions. With this paper we complete our spectroscopic survey of the fields of 58 EIS cluster candidates with estimated redshifts z&lt;=0.4 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;, Olsen et al., 2005, Cat. &lt;J/A+A/435/781&gt;). We have measured a total of 1954 galaxy redshifts in the range z=0.0065 to z=0.6706. Of the 58 systems we confirm 42 (~75%) with redshifts between z=0.095 and z=0.534.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945#table3</TD>
            <TD>2011-09-14T20:31:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/490/945&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/490/945</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/110/2166 [1]</TD>
            <TD>Variables in Sextans dSph galaxy (Mateo+ 1995)</TD>
            <TD>We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166#1</TD>
            <TD>2011-09-14T18:22:13Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/110/2166</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2166</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/110/2166 [2]</TD>
            <TD>Variables in Sextans dSph galaxy (Mateo+ 1995)</TD>
            <TD>We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166#2</TD>
            <TD>2011-09-14T18:22:13Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/110/2166&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2166</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/110/2166 [table10]</TD>
            <TD>Variables in Sextans dSph galaxy (Mateo+ 1995)</TD>
            <TD>We describe a survey for variable stars in the Sextans dwarf spheroidal (dSph) galaxy based on the analysis of 113 B and 48 V CCD images of four fields covering a total area of 18'x18'. We have identified 44 variables: 36 RR Lyr star, 6 anomalous Cepheids, one long-period red variable, all probable members of Sextans, and one foreground contact binary. We have used the pulsating stars to derive a true distance modulus of 19.67+/-0.15 for Sextans (or D=86+/-6kpc), where the error is primarily due to uncertainties in the luminosity-metallicity relation for RR Lyr stars. Based on our new data we conclude that [Fe/H]_Sex=-1.6+/-0.2, somewhat higher than the value from Suntzeff et al. (1993ApJ...418..208S) obtained from the analysis of fiber spectroscopy of the near-IR Calcium triplet. We present a new deep color-magnitude diagram for Sextans which reveals the presence of anomalous Cepheids in the galaxy. This young population may represent as much as 25% of the total stellar content of Sextans. We find a surprisingly strong correlation between the frequency of anomalous Cepheids in dSph galaxies and galaxian luminosity and speculate on the possible origin of this strange effect. The RR Lyr stars in Sextans do not exhibit the Oosterhoff dichotomy observed in globular clusters and in the Galactic halo field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166#table10</TD>
            <TD>2011-09-14T18:22:13Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/110/2166</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/110/2166&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/110/2166</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/202 [1]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1997)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog &lt;VII/195&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/202#1</TD>
            <TD>2012-09-24T09:01:19Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1997</TD>
            <TD>ivo://CDS.VizieR/VII/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/202</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/202</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/202 [2]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1997)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog &lt;VII/195&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/202#2</TD>
            <TD>2012-09-24T09:01:19Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1997</TD>
            <TD>ivo://CDS.VizieR/VII/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/202&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/202</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/202 [catalog]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1997)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 147 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: May 15, 1997, and supersedes the previous version (Catalog &lt;VII/195&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/202#catalog</TD>
            <TD>2012-09-24T09:01:19Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1997</TD>
            <TD>ivo://CDS.VizieR/VII/202</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/202&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/202</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/490/945 [1]</TD>
            <TD>Redshifs of galaxies in 23 EIS fields (Grove+, 2008)</TD>
            <TD>We have carried out a spectroscopic survey of low-redshift galaxy systems identified by the matched-filter technique in a moderately deep I-band survey. We present new redshifts for 747 galaxies in 23 ESO Imaging Survey (EIS) cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space for identifying groups/clusters of galaxies corresponding to the original EIS matched-filter cluster candidates. In this way we spectroscopically confirm systems in 10 of the 23 cluster candidate fields with a matched-filter estimated redshift z_MF_=0.3-0.4 and with spectroscopic redshifts in the range from z=0.158 to z=0.534, with the observations favouring the confirmation of systems at the lower redshift end. After careful analysis of the redshift distribution, one system was split into two very close clumps in redshift space. We find that the systems identified in the present paper span a broad range of velocity dispersion and richness. The measured one-dimensional velocity dispersion range from 175km/s to 497km/s, consistent with the values obtained in previous papers using much larger samples for systems over the same redshift range. Both undersampling and contamination by substructures contribute to the uncertainty of these measurements. The richness range corresponds to clusters with an estimated total luminosity in the range 12L^*^-65L^*^, but these estimates are very uncertain as are their relation to the velocity dispersion (mass) of the systems. From the analysis of the colours of the galaxy populations we find that ~60% of the spectroscopically confirmed systems have a "significant" red sequence. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions. With this paper we complete our spectroscopic survey of the fields of 58 EIS cluster candidates with estimated redshifts z&lt;=0.4 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;, Olsen et al., 2005, Cat. &lt;J/A+A/435/781&gt;). We have measured a total of 1954 galaxy redshifts in the range z=0.0065 to z=0.6706. Of the 58 systems we confirm 42 (~75%) with redshifts between z=0.095 and z=0.534.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945#1</TD>
            <TD>2011-09-14T20:31:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/490/945</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/490/945</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/490/945 [2]</TD>
            <TD>Redshifs of galaxies in 23 EIS fields (Grove+, 2008)</TD>
            <TD>We have carried out a spectroscopic survey of low-redshift galaxy systems identified by the matched-filter technique in a moderately deep I-band survey. We present new redshifts for 747 galaxies in 23 ESO Imaging Survey (EIS) cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space for identifying groups/clusters of galaxies corresponding to the original EIS matched-filter cluster candidates. In this way we spectroscopically confirm systems in 10 of the 23 cluster candidate fields with a matched-filter estimated redshift z_MF_=0.3-0.4 and with spectroscopic redshifts in the range from z=0.158 to z=0.534, with the observations favouring the confirmation of systems at the lower redshift end. After careful analysis of the redshift distribution, one system was split into two very close clumps in redshift space. We find that the systems identified in the present paper span a broad range of velocity dispersion and richness. The measured one-dimensional velocity dispersion range from 175km/s to 497km/s, consistent with the values obtained in previous papers using much larger samples for systems over the same redshift range. Both undersampling and contamination by substructures contribute to the uncertainty of these measurements. The richness range corresponds to clusters with an estimated total luminosity in the range 12L^*^-65L^*^, but these estimates are very uncertain as are their relation to the velocity dispersion (mass) of the systems. From the analysis of the colours of the galaxy populations we find that ~60% of the spectroscopically confirmed systems have a "significant" red sequence. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions. With this paper we complete our spectroscopic survey of the fields of 58 EIS cluster candidates with estimated redshifts z&lt;=0.4 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;, Olsen et al., 2005, Cat. &lt;J/A+A/435/781&gt;). We have measured a total of 1954 galaxy redshifts in the range z=0.0065 to z=0.6706. Of the 58 systems we confirm 42 (~75%) with redshifts between z=0.095 and z=0.534.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945#2</TD>
            <TD>2011-09-14T20:31:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/490/945&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/490/945</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/490/945 [table3]</TD>
            <TD>Redshifs of galaxies in 23 EIS fields (Grove+, 2008)</TD>
            <TD>We have carried out a spectroscopic survey of low-redshift galaxy systems identified by the matched-filter technique in a moderately deep I-band survey. We present new redshifts for 747 galaxies in 23 ESO Imaging Survey (EIS) cluster fields. We use the "gap"-technique to search for significant overdensities in redshift space for identifying groups/clusters of galaxies corresponding to the original EIS matched-filter cluster candidates. In this way we spectroscopically confirm systems in 10 of the 23 cluster candidate fields with a matched-filter estimated redshift z_MF_=0.3-0.4 and with spectroscopic redshifts in the range from z=0.158 to z=0.534, with the observations favouring the confirmation of systems at the lower redshift end. After careful analysis of the redshift distribution, one system was split into two very close clumps in redshift space. We find that the systems identified in the present paper span a broad range of velocity dispersion and richness. The measured one-dimensional velocity dispersion range from 175km/s to 497km/s, consistent with the values obtained in previous papers using much larger samples for systems over the same redshift range. Both undersampling and contamination by substructures contribute to the uncertainty of these measurements. The richness range corresponds to clusters with an estimated total luminosity in the range 12L^*^-65L^*^, but these estimates are very uncertain as are their relation to the velocity dispersion (mass) of the systems. From the analysis of the colours of the galaxy populations we find that ~60% of the spectroscopically confirmed systems have a "significant" red sequence. We find that the colour of the red sequence galaxies matches passive stellar evolution predictions. With this paper we complete our spectroscopic survey of the fields of 58 EIS cluster candidates with estimated redshifts z&lt;=0.4 (see also Hansen et al., 2002, Cat. &lt;J/A+A/388/1&gt;; Olsen et al., 2003, Cat. &lt;J/A+A/409/439&gt;, Olsen et al., 2005, Cat. &lt;J/A+A/435/781&gt;). We have measured a total of 1954 galaxy redshifts in the range z=0.0065 to z=0.6706. Of the 58 systems we confirm 42 (~75%) with redshifts between z=0.095 and z=0.534.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945#table3</TD>
            <TD>2011-09-14T20:31:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/490/945</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/490/945&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/490/945</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/499/357 [1]</TD>
            <TD>REFLEX galaxies redshifts (Guzzo+, 2009)</TD>
            <TD>We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalogue of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination +2.50{deg} and at high galactic latitude (|b|&lt;20{deg}). The full survey includes 447 galaxy clusters with a median redshift of 0.08 and is better than 90% complete to a limiting flux of f_X_=3x10^-12^ergs/s/cm^2^ (3fW/m^2^, 0.1 to 2.4keV), representing the largest statistically homogeneous sample of clusters to date drawn from the ROSAT All-Sky Survey (RASS). Here we describe the details of the spectroscopic observations carried out at the ESO 1.5m, 2.2m and 3.6m telescopes, the data reduction and redshift measurements techniques. The spectra typically cover the wavelength range 3600-7500{AA} at a two-pixel resolution of ~14{AA} . From calibrations and external checks the redshifts are accurate to a typical rms error of +/-100km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357#1</TD>
            <TD>2011-09-14T21:08:30Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/499/357</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/499/357</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/499/357 [2]</TD>
            <TD>REFLEX galaxies redshifts (Guzzo+, 2009)</TD>
            <TD>We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalogue of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination +2.50{deg} and at high galactic latitude (|b|&lt;20{deg}). The full survey includes 447 galaxy clusters with a median redshift of 0.08 and is better than 90% complete to a limiting flux of f_X_=3x10^-12^ergs/s/cm^2^ (3fW/m^2^, 0.1 to 2.4keV), representing the largest statistically homogeneous sample of clusters to date drawn from the ROSAT All-Sky Survey (RASS). Here we describe the details of the spectroscopic observations carried out at the ESO 1.5m, 2.2m and 3.6m telescopes, the data reduction and redshift measurements techniques. The spectra typically cover the wavelength range 3600-7500{AA} at a two-pixel resolution of ~14{AA} . From calibrations and external checks the redshifts are accurate to a typical rms error of +/-100km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357#2</TD>
            <TD>2011-09-14T21:08:30Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/499/357&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/499/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/499/357 [table2]</TD>
            <TD>REFLEX galaxies redshifts (Guzzo+, 2009)</TD>
            <TD>We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalogue of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination +2.50{deg} and at high galactic latitude (|b|&lt;20{deg}). The full survey includes 447 galaxy clusters with a median redshift of 0.08 and is better than 90% complete to a limiting flux of f_X_=3x10^-12^ergs/s/cm^2^ (3fW/m^2^, 0.1 to 2.4keV), representing the largest statistically homogeneous sample of clusters to date drawn from the ROSAT All-Sky Survey (RASS). Here we describe the details of the spectroscopic observations carried out at the ESO 1.5m, 2.2m and 3.6m telescopes, the data reduction and redshift measurements techniques. The spectra typically cover the wavelength range 3600-7500{AA} at a two-pixel resolution of ~14{AA} . From calibrations and external checks the redshifts are accurate to a typical rms error of +/-100km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357#table2</TD>
            <TD>2011-09-14T21:08:30Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357</TD>
            <TD>ConeSearch</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/111/696 [1]</TD>
            <TD>Rotation curves of Seyfert galaxies with companions (Keel 1996)</TD>
            <TD>This paper presents imaging and optical spectroscopy of paired Seyfert galaxies and their companions. The aim is to seek common properties of Seyfert galaxies in interacting systems, which might provide evidence of AGN triggering in a way independent of the usual two-sample statistics which have proven ambiguous on this issue. Three kinds of comparison have been made -- the kinds of interactions involving Seyfert galaxies, the relative luminosities of the Seyferts and their companions, and the level of kinematic disturbance as measured from rotation curves. (1) Dynamics and tidal features have been used to determine (or at least limit) the sense of orbital motion (direct/ retrograde/polar with respect to the Seyfert galaxy's disk) for many of these pairs. There is no obviously preferred kind of interaction -- direct, polar, and retrograde encounters are all well represented, despite the gross differences in dynamical response of a disk to these various kinds of encounter. To the extent that triggering of Seyfert nuclei occurs due to tidal encounters, the existence of a perturbation seems more important than its exact duration or detailed effects on the disk. However, the ratio of merging to paired Seyferts is higher than for disk galaxies in general, consistent with more effective triggering of AGN in this specific phase; the implied time scale for enhanced occurrence during mergers is the same as the timescape for merger remnants to appear as such, a few disk-edge crossing times (typically several times 10^8yr). (2) Seyfert nuclei occur preferentially in the brighter members of galaxy pairs, by a median of 0.93mag after making the maximal correction for contaminating nonstellar light in the nuclei. Only about 1/3 of this effect can be accounted for by the known tendency of Seyfert nuclei to occur in more luminous galaxies. Enhancement of AGN by interactions is evidently more effective for more luminous galaxies (though this will also be the case if both star formation and AGN occurrence are enhanced in the same galaxies). (3) The rotation curves of the paired Seyferts show systematically small regions of rising or solid-body rotation compared to the disk radius, as a group comparable to Sa but very different from Sb or Sc galaxies (even for Seyfert galaxies with Hubble type later than Sa). There is weak evidence that this difference is also present with respect to more isolated Seyfert galaxies. Despite the obvious utility of a dynamically disturbed disk for transport of angular momentum and "feeding the monster," Seyfert galaxies in pairs actually have smaller kinematic disturbances (measured by the maximum departure from a symmetric rotation curve, normalized to the full rotation amplitude) than found in a complete sample of non-Seyfert spirals in pairs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/111/696#1</TD>
            <TD>2011-09-14T18:22:26Z</TD>
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            <TD>#Research#</TD>
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            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/111/696</TD>
            <TD />
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            <TD>WebBrowser</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/111/696</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/111/696 [2]</TD>
            <TD>Rotation curves of Seyfert galaxies with companions (Keel 1996)</TD>
            <TD>This paper presents imaging and optical spectroscopy of paired Seyfert galaxies and their companions. The aim is to seek common properties of Seyfert galaxies in interacting systems, which might provide evidence of AGN triggering in a way independent of the usual two-sample statistics which have proven ambiguous on this issue. Three kinds of comparison have been made -- the kinds of interactions involving Seyfert galaxies, the relative luminosities of the Seyferts and their companions, and the level of kinematic disturbance as measured from rotation curves. (1) Dynamics and tidal features have been used to determine (or at least limit) the sense of orbital motion (direct/ retrograde/polar with respect to the Seyfert galaxy's disk) for many of these pairs. There is no obviously preferred kind of interaction -- direct, polar, and retrograde encounters are all well represented, despite the gross differences in dynamical response of a disk to these various kinds of encounter. To the extent that triggering of Seyfert nuclei occurs due to tidal encounters, the existence of a perturbation seems more important than its exact duration or detailed effects on the disk. However, the ratio of merging to paired Seyferts is higher than for disk galaxies in general, consistent with more effective triggering of AGN in this specific phase; the implied time scale for enhanced occurrence during mergers is the same as the timescape for merger remnants to appear as such, a few disk-edge crossing times (typically several times 10^8yr). (2) Seyfert nuclei occur preferentially in the brighter members of galaxy pairs, by a median of 0.93mag after making the maximal correction for contaminating nonstellar light in the nuclei. Only about 1/3 of this effect can be accounted for by the known tendency of Seyfert nuclei to occur in more luminous galaxies. Enhancement of AGN by interactions is evidently more effective for more luminous galaxies (though this will also be the case if both star formation and AGN occurrence are enhanced in the same galaxies). (3) The rotation curves of the paired Seyferts show systematically small regions of rising or solid-body rotation compared to the disk radius, as a group comparable to Sa but very different from Sb or Sc galaxies (even for Seyfert galaxies with Hubble type later than Sa). There is weak evidence that this difference is also present with respect to more isolated Seyfert galaxies. Despite the obvious utility of a dynamically disturbed disk for transport of angular momentum and "feeding the monster," Seyfert galaxies in pairs actually have smaller kinematic disturbances (measured by the maximum departure from a symmetric rotation curve, normalized to the full rotation amplitude) than found in a complete sample of non-Seyfert spirals in pairs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/111/696#2</TD>
            <TD>2011-09-14T18:22:26Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/111/696</TD>
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            <TD>ParamHTTP</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/111/696</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/499/357 [1]</TD>
            <TD>REFLEX galaxies redshifts (Guzzo+, 2009)</TD>
            <TD>We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalogue of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination +2.50{deg} and at high galactic latitude (|b|&lt;20{deg}). The full survey includes 447 galaxy clusters with a median redshift of 0.08 and is better than 90% complete to a limiting flux of f_X_=3x10^-12^ergs/s/cm^2^ (3fW/m^2^, 0.1 to 2.4keV), representing the largest statistically homogeneous sample of clusters to date drawn from the ROSAT All-Sky Survey (RASS). Here we describe the details of the spectroscopic observations carried out at the ESO 1.5m, 2.2m and 3.6m telescopes, the data reduction and redshift measurements techniques. The spectra typically cover the wavelength range 3600-7500{AA} at a two-pixel resolution of ~14{AA} . From calibrations and external checks the redshifts are accurate to a typical rms error of +/-100km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357#1</TD>
            <TD>2011-09-14T21:08:30Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357</TD>
            <TD />
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/499/357</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/499/357</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/499/357 [2]</TD>
            <TD>REFLEX galaxies redshifts (Guzzo+, 2009)</TD>
            <TD>We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalogue of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination +2.50{deg} and at high galactic latitude (|b|&lt;20{deg}). The full survey includes 447 galaxy clusters with a median redshift of 0.08 and is better than 90% complete to a limiting flux of f_X_=3x10^-12^ergs/s/cm^2^ (3fW/m^2^, 0.1 to 2.4keV), representing the largest statistically homogeneous sample of clusters to date drawn from the ROSAT All-Sky Survey (RASS). Here we describe the details of the spectroscopic observations carried out at the ESO 1.5m, 2.2m and 3.6m telescopes, the data reduction and redshift measurements techniques. The spectra typically cover the wavelength range 3600-7500{AA} at a two-pixel resolution of ~14{AA} . From calibrations and external checks the redshifts are accurate to a typical rms error of +/-100km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357#2</TD>
            <TD>2011-09-14T21:08:30Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
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            <TD>15-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/499/357&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/499/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/499/357 [table2]</TD>
            <TD>REFLEX galaxies redshifts (Guzzo+, 2009)</TD>
            <TD>We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalogue of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination +2.50{deg} and at high galactic latitude (|b|&lt;20{deg}). The full survey includes 447 galaxy clusters with a median redshift of 0.08 and is better than 90% complete to a limiting flux of f_X_=3x10^-12^ergs/s/cm^2^ (3fW/m^2^, 0.1 to 2.4keV), representing the largest statistically homogeneous sample of clusters to date drawn from the ROSAT All-Sky Survey (RASS). Here we describe the details of the spectroscopic observations carried out at the ESO 1.5m, 2.2m and 3.6m telescopes, the data reduction and redshift measurements techniques. The spectra typically cover the wavelength range 3600-7500{AA} at a two-pixel resolution of ~14{AA} . From calibrations and external checks the redshifts are accurate to a typical rms error of +/-100km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357#table2</TD>
            <TD>2011-09-14T21:08:30Z</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/488/1167 [1]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#1</TD>
            <TD>2011-09-14T20:29:37Z</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD />
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/488/1167</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/1167</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/488/1167 [2]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#2</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/488/1167 [Bulge]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#Bulge</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>Catalog</TD>
            <TD>J/A+A/488/1167 [nonBulge]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#nonBulge</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
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            <TD>04-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/499/357 [1]</TD>
            <TD>REFLEX galaxies redshifts (Guzzo+, 2009)</TD>
            <TD>We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalogue of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination +2.50{deg} and at high galactic latitude (|b|&lt;20{deg}). The full survey includes 447 galaxy clusters with a median redshift of 0.08 and is better than 90% complete to a limiting flux of f_X_=3x10^-12^ergs/s/cm^2^ (3fW/m^2^, 0.1 to 2.4keV), representing the largest statistically homogeneous sample of clusters to date drawn from the ROSAT All-Sky Survey (RASS). Here we describe the details of the spectroscopic observations carried out at the ESO 1.5m, 2.2m and 3.6m telescopes, the data reduction and redshift measurements techniques. The spectra typically cover the wavelength range 3600-7500{AA} at a two-pixel resolution of ~14{AA} . From calibrations and external checks the redshifts are accurate to a typical rms error of +/-100km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357#1</TD>
            <TD>2011-09-14T21:08:30Z</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/499/357</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/499/357</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/499/357 [2]</TD>
            <TD>REFLEX galaxies redshifts (Guzzo+, 2009)</TD>
            <TD>We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalogue of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination +2.50{deg} and at high galactic latitude (|b|&lt;20{deg}). The full survey includes 447 galaxy clusters with a median redshift of 0.08 and is better than 90% complete to a limiting flux of f_X_=3x10^-12^ergs/s/cm^2^ (3fW/m^2^, 0.1 to 2.4keV), representing the largest statistically homogeneous sample of clusters to date drawn from the ROSAT All-Sky Survey (RASS). Here we describe the details of the spectroscopic observations carried out at the ESO 1.5m, 2.2m and 3.6m telescopes, the data reduction and redshift measurements techniques. The spectra typically cover the wavelength range 3600-7500{AA} at a two-pixel resolution of ~14{AA} . From calibrations and external checks the redshifts are accurate to a typical rms error of +/-100km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357#2</TD>
            <TD>2011-09-14T21:08:30Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/499/357&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/499/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/499/357 [table2]</TD>
            <TD>REFLEX galaxies redshifts (Guzzo+, 2009)</TD>
            <TD>We present the final data from the spectroscopic survey of the ROSAT-ESO Flux-Limited X-ray (REFLEX) catalogue of galaxy clusters. The REFLEX survey covers 4.24 steradians (34% of the entire sky) below a declination +2.50{deg} and at high galactic latitude (|b|&lt;20{deg}). The full survey includes 447 galaxy clusters with a median redshift of 0.08 and is better than 90% complete to a limiting flux of f_X_=3x10^-12^ergs/s/cm^2^ (3fW/m^2^, 0.1 to 2.4keV), representing the largest statistically homogeneous sample of clusters to date drawn from the ROSAT All-Sky Survey (RASS). Here we describe the details of the spectroscopic observations carried out at the ESO 1.5m, 2.2m and 3.6m telescopes, the data reduction and redshift measurements techniques. The spectra typically cover the wavelength range 3600-7500{AA} at a two-pixel resolution of ~14{AA} . From calibrations and external checks the redshifts are accurate to a typical rms error of +/-100km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357#table2</TD>
            <TD>2011-09-14T21:08:30Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/499/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/499/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/499/357</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/488/1167 [1]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#1</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/488/1167</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/1167</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/488/1167 [2]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#2</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/488/1167&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/1167</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/488/1167 [Bulge]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#Bulge</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/488/1167&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/1167</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/488/1167 [nonBulge]</TD>
            <TD>Photometry of bulges at intermediate z (Dominguez-Palmero+, 2008)</TD>
            <TD>Analysis of bulges to redshifts of up to z=1 have provided ambiguous results as to whether bulges as a class are old structures akin to elliptical galaxies or younger products of the evolution of their host disks. We aim to define a sample of intermediate-z disk galaxies harbouring central bulges, and a complementary sample of disk galaxies without measurable bulges. We intend to provide colour profiles for both samples, as well as measurements of nuclear, disk, and global colours, which may be used to constrain the relative ages of bulges and disks. We select a diameter-limited sample of galaxies in images from the HST/WFPC2 (Wide-Field Planetary Camera 2 at the Hubble Space Telescope) Groth Strip survey, which is divided into two subsamples of higher and lower inclination to assess the role of dust in the measured quantities. Mergers are visually identified and excluded. We take special care to control the pollution by ellipticals. The bulge sample is defined with a criterion based on nuclear surface brightness excess over the inward extrapolation of the exponential law fitted to the outer regions of the galaxies. We extract colour profiles on the semi-minor axis least affected by dust in the disk, and measure nuclear colours at 0.85kpc from the centre over those profiles. Disk colours are measured on major axis profiles; global colours are obtained from 2.6" diameter apertures. Colour transformations and K-corrections are calculated using SEDs covering bands UBVIJK, from the GOYA photometric survey. We obtain a parent sample containing 248 galaxies with known redshifts, spectroscopic or photometric, spanning 0.1&lt;z&lt;1.2. The bulge subsample comprises 54 galaxies (21.8% of the total), while the subsample with no measureable bulges is 55.2% of the total (137 galaxies). The remainder (23%) is composed of mergers. We list nuclear, disk, and global colours (observed and rest-frame) and magnitudes (apparent and absolute), as well as galaxy colour gradients for the samples with and without bulges, and make them available in electronic format. We also provide images, colour maps, plots of spectral energy distributions, major-axis surface brightness profiles, and minor-axis colour profiles for both samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167#nonBulge</TD>
            <TD>2011-09-14T20:29:37Z</TD>
            <TD>#Photometry#Galaxies#Photometry:surface#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/488/1167</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/488/1167&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/488/1167</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/111/696 [1]</TD>
            <TD>Rotation curves of Seyfert galaxies with companions (Keel 1996)</TD>
            <TD>This paper presents imaging and optical spectroscopy of paired Seyfert galaxies and their companions. The aim is to seek common properties of Seyfert galaxies in interacting systems, which might provide evidence of AGN triggering in a way independent of the usual two-sample statistics which have proven ambiguous on this issue. Three kinds of comparison have been made -- the kinds of interactions involving Seyfert galaxies, the relative luminosities of the Seyferts and their companions, and the level of kinematic disturbance as measured from rotation curves. (1) Dynamics and tidal features have been used to determine (or at least limit) the sense of orbital motion (direct/ retrograde/polar with respect to the Seyfert galaxy's disk) for many of these pairs. There is no obviously preferred kind of interaction -- direct, polar, and retrograde encounters are all well represented, despite the gross differences in dynamical response of a disk to these various kinds of encounter. To the extent that triggering of Seyfert nuclei occurs due to tidal encounters, the existence of a perturbation seems more important than its exact duration or detailed effects on the disk. However, the ratio of merging to paired Seyferts is higher than for disk galaxies in general, consistent with more effective triggering of AGN in this specific phase; the implied time scale for enhanced occurrence during mergers is the same as the timescape for merger remnants to appear as such, a few disk-edge crossing times (typically several times 10^8yr). (2) Seyfert nuclei occur preferentially in the brighter members of galaxy pairs, by a median of 0.93mag after making the maximal correction for contaminating nonstellar light in the nuclei. Only about 1/3 of this effect can be accounted for by the known tendency of Seyfert nuclei to occur in more luminous galaxies. Enhancement of AGN by interactions is evidently more effective for more luminous galaxies (though this will also be the case if both star formation and AGN occurrence are enhanced in the same galaxies). (3) The rotation curves of the paired Seyferts show systematically small regions of rising or solid-body rotation compared to the disk radius, as a group comparable to Sa but very different from Sb or Sc galaxies (even for Seyfert galaxies with Hubble type later than Sa). There is weak evidence that this difference is also present with respect to more isolated Seyfert galaxies. Despite the obvious utility of a dynamically disturbed disk for transport of angular momentum and "feeding the monster," Seyfert galaxies in pairs actually have smaller kinematic disturbances (measured by the maximum departure from a symmetric rotation curve, normalized to the full rotation amplitude) than found in a complete sample of non-Seyfert spirals in pairs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/111/696#1</TD>
            <TD>2011-09-14T18:22:26Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/111/696</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/111/696</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/111/696</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/111/696 [2]</TD>
            <TD>Rotation curves of Seyfert galaxies with companions (Keel 1996)</TD>
            <TD>This paper presents imaging and optical spectroscopy of paired Seyfert galaxies and their companions. The aim is to seek common properties of Seyfert galaxies in interacting systems, which might provide evidence of AGN triggering in a way independent of the usual two-sample statistics which have proven ambiguous on this issue. Three kinds of comparison have been made -- the kinds of interactions involving Seyfert galaxies, the relative luminosities of the Seyferts and their companions, and the level of kinematic disturbance as measured from rotation curves. (1) Dynamics and tidal features have been used to determine (or at least limit) the sense of orbital motion (direct/ retrograde/polar with respect to the Seyfert galaxy's disk) for many of these pairs. There is no obviously preferred kind of interaction -- direct, polar, and retrograde encounters are all well represented, despite the gross differences in dynamical response of a disk to these various kinds of encounter. To the extent that triggering of Seyfert nuclei occurs due to tidal encounters, the existence of a perturbation seems more important than its exact duration or detailed effects on the disk. However, the ratio of merging to paired Seyferts is higher than for disk galaxies in general, consistent with more effective triggering of AGN in this specific phase; the implied time scale for enhanced occurrence during mergers is the same as the timescape for merger remnants to appear as such, a few disk-edge crossing times (typically several times 10^8yr). (2) Seyfert nuclei occur preferentially in the brighter members of galaxy pairs, by a median of 0.93mag after making the maximal correction for contaminating nonstellar light in the nuclei. Only about 1/3 of this effect can be accounted for by the known tendency of Seyfert nuclei to occur in more luminous galaxies. Enhancement of AGN by interactions is evidently more effective for more luminous galaxies (though this will also be the case if both star formation and AGN occurrence are enhanced in the same galaxies). (3) The rotation curves of the paired Seyferts show systematically small regions of rising or solid-body rotation compared to the disk radius, as a group comparable to Sa but very different from Sb or Sc galaxies (even for Seyfert galaxies with Hubble type later than Sa). There is weak evidence that this difference is also present with respect to more isolated Seyfert galaxies. Despite the obvious utility of a dynamically disturbed disk for transport of angular momentum and "feeding the monster," Seyfert galaxies in pairs actually have smaller kinematic disturbances (measured by the maximum departure from a symmetric rotation curve, normalized to the full rotation amplitude) than found in a complete sample of non-Seyfert spirals in pairs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/111/696#2</TD>
            <TD>2011-09-14T18:22:26Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/111/696</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/111/696&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/111/696</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/514/A102 [1]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#1</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/514/A102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/514/A102 [2]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#2</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2f]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2f</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2c]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2c</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2g]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2g</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2i]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2i</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2b]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2b</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2h]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2h</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2a]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2a</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2d]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2d</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2j]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2j</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2e]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2e</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1023 [1]</TD>
            <TD>U-band dropouts in Hubble Ultra Deep Field (Wadadekar+, 2006)</TD>
            <TD>In this paper we analyze the HUDF WFPC2 (F300W) parallels that overlap substantially over the GOODS-S area, i.e., the epoch1-orient 310/314 image (see Fig. 1 of de Mello et al. (2006AJ....131..216D) for a finding chart of this area relative to the GOODS-S field). The other WFPC2 parallel field (epoch 2-orient 40/44) overlaps with the Galaxy Evolution from Morphology and SEDs (Rix et al., 2004ApJS..152..163R) survey area; because of the lack of B-band data this region cannot be studied in the same way and is not considered further in this paper.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023#1</TD>
            <TD>2011-09-14T20:30:07Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1023</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1023</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1023 [2]</TD>
            <TD>U-band dropouts in Hubble Ultra Deep Field (Wadadekar+, 2006)</TD>
            <TD>In this paper we analyze the HUDF WFPC2 (F300W) parallels that overlap substantially over the GOODS-S area, i.e., the epoch1-orient 310/314 image (see Fig. 1 of de Mello et al. (2006AJ....131..216D) for a finding chart of this area relative to the GOODS-S field). The other WFPC2 parallel field (epoch 2-orient 40/44) overlaps with the Galaxy Evolution from Morphology and SEDs (Rix et al., 2004ApJS..152..163R) survey area; because of the lack of B-band data this region cannot be studied in the same way and is not considered further in this paper.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023#2</TD>
            <TD>2011-09-14T20:30:07Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1023&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1023</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1023 [table2]</TD>
            <TD>U-band dropouts in Hubble Ultra Deep Field (Wadadekar+, 2006)</TD>
            <TD>In this paper we analyze the HUDF WFPC2 (F300W) parallels that overlap substantially over the GOODS-S area, i.e., the epoch1-orient 310/314 image (see Fig. 1 of de Mello et al. (2006AJ....131..216D) for a finding chart of this area relative to the GOODS-S field). The other WFPC2 parallel field (epoch 2-orient 40/44) overlaps with the Galaxy Evolution from Morphology and SEDs (Rix et al., 2004ApJS..152..163R) survey area; because of the lack of B-band data this region cannot be studied in the same way and is not considered further in this paper.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023#table2</TD>
            <TD>2011-09-14T20:30:07Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1023&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1023</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/514/A102 [1]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#1</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/514/A102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/514/A102 [2]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#2</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2f]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2f</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2c]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2c</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2g]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2g</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2i]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2i</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2b]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2b</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2h]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2h</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2a]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2a</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2d]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2d</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2j]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2j</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2e]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2e</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/514/A102 [1]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#1</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/514/A102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/514/A102 [2]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#2</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2f]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2f</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2c]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2c</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2g]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2g</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2i]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2i</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2b]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2b</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2h]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2h</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2a]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2a</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2d]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2d</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2j]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2j</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/514/A102 [table2e]</TD>
            <TD>SDSS DR7 groups of galaxies (Tago+, 2010)</TD>
            <TD>We extract groups of galaxies as flux-limited and volume-limited samples from the SDSS Data Release 7 to study the supercluster-void network and environmental properties of groups therein. Volume-limited catalogues are particularly useful for comparison of numerical simulations of dark matter halos and the large-scale structure with observations. Extraction of a volume-limited sample of galaxies and groups requires special care to avoid excluding too much observational data. We use a modified friends-of-friends (FoF) method with a slightly variable linking length to obtain a preliminary flux-limited sample. We use the flux-limited groups as the basic sample to include as many galaxies as possible in the volume-limited samples. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by magnitude dilution of a nearby group sub-sample to follow the properties of groups with higher luminosity limits. Our final flux-limited sample contains 78800 groups, and volume-limited subsamples with absolute magnitude limits M_r_=-18, -19, -20, and -21 contain 5463, 12590, 18973, and 9139 groups, respectively, in the DR7 main galaxy main area survey. The spatial number densities of our groups within the subsamples, as well as the mean sizes and rms velocities of our groups practically do not change from sub-sample to sub-sample. This means that the catalogues are homogeneous and well suited for comparison with simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102#table2e</TD>
            <TD>2011-09-14T21:09:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/514/A102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/514/A102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/514/A102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1023 [1]</TD>
            <TD>U-band dropouts in Hubble Ultra Deep Field (Wadadekar+, 2006)</TD>
            <TD>In this paper we analyze the HUDF WFPC2 (F300W) parallels that overlap substantially over the GOODS-S area, i.e., the epoch1-orient 310/314 image (see Fig. 1 of de Mello et al. (2006AJ....131..216D) for a finding chart of this area relative to the GOODS-S field). The other WFPC2 parallel field (epoch 2-orient 40/44) overlaps with the Galaxy Evolution from Morphology and SEDs (Rix et al., 2004ApJS..152..163R) survey area; because of the lack of B-band data this region cannot be studied in the same way and is not considered further in this paper.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023#1</TD>
            <TD>2011-09-14T20:30:07Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1023</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1023</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1023 [2]</TD>
            <TD>U-band dropouts in Hubble Ultra Deep Field (Wadadekar+, 2006)</TD>
            <TD>In this paper we analyze the HUDF WFPC2 (F300W) parallels that overlap substantially over the GOODS-S area, i.e., the epoch1-orient 310/314 image (see Fig. 1 of de Mello et al. (2006AJ....131..216D) for a finding chart of this area relative to the GOODS-S field). The other WFPC2 parallel field (epoch 2-orient 40/44) overlaps with the Galaxy Evolution from Morphology and SEDs (Rix et al., 2004ApJS..152..163R) survey area; because of the lack of B-band data this region cannot be studied in the same way and is not considered further in this paper.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023#2</TD>
            <TD>2011-09-14T20:30:07Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1023&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1023</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1023 [table2]</TD>
            <TD>U-band dropouts in Hubble Ultra Deep Field (Wadadekar+, 2006)</TD>
            <TD>In this paper we analyze the HUDF WFPC2 (F300W) parallels that overlap substantially over the GOODS-S area, i.e., the epoch1-orient 310/314 image (see Fig. 1 of de Mello et al. (2006AJ....131..216D) for a finding chart of this area relative to the GOODS-S field). The other WFPC2 parallel field (epoch 2-orient 40/44) overlaps with the Galaxy Evolution from Morphology and SEDs (Rix et al., 2004ApJS..152..163R) survey area; because of the lack of B-band data this region cannot be studied in the same way and is not considered further in this paper.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023#table2</TD>
            <TD>2011-09-14T20:30:07Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1023&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1023</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/2455 [1]</TD>
            <TD>Gemini Deep Deep Survey (GDDS) (Abraham+, 2004)</TD>
            <TD>The Gemini Deep Deep Survey (GDDS) is an ultradeep (K&lt;20.6mag, I&lt;24.5mag) redshift survey targeting galaxies in the "redshift desert" between z=1 and z=2. The primary goal of the survey is to constrain the space density at high redshift of evolved high-mass galaxies. We obtained 309 spectra in four widely separated 30-arcmin^2^ fields using the Gemini North telescope and the Gemini Multi-Object Spectrograph (GMOS). The spectra define a one-in-two sparse sample of the reddest and most luminous galaxies near the I-K versus I color-magnitude track mapped out by passively evolving galaxies in the redshift interval 0.8&lt;z&lt;1.8. This sample is augmented by a one-in-seven sparse sample of the remaining high-redshift galaxy population. The GMOS spectrograph was operating in a nod-and-shuffle mode, which enabled us to remove sky contamination with high precision, even for typical exposures times of 20-30hr per field. The resulting spectra are the deepest ever obtained. In this paper we present our sample of 309 spectra, along with redshifts, identifications of spectral features, and photometry. This makes the GDDS the largest and most complete infrared-selected survey probing the redshift desert. The seven-band (VRIz'JHK_s_) photometry is taken from the Las Campanas Infrared Survey (Cat. &lt;VII/228&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455#1</TD>
            <TD>2011-09-14T19:43:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/2455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/2455 [2]</TD>
            <TD>Gemini Deep Deep Survey (GDDS) (Abraham+, 2004)</TD>
            <TD>The Gemini Deep Deep Survey (GDDS) is an ultradeep (K&lt;20.6mag, I&lt;24.5mag) redshift survey targeting galaxies in the "redshift desert" between z=1 and z=2. The primary goal of the survey is to constrain the space density at high redshift of evolved high-mass galaxies. We obtained 309 spectra in four widely separated 30-arcmin^2^ fields using the Gemini North telescope and the Gemini Multi-Object Spectrograph (GMOS). The spectra define a one-in-two sparse sample of the reddest and most luminous galaxies near the I-K versus I color-magnitude track mapped out by passively evolving galaxies in the redshift interval 0.8&lt;z&lt;1.8. This sample is augmented by a one-in-seven sparse sample of the remaining high-redshift galaxy population. The GMOS spectrograph was operating in a nod-and-shuffle mode, which enabled us to remove sky contamination with high precision, even for typical exposures times of 20-30hr per field. The resulting spectra are the deepest ever obtained. In this paper we present our sample of 309 spectra, along with redshifts, identifications of spectral features, and photometry. This makes the GDDS the largest and most complete infrared-selected survey probing the redshift desert. The seven-band (VRIz'JHK_s_) photometry is taken from the Las Campanas Infrared Survey (Cat. &lt;VII/228&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455#2</TD>
            <TD>2011-09-14T19:43:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/2455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2455</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/684/905 [1]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#1</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/684/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/684/905 [2]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#2</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/684/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/905 [table3]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#table3</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/905 [table1]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#table1</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1023 [1]</TD>
            <TD>U-band dropouts in Hubble Ultra Deep Field (Wadadekar+, 2006)</TD>
            <TD>In this paper we analyze the HUDF WFPC2 (F300W) parallels that overlap substantially over the GOODS-S area, i.e., the epoch1-orient 310/314 image (see Fig. 1 of de Mello et al. (2006AJ....131..216D) for a finding chart of this area relative to the GOODS-S field). The other WFPC2 parallel field (epoch 2-orient 40/44) overlaps with the Galaxy Evolution from Morphology and SEDs (Rix et al., 2004ApJS..152..163R) survey area; because of the lack of B-band data this region cannot be studied in the same way and is not considered further in this paper.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023#1</TD>
            <TD>2011-09-14T20:30:07Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1023</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1023</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1023 [2]</TD>
            <TD>U-band dropouts in Hubble Ultra Deep Field (Wadadekar+, 2006)</TD>
            <TD>In this paper we analyze the HUDF WFPC2 (F300W) parallels that overlap substantially over the GOODS-S area, i.e., the epoch1-orient 310/314 image (see Fig. 1 of de Mello et al. (2006AJ....131..216D) for a finding chart of this area relative to the GOODS-S field). The other WFPC2 parallel field (epoch 2-orient 40/44) overlaps with the Galaxy Evolution from Morphology and SEDs (Rix et al., 2004ApJS..152..163R) survey area; because of the lack of B-band data this region cannot be studied in the same way and is not considered further in this paper.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023#2</TD>
            <TD>2011-09-14T20:30:07Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1023&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1023</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1023 [table2]</TD>
            <TD>U-band dropouts in Hubble Ultra Deep Field (Wadadekar+, 2006)</TD>
            <TD>In this paper we analyze the HUDF WFPC2 (F300W) parallels that overlap substantially over the GOODS-S area, i.e., the epoch1-orient 310/314 image (see Fig. 1 of de Mello et al. (2006AJ....131..216D) for a finding chart of this area relative to the GOODS-S field). The other WFPC2 parallel field (epoch 2-orient 40/44) overlaps with the Galaxy Evolution from Morphology and SEDs (Rix et al., 2004ApJS..152..163R) survey area; because of the lack of B-band data this region cannot be studied in the same way and is not considered further in this paper.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023#table2</TD>
            <TD>2011-09-14T20:30:07Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1023</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1023&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1023</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/2455 [1]</TD>
            <TD>Gemini Deep Deep Survey (GDDS) (Abraham+, 2004)</TD>
            <TD>The Gemini Deep Deep Survey (GDDS) is an ultradeep (K&lt;20.6mag, I&lt;24.5mag) redshift survey targeting galaxies in the "redshift desert" between z=1 and z=2. The primary goal of the survey is to constrain the space density at high redshift of evolved high-mass galaxies. We obtained 309 spectra in four widely separated 30-arcmin^2^ fields using the Gemini North telescope and the Gemini Multi-Object Spectrograph (GMOS). The spectra define a one-in-two sparse sample of the reddest and most luminous galaxies near the I-K versus I color-magnitude track mapped out by passively evolving galaxies in the redshift interval 0.8&lt;z&lt;1.8. This sample is augmented by a one-in-seven sparse sample of the remaining high-redshift galaxy population. The GMOS spectrograph was operating in a nod-and-shuffle mode, which enabled us to remove sky contamination with high precision, even for typical exposures times of 20-30hr per field. The resulting spectra are the deepest ever obtained. In this paper we present our sample of 309 spectra, along with redshifts, identifications of spectral features, and photometry. This makes the GDDS the largest and most complete infrared-selected survey probing the redshift desert. The seven-band (VRIz'JHK_s_) photometry is taken from the Las Campanas Infrared Survey (Cat. &lt;VII/228&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455#1</TD>
            <TD>2011-09-14T19:43:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/2455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/2455 [2]</TD>
            <TD>Gemini Deep Deep Survey (GDDS) (Abraham+, 2004)</TD>
            <TD>The Gemini Deep Deep Survey (GDDS) is an ultradeep (K&lt;20.6mag, I&lt;24.5mag) redshift survey targeting galaxies in the "redshift desert" between z=1 and z=2. The primary goal of the survey is to constrain the space density at high redshift of evolved high-mass galaxies. We obtained 309 spectra in four widely separated 30-arcmin^2^ fields using the Gemini North telescope and the Gemini Multi-Object Spectrograph (GMOS). The spectra define a one-in-two sparse sample of the reddest and most luminous galaxies near the I-K versus I color-magnitude track mapped out by passively evolving galaxies in the redshift interval 0.8&lt;z&lt;1.8. This sample is augmented by a one-in-seven sparse sample of the remaining high-redshift galaxy population. The GMOS spectrograph was operating in a nod-and-shuffle mode, which enabled us to remove sky contamination with high precision, even for typical exposures times of 20-30hr per field. The resulting spectra are the deepest ever obtained. In this paper we present our sample of 309 spectra, along with redshifts, identifications of spectral features, and photometry. This makes the GDDS the largest and most complete infrared-selected survey probing the redshift desert. The seven-band (VRIz'JHK_s_) photometry is taken from the Las Campanas Infrared Survey (Cat. &lt;VII/228&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455#2</TD>
            <TD>2011-09-14T19:43:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/2455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2455</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/684/905 [1]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#1</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/684/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/684/905 [2]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#2</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/684/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/905 [table3]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#table3</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/905 [table1]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#table1</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/372/1621 [1]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)</TD>
            <TD>We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-m SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/XMM-Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720arcmin^2^ with a rms noise level of about 2mJy and have uncovered &gt;100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We &gt;also find that a 850-m survey complete down to 2mJy would resolve &gt;20-30 per cent of the far-infrared background into point sources.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621#1</TD>
            <TD>2011-09-14T20:30:09Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/372/1621</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1621</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/372/1621 [2]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)</TD>
            <TD>We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-m SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/XMM-Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720arcmin^2^ with a rms noise level of about 2mJy and have uncovered &gt;100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We &gt;also find that a 850-m survey complete down to 2mJy would resolve &gt;20-30 per cent of the far-infrared background into point sources.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621#2</TD>
            <TD>2011-09-14T20:30:09Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/372/1621&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1621</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/372/1621 [table2]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)</TD>
            <TD>We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-m SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/XMM-Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720arcmin^2^ with a rms noise level of about 2mJy and have uncovered &gt;100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We &gt;also find that a 850-m survey complete down to 2mJy would resolve &gt;20-30 per cent of the far-infrared background into point sources.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621#table2</TD>
            <TD>2011-09-14T20:30:09Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/372/1621&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1621</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/684/905 [1]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#1</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/684/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/684/905 [2]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#2</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/684/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/905 [table3]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#table3</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/684/905 [table1]</TD>
            <TD>z&gt;1 galaxy clusters from IRAC Shallow Survey (Eisenhardt+, 2008)</TD>
            <TD>The IRAC Shallow Survey (Eisenhardt et al., 2004ApJS..154...48E) covers ~8.5deg^2^ and reaches an aperture-corrected 5{sigma} depth of ~19.1 and 18.3mag (Vega) at 3.6 and 4.5um in 3" diameter apertures. This paper uses the NOAO Deep Wide-Field Survey (NDWFS) third data release (DR3) images and SExtractor catalogs which can be obtained through the NOAO data archive. Most of the high-redshift optical spectroscopic confirmation of ISCS clusters has been obtained at Keck Observatory, with DEIMOS and LRIS, and with FOCAS on Subaru, between 2005 June and 2007 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905#table1</TD>
            <TD>2011-09-14T21:12:14Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/684/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/684/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/684/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/2455 [1]</TD>
            <TD>Gemini Deep Deep Survey (GDDS) (Abraham+, 2004)</TD>
            <TD>The Gemini Deep Deep Survey (GDDS) is an ultradeep (K&lt;20.6mag, I&lt;24.5mag) redshift survey targeting galaxies in the "redshift desert" between z=1 and z=2. The primary goal of the survey is to constrain the space density at high redshift of evolved high-mass galaxies. We obtained 309 spectra in four widely separated 30-arcmin^2^ fields using the Gemini North telescope and the Gemini Multi-Object Spectrograph (GMOS). The spectra define a one-in-two sparse sample of the reddest and most luminous galaxies near the I-K versus I color-magnitude track mapped out by passively evolving galaxies in the redshift interval 0.8&lt;z&lt;1.8. This sample is augmented by a one-in-seven sparse sample of the remaining high-redshift galaxy population. The GMOS spectrograph was operating in a nod-and-shuffle mode, which enabled us to remove sky contamination with high precision, even for typical exposures times of 20-30hr per field. The resulting spectra are the deepest ever obtained. In this paper we present our sample of 309 spectra, along with redshifts, identifications of spectral features, and photometry. This makes the GDDS the largest and most complete infrared-selected survey probing the redshift desert. The seven-band (VRIz'JHK_s_) photometry is taken from the Las Campanas Infrared Survey (Cat. &lt;VII/228&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455#1</TD>
            <TD>2011-09-14T19:43:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/2455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/2455 [2]</TD>
            <TD>Gemini Deep Deep Survey (GDDS) (Abraham+, 2004)</TD>
            <TD>The Gemini Deep Deep Survey (GDDS) is an ultradeep (K&lt;20.6mag, I&lt;24.5mag) redshift survey targeting galaxies in the "redshift desert" between z=1 and z=2. The primary goal of the survey is to constrain the space density at high redshift of evolved high-mass galaxies. We obtained 309 spectra in four widely separated 30-arcmin^2^ fields using the Gemini North telescope and the Gemini Multi-Object Spectrograph (GMOS). The spectra define a one-in-two sparse sample of the reddest and most luminous galaxies near the I-K versus I color-magnitude track mapped out by passively evolving galaxies in the redshift interval 0.8&lt;z&lt;1.8. This sample is augmented by a one-in-seven sparse sample of the remaining high-redshift galaxy population. The GMOS spectrograph was operating in a nod-and-shuffle mode, which enabled us to remove sky contamination with high precision, even for typical exposures times of 20-30hr per field. The resulting spectra are the deepest ever obtained. In this paper we present our sample of 309 spectra, along with redshifts, identifications of spectral features, and photometry. This makes the GDDS the largest and most complete infrared-selected survey probing the redshift desert. The seven-band (VRIz'JHK_s_) photometry is taken from the Las Campanas Infrared Survey (Cat. &lt;VII/228&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455#2</TD>
            <TD>2011-09-14T19:43:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/2455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2455</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/372/1621 [1]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)</TD>
            <TD>We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-m SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/XMM-Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720arcmin^2^ with a rms noise level of about 2mJy and have uncovered &gt;100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We &gt;also find that a 850-m survey complete down to 2mJy would resolve &gt;20-30 per cent of the far-infrared background into point sources.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621#1</TD>
            <TD>2011-09-14T20:30:09Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/372/1621</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1621</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/372/1621 [2]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)</TD>
            <TD>We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-m SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/XMM-Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720arcmin^2^ with a rms noise level of about 2mJy and have uncovered &gt;100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We &gt;also find that a 850-m survey complete down to 2mJy would resolve &gt;20-30 per cent of the far-infrared background into point sources.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621#2</TD>
            <TD>2011-09-14T20:30:09Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/372/1621&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1621</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/372/1621 [table2]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)</TD>
            <TD>We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-m SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/XMM-Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720arcmin^2^ with a rms noise level of about 2mJy and have uncovered &gt;100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We &gt;also find that a 850-m survey complete down to 2mJy would resolve &gt;20-30 per cent of the far-infrared background into point sources.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621#table2</TD>
            <TD>2011-09-14T20:30:09Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/372/1621&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1621</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/71/297 [1]</TD>
            <TD>CCD UBV photometry of stars in Sex A (Aparicio+, 1987)</TD>
            <TD>CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985AJ.....90.1019S) and Hoessel et al. (1983ApJ...274..577H) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, {mu}=25.6. A similar value for the distance modulus is obtained from the colour-colour diagram. Colour-colour and colour-magnitude diagrams for the whole galaxy and for different parts are presented indicating a general star formation activity all over Sextans A. The contribution of stars brighter than M_pg_=-3 to the total blue light of the galaxy amounts to 25%, a much higher value than what is found for other dwarf irregular galaxies in the Local Group. The integrated birthrate per unit mass of massive stars for the galaxy is found to be much higher than in the Magellanic Clouds, suggesting that the rate in Sextans A was probably smaller in the past. Different slopes for high mass and low mass IMF parts are needed to account for its low surface brightness. The formation of massive stars seems to be favoured for systems of decreasing mass or, given the relation between total mass and metal content, for galaxies of decreasing metallicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297#1</TD>
            <TD>2011-09-14T21:13:13Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/71/297</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/71/297</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/71/297 [2]</TD>
            <TD>CCD UBV photometry of stars in Sex A (Aparicio+, 1987)</TD>
            <TD>CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985AJ.....90.1019S) and Hoessel et al. (1983ApJ...274..577H) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, {mu}=25.6. A similar value for the distance modulus is obtained from the colour-colour diagram. Colour-colour and colour-magnitude diagrams for the whole galaxy and for different parts are presented indicating a general star formation activity all over Sextans A. The contribution of stars brighter than M_pg_=-3 to the total blue light of the galaxy amounts to 25%, a much higher value than what is found for other dwarf irregular galaxies in the Local Group. The integrated birthrate per unit mass of massive stars for the galaxy is found to be much higher than in the Magellanic Clouds, suggesting that the rate in Sextans A was probably smaller in the past. Different slopes for high mass and low mass IMF parts are needed to account for its low surface brightness. The formation of massive stars seems to be favoured for systems of decreasing mass or, given the relation between total mass and metal content, for galaxies of decreasing metallicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297#2</TD>
            <TD>2011-09-14T21:13:13Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/71/297&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/71/297</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/71/297 [table2]</TD>
            <TD>CCD UBV photometry of stars in Sex A (Aparicio+, 1987)</TD>
            <TD>CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985AJ.....90.1019S) and Hoessel et al. (1983ApJ...274..577H) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, {mu}=25.6. A similar value for the distance modulus is obtained from the colour-colour diagram. Colour-colour and colour-magnitude diagrams for the whole galaxy and for different parts are presented indicating a general star formation activity all over Sextans A. The contribution of stars brighter than M_pg_=-3 to the total blue light of the galaxy amounts to 25%, a much higher value than what is found for other dwarf irregular galaxies in the Local Group. The integrated birthrate per unit mass of massive stars for the galaxy is found to be much higher than in the Magellanic Clouds, suggesting that the rate in Sextans A was probably smaller in the past. Different slopes for high mass and low mass IMF parts are needed to account for its low surface brightness. The formation of massive stars seems to be favoured for systems of decreasing mass or, given the relation between total mass and metal content, for galaxies of decreasing metallicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297#table2</TD>
            <TD>2011-09-14T21:13:13Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/71/297&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/71/297</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/621/673 [1]</TD>
            <TD>Line indices for 124 early-type galaxies (Thomas+, 2005)</TD>
            <TD>The aim of this paper is to set constraints on the epochs of early-type galaxy formation through the "archaeology" of the stellar populations in local galaxies. Using our models of absorption-line indices that account for variable abundance ratios, we derive ages, total metallicities, and element ratios of 124 early-type galaxies in high- and low-density environments. The data are analyzed by comparison with mock galaxy samples created through Monte Carlo simulations taking the typical average observational errors into account, in order to eliminate artifacts caused by correlated errors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673#1</TD>
            <TD>2011-09-14T19:44:28Z</TD>
            <TD>#Abundances#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/621/673</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/621/673</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/621/673 [2]</TD>
            <TD>Line indices for 124 early-type galaxies (Thomas+, 2005)</TD>
            <TD>The aim of this paper is to set constraints on the epochs of early-type galaxy formation through the "archaeology" of the stellar populations in local galaxies. Using our models of absorption-line indices that account for variable abundance ratios, we derive ages, total metallicities, and element ratios of 124 early-type galaxies in high- and low-density environments. The data are analyzed by comparison with mock galaxy samples created through Monte Carlo simulations taking the typical average observational errors into account, in order to eliminate artifacts caused by correlated errors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673#2</TD>
            <TD>2011-09-14T19:44:28Z</TD>
            <TD>#Abundances#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/621/673&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/621/673</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/621/673 [galaxies]</TD>
            <TD>Line indices for 124 early-type galaxies (Thomas+, 2005)</TD>
            <TD>The aim of this paper is to set constraints on the epochs of early-type galaxy formation through the "archaeology" of the stellar populations in local galaxies. Using our models of absorption-line indices that account for variable abundance ratios, we derive ages, total metallicities, and element ratios of 124 early-type galaxies in high- and low-density environments. The data are analyzed by comparison with mock galaxy samples created through Monte Carlo simulations taking the typical average observational errors into account, in order to eliminate artifacts caused by correlated errors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673#galaxies</TD>
            <TD>2011-09-14T19:44:28Z</TD>
            <TD>#Abundances#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/621/673&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/621/673</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/372/1621 [1]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)</TD>
            <TD>We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-m SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/XMM-Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720arcmin^2^ with a rms noise level of about 2mJy and have uncovered &gt;100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We &gt;also find that a 850-m survey complete down to 2mJy would resolve &gt;20-30 per cent of the far-infrared background into point sources.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621#1</TD>
            <TD>2011-09-14T20:30:09Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/372/1621</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1621</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/372/1621 [2]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)</TD>
            <TD>We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-m SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/XMM-Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720arcmin^2^ with a rms noise level of about 2mJy and have uncovered &gt;100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We &gt;also find that a 850-m survey complete down to 2mJy would resolve &gt;20-30 per cent of the far-infrared background into point sources.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621#2</TD>
            <TD>2011-09-14T20:30:09Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/372/1621&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1621</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/372/1621 [table2]</TD>
            <TD>SCUBA Half-Degree Extragalactic Survey. II (Coppin+, 2006)</TD>
            <TD>We present maps, source catalogue and number counts of the largest, most complete and unbiased extragalactic submillimetre survey: the 850-m SCUBA Half-Degree Extragalactic Survey (SHADES). Using the Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT), SHADES mapped two separate regions of sky: the Subaru/XMM-Newton Deep Field (SXDF) and the Lockman Hole East (LH). Encompassing 93 per cent of the overall acquired data (i.e. data taken up to 2004 February 1), these SCUBA maps cover 720arcmin^2^ with a rms noise level of about 2mJy and have uncovered &gt;100 submillimetre galaxies. In order to ensure the utmost robustness of the resulting source catalogue, data reduction was independently carried out by four subgroups within the SHADES team, providing an unprecedented degree of reliability with respect to other SCUBA catalogues available from the literature. Individual source lists from the four groups were combined to produce a robust 120-object SHADES catalogue; an invaluable resource for follow-up campaigns aiming to study the properties of a complete and consistent sample of submillimetre galaxies. For the first time, we present deboosted flux densities for each submillimetre galaxy found in a large survey. Extensive simulations and tests were performed separately by each group in order to confirm the robustness of the source candidates and to evaluate the effects of false detections, completeness and flux density boosting. Corrections for these effects were then applied to the data to derive the submillimetre galaxy source counts. SHADES has a high enough number of detected sources that meaningful differential counts can be estimated, unlike most submillimetre surveys which have to consider integral counts. We present differential and integral source number counts and find that the differential counts are better fit with a broken power law or a Schechter function than with a single power law; the SHADES data alone significantly show that a break is required at several mJy, although the precise position of the break is not well constrained. We &gt;also find that a 850-m survey complete down to 2mJy would resolve &gt;20-30 per cent of the far-infrared background into point sources.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621#table2</TD>
            <TD>2011-09-14T20:30:09Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/372/1621</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/372/1621&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/372/1621</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/621/673 [1]</TD>
            <TD>Line indices for 124 early-type galaxies (Thomas+, 2005)</TD>
            <TD>The aim of this paper is to set constraints on the epochs of early-type galaxy formation through the "archaeology" of the stellar populations in local galaxies. Using our models of absorption-line indices that account for variable abundance ratios, we derive ages, total metallicities, and element ratios of 124 early-type galaxies in high- and low-density environments. The data are analyzed by comparison with mock galaxy samples created through Monte Carlo simulations taking the typical average observational errors into account, in order to eliminate artifacts caused by correlated errors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673#1</TD>
            <TD>2011-09-14T19:44:28Z</TD>
            <TD>#Abundances#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/621/673</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/621/673</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/621/673 [2]</TD>
            <TD>Line indices for 124 early-type galaxies (Thomas+, 2005)</TD>
            <TD>The aim of this paper is to set constraints on the epochs of early-type galaxy formation through the "archaeology" of the stellar populations in local galaxies. Using our models of absorption-line indices that account for variable abundance ratios, we derive ages, total metallicities, and element ratios of 124 early-type galaxies in high- and low-density environments. The data are analyzed by comparison with mock galaxy samples created through Monte Carlo simulations taking the typical average observational errors into account, in order to eliminate artifacts caused by correlated errors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673#2</TD>
            <TD>2011-09-14T19:44:28Z</TD>
            <TD>#Abundances#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/621/673&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/621/673</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/621/673 [galaxies]</TD>
            <TD>Line indices for 124 early-type galaxies (Thomas+, 2005)</TD>
            <TD>The aim of this paper is to set constraints on the epochs of early-type galaxy formation through the "archaeology" of the stellar populations in local galaxies. Using our models of absorption-line indices that account for variable abundance ratios, we derive ages, total metallicities, and element ratios of 124 early-type galaxies in high- and low-density environments. The data are analyzed by comparison with mock galaxy samples created through Monte Carlo simulations taking the typical average observational errors into account, in order to eliminate artifacts caused by correlated errors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673#galaxies</TD>
            <TD>2011-09-14T19:44:28Z</TD>
            <TD>#Abundances#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/621/673&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/621/673</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/71/297 [1]</TD>
            <TD>CCD UBV photometry of stars in Sex A (Aparicio+, 1987)</TD>
            <TD>CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985AJ.....90.1019S) and Hoessel et al. (1983ApJ...274..577H) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, {mu}=25.6. A similar value for the distance modulus is obtained from the colour-colour diagram. Colour-colour and colour-magnitude diagrams for the whole galaxy and for different parts are presented indicating a general star formation activity all over Sextans A. The contribution of stars brighter than M_pg_=-3 to the total blue light of the galaxy amounts to 25%, a much higher value than what is found for other dwarf irregular galaxies in the Local Group. The integrated birthrate per unit mass of massive stars for the galaxy is found to be much higher than in the Magellanic Clouds, suggesting that the rate in Sextans A was probably smaller in the past. Different slopes for high mass and low mass IMF parts are needed to account for its low surface brightness. The formation of massive stars seems to be favoured for systems of decreasing mass or, given the relation between total mass and metal content, for galaxies of decreasing metallicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297#1</TD>
            <TD>2011-09-14T21:13:13Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/71/297</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/71/297</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/71/297 [2]</TD>
            <TD>CCD UBV photometry of stars in Sex A (Aparicio+, 1987)</TD>
            <TD>CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985AJ.....90.1019S) and Hoessel et al. (1983ApJ...274..577H) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, {mu}=25.6. A similar value for the distance modulus is obtained from the colour-colour diagram. Colour-colour and colour-magnitude diagrams for the whole galaxy and for different parts are presented indicating a general star formation activity all over Sextans A. The contribution of stars brighter than M_pg_=-3 to the total blue light of the galaxy amounts to 25%, a much higher value than what is found for other dwarf irregular galaxies in the Local Group. The integrated birthrate per unit mass of massive stars for the galaxy is found to be much higher than in the Magellanic Clouds, suggesting that the rate in Sextans A was probably smaller in the past. Different slopes for high mass and low mass IMF parts are needed to account for its low surface brightness. The formation of massive stars seems to be favoured for systems of decreasing mass or, given the relation between total mass and metal content, for galaxies of decreasing metallicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297#2</TD>
            <TD>2011-09-14T21:13:13Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/71/297&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/71/297</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/71/297 [table2]</TD>
            <TD>CCD UBV photometry of stars in Sex A (Aparicio+, 1987)</TD>
            <TD>CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985AJ.....90.1019S) and Hoessel et al. (1983ApJ...274..577H) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, {mu}=25.6. A similar value for the distance modulus is obtained from the colour-colour diagram. Colour-colour and colour-magnitude diagrams for the whole galaxy and for different parts are presented indicating a general star formation activity all over Sextans A. The contribution of stars brighter than M_pg_=-3 to the total blue light of the galaxy amounts to 25%, a much higher value than what is found for other dwarf irregular galaxies in the Local Group. The integrated birthrate per unit mass of massive stars for the galaxy is found to be much higher than in the Magellanic Clouds, suggesting that the rate in Sextans A was probably smaller in the past. Different slopes for high mass and low mass IMF parts are needed to account for its low surface brightness. The formation of massive stars seems to be favoured for systems of decreasing mass or, given the relation between total mass and metal content, for galaxies of decreasing metallicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297#table2</TD>
            <TD>2011-09-14T21:13:13Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/71/297&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/71/297</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/507/1277 [1]</TD>
            <TD>Multiwavelength photometry of CDFS X-ray sources (Brusa+, 2009)</TD>
            <TD>The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277#1</TD>
            <TD>2011-09-14T21:08:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/507/1277</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/1277</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/507/1277 [2]</TD>
            <TD>Multiwavelength photometry of CDFS X-ray sources (Brusa+, 2009)</TD>
            <TD>The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277#2</TD>
            <TD>2011-09-14T21:08:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/507/1277&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/1277</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/507/1277 [table1]</TD>
            <TD>Multiwavelength photometry of CDFS X-ray sources (Brusa+, 2009)</TD>
            <TD>The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277#table1</TD>
            <TD>2011-09-14T21:08:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/507/1277&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/1277</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/621/673 [1]</TD>
            <TD>Line indices for 124 early-type galaxies (Thomas+, 2005)</TD>
            <TD>The aim of this paper is to set constraints on the epochs of early-type galaxy formation through the "archaeology" of the stellar populations in local galaxies. Using our models of absorption-line indices that account for variable abundance ratios, we derive ages, total metallicities, and element ratios of 124 early-type galaxies in high- and low-density environments. The data are analyzed by comparison with mock galaxy samples created through Monte Carlo simulations taking the typical average observational errors into account, in order to eliminate artifacts caused by correlated errors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673#1</TD>
            <TD>2011-09-14T19:44:28Z</TD>
            <TD>#Abundances#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/621/673</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/621/673</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/621/673 [2]</TD>
            <TD>Line indices for 124 early-type galaxies (Thomas+, 2005)</TD>
            <TD>The aim of this paper is to set constraints on the epochs of early-type galaxy formation through the "archaeology" of the stellar populations in local galaxies. Using our models of absorption-line indices that account for variable abundance ratios, we derive ages, total metallicities, and element ratios of 124 early-type galaxies in high- and low-density environments. The data are analyzed by comparison with mock galaxy samples created through Monte Carlo simulations taking the typical average observational errors into account, in order to eliminate artifacts caused by correlated errors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673#2</TD>
            <TD>2011-09-14T19:44:28Z</TD>
            <TD>#Abundances#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/621/673&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/621/673</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/621/673 [galaxies]</TD>
            <TD>Line indices for 124 early-type galaxies (Thomas+, 2005)</TD>
            <TD>The aim of this paper is to set constraints on the epochs of early-type galaxy formation through the "archaeology" of the stellar populations in local galaxies. Using our models of absorption-line indices that account for variable abundance ratios, we derive ages, total metallicities, and element ratios of 124 early-type galaxies in high- and low-density environments. The data are analyzed by comparison with mock galaxy samples created through Monte Carlo simulations taking the typical average observational errors into account, in order to eliminate artifacts caused by correlated errors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673#galaxies</TD>
            <TD>2011-09-14T19:44:28Z</TD>
            <TD>#Abundances#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/621/673</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/621/673&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/621/673</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/71/297 [1]</TD>
            <TD>CCD UBV photometry of stars in Sex A (Aparicio+, 1987)</TD>
            <TD>CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985AJ.....90.1019S) and Hoessel et al. (1983ApJ...274..577H) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, {mu}=25.6. A similar value for the distance modulus is obtained from the colour-colour diagram. Colour-colour and colour-magnitude diagrams for the whole galaxy and for different parts are presented indicating a general star formation activity all over Sextans A. The contribution of stars brighter than M_pg_=-3 to the total blue light of the galaxy amounts to 25%, a much higher value than what is found for other dwarf irregular galaxies in the Local Group. The integrated birthrate per unit mass of massive stars for the galaxy is found to be much higher than in the Magellanic Clouds, suggesting that the rate in Sextans A was probably smaller in the past. Different slopes for high mass and low mass IMF parts are needed to account for its low surface brightness. The formation of massive stars seems to be favoured for systems of decreasing mass or, given the relation between total mass and metal content, for galaxies of decreasing metallicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297#1</TD>
            <TD>2011-09-14T21:13:13Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/71/297</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/71/297</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/71/297 [2]</TD>
            <TD>CCD UBV photometry of stars in Sex A (Aparicio+, 1987)</TD>
            <TD>CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985AJ.....90.1019S) and Hoessel et al. (1983ApJ...274..577H) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, {mu}=25.6. A similar value for the distance modulus is obtained from the colour-colour diagram. Colour-colour and colour-magnitude diagrams for the whole galaxy and for different parts are presented indicating a general star formation activity all over Sextans A. The contribution of stars brighter than M_pg_=-3 to the total blue light of the galaxy amounts to 25%, a much higher value than what is found for other dwarf irregular galaxies in the Local Group. The integrated birthrate per unit mass of massive stars for the galaxy is found to be much higher than in the Magellanic Clouds, suggesting that the rate in Sextans A was probably smaller in the past. Different slopes for high mass and low mass IMF parts are needed to account for its low surface brightness. The formation of massive stars seems to be favoured for systems of decreasing mass or, given the relation between total mass and metal content, for galaxies of decreasing metallicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297#2</TD>
            <TD>2011-09-14T21:13:13Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/71/297&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/71/297</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/71/297 [table2]</TD>
            <TD>CCD UBV photometry of stars in Sex A (Aparicio+, 1987)</TD>
            <TD>CCD UBV photometry of 2279 stars in Sextans A is presented. Differences with the photometric scales of Sandage and Carlson (1985AJ.....90.1019S) and Hoessel et al. (1983ApJ...274..577H) are discussed; recalibration of the Sandage and Carlson data for Cepheids in Sextans A results in a smaller value for the distance modulus, {mu}=25.6. A similar value for the distance modulus is obtained from the colour-colour diagram. Colour-colour and colour-magnitude diagrams for the whole galaxy and for different parts are presented indicating a general star formation activity all over Sextans A. The contribution of stars brighter than M_pg_=-3 to the total blue light of the galaxy amounts to 25%, a much higher value than what is found for other dwarf irregular galaxies in the Local Group. The integrated birthrate per unit mass of massive stars for the galaxy is found to be much higher than in the Magellanic Clouds, suggesting that the rate in Sextans A was probably smaller in the past. Different slopes for high mass and low mass IMF parts are needed to account for its low surface brightness. The formation of massive stars seems to be favoured for systems of decreasing mass or, given the relation between total mass and metal content, for galaxies of decreasing metallicity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297#table2</TD>
            <TD>2011-09-14T21:13:13Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/71/297</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/71/297&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/71/297</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/507/1277 [1]</TD>
            <TD>Multiwavelength photometry of CDFS X-ray sources (Brusa+, 2009)</TD>
            <TD>The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277#1</TD>
            <TD>2011-09-14T21:08:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/507/1277</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/1277</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/507/1277 [2]</TD>
            <TD>Multiwavelength photometry of CDFS X-ray sources (Brusa+, 2009)</TD>
            <TD>The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277#2</TD>
            <TD>2011-09-14T21:08:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/507/1277&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/1277</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/507/1277 [table1]</TD>
            <TD>Multiwavelength photometry of CDFS X-ray sources (Brusa+, 2009)</TD>
            <TD>The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277#table1</TD>
            <TD>2011-09-14T21:08:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/507/1277&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/1277</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/18 [1]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#1</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/18 [2]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#2</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/18 [table12]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#table12</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/18 [table34]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#table34</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1292 [1]</TD>
            <TD>KISS III. [O III]-selected survey list (Salzer+, 2002)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is an objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors, and it is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our blue spectral data, which cover the wavelength range 4800-5500{AA}. In most cases, the detected emission line is [O III] {lambda}5007. The current survey list covers a 1{deg}-wide strip located at {delta}=29{deg}30' (B1950.0) and spanning the right ascension range 8h30min to 17h0min. An area of 116.6d{deg}^2^ is covered. A total of 223 candidate emission-line objects have been selected for inclusion in the survey list (1.91{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift, emission-line flux, and equivalent width based on measurements of the digital objective-prism spectra. The median apparent magnitude of the sample is B=18.2, and galaxies with redshifts approaching z=0.1 are detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292#1</TD>
            <TD>2011-09-14T19:44:30Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1292</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1292</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1292 [2]</TD>
            <TD>KISS III. [O III]-selected survey list (Salzer+, 2002)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is an objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors, and it is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our blue spectral data, which cover the wavelength range 4800-5500{AA}. In most cases, the detected emission line is [O III] {lambda}5007. The current survey list covers a 1{deg}-wide strip located at {delta}=29{deg}30' (B1950.0) and spanning the right ascension range 8h30min to 17h0min. An area of 116.6d{deg}^2^ is covered. A total of 223 candidate emission-line objects have been selected for inclusion in the survey list (1.91{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift, emission-line flux, and equivalent width based on measurements of the digital objective-prism spectra. The median apparent magnitude of the sample is B=18.2, and galaxies with redshifts approaching z=0.1 are detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292#2</TD>
            <TD>2011-09-14T19:44:30Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1292&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1292</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/507/1277 [1]</TD>
            <TD>Multiwavelength photometry of CDFS X-ray sources (Brusa+, 2009)</TD>
            <TD>The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277#1</TD>
            <TD>2011-09-14T21:08:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/507/1277</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/1277</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/507/1277 [2]</TD>
            <TD>Multiwavelength photometry of CDFS X-ray sources (Brusa+, 2009)</TD>
            <TD>The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277#2</TD>
            <TD>2011-09-14T21:08:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/507/1277&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/1277</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/507/1277 [table1]</TD>
            <TD>Multiwavelength photometry of CDFS X-ray sources (Brusa+, 2009)</TD>
            <TD>The co-evolution of host galaxies and the active black holes which reside in their centre is one of the most important topics in modern observational cosmology. Here we present a study of the properties of obscured active galactic nuclei (AGN) detected in the CDFS 1 Ms observation and their host galaxies. We limited the analysis to the MUSIC area, for which deep K-band observations obtained with ISAAC@VLT are available, ensuring accurate identifications of the counterparts of the X-ray sources as well as reliable determination of photometric redshifts and galaxy parameters, such as stellar masses and star formation rates. In particular, we: 1) refined the X-ray/infrared/optical association of 179 sources in the MUSIC area detected in the Chandra observation; 2) studied the host galaxies observed and rest frame colors and properties.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277#table1</TD>
            <TD>2011-09-14T21:08:09Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/507/1277</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/507/1277&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/507/1277</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/18 [1]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#1</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/18 [2]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#2</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/18 [table12]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#table12</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/18 [table34]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#table34</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1292 [1]</TD>
            <TD>KISS III. [O III]-selected survey list (Salzer+, 2002)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is an objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors, and it is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our blue spectral data, which cover the wavelength range 4800-5500{AA}. In most cases, the detected emission line is [O III] {lambda}5007. The current survey list covers a 1{deg}-wide strip located at {delta}=29{deg}30' (B1950.0) and spanning the right ascension range 8h30min to 17h0min. An area of 116.6d{deg}^2^ is covered. A total of 223 candidate emission-line objects have been selected for inclusion in the survey list (1.91{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift, emission-line flux, and equivalent width based on measurements of the digital objective-prism spectra. The median apparent magnitude of the sample is B=18.2, and galaxies with redshifts approaching z=0.1 are detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292#1</TD>
            <TD>2011-09-14T19:44:30Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1292</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1292</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1292 [2]</TD>
            <TD>KISS III. [O III]-selected survey list (Salzer+, 2002)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is an objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors, and it is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our blue spectral data, which cover the wavelength range 4800-5500{AA}. In most cases, the detected emission line is [O III] {lambda}5007. The current survey list covers a 1{deg}-wide strip located at {delta}=29{deg}30' (B1950.0) and spanning the right ascension range 8h30min to 17h0min. An area of 116.6d{deg}^2^ is covered. A total of 223 candidate emission-line objects have been selected for inclusion in the survey list (1.91{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift, emission-line flux, and equivalent width based on measurements of the digital objective-prism spectra. The median apparent magnitude of the sample is B=18.2, and galaxies with redshifts approaching z=0.1 are detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292#2</TD>
            <TD>2011-09-14T19:44:30Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1292&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1292</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/509/A81 [1]</TD>
            <TD>Candidate clusters detected in six CFHTLS fields (Adami+, 2010)</TD>
            <TD>Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1x1deg^2^), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i'=25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81#1</TD>
            <TD>2011-09-14T21:08:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/509/A81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/509/A81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/509/A81 [2]</TD>
            <TD>Candidate clusters detected in six CFHTLS fields (Adami+, 2010)</TD>
            <TD>Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1x1deg^2^), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i'=25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81#2</TD>
            <TD>2011-09-14T21:08:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/509/A81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/509/A81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/509/A81 [tablea]</TD>
            <TD>Candidate clusters detected in six CFHTLS fields (Adami+, 2010)</TD>
            <TD>Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1x1deg^2^), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i'=25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81#tablea</TD>
            <TD>2011-09-14T21:08:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/509/A81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/509/A81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/18 [1]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#1</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/18 [2]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#2</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/18 [table12]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#table12</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/18 [table34]</TD>
            <TD>LMC SAGE. New candidate YSOs (Whitney+, 2008)</TD>
            <TD>We present ~1000 new candidate Young Stellar Objects (YSOs) in the Large Magellanic Cloud selected from Spitzer Space Telescope data, as part of the Surveying the Agents of a Galaxy's Evolution (SAGE) Legacy program. The YSOs, detected by their excess infrared (IR) emission, represent early stages of evolution, still surrounded by disks and/or infalling envelopes. Previously, fewer than 20 such YSOs were known. The candidate YSOs were selected from the SAGE Point Source Catalog from regions of color-magnitude space least confused with other IR-bright populations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18#table34</TD>
            <TD>2011-09-14T21:27:35Z</TD>
            <TD>#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1292 [1]</TD>
            <TD>KISS III. [O III]-selected survey list (Salzer+, 2002)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is an objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors, and it is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our blue spectral data, which cover the wavelength range 4800-5500{AA}. In most cases, the detected emission line is [O III] {lambda}5007. The current survey list covers a 1{deg}-wide strip located at {delta}=29{deg}30' (B1950.0) and spanning the right ascension range 8h30min to 17h0min. An area of 116.6d{deg}^2^ is covered. A total of 223 candidate emission-line objects have been selected for inclusion in the survey list (1.91{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift, emission-line flux, and equivalent width based on measurements of the digital objective-prism spectra. The median apparent magnitude of the sample is B=18.2, and galaxies with redshifts approaching z=0.1 are detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292#1</TD>
            <TD>2011-09-14T19:44:30Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1292</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1292</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1292 [2]</TD>
            <TD>KISS III. [O III]-selected survey list (Salzer+, 2002)</TD>
            <TD>The KPNO International Spectroscopic Survey (KISS) is an objective-prism survey for extragalactic emission-line objects. It combines many of the features of previous slitless spectroscopic surveys with the advantages of modern CCD detectors, and it is the first purely digital objective-prism survey for emission-line galaxies. Here we present the first list of emission-line galaxy candidates selected from our blue spectral data, which cover the wavelength range 4800-5500{AA}. In most cases, the detected emission line is [O III] {lambda}5007. The current survey list covers a 1{deg}-wide strip located at {delta}=29{deg}30' (B1950.0) and spanning the right ascension range 8h30min to 17h0min. An area of 116.6d{deg}^2^ is covered. A total of 223 candidate emission-line objects have been selected for inclusion in the survey list (1.91{deg}^-2^). We tabulate accurate coordinates and photometry for each source, as well as estimates of the redshift, emission-line flux, and equivalent width based on measurements of the digital objective-prism spectra. The median apparent magnitude of the sample is B=18.2, and galaxies with redshifts approaching z=0.1 are detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292#2</TD>
            <TD>2011-09-14T19:44:30Z</TD>
            <TD>#Equivalent_widths#Seyfert_Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1292</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1292&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1292</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/509/A81 [1]</TD>
            <TD>Candidate clusters detected in six CFHTLS fields (Adami+, 2010)</TD>
            <TD>Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1x1deg^2^), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i'=25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81#1</TD>
            <TD>2011-09-14T21:08:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/509/A81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/509/A81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/509/A81 [2]</TD>
            <TD>Candidate clusters detected in six CFHTLS fields (Adami+, 2010)</TD>
            <TD>Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1x1deg^2^), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i'=25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81#2</TD>
            <TD>2011-09-14T21:08:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/509/A81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/509/A81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/509/A81 [tablea]</TD>
            <TD>Candidate clusters detected in six CFHTLS fields (Adami+, 2010)</TD>
            <TD>Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1x1deg^2^), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i'=25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81#tablea</TD>
            <TD>2011-09-14T21:08:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/509/A81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/509/A81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/691/705 [1]</TD>
            <TD>AGN host galaxy morphologies in COSMOS (Gabor+, 2009)</TD>
            <TD>COSMOS (Scoville et al. 2007ApJS..172....1S), a Hubble Space Telescope Treasury project, includes coverage of a 2deg^2^ field from X-ray wavelengths to UV, optical, IR, and radio. The cornerstone data set, which we use for the bulk of our analysis, consists of 583 orbits taken with Hubble's Advanced Camera for Surveys (ACS) with the F814W filter (see Koekemoer et al. 2007ApJS..172..196K for a complete description). Ancillary observations include XMM-Newton X-ray imaging (Hasinger et al. 2007, Cat. J/ApJS/172/29), VLA radio maps (Schinnerer et al. 2007, Cat. J/ApJS/172/46), and VLT/VIMOS (Lilly et al. 2007, Cat. J/ApJS/172/70) and Magellan/IMACS optical spectroscopy (Trump et al. 2007, Cat. J/ApJS/172/383; 2009ApJ...700...49T; 2009ApJ...706..797T).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705#1</TD>
            <TD>2011-09-14T21:30:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/691/705</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/691/705</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/691/705 [2]</TD>
            <TD>AGN host galaxy morphologies in COSMOS (Gabor+, 2009)</TD>
            <TD>COSMOS (Scoville et al. 2007ApJS..172....1S), a Hubble Space Telescope Treasury project, includes coverage of a 2deg^2^ field from X-ray wavelengths to UV, optical, IR, and radio. The cornerstone data set, which we use for the bulk of our analysis, consists of 583 orbits taken with Hubble's Advanced Camera for Surveys (ACS) with the F814W filter (see Koekemoer et al. 2007ApJS..172..196K for a complete description). Ancillary observations include XMM-Newton X-ray imaging (Hasinger et al. 2007, Cat. J/ApJS/172/29), VLA radio maps (Schinnerer et al. 2007, Cat. J/ApJS/172/46), and VLT/VIMOS (Lilly et al. 2007, Cat. J/ApJS/172/70) and Magellan/IMACS optical spectroscopy (Trump et al. 2007, Cat. J/ApJS/172/383; 2009ApJ...700...49T; 2009ApJ...706..797T).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705#2</TD>
            <TD>2011-09-14T21:30:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/691/705&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/691/705</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/691/705 [table2]</TD>
            <TD>AGN host galaxy morphologies in COSMOS (Gabor+, 2009)</TD>
            <TD>COSMOS (Scoville et al. 2007ApJS..172....1S), a Hubble Space Telescope Treasury project, includes coverage of a 2deg^2^ field from X-ray wavelengths to UV, optical, IR, and radio. The cornerstone data set, which we use for the bulk of our analysis, consists of 583 orbits taken with Hubble's Advanced Camera for Surveys (ACS) with the F814W filter (see Koekemoer et al. 2007ApJS..172..196K for a complete description). Ancillary observations include XMM-Newton X-ray imaging (Hasinger et al. 2007, Cat. J/ApJS/172/29), VLA radio maps (Schinnerer et al. 2007, Cat. J/ApJS/172/46), and VLT/VIMOS (Lilly et al. 2007, Cat. J/ApJS/172/70) and Magellan/IMACS optical spectroscopy (Trump et al. 2007, Cat. J/ApJS/172/383; 2009ApJ...700...49T; 2009ApJ...706..797T).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705#table2</TD>
            <TD>2011-09-14T21:30:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/691/705&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/691/705</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/509/A81 [1]</TD>
            <TD>Candidate clusters detected in six CFHTLS fields (Adami+, 2010)</TD>
            <TD>Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1x1deg^2^), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i'=25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81#1</TD>
            <TD>2011-09-14T21:08:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/509/A81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/509/A81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/509/A81 [2]</TD>
            <TD>Candidate clusters detected in six CFHTLS fields (Adami+, 2010)</TD>
            <TD>Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1x1deg^2^), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i'=25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81#2</TD>
            <TD>2011-09-14T21:08:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/509/A81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/509/A81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/509/A81 [tablea]</TD>
            <TD>Candidate clusters detected in six CFHTLS fields (Adami+, 2010)</TD>
            <TD>Counting clusters is one of the methods to constrain cosmological parameters, but has been limited up to now both by the redshift range and by the relatively small sizes of the homogeneously surveyed areas. In order to enlarge publicly available optical cluster catalogs, in particular at high redshift, we have performed a systematic search for clusters of galaxies in the Canada France Hawaii Telescope Legacy Survey (CFHTLS). We considered the deep 2, 3 and 4 CFHTLS Deep fields (each 1x1deg^2^), as well as the wide 1, 3 and 4 CFHTLS Wide fields. We used the Le Phare photometric redshifts for the galaxies detected in these fields with magnitude limits of i'=25 and 23 for the Deep and Wide fields respectively. We then constructed galaxy density maps in photometric redshift bins of 0.1 based on an adaptive kernel technique and detected structures with SExtractor at various detection levels. In order to assess the validity of our cluster detection rates, we applied a similar procedure to galaxies in Millennium simulations. We measured the correlation function of our cluster candidates. We analyzed large scale properties and substructures, including filaments, by applying a minimal spanning tree algorithm both to our data and to the Millennium simulations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81#tablea</TD>
            <TD>2011-09-14T21:08:53Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/509/A81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/509/A81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/509/A81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/2062 [1]</TD>
            <TD>SDSS DR1 isolated galaxies (Allam+, 2005)</TD>
            <TD>We present a new catalog of isolated galaxies obtained through an automated systematic search. These 2980 isolated galaxies were found in ~2099{deg}^2^ of sky in the Sloan Digital Sky Survey Data Release 1 (SDSS DR1, http://www.sdss.org/dr1/) photometry. The selection algorithm, implementing a variation on the criteria developed by Karachentseva in 1973, proved to be very efficient and fast. This catalog will be useful for studies of the general galaxy characteristics. Here we report on our results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062#1</TD>
            <TD>2011-09-14T19:45:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/2062</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/2062</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/2062 [2]</TD>
            <TD>SDSS DR1 isolated galaxies (Allam+, 2005)</TD>
            <TD>We present a new catalog of isolated galaxies obtained through an automated systematic search. These 2980 isolated galaxies were found in ~2099{deg}^2^ of sky in the Sloan Digital Sky Survey Data Release 1 (SDSS DR1, http://www.sdss.org/dr1/) photometry. The selection algorithm, implementing a variation on the criteria developed by Karachentseva in 1973, proved to be very efficient and fast. This catalog will be useful for studies of the general galaxy characteristics. Here we report on our results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062#2</TD>
            <TD>2011-09-14T19:45:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/2062&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/2062</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/2062 [table1]</TD>
            <TD>SDSS DR1 isolated galaxies (Allam+, 2005)</TD>
            <TD>We present a new catalog of isolated galaxies obtained through an automated systematic search. These 2980 isolated galaxies were found in ~2099{deg}^2^ of sky in the Sloan Digital Sky Survey Data Release 1 (SDSS DR1, http://www.sdss.org/dr1/) photometry. The selection algorithm, implementing a variation on the criteria developed by Karachentseva in 1973, proved to be very efficient and fast. This catalog will be useful for studies of the general galaxy characteristics. Here we report on our results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062#table1</TD>
            <TD>2011-09-14T19:45:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/2062&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/2062</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/691/705 [1]</TD>
            <TD>AGN host galaxy morphologies in COSMOS (Gabor+, 2009)</TD>
            <TD>COSMOS (Scoville et al. 2007ApJS..172....1S), a Hubble Space Telescope Treasury project, includes coverage of a 2deg^2^ field from X-ray wavelengths to UV, optical, IR, and radio. The cornerstone data set, which we use for the bulk of our analysis, consists of 583 orbits taken with Hubble's Advanced Camera for Surveys (ACS) with the F814W filter (see Koekemoer et al. 2007ApJS..172..196K for a complete description). Ancillary observations include XMM-Newton X-ray imaging (Hasinger et al. 2007, Cat. J/ApJS/172/29), VLA radio maps (Schinnerer et al. 2007, Cat. J/ApJS/172/46), and VLT/VIMOS (Lilly et al. 2007, Cat. J/ApJS/172/70) and Magellan/IMACS optical spectroscopy (Trump et al. 2007, Cat. J/ApJS/172/383; 2009ApJ...700...49T; 2009ApJ...706..797T).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705#1</TD>
            <TD>2011-09-14T21:30:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/691/705</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/691/705</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/691/705 [2]</TD>
            <TD>AGN host galaxy morphologies in COSMOS (Gabor+, 2009)</TD>
            <TD>COSMOS (Scoville et al. 2007ApJS..172....1S), a Hubble Space Telescope Treasury project, includes coverage of a 2deg^2^ field from X-ray wavelengths to UV, optical, IR, and radio. The cornerstone data set, which we use for the bulk of our analysis, consists of 583 orbits taken with Hubble's Advanced Camera for Surveys (ACS) with the F814W filter (see Koekemoer et al. 2007ApJS..172..196K for a complete description). Ancillary observations include XMM-Newton X-ray imaging (Hasinger et al. 2007, Cat. J/ApJS/172/29), VLA radio maps (Schinnerer et al. 2007, Cat. J/ApJS/172/46), and VLT/VIMOS (Lilly et al. 2007, Cat. J/ApJS/172/70) and Magellan/IMACS optical spectroscopy (Trump et al. 2007, Cat. J/ApJS/172/383; 2009ApJ...700...49T; 2009ApJ...706..797T).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705#2</TD>
            <TD>2011-09-14T21:30:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/691/705&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/691/705</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/691/705 [table2]</TD>
            <TD>AGN host galaxy morphologies in COSMOS (Gabor+, 2009)</TD>
            <TD>COSMOS (Scoville et al. 2007ApJS..172....1S), a Hubble Space Telescope Treasury project, includes coverage of a 2deg^2^ field from X-ray wavelengths to UV, optical, IR, and radio. The cornerstone data set, which we use for the bulk of our analysis, consists of 583 orbits taken with Hubble's Advanced Camera for Surveys (ACS) with the F814W filter (see Koekemoer et al. 2007ApJS..172..196K for a complete description). Ancillary observations include XMM-Newton X-ray imaging (Hasinger et al. 2007, Cat. J/ApJS/172/29), VLA radio maps (Schinnerer et al. 2007, Cat. J/ApJS/172/46), and VLT/VIMOS (Lilly et al. 2007, Cat. J/ApJS/172/70) and Magellan/IMACS optical spectroscopy (Trump et al. 2007, Cat. J/ApJS/172/383; 2009ApJ...700...49T; 2009ApJ...706..797T).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705#table2</TD>
            <TD>2011-09-14T21:30:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/691/705&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/691/705</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/506/1071 [1]</TD>
            <TD>Galaxy morphology in 5 medium redshift clusters (Ascaso+, 2009)</TD>
            <TD>Following the study presented in our previous paper, based on the Nordic Optical Telescope (NOT) sample, which consists of five clusters of galaxies within the redshift range 0.18&lt;=z&lt;=0.25 imaged in the central 0.5-2Mpc in very good seeing conditions, we have studied the quantitative morphology of their bright galaxy population. We analyzed the surface brightness profiles of the galaxy population in those clusters, after performing simulations in order to check the reliability of the fits. We also derived a quantitative morphological classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071#1</TD>
            <TD>2011-09-14T21:10:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/506/1071</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/506/1071</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/506/1071 [2]</TD>
            <TD>Galaxy morphology in 5 medium redshift clusters (Ascaso+, 2009)</TD>
            <TD>Following the study presented in our previous paper, based on the Nordic Optical Telescope (NOT) sample, which consists of five clusters of galaxies within the redshift range 0.18&lt;=z&lt;=0.25 imaged in the central 0.5-2Mpc in very good seeing conditions, we have studied the quantitative morphology of their bright galaxy population. We analyzed the surface brightness profiles of the galaxy population in those clusters, after performing simulations in order to check the reliability of the fits. We also derived a quantitative morphological classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071#2</TD>
            <TD>2011-09-14T21:10:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/506/1071&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/506/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/506/1071 [tablea1]</TD>
            <TD>Galaxy morphology in 5 medium redshift clusters (Ascaso+, 2009)</TD>
            <TD>Following the study presented in our previous paper, based on the Nordic Optical Telescope (NOT) sample, which consists of five clusters of galaxies within the redshift range 0.18&lt;=z&lt;=0.25 imaged in the central 0.5-2Mpc in very good seeing conditions, we have studied the quantitative morphology of their bright galaxy population. We analyzed the surface brightness profiles of the galaxy population in those clusters, after performing simulations in order to check the reliability of the fits. We also derived a quantitative morphological classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071#tablea1</TD>
            <TD>2011-09-14T21:10:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/506/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/506/1071</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/691/705 [1]</TD>
            <TD>AGN host galaxy morphologies in COSMOS (Gabor+, 2009)</TD>
            <TD>COSMOS (Scoville et al. 2007ApJS..172....1S), a Hubble Space Telescope Treasury project, includes coverage of a 2deg^2^ field from X-ray wavelengths to UV, optical, IR, and radio. The cornerstone data set, which we use for the bulk of our analysis, consists of 583 orbits taken with Hubble's Advanced Camera for Surveys (ACS) with the F814W filter (see Koekemoer et al. 2007ApJS..172..196K for a complete description). Ancillary observations include XMM-Newton X-ray imaging (Hasinger et al. 2007, Cat. J/ApJS/172/29), VLA radio maps (Schinnerer et al. 2007, Cat. J/ApJS/172/46), and VLT/VIMOS (Lilly et al. 2007, Cat. J/ApJS/172/70) and Magellan/IMACS optical spectroscopy (Trump et al. 2007, Cat. J/ApJS/172/383; 2009ApJ...700...49T; 2009ApJ...706..797T).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705#1</TD>
            <TD>2011-09-14T21:30:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/691/705</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/691/705</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/691/705 [2]</TD>
            <TD>AGN host galaxy morphologies in COSMOS (Gabor+, 2009)</TD>
            <TD>COSMOS (Scoville et al. 2007ApJS..172....1S), a Hubble Space Telescope Treasury project, includes coverage of a 2deg^2^ field from X-ray wavelengths to UV, optical, IR, and radio. The cornerstone data set, which we use for the bulk of our analysis, consists of 583 orbits taken with Hubble's Advanced Camera for Surveys (ACS) with the F814W filter (see Koekemoer et al. 2007ApJS..172..196K for a complete description). Ancillary observations include XMM-Newton X-ray imaging (Hasinger et al. 2007, Cat. J/ApJS/172/29), VLA radio maps (Schinnerer et al. 2007, Cat. J/ApJS/172/46), and VLT/VIMOS (Lilly et al. 2007, Cat. J/ApJS/172/70) and Magellan/IMACS optical spectroscopy (Trump et al. 2007, Cat. J/ApJS/172/383; 2009ApJ...700...49T; 2009ApJ...706..797T).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705#2</TD>
            <TD>2011-09-14T21:30:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/691/705&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/691/705</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/691/705 [table2]</TD>
            <TD>AGN host galaxy morphologies in COSMOS (Gabor+, 2009)</TD>
            <TD>COSMOS (Scoville et al. 2007ApJS..172....1S), a Hubble Space Telescope Treasury project, includes coverage of a 2deg^2^ field from X-ray wavelengths to UV, optical, IR, and radio. The cornerstone data set, which we use for the bulk of our analysis, consists of 583 orbits taken with Hubble's Advanced Camera for Surveys (ACS) with the F814W filter (see Koekemoer et al. 2007ApJS..172..196K for a complete description). Ancillary observations include XMM-Newton X-ray imaging (Hasinger et al. 2007, Cat. J/ApJS/172/29), VLA radio maps (Schinnerer et al. 2007, Cat. J/ApJS/172/46), and VLT/VIMOS (Lilly et al. 2007, Cat. J/ApJS/172/70) and Magellan/IMACS optical spectroscopy (Trump et al. 2007, Cat. J/ApJS/172/383; 2009ApJ...700...49T; 2009ApJ...706..797T).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705#table2</TD>
            <TD>2011-09-14T21:30:42Z</TD>
            <TD>#AGN#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/691/705</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/691/705&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/691/705</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/506/1071 [1]</TD>
            <TD>Galaxy morphology in 5 medium redshift clusters (Ascaso+, 2009)</TD>
            <TD>Following the study presented in our previous paper, based on the Nordic Optical Telescope (NOT) sample, which consists of five clusters of galaxies within the redshift range 0.18&lt;=z&lt;=0.25 imaged in the central 0.5-2Mpc in very good seeing conditions, we have studied the quantitative morphology of their bright galaxy population. We analyzed the surface brightness profiles of the galaxy population in those clusters, after performing simulations in order to check the reliability of the fits. We also derived a quantitative morphological classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071#1</TD>
            <TD>2011-09-14T21:10:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/506/1071</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/506/1071</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/506/1071 [2]</TD>
            <TD>Galaxy morphology in 5 medium redshift clusters (Ascaso+, 2009)</TD>
            <TD>Following the study presented in our previous paper, based on the Nordic Optical Telescope (NOT) sample, which consists of five clusters of galaxies within the redshift range 0.18&lt;=z&lt;=0.25 imaged in the central 0.5-2Mpc in very good seeing conditions, we have studied the quantitative morphology of their bright galaxy population. We analyzed the surface brightness profiles of the galaxy population in those clusters, after performing simulations in order to check the reliability of the fits. We also derived a quantitative morphological classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071#2</TD>
            <TD>2011-09-14T21:10:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/506/1071&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/506/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/506/1071 [tablea1]</TD>
            <TD>Galaxy morphology in 5 medium redshift clusters (Ascaso+, 2009)</TD>
            <TD>Following the study presented in our previous paper, based on the Nordic Optical Telescope (NOT) sample, which consists of five clusters of galaxies within the redshift range 0.18&lt;=z&lt;=0.25 imaged in the central 0.5-2Mpc in very good seeing conditions, we have studied the quantitative morphology of their bright galaxy population. We analyzed the surface brightness profiles of the galaxy population in those clusters, after performing simulations in order to check the reliability of the fits. We also derived a quantitative morphological classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071#tablea1</TD>
            <TD>2011-09-14T21:10:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/506/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/506/1071</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/2062 [1]</TD>
            <TD>SDSS DR1 isolated galaxies (Allam+, 2005)</TD>
            <TD>We present a new catalog of isolated galaxies obtained through an automated systematic search. These 2980 isolated galaxies were found in ~2099{deg}^2^ of sky in the Sloan Digital Sky Survey Data Release 1 (SDSS DR1, http://www.sdss.org/dr1/) photometry. The selection algorithm, implementing a variation on the criteria developed by Karachentseva in 1973, proved to be very efficient and fast. This catalog will be useful for studies of the general galaxy characteristics. Here we report on our results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062#1</TD>
            <TD>2011-09-14T19:45:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/2062</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/2062</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/2062 [2]</TD>
            <TD>SDSS DR1 isolated galaxies (Allam+, 2005)</TD>
            <TD>We present a new catalog of isolated galaxies obtained through an automated systematic search. These 2980 isolated galaxies were found in ~2099{deg}^2^ of sky in the Sloan Digital Sky Survey Data Release 1 (SDSS DR1, http://www.sdss.org/dr1/) photometry. The selection algorithm, implementing a variation on the criteria developed by Karachentseva in 1973, proved to be very efficient and fast. This catalog will be useful for studies of the general galaxy characteristics. Here we report on our results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062#2</TD>
            <TD>2011-09-14T19:45:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/2062&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/2062</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/2062 [table1]</TD>
            <TD>SDSS DR1 isolated galaxies (Allam+, 2005)</TD>
            <TD>We present a new catalog of isolated galaxies obtained through an automated systematic search. These 2980 isolated galaxies were found in ~2099{deg}^2^ of sky in the Sloan Digital Sky Survey Data Release 1 (SDSS DR1, http://www.sdss.org/dr1/) photometry. The selection algorithm, implementing a variation on the criteria developed by Karachentseva in 1973, proved to be very efficient and fast. This catalog will be useful for studies of the general galaxy characteristics. Here we report on our results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062#table1</TD>
            <TD>2011-09-14T19:45:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/2062&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/2062</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/724/714 [1]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#1</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/724/714</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/724/714 [2]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#2</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/724/714&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/724/714 [tablea1]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#tablea1</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/724/714&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/724/714 [tablea2]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#tablea2</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/724/714&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/506/1071 [1]</TD>
            <TD>Galaxy morphology in 5 medium redshift clusters (Ascaso+, 2009)</TD>
            <TD>Following the study presented in our previous paper, based on the Nordic Optical Telescope (NOT) sample, which consists of five clusters of galaxies within the redshift range 0.18&lt;=z&lt;=0.25 imaged in the central 0.5-2Mpc in very good seeing conditions, we have studied the quantitative morphology of their bright galaxy population. We analyzed the surface brightness profiles of the galaxy population in those clusters, after performing simulations in order to check the reliability of the fits. We also derived a quantitative morphological classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071#1</TD>
            <TD>2011-09-14T21:10:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/506/1071</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/506/1071</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/506/1071 [2]</TD>
            <TD>Galaxy morphology in 5 medium redshift clusters (Ascaso+, 2009)</TD>
            <TD>Following the study presented in our previous paper, based on the Nordic Optical Telescope (NOT) sample, which consists of five clusters of galaxies within the redshift range 0.18&lt;=z&lt;=0.25 imaged in the central 0.5-2Mpc in very good seeing conditions, we have studied the quantitative morphology of their bright galaxy population. We analyzed the surface brightness profiles of the galaxy population in those clusters, after performing simulations in order to check the reliability of the fits. We also derived a quantitative morphological classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071#2</TD>
            <TD>2011-09-14T21:10:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/506/1071&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/506/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/506/1071 [tablea1]</TD>
            <TD>Galaxy morphology in 5 medium redshift clusters (Ascaso+, 2009)</TD>
            <TD>Following the study presented in our previous paper, based on the Nordic Optical Telescope (NOT) sample, which consists of five clusters of galaxies within the redshift range 0.18&lt;=z&lt;=0.25 imaged in the central 0.5-2Mpc in very good seeing conditions, we have studied the quantitative morphology of their bright galaxy population. We analyzed the surface brightness profiles of the galaxy population in those clusters, after performing simulations in order to check the reliability of the fits. We also derived a quantitative morphological classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071#tablea1</TD>
            <TD>2011-09-14T21:10:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/506/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/506/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/506/1071</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/2062 [1]</TD>
            <TD>SDSS DR1 isolated galaxies (Allam+, 2005)</TD>
            <TD>We present a new catalog of isolated galaxies obtained through an automated systematic search. These 2980 isolated galaxies were found in ~2099{deg}^2^ of sky in the Sloan Digital Sky Survey Data Release 1 (SDSS DR1, http://www.sdss.org/dr1/) photometry. The selection algorithm, implementing a variation on the criteria developed by Karachentseva in 1973, proved to be very efficient and fast. This catalog will be useful for studies of the general galaxy characteristics. Here we report on our results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062#1</TD>
            <TD>2011-09-14T19:45:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/2062</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/2062</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/2062 [2]</TD>
            <TD>SDSS DR1 isolated galaxies (Allam+, 2005)</TD>
            <TD>We present a new catalog of isolated galaxies obtained through an automated systematic search. These 2980 isolated galaxies were found in ~2099{deg}^2^ of sky in the Sloan Digital Sky Survey Data Release 1 (SDSS DR1, http://www.sdss.org/dr1/) photometry. The selection algorithm, implementing a variation on the criteria developed by Karachentseva in 1973, proved to be very efficient and fast. This catalog will be useful for studies of the general galaxy characteristics. Here we report on our results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062#2</TD>
            <TD>2011-09-14T19:45:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/2062&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/2062</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/2062 [table1]</TD>
            <TD>SDSS DR1 isolated galaxies (Allam+, 2005)</TD>
            <TD>We present a new catalog of isolated galaxies obtained through an automated systematic search. These 2980 isolated galaxies were found in ~2099{deg}^2^ of sky in the Sloan Digital Sky Survey Data Release 1 (SDSS DR1, http://www.sdss.org/dr1/) photometry. The selection algorithm, implementing a variation on the criteria developed by Karachentseva in 1973, proved to be very efficient and fast. This catalog will be useful for studies of the general galaxy characteristics. Here we report on our results.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062#table1</TD>
            <TD>2011-09-14T19:45:49Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/2062</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/2062&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/2062</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/724/714 [1]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#1</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/724/714</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/724/714 [2]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#2</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/724/714&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/724/714 [tablea1]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#tablea1</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/724/714&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/724/714 [tablea2]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#tablea2</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/724/714&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/526/A72 [1]</TD>
            <TD>Physical param. of EGS early-type gal. (Fernandez Lorenzo+, 2011)</TD>
            <TD>Physical parameters for 135 early-type galaxies in the Extended Groth Strip. For each galaxy equatorial coordinates, total magnitudes in B and g-bands, redshift, velocity dispersion, effective radius, surface brightness, stellar mass, Sersic index, type (elliptical or lenticular) and signal-to-noise of the spectrum are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72#1</TD>
            <TD>2011-09-14T21:11:46Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/526/A72</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A72</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/526/A72 [2]</TD>
            <TD>Physical param. of EGS early-type gal. (Fernandez Lorenzo+, 2011)</TD>
            <TD>Physical parameters for 135 early-type galaxies in the Extended Groth Strip. For each galaxy equatorial coordinates, total magnitudes in B and g-bands, redshift, velocity dispersion, effective radius, surface brightness, stellar mass, Sersic index, type (elliptical or lenticular) and signal-to-noise of the spectrum are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72#2</TD>
            <TD>2011-09-14T21:11:46Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/526/A72&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A72</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/526/A72 [table1]</TD>
            <TD>Physical param. of EGS early-type gal. (Fernandez Lorenzo+, 2011)</TD>
            <TD>Physical parameters for 135 early-type galaxies in the Extended Groth Strip. For each galaxy equatorial coordinates, total magnitudes in B and g-bands, redshift, velocity dispersion, effective radius, surface brightness, stellar mass, Sersic index, type (elliptical or lenticular) and signal-to-noise of the spectrum are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72#table1</TD>
            <TD>2011-09-14T21:11:46Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/526/A72&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A72</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/145/199 [1]</TD>
            <TD>Optical spectroscopic atlas of low-redshift AGN (Marziani+, 2003)</TD>
            <TD>We present a spectral atlas of the H{beta} region for 215 type 1 AGNs (luminous Seyfert 1/radio galaxy nuclei and low-z quasars) up to z~0.8. Line profiles and measures were derived from the database of intermediate resolution spectra (R&gt;~1000) with average continuum level S/N ratio ~30. Parameters including rest frame equivalent width and FWHM are provided for the FeII_opt_ blend at {lambda}4570, H{beta}, HeII {lambda}4686, and the [OIII] {lambda}{lambda}4959, 5007 emission lines. We extract clean broad component H{beta} profiles and provide wavelength measurements at 0, 1/4, 1/2, 3/4, and 0.9 peak intensity levels in order to permit a quantitative definition of the H{beta} broad component for statistical studies. We also discuss sources of uncertainty, selection effects, and biases in our sample. The data are especially important for tests of the eigenvector 1 parameter space occupation and correlation. We show that the I Zw 1 template FeII_opt_ spectrum reproduces well the observed FeII_opt_ emission for a wide range of line width and strength. A detailed analysis of the data within the eigenvector 1 context is deferred to a companion paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199#1</TD>
            <TD>2011-09-14T19:46:22Z</TD>
            <TD>#AGN#Equivalent_widths#Spectroscopy#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/145/199</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/199</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/145/199 [2]</TD>
            <TD>Optical spectroscopic atlas of low-redshift AGN (Marziani+, 2003)</TD>
            <TD>We present a spectral atlas of the H{beta} region for 215 type 1 AGNs (luminous Seyfert 1/radio galaxy nuclei and low-z quasars) up to z~0.8. Line profiles and measures were derived from the database of intermediate resolution spectra (R&gt;~1000) with average continuum level S/N ratio ~30. Parameters including rest frame equivalent width and FWHM are provided for the FeII_opt_ blend at {lambda}4570, H{beta}, HeII {lambda}4686, and the [OIII] {lambda}{lambda}4959, 5007 emission lines. We extract clean broad component H{beta} profiles and provide wavelength measurements at 0, 1/4, 1/2, 3/4, and 0.9 peak intensity levels in order to permit a quantitative definition of the H{beta} broad component for statistical studies. We also discuss sources of uncertainty, selection effects, and biases in our sample. The data are especially important for tests of the eigenvector 1 parameter space occupation and correlation. We show that the I Zw 1 template FeII_opt_ spectrum reproduces well the observed FeII_opt_ emission for a wide range of line width and strength. A detailed analysis of the data within the eigenvector 1 context is deferred to a companion paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199#2</TD>
            <TD>2011-09-14T19:46:22Z</TD>
            <TD>#AGN#Equivalent_widths#Spectroscopy#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/145/199&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/199</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/199 [table2]</TD>
            <TD>Optical spectroscopic atlas of low-redshift AGN (Marziani+, 2003)</TD>
            <TD>We present a spectral atlas of the H{beta} region for 215 type 1 AGNs (luminous Seyfert 1/radio galaxy nuclei and low-z quasars) up to z~0.8. Line profiles and measures were derived from the database of intermediate resolution spectra (R&gt;~1000) with average continuum level S/N ratio ~30. Parameters including rest frame equivalent width and FWHM are provided for the FeII_opt_ blend at {lambda}4570, H{beta}, HeII {lambda}4686, and the [OIII] {lambda}{lambda}4959, 5007 emission lines. We extract clean broad component H{beta} profiles and provide wavelength measurements at 0, 1/4, 1/2, 3/4, and 0.9 peak intensity levels in order to permit a quantitative definition of the H{beta} broad component for statistical studies. We also discuss sources of uncertainty, selection effects, and biases in our sample. The data are especially important for tests of the eigenvector 1 parameter space occupation and correlation. We show that the I Zw 1 template FeII_opt_ spectrum reproduces well the observed FeII_opt_ emission for a wide range of line width and strength. A detailed analysis of the data within the eigenvector 1 context is deferred to a companion paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199#table2</TD>
            <TD>2011-09-14T19:46:22Z</TD>
            <TD>#AGN#Equivalent_widths#Spectroscopy#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/199&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/199</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/526/A72 [1]</TD>
            <TD>Physical param. of EGS early-type gal. (Fernandez Lorenzo+, 2011)</TD>
            <TD>Physical parameters for 135 early-type galaxies in the Extended Groth Strip. For each galaxy equatorial coordinates, total magnitudes in B and g-bands, redshift, velocity dispersion, effective radius, surface brightness, stellar mass, Sersic index, type (elliptical or lenticular) and signal-to-noise of the spectrum are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72#1</TD>
            <TD>2011-09-14T21:11:46Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/526/A72</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A72</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/526/A72 [2]</TD>
            <TD>Physical param. of EGS early-type gal. (Fernandez Lorenzo+, 2011)</TD>
            <TD>Physical parameters for 135 early-type galaxies in the Extended Groth Strip. For each galaxy equatorial coordinates, total magnitudes in B and g-bands, redshift, velocity dispersion, effective radius, surface brightness, stellar mass, Sersic index, type (elliptical or lenticular) and signal-to-noise of the spectrum are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72#2</TD>
            <TD>2011-09-14T21:11:46Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/526/A72&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A72</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/526/A72 [table1]</TD>
            <TD>Physical param. of EGS early-type gal. (Fernandez Lorenzo+, 2011)</TD>
            <TD>Physical parameters for 135 early-type galaxies in the Extended Groth Strip. For each galaxy equatorial coordinates, total magnitudes in B and g-bands, redshift, velocity dispersion, effective radius, surface brightness, stellar mass, Sersic index, type (elliptical or lenticular) and signal-to-noise of the spectrum are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72#table1</TD>
            <TD>2011-09-14T21:11:46Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/526/A72&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A72</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/724/714 [1]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#1</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/724/714</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/724/714 [2]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#2</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/724/714&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/724/714 [tablea1]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#tablea1</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/724/714&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/724/714 [tablea2]</TD>
            <TD>Velocity dispersions of MS1054-03 &amp; Coma galaxies (Holden+, 2010)</TD>
            <TD>We based our sample on a magnitude-limited survey of galaxies in the field of MS 1054-03. The original selection was done using a limiting magnitude of J=21.2mag (Vega) from a catalog of galaxies observed with the CFH12K at CFHT and the WIRC camera on the du Pont. Each galaxy in this sample had either a spectroscopic redshift, or a photometric redshift from a catalog of BVRIJH imaging data. Galaxies with spectroscopic redshifts were preferred in our selection. These photometric redshifts, the catalog construction, and the spectroscopic subsample will be discussed in a later paper. The ACS imaging used in this paper comes from two separate programs. The first, discussed in Blakeslee et al. (2006, Cat. J/ApJ/644/30), used the F606W, F775W, and F850LP filters to image the center of the cluster. The second program imaged the outer regions of MS 1054-03 with the V606 and the F814W, or I814 filter. The spectral data were acquired over two observing runs in 2008 January and March on the DEIMOS spectrograph. Our low-redshift comparison sample is a subset of the Coma sample from Holden et al. (2007ApJ...670..190H).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714#tablea2</TD>
            <TD>2012-09-22T14:53:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/714</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/724/714&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/714</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/145/199 [1]</TD>
            <TD>Optical spectroscopic atlas of low-redshift AGN (Marziani+, 2003)</TD>
            <TD>We present a spectral atlas of the H{beta} region for 215 type 1 AGNs (luminous Seyfert 1/radio galaxy nuclei and low-z quasars) up to z~0.8. Line profiles and measures were derived from the database of intermediate resolution spectra (R&gt;~1000) with average continuum level S/N ratio ~30. Parameters including rest frame equivalent width and FWHM are provided for the FeII_opt_ blend at {lambda}4570, H{beta}, HeII {lambda}4686, and the [OIII] {lambda}{lambda}4959, 5007 emission lines. We extract clean broad component H{beta} profiles and provide wavelength measurements at 0, 1/4, 1/2, 3/4, and 0.9 peak intensity levels in order to permit a quantitative definition of the H{beta} broad component for statistical studies. We also discuss sources of uncertainty, selection effects, and biases in our sample. The data are especially important for tests of the eigenvector 1 parameter space occupation and correlation. We show that the I Zw 1 template FeII_opt_ spectrum reproduces well the observed FeII_opt_ emission for a wide range of line width and strength. A detailed analysis of the data within the eigenvector 1 context is deferred to a companion paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199#1</TD>
            <TD>2011-09-14T19:46:22Z</TD>
            <TD>#AGN#Equivalent_widths#Spectroscopy#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/145/199</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/199</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/145/199 [2]</TD>
            <TD>Optical spectroscopic atlas of low-redshift AGN (Marziani+, 2003)</TD>
            <TD>We present a spectral atlas of the H{beta} region for 215 type 1 AGNs (luminous Seyfert 1/radio galaxy nuclei and low-z quasars) up to z~0.8. Line profiles and measures were derived from the database of intermediate resolution spectra (R&gt;~1000) with average continuum level S/N ratio ~30. Parameters including rest frame equivalent width and FWHM are provided for the FeII_opt_ blend at {lambda}4570, H{beta}, HeII {lambda}4686, and the [OIII] {lambda}{lambda}4959, 5007 emission lines. We extract clean broad component H{beta} profiles and provide wavelength measurements at 0, 1/4, 1/2, 3/4, and 0.9 peak intensity levels in order to permit a quantitative definition of the H{beta} broad component for statistical studies. We also discuss sources of uncertainty, selection effects, and biases in our sample. The data are especially important for tests of the eigenvector 1 parameter space occupation and correlation. We show that the I Zw 1 template FeII_opt_ spectrum reproduces well the observed FeII_opt_ emission for a wide range of line width and strength. A detailed analysis of the data within the eigenvector 1 context is deferred to a companion paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199#2</TD>
            <TD>2011-09-14T19:46:22Z</TD>
            <TD>#AGN#Equivalent_widths#Spectroscopy#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/145/199&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/199</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/199 [table2]</TD>
            <TD>Optical spectroscopic atlas of low-redshift AGN (Marziani+, 2003)</TD>
            <TD>We present a spectral atlas of the H{beta} region for 215 type 1 AGNs (luminous Seyfert 1/radio galaxy nuclei and low-z quasars) up to z~0.8. Line profiles and measures were derived from the database of intermediate resolution spectra (R&gt;~1000) with average continuum level S/N ratio ~30. Parameters including rest frame equivalent width and FWHM are provided for the FeII_opt_ blend at {lambda}4570, H{beta}, HeII {lambda}4686, and the [OIII] {lambda}{lambda}4959, 5007 emission lines. We extract clean broad component H{beta} profiles and provide wavelength measurements at 0, 1/4, 1/2, 3/4, and 0.9 peak intensity levels in order to permit a quantitative definition of the H{beta} broad component for statistical studies. We also discuss sources of uncertainty, selection effects, and biases in our sample. The data are especially important for tests of the eigenvector 1 parameter space occupation and correlation. We show that the I Zw 1 template FeII_opt_ spectrum reproduces well the observed FeII_opt_ emission for a wide range of line width and strength. A detailed analysis of the data within the eigenvector 1 context is deferred to a companion paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199#table2</TD>
            <TD>2011-09-14T19:46:22Z</TD>
            <TD>#AGN#Equivalent_widths#Spectroscopy#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/199&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/199</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/526/A72 [1]</TD>
            <TD>Physical param. of EGS early-type gal. (Fernandez Lorenzo+, 2011)</TD>
            <TD>Physical parameters for 135 early-type galaxies in the Extended Groth Strip. For each galaxy equatorial coordinates, total magnitudes in B and g-bands, redshift, velocity dispersion, effective radius, surface brightness, stellar mass, Sersic index, type (elliptical or lenticular) and signal-to-noise of the spectrum are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72#1</TD>
            <TD>2011-09-14T21:11:46Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/526/A72</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A72</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/526/A72 [2]</TD>
            <TD>Physical param. of EGS early-type gal. (Fernandez Lorenzo+, 2011)</TD>
            <TD>Physical parameters for 135 early-type galaxies in the Extended Groth Strip. For each galaxy equatorial coordinates, total magnitudes in B and g-bands, redshift, velocity dispersion, effective radius, surface brightness, stellar mass, Sersic index, type (elliptical or lenticular) and signal-to-noise of the spectrum are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72#2</TD>
            <TD>2011-09-14T21:11:46Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/526/A72&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A72</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/526/A72 [table1]</TD>
            <TD>Physical param. of EGS early-type gal. (Fernandez Lorenzo+, 2011)</TD>
            <TD>Physical parameters for 135 early-type galaxies in the Extended Groth Strip. For each galaxy equatorial coordinates, total magnitudes in B and g-bands, redshift, velocity dispersion, effective radius, surface brightness, stellar mass, Sersic index, type (elliptical or lenticular) and signal-to-noise of the spectrum are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72#table1</TD>
            <TD>2011-09-14T21:11:46Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/526/A72</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/526/A72&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/526/A72</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/582/668 [1]</TD>
            <TD>Colours and H{alpha} in galaxy pairs (Barton Gillespie+, 2003)</TD>
            <TD>In this paper, we concentrate on the photometric properties of the galaxies in the overlap of the spectroscopic and photometric samples (190 galaxies comprising all or part of 78 pairs and 13 compact groups; hereafter the SP sample). We have H{alpha} rotation curves for 103 of these galaxies; 89 provide useful measurements of Vc, the velocity width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668#1</TD>
            <TD>2012-09-24T07:24:01Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/582/668</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/582/668</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/582/668 [2]</TD>
            <TD>Colours and H{alpha} in galaxy pairs (Barton Gillespie+, 2003)</TD>
            <TD>In this paper, we concentrate on the photometric properties of the galaxies in the overlap of the spectroscopic and photometric samples (190 galaxies comprising all or part of 78 pairs and 13 compact groups; hereafter the SP sample). We have H{alpha} rotation curves for 103 of these galaxies; 89 provide useful measurements of Vc, the velocity width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668#2</TD>
            <TD>2012-09-24T07:24:01Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/582/668&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/582/668</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/582/668 [table1]</TD>
            <TD>Colours and H{alpha} in galaxy pairs (Barton Gillespie+, 2003)</TD>
            <TD>In this paper, we concentrate on the photometric properties of the galaxies in the overlap of the spectroscopic and photometric samples (190 galaxies comprising all or part of 78 pairs and 13 compact groups; hereafter the SP sample). We have H{alpha} rotation curves for 103 of these galaxies; 89 provide useful measurements of Vc, the velocity width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668#table1</TD>
            <TD>2012-09-24T07:24:01Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/582/668&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/582/668</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/523/A61 [1]</TD>
            <TD>INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2010)</TD>
            <TD>This paper is the second in a series devoted to the hard X-ray (17-60keV) whole sky survey performed by the INTEGRAL observatory over seven years. Here we present a catalog of detected sources that includes 521 objects, 449 of which exceed a 5{sigma} detection threshold on the time-averaged map of the sky, and 53 were detected in various subsamples of exposures. Among the identified sources with known and suspected nature, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b|&gt;5deg) and Galactic (|b|&lt;5deg) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61#1</TD>
            <TD>2011-09-14T21:11:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/523/A61</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/523/A61</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/523/A61 [2]</TD>
            <TD>INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2010)</TD>
            <TD>This paper is the second in a series devoted to the hard X-ray (17-60keV) whole sky survey performed by the INTEGRAL observatory over seven years. Here we present a catalog of detected sources that includes 521 objects, 449 of which exceed a 5{sigma} detection threshold on the time-averaged map of the sky, and 53 were detected in various subsamples of exposures. Among the identified sources with known and suspected nature, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b|&gt;5deg) and Galactic (|b|&lt;5deg) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61#2</TD>
            <TD>2011-09-14T21:11:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/523/A61&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/523/A61</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/523/A61 [table2]</TD>
            <TD>INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2010)</TD>
            <TD>This paper is the second in a series devoted to the hard X-ray (17-60keV) whole sky survey performed by the INTEGRAL observatory over seven years. Here we present a catalog of detected sources that includes 521 objects, 449 of which exceed a 5{sigma} detection threshold on the time-averaged map of the sky, and 53 were detected in various subsamples of exposures. Among the identified sources with known and suspected nature, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b|&gt;5deg) and Galactic (|b|&lt;5deg) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61#table2</TD>
            <TD>2011-09-14T21:11:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/523/A61&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/523/A61</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/145/199 [1]</TD>
            <TD>Optical spectroscopic atlas of low-redshift AGN (Marziani+, 2003)</TD>
            <TD>We present a spectral atlas of the H{beta} region for 215 type 1 AGNs (luminous Seyfert 1/radio galaxy nuclei and low-z quasars) up to z~0.8. Line profiles and measures were derived from the database of intermediate resolution spectra (R&gt;~1000) with average continuum level S/N ratio ~30. Parameters including rest frame equivalent width and FWHM are provided for the FeII_opt_ blend at {lambda}4570, H{beta}, HeII {lambda}4686, and the [OIII] {lambda}{lambda}4959, 5007 emission lines. We extract clean broad component H{beta} profiles and provide wavelength measurements at 0, 1/4, 1/2, 3/4, and 0.9 peak intensity levels in order to permit a quantitative definition of the H{beta} broad component for statistical studies. We also discuss sources of uncertainty, selection effects, and biases in our sample. The data are especially important for tests of the eigenvector 1 parameter space occupation and correlation. We show that the I Zw 1 template FeII_opt_ spectrum reproduces well the observed FeII_opt_ emission for a wide range of line width and strength. A detailed analysis of the data within the eigenvector 1 context is deferred to a companion paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199#1</TD>
            <TD>2011-09-14T19:46:22Z</TD>
            <TD>#AGN#Equivalent_widths#Spectroscopy#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/145/199</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/199</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/145/199 [2]</TD>
            <TD>Optical spectroscopic atlas of low-redshift AGN (Marziani+, 2003)</TD>
            <TD>We present a spectral atlas of the H{beta} region for 215 type 1 AGNs (luminous Seyfert 1/radio galaxy nuclei and low-z quasars) up to z~0.8. Line profiles and measures were derived from the database of intermediate resolution spectra (R&gt;~1000) with average continuum level S/N ratio ~30. Parameters including rest frame equivalent width and FWHM are provided for the FeII_opt_ blend at {lambda}4570, H{beta}, HeII {lambda}4686, and the [OIII] {lambda}{lambda}4959, 5007 emission lines. We extract clean broad component H{beta} profiles and provide wavelength measurements at 0, 1/4, 1/2, 3/4, and 0.9 peak intensity levels in order to permit a quantitative definition of the H{beta} broad component for statistical studies. We also discuss sources of uncertainty, selection effects, and biases in our sample. The data are especially important for tests of the eigenvector 1 parameter space occupation and correlation. We show that the I Zw 1 template FeII_opt_ spectrum reproduces well the observed FeII_opt_ emission for a wide range of line width and strength. A detailed analysis of the data within the eigenvector 1 context is deferred to a companion paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199#2</TD>
            <TD>2011-09-14T19:46:22Z</TD>
            <TD>#AGN#Equivalent_widths#Spectroscopy#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/145/199&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/199</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/145/199 [table2]</TD>
            <TD>Optical spectroscopic atlas of low-redshift AGN (Marziani+, 2003)</TD>
            <TD>We present a spectral atlas of the H{beta} region for 215 type 1 AGNs (luminous Seyfert 1/radio galaxy nuclei and low-z quasars) up to z~0.8. Line profiles and measures were derived from the database of intermediate resolution spectra (R&gt;~1000) with average continuum level S/N ratio ~30. Parameters including rest frame equivalent width and FWHM are provided for the FeII_opt_ blend at {lambda}4570, H{beta}, HeII {lambda}4686, and the [OIII] {lambda}{lambda}4959, 5007 emission lines. We extract clean broad component H{beta} profiles and provide wavelength measurements at 0, 1/4, 1/2, 3/4, and 0.9 peak intensity levels in order to permit a quantitative definition of the H{beta} broad component for statistical studies. We also discuss sources of uncertainty, selection effects, and biases in our sample. The data are especially important for tests of the eigenvector 1 parameter space occupation and correlation. We show that the I Zw 1 template FeII_opt_ spectrum reproduces well the observed FeII_opt_ emission for a wide range of line width and strength. A detailed analysis of the data within the eigenvector 1 context is deferred to a companion paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199#table2</TD>
            <TD>2011-09-14T19:46:22Z</TD>
            <TD>#AGN#Equivalent_widths#Spectroscopy#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/145/199</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/145/199&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/145/199</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/582/668 [1]</TD>
            <TD>Colours and H{alpha} in galaxy pairs (Barton Gillespie+, 2003)</TD>
            <TD>In this paper, we concentrate on the photometric properties of the galaxies in the overlap of the spectroscopic and photometric samples (190 galaxies comprising all or part of 78 pairs and 13 compact groups; hereafter the SP sample). We have H{alpha} rotation curves for 103 of these galaxies; 89 provide useful measurements of Vc, the velocity width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668#1</TD>
            <TD>2012-09-24T07:24:01Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/582/668</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/582/668</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/582/668 [2]</TD>
            <TD>Colours and H{alpha} in galaxy pairs (Barton Gillespie+, 2003)</TD>
            <TD>In this paper, we concentrate on the photometric properties of the galaxies in the overlap of the spectroscopic and photometric samples (190 galaxies comprising all or part of 78 pairs and 13 compact groups; hereafter the SP sample). We have H{alpha} rotation curves for 103 of these galaxies; 89 provide useful measurements of Vc, the velocity width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668#2</TD>
            <TD>2012-09-24T07:24:01Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/582/668&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/582/668</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/582/668 [table1]</TD>
            <TD>Colours and H{alpha} in galaxy pairs (Barton Gillespie+, 2003)</TD>
            <TD>In this paper, we concentrate on the photometric properties of the galaxies in the overlap of the spectroscopic and photometric samples (190 galaxies comprising all or part of 78 pairs and 13 compact groups; hereafter the SP sample). We have H{alpha} rotation curves for 103 of these galaxies; 89 provide useful measurements of Vc, the velocity width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668#table1</TD>
            <TD>2012-09-24T07:24:01Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/582/668&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/582/668</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/523/A61 [1]</TD>
            <TD>INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2010)</TD>
            <TD>This paper is the second in a series devoted to the hard X-ray (17-60keV) whole sky survey performed by the INTEGRAL observatory over seven years. Here we present a catalog of detected sources that includes 521 objects, 449 of which exceed a 5{sigma} detection threshold on the time-averaged map of the sky, and 53 were detected in various subsamples of exposures. Among the identified sources with known and suspected nature, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b|&gt;5deg) and Galactic (|b|&lt;5deg) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61#1</TD>
            <TD>2011-09-14T21:11:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/523/A61</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/523/A61</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/523/A61 [2]</TD>
            <TD>INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2010)</TD>
            <TD>This paper is the second in a series devoted to the hard X-ray (17-60keV) whole sky survey performed by the INTEGRAL observatory over seven years. Here we present a catalog of detected sources that includes 521 objects, 449 of which exceed a 5{sigma} detection threshold on the time-averaged map of the sky, and 53 were detected in various subsamples of exposures. Among the identified sources with known and suspected nature, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b|&gt;5deg) and Galactic (|b|&lt;5deg) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61#2</TD>
            <TD>2011-09-14T21:11:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/523/A61&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/523/A61</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/523/A61 [table2]</TD>
            <TD>INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2010)</TD>
            <TD>This paper is the second in a series devoted to the hard X-ray (17-60keV) whole sky survey performed by the INTEGRAL observatory over seven years. Here we present a catalog of detected sources that includes 521 objects, 449 of which exceed a 5{sigma} detection threshold on the time-averaged map of the sky, and 53 were detected in various subsamples of exposures. Among the identified sources with known and suspected nature, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b|&gt;5deg) and Galactic (|b|&lt;5deg) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61#table2</TD>
            <TD>2011-09-14T21:11:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/523/A61&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/523/A61</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/582/668 [1]</TD>
            <TD>Colours and H{alpha} in galaxy pairs (Barton Gillespie+, 2003)</TD>
            <TD>In this paper, we concentrate on the photometric properties of the galaxies in the overlap of the spectroscopic and photometric samples (190 galaxies comprising all or part of 78 pairs and 13 compact groups; hereafter the SP sample). We have H{alpha} rotation curves for 103 of these galaxies; 89 provide useful measurements of Vc, the velocity width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668#1</TD>
            <TD>2012-09-24T07:24:01Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/582/668</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/582/668</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/582/668 [2]</TD>
            <TD>Colours and H{alpha} in galaxy pairs (Barton Gillespie+, 2003)</TD>
            <TD>In this paper, we concentrate on the photometric properties of the galaxies in the overlap of the spectroscopic and photometric samples (190 galaxies comprising all or part of 78 pairs and 13 compact groups; hereafter the SP sample). We have H{alpha} rotation curves for 103 of these galaxies; 89 provide useful measurements of Vc, the velocity width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668#2</TD>
            <TD>2012-09-24T07:24:01Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/582/668&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/582/668</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/582/668 [table1]</TD>
            <TD>Colours and H{alpha} in galaxy pairs (Barton Gillespie+, 2003)</TD>
            <TD>In this paper, we concentrate on the photometric properties of the galaxies in the overlap of the spectroscopic and photometric samples (190 galaxies comprising all or part of 78 pairs and 13 compact groups; hereafter the SP sample). We have H{alpha} rotation curves for 103 of these galaxies; 89 provide useful measurements of Vc, the velocity width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668#table1</TD>
            <TD>2012-09-24T07:24:01Z</TD>
            <TD>#Photometry#Equivalent_widths#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/582/668</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/582/668&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/582/668</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/523/A61 [1]</TD>
            <TD>INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2010)</TD>
            <TD>This paper is the second in a series devoted to the hard X-ray (17-60keV) whole sky survey performed by the INTEGRAL observatory over seven years. Here we present a catalog of detected sources that includes 521 objects, 449 of which exceed a 5{sigma} detection threshold on the time-averaged map of the sky, and 53 were detected in various subsamples of exposures. Among the identified sources with known and suspected nature, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b|&gt;5deg) and Galactic (|b|&lt;5deg) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61#1</TD>
            <TD>2011-09-14T21:11:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/523/A61</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/523/A61</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/523/A61 [2]</TD>
            <TD>INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2010)</TD>
            <TD>This paper is the second in a series devoted to the hard X-ray (17-60keV) whole sky survey performed by the INTEGRAL observatory over seven years. Here we present a catalog of detected sources that includes 521 objects, 449 of which exceed a 5{sigma} detection threshold on the time-averaged map of the sky, and 53 were detected in various subsamples of exposures. Among the identified sources with known and suspected nature, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b|&gt;5deg) and Galactic (|b|&lt;5deg) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61#2</TD>
            <TD>2011-09-14T21:11:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/523/A61&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/523/A61</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/523/A61 [table2]</TD>
            <TD>INTEGRAL all-sky survey of hard X-ray sources (Krivonos+, 2010)</TD>
            <TD>This paper is the second in a series devoted to the hard X-ray (17-60keV) whole sky survey performed by the INTEGRAL observatory over seven years. Here we present a catalog of detected sources that includes 521 objects, 449 of which exceed a 5{sigma} detection threshold on the time-averaged map of the sky, and 53 were detected in various subsamples of exposures. Among the identified sources with known and suspected nature, 262 are Galactic (101 low-mass X-ray binaries, 94 high-mass X-ray binaries, 37 cataclysmic variables, and 30 of other types) and 221 are extragalactic, including 217 active galactic nuclei (AGNs) and 4 galaxy clusters. The extragalactic (|b|&gt;5deg) and Galactic (|b|&lt;5deg) persistently detected source samples have high identification completeness (respectively ~96% and ~93%) and are valuable for population studies.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61#table2</TD>
            <TD>2011-09-14T21:11:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/523/A61</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/523/A61&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/523/A61</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/247 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#1</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/247</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/247 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#2</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/116/247&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/116/247 [table2]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#table2</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/116/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/116/247 [table3]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#table3</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/116/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/379/35 [1]</TD>
            <TD>Radio-optically selected galaxy clusters. II. (Zanichelli+, 2001)</TD>
            <TD>File table1.dat contains data relative to spectroscopic and photometric observations of galaxies in 12 radio-optically selected candidate clusters. Observations have been acquired with the 3.6m ESO telescope, Chile. For each galaxy in the cluster, a sequential number, the magnitude in r-Gunn filter, the measured velocity, velocity rms, and notes to identify particular objects (emission galaxies, radiogalaxies and stars) are given.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35#1</TD>
            <TD>2012-09-24T07:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/379/35</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/35</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/379/35 [2]</TD>
            <TD>Radio-optically selected galaxy clusters. II. (Zanichelli+, 2001)</TD>
            <TD>File table1.dat contains data relative to spectroscopic and photometric observations of galaxies in 12 radio-optically selected candidate clusters. Observations have been acquired with the 3.6m ESO telescope, Chile. For each galaxy in the cluster, a sequential number, the magnitude in r-Gunn filter, the measured velocity, velocity rms, and notes to identify particular objects (emission galaxies, radiogalaxies and stars) are given.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35#2</TD>
            <TD>2012-09-24T07:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/379/35&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/379/35 [table2]</TD>
            <TD>Radio-optically selected galaxy clusters. II. (Zanichelli+, 2001)</TD>
            <TD>File table1.dat contains data relative to spectroscopic and photometric observations of galaxies in 12 radio-optically selected candidate clusters. Observations have been acquired with the 3.6m ESO telescope, Chile. For each galaxy in the cluster, a sequential number, the magnitude in r-Gunn filter, the measured velocity, velocity rms, and notes to identify particular objects (emission galaxies, radiogalaxies and stars) are given.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35#table2</TD>
            <TD>2012-09-24T07:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/379/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/35</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/404/1490 [1]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#1</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/404/1490</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/404/1490 [2]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#2</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/404/1490&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/404/1490 [table2]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#table2</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/404/1490&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/404/1490 [table1]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#table1</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/404/1490&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/247 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#1</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/247</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/247 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#2</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/116/247&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/116/247 [table2]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#table2</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/116/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/116/247 [table3]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#table3</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/116/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/379/35 [1]</TD>
            <TD>Radio-optically selected galaxy clusters. II. (Zanichelli+, 2001)</TD>
            <TD>File table1.dat contains data relative to spectroscopic and photometric observations of galaxies in 12 radio-optically selected candidate clusters. Observations have been acquired with the 3.6m ESO telescope, Chile. For each galaxy in the cluster, a sequential number, the magnitude in r-Gunn filter, the measured velocity, velocity rms, and notes to identify particular objects (emission galaxies, radiogalaxies and stars) are given.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35#1</TD>
            <TD>2012-09-24T07:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/379/35</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/35</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/379/35 [2]</TD>
            <TD>Radio-optically selected galaxy clusters. II. (Zanichelli+, 2001)</TD>
            <TD>File table1.dat contains data relative to spectroscopic and photometric observations of galaxies in 12 radio-optically selected candidate clusters. Observations have been acquired with the 3.6m ESO telescope, Chile. For each galaxy in the cluster, a sequential number, the magnitude in r-Gunn filter, the measured velocity, velocity rms, and notes to identify particular objects (emission galaxies, radiogalaxies and stars) are given.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35#2</TD>
            <TD>2012-09-24T07:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/379/35&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/379/35 [table2]</TD>
            <TD>Radio-optically selected galaxy clusters. II. (Zanichelli+, 2001)</TD>
            <TD>File table1.dat contains data relative to spectroscopic and photometric observations of galaxies in 12 radio-optically selected candidate clusters. Observations have been acquired with the 3.6m ESO telescope, Chile. For each galaxy in the cluster, a sequential number, the magnitude in r-Gunn filter, the measured velocity, velocity rms, and notes to identify particular objects (emission galaxies, radiogalaxies and stars) are given.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35#table2</TD>
            <TD>2012-09-24T07:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/379/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/35</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/404/1490 [1]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#1</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/404/1490</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/404/1490 [2]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#2</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/404/1490&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/404/1490 [table2]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#table2</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/404/1490&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/404/1490 [table1]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#table1</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/404/1490&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/116/247 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#1</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/116/247</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/116/247 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#2</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/116/247&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/116/247 [table2]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#table2</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/116/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/116/247 [table3]</TD>
            <TD>CNOC cluster redshift survey catalogs. VI. (Ellingson+ 1998)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247#table3</TD>
            <TD>2011-09-14T19:46:53Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/116/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/116/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/116/247</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/404/1490 [1]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#1</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/404/1490</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/404/1490 [2]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#2</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/404/1490&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/404/1490 [table2]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#table2</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/404/1490&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/404/1490 [table1]</TD>
            <TD>Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)</TD>
            <TD>We compare the apparent axial ratio distributions of the brightest cluster galaxies (BCGs) and normal ellipticals (Es) in our sample of 75 galaxy clusters from the WIde-field Nearby Galaxy-cluster Survey (WINGS). Most BCGs in our clusters (69 per cent) are classified as cD galaxies. The sample of cDs has been completed by 14 additional cDs (non-BCGs) we found in our clusters. We deproject the apparent axial ratio distributions of Es, BCGs and cDs using a bivariate version of the Lucy rectification algorithm, whose results are supported by an independent Monte Carlo technique. Finally, we compare the intrinsic shape distribution of BCGs to the corresponding shape distribution of the central part of cluster-sized dark matter haloes extracted from the GIF2 Lambda cold dark matter ({LAMBDA}CDM) N-body simulations (Gao et al., 2004MNRAS.355..819G).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490#table1</TD>
            <TD>2011-09-14T21:12:45Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Nov-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/1490</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/404/1490&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/1490</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/355/1251 [1]</TD>
            <TD>Bar-induced strengths in spiral galaxies (Laurikainen+, 2004)</TD>
            <TD>Bar-induced perturbation strengths are calculated for a well-defined magnitude-limited sample of 180 spiral galaxies, based on the Ohio State University Bright Galaxy Survey. We use a gravitational torque method, the ratio of the maximal tangential force to the mean axisymmetric radial force, as a quantitative measure of the bar strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251#1</TD>
            <TD>2011-09-14T19:46:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/355/1251</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/355/1251</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/355/1251 [2]</TD>
            <TD>Bar-induced strengths in spiral galaxies (Laurikainen+, 2004)</TD>
            <TD>Bar-induced perturbation strengths are calculated for a well-defined magnitude-limited sample of 180 spiral galaxies, based on the Ohio State University Bright Galaxy Survey. We use a gravitational torque method, the ratio of the maximal tangential force to the mean axisymmetric radial force, as a quantitative measure of the bar strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251#2</TD>
            <TD>2011-09-14T19:46:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/355/1251&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/355/1251</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/355/1251 [table2]</TD>
            <TD>Bar-induced strengths in spiral galaxies (Laurikainen+, 2004)</TD>
            <TD>Bar-induced perturbation strengths are calculated for a well-defined magnitude-limited sample of 180 spiral galaxies, based on the Ohio State University Bright Galaxy Survey. We use a gravitational torque method, the ratio of the maximal tangential force to the mean axisymmetric radial force, as a quantitative measure of the bar strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251#table2</TD>
            <TD>2011-09-14T19:46:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/355/1251&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/355/1251</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/379/35 [1]</TD>
            <TD>Radio-optically selected galaxy clusters. II. (Zanichelli+, 2001)</TD>
            <TD>File table1.dat contains data relative to spectroscopic and photometric observations of galaxies in 12 radio-optically selected candidate clusters. Observations have been acquired with the 3.6m ESO telescope, Chile. For each galaxy in the cluster, a sequential number, the magnitude in r-Gunn filter, the measured velocity, velocity rms, and notes to identify particular objects (emission galaxies, radiogalaxies and stars) are given.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35#1</TD>
            <TD>2012-09-24T07:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/379/35</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/35</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/379/35 [2]</TD>
            <TD>Radio-optically selected galaxy clusters. II. (Zanichelli+, 2001)</TD>
            <TD>File table1.dat contains data relative to spectroscopic and photometric observations of galaxies in 12 radio-optically selected candidate clusters. Observations have been acquired with the 3.6m ESO telescope, Chile. For each galaxy in the cluster, a sequential number, the magnitude in r-Gunn filter, the measured velocity, velocity rms, and notes to identify particular objects (emission galaxies, radiogalaxies and stars) are given.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35#2</TD>
            <TD>2012-09-24T07:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/379/35&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/35</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/379/35 [table2]</TD>
            <TD>Radio-optically selected galaxy clusters. II. (Zanichelli+, 2001)</TD>
            <TD>File table1.dat contains data relative to spectroscopic and photometric observations of galaxies in 12 radio-optically selected candidate clusters. Observations have been acquired with the 3.6m ESO telescope, Chile. For each galaxy in the cluster, a sequential number, the magnitude in r-Gunn filter, the measured velocity, velocity rms, and notes to identify particular objects (emission galaxies, radiogalaxies and stars) are given.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35#table2</TD>
            <TD>2012-09-24T07:25:46Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/35</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/379/35&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/35</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/686/749 [1]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#1</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/686/749</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/686/749 [2]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#2</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [42sne]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#42sne</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [table11]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#table11</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [table1]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#table1</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [table9]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#table9</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/355/1251 [1]</TD>
            <TD>Bar-induced strengths in spiral galaxies (Laurikainen+, 2004)</TD>
            <TD>Bar-induced perturbation strengths are calculated for a well-defined magnitude-limited sample of 180 spiral galaxies, based on the Ohio State University Bright Galaxy Survey. We use a gravitational torque method, the ratio of the maximal tangential force to the mean axisymmetric radial force, as a quantitative measure of the bar strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251#1</TD>
            <TD>2011-09-14T19:46:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/355/1251</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/355/1251</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/355/1251 [2]</TD>
            <TD>Bar-induced strengths in spiral galaxies (Laurikainen+, 2004)</TD>
            <TD>Bar-induced perturbation strengths are calculated for a well-defined magnitude-limited sample of 180 spiral galaxies, based on the Ohio State University Bright Galaxy Survey. We use a gravitational torque method, the ratio of the maximal tangential force to the mean axisymmetric radial force, as a quantitative measure of the bar strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251#2</TD>
            <TD>2011-09-14T19:46:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/355/1251&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/355/1251</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/355/1251 [table2]</TD>
            <TD>Bar-induced strengths in spiral galaxies (Laurikainen+, 2004)</TD>
            <TD>Bar-induced perturbation strengths are calculated for a well-defined magnitude-limited sample of 180 spiral galaxies, based on the Ohio State University Bright Galaxy Survey. We use a gravitational torque method, the ratio of the maximal tangential force to the mean axisymmetric radial force, as a quantitative measure of the bar strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251#table2</TD>
            <TD>2011-09-14T19:46:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/355/1251&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/355/1251</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/87 [1]</TD>
            <TD>ROSAT RASS II observations of IRAS galaxies (Boller+ 1998)</TD>
            <TD>The 120000 X-ray sources detected in the RASS II processing of the ROSAT All-Sky Survey are correlated with the 14315 IRAS galaxies selected from the IRAS Point Source Catalogue: 372 IRAS galaxies show X-ray emission within a distance of 100 arcsec from the infrared position. By inspecting the structure of the X-ray emission in overlays on optical images we quantify the likelihood that the X-rays originate from the IRAS galaxy. For 197 objects the soft X-ray emission is very likely associated with the IRAS galaxy. Their soft X-ray properties are determined and compared with their far-infrared emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87#1</TD>
            <TD>2012-09-24T07:28:18Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/87 [2]</TD>
            <TD>ROSAT RASS II observations of IRAS galaxies (Boller+ 1998)</TD>
            <TD>The 120000 X-ray sources detected in the RASS II processing of the ROSAT All-Sky Survey are correlated with the 14315 IRAS galaxies selected from the IRAS Point Source Catalogue: 372 IRAS galaxies show X-ray emission within a distance of 100 arcsec from the infrared position. By inspecting the structure of the X-ray emission in overlays on optical images we quantify the likelihood that the X-rays originate from the IRAS galaxy. For 197 objects the soft X-ray emission is very likely associated with the IRAS galaxy. Their soft X-ray properties are determined and compared with their far-infrared emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87#2</TD>
            <TD>2012-09-24T07:28:18Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/129/87 [table3]</TD>
            <TD>ROSAT RASS II observations of IRAS galaxies (Boller+ 1998)</TD>
            <TD>The 120000 X-ray sources detected in the RASS II processing of the ROSAT All-Sky Survey are correlated with the 14315 IRAS galaxies selected from the IRAS Point Source Catalogue: 372 IRAS galaxies show X-ray emission within a distance of 100 arcsec from the infrared position. By inspecting the structure of the X-ray emission in overlays on optical images we quantify the likelihood that the X-rays originate from the IRAS galaxy. For 197 objects the soft X-ray emission is very likely associated with the IRAS galaxy. Their soft X-ray properties are determined and compared with their far-infrared emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87#table3</TD>
            <TD>2012-09-24T07:28:18Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/129/87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/87</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/686/749 [1]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#1</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/686/749</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/686/749 [2]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#2</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [42sne]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#42sne</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [table11]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#table11</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [table1]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#table1</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [table9]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#table9</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/355/1251 [1]</TD>
            <TD>Bar-induced strengths in spiral galaxies (Laurikainen+, 2004)</TD>
            <TD>Bar-induced perturbation strengths are calculated for a well-defined magnitude-limited sample of 180 spiral galaxies, based on the Ohio State University Bright Galaxy Survey. We use a gravitational torque method, the ratio of the maximal tangential force to the mean axisymmetric radial force, as a quantitative measure of the bar strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251#1</TD>
            <TD>2011-09-14T19:46:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/355/1251</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/355/1251</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/355/1251 [2]</TD>
            <TD>Bar-induced strengths in spiral galaxies (Laurikainen+, 2004)</TD>
            <TD>Bar-induced perturbation strengths are calculated for a well-defined magnitude-limited sample of 180 spiral galaxies, based on the Ohio State University Bright Galaxy Survey. We use a gravitational torque method, the ratio of the maximal tangential force to the mean axisymmetric radial force, as a quantitative measure of the bar strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251#2</TD>
            <TD>2011-09-14T19:46:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/355/1251&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/355/1251</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/355/1251 [table2]</TD>
            <TD>Bar-induced strengths in spiral galaxies (Laurikainen+, 2004)</TD>
            <TD>Bar-induced perturbation strengths are calculated for a well-defined magnitude-limited sample of 180 spiral galaxies, based on the Ohio State University Bright Galaxy Survey. We use a gravitational torque method, the ratio of the maximal tangential force to the mean axisymmetric radial force, as a quantitative measure of the bar strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251#table2</TD>
            <TD>2011-09-14T19:46:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/355/1251</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/355/1251&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/355/1251</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/87 [1]</TD>
            <TD>ROSAT RASS II observations of IRAS galaxies (Boller+ 1998)</TD>
            <TD>The 120000 X-ray sources detected in the RASS II processing of the ROSAT All-Sky Survey are correlated with the 14315 IRAS galaxies selected from the IRAS Point Source Catalogue: 372 IRAS galaxies show X-ray emission within a distance of 100 arcsec from the infrared position. By inspecting the structure of the X-ray emission in overlays on optical images we quantify the likelihood that the X-rays originate from the IRAS galaxy. For 197 objects the soft X-ray emission is very likely associated with the IRAS galaxy. Their soft X-ray properties are determined and compared with their far-infrared emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87#1</TD>
            <TD>2012-09-24T07:28:18Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/87 [2]</TD>
            <TD>ROSAT RASS II observations of IRAS galaxies (Boller+ 1998)</TD>
            <TD>The 120000 X-ray sources detected in the RASS II processing of the ROSAT All-Sky Survey are correlated with the 14315 IRAS galaxies selected from the IRAS Point Source Catalogue: 372 IRAS galaxies show X-ray emission within a distance of 100 arcsec from the infrared position. By inspecting the structure of the X-ray emission in overlays on optical images we quantify the likelihood that the X-rays originate from the IRAS galaxy. For 197 objects the soft X-ray emission is very likely associated with the IRAS galaxy. Their soft X-ray properties are determined and compared with their far-infrared emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87#2</TD>
            <TD>2012-09-24T07:28:18Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/129/87 [table3]</TD>
            <TD>ROSAT RASS II observations of IRAS galaxies (Boller+ 1998)</TD>
            <TD>The 120000 X-ray sources detected in the RASS II processing of the ROSAT All-Sky Survey are correlated with the 14315 IRAS galaxies selected from the IRAS Point Source Catalogue: 372 IRAS galaxies show X-ray emission within a distance of 100 arcsec from the infrared position. By inspecting the structure of the X-ray emission in overlays on optical images we quantify the likelihood that the X-rays originate from the IRAS galaxy. For 197 objects the soft X-ray emission is very likely associated with the IRAS galaxy. Their soft X-ray properties are determined and compared with their far-infrared emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87#table3</TD>
            <TD>2012-09-24T07:28:18Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/129/87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/87</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/686/749 [1]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#1</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/686/749</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/686/749 [2]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#2</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [42sne]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#42sne</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [table11]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#table11</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [table1]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#table1</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/686/749 [table9]</TD>
            <TD>Improved cosmological constraints from SNe (Kowalski+, 2008)</TD>
            <TD>The SN light curve data presented in this paper were obtained as part of the SCP Nearby 1999 Supernova Campaign (Aldering 2000AIPC..522...75A) and was performed in collaboration with a number of wide-field CCD imaging teams: EROS-II, NGSS, QUEST-I, NEAT, and Spacewatch. Photometric follow-up observations were obtained with the LICK 1m, YALO 1m, CTIO 0.9m, CTIO 1.5m, MARLY, Danish 1.5m, ESO 3.6m, KPNO 2.1m, JKT 1m, CFHT 3.6m, KECK-I 10m, WIYN 3.5m, and MLO 1m telescopes. These consist of UBVRI photometry with a nominal cadence of 3-7 days. The follow-up observations were performed between February and 1999 June, and additional reference images to determine the contribution of host galaxy light contamination were obtained in spring 2000.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749#table9</TD>
            <TD>2011-09-14T21:13:19Z</TD>
            <TD>#Photometry:wide-band#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/686/749</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/686/749&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/686/749</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/433/497 [1]</TD>
            <TD>Nearby early-type galaxies with ionized gas. I. (Rampazzo+, 2005)</TD>
            <TD>With the aim of building a data-set of spectral properties of well studied early-type galaxies showing emission lines, we present intermediate resolution spectra of 50 galaxies in the nearby Universe. The sample, which covers several of the E and S0 morphological sub-classes, is biased toward objects that might be expected to have ongoing and recent star formation, at least in small amounts, because of the presence of the emission lines. The emission is expected to come from the combination of active galactic nuclei and star formation regions within the galaxies. Sample galaxies are located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. Our long-slit spectra cover the 3700-7250{AA} wavelength range with a spectral resolution of approximately 7.6{AA} at 5550{AA}. The specific aim of this paper, and our first step in the investigation, is to map the underlying galaxy stellar population by measuring, along the slit positioned along the galaxy major axis, line-strength indices at several, homogeneous galacto-centric distances. For each object we extracted 7 luminosity-weighted apertures (with radii 1.5", 2.5", 10", r_e/10_, r_e/8_, r_e/4_ and r_e/2_) corrected for the galaxy ellipticity and 4 gradients (0&lt;r&lt;r_e/16_, r_e/16_&lt;r&lt;r_e/8_, r_e/8_&lt;r&lt;r_e/4_ and r_e/4_&lt;r&lt;r_e/2_). For each aperture and gradient we measured 25 line-strength indices: 21 of the set defined by the Lick-IDS ``standard'' system (Trager et al., 1998, Cat. J/ApJS/116/1) and 4 introduced by Worthey &amp; Ottaviani (1997, Cat. J/ApJS/111/377). Line-strength indices have been transformed to the Lick-IDS system. Indices derived then include H{beta}, Mg_1_, Mg_2_, Mgb, MgFe, Fe5270, Fe5335 commonly used in classic index-index diagrams. The paper introduces the sample, presents the observations, describes the data reduction procedures, the extraction of apertures and gradients, the determination and correction of the line-strength indices, the procedure adopted to transform them into the Lick-IDS System and the procedures adopted for the emission correction. We finally discuss the comparisons between our dataset and line-strength indices available in the literature. A significant fraction, about 60%, of galaxies in the present sample has one previous measurement in the Lick-IDS system but basically restricted within the r_e/8_ region. Line-strength measures obtained both from apertures and gradients outside this area and within the r_e/8_ region, with the present radial mapping, are completely new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497#1</TD>
            <TD>2011-09-14T20:01:35Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/433/497</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/433/497</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/433/497 [2]</TD>
            <TD>Nearby early-type galaxies with ionized gas. I. (Rampazzo+, 2005)</TD>
            <TD>With the aim of building a data-set of spectral properties of well studied early-type galaxies showing emission lines, we present intermediate resolution spectra of 50 galaxies in the nearby Universe. The sample, which covers several of the E and S0 morphological sub-classes, is biased toward objects that might be expected to have ongoing and recent star formation, at least in small amounts, because of the presence of the emission lines. The emission is expected to come from the combination of active galactic nuclei and star formation regions within the galaxies. Sample galaxies are located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. Our long-slit spectra cover the 3700-7250{AA} wavelength range with a spectral resolution of approximately 7.6{AA} at 5550{AA}. The specific aim of this paper, and our first step in the investigation, is to map the underlying galaxy stellar population by measuring, along the slit positioned along the galaxy major axis, line-strength indices at several, homogeneous galacto-centric distances. For each object we extracted 7 luminosity-weighted apertures (with radii 1.5", 2.5", 10", r_e/10_, r_e/8_, r_e/4_ and r_e/2_) corrected for the galaxy ellipticity and 4 gradients (0&lt;r&lt;r_e/16_, r_e/16_&lt;r&lt;r_e/8_, r_e/8_&lt;r&lt;r_e/4_ and r_e/4_&lt;r&lt;r_e/2_). For each aperture and gradient we measured 25 line-strength indices: 21 of the set defined by the Lick-IDS ``standard'' system (Trager et al., 1998, Cat. J/ApJS/116/1) and 4 introduced by Worthey &amp; Ottaviani (1997, Cat. J/ApJS/111/377). Line-strength indices have been transformed to the Lick-IDS system. Indices derived then include H{beta}, Mg_1_, Mg_2_, Mgb, MgFe, Fe5270, Fe5335 commonly used in classic index-index diagrams. The paper introduces the sample, presents the observations, describes the data reduction procedures, the extraction of apertures and gradients, the determination and correction of the line-strength indices, the procedure adopted to transform them into the Lick-IDS System and the procedures adopted for the emission correction. We finally discuss the comparisons between our dataset and line-strength indices available in the literature. A significant fraction, about 60%, of galaxies in the present sample has one previous measurement in the Lick-IDS system but basically restricted within the r_e/8_ region. Line-strength measures obtained both from apertures and gradients outside this area and within the r_e/8_ region, with the present radial mapping, are completely new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497#2</TD>
            <TD>2011-09-14T20:01:35Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/433/497&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/433/497</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/433/497 [table1]</TD>
            <TD>Nearby early-type galaxies with ionized gas. I. (Rampazzo+, 2005)</TD>
            <TD>With the aim of building a data-set of spectral properties of well studied early-type galaxies showing emission lines, we present intermediate resolution spectra of 50 galaxies in the nearby Universe. The sample, which covers several of the E and S0 morphological sub-classes, is biased toward objects that might be expected to have ongoing and recent star formation, at least in small amounts, because of the presence of the emission lines. The emission is expected to come from the combination of active galactic nuclei and star formation regions within the galaxies. Sample galaxies are located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. Our long-slit spectra cover the 3700-7250{AA} wavelength range with a spectral resolution of approximately 7.6{AA} at 5550{AA}. The specific aim of this paper, and our first step in the investigation, is to map the underlying galaxy stellar population by measuring, along the slit positioned along the galaxy major axis, line-strength indices at several, homogeneous galacto-centric distances. For each object we extracted 7 luminosity-weighted apertures (with radii 1.5", 2.5", 10", r_e/10_, r_e/8_, r_e/4_ and r_e/2_) corrected for the galaxy ellipticity and 4 gradients (0&lt;r&lt;r_e/16_, r_e/16_&lt;r&lt;r_e/8_, r_e/8_&lt;r&lt;r_e/4_ and r_e/4_&lt;r&lt;r_e/2_). For each aperture and gradient we measured 25 line-strength indices: 21 of the set defined by the Lick-IDS ``standard'' system (Trager et al., 1998, Cat. J/ApJS/116/1) and 4 introduced by Worthey &amp; Ottaviani (1997, Cat. J/ApJS/111/377). Line-strength indices have been transformed to the Lick-IDS system. Indices derived then include H{beta}, Mg_1_, Mg_2_, Mgb, MgFe, Fe5270, Fe5335 commonly used in classic index-index diagrams. The paper introduces the sample, presents the observations, describes the data reduction procedures, the extraction of apertures and gradients, the determination and correction of the line-strength indices, the procedure adopted to transform them into the Lick-IDS System and the procedures adopted for the emission correction. We finally discuss the comparisons between our dataset and line-strength indices available in the literature. A significant fraction, about 60%, of galaxies in the present sample has one previous measurement in the Lick-IDS system but basically restricted within the r_e/8_ region. Line-strength measures obtained both from apertures and gradients outside this area and within the r_e/8_ region, with the present radial mapping, are completely new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497#table1</TD>
            <TD>2011-09-14T20:01:35Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/433/497&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/433/497</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/129/87 [1]</TD>
            <TD>ROSAT RASS II observations of IRAS galaxies (Boller+ 1998)</TD>
            <TD>The 120000 X-ray sources detected in the RASS II processing of the ROSAT All-Sky Survey are correlated with the 14315 IRAS galaxies selected from the IRAS Point Source Catalogue: 372 IRAS galaxies show X-ray emission within a distance of 100 arcsec from the infrared position. By inspecting the structure of the X-ray emission in overlays on optical images we quantify the likelihood that the X-rays originate from the IRAS galaxy. For 197 objects the soft X-ray emission is very likely associated with the IRAS galaxy. Their soft X-ray properties are determined and compared with their far-infrared emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87#1</TD>
            <TD>2012-09-24T07:28:18Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/129/87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/129/87 [2]</TD>
            <TD>ROSAT RASS II observations of IRAS galaxies (Boller+ 1998)</TD>
            <TD>The 120000 X-ray sources detected in the RASS II processing of the ROSAT All-Sky Survey are correlated with the 14315 IRAS galaxies selected from the IRAS Point Source Catalogue: 372 IRAS galaxies show X-ray emission within a distance of 100 arcsec from the infrared position. By inspecting the structure of the X-ray emission in overlays on optical images we quantify the likelihood that the X-rays originate from the IRAS galaxy. For 197 objects the soft X-ray emission is very likely associated with the IRAS galaxy. Their soft X-ray properties are determined and compared with their far-infrared emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87#2</TD>
            <TD>2012-09-24T07:28:18Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/129/87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/129/87 [table3]</TD>
            <TD>ROSAT RASS II observations of IRAS galaxies (Boller+ 1998)</TD>
            <TD>The 120000 X-ray sources detected in the RASS II processing of the ROSAT All-Sky Survey are correlated with the 14315 IRAS galaxies selected from the IRAS Point Source Catalogue: 372 IRAS galaxies show X-ray emission within a distance of 100 arcsec from the infrared position. By inspecting the structure of the X-ray emission in overlays on optical images we quantify the likelihood that the X-rays originate from the IRAS galaxy. For 197 objects the soft X-ray emission is very likely associated with the IRAS galaxy. Their soft X-ray properties are determined and compared with their far-infrared emission.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87#table3</TD>
            <TD>2012-09-24T07:28:18Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/129/87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/129/87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/129/87</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/403/683 [1]</TD>
            <TD>GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)</TD>
            <TD>We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality HI-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^10^M_{sun}_ and redshifts 0.025&lt;z&lt;0.05, selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5-5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the HI gas fraction with galaxy structure and NUV-r colour.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683#1</TD>
            <TD>2011-09-14T21:25:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/403/683</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/683</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/403/683 [2]</TD>
            <TD>GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)</TD>
            <TD>We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality HI-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^10^M_{sun}_ and redshifts 0.025&lt;z&lt;0.05, selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5-5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the HI gas fraction with galaxy structure and NUV-r colour.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683#2</TD>
            <TD>2011-09-14T21:25:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/403/683&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/683</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/683 [table1]</TD>
            <TD>GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)</TD>
            <TD>We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality HI-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^10^M_{sun}_ and redshifts 0.025&lt;z&lt;0.05, selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5-5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the HI gas fraction with galaxy structure and NUV-r colour.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683#table1</TD>
            <TD>2011-09-14T21:25:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/683&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/683</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/433/497 [1]</TD>
            <TD>Nearby early-type galaxies with ionized gas. I. (Rampazzo+, 2005)</TD>
            <TD>With the aim of building a data-set of spectral properties of well studied early-type galaxies showing emission lines, we present intermediate resolution spectra of 50 galaxies in the nearby Universe. The sample, which covers several of the E and S0 morphological sub-classes, is biased toward objects that might be expected to have ongoing and recent star formation, at least in small amounts, because of the presence of the emission lines. The emission is expected to come from the combination of active galactic nuclei and star formation regions within the galaxies. Sample galaxies are located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. Our long-slit spectra cover the 3700-7250{AA} wavelength range with a spectral resolution of approximately 7.6{AA} at 5550{AA}. The specific aim of this paper, and our first step in the investigation, is to map the underlying galaxy stellar population by measuring, along the slit positioned along the galaxy major axis, line-strength indices at several, homogeneous galacto-centric distances. For each object we extracted 7 luminosity-weighted apertures (with radii 1.5", 2.5", 10", r_e/10_, r_e/8_, r_e/4_ and r_e/2_) corrected for the galaxy ellipticity and 4 gradients (0&lt;r&lt;r_e/16_, r_e/16_&lt;r&lt;r_e/8_, r_e/8_&lt;r&lt;r_e/4_ and r_e/4_&lt;r&lt;r_e/2_). For each aperture and gradient we measured 25 line-strength indices: 21 of the set defined by the Lick-IDS ``standard'' system (Trager et al., 1998, Cat. J/ApJS/116/1) and 4 introduced by Worthey &amp; Ottaviani (1997, Cat. J/ApJS/111/377). Line-strength indices have been transformed to the Lick-IDS system. Indices derived then include H{beta}, Mg_1_, Mg_2_, Mgb, MgFe, Fe5270, Fe5335 commonly used in classic index-index diagrams. The paper introduces the sample, presents the observations, describes the data reduction procedures, the extraction of apertures and gradients, the determination and correction of the line-strength indices, the procedure adopted to transform them into the Lick-IDS System and the procedures adopted for the emission correction. We finally discuss the comparisons between our dataset and line-strength indices available in the literature. A significant fraction, about 60%, of galaxies in the present sample has one previous measurement in the Lick-IDS system but basically restricted within the r_e/8_ region. Line-strength measures obtained both from apertures and gradients outside this area and within the r_e/8_ region, with the present radial mapping, are completely new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497#1</TD>
            <TD>2011-09-14T20:01:35Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/433/497</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/433/497</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/433/497 [2]</TD>
            <TD>Nearby early-type galaxies with ionized gas. I. (Rampazzo+, 2005)</TD>
            <TD>With the aim of building a data-set of spectral properties of well studied early-type galaxies showing emission lines, we present intermediate resolution spectra of 50 galaxies in the nearby Universe. The sample, which covers several of the E and S0 morphological sub-classes, is biased toward objects that might be expected to have ongoing and recent star formation, at least in small amounts, because of the presence of the emission lines. The emission is expected to come from the combination of active galactic nuclei and star formation regions within the galaxies. Sample galaxies are located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. Our long-slit spectra cover the 3700-7250{AA} wavelength range with a spectral resolution of approximately 7.6{AA} at 5550{AA}. The specific aim of this paper, and our first step in the investigation, is to map the underlying galaxy stellar population by measuring, along the slit positioned along the galaxy major axis, line-strength indices at several, homogeneous galacto-centric distances. For each object we extracted 7 luminosity-weighted apertures (with radii 1.5", 2.5", 10", r_e/10_, r_e/8_, r_e/4_ and r_e/2_) corrected for the galaxy ellipticity and 4 gradients (0&lt;r&lt;r_e/16_, r_e/16_&lt;r&lt;r_e/8_, r_e/8_&lt;r&lt;r_e/4_ and r_e/4_&lt;r&lt;r_e/2_). For each aperture and gradient we measured 25 line-strength indices: 21 of the set defined by the Lick-IDS ``standard'' system (Trager et al., 1998, Cat. J/ApJS/116/1) and 4 introduced by Worthey &amp; Ottaviani (1997, Cat. J/ApJS/111/377). Line-strength indices have been transformed to the Lick-IDS system. Indices derived then include H{beta}, Mg_1_, Mg_2_, Mgb, MgFe, Fe5270, Fe5335 commonly used in classic index-index diagrams. The paper introduces the sample, presents the observations, describes the data reduction procedures, the extraction of apertures and gradients, the determination and correction of the line-strength indices, the procedure adopted to transform them into the Lick-IDS System and the procedures adopted for the emission correction. We finally discuss the comparisons between our dataset and line-strength indices available in the literature. A significant fraction, about 60%, of galaxies in the present sample has one previous measurement in the Lick-IDS system but basically restricted within the r_e/8_ region. Line-strength measures obtained both from apertures and gradients outside this area and within the r_e/8_ region, with the present radial mapping, are completely new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497#2</TD>
            <TD>2011-09-14T20:01:35Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/433/497&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/433/497</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/433/497 [table1]</TD>
            <TD>Nearby early-type galaxies with ionized gas. I. (Rampazzo+, 2005)</TD>
            <TD>With the aim of building a data-set of spectral properties of well studied early-type galaxies showing emission lines, we present intermediate resolution spectra of 50 galaxies in the nearby Universe. The sample, which covers several of the E and S0 morphological sub-classes, is biased toward objects that might be expected to have ongoing and recent star formation, at least in small amounts, because of the presence of the emission lines. The emission is expected to come from the combination of active galactic nuclei and star formation regions within the galaxies. Sample galaxies are located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. Our long-slit spectra cover the 3700-7250{AA} wavelength range with a spectral resolution of approximately 7.6{AA} at 5550{AA}. The specific aim of this paper, and our first step in the investigation, is to map the underlying galaxy stellar population by measuring, along the slit positioned along the galaxy major axis, line-strength indices at several, homogeneous galacto-centric distances. For each object we extracted 7 luminosity-weighted apertures (with radii 1.5", 2.5", 10", r_e/10_, r_e/8_, r_e/4_ and r_e/2_) corrected for the galaxy ellipticity and 4 gradients (0&lt;r&lt;r_e/16_, r_e/16_&lt;r&lt;r_e/8_, r_e/8_&lt;r&lt;r_e/4_ and r_e/4_&lt;r&lt;r_e/2_). For each aperture and gradient we measured 25 line-strength indices: 21 of the set defined by the Lick-IDS ``standard'' system (Trager et al., 1998, Cat. J/ApJS/116/1) and 4 introduced by Worthey &amp; Ottaviani (1997, Cat. J/ApJS/111/377). Line-strength indices have been transformed to the Lick-IDS system. Indices derived then include H{beta}, Mg_1_, Mg_2_, Mgb, MgFe, Fe5270, Fe5335 commonly used in classic index-index diagrams. The paper introduces the sample, presents the observations, describes the data reduction procedures, the extraction of apertures and gradients, the determination and correction of the line-strength indices, the procedure adopted to transform them into the Lick-IDS System and the procedures adopted for the emission correction. We finally discuss the comparisons between our dataset and line-strength indices available in the literature. A significant fraction, about 60%, of galaxies in the present sample has one previous measurement in the Lick-IDS system but basically restricted within the r_e/8_ region. Line-strength measures obtained both from apertures and gradients outside this area and within the r_e/8_ region, with the present radial mapping, are completely new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497#table1</TD>
            <TD>2011-09-14T20:01:35Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/433/497&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/433/497</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/344/704 [1]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#1</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/344/704</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/344/704 [2]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#2</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/344/704&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/704 [table2]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#table2</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/704&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/704 [table1]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#table1</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/704&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/403/683 [1]</TD>
            <TD>GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)</TD>
            <TD>We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality HI-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^10^M_{sun}_ and redshifts 0.025&lt;z&lt;0.05, selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5-5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the HI gas fraction with galaxy structure and NUV-r colour.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683#1</TD>
            <TD>2011-09-14T21:25:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/403/683</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/683</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/403/683 [2]</TD>
            <TD>GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)</TD>
            <TD>We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality HI-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^10^M_{sun}_ and redshifts 0.025&lt;z&lt;0.05, selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5-5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the HI gas fraction with galaxy structure and NUV-r colour.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683#2</TD>
            <TD>2011-09-14T21:25:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/403/683&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/683</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/683 [table1]</TD>
            <TD>GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)</TD>
            <TD>We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality HI-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^10^M_{sun}_ and redshifts 0.025&lt;z&lt;0.05, selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5-5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the HI gas fraction with galaxy structure and NUV-r colour.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683#table1</TD>
            <TD>2011-09-14T21:25:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/683&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/683</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/433/497 [1]</TD>
            <TD>Nearby early-type galaxies with ionized gas. I. (Rampazzo+, 2005)</TD>
            <TD>With the aim of building a data-set of spectral properties of well studied early-type galaxies showing emission lines, we present intermediate resolution spectra of 50 galaxies in the nearby Universe. The sample, which covers several of the E and S0 morphological sub-classes, is biased toward objects that might be expected to have ongoing and recent star formation, at least in small amounts, because of the presence of the emission lines. The emission is expected to come from the combination of active galactic nuclei and star formation regions within the galaxies. Sample galaxies are located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. Our long-slit spectra cover the 3700-7250{AA} wavelength range with a spectral resolution of approximately 7.6{AA} at 5550{AA}. The specific aim of this paper, and our first step in the investigation, is to map the underlying galaxy stellar population by measuring, along the slit positioned along the galaxy major axis, line-strength indices at several, homogeneous galacto-centric distances. For each object we extracted 7 luminosity-weighted apertures (with radii 1.5", 2.5", 10", r_e/10_, r_e/8_, r_e/4_ and r_e/2_) corrected for the galaxy ellipticity and 4 gradients (0&lt;r&lt;r_e/16_, r_e/16_&lt;r&lt;r_e/8_, r_e/8_&lt;r&lt;r_e/4_ and r_e/4_&lt;r&lt;r_e/2_). For each aperture and gradient we measured 25 line-strength indices: 21 of the set defined by the Lick-IDS ``standard'' system (Trager et al., 1998, Cat. J/ApJS/116/1) and 4 introduced by Worthey &amp; Ottaviani (1997, Cat. J/ApJS/111/377). Line-strength indices have been transformed to the Lick-IDS system. Indices derived then include H{beta}, Mg_1_, Mg_2_, Mgb, MgFe, Fe5270, Fe5335 commonly used in classic index-index diagrams. The paper introduces the sample, presents the observations, describes the data reduction procedures, the extraction of apertures and gradients, the determination and correction of the line-strength indices, the procedure adopted to transform them into the Lick-IDS System and the procedures adopted for the emission correction. We finally discuss the comparisons between our dataset and line-strength indices available in the literature. A significant fraction, about 60%, of galaxies in the present sample has one previous measurement in the Lick-IDS system but basically restricted within the r_e/8_ region. Line-strength measures obtained both from apertures and gradients outside this area and within the r_e/8_ region, with the present radial mapping, are completely new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497#1</TD>
            <TD>2011-09-14T20:01:35Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/433/497</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/433/497</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/433/497 [2]</TD>
            <TD>Nearby early-type galaxies with ionized gas. I. (Rampazzo+, 2005)</TD>
            <TD>With the aim of building a data-set of spectral properties of well studied early-type galaxies showing emission lines, we present intermediate resolution spectra of 50 galaxies in the nearby Universe. The sample, which covers several of the E and S0 morphological sub-classes, is biased toward objects that might be expected to have ongoing and recent star formation, at least in small amounts, because of the presence of the emission lines. The emission is expected to come from the combination of active galactic nuclei and star formation regions within the galaxies. Sample galaxies are located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. Our long-slit spectra cover the 3700-7250{AA} wavelength range with a spectral resolution of approximately 7.6{AA} at 5550{AA}. The specific aim of this paper, and our first step in the investigation, is to map the underlying galaxy stellar population by measuring, along the slit positioned along the galaxy major axis, line-strength indices at several, homogeneous galacto-centric distances. For each object we extracted 7 luminosity-weighted apertures (with radii 1.5", 2.5", 10", r_e/10_, r_e/8_, r_e/4_ and r_e/2_) corrected for the galaxy ellipticity and 4 gradients (0&lt;r&lt;r_e/16_, r_e/16_&lt;r&lt;r_e/8_, r_e/8_&lt;r&lt;r_e/4_ and r_e/4_&lt;r&lt;r_e/2_). For each aperture and gradient we measured 25 line-strength indices: 21 of the set defined by the Lick-IDS ``standard'' system (Trager et al., 1998, Cat. J/ApJS/116/1) and 4 introduced by Worthey &amp; Ottaviani (1997, Cat. J/ApJS/111/377). Line-strength indices have been transformed to the Lick-IDS system. Indices derived then include H{beta}, Mg_1_, Mg_2_, Mgb, MgFe, Fe5270, Fe5335 commonly used in classic index-index diagrams. The paper introduces the sample, presents the observations, describes the data reduction procedures, the extraction of apertures and gradients, the determination and correction of the line-strength indices, the procedure adopted to transform them into the Lick-IDS System and the procedures adopted for the emission correction. We finally discuss the comparisons between our dataset and line-strength indices available in the literature. A significant fraction, about 60%, of galaxies in the present sample has one previous measurement in the Lick-IDS system but basically restricted within the r_e/8_ region. Line-strength measures obtained both from apertures and gradients outside this area and within the r_e/8_ region, with the present radial mapping, are completely new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497#2</TD>
            <TD>2011-09-14T20:01:35Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/433/497&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/433/497</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/433/497 [table1]</TD>
            <TD>Nearby early-type galaxies with ionized gas. I. (Rampazzo+, 2005)</TD>
            <TD>With the aim of building a data-set of spectral properties of well studied early-type galaxies showing emission lines, we present intermediate resolution spectra of 50 galaxies in the nearby Universe. The sample, which covers several of the E and S0 morphological sub-classes, is biased toward objects that might be expected to have ongoing and recent star formation, at least in small amounts, because of the presence of the emission lines. The emission is expected to come from the combination of active galactic nuclei and star formation regions within the galaxies. Sample galaxies are located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. Our long-slit spectra cover the 3700-7250{AA} wavelength range with a spectral resolution of approximately 7.6{AA} at 5550{AA}. The specific aim of this paper, and our first step in the investigation, is to map the underlying galaxy stellar population by measuring, along the slit positioned along the galaxy major axis, line-strength indices at several, homogeneous galacto-centric distances. For each object we extracted 7 luminosity-weighted apertures (with radii 1.5", 2.5", 10", r_e/10_, r_e/8_, r_e/4_ and r_e/2_) corrected for the galaxy ellipticity and 4 gradients (0&lt;r&lt;r_e/16_, r_e/16_&lt;r&lt;r_e/8_, r_e/8_&lt;r&lt;r_e/4_ and r_e/4_&lt;r&lt;r_e/2_). For each aperture and gradient we measured 25 line-strength indices: 21 of the set defined by the Lick-IDS ``standard'' system (Trager et al., 1998, Cat. J/ApJS/116/1) and 4 introduced by Worthey &amp; Ottaviani (1997, Cat. J/ApJS/111/377). Line-strength indices have been transformed to the Lick-IDS system. Indices derived then include H{beta}, Mg_1_, Mg_2_, Mgb, MgFe, Fe5270, Fe5335 commonly used in classic index-index diagrams. The paper introduces the sample, presents the observations, describes the data reduction procedures, the extraction of apertures and gradients, the determination and correction of the line-strength indices, the procedure adopted to transform them into the Lick-IDS System and the procedures adopted for the emission correction. We finally discuss the comparisons between our dataset and line-strength indices available in the literature. A significant fraction, about 60%, of galaxies in the present sample has one previous measurement in the Lick-IDS system but basically restricted within the r_e/8_ region. Line-strength measures obtained both from apertures and gradients outside this area and within the r_e/8_ region, with the present radial mapping, are completely new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497#table1</TD>
            <TD>2011-09-14T20:01:35Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/433/497</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/433/497&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/433/497</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/403/683 [1]</TD>
            <TD>GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)</TD>
            <TD>We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality HI-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^10^M_{sun}_ and redshifts 0.025&lt;z&lt;0.05, selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5-5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the HI gas fraction with galaxy structure and NUV-r colour.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683#1</TD>
            <TD>2011-09-14T21:25:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/403/683</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/683</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/403/683 [2]</TD>
            <TD>GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)</TD>
            <TD>We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality HI-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^10^M_{sun}_ and redshifts 0.025&lt;z&lt;0.05, selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5-5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the HI gas fraction with galaxy structure and NUV-r colour.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683#2</TD>
            <TD>2011-09-14T21:25:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/403/683&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/683</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/403/683 [table1]</TD>
            <TD>GALEX Arecibo SDSS survey (GASS) (Catinella+, 2010)</TD>
            <TD>We introduce the GALEX Arecibo SDSS Survey (GASS), an on-going large programme that is gathering high quality HI-line spectra using the Arecibo radio telescope for an unbiased sample of ~1000 galaxies with stellar masses greater than 10^10^M_{sun}_ and redshifts 0.025&lt;z&lt;0.05, selected from the Sloan Digital Sky Survey (SDSS) spectroscopic and Galaxy Evolution Explorer (GALEX) imaging surveys. The galaxies are observed until detected or until a low gas mass fraction limit (1.5-5 per cent) is reached. This paper presents the first Data Release, consisting of ~20 per cent of the final GASS sample. We use this data set to explore the main scaling relations of the HI gas fraction with galaxy structure and NUV-r colour.</TD>
            <TD>CDS</TD>
            <TD>#UV#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683#table1</TD>
            <TD>2011-09-14T21:25:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/403/683</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/403/683&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/403/683</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/344/704 [1]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#1</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/344/704</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/344/704 [2]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#2</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/344/704&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/704 [table2]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#table2</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/704&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/704 [table1]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#table1</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/704&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/3213 [1]</TD>
            <TD>BVR imaging survey of nine early-type galaxies (Marcum+, 2004)</TD>
            <TD>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213#1</TD>
            <TD>2011-09-14T20:01:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/3213</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3213</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/3213 [2]</TD>
            <TD>BVR imaging survey of nine early-type galaxies (Marcum+, 2004)</TD>
            <TD>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213#2</TD>
            <TD>2011-09-14T20:01:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/3213&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3213</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/3213 [galaxies]</TD>
            <TD>BVR imaging survey of nine early-type galaxies (Marcum+, 2004)</TD>
            <TD>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213#galaxies</TD>
            <TD>2011-09-14T20:01:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/3213&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3213</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/405/2302 [1]</TD>
            <TD>Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</TD>
            <TD>A systematic investigation of the relationship between different redshift estimation schemes for more than 91000 quasars in the Sloan Digital Sky Survey (SDSS) Data Release 6 is presented. The publicly available SDSS quasar redshifts are shown to possess systematic biases of {Delta}z/(1+z)&gt;=0.002 (600km/s) over both small ({delta}z~=0.1) and large ({delta}z~=1) redshift intervals. Empirical relationships between redshifts based on (i) CaII H&amp;K host galaxy absorption, (ii) quasar [OII] {lambda}{lambda}3728, (iii) [OIII] {lambda}{lambda} 4960, 5008 emission and (iv) cross-correlation (with a master-quasar template) that includes, at increasing quasar redshift, the prominent MgII {lambda}{lambda} 2799, CIII] {lambda}{lambda} 1908 and CIV {lambda}{lambda} 1549 emission lines are established as a function of quasar redshift and luminosity. New redshifts in the resulting catalogue possess systematic biases, a factor of ~=20 lower compared to the SDSS redshift values; systematic effects are reduced to the level of {Delta}z/(1+z) (30km/s) per unit redshift or &lt;=2.5x10^-5^ per unit absolute magnitude. Redshift errors, including components due both to internal reproducibility and to the intrinsic quasar-to-quasar variation among the population, are available for all quasars in the catalogue. The improved redshifts and their associated errors have wide applicability in areas such as quasar absorption outflows, quasar clustering, quasar-galaxy clustering and proximity-effect determinations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302#1</TD>
            <TD>2011-09-14T21:26:28Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/405/2302</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/2302</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/405/2302 [2]</TD>
            <TD>Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</TD>
            <TD>A systematic investigation of the relationship between different redshift estimation schemes for more than 91000 quasars in the Sloan Digital Sky Survey (SDSS) Data Release 6 is presented. The publicly available SDSS quasar redshifts are shown to possess systematic biases of {Delta}z/(1+z)&gt;=0.002 (600km/s) over both small ({delta}z~=0.1) and large ({delta}z~=1) redshift intervals. Empirical relationships between redshifts based on (i) CaII H&amp;K host galaxy absorption, (ii) quasar [OII] {lambda}{lambda}3728, (iii) [OIII] {lambda}{lambda} 4960, 5008 emission and (iv) cross-correlation (with a master-quasar template) that includes, at increasing quasar redshift, the prominent MgII {lambda}{lambda} 2799, CIII] {lambda}{lambda} 1908 and CIV {lambda}{lambda} 1549 emission lines are established as a function of quasar redshift and luminosity. New redshifts in the resulting catalogue possess systematic biases, a factor of ~=20 lower compared to the SDSS redshift values; systematic effects are reduced to the level of {Delta}z/(1+z) (30km/s) per unit redshift or &lt;=2.5x10^-5^ per unit absolute magnitude. Redshift errors, including components due both to internal reproducibility and to the intrinsic quasar-to-quasar variation among the population, are available for all quasars in the catalogue. The improved redshifts and their associated errors have wide applicability in areas such as quasar absorption outflows, quasar clustering, quasar-galaxy clustering and proximity-effect determinations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302#2</TD>
            <TD>2011-09-14T21:26:28Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/405/2302&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/2302</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/405/2302 [table4]</TD>
            <TD>Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</TD>
            <TD>A systematic investigation of the relationship between different redshift estimation schemes for more than 91000 quasars in the Sloan Digital Sky Survey (SDSS) Data Release 6 is presented. The publicly available SDSS quasar redshifts are shown to possess systematic biases of {Delta}z/(1+z)&gt;=0.002 (600km/s) over both small ({delta}z~=0.1) and large ({delta}z~=1) redshift intervals. Empirical relationships between redshifts based on (i) CaII H&amp;K host galaxy absorption, (ii) quasar [OII] {lambda}{lambda}3728, (iii) [OIII] {lambda}{lambda} 4960, 5008 emission and (iv) cross-correlation (with a master-quasar template) that includes, at increasing quasar redshift, the prominent MgII {lambda}{lambda} 2799, CIII] {lambda}{lambda} 1908 and CIV {lambda}{lambda} 1549 emission lines are established as a function of quasar redshift and luminosity. New redshifts in the resulting catalogue possess systematic biases, a factor of ~=20 lower compared to the SDSS redshift values; systematic effects are reduced to the level of {Delta}z/(1+z) (30km/s) per unit redshift or &lt;=2.5x10^-5^ per unit absolute magnitude. Redshift errors, including components due both to internal reproducibility and to the intrinsic quasar-to-quasar variation among the population, are available for all quasars in the catalogue. The improved redshifts and their associated errors have wide applicability in areas such as quasar absorption outflows, quasar clustering, quasar-galaxy clustering and proximity-effect determinations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302#table4</TD>
            <TD>2011-09-14T21:26:28Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/405/2302&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/2302</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/344/704 [1]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#1</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/344/704</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/344/704 [2]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#2</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/344/704&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/704 [table2]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#table2</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/704&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/344/704 [table1]</TD>
            <TD>Planetary nebulae as standard candles. III. (Jacoby+, 1989)</TD>
            <TD>We present the results of a survey for planetary nebulae in the nearby Sb galaxy M81 (NGC 3031). Using the Kitt Peak 4m telescope and a TI CCD, we identify 185 planetary nebula candidates. Photometry of the nebulae extends nearly 2.5mag below the brightest candidate, although the sample is statistically homogeneous and complete for only 88 nebulae representing the top 1.2mag of the luminosity function.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704#table1</TD>
            <TD>2012-09-24T08:14:08Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/344/704</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/344/704&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/344/704</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/3213 [1]</TD>
            <TD>BVR imaging survey of nine early-type galaxies (Marcum+, 2004)</TD>
            <TD>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213#1</TD>
            <TD>2011-09-14T20:01:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/3213</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3213</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/3213 [2]</TD>
            <TD>BVR imaging survey of nine early-type galaxies (Marcum+, 2004)</TD>
            <TD>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213#2</TD>
            <TD>2011-09-14T20:01:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/3213&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3213</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/3213 [galaxies]</TD>
            <TD>BVR imaging survey of nine early-type galaxies (Marcum+, 2004)</TD>
            <TD>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213#galaxies</TD>
            <TD>2011-09-14T20:01:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/3213&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3213</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/405/2302 [1]</TD>
            <TD>Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</TD>
            <TD>A systematic investigation of the relationship between different redshift estimation schemes for more than 91000 quasars in the Sloan Digital Sky Survey (SDSS) Data Release 6 is presented. The publicly available SDSS quasar redshifts are shown to possess systematic biases of {Delta}z/(1+z)&gt;=0.002 (600km/s) over both small ({delta}z~=0.1) and large ({delta}z~=1) redshift intervals. Empirical relationships between redshifts based on (i) CaII H&amp;K host galaxy absorption, (ii) quasar [OII] {lambda}{lambda}3728, (iii) [OIII] {lambda}{lambda} 4960, 5008 emission and (iv) cross-correlation (with a master-quasar template) that includes, at increasing quasar redshift, the prominent MgII {lambda}{lambda} 2799, CIII] {lambda}{lambda} 1908 and CIV {lambda}{lambda} 1549 emission lines are established as a function of quasar redshift and luminosity. New redshifts in the resulting catalogue possess systematic biases, a factor of ~=20 lower compared to the SDSS redshift values; systematic effects are reduced to the level of {Delta}z/(1+z) (30km/s) per unit redshift or &lt;=2.5x10^-5^ per unit absolute magnitude. Redshift errors, including components due both to internal reproducibility and to the intrinsic quasar-to-quasar variation among the population, are available for all quasars in the catalogue. The improved redshifts and their associated errors have wide applicability in areas such as quasar absorption outflows, quasar clustering, quasar-galaxy clustering and proximity-effect determinations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302#1</TD>
            <TD>2011-09-14T21:26:28Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/405/2302</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/2302</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/405/2302 [2]</TD>
            <TD>Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</TD>
            <TD>A systematic investigation of the relationship between different redshift estimation schemes for more than 91000 quasars in the Sloan Digital Sky Survey (SDSS) Data Release 6 is presented. The publicly available SDSS quasar redshifts are shown to possess systematic biases of {Delta}z/(1+z)&gt;=0.002 (600km/s) over both small ({delta}z~=0.1) and large ({delta}z~=1) redshift intervals. Empirical relationships between redshifts based on (i) CaII H&amp;K host galaxy absorption, (ii) quasar [OII] {lambda}{lambda}3728, (iii) [OIII] {lambda}{lambda} 4960, 5008 emission and (iv) cross-correlation (with a master-quasar template) that includes, at increasing quasar redshift, the prominent MgII {lambda}{lambda} 2799, CIII] {lambda}{lambda} 1908 and CIV {lambda}{lambda} 1549 emission lines are established as a function of quasar redshift and luminosity. New redshifts in the resulting catalogue possess systematic biases, a factor of ~=20 lower compared to the SDSS redshift values; systematic effects are reduced to the level of {Delta}z/(1+z) (30km/s) per unit redshift or &lt;=2.5x10^-5^ per unit absolute magnitude. Redshift errors, including components due both to internal reproducibility and to the intrinsic quasar-to-quasar variation among the population, are available for all quasars in the catalogue. The improved redshifts and their associated errors have wide applicability in areas such as quasar absorption outflows, quasar clustering, quasar-galaxy clustering and proximity-effect determinations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302#2</TD>
            <TD>2011-09-14T21:26:28Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/405/2302&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/2302</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/405/2302 [table4]</TD>
            <TD>Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</TD>
            <TD>A systematic investigation of the relationship between different redshift estimation schemes for more than 91000 quasars in the Sloan Digital Sky Survey (SDSS) Data Release 6 is presented. The publicly available SDSS quasar redshifts are shown to possess systematic biases of {Delta}z/(1+z)&gt;=0.002 (600km/s) over both small ({delta}z~=0.1) and large ({delta}z~=1) redshift intervals. Empirical relationships between redshifts based on (i) CaII H&amp;K host galaxy absorption, (ii) quasar [OII] {lambda}{lambda}3728, (iii) [OIII] {lambda}{lambda} 4960, 5008 emission and (iv) cross-correlation (with a master-quasar template) that includes, at increasing quasar redshift, the prominent MgII {lambda}{lambda} 2799, CIII] {lambda}{lambda} 1908 and CIV {lambda}{lambda} 1549 emission lines are established as a function of quasar redshift and luminosity. New redshifts in the resulting catalogue possess systematic biases, a factor of ~=20 lower compared to the SDSS redshift values; systematic effects are reduced to the level of {Delta}z/(1+z) (30km/s) per unit redshift or &lt;=2.5x10^-5^ per unit absolute magnitude. Redshift errors, including components due both to internal reproducibility and to the intrinsic quasar-to-quasar variation among the population, are available for all quasars in the catalogue. The improved redshifts and their associated errors have wide applicability in areas such as quasar absorption outflows, quasar clustering, quasar-galaxy clustering and proximity-effect determinations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302#table4</TD>
            <TD>2011-09-14T21:26:28Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/405/2302&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/2302</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/118/1131 [1]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#1</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/118/1131</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/118/1131 [2]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#2</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/118/1131&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/118/1131 [table6]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#table6</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/118/1131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/118/1131 [table4]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#table4</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/118/1131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/405/2302 [1]</TD>
            <TD>Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</TD>
            <TD>A systematic investigation of the relationship between different redshift estimation schemes for more than 91000 quasars in the Sloan Digital Sky Survey (SDSS) Data Release 6 is presented. The publicly available SDSS quasar redshifts are shown to possess systematic biases of {Delta}z/(1+z)&gt;=0.002 (600km/s) over both small ({delta}z~=0.1) and large ({delta}z~=1) redshift intervals. Empirical relationships between redshifts based on (i) CaII H&amp;K host galaxy absorption, (ii) quasar [OII] {lambda}{lambda}3728, (iii) [OIII] {lambda}{lambda} 4960, 5008 emission and (iv) cross-correlation (with a master-quasar template) that includes, at increasing quasar redshift, the prominent MgII {lambda}{lambda} 2799, CIII] {lambda}{lambda} 1908 and CIV {lambda}{lambda} 1549 emission lines are established as a function of quasar redshift and luminosity. New redshifts in the resulting catalogue possess systematic biases, a factor of ~=20 lower compared to the SDSS redshift values; systematic effects are reduced to the level of {Delta}z/(1+z) (30km/s) per unit redshift or &lt;=2.5x10^-5^ per unit absolute magnitude. Redshift errors, including components due both to internal reproducibility and to the intrinsic quasar-to-quasar variation among the population, are available for all quasars in the catalogue. The improved redshifts and their associated errors have wide applicability in areas such as quasar absorption outflows, quasar clustering, quasar-galaxy clustering and proximity-effect determinations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302#1</TD>
            <TD>2011-09-14T21:26:28Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/405/2302</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/2302</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/405/2302 [2]</TD>
            <TD>Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</TD>
            <TD>A systematic investigation of the relationship between different redshift estimation schemes for more than 91000 quasars in the Sloan Digital Sky Survey (SDSS) Data Release 6 is presented. The publicly available SDSS quasar redshifts are shown to possess systematic biases of {Delta}z/(1+z)&gt;=0.002 (600km/s) over both small ({delta}z~=0.1) and large ({delta}z~=1) redshift intervals. Empirical relationships between redshifts based on (i) CaII H&amp;K host galaxy absorption, (ii) quasar [OII] {lambda}{lambda}3728, (iii) [OIII] {lambda}{lambda} 4960, 5008 emission and (iv) cross-correlation (with a master-quasar template) that includes, at increasing quasar redshift, the prominent MgII {lambda}{lambda} 2799, CIII] {lambda}{lambda} 1908 and CIV {lambda}{lambda} 1549 emission lines are established as a function of quasar redshift and luminosity. New redshifts in the resulting catalogue possess systematic biases, a factor of ~=20 lower compared to the SDSS redshift values; systematic effects are reduced to the level of {Delta}z/(1+z) (30km/s) per unit redshift or &lt;=2.5x10^-5^ per unit absolute magnitude. Redshift errors, including components due both to internal reproducibility and to the intrinsic quasar-to-quasar variation among the population, are available for all quasars in the catalogue. The improved redshifts and their associated errors have wide applicability in areas such as quasar absorption outflows, quasar clustering, quasar-galaxy clustering and proximity-effect determinations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302#2</TD>
            <TD>2011-09-14T21:26:28Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/405/2302&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/2302</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/405/2302 [table4]</TD>
            <TD>Improved redshifts for SDSS quasar spectra (Hewett+, 2010)</TD>
            <TD>A systematic investigation of the relationship between different redshift estimation schemes for more than 91000 quasars in the Sloan Digital Sky Survey (SDSS) Data Release 6 is presented. The publicly available SDSS quasar redshifts are shown to possess systematic biases of {Delta}z/(1+z)&gt;=0.002 (600km/s) over both small ({delta}z~=0.1) and large ({delta}z~=1) redshift intervals. Empirical relationships between redshifts based on (i) CaII H&amp;K host galaxy absorption, (ii) quasar [OII] {lambda}{lambda}3728, (iii) [OIII] {lambda}{lambda} 4960, 5008 emission and (iv) cross-correlation (with a master-quasar template) that includes, at increasing quasar redshift, the prominent MgII {lambda}{lambda} 2799, CIII] {lambda}{lambda} 1908 and CIV {lambda}{lambda} 1549 emission lines are established as a function of quasar redshift and luminosity. New redshifts in the resulting catalogue possess systematic biases, a factor of ~=20 lower compared to the SDSS redshift values; systematic effects are reduced to the level of {Delta}z/(1+z) (30km/s) per unit redshift or &lt;=2.5x10^-5^ per unit absolute magnitude. Redshift errors, including components due both to internal reproducibility and to the intrinsic quasar-to-quasar variation among the population, are available for all quasars in the catalogue. The improved redshifts and their associated errors have wide applicability in areas such as quasar absorption outflows, quasar clustering, quasar-galaxy clustering and proximity-effect determinations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302#table4</TD>
            <TD>2011-09-14T21:26:28Z</TD>
            <TD>#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/405/2302</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/405/2302&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/405/2302</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/3213 [1]</TD>
            <TD>BVR imaging survey of nine early-type galaxies (Marcum+, 2004)</TD>
            <TD>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213#1</TD>
            <TD>2011-09-14T20:01:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/3213</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3213</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/3213 [2]</TD>
            <TD>BVR imaging survey of nine early-type galaxies (Marcum+, 2004)</TD>
            <TD>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213#2</TD>
            <TD>2011-09-14T20:01:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/3213&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3213</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/3213 [galaxies]</TD>
            <TD>BVR imaging survey of nine early-type galaxies (Marcum+, 2004)</TD>
            <TD>We have conducted a BVR imaging survey of nine early-type galaxies previously verified to exist in extremely isolated environments. Our goals are to establish a baseline of morphological and photometric properties for spheroidal systems evolving in extremely low-density environments and to compare these properties with signatures predicted for merged galaxy groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213#galaxies</TD>
            <TD>2011-09-14T20:01:39Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3213</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/3213&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3213</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/118/1131 [1]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#1</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/118/1131</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/118/1131 [2]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#2</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/118/1131&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/118/1131 [table6]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#table6</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/118/1131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/118/1131 [table4]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#table4</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/118/1131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/2295 [1]</TD>
            <TD>Ultra-compact dwarf candidates in Abell S0740 (Blakeslee+, 2008)</TD>
            <TD>ESO 325-G004 was imaged with the ACS/WFC in the F475W, F625W, and F814W filters. Throughout this paper, we refer to magnitudes in these filters as g475, r625, and I814, respectively. The galaxy was initially observed in F814W and F475W as part of the HST GO Program 10429 during 2005 January. There were 22 F814W exposures of varying times totaling 18882s, and three exposures in F475W of 367s each. In 2006 February, further imaging of the ESO 325-G004 field was carried out by the HST DD Program 10710 for a Hubble Heritage public release image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295#1</TD>
            <TD>2011-09-14T21:29:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/2295</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2295</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/2295 [2]</TD>
            <TD>Ultra-compact dwarf candidates in Abell S0740 (Blakeslee+, 2008)</TD>
            <TD>ESO 325-G004 was imaged with the ACS/WFC in the F475W, F625W, and F814W filters. Throughout this paper, we refer to magnitudes in these filters as g475, r625, and I814, respectively. The galaxy was initially observed in F814W and F475W as part of the HST GO Program 10429 during 2005 January. There were 22 F814W exposures of varying times totaling 18882s, and three exposures in F475W of 367s each. In 2006 February, further imaging of the ESO 325-G004 field was carried out by the HST DD Program 10710 for a Hubble Heritage public release image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295#2</TD>
            <TD>2011-09-14T21:29:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/2295&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2295</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/2295 [table1]</TD>
            <TD>Ultra-compact dwarf candidates in Abell S0740 (Blakeslee+, 2008)</TD>
            <TD>ESO 325-G004 was imaged with the ACS/WFC in the F475W, F625W, and F814W filters. Throughout this paper, we refer to magnitudes in these filters as g475, r625, and I814, respectively. The galaxy was initially observed in F814W and F475W as part of the HST GO Program 10429 during 2005 January. There were 22 F814W exposures of varying times totaling 18882s, and three exposures in F475W of 367s each. In 2006 February, further imaging of the ESO 325-G004 field was carried out by the HST DD Program 10710 for a Hubble Heritage public release image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295#table1</TD>
            <TD>2011-09-14T21:29:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/2295&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2295</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/431/143 [1]</TD>
            <TD>Field horizontal-branch stars in the Galaxy (Christlieb+, 2005)</TD>
            <TD>Table A.1 contains photometry (UBV, c_1_), and Balmer line equivalent width sums, as derived directly from HES spectra, as well as coordinates of the 8321 candidate field horizontal-branch stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143#1</TD>
            <TD>2011-09-14T20:12:12Z</TD>
            <TD>#Positional_Data#Photometry#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/431/143</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/431/143</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/431/143 [2]</TD>
            <TD>Field horizontal-branch stars in the Galaxy (Christlieb+, 2005)</TD>
            <TD>Table A.1 contains photometry (UBV, c_1_), and Balmer line equivalent width sums, as derived directly from HES spectra, as well as coordinates of the 8321 candidate field horizontal-branch stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143#2</TD>
            <TD>2011-09-14T20:12:12Z</TD>
            <TD>#Positional_Data#Photometry#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/431/143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/431/143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/431/143 [tabla1]</TD>
            <TD>Field horizontal-branch stars in the Galaxy (Christlieb+, 2005)</TD>
            <TD>Table A.1 contains photometry (UBV, c_1_), and Balmer line equivalent width sums, as derived directly from HES spectra, as well as coordinates of the 8321 candidate field horizontal-branch stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143#tabla1</TD>
            <TD>2011-09-14T20:12:12Z</TD>
            <TD>#Positional_Data#Photometry#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/431/143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/431/143</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/2295 [1]</TD>
            <TD>Ultra-compact dwarf candidates in Abell S0740 (Blakeslee+, 2008)</TD>
            <TD>ESO 325-G004 was imaged with the ACS/WFC in the F475W, F625W, and F814W filters. Throughout this paper, we refer to magnitudes in these filters as g475, r625, and I814, respectively. The galaxy was initially observed in F814W and F475W as part of the HST GO Program 10429 during 2005 January. There were 22 F814W exposures of varying times totaling 18882s, and three exposures in F475W of 367s each. In 2006 February, further imaging of the ESO 325-G004 field was carried out by the HST DD Program 10710 for a Hubble Heritage public release image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295#1</TD>
            <TD>2011-09-14T21:29:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/2295</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2295</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/2295 [2]</TD>
            <TD>Ultra-compact dwarf candidates in Abell S0740 (Blakeslee+, 2008)</TD>
            <TD>ESO 325-G004 was imaged with the ACS/WFC in the F475W, F625W, and F814W filters. Throughout this paper, we refer to magnitudes in these filters as g475, r625, and I814, respectively. The galaxy was initially observed in F814W and F475W as part of the HST GO Program 10429 during 2005 January. There were 22 F814W exposures of varying times totaling 18882s, and three exposures in F475W of 367s each. In 2006 February, further imaging of the ESO 325-G004 field was carried out by the HST DD Program 10710 for a Hubble Heritage public release image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295#2</TD>
            <TD>2011-09-14T21:29:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/2295&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2295</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/2295 [table1]</TD>
            <TD>Ultra-compact dwarf candidates in Abell S0740 (Blakeslee+, 2008)</TD>
            <TD>ESO 325-G004 was imaged with the ACS/WFC in the F475W, F625W, and F814W filters. Throughout this paper, we refer to magnitudes in these filters as g475, r625, and I814, respectively. The galaxy was initially observed in F814W and F475W as part of the HST GO Program 10429 during 2005 January. There were 22 F814W exposures of varying times totaling 18882s, and three exposures in F475W of 367s each. In 2006 February, further imaging of the ESO 325-G004 field was carried out by the HST DD Program 10710 for a Hubble Heritage public release image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295#table1</TD>
            <TD>2011-09-14T21:29:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/2295&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2295</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/118/1131 [1]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#1</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/118/1131</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/118/1131 [2]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#2</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/118/1131&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/118/1131 [table6]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#table6</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/118/1131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/118/1131 [table4]</TD>
            <TD>Radial velocities in A3565 and A3560 (Willmer+, 1999)</TD>
            <TD>We report 102 new redshifts and magnitudes for a sample of galaxies to R_F_~15.5mag in a 2.17{deg}x2.17{deg} region centered on the galaxy IC 4296, the most luminous member of the A3565 Cluster. The sample of galaxies was defined from scans of an on-film copy of the ESO/Uppsala survey field 383 in the R band (IIIa-F emulsion plus GG 630 filter; hereafter ESO-LV) using the Observatsrio Nacional PDS 1010A microdensitometer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131#table4</TD>
            <TD>2012-09-24T08:53:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1131</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/118/1131&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1131</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/136/2295 [1]</TD>
            <TD>Ultra-compact dwarf candidates in Abell S0740 (Blakeslee+, 2008)</TD>
            <TD>ESO 325-G004 was imaged with the ACS/WFC in the F475W, F625W, and F814W filters. Throughout this paper, we refer to magnitudes in these filters as g475, r625, and I814, respectively. The galaxy was initially observed in F814W and F475W as part of the HST GO Program 10429 during 2005 January. There were 22 F814W exposures of varying times totaling 18882s, and three exposures in F475W of 367s each. In 2006 February, further imaging of the ESO 325-G004 field was carried out by the HST DD Program 10710 for a Hubble Heritage public release image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295#1</TD>
            <TD>2011-09-14T21:29:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/136/2295</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2295</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/136/2295 [2]</TD>
            <TD>Ultra-compact dwarf candidates in Abell S0740 (Blakeslee+, 2008)</TD>
            <TD>ESO 325-G004 was imaged with the ACS/WFC in the F475W, F625W, and F814W filters. Throughout this paper, we refer to magnitudes in these filters as g475, r625, and I814, respectively. The galaxy was initially observed in F814W and F475W as part of the HST GO Program 10429 during 2005 January. There were 22 F814W exposures of varying times totaling 18882s, and three exposures in F475W of 367s each. In 2006 February, further imaging of the ESO 325-G004 field was carried out by the HST DD Program 10710 for a Hubble Heritage public release image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295#2</TD>
            <TD>2011-09-14T21:29:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/136/2295&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2295</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/136/2295 [table1]</TD>
            <TD>Ultra-compact dwarf candidates in Abell S0740 (Blakeslee+, 2008)</TD>
            <TD>ESO 325-G004 was imaged with the ACS/WFC in the F475W, F625W, and F814W filters. Throughout this paper, we refer to magnitudes in these filters as g475, r625, and I814, respectively. The galaxy was initially observed in F814W and F475W as part of the HST GO Program 10429 during 2005 January. There were 22 F814W exposures of varying times totaling 18882s, and three exposures in F475W of 367s each. In 2006 February, further imaging of the ESO 325-G004 field was carried out by the HST DD Program 10710 for a Hubble Heritage public release image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295#table1</TD>
            <TD>2011-09-14T21:29:54Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/136/2295</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/136/2295&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/136/2295</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/431/143 [1]</TD>
            <TD>Field horizontal-branch stars in the Galaxy (Christlieb+, 2005)</TD>
            <TD>Table A.1 contains photometry (UBV, c_1_), and Balmer line equivalent width sums, as derived directly from HES spectra, as well as coordinates of the 8321 candidate field horizontal-branch stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143#1</TD>
            <TD>2011-09-14T20:12:12Z</TD>
            <TD>#Positional_Data#Photometry#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/431/143</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/431/143</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/431/143 [2]</TD>
            <TD>Field horizontal-branch stars in the Galaxy (Christlieb+, 2005)</TD>
            <TD>Table A.1 contains photometry (UBV, c_1_), and Balmer line equivalent width sums, as derived directly from HES spectra, as well as coordinates of the 8321 candidate field horizontal-branch stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143#2</TD>
            <TD>2011-09-14T20:12:12Z</TD>
            <TD>#Positional_Data#Photometry#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/431/143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/431/143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/431/143 [tabla1]</TD>
            <TD>Field horizontal-branch stars in the Galaxy (Christlieb+, 2005)</TD>
            <TD>Table A.1 contains photometry (UBV, c_1_), and Balmer line equivalent width sums, as derived directly from HES spectra, as well as coordinates of the 8321 candidate field horizontal-branch stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143#tabla1</TD>
            <TD>2011-09-14T20:12:12Z</TD>
            <TD>#Positional_Data#Photometry#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/431/143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/431/143</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/171/261 [1]</TD>
            <TD>Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)</TD>
            <TD>We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109{alpha} and H110{alpha}) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261#1</TD>
            <TD>2012-09-24T08:56:36Z</TD>
            <TD>#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/171/261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/171/261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/171/261 [2]</TD>
            <TD>Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)</TD>
            <TD>We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109{alpha} and H110{alpha}) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261#2</TD>
            <TD>2012-09-24T08:56:36Z</TD>
            <TD>#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/171/261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/171/261</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/171/261 [table1]</TD>
            <TD>Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)</TD>
            <TD>We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109{alpha} and H110{alpha}) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261#table1</TD>
            <TD>2012-09-24T08:56:36Z</TD>
            <TD>#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/171/261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/171/261</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/4377 [1]</TD>
            <TD>List of SEGUE plate pairs (Yanny+, 2009)</TD>
            <TD>The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ~240000 moderate-resolution (R~1800) spectra from 3900{AA} to 9000{AA} of fainter Milky Way stars (14.0&lt;g&lt;20.3) of a wide variety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and populations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the sky. Radial velocity accuracies for stars are {sigma}(RV)~4km/s at g&lt;18, degrading to {sigma}(RV)~15km/s at g~20. For stars with signal-to-noise ratio &gt;10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500deg^2^ of additional ugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry ({sigma}(g,r,i) ~2%), ({sigma}(u,z)~3%) and astrometry (~0.1") for spectroscopic target selection. The stellar spectra, imaging data, and derived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7. Individual images of spectra in this data set may be examined by fetching from the DAS, with a link like wget http://das.sdss.org/spectro/1d_26/1880/gif/spPlot-53262-1880-014.gif A FITS data file of the calibrated 1D spectrum is available from wget http://das.sdss.org/spectro/1d_26/1880/1d/spSpec-53262-1880-014.fit</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377#1</TD>
            <TD>2011-09-14T21:30:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/4377</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4377</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/4377 [2]</TD>
            <TD>List of SEGUE plate pairs (Yanny+, 2009)</TD>
            <TD>The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ~240000 moderate-resolution (R~1800) spectra from 3900{AA} to 9000{AA} of fainter Milky Way stars (14.0&lt;g&lt;20.3) of a wide variety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and populations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the sky. Radial velocity accuracies for stars are {sigma}(RV)~4km/s at g&lt;18, degrading to {sigma}(RV)~15km/s at g~20. For stars with signal-to-noise ratio &gt;10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500deg^2^ of additional ugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry ({sigma}(g,r,i) ~2%), ({sigma}(u,z)~3%) and astrometry (~0.1") for spectroscopic target selection. The stellar spectra, imaging data, and derived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7. Individual images of spectra in this data set may be examined by fetching from the DAS, with a link like wget http://das.sdss.org/spectro/1d_26/1880/gif/spPlot-53262-1880-014.gif A FITS data file of the calibrated 1D spectrum is available from wget http://das.sdss.org/spectro/1d_26/1880/1d/spSpec-53262-1880-014.fit</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377#2</TD>
            <TD>2011-09-14T21:30:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/4377&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4377</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4377 [table3]</TD>
            <TD>List of SEGUE plate pairs (Yanny+, 2009)</TD>
            <TD>The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ~240000 moderate-resolution (R~1800) spectra from 3900{AA} to 9000{AA} of fainter Milky Way stars (14.0&lt;g&lt;20.3) of a wide variety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and populations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the sky. Radial velocity accuracies for stars are {sigma}(RV)~4km/s at g&lt;18, degrading to {sigma}(RV)~15km/s at g~20. For stars with signal-to-noise ratio &gt;10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500deg^2^ of additional ugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry ({sigma}(g,r,i) ~2%), ({sigma}(u,z)~3%) and astrometry (~0.1") for spectroscopic target selection. The stellar spectra, imaging data, and derived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7. Individual images of spectra in this data set may be examined by fetching from the DAS, with a link like wget http://das.sdss.org/spectro/1d_26/1880/gif/spPlot-53262-1880-014.gif A FITS data file of the calibrated 1D spectrum is available from wget http://das.sdss.org/spectro/1d_26/1880/1d/spSpec-53262-1880-014.fit</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377#table3</TD>
            <TD>2011-09-14T21:30:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4377&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4377</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/431/143 [1]</TD>
            <TD>Field horizontal-branch stars in the Galaxy (Christlieb+, 2005)</TD>
            <TD>Table A.1 contains photometry (UBV, c_1_), and Balmer line equivalent width sums, as derived directly from HES spectra, as well as coordinates of the 8321 candidate field horizontal-branch stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143#1</TD>
            <TD>2011-09-14T20:12:12Z</TD>
            <TD>#Positional_Data#Photometry#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/431/143</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/431/143</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/431/143 [2]</TD>
            <TD>Field horizontal-branch stars in the Galaxy (Christlieb+, 2005)</TD>
            <TD>Table A.1 contains photometry (UBV, c_1_), and Balmer line equivalent width sums, as derived directly from HES spectra, as well as coordinates of the 8321 candidate field horizontal-branch stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143#2</TD>
            <TD>2011-09-14T20:12:12Z</TD>
            <TD>#Positional_Data#Photometry#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/431/143&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/431/143</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/431/143 [tabla1]</TD>
            <TD>Field horizontal-branch stars in the Galaxy (Christlieb+, 2005)</TD>
            <TD>Table A.1 contains photometry (UBV, c_1_), and Balmer line equivalent width sums, as derived directly from HES spectra, as well as coordinates of the 8321 candidate field horizontal-branch stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143#tabla1</TD>
            <TD>2011-09-14T20:12:12Z</TD>
            <TD>#Positional_Data#Photometry#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/431/143</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/431/143&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/431/143</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/4377 [1]</TD>
            <TD>List of SEGUE plate pairs (Yanny+, 2009)</TD>
            <TD>The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ~240000 moderate-resolution (R~1800) spectra from 3900{AA} to 9000{AA} of fainter Milky Way stars (14.0&lt;g&lt;20.3) of a wide variety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and populations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the sky. Radial velocity accuracies for stars are {sigma}(RV)~4km/s at g&lt;18, degrading to {sigma}(RV)~15km/s at g~20. For stars with signal-to-noise ratio &gt;10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500deg^2^ of additional ugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry ({sigma}(g,r,i) ~2%), ({sigma}(u,z)~3%) and astrometry (~0.1") for spectroscopic target selection. The stellar spectra, imaging data, and derived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7. Individual images of spectra in this data set may be examined by fetching from the DAS, with a link like wget http://das.sdss.org/spectro/1d_26/1880/gif/spPlot-53262-1880-014.gif A FITS data file of the calibrated 1D spectrum is available from wget http://das.sdss.org/spectro/1d_26/1880/1d/spSpec-53262-1880-014.fit</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377#1</TD>
            <TD>2011-09-14T21:30:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/4377</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4377</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/4377 [2]</TD>
            <TD>List of SEGUE plate pairs (Yanny+, 2009)</TD>
            <TD>The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ~240000 moderate-resolution (R~1800) spectra from 3900{AA} to 9000{AA} of fainter Milky Way stars (14.0&lt;g&lt;20.3) of a wide variety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and populations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the sky. Radial velocity accuracies for stars are {sigma}(RV)~4km/s at g&lt;18, degrading to {sigma}(RV)~15km/s at g~20. For stars with signal-to-noise ratio &gt;10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500deg^2^ of additional ugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry ({sigma}(g,r,i) ~2%), ({sigma}(u,z)~3%) and astrometry (~0.1") for spectroscopic target selection. The stellar spectra, imaging data, and derived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7. Individual images of spectra in this data set may be examined by fetching from the DAS, with a link like wget http://das.sdss.org/spectro/1d_26/1880/gif/spPlot-53262-1880-014.gif A FITS data file of the calibrated 1D spectrum is available from wget http://das.sdss.org/spectro/1d_26/1880/1d/spSpec-53262-1880-014.fit</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377#2</TD>
            <TD>2011-09-14T21:30:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/4377&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4377</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4377 [table3]</TD>
            <TD>List of SEGUE plate pairs (Yanny+, 2009)</TD>
            <TD>The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ~240000 moderate-resolution (R~1800) spectra from 3900{AA} to 9000{AA} of fainter Milky Way stars (14.0&lt;g&lt;20.3) of a wide variety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and populations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the sky. Radial velocity accuracies for stars are {sigma}(RV)~4km/s at g&lt;18, degrading to {sigma}(RV)~15km/s at g~20. For stars with signal-to-noise ratio &gt;10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500deg^2^ of additional ugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry ({sigma}(g,r,i) ~2%), ({sigma}(u,z)~3%) and astrometry (~0.1") for spectroscopic target selection. The stellar spectra, imaging data, and derived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7. Individual images of spectra in this data set may be examined by fetching from the DAS, with a link like wget http://das.sdss.org/spectro/1d_26/1880/gif/spPlot-53262-1880-014.gif A FITS data file of the calibrated 1D spectrum is available from wget http://das.sdss.org/spectro/1d_26/1880/1d/spSpec-53262-1880-014.fit</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377#table3</TD>
            <TD>2011-09-14T21:30:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4377&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4377</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/171/261 [1]</TD>
            <TD>Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)</TD>
            <TD>We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109{alpha} and H110{alpha}) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261#1</TD>
            <TD>2012-09-24T08:56:36Z</TD>
            <TD>#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/171/261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/171/261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/171/261 [2]</TD>
            <TD>Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)</TD>
            <TD>We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109{alpha} and H110{alpha}) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261#2</TD>
            <TD>2012-09-24T08:56:36Z</TD>
            <TD>#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/171/261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/171/261</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/171/261 [table1]</TD>
            <TD>Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)</TD>
            <TD>We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109{alpha} and H110{alpha}) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261#table1</TD>
            <TD>2012-09-24T08:56:36Z</TD>
            <TD>#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/171/261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/171/261</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/426/11 [1]</TD>
            <TD>XMM-Newton survey of M33 (Pietsch+, 2004)</TD>
            <TD>In an XMM-Newton raster observation of the bright Local Group spiral galaxy M 33 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 10^35^erg/s - more than a factor of 10 deeper than earlier ROSAT observations. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. We correlate these newly detected sources with earlier M 33 X-ray catalogues and information from optical, infra-red and radio wavelengths. As M 33 sources we detect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations we would expect 175 to 210 background sources in this field. This indicates that about half of the sources detected are within M 33.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11#1</TD>
            <TD>2011-09-14T20:34:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/426/11</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/426/11</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/426/11 [2]</TD>
            <TD>XMM-Newton survey of M33 (Pietsch+, 2004)</TD>
            <TD>In an XMM-Newton raster observation of the bright Local Group spiral galaxy M 33 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 10^35^erg/s - more than a factor of 10 deeper than earlier ROSAT observations. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. We correlate these newly detected sources with earlier M 33 X-ray catalogues and information from optical, infra-red and radio wavelengths. As M 33 sources we detect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations we would expect 175 to 210 background sources in this field. This indicates that about half of the sources detected are within M 33.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11#2</TD>
            <TD>2011-09-14T20:34:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/426/11&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/426/11</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/426/11 [table3]</TD>
            <TD>XMM-Newton survey of M33 (Pietsch+, 2004)</TD>
            <TD>In an XMM-Newton raster observation of the bright Local Group spiral galaxy M 33 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 10^35^erg/s - more than a factor of 10 deeper than earlier ROSAT observations. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. We correlate these newly detected sources with earlier M 33 X-ray catalogues and information from optical, infra-red and radio wavelengths. As M 33 sources we detect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations we would expect 175 to 210 background sources in this field. This indicates that about half of the sources detected are within M 33.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11#table3</TD>
            <TD>2011-09-14T20:34:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/426/11&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/426/11</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/4377 [1]</TD>
            <TD>List of SEGUE plate pairs (Yanny+, 2009)</TD>
            <TD>The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ~240000 moderate-resolution (R~1800) spectra from 3900{AA} to 9000{AA} of fainter Milky Way stars (14.0&lt;g&lt;20.3) of a wide variety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and populations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the sky. Radial velocity accuracies for stars are {sigma}(RV)~4km/s at g&lt;18, degrading to {sigma}(RV)~15km/s at g~20. For stars with signal-to-noise ratio &gt;10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500deg^2^ of additional ugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry ({sigma}(g,r,i) ~2%), ({sigma}(u,z)~3%) and astrometry (~0.1") for spectroscopic target selection. The stellar spectra, imaging data, and derived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7. Individual images of spectra in this data set may be examined by fetching from the DAS, with a link like wget http://das.sdss.org/spectro/1d_26/1880/gif/spPlot-53262-1880-014.gif A FITS data file of the calibrated 1D spectrum is available from wget http://das.sdss.org/spectro/1d_26/1880/1d/spSpec-53262-1880-014.fit</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377#1</TD>
            <TD>2011-09-14T21:30:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/4377</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4377</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/4377 [2]</TD>
            <TD>List of SEGUE plate pairs (Yanny+, 2009)</TD>
            <TD>The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ~240000 moderate-resolution (R~1800) spectra from 3900{AA} to 9000{AA} of fainter Milky Way stars (14.0&lt;g&lt;20.3) of a wide variety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and populations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the sky. Radial velocity accuracies for stars are {sigma}(RV)~4km/s at g&lt;18, degrading to {sigma}(RV)~15km/s at g~20. For stars with signal-to-noise ratio &gt;10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500deg^2^ of additional ugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry ({sigma}(g,r,i) ~2%), ({sigma}(u,z)~3%) and astrometry (~0.1") for spectroscopic target selection. The stellar spectra, imaging data, and derived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7. Individual images of spectra in this data set may be examined by fetching from the DAS, with a link like wget http://das.sdss.org/spectro/1d_26/1880/gif/spPlot-53262-1880-014.gif A FITS data file of the calibrated 1D spectrum is available from wget http://das.sdss.org/spectro/1d_26/1880/1d/spSpec-53262-1880-014.fit</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377#2</TD>
            <TD>2011-09-14T21:30:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/4377&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4377</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/4377 [table3]</TD>
            <TD>List of SEGUE plate pairs (Yanny+, 2009)</TD>
            <TD>The Sloan Extension for Galactic Understanding and Exploration (SEGUE) Survey obtained ~240000 moderate-resolution (R~1800) spectra from 3900{AA} to 9000{AA} of fainter Milky Way stars (14.0&lt;g&lt;20.3) of a wide variety of spectral types, both main-sequence and evolved objects, with the goal of studying the kinematics and populations of our Galaxy and its halo. The spectra are clustered in 212 regions spaced over three quarters of the sky. Radial velocity accuracies for stars are {sigma}(RV)~4km/s at g&lt;18, degrading to {sigma}(RV)~15km/s at g~20. For stars with signal-to-noise ratio &gt;10 per resolution element, stellar atmospheric parameters are estimated, including metallicity, surface gravity, and effective temperature. SEGUE obtained 3500deg^2^ of additional ugriz imaging (primarily at low Galactic latitudes) providing precise multicolor photometry ({sigma}(g,r,i) ~2%), ({sigma}(u,z)~3%) and astrometry (~0.1") for spectroscopic target selection. The stellar spectra, imaging data, and derived parameter catalogs for this survey are publicly available as part of Sloan Digital Sky Survey Data Release 7. Individual images of spectra in this data set may be examined by fetching from the DAS, with a link like wget http://das.sdss.org/spectro/1d_26/1880/gif/spPlot-53262-1880-014.gif A FITS data file of the calibrated 1D spectrum is available from wget http://das.sdss.org/spectro/1d_26/1880/1d/spSpec-53262-1880-014.fit</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377#table3</TD>
            <TD>2011-09-14T21:30:32Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/4377</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/4377&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/4377</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/171/261 [1]</TD>
            <TD>Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)</TD>
            <TD>We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109{alpha} and H110{alpha}) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261#1</TD>
            <TD>2012-09-24T08:56:36Z</TD>
            <TD>#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/171/261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/171/261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/171/261 [2]</TD>
            <TD>Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)</TD>
            <TD>We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109{alpha} and H110{alpha}) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261#2</TD>
            <TD>2012-09-24T08:56:36Z</TD>
            <TD>#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/171/261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/171/261</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/171/261 [table1]</TD>
            <TD>Radio Recombination Lines of Southern HII Regions (Caswell+ 1987)</TD>
            <TD>We tabulate velocities and other parameters of hydrogen recombination lines near 5GHz (H109{alpha} and H110{alpha}) for 316 HII regions observed with the Parkes 64-m radio telescope. Results of a new search for formaldehyde absorption are also listed. Source selection was based on the 5GHz continuum southern galactic plane survey of Haynes et al. (1978, 1979). Data is given for most H II regions in the galactic longitude range 210 to 360 degrees that show 5GHz continuum brightness temperature exceeding 1K (as observed with the 4 arcminute beam of the Parkes 64-m telescope), together with a selection of sources that are weaker or outside of this longitude range. Tabulated data include source coordinates, peak brightness, flux density, and angular size from the 5GHz continuum survey; radial velocities of detected formaldehyde absorption lines; recombination line peak brightness, radial velocity, and line width; derived electron temperature assuming LTE; derived kinematic distance from the Sun and galactocentric radius; and presence or absence of a visible optical counterpart. In cases where kinematic distance is ambiguous, both near and far distances are tabulated; a flag is given if there is a strong preference for near or far distance based on information such as H I or H2CO absorption measurements or visibility of an optical counterpart. Many of these radio HII regions lie beyond the range of optical detection, at distances exceeding several kpc; they thus provide a comprehensive coverage of the southern HII regions in the Galaxy over the longitude range 210 to 360 degrees and constitute a vital data base for the study of galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261#table1</TD>
            <TD>2012-09-24T08:56:36Z</TD>
            <TD>#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/171/261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/171/261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/171/261</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/426/11 [1]</TD>
            <TD>XMM-Newton survey of M33 (Pietsch+, 2004)</TD>
            <TD>In an XMM-Newton raster observation of the bright Local Group spiral galaxy M 33 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 10^35^erg/s - more than a factor of 10 deeper than earlier ROSAT observations. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. We correlate these newly detected sources with earlier M 33 X-ray catalogues and information from optical, infra-red and radio wavelengths. As M 33 sources we detect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations we would expect 175 to 210 background sources in this field. This indicates that about half of the sources detected are within M 33.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11#1</TD>
            <TD>2011-09-14T20:34:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/426/11</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/426/11</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/426/11 [2]</TD>
            <TD>XMM-Newton survey of M33 (Pietsch+, 2004)</TD>
            <TD>In an XMM-Newton raster observation of the bright Local Group spiral galaxy M 33 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 10^35^erg/s - more than a factor of 10 deeper than earlier ROSAT observations. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. We correlate these newly detected sources with earlier M 33 X-ray catalogues and information from optical, infra-red and radio wavelengths. As M 33 sources we detect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations we would expect 175 to 210 background sources in this field. This indicates that about half of the sources detected are within M 33.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11#2</TD>
            <TD>2011-09-14T20:34:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/426/11&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/426/11</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/426/11 [table3]</TD>
            <TD>XMM-Newton survey of M33 (Pietsch+, 2004)</TD>
            <TD>In an XMM-Newton raster observation of the bright Local Group spiral galaxy M 33 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 10^35^erg/s - more than a factor of 10 deeper than earlier ROSAT observations. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. We correlate these newly detected sources with earlier M 33 X-ray catalogues and information from optical, infra-red and radio wavelengths. As M 33 sources we detect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations we would expect 175 to 210 background sources in this field. This indicates that about half of the sources detected are within M 33.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11#table3</TD>
            <TD>2011-09-14T20:34:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/426/11&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/426/11</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/2130 [1]</TD>
            <TD>ALFA-ZOA precursor observation (Henning+, 2010)</TD>
            <TD>The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totaling 138deg^2^, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have Two Micron All Sky Survey counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130#1</TD>
            <TD>2012-07-14T22:39:33Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/2130</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/2130</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/2130 [2]</TD>
            <TD>ALFA-ZOA precursor observation (Henning+, 2010)</TD>
            <TD>The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totaling 138deg^2^, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have Two Micron All Sky Survey counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130#2</TD>
            <TD>2012-07-14T22:39:33Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/2130&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/2130</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/2130 [table1]</TD>
            <TD>ALFA-ZOA precursor observation (Henning+, 2010)</TD>
            <TD>The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totaling 138deg^2^, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have Two Micron All Sky Survey counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130#table1</TD>
            <TD>2012-07-14T22:39:33Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/2130&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/2130</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/278/1025 [1]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#1</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/278/1025</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/278/1025 [2]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#2</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/278/1025&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/278/1025 [fields]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#fields</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/278/1025&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/278/1025 [galaxy]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#galaxy</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/278/1025&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/2130 [1]</TD>
            <TD>ALFA-ZOA precursor observation (Henning+, 2010)</TD>
            <TD>The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totaling 138deg^2^, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have Two Micron All Sky Survey counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130#1</TD>
            <TD>2012-07-14T22:39:33Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/2130</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/2130</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/2130 [2]</TD>
            <TD>ALFA-ZOA precursor observation (Henning+, 2010)</TD>
            <TD>The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totaling 138deg^2^, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have Two Micron All Sky Survey counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130#2</TD>
            <TD>2012-07-14T22:39:33Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/2130&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/2130</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/2130 [table1]</TD>
            <TD>ALFA-ZOA precursor observation (Henning+, 2010)</TD>
            <TD>The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totaling 138deg^2^, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have Two Micron All Sky Survey counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130#table1</TD>
            <TD>2012-07-14T22:39:33Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/2130&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/2130</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/426/11 [1]</TD>
            <TD>XMM-Newton survey of M33 (Pietsch+, 2004)</TD>
            <TD>In an XMM-Newton raster observation of the bright Local Group spiral galaxy M 33 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 10^35^erg/s - more than a factor of 10 deeper than earlier ROSAT observations. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. We correlate these newly detected sources with earlier M 33 X-ray catalogues and information from optical, infra-red and radio wavelengths. As M 33 sources we detect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations we would expect 175 to 210 background sources in this field. This indicates that about half of the sources detected are within M 33.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11#1</TD>
            <TD>2011-09-14T20:34:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/426/11</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/426/11</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/426/11 [2]</TD>
            <TD>XMM-Newton survey of M33 (Pietsch+, 2004)</TD>
            <TD>In an XMM-Newton raster observation of the bright Local Group spiral galaxy M 33 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 10^35^erg/s - more than a factor of 10 deeper than earlier ROSAT observations. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. We correlate these newly detected sources with earlier M 33 X-ray catalogues and information from optical, infra-red and radio wavelengths. As M 33 sources we detect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations we would expect 175 to 210 background sources in this field. This indicates that about half of the sources detected are within M 33.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11#2</TD>
            <TD>2011-09-14T20:34:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/426/11&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/426/11</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/426/11 [table3]</TD>
            <TD>XMM-Newton survey of M33 (Pietsch+, 2004)</TD>
            <TD>In an XMM-Newton raster observation of the bright Local Group spiral galaxy M 33 we study the population of X-ray sources (X-ray binaries, supernova remnants) down to a 0.2-4.5keV luminosity of 10^35^erg/s - more than a factor of 10 deeper than earlier ROSAT observations. EPIC hardness ratios and optical and radio information are used to distinguish between different source classes. The survey detects 408 sources in an area of 0.80 square degree. We correlate these newly detected sources with earlier M 33 X-ray catalogues and information from optical, infra-red and radio wavelengths. As M 33 sources we detect 21 supernova remnants (SNR) and 23 SNR candidates, 5 super-soft sources and 2 X-ray binaries (XRBs). There are 267 sources classified as hard, which may either be XRBs or Crab-like SNRs in M 33 or background AGN. The 44 confirmed and candidate SNRs more than double the number of X-ray detected SNRs in M 33. 16 of these are proposed as SNR candidates from the X-ray data for the first time. On the other hand, there are several sources not connected to M 33: five foreground stars, 30 foreground star candidates, 12 active galactic nucleus candidates, one background galaxy and one background galaxy candidate. Extrapolating from deep field observations we would expect 175 to 210 background sources in this field. This indicates that about half of the sources detected are within M 33.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11#table3</TD>
            <TD>2011-09-14T20:34:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/426/11</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/426/11&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/426/11</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/2130 [1]</TD>
            <TD>ALFA-ZOA precursor observation (Henning+, 2010)</TD>
            <TD>The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totaling 138deg^2^, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have Two Micron All Sky Survey counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130#1</TD>
            <TD>2012-07-14T22:39:33Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/2130</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/2130</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/2130 [2]</TD>
            <TD>ALFA-ZOA precursor observation (Henning+, 2010)</TD>
            <TD>The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totaling 138deg^2^, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have Two Micron All Sky Survey counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130#2</TD>
            <TD>2012-07-14T22:39:33Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/2130&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/2130</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/2130 [table1]</TD>
            <TD>ALFA-ZOA precursor observation (Henning+, 2010)</TD>
            <TD>The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totaling 138deg^2^, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have Two Micron All Sky Survey counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130#table1</TD>
            <TD>2012-07-14T22:39:33Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/2130</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/2130&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/2130</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/278/1025 [1]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#1</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/278/1025</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/278/1025 [2]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#2</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/278/1025&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/278/1025 [fields]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#fields</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/278/1025&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/278/1025 [galaxy]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#galaxy</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/278/1025&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/497/667 [1]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#1</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/497/667</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/497/667 [2]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#2</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/497/667&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/497/667 [tabled3]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#tabled3</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/497/667&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/497/667 [wings]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#wings</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/497/667&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/341/1093 [1]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#1</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/341/1093</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/341/1093 [2]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#2</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/341/1093 [fields]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#fields</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/341/1093 [extsrcs]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#extsrcs</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/341/1093 [clusters]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#clusters</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/278/1025 [1]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#1</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/278/1025</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/278/1025 [2]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#2</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/278/1025&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/278/1025 [fields]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#fields</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/278/1025&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/278/1025 [galaxy]</TD>
            <TD>The APM Bright Galaxy Catalogue (Loveday 1996)</TD>
            <TD>The APM Bright Galaxy Catalogue lists positions, magnitudes, shapes and morphological types for 14,681 galaxies brighter than b(J) magnitude 16.44 over a 4,180 square degree area of the southern sky. Galaxy and stellar images have been located from glass copy plates of the United Kingdom Schmidt Telescope (UKST) IIIaJ sky survey using the Automated Photographic Measuring (APM) facility in Cambridge, England. The majority of stellar images are rejected by the regularity of their image surface brightness profiles. Remaining images are inspected by eye on film copies of the survey material and classed as stellar, multiple stellar, galaxy, merger or noise. Galaxies are further classified as elliptical, lenticular, spiral, irregular or uncertain. The 180 survey fields are put onto a uniform photometric system by comparing the magnitudes of galaxies in the overlap regions between neighbouring plates. The magnitude zero-point, photometric uniformity and photographic saturation are checked with CCD photometry. Finally, the completeness and reliability of the catalogue is assessed using various internal tests and by comparing with several independently constructed galaxy catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025#galaxy</TD>
            <TD>2012-09-24T08:59:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/278/1025</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/278/1025&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/278/1025</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/497/667 [1]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#1</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/497/667</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/497/667 [2]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#2</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/497/667&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/497/667 [tabled3]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#tabled3</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/497/667&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/497/667 [wings]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#wings</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/497/667&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/341/1093 [1]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#1</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/341/1093</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/341/1093 [2]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#2</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/341/1093 [fields]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#fields</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/341/1093 [extsrcs]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#extsrcs</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/341/1093 [clusters]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#clusters</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/221 [1]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#1</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/221 [2]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#2</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/221 [psczcg]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#psczcg</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/221 [pscz]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#pscz</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/341/1093 [1]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#1</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/341/1093</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/341/1093 [2]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#2</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/341/1093 [fields]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#fields</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/341/1093 [extsrcs]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#extsrcs</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/341/1093 [clusters]</TD>
            <TD>The Southern SHARC catalogue (Burke+, 2003)</TD>
            <TD>The Southern Serendipitous High-redshift Archival Cluster (SHARC) catalogue is a X-ray selected catalogue of galaxy clusters detected in deep ROSAT observations. The survey area is 17.7deg^2^ and is selected from long (greater than 10ks) ROSAT exposures with a declination &lt;+20deg and excluding the Galactic plane (excluding galactic latitudes within the range [-20,20]deg). Optical follow-up was performed to confirm the presence of a galaxy cluster and measure its redshift. The final catalogue contains 32 galaxy clusters with redshifts between 0.05 and 0.70 and X-ray luminosities between 7x10^35^W and 4x10^37^W. Above a redshift of 0.3 - which forms the primary subsample of the survey - there are 16 clusters; the X-ray luminosities of these clusters are all greater than 2x10^36 W. All X-ray luminosities are quoted in the 0.5-2.0keV band and were calculated using an Einstein-de Sitter cosmology with H_0_ set to 50km/s/Mpc.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093#clusters</TD>
            <TD>2012-09-24T07:17:19Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/341/1093</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/341/1093&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/341/1093</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/497/667 [1]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#1</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/497/667</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/497/667 [2]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#2</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/497/667&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/497/667 [tabled3]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#tabled3</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/497/667&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/497/667 [wings]</TD>
            <TD>WINGS: Deep optical phot. of 77 nearby clusters (Varela+, 2009)</TD>
            <TD>This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04&lt;z&lt;0.07) located far from the galactic plane (|b|&gt;200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V&lt;20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667#wings</TD>
            <TD>2011-09-14T20:34:31Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/497/667</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/497/667&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/497/667</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/221 [1]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#1</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/221 [2]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#2</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/221 [psczcg]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#psczcg</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/221 [pscz]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#pscz</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/469 [1]</TD>
            <TD>First list of the Karachentsev catalog (Huchtmeier+, 2000)</TD>
            <TD>We present HI observations of the galaxies in the first list of the Karachentsev catalog of previously unknown nearby dwarf galaxies (Karachentseva &amp; Karachentsev, 1998, Cat. &lt;J/A+AS/127/409&gt;). This survey covers all known nearby galaxy groups within the Local Volume (i.e. within 10Mpc) and their environment, that is about 25% of the total sky. A total of 257 galaxies have been observed with a detection rate of 60%. We searched a frequency band corresponding to heliocentric radial velocities from -470km/s to ~+4000km/s. Non-detections are either due to limited coverage in radial velocity, confusion with Local HI (mainly in the velocity range -140km/s to +20km/s), or lack of sensitivity for very weak emission. 25% of the detected galaxies are located within the Local Volume. Those galaxies are dwarf galaxies judged by their optical linear diameter (1.4+/-0.2kpc on the average), their mean total HI mass (4.6x10^7^M_{sun}_), and their observed linewidths (39km/s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469#1</TD>
            <TD>2012-09-24T07:17:48Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/469</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/469</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/469 [2]</TD>
            <TD>First list of the Karachentsev catalog (Huchtmeier+, 2000)</TD>
            <TD>We present HI observations of the galaxies in the first list of the Karachentsev catalog of previously unknown nearby dwarf galaxies (Karachentseva &amp; Karachentsev, 1998, Cat. &lt;J/A+AS/127/409&gt;). This survey covers all known nearby galaxy groups within the Local Volume (i.e. within 10Mpc) and their environment, that is about 25% of the total sky. A total of 257 galaxies have been observed with a detection rate of 60%. We searched a frequency band corresponding to heliocentric radial velocities from -470km/s to ~+4000km/s. Non-detections are either due to limited coverage in radial velocity, confusion with Local HI (mainly in the velocity range -140km/s to +20km/s), or lack of sensitivity for very weak emission. 25% of the detected galaxies are located within the Local Volume. Those galaxies are dwarf galaxies judged by their optical linear diameter (1.4+/-0.2kpc on the average), their mean total HI mass (4.6x10^7^M_{sun}_), and their observed linewidths (39km/s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469#2</TD>
            <TD>2012-09-24T07:17:48Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/469&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/469</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/469 [table1]</TD>
            <TD>First list of the Karachentsev catalog (Huchtmeier+, 2000)</TD>
            <TD>We present HI observations of the galaxies in the first list of the Karachentsev catalog of previously unknown nearby dwarf galaxies (Karachentseva &amp; Karachentsev, 1998, Cat. &lt;J/A+AS/127/409&gt;). This survey covers all known nearby galaxy groups within the Local Volume (i.e. within 10Mpc) and their environment, that is about 25% of the total sky. A total of 257 galaxies have been observed with a detection rate of 60%. We searched a frequency band corresponding to heliocentric radial velocities from -470km/s to ~+4000km/s. Non-detections are either due to limited coverage in radial velocity, confusion with Local HI (mainly in the velocity range -140km/s to +20km/s), or lack of sensitivity for very weak emission. 25% of the detected galaxies are located within the Local Volume. Those galaxies are dwarf galaxies judged by their optical linear diameter (1.4+/-0.2kpc on the average), their mean total HI mass (4.6x10^7^M_{sun}_), and their observed linewidths (39km/s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469#table1</TD>
            <TD>2012-09-24T07:17:48Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/469&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/469</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/1780 [1]</TD>
            <TD>GALEX/SDSS quasar catalog (Trammell+, 2007)</TD>
            <TD>We present an analysis of the broadband UV and optical properties of z~&lt;3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7". Most of the DR3 sample quasars are detected in the near-UV until z~1.7, with the near-UV detection fraction dropping to ~50% by z~2.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780#1</TD>
            <TD>2011-09-14T20:46:03Z</TD>
            <TD>#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/1780</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/1780</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/1780 [2]</TD>
            <TD>GALEX/SDSS quasar catalog (Trammell+, 2007)</TD>
            <TD>We present an analysis of the broadband UV and optical properties of z~&lt;3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7". Most of the DR3 sample quasars are detected in the near-UV until z~1.7, with the near-UV detection fraction dropping to ~50% by z~2.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780#2</TD>
            <TD>2011-09-14T20:46:03Z</TD>
            <TD>#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/1780&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/1780</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/1780 [table2]</TD>
            <TD>GALEX/SDSS quasar catalog (Trammell+, 2007)</TD>
            <TD>We present an analysis of the broadband UV and optical properties of z~&lt;3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7". Most of the DR3 sample quasars are detected in the near-UV until z~1.7, with the near-UV detection fraction dropping to ~50% by z~2.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780#table2</TD>
            <TD>2011-09-14T20:46:03Z</TD>
            <TD>#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/1780&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/1780</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/221 [1]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#1</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/221 [2]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#2</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/221 [psczcg]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#psczcg</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/221 [pscz]</TD>
            <TD>PSCz catalog (Saunders+, 2000)</TD>
            <TD>The PSCz survey consists of redshifts, infra-red and optical photometry, and assorted other information for 18351 IRAS sources, mostly selected from the Point Source Catalog. The survey was designed to select almost all galaxies with flux brighter than 0.595Jy at 60 microns, over the 84% of the sky with extinction small enough that reliable and complete optical identification and spectroscopy was possible. Some of the sources are not galaxies and some are multiple entries for the same galaxy as described below. There are in total 15411 galaxies or possible galaxies, for which redshifts are available for 14677. The galaxies without redshift are mostly distant or at low latitude, as described below. Many of these galaxies have now been observed as part of the BTP project (Saunders et al 1999, astro-ph/9909174 "The Behind the Plane Survey"), and their redshifts will be included in future revisions of the catalogue. The main catalogue is "pscz.dat". There is also a short version of the catalogue, "psczvs.dat", containing sufficient information for most studies. They correspond to the version 2.2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VII/221#pscz</TD>
            <TD>2012-09-28T08:13:47Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/VII/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/469 [1]</TD>
            <TD>First list of the Karachentsev catalog (Huchtmeier+, 2000)</TD>
            <TD>We present HI observations of the galaxies in the first list of the Karachentsev catalog of previously unknown nearby dwarf galaxies (Karachentseva &amp; Karachentsev, 1998, Cat. &lt;J/A+AS/127/409&gt;). This survey covers all known nearby galaxy groups within the Local Volume (i.e. within 10Mpc) and their environment, that is about 25% of the total sky. A total of 257 galaxies have been observed with a detection rate of 60%. We searched a frequency band corresponding to heliocentric radial velocities from -470km/s to ~+4000km/s. Non-detections are either due to limited coverage in radial velocity, confusion with Local HI (mainly in the velocity range -140km/s to +20km/s), or lack of sensitivity for very weak emission. 25% of the detected galaxies are located within the Local Volume. Those galaxies are dwarf galaxies judged by their optical linear diameter (1.4+/-0.2kpc on the average), their mean total HI mass (4.6x10^7^M_{sun}_), and their observed linewidths (39km/s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469#1</TD>
            <TD>2012-09-24T07:17:48Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/469</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/469</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/469 [2]</TD>
            <TD>First list of the Karachentsev catalog (Huchtmeier+, 2000)</TD>
            <TD>We present HI observations of the galaxies in the first list of the Karachentsev catalog of previously unknown nearby dwarf galaxies (Karachentseva &amp; Karachentsev, 1998, Cat. &lt;J/A+AS/127/409&gt;). This survey covers all known nearby galaxy groups within the Local Volume (i.e. within 10Mpc) and their environment, that is about 25% of the total sky. A total of 257 galaxies have been observed with a detection rate of 60%. We searched a frequency band corresponding to heliocentric radial velocities from -470km/s to ~+4000km/s. Non-detections are either due to limited coverage in radial velocity, confusion with Local HI (mainly in the velocity range -140km/s to +20km/s), or lack of sensitivity for very weak emission. 25% of the detected galaxies are located within the Local Volume. Those galaxies are dwarf galaxies judged by their optical linear diameter (1.4+/-0.2kpc on the average), their mean total HI mass (4.6x10^7^M_{sun}_), and their observed linewidths (39km/s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469#2</TD>
            <TD>2012-09-24T07:17:48Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/469&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/469</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/469 [table1]</TD>
            <TD>First list of the Karachentsev catalog (Huchtmeier+, 2000)</TD>
            <TD>We present HI observations of the galaxies in the first list of the Karachentsev catalog of previously unknown nearby dwarf galaxies (Karachentseva &amp; Karachentsev, 1998, Cat. &lt;J/A+AS/127/409&gt;). This survey covers all known nearby galaxy groups within the Local Volume (i.e. within 10Mpc) and their environment, that is about 25% of the total sky. A total of 257 galaxies have been observed with a detection rate of 60%. We searched a frequency band corresponding to heliocentric radial velocities from -470km/s to ~+4000km/s. Non-detections are either due to limited coverage in radial velocity, confusion with Local HI (mainly in the velocity range -140km/s to +20km/s), or lack of sensitivity for very weak emission. 25% of the detected galaxies are located within the Local Volume. Those galaxies are dwarf galaxies judged by their optical linear diameter (1.4+/-0.2kpc on the average), their mean total HI mass (4.6x10^7^M_{sun}_), and their observed linewidths (39km/s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469#table1</TD>
            <TD>2012-09-24T07:17:48Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/469&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/469</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/201/31 [1]</TD>
            <TD>Emission-line galaxies from SDSS. I. (Ge+, 2012)</TD>
            <TD>For the goal of selecting pp-galaxies, we develop a series of automatic algorithms in light of Monte Carlo simulations. We apply the algorithms to SDSS galaxy spectra and get candidates from the pp-galaxies. Then we visually inspect the candidate spectra to establish the final sample. We start from the database of the MPA-JHU SDSS-DR7 galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31#1</TD>
            <TD>2012-12-28T08:53:43Z</TD>
            <TD>#AGN#Galaxies:spectra#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/201/31</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/201/31</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/201/31 [2]</TD>
            <TD>Emission-line galaxies from SDSS. I. (Ge+, 2012)</TD>
            <TD>For the goal of selecting pp-galaxies, we develop a series of automatic algorithms in light of Monte Carlo simulations. We apply the algorithms to SDSS galaxy spectra and get candidates from the pp-galaxies. Then we visually inspect the candidate spectra to establish the final sample. We start from the database of the MPA-JHU SDSS-DR7 galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31#2</TD>
            <TD>2012-12-28T08:53:43Z</TD>
            <TD>#AGN#Galaxies:spectra#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/201/31&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/201/31</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/201/31 [emgal]</TD>
            <TD>Emission-line galaxies from SDSS. I. (Ge+, 2012)</TD>
            <TD>For the goal of selecting pp-galaxies, we develop a series of automatic algorithms in light of Monte Carlo simulations. We apply the algorithms to SDSS galaxy spectra and get candidates from the pp-galaxies. Then we visually inspect the candidate spectra to establish the final sample. We start from the database of the MPA-JHU SDSS-DR7 galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31#emgal</TD>
            <TD>2012-12-28T08:53:43Z</TD>
            <TD>#AGN#Galaxies:spectra#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/201/31&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/201/31</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/469 [1]</TD>
            <TD>First list of the Karachentsev catalog (Huchtmeier+, 2000)</TD>
            <TD>We present HI observations of the galaxies in the first list of the Karachentsev catalog of previously unknown nearby dwarf galaxies (Karachentseva &amp; Karachentsev, 1998, Cat. &lt;J/A+AS/127/409&gt;). This survey covers all known nearby galaxy groups within the Local Volume (i.e. within 10Mpc) and their environment, that is about 25% of the total sky. A total of 257 galaxies have been observed with a detection rate of 60%. We searched a frequency band corresponding to heliocentric radial velocities from -470km/s to ~+4000km/s. Non-detections are either due to limited coverage in radial velocity, confusion with Local HI (mainly in the velocity range -140km/s to +20km/s), or lack of sensitivity for very weak emission. 25% of the detected galaxies are located within the Local Volume. Those galaxies are dwarf galaxies judged by their optical linear diameter (1.4+/-0.2kpc on the average), their mean total HI mass (4.6x10^7^M_{sun}_), and their observed linewidths (39km/s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469#1</TD>
            <TD>2012-09-24T07:17:48Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/469</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/469</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/469 [2]</TD>
            <TD>First list of the Karachentsev catalog (Huchtmeier+, 2000)</TD>
            <TD>We present HI observations of the galaxies in the first list of the Karachentsev catalog of previously unknown nearby dwarf galaxies (Karachentseva &amp; Karachentsev, 1998, Cat. &lt;J/A+AS/127/409&gt;). This survey covers all known nearby galaxy groups within the Local Volume (i.e. within 10Mpc) and their environment, that is about 25% of the total sky. A total of 257 galaxies have been observed with a detection rate of 60%. We searched a frequency band corresponding to heliocentric radial velocities from -470km/s to ~+4000km/s. Non-detections are either due to limited coverage in radial velocity, confusion with Local HI (mainly in the velocity range -140km/s to +20km/s), or lack of sensitivity for very weak emission. 25% of the detected galaxies are located within the Local Volume. Those galaxies are dwarf galaxies judged by their optical linear diameter (1.4+/-0.2kpc on the average), their mean total HI mass (4.6x10^7^M_{sun}_), and their observed linewidths (39km/s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469#2</TD>
            <TD>2012-09-24T07:17:48Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/469&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/469</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/469 [table1]</TD>
            <TD>First list of the Karachentsev catalog (Huchtmeier+, 2000)</TD>
            <TD>We present HI observations of the galaxies in the first list of the Karachentsev catalog of previously unknown nearby dwarf galaxies (Karachentseva &amp; Karachentsev, 1998, Cat. &lt;J/A+AS/127/409&gt;). This survey covers all known nearby galaxy groups within the Local Volume (i.e. within 10Mpc) and their environment, that is about 25% of the total sky. A total of 257 galaxies have been observed with a detection rate of 60%. We searched a frequency band corresponding to heliocentric radial velocities from -470km/s to ~+4000km/s. Non-detections are either due to limited coverage in radial velocity, confusion with Local HI (mainly in the velocity range -140km/s to +20km/s), or lack of sensitivity for very weak emission. 25% of the detected galaxies are located within the Local Volume. Those galaxies are dwarf galaxies judged by their optical linear diameter (1.4+/-0.2kpc on the average), their mean total HI mass (4.6x10^7^M_{sun}_), and their observed linewidths (39km/s).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469#table1</TD>
            <TD>2012-09-24T07:17:48Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/469</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/469&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/469</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/1780 [1]</TD>
            <TD>GALEX/SDSS quasar catalog (Trammell+, 2007)</TD>
            <TD>We present an analysis of the broadband UV and optical properties of z~&lt;3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7". Most of the DR3 sample quasars are detected in the near-UV until z~1.7, with the near-UV detection fraction dropping to ~50% by z~2.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780#1</TD>
            <TD>2011-09-14T20:46:03Z</TD>
            <TD>#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/1780</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/1780</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/1780 [2]</TD>
            <TD>GALEX/SDSS quasar catalog (Trammell+, 2007)</TD>
            <TD>We present an analysis of the broadband UV and optical properties of z~&lt;3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7". Most of the DR3 sample quasars are detected in the near-UV until z~1.7, with the near-UV detection fraction dropping to ~50% by z~2.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780#2</TD>
            <TD>2011-09-14T20:46:03Z</TD>
            <TD>#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/1780&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/1780</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/1780 [table2]</TD>
            <TD>GALEX/SDSS quasar catalog (Trammell+, 2007)</TD>
            <TD>We present an analysis of the broadband UV and optical properties of z~&lt;3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7". Most of the DR3 sample quasars are detected in the near-UV until z~1.7, with the near-UV detection fraction dropping to ~50% by z~2.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780#table2</TD>
            <TD>2011-09-14T20:46:03Z</TD>
            <TD>#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/1780&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/1780</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/201/31 [1]</TD>
            <TD>Emission-line galaxies from SDSS. I. (Ge+, 2012)</TD>
            <TD>For the goal of selecting pp-galaxies, we develop a series of automatic algorithms in light of Monte Carlo simulations. We apply the algorithms to SDSS galaxy spectra and get candidates from the pp-galaxies. Then we visually inspect the candidate spectra to establish the final sample. We start from the database of the MPA-JHU SDSS-DR7 galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31#1</TD>
            <TD>2012-12-28T08:53:43Z</TD>
            <TD>#AGN#Galaxies:spectra#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/201/31</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/201/31</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/201/31 [2]</TD>
            <TD>Emission-line galaxies from SDSS. I. (Ge+, 2012)</TD>
            <TD>For the goal of selecting pp-galaxies, we develop a series of automatic algorithms in light of Monte Carlo simulations. We apply the algorithms to SDSS galaxy spectra and get candidates from the pp-galaxies. Then we visually inspect the candidate spectra to establish the final sample. We start from the database of the MPA-JHU SDSS-DR7 galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31#2</TD>
            <TD>2012-12-28T08:53:43Z</TD>
            <TD>#AGN#Galaxies:spectra#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/201/31&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/201/31</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/201/31 [emgal]</TD>
            <TD>Emission-line galaxies from SDSS. I. (Ge+, 2012)</TD>
            <TD>For the goal of selecting pp-galaxies, we develop a series of automatic algorithms in light of Monte Carlo simulations. We apply the algorithms to SDSS galaxy spectra and get candidates from the pp-galaxies. Then we visually inspect the candidate spectra to establish the final sample. We start from the database of the MPA-JHU SDSS-DR7 galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31#emgal</TD>
            <TD>2012-12-28T08:53:43Z</TD>
            <TD>#AGN#Galaxies:spectra#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/201/31&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/201/31</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/416/62 [1]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#1</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/416/62</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/416/62 [2]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#2</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/416/62&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/62 [table7]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#table7</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/62 [tab3-5]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#tab3-5</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/1780 [1]</TD>
            <TD>GALEX/SDSS quasar catalog (Trammell+, 2007)</TD>
            <TD>We present an analysis of the broadband UV and optical properties of z~&lt;3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7". Most of the DR3 sample quasars are detected in the near-UV until z~1.7, with the near-UV detection fraction dropping to ~50% by z~2.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780#1</TD>
            <TD>2011-09-14T20:46:03Z</TD>
            <TD>#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/1780</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/1780</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/1780 [2]</TD>
            <TD>GALEX/SDSS quasar catalog (Trammell+, 2007)</TD>
            <TD>We present an analysis of the broadband UV and optical properties of z~&lt;3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7". Most of the DR3 sample quasars are detected in the near-UV until z~1.7, with the near-UV detection fraction dropping to ~50% by z~2.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780#2</TD>
            <TD>2011-09-14T20:46:03Z</TD>
            <TD>#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/1780&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/1780</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/1780 [table2]</TD>
            <TD>GALEX/SDSS quasar catalog (Trammell+, 2007)</TD>
            <TD>We present an analysis of the broadband UV and optical properties of z~&lt;3.4 quasars matched in the Galaxy Evolution Explorer (GALEX) General Data Release 1 (GR1) and the Sloan Digital Sky Survey (SDSS) Data Release 3 (DR3). Of the 6371 SDSS DR3 quasars covered by 204 GALEX GR1 tiles, 5380 (84%) have near-UV detections, while 3034 (48%) have both near-UV and far-UV detections using a matching radius of 7". Most of the DR3 sample quasars are detected in the near-UV until z~1.7, with the near-UV detection fraction dropping to ~50% by z~2.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780#table2</TD>
            <TD>2011-09-14T20:46:03Z</TD>
            <TD>#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/1780</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/1780&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/1780</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/416/62 [1]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#1</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/416/62</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/416/62 [2]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#2</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/416/62&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/62 [table7]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#table7</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/62 [tab3-5]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#tab3-5</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/201/31 [1]</TD>
            <TD>Emission-line galaxies from SDSS. I. (Ge+, 2012)</TD>
            <TD>For the goal of selecting pp-galaxies, we develop a series of automatic algorithms in light of Monte Carlo simulations. We apply the algorithms to SDSS galaxy spectra and get candidates from the pp-galaxies. Then we visually inspect the candidate spectra to establish the final sample. We start from the database of the MPA-JHU SDSS-DR7 galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31#1</TD>
            <TD>2012-12-28T08:53:43Z</TD>
            <TD>#AGN#Galaxies:spectra#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/201/31</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/201/31</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/201/31 [2]</TD>
            <TD>Emission-line galaxies from SDSS. I. (Ge+, 2012)</TD>
            <TD>For the goal of selecting pp-galaxies, we develop a series of automatic algorithms in light of Monte Carlo simulations. We apply the algorithms to SDSS galaxy spectra and get candidates from the pp-galaxies. Then we visually inspect the candidate spectra to establish the final sample. We start from the database of the MPA-JHU SDSS-DR7 galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31#2</TD>
            <TD>2012-12-28T08:53:43Z</TD>
            <TD>#AGN#Galaxies:spectra#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/201/31&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/201/31</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/201/31 [emgal]</TD>
            <TD>Emission-line galaxies from SDSS. I. (Ge+, 2012)</TD>
            <TD>For the goal of selecting pp-galaxies, we develop a series of automatic algorithms in light of Monte Carlo simulations. We apply the algorithms to SDSS galaxy spectra and get candidates from the pp-galaxies. Then we visually inspect the candidate spectra to establish the final sample. We start from the database of the MPA-JHU SDSS-DR7 galaxy sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31#emgal</TD>
            <TD>2012-12-28T08:53:43Z</TD>
            <TD>#AGN#Galaxies:spectra#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/201/31</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/201/31&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/201/31</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/293 [1]</TD>
            <TD>UV-Optical galaxy color-magnitude diagram I. (Wyder+, 2007)</TD>
            <TD>The UV data presented here are derived from the GALEX Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). The data set used in our analysis is taken from the union of the GALEX first data release (GR1) with the GALEX internal release IR1.1. The GALEX MIS catalogs were matched with the SDSS MPA/JHU DR4 value-added catalogs.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/293#1</TD>
            <TD>2011-09-14T20:46:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/293 [2]</TD>
            <TD>UV-Optical galaxy color-magnitude diagram I. (Wyder+, 2007)</TD>
            <TD>The UV data presented here are derived from the GALEX Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). The data set used in our analysis is taken from the union of the GALEX first data release (GR1) with the GALEX internal release IR1.1. The GALEX MIS catalogs were matched with the SDSS MPA/JHU DR4 value-added catalogs.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/293#2</TD>
            <TD>2011-09-14T20:46:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/293</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/416/62 [1]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#1</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/416/62</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/416/62 [2]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#2</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/416/62&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/62 [table7]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#table7</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/62 [tab3-5]</TD>
            <TD>Planetary nebulae as standard candles. IX. (McMillan+, 1993)</TD>
            <TD>We present the results of a planetary nebula (PN) survey of three galaxies in the Fornax Cluster performed with the Cerro Tololo 4m telescope and on-band off-band [O III] {lambda}5007 interference filters. In all, we detected 224 PN candidates : 105 in the peculiar SO/Sa galaxy NGC 1316 (Fornax A), 47 in the E2 galaxy NGC 1404, and 72 in the central cD of the cluster NGC 1399. Using statistically complete samples of planetaries and the procedures described in previous papers in the series, we derive distances to these galaxies from the planetary nebula luminosity function (PNLF).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62#tab3-5</TD>
            <TD>2012-09-24T07:24:47Z</TD>
            <TD>#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/62</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/62&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/62</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/406/1595 [1]</TD>
            <TD>Scalelength of 30000 SDSS disc galaxies (Fathi+, 2010)</TD>
            <TD>Disc scalelength (h) for 30000 galaxies from the Sloan Digitized Sky Survey (SDSS) Data Release 7, in the r-band. Also included is the Asymmetry parameter for each galaxy. Virtual Observatory methods and tools were used to define, retrieve and analyze the images for this unprecedentedly large sample classified as spiral galaxies in the LEDA catalogue. These parameters are also available for all other SDSS bands (u,g,i,z), and they can be retrieved from the Author. An extensive discussion about the errors involved in the derived parameters can be found in Fathi et al. (2010MNRAS.406.1595F) and Fathi (2010ApJ...722L.120F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595#1</TD>
            <TD>2012-12-18T14:03:55Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/406/1595</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1595</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/406/1595 [2]</TD>
            <TD>Scalelength of 30000 SDSS disc galaxies (Fathi+, 2010)</TD>
            <TD>Disc scalelength (h) for 30000 galaxies from the Sloan Digitized Sky Survey (SDSS) Data Release 7, in the r-band. Also included is the Asymmetry parameter for each galaxy. Virtual Observatory methods and tools were used to define, retrieve and analyze the images for this unprecedentedly large sample classified as spiral galaxies in the LEDA catalogue. These parameters are also available for all other SDSS bands (u,g,i,z), and they can be retrieved from the Author. An extensive discussion about the errors involved in the derived parameters can be found in Fathi et al. (2010MNRAS.406.1595F) and Fathi (2010ApJ...722L.120F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595#2</TD>
            <TD>2012-12-18T14:03:55Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/406/1595&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1595</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/406/1595 [sdssh]</TD>
            <TD>Scalelength of 30000 SDSS disc galaxies (Fathi+, 2010)</TD>
            <TD>Disc scalelength (h) for 30000 galaxies from the Sloan Digitized Sky Survey (SDSS) Data Release 7, in the r-band. Also included is the Asymmetry parameter for each galaxy. Virtual Observatory methods and tools were used to define, retrieve and analyze the images for this unprecedentedly large sample classified as spiral galaxies in the LEDA catalogue. These parameters are also available for all other SDSS bands (u,g,i,z), and they can be retrieved from the Author. An extensive discussion about the errors involved in the derived parameters can be found in Fathi et al. (2010MNRAS.406.1595F) and Fathi (2010ApJ...722L.120F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595#sdssh</TD>
            <TD>2012-12-18T14:03:55Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/406/1595&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1595</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2490 [1]</TD>
            <TD>RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002)</TD>
            <TD>With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12km/s) and metallicities (+/-0.26dex) for over 200 members of the M31 globular cluster population out to a radius of 1.5{deg} from the galaxy center. Many of these clusters have no previous published radial velocity or [Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490#1</TD>
            <TD>2012-09-24T08:34:41Z</TD>
            <TD>#Abundances#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/2490</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2490</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2490 [2]</TD>
            <TD>RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002)</TD>
            <TD>With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12km/s) and metallicities (+/-0.26dex) for over 200 members of the M31 globular cluster population out to a radius of 1.5{deg} from the galaxy center. Many of these clusters have no previous published radial velocity or [Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490#2</TD>
            <TD>2012-09-24T08:34:41Z</TD>
            <TD>#Abundances#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/2490&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2490</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2490 [table3]</TD>
            <TD>RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002)</TD>
            <TD>With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12km/s) and metallicities (+/-0.26dex) for over 200 members of the M31 globular cluster population out to a radius of 1.5{deg} from the galaxy center. Many of these clusters have no previous published radial velocity or [Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490#table3</TD>
            <TD>2012-09-24T08:34:41Z</TD>
            <TD>#Abundances#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2490&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2490</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/293 [1]</TD>
            <TD>UV-Optical galaxy color-magnitude diagram I. (Wyder+, 2007)</TD>
            <TD>The UV data presented here are derived from the GALEX Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). The data set used in our analysis is taken from the union of the GALEX first data release (GR1) with the GALEX internal release IR1.1. The GALEX MIS catalogs were matched with the SDSS MPA/JHU DR4 value-added catalogs.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/293#1</TD>
            <TD>2011-09-14T20:46:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/293 [2]</TD>
            <TD>UV-Optical galaxy color-magnitude diagram I. (Wyder+, 2007)</TD>
            <TD>The UV data presented here are derived from the GALEX Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). The data set used in our analysis is taken from the union of the GALEX first data release (GR1) with the GALEX internal release IR1.1. The GALEX MIS catalogs were matched with the SDSS MPA/JHU DR4 value-added catalogs.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/293#2</TD>
            <TD>2011-09-14T20:46:04Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/293</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/406/1595 [1]</TD>
            <TD>Scalelength of 30000 SDSS disc galaxies (Fathi+, 2010)</TD>
            <TD>Disc scalelength (h) for 30000 galaxies from the Sloan Digitized Sky Survey (SDSS) Data Release 7, in the r-band. Also included is the Asymmetry parameter for each galaxy. Virtual Observatory methods and tools were used to define, retrieve and analyze the images for this unprecedentedly large sample classified as spiral galaxies in the LEDA catalogue. These parameters are also available for all other SDSS bands (u,g,i,z), and they can be retrieved from the Author. An extensive discussion about the errors involved in the derived parameters can be found in Fathi et al. (2010MNRAS.406.1595F) and Fathi (2010ApJ...722L.120F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595#1</TD>
            <TD>2012-12-18T14:03:55Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/406/1595</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1595</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/406/1595 [2]</TD>
            <TD>Scalelength of 30000 SDSS disc galaxies (Fathi+, 2010)</TD>
            <TD>Disc scalelength (h) for 30000 galaxies from the Sloan Digitized Sky Survey (SDSS) Data Release 7, in the r-band. Also included is the Asymmetry parameter for each galaxy. Virtual Observatory methods and tools were used to define, retrieve and analyze the images for this unprecedentedly large sample classified as spiral galaxies in the LEDA catalogue. These parameters are also available for all other SDSS bands (u,g,i,z), and they can be retrieved from the Author. An extensive discussion about the errors involved in the derived parameters can be found in Fathi et al. (2010MNRAS.406.1595F) and Fathi (2010ApJ...722L.120F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595#2</TD>
            <TD>2012-12-18T14:03:55Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/406/1595&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1595</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/406/1595 [sdssh]</TD>
            <TD>Scalelength of 30000 SDSS disc galaxies (Fathi+, 2010)</TD>
            <TD>Disc scalelength (h) for 30000 galaxies from the Sloan Digitized Sky Survey (SDSS) Data Release 7, in the r-band. Also included is the Asymmetry parameter for each galaxy. Virtual Observatory methods and tools were used to define, retrieve and analyze the images for this unprecedentedly large sample classified as spiral galaxies in the LEDA catalogue. These parameters are also available for all other SDSS bands (u,g,i,z), and they can be retrieved from the Author. An extensive discussion about the errors involved in the derived parameters can be found in Fathi et al. (2010MNRAS.406.1595F) and Fathi (2010ApJ...722L.120F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595#sdssh</TD>
            <TD>2012-12-18T14:03:55Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/406/1595&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1595</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2490 [1]</TD>
            <TD>RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002)</TD>
            <TD>With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12km/s) and metallicities (+/-0.26dex) for over 200 members of the M31 globular cluster population out to a radius of 1.5{deg} from the galaxy center. Many of these clusters have no previous published radial velocity or [Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490#1</TD>
            <TD>2012-09-24T08:34:41Z</TD>
            <TD>#Abundances#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/2490</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2490</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2490 [2]</TD>
            <TD>RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002)</TD>
            <TD>With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12km/s) and metallicities (+/-0.26dex) for over 200 members of the M31 globular cluster population out to a radius of 1.5{deg} from the galaxy center. Many of these clusters have no previous published radial velocity or [Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490#2</TD>
            <TD>2012-09-24T08:34:41Z</TD>
            <TD>#Abundances#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/2490&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2490</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2490 [table3]</TD>
            <TD>RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002)</TD>
            <TD>With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12km/s) and metallicities (+/-0.26dex) for over 200 members of the M31 globular cluster population out to a radius of 1.5{deg} from the galaxy center. Many of these clusters have no previous published radial velocity or [Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490#table3</TD>
            <TD>2012-09-24T08:34:41Z</TD>
            <TD>#Abundances#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2490&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2490</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/594 [1]</TD>
            <TD>Araucaria project: Cepheids in WLM galaxy (Pietrzynski+, 2007)</TD>
            <TD>All the data presented in this paper were collected with the Warsaw 1.3m telescope at Las Campanas Observatory. The V images of WLM were secured on 101 different nights between 2001 December and 2003 December. In addition, 24 I-band images were collected in 2003.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594#1</TD>
            <TD>2011-09-14T20:47:41Z</TD>
            <TD>#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/594</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/594</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/594 [2]</TD>
            <TD>Araucaria project: Cepheids in WLM galaxy (Pietrzynski+, 2007)</TD>
            <TD>All the data presented in this paper were collected with the Warsaw 1.3m telescope at Las Campanas Observatory. The V images of WLM were secured on 101 different nights between 2001 December and 2003 December. In addition, 24 I-band images were collected in 2003.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594#2</TD>
            <TD>2011-09-14T20:47:41Z</TD>
            <TD>#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/594&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/594</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/594 [table1]</TD>
            <TD>Araucaria project: Cepheids in WLM galaxy (Pietrzynski+, 2007)</TD>
            <TD>All the data presented in this paper were collected with the Warsaw 1.3m telescope at Las Campanas Observatory. The V images of WLM were secured on 101 different nights between 2001 December and 2003 December. In addition, 24 I-band images were collected in 2003.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594#table1</TD>
            <TD>2011-09-14T20:47:41Z</TD>
            <TD>#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/594&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/594</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/406/1595 [1]</TD>
            <TD>Scalelength of 30000 SDSS disc galaxies (Fathi+, 2010)</TD>
            <TD>Disc scalelength (h) for 30000 galaxies from the Sloan Digitized Sky Survey (SDSS) Data Release 7, in the r-band. Also included is the Asymmetry parameter for each galaxy. Virtual Observatory methods and tools were used to define, retrieve and analyze the images for this unprecedentedly large sample classified as spiral galaxies in the LEDA catalogue. These parameters are also available for all other SDSS bands (u,g,i,z), and they can be retrieved from the Author. An extensive discussion about the errors involved in the derived parameters can be found in Fathi et al. (2010MNRAS.406.1595F) and Fathi (2010ApJ...722L.120F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595#1</TD>
            <TD>2012-12-18T14:03:55Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/406/1595</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1595</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/406/1595 [2]</TD>
            <TD>Scalelength of 30000 SDSS disc galaxies (Fathi+, 2010)</TD>
            <TD>Disc scalelength (h) for 30000 galaxies from the Sloan Digitized Sky Survey (SDSS) Data Release 7, in the r-band. Also included is the Asymmetry parameter for each galaxy. Virtual Observatory methods and tools were used to define, retrieve and analyze the images for this unprecedentedly large sample classified as spiral galaxies in the LEDA catalogue. These parameters are also available for all other SDSS bands (u,g,i,z), and they can be retrieved from the Author. An extensive discussion about the errors involved in the derived parameters can be found in Fathi et al. (2010MNRAS.406.1595F) and Fathi (2010ApJ...722L.120F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595#2</TD>
            <TD>2012-12-18T14:03:55Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/406/1595&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1595</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/406/1595 [sdssh]</TD>
            <TD>Scalelength of 30000 SDSS disc galaxies (Fathi+, 2010)</TD>
            <TD>Disc scalelength (h) for 30000 galaxies from the Sloan Digitized Sky Survey (SDSS) Data Release 7, in the r-band. Also included is the Asymmetry parameter for each galaxy. Virtual Observatory methods and tools were used to define, retrieve and analyze the images for this unprecedentedly large sample classified as spiral galaxies in the LEDA catalogue. These parameters are also available for all other SDSS bands (u,g,i,z), and they can be retrieved from the Author. An extensive discussion about the errors involved in the derived parameters can be found in Fathi et al. (2010MNRAS.406.1595F) and Fathi (2010ApJ...722L.120F)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595#sdssh</TD>
            <TD>2012-12-18T14:03:55Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/406/1595</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/406/1595&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/406/1595</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2490 [1]</TD>
            <TD>RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002)</TD>
            <TD>With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12km/s) and metallicities (+/-0.26dex) for over 200 members of the M31 globular cluster population out to a radius of 1.5{deg} from the galaxy center. Many of these clusters have no previous published radial velocity or [Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490#1</TD>
            <TD>2012-09-24T08:34:41Z</TD>
            <TD>#Abundances#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/2490</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2490</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2490 [2]</TD>
            <TD>RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002)</TD>
            <TD>With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12km/s) and metallicities (+/-0.26dex) for over 200 members of the M31 globular cluster population out to a radius of 1.5{deg} from the galaxy center. Many of these clusters have no previous published radial velocity or [Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490#2</TD>
            <TD>2012-09-24T08:34:41Z</TD>
            <TD>#Abundances#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/2490&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2490</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2490 [table3]</TD>
            <TD>RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002)</TD>
            <TD>With the ultimate aim of distinguishing between various models describing the formation of galaxy halos (e.g., radial or multiphase collapse and random mergers), we have completed a spectroscopic study of the globular cluster system of M31. We present the results of deep intermediate-resolution fiber-optic spectroscopy of several hundred of the M31 globular clusters using the Wide Field Fibre Optic Spectrograph at the William Herschel Telescope in La Palma, Canary Islands. These observations have yielded precise radial velocities (+/-12km/s) and metallicities (+/-0.26dex) for over 200 members of the M31 globular cluster population out to a radius of 1.5{deg} from the galaxy center. Many of these clusters have no previous published radial velocity or [Fe/H] estimates, and the remainder typically represent significant improvements over earlier determinations. We present analyses of the spatial, kinematic, and metal abundance properties of the M31 globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490#table3</TD>
            <TD>2012-09-24T08:34:41Z</TD>
            <TD>#Abundances#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2490</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>J/ApJ/378/65 [1]</TD>
            <TD>8.4GHz observations of compact starbursts (Condon+ 1991)</TD>
            <TD>The 40 ultraluminous (log(LFIR/L_{sun}_&gt;=11.25) galaxies in the IRAS Bright Galaxy Sample of sources stronger than S=5.24Jy at {lambda}=60{mu}m were mapped with approximately 0.25-arcsec resolution at 8.44GHz. Twenty-five contain diffuse radio sources obeying the FIR-radio correlation; these are almost certainly starburst galaxies. Fourteen other galaxies have nearly blackbody FIR spectra with color temperatures between 60 and 80K so their (unmeasured) FIR angular sizes must exceed approximately 0.25-arcsec, yet they contain compact (but usually resolved) radio sources smaller than this limit. The unique radio and FIR properties of these galaxies can be modeled by ultraluminous nuclear starbursts so dense that they are optically thick to free-free absorption at {nu}~1.49GHz and dust absorption at {lambda}~25{mu}m. Only one galaxy (UGC 08058 = Mrk 231) is a dominated by a variable radio source too compact to be an ultraluminous starburst; it must be powered by a 'monster'.</TD>
            <TD>CDS</TD>
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            <TD>J/ApJ/378/65 [2]</TD>
            <TD>8.4GHz observations of compact starbursts (Condon+ 1991)</TD>
            <TD>The 40 ultraluminous (log(LFIR/L_{sun}_&gt;=11.25) galaxies in the IRAS Bright Galaxy Sample of sources stronger than S=5.24Jy at {lambda}=60{mu}m were mapped with approximately 0.25-arcsec resolution at 8.44GHz. Twenty-five contain diffuse radio sources obeying the FIR-radio correlation; these are almost certainly starburst galaxies. Fourteen other galaxies have nearly blackbody FIR spectra with color temperatures between 60 and 80K so their (unmeasured) FIR angular sizes must exceed approximately 0.25-arcsec, yet they contain compact (but usually resolved) radio sources smaller than this limit. The unique radio and FIR properties of these galaxies can be modeled by ultraluminous nuclear starbursts so dense that they are optically thick to free-free absorption at {nu}~1.49GHz and dust absorption at {lambda}~25{mu}m. Only one galaxy (UGC 08058 = Mrk 231) is a dominated by a variable radio source too compact to be an ultraluminous starburst; it must be powered by a 'monster'.</TD>
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            <TD>8.4GHz observations of compact starbursts (Condon+ 1991)</TD>
            <TD>The 40 ultraluminous (log(LFIR/L_{sun}_&gt;=11.25) galaxies in the IRAS Bright Galaxy Sample of sources stronger than S=5.24Jy at {lambda}=60{mu}m were mapped with approximately 0.25-arcsec resolution at 8.44GHz. Twenty-five contain diffuse radio sources obeying the FIR-radio correlation; these are almost certainly starburst galaxies. Fourteen other galaxies have nearly blackbody FIR spectra with color temperatures between 60 and 80K so their (unmeasured) FIR angular sizes must exceed approximately 0.25-arcsec, yet they contain compact (but usually resolved) radio sources smaller than this limit. The unique radio and FIR properties of these galaxies can be modeled by ultraluminous nuclear starbursts so dense that they are optically thick to free-free absorption at {nu}~1.49GHz and dust absorption at {lambda}~25{mu}m. Only one galaxy (UGC 08058 = Mrk 231) is a dominated by a variable radio source too compact to be an ultraluminous starburst; it must be powered by a 'monster'.</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/378/65 [1]</TD>
            <TD>8.4GHz observations of compact starbursts (Condon+ 1991)</TD>
            <TD>The 40 ultraluminous (log(LFIR/L_{sun}_&gt;=11.25) galaxies in the IRAS Bright Galaxy Sample of sources stronger than S=5.24Jy at {lambda}=60{mu}m were mapped with approximately 0.25-arcsec resolution at 8.44GHz. Twenty-five contain diffuse radio sources obeying the FIR-radio correlation; these are almost certainly starburst galaxies. Fourteen other galaxies have nearly blackbody FIR spectra with color temperatures between 60 and 80K so their (unmeasured) FIR angular sizes must exceed approximately 0.25-arcsec, yet they contain compact (but usually resolved) radio sources smaller than this limit. The unique radio and FIR properties of these galaxies can be modeled by ultraluminous nuclear starbursts so dense that they are optically thick to free-free absorption at {nu}~1.49GHz and dust absorption at {lambda}~25{mu}m. Only one galaxy (UGC 08058 = Mrk 231) is a dominated by a variable radio source too compact to be an ultraluminous starburst; it must be powered by a 'monster'.</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJ/378/65 [2]</TD>
            <TD>8.4GHz observations of compact starbursts (Condon+ 1991)</TD>
            <TD>The 40 ultraluminous (log(LFIR/L_{sun}_&gt;=11.25) galaxies in the IRAS Bright Galaxy Sample of sources stronger than S=5.24Jy at {lambda}=60{mu}m were mapped with approximately 0.25-arcsec resolution at 8.44GHz. Twenty-five contain diffuse radio sources obeying the FIR-radio correlation; these are almost certainly starburst galaxies. Fourteen other galaxies have nearly blackbody FIR spectra with color temperatures between 60 and 80K so their (unmeasured) FIR angular sizes must exceed approximately 0.25-arcsec, yet they contain compact (but usually resolved) radio sources smaller than this limit. The unique radio and FIR properties of these galaxies can be modeled by ultraluminous nuclear starbursts so dense that they are optically thick to free-free absorption at {nu}~1.49GHz and dust absorption at {lambda}~25{mu}m. Only one galaxy (UGC 08058 = Mrk 231) is a dominated by a variable radio source too compact to be an ultraluminous starburst; it must be powered by a 'monster'.</TD>
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            <TD>J/ApJ/378/65 [table2]</TD>
            <TD>8.4GHz observations of compact starbursts (Condon+ 1991)</TD>
            <TD>The 40 ultraluminous (log(LFIR/L_{sun}_&gt;=11.25) galaxies in the IRAS Bright Galaxy Sample of sources stronger than S=5.24Jy at {lambda}=60{mu}m were mapped with approximately 0.25-arcsec resolution at 8.44GHz. Twenty-five contain diffuse radio sources obeying the FIR-radio correlation; these are almost certainly starburst galaxies. Fourteen other galaxies have nearly blackbody FIR spectra with color temperatures between 60 and 80K so their (unmeasured) FIR angular sizes must exceed approximately 0.25-arcsec, yet they contain compact (but usually resolved) radio sources smaller than this limit. The unique radio and FIR properties of these galaxies can be modeled by ultraluminous nuclear starbursts so dense that they are optically thick to free-free absorption at {nu}~1.49GHz and dust absorption at {lambda}~25{mu}m. Only one galaxy (UGC 08058 = Mrk 231) is a dominated by a variable radio source too compact to be an ultraluminous starburst; it must be powered by a 'monster'.</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/113/950 [1]</TD>
            <TD>Kinematic Profiles of S0 Galaxies (Fisher 1997)</TD>
            <TD>Stellar rotation curves, velocity dispersion profiles, and line of sight velocity distributions (LOSVD) as derived from absorption-lines are presented for the major axes of 18 S0 and two elliptical galaxies. Ionized gas rotation curves and dispersions were measured from the [OIII] 5007A emission line in the 9 S0 galaxies displaying this feature. Minor-axis results are given for 14 of the S0 galaxies and one of the ellipticals. A wide range of behaviors are observed in the rotation and velocity dispersion profiles. These variations could be the result of the superposition of stars and gas belonging to the disks and bulges as well as the possible influences of bars, nuclear disks, and warps. Deviations from a Gaussian LOSVD are found along the major axes of all the galaxies in our sample. As parametrised by the Gauss-Hermite series of orthogonal functions, asymmetric deviations are always found in the inner regions of the S0 galaxies such that the prograde wing of the LOSVD is steeper than the retrograde wing. This is similar to the behavior observed in elliptical galaxies. However, at larger radii these asymmetries can change their sign. We find that in 9 of the 18 S0 galaxies a high-speed tail to the LOSVD develops along the major-axis beyond the central regions. In 3 of these 9 objects the LOSVD asymmetries display a second change of sign with radius such that a low-speed tail is again present and persists to our last measured values. No correlations were found between the sizes of the stellar velocity dispersion gradients and either central velocity dispersion, absolute magnitude, disk-to-bulge ratio, Mg2 or Fe line strength gradients. For the objects in our sample with edge-on orientations a comparison between the minor-axis 'bulge' velocity dispersion gradients and those found in elliptical galaxies indicates that the S0 bulges display, on average, logarithmic gradients approximately 4 times steeper than those found in normal luminous ellipticals. A number of galaxies show particularly interesting features. For the LINER S0 galaxy NGC 3998 we find that the velocity dispersion profiles of both the stars and gas rise sharply towards the center reaching nuclear values of sigma~320km/s. Nuclear disks of rapidly rotating gas are found in NGC 4350 and NGC 4762. A nuclear stellar disk is apparent in the edge-on galaxy NGC 4111 and an extended disk of counterrotating gas is observed in the barred S0 NGC 3941.</TD>
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            <TD>HTTP Request</TD>
            <TD>J/AJ/113/950 [2]</TD>
            <TD>Kinematic Profiles of S0 Galaxies (Fisher 1997)</TD>
            <TD>Stellar rotation curves, velocity dispersion profiles, and line of sight velocity distributions (LOSVD) as derived from absorption-lines are presented for the major axes of 18 S0 and two elliptical galaxies. Ionized gas rotation curves and dispersions were measured from the [OIII] 5007A emission line in the 9 S0 galaxies displaying this feature. Minor-axis results are given for 14 of the S0 galaxies and one of the ellipticals. A wide range of behaviors are observed in the rotation and velocity dispersion profiles. These variations could be the result of the superposition of stars and gas belonging to the disks and bulges as well as the possible influences of bars, nuclear disks, and warps. Deviations from a Gaussian LOSVD are found along the major axes of all the galaxies in our sample. As parametrised by the Gauss-Hermite series of orthogonal functions, asymmetric deviations are always found in the inner regions of the S0 galaxies such that the prograde wing of the LOSVD is steeper than the retrograde wing. This is similar to the behavior observed in elliptical galaxies. However, at larger radii these asymmetries can change their sign. We find that in 9 of the 18 S0 galaxies a high-speed tail to the LOSVD develops along the major-axis beyond the central regions. In 3 of these 9 objects the LOSVD asymmetries display a second change of sign with radius such that a low-speed tail is again present and persists to our last measured values. No correlations were found between the sizes of the stellar velocity dispersion gradients and either central velocity dispersion, absolute magnitude, disk-to-bulge ratio, Mg2 or Fe line strength gradients. For the objects in our sample with edge-on orientations a comparison between the minor-axis 'bulge' velocity dispersion gradients and those found in elliptical galaxies indicates that the S0 bulges display, on average, logarithmic gradients approximately 4 times steeper than those found in normal luminous ellipticals. A number of galaxies show particularly interesting features. For the LINER S0 galaxy NGC 3998 we find that the velocity dispersion profiles of both the stars and gas rise sharply towards the center reaching nuclear values of sigma~320km/s. Nuclear disks of rapidly rotating gas are found in NGC 4350 and NGC 4762. A nuclear stellar disk is apparent in the edge-on galaxy NGC 4111 and an extended disk of counterrotating gas is observed in the barred S0 NGC 3941.</TD>
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            <TD>J/ApJ/378/65 [1]</TD>
            <TD>8.4GHz observations of compact starbursts (Condon+ 1991)</TD>
            <TD>The 40 ultraluminous (log(LFIR/L_{sun}_&gt;=11.25) galaxies in the IRAS Bright Galaxy Sample of sources stronger than S=5.24Jy at {lambda}=60{mu}m were mapped with approximately 0.25-arcsec resolution at 8.44GHz. Twenty-five contain diffuse radio sources obeying the FIR-radio correlation; these are almost certainly starburst galaxies. Fourteen other galaxies have nearly blackbody FIR spectra with color temperatures between 60 and 80K so their (unmeasured) FIR angular sizes must exceed approximately 0.25-arcsec, yet they contain compact (but usually resolved) radio sources smaller than this limit. The unique radio and FIR properties of these galaxies can be modeled by ultraluminous nuclear starbursts so dense that they are optically thick to free-free absorption at {nu}~1.49GHz and dust absorption at {lambda}~25{mu}m. Only one galaxy (UGC 08058 = Mrk 231) is a dominated by a variable radio source too compact to be an ultraluminous starburst; it must be powered by a 'monster'.</TD>
            <TD>CDS</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJ/378/65 [2]</TD>
            <TD>8.4GHz observations of compact starbursts (Condon+ 1991)</TD>
            <TD>The 40 ultraluminous (log(LFIR/L_{sun}_&gt;=11.25) galaxies in the IRAS Bright Galaxy Sample of sources stronger than S=5.24Jy at {lambda}=60{mu}m were mapped with approximately 0.25-arcsec resolution at 8.44GHz. Twenty-five contain diffuse radio sources obeying the FIR-radio correlation; these are almost certainly starburst galaxies. Fourteen other galaxies have nearly blackbody FIR spectra with color temperatures between 60 and 80K so their (unmeasured) FIR angular sizes must exceed approximately 0.25-arcsec, yet they contain compact (but usually resolved) radio sources smaller than this limit. The unique radio and FIR properties of these galaxies can be modeled by ultraluminous nuclear starbursts so dense that they are optically thick to free-free absorption at {nu}~1.49GHz and dust absorption at {lambda}~25{mu}m. Only one galaxy (UGC 08058 = Mrk 231) is a dominated by a variable radio source too compact to be an ultraluminous starburst; it must be powered by a 'monster'.</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJ/378/65 [table2]</TD>
            <TD>8.4GHz observations of compact starbursts (Condon+ 1991)</TD>
            <TD>The 40 ultraluminous (log(LFIR/L_{sun}_&gt;=11.25) galaxies in the IRAS Bright Galaxy Sample of sources stronger than S=5.24Jy at {lambda}=60{mu}m were mapped with approximately 0.25-arcsec resolution at 8.44GHz. Twenty-five contain diffuse radio sources obeying the FIR-radio correlation; these are almost certainly starburst galaxies. Fourteen other galaxies have nearly blackbody FIR spectra with color temperatures between 60 and 80K so their (unmeasured) FIR angular sizes must exceed approximately 0.25-arcsec, yet they contain compact (but usually resolved) radio sources smaller than this limit. The unique radio and FIR properties of these galaxies can be modeled by ultraluminous nuclear starbursts so dense that they are optically thick to free-free absorption at {nu}~1.49GHz and dust absorption at {lambda}~25{mu}m. Only one galaxy (UGC 08058 = Mrk 231) is a dominated by a variable radio source too compact to be an ultraluminous starburst; it must be powered by a 'monster'.</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/113/950 [1]</TD>
            <TD>Kinematic Profiles of S0 Galaxies (Fisher 1997)</TD>
            <TD>Stellar rotation curves, velocity dispersion profiles, and line of sight velocity distributions (LOSVD) as derived from absorption-lines are presented for the major axes of 18 S0 and two elliptical galaxies. Ionized gas rotation curves and dispersions were measured from the [OIII] 5007A emission line in the 9 S0 galaxies displaying this feature. Minor-axis results are given for 14 of the S0 galaxies and one of the ellipticals. A wide range of behaviors are observed in the rotation and velocity dispersion profiles. These variations could be the result of the superposition of stars and gas belonging to the disks and bulges as well as the possible influences of bars, nuclear disks, and warps. Deviations from a Gaussian LOSVD are found along the major axes of all the galaxies in our sample. As parametrised by the Gauss-Hermite series of orthogonal functions, asymmetric deviations are always found in the inner regions of the S0 galaxies such that the prograde wing of the LOSVD is steeper than the retrograde wing. This is similar to the behavior observed in elliptical galaxies. However, at larger radii these asymmetries can change their sign. We find that in 9 of the 18 S0 galaxies a high-speed tail to the LOSVD develops along the major-axis beyond the central regions. In 3 of these 9 objects the LOSVD asymmetries display a second change of sign with radius such that a low-speed tail is again present and persists to our last measured values. No correlations were found between the sizes of the stellar velocity dispersion gradients and either central velocity dispersion, absolute magnitude, disk-to-bulge ratio, Mg2 or Fe line strength gradients. For the objects in our sample with edge-on orientations a comparison between the minor-axis 'bulge' velocity dispersion gradients and those found in elliptical galaxies indicates that the S0 bulges display, on average, logarithmic gradients approximately 4 times steeper than those found in normal luminous ellipticals. A number of galaxies show particularly interesting features. For the LINER S0 galaxy NGC 3998 we find that the velocity dispersion profiles of both the stars and gas rise sharply towards the center reaching nuclear values of sigma~320km/s. Nuclear disks of rapidly rotating gas are found in NGC 4350 and NGC 4762. A nuclear stellar disk is apparent in the edge-on galaxy NGC 4111 and an extended disk of counterrotating gas is observed in the barred S0 NGC 3941.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/950#1</TD>
            <TD>2011-09-14T18:22:42Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/950</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/113/950</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/950</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/113/950 [2]</TD>
            <TD>Kinematic Profiles of S0 Galaxies (Fisher 1997)</TD>
            <TD>Stellar rotation curves, velocity dispersion profiles, and line of sight velocity distributions (LOSVD) as derived from absorption-lines are presented for the major axes of 18 S0 and two elliptical galaxies. Ionized gas rotation curves and dispersions were measured from the [OIII] 5007A emission line in the 9 S0 galaxies displaying this feature. Minor-axis results are given for 14 of the S0 galaxies and one of the ellipticals. A wide range of behaviors are observed in the rotation and velocity dispersion profiles. These variations could be the result of the superposition of stars and gas belonging to the disks and bulges as well as the possible influences of bars, nuclear disks, and warps. Deviations from a Gaussian LOSVD are found along the major axes of all the galaxies in our sample. As parametrised by the Gauss-Hermite series of orthogonal functions, asymmetric deviations are always found in the inner regions of the S0 galaxies such that the prograde wing of the LOSVD is steeper than the retrograde wing. This is similar to the behavior observed in elliptical galaxies. However, at larger radii these asymmetries can change their sign. We find that in 9 of the 18 S0 galaxies a high-speed tail to the LOSVD develops along the major-axis beyond the central regions. In 3 of these 9 objects the LOSVD asymmetries display a second change of sign with radius such that a low-speed tail is again present and persists to our last measured values. No correlations were found between the sizes of the stellar velocity dispersion gradients and either central velocity dispersion, absolute magnitude, disk-to-bulge ratio, Mg2 or Fe line strength gradients. For the objects in our sample with edge-on orientations a comparison between the minor-axis 'bulge' velocity dispersion gradients and those found in elliptical galaxies indicates that the S0 bulges display, on average, logarithmic gradients approximately 4 times steeper than those found in normal luminous ellipticals. A number of galaxies show particularly interesting features. For the LINER S0 galaxy NGC 3998 we find that the velocity dispersion profiles of both the stars and gas rise sharply towards the center reaching nuclear values of sigma~320km/s. Nuclear disks of rapidly rotating gas are found in NGC 4350 and NGC 4762. A nuclear stellar disk is apparent in the edge-on galaxy NGC 4111 and an extended disk of counterrotating gas is observed in the barred S0 NGC 3941.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/950#2</TD>
            <TD>2011-09-14T18:22:42Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/113/950</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/113/950&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/113/950</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/548/A52 [1]</TD>
            <TD>Molecular cloud formation in M 33 (Braine+, 2012)</TD>
            <TD>The amount of H_2_ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1-0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52#1</TD>
            <TD>2012-11-21T15:03:41Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/548/A52</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A52</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/548/A52 [2]</TD>
            <TD>Molecular cloud formation in M 33 (Braine+, 2012)</TD>
            <TD>The amount of H_2_ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1-0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52#2</TD>
            <TD>2012-11-21T15:03:41Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/548/A52&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A52</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A52 [list]</TD>
            <TD>Molecular cloud formation in M 33 (Braine+, 2012)</TD>
            <TD>The amount of H_2_ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1-0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52#list</TD>
            <TD>2012-11-21T15:03:41Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A52&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A52</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/416/36 [1]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#1</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/416/36</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/416/36 [2]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#2</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/416/36&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/36 [table1a]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#table1a</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/36 [table1]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#table1</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/548/A52 [1]</TD>
            <TD>Molecular cloud formation in M 33 (Braine+, 2012)</TD>
            <TD>The amount of H_2_ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1-0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52#1</TD>
            <TD>2012-11-21T15:03:41Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/548/A52</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A52</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/548/A52 [2]</TD>
            <TD>Molecular cloud formation in M 33 (Braine+, 2012)</TD>
            <TD>The amount of H_2_ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1-0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52#2</TD>
            <TD>2012-11-21T15:03:41Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/548/A52&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A52</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A52 [list]</TD>
            <TD>Molecular cloud formation in M 33 (Braine+, 2012)</TD>
            <TD>The amount of H_2_ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1-0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52#list</TD>
            <TD>2012-11-21T15:03:41Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A52&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A52</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/594 [1]</TD>
            <TD>Araucaria project: Cepheids in WLM galaxy (Pietrzynski+, 2007)</TD>
            <TD>All the data presented in this paper were collected with the Warsaw 1.3m telescope at Las Campanas Observatory. The V images of WLM were secured on 101 different nights between 2001 December and 2003 December. In addition, 24 I-band images were collected in 2003.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594#1</TD>
            <TD>2011-09-14T20:47:41Z</TD>
            <TD>#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/594</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/594</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/594 [2]</TD>
            <TD>Araucaria project: Cepheids in WLM galaxy (Pietrzynski+, 2007)</TD>
            <TD>All the data presented in this paper were collected with the Warsaw 1.3m telescope at Las Campanas Observatory. The V images of WLM were secured on 101 different nights between 2001 December and 2003 December. In addition, 24 I-band images were collected in 2003.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594#2</TD>
            <TD>2011-09-14T20:47:41Z</TD>
            <TD>#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/594&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/594</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/594 [table1]</TD>
            <TD>Araucaria project: Cepheids in WLM galaxy (Pietrzynski+, 2007)</TD>
            <TD>All the data presented in this paper were collected with the Warsaw 1.3m telescope at Las Campanas Observatory. The V images of WLM were secured on 101 different nights between 2001 December and 2003 December. In addition, 24 I-band images were collected in 2003.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594#table1</TD>
            <TD>2011-09-14T20:47:41Z</TD>
            <TD>#Galaxies#Stars:variable#</TD>
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            <TD>#Research#</TD>
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            <TD>14-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/594&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/594</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/416/36 [1]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#1</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/416/36</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/416/36 [2]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#2</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/416/36&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/36 [table1a]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#table1a</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/36 [table1]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#table1</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/416/36 [1]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#1</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/416/36</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/416/36 [2]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#2</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/416/36&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/36 [table1a]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#table1a</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/416/36 [table1]</TD>
            <TD>Dynamics of the Galaxy Cluster Abell 2634 (Pinkney+ 1993)</TD>
            <TD>All velocities are heliocentric and in km/s. vz1 are reliable velocities (based on the cross-correlation peak) while vz2 are velocities which may be based on the wrong CCF peak altogether. The dividing line between C1 and C2 was taken to be a Tonry and Davis "r" value of the cross-correlation function of 3.5. The velocity errors for vz1 were calculated using a best-fit solution of error vs Tonry and Davis "r" value. This curve was calibrated using redundant observations. The vz2 and unmeasured velocities have a 300 km/s error. This is conservative IF the correct CCF peak was chosen. This file includes 512 objects identified after Batuskis initial search, plus some of Batuskis which didn't seem to match any of the 512 (these have 4-digit ids). Four are from the literature and also did not seem to match the author's positions. They are labeled, S, Z, or L.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36#table1</TD>
            <TD>2011-09-14T18:23:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1994-07-18</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/416/36</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/416/36&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/416/36</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/548/A52 [1]</TD>
            <TD>Molecular cloud formation in M 33 (Braine+, 2012)</TD>
            <TD>The amount of H_2_ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1-0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52#1</TD>
            <TD>2012-11-21T15:03:41Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/548/A52</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A52</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/548/A52 [2]</TD>
            <TD>Molecular cloud formation in M 33 (Braine+, 2012)</TD>
            <TD>The amount of H_2_ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1-0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52#2</TD>
            <TD>2012-11-21T15:03:41Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/548/A52&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A52</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/548/A52 [list]</TD>
            <TD>Molecular cloud formation in M 33 (Braine+, 2012)</TD>
            <TD>The amount of H_2_ present in spiral galaxies remains uncertain, particularly in the dim outer regions and in low-metallicity environments. We present high-resolution CO(1-0) observations with the Plateau de Bure interferometer of the most distant molecular cloud in the local group galaxy M33. The cloud is a single entity rather than a set of smaller clouds within the broad beam of the original single-dish observations. The interferometer and single-dish fluxes are very similar and the line widths are indistinguishable, despite the difference in beamsize.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52#list</TD>
            <TD>2012-11-21T15:03:41Z</TD>
            <TD>#Galaxies#Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/548/A52</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/548/A52&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/548/A52</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/28 [1]</TD>
            <TD>VLT Lyman-break galaxy redshift survey. II. (Crighton+, 2011)</TD>
            <TD>We obtained galaxy spectra for this project using the VIMOS multi-object spectrograph on the VLT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28#1</TD>
            <TD>2012-12-20T15:39:52Z</TD>
            <TD>#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/28 [2]</TD>
            <TD>VLT Lyman-break galaxy redshift survey. II. (Crighton+, 2011)</TD>
            <TD>We obtained galaxy spectra for this project using the VIMOS multi-object spectrograph on the VLT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28#2</TD>
            <TD>2012-12-20T15:39:52Z</TD>
            <TD>#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/28 [tablec1]</TD>
            <TD>VLT Lyman-break galaxy redshift survey. II. (Crighton+, 2011)</TD>
            <TD>We obtained galaxy spectra for this project using the VIMOS multi-object spectrograph on the VLT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28#tablec1</TD>
            <TD>2012-12-20T15:39:52Z</TD>
            <TD>#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/594 [1]</TD>
            <TD>Araucaria project: Cepheids in WLM galaxy (Pietrzynski+, 2007)</TD>
            <TD>All the data presented in this paper were collected with the Warsaw 1.3m telescope at Las Campanas Observatory. The V images of WLM were secured on 101 different nights between 2001 December and 2003 December. In addition, 24 I-band images were collected in 2003.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594#1</TD>
            <TD>2011-09-14T20:47:41Z</TD>
            <TD>#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/594</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/594</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/594 [2]</TD>
            <TD>Araucaria project: Cepheids in WLM galaxy (Pietrzynski+, 2007)</TD>
            <TD>All the data presented in this paper were collected with the Warsaw 1.3m telescope at Las Campanas Observatory. The V images of WLM were secured on 101 different nights between 2001 December and 2003 December. In addition, 24 I-band images were collected in 2003.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594#2</TD>
            <TD>2011-09-14T20:47:41Z</TD>
            <TD>#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/594&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/594</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/594 [table1]</TD>
            <TD>Araucaria project: Cepheids in WLM galaxy (Pietrzynski+, 2007)</TD>
            <TD>All the data presented in this paper were collected with the Warsaw 1.3m telescope at Las Campanas Observatory. The V images of WLM were secured on 101 different nights between 2001 December and 2003 December. In addition, 24 I-band images were collected in 2003.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594#table1</TD>
            <TD>2011-09-14T20:47:41Z</TD>
            <TD>#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/594</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/594&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/594</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/197 [1]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#1</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/197</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/197 [2]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#2</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/197&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/197 [galaxies]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#galaxies</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/197 [table3]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#table3</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/28 [1]</TD>
            <TD>VLT Lyman-break galaxy redshift survey. II. (Crighton+, 2011)</TD>
            <TD>We obtained galaxy spectra for this project using the VIMOS multi-object spectrograph on the VLT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28#1</TD>
            <TD>2012-12-20T15:39:52Z</TD>
            <TD>#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/28 [2]</TD>
            <TD>VLT Lyman-break galaxy redshift survey. II. (Crighton+, 2011)</TD>
            <TD>We obtained galaxy spectra for this project using the VIMOS multi-object spectrograph on the VLT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28#2</TD>
            <TD>2012-12-20T15:39:52Z</TD>
            <TD>#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/28 [tablec1]</TD>
            <TD>VLT Lyman-break galaxy redshift survey. II. (Crighton+, 2011)</TD>
            <TD>We obtained galaxy spectra for this project using the VIMOS multi-object spectrograph on the VLT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28#tablec1</TD>
            <TD>2012-12-20T15:39:52Z</TD>
            <TD>#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/392/19 [1]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#1</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/392/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/392/19 [2]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#2</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/392/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/19 [tablea1]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#tablea1</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/19 [2slaqqso]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#2slaqqso</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/197 [1]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#1</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/197</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/197 [2]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#2</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/197&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/197 [galaxies]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#galaxies</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/197 [table3]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#table3</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/28 [1]</TD>
            <TD>VLT Lyman-break galaxy redshift survey. II. (Crighton+, 2011)</TD>
            <TD>We obtained galaxy spectra for this project using the VIMOS multi-object spectrograph on the VLT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28#1</TD>
            <TD>2012-12-20T15:39:52Z</TD>
            <TD>#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/28 [2]</TD>
            <TD>VLT Lyman-break galaxy redshift survey. II. (Crighton+, 2011)</TD>
            <TD>We obtained galaxy spectra for this project using the VIMOS multi-object spectrograph on the VLT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28#2</TD>
            <TD>2012-12-20T15:39:52Z</TD>
            <TD>#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/28 [tablec1]</TD>
            <TD>VLT Lyman-break galaxy redshift survey. II. (Crighton+, 2011)</TD>
            <TD>We obtained galaxy spectra for this project using the VIMOS multi-object spectrograph on the VLT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28#tablec1</TD>
            <TD>2012-12-20T15:39:52Z</TD>
            <TD>#Equivalent_widths#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/392/19 [1]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#1</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/392/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/392/19 [2]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#2</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/392/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/19 [tablea1]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#tablea1</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/19 [2slaqqso]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#2slaqqso</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/197 [1]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#1</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/197</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/197 [2]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#2</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/197&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/197 [galaxies]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#galaxies</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/197 [table3]</TD>
            <TD>Close pairs of galaxies (Woods+, 2006)</TD>
            <TD>We study star formation in a sample of 345 galaxies in 167 pairs and compact groups drawn from the original CfA2 Redshift Survey and from a follow-up search for companions. We construct our sample with attention to including pairs with luminosity contrast |{Delta}m_R_|&gt;=2. These 57 galaxies with |{Delta}m_R_|&gt;=2 provide a set of nearby representative cases of minor interactions, a central feature of the hierarchical galaxy formation model. Here we report the redshifts and positions of the 345 galaxies in our sample and of 136 galaxies in apparent pairs that are superpositions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197#table3</TD>
            <TD>2012-12-21T13:02:08Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/197</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/31/563 [1]</TD>
            <TD>HI observations of flat galaxies (Mitronova+, 2005)</TD>
            <TD>Results of HI observations with the 100-m Effelsberg radio telescope are presented for 94 edge-on spiral galaxies from the Revised Flat Galaxy Catalog (Karachentsev et al., 1999, Cat. &lt;VII/219&gt;) and 14 galaxies from the 2MASS-selected Flat Galaxy Catalog (Mitronova et al., 2004, Bull. Spec. Astron. Obs. Russ. Acad. Sci. 57, 5). The HI line fluxes, heliocentric radial velocities and the HI line widths are given for 65 detected galaxies. Their HI profiles are shown as a mosaic. We calculated some global parameters of the galaxies and discuss linear correlations between them. Total (indicative) mass-to-luminosity ratio for the sample galaxies is ranked within 0.4-8.2 with the mean value 3.8 (M_{sun}_/L_{sun}_), and the mean fraction of hydrogen mass is 0.13. For 43 undetected objects their rms noise is also given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563#1</TD>
            <TD>2011-09-14T19:44:01Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/31/563</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/31/563</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/31/563 [2]</TD>
            <TD>HI observations of flat galaxies (Mitronova+, 2005)</TD>
            <TD>Results of HI observations with the 100-m Effelsberg radio telescope are presented for 94 edge-on spiral galaxies from the Revised Flat Galaxy Catalog (Karachentsev et al., 1999, Cat. &lt;VII/219&gt;) and 14 galaxies from the 2MASS-selected Flat Galaxy Catalog (Mitronova et al., 2004, Bull. Spec. Astron. Obs. Russ. Acad. Sci. 57, 5). The HI line fluxes, heliocentric radial velocities and the HI line widths are given for 65 detected galaxies. Their HI profiles are shown as a mosaic. We calculated some global parameters of the galaxies and discuss linear correlations between them. Total (indicative) mass-to-luminosity ratio for the sample galaxies is ranked within 0.4-8.2 with the mean value 3.8 (M_{sun}_/L_{sun}_), and the mean fraction of hydrogen mass is 0.13. For 43 undetected objects their rms noise is also given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563#2</TD>
            <TD>2011-09-14T19:44:01Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/31/563&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/31/563</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/392/19 [1]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#1</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/392/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/392/19 [2]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#2</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/392/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/19 [tablea1]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#tablea1</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/392/19 [2slaqqso]</TD>
            <TD>The 2dF-SDSS QSO survey (Croom+, 2009)</TD>
            <TD>We present the final spectroscopic QSO catalogue from the 2dF-SDSS LRG (luminous red galaxy) and QSO (2SLAQ) survey. This is a deep, 18&lt;g&lt;21.85 (extinction corrected), sample aimed at probing in detail the faint end of the broad line active galactic nuclei luminosity distribution at z&lt;=2.6. The candidate QSOs were selected from SDSS photometry and observed spectroscopically with the 2dF spectrograph on the Anglo-Australian Telescope. This sample covers an area of 191.9 deg2 and contains new spectra of 16326 objects, of which 8764 are QSOs and 7623 are newly discovered [the remainder were previously identified by the 2dF QSO Redshift Survey (2QZ) and SDSS]. The full QSO sample (including objects previously observed in the SDSS and 2QZ surveys) contains 12702 QSOs. The new 2SLAQ spectroscopic data set also contains 2343 Galactic stars, including 362 white dwarfs, and 2924 narrow emission-line galaxies with a median redshift of z=0.22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19#2slaqqso</TD>
            <TD>2011-09-14T20:48:57Z</TD>
            <TD>#Photometry:wide-band#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/392/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/392/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/392/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/442/165 [1]</TD>
            <TD>IJKs photometry of late-type stars in Draco dSph (Cioni+, 2005)</TD>
            <TD>Photometry of 2570 stars detected in IJKs covering the Draco dwarf Local Group galaxy is presented. For each stars equatorial coordinates, magnitudes and errors are given as well as source extraction flags.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165#1</TD>
            <TD>2011-09-14T19:43:47Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/442/165</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/165</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/442/165 [2]</TD>
            <TD>IJKs photometry of late-type stars in Draco dSph (Cioni+, 2005)</TD>
            <TD>Photometry of 2570 stars detected in IJKs covering the Draco dwarf Local Group galaxy is presented. For each stars equatorial coordinates, magnitudes and errors are given as well as source extraction flags.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165#2</TD>
            <TD>2011-09-14T19:43:47Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/442/165&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/165</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/31/563 [1]</TD>
            <TD>HI observations of flat galaxies (Mitronova+, 2005)</TD>
            <TD>Results of HI observations with the 100-m Effelsberg radio telescope are presented for 94 edge-on spiral galaxies from the Revised Flat Galaxy Catalog (Karachentsev et al., 1999, Cat. &lt;VII/219&gt;) and 14 galaxies from the 2MASS-selected Flat Galaxy Catalog (Mitronova et al., 2004, Bull. Spec. Astron. Obs. Russ. Acad. Sci. 57, 5). The HI line fluxes, heliocentric radial velocities and the HI line widths are given for 65 detected galaxies. Their HI profiles are shown as a mosaic. We calculated some global parameters of the galaxies and discuss linear correlations between them. Total (indicative) mass-to-luminosity ratio for the sample galaxies is ranked within 0.4-8.2 with the mean value 3.8 (M_{sun}_/L_{sun}_), and the mean fraction of hydrogen mass is 0.13. For 43 undetected objects their rms noise is also given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563#1</TD>
            <TD>2011-09-14T19:44:01Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/31/563</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/31/563</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/31/563 [2]</TD>
            <TD>HI observations of flat galaxies (Mitronova+, 2005)</TD>
            <TD>Results of HI observations with the 100-m Effelsberg radio telescope are presented for 94 edge-on spiral galaxies from the Revised Flat Galaxy Catalog (Karachentsev et al., 1999, Cat. &lt;VII/219&gt;) and 14 galaxies from the 2MASS-selected Flat Galaxy Catalog (Mitronova et al., 2004, Bull. Spec. Astron. Obs. Russ. Acad. Sci. 57, 5). The HI line fluxes, heliocentric radial velocities and the HI line widths are given for 65 detected galaxies. Their HI profiles are shown as a mosaic. We calculated some global parameters of the galaxies and discuss linear correlations between them. Total (indicative) mass-to-luminosity ratio for the sample galaxies is ranked within 0.4-8.2 with the mean value 3.8 (M_{sun}_/L_{sun}_), and the mean fraction of hydrogen mass is 0.13. For 43 undetected objects their rms noise is also given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563#2</TD>
            <TD>2011-09-14T19:44:01Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/31/563&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/31/563</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/389/1074 [1]</TD>
            <TD>LX-{sigma} relation of galaxy clusters (Shen+, 2008)</TD>
            <TD>We use the RASS to study the X-ray properties of our sample of groups and clusters. The RASS mapped the sky in the soft X-ray band (0.1-2.4keV) with exposure time varying between 400 and 40000s, depending on direction on the sky. The resolution of the RASS images is 45 arcsec.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074#1</TD>
            <TD>2011-09-14T20:48:58Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/389/1074</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1074</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/389/1074 [2]</TD>
            <TD>LX-{sigma} relation of galaxy clusters (Shen+, 2008)</TD>
            <TD>We use the RASS to study the X-ray properties of our sample of groups and clusters. The RASS mapped the sky in the soft X-ray band (0.1-2.4keV) with exposure time varying between 400 and 40000s, depending on direction on the sky. The resolution of the RASS images is 45 arcsec.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074#2</TD>
            <TD>2011-09-14T20:48:58Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/389/1074&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1074</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1074 [tablea1]</TD>
            <TD>LX-{sigma} relation of galaxy clusters (Shen+, 2008)</TD>
            <TD>We use the RASS to study the X-ray properties of our sample of groups and clusters. The RASS mapped the sky in the soft X-ray band (0.1-2.4keV) with exposure time varying between 400 and 40000s, depending on direction on the sky. The resolution of the RASS images is 45 arcsec.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074#tablea1</TD>
            <TD>2011-09-14T20:48:58Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1074&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1074</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/442/165 [1]</TD>
            <TD>IJKs photometry of late-type stars in Draco dSph (Cioni+, 2005)</TD>
            <TD>Photometry of 2570 stars detected in IJKs covering the Draco dwarf Local Group galaxy is presented. For each stars equatorial coordinates, magnitudes and errors are given as well as source extraction flags.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165#1</TD>
            <TD>2011-09-14T19:43:47Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/442/165</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/165</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/442/165 [2]</TD>
            <TD>IJKs photometry of late-type stars in Draco dSph (Cioni+, 2005)</TD>
            <TD>Photometry of 2570 stars detected in IJKs covering the Draco dwarf Local Group galaxy is presented. For each stars equatorial coordinates, magnitudes and errors are given as well as source extraction flags.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165#2</TD>
            <TD>2011-09-14T19:43:47Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/442/165&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/165</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/31/563 [1]</TD>
            <TD>HI observations of flat galaxies (Mitronova+, 2005)</TD>
            <TD>Results of HI observations with the 100-m Effelsberg radio telescope are presented for 94 edge-on spiral galaxies from the Revised Flat Galaxy Catalog (Karachentsev et al., 1999, Cat. &lt;VII/219&gt;) and 14 galaxies from the 2MASS-selected Flat Galaxy Catalog (Mitronova et al., 2004, Bull. Spec. Astron. Obs. Russ. Acad. Sci. 57, 5). The HI line fluxes, heliocentric radial velocities and the HI line widths are given for 65 detected galaxies. Their HI profiles are shown as a mosaic. We calculated some global parameters of the galaxies and discuss linear correlations between them. Total (indicative) mass-to-luminosity ratio for the sample galaxies is ranked within 0.4-8.2 with the mean value 3.8 (M_{sun}_/L_{sun}_), and the mean fraction of hydrogen mass is 0.13. For 43 undetected objects their rms noise is also given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563#1</TD>
            <TD>2011-09-14T19:44:01Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/31/563</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/31/563</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/31/563 [2]</TD>
            <TD>HI observations of flat galaxies (Mitronova+, 2005)</TD>
            <TD>Results of HI observations with the 100-m Effelsberg radio telescope are presented for 94 edge-on spiral galaxies from the Revised Flat Galaxy Catalog (Karachentsev et al., 1999, Cat. &lt;VII/219&gt;) and 14 galaxies from the 2MASS-selected Flat Galaxy Catalog (Mitronova et al., 2004, Bull. Spec. Astron. Obs. Russ. Acad. Sci. 57, 5). The HI line fluxes, heliocentric radial velocities and the HI line widths are given for 65 detected galaxies. Their HI profiles are shown as a mosaic. We calculated some global parameters of the galaxies and discuss linear correlations between them. Total (indicative) mass-to-luminosity ratio for the sample galaxies is ranked within 0.4-8.2 with the mean value 3.8 (M_{sun}_/L_{sun}_), and the mean fraction of hydrogen mass is 0.13. For 43 undetected objects their rms noise is also given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563#2</TD>
            <TD>2011-09-14T19:44:01Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/31/563</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/31/563&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/31/563</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/442/165 [1]</TD>
            <TD>IJKs photometry of late-type stars in Draco dSph (Cioni+, 2005)</TD>
            <TD>Photometry of 2570 stars detected in IJKs covering the Draco dwarf Local Group galaxy is presented. For each stars equatorial coordinates, magnitudes and errors are given as well as source extraction flags.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165#1</TD>
            <TD>2011-09-14T19:43:47Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/442/165</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/165</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/442/165 [2]</TD>
            <TD>IJKs photometry of late-type stars in Draco dSph (Cioni+, 2005)</TD>
            <TD>Photometry of 2570 stars detected in IJKs covering the Draco dwarf Local Group galaxy is presented. For each stars equatorial coordinates, magnitudes and errors are given as well as source extraction flags.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165#2</TD>
            <TD>2011-09-14T19:43:47Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/165</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/442/165&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/165</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/389/1074 [1]</TD>
            <TD>LX-{sigma} relation of galaxy clusters (Shen+, 2008)</TD>
            <TD>We use the RASS to study the X-ray properties of our sample of groups and clusters. The RASS mapped the sky in the soft X-ray band (0.1-2.4keV) with exposure time varying between 400 and 40000s, depending on direction on the sky. The resolution of the RASS images is 45 arcsec.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074#1</TD>
            <TD>2011-09-14T20:48:58Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/389/1074</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1074</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/389/1074 [2]</TD>
            <TD>LX-{sigma} relation of galaxy clusters (Shen+, 2008)</TD>
            <TD>We use the RASS to study the X-ray properties of our sample of groups and clusters. The RASS mapped the sky in the soft X-ray band (0.1-2.4keV) with exposure time varying between 400 and 40000s, depending on direction on the sky. The resolution of the RASS images is 45 arcsec.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074#2</TD>
            <TD>2011-09-14T20:48:58Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/389/1074&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1074</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1074 [tablea1]</TD>
            <TD>LX-{sigma} relation of galaxy clusters (Shen+, 2008)</TD>
            <TD>We use the RASS to study the X-ray properties of our sample of groups and clusters. The RASS mapped the sky in the soft X-ray band (0.1-2.4keV) with exposure time varying between 400 and 40000s, depending on direction on the sky. The resolution of the RASS images is 45 arcsec.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074#tablea1</TD>
            <TD>2011-09-14T20:48:58Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1074&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1074</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/1237 [1]</TD>
            <TD>SARS galaxy luminosity profiles (Coenda+, 2005)</TD>
            <TD>We have analyzed CCD images of 14 Abell clusters in the R filter of the Southern Abell Clusters Redshifts Survey (SARS) with cz&lt;40,000km/s. We have obtained the luminosity profiles for 507 galaxies, of which 232 (46%) have known redshifts. In order to fit the luminosity profiles, we used the de Vaucouleurs law for bulge systems and an exponential profile for disk systems, and we also fitted the Sersic's law (r^n^) to all galaxy profiles.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237#1</TD>
            <TD>2011-09-14T19:44:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/1237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/1237 [2]</TD>
            <TD>SARS galaxy luminosity profiles (Coenda+, 2005)</TD>
            <TD>We have analyzed CCD images of 14 Abell clusters in the R filter of the Southern Abell Clusters Redshifts Survey (SARS) with cz&lt;40,000km/s. We have obtained the luminosity profiles for 507 galaxies, of which 232 (46%) have known redshifts. In order to fit the luminosity profiles, we used the de Vaucouleurs law for bulge systems and an exponential profile for disk systems, and we also fitted the Sersic's law (r^n^) to all galaxy profiles.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237#2</TD>
            <TD>2011-09-14T19:44:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/1237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/1237 [1]</TD>
            <TD>SARS galaxy luminosity profiles (Coenda+, 2005)</TD>
            <TD>We have analyzed CCD images of 14 Abell clusters in the R filter of the Southern Abell Clusters Redshifts Survey (SARS) with cz&lt;40,000km/s. We have obtained the luminosity profiles for 507 galaxies, of which 232 (46%) have known redshifts. In order to fit the luminosity profiles, we used the de Vaucouleurs law for bulge systems and an exponential profile for disk systems, and we also fitted the Sersic's law (r^n^) to all galaxy profiles.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237#1</TD>
            <TD>2011-09-14T19:44:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/1237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/1237 [2]</TD>
            <TD>SARS galaxy luminosity profiles (Coenda+, 2005)</TD>
            <TD>We have analyzed CCD images of 14 Abell clusters in the R filter of the Southern Abell Clusters Redshifts Survey (SARS) with cz&lt;40,000km/s. We have obtained the luminosity profiles for 507 galaxies, of which 232 (46%) have known redshifts. In order to fit the luminosity profiles, we used the de Vaucouleurs law for bulge systems and an exponential profile for disk systems, and we also fitted the Sersic's law (r^n^) to all galaxy profiles.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237#2</TD>
            <TD>2011-09-14T19:44:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/1237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/389/1074 [1]</TD>
            <TD>LX-{sigma} relation of galaxy clusters (Shen+, 2008)</TD>
            <TD>We use the RASS to study the X-ray properties of our sample of groups and clusters. The RASS mapped the sky in the soft X-ray band (0.1-2.4keV) with exposure time varying between 400 and 40000s, depending on direction on the sky. The resolution of the RASS images is 45 arcsec.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074#1</TD>
            <TD>2011-09-14T20:48:58Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/389/1074</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1074</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/389/1074 [2]</TD>
            <TD>LX-{sigma} relation of galaxy clusters (Shen+, 2008)</TD>
            <TD>We use the RASS to study the X-ray properties of our sample of groups and clusters. The RASS mapped the sky in the soft X-ray band (0.1-2.4keV) with exposure time varying between 400 and 40000s, depending on direction on the sky. The resolution of the RASS images is 45 arcsec.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074#2</TD>
            <TD>2011-09-14T20:48:58Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/389/1074&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1074</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/389/1074 [tablea1]</TD>
            <TD>LX-{sigma} relation of galaxy clusters (Shen+, 2008)</TD>
            <TD>We use the RASS to study the X-ray properties of our sample of groups and clusters. The RASS mapped the sky in the soft X-ray band (0.1-2.4keV) with exposure time varying between 400 and 40000s, depending on direction on the sky. The resolution of the RASS images is 45 arcsec.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074#tablea1</TD>
            <TD>2011-09-14T20:48:58Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/389/1074</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/389/1074&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/389/1074</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/1237 [1]</TD>
            <TD>SARS galaxy luminosity profiles (Coenda+, 2005)</TD>
            <TD>We have analyzed CCD images of 14 Abell clusters in the R filter of the Southern Abell Clusters Redshifts Survey (SARS) with cz&lt;40,000km/s. We have obtained the luminosity profiles for 507 galaxies, of which 232 (46%) have known redshifts. In order to fit the luminosity profiles, we used the de Vaucouleurs law for bulge systems and an exponential profile for disk systems, and we also fitted the Sersic's law (r^n^) to all galaxy profiles.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237#1</TD>
            <TD>2011-09-14T19:44:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/1237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/1237 [2]</TD>
            <TD>SARS galaxy luminosity profiles (Coenda+, 2005)</TD>
            <TD>We have analyzed CCD images of 14 Abell clusters in the R filter of the Southern Abell Clusters Redshifts Survey (SARS) with cz&lt;40,000km/s. We have obtained the luminosity profiles for 507 galaxies, of which 232 (46%) have known redshifts. In order to fit the luminosity profiles, we used the de Vaucouleurs law for bulge systems and an exponential profile for disk systems, and we also fitted the Sersic's law (r^n^) to all galaxy profiles.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237#2</TD>
            <TD>2011-09-14T19:44:09Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/1237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/1237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/1237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/2329 [1]</TD>
            <TD>Spectroscopy of hot stars in the halo. III (Wilhelm+, 1999)</TD>
            <TD>We present results from an analysis of medium-resolution spectroscopy and UBV photometry for a sample of 1121 A-type stars in the halo (and disk) of the Galaxy. A previously developed calibration technique is used to assign estimates of effective temperature, surface gravity, and stellar metal abundance, as parametrized by [Fe/H]. Radial velocities are reported with an accuracy of {~}10 km.s^-1^. Distance estimates are obtained for the stars with well-determined luminosity classes. Note that although we refer to "A-type" stars, which dominate the present sample, the present data set includes roughly 100 stars of later spectral types, as a result of the temperature range we have chosen to explore in this paper (6000 K {&lt;=} T_eff_ {&lt;=} 10,000 K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329#1</TD>
            <TD>2011-09-14T19:45:07Z</TD>
            <TD>#Abundances#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/2329</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2329</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/2329 [2]</TD>
            <TD>Spectroscopy of hot stars in the halo. III (Wilhelm+, 1999)</TD>
            <TD>We present results from an analysis of medium-resolution spectroscopy and UBV photometry for a sample of 1121 A-type stars in the halo (and disk) of the Galaxy. A previously developed calibration technique is used to assign estimates of effective temperature, surface gravity, and stellar metal abundance, as parametrized by [Fe/H]. Radial velocities are reported with an accuracy of {~}10 km.s^-1^. Distance estimates are obtained for the stars with well-determined luminosity classes. Note that although we refer to "A-type" stars, which dominate the present sample, the present data set includes roughly 100 stars of later spectral types, as a result of the temperature range we have chosen to explore in this paper (6000 K {&lt;=} T_eff_ {&lt;=} 10,000 K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/117/2329</TD>
            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/2329&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2329</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/2329 [1]</TD>
            <TD>Spectroscopy of hot stars in the halo. III (Wilhelm+, 1999)</TD>
            <TD>We present results from an analysis of medium-resolution spectroscopy and UBV photometry for a sample of 1121 A-type stars in the halo (and disk) of the Galaxy. A previously developed calibration technique is used to assign estimates of effective temperature, surface gravity, and stellar metal abundance, as parametrized by [Fe/H]. Radial velocities are reported with an accuracy of {~}10 km.s^-1^. Distance estimates are obtained for the stars with well-determined luminosity classes. Note that although we refer to "A-type" stars, which dominate the present sample, the present data set includes roughly 100 stars of later spectral types, as a result of the temperature range we have chosen to explore in this paper (6000 K {&lt;=} T_eff_ {&lt;=} 10,000 K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329#1</TD>
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            <TD>25-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/2329</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2329</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/2329 [2]</TD>
            <TD>Spectroscopy of hot stars in the halo. III (Wilhelm+, 1999)</TD>
            <TD>We present results from an analysis of medium-resolution spectroscopy and UBV photometry for a sample of 1121 A-type stars in the halo (and disk) of the Galaxy. A previously developed calibration technique is used to assign estimates of effective temperature, surface gravity, and stellar metal abundance, as parametrized by [Fe/H]. Radial velocities are reported with an accuracy of {~}10 km.s^-1^. Distance estimates are obtained for the stars with well-determined luminosity classes. Note that although we refer to "A-type" stars, which dominate the present sample, the present data set includes roughly 100 stars of later spectral types, as a result of the temperature range we have chosen to explore in this paper (6000 K {&lt;=} T_eff_ {&lt;=} 10,000 K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329#2</TD>
            <TD>2011-09-14T19:45:07Z</TD>
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            <TD>25-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/2329&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2329</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/2329 [1]</TD>
            <TD>Spectroscopy of hot stars in the halo. III (Wilhelm+, 1999)</TD>
            <TD>We present results from an analysis of medium-resolution spectroscopy and UBV photometry for a sample of 1121 A-type stars in the halo (and disk) of the Galaxy. A previously developed calibration technique is used to assign estimates of effective temperature, surface gravity, and stellar metal abundance, as parametrized by [Fe/H]. Radial velocities are reported with an accuracy of {~}10 km.s^-1^. Distance estimates are obtained for the stars with well-determined luminosity classes. Note that although we refer to "A-type" stars, which dominate the present sample, the present data set includes roughly 100 stars of later spectral types, as a result of the temperature range we have chosen to explore in this paper (6000 K {&lt;=} T_eff_ {&lt;=} 10,000 K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329#1</TD>
            <TD>2011-09-14T19:45:07Z</TD>
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            <TD>25-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/2329</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2329</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/2329 [2]</TD>
            <TD>Spectroscopy of hot stars in the halo. III (Wilhelm+, 1999)</TD>
            <TD>We present results from an analysis of medium-resolution spectroscopy and UBV photometry for a sample of 1121 A-type stars in the halo (and disk) of the Galaxy. A previously developed calibration technique is used to assign estimates of effective temperature, surface gravity, and stellar metal abundance, as parametrized by [Fe/H]. Radial velocities are reported with an accuracy of {~}10 km.s^-1^. Distance estimates are obtained for the stars with well-determined luminosity classes. Note that although we refer to "A-type" stars, which dominate the present sample, the present data set includes roughly 100 stars of later spectral types, as a result of the temperature range we have chosen to explore in this paper (6000 K {&lt;=} T_eff_ {&lt;=} 10,000 K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329#2</TD>
            <TD>2011-09-14T19:45:07Z</TD>
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            <TD>25-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2329</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/2329&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2329</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/181/233 [1]</TD>
            <TD>Catalog of merging galaxies (Hwang+, 2009)</TD>
            <TD>In this supplement, we present a catalog and images of morphologically identified merging galaxies in Red Sequence Cluster Survey 2 (RCS2) (Yee et al., 2007ASPC..379..103Y). RCS2 is a large sky survey using the Canada-France-Hawaii Telescope (CFHT) to look for galaxy clusters out to z~1.</TD>
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            <TD>ivo://CDS.VizieR/J/ApJS/181/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/181/233</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/181/233</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/181/233 [2]</TD>
            <TD>Catalog of merging galaxies (Hwang+, 2009)</TD>
            <TD>In this supplement, we present a catalog and images of morphologically identified merging galaxies in Red Sequence Cluster Survey 2 (RCS2) (Yee et al., 2007ASPC..379..103Y). RCS2 is a large sky survey using the Canada-France-Hawaii Telescope (CFHT) to look for galaxy clusters out to z~1.</TD>
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            <TD>ivo://CDS.VizieR/J/ApJS/181/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/181/233&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/181/233</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/181/233 [table1]</TD>
            <TD>Catalog of merging galaxies (Hwang+, 2009)</TD>
            <TD>In this supplement, we present a catalog and images of morphologically identified merging galaxies in Red Sequence Cluster Survey 2 (RCS2) (Yee et al., 2007ASPC..379..103Y). RCS2 is a large sky survey using the Canada-France-Hawaii Telescope (CFHT) to look for galaxy clusters out to z~1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233#table1</TD>
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            <TD>26-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/181/233&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/181/233</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/16 [1]</TD>
            <TD>HIPASS Bright Galaxy Catalog (Koribalski+, 2004)</TD>
            <TD>We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 HI brightest galaxies in the southern sky as obtained from the HI Parkes All-Sky Survey (HIPASS, Cat. &lt;VIII/73&gt;). The selection of the brightest sources is based on their HI peak flux density (S_peak_&gt;~116mJy) as measured from the spatially integrated HIPASS spectrum. The derived HI masses range from ~10^7^ to 4x10^10^M_Sun_. While the BGC (z&lt;0.03) is complete in S_peak_, only a subset of ~500 sources can be considered complete in integrated HI flux density (F_HI_&gt;~25Jy.km/s). The HIPASS BGC contains a total of 158 new redshifts. These belong to 91 new sources for which no optical or infrared counterparts have previously been catalogued, an additional 51 galaxies for which no redshifts were previously known, and 16 galaxies for which the catalogued optical velocities disagree.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
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            <TD>11-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/16</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/16</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/16 [2]</TD>
            <TD>HIPASS Bright Galaxy Catalog (Koribalski+, 2004)</TD>
            <TD>We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 HI brightest galaxies in the southern sky as obtained from the HI Parkes All-Sky Survey (HIPASS, Cat. &lt;VIII/73&gt;). The selection of the brightest sources is based on their HI peak flux density (S_peak_&gt;~116mJy) as measured from the spatially integrated HIPASS spectrum. The derived HI masses range from ~10^7^ to 4x10^10^M_Sun_. While the BGC (z&lt;0.03) is complete in S_peak_, only a subset of ~500 sources can be considered complete in integrated HI flux density (F_HI_&gt;~25Jy.km/s). The HIPASS BGC contains a total of 158 new redshifts. These belong to 91 new sources for which no optical or infrared counterparts have previously been catalogued, an additional 51 galaxies for which no redshifts were previously known, and 16 galaxies for which the catalogued optical velocities disagree.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
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            <TD>11-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/16&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/16</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/181/233 [1]</TD>
            <TD>Catalog of merging galaxies (Hwang+, 2009)</TD>
            <TD>In this supplement, we present a catalog and images of morphologically identified merging galaxies in Red Sequence Cluster Survey 2 (RCS2) (Yee et al., 2007ASPC..379..103Y). RCS2 is a large sky survey using the Canada-France-Hawaii Telescope (CFHT) to look for galaxy clusters out to z~1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>26-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/181/233</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/181/233</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/181/233 [2]</TD>
            <TD>Catalog of merging galaxies (Hwang+, 2009)</TD>
            <TD>In this supplement, we present a catalog and images of morphologically identified merging galaxies in Red Sequence Cluster Survey 2 (RCS2) (Yee et al., 2007ASPC..379..103Y). RCS2 is a large sky survey using the Canada-France-Hawaii Telescope (CFHT) to look for galaxy clusters out to z~1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233#2</TD>
            <TD>2011-09-14T20:48:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>26-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/181/233&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/181/233</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/181/233 [table1]</TD>
            <TD>Catalog of merging galaxies (Hwang+, 2009)</TD>
            <TD>In this supplement, we present a catalog and images of morphologically identified merging galaxies in Red Sequence Cluster Survey 2 (RCS2) (Yee et al., 2007ASPC..379..103Y). RCS2 is a large sky survey using the Canada-France-Hawaii Telescope (CFHT) to look for galaxy clusters out to z~1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233#table1</TD>
            <TD>2011-09-14T20:48:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/181/233&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/181/233</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/16 [1]</TD>
            <TD>HIPASS Bright Galaxy Catalog (Koribalski+, 2004)</TD>
            <TD>We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 HI brightest galaxies in the southern sky as obtained from the HI Parkes All-Sky Survey (HIPASS, Cat. &lt;VIII/73&gt;). The selection of the brightest sources is based on their HI peak flux density (S_peak_&gt;~116mJy) as measured from the spatially integrated HIPASS spectrum. The derived HI masses range from ~10^7^ to 4x10^10^M_Sun_. While the BGC (z&lt;0.03) is complete in S_peak_, only a subset of ~500 sources can be considered complete in integrated HI flux density (F_HI_&gt;~25Jy.km/s). The HIPASS BGC contains a total of 158 new redshifts. These belong to 91 new sources for which no optical or infrared counterparts have previously been catalogued, an additional 51 galaxies for which no redshifts were previously known, and 16 galaxies for which the catalogued optical velocities disagree.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16#1</TD>
            <TD>2011-09-14T19:45:31Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/16</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/16</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/16 [2]</TD>
            <TD>HIPASS Bright Galaxy Catalog (Koribalski+, 2004)</TD>
            <TD>We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 HI brightest galaxies in the southern sky as obtained from the HI Parkes All-Sky Survey (HIPASS, Cat. &lt;VIII/73&gt;). The selection of the brightest sources is based on their HI peak flux density (S_peak_&gt;~116mJy) as measured from the spatially integrated HIPASS spectrum. The derived HI masses range from ~10^7^ to 4x10^10^M_Sun_. While the BGC (z&lt;0.03) is complete in S_peak_, only a subset of ~500 sources can be considered complete in integrated HI flux density (F_HI_&gt;~25Jy.km/s). The HIPASS BGC contains a total of 158 new redshifts. These belong to 91 new sources for which no optical or infrared counterparts have previously been catalogued, an additional 51 galaxies for which no redshifts were previously known, and 16 galaxies for which the catalogued optical velocities disagree.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16#2</TD>
            <TD>2011-09-14T19:45:31Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/16&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/16</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/16 [1]</TD>
            <TD>HIPASS Bright Galaxy Catalog (Koribalski+, 2004)</TD>
            <TD>We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 HI brightest galaxies in the southern sky as obtained from the HI Parkes All-Sky Survey (HIPASS, Cat. &lt;VIII/73&gt;). The selection of the brightest sources is based on their HI peak flux density (S_peak_&gt;~116mJy) as measured from the spatially integrated HIPASS spectrum. The derived HI masses range from ~10^7^ to 4x10^10^M_Sun_. While the BGC (z&lt;0.03) is complete in S_peak_, only a subset of ~500 sources can be considered complete in integrated HI flux density (F_HI_&gt;~25Jy.km/s). The HIPASS BGC contains a total of 158 new redshifts. These belong to 91 new sources for which no optical or infrared counterparts have previously been catalogued, an additional 51 galaxies for which no redshifts were previously known, and 16 galaxies for which the catalogued optical velocities disagree.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16#1</TD>
            <TD>2011-09-14T19:45:31Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/16</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/16</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/16 [2]</TD>
            <TD>HIPASS Bright Galaxy Catalog (Koribalski+, 2004)</TD>
            <TD>We present the HIPASS Bright Galaxy Catalog (BGC), which contains the 1000 HI brightest galaxies in the southern sky as obtained from the HI Parkes All-Sky Survey (HIPASS, Cat. &lt;VIII/73&gt;). The selection of the brightest sources is based on their HI peak flux density (S_peak_&gt;~116mJy) as measured from the spatially integrated HIPASS spectrum. The derived HI masses range from ~10^7^ to 4x10^10^M_Sun_. While the BGC (z&lt;0.03) is complete in S_peak_, only a subset of ~500 sources can be considered complete in integrated HI flux density (F_HI_&gt;~25Jy.km/s). The HIPASS BGC contains a total of 158 new redshifts. These belong to 91 new sources for which no optical or infrared counterparts have previously been catalogued, an additional 51 galaxies for which no redshifts were previously known, and 16 galaxies for which the catalogued optical velocities disagree.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16#2</TD>
            <TD>2011-09-14T19:45:31Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/16</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/16&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/16</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/181/233 [1]</TD>
            <TD>Catalog of merging galaxies (Hwang+, 2009)</TD>
            <TD>In this supplement, we present a catalog and images of morphologically identified merging galaxies in Red Sequence Cluster Survey 2 (RCS2) (Yee et al., 2007ASPC..379..103Y). RCS2 is a large sky survey using the Canada-France-Hawaii Telescope (CFHT) to look for galaxy clusters out to z~1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233#1</TD>
            <TD>2011-09-14T20:48:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/181/233</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/181/233</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/181/233 [2]</TD>
            <TD>Catalog of merging galaxies (Hwang+, 2009)</TD>
            <TD>In this supplement, we present a catalog and images of morphologically identified merging galaxies in Red Sequence Cluster Survey 2 (RCS2) (Yee et al., 2007ASPC..379..103Y). RCS2 is a large sky survey using the Canada-France-Hawaii Telescope (CFHT) to look for galaxy clusters out to z~1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233#2</TD>
            <TD>2011-09-14T20:48:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/181/233&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/181/233</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/181/233 [table1]</TD>
            <TD>Catalog of merging galaxies (Hwang+, 2009)</TD>
            <TD>In this supplement, we present a catalog and images of morphologically identified merging galaxies in Red Sequence Cluster Survey 2 (RCS2) (Yee et al., 2007ASPC..379..103Y). RCS2 is a large sky survey using the Canada-France-Hawaii Telescope (CFHT) to look for galaxy clusters out to z~1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233#table1</TD>
            <TD>2011-09-14T20:48:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/181/233</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/181/233&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/181/233</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/602/231 [1]</TD>
            <TD>Chandra X-ray point sources in nearby galaxies (Colbert+, 2004)</TD>
            <TD>We have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies and present the results of 1441 X-ray point sources that were detected in these galaxies. The total point-source X-ray (0.3-8.0keV) luminosity L_XP_ is well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP_ and both the old and young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass M and star formation rate SFR.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231#1</TD>
            <TD>2011-09-14T19:45:36Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/602/231</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/602/231</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/602/231 [2]</TD>
            <TD>Chandra X-ray point sources in nearby galaxies (Colbert+, 2004)</TD>
            <TD>We have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies and present the results of 1441 X-ray point sources that were detected in these galaxies. The total point-source X-ray (0.3-8.0keV) luminosity L_XP_ is well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP_ and both the old and young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass M and star formation rate SFR.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231#2</TD>
            <TD>2011-09-14T19:45:36Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/602/231&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/602/231</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/602/231 [table1]</TD>
            <TD>Chandra X-ray point sources in nearby galaxies (Colbert+, 2004)</TD>
            <TD>We have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies and present the results of 1441 X-ray point sources that were detected in these galaxies. The total point-source X-ray (0.3-8.0keV) luminosity L_XP_ is well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP_ and both the old and young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass M and star formation rate SFR.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231#table1</TD>
            <TD>2011-09-14T19:45:36Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/602/231&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/602/231</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/602/231 [1]</TD>
            <TD>Chandra X-ray point sources in nearby galaxies (Colbert+, 2004)</TD>
            <TD>We have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies and present the results of 1441 X-ray point sources that were detected in these galaxies. The total point-source X-ray (0.3-8.0keV) luminosity L_XP_ is well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP_ and both the old and young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass M and star formation rate SFR.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231#1</TD>
            <TD>2011-09-14T19:45:36Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/602/231</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/602/231</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/602/231 [2]</TD>
            <TD>Chandra X-ray point sources in nearby galaxies (Colbert+, 2004)</TD>
            <TD>We have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies and present the results of 1441 X-ray point sources that were detected in these galaxies. The total point-source X-ray (0.3-8.0keV) luminosity L_XP_ is well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP_ and both the old and young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass M and star formation rate SFR.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231#2</TD>
            <TD>2011-09-14T19:45:36Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/602/231&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/602/231</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/602/231 [table1]</TD>
            <TD>Chandra X-ray point sources in nearby galaxies (Colbert+, 2004)</TD>
            <TD>We have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies and present the results of 1441 X-ray point sources that were detected in these galaxies. The total point-source X-ray (0.3-8.0keV) luminosity L_XP_ is well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP_ and both the old and young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass M and star formation rate SFR.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231#table1</TD>
            <TD>2011-09-14T19:45:36Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/602/231&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/602/231</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/602/231 [1]</TD>
            <TD>Chandra X-ray point sources in nearby galaxies (Colbert+, 2004)</TD>
            <TD>We have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies and present the results of 1441 X-ray point sources that were detected in these galaxies. The total point-source X-ray (0.3-8.0keV) luminosity L_XP_ is well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP_ and both the old and young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass M and star formation rate SFR.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231#1</TD>
            <TD>2011-09-14T19:45:36Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/602/231</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/602/231</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/602/231 [2]</TD>
            <TD>Chandra X-ray point sources in nearby galaxies (Colbert+, 2004)</TD>
            <TD>We have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies and present the results of 1441 X-ray point sources that were detected in these galaxies. The total point-source X-ray (0.3-8.0keV) luminosity L_XP_ is well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP_ and both the old and young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass M and star formation rate SFR.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231#2</TD>
            <TD>2011-09-14T19:45:36Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/602/231&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/602/231</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/602/231 [table1]</TD>
            <TD>Chandra X-ray point sources in nearby galaxies (Colbert+, 2004)</TD>
            <TD>We have analyzed Chandra ACIS observations of 32 nearby spiral and elliptical galaxies and present the results of 1441 X-ray point sources that were detected in these galaxies. The total point-source X-ray (0.3-8.0keV) luminosity L_XP_ is well correlated with the B-band, K-band, and FIR+UV luminosities of spiral host galaxies and is well correlated with the B-band and K-band luminosities of elliptical galaxies. This suggests an intimate connection between L_XP_ and both the old and young stellar populations, for which K and FIR+UV luminosities are reasonable proxies for the galaxy mass M and star formation rate SFR.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231#table1</TD>
            <TD>2011-09-14T19:45:36Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/602/231</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/602/231&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/602/231</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/1508 [1]</TD>
            <TD>Galaxy morphology catalog (van den Berg+, 2007)</TD>
            <TD>Careful inspection of large-scale photographs of Shapley-Ames galaxies seems to show a smooth transition between the morphological characteristics of galaxies located on the narrow red and on the broad blue sequences in the galaxian color-magnitude diagram. In other words, there does not appear to be a dichotomy between blue and red galaxies. Both the colors and the morphologies of galaxies are found to correlate strongly with their environments. Red and early-type Shapley-Ames galaxies are dominant in clusters, whereas blue late-type star-forming objects dominate the general field. Interestingly, the colors and morphologies of galaxies in small groups resemble the field and differ from those in clusters. As noted by Baade, the presence of dust and star formation are very closely correlated, except in a few galaxies that probably had unusual evolutionary histories. Over the entire range from S0 to Sc there is no significant difference between the integrated colors of normal and barred objects, suggesting that the formation of a bar does not significantly affect the stellar evolutionary history of a galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508#1</TD>
            <TD>2011-09-14T20:49:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/1508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/1508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/1508 [2]</TD>
            <TD>Galaxy morphology catalog (van den Berg+, 2007)</TD>
            <TD>Careful inspection of large-scale photographs of Shapley-Ames galaxies seems to show a smooth transition between the morphological characteristics of galaxies located on the narrow red and on the broad blue sequences in the galaxian color-magnitude diagram. In other words, there does not appear to be a dichotomy between blue and red galaxies. Both the colors and the morphologies of galaxies are found to correlate strongly with their environments. Red and early-type Shapley-Ames galaxies are dominant in clusters, whereas blue late-type star-forming objects dominate the general field. Interestingly, the colors and morphologies of galaxies in small groups resemble the field and differ from those in clusters. As noted by Baade, the presence of dust and star formation are very closely correlated, except in a few galaxies that probably had unusual evolutionary histories. Over the entire range from S0 to Sc there is no significant difference between the integrated colors of normal and barred objects, suggesting that the formation of a bar does not significantly affect the stellar evolutionary history of a galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508#2</TD>
            <TD>2011-09-14T20:49:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/1508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/1508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/1508 [table1]</TD>
            <TD>Galaxy morphology catalog (van den Berg+, 2007)</TD>
            <TD>Careful inspection of large-scale photographs of Shapley-Ames galaxies seems to show a smooth transition between the morphological characteristics of galaxies located on the narrow red and on the broad blue sequences in the galaxian color-magnitude diagram. In other words, there does not appear to be a dichotomy between blue and red galaxies. Both the colors and the morphologies of galaxies are found to correlate strongly with their environments. Red and early-type Shapley-Ames galaxies are dominant in clusters, whereas blue late-type star-forming objects dominate the general field. Interestingly, the colors and morphologies of galaxies in small groups resemble the field and differ from those in clusters. As noted by Baade, the presence of dust and star formation are very closely correlated, except in a few galaxies that probably had unusual evolutionary histories. Over the entire range from S0 to Sc there is no significant difference between the integrated colors of normal and barred objects, suggesting that the formation of a bar does not significantly affect the stellar evolutionary history of a galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508#table1</TD>
            <TD>2011-09-14T20:49:15Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/1508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/1508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/588/218 [1]</TD>
            <TD>i*g* photometry of SDSS EDR galaxies (Abraham+, 2003)</TD>
            <TD>In this paper we present a new statistic for quantifying galaxy morphology based on measurements of the Gini coefficient of galaxy light distributions. This statistic is easy to measure and is commonly used in econometrics to measure how wealth is distributed in human populations. When applied to galaxy images, the Gini coefficient provides a quantitative measure of the inequality with which a galaxy's light is distributed among its constituent pixels. We measure the Gini coefficient of local galaxies in the Early Data Release of the Sloan Digital Sky Survey and demonstrate that this quantity is closely correlated with measurements of central concentration, but with significant scatter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/218#1</TD>
            <TD>2011-09-14T19:46:00Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/218</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/588/218</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/218</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/588/218 [2]</TD>
            <TD>i*g* photometry of SDSS EDR galaxies (Abraham+, 2003)</TD>
            <TD>In this paper we present a new statistic for quantifying galaxy morphology based on measurements of the Gini coefficient of galaxy light distributions. This statistic is easy to measure and is commonly used in econometrics to measure how wealth is distributed in human populations. When applied to galaxy images, the Gini coefficient provides a quantitative measure of the inequality with which a galaxy's light is distributed among its constituent pixels. We measure the Gini coefficient of local galaxies in the Early Data Release of the Sloan Digital Sky Survey and demonstrate that this quantity is closely correlated with measurements of central concentration, but with significant scatter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/218#2</TD>
            <TD>2011-09-14T19:46:00Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
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            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/218</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/588/218&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/218</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/588/218 [1]</TD>
            <TD>i*g* photometry of SDSS EDR galaxies (Abraham+, 2003)</TD>
            <TD>In this paper we present a new statistic for quantifying galaxy morphology based on measurements of the Gini coefficient of galaxy light distributions. This statistic is easy to measure and is commonly used in econometrics to measure how wealth is distributed in human populations. When applied to galaxy images, the Gini coefficient provides a quantitative measure of the inequality with which a galaxy's light is distributed among its constituent pixels. We measure the Gini coefficient of local galaxies in the Early Data Release of the Sloan Digital Sky Survey and demonstrate that this quantity is closely correlated with measurements of central concentration, but with significant scatter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/218#1</TD>
            <TD>2011-09-14T19:46:00Z</TD>
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            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/218</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/588/218</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/218</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/588/218 [2]</TD>
            <TD>i*g* photometry of SDSS EDR galaxies (Abraham+, 2003)</TD>
            <TD>In this paper we present a new statistic for quantifying galaxy morphology based on measurements of the Gini coefficient of galaxy light distributions. This statistic is easy to measure and is commonly used in econometrics to measure how wealth is distributed in human populations. When applied to galaxy images, the Gini coefficient provides a quantitative measure of the inequality with which a galaxy's light is distributed among its constituent pixels. We measure the Gini coefficient of local galaxies in the Early Data Release of the Sloan Digital Sky Survey and demonstrate that this quantity is closely correlated with measurements of central concentration, but with significant scatter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/218#2</TD>
            <TD>2011-09-14T19:46:00Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
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            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/218</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/588/218&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/218</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/1508 [1]</TD>
            <TD>Galaxy morphology catalog (van den Berg+, 2007)</TD>
            <TD>Careful inspection of large-scale photographs of Shapley-Ames galaxies seems to show a smooth transition between the morphological characteristics of galaxies located on the narrow red and on the broad blue sequences in the galaxian color-magnitude diagram. In other words, there does not appear to be a dichotomy between blue and red galaxies. Both the colors and the morphologies of galaxies are found to correlate strongly with their environments. Red and early-type Shapley-Ames galaxies are dominant in clusters, whereas blue late-type star-forming objects dominate the general field. Interestingly, the colors and morphologies of galaxies in small groups resemble the field and differ from those in clusters. As noted by Baade, the presence of dust and star formation are very closely correlated, except in a few galaxies that probably had unusual evolutionary histories. Over the entire range from S0 to Sc there is no significant difference between the integrated colors of normal and barred objects, suggesting that the formation of a bar does not significantly affect the stellar evolutionary history of a galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508#1</TD>
            <TD>2011-09-14T20:49:15Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/1508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/1508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/1508 [2]</TD>
            <TD>Galaxy morphology catalog (van den Berg+, 2007)</TD>
            <TD>Careful inspection of large-scale photographs of Shapley-Ames galaxies seems to show a smooth transition between the morphological characteristics of galaxies located on the narrow red and on the broad blue sequences in the galaxian color-magnitude diagram. In other words, there does not appear to be a dichotomy between blue and red galaxies. Both the colors and the morphologies of galaxies are found to correlate strongly with their environments. Red and early-type Shapley-Ames galaxies are dominant in clusters, whereas blue late-type star-forming objects dominate the general field. Interestingly, the colors and morphologies of galaxies in small groups resemble the field and differ from those in clusters. As noted by Baade, the presence of dust and star formation are very closely correlated, except in a few galaxies that probably had unusual evolutionary histories. Over the entire range from S0 to Sc there is no significant difference between the integrated colors of normal and barred objects, suggesting that the formation of a bar does not significantly affect the stellar evolutionary history of a galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508#2</TD>
            <TD>2011-09-14T20:49:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/1508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/1508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/1508 [table1]</TD>
            <TD>Galaxy morphology catalog (van den Berg+, 2007)</TD>
            <TD>Careful inspection of large-scale photographs of Shapley-Ames galaxies seems to show a smooth transition between the morphological characteristics of galaxies located on the narrow red and on the broad blue sequences in the galaxian color-magnitude diagram. In other words, there does not appear to be a dichotomy between blue and red galaxies. Both the colors and the morphologies of galaxies are found to correlate strongly with their environments. Red and early-type Shapley-Ames galaxies are dominant in clusters, whereas blue late-type star-forming objects dominate the general field. Interestingly, the colors and morphologies of galaxies in small groups resemble the field and differ from those in clusters. As noted by Baade, the presence of dust and star formation are very closely correlated, except in a few galaxies that probably had unusual evolutionary histories. Over the entire range from S0 to Sc there is no significant difference between the integrated colors of normal and barred objects, suggesting that the formation of a bar does not significantly affect the stellar evolutionary history of a galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508#table1</TD>
            <TD>2011-09-14T20:49:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/1508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/1508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/144/21 [1]</TD>
            <TD>Galaxy and Magellanic Clouds OB and WR stars (Robert+, 2003)</TD>
            <TD>Our far-UV libraries contain spectra of OB and Wolf-Rayet (WR) stars collected with FUSE mainly during its first cycle (1999 December to 2000 December). The FUSE instrument provides redundant wavelength coverage by means of eight independent spectra, each covering a ~100{AA} region between 905 and 1187{AA} at a resolving power of ~20,000. A detailed description of FUSE can be found in Moos et al. (2000ApJ...538L...1M) and Sahnow et al. (2000ApJ...538L...7S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21#1</TD>
            <TD>2011-09-14T19:46:24Z</TD>
            <TD>#Spectral_Classification#Photometry:wide-band#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/144/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/144/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/144/21 [2]</TD>
            <TD>Galaxy and Magellanic Clouds OB and WR stars (Robert+, 2003)</TD>
            <TD>Our far-UV libraries contain spectra of OB and Wolf-Rayet (WR) stars collected with FUSE mainly during its first cycle (1999 December to 2000 December). The FUSE instrument provides redundant wavelength coverage by means of eight independent spectra, each covering a ~100{AA} region between 905 and 1187{AA} at a resolving power of ~20,000. A detailed description of FUSE can be found in Moos et al. (2000ApJ...538L...1M) and Sahnow et al. (2000ApJ...538L...7S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21#2</TD>
            <TD>2011-09-14T19:46:24Z</TD>
            <TD>#Spectral_Classification#Photometry:wide-band#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/144/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/144/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/1508 [1]</TD>
            <TD>Galaxy morphology catalog (van den Berg+, 2007)</TD>
            <TD>Careful inspection of large-scale photographs of Shapley-Ames galaxies seems to show a smooth transition between the morphological characteristics of galaxies located on the narrow red and on the broad blue sequences in the galaxian color-magnitude diagram. In other words, there does not appear to be a dichotomy between blue and red galaxies. Both the colors and the morphologies of galaxies are found to correlate strongly with their environments. Red and early-type Shapley-Ames galaxies are dominant in clusters, whereas blue late-type star-forming objects dominate the general field. Interestingly, the colors and morphologies of galaxies in small groups resemble the field and differ from those in clusters. As noted by Baade, the presence of dust and star formation are very closely correlated, except in a few galaxies that probably had unusual evolutionary histories. Over the entire range from S0 to Sc there is no significant difference between the integrated colors of normal and barred objects, suggesting that the formation of a bar does not significantly affect the stellar evolutionary history of a galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508#1</TD>
            <TD>2011-09-14T20:49:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/1508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/1508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/1508 [2]</TD>
            <TD>Galaxy morphology catalog (van den Berg+, 2007)</TD>
            <TD>Careful inspection of large-scale photographs of Shapley-Ames galaxies seems to show a smooth transition between the morphological characteristics of galaxies located on the narrow red and on the broad blue sequences in the galaxian color-magnitude diagram. In other words, there does not appear to be a dichotomy between blue and red galaxies. Both the colors and the morphologies of galaxies are found to correlate strongly with their environments. Red and early-type Shapley-Ames galaxies are dominant in clusters, whereas blue late-type star-forming objects dominate the general field. Interestingly, the colors and morphologies of galaxies in small groups resemble the field and differ from those in clusters. As noted by Baade, the presence of dust and star formation are very closely correlated, except in a few galaxies that probably had unusual evolutionary histories. Over the entire range from S0 to Sc there is no significant difference between the integrated colors of normal and barred objects, suggesting that the formation of a bar does not significantly affect the stellar evolutionary history of a galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508#2</TD>
            <TD>2011-09-14T20:49:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/1508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/1508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/1508 [table1]</TD>
            <TD>Galaxy morphology catalog (van den Berg+, 2007)</TD>
            <TD>Careful inspection of large-scale photographs of Shapley-Ames galaxies seems to show a smooth transition between the morphological characteristics of galaxies located on the narrow red and on the broad blue sequences in the galaxian color-magnitude diagram. In other words, there does not appear to be a dichotomy between blue and red galaxies. Both the colors and the morphologies of galaxies are found to correlate strongly with their environments. Red and early-type Shapley-Ames galaxies are dominant in clusters, whereas blue late-type star-forming objects dominate the general field. Interestingly, the colors and morphologies of galaxies in small groups resemble the field and differ from those in clusters. As noted by Baade, the presence of dust and star formation are very closely correlated, except in a few galaxies that probably had unusual evolutionary histories. Over the entire range from S0 to Sc there is no significant difference between the integrated colors of normal and barred objects, suggesting that the formation of a bar does not significantly affect the stellar evolutionary history of a galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508#table1</TD>
            <TD>2011-09-14T20:49:15Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/1508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/1508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/1508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/144/21 [1]</TD>
            <TD>Galaxy and Magellanic Clouds OB and WR stars (Robert+, 2003)</TD>
            <TD>Our far-UV libraries contain spectra of OB and Wolf-Rayet (WR) stars collected with FUSE mainly during its first cycle (1999 December to 2000 December). The FUSE instrument provides redundant wavelength coverage by means of eight independent spectra, each covering a ~100{AA} region between 905 and 1187{AA} at a resolving power of ~20,000. A detailed description of FUSE can be found in Moos et al. (2000ApJ...538L...1M) and Sahnow et al. (2000ApJ...538L...7S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21#1</TD>
            <TD>2011-09-14T19:46:24Z</TD>
            <TD>#Spectral_Classification#Photometry:wide-band#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/144/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/144/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/144/21 [2]</TD>
            <TD>Galaxy and Magellanic Clouds OB and WR stars (Robert+, 2003)</TD>
            <TD>Our far-UV libraries contain spectra of OB and Wolf-Rayet (WR) stars collected with FUSE mainly during its first cycle (1999 December to 2000 December). The FUSE instrument provides redundant wavelength coverage by means of eight independent spectra, each covering a ~100{AA} region between 905 and 1187{AA} at a resolving power of ~20,000. A detailed description of FUSE can be found in Moos et al. (2000ApJ...538L...1M) and Sahnow et al. (2000ApJ...538L...7S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21#2</TD>
            <TD>2011-09-14T19:46:24Z</TD>
            <TD>#Spectral_Classification#Photometry:wide-band#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/144/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/144/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/144/21 [1]</TD>
            <TD>Galaxy and Magellanic Clouds OB and WR stars (Robert+, 2003)</TD>
            <TD>Our far-UV libraries contain spectra of OB and Wolf-Rayet (WR) stars collected with FUSE mainly during its first cycle (1999 December to 2000 December). The FUSE instrument provides redundant wavelength coverage by means of eight independent spectra, each covering a ~100{AA} region between 905 and 1187{AA} at a resolving power of ~20,000. A detailed description of FUSE can be found in Moos et al. (2000ApJ...538L...1M) and Sahnow et al. (2000ApJ...538L...7S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21#1</TD>
            <TD>2011-09-14T19:46:24Z</TD>
            <TD>#Spectral_Classification#Photometry:wide-band#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/144/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/144/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/144/21 [2]</TD>
            <TD>Galaxy and Magellanic Clouds OB and WR stars (Robert+, 2003)</TD>
            <TD>Our far-UV libraries contain spectra of OB and Wolf-Rayet (WR) stars collected with FUSE mainly during its first cycle (1999 December to 2000 December). The FUSE instrument provides redundant wavelength coverage by means of eight independent spectra, each covering a ~100{AA} region between 905 and 1187{AA} at a resolving power of ~20,000. A detailed description of FUSE can be found in Moos et al. (2000ApJ...538L...1M) and Sahnow et al. (2000ApJ...538L...7S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21#2</TD>
            <TD>2011-09-14T19:46:24Z</TD>
            <TD>#Spectral_Classification#Photometry:wide-band#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/144/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/144/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/144/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/134 [1]</TD>
            <TD>Atlas of Radio/X-ray associations (ARXA) (Flesch, 2010)</TD>
            <TD>This is a compendium of all catalogued or APM/USNO-A optical objects which are found to be associated to XMM, Chandra, RASS, HRI, PSPC or WGA X-ray detections, or to NVSS, FIRST or SUMSS radio detections. All detections are displayed, plus double radio lobes where found. The counts are: Optical objects - 602,570 NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778 Chandra associations - 32,951 ROSAT RASS - 47,486 ROSAT HRI - 15,523 ROSAT PSPC - 35,607 WGA - 24,226 Each optical object is shown as one line bearing the J2000 coordinates, the object name (from the literature where available), APM &amp; USNO-A sourced red &amp; blue photometry, redshift, the source catalogs for the name and redshift, calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. Questions or comments may be directed to eric@flesch.org.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/134#1</TD>
            <TD>2011-09-14T20:52:45Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/V/134</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/134</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/134</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/134 [2]</TD>
            <TD>Atlas of Radio/X-ray associations (ARXA) (Flesch, 2010)</TD>
            <TD>This is a compendium of all catalogued or APM/USNO-A optical objects which are found to be associated to XMM, Chandra, RASS, HRI, PSPC or WGA X-ray detections, or to NVSS, FIRST or SUMSS radio detections. All detections are displayed, plus double radio lobes where found. The counts are: Optical objects - 602,570 NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778 Chandra associations - 32,951 ROSAT RASS - 47,486 ROSAT HRI - 15,523 ROSAT PSPC - 35,607 WGA - 24,226 Each optical object is shown as one line bearing the J2000 coordinates, the object name (from the literature where available), APM &amp; USNO-A sourced red &amp; blue photometry, redshift, the source catalogs for the name and redshift, calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. Questions or comments may be directed to eric@flesch.org.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/134#2</TD>
            <TD>2011-09-14T20:52:45Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/V/134</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/134&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/134</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/134 [arxa]</TD>
            <TD>Atlas of Radio/X-ray associations (ARXA) (Flesch, 2010)</TD>
            <TD>This is a compendium of all catalogued or APM/USNO-A optical objects which are found to be associated to XMM, Chandra, RASS, HRI, PSPC or WGA X-ray detections, or to NVSS, FIRST or SUMSS radio detections. All detections are displayed, plus double radio lobes where found. The counts are: Optical objects - 602,570 NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778 Chandra associations - 32,951 ROSAT RASS - 47,486 ROSAT HRI - 15,523 ROSAT PSPC - 35,607 WGA - 24,226 Each optical object is shown as one line bearing the J2000 coordinates, the object name (from the literature where available), APM &amp; USNO-A sourced red &amp; blue photometry, redshift, the source catalogs for the name and redshift, calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. Questions or comments may be directed to eric@flesch.org.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/134#arxa</TD>
            <TD>2011-09-14T20:52:45Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/V/134</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/134&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/134</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/445/857 [1]</TD>
            <TD>DPOSS II compact group survey (Pompei+, 2006)</TD>
            <TD>Observed candidate galaxy members of DPOSS II compact groups. We list here the name of each galaxy, defined by the name of its group, followed by a letter A through E in order of decreasing brightness; its coordinates at the year 2000, its heliocentric radial velocity with its associated error. Finally in the last two columns of the table we describe what lines dominate the spectrum: absorption, emission or a mixed kind of spectrum and which emission lines have been observed in the spectrum itself. Mis-identification of star/galaxy and other problems found in the spectrum are also indicated in the last column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857#1</TD>
            <TD>2011-09-14T19:46:52Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/445/857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/445/857 [2]</TD>
            <TD>DPOSS II compact group survey (Pompei+, 2006)</TD>
            <TD>Observed candidate galaxy members of DPOSS II compact groups. We list here the name of each galaxy, defined by the name of its group, followed by a letter A through E in order of decreasing brightness; its coordinates at the year 2000, its heliocentric radial velocity with its associated error. Finally in the last two columns of the table we describe what lines dominate the spectrum: absorption, emission or a mixed kind of spectrum and which emission lines have been observed in the spectrum itself. Mis-identification of star/galaxy and other problems found in the spectrum are also indicated in the last column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857#2</TD>
            <TD>2011-09-14T19:46:52Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/445/857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/445/857 [1]</TD>
            <TD>DPOSS II compact group survey (Pompei+, 2006)</TD>
            <TD>Observed candidate galaxy members of DPOSS II compact groups. We list here the name of each galaxy, defined by the name of its group, followed by a letter A through E in order of decreasing brightness; its coordinates at the year 2000, its heliocentric radial velocity with its associated error. Finally in the last two columns of the table we describe what lines dominate the spectrum: absorption, emission or a mixed kind of spectrum and which emission lines have been observed in the spectrum itself. Mis-identification of star/galaxy and other problems found in the spectrum are also indicated in the last column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857#1</TD>
            <TD>2011-09-14T19:46:52Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/445/857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/445/857 [2]</TD>
            <TD>DPOSS II compact group survey (Pompei+, 2006)</TD>
            <TD>Observed candidate galaxy members of DPOSS II compact groups. We list here the name of each galaxy, defined by the name of its group, followed by a letter A through E in order of decreasing brightness; its coordinates at the year 2000, its heliocentric radial velocity with its associated error. Finally in the last two columns of the table we describe what lines dominate the spectrum: absorption, emission or a mixed kind of spectrum and which emission lines have been observed in the spectrum itself. Mis-identification of star/galaxy and other problems found in the spectrum are also indicated in the last column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857#2</TD>
            <TD>2011-09-14T19:46:52Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/445/857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/445/857 [1]</TD>
            <TD>DPOSS II compact group survey (Pompei+, 2006)</TD>
            <TD>Observed candidate galaxy members of DPOSS II compact groups. We list here the name of each galaxy, defined by the name of its group, followed by a letter A through E in order of decreasing brightness; its coordinates at the year 2000, its heliocentric radial velocity with its associated error. Finally in the last two columns of the table we describe what lines dominate the spectrum: absorption, emission or a mixed kind of spectrum and which emission lines have been observed in the spectrum itself. Mis-identification of star/galaxy and other problems found in the spectrum are also indicated in the last column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857#1</TD>
            <TD>2011-09-14T19:46:52Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/445/857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/445/857 [2]</TD>
            <TD>DPOSS II compact group survey (Pompei+, 2006)</TD>
            <TD>Observed candidate galaxy members of DPOSS II compact groups. We list here the name of each galaxy, defined by the name of its group, followed by a letter A through E in order of decreasing brightness; its coordinates at the year 2000, its heliocentric radial velocity with its associated error. Finally in the last two columns of the table we describe what lines dominate the spectrum: absorption, emission or a mixed kind of spectrum and which emission lines have been observed in the spectrum itself. Mis-identification of star/galaxy and other problems found in the spectrum are also indicated in the last column of the table.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857#2</TD>
            <TD>2011-09-14T19:46:52Z</TD>
            <TD>#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/445/857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>III/193 [1]</TD>
            <TD>Chemical Abundances in Late-Type Stars (Thevenin, 1998)</TD>
            <TD>The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. &lt;III/200&gt;). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/193#1</TD>
            <TD>2011-09-14T19:55:53Z</TD>
            <TD>#Abundances#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/III/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=III/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>III/193 [2]</TD>
            <TD>Chemical Abundances in Late-Type Stars (Thevenin, 1998)</TD>
            <TD>The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. &lt;III/200&gt;). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/193#2</TD>
            <TD>2011-09-14T19:55:53Z</TD>
            <TD>#Abundances#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/III/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=III/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>III/193 [catalog]</TD>
            <TD>Chemical Abundances in Late-Type Stars (Thevenin, 1998)</TD>
            <TD>The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. &lt;III/200&gt;). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/193#catalog</TD>
            <TD>2011-09-14T19:55:53Z</TD>
            <TD>#Abundances#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/III/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=III/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>III/193 [1]</TD>
            <TD>Chemical Abundances in Late-Type Stars (Thevenin, 1998)</TD>
            <TD>The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. &lt;III/200&gt;). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/193#1</TD>
            <TD>2011-09-14T19:55:53Z</TD>
            <TD>#Abundances#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/III/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=III/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>III/193 [2]</TD>
            <TD>Chemical Abundances in Late-Type Stars (Thevenin, 1998)</TD>
            <TD>The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. &lt;III/200&gt;). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/193#2</TD>
            <TD>2011-09-14T19:55:53Z</TD>
            <TD>#Abundances#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/III/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=III/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>III/193 [catalog]</TD>
            <TD>Chemical Abundances in Late-Type Stars (Thevenin, 1998)</TD>
            <TD>The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. &lt;III/200&gt;). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/193#catalog</TD>
            <TD>2011-09-14T19:55:53Z</TD>
            <TD>#Abundances#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/III/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=III/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>III/193 [1]</TD>
            <TD>Chemical Abundances in Late-Type Stars (Thevenin, 1998)</TD>
            <TD>The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. &lt;III/200&gt;). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/193#1</TD>
            <TD>2011-09-14T19:55:53Z</TD>
            <TD>#Abundances#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/III/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=III/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>III/193 [2]</TD>
            <TD>Chemical Abundances in Late-Type Stars (Thevenin, 1998)</TD>
            <TD>The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. &lt;III/200&gt;). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/193#2</TD>
            <TD>2011-09-14T19:55:53Z</TD>
            <TD>#Abundances#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/III/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=III/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>III/193 [catalog]</TD>
            <TD>Chemical Abundances in Late-Type Stars (Thevenin, 1998)</TD>
            <TD>The catalogue includes chemical abundances determinations (from Li to Eu) and atmospheric parameters (Teff, logg, microturbulent velocity) obtained from re-analyses of 1108 Late-Type Stars. It contains field stars of the Galaxy, of open and globular cluster stars, and stars belonging to the LMC and the SMC. Almost all of these stars are referenced in the Cayrel de Strobel et al.'s [Fe/H] catalog (see cat. &lt;III/200&gt;). Most of the abundance results are very reliable within 0.2dex when using different sources of equivalent widths taken from the literature for a given star.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/193#catalog</TD>
            <TD>2011-09-14T19:55:53Z</TD>
            <TD>#Abundances#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1998</TD>
            <TD>ivo://CDS.VizieR/III/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=III/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/1558 [1]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#1</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/1558</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/1558 [2]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#2</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/1558&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/1558 [table5]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#table5</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/1558&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/1558 [table1]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#table1</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/1558&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/1558 [1]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#1</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/1558</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/1558 [2]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#2</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/1558&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/1558 [table5]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#table5</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/1558&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/1558 [table1]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#table1</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/1558&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/1558 [1]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#1</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/1558</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/1558 [2]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#2</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/1558&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/1558 [table5]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#table5</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/1558&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/1558 [table1]</TD>
            <TD>NOAO Fundamental Plane Survey (Smith+, 2004)</TD>
            <TD>We introduce the NOAO Fundamental Plane Survey (NFPS), a wide-field imaging/spectroscopic study of rich, low-redshift galaxy clusters. The survey targets X-ray-selected clusters at 0.010&lt;z&lt;0.067, distributed over the whole sky, with imaging and spectroscopic observations obtained for 93 clusters. This data set will be used in investigations of galaxy properties in the cluster environment and of large-scale velocity fields through the fundamental plane. In this paper, we present details of the cluster sample construction and the strategies employed to select early-type galaxy samples for spectroscopy. Details of the spectroscopic observations are reported. From observations of 5479 red galaxies, we present redshift measurements for 5388 objects and internal velocity dispersions for 4131. The velocity dispersions have a median estimated error ~7%. The NFPS has ~15% overlap with previously published velocity dispersion data sets. Comparisons to these external catalogs are presented and indicate typical external errors of ~8%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558#table1</TD>
            <TD>2011-09-14T20:01:31Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1558</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/1558&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1558</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/438/507 [1]</TD>
            <TD>Degree of lopsidedness for galaxies (Bournaud+, 2005)</TD>
            <TD>To quantify the amplitude of the m=1 mode both in the disk surface density and in the potential, we use near-infrared images from the Ohio State University Bright Galaxy Survey (OSUBGS, Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507#1</TD>
            <TD>2011-09-14T20:01:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/438/507</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/438/507</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/438/507 [2]</TD>
            <TD>Degree of lopsidedness for galaxies (Bournaud+, 2005)</TD>
            <TD>To quantify the amplitude of the m=1 mode both in the disk surface density and in the potential, we use near-infrared images from the Ohio State University Bright Galaxy Survey (OSUBGS, Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507#2</TD>
            <TD>2011-09-14T20:01:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/438/507&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/438/507</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/438/507 [tablea1]</TD>
            <TD>Degree of lopsidedness for galaxies (Bournaud+, 2005)</TD>
            <TD>To quantify the amplitude of the m=1 mode both in the disk surface density and in the potential, we use near-infrared images from the Ohio State University Bright Galaxy Survey (OSUBGS, Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507#tablea1</TD>
            <TD>2011-09-14T20:01:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/438/507&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/438/507</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/438/507 [1]</TD>
            <TD>Degree of lopsidedness for galaxies (Bournaud+, 2005)</TD>
            <TD>To quantify the amplitude of the m=1 mode both in the disk surface density and in the potential, we use near-infrared images from the Ohio State University Bright Galaxy Survey (OSUBGS, Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507#1</TD>
            <TD>2011-09-14T20:01:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/438/507</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/438/507</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/438/507 [2]</TD>
            <TD>Degree of lopsidedness for galaxies (Bournaud+, 2005)</TD>
            <TD>To quantify the amplitude of the m=1 mode both in the disk surface density and in the potential, we use near-infrared images from the Ohio State University Bright Galaxy Survey (OSUBGS, Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507#2</TD>
            <TD>2011-09-14T20:01:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/438/507&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/438/507</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/438/507 [tablea1]</TD>
            <TD>Degree of lopsidedness for galaxies (Bournaud+, 2005)</TD>
            <TD>To quantify the amplitude of the m=1 mode both in the disk surface density and in the potential, we use near-infrared images from the Ohio State University Bright Galaxy Survey (OSUBGS, Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507#tablea1</TD>
            <TD>2011-09-14T20:01:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/438/507&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/438/507</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/438/507 [1]</TD>
            <TD>Degree of lopsidedness for galaxies (Bournaud+, 2005)</TD>
            <TD>To quantify the amplitude of the m=1 mode both in the disk surface density and in the potential, we use near-infrared images from the Ohio State University Bright Galaxy Survey (OSUBGS, Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507#1</TD>
            <TD>2011-09-14T20:01:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/438/507</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/438/507</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/438/507 [2]</TD>
            <TD>Degree of lopsidedness for galaxies (Bournaud+, 2005)</TD>
            <TD>To quantify the amplitude of the m=1 mode both in the disk surface density and in the potential, we use near-infrared images from the Ohio State University Bright Galaxy Survey (OSUBGS, Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507#2</TD>
            <TD>2011-09-14T20:01:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/438/507&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/438/507</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/438/507 [tablea1]</TD>
            <TD>Degree of lopsidedness for galaxies (Bournaud+, 2005)</TD>
            <TD>To quantify the amplitude of the m=1 mode both in the disk surface density and in the potential, we use near-infrared images from the Ohio State University Bright Galaxy Survey (OSUBGS, Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507#tablea1</TD>
            <TD>2011-09-14T20:01:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/438/507</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/438/507&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/438/507</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/140/265 [1]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#1</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/140/265</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/140/265 [2]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#2</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table4]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table4</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table3]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table3</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table5]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table5</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table2]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table2</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table6]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table6</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/140/265 [1]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#1</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/140/265</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/140/265 [2]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#2</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table4]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table4</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table3]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table3</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table5]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table5</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table2]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table2</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table6]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table6</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/140/265 [1]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#1</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/140/265</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/140/265 [2]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#2</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table4]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table4</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table3]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table3</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table5]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table5</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table2]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table2</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/140/265 [table6]</TD>
            <TD>WARPS survey. VI. (Perlman+, 2002)</TD>
            <TD>We present in catalog form the optical identifications for objects from the first phase of the Wide Angle ROSAT Pointed Survey (WARPS). WARPS is a serendipitous survey of relatively deep, pointed ROSAT observations for clusters of galaxies. The X-ray source detection algorithm used by WARPS is Voronoi Tessellation and Percolation (VTP), a technique which is equally sensitive to point sources and extended sources of low surface brightness. WARPS-I is based on the central regions of 86 ROSAT PSPC fields, covering an area of 16.2 square degrees. We describe here the X-ray source screening and optical identification process for WARPS-I, which yielded 34 clusters at 0.06&lt;z&lt;0.75. Twenty-two of these clusters form a complete, statistically well-defined sample drawn from 75 of these 86 fields, covering an area of 14.1 square degrees, with a flux limit of F(0.5x2.0keV)=6.5x10^-14^erg/cm^2^/s. This sample can be used to study the properties and evolution of the gas, galaxy and dark matter content of clusters and to constrain cosmological parameters. We compare in detail the identification process and findings of WARPS to those from other recently published X-ray surveys for clusters, including RDCS, SHARC-Bright, SHARC-south, and the CfA 160deg^2^ survey.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265#table6</TD>
            <TD>2011-09-14T20:11:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/140/265</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/140/265&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/140/265</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/375/115 [1]</TD>
            <TD>ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007)</TD>
            <TD>We present a result of cross-correlating the Infrared Astronomical Satellite Faint Source Catalogue with the spectroscopic catalogues of galaxies in the Fourth Data Release of the Sloan Digital Sky Survey, the Final Data Release of the 2dF Galaxy Redshift Survey (2dFGRS) and the Second Data Release of the 6dF Galaxy Survey. We have identified 324 ultraluminous infrared galaxies (ULIRGs) including 190 newly discovered ULIRGs, and two hyperluminous infrared galaxies. Adding these new ULIRGs, we increase the number of known ULIRGs by about 30 per cent. The reliability of the cross-correlation is estimated using the likelihood ratio method.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115#1</TD>
            <TD>2011-09-14T20:16:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/375/115</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/115</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/375/115 [2]</TD>
            <TD>ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007)</TD>
            <TD>We present a result of cross-correlating the Infrared Astronomical Satellite Faint Source Catalogue with the spectroscopic catalogues of galaxies in the Fourth Data Release of the Sloan Digital Sky Survey, the Final Data Release of the 2dF Galaxy Redshift Survey (2dFGRS) and the Second Data Release of the 6dF Galaxy Survey. We have identified 324 ultraluminous infrared galaxies (ULIRGs) including 190 newly discovered ULIRGs, and two hyperluminous infrared galaxies. Adding these new ULIRGs, we increase the number of known ULIRGs by about 30 per cent. The reliability of the cross-correlation is estimated using the likelihood ratio method.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115#2</TD>
            <TD>2011-09-14T20:16:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/375/115&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/115 [ULIRG]</TD>
            <TD>ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007)</TD>
            <TD>We present a result of cross-correlating the Infrared Astronomical Satellite Faint Source Catalogue with the spectroscopic catalogues of galaxies in the Fourth Data Release of the Sloan Digital Sky Survey, the Final Data Release of the 2dF Galaxy Redshift Survey (2dFGRS) and the Second Data Release of the 6dF Galaxy Survey. We have identified 324 ultraluminous infrared galaxies (ULIRGs) including 190 newly discovered ULIRGs, and two hyperluminous infrared galaxies. Adding these new ULIRGs, we increase the number of known ULIRGs by about 30 per cent. The reliability of the cross-correlation is estimated using the likelihood ratio method.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115#ULIRG</TD>
            <TD>2011-09-14T20:16:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/115</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/375/115 [1]</TD>
            <TD>ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007)</TD>
            <TD>We present a result of cross-correlating the Infrared Astronomical Satellite Faint Source Catalogue with the spectroscopic catalogues of galaxies in the Fourth Data Release of the Sloan Digital Sky Survey, the Final Data Release of the 2dF Galaxy Redshift Survey (2dFGRS) and the Second Data Release of the 6dF Galaxy Survey. We have identified 324 ultraluminous infrared galaxies (ULIRGs) including 190 newly discovered ULIRGs, and two hyperluminous infrared galaxies. Adding these new ULIRGs, we increase the number of known ULIRGs by about 30 per cent. The reliability of the cross-correlation is estimated using the likelihood ratio method.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115#1</TD>
            <TD>2011-09-14T20:16:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/375/115</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/115</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/375/115 [2]</TD>
            <TD>ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007)</TD>
            <TD>We present a result of cross-correlating the Infrared Astronomical Satellite Faint Source Catalogue with the spectroscopic catalogues of galaxies in the Fourth Data Release of the Sloan Digital Sky Survey, the Final Data Release of the 2dF Galaxy Redshift Survey (2dFGRS) and the Second Data Release of the 6dF Galaxy Survey. We have identified 324 ultraluminous infrared galaxies (ULIRGs) including 190 newly discovered ULIRGs, and two hyperluminous infrared galaxies. Adding these new ULIRGs, we increase the number of known ULIRGs by about 30 per cent. The reliability of the cross-correlation is estimated using the likelihood ratio method.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115#2</TD>
            <TD>2011-09-14T20:16:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/375/115&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/115 [ULIRG]</TD>
            <TD>ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007)</TD>
            <TD>We present a result of cross-correlating the Infrared Astronomical Satellite Faint Source Catalogue with the spectroscopic catalogues of galaxies in the Fourth Data Release of the Sloan Digital Sky Survey, the Final Data Release of the 2dF Galaxy Redshift Survey (2dFGRS) and the Second Data Release of the 6dF Galaxy Survey. We have identified 324 ultraluminous infrared galaxies (ULIRGs) including 190 newly discovered ULIRGs, and two hyperluminous infrared galaxies. Adding these new ULIRGs, we increase the number of known ULIRGs by about 30 per cent. The reliability of the cross-correlation is estimated using the likelihood ratio method.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115#ULIRG</TD>
            <TD>2011-09-14T20:16:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/115</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/375/115 [1]</TD>
            <TD>ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007)</TD>
            <TD>We present a result of cross-correlating the Infrared Astronomical Satellite Faint Source Catalogue with the spectroscopic catalogues of galaxies in the Fourth Data Release of the Sloan Digital Sky Survey, the Final Data Release of the 2dF Galaxy Redshift Survey (2dFGRS) and the Second Data Release of the 6dF Galaxy Survey. We have identified 324 ultraluminous infrared galaxies (ULIRGs) including 190 newly discovered ULIRGs, and two hyperluminous infrared galaxies. Adding these new ULIRGs, we increase the number of known ULIRGs by about 30 per cent. The reliability of the cross-correlation is estimated using the likelihood ratio method.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115#1</TD>
            <TD>2011-09-14T20:16:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/375/115</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/115</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/375/115 [2]</TD>
            <TD>ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007)</TD>
            <TD>We present a result of cross-correlating the Infrared Astronomical Satellite Faint Source Catalogue with the spectroscopic catalogues of galaxies in the Fourth Data Release of the Sloan Digital Sky Survey, the Final Data Release of the 2dF Galaxy Redshift Survey (2dFGRS) and the Second Data Release of the 6dF Galaxy Survey. We have identified 324 ultraluminous infrared galaxies (ULIRGs) including 190 newly discovered ULIRGs, and two hyperluminous infrared galaxies. Adding these new ULIRGs, we increase the number of known ULIRGs by about 30 per cent. The reliability of the cross-correlation is estimated using the likelihood ratio method.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115#2</TD>
            <TD>2011-09-14T20:16:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/375/115&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/115</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/115 [ULIRG]</TD>
            <TD>ULIRGs galaxies in SDSS, 2dF and 6dF (Hwang+, 2007)</TD>
            <TD>We present a result of cross-correlating the Infrared Astronomical Satellite Faint Source Catalogue with the spectroscopic catalogues of galaxies in the Fourth Data Release of the Sloan Digital Sky Survey, the Final Data Release of the 2dF Galaxy Redshift Survey (2dFGRS) and the Second Data Release of the 6dF Galaxy Survey. We have identified 324 ultraluminous infrared galaxies (ULIRGs) including 190 newly discovered ULIRGs, and two hyperluminous infrared galaxies. Adding these new ULIRGs, we increase the number of known ULIRGs by about 30 per cent. The reliability of the cross-correlation is estimated using the likelihood ratio method.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115#ULIRG</TD>
            <TD>2011-09-14T20:16:10Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/115</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/115&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/115</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/134 [1]</TD>
            <TD>Atlas of Radio/X-ray associations (ARXA) (Flesch, 2010)</TD>
            <TD>This is a compendium of all catalogued or APM/USNO-A optical objects which are found to be associated to XMM, Chandra, RASS, HRI, PSPC or WGA X-ray detections, or to NVSS, FIRST or SUMSS radio detections. All detections are displayed, plus double radio lobes where found. The counts are: Optical objects - 602,570 NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778 Chandra associations - 32,951 ROSAT RASS - 47,486 ROSAT HRI - 15,523 ROSAT PSPC - 35,607 WGA - 24,226 Each optical object is shown as one line bearing the J2000 coordinates, the object name (from the literature where available), APM &amp; USNO-A sourced red &amp; blue photometry, redshift, the source catalogs for the name and redshift, calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. Questions or comments may be directed to eric@flesch.org.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/134#1</TD>
            <TD>2011-09-14T20:52:45Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/V/134</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/134</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/134</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/134 [2]</TD>
            <TD>Atlas of Radio/X-ray associations (ARXA) (Flesch, 2010)</TD>
            <TD>This is a compendium of all catalogued or APM/USNO-A optical objects which are found to be associated to XMM, Chandra, RASS, HRI, PSPC or WGA X-ray detections, or to NVSS, FIRST or SUMSS radio detections. All detections are displayed, plus double radio lobes where found. The counts are: Optical objects - 602,570 NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778 Chandra associations - 32,951 ROSAT RASS - 47,486 ROSAT HRI - 15,523 ROSAT PSPC - 35,607 WGA - 24,226 Each optical object is shown as one line bearing the J2000 coordinates, the object name (from the literature where available), APM &amp; USNO-A sourced red &amp; blue photometry, redshift, the source catalogs for the name and redshift, calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. Questions or comments may be directed to eric@flesch.org.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/134#2</TD>
            <TD>2011-09-14T20:52:45Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/V/134</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/134&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/134</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/134 [arxa]</TD>
            <TD>Atlas of Radio/X-ray associations (ARXA) (Flesch, 2010)</TD>
            <TD>This is a compendium of all catalogued or APM/USNO-A optical objects which are found to be associated to XMM, Chandra, RASS, HRI, PSPC or WGA X-ray detections, or to NVSS, FIRST or SUMSS radio detections. All detections are displayed, plus double radio lobes where found. The counts are: Optical objects - 602,570 NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778 Chandra associations - 32,951 ROSAT RASS - 47,486 ROSAT HRI - 15,523 ROSAT PSPC - 35,607 WGA - 24,226 Each optical object is shown as one line bearing the J2000 coordinates, the object name (from the literature where available), APM &amp; USNO-A sourced red &amp; blue photometry, redshift, the source catalogs for the name and redshift, calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. Questions or comments may be directed to eric@flesch.org.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/134#arxa</TD>
            <TD>2011-09-14T20:52:45Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/V/134</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/134&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/134</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/501 [1]</TD>
            <TD>JKs photometry of WLM galaxy carbon stars (Valcheva+, 2007)</TD>
            <TD>The observations of WLM were made in Dec. 2004 under non-photometric conditions. To estimate the foreground contamination, an additional field located 14.8' South from the center of the galaxy, far enough to eliminate the galaxy contribution, was observed in July 2006 (hereafter "clear sky" field). The near-IR imaged and spectrograph SofI (Son of ISAAC) at the ESO NTT (New Technology Telescope) on La Silla was used.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501#1</TD>
            <TD>2011-09-14T20:16:19Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/501</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/501</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/501 [2]</TD>
            <TD>JKs photometry of WLM galaxy carbon stars (Valcheva+, 2007)</TD>
            <TD>The observations of WLM were made in Dec. 2004 under non-photometric conditions. To estimate the foreground contamination, an additional field located 14.8' South from the center of the galaxy, far enough to eliminate the galaxy contribution, was observed in July 2006 (hereafter "clear sky" field). The near-IR imaged and spectrograph SofI (Son of ISAAC) at the ESO NTT (New Technology Telescope) on La Silla was used.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501#2</TD>
            <TD>2011-09-14T20:16:19Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/501&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/501</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/501 [table1]</TD>
            <TD>JKs photometry of WLM galaxy carbon stars (Valcheva+, 2007)</TD>
            <TD>The observations of WLM were made in Dec. 2004 under non-photometric conditions. To estimate the foreground contamination, an additional field located 14.8' South from the center of the galaxy, far enough to eliminate the galaxy contribution, was observed in July 2006 (hereafter "clear sky" field). The near-IR imaged and spectrograph SofI (Son of ISAAC) at the ESO NTT (New Technology Telescope) on La Silla was used.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501#table1</TD>
            <TD>2011-09-14T20:16:19Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/501&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/501</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/501 [1]</TD>
            <TD>JKs photometry of WLM galaxy carbon stars (Valcheva+, 2007)</TD>
            <TD>The observations of WLM were made in Dec. 2004 under non-photometric conditions. To estimate the foreground contamination, an additional field located 14.8' South from the center of the galaxy, far enough to eliminate the galaxy contribution, was observed in July 2006 (hereafter "clear sky" field). The near-IR imaged and spectrograph SofI (Son of ISAAC) at the ESO NTT (New Technology Telescope) on La Silla was used.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501#1</TD>
            <TD>2011-09-14T20:16:19Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/501</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/501</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/501 [2]</TD>
            <TD>JKs photometry of WLM galaxy carbon stars (Valcheva+, 2007)</TD>
            <TD>The observations of WLM were made in Dec. 2004 under non-photometric conditions. To estimate the foreground contamination, an additional field located 14.8' South from the center of the galaxy, far enough to eliminate the galaxy contribution, was observed in July 2006 (hereafter "clear sky" field). The near-IR imaged and spectrograph SofI (Son of ISAAC) at the ESO NTT (New Technology Telescope) on La Silla was used.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501#2</TD>
            <TD>2011-09-14T20:16:19Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/501&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/501</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/501 [table1]</TD>
            <TD>JKs photometry of WLM galaxy carbon stars (Valcheva+, 2007)</TD>
            <TD>The observations of WLM were made in Dec. 2004 under non-photometric conditions. To estimate the foreground contamination, an additional field located 14.8' South from the center of the galaxy, far enough to eliminate the galaxy contribution, was observed in July 2006 (hereafter "clear sky" field). The near-IR imaged and spectrograph SofI (Son of ISAAC) at the ESO NTT (New Technology Telescope) on La Silla was used.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501#table1</TD>
            <TD>2011-09-14T20:16:19Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/501&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/501</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/466/501 [1]</TD>
            <TD>JKs photometry of WLM galaxy carbon stars (Valcheva+, 2007)</TD>
            <TD>The observations of WLM were made in Dec. 2004 under non-photometric conditions. To estimate the foreground contamination, an additional field located 14.8' South from the center of the galaxy, far enough to eliminate the galaxy contribution, was observed in July 2006 (hereafter "clear sky" field). The near-IR imaged and spectrograph SofI (Son of ISAAC) at the ESO NTT (New Technology Telescope) on La Silla was used.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501#1</TD>
            <TD>2011-09-14T20:16:19Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/466/501</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/501</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/466/501 [2]</TD>
            <TD>JKs photometry of WLM galaxy carbon stars (Valcheva+, 2007)</TD>
            <TD>The observations of WLM were made in Dec. 2004 under non-photometric conditions. To estimate the foreground contamination, an additional field located 14.8' South from the center of the galaxy, far enough to eliminate the galaxy contribution, was observed in July 2006 (hereafter "clear sky" field). The near-IR imaged and spectrograph SofI (Son of ISAAC) at the ESO NTT (New Technology Telescope) on La Silla was used.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501#2</TD>
            <TD>2011-09-14T20:16:19Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/466/501&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/501</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/466/501 [table1]</TD>
            <TD>JKs photometry of WLM galaxy carbon stars (Valcheva+, 2007)</TD>
            <TD>The observations of WLM were made in Dec. 2004 under non-photometric conditions. To estimate the foreground contamination, an additional field located 14.8' South from the center of the galaxy, far enough to eliminate the galaxy contribution, was observed in July 2006 (hereafter "clear sky" field). The near-IR imaged and spectrograph SofI (Son of ISAAC) at the ESO NTT (New Technology Telescope) on La Silla was used.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501#table1</TD>
            <TD>2011-09-14T20:16:19Z</TD>
            <TD>#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/466/501</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/466/501&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/466/501</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/378 [1]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#1</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/378</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/378 [2]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#2</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/378&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/378 [table3]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#table3</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/378&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/378 [table4]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#table4</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/378&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/378 [1]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#1</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/378</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/378 [2]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#2</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/378&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/378 [table3]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#table3</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/378&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/378 [table4]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#table4</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/378&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/378 [1]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#1</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/378</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/378 [2]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#2</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/378&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/378 [table3]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#table3</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/378&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/378 [table4]</TD>
            <TD>HST and UV photometry of NGC 6822 (Bianchi+, 2006)</TD>
            <TD>HST imaging of different regions in NGC 6822 were obtained between 2000 June 16 and 2002 May 24 as part of the program GO-8675 (principal investigator L. Bianchi) to study the massive star content of this galaxy, with the WFPC2 and the STIS imagers.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378#table4</TD>
            <TD>2011-09-14T20:16:27Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/378</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/378&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/378</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/3492 [1]</TD>
            <TD>JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)</TD>
            <TD>Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492#1</TD>
            <TD>2012-04-19T15:26:16Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/3492</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3492</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/3492 [2]</TD>
            <TD>JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)</TD>
            <TD>Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492#2</TD>
            <TD>2012-04-19T15:26:16Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/3492&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3492</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/3492 [table2]</TD>
            <TD>JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)</TD>
            <TD>Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492#table2</TD>
            <TD>2012-04-19T15:26:16Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/3492&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3492</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/3492 [1]</TD>
            <TD>JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)</TD>
            <TD>Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492#1</TD>
            <TD>2012-04-19T15:26:16Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/3492</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3492</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/3492 [2]</TD>
            <TD>JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)</TD>
            <TD>Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492#2</TD>
            <TD>2012-04-19T15:26:16Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/3492&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3492</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/3492 [table2]</TD>
            <TD>JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)</TD>
            <TD>Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492#table2</TD>
            <TD>2012-04-19T15:26:16Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/3492&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3492</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/3492 [1]</TD>
            <TD>JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)</TD>
            <TD>Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492#1</TD>
            <TD>2012-04-19T15:26:16Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/3492</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3492</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/3492 [2]</TD>
            <TD>JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)</TD>
            <TD>Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492#2</TD>
            <TD>2012-04-19T15:26:16Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/3492&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3492</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/3492 [table2]</TD>
            <TD>JHKs photometry of Sculptor dSph galaxy (Menzies+, 2011)</TD>
            <TD>Observations were made with the SIRIUS camera on the Japanese-South African Infrared Survey Facility (IRSF) at SAAO, Sutherland.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492#table2</TD>
            <TD>2012-04-19T15:26:16Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3492</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/3492&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3492</TD>
          </TR>
          <TR>
            <TD>Spectra</TD>
            <TD>GALEX</TD>
            <TD>Galexy Evolution Explorer</TD>
            <TD>The Galexy Evolution Explorer (GALEX), GALEX was successfully launched on April 28, 2003. GALEX data products include a series of all sky surveys and deep sky surveys in the imaging mode and partial surveys in the near and far UV spectroscopic modes. These are respectively, the Nearby Galaxy Survey (NGS), Deep (DIS), Medium (MIS), and All Sky Surveys (AIS:imaging) and a somewhat smaller Spectroscopic (SPECTRA:imaging or "grism") survey. This service provides access to the GALEX SPECTRA survey as a 'Spectral Cutout Service' where the BAND parameter defines the region of spectra to extract for retreival. Ommitting the BAND parameter will allow for retreival of the entire spectra dataset for each object.</TD>
            <TD>MAST</TD>
            <TD>#UV#</TD>
            <TD>ivo://mast.stsci.edu/ssap/galex#1</TD>
            <TD>2010-01-06T12:14:44Z</TD>
            <TD>#UV Astronomy#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>1.0</TD>
            <TD>ivo://mast.stsci.edu/ssap/galex</TD>
            <TD>SimpleSpectralAccess</TD>
            <TD>ivo://ivoa.net/std/SSA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD>1.0</TD>
            <TD>std</TD>
            <TD>http://galex.stsci.edu/gxWS/SSAP/gxSSAP.aspx?</TD>
            <TD>180.0</TD>
            <TD>0</TD>
            <TD />
            <TD>http://archive.stsci.edu/</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/176/374 [1]</TD>
            <TD>WARPS-II Cluster catalog. VII. (Horner+, 2008)</TD>
            <TD>We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7deg^2^. Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z=0.029 to z=0.92 with a median redshift of z=0.29 and find 59 clusters with z&gt;=0.3 (29 not previously reported in the literature) and 11 clusters with z&gt;=0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5x10^-14^ergs/cm^2^/s (0.5-2.0keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374#1</TD>
            <TD>2011-09-14T20:36:16Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/176/374</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/374</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/176/374 [2]</TD>
            <TD>WARPS-II Cluster catalog. VII. (Horner+, 2008)</TD>
            <TD>We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7deg^2^. Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z=0.029 to z=0.92 with a median redshift of z=0.29 and find 59 clusters with z&gt;=0.3 (29 not previously reported in the literature) and 11 clusters with z&gt;=0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5x10^-14^ergs/cm^2^/s (0.5-2.0keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374#2</TD>
            <TD>2011-09-14T20:36:16Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/176/374&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/374</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/176/374 [warps]</TD>
            <TD>WARPS-II Cluster catalog. VII. (Horner+, 2008)</TD>
            <TD>We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7deg^2^. Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z=0.029 to z=0.92 with a median redshift of z=0.29 and find 59 clusters with z&gt;=0.3 (29 not previously reported in the literature) and 11 clusters with z&gt;=0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5x10^-14^ergs/cm^2^/s (0.5-2.0keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374#warps</TD>
            <TD>2011-09-14T20:36:16Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/176/374&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/374</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/176/374 [1]</TD>
            <TD>WARPS-II Cluster catalog. VII. (Horner+, 2008)</TD>
            <TD>We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7deg^2^. Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z=0.029 to z=0.92 with a median redshift of z=0.29 and find 59 clusters with z&gt;=0.3 (29 not previously reported in the literature) and 11 clusters with z&gt;=0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5x10^-14^ergs/cm^2^/s (0.5-2.0keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374#1</TD>
            <TD>2011-09-14T20:36:16Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/176/374</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/374</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/176/374 [2]</TD>
            <TD>WARPS-II Cluster catalog. VII. (Horner+, 2008)</TD>
            <TD>We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7deg^2^. Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z=0.029 to z=0.92 with a median redshift of z=0.29 and find 59 clusters with z&gt;=0.3 (29 not previously reported in the literature) and 11 clusters with z&gt;=0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5x10^-14^ergs/cm^2^/s (0.5-2.0keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374#2</TD>
            <TD>2011-09-14T20:36:16Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/176/374&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/374</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/176/374 [warps]</TD>
            <TD>WARPS-II Cluster catalog. VII. (Horner+, 2008)</TD>
            <TD>We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7deg^2^. Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z=0.029 to z=0.92 with a median redshift of z=0.29 and find 59 clusters with z&gt;=0.3 (29 not previously reported in the literature) and 11 clusters with z&gt;=0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5x10^-14^ergs/cm^2^/s (0.5-2.0keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374#warps</TD>
            <TD>2011-09-14T20:36:16Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/176/374&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/374</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/176/374 [1]</TD>
            <TD>WARPS-II Cluster catalog. VII. (Horner+, 2008)</TD>
            <TD>We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7deg^2^. Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z=0.029 to z=0.92 with a median redshift of z=0.29 and find 59 clusters with z&gt;=0.3 (29 not previously reported in the literature) and 11 clusters with z&gt;=0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5x10^-14^ergs/cm^2^/s (0.5-2.0keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374#1</TD>
            <TD>2011-09-14T20:36:16Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/176/374</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/374</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/176/374 [2]</TD>
            <TD>WARPS-II Cluster catalog. VII. (Horner+, 2008)</TD>
            <TD>We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7deg^2^. Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z=0.029 to z=0.92 with a median redshift of z=0.29 and find 59 clusters with z&gt;=0.3 (29 not previously reported in the literature) and 11 clusters with z&gt;=0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5x10^-14^ergs/cm^2^/s (0.5-2.0keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374#2</TD>
            <TD>2011-09-14T20:36:16Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/176/374&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/374</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/176/374 [warps]</TD>
            <TD>WARPS-II Cluster catalog. VII. (Horner+, 2008)</TD>
            <TD>We present the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7deg^2^. Of these 125 clusters, 53 have not been previously reported in the literature. We have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z=0.029 to z=0.92 with a median redshift of z=0.29 and find 59 clusters with z&gt;=0.3 (29 not previously reported in the literature) and 11 clusters with z&gt;=0.6 (6 not previously reported). We also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5x10^-14^ergs/cm^2^/s (0.5-2.0keV). Here we provide the cluster catalog and finder charts consisting of X-ray overlays on optical CCD images. We also compare our redshifts, fluxes, and detection methods to other similar published cluster surveys and find no serious issues with our measurements or completeness.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374#warps</TD>
            <TD>2011-09-14T20:36:16Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/374</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/176/374&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/374</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/660/146 [1]</TD>
            <TD>HE 1104-1805 differential light curves (Poindexter+, 2007)</TD>
            <TD>HE 1104-1805 was originally observed with HST by Lehar et al. (2000ApJ...536..584L), but we obtained deeper NICMOS NIC2 F160W (H band) observations as part of GO-9375 on 2003 December 17 (HJD 2452990.9), with the aim of improving the lens galaxy astrometry and profile and studying the quasar host galaxy. We observed HE 1104-1805 with Spitzer and the Infrared Array Camera (IRAC) on 2005 June 15 and 2006 January 2 as part of Spitzer program 20451.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/146#1</TD>
            <TD>2011-09-14T20:42:40Z</TD>
            <TD>#Photometry#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/146</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/660/146</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/146</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/660/146 [2]</TD>
            <TD>HE 1104-1805 differential light curves (Poindexter+, 2007)</TD>
            <TD>HE 1104-1805 was originally observed with HST by Lehar et al. (2000ApJ...536..584L), but we obtained deeper NICMOS NIC2 F160W (H band) observations as part of GO-9375 on 2003 December 17 (HJD 2452990.9), with the aim of improving the lens galaxy astrometry and profile and studying the quasar host galaxy. We observed HE 1104-1805 with Spitzer and the Infrared Array Camera (IRAC) on 2005 June 15 and 2006 January 2 as part of Spitzer program 20451.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/146#2</TD>
            <TD>2011-09-14T20:42:40Z</TD>
            <TD>#Photometry#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/146</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/660/146&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/146</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/660/146 [1]</TD>
            <TD>HE 1104-1805 differential light curves (Poindexter+, 2007)</TD>
            <TD>HE 1104-1805 was originally observed with HST by Lehar et al. (2000ApJ...536..584L), but we obtained deeper NICMOS NIC2 F160W (H band) observations as part of GO-9375 on 2003 December 17 (HJD 2452990.9), with the aim of improving the lens galaxy astrometry and profile and studying the quasar host galaxy. We observed HE 1104-1805 with Spitzer and the Infrared Array Camera (IRAC) on 2005 June 15 and 2006 January 2 as part of Spitzer program 20451.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/146#1</TD>
            <TD>2011-09-14T20:42:40Z</TD>
            <TD>#Photometry#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/146</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/660/146</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/146</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/660/146 [2]</TD>
            <TD>HE 1104-1805 differential light curves (Poindexter+, 2007)</TD>
            <TD>HE 1104-1805 was originally observed with HST by Lehar et al. (2000ApJ...536..584L), but we obtained deeper NICMOS NIC2 F160W (H band) observations as part of GO-9375 on 2003 December 17 (HJD 2452990.9), with the aim of improving the lens galaxy astrometry and profile and studying the quasar host galaxy. We observed HE 1104-1805 with Spitzer and the Infrared Array Camera (IRAC) on 2005 June 15 and 2006 January 2 as part of Spitzer program 20451.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/146#2</TD>
            <TD>2011-09-14T20:42:40Z</TD>
            <TD>#Photometry#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/146</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/660/146&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/146</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/662/224 [1]</TD>
            <TD>Second CIZA subsample (Kocevski+, 2007)</TD>
            <TD>The CIZA survey is the first systematic search for X-ray-luminous galaxy clusters behind the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224#1</TD>
            <TD>2011-09-14T20:46:05Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/662/224</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/224</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/662/224 [2]</TD>
            <TD>Second CIZA subsample (Kocevski+, 2007)</TD>
            <TD>The CIZA survey is the first systematic search for X-ray-luminous galaxy clusters behind the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224#2</TD>
            <TD>2011-09-14T20:46:05Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/662/224&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/224</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/662/224 [table2]</TD>
            <TD>Second CIZA subsample (Kocevski+, 2007)</TD>
            <TD>The CIZA survey is the first systematic search for X-ray-luminous galaxy clusters behind the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224#table2</TD>
            <TD>2011-09-14T20:46:05Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/662/224&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/224</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/134 [1]</TD>
            <TD>Atlas of Radio/X-ray associations (ARXA) (Flesch, 2010)</TD>
            <TD>This is a compendium of all catalogued or APM/USNO-A optical objects which are found to be associated to XMM, Chandra, RASS, HRI, PSPC or WGA X-ray detections, or to NVSS, FIRST or SUMSS radio detections. All detections are displayed, plus double radio lobes where found. The counts are: Optical objects - 602,570 NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778 Chandra associations - 32,951 ROSAT RASS - 47,486 ROSAT HRI - 15,523 ROSAT PSPC - 35,607 WGA - 24,226 Each optical object is shown as one line bearing the J2000 coordinates, the object name (from the literature where available), APM &amp; USNO-A sourced red &amp; blue photometry, redshift, the source catalogs for the name and redshift, calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. Questions or comments may be directed to eric@flesch.org.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/134#1</TD>
            <TD>2011-09-14T20:52:45Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/V/134</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/134</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/134</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/134 [2]</TD>
            <TD>Atlas of Radio/X-ray associations (ARXA) (Flesch, 2010)</TD>
            <TD>This is a compendium of all catalogued or APM/USNO-A optical objects which are found to be associated to XMM, Chandra, RASS, HRI, PSPC or WGA X-ray detections, or to NVSS, FIRST or SUMSS radio detections. All detections are displayed, plus double radio lobes where found. The counts are: Optical objects - 602,570 NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778 Chandra associations - 32,951 ROSAT RASS - 47,486 ROSAT HRI - 15,523 ROSAT PSPC - 35,607 WGA - 24,226 Each optical object is shown as one line bearing the J2000 coordinates, the object name (from the literature where available), APM &amp; USNO-A sourced red &amp; blue photometry, redshift, the source catalogs for the name and redshift, calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. Questions or comments may be directed to eric@flesch.org.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/134#2</TD>
            <TD>2011-09-14T20:52:45Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/V/134</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/134&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/134</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/134 [arxa]</TD>
            <TD>Atlas of Radio/X-ray associations (ARXA) (Flesch, 2010)</TD>
            <TD>This is a compendium of all catalogued or APM/USNO-A optical objects which are found to be associated to XMM, Chandra, RASS, HRI, PSPC or WGA X-ray detections, or to NVSS, FIRST or SUMSS radio detections. All detections are displayed, plus double radio lobes where found. The counts are: Optical objects - 602,570 NVSS - 266,148 core associations, plus 8309 double lobes. FIRST - 173,383 core associations, plus 12,844 double lobes. SUMSS - 59,138 core associations, plus 2529 double lobes. XMM associations - 57,778 Chandra associations - 32,951 ROSAT RASS - 47,486 ROSAT HRI - 15,523 ROSAT PSPC - 35,607 WGA - 24,226 Each optical object is shown as one line bearing the J2000 coordinates, the object name (from the literature where available), APM &amp; USNO-A sourced red &amp; blue photometry, redshift, the source catalogs for the name and redshift, calculated odds that the object is a quasar, galaxy, star, or erroneous association, and the radio &amp; X-ray identifiers, up to 10 of them possible although usually just 1 or 2. Questions or comments may be directed to eric@flesch.org.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Radio#</TD>
            <TD>ivo://CDS.VizieR/V/134#arxa</TD>
            <TD>2011-09-14T20:52:45Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/V/134</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/134&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/134</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/662/224 [1]</TD>
            <TD>Second CIZA subsample (Kocevski+, 2007)</TD>
            <TD>The CIZA survey is the first systematic search for X-ray-luminous galaxy clusters behind the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224#1</TD>
            <TD>2011-09-14T20:46:05Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/662/224</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/224</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/662/224 [2]</TD>
            <TD>Second CIZA subsample (Kocevski+, 2007)</TD>
            <TD>The CIZA survey is the first systematic search for X-ray-luminous galaxy clusters behind the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224#2</TD>
            <TD>2011-09-14T20:46:05Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/662/224&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/224</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/662/224 [table2]</TD>
            <TD>Second CIZA subsample (Kocevski+, 2007)</TD>
            <TD>The CIZA survey is the first systematic search for X-ray-luminous galaxy clusters behind the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224#table2</TD>
            <TD>2011-09-14T20:46:05Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/662/224&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/224</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/662/224 [1]</TD>
            <TD>Second CIZA subsample (Kocevski+, 2007)</TD>
            <TD>The CIZA survey is the first systematic search for X-ray-luminous galaxy clusters behind the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224#1</TD>
            <TD>2011-09-14T20:46:05Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/662/224</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/224</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/662/224 [2]</TD>
            <TD>Second CIZA subsample (Kocevski+, 2007)</TD>
            <TD>The CIZA survey is the first systematic search for X-ray-luminous galaxy clusters behind the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224#2</TD>
            <TD>2011-09-14T20:46:05Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/662/224&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/224</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/662/224 [table2]</TD>
            <TD>Second CIZA subsample (Kocevski+, 2007)</TD>
            <TD>The CIZA survey is the first systematic search for X-ray-luminous galaxy clusters behind the Galactic plane.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224#table2</TD>
            <TD>2011-09-14T20:46:05Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/224</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/662/224&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/224</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/682/964 [1]</TD>
            <TD>Sloan lens ACS survey. V. (Bolton+, 2008)</TD>
            <TD>The gravitational lenses presented in this work were all selected from the spectroscopic database of the SDSS based on the presence of absorption-dominated galaxy continuum at one redshift and nebular emission lines (Balmer series, [OII] 3727, or [OIII] 5007) at another, higher redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964#1</TD>
            <TD>2011-09-14T20:47:25Z</TD>
            <TD>#Gravitational_lensing#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/682/964</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/964</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/682/964 [2]</TD>
            <TD>Sloan lens ACS survey. V. (Bolton+, 2008)</TD>
            <TD>The gravitational lenses presented in this work were all selected from the spectroscopic database of the SDSS based on the presence of absorption-dominated galaxy continuum at one redshift and nebular emission lines (Balmer series, [OII] 3727, or [OIII] 5007) at another, higher redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964#2</TD>
            <TD>2011-09-14T20:47:25Z</TD>
            <TD>#Gravitational_lensing#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/682/964&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/964</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/682/964 [table4]</TD>
            <TD>Sloan lens ACS survey. V. (Bolton+, 2008)</TD>
            <TD>The gravitational lenses presented in this work were all selected from the spectroscopic database of the SDSS based on the presence of absorption-dominated galaxy continuum at one redshift and nebular emission lines (Balmer series, [OII] 3727, or [OIII] 5007) at another, higher redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964#table4</TD>
            <TD>2011-09-14T20:47:25Z</TD>
            <TD>#Gravitational_lensing#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/682/964&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/964</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/682/964 [1]</TD>
            <TD>Sloan lens ACS survey. V. (Bolton+, 2008)</TD>
            <TD>The gravitational lenses presented in this work were all selected from the spectroscopic database of the SDSS based on the presence of absorption-dominated galaxy continuum at one redshift and nebular emission lines (Balmer series, [OII] 3727, or [OIII] 5007) at another, higher redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964#1</TD>
            <TD>2011-09-14T20:47:25Z</TD>
            <TD>#Gravitational_lensing#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/682/964</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/964</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/682/964 [2]</TD>
            <TD>Sloan lens ACS survey. V. (Bolton+, 2008)</TD>
            <TD>The gravitational lenses presented in this work were all selected from the spectroscopic database of the SDSS based on the presence of absorption-dominated galaxy continuum at one redshift and nebular emission lines (Balmer series, [OII] 3727, or [OIII] 5007) at another, higher redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964#2</TD>
            <TD>2011-09-14T20:47:25Z</TD>
            <TD>#Gravitational_lensing#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/682/964&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/964</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/682/964 [table4]</TD>
            <TD>Sloan lens ACS survey. V. (Bolton+, 2008)</TD>
            <TD>The gravitational lenses presented in this work were all selected from the spectroscopic database of the SDSS based on the presence of absorption-dominated galaxy continuum at one redshift and nebular emission lines (Balmer series, [OII] 3727, or [OIII] 5007) at another, higher redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964#table4</TD>
            <TD>2011-09-14T20:47:25Z</TD>
            <TD>#Gravitational_lensing#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/682/964&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/964</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/682/964 [1]</TD>
            <TD>Sloan lens ACS survey. V. (Bolton+, 2008)</TD>
            <TD>The gravitational lenses presented in this work were all selected from the spectroscopic database of the SDSS based on the presence of absorption-dominated galaxy continuum at one redshift and nebular emission lines (Balmer series, [OII] 3727, or [OIII] 5007) at another, higher redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964#1</TD>
            <TD>2011-09-14T20:47:25Z</TD>
            <TD>#Gravitational_lensing#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/682/964</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/964</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/682/964 [2]</TD>
            <TD>Sloan lens ACS survey. V. (Bolton+, 2008)</TD>
            <TD>The gravitational lenses presented in this work were all selected from the spectroscopic database of the SDSS based on the presence of absorption-dominated galaxy continuum at one redshift and nebular emission lines (Balmer series, [OII] 3727, or [OIII] 5007) at another, higher redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964#2</TD>
            <TD>2011-09-14T20:47:25Z</TD>
            <TD>#Gravitational_lensing#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/682/964&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/964</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/682/964 [table4]</TD>
            <TD>Sloan lens ACS survey. V. (Bolton+, 2008)</TD>
            <TD>The gravitational lenses presented in this work were all selected from the spectroscopic database of the SDSS based on the presence of absorption-dominated galaxy continuum at one redshift and nebular emission lines (Balmer series, [OII] 3727, or [OIII] 5007) at another, higher redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964#table4</TD>
            <TD>2011-09-14T20:47:25Z</TD>
            <TD>#Gravitational_lensing#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/682/964</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/682/964&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/682/964</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/176/414 [1]</TD>
            <TD>Galaxy clusters in the SDSS-DR5 (Yoon+, 2008)</TD>
            <TD>Recent large-scale galaxy spectroscopic surveys, such as the Sloan Digital Sky Survey (SDSS), enable us to execute a systematic, relatively unbiased search for galaxy clusters. Such surveys make it possible to measure the 3D distribution of galaxies but are hampered by the incompleteness problem due to fiber collisions. In this study we aim to develop a density-measuring technique that alleviates the problem and derives densities more accurately by adding additional cluster member galaxies that follow optical color-magnitude relations for the given redshift. The new density measured with both spectroscopic and photometric data shows a good agreement with apparent information on cluster images and is supported by follow-up observations. By adopting this new method, a total of 924 robust galaxy clusters are found from the SDSS DR5 database in the redshift range 0.05&lt;z&lt;0.1, of which 212 are new. Local maximum-density galaxies successfully represent cluster centers. We provide the cluster catalog including a number of cluster parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414#1</TD>
            <TD>2011-09-14T20:47:49Z</TD>
            <TD>#Clusters_of_galaxies#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/176/414</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/414</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/176/414 [2]</TD>
            <TD>Galaxy clusters in the SDSS-DR5 (Yoon+, 2008)</TD>
            <TD>Recent large-scale galaxy spectroscopic surveys, such as the Sloan Digital Sky Survey (SDSS), enable us to execute a systematic, relatively unbiased search for galaxy clusters. Such surveys make it possible to measure the 3D distribution of galaxies but are hampered by the incompleteness problem due to fiber collisions. In this study we aim to develop a density-measuring technique that alleviates the problem and derives densities more accurately by adding additional cluster member galaxies that follow optical color-magnitude relations for the given redshift. The new density measured with both spectroscopic and photometric data shows a good agreement with apparent information on cluster images and is supported by follow-up observations. By adopting this new method, a total of 924 robust galaxy clusters are found from the SDSS DR5 database in the redshift range 0.05&lt;z&lt;0.1, of which 212 are new. Local maximum-density galaxies successfully represent cluster centers. We provide the cluster catalog including a number of cluster parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414#2</TD>
            <TD>2011-09-14T20:47:49Z</TD>
            <TD>#Clusters_of_galaxies#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/176/414&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/414</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/176/414 [table1]</TD>
            <TD>Galaxy clusters in the SDSS-DR5 (Yoon+, 2008)</TD>
            <TD>Recent large-scale galaxy spectroscopic surveys, such as the Sloan Digital Sky Survey (SDSS), enable us to execute a systematic, relatively unbiased search for galaxy clusters. Such surveys make it possible to measure the 3D distribution of galaxies but are hampered by the incompleteness problem due to fiber collisions. In this study we aim to develop a density-measuring technique that alleviates the problem and derives densities more accurately by adding additional cluster member galaxies that follow optical color-magnitude relations for the given redshift. The new density measured with both spectroscopic and photometric data shows a good agreement with apparent information on cluster images and is supported by follow-up observations. By adopting this new method, a total of 924 robust galaxy clusters are found from the SDSS DR5 database in the redshift range 0.05&lt;z&lt;0.1, of which 212 are new. Local maximum-density galaxies successfully represent cluster centers. We provide the cluster catalog including a number of cluster parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414#table1</TD>
            <TD>2011-09-14T20:47:49Z</TD>
            <TD>#Clusters_of_galaxies#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/176/414&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/414</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/176/414 [1]</TD>
            <TD>Galaxy clusters in the SDSS-DR5 (Yoon+, 2008)</TD>
            <TD>Recent large-scale galaxy spectroscopic surveys, such as the Sloan Digital Sky Survey (SDSS), enable us to execute a systematic, relatively unbiased search for galaxy clusters. Such surveys make it possible to measure the 3D distribution of galaxies but are hampered by the incompleteness problem due to fiber collisions. In this study we aim to develop a density-measuring technique that alleviates the problem and derives densities more accurately by adding additional cluster member galaxies that follow optical color-magnitude relations for the given redshift. The new density measured with both spectroscopic and photometric data shows a good agreement with apparent information on cluster images and is supported by follow-up observations. By adopting this new method, a total of 924 robust galaxy clusters are found from the SDSS DR5 database in the redshift range 0.05&lt;z&lt;0.1, of which 212 are new. Local maximum-density galaxies successfully represent cluster centers. We provide the cluster catalog including a number of cluster parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414#1</TD>
            <TD>2011-09-14T20:47:49Z</TD>
            <TD>#Clusters_of_galaxies#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/176/414</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/414</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/176/414 [2]</TD>
            <TD>Galaxy clusters in the SDSS-DR5 (Yoon+, 2008)</TD>
            <TD>Recent large-scale galaxy spectroscopic surveys, such as the Sloan Digital Sky Survey (SDSS), enable us to execute a systematic, relatively unbiased search for galaxy clusters. Such surveys make it possible to measure the 3D distribution of galaxies but are hampered by the incompleteness problem due to fiber collisions. In this study we aim to develop a density-measuring technique that alleviates the problem and derives densities more accurately by adding additional cluster member galaxies that follow optical color-magnitude relations for the given redshift. The new density measured with both spectroscopic and photometric data shows a good agreement with apparent information on cluster images and is supported by follow-up observations. By adopting this new method, a total of 924 robust galaxy clusters are found from the SDSS DR5 database in the redshift range 0.05&lt;z&lt;0.1, of which 212 are new. Local maximum-density galaxies successfully represent cluster centers. We provide the cluster catalog including a number of cluster parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414#2</TD>
            <TD>2011-09-14T20:47:49Z</TD>
            <TD>#Clusters_of_galaxies#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/176/414&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/414</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/176/414 [table1]</TD>
            <TD>Galaxy clusters in the SDSS-DR5 (Yoon+, 2008)</TD>
            <TD>Recent large-scale galaxy spectroscopic surveys, such as the Sloan Digital Sky Survey (SDSS), enable us to execute a systematic, relatively unbiased search for galaxy clusters. Such surveys make it possible to measure the 3D distribution of galaxies but are hampered by the incompleteness problem due to fiber collisions. In this study we aim to develop a density-measuring technique that alleviates the problem and derives densities more accurately by adding additional cluster member galaxies that follow optical color-magnitude relations for the given redshift. The new density measured with both spectroscopic and photometric data shows a good agreement with apparent information on cluster images and is supported by follow-up observations. By adopting this new method, a total of 924 robust galaxy clusters are found from the SDSS DR5 database in the redshift range 0.05&lt;z&lt;0.1, of which 212 are new. Local maximum-density galaxies successfully represent cluster centers. We provide the cluster catalog including a number of cluster parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414#table1</TD>
            <TD>2011-09-14T20:47:49Z</TD>
            <TD>#Clusters_of_galaxies#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/176/414&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/414</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/176/414 [1]</TD>
            <TD>Galaxy clusters in the SDSS-DR5 (Yoon+, 2008)</TD>
            <TD>Recent large-scale galaxy spectroscopic surveys, such as the Sloan Digital Sky Survey (SDSS), enable us to execute a systematic, relatively unbiased search for galaxy clusters. Such surveys make it possible to measure the 3D distribution of galaxies but are hampered by the incompleteness problem due to fiber collisions. In this study we aim to develop a density-measuring technique that alleviates the problem and derives densities more accurately by adding additional cluster member galaxies that follow optical color-magnitude relations for the given redshift. The new density measured with both spectroscopic and photometric data shows a good agreement with apparent information on cluster images and is supported by follow-up observations. By adopting this new method, a total of 924 robust galaxy clusters are found from the SDSS DR5 database in the redshift range 0.05&lt;z&lt;0.1, of which 212 are new. Local maximum-density galaxies successfully represent cluster centers. We provide the cluster catalog including a number of cluster parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414#1</TD>
            <TD>2011-09-14T20:47:49Z</TD>
            <TD>#Clusters_of_galaxies#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/176/414</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/414</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/176/414 [2]</TD>
            <TD>Galaxy clusters in the SDSS-DR5 (Yoon+, 2008)</TD>
            <TD>Recent large-scale galaxy spectroscopic surveys, such as the Sloan Digital Sky Survey (SDSS), enable us to execute a systematic, relatively unbiased search for galaxy clusters. Such surveys make it possible to measure the 3D distribution of galaxies but are hampered by the incompleteness problem due to fiber collisions. In this study we aim to develop a density-measuring technique that alleviates the problem and derives densities more accurately by adding additional cluster member galaxies that follow optical color-magnitude relations for the given redshift. The new density measured with both spectroscopic and photometric data shows a good agreement with apparent information on cluster images and is supported by follow-up observations. By adopting this new method, a total of 924 robust galaxy clusters are found from the SDSS DR5 database in the redshift range 0.05&lt;z&lt;0.1, of which 212 are new. Local maximum-density galaxies successfully represent cluster centers. We provide the cluster catalog including a number of cluster parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414#2</TD>
            <TD>2011-09-14T20:47:49Z</TD>
            <TD>#Clusters_of_galaxies#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/176/414&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/414</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/176/414 [table1]</TD>
            <TD>Galaxy clusters in the SDSS-DR5 (Yoon+, 2008)</TD>
            <TD>Recent large-scale galaxy spectroscopic surveys, such as the Sloan Digital Sky Survey (SDSS), enable us to execute a systematic, relatively unbiased search for galaxy clusters. Such surveys make it possible to measure the 3D distribution of galaxies but are hampered by the incompleteness problem due to fiber collisions. In this study we aim to develop a density-measuring technique that alleviates the problem and derives densities more accurately by adding additional cluster member galaxies that follow optical color-magnitude relations for the given redshift. The new density measured with both spectroscopic and photometric data shows a good agreement with apparent information on cluster images and is supported by follow-up observations. By adopting this new method, a total of 924 robust galaxy clusters are found from the SDSS DR5 database in the redshift range 0.05&lt;z&lt;0.1, of which 212 are new. Local maximum-density galaxies successfully represent cluster centers. We provide the cluster catalog including a number of cluster parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414#table1</TD>
            <TD>2011-09-14T20:47:49Z</TD>
            <TD>#Clusters_of_galaxies#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/176/414</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/176/414&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/176/414</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/449/592 [1]</TD>
            <TD>NGC 5128 PN. III. (Hui+ 1995)</TD>
            <TD>We present a study of the halo dynamics and mass distributions of the nearby giant elliptical galaxy NGC 5128 using planetary nebulae (PNs) as test particles. Radial velocities of 433 PNs were obtained with multifiber spectrographs on both the Anglo-Australian Telescope (AAT) and the Cerro Tololo Inter-American Observatory (CTIO) 4m telescope. The velocities were measured from the [O III]{lambda}5007 emission line with a typical 1{sigma} error of +/-4km/s and +/-30km/s for the AAT and the CTIO data, respectively. These PNs cover the entire galaxy to a radius of 10kpc and extend along the photometric major axis out to 20kpc. The PN velocity field shows the distinctive characteristics of a triaxial potential: the galaxy's rotation axis is offset from its photometric minor axis by 39+/-10deg; the rotation axis and the line of maximum rotation are likely not orthogonal. We also find that the ordered motions of the stars become more important with increasing radius compared to their random motions. The rotation reaches approximately 100km/s and 50km/s along the photometric major and minor axes, giving a local V/{sigma} ratio of about 1.0 and 0.5, respectively. The aximuthal variation of the velocity dispersion appears to be modulated by rotation, i.e., it reaches a maximum where the largest rotation is observed and drops to a minimum at zero rotation. The amplitude of this modulation is about 20km/s, compared to a mean dispersion velocity of 110km/s. The kinematics of the globular clusters depend on the metallicity. Taking [Fe/H]=-1.0 as the dividing point, the metal-poor clusters do not show any significant rotation. However the metal-rich clusters show both major and minor axis rotation, and the amplitudes of the rotation are similar to that of the PNs. The stellar velocity dispersion measured from absorption-line spectra together with an H{alpha} rotation curve of the dust lane suggest that the stellar orbits are isotropic and the mass-to-light ratio (M/L_B_) is 3.9 in the central region of the galaxy. By applying the isotropic Jeans equation to the observed PN major axis rotation and velocity dispersion, we show that the M/L_B_ increases with radius, suggesting the presence of dark matter in the halo. Within a 25kpc radius, the total mass of the galaxy is 3.1x10^11^M_{sun}_ and M/L_B_=10. The rotation velocity of the recently detected H I ring at a radius of 15kpc confirms our mass model. The misalignment of the rotation axis relative to the photometric minor axis, combined with the knowledge of the dust lane orientation, allows us to uniquely determine the observer's viewing direction. The true shape of the galaxy is nearly spherical yet sufficiently triaxial to impose a distinctive gravitational signature on the kinematics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/592#1</TD>
            <TD>2011-09-14T18:23:30Z</TD>
            <TD>#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/592</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/449/592</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/592</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/449/592 [2]</TD>
            <TD>NGC 5128 PN. III. (Hui+ 1995)</TD>
            <TD>We present a study of the halo dynamics and mass distributions of the nearby giant elliptical galaxy NGC 5128 using planetary nebulae (PNs) as test particles. Radial velocities of 433 PNs were obtained with multifiber spectrographs on both the Anglo-Australian Telescope (AAT) and the Cerro Tololo Inter-American Observatory (CTIO) 4m telescope. The velocities were measured from the [O III]{lambda}5007 emission line with a typical 1{sigma} error of +/-4km/s and +/-30km/s for the AAT and the CTIO data, respectively. These PNs cover the entire galaxy to a radius of 10kpc and extend along the photometric major axis out to 20kpc. The PN velocity field shows the distinctive characteristics of a triaxial potential: the galaxy's rotation axis is offset from its photometric minor axis by 39+/-10deg; the rotation axis and the line of maximum rotation are likely not orthogonal. We also find that the ordered motions of the stars become more important with increasing radius compared to their random motions. The rotation reaches approximately 100km/s and 50km/s along the photometric major and minor axes, giving a local V/{sigma} ratio of about 1.0 and 0.5, respectively. The aximuthal variation of the velocity dispersion appears to be modulated by rotation, i.e., it reaches a maximum where the largest rotation is observed and drops to a minimum at zero rotation. The amplitude of this modulation is about 20km/s, compared to a mean dispersion velocity of 110km/s. The kinematics of the globular clusters depend on the metallicity. Taking [Fe/H]=-1.0 as the dividing point, the metal-poor clusters do not show any significant rotation. However the metal-rich clusters show both major and minor axis rotation, and the amplitudes of the rotation are similar to that of the PNs. The stellar velocity dispersion measured from absorption-line spectra together with an H{alpha} rotation curve of the dust lane suggest that the stellar orbits are isotropic and the mass-to-light ratio (M/L_B_) is 3.9 in the central region of the galaxy. By applying the isotropic Jeans equation to the observed PN major axis rotation and velocity dispersion, we show that the M/L_B_ increases with radius, suggesting the presence of dark matter in the halo. Within a 25kpc radius, the total mass of the galaxy is 3.1x10^11^M_{sun}_ and M/L_B_=10. The rotation velocity of the recently detected H I ring at a radius of 15kpc confirms our mass model. The misalignment of the rotation axis relative to the photometric minor axis, combined with the knowledge of the dust lane orientation, allows us to uniquely determine the observer's viewing direction. The true shape of the galaxy is nearly spherical yet sufficiently triaxial to impose a distinctive gravitational signature on the kinematics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/592#2</TD>
            <TD>2011-09-14T18:23:30Z</TD>
            <TD>#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/592</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/449/592&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/592</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/897 [1]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#1</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/897</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/897 [2]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#2</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/897&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/897 [table1]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#table1</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/897&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/897 [table2]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#table2</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/897&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/897 [1]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#1</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/897</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/897 [2]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#2</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/897&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/897 [table1]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#table1</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/897&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/897 [table2]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#table2</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/897&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/897 [1]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#1</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/897</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/897 [2]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#2</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/897&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/897 [table1]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#table1</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/897&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/897 [table2]</TD>
            <TD>Radio sources toward galaxy clusters at 30GHz (Coble+, 2007)</TD>
            <TD>The 28.5GHz observations were carried out with BIMA during the summers of 1996-2002 and OVRO during the summers of 1995-2001 as part of the OVRO/BIMA SZE imaging project (see, e.g., Reese et al., 2002ApJ...581...53R and Grego et al., 2001ApJ...552....2G). A total of 62 cluster fields were observed at BIMA, and 55 cluster fields were observed at OVRO. A total of 28 cluster fields were observed at both BIMA and OVRO, yielding observations of 89 unique cluster fields. For the BIMA CMB fine-scale anisotropy project (Dawson et al., 2002ApJ...581...86D, 2006, Cat. &lt;J/ApJ/647/13&gt;), a total of 18 noncluster fields were observed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897#table2</TD>
            <TD>2011-09-14T20:47:51Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/897</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/897&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/897</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/449/592 [1]</TD>
            <TD>NGC 5128 PN. III. (Hui+ 1995)</TD>
            <TD>We present a study of the halo dynamics and mass distributions of the nearby giant elliptical galaxy NGC 5128 using planetary nebulae (PNs) as test particles. Radial velocities of 433 PNs were obtained with multifiber spectrographs on both the Anglo-Australian Telescope (AAT) and the Cerro Tololo Inter-American Observatory (CTIO) 4m telescope. The velocities were measured from the [O III]{lambda}5007 emission line with a typical 1{sigma} error of +/-4km/s and +/-30km/s for the AAT and the CTIO data, respectively. These PNs cover the entire galaxy to a radius of 10kpc and extend along the photometric major axis out to 20kpc. The PN velocity field shows the distinctive characteristics of a triaxial potential: the galaxy's rotation axis is offset from its photometric minor axis by 39+/-10deg; the rotation axis and the line of maximum rotation are likely not orthogonal. We also find that the ordered motions of the stars become more important with increasing radius compared to their random motions. The rotation reaches approximately 100km/s and 50km/s along the photometric major and minor axes, giving a local V/{sigma} ratio of about 1.0 and 0.5, respectively. The aximuthal variation of the velocity dispersion appears to be modulated by rotation, i.e., it reaches a maximum where the largest rotation is observed and drops to a minimum at zero rotation. The amplitude of this modulation is about 20km/s, compared to a mean dispersion velocity of 110km/s. The kinematics of the globular clusters depend on the metallicity. Taking [Fe/H]=-1.0 as the dividing point, the metal-poor clusters do not show any significant rotation. However the metal-rich clusters show both major and minor axis rotation, and the amplitudes of the rotation are similar to that of the PNs. The stellar velocity dispersion measured from absorption-line spectra together with an H{alpha} rotation curve of the dust lane suggest that the stellar orbits are isotropic and the mass-to-light ratio (M/L_B_) is 3.9 in the central region of the galaxy. By applying the isotropic Jeans equation to the observed PN major axis rotation and velocity dispersion, we show that the M/L_B_ increases with radius, suggesting the presence of dark matter in the halo. Within a 25kpc radius, the total mass of the galaxy is 3.1x10^11^M_{sun}_ and M/L_B_=10. The rotation velocity of the recently detected H I ring at a radius of 15kpc confirms our mass model. The misalignment of the rotation axis relative to the photometric minor axis, combined with the knowledge of the dust lane orientation, allows us to uniquely determine the observer's viewing direction. The true shape of the galaxy is nearly spherical yet sufficiently triaxial to impose a distinctive gravitational signature on the kinematics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/592#1</TD>
            <TD>2011-09-14T18:23:30Z</TD>
            <TD>#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/592</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/449/592</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/592</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/449/592 [2]</TD>
            <TD>NGC 5128 PN. III. (Hui+ 1995)</TD>
            <TD>We present a study of the halo dynamics and mass distributions of the nearby giant elliptical galaxy NGC 5128 using planetary nebulae (PNs) as test particles. Radial velocities of 433 PNs were obtained with multifiber spectrographs on both the Anglo-Australian Telescope (AAT) and the Cerro Tololo Inter-American Observatory (CTIO) 4m telescope. The velocities were measured from the [O III]{lambda}5007 emission line with a typical 1{sigma} error of +/-4km/s and +/-30km/s for the AAT and the CTIO data, respectively. These PNs cover the entire galaxy to a radius of 10kpc and extend along the photometric major axis out to 20kpc. The PN velocity field shows the distinctive characteristics of a triaxial potential: the galaxy's rotation axis is offset from its photometric minor axis by 39+/-10deg; the rotation axis and the line of maximum rotation are likely not orthogonal. We also find that the ordered motions of the stars become more important with increasing radius compared to their random motions. The rotation reaches approximately 100km/s and 50km/s along the photometric major and minor axes, giving a local V/{sigma} ratio of about 1.0 and 0.5, respectively. The aximuthal variation of the velocity dispersion appears to be modulated by rotation, i.e., it reaches a maximum where the largest rotation is observed and drops to a minimum at zero rotation. The amplitude of this modulation is about 20km/s, compared to a mean dispersion velocity of 110km/s. The kinematics of the globular clusters depend on the metallicity. Taking [Fe/H]=-1.0 as the dividing point, the metal-poor clusters do not show any significant rotation. However the metal-rich clusters show both major and minor axis rotation, and the amplitudes of the rotation are similar to that of the PNs. The stellar velocity dispersion measured from absorption-line spectra together with an H{alpha} rotation curve of the dust lane suggest that the stellar orbits are isotropic and the mass-to-light ratio (M/L_B_) is 3.9 in the central region of the galaxy. By applying the isotropic Jeans equation to the observed PN major axis rotation and velocity dispersion, we show that the M/L_B_ increases with radius, suggesting the presence of dark matter in the halo. Within a 25kpc radius, the total mass of the galaxy is 3.1x10^11^M_{sun}_ and M/L_B_=10. The rotation velocity of the recently detected H I ring at a radius of 15kpc confirms our mass model. The misalignment of the rotation axis relative to the photometric minor axis, combined with the knowledge of the dust lane orientation, allows us to uniquely determine the observer's viewing direction. The true shape of the galaxy is nearly spherical yet sufficiently triaxial to impose a distinctive gravitational signature on the kinematics.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/592#2</TD>
            <TD>2011-09-14T18:23:30Z</TD>
            <TD>#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/592</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/449/592&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/592</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/447 [1]</TD>
            <TD>Catalog of star cluster candidates in M 33 (Sarajedini+, 2007)</TD>
            <TD>We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHKS filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447#1</TD>
            <TD>2011-09-14T20:49:25Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/447</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/447</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/447 [2]</TD>
            <TD>Catalog of star cluster candidates in M 33 (Sarajedini+, 2007)</TD>
            <TD>We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHKS filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447#2</TD>
            <TD>2011-09-14T20:49:25Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/447&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/447</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/447 [table3]</TD>
            <TD>Catalog of star cluster candidates in M 33 (Sarajedini+, 2007)</TD>
            <TD>We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHKS filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447#table3</TD>
            <TD>2011-09-14T20:49:25Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/447&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/447</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/452/238 [1]</TD>
            <TD>HST photometry of I Zw 18 massive stars (Hunter+ 1995)</TD>
            <TD>Blue compact dwarf galaxies are tiny galaxies that are dominated by intense star-forming regions. Thus, they have been thought to represent a different and extreme environment for star formation compared to the Milky Way and many other nearby galaxies. In this paper we use images obtained with the Hubble Space Telescope to resolve the main body of one of these galaxies, I Zw 18, into stars for the first time. This galaxy is also one of the most metal-poor galaxies known and is sometimes argued to be evolutionarily young. Broadband colors are used to determine the bulk characteristics of the resolved stellar population to an F555W magnitude of about 26, or M_(V,0)~-4 (O9.5 V star). Narrow-band images are used to look for emission characteristic of Wolf-Rayet stars. Color-magnitude diagrams reveal a broad main sequence of massive stars as well as blue and red supergiants, although there is a surprising lack of Wolf-Rayet stars. About half the massive stars are located in two groups, corresponding to the two knots of emission identified in ground-based images, and the rest are distributed between these regions and in the outer parts of the galaxy. We find that the northwestern of these two regions resolves in Halpha images into a small H II region plus a complicated shell structure that encircles the northern stellar association. There are additional, larger loops and filaments of ionized gas up to 450pc from the center of the galaxy. While the shell could be as young as the stars it encircles, the larger ionized gas structures must be older for reasonable models, and their presence implies that there has been a previous generation of massive stars at least several tens of millions of years ago. However, we find no evidence in these data for stars that must be older than this. The larger sites of most recent star formation are located northwest and south of the central part of the galaxy. Thus, we find that I Zw 18 is somewhat more complicated than had previously been thought, both in terms of its star formation history and the state of its interstellar medium. At the same time, however, the stellar populations look relatively normal, and the spatial concentration of massive stars is closer to that of large OB associations in nearby galaxies rather than to that exemplified by the compact cluster R136 in the Large Magellanic Cloud.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/452/238#1</TD>
            <TD>2011-09-14T18:23:30Z</TD>
            <TD>#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/452/238</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/452/238</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/452/238</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/452/238 [2]</TD>
            <TD>HST photometry of I Zw 18 massive stars (Hunter+ 1995)</TD>
            <TD>Blue compact dwarf galaxies are tiny galaxies that are dominated by intense star-forming regions. Thus, they have been thought to represent a different and extreme environment for star formation compared to the Milky Way and many other nearby galaxies. In this paper we use images obtained with the Hubble Space Telescope to resolve the main body of one of these galaxies, I Zw 18, into stars for the first time. This galaxy is also one of the most metal-poor galaxies known and is sometimes argued to be evolutionarily young. Broadband colors are used to determine the bulk characteristics of the resolved stellar population to an F555W magnitude of about 26, or M_(V,0)~-4 (O9.5 V star). Narrow-band images are used to look for emission characteristic of Wolf-Rayet stars. Color-magnitude diagrams reveal a broad main sequence of massive stars as well as blue and red supergiants, although there is a surprising lack of Wolf-Rayet stars. About half the massive stars are located in two groups, corresponding to the two knots of emission identified in ground-based images, and the rest are distributed between these regions and in the outer parts of the galaxy. We find that the northwestern of these two regions resolves in Halpha images into a small H II region plus a complicated shell structure that encircles the northern stellar association. There are additional, larger loops and filaments of ionized gas up to 450pc from the center of the galaxy. While the shell could be as young as the stars it encircles, the larger ionized gas structures must be older for reasonable models, and their presence implies that there has been a previous generation of massive stars at least several tens of millions of years ago. However, we find no evidence in these data for stars that must be older than this. The larger sites of most recent star formation are located northwest and south of the central part of the galaxy. Thus, we find that I Zw 18 is somewhat more complicated than had previously been thought, both in terms of its star formation history and the state of its interstellar medium. At the same time, however, the stellar populations look relatively normal, and the spatial concentration of massive stars is closer to that of large OB associations in nearby galaxies rather than to that exemplified by the compact cluster R136 in the Large Magellanic Cloud.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/452/238#2</TD>
            <TD>2011-09-14T18:23:30Z</TD>
            <TD>#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/452/238</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/452/238&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/452/238</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/619/193 [1]</TD>
            <TD>Catalog of nearby cluster galaxy photometry (McIntosh+, 2005)</TD>
            <TD>We observed clusters A85, A496, and A754 during two runs at the Kitt Peak National Observatory (KPNO) 0.9m Telescope with the NOAO Mosaic Wide-Field Imager. We used the engineering-grade Mosaic for the V data in 1997 November and the science-grade Mosaic with thinned CCDs for the U band in 2000 January.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193#1</TD>
            <TD>2011-09-14T19:44:16Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/619/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/619/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/619/193 [2]</TD>
            <TD>Catalog of nearby cluster galaxy photometry (McIntosh+, 2005)</TD>
            <TD>We observed clusters A85, A496, and A754 during two runs at the Kitt Peak National Observatory (KPNO) 0.9m Telescope with the NOAO Mosaic Wide-Field Imager. We used the engineering-grade Mosaic for the V data in 1997 November and the science-grade Mosaic with thinned CCDs for the U band in 2000 January.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193#2</TD>
            <TD>2011-09-14T19:44:16Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/619/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/619/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/619/193 [table6]</TD>
            <TD>Catalog of nearby cluster galaxy photometry (McIntosh+, 2005)</TD>
            <TD>We observed clusters A85, A496, and A754 during two runs at the Kitt Peak National Observatory (KPNO) 0.9m Telescope with the NOAO Mosaic Wide-Field Imager. We used the engineering-grade Mosaic for the V data in 1997 November and the science-grade Mosaic with thinned CCDs for the U band in 2000 January.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193#table6</TD>
            <TD>2011-09-14T19:44:16Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/619/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/619/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/447 [1]</TD>
            <TD>Catalog of star cluster candidates in M 33 (Sarajedini+, 2007)</TD>
            <TD>We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHKS filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447#1</TD>
            <TD>2011-09-14T20:49:25Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/447</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/447</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/447 [2]</TD>
            <TD>Catalog of star cluster candidates in M 33 (Sarajedini+, 2007)</TD>
            <TD>We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHKS filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447#2</TD>
            <TD>2011-09-14T20:49:25Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/447&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/447</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/447 [table3]</TD>
            <TD>Catalog of star cluster candidates in M 33 (Sarajedini+, 2007)</TD>
            <TD>We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHKS filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447#table3</TD>
            <TD>2011-09-14T20:49:25Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/447&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/447</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/447 [1]</TD>
            <TD>Catalog of star cluster candidates in M 33 (Sarajedini+, 2007)</TD>
            <TD>We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHKS filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447#1</TD>
            <TD>2011-09-14T20:49:25Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/447</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/447</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/447 [2]</TD>
            <TD>Catalog of star cluster candidates in M 33 (Sarajedini+, 2007)</TD>
            <TD>We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHKS filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447#2</TD>
            <TD>2011-09-14T20:49:25Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/447&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/447</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/447 [table3]</TD>
            <TD>Catalog of star cluster candidates in M 33 (Sarajedini+, 2007)</TD>
            <TD>We present a new catalog of star cluster candidates in the nearby spiral galaxy M33. It is based on eight existing catalogs wherein we have cross-referenced identifications and endeavored to resolve inconsistencies between them. Our catalog contains 451 candidates, of which 255 are confirmed clusters based on Hubble Space Telescope and high-resolution ground-based imaging. The catalog contains precise cluster positions (right ascension and declination), magnitudes and colors in the UBVRIJHKS filters, metallicities, radial velocities, masses and ages, where available, and galactocentric distances for each cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447#table3</TD>
            <TD>2011-09-14T20:49:25Z</TD>
            <TD>#Associations#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/447</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/447&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/447</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/35/829 [1]</TD>
            <TD>Star clusters in IC 10 (Tikhonov+, 2009)</TD>
            <TD>To study the stellar structure of this galaxy, we used both ground-based observations with the 6-m BTA telescope and the 1-m Zeiss telescope at the Special Astrophysical Observatory and archival data from the Hubble Space Telescope (HST) with the WFPC2, ACS/WFC, and STIS cameras.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829#1</TD>
            <TD>2011-09-14T20:53:16Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/35/829</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/829</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/35/829 [2]</TD>
            <TD>Star clusters in IC 10 (Tikhonov+, 2009)</TD>
            <TD>To study the stellar structure of this galaxy, we used both ground-based observations with the 6-m BTA telescope and the 1-m Zeiss telescope at the Special Astrophysical Observatory and archival data from the Hubble Space Telescope (HST) with the WFPC2, ACS/WFC, and STIS cameras.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829#2</TD>
            <TD>2011-09-14T20:53:16Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/35/829&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/829</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/35/829 [table3]</TD>
            <TD>Star clusters in IC 10 (Tikhonov+, 2009)</TD>
            <TD>To study the stellar structure of this galaxy, we used both ground-based observations with the 6-m BTA telescope and the 1-m Zeiss telescope at the Special Astrophysical Observatory and archival data from the Hubble Space Telescope (HST) with the WFPC2, ACS/WFC, and STIS cameras.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829#table3</TD>
            <TD>2011-09-14T20:53:16Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/35/829&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/829</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/35/829 [1]</TD>
            <TD>Star clusters in IC 10 (Tikhonov+, 2009)</TD>
            <TD>To study the stellar structure of this galaxy, we used both ground-based observations with the 6-m BTA telescope and the 1-m Zeiss telescope at the Special Astrophysical Observatory and archival data from the Hubble Space Telescope (HST) with the WFPC2, ACS/WFC, and STIS cameras.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829#1</TD>
            <TD>2011-09-14T20:53:16Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/35/829</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/829</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/35/829 [2]</TD>
            <TD>Star clusters in IC 10 (Tikhonov+, 2009)</TD>
            <TD>To study the stellar structure of this galaxy, we used both ground-based observations with the 6-m BTA telescope and the 1-m Zeiss telescope at the Special Astrophysical Observatory and archival data from the Hubble Space Telescope (HST) with the WFPC2, ACS/WFC, and STIS cameras.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829#2</TD>
            <TD>2011-09-14T20:53:16Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/35/829&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/829</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/35/829 [table3]</TD>
            <TD>Star clusters in IC 10 (Tikhonov+, 2009)</TD>
            <TD>To study the stellar structure of this galaxy, we used both ground-based observations with the 6-m BTA telescope and the 1-m Zeiss telescope at the Special Astrophysical Observatory and archival data from the Hubble Space Telescope (HST) with the WFPC2, ACS/WFC, and STIS cameras.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829#table3</TD>
            <TD>2011-09-14T20:53:16Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/35/829&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/829</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/35/829 [1]</TD>
            <TD>Star clusters in IC 10 (Tikhonov+, 2009)</TD>
            <TD>To study the stellar structure of this galaxy, we used both ground-based observations with the 6-m BTA telescope and the 1-m Zeiss telescope at the Special Astrophysical Observatory and archival data from the Hubble Space Telescope (HST) with the WFPC2, ACS/WFC, and STIS cameras.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829#1</TD>
            <TD>2011-09-14T20:53:16Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/35/829</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/829</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/35/829 [2]</TD>
            <TD>Star clusters in IC 10 (Tikhonov+, 2009)</TD>
            <TD>To study the stellar structure of this galaxy, we used both ground-based observations with the 6-m BTA telescope and the 1-m Zeiss telescope at the Special Astrophysical Observatory and archival data from the Hubble Space Telescope (HST) with the WFPC2, ACS/WFC, and STIS cameras.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829#2</TD>
            <TD>2011-09-14T20:53:16Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/35/829&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/829</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/35/829 [table3]</TD>
            <TD>Star clusters in IC 10 (Tikhonov+, 2009)</TD>
            <TD>To study the stellar structure of this galaxy, we used both ground-based observations with the 6-m BTA telescope and the 1-m Zeiss telescope at the Special Astrophysical Observatory and archival data from the Hubble Space Telescope (HST) with the WFPC2, ACS/WFC, and STIS cameras.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829#table3</TD>
            <TD>2011-09-14T20:53:16Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/829</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/35/829&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/829</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/352/1245 [1]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#1</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/352/1245</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/352/1245 [2]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#2</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/352/1245&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/1245 [table3]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#table3</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/1245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/1245 [table4]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#table4</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/1245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/352/1245 [1]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#1</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/352/1245</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/352/1245 [2]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#2</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/352/1245&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/1245 [table3]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#table3</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/1245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/1245 [table4]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#table4</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/1245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/122/431 [1]</TD>
            <TD>Star Clusters in M33 (Chandar+, 1999)</TD>
            <TD>++++Lrecl of file 'table3.dat' (101) increased to 105 %B In this paper we present the discovery of 60 star clusters in 20 multiband Hubble Space Telescope (HST) WFPC2 fields in M33. The fields sample a variety of environments, from outer regions to spiral arms and central regions, as well as a range of galactocentric distances. The HST spatial resolution allowed us to penetrate the crowded, spiral arm regions of M33 yielding the first unbiased, representative sample of star clusters for this galaxy. We discuss the separation of clusters from stellar sources, and from other extended sources such as star-forming regions, H II regions, and supernova remnants. For the clusters we present multiband images and discuss morphology, location, and integrated photometry. Measured cluster colors and magnitudes are presented. The cluster density in our sample as a function of galactocentric distance yields an estimate of 690 total clusters in M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431#1</TD>
            <TD>2011-09-14T20:53:00Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/122/431</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/431</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/122/431 [2]</TD>
            <TD>Star Clusters in M33 (Chandar+, 1999)</TD>
            <TD>++++Lrecl of file 'table3.dat' (101) increased to 105 %B In this paper we present the discovery of 60 star clusters in 20 multiband Hubble Space Telescope (HST) WFPC2 fields in M33. The fields sample a variety of environments, from outer regions to spiral arms and central regions, as well as a range of galactocentric distances. The HST spatial resolution allowed us to penetrate the crowded, spiral arm regions of M33 yielding the first unbiased, representative sample of star clusters for this galaxy. We discuss the separation of clusters from stellar sources, and from other extended sources such as star-forming regions, H II regions, and supernova remnants. For the clusters we present multiband images and discuss morphology, location, and integrated photometry. Measured cluster colors and magnitudes are presented. The cluster density in our sample as a function of galactocentric distance yields an estimate of 690 total clusters in M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431#2</TD>
            <TD>2011-09-14T20:53:00Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/122/431&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/431</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/431 [table2]</TD>
            <TD>Star Clusters in M33 (Chandar+, 1999)</TD>
            <TD>++++Lrecl of file 'table3.dat' (101) increased to 105 %B In this paper we present the discovery of 60 star clusters in 20 multiband Hubble Space Telescope (HST) WFPC2 fields in M33. The fields sample a variety of environments, from outer regions to spiral arms and central regions, as well as a range of galactocentric distances. The HST spatial resolution allowed us to penetrate the crowded, spiral arm regions of M33 yielding the first unbiased, representative sample of star clusters for this galaxy. We discuss the separation of clusters from stellar sources, and from other extended sources such as star-forming regions, H II regions, and supernova remnants. For the clusters we present multiband images and discuss morphology, location, and integrated photometry. Measured cluster colors and magnitudes are presented. The cluster density in our sample as a function of galactocentric distance yields an estimate of 690 total clusters in M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431#table2</TD>
            <TD>2011-09-14T20:53:00Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/431&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/431</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/352/1245 [1]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#1</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/352/1245</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/352/1245 [2]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#2</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/352/1245&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/1245 [table3]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#table3</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/1245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/352/1245 [table4]</TD>
            <TD>Faint 1.4GHz radio sources in 2dFGRS (Chan+, 2004)</TD>
            <TD>We have used the Australia Telescope Compact Array (ATCA) to search for faint radio sources in a ~3deg^2^ region of sky covered by the 2dF Galaxy Redshift Survey (2dFGRS, Cat. &lt;VII/226&gt;). Over the region surveyed, the 1{sigma} noise level at 1.4GHz ranges from 20Jy to 1mJy. The survey region includes 365 2dFGRS galaxies, of which 316 have good-quality spectra (176 early-type galaxies or active galactic nuclei, and 140 star-forming galaxies). The fraction of 2dFGRS galaxies detected as radio sources in our survey rises from ~4% at a 3{sigma} detection limit of 0.3mJy to 12% at 75{mu}Jy, with roughly equal numbers of star-forming galaxies and active galactic nuclei (AGNs) being detected.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245#table4</TD>
            <TD>2011-09-14T20:54:31Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/352/1245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/352/1245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/352/1245</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/185/20 [1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/185/20</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/185/20 [2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/185/20&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/185/20 [table1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#table1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/185/20&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/185/20 [table2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#table2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/185/20&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/185/20 [1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/185/20</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/185/20 [2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/185/20&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/185/20 [table1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#table1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/185/20&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/185/20 [table2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#table2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/185/20&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/185/20 [1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/185/20</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/185/20 [2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/185/20&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/185/20 [table1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#table1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/185/20&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/185/20 [table2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Absorption along quasar sightlines remains among the most sensitive direct measures of HeII reionization in much of the intergalactic medium (IGM). Until recently, fewer than a half-dozen unobscured quasar sightlines suitable for the HeII Gunn-Peterson test were known; although these handful demonstrated great promise, the small sample size limited confidence in cosmological inferences. We have recently added nine more such clean HeII quasars, exploiting Sloan Digital Sky Survey (SDSS) quasar samples, broadband ultraviolet (UV) imaging from Galaxy Evolution Explorer (GALEX), and high-yield UV spectroscopic confirmations from Hubble Space Telescope (HST). Here we markedly expand this approach by cross-correlating SDSS DR7 and GALEX GR4+5 to catalog 428 SDSS and 165 other quasars with z&gt;2.78 having likely (~70%) GALEX detections, suggesting they are bright into the far-UV. Reconnaissance HST Cycle 16 Supplemental prism data for 29 of these new quasar-GALEX matches spectroscopically confirm 17 as indeed far-UV bright. At least 10 of these confirmations have clean sightlines all the way down to HeII Ly{alpha}, substantially expanding the number of known clean HeII quasars, and reaffirming the order of magnitude enhanced efficiency of our selection technique. Combined confirmations from this and our past programs yield more than 20 HeII quasars, quintupling the sample. These provide substantial progress toward a sample of HeII quasar sightlines large enough, and spanning a sufficient redshift range, to enable statistical IGM studies that may avoid individual object peculiarity and sightline variance. Our expanded catalog of hundreds of high-likelihood far-UV-bright QSOs additionally will be useful for understanding the extreme-UV properties of the quasars themselves.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20#table2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/185/20</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/185/20&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/185/20</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/401/1587 [1]</TD>
            <TD>RIK photometry of far-IR sources in NGP (Vaisanen+, 2010)</TD>
            <TD>Table A.2 lists the full photometric catalog of the ISOPHOT EBL project North Galactic Pole fields acquired with the Nordic Optical Telescope, using the ALFOSC (in R and I band) and NOTCAM (in K band) instruments. The photometry is performed with SExtractor and both "total" and aperture magnitudes are given using the AUTO and APER (with 2.7" diameter) magnitudes, as well as the star/galaxy CLASS parameter. The photometry is matched with the SDSS and the ugriz magnitudes are also given. All objects falling within 60" of a given ISOPHOT far-IR source are indicated - these areas are analysed in the Paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587#1</TD>
            <TD>2011-09-14T20:57:27Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/401/1587</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/401/1587</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/401/1587 [2]</TD>
            <TD>RIK photometry of far-IR sources in NGP (Vaisanen+, 2010)</TD>
            <TD>Table A.2 lists the full photometric catalog of the ISOPHOT EBL project North Galactic Pole fields acquired with the Nordic Optical Telescope, using the ALFOSC (in R and I band) and NOTCAM (in K band) instruments. The photometry is performed with SExtractor and both "total" and aperture magnitudes are given using the AUTO and APER (with 2.7" diameter) magnitudes, as well as the star/galaxy CLASS parameter. The photometry is matched with the SDSS and the ugriz magnitudes are also given. All objects falling within 60" of a given ISOPHOT far-IR source are indicated - these areas are analysed in the Paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587#2</TD>
            <TD>2011-09-14T20:57:27Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/401/1587&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/401/1587</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/401/1587 [tablea2]</TD>
            <TD>RIK photometry of far-IR sources in NGP (Vaisanen+, 2010)</TD>
            <TD>Table A.2 lists the full photometric catalog of the ISOPHOT EBL project North Galactic Pole fields acquired with the Nordic Optical Telescope, using the ALFOSC (in R and I band) and NOTCAM (in K band) instruments. The photometry is performed with SExtractor and both "total" and aperture magnitudes are given using the AUTO and APER (with 2.7" diameter) magnitudes, as well as the star/galaxy CLASS parameter. The photometry is matched with the SDSS and the ugriz magnitudes are also given. All objects falling within 60" of a given ISOPHOT far-IR source are indicated - these areas are analysed in the Paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587#tablea2</TD>
            <TD>2011-09-14T20:57:27Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/401/1587&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/401/1587</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/401/1587 [1]</TD>
            <TD>RIK photometry of far-IR sources in NGP (Vaisanen+, 2010)</TD>
            <TD>Table A.2 lists the full photometric catalog of the ISOPHOT EBL project North Galactic Pole fields acquired with the Nordic Optical Telescope, using the ALFOSC (in R and I band) and NOTCAM (in K band) instruments. The photometry is performed with SExtractor and both "total" and aperture magnitudes are given using the AUTO and APER (with 2.7" diameter) magnitudes, as well as the star/galaxy CLASS parameter. The photometry is matched with the SDSS and the ugriz magnitudes are also given. All objects falling within 60" of a given ISOPHOT far-IR source are indicated - these areas are analysed in the Paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587#1</TD>
            <TD>2011-09-14T20:57:27Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/401/1587</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/401/1587</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/401/1587 [2]</TD>
            <TD>RIK photometry of far-IR sources in NGP (Vaisanen+, 2010)</TD>
            <TD>Table A.2 lists the full photometric catalog of the ISOPHOT EBL project North Galactic Pole fields acquired with the Nordic Optical Telescope, using the ALFOSC (in R and I band) and NOTCAM (in K band) instruments. The photometry is performed with SExtractor and both "total" and aperture magnitudes are given using the AUTO and APER (with 2.7" diameter) magnitudes, as well as the star/galaxy CLASS parameter. The photometry is matched with the SDSS and the ugriz magnitudes are also given. All objects falling within 60" of a given ISOPHOT far-IR source are indicated - these areas are analysed in the Paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587#2</TD>
            <TD>2011-09-14T20:57:27Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/401/1587&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/401/1587</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/401/1587 [tablea2]</TD>
            <TD>RIK photometry of far-IR sources in NGP (Vaisanen+, 2010)</TD>
            <TD>Table A.2 lists the full photometric catalog of the ISOPHOT EBL project North Galactic Pole fields acquired with the Nordic Optical Telescope, using the ALFOSC (in R and I band) and NOTCAM (in K band) instruments. The photometry is performed with SExtractor and both "total" and aperture magnitudes are given using the AUTO and APER (with 2.7" diameter) magnitudes, as well as the star/galaxy CLASS parameter. The photometry is matched with the SDSS and the ugriz magnitudes are also given. All objects falling within 60" of a given ISOPHOT far-IR source are indicated - these areas are analysed in the Paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587#tablea2</TD>
            <TD>2011-09-14T20:57:27Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/401/1587&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/401/1587</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/401/1587 [1]</TD>
            <TD>RIK photometry of far-IR sources in NGP (Vaisanen+, 2010)</TD>
            <TD>Table A.2 lists the full photometric catalog of the ISOPHOT EBL project North Galactic Pole fields acquired with the Nordic Optical Telescope, using the ALFOSC (in R and I band) and NOTCAM (in K band) instruments. The photometry is performed with SExtractor and both "total" and aperture magnitudes are given using the AUTO and APER (with 2.7" diameter) magnitudes, as well as the star/galaxy CLASS parameter. The photometry is matched with the SDSS and the ugriz magnitudes are also given. All objects falling within 60" of a given ISOPHOT far-IR source are indicated - these areas are analysed in the Paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587#1</TD>
            <TD>2011-09-14T20:57:27Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/401/1587</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/401/1587</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/401/1587 [2]</TD>
            <TD>RIK photometry of far-IR sources in NGP (Vaisanen+, 2010)</TD>
            <TD>Table A.2 lists the full photometric catalog of the ISOPHOT EBL project North Galactic Pole fields acquired with the Nordic Optical Telescope, using the ALFOSC (in R and I band) and NOTCAM (in K band) instruments. The photometry is performed with SExtractor and both "total" and aperture magnitudes are given using the AUTO and APER (with 2.7" diameter) magnitudes, as well as the star/galaxy CLASS parameter. The photometry is matched with the SDSS and the ugriz magnitudes are also given. All objects falling within 60" of a given ISOPHOT far-IR source are indicated - these areas are analysed in the Paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587#2</TD>
            <TD>2011-09-14T20:57:27Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/401/1587&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/401/1587</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/401/1587 [tablea2]</TD>
            <TD>RIK photometry of far-IR sources in NGP (Vaisanen+, 2010)</TD>
            <TD>Table A.2 lists the full photometric catalog of the ISOPHOT EBL project North Galactic Pole fields acquired with the Nordic Optical Telescope, using the ALFOSC (in R and I band) and NOTCAM (in K band) instruments. The photometry is performed with SExtractor and both "total" and aperture magnitudes are given using the AUTO and APER (with 2.7" diameter) magnitudes, as well as the star/galaxy CLASS parameter. The photometry is matched with the SDSS and the ugriz magnitudes are also given. All objects falling within 60" of a given ISOPHOT far-IR source are indicated - these areas are analysed in the Paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587#tablea2</TD>
            <TD>2011-09-14T20:57:27Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/401/1587</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/401/1587&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/401/1587</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/674/L81 [1]</TD>
            <TD>Variable stars in dwarf galaxy CVn I (Kuehn+, 2008)</TD>
            <TD>BV and Cousins I time-series photometry of CVn I was obtained in 2006 May and 2007 April and May at the 2.3m Wyoming Infrared Observatory telescope (WIRO), using the prime focus CCD camera. Additional BVI photometry was obtained at the 4.2m William Herschel Telescope (WHT) in 2007 April using the Prime Focus Imaging Camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81#1</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/674/L81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/L81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/674/L81 [2]</TD>
            <TD>Variable stars in dwarf galaxy CVn I (Kuehn+, 2008)</TD>
            <TD>BV and Cousins I time-series photometry of CVn I was obtained in 2006 May and 2007 April and May at the 2.3m Wyoming Infrared Observatory telescope (WIRO), using the prime focus CCD camera. Additional BVI photometry was obtained at the 4.2m William Herschel Telescope (WHT) in 2007 April using the Prime Focus Imaging Camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81#2</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/674/L81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/L81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/674/L81 [table1]</TD>
            <TD>Variable stars in dwarf galaxy CVn I (Kuehn+, 2008)</TD>
            <TD>BV and Cousins I time-series photometry of CVn I was obtained in 2006 May and 2007 April and May at the 2.3m Wyoming Infrared Observatory telescope (WIRO), using the prime focus CCD camera. Additional BVI photometry was obtained at the 4.2m William Herschel Telescope (WHT) in 2007 April using the Prime Focus Imaging Camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81#table1</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/674/L81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/L81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/674/L81 [1]</TD>
            <TD>Variable stars in dwarf galaxy CVn I (Kuehn+, 2008)</TD>
            <TD>BV and Cousins I time-series photometry of CVn I was obtained in 2006 May and 2007 April and May at the 2.3m Wyoming Infrared Observatory telescope (WIRO), using the prime focus CCD camera. Additional BVI photometry was obtained at the 4.2m William Herschel Telescope (WHT) in 2007 April using the Prime Focus Imaging Camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81#1</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/674/L81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/L81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/674/L81 [2]</TD>
            <TD>Variable stars in dwarf galaxy CVn I (Kuehn+, 2008)</TD>
            <TD>BV and Cousins I time-series photometry of CVn I was obtained in 2006 May and 2007 April and May at the 2.3m Wyoming Infrared Observatory telescope (WIRO), using the prime focus CCD camera. Additional BVI photometry was obtained at the 4.2m William Herschel Telescope (WHT) in 2007 April using the Prime Focus Imaging Camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81#2</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/674/L81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/L81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/674/L81 [table1]</TD>
            <TD>Variable stars in dwarf galaxy CVn I (Kuehn+, 2008)</TD>
            <TD>BV and Cousins I time-series photometry of CVn I was obtained in 2006 May and 2007 April and May at the 2.3m Wyoming Infrared Observatory telescope (WIRO), using the prime focus CCD camera. Additional BVI photometry was obtained at the 4.2m William Herschel Telescope (WHT) in 2007 April using the Prime Focus Imaging Camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81#table1</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/674/L81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/L81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/674/L81 [1]</TD>
            <TD>Variable stars in dwarf galaxy CVn I (Kuehn+, 2008)</TD>
            <TD>BV and Cousins I time-series photometry of CVn I was obtained in 2006 May and 2007 April and May at the 2.3m Wyoming Infrared Observatory telescope (WIRO), using the prime focus CCD camera. Additional BVI photometry was obtained at the 4.2m William Herschel Telescope (WHT) in 2007 April using the Prime Focus Imaging Camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81#1</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/674/L81</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/L81</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/674/L81 [2]</TD>
            <TD>Variable stars in dwarf galaxy CVn I (Kuehn+, 2008)</TD>
            <TD>BV and Cousins I time-series photometry of CVn I was obtained in 2006 May and 2007 April and May at the 2.3m Wyoming Infrared Observatory telescope (WIRO), using the prime focus CCD camera. Additional BVI photometry was obtained at the 4.2m William Herschel Telescope (WHT) in 2007 April using the Prime Focus Imaging Camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81#2</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/674/L81&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/L81</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/674/L81 [table1]</TD>
            <TD>Variable stars in dwarf galaxy CVn I (Kuehn+, 2008)</TD>
            <TD>BV and Cousins I time-series photometry of CVn I was obtained in 2006 May and 2007 April and May at the 2.3m Wyoming Infrared Observatory telescope (WIRO), using the prime focus CCD camera. Additional BVI photometry was obtained at the 4.2m William Herschel Telescope (WHT) in 2007 April using the Prime Focus Imaging Camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81#table1</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Photometry#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/L81</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/674/L81&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/L81</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/643/1011 [1]</TD>
            <TD>Early-type stars in the center of the Galaxy (Paumard+, 2006)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011#1</TD>
            <TD>2011-09-14T20:59:47Z</TD>
            <TD>#Stars#Velocities#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/643/1011</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/643/1011</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/643/1011 [2]</TD>
            <TD>Early-type stars in the center of the Galaxy (Paumard+, 2006)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011#2</TD>
            <TD>2011-09-14T20:59:47Z</TD>
            <TD>#Stars#Velocities#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/643/1011&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/643/1011</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/643/1011 [table2]</TD>
            <TD>Early-type stars in the center of the Galaxy (Paumard+, 2006)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011#table2</TD>
            <TD>2011-09-14T20:59:47Z</TD>
            <TD>#Stars#Velocities#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/643/1011&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/643/1011</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/643/1011 [1]</TD>
            <TD>Early-type stars in the center of the Galaxy (Paumard+, 2006)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011#1</TD>
            <TD>2011-09-14T20:59:47Z</TD>
            <TD>#Stars#Velocities#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/643/1011</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/643/1011</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/643/1011 [2]</TD>
            <TD>Early-type stars in the center of the Galaxy (Paumard+, 2006)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011#2</TD>
            <TD>2011-09-14T20:59:47Z</TD>
            <TD>#Stars#Velocities#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/643/1011&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/643/1011</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/643/1011 [table2]</TD>
            <TD>Early-type stars in the center of the Galaxy (Paumard+, 2006)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011#table2</TD>
            <TD>2011-09-14T20:59:47Z</TD>
            <TD>#Stars#Velocities#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/643/1011&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/643/1011</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/122/431 [1]</TD>
            <TD>Star Clusters in M33 (Chandar+, 1999)</TD>
            <TD>++++Lrecl of file 'table3.dat' (101) increased to 105 %B In this paper we present the discovery of 60 star clusters in 20 multiband Hubble Space Telescope (HST) WFPC2 fields in M33. The fields sample a variety of environments, from outer regions to spiral arms and central regions, as well as a range of galactocentric distances. The HST spatial resolution allowed us to penetrate the crowded, spiral arm regions of M33 yielding the first unbiased, representative sample of star clusters for this galaxy. We discuss the separation of clusters from stellar sources, and from other extended sources such as star-forming regions, H II regions, and supernova remnants. For the clusters we present multiband images and discuss morphology, location, and integrated photometry. Measured cluster colors and magnitudes are presented. The cluster density in our sample as a function of galactocentric distance yields an estimate of 690 total clusters in M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431#1</TD>
            <TD>2011-09-14T20:53:00Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/122/431</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/431</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/122/431 [2]</TD>
            <TD>Star Clusters in M33 (Chandar+, 1999)</TD>
            <TD>++++Lrecl of file 'table3.dat' (101) increased to 105 %B In this paper we present the discovery of 60 star clusters in 20 multiband Hubble Space Telescope (HST) WFPC2 fields in M33. The fields sample a variety of environments, from outer regions to spiral arms and central regions, as well as a range of galactocentric distances. The HST spatial resolution allowed us to penetrate the crowded, spiral arm regions of M33 yielding the first unbiased, representative sample of star clusters for this galaxy. We discuss the separation of clusters from stellar sources, and from other extended sources such as star-forming regions, H II regions, and supernova remnants. For the clusters we present multiband images and discuss morphology, location, and integrated photometry. Measured cluster colors and magnitudes are presented. The cluster density in our sample as a function of galactocentric distance yields an estimate of 690 total clusters in M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431#2</TD>
            <TD>2011-09-14T20:53:00Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/122/431&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/431</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/431 [table2]</TD>
            <TD>Star Clusters in M33 (Chandar+, 1999)</TD>
            <TD>++++Lrecl of file 'table3.dat' (101) increased to 105 %B In this paper we present the discovery of 60 star clusters in 20 multiband Hubble Space Telescope (HST) WFPC2 fields in M33. The fields sample a variety of environments, from outer regions to spiral arms and central regions, as well as a range of galactocentric distances. The HST spatial resolution allowed us to penetrate the crowded, spiral arm regions of M33 yielding the first unbiased, representative sample of star clusters for this galaxy. We discuss the separation of clusters from stellar sources, and from other extended sources such as star-forming regions, H II regions, and supernova remnants. For the clusters we present multiband images and discuss morphology, location, and integrated photometry. Measured cluster colors and magnitudes are presented. The cluster density in our sample as a function of galactocentric distance yields an estimate of 690 total clusters in M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431#table2</TD>
            <TD>2011-09-14T20:53:00Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/431&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/431</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/643/1011 [1]</TD>
            <TD>Early-type stars in the center of the Galaxy (Paumard+, 2006)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011#1</TD>
            <TD>2011-09-14T20:59:47Z</TD>
            <TD>#Stars#Velocities#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/643/1011</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/643/1011</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/643/1011 [2]</TD>
            <TD>Early-type stars in the center of the Galaxy (Paumard+, 2006)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011#2</TD>
            <TD>2011-09-14T20:59:47Z</TD>
            <TD>#Stars#Velocities#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/643/1011&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/643/1011</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/643/1011 [table2]</TD>
            <TD>Early-type stars in the center of the Galaxy (Paumard+, 2006)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011#table2</TD>
            <TD>2011-09-14T20:59:47Z</TD>
            <TD>#Stars#Velocities#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/643/1011</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/643/1011&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/643/1011</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/671/323 [1]</TD>
            <TD>Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323#1</TD>
            <TD>2011-09-14T21:00:58Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/671/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/671/323 [2]</TD>
            <TD>Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323#2</TD>
            <TD>2011-09-14T21:00:58Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/671/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/671/323 [table1]</TD>
            <TD>Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323#table1</TD>
            <TD>2011-09-14T21:00:58Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/671/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/671/323 [1]</TD>
            <TD>Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323#1</TD>
            <TD>2011-09-14T21:00:58Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/671/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/671/323 [2]</TD>
            <TD>Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323#2</TD>
            <TD>2011-09-14T21:00:58Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/671/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/671/323 [table1]</TD>
            <TD>Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323#table1</TD>
            <TD>2011-09-14T21:00:58Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/671/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/671/323 [1]</TD>
            <TD>Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323#1</TD>
            <TD>2011-09-14T21:00:58Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/671/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/671/323 [2]</TD>
            <TD>Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323#2</TD>
            <TD>2011-09-14T21:00:58Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/671/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/671/323 [table1]</TD>
            <TD>Spitzer Spectra of a 10mJy galaxy sample (Houck+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323#table1</TD>
            <TD>2011-09-14T21:00:58Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/671/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/671/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/671/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/462/449 [1]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#1</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/462/449</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/462/449 [2]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#2</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/462/449&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/462/449 [table1]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#table1</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/462/449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/462/449 [table2]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#table2</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/462/449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/122/431 [1]</TD>
            <TD>Star Clusters in M33 (Chandar+, 1999)</TD>
            <TD>++++Lrecl of file 'table3.dat' (101) increased to 105 %B In this paper we present the discovery of 60 star clusters in 20 multiband Hubble Space Telescope (HST) WFPC2 fields in M33. The fields sample a variety of environments, from outer regions to spiral arms and central regions, as well as a range of galactocentric distances. The HST spatial resolution allowed us to penetrate the crowded, spiral arm regions of M33 yielding the first unbiased, representative sample of star clusters for this galaxy. We discuss the separation of clusters from stellar sources, and from other extended sources such as star-forming regions, H II regions, and supernova remnants. For the clusters we present multiband images and discuss morphology, location, and integrated photometry. Measured cluster colors and magnitudes are presented. The cluster density in our sample as a function of galactocentric distance yields an estimate of 690 total clusters in M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431#1</TD>
            <TD>2011-09-14T20:53:00Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/122/431</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/431</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/122/431 [2]</TD>
            <TD>Star Clusters in M33 (Chandar+, 1999)</TD>
            <TD>++++Lrecl of file 'table3.dat' (101) increased to 105 %B In this paper we present the discovery of 60 star clusters in 20 multiband Hubble Space Telescope (HST) WFPC2 fields in M33. The fields sample a variety of environments, from outer regions to spiral arms and central regions, as well as a range of galactocentric distances. The HST spatial resolution allowed us to penetrate the crowded, spiral arm regions of M33 yielding the first unbiased, representative sample of star clusters for this galaxy. We discuss the separation of clusters from stellar sources, and from other extended sources such as star-forming regions, H II regions, and supernova remnants. For the clusters we present multiband images and discuss morphology, location, and integrated photometry. Measured cluster colors and magnitudes are presented. The cluster density in our sample as a function of galactocentric distance yields an estimate of 690 total clusters in M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431#2</TD>
            <TD>2011-09-14T20:53:00Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/122/431&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/431</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/431 [table2]</TD>
            <TD>Star Clusters in M33 (Chandar+, 1999)</TD>
            <TD>++++Lrecl of file 'table3.dat' (101) increased to 105 %B In this paper we present the discovery of 60 star clusters in 20 multiband Hubble Space Telescope (HST) WFPC2 fields in M33. The fields sample a variety of environments, from outer regions to spiral arms and central regions, as well as a range of galactocentric distances. The HST spatial resolution allowed us to penetrate the crowded, spiral arm regions of M33 yielding the first unbiased, representative sample of star clusters for this galaxy. We discuss the separation of clusters from stellar sources, and from other extended sources such as star-forming regions, H II regions, and supernova remnants. For the clusters we present multiband images and discuss morphology, location, and integrated photometry. Measured cluster colors and magnitudes are presented. The cluster density in our sample as a function of galactocentric distance yields an estimate of 690 total clusters in M33.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431#table2</TD>
            <TD>2011-09-14T20:53:00Z</TD>
            <TD>#Globular_Clusters#Open_Clusters#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/431</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/431&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/431</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/462/449 [1]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#1</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/462/449</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/462/449 [2]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#2</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/462/449&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/462/449 [table1]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#table1</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/462/449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/462/449 [table2]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#table2</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/462/449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/462/449 [1]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#1</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/462/449</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/462/449 [2]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#2</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/462/449&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/462/449 [table1]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#table1</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/462/449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/462/449 [table2]</TD>
            <TD>Chandra point-source counts in galaxy cluster (Branchesi+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449#table2</TD>
            <TD>2011-09-14T21:00:59Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/449</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/462/449&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/449</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/197/22 [1]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)</TD>
            <TD>Paper I (Cat. J/ApJS/197/21) describes the observing strategy, data reductions, and photometric calibration of the optical imaging component of the project. The broadband BVRI images have a field of view of 8.9'x8.9' and a pixel scale of 0.259", which is well matched to the good seeing typically achieved with the du Pont 2.5m telescope at Las Campanas Observatory during the period 2003 February to 2006 June.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22#1</TD>
            <TD>2012-02-20T16:05:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/197/22</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/22</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/197/22 [2]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)</TD>
            <TD>Paper I (Cat. J/ApJS/197/21) describes the observing strategy, data reductions, and photometric calibration of the optical imaging component of the project. The broadband BVRI images have a field of view of 8.9'x8.9' and a pixel scale of 0.259", which is well matched to the good seeing typically achieved with the du Pont 2.5m telescope at Las Campanas Observatory during the period 2003 February to 2006 June.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22#2</TD>
            <TD>2012-02-20T16:05:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/197/22&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/197/22 [cgs]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)</TD>
            <TD>Paper I (Cat. J/ApJS/197/21) describes the observing strategy, data reductions, and photometric calibration of the optical imaging component of the project. The broadband BVRI images have a field of view of 8.9'x8.9' and a pixel scale of 0.259", which is well matched to the good seeing typically achieved with the du Pont 2.5m telescope at Las Campanas Observatory during the period 2003 February to 2006 June.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22#cgs</TD>
            <TD>2012-02-20T16:05:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/197/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/22</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/197/22 [1]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)</TD>
            <TD>Paper I (Cat. J/ApJS/197/21) describes the observing strategy, data reductions, and photometric calibration of the optical imaging component of the project. The broadband BVRI images have a field of view of 8.9'x8.9' and a pixel scale of 0.259", which is well matched to the good seeing typically achieved with the du Pont 2.5m telescope at Las Campanas Observatory during the period 2003 February to 2006 June.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22#1</TD>
            <TD>2012-02-20T16:05:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/197/22</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/22</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/197/22 [2]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)</TD>
            <TD>Paper I (Cat. J/ApJS/197/21) describes the observing strategy, data reductions, and photometric calibration of the optical imaging component of the project. The broadband BVRI images have a field of view of 8.9'x8.9' and a pixel scale of 0.259", which is well matched to the good seeing typically achieved with the du Pont 2.5m telescope at Las Campanas Observatory during the period 2003 February to 2006 June.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22#2</TD>
            <TD>2012-02-20T16:05:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/197/22&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/197/22 [cgs]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)</TD>
            <TD>Paper I (Cat. J/ApJS/197/21) describes the observing strategy, data reductions, and photometric calibration of the optical imaging component of the project. The broadband BVRI images have a field of view of 8.9'x8.9' and a pixel scale of 0.259", which is well matched to the good seeing typically achieved with the du Pont 2.5m telescope at Las Campanas Observatory during the period 2003 February to 2006 June.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22#cgs</TD>
            <TD>2012-02-20T16:05:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/197/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/22</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/197/22 [1]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)</TD>
            <TD>Paper I (Cat. J/ApJS/197/21) describes the observing strategy, data reductions, and photometric calibration of the optical imaging component of the project. The broadband BVRI images have a field of view of 8.9'x8.9' and a pixel scale of 0.259", which is well matched to the good seeing typically achieved with the du Pont 2.5m telescope at Las Campanas Observatory during the period 2003 February to 2006 June.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22#1</TD>
            <TD>2012-02-20T16:05:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/197/22</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/22</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/197/22 [2]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)</TD>
            <TD>Paper I (Cat. J/ApJS/197/21) describes the observing strategy, data reductions, and photometric calibration of the optical imaging component of the project. The broadband BVRI images have a field of view of 8.9'x8.9' and a pixel scale of 0.259", which is well matched to the good seeing typically achieved with the du Pont 2.5m telescope at Las Campanas Observatory during the period 2003 February to 2006 June.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22#2</TD>
            <TD>2012-02-20T16:05:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/197/22&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/22</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/197/22 [cgs]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (GGS). II. (Li+, 2011)</TD>
            <TD>Paper I (Cat. J/ApJS/197/21) describes the observing strategy, data reductions, and photometric calibration of the optical imaging component of the project. The broadband BVRI images have a field of view of 8.9'x8.9' and a pixel scale of 0.259", which is well matched to the good seeing typically achieved with the du Pont 2.5m telescope at Las Campanas Observatory during the period 2003 February to 2006 June.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22#cgs</TD>
            <TD>2012-02-20T16:05:00Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/22</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/197/22&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/22</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/700/654 [1]</TD>
            <TD>Keck spectroscopy of extragalactic HII regions (Esteban+ 2009)</TD>
            <TD>The observations of the sample objects, except NGC 5447-a bright HII region in the galaxy M101-were made on 2006 April 20 and 21 and November 14 with the High Resolution Echelle Spectrometer (HIRES) at the Keck I telescope on Mauna Kea Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654#1</TD>
            <TD>2012-03-31T17:02:22Z</TD>
            <TD>#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/700/654</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/654</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/700/654 [2]</TD>
            <TD>Keck spectroscopy of extragalactic HII regions (Esteban+ 2009)</TD>
            <TD>The observations of the sample objects, except NGC 5447-a bright HII region in the galaxy M101-were made on 2006 April 20 and 21 and November 14 with the High Resolution Echelle Spectrometer (HIRES) at the Keck I telescope on Mauna Kea Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654#2</TD>
            <TD>2012-03-31T17:02:22Z</TD>
            <TD>#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/700/654&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/654</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/700/654 [sources]</TD>
            <TD>Keck spectroscopy of extragalactic HII regions (Esteban+ 2009)</TD>
            <TD>The observations of the sample objects, except NGC 5447-a bright HII region in the galaxy M101-were made on 2006 April 20 and 21 and November 14 with the High Resolution Echelle Spectrometer (HIRES) at the Keck I telescope on Mauna Kea Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654#sources</TD>
            <TD>2012-03-31T17:02:22Z</TD>
            <TD>#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/700/654&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/654</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/700/654 [1]</TD>
            <TD>Keck spectroscopy of extragalactic HII regions (Esteban+ 2009)</TD>
            <TD>The observations of the sample objects, except NGC 5447-a bright HII region in the galaxy M101-were made on 2006 April 20 and 21 and November 14 with the High Resolution Echelle Spectrometer (HIRES) at the Keck I telescope on Mauna Kea Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654#1</TD>
            <TD>2012-03-31T17:02:22Z</TD>
            <TD>#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/700/654</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/654</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/700/654 [2]</TD>
            <TD>Keck spectroscopy of extragalactic HII regions (Esteban+ 2009)</TD>
            <TD>The observations of the sample objects, except NGC 5447-a bright HII region in the galaxy M101-were made on 2006 April 20 and 21 and November 14 with the High Resolution Echelle Spectrometer (HIRES) at the Keck I telescope on Mauna Kea Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654#2</TD>
            <TD>2012-03-31T17:02:22Z</TD>
            <TD>#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/700/654&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/654</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/700/654 [sources]</TD>
            <TD>Keck spectroscopy of extragalactic HII regions (Esteban+ 2009)</TD>
            <TD>The observations of the sample objects, except NGC 5447-a bright HII region in the galaxy M101-were made on 2006 April 20 and 21 and November 14 with the High Resolution Echelle Spectrometer (HIRES) at the Keck I telescope on Mauna Kea Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654#sources</TD>
            <TD>2012-03-31T17:02:22Z</TD>
            <TD>#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/700/654&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/654</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/700/654 [1]</TD>
            <TD>Keck spectroscopy of extragalactic HII regions (Esteban+ 2009)</TD>
            <TD>The observations of the sample objects, except NGC 5447-a bright HII region in the galaxy M101-were made on 2006 April 20 and 21 and November 14 with the High Resolution Echelle Spectrometer (HIRES) at the Keck I telescope on Mauna Kea Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654#1</TD>
            <TD>2012-03-31T17:02:22Z</TD>
            <TD>#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/700/654</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/654</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/700/654 [2]</TD>
            <TD>Keck spectroscopy of extragalactic HII regions (Esteban+ 2009)</TD>
            <TD>The observations of the sample objects, except NGC 5447-a bright HII region in the galaxy M101-were made on 2006 April 20 and 21 and November 14 with the High Resolution Echelle Spectrometer (HIRES) at the Keck I telescope on Mauna Kea Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654#2</TD>
            <TD>2012-03-31T17:02:22Z</TD>
            <TD>#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/700/654&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/654</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/700/654 [sources]</TD>
            <TD>Keck spectroscopy of extragalactic HII regions (Esteban+ 2009)</TD>
            <TD>The observations of the sample objects, except NGC 5447-a bright HII region in the galaxy M101-were made on 2006 April 20 and 21 and November 14 with the High Resolution Echelle Spectrometer (HIRES) at the Keck I telescope on Mauna Kea Observatory.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654#sources</TD>
            <TD>2012-03-31T17:02:22Z</TD>
            <TD>#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/700/654</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/700/654&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/700/654</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/317/54 [1]</TD>
            <TD>Fornax cluster 1 and 3 photometry (Jorgensen+ 1997)</TD>
            <TD>We have performed photometric CCD observations of the giant and horizontal branches of the globular cluster1, and of the giant branch of cluster3, in the Fornax dwarf spheroidal galaxy. The observations were performed in the V and I standard broad-band filters as well as through two narrow-band filters especially designed to distinguish between carbon and M type stars. The AGB is richly populated with carbon-rich stars, and all of them are considerably below the theoretical lower luminosity limit for such stars. If the Fornax clusters are interpreted as resembling an earlier epoch of the Galactic globular clusters, the low luminosities of the carbon stars therefore point to a larger role of the low-mass stars in the chemical enrichment of our Galaxy. The giant branches of the Fornax clusters are much broader than canonical giant branches in Galactic globulars, and the AGB is more well populated. We suggest that the morphology and stellar population of the giant branches indicate that the dwarf galaxies are =~3Gyr younger than the Galactic halo, which in turn seems to be =~3Gyr younger than the Galactic globular clusters. For a description of the N2-N3 photometric system, see e.g. &lt;GCPD/39&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/317/54#1</TD>
            <TD>2011-09-14T18:49:23Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/317/54</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/317/54</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/317/54</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/317/54 [2]</TD>
            <TD>Fornax cluster 1 and 3 photometry (Jorgensen+ 1997)</TD>
            <TD>We have performed photometric CCD observations of the giant and horizontal branches of the globular cluster1, and of the giant branch of cluster3, in the Fornax dwarf spheroidal galaxy. The observations were performed in the V and I standard broad-band filters as well as through two narrow-band filters especially designed to distinguish between carbon and M type stars. The AGB is richly populated with carbon-rich stars, and all of them are considerably below the theoretical lower luminosity limit for such stars. If the Fornax clusters are interpreted as resembling an earlier epoch of the Galactic globular clusters, the low luminosities of the carbon stars therefore point to a larger role of the low-mass stars in the chemical enrichment of our Galaxy. The giant branches of the Fornax clusters are much broader than canonical giant branches in Galactic globulars, and the AGB is more well populated. We suggest that the morphology and stellar population of the giant branches indicate that the dwarf galaxies are =~3Gyr younger than the Galactic halo, which in turn seems to be =~3Gyr younger than the Galactic globular clusters. For a description of the N2-N3 photometric system, see e.g. &lt;GCPD/39&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/317/54#2</TD>
            <TD>2011-09-14T18:49:23Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/317/54</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/317/54&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/317/54</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/317/54 [1]</TD>
            <TD>Fornax cluster 1 and 3 photometry (Jorgensen+ 1997)</TD>
            <TD>We have performed photometric CCD observations of the giant and horizontal branches of the globular cluster1, and of the giant branch of cluster3, in the Fornax dwarf spheroidal galaxy. The observations were performed in the V and I standard broad-band filters as well as through two narrow-band filters especially designed to distinguish between carbon and M type stars. The AGB is richly populated with carbon-rich stars, and all of them are considerably below the theoretical lower luminosity limit for such stars. If the Fornax clusters are interpreted as resembling an earlier epoch of the Galactic globular clusters, the low luminosities of the carbon stars therefore point to a larger role of the low-mass stars in the chemical enrichment of our Galaxy. The giant branches of the Fornax clusters are much broader than canonical giant branches in Galactic globulars, and the AGB is more well populated. We suggest that the morphology and stellar population of the giant branches indicate that the dwarf galaxies are =~3Gyr younger than the Galactic halo, which in turn seems to be =~3Gyr younger than the Galactic globular clusters. For a description of the N2-N3 photometric system, see e.g. &lt;GCPD/39&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/317/54#1</TD>
            <TD>2011-09-14T18:49:23Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/317/54</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/317/54</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/317/54</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/317/54 [2]</TD>
            <TD>Fornax cluster 1 and 3 photometry (Jorgensen+ 1997)</TD>
            <TD>We have performed photometric CCD observations of the giant and horizontal branches of the globular cluster1, and of the giant branch of cluster3, in the Fornax dwarf spheroidal galaxy. The observations were performed in the V and I standard broad-band filters as well as through two narrow-band filters especially designed to distinguish between carbon and M type stars. The AGB is richly populated with carbon-rich stars, and all of them are considerably below the theoretical lower luminosity limit for such stars. If the Fornax clusters are interpreted as resembling an earlier epoch of the Galactic globular clusters, the low luminosities of the carbon stars therefore point to a larger role of the low-mass stars in the chemical enrichment of our Galaxy. The giant branches of the Fornax clusters are much broader than canonical giant branches in Galactic globulars, and the AGB is more well populated. We suggest that the morphology and stellar population of the giant branches indicate that the dwarf galaxies are =~3Gyr younger than the Galactic halo, which in turn seems to be =~3Gyr younger than the Galactic globular clusters. For a description of the N2-N3 photometric system, see e.g. &lt;GCPD/39&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/317/54#2</TD>
            <TD>2011-09-14T18:49:23Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/317/54</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/317/54&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/317/54</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/114/215 [1]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#1</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/114/215</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/114/215 [2]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#2</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table7]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table7</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table1]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table1</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table6]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table6</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table3]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table3</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table4]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table4</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table5]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table5</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/114/215 [1]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#1</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/114/215</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/114/215 [2]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#2</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table7]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table7</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table1]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table1</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table6]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table6</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table3]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table3</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table4]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table4</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table5]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table5</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/114/215 [1]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#1</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/114/215</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/114/215 [2]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#2</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table7]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table7</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table1]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table1</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table6]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table6</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table3]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table3</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table4]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table4</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/215 [table5]</TD>
            <TD>New SNR candidates in M31 (Magnier+, 1995)</TD>
            <TD>We have performed a CCD H{alpha}, [SII], V survey of ~1.0 square degree of the disk of M 31 to search for new supernova remnant (SNR) candidates. We have identified candidates based on a combination of criteria: optical line-flux ratios, the presence or absence of ionizing blue stars, and optical morphology. We have identified a total of 178 candidate SNRs, divided into three confidence categories: 13 with the highest confidence, 54 with moderate confidence, and 111 with the lowest confidence. We have also identified 14 large structures with the characteristics of the superbubbles seen in the Galaxy and Magellanic Clouds. Of our 178 candidates, 15 have been identified in previous searches (Braun &amp; Walterbos 1993; Blair et al. 1981; D'Odorico et al. 1980). We present finding charts of all candidate SNRs and the superbubbles we have noted. We also present a detailed discussion of SNR searches in the Local Group.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215#table5</TD>
            <TD>2011-09-14T18:49:44Z</TD>
            <TD>#HII_regions#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/215</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/215&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/215</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/1016 [1]</TD>
            <TD>Kinematics of local RR lyrae stars. I. (Layden, 1994)</TD>
            <TD>In order to study the structure and formation history of the galaxy, we have obtained low-to-moderate dispersion spectra of 302 nearby RR Lyrae variables of Bailey type "ab". We derived abundances, typically accurate to 0.15-0.20dex and calibrated to the Zinn &amp; West (1984ApJS...55...45Z) globular cluster metallicity scale, from the pseudo-equivalent widths of the Ca II K, Hdelta, Hgamma, and Hbeta lines. Radial velocities accurate to between 2 and 30km/s were obtained from the spectra and from the literature. Distances accurate to between 5% and 20% were derived from published apparent magnitudes and Burstein &amp; Heiles (1982AJ.....87.1165B) reddenings. The metallicity distribution of the RR Lyrae stars peaks at [Fe/H]_K_ =~ -1.5, and is narrower than that of the Ryan &amp; Norris (1991AJ....101.1865R) subdwarfs, as expected since the most metal-rich and metal-poor progenitors preferentially appear as stable red and blue horizontal branch stars, rather than as RR Lyrae. The metal-rich tail of the RR Lyrae distribution extends to [Fe/H]_K_{approx}0, and a qualitative analysis of the distribution of distances from the galactic plane shows that the stars in this tail (i.e., [Fe/H]_K_&gt;-1.0) are more concentrated to the plane than the more metal-poor stars. The abundance distribution of the local RR Lyrae stars is in excellent agreement with the changing abundance distributions of distant RR Lyrae stars as a function of galactocentric distance, as derived by Suntzeff et al. (1991ApJ...367..528S), who ascribed this change to systematic variations in horizontal branch morphology (probably age variations) with galactocentric distance. The abundance distribution of the local RR Lyrae stars also agrees well with those of the distant RR Lyrae stars as a function of distance from the galactic plane. There is no evidence for an abundance gradient in this direction, suggesting that gaseous dissipation did not play a major role in the formation of the outer halo.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1016#1</TD>
            <TD>2011-09-14T18:50:06Z</TD>
            <TD>#Abundances#Photometry#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1016</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/1016</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1016</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/1016 [2]</TD>
            <TD>Kinematics of local RR lyrae stars. I. (Layden, 1994)</TD>
            <TD>In order to study the structure and formation history of the galaxy, we have obtained low-to-moderate dispersion spectra of 302 nearby RR Lyrae variables of Bailey type "ab". We derived abundances, typically accurate to 0.15-0.20dex and calibrated to the Zinn &amp; West (1984ApJS...55...45Z) globular cluster metallicity scale, from the pseudo-equivalent widths of the Ca II K, Hdelta, Hgamma, and Hbeta lines. Radial velocities accurate to between 2 and 30km/s were obtained from the spectra and from the literature. Distances accurate to between 5% and 20% were derived from published apparent magnitudes and Burstein &amp; Heiles (1982AJ.....87.1165B) reddenings. The metallicity distribution of the RR Lyrae stars peaks at [Fe/H]_K_ =~ -1.5, and is narrower than that of the Ryan &amp; Norris (1991AJ....101.1865R) subdwarfs, as expected since the most metal-rich and metal-poor progenitors preferentially appear as stable red and blue horizontal branch stars, rather than as RR Lyrae. The metal-rich tail of the RR Lyrae distribution extends to [Fe/H]_K_{approx}0, and a qualitative analysis of the distribution of distances from the galactic plane shows that the stars in this tail (i.e., [Fe/H]_K_&gt;-1.0) are more concentrated to the plane than the more metal-poor stars. The abundance distribution of the local RR Lyrae stars is in excellent agreement with the changing abundance distributions of distant RR Lyrae stars as a function of galactocentric distance, as derived by Suntzeff et al. (1991ApJ...367..528S), who ascribed this change to systematic variations in horizontal branch morphology (probably age variations) with galactocentric distance. The abundance distribution of the local RR Lyrae stars also agrees well with those of the distant RR Lyrae stars as a function of distance from the galactic plane. There is no evidence for an abundance gradient in this direction, suggesting that gaseous dissipation did not play a major role in the formation of the outer halo.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1016#2</TD>
            <TD>2011-09-14T18:50:06Z</TD>
            <TD>#Abundances#Photometry#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1016</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/1016&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1016</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/35/403 [1]</TD>
            <TD>Optical Variabilities in 3C 120 (Doroshenko+, 2009)</TD>
            <TD>Based on our UBVRI observations and X-ray data from the RXTE satellite we have investigated the variabilities of the Seyfert Galaxy 3C 120 over the period 1996-2008.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/403#1</TD>
            <TD>2011-09-14T20:53:32Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/35/403</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/403</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/35/403 [2]</TD>
            <TD>Optical Variabilities in 3C 120 (Doroshenko+, 2009)</TD>
            <TD>Based on our UBVRI observations and X-ray data from the RXTE satellite we have investigated the variabilities of the Seyfert Galaxy 3C 120 over the period 1996-2008.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/403#2</TD>
            <TD>2011-09-14T20:53:32Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/35/403&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/403</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/1016 [1]</TD>
            <TD>Kinematics of local RR lyrae stars. I. (Layden, 1994)</TD>
            <TD>In order to study the structure and formation history of the galaxy, we have obtained low-to-moderate dispersion spectra of 302 nearby RR Lyrae variables of Bailey type "ab". We derived abundances, typically accurate to 0.15-0.20dex and calibrated to the Zinn &amp; West (1984ApJS...55...45Z) globular cluster metallicity scale, from the pseudo-equivalent widths of the Ca II K, Hdelta, Hgamma, and Hbeta lines. Radial velocities accurate to between 2 and 30km/s were obtained from the spectra and from the literature. Distances accurate to between 5% and 20% were derived from published apparent magnitudes and Burstein &amp; Heiles (1982AJ.....87.1165B) reddenings. The metallicity distribution of the RR Lyrae stars peaks at [Fe/H]_K_ =~ -1.5, and is narrower than that of the Ryan &amp; Norris (1991AJ....101.1865R) subdwarfs, as expected since the most metal-rich and metal-poor progenitors preferentially appear as stable red and blue horizontal branch stars, rather than as RR Lyrae. The metal-rich tail of the RR Lyrae distribution extends to [Fe/H]_K_{approx}0, and a qualitative analysis of the distribution of distances from the galactic plane shows that the stars in this tail (i.e., [Fe/H]_K_&gt;-1.0) are more concentrated to the plane than the more metal-poor stars. The abundance distribution of the local RR Lyrae stars is in excellent agreement with the changing abundance distributions of distant RR Lyrae stars as a function of galactocentric distance, as derived by Suntzeff et al. (1991ApJ...367..528S), who ascribed this change to systematic variations in horizontal branch morphology (probably age variations) with galactocentric distance. The abundance distribution of the local RR Lyrae stars also agrees well with those of the distant RR Lyrae stars as a function of distance from the galactic plane. There is no evidence for an abundance gradient in this direction, suggesting that gaseous dissipation did not play a major role in the formation of the outer halo.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1016#1</TD>
            <TD>2011-09-14T18:50:06Z</TD>
            <TD>#Abundances#Photometry#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1016</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/1016</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1016</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/1016 [2]</TD>
            <TD>Kinematics of local RR lyrae stars. I. (Layden, 1994)</TD>
            <TD>In order to study the structure and formation history of the galaxy, we have obtained low-to-moderate dispersion spectra of 302 nearby RR Lyrae variables of Bailey type "ab". We derived abundances, typically accurate to 0.15-0.20dex and calibrated to the Zinn &amp; West (1984ApJS...55...45Z) globular cluster metallicity scale, from the pseudo-equivalent widths of the Ca II K, Hdelta, Hgamma, and Hbeta lines. Radial velocities accurate to between 2 and 30km/s were obtained from the spectra and from the literature. Distances accurate to between 5% and 20% were derived from published apparent magnitudes and Burstein &amp; Heiles (1982AJ.....87.1165B) reddenings. The metallicity distribution of the RR Lyrae stars peaks at [Fe/H]_K_ =~ -1.5, and is narrower than that of the Ryan &amp; Norris (1991AJ....101.1865R) subdwarfs, as expected since the most metal-rich and metal-poor progenitors preferentially appear as stable red and blue horizontal branch stars, rather than as RR Lyrae. The metal-rich tail of the RR Lyrae distribution extends to [Fe/H]_K_{approx}0, and a qualitative analysis of the distribution of distances from the galactic plane shows that the stars in this tail (i.e., [Fe/H]_K_&gt;-1.0) are more concentrated to the plane than the more metal-poor stars. The abundance distribution of the local RR Lyrae stars is in excellent agreement with the changing abundance distributions of distant RR Lyrae stars as a function of galactocentric distance, as derived by Suntzeff et al. (1991ApJ...367..528S), who ascribed this change to systematic variations in horizontal branch morphology (probably age variations) with galactocentric distance. The abundance distribution of the local RR Lyrae stars also agrees well with those of the distant RR Lyrae stars as a function of distance from the galactic plane. There is no evidence for an abundance gradient in this direction, suggesting that gaseous dissipation did not play a major role in the formation of the outer halo.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1016#2</TD>
            <TD>2011-09-14T18:50:06Z</TD>
            <TD>#Abundances#Photometry#Velocities#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1016</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/1016&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1016</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/584 [1]</TD>
            <TD>Cl J0023+0423 and Cl J1604+4304 morphology (Lubin+ 1998)</TD>
            <TD>We present a detailed morphological analysis of the galaxy populations in the first two clusters to be completed in an extensive observational study of nine high-redshift clusters of galaxies. These two clusters, Cl 0023+0423 and Cl 1604+4304, are at redshifts of z=0.84 and z=0.90, respectively. The morphological studies are based on high angular resolution imagery taken with Wide Field Planetary Camera 2 aboard the Hubble Space Telescope. These data are combined with deep, ground-based BVRI photometry and spectra taken with the Keck 10m telescopes. The morphological classifications presented in this paper consist of two parts. First, we provide a quantitative description of the structural properties of ~600 galaxies per cluster field using the Medium Deep Survey automated data reduction and object classification software. This analysis includes the galaxy position, photometry, and best-fit bulge+disk model. Second, for the brightest subsample of ~200 galaxies per cluster field, we provide a more detailed morphological description through a visual classification based on the revised Hubble classification scheme.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/584#1</TD>
            <TD>2011-09-14T18:52:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/584</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/584</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/584</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/584 [2]</TD>
            <TD>Cl J0023+0423 and Cl J1604+4304 morphology (Lubin+ 1998)</TD>
            <TD>We present a detailed morphological analysis of the galaxy populations in the first two clusters to be completed in an extensive observational study of nine high-redshift clusters of galaxies. These two clusters, Cl 0023+0423 and Cl 1604+4304, are at redshifts of z=0.84 and z=0.90, respectively. The morphological studies are based on high angular resolution imagery taken with Wide Field Planetary Camera 2 aboard the Hubble Space Telescope. These data are combined with deep, ground-based BVRI photometry and spectra taken with the Keck 10m telescopes. The morphological classifications presented in this paper consist of two parts. First, we provide a quantitative description of the structural properties of ~600 galaxies per cluster field using the Medium Deep Survey automated data reduction and object classification software. This analysis includes the galaxy position, photometry, and best-fit bulge+disk model. Second, for the brightest subsample of ~200 galaxies per cluster field, we provide a more detailed morphological description through a visual classification based on the revised Hubble classification scheme.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/584#2</TD>
            <TD>2011-09-14T18:52:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/584</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/584&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/584</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/584 [1]</TD>
            <TD>Cl J0023+0423 and Cl J1604+4304 morphology (Lubin+ 1998)</TD>
            <TD>We present a detailed morphological analysis of the galaxy populations in the first two clusters to be completed in an extensive observational study of nine high-redshift clusters of galaxies. These two clusters, Cl 0023+0423 and Cl 1604+4304, are at redshifts of z=0.84 and z=0.90, respectively. The morphological studies are based on high angular resolution imagery taken with Wide Field Planetary Camera 2 aboard the Hubble Space Telescope. These data are combined with deep, ground-based BVRI photometry and spectra taken with the Keck 10m telescopes. The morphological classifications presented in this paper consist of two parts. First, we provide a quantitative description of the structural properties of ~600 galaxies per cluster field using the Medium Deep Survey automated data reduction and object classification software. This analysis includes the galaxy position, photometry, and best-fit bulge+disk model. Second, for the brightest subsample of ~200 galaxies per cluster field, we provide a more detailed morphological description through a visual classification based on the revised Hubble classification scheme.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/584#1</TD>
            <TD>2011-09-14T18:52:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/584</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/584</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/584</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/584 [2]</TD>
            <TD>Cl J0023+0423 and Cl J1604+4304 morphology (Lubin+ 1998)</TD>
            <TD>We present a detailed morphological analysis of the galaxy populations in the first two clusters to be completed in an extensive observational study of nine high-redshift clusters of galaxies. These two clusters, Cl 0023+0423 and Cl 1604+4304, are at redshifts of z=0.84 and z=0.90, respectively. The morphological studies are based on high angular resolution imagery taken with Wide Field Planetary Camera 2 aboard the Hubble Space Telescope. These data are combined with deep, ground-based BVRI photometry and spectra taken with the Keck 10m telescopes. The morphological classifications presented in this paper consist of two parts. First, we provide a quantitative description of the structural properties of ~600 galaxies per cluster field using the Medium Deep Survey automated data reduction and object classification software. This analysis includes the galaxy position, photometry, and best-fit bulge+disk model. Second, for the brightest subsample of ~200 galaxies per cluster field, we provide a more detailed morphological description through a visual classification based on the revised Hubble classification scheme.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/584#2</TD>
            <TD>2011-09-14T18:52:57Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/584</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/584&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/584</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/452/238 [1]</TD>
            <TD>HST photometry of I Zw 18 massive stars (Hunter+ 1995)</TD>
            <TD>Blue compact dwarf galaxies are tiny galaxies that are dominated by intense star-forming regions. Thus, they have been thought to represent a different and extreme environment for star formation compared to the Milky Way and many other nearby galaxies. In this paper we use images obtained with the Hubble Space Telescope to resolve the main body of one of these galaxies, I Zw 18, into stars for the first time. This galaxy is also one of the most metal-poor galaxies known and is sometimes argued to be evolutionarily young. Broadband colors are used to determine the bulk characteristics of the resolved stellar population to an F555W magnitude of about 26, or M_(V,0)~-4 (O9.5 V star). Narrow-band images are used to look for emission characteristic of Wolf-Rayet stars. Color-magnitude diagrams reveal a broad main sequence of massive stars as well as blue and red supergiants, although there is a surprising lack of Wolf-Rayet stars. About half the massive stars are located in two groups, corresponding to the two knots of emission identified in ground-based images, and the rest are distributed between these regions and in the outer parts of the galaxy. We find that the northwestern of these two regions resolves in Halpha images into a small H II region plus a complicated shell structure that encircles the northern stellar association. There are additional, larger loops and filaments of ionized gas up to 450pc from the center of the galaxy. While the shell could be as young as the stars it encircles, the larger ionized gas structures must be older for reasonable models, and their presence implies that there has been a previous generation of massive stars at least several tens of millions of years ago. However, we find no evidence in these data for stars that must be older than this. The larger sites of most recent star formation are located northwest and south of the central part of the galaxy. Thus, we find that I Zw 18 is somewhat more complicated than had previously been thought, both in terms of its star formation history and the state of its interstellar medium. At the same time, however, the stellar populations look relatively normal, and the spatial concentration of massive stars is closer to that of large OB associations in nearby galaxies rather than to that exemplified by the compact cluster R136 in the Large Magellanic Cloud.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/452/238#1</TD>
            <TD>2011-09-14T18:23:30Z</TD>
            <TD>#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/452/238</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/452/238</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/452/238</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/452/238 [2]</TD>
            <TD>HST photometry of I Zw 18 massive stars (Hunter+ 1995)</TD>
            <TD>Blue compact dwarf galaxies are tiny galaxies that are dominated by intense star-forming regions. Thus, they have been thought to represent a different and extreme environment for star formation compared to the Milky Way and many other nearby galaxies. In this paper we use images obtained with the Hubble Space Telescope to resolve the main body of one of these galaxies, I Zw 18, into stars for the first time. This galaxy is also one of the most metal-poor galaxies known and is sometimes argued to be evolutionarily young. Broadband colors are used to determine the bulk characteristics of the resolved stellar population to an F555W magnitude of about 26, or M_(V,0)~-4 (O9.5 V star). Narrow-band images are used to look for emission characteristic of Wolf-Rayet stars. Color-magnitude diagrams reveal a broad main sequence of massive stars as well as blue and red supergiants, although there is a surprising lack of Wolf-Rayet stars. About half the massive stars are located in two groups, corresponding to the two knots of emission identified in ground-based images, and the rest are distributed between these regions and in the outer parts of the galaxy. We find that the northwestern of these two regions resolves in Halpha images into a small H II region plus a complicated shell structure that encircles the northern stellar association. There are additional, larger loops and filaments of ionized gas up to 450pc from the center of the galaxy. While the shell could be as young as the stars it encircles, the larger ionized gas structures must be older for reasonable models, and their presence implies that there has been a previous generation of massive stars at least several tens of millions of years ago. However, we find no evidence in these data for stars that must be older than this. The larger sites of most recent star formation are located northwest and south of the central part of the galaxy. Thus, we find that I Zw 18 is somewhat more complicated than had previously been thought, both in terms of its star formation history and the state of its interstellar medium. At the same time, however, the stellar populations look relatively normal, and the spatial concentration of massive stars is closer to that of large OB associations in nearby galaxies rather than to that exemplified by the compact cluster R136 in the Large Magellanic Cloud.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/452/238#2</TD>
            <TD>2011-09-14T18:23:30Z</TD>
            <TD>#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/452/238</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/452/238&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/452/238</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/135/511 [1]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#1</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/135/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/135/511 [2]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#2</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table1]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table1</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table3]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table3</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table4]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table4</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table5]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table5</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/473/822 [1]</TD>
            <TD>APS Catalog of Galaxies behind Virgo (Hoffman+ 1996)</TD>
            <TD>Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. &lt;VII/49&gt;) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822#1</TD>
            <TD>2011-09-14T18:23:43Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/473/822</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/473/822</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/473/822 [2]</TD>
            <TD>APS Catalog of Galaxies behind Virgo (Hoffman+ 1996)</TD>
            <TD>Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. &lt;VII/49&gt;) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822#2</TD>
            <TD>2011-09-14T18:23:43Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/473/822&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/473/822</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/473/822 [table3]</TD>
            <TD>APS Catalog of Galaxies behind Virgo (Hoffman+ 1996)</TD>
            <TD>Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. &lt;VII/49&gt;) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822#table3</TD>
            <TD>2011-09-14T18:23:43Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/473/822&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/473/822</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/135/511 [1]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#1</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/135/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/135/511 [2]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#2</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table1]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table1</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table3]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table3</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table4]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table4</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table5]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table5</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/135/511 [1]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#1</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/135/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/135/511 [2]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#2</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table1]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table1</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table3]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table3</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table4]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table4</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/135/511 [table5]</TD>
            <TD>The Hamburg/SAO Survey for ELGs (Ugryumov+ 1999)</TD>
            <TD>We present first results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia) which is based on the digitized objective-prism photoplates database of the Hamburg Quasar Survey (HQS). The main goal of this survey is the search for emission-line galaxies (ELG) in order to create a new deep sample of blue compact galaxies (BCG) in a large sky area. Another important goal of this work is to search for new extremely low-metallicity galaxies. We present the first results of spectroscopy obtained with the 2.2m telescope at the German-Spanish Observatory at Calar Alto, and with the 6m telescope at the Russian Special Astrophysical Observatory. The primary ELG candidate selection criteria applied were a blue continuum (near 4000{AA}) and the presence of emission lines close to 5000A recognized on digitized prism spectra of galaxies with magnitudes in the range B =16.0-19.5. The spectroscopy resulted in the detection or/and quantitative spectral classification of 74 emission-line objects. Of them 55 are newly discovered, and 19 were already known as galaxies before. 11 of the latter have redshifts and are known ELGs. For most of the known galaxies emission line ratios were measured for the first time and an improved classification is presented. 47 objects are classified as BCGs, one as Sy2 galaxy, six as probable LINERs, and four as new QSOs. The remaining galaxies do not show significant H{beta} and [OIII]4959,5007{AA} emission lines, and are likely either low-ionization starburst or dwarf amorphous nuclear starburst galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511#table5</TD>
            <TD>2011-09-14T18:53:45Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/135/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/135/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/135/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/21/652 [1]</TD>
            <TD>Optical variability in NGC 7469 (Lyuty+, 1995)</TD>
            <TD>The results of three-color UBV observations of rapid variability in the nucleus of the Seyfert galaxy NGC 7469 carried out in 1990-1994 are presented. The observations have been carried out during 15 different nights using the 60- and 125-cm telescopes with time resolution of 6-8min (50 hours monitoring) with the aperture of 27.5". The mean errors of one measurement are 1.8, 1.2 and 1.4% for U, B and V. The data set length during one night is from 2 up to 5h. The different nights show the variations at different level: from weak, when the standard deviation during the night exceeds the error of one measurement only by 10-20%, up to strong ones, when the standard deviation exceeds the error of the measurement by factor two.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/21/652#1</TD>
            <TD>2011-09-14T18:54:02Z</TD>
            <TD>#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/21/652</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/21/652</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/21/652</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/21/652 [2]</TD>
            <TD>Optical variability in NGC 7469 (Lyuty+, 1995)</TD>
            <TD>The results of three-color UBV observations of rapid variability in the nucleus of the Seyfert galaxy NGC 7469 carried out in 1990-1994 are presented. The observations have been carried out during 15 different nights using the 60- and 125-cm telescopes with time resolution of 6-8min (50 hours monitoring) with the aperture of 27.5". The mean errors of one measurement are 1.8, 1.2 and 1.4% for U, B and V. The data set length during one night is from 2 up to 5h. The different nights show the variations at different level: from weak, when the standard deviation during the night exceeds the error of one measurement only by 10-20%, up to strong ones, when the standard deviation exceeds the error of the measurement by factor two.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/21/652#2</TD>
            <TD>2011-09-14T18:54:02Z</TD>
            <TD>#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/21/652</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/21/652&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/21/652</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/21/652 [1]</TD>
            <TD>Optical variability in NGC 7469 (Lyuty+, 1995)</TD>
            <TD>The results of three-color UBV observations of rapid variability in the nucleus of the Seyfert galaxy NGC 7469 carried out in 1990-1994 are presented. The observations have been carried out during 15 different nights using the 60- and 125-cm telescopes with time resolution of 6-8min (50 hours monitoring) with the aperture of 27.5". The mean errors of one measurement are 1.8, 1.2 and 1.4% for U, B and V. The data set length during one night is from 2 up to 5h. The different nights show the variations at different level: from weak, when the standard deviation during the night exceeds the error of one measurement only by 10-20%, up to strong ones, when the standard deviation exceeds the error of the measurement by factor two.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/21/652#1</TD>
            <TD>2011-09-14T18:54:02Z</TD>
            <TD>#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/21/652</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/21/652</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/21/652</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/21/652 [2]</TD>
            <TD>Optical variability in NGC 7469 (Lyuty+, 1995)</TD>
            <TD>The results of three-color UBV observations of rapid variability in the nucleus of the Seyfert galaxy NGC 7469 carried out in 1990-1994 are presented. The observations have been carried out during 15 different nights using the 60- and 125-cm telescopes with time resolution of 6-8min (50 hours monitoring) with the aperture of 27.5". The mean errors of one measurement are 1.8, 1.2 and 1.4% for U, B and V. The data set length during one night is from 2 up to 5h. The different nights show the variations at different level: from weak, when the standard deviation during the night exceeds the error of one measurement only by 10-20%, up to strong ones, when the standard deviation exceeds the error of the measurement by factor two.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/21/652#2</TD>
            <TD>2011-09-14T18:54:02Z</TD>
            <TD>#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/21/652</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/21/652&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/21/652</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1094 [1]</TD>
            <TD>MAPS-PP catalog of galaxies (Cabanela+, 1998)</TD>
            <TD>A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094#1</TD>
            <TD>2011-09-14T18:54:09Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1094</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1094</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1094 [2]</TD>
            <TD>MAPS-PP catalog of galaxies (Cabanela+, 1998)</TD>
            <TD>A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094#2</TD>
            <TD>2011-09-14T18:54:09Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1094&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1094</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1094 [table2]</TD>
            <TD>MAPS-PP catalog of galaxies (Cabanela+, 1998)</TD>
            <TD>A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094#table2</TD>
            <TD>2011-09-14T18:54:09Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1094&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1094</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1094 [1]</TD>
            <TD>MAPS-PP catalog of galaxies (Cabanela+, 1998)</TD>
            <TD>A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094#1</TD>
            <TD>2011-09-14T18:54:09Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1094</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1094</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1094 [2]</TD>
            <TD>MAPS-PP catalog of galaxies (Cabanela+, 1998)</TD>
            <TD>A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094#2</TD>
            <TD>2011-09-14T18:54:09Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1094&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1094</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1094 [table2]</TD>
            <TD>MAPS-PP catalog of galaxies (Cabanela+, 1998)</TD>
            <TD>A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094#table2</TD>
            <TD>2011-09-14T18:54:09Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1094&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1094</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1094 [1]</TD>
            <TD>MAPS-PP catalog of galaxies (Cabanela+, 1998)</TD>
            <TD>A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094#1</TD>
            <TD>2011-09-14T18:54:09Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1094</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1094</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1094 [2]</TD>
            <TD>MAPS-PP catalog of galaxies (Cabanela+, 1998)</TD>
            <TD>A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094#2</TD>
            <TD>2011-09-14T18:54:09Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1094&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1094</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/1094 [table2]</TD>
            <TD>MAPS-PP catalog of galaxies (Cabanela+, 1998)</TD>
            <TD>A search for preferential galaxy alignments in the Pisces-Perseus Supercluster (PPS) is made using the Minnesota Automated Plate Scanner Pisces-Perseus Survey (MAPS-PP). The MAPS-PP is a catalog of ~1400 galaxies with a (roughly) isophotal diameter greater than 30" constructed from digitized scans of the blue and red plates of the Palomar Observatory Sky Survey covering the PPS. This is the largest sample of galaxies applied to a search of galaxy alignments in this supercluster, and it has been used in combination with previously published redshifts to construct the deepest PPS galaxy luminosity function to date. While previous studies have relied extensively on catalogs with visually estimated parameters for both sample selection and determination of galaxy orientation, the MAPS-PP uses selection criteria and measurements that are entirely machine and computer based. Therefore, it is not susceptible to some of the biases, such as the diameter inclination effect, known to exist in some other galaxy catalogs. The presence of anisotropic galaxy distributions is determined by use of the Kuiper statistic, a robust alternative to the chi^2 statistic more traditionally used in these studies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094#table2</TD>
            <TD>2011-09-14T18:54:09Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1094</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/1094&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1094</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/300/417 [1]</TD>
            <TD>Durham/UKST Galaxy Redshift Survey (Ratcliffe+, 1998)</TD>
            <TD>We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417#1</TD>
            <TD>2011-09-14T18:54:31Z</TD>
            <TD>#Galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/300/417</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/417</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/300/417 [2]</TD>
            <TD>Durham/UKST Galaxy Redshift Survey (Ratcliffe+, 1998)</TD>
            <TD>We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417#2</TD>
            <TD>2011-09-14T18:54:31Z</TD>
            <TD>#Galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/300/417&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/417</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/300/417 [table5]</TD>
            <TD>Durham/UKST Galaxy Redshift Survey (Ratcliffe+, 1998)</TD>
            <TD>We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417#table5</TD>
            <TD>2011-09-14T18:54:31Z</TD>
            <TD>#Galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/300/417&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/417</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/300/417 [1]</TD>
            <TD>Durham/UKST Galaxy Redshift Survey (Ratcliffe+, 1998)</TD>
            <TD>We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417#1</TD>
            <TD>2011-09-14T18:54:31Z</TD>
            <TD>#Galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/300/417</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/417</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/300/417 [2]</TD>
            <TD>Durham/UKST Galaxy Redshift Survey (Ratcliffe+, 1998)</TD>
            <TD>We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417#2</TD>
            <TD>2011-09-14T18:54:31Z</TD>
            <TD>#Galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/300/417&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/417</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/300/417 [table5]</TD>
            <TD>Durham/UKST Galaxy Redshift Survey (Ratcliffe+, 1998)</TD>
            <TD>We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417#table5</TD>
            <TD>2011-09-14T18:54:31Z</TD>
            <TD>#Galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/300/417&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/417</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/300/417 [1]</TD>
            <TD>Durham/UKST Galaxy Redshift Survey (Ratcliffe+, 1998)</TD>
            <TD>We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417#1</TD>
            <TD>2011-09-14T18:54:31Z</TD>
            <TD>#Galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/300/417</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/417</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/300/417 [2]</TD>
            <TD>Durham/UKST Galaxy Redshift Survey (Ratcliffe+, 1998)</TD>
            <TD>We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417#2</TD>
            <TD>2011-09-14T18:54:31Z</TD>
            <TD>#Galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/300/417&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/417</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/300/417 [table5]</TD>
            <TD>Durham/UKST Galaxy Redshift Survey (Ratcliffe+, 1998)</TD>
            <TD>We present the radial velocities and blue, optical magnitudes for all of the galaxies within the Durham/UKST Galaxy Redshift Survey. This catalogue consists of ~2500 galaxy redshifts to a limiting apparent magnitude of B_J_~17mag, covering a ~1500deg^2^ area around the South Galactic Pole. The galaxies in this survey were selected from the Edinburgh/Durham Southern Galaxy Catalogue and were sampled, in order of apparent magnitude, at a rate of one galaxy in every three. The spectroscopy was performed at the 1.2-m UK Schmidt Telescope in Australia using the FLAIR multi-object spectrograph. We show that our radial velocity measurements made with this instrument have an empirical accuracy of +/-150km/s. The observational techniques and data reduction procedures used in the construction of this survey are also discussed. This survey demonstrates that the UKST can be used to make a three-dimensional map of the large-scale galaxy distribution, via a redshift survey to b_J_~17mag, over a wide area of the sky.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417#table5</TD>
            <TD>2011-09-14T18:54:31Z</TD>
            <TD>#Galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/300/417</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/300/417&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/300/417</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/58 [1]</TD>
            <TD>[Fe/H], Vel, Orbits of F2-K5 Dwarfs 80pc from Sun (Marsakov+ 1988)</TD>
            <TD>In this catalog, metallicities, distances, components of space velocities and parameters of osculating orbits are calculated for 1065 F2-K5 dwarfs with UBV photometric data, proper motions and radial velocities. The present sample is composed on the base of the Ochsenbein (1980) catalogue and contains the stars of the V (IV-V) luminosity class, within the colour range 0.35&lt;B-V&lt;1.10 (which corresponds to the spectral class range F2-K5). Sandage's (1969) Hyades sequence was used to determine the value delta (U-B) for each star. The authors calibrated the ultraviolet excess in terms of [Fe/H] separately for the four of the temperature index (B-V) where delta(U-B) practically does not depend on the effective temperature. Intervals in (B-V) correspond to the following division on spectral class intervals: F2-F9, G0-G4, and G5-G9, K0-K5. Metallicity is calculated from the formulae: [Fe/H]=-5.3*delta(U-B)+0.02 for stars F2-F9 [Fe/H]=-5.1*delta(U-B)+0.13 for stars G0-G4 [Fe/H]=-5.4*delta(U-B)+0.02 for stars G5-G9 [Fe/H]=-4.7*delta(U-B)-0.04 for stars K0-K5 These relations follow from the assumption that mean metallicity and metallicity dispersion for stars of all spectral classes are the same. Distances to the stars were calculated from spectral parallaxes. Absolute magnitudes (M(V)) were obtained from the Sp,M(V)-relation for dwarfs (Straizys, 1982). The sample includes only stars nearer than 80 pc because reddening is negligible for them. The obtained distances together with radial velocities and proper motions are used to calculate the components of space velocities. The eccentricities, apogalactic and perigalactic distances of the stars were calculated from the osculating orbit approximation according to the galaxy model from the paper by Eggen et al. (1962).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/58#1</TD>
            <TD>2011-09-14T18:54:47Z</TD>
            <TD>#Abundances#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/V/58</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/58</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/58</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/58 [2]</TD>
            <TD>[Fe/H], Vel, Orbits of F2-K5 Dwarfs 80pc from Sun (Marsakov+ 1988)</TD>
            <TD>In this catalog, metallicities, distances, components of space velocities and parameters of osculating orbits are calculated for 1065 F2-K5 dwarfs with UBV photometric data, proper motions and radial velocities. The present sample is composed on the base of the Ochsenbein (1980) catalogue and contains the stars of the V (IV-V) luminosity class, within the colour range 0.35&lt;B-V&lt;1.10 (which corresponds to the spectral class range F2-K5). Sandage's (1969) Hyades sequence was used to determine the value delta (U-B) for each star. The authors calibrated the ultraviolet excess in terms of [Fe/H] separately for the four of the temperature index (B-V) where delta(U-B) practically does not depend on the effective temperature. Intervals in (B-V) correspond to the following division on spectral class intervals: F2-F9, G0-G4, and G5-G9, K0-K5. Metallicity is calculated from the formulae: [Fe/H]=-5.3*delta(U-B)+0.02 for stars F2-F9 [Fe/H]=-5.1*delta(U-B)+0.13 for stars G0-G4 [Fe/H]=-5.4*delta(U-B)+0.02 for stars G5-G9 [Fe/H]=-4.7*delta(U-B)-0.04 for stars K0-K5 These relations follow from the assumption that mean metallicity and metallicity dispersion for stars of all spectral classes are the same. Distances to the stars were calculated from spectral parallaxes. Absolute magnitudes (M(V)) were obtained from the Sp,M(V)-relation for dwarfs (Straizys, 1982). The sample includes only stars nearer than 80 pc because reddening is negligible for them. The obtained distances together with radial velocities and proper motions are used to calculate the components of space velocities. The eccentricities, apogalactic and perigalactic distances of the stars were calculated from the osculating orbit approximation according to the galaxy model from the paper by Eggen et al. (1962).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/58#2</TD>
            <TD>2011-09-14T18:54:47Z</TD>
            <TD>#Abundances#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/V/58</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/58&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/58</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/619/193 [1]</TD>
            <TD>Catalog of nearby cluster galaxy photometry (McIntosh+, 2005)</TD>
            <TD>We observed clusters A85, A496, and A754 during two runs at the Kitt Peak National Observatory (KPNO) 0.9m Telescope with the NOAO Mosaic Wide-Field Imager. We used the engineering-grade Mosaic for the V data in 1997 November and the science-grade Mosaic with thinned CCDs for the U band in 2000 January.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193#1</TD>
            <TD>2011-09-14T19:44:16Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/619/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/619/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/619/193 [2]</TD>
            <TD>Catalog of nearby cluster galaxy photometry (McIntosh+, 2005)</TD>
            <TD>We observed clusters A85, A496, and A754 during two runs at the Kitt Peak National Observatory (KPNO) 0.9m Telescope with the NOAO Mosaic Wide-Field Imager. We used the engineering-grade Mosaic for the V data in 1997 November and the science-grade Mosaic with thinned CCDs for the U band in 2000 January.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193#2</TD>
            <TD>2011-09-14T19:44:16Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/619/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/619/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/619/193 [table6]</TD>
            <TD>Catalog of nearby cluster galaxy photometry (McIntosh+, 2005)</TD>
            <TD>We observed clusters A85, A496, and A754 during two runs at the Kitt Peak National Observatory (KPNO) 0.9m Telescope with the NOAO Mosaic Wide-Field Imager. We used the engineering-grade Mosaic for the V data in 1997 November and the science-grade Mosaic with thinned CCDs for the U band in 2000 January.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193#table6</TD>
            <TD>2011-09-14T19:44:16Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/619/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/619/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/473/822 [1]</TD>
            <TD>APS Catalog of Galaxies behind Virgo (Hoffman+ 1996)</TD>
            <TD>Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. &lt;VII/49&gt;) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822#1</TD>
            <TD>2011-09-14T18:23:43Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/473/822</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/473/822</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/473/822 [2]</TD>
            <TD>APS Catalog of Galaxies behind Virgo (Hoffman+ 1996)</TD>
            <TD>Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. &lt;VII/49&gt;) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822#2</TD>
            <TD>2011-09-14T18:23:43Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/473/822&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/473/822</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/473/822 [table3]</TD>
            <TD>APS Catalog of Galaxies behind Virgo (Hoffman+ 1996)</TD>
            <TD>Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. &lt;VII/49&gt;) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822#table3</TD>
            <TD>2011-09-14T18:23:43Z</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/473/822&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/473/822</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/58 [1]</TD>
            <TD>[Fe/H], Vel, Orbits of F2-K5 Dwarfs 80pc from Sun (Marsakov+ 1988)</TD>
            <TD>In this catalog, metallicities, distances, components of space velocities and parameters of osculating orbits are calculated for 1065 F2-K5 dwarfs with UBV photometric data, proper motions and radial velocities. The present sample is composed on the base of the Ochsenbein (1980) catalogue and contains the stars of the V (IV-V) luminosity class, within the colour range 0.35&lt;B-V&lt;1.10 (which corresponds to the spectral class range F2-K5). Sandage's (1969) Hyades sequence was used to determine the value delta (U-B) for each star. The authors calibrated the ultraviolet excess in terms of [Fe/H] separately for the four of the temperature index (B-V) where delta(U-B) practically does not depend on the effective temperature. Intervals in (B-V) correspond to the following division on spectral class intervals: F2-F9, G0-G4, and G5-G9, K0-K5. Metallicity is calculated from the formulae: [Fe/H]=-5.3*delta(U-B)+0.02 for stars F2-F9 [Fe/H]=-5.1*delta(U-B)+0.13 for stars G0-G4 [Fe/H]=-5.4*delta(U-B)+0.02 for stars G5-G9 [Fe/H]=-4.7*delta(U-B)-0.04 for stars K0-K5 These relations follow from the assumption that mean metallicity and metallicity dispersion for stars of all spectral classes are the same. Distances to the stars were calculated from spectral parallaxes. Absolute magnitudes (M(V)) were obtained from the Sp,M(V)-relation for dwarfs (Straizys, 1982). The sample includes only stars nearer than 80 pc because reddening is negligible for them. The obtained distances together with radial velocities and proper motions are used to calculate the components of space velocities. The eccentricities, apogalactic and perigalactic distances of the stars were calculated from the osculating orbit approximation according to the galaxy model from the paper by Eggen et al. (1962).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/58#1</TD>
            <TD>2011-09-14T18:54:47Z</TD>
            <TD>#Abundances#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/V/58</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/58</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/58</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/58 [2]</TD>
            <TD>[Fe/H], Vel, Orbits of F2-K5 Dwarfs 80pc from Sun (Marsakov+ 1988)</TD>
            <TD>In this catalog, metallicities, distances, components of space velocities and parameters of osculating orbits are calculated for 1065 F2-K5 dwarfs with UBV photometric data, proper motions and radial velocities. The present sample is composed on the base of the Ochsenbein (1980) catalogue and contains the stars of the V (IV-V) luminosity class, within the colour range 0.35&lt;B-V&lt;1.10 (which corresponds to the spectral class range F2-K5). Sandage's (1969) Hyades sequence was used to determine the value delta (U-B) for each star. The authors calibrated the ultraviolet excess in terms of [Fe/H] separately for the four of the temperature index (B-V) where delta(U-B) practically does not depend on the effective temperature. Intervals in (B-V) correspond to the following division on spectral class intervals: F2-F9, G0-G4, and G5-G9, K0-K5. Metallicity is calculated from the formulae: [Fe/H]=-5.3*delta(U-B)+0.02 for stars F2-F9 [Fe/H]=-5.1*delta(U-B)+0.13 for stars G0-G4 [Fe/H]=-5.4*delta(U-B)+0.02 for stars G5-G9 [Fe/H]=-4.7*delta(U-B)-0.04 for stars K0-K5 These relations follow from the assumption that mean metallicity and metallicity dispersion for stars of all spectral classes are the same. Distances to the stars were calculated from spectral parallaxes. Absolute magnitudes (M(V)) were obtained from the Sp,M(V)-relation for dwarfs (Straizys, 1982). The sample includes only stars nearer than 80 pc because reddening is negligible for them. The obtained distances together with radial velocities and proper motions are used to calculate the components of space velocities. The eccentricities, apogalactic and perigalactic distances of the stars were calculated from the osculating orbit approximation according to the galaxy model from the paper by Eggen et al. (1962).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/58#2</TD>
            <TD>2011-09-14T18:54:47Z</TD>
            <TD>#Abundances#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/V/58</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/58&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/58</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/473/822 [1]</TD>
            <TD>APS Catalog of Galaxies behind Virgo (Hoffman+ 1996)</TD>
            <TD>Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. &lt;VII/49&gt;) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822#1</TD>
            <TD>2011-09-14T18:23:43Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/473/822</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/473/822</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/473/822 [2]</TD>
            <TD>APS Catalog of Galaxies behind Virgo (Hoffman+ 1996)</TD>
            <TD>Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. &lt;VII/49&gt;) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822#2</TD>
            <TD>2011-09-14T18:23:43Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/473/822&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/473/822</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/473/822 [table3]</TD>
            <TD>APS Catalog of Galaxies behind Virgo (Hoffman+ 1996)</TD>
            <TD>Table 3 lists the galaxies found by the scanner in each of the 17 fields. The table is organized by CGCG (see Cat. &lt;VII/49&gt;) field, with a local running reference number ordered by increasing right ascension within that field. B24 is our estimate of the faintest B magnitude consistent with the four threshold crossings for each galaxy, and Btot is our attempt to estimate the total B magnitude extrapolated to zero surface brightness. The diameters of circles with areas equal to the ellipses fit to the four threshold crossings are given, along with the ellipticities of those ellipses. For broken images ("clumps"), only the ellipticity of the outermost ellipse is given. On the second line for each galaxy, we give corresponding measurements of R24, diameters and ellipticities from the E plate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822#table3</TD>
            <TD>2011-09-14T18:23:43Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/473/822</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/473/822&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/473/822</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/58 [1]</TD>
            <TD>[Fe/H], Vel, Orbits of F2-K5 Dwarfs 80pc from Sun (Marsakov+ 1988)</TD>
            <TD>In this catalog, metallicities, distances, components of space velocities and parameters of osculating orbits are calculated for 1065 F2-K5 dwarfs with UBV photometric data, proper motions and radial velocities. The present sample is composed on the base of the Ochsenbein (1980) catalogue and contains the stars of the V (IV-V) luminosity class, within the colour range 0.35&lt;B-V&lt;1.10 (which corresponds to the spectral class range F2-K5). Sandage's (1969) Hyades sequence was used to determine the value delta (U-B) for each star. The authors calibrated the ultraviolet excess in terms of [Fe/H] separately for the four of the temperature index (B-V) where delta(U-B) practically does not depend on the effective temperature. Intervals in (B-V) correspond to the following division on spectral class intervals: F2-F9, G0-G4, and G5-G9, K0-K5. Metallicity is calculated from the formulae: [Fe/H]=-5.3*delta(U-B)+0.02 for stars F2-F9 [Fe/H]=-5.1*delta(U-B)+0.13 for stars G0-G4 [Fe/H]=-5.4*delta(U-B)+0.02 for stars G5-G9 [Fe/H]=-4.7*delta(U-B)-0.04 for stars K0-K5 These relations follow from the assumption that mean metallicity and metallicity dispersion for stars of all spectral classes are the same. Distances to the stars were calculated from spectral parallaxes. Absolute magnitudes (M(V)) were obtained from the Sp,M(V)-relation for dwarfs (Straizys, 1982). The sample includes only stars nearer than 80 pc because reddening is negligible for them. The obtained distances together with radial velocities and proper motions are used to calculate the components of space velocities. The eccentricities, apogalactic and perigalactic distances of the stars were calculated from the osculating orbit approximation according to the galaxy model from the paper by Eggen et al. (1962).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/58#1</TD>
            <TD>2011-09-14T18:54:47Z</TD>
            <TD>#Abundances#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/V/58</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/58</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/58</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/58 [2]</TD>
            <TD>[Fe/H], Vel, Orbits of F2-K5 Dwarfs 80pc from Sun (Marsakov+ 1988)</TD>
            <TD>In this catalog, metallicities, distances, components of space velocities and parameters of osculating orbits are calculated for 1065 F2-K5 dwarfs with UBV photometric data, proper motions and radial velocities. The present sample is composed on the base of the Ochsenbein (1980) catalogue and contains the stars of the V (IV-V) luminosity class, within the colour range 0.35&lt;B-V&lt;1.10 (which corresponds to the spectral class range F2-K5). Sandage's (1969) Hyades sequence was used to determine the value delta (U-B) for each star. The authors calibrated the ultraviolet excess in terms of [Fe/H] separately for the four of the temperature index (B-V) where delta(U-B) practically does not depend on the effective temperature. Intervals in (B-V) correspond to the following division on spectral class intervals: F2-F9, G0-G4, and G5-G9, K0-K5. Metallicity is calculated from the formulae: [Fe/H]=-5.3*delta(U-B)+0.02 for stars F2-F9 [Fe/H]=-5.1*delta(U-B)+0.13 for stars G0-G4 [Fe/H]=-5.4*delta(U-B)+0.02 for stars G5-G9 [Fe/H]=-4.7*delta(U-B)-0.04 for stars K0-K5 These relations follow from the assumption that mean metallicity and metallicity dispersion for stars of all spectral classes are the same. Distances to the stars were calculated from spectral parallaxes. Absolute magnitudes (M(V)) were obtained from the Sp,M(V)-relation for dwarfs (Straizys, 1982). The sample includes only stars nearer than 80 pc because reddening is negligible for them. The obtained distances together with radial velocities and proper motions are used to calculate the components of space velocities. The eccentricities, apogalactic and perigalactic distances of the stars were calculated from the osculating orbit approximation according to the galaxy model from the paper by Eggen et al. (1962).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/58#2</TD>
            <TD>2011-09-14T18:54:47Z</TD>
            <TD>#Abundances#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/V/58</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/58&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/58</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/619/193 [1]</TD>
            <TD>Catalog of nearby cluster galaxy photometry (McIntosh+, 2005)</TD>
            <TD>We observed clusters A85, A496, and A754 during two runs at the Kitt Peak National Observatory (KPNO) 0.9m Telescope with the NOAO Mosaic Wide-Field Imager. We used the engineering-grade Mosaic for the V data in 1997 November and the science-grade Mosaic with thinned CCDs for the U band in 2000 January.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193#1</TD>
            <TD>2011-09-14T19:44:16Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/619/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/619/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/619/193 [2]</TD>
            <TD>Catalog of nearby cluster galaxy photometry (McIntosh+, 2005)</TD>
            <TD>We observed clusters A85, A496, and A754 during two runs at the Kitt Peak National Observatory (KPNO) 0.9m Telescope with the NOAO Mosaic Wide-Field Imager. We used the engineering-grade Mosaic for the V data in 1997 November and the science-grade Mosaic with thinned CCDs for the U band in 2000 January.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193#2</TD>
            <TD>2011-09-14T19:44:16Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/619/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/619/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/619/193 [table6]</TD>
            <TD>Catalog of nearby cluster galaxy photometry (McIntosh+, 2005)</TD>
            <TD>We observed clusters A85, A496, and A754 during two runs at the Kitt Peak National Observatory (KPNO) 0.9m Telescope with the NOAO Mosaic Wide-Field Imager. We used the engineering-grade Mosaic for the V data in 1997 November and the science-grade Mosaic with thinned CCDs for the U band in 2000 January.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193#table6</TD>
            <TD>2011-09-14T19:44:16Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/619/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/619/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/619/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/73/671 [1]</TD>
            <TD>M87 globular clusters photometry (Couture+, 1990)</TD>
            <TD>We present CCD photometry in B, V, and I for a sample of globular clusters in the Virgo central giant elliptical galaxy M87. Our measured sample comprises 270 objects brighter than V~23.4mag and with distances r&gt;25" (&gt;2kpc) from the center of the galaxy. In agreement with the recent study of Cohen, we find no detectable gradient of mean cluster color (metallicity) in (B-V) or (V-I) with radial distance. The cluster system does, however, display a large dispersion in color at any radius, corresponding to sigma([Fe/H])~0.6 about a mean metallicity (Fe/H]&gt;~-1.1 according to our color index scale. The difference in mean color between the globular clusters and the underlying halo light of the galaxy itself, found previously by Strom and coworkers and by Cohen, shows up strongly in all of our color indices; we find virtually no clusters as red as mean color of the halo stars at any radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/671#1</TD>
            <TD>2011-09-14T18:24:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/671</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/73/671</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/671</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/73/671 [2]</TD>
            <TD>M87 globular clusters photometry (Couture+, 1990)</TD>
            <TD>We present CCD photometry in B, V, and I for a sample of globular clusters in the Virgo central giant elliptical galaxy M87. Our measured sample comprises 270 objects brighter than V~23.4mag and with distances r&gt;25" (&gt;2kpc) from the center of the galaxy. In agreement with the recent study of Cohen, we find no detectable gradient of mean cluster color (metallicity) in (B-V) or (V-I) with radial distance. The cluster system does, however, display a large dispersion in color at any radius, corresponding to sigma([Fe/H])~0.6 about a mean metallicity (Fe/H]&gt;~-1.1 according to our color index scale. The difference in mean color between the globular clusters and the underlying halo light of the galaxy itself, found previously by Strom and coworkers and by Cohen, shows up strongly in all of our color indices; we find virtually no clusters as red as mean color of the halo stars at any radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/671#2</TD>
            <TD>2011-09-14T18:24:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/671</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/73/671&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/671</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/201 [1]</TD>
            <TD>Sternberg SN Catalogue, 1994Sep. (Tsvetkov+, 1995)</TD>
            <TD>We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/201#1</TD>
            <TD>2011-09-14T18:54:49Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/II/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/201</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/201</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/201 [2]</TD>
            <TD>Sternberg SN Catalogue, 1994Sep. (Tsvetkov+, 1995)</TD>
            <TD>We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/201#2</TD>
            <TD>2011-09-14T18:54:49Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/II/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/201&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/201 [catalog]</TD>
            <TD>Sternberg SN Catalogue, 1994Sep. (Tsvetkov+, 1995)</TD>
            <TD>We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/201#catalog</TD>
            <TD>2011-09-14T18:54:49Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/II/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/201</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/73/671 [1]</TD>
            <TD>M87 globular clusters photometry (Couture+, 1990)</TD>
            <TD>We present CCD photometry in B, V, and I for a sample of globular clusters in the Virgo central giant elliptical galaxy M87. Our measured sample comprises 270 objects brighter than V~23.4mag and with distances r&gt;25" (&gt;2kpc) from the center of the galaxy. In agreement with the recent study of Cohen, we find no detectable gradient of mean cluster color (metallicity) in (B-V) or (V-I) with radial distance. The cluster system does, however, display a large dispersion in color at any radius, corresponding to sigma([Fe/H])~0.6 about a mean metallicity (Fe/H]&gt;~-1.1 according to our color index scale. The difference in mean color between the globular clusters and the underlying halo light of the galaxy itself, found previously by Strom and coworkers and by Cohen, shows up strongly in all of our color indices; we find virtually no clusters as red as mean color of the halo stars at any radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/671#1</TD>
            <TD>2011-09-14T18:24:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/671</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/73/671</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/671</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/73/671 [2]</TD>
            <TD>M87 globular clusters photometry (Couture+, 1990)</TD>
            <TD>We present CCD photometry in B, V, and I for a sample of globular clusters in the Virgo central giant elliptical galaxy M87. Our measured sample comprises 270 objects brighter than V~23.4mag and with distances r&gt;25" (&gt;2kpc) from the center of the galaxy. In agreement with the recent study of Cohen, we find no detectable gradient of mean cluster color (metallicity) in (B-V) or (V-I) with radial distance. The cluster system does, however, display a large dispersion in color at any radius, corresponding to sigma([Fe/H])~0.6 about a mean metallicity (Fe/H]&gt;~-1.1 according to our color index scale. The difference in mean color between the globular clusters and the underlying halo light of the galaxy itself, found previously by Strom and coworkers and by Cohen, shows up strongly in all of our color indices; we find virtually no clusters as red as mean color of the halo stars at any radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/671#2</TD>
            <TD>2011-09-14T18:24:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/671</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/73/671&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/671</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/201 [1]</TD>
            <TD>Sternberg SN Catalogue, 1994Sep. (Tsvetkov+, 1995)</TD>
            <TD>We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/201#1</TD>
            <TD>2011-09-14T18:54:49Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/II/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/201</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/201</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/201 [2]</TD>
            <TD>Sternberg SN Catalogue, 1994Sep. (Tsvetkov+, 1995)</TD>
            <TD>We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/201#2</TD>
            <TD>2011-09-14T18:54:49Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/II/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/201&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/201 [catalog]</TD>
            <TD>Sternberg SN Catalogue, 1994Sep. (Tsvetkov+, 1995)</TD>
            <TD>We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/201#catalog</TD>
            <TD>2011-09-14T18:54:49Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/II/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/201</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/92/219 [1]</TD>
            <TD>Catalog of recent supernovae (van den Bergh 1994)</TD>
            <TD>A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219#1</TD>
            <TD>2011-09-14T18:24:14Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/92/219</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/92/219</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/92/219 [2]</TD>
            <TD>Catalog of recent supernovae (van den Bergh 1994)</TD>
            <TD>A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219#2</TD>
            <TD>2011-09-14T18:24:14Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/92/219&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/92/219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/92/219 [table1]</TD>
            <TD>Catalog of recent supernovae (van den Bergh 1994)</TD>
            <TD>A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219#table1</TD>
            <TD>2011-09-14T18:24:14Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/92/219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/92/219</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/201 [1]</TD>
            <TD>Sternberg SN Catalogue, 1994Sep. (Tsvetkov+, 1995)</TD>
            <TD>We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/201#1</TD>
            <TD>2011-09-14T18:54:49Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/II/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/201</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/201</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/201 [2]</TD>
            <TD>Sternberg SN Catalogue, 1994Sep. (Tsvetkov+, 1995)</TD>
            <TD>We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/201#2</TD>
            <TD>2011-09-14T18:54:49Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/II/201</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/201&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/201</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/201 [catalog]</TD>
            <TD>Sternberg SN Catalogue, 1994Sep. (Tsvetkov+, 1995)</TD>
            <TD>We present a revised version of "Sternberg Astronomical Institute Supernova Catalogue" which includes data on 930 extragalactic supernovae (SNe) discovered up to September 1, 1994 and the main data on their parent galaxies. The description of previous version was presented by Tsvetkov and Bartunov (1993). The main improvements are the following: 1. The RC3 catalogue (de Vaucouleurs et al., 1991) was used instead of the RC2 as main source of data for parent galaxies. 2. For recent supernovae we included some magnitudes at maximum light from Hamuy et al. (1993) and compared our data with those of van den Bergh (1993). We also corrected some velocities of galaxies according to Huchra et al. (1994). 3. Some galaxy identifications from the MCG ( M ) were replaced by the ones from the PGC and the UGC. The identifications were adopted with this order of preference: NGC (IC) - UGC (ESO) - MCG - PGC - others 4. Photographic magnitudes from the PGC ( marked '*' ) and from IAU circulars ( marked 'C' ) were used when no other data were available. 5. Some errors were found in the previous version, and many new identifications for the galaxies previously listed as "ANON" were adopted. 6. We included several precise astrometric positions of SNe from Porter (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/II/201#catalog</TD>
            <TD>2011-09-14T18:54:49Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/II/201</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/201&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/201</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/92/219 [1]</TD>
            <TD>Catalog of recent supernovae (van den Bergh 1994)</TD>
            <TD>A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219#1</TD>
            <TD>2011-09-14T18:24:14Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/92/219</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/92/219</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/92/219 [2]</TD>
            <TD>Catalog of recent supernovae (van den Bergh 1994)</TD>
            <TD>A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219#2</TD>
            <TD>2011-09-14T18:24:14Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/92/219&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/92/219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/92/219 [table1]</TD>
            <TD>Catalog of recent supernovae (van den Bergh 1994)</TD>
            <TD>A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219#table1</TD>
            <TD>2011-09-14T18:24:14Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/92/219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/92/219</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/507/655 [1]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#1</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/507/655</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/507/655 [2]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#2</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table17]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table17</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table5]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table5</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table19]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table19</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table12]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table12</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table18]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table18</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table20]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table20</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/92/219 [1]</TD>
            <TD>Catalog of recent supernovae (van den Bergh 1994)</TD>
            <TD>A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219#1</TD>
            <TD>2011-09-14T18:24:14Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/92/219</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/92/219</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/92/219 [2]</TD>
            <TD>Catalog of recent supernovae (van den Bergh 1994)</TD>
            <TD>A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219#2</TD>
            <TD>2011-09-14T18:24:14Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/92/219&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/92/219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/92/219 [table1]</TD>
            <TD>Catalog of recent supernovae (van den Bergh 1994)</TD>
            <TD>A listing is given of all supernovae discovered between 1989 January 1 and 1993 April 1. The data show no evidence for a significant dependence of the discovery probability of supernovae on parent galaxy inclination to the line of sight. If no inclination corrections need to be applied, then the supernova rates in spirals are only about half as large as previously believed. The mean linear separation of supernovae of type II (SNe II) from the center of their parent galaxy increases with increasing distance (Shaw effect). The Shaw effect appears less evident, or absent, for (more luminous) supernovae of type Ia. The data are consistent with, but do not prove, the hypothesis that (presumably reddened) SNe II are more likely to be discovered in the red than in the blue. Due to intensive surveillance, most bright SNe Ia tend to be found before maximum, whereas the majority of faint SNe Ia are discovered after maximum light.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219#table1</TD>
            <TD>2011-09-14T18:24:14Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/92/219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/92/219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/92/219</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/507/655 [1]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#1</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/507/655</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/507/655 [2]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#2</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table17]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table17</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table5]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table5</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table19]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table19</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table12]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table12</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table18]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table18</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table20]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table20</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/35/403 [1]</TD>
            <TD>Optical Variabilities in 3C 120 (Doroshenko+, 2009)</TD>
            <TD>Based on our UBVRI observations and X-ray data from the RXTE satellite we have investigated the variabilities of the Seyfert Galaxy 3C 120 over the period 1996-2008.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/403#1</TD>
            <TD>2011-09-14T20:53:32Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/35/403</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/403</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/35/403 [2]</TD>
            <TD>Optical Variabilities in 3C 120 (Doroshenko+, 2009)</TD>
            <TD>Based on our UBVRI observations and X-ray data from the RXTE satellite we have investigated the variabilities of the Seyfert Galaxy 3C 120 over the period 1996-2008.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/403#2</TD>
            <TD>2011-09-14T20:53:32Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/403</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/35/403&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/403</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/157/1 [1]</TD>
            <TD>Red-Sequence Cluster Survey (Gladders+, 2005)</TD>
            <TD>The Red-Sequence Cluster Survey (RCS) is a ~100{deg}^2^, two-filter imaging survey in the R_C_ and z' filters, designed primarily to locate and characterize galaxy clusters to redshifts as high as z=1.4. This paper provides a detailed description of the survey strategy and execution, including a thorough discussion of the photometric and astrometric calibration of the survey data. These catalogs, representing about 10% of the total survey and comprising a total of 429 candidate clusters and groups, contain a total of 67 cluster candidates at a photometric redshift of 0.9&lt;z&lt;1.4, down to the chosen significance threshold of 3.29{sigma}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1#1</TD>
            <TD>2011-09-14T19:44:25Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/157/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/157/1 [2]</TD>
            <TD>Red-Sequence Cluster Survey (Gladders+, 2005)</TD>
            <TD>The Red-Sequence Cluster Survey (RCS) is a ~100{deg}^2^, two-filter imaging survey in the R_C_ and z' filters, designed primarily to locate and characterize galaxy clusters to redshifts as high as z=1.4. This paper provides a detailed description of the survey strategy and execution, including a thorough discussion of the photometric and astrometric calibration of the survey data. These catalogs, representing about 10% of the total survey and comprising a total of 429 candidate clusters and groups, contain a total of 67 cluster candidates at a photometric redshift of 0.9&lt;z&lt;1.4, down to the chosen significance threshold of 3.29{sigma}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1#2</TD>
            <TD>2011-09-14T19:44:25Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/157/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/507/655 [1]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#1</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/507/655</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/507/655 [2]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#2</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table17]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table17</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table5]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table5</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table19]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table19</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table12]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table12</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table18]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table18</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/507/655 [table20]</TD>
            <TD>VI photometry of new Cepheids in NGC 2541 (Ferrarese+, 1998)</TD>
            <TD>We report the detection of Cepheids and a new distance to the spiral galaxy NGC 2541, based on data obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope (HST). A total of 25 exposures (divided into 13 epochs) were obtained using the F555W filter (transformed to Johnson V), and nine exposures were obtained (divided into five epochs) using the F814W filter (transformed to Cousins I). Photometric reduction of the data is performed using two independent packages, DoPHOT and DAOPHOT II/ALLFRAME, which give very good agreement in the measured magnitudes. A total of 34 bona fide Cepheids, with periods ranging from 12 to over 60 days, are identified based on both sets of photometry. By fitting V and I period-luminosity relations, apparent distance moduli are derived assuming a Large Magellanic Cloud distance modulus and mean color excess of {mu}_LMC_=18.50+/-0.10mag and E(B-V)=0.10mag, respectively. Adopting A(V)/E(V-I)=2.45, we obtain a true distance modulus to NGC 2541 of {mu}_0_=30.47+/-0.11 (random) +/-0.12 (systematic) mag (D=12.4+/-0.6 [random] +/-0.7 [systematic] Mpc), and a total (Galactic plus internal) mean color excess E(B-V)=0.08+/-0.05 (internal error) mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655#table20</TD>
            <TD>2011-09-14T18:55:26Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/507/655</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/507/655&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/507/655</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/668/643 [1]</TD>
            <TD>Multiply imaged gravitational lens systems (Limousin+, 2007)</TD>
            <TD>We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z=0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643#1</TD>
            <TD>2011-09-14T20:53:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/668/643</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/668/643</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/668/643 [2]</TD>
            <TD>Multiply imaged gravitational lens systems (Limousin+, 2007)</TD>
            <TD>We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z=0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643#2</TD>
            <TD>2011-09-14T20:53:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/668/643&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/668/643</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/668/643 [table1]</TD>
            <TD>Multiply imaged gravitational lens systems (Limousin+, 2007)</TD>
            <TD>We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z=0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643#table1</TD>
            <TD>2011-09-14T20:53:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/668/643&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/668/643</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/157/1 [1]</TD>
            <TD>Red-Sequence Cluster Survey (Gladders+, 2005)</TD>
            <TD>The Red-Sequence Cluster Survey (RCS) is a ~100{deg}^2^, two-filter imaging survey in the R_C_ and z' filters, designed primarily to locate and characterize galaxy clusters to redshifts as high as z=1.4. This paper provides a detailed description of the survey strategy and execution, including a thorough discussion of the photometric and astrometric calibration of the survey data. These catalogs, representing about 10% of the total survey and comprising a total of 429 candidate clusters and groups, contain a total of 67 cluster candidates at a photometric redshift of 0.9&lt;z&lt;1.4, down to the chosen significance threshold of 3.29{sigma}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1#1</TD>
            <TD>2011-09-14T19:44:25Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/157/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/157/1 [2]</TD>
            <TD>Red-Sequence Cluster Survey (Gladders+, 2005)</TD>
            <TD>The Red-Sequence Cluster Survey (RCS) is a ~100{deg}^2^, two-filter imaging survey in the R_C_ and z' filters, designed primarily to locate and characterize galaxy clusters to redshifts as high as z=1.4. This paper provides a detailed description of the survey strategy and execution, including a thorough discussion of the photometric and astrometric calibration of the survey data. These catalogs, representing about 10% of the total survey and comprising a total of 429 candidate clusters and groups, contain a total of 67 cluster candidates at a photometric redshift of 0.9&lt;z&lt;1.4, down to the chosen significance threshold of 3.29{sigma}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1#2</TD>
            <TD>2011-09-14T19:44:25Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/157/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/1856 [1]</TD>
            <TD>Dwarf Cepheids in Carina (Mateo+, 1998)</TD>
            <TD>We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, &amp; Lutz (1994, Cat. &lt;J/AJ/108/222&gt; and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856#1</TD>
            <TD>2011-09-14T18:55:35Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/1856</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1856</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/1856 [2]</TD>
            <TD>Dwarf Cepheids in Carina (Mateo+, 1998)</TD>
            <TD>We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, &amp; Lutz (1994, Cat. &lt;J/AJ/108/222&gt; and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856#2</TD>
            <TD>2011-09-14T18:55:35Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/1856&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/1856 [table2]</TD>
            <TD>Dwarf Cepheids in Carina (Mateo+, 1998)</TD>
            <TD>We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, &amp; Lutz (1994, Cat. &lt;J/AJ/108/222&gt; and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856#table2</TD>
            <TD>2011-09-14T18:55:35Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/1856&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1856</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/668/643 [1]</TD>
            <TD>Multiply imaged gravitational lens systems (Limousin+, 2007)</TD>
            <TD>We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z=0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643#1</TD>
            <TD>2011-09-14T20:53:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/668/643</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/668/643</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/668/643 [2]</TD>
            <TD>Multiply imaged gravitational lens systems (Limousin+, 2007)</TD>
            <TD>We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z=0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643#2</TD>
            <TD>2011-09-14T20:53:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/668/643&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/668/643</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/668/643 [table1]</TD>
            <TD>Multiply imaged gravitational lens systems (Limousin+, 2007)</TD>
            <TD>We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z=0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643#table1</TD>
            <TD>2011-09-14T20:53:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/668/643&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/668/643</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/157/1 [1]</TD>
            <TD>Red-Sequence Cluster Survey (Gladders+, 2005)</TD>
            <TD>The Red-Sequence Cluster Survey (RCS) is a ~100{deg}^2^, two-filter imaging survey in the R_C_ and z' filters, designed primarily to locate and characterize galaxy clusters to redshifts as high as z=1.4. This paper provides a detailed description of the survey strategy and execution, including a thorough discussion of the photometric and astrometric calibration of the survey data. These catalogs, representing about 10% of the total survey and comprising a total of 429 candidate clusters and groups, contain a total of 67 cluster candidates at a photometric redshift of 0.9&lt;z&lt;1.4, down to the chosen significance threshold of 3.29{sigma}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1#1</TD>
            <TD>2011-09-14T19:44:25Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/157/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/157/1 [2]</TD>
            <TD>Red-Sequence Cluster Survey (Gladders+, 2005)</TD>
            <TD>The Red-Sequence Cluster Survey (RCS) is a ~100{deg}^2^, two-filter imaging survey in the R_C_ and z' filters, designed primarily to locate and characterize galaxy clusters to redshifts as high as z=1.4. This paper provides a detailed description of the survey strategy and execution, including a thorough discussion of the photometric and astrometric calibration of the survey data. These catalogs, representing about 10% of the total survey and comprising a total of 429 candidate clusters and groups, contain a total of 67 cluster candidates at a photometric redshift of 0.9&lt;z&lt;1.4, down to the chosen significance threshold of 3.29{sigma}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1#2</TD>
            <TD>2011-09-14T19:44:25Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/157/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/157/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/157/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/1856 [1]</TD>
            <TD>Dwarf Cepheids in Carina (Mateo+, 1998)</TD>
            <TD>We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, &amp; Lutz (1994, Cat. &lt;J/AJ/108/222&gt; and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856#1</TD>
            <TD>2011-09-14T18:55:35Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/1856</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1856</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/1856 [2]</TD>
            <TD>Dwarf Cepheids in Carina (Mateo+, 1998)</TD>
            <TD>We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, &amp; Lutz (1994, Cat. &lt;J/AJ/108/222&gt; and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856#2</TD>
            <TD>2011-09-14T18:55:35Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/1856&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/1856 [table2]</TD>
            <TD>Dwarf Cepheids in Carina (Mateo+, 1998)</TD>
            <TD>We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, &amp; Lutz (1994, Cat. &lt;J/AJ/108/222&gt; and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856#table2</TD>
            <TD>2011-09-14T18:55:35Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/1856&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1856</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/668/643 [1]</TD>
            <TD>Multiply imaged gravitational lens systems (Limousin+, 2007)</TD>
            <TD>We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z=0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643#1</TD>
            <TD>2011-09-14T20:53:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/668/643</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/668/643</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/668/643 [2]</TD>
            <TD>Multiply imaged gravitational lens systems (Limousin+, 2007)</TD>
            <TD>We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z=0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643#2</TD>
            <TD>2011-09-14T20:53:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/668/643&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/668/643</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/668/643 [table1]</TD>
            <TD>Multiply imaged gravitational lens systems (Limousin+, 2007)</TD>
            <TD>We present a reconstruction of the mass distribution of galaxy cluster Abell 1689 at z=0.18 using detected strong lensing features from deep ACS observations and extensive ground based spectroscopy. Earlier analyses have reported up to 32 multiply imaged systems in this cluster, of which only 3 were spectroscopically confirmed. In this work, we present a parametric strong lensing mass reconstruction using 34 multiply imaged systems of which 24 have newly determined spectroscopic redshifts, which is a major step forward in building a robust mass model. In turn, the new spectroscopic data allows a more secure identification of multiply imaged systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643#table1</TD>
            <TD>2011-09-14T20:53:47Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Nov-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/668/643</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/668/643&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/668/643</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/3137 [1]</TD>
            <TD>Hawaii redshifts in the ACS-GOODS region (Cowie+, 2004)</TD>
            <TD>We report the results of an extensive spectroscopic survey of galaxies in the roughly 160 arcmin^2^ ACS-GOODS region surrounding the Hubble Deep Field North (HDF-N). We have identified 892 galaxies or stars with z&lt;24, R&lt;24.5, or B&lt;25 in the region. The spectra were obtained with either the DEIMOS or LRIS spectrographs on the Keck 10m telescopes. The results are compared with photometric redshift estimates and with redshifts from the literature, as well as with the redshifts of a parallel effort led by a group at Keck. Our sample, when combined with the literature data, provides identifications for 1324 sources. We use our results to determine the redshift distributions with magnitude, to analyze the rest-frame color distributions with redshift and spectral type, and to investigate the dependence of the X-ray galaxy properties on the local galaxy density in the redshift interval z=0-1.5. We find the rather surprising result that the galaxy X-ray properties are not strongly dependent on the local galaxy density for galaxies in the same luminosity range.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3137#1</TD>
            <TD>2011-09-14T19:44:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3137</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/3137</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3137</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/3137 [2]</TD>
            <TD>Hawaii redshifts in the ACS-GOODS region (Cowie+, 2004)</TD>
            <TD>We report the results of an extensive spectroscopic survey of galaxies in the roughly 160 arcmin^2^ ACS-GOODS region surrounding the Hubble Deep Field North (HDF-N). We have identified 892 galaxies or stars with z&lt;24, R&lt;24.5, or B&lt;25 in the region. The spectra were obtained with either the DEIMOS or LRIS spectrographs on the Keck 10m telescopes. The results are compared with photometric redshift estimates and with redshifts from the literature, as well as with the redshifts of a parallel effort led by a group at Keck. Our sample, when combined with the literature data, provides identifications for 1324 sources. We use our results to determine the redshift distributions with magnitude, to analyze the rest-frame color distributions with redshift and spectral type, and to investigate the dependence of the X-ray galaxy properties on the local galaxy density in the redshift interval z=0-1.5. We find the rather surprising result that the galaxy X-ray properties are not strongly dependent on the local galaxy density for galaxies in the same luminosity range.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3137#2</TD>
            <TD>2011-09-14T19:44:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3137</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/3137&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3137</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/1856 [1]</TD>
            <TD>Dwarf Cepheids in Carina (Mateo+, 1998)</TD>
            <TD>We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, &amp; Lutz (1994, Cat. &lt;J/AJ/108/222&gt; and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856#1</TD>
            <TD>2011-09-14T18:55:35Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/1856</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1856</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/1856 [2]</TD>
            <TD>Dwarf Cepheids in Carina (Mateo+, 1998)</TD>
            <TD>We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, &amp; Lutz (1994, Cat. &lt;J/AJ/108/222&gt; and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856#2</TD>
            <TD>2011-09-14T18:55:35Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/1856&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1856</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/1856 [table2]</TD>
            <TD>Dwarf Cepheids in Carina (Mateo+, 1998)</TD>
            <TD>We have discovered 20 dwarf Cepheids (DCs) in the Carina dwarf spheroidal galaxy from an analysis of individual CCD images obtained for a deep photometric study of the system. These short-period pulsating variable stars are by far the most distant (~100kpc) and faintest (V~23.0) DCs known. The Carina DCs obey a well-defined period-luminosity relation, allowing us to readily distinguish between overtone and fundamental pulsators in nearly every case. Unlike RR Lyrae stars, the pulsation mode turns out to be uncorrelated with light-curve shape, and the overtone pulsators do not tend toward shorter periods compared with the fundamental pulsators. Using the period-luminosity relations from Nemec, Nemec, &amp; Lutz (1994, Cat. &lt;J/AJ/108/222&gt; and McNamara (1995AJ....109.1751M), we derive (m-M)_0_=20.06+/-0.12, for E(B-V)=0.025 and [Fe/H]=-2.0, in good agreement with recent, independent estimates of the distance/reddening of Carina. The error reflects the uncertainties in the DC distance scale, and in the metallicity and reddening of Carina. The frequency of DCs among upper-main-sequence stars in Carina is approximately 3%. The ratio of dwarf Cepheids to RR Lyrae stars in Carina is 0.13+/-0.10, though this result is highly sensitive to the star formation history of Carina and the evolution of the horizontal branch.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856#table2</TD>
            <TD>2011-09-14T18:55:35Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1856</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/1856&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1856</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/184/271 [1]</TD>
            <TD>Photometry of galaxies in 3 clusters (Chiboucas+, 2009)</TD>
            <TD>We have acquired ground-based imaging for the clusters in our sample using GMOS on the Gemini-North 8m telescope. For each of our clusters we have obtained new ACS imaging or used archival HST data to study the galaxy structural parameters with high-resolution data having FWHM=0.1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271#1</TD>
            <TD>2011-09-14T20:56:46Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/184/271</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/184/271</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/184/271 [2]</TD>
            <TD>Photometry of galaxies in 3 clusters (Chiboucas+, 2009)</TD>
            <TD>We have acquired ground-based imaging for the clusters in our sample using GMOS on the Gemini-North 8m telescope. For each of our clusters we have obtained new ACS imaging or used archival HST data to study the galaxy structural parameters with high-resolution data having FWHM=0.1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271#2</TD>
            <TD>2011-09-14T20:56:46Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/184/271&amp;</TD>
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            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/184/271</TD>
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            <TD>J/ApJS/184/271 [galaxies]</TD>
            <TD>Photometry of galaxies in 3 clusters (Chiboucas+, 2009)</TD>
            <TD>We have acquired ground-based imaging for the clusters in our sample using GMOS on the Gemini-North 8m telescope. For each of our clusters we have obtained new ACS imaging or used archival HST data to study the galaxy structural parameters with high-resolution data having FWHM=0.1".</TD>
            <TD>CDS</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/127/3137 [1]</TD>
            <TD>Hawaii redshifts in the ACS-GOODS region (Cowie+, 2004)</TD>
            <TD>We report the results of an extensive spectroscopic survey of galaxies in the roughly 160 arcmin^2^ ACS-GOODS region surrounding the Hubble Deep Field North (HDF-N). We have identified 892 galaxies or stars with z&lt;24, R&lt;24.5, or B&lt;25 in the region. The spectra were obtained with either the DEIMOS or LRIS spectrographs on the Keck 10m telescopes. The results are compared with photometric redshift estimates and with redshifts from the literature, as well as with the redshifts of a parallel effort led by a group at Keck. Our sample, when combined with the literature data, provides identifications for 1324 sources. We use our results to determine the redshift distributions with magnitude, to analyze the rest-frame color distributions with redshift and spectral type, and to investigate the dependence of the X-ray galaxy properties on the local galaxy density in the redshift interval z=0-1.5. We find the rather surprising result that the galaxy X-ray properties are not strongly dependent on the local galaxy density for galaxies in the same luminosity range.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
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            <TD>03-Dec-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3137</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/3137</TD>
            <TD />
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3137</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/3137 [2]</TD>
            <TD>Hawaii redshifts in the ACS-GOODS region (Cowie+, 2004)</TD>
            <TD>We report the results of an extensive spectroscopic survey of galaxies in the roughly 160 arcmin^2^ ACS-GOODS region surrounding the Hubble Deep Field North (HDF-N). We have identified 892 galaxies or stars with z&lt;24, R&lt;24.5, or B&lt;25 in the region. The spectra were obtained with either the DEIMOS or LRIS spectrographs on the Keck 10m telescopes. The results are compared with photometric redshift estimates and with redshifts from the literature, as well as with the redshifts of a parallel effort led by a group at Keck. Our sample, when combined with the literature data, provides identifications for 1324 sources. We use our results to determine the redshift distributions with magnitude, to analyze the rest-frame color distributions with redshift and spectral type, and to investigate the dependence of the X-ray galaxy properties on the local galaxy density in the redshift interval z=0-1.5. We find the rather surprising result that the galaxy X-ray properties are not strongly dependent on the local galaxy density for galaxies in the same luminosity range.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3137#2</TD>
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            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/3137&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3137</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/193 [1]</TD>
            <TD>RR Lyrae V light curves (Layden, 1998)</TD>
            <TD>I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD />
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            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/193</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/193</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/193 [2]</TD>
            <TD>RR Lyrae V light curves (Layden, 1998)</TD>
            <TD>I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T18:56:30Z</TD>
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            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/193&amp;</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/193 [table3]</TD>
            <TD>RR Lyrae V light curves (Layden, 1998)</TD>
            <TD>I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193#table3</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/193&amp;</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/193</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/184/271 [1]</TD>
            <TD>Photometry of galaxies in 3 clusters (Chiboucas+, 2009)</TD>
            <TD>We have acquired ground-based imaging for the clusters in our sample using GMOS on the Gemini-North 8m telescope. For each of our clusters we have obtained new ACS imaging or used archival HST data to study the galaxy structural parameters with high-resolution data having FWHM=0.1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>26-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/184/271</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/184/271</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJS/184/271 [2]</TD>
            <TD>Photometry of galaxies in 3 clusters (Chiboucas+, 2009)</TD>
            <TD>We have acquired ground-based imaging for the clusters in our sample using GMOS on the Gemini-North 8m telescope. For each of our clusters we have obtained new ACS imaging or used archival HST data to study the galaxy structural parameters with high-resolution data having FWHM=0.1".</TD>
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            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/184/271&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/184/271</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/184/271 [galaxies]</TD>
            <TD>Photometry of galaxies in 3 clusters (Chiboucas+, 2009)</TD>
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            <TD>#Optical#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/184/271&amp;</TD>
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            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/184/271</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/193 [1]</TD>
            <TD>RR Lyrae V light curves (Layden, 1998)</TD>
            <TD>I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193#1</TD>
            <TD>2011-09-14T18:56:30Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
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            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/193 [2]</TD>
            <TD>RR Lyrae V light curves (Layden, 1998)</TD>
            <TD>I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193#2</TD>
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            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/193&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/193</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/193 [table3]</TD>
            <TD>RR Lyrae V light curves (Layden, 1998)</TD>
            <TD>I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/193</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/3137 [1]</TD>
            <TD>Hawaii redshifts in the ACS-GOODS region (Cowie+, 2004)</TD>
            <TD>We report the results of an extensive spectroscopic survey of galaxies in the roughly 160 arcmin^2^ ACS-GOODS region surrounding the Hubble Deep Field North (HDF-N). We have identified 892 galaxies or stars with z&lt;24, R&lt;24.5, or B&lt;25 in the region. The spectra were obtained with either the DEIMOS or LRIS spectrographs on the Keck 10m telescopes. The results are compared with photometric redshift estimates and with redshifts from the literature, as well as with the redshifts of a parallel effort led by a group at Keck. Our sample, when combined with the literature data, provides identifications for 1324 sources. We use our results to determine the redshift distributions with magnitude, to analyze the rest-frame color distributions with redshift and spectral type, and to investigate the dependence of the X-ray galaxy properties on the local galaxy density in the redshift interval z=0-1.5. We find the rather surprising result that the galaxy X-ray properties are not strongly dependent on the local galaxy density for galaxies in the same luminosity range.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3137#1</TD>
            <TD>2011-09-14T19:44:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3137</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/3137</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3137</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/3137 [2]</TD>
            <TD>Hawaii redshifts in the ACS-GOODS region (Cowie+, 2004)</TD>
            <TD>We report the results of an extensive spectroscopic survey of galaxies in the roughly 160 arcmin^2^ ACS-GOODS region surrounding the Hubble Deep Field North (HDF-N). We have identified 892 galaxies or stars with z&lt;24, R&lt;24.5, or B&lt;25 in the region. The spectra were obtained with either the DEIMOS or LRIS spectrographs on the Keck 10m telescopes. The results are compared with photometric redshift estimates and with redshifts from the literature, as well as with the redshifts of a parallel effort led by a group at Keck. Our sample, when combined with the literature data, provides identifications for 1324 sources. We use our results to determine the redshift distributions with magnitude, to analyze the rest-frame color distributions with redshift and spectral type, and to investigate the dependence of the X-ray galaxy properties on the local galaxy density in the redshift interval z=0-1.5. We find the rather surprising result that the galaxy X-ray properties are not strongly dependent on the local galaxy density for galaxies in the same luminosity range.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/3137#2</TD>
            <TD>2011-09-14T19:44:36Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/127/3137</TD>
            <TD />
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/3137&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/3137</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/193 [1]</TD>
            <TD>RR Lyrae V light curves (Layden, 1998)</TD>
            <TD>I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193#1</TD>
            <TD>2011-09-14T18:56:30Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/193</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/193</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/193 [2]</TD>
            <TD>RR Lyrae V light curves (Layden, 1998)</TD>
            <TD>I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193#2</TD>
            <TD>2011-09-14T18:56:30Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/193&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/193</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/193 [table3]</TD>
            <TD>RR Lyrae V light curves (Layden, 1998)</TD>
            <TD>I present V-band CCD photometry for a sample of 103 RR Lyrae variables selected from the General Catalogue of Variable Stars to lie in the inner halo of the Galaxy. I also describe a method for obtaining the mean apparent magnitude and the epoch at maximum light of an RR Lyrae star. The method requires as few as five photometric observations, and simulations demonstrate that the associated errors are relatively small. I employ this method to derive the mean magnitudes and maximum light epochs of the 103 RR Lyrae stars observed. These stars were selected, based on their Galactic coordinates and original photographic photometry, to lie near their orbital tangent points, thus providing a sample well suited for measuring the rotational kinematics of the inner halo. Using interstellar reddenings from the literature and the observed mean V magnitudes, I derive distances for these stars and show that their actual locations in the Galaxy are indeed suitable for use in a kinematic study, despite the large zero-point errors in the survey photographic photometry.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193#table3</TD>
            <TD>2011-09-14T18:56:30Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/193</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/193&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/193</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/184/271 [1]</TD>
            <TD>Photometry of galaxies in 3 clusters (Chiboucas+, 2009)</TD>
            <TD>We have acquired ground-based imaging for the clusters in our sample using GMOS on the Gemini-North 8m telescope. For each of our clusters we have obtained new ACS imaging or used archival HST data to study the galaxy structural parameters with high-resolution data having FWHM=0.1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271#1</TD>
            <TD>2011-09-14T20:56:46Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/184/271</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/184/271</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/184/271 [2]</TD>
            <TD>Photometry of galaxies in 3 clusters (Chiboucas+, 2009)</TD>
            <TD>We have acquired ground-based imaging for the clusters in our sample using GMOS on the Gemini-North 8m telescope. For each of our clusters we have obtained new ACS imaging or used archival HST data to study the galaxy structural parameters with high-resolution data having FWHM=0.1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271#2</TD>
            <TD>2011-09-14T20:56:46Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/184/271&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/184/271</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/184/271 [galaxies]</TD>
            <TD>Photometry of galaxies in 3 clusters (Chiboucas+, 2009)</TD>
            <TD>We have acquired ground-based imaging for the clusters in our sample using GMOS on the Gemini-North 8m telescope. For each of our clusters we have obtained new ACS imaging or used archival HST data to study the galaxy structural parameters with high-resolution data having FWHM=0.1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271#galaxies</TD>
            <TD>2011-09-14T20:56:46Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/184/271</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/184/271&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/184/271</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/538 [1]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538#1</TD>
            <TD>2011-09-14T19:45:04Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/538</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/538</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/538 [2]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538#2</TD>
            <TD>2011-09-14T19:45:04Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/538&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/538</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/538 [table1]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538#table1</TD>
            <TD>2011-09-14T19:45:04Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/538&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/538</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/538 [ubv]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538#ubv</TD>
            <TD>2011-09-14T19:45:04Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/538&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/538</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/2587 [1]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/2587#1</TD>
            <TD>2011-09-14T18:57:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/2587</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/2587</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/2587</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/2587 [2]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/2587#2</TD>
            <TD>2011-09-14T18:57:07Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/2587</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/2587&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/2587</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/2587 [table2]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/115/2587 [table1]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJS/186/427 [1]</TD>
            <TD>Detailed morphology of SDSS galaxies (Nair+, 2010)</TD>
            <TD>We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. &lt;II/267&gt;). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01&lt;z&lt;0.1 down to an apparent extinction-corrected limit of g&lt;16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.</TD>
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            <TD>J/ApJS/186/427 [2]</TD>
            <TD>Detailed morphology of SDSS galaxies (Nair+, 2010)</TD>
            <TD>We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. &lt;II/267&gt;). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01&lt;z&lt;0.1 down to an apparent extinction-corrected limit of g&lt;16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.</TD>
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            <TD>Detailed morphology of SDSS galaxies (Nair+, 2010)</TD>
            <TD>We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. &lt;II/267&gt;). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01&lt;z&lt;0.1 down to an apparent extinction-corrected limit of g&lt;16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/115/2587 [1]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/2587#1</TD>
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            <TD>WebBrowser</TD>
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            <TD>HTTP Request</TD>
            <TD>J/AJ/115/2587 [2]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/2587#2</TD>
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            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>Web Page</TD>
            <TD>J/AJ/108/538 [1]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/538 [2]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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          <TR>
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            <TD>J/AJ/108/538 [table1]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/108/538 [ubv]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
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            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/538</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/2587 [1]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
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            <TD>31-Aug-1998</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/2587</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/2587</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/2587 [2]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
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            <TD>2011-09-14T18:57:07Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD />
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/2587&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/2587</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/2587 [table2]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/2587#table2</TD>
            <TD>2011-09-14T18:57:07Z</TD>
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            <TD>31-Aug-1998</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/2587&amp;</TD>
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            <TD>9999</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/115/2587 [table1]</TD>
            <TD>Einstein IPC database ultrasoft survey (Thompson+ 1998)</TD>
            <TD>We have carried out a survey of the entire Einstein IPC database (a total of 5934 sources) to select objects with strong components of ultrasoft X-ray emission (i.e., emission below 0.5keV). The selection criteria are based on ratios of counts within three broad energy bands (i.e., X-ray "colors"). A total of 516 objects have been selected, with 202 (39%) having been identified through correlations with other databases. Of the currently identified objects, 45% are active galactic nuclei, 28% are stellar objects, 6% are "normal" galaxies and galaxy clusters, and the remaining 21% are "nonstellar" Galactic objects such as cataclysmic variables, pulsars, and white dwarfs. We present a discussion of the survey selection procedure, the list of selected sources, and discussions of interesting objects from the aforementioned groups. We discuss the remarkable success of our rather "low resolution" method of estimating spectral shape and present plans for follow-up studies of the as yet unidentified sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/2587#table1</TD>
            <TD>2011-09-14T18:57:07Z</TD>
            <TD>##</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-1998</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/2587&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/2587</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/186/427 [1]</TD>
            <TD>Detailed morphology of SDSS galaxies (Nair+, 2010)</TD>
            <TD>We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. &lt;II/267&gt;). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01&lt;z&lt;0.1 down to an apparent extinction-corrected limit of g&lt;16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/ApJS/186/427#1</TD>
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            <TD />
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            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/186/427</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/186/427</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJS/186/427 [2]</TD>
            <TD>Detailed morphology of SDSS galaxies (Nair+, 2010)</TD>
            <TD>We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. &lt;II/267&gt;). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01&lt;z&lt;0.1 down to an apparent extinction-corrected limit of g&lt;16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/186/427#2</TD>
            <TD>2011-09-14T20:57:33Z</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJS/186/427 [table2]</TD>
            <TD>Detailed morphology of SDSS galaxies (Nair+, 2010)</TD>
            <TD>We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. &lt;II/267&gt;). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01&lt;z&lt;0.1 down to an apparent extinction-corrected limit of g&lt;16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.</TD>
            <TD>CDS</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>J/AJ/108/538 [1]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538#1</TD>
            <TD>2011-09-14T19:45:04Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>21-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/538</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/538</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/538 [2]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538#2</TD>
            <TD>2011-09-14T19:45:04Z</TD>
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            <TD>#Catalog#</TD>
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            <TD>21-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/538&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/538</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/538 [table1]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538#table1</TD>
            <TD>2011-09-14T19:45:04Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>21-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/538&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/538 [ubv]</TD>
            <TD>Metal-poor MS stars UBV photometry (Preston+ 1994)</TD>
            <TD>From analysis of a photometrically selected sample of 175 metal-poor field stars with main sequence gravities (hereafter BMPs) and UBV colors blueward of the most metal-poor globular cluster main-sequence turnoffs, 0.15&lt;(B-V)_0_&lt;0.35, and properties of the candidate lists of the HK objective prism survey, we calculate the space density and a suitably defined specific frequency of BMPs within ~2kpc of the Sun. We consider two cases. If we adopt the luminosities and color distribution of globular cluster blue stragglers (hereafter BS) for BMPs, the BMP space density, is ~350kpc^-3^, from which we obtain a specific frequency S(BMP)~8, a value 9 times larger than that of BSs in globular clusters. From this result, we conclude that cluster-type BSs are but a minor component of the field BMPs and that the remainder must be of a different nature. If we adopt luminosities of metal-poor models halfway between the Zero Age Main Sequence and the phase of core hydrogen exhaustion, we obtain a space density of 450(+300,-150)kpc^-3^ and a specific frequency S(BMP)=10(+5,-3). From a subsample of 107 BMPs with available radial velocities we derive a galactic rotation of 128km/s and an isotropic velocity dispersion of {sigma}~90km/s, values intermediate between those of halo and thick-disk populations. From analysis of a larger sample of stars on 0.15&lt;(B-V)0&lt;0.35 binned by a crude line-blanketing parameter, we find that our results are insensitive to adopted BMP selection criteria: none of these subsamples of A- and early F-type stars above the galactic plane possess disk kinematics. The region of the UBV two-color diagram occupied by BMPs could be populated by metal-deficient, main-sequence gravity stars with ages substantially younger than those of the metal-poor halo. Because we cannot imagine how or where the observed local population of BMPs could have been produced within our galaxy during the past 3 to 10Gyr, we suggest that BMPs are the bluest members of metal-poor intermediate-age main sequences accreted, probably, from dwarf spheroidal satellites of the Milky Way during the past 10Gyr. We discuss observational consequences of this suggestion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538#ubv</TD>
            <TD>2011-09-14T19:45:04Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Mar-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/538</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/538&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/538</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/140/55 [1]</TD>
            <TD>Pulsation of galactic long-period variables (Barthes+, 1999)</TD>
            <TD>The absolute K magnitudes and kinematic parameters of about 350 oxygen-rich Long-Period Variable stars are calibrated, by means of an up-to-date maximum-likelihood method, using Hipparcos parallaxes and proper motions together with radial velocities and, as additional data, periods and V-K colour indices. Four groups, differing by their kinematics and mean magnitudes, are found. For each of them, we also obtain the distributions of magnitude, period and de-reddened colour of the base population, as well as de-biased period-luminosity-colour relations and their two-dimensional projections. The SRa semiregulars do not seem to constitute a separate class of LPVs. The SRb appear to belong to two populations of different ages. In a PL diagram, they constitute two evolutionary sequences towards the Mira stage. The Miras of the disk appear to pulsate on a lower-order mode. The slopes of their de-biased PL and PC relations are found to be very different from the ones of the Oxygen Miras of the LMC. This suggests that a significant number of so-called Miras of the LMC are misclassified. This also suggests that the Miras of the LMC do not constitute a homogeneous group, but include a significant proportion of metal-deficient stars, suggesting a relatively smooth star formation history. As a consequence, one may not trivially transpose the LMC period-luminosity relation from one galaxy to the other.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/55#1</TD>
            <TD>2011-09-14T18:57:24Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/55</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/140/55</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/55</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/140/55 [2]</TD>
            <TD>Pulsation of galactic long-period variables (Barthes+, 1999)</TD>
            <TD>The absolute K magnitudes and kinematic parameters of about 350 oxygen-rich Long-Period Variable stars are calibrated, by means of an up-to-date maximum-likelihood method, using Hipparcos parallaxes and proper motions together with radial velocities and, as additional data, periods and V-K colour indices. Four groups, differing by their kinematics and mean magnitudes, are found. For each of them, we also obtain the distributions of magnitude, period and de-reddened colour of the base population, as well as de-biased period-luminosity-colour relations and their two-dimensional projections. The SRa semiregulars do not seem to constitute a separate class of LPVs. The SRb appear to belong to two populations of different ages. In a PL diagram, they constitute two evolutionary sequences towards the Mira stage. The Miras of the disk appear to pulsate on a lower-order mode. The slopes of their de-biased PL and PC relations are found to be very different from the ones of the Oxygen Miras of the LMC. This suggests that a significant number of so-called Miras of the LMC are misclassified. This also suggests that the Miras of the LMC do not constitute a homogeneous group, but include a significant proportion of metal-deficient stars, suggesting a relatively smooth star formation history. As a consequence, one may not trivially transpose the LMC period-luminosity relation from one galaxy to the other.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/55#2</TD>
            <TD>2011-09-14T18:57:24Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/55</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/140/55&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/55</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/186/427 [1]</TD>
            <TD>Detailed morphology of SDSS galaxies (Nair+, 2010)</TD>
            <TD>We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. &lt;II/267&gt;). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01&lt;z&lt;0.1 down to an apparent extinction-corrected limit of g&lt;16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/186/427#1</TD>
            <TD>2011-09-14T20:57:33Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/186/427</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/186/427</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/186/427</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/186/427 [2]</TD>
            <TD>Detailed morphology of SDSS galaxies (Nair+, 2010)</TD>
            <TD>We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. &lt;II/267&gt;). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01&lt;z&lt;0.1 down to an apparent extinction-corrected limit of g&lt;16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/186/427#2</TD>
            <TD>2011-09-14T20:57:33Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/186/427</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/186/427&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/186/427</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/186/427 [table2]</TD>
            <TD>Detailed morphology of SDSS galaxies (Nair+, 2010)</TD>
            <TD>We present a catalog of detailed visual classifications for 14034 galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 4 (DR4, Cat. &lt;II/267&gt;). Our sample includes nearly all spectroscopically targeted galaxies in the redshift range 0.01&lt;z&lt;0.1 down to an apparent extinction-corrected limit of g&lt;16mag. In addition to T-Types, we record the existence of bars, rings, lenses, tails, warps, dust lanes, arm flocculence, and multiplicity. This sample defines a comprehensive local galaxy sample which we will use in future papers to study low-redshift morphology. It will also prove useful for calibrating automated galaxy classification algorithms. In this paper, we describe the classification methodology used, detail the systematics and biases of our sample, and summarize the overall statistical properties of the sample, noting the most obvious trends that are relevant for general comparisons of our catalog with previously published work.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/186/427#table2</TD>
            <TD>2011-09-14T20:57:33Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/186/427</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/186/427&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/186/427</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/899 [1]</TD>
            <TD>Blue HB stars in SDSS (Sirko+, 2004)</TD>
            <TD>We isolate samples of 733 bright (g&lt;18) and 437 faint (g&gt;18) high Galactic latitude blue horizontal-branch stars with photometry and spectroscopy in the Sloan Digital Sky Survey (SDSS). Comparison of independent photometric and spectroscopic selection criteria indicates that contamination from F and blue straggler stars is less than 10% for bright stars (g&lt;18) and about 25% for faint stars (g&gt;18), and this is qualitatively confirmed by proper motions based on the USNO-A (&lt;I/252&gt;) catalog as first epoch. Analysis of repeated observations shows that the errors in radial velocity are ~26km/s. A relation between absolute magnitude and color is established using the horizontal branches of halo globular clusters observed by SDSS. Bolometric corrections and colors are synthesized in the SDSS filters from model spectra. The redder stars agree well in absolute magnitude with accepted values for RR Lyrae stars. The resulting photometric distances are accurate to about 0.2mag, with a median of about 25kpc. Modest clumps in phase space exist and are consistent with the previously reported tidal stream of the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899#1</TD>
            <TD>2011-09-14T19:45:13Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/899</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/899</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/899 [2]</TD>
            <TD>Blue HB stars in SDSS (Sirko+, 2004)</TD>
            <TD>We isolate samples of 733 bright (g&lt;18) and 437 faint (g&gt;18) high Galactic latitude blue horizontal-branch stars with photometry and spectroscopy in the Sloan Digital Sky Survey (SDSS). Comparison of independent photometric and spectroscopic selection criteria indicates that contamination from F and blue straggler stars is less than 10% for bright stars (g&lt;18) and about 25% for faint stars (g&gt;18), and this is qualitatively confirmed by proper motions based on the USNO-A (&lt;I/252&gt;) catalog as first epoch. Analysis of repeated observations shows that the errors in radial velocity are ~26km/s. A relation between absolute magnitude and color is established using the horizontal branches of halo globular clusters observed by SDSS. Bolometric corrections and colors are synthesized in the SDSS filters from model spectra. The redder stars agree well in absolute magnitude with accepted values for RR Lyrae stars. The resulting photometric distances are accurate to about 0.2mag, with a median of about 25kpc. Modest clumps in phase space exist and are consistent with the previously reported tidal stream of the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899#2</TD>
            <TD>2011-09-14T19:45:13Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/899&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/899</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/400/1962 [1]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#1</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/400/1962</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/400/1962 [2]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#2</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/400/1962 [table2]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#table2</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/400/1962 [tableb]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#tableb</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/400/1962 [tablea]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#tablea</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/899 [1]</TD>
            <TD>Blue HB stars in SDSS (Sirko+, 2004)</TD>
            <TD>We isolate samples of 733 bright (g&lt;18) and 437 faint (g&gt;18) high Galactic latitude blue horizontal-branch stars with photometry and spectroscopy in the Sloan Digital Sky Survey (SDSS). Comparison of independent photometric and spectroscopic selection criteria indicates that contamination from F and blue straggler stars is less than 10% for bright stars (g&lt;18) and about 25% for faint stars (g&gt;18), and this is qualitatively confirmed by proper motions based on the USNO-A (&lt;I/252&gt;) catalog as first epoch. Analysis of repeated observations shows that the errors in radial velocity are ~26km/s. A relation between absolute magnitude and color is established using the horizontal branches of halo globular clusters observed by SDSS. Bolometric corrections and colors are synthesized in the SDSS filters from model spectra. The redder stars agree well in absolute magnitude with accepted values for RR Lyrae stars. The resulting photometric distances are accurate to about 0.2mag, with a median of about 25kpc. Modest clumps in phase space exist and are consistent with the previously reported tidal stream of the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899#1</TD>
            <TD>2011-09-14T19:45:13Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/899</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/899</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/899 [2]</TD>
            <TD>Blue HB stars in SDSS (Sirko+, 2004)</TD>
            <TD>We isolate samples of 733 bright (g&lt;18) and 437 faint (g&gt;18) high Galactic latitude blue horizontal-branch stars with photometry and spectroscopy in the Sloan Digital Sky Survey (SDSS). Comparison of independent photometric and spectroscopic selection criteria indicates that contamination from F and blue straggler stars is less than 10% for bright stars (g&lt;18) and about 25% for faint stars (g&gt;18), and this is qualitatively confirmed by proper motions based on the USNO-A (&lt;I/252&gt;) catalog as first epoch. Analysis of repeated observations shows that the errors in radial velocity are ~26km/s. A relation between absolute magnitude and color is established using the horizontal branches of halo globular clusters observed by SDSS. Bolometric corrections and colors are synthesized in the SDSS filters from model spectra. The redder stars agree well in absolute magnitude with accepted values for RR Lyrae stars. The resulting photometric distances are accurate to about 0.2mag, with a median of about 25kpc. Modest clumps in phase space exist and are consistent with the previously reported tidal stream of the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899#2</TD>
            <TD>2011-09-14T19:45:13Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/899&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/899</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/140/55 [1]</TD>
            <TD>Pulsation of galactic long-period variables (Barthes+, 1999)</TD>
            <TD>The absolute K magnitudes and kinematic parameters of about 350 oxygen-rich Long-Period Variable stars are calibrated, by means of an up-to-date maximum-likelihood method, using Hipparcos parallaxes and proper motions together with radial velocities and, as additional data, periods and V-K colour indices. Four groups, differing by their kinematics and mean magnitudes, are found. For each of them, we also obtain the distributions of magnitude, period and de-reddened colour of the base population, as well as de-biased period-luminosity-colour relations and their two-dimensional projections. The SRa semiregulars do not seem to constitute a separate class of LPVs. The SRb appear to belong to two populations of different ages. In a PL diagram, they constitute two evolutionary sequences towards the Mira stage. The Miras of the disk appear to pulsate on a lower-order mode. The slopes of their de-biased PL and PC relations are found to be very different from the ones of the Oxygen Miras of the LMC. This suggests that a significant number of so-called Miras of the LMC are misclassified. This also suggests that the Miras of the LMC do not constitute a homogeneous group, but include a significant proportion of metal-deficient stars, suggesting a relatively smooth star formation history. As a consequence, one may not trivially transpose the LMC period-luminosity relation from one galaxy to the other.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/55#1</TD>
            <TD>2011-09-14T18:57:24Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/55</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/140/55</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/55</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/140/55 [2]</TD>
            <TD>Pulsation of galactic long-period variables (Barthes+, 1999)</TD>
            <TD>The absolute K magnitudes and kinematic parameters of about 350 oxygen-rich Long-Period Variable stars are calibrated, by means of an up-to-date maximum-likelihood method, using Hipparcos parallaxes and proper motions together with radial velocities and, as additional data, periods and V-K colour indices. Four groups, differing by their kinematics and mean magnitudes, are found. For each of them, we also obtain the distributions of magnitude, period and de-reddened colour of the base population, as well as de-biased period-luminosity-colour relations and their two-dimensional projections. The SRa semiregulars do not seem to constitute a separate class of LPVs. The SRb appear to belong to two populations of different ages. In a PL diagram, they constitute two evolutionary sequences towards the Mira stage. The Miras of the disk appear to pulsate on a lower-order mode. The slopes of their de-biased PL and PC relations are found to be very different from the ones of the Oxygen Miras of the LMC. This suggests that a significant number of so-called Miras of the LMC are misclassified. This also suggests that the Miras of the LMC do not constitute a homogeneous group, but include a significant proportion of metal-deficient stars, suggesting a relatively smooth star formation history. As a consequence, one may not trivially transpose the LMC period-luminosity relation from one galaxy to the other.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/55#2</TD>
            <TD>2011-09-14T18:57:24Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/55</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/140/55&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/55</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/400/1962 [1]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#1</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/400/1962</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/400/1962 [2]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#2</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/400/1962 [table2]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#table2</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/400/1962 [tableb]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#tableb</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/400/1962 [tablea]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#tablea</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/899 [1]</TD>
            <TD>Blue HB stars in SDSS (Sirko+, 2004)</TD>
            <TD>We isolate samples of 733 bright (g&lt;18) and 437 faint (g&gt;18) high Galactic latitude blue horizontal-branch stars with photometry and spectroscopy in the Sloan Digital Sky Survey (SDSS). Comparison of independent photometric and spectroscopic selection criteria indicates that contamination from F and blue straggler stars is less than 10% for bright stars (g&lt;18) and about 25% for faint stars (g&gt;18), and this is qualitatively confirmed by proper motions based on the USNO-A (&lt;I/252&gt;) catalog as first epoch. Analysis of repeated observations shows that the errors in radial velocity are ~26km/s. A relation between absolute magnitude and color is established using the horizontal branches of halo globular clusters observed by SDSS. Bolometric corrections and colors are synthesized in the SDSS filters from model spectra. The redder stars agree well in absolute magnitude with accepted values for RR Lyrae stars. The resulting photometric distances are accurate to about 0.2mag, with a median of about 25kpc. Modest clumps in phase space exist and are consistent with the previously reported tidal stream of the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899#1</TD>
            <TD>2011-09-14T19:45:13Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/899</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/899</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/899 [2]</TD>
            <TD>Blue HB stars in SDSS (Sirko+, 2004)</TD>
            <TD>We isolate samples of 733 bright (g&lt;18) and 437 faint (g&gt;18) high Galactic latitude blue horizontal-branch stars with photometry and spectroscopy in the Sloan Digital Sky Survey (SDSS). Comparison of independent photometric and spectroscopic selection criteria indicates that contamination from F and blue straggler stars is less than 10% for bright stars (g&lt;18) and about 25% for faint stars (g&gt;18), and this is qualitatively confirmed by proper motions based on the USNO-A (&lt;I/252&gt;) catalog as first epoch. Analysis of repeated observations shows that the errors in radial velocity are ~26km/s. A relation between absolute magnitude and color is established using the horizontal branches of halo globular clusters observed by SDSS. Bolometric corrections and colors are synthesized in the SDSS filters from model spectra. The redder stars agree well in absolute magnitude with accepted values for RR Lyrae stars. The resulting photometric distances are accurate to about 0.2mag, with a median of about 25kpc. Modest clumps in phase space exist and are consistent with the previously reported tidal stream of the Sagittarius dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899#2</TD>
            <TD>2011-09-14T19:45:13Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/899</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/899&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/899</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/352/39 [1]</TD>
            <TD>Great Attractor region redshifts (Woudt+, 1999)</TD>
            <TD>In the third of a series of papers on large-scale structures behind the southern Milky Way, we report here on redshifts obtained at the South African Astronomical Observatory (SAAO) in the Great Attractor region (318{deg}&lt;~l&lt;~340{deg}, |b|&lt;=10{deg}, Woudt, 1998, Ph. D. Thesis, University of Cape Town). This region encompasses the peak in the reconstructed mass density field, associated with the Great Attractor (Kolatt et al., 1995MNRAS.275..797K, Dekel et al., 1999ApJ...522....1D) and covers the crossing of the Supergalactic Plane with the Galactic Plane. Our deep optical galaxy search in the Zone of Avoidance (ZOA) in this region (Woudt, 1998, Ph. D. Thesis, University of Cape Town) has resulted in the detection of 4423 galaxies with observed diameters larger than 0.2arcmin. We have obtained reliable redshifts for 309 galaxies of the 4423 galaxies with the ``Unit'' spectrograph (first with a Reticon, then with a CCD detector) at the 1.9-m telescope of the SAAO. An additional 13 tentative redshifts are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39#1</TD>
            <TD>2011-09-14T18:57:33Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/352/39</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/352/39</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/352/39 [2]</TD>
            <TD>Great Attractor region redshifts (Woudt+, 1999)</TD>
            <TD>In the third of a series of papers on large-scale structures behind the southern Milky Way, we report here on redshifts obtained at the South African Astronomical Observatory (SAAO) in the Great Attractor region (318{deg}&lt;~l&lt;~340{deg}, |b|&lt;=10{deg}, Woudt, 1998, Ph. D. Thesis, University of Cape Town). This region encompasses the peak in the reconstructed mass density field, associated with the Great Attractor (Kolatt et al., 1995MNRAS.275..797K, Dekel et al., 1999ApJ...522....1D) and covers the crossing of the Supergalactic Plane with the Galactic Plane. Our deep optical galaxy search in the Zone of Avoidance (ZOA) in this region (Woudt, 1998, Ph. D. Thesis, University of Cape Town) has resulted in the detection of 4423 galaxies with observed diameters larger than 0.2arcmin. We have obtained reliable redshifts for 309 galaxies of the 4423 galaxies with the ``Unit'' spectrograph (first with a Reticon, then with a CCD detector) at the 1.9-m telescope of the SAAO. An additional 13 tentative redshifts are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39#2</TD>
            <TD>2011-09-14T18:57:33Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/352/39&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/352/39</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/400/1962 [1]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#1</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/400/1962</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/400/1962 [2]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#2</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/400/1962 [table2]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#table2</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/400/1962 [tableb]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#tableb</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/400/1962 [tablea]</TD>
            <TD>Southern GEMS groups. II. (Kilborn+, 2009)</TD>
            <TD>The full GEMS (Group Evolution Multi-wavelength Study) sample includes 60 galaxy groups, chosen from 10 optical catalogues, the majority with recession velocities between 1000 and 3000km/s and with a ROSAT PSPC (position sensitive proportional counter) exposure time of more than 10000s within 20-arcmin of the group position. We chose 16 groups that were near or south of declination 0{deg}, for wide-field HI imaging at Parkes. The groups selected for HI observations have a variety of X-ray properties, from just the central galaxy being detected (six groups), to diffuse group-scale X-ray emission (eight groups), to no X-ray detection at all (two groups).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962#tablea</TD>
            <TD>2011-09-14T21:00:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/400/1962</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/400/1962&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/400/1962</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/352/39 [1]</TD>
            <TD>Great Attractor region redshifts (Woudt+, 1999)</TD>
            <TD>In the third of a series of papers on large-scale structures behind the southern Milky Way, we report here on redshifts obtained at the South African Astronomical Observatory (SAAO) in the Great Attractor region (318{deg}&lt;~l&lt;~340{deg}, |b|&lt;=10{deg}, Woudt, 1998, Ph. D. Thesis, University of Cape Town). This region encompasses the peak in the reconstructed mass density field, associated with the Great Attractor (Kolatt et al., 1995MNRAS.275..797K, Dekel et al., 1999ApJ...522....1D) and covers the crossing of the Supergalactic Plane with the Galactic Plane. Our deep optical galaxy search in the Zone of Avoidance (ZOA) in this region (Woudt, 1998, Ph. D. Thesis, University of Cape Town) has resulted in the detection of 4423 galaxies with observed diameters larger than 0.2arcmin. We have obtained reliable redshifts for 309 galaxies of the 4423 galaxies with the ``Unit'' spectrograph (first with a Reticon, then with a CCD detector) at the 1.9-m telescope of the SAAO. An additional 13 tentative redshifts are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39#1</TD>
            <TD>2011-09-14T18:57:33Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/352/39</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/352/39</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/352/39 [2]</TD>
            <TD>Great Attractor region redshifts (Woudt+, 1999)</TD>
            <TD>In the third of a series of papers on large-scale structures behind the southern Milky Way, we report here on redshifts obtained at the South African Astronomical Observatory (SAAO) in the Great Attractor region (318{deg}&lt;~l&lt;~340{deg}, |b|&lt;=10{deg}, Woudt, 1998, Ph. D. Thesis, University of Cape Town). This region encompasses the peak in the reconstructed mass density field, associated with the Great Attractor (Kolatt et al., 1995MNRAS.275..797K, Dekel et al., 1999ApJ...522....1D) and covers the crossing of the Supergalactic Plane with the Galactic Plane. Our deep optical galaxy search in the Zone of Avoidance (ZOA) in this region (Woudt, 1998, Ph. D. Thesis, University of Cape Town) has resulted in the detection of 4423 galaxies with observed diameters larger than 0.2arcmin. We have obtained reliable redshifts for 309 galaxies of the 4423 galaxies with the ``Unit'' spectrograph (first with a Reticon, then with a CCD detector) at the 1.9-m telescope of the SAAO. An additional 13 tentative redshifts are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39#2</TD>
            <TD>2011-09-14T18:57:33Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/352/39&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/352/39</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/1183 [1]</TD>
            <TD>Major galaxy mergers at z&lt;~3 (Conselice+, 2003)</TD>
            <TD>The images we use for our morphological analyses were acquired with the Hubble Space Telescope as part of the Hubble Deep Field North optical and near-infrared campaigns. Optical data from the Wide Field Planetary Camera 2 (WFPC2) of the HDF-N are combined with near-infrared (NIR) observations of the same field taken with the Near Infrared Camera and Multi-Object Spectrometer (NICMOS). The optical data consist of images in the WFPC2 filters: F300W (U), F450W (B), F606W (V), and F814W (I). The NICMOS HDF-N images were taken in 1998 June with observations in the F110W (J) and F160W (H) near-infrared bands. We also use a deep K-band image obtained with the Kitt Peak Mayall 4m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183#1</TD>
            <TD>2011-09-14T19:45:22Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/1183</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1183</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/1183 [2]</TD>
            <TD>Major galaxy mergers at z&lt;~3 (Conselice+, 2003)</TD>
            <TD>The images we use for our morphological analyses were acquired with the Hubble Space Telescope as part of the Hubble Deep Field North optical and near-infrared campaigns. Optical data from the Wide Field Planetary Camera 2 (WFPC2) of the HDF-N are combined with near-infrared (NIR) observations of the same field taken with the Near Infrared Camera and Multi-Object Spectrometer (NICMOS). The optical data consist of images in the WFPC2 filters: F300W (U), F450W (B), F606W (V), and F814W (I). The NICMOS HDF-N images were taken in 1998 June with observations in the F110W (J) and F160W (H) near-infrared bands. We also use a deep K-band image obtained with the Kitt Peak Mayall 4m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183#2</TD>
            <TD>2011-09-14T19:45:22Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/1183&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1183</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/352/39 [1]</TD>
            <TD>Great Attractor region redshifts (Woudt+, 1999)</TD>
            <TD>In the third of a series of papers on large-scale structures behind the southern Milky Way, we report here on redshifts obtained at the South African Astronomical Observatory (SAAO) in the Great Attractor region (318{deg}&lt;~l&lt;~340{deg}, |b|&lt;=10{deg}, Woudt, 1998, Ph. D. Thesis, University of Cape Town). This region encompasses the peak in the reconstructed mass density field, associated with the Great Attractor (Kolatt et al., 1995MNRAS.275..797K, Dekel et al., 1999ApJ...522....1D) and covers the crossing of the Supergalactic Plane with the Galactic Plane. Our deep optical galaxy search in the Zone of Avoidance (ZOA) in this region (Woudt, 1998, Ph. D. Thesis, University of Cape Town) has resulted in the detection of 4423 galaxies with observed diameters larger than 0.2arcmin. We have obtained reliable redshifts for 309 galaxies of the 4423 galaxies with the ``Unit'' spectrograph (first with a Reticon, then with a CCD detector) at the 1.9-m telescope of the SAAO. An additional 13 tentative redshifts are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39#1</TD>
            <TD>2011-09-14T18:57:33Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/352/39</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/352/39</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/352/39 [2]</TD>
            <TD>Great Attractor region redshifts (Woudt+, 1999)</TD>
            <TD>In the third of a series of papers on large-scale structures behind the southern Milky Way, we report here on redshifts obtained at the South African Astronomical Observatory (SAAO) in the Great Attractor region (318{deg}&lt;~l&lt;~340{deg}, |b|&lt;=10{deg}, Woudt, 1998, Ph. D. Thesis, University of Cape Town). This region encompasses the peak in the reconstructed mass density field, associated with the Great Attractor (Kolatt et al., 1995MNRAS.275..797K, Dekel et al., 1999ApJ...522....1D) and covers the crossing of the Supergalactic Plane with the Galactic Plane. Our deep optical galaxy search in the Zone of Avoidance (ZOA) in this region (Woudt, 1998, Ph. D. Thesis, University of Cape Town) has resulted in the detection of 4423 galaxies with observed diameters larger than 0.2arcmin. We have obtained reliable redshifts for 309 galaxies of the 4423 galaxies with the ``Unit'' spectrograph (first with a Reticon, then with a CCD detector) at the 1.9-m telescope of the SAAO. An additional 13 tentative redshifts are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39#2</TD>
            <TD>2011-09-14T18:57:33Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/352/39</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/352/39&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/352/39</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/187/275 [1]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#1</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/187/275</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/187/275 [2]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#2</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/187/275&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/187/275 [novae]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#novae</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/187/275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/187/275 [table4]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#table4</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/187/275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/405 [1]</TD>
            <TD>Montreal Blue Galaxy Survey. II. (Coziol+, 1994)</TD>
            <TD>We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B&lt;15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405#1</TD>
            <TD>2011-09-14T18:57:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/405</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/405</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/405 [2]</TD>
            <TD>Montreal Blue Galaxy Survey. II. (Coziol+, 1994)</TD>
            <TD>We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B&lt;15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405#2</TD>
            <TD>2011-09-14T18:57:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/405&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/405</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/405 [table1]</TD>
            <TD>Montreal Blue Galaxy Survey. II. (Coziol+, 1994)</TD>
            <TD>We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B&lt;15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405#table1</TD>
            <TD>2011-09-14T18:57:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/405&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/405</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/405 [1]</TD>
            <TD>Montreal Blue Galaxy Survey. II. (Coziol+, 1994)</TD>
            <TD>We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B&lt;15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405#1</TD>
            <TD>2011-09-14T18:57:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/405</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/405</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/405 [2]</TD>
            <TD>Montreal Blue Galaxy Survey. II. (Coziol+, 1994)</TD>
            <TD>We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B&lt;15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405#2</TD>
            <TD>2011-09-14T18:57:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/405&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/405</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/405 [table1]</TD>
            <TD>Montreal Blue Galaxy Survey. II. (Coziol+, 1994)</TD>
            <TD>We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B&lt;15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405#table1</TD>
            <TD>2011-09-14T18:57:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/405&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/405</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/405 [1]</TD>
            <TD>Montreal Blue Galaxy Survey. II. (Coziol+, 1994)</TD>
            <TD>We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B&lt;15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405#1</TD>
            <TD>2011-09-14T18:57:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/405</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/405</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/405 [2]</TD>
            <TD>Montreal Blue Galaxy Survey. II. (Coziol+, 1994)</TD>
            <TD>We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B&lt;15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405#2</TD>
            <TD>2011-09-14T18:57:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/405&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/405</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/405 [table1]</TD>
            <TD>Montreal Blue Galaxy Survey. II. (Coziol+, 1994)</TD>
            <TD>We present and discuss the second list of the Montreal Blue Galaxy survey. Following the inspection of 71 plates, we found 237 new candidates with B&lt;15.5. 73 percent of them are also detected by IRAS. Spectrophotometry was carried out, at medium resolution, for a subset of 40 objects leading to the identification of three new AGNs and producing 13 new radial velocities. Spectral classification of our candidates confirms our previous finding that the majority of our candidates are starburst nucleus galaxies similar to the objects studied by Balzano [1983ApJ...268..602B]. Our survey is biased against the high excitation starburst H II galaxies and the LINER galaxies. Metallicities of our galaxies are found to be from log(O/H)=8.4 to 9.0, which suggests galaxies in advanced stages of chemical evolution.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405#table1</TD>
            <TD>2011-09-14T18:57:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Feb-1995</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/405</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/405&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/405</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/471/694 [1]</TD>
            <TD>Abell 2390 Gunn photometry and equivalent widths (Abraham+ 1996)</TD>
            <TD>The galaxy population in the intermediate-redshift (z=0.228) rich cluster Abell 2390 is investigated. We present velocities, colors, and morphological information for an exceptionally large sample of 323 galaxies (216 cluster members) in a 46'x7' (6h^-1^Mpcx1h^-1^Mpc) strip centered on the cD galaxy. This sample of confirmed cluster members is second only to that for the Coma cluster in terms of sample size and spatial coverage in the cluster rest frame and it is the first to trace the transition between a rich cluster and the field at intermediate redshift. The galaxy population in the cluster changes gradually from a very evolved, early-type population in the inner 0.4h^-1^Mpc of the cluster to a progressively later type population in the extensive outer envelope of the cluster from 1 to 3h^-1^Mpc in radius. Radial gradients in galaxy gr color, 4000{AA} break, H{delta} and [O II] line strengths, and morphology are seen in the cluster and are investigated by comparing the data to models computed with the GISSEL spectral synthesis package. The results suggest that the cluster has been built up gradually by the infall of field galaxies over ~8Gyr and that star formation has been truncated in infalling galaxies during the accretion process. The morphological composition of the cluster is shown to be consistent with such a scenario. If true for other clusters, infall-truncated star formation as seen in Abell 2390 may explain both the Butcher-Oemler effect and the large fraction of S0 galaxies in clusters. Only &lt;5% of the galaxies observed in Abell 2390 exhibit evidence for star formation at levels stronger than those seen in typical late-type systems. This suggests that starbursts do not play a major role in driving cluster galaxy evolution at the redshift of Abell 2390, although infall-induced starbursts leading to truncated star formation may have played a role in the earlier history of the cluster. Evidence is found for at least one subcomponent on the west side of the cluster, which is likely to be infalling at the epoch of observation. For a description of the Gunn photometric system, see e.g. &lt;GCPD/38&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/694#1</TD>
            <TD>2011-09-14T18:58:00Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/471/694</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/694</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/471/694 [2]</TD>
            <TD>Abell 2390 Gunn photometry and equivalent widths (Abraham+ 1996)</TD>
            <TD>The galaxy population in the intermediate-redshift (z=0.228) rich cluster Abell 2390 is investigated. We present velocities, colors, and morphological information for an exceptionally large sample of 323 galaxies (216 cluster members) in a 46'x7' (6h^-1^Mpcx1h^-1^Mpc) strip centered on the cD galaxy. This sample of confirmed cluster members is second only to that for the Coma cluster in terms of sample size and spatial coverage in the cluster rest frame and it is the first to trace the transition between a rich cluster and the field at intermediate redshift. The galaxy population in the cluster changes gradually from a very evolved, early-type population in the inner 0.4h^-1^Mpc of the cluster to a progressively later type population in the extensive outer envelope of the cluster from 1 to 3h^-1^Mpc in radius. Radial gradients in galaxy gr color, 4000{AA} break, H{delta} and [O II] line strengths, and morphology are seen in the cluster and are investigated by comparing the data to models computed with the GISSEL spectral synthesis package. The results suggest that the cluster has been built up gradually by the infall of field galaxies over ~8Gyr and that star formation has been truncated in infalling galaxies during the accretion process. The morphological composition of the cluster is shown to be consistent with such a scenario. If true for other clusters, infall-truncated star formation as seen in Abell 2390 may explain both the Butcher-Oemler effect and the large fraction of S0 galaxies in clusters. Only &lt;5% of the galaxies observed in Abell 2390 exhibit evidence for star formation at levels stronger than those seen in typical late-type systems. This suggests that starbursts do not play a major role in driving cluster galaxy evolution at the redshift of Abell 2390, although infall-induced starbursts leading to truncated star formation may have played a role in the earlier history of the cluster. Evidence is found for at least one subcomponent on the west side of the cluster, which is likely to be infalling at the epoch of observation. For a description of the Gunn photometric system, see e.g. &lt;GCPD/38&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/694#2</TD>
            <TD>2011-09-14T18:58:00Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/471/694&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/694</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/187/275 [1]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#1</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/187/275</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/187/275 [2]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#2</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/187/275&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/187/275 [novae]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#novae</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/187/275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/187/275 [table4]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#table4</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/187/275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/1183 [1]</TD>
            <TD>Major galaxy mergers at z&lt;~3 (Conselice+, 2003)</TD>
            <TD>The images we use for our morphological analyses were acquired with the Hubble Space Telescope as part of the Hubble Deep Field North optical and near-infrared campaigns. Optical data from the Wide Field Planetary Camera 2 (WFPC2) of the HDF-N are combined with near-infrared (NIR) observations of the same field taken with the Near Infrared Camera and Multi-Object Spectrometer (NICMOS). The optical data consist of images in the WFPC2 filters: F300W (U), F450W (B), F606W (V), and F814W (I). The NICMOS HDF-N images were taken in 1998 June with observations in the F110W (J) and F160W (H) near-infrared bands. We also use a deep K-band image obtained with the Kitt Peak Mayall 4m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183#1</TD>
            <TD>2011-09-14T19:45:22Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/1183</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1183</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/1183 [2]</TD>
            <TD>Major galaxy mergers at z&lt;~3 (Conselice+, 2003)</TD>
            <TD>The images we use for our morphological analyses were acquired with the Hubble Space Telescope as part of the Hubble Deep Field North optical and near-infrared campaigns. Optical data from the Wide Field Planetary Camera 2 (WFPC2) of the HDF-N are combined with near-infrared (NIR) observations of the same field taken with the Near Infrared Camera and Multi-Object Spectrometer (NICMOS). The optical data consist of images in the WFPC2 filters: F300W (U), F450W (B), F606W (V), and F814W (I). The NICMOS HDF-N images were taken in 1998 June with observations in the F110W (J) and F160W (H) near-infrared bands. We also use a deep K-band image obtained with the Kitt Peak Mayall 4m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183#2</TD>
            <TD>2011-09-14T19:45:22Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/1183&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1183</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/471/694 [1]</TD>
            <TD>Abell 2390 Gunn photometry and equivalent widths (Abraham+ 1996)</TD>
            <TD>The galaxy population in the intermediate-redshift (z=0.228) rich cluster Abell 2390 is investigated. We present velocities, colors, and morphological information for an exceptionally large sample of 323 galaxies (216 cluster members) in a 46'x7' (6h^-1^Mpcx1h^-1^Mpc) strip centered on the cD galaxy. This sample of confirmed cluster members is second only to that for the Coma cluster in terms of sample size and spatial coverage in the cluster rest frame and it is the first to trace the transition between a rich cluster and the field at intermediate redshift. The galaxy population in the cluster changes gradually from a very evolved, early-type population in the inner 0.4h^-1^Mpc of the cluster to a progressively later type population in the extensive outer envelope of the cluster from 1 to 3h^-1^Mpc in radius. Radial gradients in galaxy gr color, 4000{AA} break, H{delta} and [O II] line strengths, and morphology are seen in the cluster and are investigated by comparing the data to models computed with the GISSEL spectral synthesis package. The results suggest that the cluster has been built up gradually by the infall of field galaxies over ~8Gyr and that star formation has been truncated in infalling galaxies during the accretion process. The morphological composition of the cluster is shown to be consistent with such a scenario. If true for other clusters, infall-truncated star formation as seen in Abell 2390 may explain both the Butcher-Oemler effect and the large fraction of S0 galaxies in clusters. Only &lt;5% of the galaxies observed in Abell 2390 exhibit evidence for star formation at levels stronger than those seen in typical late-type systems. This suggests that starbursts do not play a major role in driving cluster galaxy evolution at the redshift of Abell 2390, although infall-induced starbursts leading to truncated star formation may have played a role in the earlier history of the cluster. Evidence is found for at least one subcomponent on the west side of the cluster, which is likely to be infalling at the epoch of observation. For a description of the Gunn photometric system, see e.g. &lt;GCPD/38&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/694#1</TD>
            <TD>2011-09-14T18:58:00Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/471/694</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/694</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/471/694 [2]</TD>
            <TD>Abell 2390 Gunn photometry and equivalent widths (Abraham+ 1996)</TD>
            <TD>The galaxy population in the intermediate-redshift (z=0.228) rich cluster Abell 2390 is investigated. We present velocities, colors, and morphological information for an exceptionally large sample of 323 galaxies (216 cluster members) in a 46'x7' (6h^-1^Mpcx1h^-1^Mpc) strip centered on the cD galaxy. This sample of confirmed cluster members is second only to that for the Coma cluster in terms of sample size and spatial coverage in the cluster rest frame and it is the first to trace the transition between a rich cluster and the field at intermediate redshift. The galaxy population in the cluster changes gradually from a very evolved, early-type population in the inner 0.4h^-1^Mpc of the cluster to a progressively later type population in the extensive outer envelope of the cluster from 1 to 3h^-1^Mpc in radius. Radial gradients in galaxy gr color, 4000{AA} break, H{delta} and [O II] line strengths, and morphology are seen in the cluster and are investigated by comparing the data to models computed with the GISSEL spectral synthesis package. The results suggest that the cluster has been built up gradually by the infall of field galaxies over ~8Gyr and that star formation has been truncated in infalling galaxies during the accretion process. The morphological composition of the cluster is shown to be consistent with such a scenario. If true for other clusters, infall-truncated star formation as seen in Abell 2390 may explain both the Butcher-Oemler effect and the large fraction of S0 galaxies in clusters. Only &lt;5% of the galaxies observed in Abell 2390 exhibit evidence for star formation at levels stronger than those seen in typical late-type systems. This suggests that starbursts do not play a major role in driving cluster galaxy evolution at the redshift of Abell 2390, although infall-induced starbursts leading to truncated star formation may have played a role in the earlier history of the cluster. Evidence is found for at least one subcomponent on the west side of the cluster, which is likely to be infalling at the epoch of observation. For a description of the Gunn photometric system, see e.g. &lt;GCPD/38&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/694#2</TD>
            <TD>2011-09-14T18:58:00Z</TD>
            <TD>#Clusters_of_galaxies#Equivalent_widths#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/471/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/471/694&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/471/694</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/187/275 [1]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#1</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/187/275</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/187/275 [2]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#2</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/187/275&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/187/275 [novae]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#novae</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/187/275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/187/275 [table4]</TD>
            <TD>Photometric histories of recurrent novae (Schaefer, 2010)</TD>
            <TD>++++Lrecl of file 'table22.dat' (65) increased to 70 %B I collect virtually all photometry of the 10 known galactic recurrent novae (RNe) and their 37 known eruptions. This consists of my modern measures of nearly all archival plates (providing the only data for half of 37 known eruptions), my own 10000 CCD magnitudes from 1987 to present (providing virtually all of the magnitudes in quiescence for seven RNe), over 140000 visual magnitude estimates recorded by amateur astronomers (who discovered half the known eruptions), and the small scattering of magnitudes from all the literature. From this, I produce various uniform products: (1) BVRIJHK comparison star magnitudes and BV comparison star sequences to cover the entire range of eruption; (2) complete light curves for all eruptions; (3) best-fit B and V light curve templates; (4) orbital periods for all but one RN; (5) exhaustive searches for all missed eruptions; (6) measured discovery efficiencies since 1890; (7) true recurrence time scales; (8) predicted next eruption dates; (9) variations on time scales of minutes, hours, days, months, years, decades, and century; (10) uniform distances and extinctions to all RNe; (11) BV colors at peak and UBVRIJHK colors at minimum, all with extinction corrections; and (12) the spectral energy distributions over UBVRIJHK. Highlights of this work include the discoveries of one new RN, six previously unknown eruptions, and the orbital periods for half the RNe. The goal of this work is to provide uniform demographics for answering questions like the "What is the death rate of RNe in our Galaxy?" and "Are the white dwarfs gaining or losing mass over each eruption cycle?." An important use of this work is for the question of whether RNe can be the progenitors of Type Ia supernovae.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275#table4</TD>
            <TD>2011-09-14T21:00:16Z</TD>
            <TD>#Novae#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/187/275</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/187/275&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/187/275</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/120/147 [1]</TD>
            <TD>Radio sources in 14 Abell clusters (Marvel+, 1999)</TD>
            <TD>We present a VLA C-configuration imaging survey of 14 rich Abell clusters. The observations were undertaken with the intent of characterizing the galaxy orbits within the cluster by combining galaxy redshifts with indicators of orbital shape. We present maps of the observed clusters, detailed maps of resolved sources detected in the survey, comparisons with optical images of the clusters, and tables of source parameters for all detected sources with measured flux values.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147#1</TD>
            <TD>2011-09-14T18:59:19Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/120/147</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/147</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/120/147 [2]</TD>
            <TD>Radio sources in 14 Abell clusters (Marvel+, 1999)</TD>
            <TD>We present a VLA C-configuration imaging survey of 14 rich Abell clusters. The observations were undertaken with the intent of characterizing the galaxy orbits within the cluster by combining galaxy redshifts with indicators of orbital shape. We present maps of the observed clusters, detailed maps of resolved sources detected in the survey, comparisons with optical images of the clusters, and tables of source parameters for all detected sources with measured flux values.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147#2</TD>
            <TD>2011-09-14T18:59:19Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/120/147&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/147</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/1183 [1]</TD>
            <TD>Major galaxy mergers at z&lt;~3 (Conselice+, 2003)</TD>
            <TD>The images we use for our morphological analyses were acquired with the Hubble Space Telescope as part of the Hubble Deep Field North optical and near-infrared campaigns. Optical data from the Wide Field Planetary Camera 2 (WFPC2) of the HDF-N are combined with near-infrared (NIR) observations of the same field taken with the Near Infrared Camera and Multi-Object Spectrometer (NICMOS). The optical data consist of images in the WFPC2 filters: F300W (U), F450W (B), F606W (V), and F814W (I). The NICMOS HDF-N images were taken in 1998 June with observations in the F110W (J) and F160W (H) near-infrared bands. We also use a deep K-band image obtained with the Kitt Peak Mayall 4m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183#1</TD>
            <TD>2011-09-14T19:45:22Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/1183</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1183</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/1183 [2]</TD>
            <TD>Major galaxy mergers at z&lt;~3 (Conselice+, 2003)</TD>
            <TD>The images we use for our morphological analyses were acquired with the Hubble Space Telescope as part of the Hubble Deep Field North optical and near-infrared campaigns. Optical data from the Wide Field Planetary Camera 2 (WFPC2) of the HDF-N are combined with near-infrared (NIR) observations of the same field taken with the Near Infrared Camera and Multi-Object Spectrometer (NICMOS). The optical data consist of images in the WFPC2 filters: F300W (U), F450W (B), F606W (V), and F814W (I). The NICMOS HDF-N images were taken in 1998 June with observations in the F110W (J) and F160W (H) near-infrared bands. We also use a deep K-band image obtained with the Kitt Peak Mayall 4m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183#2</TD>
            <TD>2011-09-14T19:45:22Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1183</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/1183&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1183</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/2385 [1]</TD>
            <TD>Occulting galaxy pairs in SDSS (Holwerda+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385#1</TD>
            <TD>2011-09-14T21:00:49Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/2385</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2385</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/2385 [2]</TD>
            <TD>Occulting galaxy pairs in SDSS (Holwerda+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385#2</TD>
            <TD>2011-09-14T21:00:49Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/2385&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2385</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/2385 [table1]</TD>
            <TD>Occulting galaxy pairs in SDSS (Holwerda+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385#table1</TD>
            <TD>2011-09-14T21:00:49Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/2385&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2385</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/120/147 [1]</TD>
            <TD>Radio sources in 14 Abell clusters (Marvel+, 1999)</TD>
            <TD>We present a VLA C-configuration imaging survey of 14 rich Abell clusters. The observations were undertaken with the intent of characterizing the galaxy orbits within the cluster by combining galaxy redshifts with indicators of orbital shape. We present maps of the observed clusters, detailed maps of resolved sources detected in the survey, comparisons with optical images of the clusters, and tables of source parameters for all detected sources with measured flux values.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147#1</TD>
            <TD>2011-09-14T18:59:19Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/120/147</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/147</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/120/147 [2]</TD>
            <TD>Radio sources in 14 Abell clusters (Marvel+, 1999)</TD>
            <TD>We present a VLA C-configuration imaging survey of 14 rich Abell clusters. The observations were undertaken with the intent of characterizing the galaxy orbits within the cluster by combining galaxy redshifts with indicators of orbital shape. We present maps of the observed clusters, detailed maps of resolved sources detected in the survey, comparisons with optical images of the clusters, and tables of source parameters for all detected sources with measured flux values.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147#2</TD>
            <TD>2011-09-14T18:59:19Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/120/147&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/147</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/245 [1]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy (Majewski+, 2004)</TD>
            <TD>We have obtained moderate resolution (~6km/s) spectroscopy of several hundred M giant candidates selected from Two Micron All Sky Survey photometry (Cat. &lt;II/246&gt;). Radial velocities are presented for stars mainly in the southern Galactic hemisphere, and the primary targets have Galactic positions consistent with association to the tidal tail system of the Sagittarius (Sgr) dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245#1</TD>
            <TD>2011-09-14T19:45:24Z</TD>
            <TD>#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/245</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/245</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/245 [2]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy (Majewski+, 2004)</TD>
            <TD>We have obtained moderate resolution (~6km/s) spectroscopy of several hundred M giant candidates selected from Two Micron All Sky Survey photometry (Cat. &lt;II/246&gt;). Radial velocities are presented for stars mainly in the southern Galactic hemisphere, and the primary targets have Galactic positions consistent with association to the tidal tail system of the Sagittarius (Sgr) dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245#2</TD>
            <TD>2011-09-14T19:45:24Z</TD>
            <TD>#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/245&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/245 [table3]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy (Majewski+, 2004)</TD>
            <TD>We have obtained moderate resolution (~6km/s) spectroscopy of several hundred M giant candidates selected from Two Micron All Sky Survey photometry (Cat. &lt;II/246&gt;). Radial velocities are presented for stars mainly in the southern Galactic hemisphere, and the primary targets have Galactic positions consistent with association to the tidal tail system of the Sagittarius (Sgr) dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245#table3</TD>
            <TD>2011-09-14T19:45:24Z</TD>
            <TD>#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/245</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/2385 [1]</TD>
            <TD>Occulting galaxy pairs in SDSS (Holwerda+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385#1</TD>
            <TD>2011-09-14T21:00:49Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/2385</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2385</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/2385 [2]</TD>
            <TD>Occulting galaxy pairs in SDSS (Holwerda+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385#2</TD>
            <TD>2011-09-14T21:00:49Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/2385&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2385</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/2385 [table1]</TD>
            <TD>Occulting galaxy pairs in SDSS (Holwerda+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385#table1</TD>
            <TD>2011-09-14T21:00:49Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/2385&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2385</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/120/147 [1]</TD>
            <TD>Radio sources in 14 Abell clusters (Marvel+, 1999)</TD>
            <TD>We present a VLA C-configuration imaging survey of 14 rich Abell clusters. The observations were undertaken with the intent of characterizing the galaxy orbits within the cluster by combining galaxy redshifts with indicators of orbital shape. We present maps of the observed clusters, detailed maps of resolved sources detected in the survey, comparisons with optical images of the clusters, and tables of source parameters for all detected sources with measured flux values.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147#1</TD>
            <TD>2011-09-14T18:59:19Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/120/147</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/147</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/120/147 [2]</TD>
            <TD>Radio sources in 14 Abell clusters (Marvel+, 1999)</TD>
            <TD>We present a VLA C-configuration imaging survey of 14 rich Abell clusters. The observations were undertaken with the intent of characterizing the galaxy orbits within the cluster by combining galaxy redshifts with indicators of orbital shape. We present maps of the observed clusters, detailed maps of resolved sources detected in the survey, comparisons with optical images of the clusters, and tables of source parameters for all detected sources with measured flux values.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147#2</TD>
            <TD>2011-09-14T18:59:19Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/120/147&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/147</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/245 [1]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy (Majewski+, 2004)</TD>
            <TD>We have obtained moderate resolution (~6km/s) spectroscopy of several hundred M giant candidates selected from Two Micron All Sky Survey photometry (Cat. &lt;II/246&gt;). Radial velocities are presented for stars mainly in the southern Galactic hemisphere, and the primary targets have Galactic positions consistent with association to the tidal tail system of the Sagittarius (Sgr) dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245#1</TD>
            <TD>2011-09-14T19:45:24Z</TD>
            <TD>#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/245</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/245</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/245 [2]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy (Majewski+, 2004)</TD>
            <TD>We have obtained moderate resolution (~6km/s) spectroscopy of several hundred M giant candidates selected from Two Micron All Sky Survey photometry (Cat. &lt;II/246&gt;). Radial velocities are presented for stars mainly in the southern Galactic hemisphere, and the primary targets have Galactic positions consistent with association to the tidal tail system of the Sagittarius (Sgr) dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245#2</TD>
            <TD>2011-09-14T19:45:24Z</TD>
            <TD>#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/245&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/245 [table3]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy (Majewski+, 2004)</TD>
            <TD>We have obtained moderate resolution (~6km/s) spectroscopy of several hundred M giant candidates selected from Two Micron All Sky Survey photometry (Cat. &lt;II/246&gt;). Radial velocities are presented for stars mainly in the southern Galactic hemisphere, and the primary targets have Galactic positions consistent with association to the tidal tail system of the Sagittarius (Sgr) dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245#table3</TD>
            <TD>2011-09-14T19:45:24Z</TD>
            <TD>#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/245</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/2385 [1]</TD>
            <TD>Occulting galaxy pairs in SDSS (Holwerda+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385#1</TD>
            <TD>2011-09-14T21:00:49Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/2385</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2385</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/2385 [2]</TD>
            <TD>Occulting galaxy pairs in SDSS (Holwerda+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385#2</TD>
            <TD>2011-09-14T21:00:49Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/2385&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2385</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/2385 [table1]</TD>
            <TD>Occulting galaxy pairs in SDSS (Holwerda+, 2007)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385#table1</TD>
            <TD>2011-09-14T21:00:49Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/2385</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/2385&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/2385</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/510/637 [1]</TD>
            <TD>Near IR properties of Galaxy disks (Hunt+ 1999)</TD>
            <TD>We have derived the near-infrared structural components of a sample of Seyfert and starburst (SBN) host galaxies by fitting near-infrared images with a new two-dimensional decomposition algorithm. An analysis of the fitted parameters shows that Seyfert 1 and SBN bulges resemble normal early-type bulges in structure and color, with (J-K)^c^_b_ about 0.1 mag redder than disk (J-K)^c^_d_. Seyfert 2 bulges, on the other hand, are bluer than normal, with (J-K)^c^_b_{approx}(J-K)^c^_d_. Seyfert disks (especially type 1), but not those of SBNs, are abnormally bright (in surface brightness), significantly more so than even the brightest normal disks. Seyfert disks are also compact, but similar to those in normal early-type spirals. For a given mass, Seyfert and particularly SBN galaxies are abnormally rich in neutral hydrogen, and there is strong, albeit indirect, evidence for lower mass-to-light (M/L) ratios in Seyfert and SBN disks, but normal M/L ratios in their bulges. In Seyfert and SBN galaxies, H I mass fractions and M/L ratios are anticorrelated, and we attribute the high gas mass fractions and low M/L ratios in SBNs and several Seyfert galaxies to ongoing star formation. Such abundant gas in Seyfert galaxies would be expected to inhibit bar formation, which may explain why active galaxies are not always barred.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/637#1</TD>
            <TD>2011-09-14T18:59:27Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/637</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/510/637</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/510/637</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/510/637 [2]</TD>
            <TD>Near IR properties of Galaxy disks (Hunt+ 1999)</TD>
            <TD>We have derived the near-infrared structural components of a sample of Seyfert and starburst (SBN) host galaxies by fitting near-infrared images with a new two-dimensional decomposition algorithm. An analysis of the fitted parameters shows that Seyfert 1 and SBN bulges resemble normal early-type bulges in structure and color, with (J-K)^c^_b_ about 0.1 mag redder than disk (J-K)^c^_d_. Seyfert 2 bulges, on the other hand, are bluer than normal, with (J-K)^c^_b_{approx}(J-K)^c^_d_. Seyfert disks (especially type 1), but not those of SBNs, are abnormally bright (in surface brightness), significantly more so than even the brightest normal disks. Seyfert disks are also compact, but similar to those in normal early-type spirals. For a given mass, Seyfert and particularly SBN galaxies are abnormally rich in neutral hydrogen, and there is strong, albeit indirect, evidence for lower mass-to-light (M/L) ratios in Seyfert and SBN disks, but normal M/L ratios in their bulges. In Seyfert and SBN galaxies, H I mass fractions and M/L ratios are anticorrelated, and we attribute the high gas mass fractions and low M/L ratios in SBNs and several Seyfert galaxies to ongoing star formation. Such abundant gas in Seyfert galaxies would be expected to inhibit bar formation, which may explain why active galaxies are not always barred.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/637#2</TD>
            <TD>2011-09-14T18:59:27Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/637</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/510/637&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/510/637</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/245 [1]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy (Majewski+, 2004)</TD>
            <TD>We have obtained moderate resolution (~6km/s) spectroscopy of several hundred M giant candidates selected from Two Micron All Sky Survey photometry (Cat. &lt;II/246&gt;). Radial velocities are presented for stars mainly in the southern Galactic hemisphere, and the primary targets have Galactic positions consistent with association to the tidal tail system of the Sagittarius (Sgr) dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245#1</TD>
            <TD>2011-09-14T19:45:24Z</TD>
            <TD>#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/245</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/245</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/245 [2]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy (Majewski+, 2004)</TD>
            <TD>We have obtained moderate resolution (~6km/s) spectroscopy of several hundred M giant candidates selected from Two Micron All Sky Survey photometry (Cat. &lt;II/246&gt;). Radial velocities are presented for stars mainly in the southern Galactic hemisphere, and the primary targets have Galactic positions consistent with association to the tidal tail system of the Sagittarius (Sgr) dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245#2</TD>
            <TD>2011-09-14T19:45:24Z</TD>
            <TD>#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/245&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/245</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/128/245 [table3]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy (Majewski+, 2004)</TD>
            <TD>We have obtained moderate resolution (~6km/s) spectroscopy of several hundred M giant candidates selected from Two Micron All Sky Survey photometry (Cat. &lt;II/246&gt;). Radial velocities are presented for stars mainly in the southern Galactic hemisphere, and the primary targets have Galactic positions consistent with association to the tidal tail system of the Sagittarius (Sgr) dwarf galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245#table3</TD>
            <TD>2011-09-14T19:45:24Z</TD>
            <TD>#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/245</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/128/245&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/245</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/1329 [1]</TD>
            <TD>M82 X-ray sources long-term variability (Chiang+, 2011)</TD>
            <TD>Since the X-ray sources in the central region of M82 are crowded, a high spatial resolution instrument like the Chandra X-ray Observatory is needed to resolve the images. M82 has been observed 13 times between 1999 and 2007 with Chandra; some of them were designed to observe M82 X-1 with special configurations. To study the long-term variability of the whole galaxy, we used nine Chandra data sets with relatively long exposure time and large field of view from the Chandra Data Archive.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329#1</TD>
            <TD>2012-03-31T16:22:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/1329</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1329</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/1329 [2]</TD>
            <TD>M82 X-ray sources long-term variability (Chiang+, 2011)</TD>
            <TD>Since the X-ray sources in the central region of M82 are crowded, a high spatial resolution instrument like the Chandra X-ray Observatory is needed to resolve the images. M82 has been observed 13 times between 1999 and 2007 with Chandra; some of them were designed to observe M82 X-1 with special configurations. To study the long-term variability of the whole galaxy, we used nine Chandra data sets with relatively long exposure time and large field of view from the Chandra Data Archive.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329#2</TD>
            <TD>2012-03-31T16:22:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/1329&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1329</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/1329 [table2]</TD>
            <TD>M82 X-ray sources long-term variability (Chiang+, 2011)</TD>
            <TD>Since the X-ray sources in the central region of M82 are crowded, a high spatial resolution instrument like the Chandra X-ray Observatory is needed to resolve the images. M82 has been observed 13 times between 1999 and 2007 with Chandra; some of them were designed to observe M82 X-1 with special configurations. To study the long-term variability of the whole galaxy, we used nine Chandra data sets with relatively long exposure time and large field of view from the Chandra Data Archive.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329#table2</TD>
            <TD>2012-03-31T16:22:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/1329&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1329</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/510/637 [1]</TD>
            <TD>Near IR properties of Galaxy disks (Hunt+ 1999)</TD>
            <TD>We have derived the near-infrared structural components of a sample of Seyfert and starburst (SBN) host galaxies by fitting near-infrared images with a new two-dimensional decomposition algorithm. An analysis of the fitted parameters shows that Seyfert 1 and SBN bulges resemble normal early-type bulges in structure and color, with (J-K)^c^_b_ about 0.1 mag redder than disk (J-K)^c^_d_. Seyfert 2 bulges, on the other hand, are bluer than normal, with (J-K)^c^_b_{approx}(J-K)^c^_d_. Seyfert disks (especially type 1), but not those of SBNs, are abnormally bright (in surface brightness), significantly more so than even the brightest normal disks. Seyfert disks are also compact, but similar to those in normal early-type spirals. For a given mass, Seyfert and particularly SBN galaxies are abnormally rich in neutral hydrogen, and there is strong, albeit indirect, evidence for lower mass-to-light (M/L) ratios in Seyfert and SBN disks, but normal M/L ratios in their bulges. In Seyfert and SBN galaxies, H I mass fractions and M/L ratios are anticorrelated, and we attribute the high gas mass fractions and low M/L ratios in SBNs and several Seyfert galaxies to ongoing star formation. Such abundant gas in Seyfert galaxies would be expected to inhibit bar formation, which may explain why active galaxies are not always barred.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/637#1</TD>
            <TD>2011-09-14T18:59:27Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/637</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/510/637</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/510/637</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/510/637 [2]</TD>
            <TD>Near IR properties of Galaxy disks (Hunt+ 1999)</TD>
            <TD>We have derived the near-infrared structural components of a sample of Seyfert and starburst (SBN) host galaxies by fitting near-infrared images with a new two-dimensional decomposition algorithm. An analysis of the fitted parameters shows that Seyfert 1 and SBN bulges resemble normal early-type bulges in structure and color, with (J-K)^c^_b_ about 0.1 mag redder than disk (J-K)^c^_d_. Seyfert 2 bulges, on the other hand, are bluer than normal, with (J-K)^c^_b_{approx}(J-K)^c^_d_. Seyfert disks (especially type 1), but not those of SBNs, are abnormally bright (in surface brightness), significantly more so than even the brightest normal disks. Seyfert disks are also compact, but similar to those in normal early-type spirals. For a given mass, Seyfert and particularly SBN galaxies are abnormally rich in neutral hydrogen, and there is strong, albeit indirect, evidence for lower mass-to-light (M/L) ratios in Seyfert and SBN disks, but normal M/L ratios in their bulges. In Seyfert and SBN galaxies, H I mass fractions and M/L ratios are anticorrelated, and we attribute the high gas mass fractions and low M/L ratios in SBNs and several Seyfert galaxies to ongoing star formation. Such abundant gas in Seyfert galaxies would be expected to inhibit bar formation, which may explain why active galaxies are not always barred.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/637#2</TD>
            <TD>2011-09-14T18:59:27Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/637</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/510/637&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/510/637</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/126 [1]</TD>
            <TD>MEGA-H proper motion catalog (Kharchenko, 2004)</TD>
            <TD>The catalogue MEGA-H is a result of a merging of star lists from the catalogue of stellar proper motions with respect to galaxies in 47 selected areas near the Main Meridional Section of the Galaxy (MEGA-G) (Kharchenko 1987) and from All-sky Compiled Catalogue of 2.5 Million Stars (ASCC-2.5) (Cat. &lt;I/280&gt;). Proper motions from the catalogue MEGA-G were reduced to the Hipparcos system by means of common with the ASCC-2.5 stars. The compiled proper motions in the Hipparcos system and their standard errors were computed as the weighted means. Equatorial coordinates are reduced to the equinox J2000 and epoch 1991.25. The catalogue MEGA-H contains 18169 stars. Stars are sorted in right ascension J2000 order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/126#1</TD>
            <TD>2011-09-14T19:45:37Z</TD>
            <TD>#Positional_Data#Stars#Photometry:wide-band#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/V/126</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/126</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/126</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/126 [2]</TD>
            <TD>MEGA-H proper motion catalog (Kharchenko, 2004)</TD>
            <TD>The catalogue MEGA-H is a result of a merging of star lists from the catalogue of stellar proper motions with respect to galaxies in 47 selected areas near the Main Meridional Section of the Galaxy (MEGA-G) (Kharchenko 1987) and from All-sky Compiled Catalogue of 2.5 Million Stars (ASCC-2.5) (Cat. &lt;I/280&gt;). Proper motions from the catalogue MEGA-G were reduced to the Hipparcos system by means of common with the ASCC-2.5 stars. The compiled proper motions in the Hipparcos system and their standard errors were computed as the weighted means. Equatorial coordinates are reduced to the equinox J2000 and epoch 1991.25. The catalogue MEGA-H contains 18169 stars. Stars are sorted in right ascension J2000 order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/126#2</TD>
            <TD>2011-09-14T19:45:37Z</TD>
            <TD>#Positional_Data#Stars#Photometry:wide-band#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/V/126</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/126&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/126</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/1329 [1]</TD>
            <TD>M82 X-ray sources long-term variability (Chiang+, 2011)</TD>
            <TD>Since the X-ray sources in the central region of M82 are crowded, a high spatial resolution instrument like the Chandra X-ray Observatory is needed to resolve the images. M82 has been observed 13 times between 1999 and 2007 with Chandra; some of them were designed to observe M82 X-1 with special configurations. To study the long-term variability of the whole galaxy, we used nine Chandra data sets with relatively long exposure time and large field of view from the Chandra Data Archive.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329#1</TD>
            <TD>2012-03-31T16:22:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/1329</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1329</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/1329 [2]</TD>
            <TD>M82 X-ray sources long-term variability (Chiang+, 2011)</TD>
            <TD>Since the X-ray sources in the central region of M82 are crowded, a high spatial resolution instrument like the Chandra X-ray Observatory is needed to resolve the images. M82 has been observed 13 times between 1999 and 2007 with Chandra; some of them were designed to observe M82 X-1 with special configurations. To study the long-term variability of the whole galaxy, we used nine Chandra data sets with relatively long exposure time and large field of view from the Chandra Data Archive.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329#2</TD>
            <TD>2012-03-31T16:22:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/1329&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1329</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/1329 [table2]</TD>
            <TD>M82 X-ray sources long-term variability (Chiang+, 2011)</TD>
            <TD>Since the X-ray sources in the central region of M82 are crowded, a high spatial resolution instrument like the Chandra X-ray Observatory is needed to resolve the images. M82 has been observed 13 times between 1999 and 2007 with Chandra; some of them were designed to observe M82 X-1 with special configurations. To study the long-term variability of the whole galaxy, we used nine Chandra data sets with relatively long exposure time and large field of view from the Chandra Data Archive.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329#table2</TD>
            <TD>2012-03-31T16:22:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/1329&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1329</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/510/659 [1]</TD>
            <TD>Size and Structure of AGN in NGC 5548 (Peterson+, 1999)</TD>
            <TD>We present the results of 3 yr of ground-based observations of the Seyfert 1 galaxy NGC 5548, which, combined with previously reported data, yield optical continuum and broad-line H{beta} light curves for a total of 8 yr. The light curves consist of over 800 points, with a typical spacing of a few days between observations. During this 8 yr period, the nuclear continuum has varied by more than a factor of 7, and the H{beta} emission line has varied by a factor of nearly 6. The H{beta} emission line responds to continuum variations with a time delay or lag of {=~}10--20 days, the precise value varying somewhat from year to year. We find some indications that the lag varies with continuum flux in the sense that the lag is larger when the source is brighter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/659#1</TD>
            <TD>2011-09-14T18:59:29Z</TD>
            <TD>#AGN#Photometry#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/659</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/510/659</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/510/659</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/510/659 [2]</TD>
            <TD>Size and Structure of AGN in NGC 5548 (Peterson+, 1999)</TD>
            <TD>We present the results of 3 yr of ground-based observations of the Seyfert 1 galaxy NGC 5548, which, combined with previously reported data, yield optical continuum and broad-line H{beta} light curves for a total of 8 yr. The light curves consist of over 800 points, with a typical spacing of a few days between observations. During this 8 yr period, the nuclear continuum has varied by more than a factor of 7, and the H{beta} emission line has varied by a factor of nearly 6. The H{beta} emission line responds to continuum variations with a time delay or lag of {=~}10--20 days, the precise value varying somewhat from year to year. We find some indications that the lag varies with continuum flux in the sense that the lag is larger when the source is brighter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/659#2</TD>
            <TD>2011-09-14T18:59:29Z</TD>
            <TD>#AGN#Photometry#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/659</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/510/659&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/510/659</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/126 [1]</TD>
            <TD>MEGA-H proper motion catalog (Kharchenko, 2004)</TD>
            <TD>The catalogue MEGA-H is a result of a merging of star lists from the catalogue of stellar proper motions with respect to galaxies in 47 selected areas near the Main Meridional Section of the Galaxy (MEGA-G) (Kharchenko 1987) and from All-sky Compiled Catalogue of 2.5 Million Stars (ASCC-2.5) (Cat. &lt;I/280&gt;). Proper motions from the catalogue MEGA-G were reduced to the Hipparcos system by means of common with the ASCC-2.5 stars. The compiled proper motions in the Hipparcos system and their standard errors were computed as the weighted means. Equatorial coordinates are reduced to the equinox J2000 and epoch 1991.25. The catalogue MEGA-H contains 18169 stars. Stars are sorted in right ascension J2000 order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/126#1</TD>
            <TD>2011-09-14T19:45:37Z</TD>
            <TD>#Positional_Data#Stars#Photometry:wide-band#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/V/126</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/126</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/126</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/126 [2]</TD>
            <TD>MEGA-H proper motion catalog (Kharchenko, 2004)</TD>
            <TD>The catalogue MEGA-H is a result of a merging of star lists from the catalogue of stellar proper motions with respect to galaxies in 47 selected areas near the Main Meridional Section of the Galaxy (MEGA-G) (Kharchenko 1987) and from All-sky Compiled Catalogue of 2.5 Million Stars (ASCC-2.5) (Cat. &lt;I/280&gt;). Proper motions from the catalogue MEGA-G were reduced to the Hipparcos system by means of common with the ASCC-2.5 stars. The compiled proper motions in the Hipparcos system and their standard errors were computed as the weighted means. Equatorial coordinates are reduced to the equinox J2000 and epoch 1991.25. The catalogue MEGA-H contains 18169 stars. Stars are sorted in right ascension J2000 order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/126#2</TD>
            <TD>2011-09-14T19:45:37Z</TD>
            <TD>#Positional_Data#Stars#Photometry:wide-band#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/V/126</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/126&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/126</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/1329 [1]</TD>
            <TD>M82 X-ray sources long-term variability (Chiang+, 2011)</TD>
            <TD>Since the X-ray sources in the central region of M82 are crowded, a high spatial resolution instrument like the Chandra X-ray Observatory is needed to resolve the images. M82 has been observed 13 times between 1999 and 2007 with Chandra; some of them were designed to observe M82 X-1 with special configurations. To study the long-term variability of the whole galaxy, we used nine Chandra data sets with relatively long exposure time and large field of view from the Chandra Data Archive.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329#1</TD>
            <TD>2012-03-31T16:22:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/1329</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1329</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/1329 [2]</TD>
            <TD>M82 X-ray sources long-term variability (Chiang+, 2011)</TD>
            <TD>Since the X-ray sources in the central region of M82 are crowded, a high spatial resolution instrument like the Chandra X-ray Observatory is needed to resolve the images. M82 has been observed 13 times between 1999 and 2007 with Chandra; some of them were designed to observe M82 X-1 with special configurations. To study the long-term variability of the whole galaxy, we used nine Chandra data sets with relatively long exposure time and large field of view from the Chandra Data Archive.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329#2</TD>
            <TD>2012-03-31T16:22:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/1329&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1329</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/1329 [table2]</TD>
            <TD>M82 X-ray sources long-term variability (Chiang+, 2011)</TD>
            <TD>Since the X-ray sources in the central region of M82 are crowded, a high spatial resolution instrument like the Chandra X-ray Observatory is needed to resolve the images. M82 has been observed 13 times between 1999 and 2007 with Chandra; some of them were designed to observe M82 X-1 with special configurations. To study the long-term variability of the whole galaxy, we used nine Chandra data sets with relatively long exposure time and large field of view from the Chandra Data Archive.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329#table2</TD>
            <TD>2012-03-31T16:22:05Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1329</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/1329&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1329</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/510/659 [1]</TD>
            <TD>Size and Structure of AGN in NGC 5548 (Peterson+, 1999)</TD>
            <TD>We present the results of 3 yr of ground-based observations of the Seyfert 1 galaxy NGC 5548, which, combined with previously reported data, yield optical continuum and broad-line H{beta} light curves for a total of 8 yr. The light curves consist of over 800 points, with a typical spacing of a few days between observations. During this 8 yr period, the nuclear continuum has varied by more than a factor of 7, and the H{beta} emission line has varied by a factor of nearly 6. The H{beta} emission line responds to continuum variations with a time delay or lag of {=~}10--20 days, the precise value varying somewhat from year to year. We find some indications that the lag varies with continuum flux in the sense that the lag is larger when the source is brighter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/659#1</TD>
            <TD>2011-09-14T18:59:29Z</TD>
            <TD>#AGN#Photometry#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/659</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/510/659</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/510/659</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/510/659 [2]</TD>
            <TD>Size and Structure of AGN in NGC 5548 (Peterson+, 1999)</TD>
            <TD>We present the results of 3 yr of ground-based observations of the Seyfert 1 galaxy NGC 5548, which, combined with previously reported data, yield optical continuum and broad-line H{beta} light curves for a total of 8 yr. The light curves consist of over 800 points, with a typical spacing of a few days between observations. During this 8 yr period, the nuclear continuum has varied by more than a factor of 7, and the H{beta} emission line has varied by a factor of nearly 6. The H{beta} emission line responds to continuum variations with a time delay or lag of {=~}10--20 days, the precise value varying somewhat from year to year. We find some indications that the lag varies with continuum flux in the sense that the lag is larger when the source is brighter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/659#2</TD>
            <TD>2011-09-14T18:59:29Z</TD>
            <TD>#AGN#Photometry#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/510/659</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/510/659&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/510/659</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/511/65 [1]</TD>
            <TD>Einstein images of galaxy clusters (Jones &amp; Forman, 1999)</TD>
            <TD>We present the X-ray characteristics of a sample of 368 clusters of galaxies with redshifts less than 0.2 observed with the Einstein Imaging Proportional Counter. For each cluster, we measure the 0.5-4.5keV counting rate and compute the 0.5-4.5keV source luminosity, as well as the bolometric luminosity within fixed metric radii. We detect 85% of Abell clusters with z&lt;0.1, demonstrating that the large majority of these optically selected clusters are not the results of chance superpositions. For 163 clusters, we measure their X-ray surface brightness profiles and determine their core radii. For {~}230 clusters, we then use either our measured core radii and values, or mean values derived for this sample, to measure central gas densities and gas masses. We use estimated or measured cluster gas temperatures, along with the derived gas-density profiles, to estimate total cluster masses, under the assumptions that the gas is isothermal and in hydrostatic equilibrium.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65#1</TD>
            <TD>2011-09-14T18:59:33Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/511/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/511/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/511/65 [2]</TD>
            <TD>Einstein images of galaxy clusters (Jones &amp; Forman, 1999)</TD>
            <TD>We present the X-ray characteristics of a sample of 368 clusters of galaxies with redshifts less than 0.2 observed with the Einstein Imaging Proportional Counter. For each cluster, we measure the 0.5-4.5keV counting rate and compute the 0.5-4.5keV source luminosity, as well as the bolometric luminosity within fixed metric radii. We detect 85% of Abell clusters with z&lt;0.1, demonstrating that the large majority of these optically selected clusters are not the results of chance superpositions. For 163 clusters, we measure their X-ray surface brightness profiles and determine their core radii. For {~}230 clusters, we then use either our measured core radii and values, or mean values derived for this sample, to measure central gas densities and gas masses. We use estimated or measured cluster gas temperatures, along with the derived gas-density profiles, to estimate total cluster masses, under the assumptions that the gas is isothermal and in hydrostatic equilibrium.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65#2</TD>
            <TD>2011-09-14T18:59:33Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/511/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/511/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/511/65 [1]</TD>
            <TD>Einstein images of galaxy clusters (Jones &amp; Forman, 1999)</TD>
            <TD>We present the X-ray characteristics of a sample of 368 clusters of galaxies with redshifts less than 0.2 observed with the Einstein Imaging Proportional Counter. For each cluster, we measure the 0.5-4.5keV counting rate and compute the 0.5-4.5keV source luminosity, as well as the bolometric luminosity within fixed metric radii. We detect 85% of Abell clusters with z&lt;0.1, demonstrating that the large majority of these optically selected clusters are not the results of chance superpositions. For 163 clusters, we measure their X-ray surface brightness profiles and determine their core radii. For {~}230 clusters, we then use either our measured core radii and values, or mean values derived for this sample, to measure central gas densities and gas masses. We use estimated or measured cluster gas temperatures, along with the derived gas-density profiles, to estimate total cluster masses, under the assumptions that the gas is isothermal and in hydrostatic equilibrium.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65#1</TD>
            <TD>2011-09-14T18:59:33Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/511/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/511/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/511/65 [2]</TD>
            <TD>Einstein images of galaxy clusters (Jones &amp; Forman, 1999)</TD>
            <TD>We present the X-ray characteristics of a sample of 368 clusters of galaxies with redshifts less than 0.2 observed with the Einstein Imaging Proportional Counter. For each cluster, we measure the 0.5-4.5keV counting rate and compute the 0.5-4.5keV source luminosity, as well as the bolometric luminosity within fixed metric radii. We detect 85% of Abell clusters with z&lt;0.1, demonstrating that the large majority of these optically selected clusters are not the results of chance superpositions. For 163 clusters, we measure their X-ray surface brightness profiles and determine their core radii. For {~}230 clusters, we then use either our measured core radii and values, or mean values derived for this sample, to measure central gas densities and gas masses. We use estimated or measured cluster gas temperatures, along with the derived gas-density profiles, to estimate total cluster masses, under the assumptions that the gas is isothermal and in hydrostatic equilibrium.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65#2</TD>
            <TD>2011-09-14T18:59:33Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/511/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/511/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/511/65 [1]</TD>
            <TD>Einstein images of galaxy clusters (Jones &amp; Forman, 1999)</TD>
            <TD>We present the X-ray characteristics of a sample of 368 clusters of galaxies with redshifts less than 0.2 observed with the Einstein Imaging Proportional Counter. For each cluster, we measure the 0.5-4.5keV counting rate and compute the 0.5-4.5keV source luminosity, as well as the bolometric luminosity within fixed metric radii. We detect 85% of Abell clusters with z&lt;0.1, demonstrating that the large majority of these optically selected clusters are not the results of chance superpositions. For 163 clusters, we measure their X-ray surface brightness profiles and determine their core radii. For {~}230 clusters, we then use either our measured core radii and values, or mean values derived for this sample, to measure central gas densities and gas masses. We use estimated or measured cluster gas temperatures, along with the derived gas-density profiles, to estimate total cluster masses, under the assumptions that the gas is isothermal and in hydrostatic equilibrium.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65#1</TD>
            <TD>2011-09-14T18:59:33Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/511/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/511/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/511/65 [2]</TD>
            <TD>Einstein images of galaxy clusters (Jones &amp; Forman, 1999)</TD>
            <TD>We present the X-ray characteristics of a sample of 368 clusters of galaxies with redshifts less than 0.2 observed with the Einstein Imaging Proportional Counter. For each cluster, we measure the 0.5-4.5keV counting rate and compute the 0.5-4.5keV source luminosity, as well as the bolometric luminosity within fixed metric radii. We detect 85% of Abell clusters with z&lt;0.1, demonstrating that the large majority of these optically selected clusters are not the results of chance superpositions. For 163 clusters, we measure their X-ray surface brightness profiles and determine their core radii. For {~}230 clusters, we then use either our measured core radii and values, or mean values derived for this sample, to measure central gas densities and gas masses. We use estimated or measured cluster gas temperatures, along with the derived gas-density profiles, to estimate total cluster masses, under the assumptions that the gas is isothermal and in hydrostatic equilibrium.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65#2</TD>
            <TD>2011-09-14T18:59:33Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/511/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/511/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/511/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/521/577 [1]</TD>
            <TD>HST studies of the WLM globular cluster (Hodge+, 1999)</TD>
            <TD>As part of a Cycle 6 HST GO program, we obtained four images of the WLM globular cluster on 1998 September 26. There were two exposures taken with the F814W filter of 2700 s and two with the F555W filter, one each of 2700 and 2600 s. The globular cluster was centered on the PC chip and the orientation of the camera was such that the WF chips lay approximately along the galaxy's minor axis. Photometry was then carried out using a program specifically designed to reduce undersampled WFPC2 data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/521/577#1</TD>
            <TD>2011-09-14T19:00:04Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/521/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/521/577</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/521/577</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/521/577 [2]</TD>
            <TD>HST studies of the WLM globular cluster (Hodge+, 1999)</TD>
            <TD>As part of a Cycle 6 HST GO program, we obtained four images of the WLM globular cluster on 1998 September 26. There were two exposures taken with the F814W filter of 2700 s and two with the F555W filter, one each of 2700 and 2600 s. The globular cluster was centered on the PC chip and the orientation of the camera was such that the WF chips lay approximately along the galaxy's minor axis. Photometry was then carried out using a program specifically designed to reduce undersampled WFPC2 data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/521/577#2</TD>
            <TD>2011-09-14T19:00:04Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/521/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/521/577&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/521/577</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/521/577 [1]</TD>
            <TD>HST studies of the WLM globular cluster (Hodge+, 1999)</TD>
            <TD>As part of a Cycle 6 HST GO program, we obtained four images of the WLM globular cluster on 1998 September 26. There were two exposures taken with the F814W filter of 2700 s and two with the F555W filter, one each of 2700 and 2600 s. The globular cluster was centered on the PC chip and the orientation of the camera was such that the WF chips lay approximately along the galaxy's minor axis. Photometry was then carried out using a program specifically designed to reduce undersampled WFPC2 data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/521/577#1</TD>
            <TD>2011-09-14T19:00:04Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/521/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/521/577</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/521/577</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/521/577 [2]</TD>
            <TD>HST studies of the WLM globular cluster (Hodge+, 1999)</TD>
            <TD>As part of a Cycle 6 HST GO program, we obtained four images of the WLM globular cluster on 1998 September 26. There were two exposures taken with the F814W filter of 2700 s and two with the F555W filter, one each of 2700 and 2600 s. The globular cluster was centered on the PC chip and the orientation of the camera was such that the WF chips lay approximately along the galaxy's minor axis. Photometry was then carried out using a program specifically designed to reduce undersampled WFPC2 data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/521/577#2</TD>
            <TD>2011-09-14T19:00:04Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/521/577</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/521/577&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/521/577</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/287/472 [1]</TD>
            <TD>Southern Milky Way galaxies velocities (Di Nella+ 1997)</TD>
            <TD>A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (&lt;http://www-obs.univ-lyon1.fr/base/&gt;) and COSMOS (Cat. &lt;J/A+AS/117/519&gt;) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5&lt;B_J_&lt;17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472#1</TD>
            <TD>2011-09-14T19:00:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/287/472</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/472</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/287/472 [2]</TD>
            <TD>Southern Milky Way galaxies velocities (Di Nella+ 1997)</TD>
            <TD>A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (&lt;http://www-obs.univ-lyon1.fr/base/&gt;) and COSMOS (Cat. &lt;J/A+AS/117/519&gt;) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5&lt;B_J_&lt;17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472#2</TD>
            <TD>2011-09-14T19:00:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/287/472&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/472</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/287/472 [table3]</TD>
            <TD>Southern Milky Way galaxies velocities (Di Nella+ 1997)</TD>
            <TD>A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (&lt;http://www-obs.univ-lyon1.fr/base/&gt;) and COSMOS (Cat. &lt;J/A+AS/117/519&gt;) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5&lt;B_J_&lt;17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472#table3</TD>
            <TD>2011-09-14T19:00:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/287/472&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/472</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/287/472 [1]</TD>
            <TD>Southern Milky Way galaxies velocities (Di Nella+ 1997)</TD>
            <TD>A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (&lt;http://www-obs.univ-lyon1.fr/base/&gt;) and COSMOS (Cat. &lt;J/A+AS/117/519&gt;) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5&lt;B_J_&lt;17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472#1</TD>
            <TD>2011-09-14T19:00:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/287/472</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/472</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/287/472 [2]</TD>
            <TD>Southern Milky Way galaxies velocities (Di Nella+ 1997)</TD>
            <TD>A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (&lt;http://www-obs.univ-lyon1.fr/base/&gt;) and COSMOS (Cat. &lt;J/A+AS/117/519&gt;) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5&lt;B_J_&lt;17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472#2</TD>
            <TD>2011-09-14T19:00:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/287/472&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/472</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/287/472 [table3]</TD>
            <TD>Southern Milky Way galaxies velocities (Di Nella+ 1997)</TD>
            <TD>A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (&lt;http://www-obs.univ-lyon1.fr/base/&gt;) and COSMOS (Cat. &lt;J/A+AS/117/519&gt;) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5&lt;B_J_&lt;17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472#table3</TD>
            <TD>2011-09-14T19:00:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/287/472&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/472</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/287/472 [1]</TD>
            <TD>Southern Milky Way galaxies velocities (Di Nella+ 1997)</TD>
            <TD>A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (&lt;http://www-obs.univ-lyon1.fr/base/&gt;) and COSMOS (Cat. &lt;J/A+AS/117/519&gt;) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5&lt;B_J_&lt;17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472#1</TD>
            <TD>2011-09-14T19:00:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/287/472</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/472</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/287/472 [2]</TD>
            <TD>Southern Milky Way galaxies velocities (Di Nella+ 1997)</TD>
            <TD>A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (&lt;http://www-obs.univ-lyon1.fr/base/&gt;) and COSMOS (Cat. &lt;J/A+AS/117/519&gt;) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5&lt;B_J_&lt;17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472#2</TD>
            <TD>2011-09-14T19:00:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/287/472&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/472</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/287/472 [table3]</TD>
            <TD>Southern Milky Way galaxies velocities (Di Nella+ 1997)</TD>
            <TD>A redshift survey of galaxies located in the direction of the southern Milky Way has been carried out using the FLAIR multi-objects system on the 1.2-m UK Schmidt Telescope (UKST) at the Anglo-Australian Observatory in Australia. The galaxy sample was extracted from the LEDA (&lt;http://www-obs.univ-lyon1.fr/base/&gt;) and COSMOS (Cat. &lt;J/A+AS/117/519&gt;) data bases but essentially by scanning by eye four plates of the UKST/SERC Survey in the region between the Centaurus complex and the Pavo-Indus (PI) wall. The galaxies selected have high central surface brightnesses and are distributed evenly over the whole search area. The majority of the galaxies have apparent magnitudes in the range 11.5&lt;B_J_&lt;17. Redshifts were determined for 211 galaxies with one additional object being found to be Galactic - a planetary nebula. A highly significant density enhancement is found in the galaxy distribution at 5000km/s or 67Mpc (H_0_=75km/s/Mpc). This suggests that a connection exists between the Centaurus complex and the PI wall across the zone of avoidance (ZOA) associated with the Milky Way and as such could be one of the larger structures in the nearby Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472#table3</TD>
            <TD>2011-09-14T19:00:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/287/472</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/287/472&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/287/472</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/527/199 [1]</TD>
            <TD>HST observations of old clusters in the LMC (Johnson+, 1999)</TD>
            <TD>We present V, V-I color-magnitude diagrams (CMDs) for three old star clusters in the Large Magellanic Cloud (LMC): NGC 1466, NGC 2257, and Hodge 11. Our data extend {~}3 mag below the main-sequence turnoff, allowing us to determine accurate relative ages and the blue straggler frequencies. Based on a differential comparison of the CMDs, any age difference between the three LMC clusters is less than 1.5 Gyr. Comparing their CMDs to those of M92 and M3, the LMC clusters, unless their published metallicities are significantly in error, are the same age as the old Galactic globulars. The similar ages to Galactic globulars are shown to be consistent with hierarchical clustering models of galaxy formation. The blue straggler frequencies are also similar to those of Galactic globular clusters. We derive a true distance modulus to the LMC of (m - M)_0_ = 18.46 {+/-} 0.09 [assuming (m - M)_0_ = 14.61 for M92] using these three LMC clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/527/199#1</TD>
            <TD>2011-09-14T19:00:11Z</TD>
            <TD>#Globular_Clusters#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/527/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/527/199</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/527/199</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/527/199 [2]</TD>
            <TD>HST observations of old clusters in the LMC (Johnson+, 1999)</TD>
            <TD>We present V, V-I color-magnitude diagrams (CMDs) for three old star clusters in the Large Magellanic Cloud (LMC): NGC 1466, NGC 2257, and Hodge 11. Our data extend {~}3 mag below the main-sequence turnoff, allowing us to determine accurate relative ages and the blue straggler frequencies. Based on a differential comparison of the CMDs, any age difference between the three LMC clusters is less than 1.5 Gyr. Comparing their CMDs to those of M92 and M3, the LMC clusters, unless their published metallicities are significantly in error, are the same age as the old Galactic globulars. The similar ages to Galactic globulars are shown to be consistent with hierarchical clustering models of galaxy formation. The blue straggler frequencies are also similar to those of Galactic globular clusters. We derive a true distance modulus to the LMC of (m - M)_0_ = 18.46 {+/-} 0.09 [assuming (m - M)_0_ = 14.61 for M92] using these three LMC clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/527/199#2</TD>
            <TD>2011-09-14T19:00:11Z</TD>
            <TD>#Globular_Clusters#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/527/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/527/199&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/527/199</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/527/199 [1]</TD>
            <TD>HST observations of old clusters in the LMC (Johnson+, 1999)</TD>
            <TD>We present V, V-I color-magnitude diagrams (CMDs) for three old star clusters in the Large Magellanic Cloud (LMC): NGC 1466, NGC 2257, and Hodge 11. Our data extend {~}3 mag below the main-sequence turnoff, allowing us to determine accurate relative ages and the blue straggler frequencies. Based on a differential comparison of the CMDs, any age difference between the three LMC clusters is less than 1.5 Gyr. Comparing their CMDs to those of M92 and M3, the LMC clusters, unless their published metallicities are significantly in error, are the same age as the old Galactic globulars. The similar ages to Galactic globulars are shown to be consistent with hierarchical clustering models of galaxy formation. The blue straggler frequencies are also similar to those of Galactic globular clusters. We derive a true distance modulus to the LMC of (m - M)_0_ = 18.46 {+/-} 0.09 [assuming (m - M)_0_ = 14.61 for M92] using these three LMC clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/527/199#1</TD>
            <TD>2011-09-14T19:00:11Z</TD>
            <TD>#Globular_Clusters#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/527/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/527/199</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/527/199</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/527/199 [2]</TD>
            <TD>HST observations of old clusters in the LMC (Johnson+, 1999)</TD>
            <TD>We present V, V-I color-magnitude diagrams (CMDs) for three old star clusters in the Large Magellanic Cloud (LMC): NGC 1466, NGC 2257, and Hodge 11. Our data extend {~}3 mag below the main-sequence turnoff, allowing us to determine accurate relative ages and the blue straggler frequencies. Based on a differential comparison of the CMDs, any age difference between the three LMC clusters is less than 1.5 Gyr. Comparing their CMDs to those of M92 and M3, the LMC clusters, unless their published metallicities are significantly in error, are the same age as the old Galactic globulars. The similar ages to Galactic globulars are shown to be consistent with hierarchical clustering models of galaxy formation. The blue straggler frequencies are also similar to those of Galactic globular clusters. We derive a true distance modulus to the LMC of (m - M)_0_ = 18.46 {+/-} 0.09 [assuming (m - M)_0_ = 14.61 for M92] using these three LMC clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/527/199#2</TD>
            <TD>2011-09-14T19:00:11Z</TD>
            <TD>#Globular_Clusters#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/527/199</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/527/199&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/527/199</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/417 [1]</TD>
            <TD>Hamburg/SAO Survey for ELGs. III. (Hopp+, 2000)</TD>
            <TD>We present the third list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia). This survey is based on the digitized objective-prism photoplate database of the Hamburg Quasar Survey (HQS). Here, we present new spectroscopic results of candidates which were obtained in 1998 with the 2.1m KPNO and the 2.2m Calar Alto telescopes. All candidates are selected in the declination band +35{deg} to +40{deg}. The follow-up spectroscopy with the 2m class telescopes confirmed 85 emission-line objects out of 113 observed candidates and allowed their quantitative spectral classification. For 80 of them, the redshifts are determined for the first time. For 5 previously known Emission-Line Galaxies (ELGs), line ratios are presented for the first time. We could classify 55 out of the 85 emission-line objects as BCG/HII galaxies or probable BCGs (Blue Compact Galaxies) , 4 - as QSOs, 6 - as Seyfert galaxies, 1 - as super-association in a subluminous spiral galaxy, and 11 are low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 8 ELGs. Further, for 8 more galaxies we did not detect any significant emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417#1</TD>
            <TD>2011-09-14T19:00:13Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/417</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/417</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/417 [2]</TD>
            <TD>Hamburg/SAO Survey for ELGs. III. (Hopp+, 2000)</TD>
            <TD>We present the third list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia). This survey is based on the digitized objective-prism photoplate database of the Hamburg Quasar Survey (HQS). Here, we present new spectroscopic results of candidates which were obtained in 1998 with the 2.1m KPNO and the 2.2m Calar Alto telescopes. All candidates are selected in the declination band +35{deg} to +40{deg}. The follow-up spectroscopy with the 2m class telescopes confirmed 85 emission-line objects out of 113 observed candidates and allowed their quantitative spectral classification. For 80 of them, the redshifts are determined for the first time. For 5 previously known Emission-Line Galaxies (ELGs), line ratios are presented for the first time. We could classify 55 out of the 85 emission-line objects as BCG/HII galaxies or probable BCGs (Blue Compact Galaxies) , 4 - as QSOs, 6 - as Seyfert galaxies, 1 - as super-association in a subluminous spiral galaxy, and 11 are low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 8 ELGs. Further, for 8 more galaxies we did not detect any significant emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417#2</TD>
            <TD>2011-09-14T19:00:13Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/417&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/417</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/417 [1]</TD>
            <TD>Hamburg/SAO Survey for ELGs. III. (Hopp+, 2000)</TD>
            <TD>We present the third list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia). This survey is based on the digitized objective-prism photoplate database of the Hamburg Quasar Survey (HQS). Here, we present new spectroscopic results of candidates which were obtained in 1998 with the 2.1m KPNO and the 2.2m Calar Alto telescopes. All candidates are selected in the declination band +35{deg} to +40{deg}. The follow-up spectroscopy with the 2m class telescopes confirmed 85 emission-line objects out of 113 observed candidates and allowed their quantitative spectral classification. For 80 of them, the redshifts are determined for the first time. For 5 previously known Emission-Line Galaxies (ELGs), line ratios are presented for the first time. We could classify 55 out of the 85 emission-line objects as BCG/HII galaxies or probable BCGs (Blue Compact Galaxies) , 4 - as QSOs, 6 - as Seyfert galaxies, 1 - as super-association in a subluminous spiral galaxy, and 11 are low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 8 ELGs. Further, for 8 more galaxies we did not detect any significant emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417#1</TD>
            <TD>2011-09-14T19:00:13Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/417</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/417</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/417 [2]</TD>
            <TD>Hamburg/SAO Survey for ELGs. III. (Hopp+, 2000)</TD>
            <TD>We present the third list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia). This survey is based on the digitized objective-prism photoplate database of the Hamburg Quasar Survey (HQS). Here, we present new spectroscopic results of candidates which were obtained in 1998 with the 2.1m KPNO and the 2.2m Calar Alto telescopes. All candidates are selected in the declination band +35{deg} to +40{deg}. The follow-up spectroscopy with the 2m class telescopes confirmed 85 emission-line objects out of 113 observed candidates and allowed their quantitative spectral classification. For 80 of them, the redshifts are determined for the first time. For 5 previously known Emission-Line Galaxies (ELGs), line ratios are presented for the first time. We could classify 55 out of the 85 emission-line objects as BCG/HII galaxies or probable BCGs (Blue Compact Galaxies) , 4 - as QSOs, 6 - as Seyfert galaxies, 1 - as super-association in a subluminous spiral galaxy, and 11 are low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 8 ELGs. Further, for 8 more galaxies we did not detect any significant emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417#2</TD>
            <TD>2011-09-14T19:00:13Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/417&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/417</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/126 [1]</TD>
            <TD>MEGA-H proper motion catalog (Kharchenko, 2004)</TD>
            <TD>The catalogue MEGA-H is a result of a merging of star lists from the catalogue of stellar proper motions with respect to galaxies in 47 selected areas near the Main Meridional Section of the Galaxy (MEGA-G) (Kharchenko 1987) and from All-sky Compiled Catalogue of 2.5 Million Stars (ASCC-2.5) (Cat. &lt;I/280&gt;). Proper motions from the catalogue MEGA-G were reduced to the Hipparcos system by means of common with the ASCC-2.5 stars. The compiled proper motions in the Hipparcos system and their standard errors were computed as the weighted means. Equatorial coordinates are reduced to the equinox J2000 and epoch 1991.25. The catalogue MEGA-H contains 18169 stars. Stars are sorted in right ascension J2000 order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/126#1</TD>
            <TD>2011-09-14T19:45:37Z</TD>
            <TD>#Positional_Data#Stars#Photometry:wide-band#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/V/126</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/126</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/126</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/126 [2]</TD>
            <TD>MEGA-H proper motion catalog (Kharchenko, 2004)</TD>
            <TD>The catalogue MEGA-H is a result of a merging of star lists from the catalogue of stellar proper motions with respect to galaxies in 47 selected areas near the Main Meridional Section of the Galaxy (MEGA-G) (Kharchenko 1987) and from All-sky Compiled Catalogue of 2.5 Million Stars (ASCC-2.5) (Cat. &lt;I/280&gt;). Proper motions from the catalogue MEGA-G were reduced to the Hipparcos system by means of common with the ASCC-2.5 stars. The compiled proper motions in the Hipparcos system and their standard errors were computed as the weighted means. Equatorial coordinates are reduced to the equinox J2000 and epoch 1991.25. The catalogue MEGA-H contains 18169 stars. Stars are sorted in right ascension J2000 order.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/126#2</TD>
            <TD>2011-09-14T19:45:37Z</TD>
            <TD>#Positional_Data#Stars#Photometry:wide-band#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/V/126</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/126&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/126</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/417 [1]</TD>
            <TD>Hamburg/SAO Survey for ELGs. III. (Hopp+, 2000)</TD>
            <TD>We present the third list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia). This survey is based on the digitized objective-prism photoplate database of the Hamburg Quasar Survey (HQS). Here, we present new spectroscopic results of candidates which were obtained in 1998 with the 2.1m KPNO and the 2.2m Calar Alto telescopes. All candidates are selected in the declination band +35{deg} to +40{deg}. The follow-up spectroscopy with the 2m class telescopes confirmed 85 emission-line objects out of 113 observed candidates and allowed their quantitative spectral classification. For 80 of them, the redshifts are determined for the first time. For 5 previously known Emission-Line Galaxies (ELGs), line ratios are presented for the first time. We could classify 55 out of the 85 emission-line objects as BCG/HII galaxies or probable BCGs (Blue Compact Galaxies) , 4 - as QSOs, 6 - as Seyfert galaxies, 1 - as super-association in a subluminous spiral galaxy, and 11 are low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 8 ELGs. Further, for 8 more galaxies we did not detect any significant emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417#1</TD>
            <TD>2011-09-14T19:00:13Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/417</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/417</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/417 [2]</TD>
            <TD>Hamburg/SAO Survey for ELGs. III. (Hopp+, 2000)</TD>
            <TD>We present the third list with results of the Hamburg/SAO Survey for Emission-Line Galaxies (HSS therein, SAO - Special Astrophysical Observatory, Russia). This survey is based on the digitized objective-prism photoplate database of the Hamburg Quasar Survey (HQS). Here, we present new spectroscopic results of candidates which were obtained in 1998 with the 2.1m KPNO and the 2.2m Calar Alto telescopes. All candidates are selected in the declination band +35{deg} to +40{deg}. The follow-up spectroscopy with the 2m class telescopes confirmed 85 emission-line objects out of 113 observed candidates and allowed their quantitative spectral classification. For 80 of them, the redshifts are determined for the first time. For 5 previously known Emission-Line Galaxies (ELGs), line ratios are presented for the first time. We could classify 55 out of the 85 emission-line objects as BCG/HII galaxies or probable BCGs (Blue Compact Galaxies) , 4 - as QSOs, 6 - as Seyfert galaxies, 1 - as super-association in a subluminous spiral galaxy, and 11 are low-excitation objects - either starburst nuclei (SBN), or dwarf amorphous nuclei starburst galaxies (DANS). We could not classify 8 ELGs. Further, for 8 more galaxies we did not detect any significant emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417#2</TD>
            <TD>2011-09-14T19:00:13Z</TD>
            <TD>#Galaxies:spectra#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/417</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/417&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/417</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/268/419 [1]</TD>
            <TD>HII Regions in NGC 4258 (Courtes+ 1993)</TD>
            <TD>The distribution of ionized hydrogen in the spiral galaxy NGC 4258 is revisited using Halpha images with both the Mont Megantic 160cm telescope equipped with a F/3 focal reducer and the Observatoire de Haute-Provence 120cm telescope at its newtonian F/6 focus in the direct imaging mode. The HII region distribution shows several well defined spiral structures as well as the very extended and peculiar "anomalous arms". The deprojection of these features is compared to the UV 2000A stellar arms obtained with the LAS- Geneva Observatory balloon-borne survey programme. The pitch angle of the N inner arm permits to detect the drift of the Halpha spiral structures with respect to the evolved hot stellar population in the corresponding sector of the UV arm. This phenomenon seems to systematically appear in other galaxies. The conclusion should be that the origin of the drift is mainly kinematic and of evolutionary nature and provides perhaps the best method to evaluate the effect of the density waves. The anomalous arms have no apparent UV 2000A counterpart except perhaps in the inner region of the central stellar bulge. A comparison of the Halpha morphology is made with the CO distribution and their radial velocity profiles that could renew the ballistic interpretation. A catalogue of 137 HII regions was compiled from the two sets of new CCD images, providing the X and Y off-set positions, along with the absolute flux and angular diameters corrected for observing conditions. The 1950 equatorial coordinates are given in the maps of our Halpha observations. The derived power-law luminosity function is compared to those obtained for other galaxies. Comparing previous image-tube plates, taken between 1961 and 1969, to the recent CCD data for NGC 4258, we obtain flux estimates of the HII region hosting the supernova first discovered in radio frequencies on 1983. As a result, the integrated magnitude is in fair agreement with the report by Wild (IAU Circ 3803, 1983) of a 17th mag object in the same location.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/268/419#1</TD>
            <TD>2011-09-14T18:49:10Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/268/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/268/419</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/268/419</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/268/419 [2]</TD>
            <TD>HII Regions in NGC 4258 (Courtes+ 1993)</TD>
            <TD>The distribution of ionized hydrogen in the spiral galaxy NGC 4258 is revisited using Halpha images with both the Mont Megantic 160cm telescope equipped with a F/3 focal reducer and the Observatoire de Haute-Provence 120cm telescope at its newtonian F/6 focus in the direct imaging mode. The HII region distribution shows several well defined spiral structures as well as the very extended and peculiar "anomalous arms". The deprojection of these features is compared to the UV 2000A stellar arms obtained with the LAS- Geneva Observatory balloon-borne survey programme. The pitch angle of the N inner arm permits to detect the drift of the Halpha spiral structures with respect to the evolved hot stellar population in the corresponding sector of the UV arm. This phenomenon seems to systematically appear in other galaxies. The conclusion should be that the origin of the drift is mainly kinematic and of evolutionary nature and provides perhaps the best method to evaluate the effect of the density waves. The anomalous arms have no apparent UV 2000A counterpart except perhaps in the inner region of the central stellar bulge. A comparison of the Halpha morphology is made with the CO distribution and their radial velocity profiles that could renew the ballistic interpretation. A catalogue of 137 HII regions was compiled from the two sets of new CCD images, providing the X and Y off-set positions, along with the absolute flux and angular diameters corrected for observing conditions. The 1950 equatorial coordinates are given in the maps of our Halpha observations. The derived power-law luminosity function is compared to those obtained for other galaxies. Comparing previous image-tube plates, taken between 1961 and 1969, to the recent CCD data for NGC 4258, we obtain flux estimates of the HII region hosting the supernova first discovered in radio frequencies on 1983. As a result, the integrated magnitude is in fair agreement with the report by Wild (IAU Circ 3803, 1983) of a 17th mag object in the same location.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/268/419#2</TD>
            <TD>2011-09-14T18:49:10Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/268/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/268/419&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/268/419</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/366/68 [1]</TD>
            <TD>Spectrophotometric indices from galaxy bulges (Prugniel+, 2001)</TD>
            <TD>We have measured Mg_2_, Fe5270 and Fe5335 spectrophotometric indices (LICK system) in the bulge of 89 galaxies, mostly spirals from the Heraudeau sample. The indices are reduced to a null velocity dispersion and normalized to an aperture of 0.2h^-1^kpc. The mean errors are 0.009 mag on Mg_2_, and 0.3{AA} on the iron indices. These measurements almost double the amount of similar data already available on spiral galaxies. Our data confirm the existence of the relation between Mg_2_ and sigma_0_, the central stellar velocity dispersion; and we find an even tighter relation between Mg_2_ and Vmaxrot, the maximum rotational velocity of the galaxy, deduced from HI observations. For the most massive bulges these correlations may be interpreted as a mass-metallicity relation. However, the presence of young stellar populations, traced by the detection of [OIII]{lambda}500.7nm emission, provides a clear evidence that age effects play a role. Since the contribution of the young population is anti-correlated with the mass of the galaxy, it continues the Mg_2_ vs. sigma_0_ relation toward the low sigma_0_ and globally increases its slope. We present also evidence for a new positive correlation between Fe indices and sigma_0_ and for a significant correlation between the line strength indices and the total or disk luminosity. We propose to model the whole sequence of bulges within the following framework: Bulges are composed of a primary population formed prior to the disk during the initial collapse and a secondary population formed along the evolution. The whole family of bulges can be classified in three classes: (A) The bulges dominated by a young population are generally small, have ionized gas, low velocity dispersion and low line strengths. (B) The bulges dominated by the primary population lie along the mass metallicity sequence defined for elliptical galaxies. (C) The bulges where the secondary population is significant are less Mg-overabundant than B-type bulges and deviate from the Mg_2_ vs. sigma_0_ relation of elliptical galaxies. The original data are available in Hypercat: http://www-obs.univ-lyon1.fr/hypercat The tables of measurements and the extracted 1D spectra are also available in the present archive set.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68#1</TD>
            <TD>2011-09-14T19:46:49Z</TD>
            <TD>#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/366/68</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/68</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/366/68 [2]</TD>
            <TD>Spectrophotometric indices from galaxy bulges (Prugniel+, 2001)</TD>
            <TD>We have measured Mg_2_, Fe5270 and Fe5335 spectrophotometric indices (LICK system) in the bulge of 89 galaxies, mostly spirals from the Heraudeau sample. The indices are reduced to a null velocity dispersion and normalized to an aperture of 0.2h^-1^kpc. The mean errors are 0.009 mag on Mg_2_, and 0.3{AA} on the iron indices. These measurements almost double the amount of similar data already available on spiral galaxies. Our data confirm the existence of the relation between Mg_2_ and sigma_0_, the central stellar velocity dispersion; and we find an even tighter relation between Mg_2_ and Vmaxrot, the maximum rotational velocity of the galaxy, deduced from HI observations. For the most massive bulges these correlations may be interpreted as a mass-metallicity relation. However, the presence of young stellar populations, traced by the detection of [OIII]{lambda}500.7nm emission, provides a clear evidence that age effects play a role. Since the contribution of the young population is anti-correlated with the mass of the galaxy, it continues the Mg_2_ vs. sigma_0_ relation toward the low sigma_0_ and globally increases its slope. We present also evidence for a new positive correlation between Fe indices and sigma_0_ and for a significant correlation between the line strength indices and the total or disk luminosity. We propose to model the whole sequence of bulges within the following framework: Bulges are composed of a primary population formed prior to the disk during the initial collapse and a secondary population formed along the evolution. The whole family of bulges can be classified in three classes: (A) The bulges dominated by a young population are generally small, have ionized gas, low velocity dispersion and low line strengths. (B) The bulges dominated by the primary population lie along the mass metallicity sequence defined for elliptical galaxies. (C) The bulges where the secondary population is significant are less Mg-overabundant than B-type bulges and deviate from the Mg_2_ vs. sigma_0_ relation of elliptical galaxies. The original data are available in Hypercat: http://www-obs.univ-lyon1.fr/hypercat The tables of measurements and the extracted 1D spectra are also available in the present archive set.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68#2</TD>
            <TD>2011-09-14T19:46:49Z</TD>
            <TD>#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/366/68&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/68</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/522/802 [1]</TD>
            <TD>Cepheid calibration of SN 1989B in NGC 3627 (Saha+, 1999)</TD>
            <TD>Repeated imaging observations have been made of NGC 3627 with the Hubble Space Telescope in 1997 - 1998 over an interval of 58 days. Images were obtained on 12 epochs in the F555W band and on five epochs in the F814W band. The galaxy hosted the prototypical, "Branch normal," type Ia supernova SN 1989B. A total of 83 variables have been found, of which 68 are definite Cepheid variables with periods ranging from 75 to 3.85 days. The dereddened distance modulus is determined to be (m-M)_o_=30.22{+/-}0.12 (internal uncertainty) using a subset of the Cepheid data whose reddening and error parameters are secure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/522/802#1</TD>
            <TD>2011-09-14T19:00:20Z</TD>
            <TD>#Photometry#Stars:variable#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/522/802</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/522/802</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/522/802</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/522/802 [2]</TD>
            <TD>Cepheid calibration of SN 1989B in NGC 3627 (Saha+, 1999)</TD>
            <TD>Repeated imaging observations have been made of NGC 3627 with the Hubble Space Telescope in 1997 - 1998 over an interval of 58 days. Images were obtained on 12 epochs in the F555W band and on five epochs in the F814W band. The galaxy hosted the prototypical, "Branch normal," type Ia supernova SN 1989B. A total of 83 variables have been found, of which 68 are definite Cepheid variables with periods ranging from 75 to 3.85 days. The dereddened distance modulus is determined to be (m-M)_o_=30.22{+/-}0.12 (internal uncertainty) using a subset of the Cepheid data whose reddening and error parameters are secure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/522/802#2</TD>
            <TD>2011-09-14T19:00:20Z</TD>
            <TD>#Photometry#Stars:variable#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/522/802</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/522/802&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/522/802</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/268/419 [1]</TD>
            <TD>HII Regions in NGC 4258 (Courtes+ 1993)</TD>
            <TD>The distribution of ionized hydrogen in the spiral galaxy NGC 4258 is revisited using Halpha images with both the Mont Megantic 160cm telescope equipped with a F/3 focal reducer and the Observatoire de Haute-Provence 120cm telescope at its newtonian F/6 focus in the direct imaging mode. The HII region distribution shows several well defined spiral structures as well as the very extended and peculiar "anomalous arms". The deprojection of these features is compared to the UV 2000A stellar arms obtained with the LAS- Geneva Observatory balloon-borne survey programme. The pitch angle of the N inner arm permits to detect the drift of the Halpha spiral structures with respect to the evolved hot stellar population in the corresponding sector of the UV arm. This phenomenon seems to systematically appear in other galaxies. The conclusion should be that the origin of the drift is mainly kinematic and of evolutionary nature and provides perhaps the best method to evaluate the effect of the density waves. The anomalous arms have no apparent UV 2000A counterpart except perhaps in the inner region of the central stellar bulge. A comparison of the Halpha morphology is made with the CO distribution and their radial velocity profiles that could renew the ballistic interpretation. A catalogue of 137 HII regions was compiled from the two sets of new CCD images, providing the X and Y off-set positions, along with the absolute flux and angular diameters corrected for observing conditions. The 1950 equatorial coordinates are given in the maps of our Halpha observations. The derived power-law luminosity function is compared to those obtained for other galaxies. Comparing previous image-tube plates, taken between 1961 and 1969, to the recent CCD data for NGC 4258, we obtain flux estimates of the HII region hosting the supernova first discovered in radio frequencies on 1983. As a result, the integrated magnitude is in fair agreement with the report by Wild (IAU Circ 3803, 1983) of a 17th mag object in the same location.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/268/419#1</TD>
            <TD>2011-09-14T18:49:10Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/268/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/268/419</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/268/419</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/268/419 [2]</TD>
            <TD>HII Regions in NGC 4258 (Courtes+ 1993)</TD>
            <TD>The distribution of ionized hydrogen in the spiral galaxy NGC 4258 is revisited using Halpha images with both the Mont Megantic 160cm telescope equipped with a F/3 focal reducer and the Observatoire de Haute-Provence 120cm telescope at its newtonian F/6 focus in the direct imaging mode. The HII region distribution shows several well defined spiral structures as well as the very extended and peculiar "anomalous arms". The deprojection of these features is compared to the UV 2000A stellar arms obtained with the LAS- Geneva Observatory balloon-borne survey programme. The pitch angle of the N inner arm permits to detect the drift of the Halpha spiral structures with respect to the evolved hot stellar population in the corresponding sector of the UV arm. This phenomenon seems to systematically appear in other galaxies. The conclusion should be that the origin of the drift is mainly kinematic and of evolutionary nature and provides perhaps the best method to evaluate the effect of the density waves. The anomalous arms have no apparent UV 2000A counterpart except perhaps in the inner region of the central stellar bulge. A comparison of the Halpha morphology is made with the CO distribution and their radial velocity profiles that could renew the ballistic interpretation. A catalogue of 137 HII regions was compiled from the two sets of new CCD images, providing the X and Y off-set positions, along with the absolute flux and angular diameters corrected for observing conditions. The 1950 equatorial coordinates are given in the maps of our Halpha observations. The derived power-law luminosity function is compared to those obtained for other galaxies. Comparing previous image-tube plates, taken between 1961 and 1969, to the recent CCD data for NGC 4258, we obtain flux estimates of the HII region hosting the supernova first discovered in radio frequencies on 1983. As a result, the integrated magnitude is in fair agreement with the report by Wild (IAU Circ 3803, 1983) of a 17th mag object in the same location.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/268/419#2</TD>
            <TD>2011-09-14T18:49:10Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/268/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/268/419&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/268/419</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/522/802 [1]</TD>
            <TD>Cepheid calibration of SN 1989B in NGC 3627 (Saha+, 1999)</TD>
            <TD>Repeated imaging observations have been made of NGC 3627 with the Hubble Space Telescope in 1997 - 1998 over an interval of 58 days. Images were obtained on 12 epochs in the F555W band and on five epochs in the F814W band. The galaxy hosted the prototypical, "Branch normal," type Ia supernova SN 1989B. A total of 83 variables have been found, of which 68 are definite Cepheid variables with periods ranging from 75 to 3.85 days. The dereddened distance modulus is determined to be (m-M)_o_=30.22{+/-}0.12 (internal uncertainty) using a subset of the Cepheid data whose reddening and error parameters are secure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/522/802#1</TD>
            <TD>2011-09-14T19:00:20Z</TD>
            <TD>#Photometry#Stars:variable#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/522/802</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/522/802</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/522/802</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/522/802 [2]</TD>
            <TD>Cepheid calibration of SN 1989B in NGC 3627 (Saha+, 1999)</TD>
            <TD>Repeated imaging observations have been made of NGC 3627 with the Hubble Space Telescope in 1997 - 1998 over an interval of 58 days. Images were obtained on 12 epochs in the F555W band and on five epochs in the F814W band. The galaxy hosted the prototypical, "Branch normal," type Ia supernova SN 1989B. A total of 83 variables have been found, of which 68 are definite Cepheid variables with periods ranging from 75 to 3.85 days. The dereddened distance modulus is determined to be (m-M)_o_=30.22{+/-}0.12 (internal uncertainty) using a subset of the Cepheid data whose reddening and error parameters are secure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/522/802#2</TD>
            <TD>2011-09-14T19:00:20Z</TD>
            <TD>#Photometry#Stars:variable#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/522/802</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/522/802&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/522/802</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/401 [1]</TD>
            <TD>HI survey of polar ring galaxies. II. (Huchtmeier 1997)</TD>
            <TD>We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401#1</TD>
            <TD>2011-09-14T18:49:26Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/401</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/401</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/401 [2]</TD>
            <TD>HI survey of polar ring galaxies. II. (Huchtmeier 1997)</TD>
            <TD>We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401#2</TD>
            <TD>2011-09-14T18:49:26Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/401&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/319/401 [table1]</TD>
            <TD>HI survey of polar ring galaxies. II. (Huchtmeier 1997)</TD>
            <TD>We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401#table1</TD>
            <TD>2011-09-14T18:49:26Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/319/401&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/401</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/523/540 [1]</TD>
            <TD>VI photometry of new Cepheids in NGC 3319 (Sakai+, 1999)</TD>
            <TD>The distance to NGC 3319 has been determined from Cepheid variable stars as part of the Hubble Space Telescope Key Project on the Extragalactic Distance Scale. Thirteen and four epochs of observations, using filters F555W (V) and F814W (I), respectively, were made with the Wide Field Planetary Camera 2. Thirty-three Cepheid variables between periods of 8 and 47 days were discovered. Adopting a Large Magellanic Cloud distance modulus of 18.50{+/-}0.10 mag and extinction of E(V-I)=0.13 mag, a true reddening-corrected distance modulus (based on an analysis employing the ALLFRAME software package) of 30.78 {+/-}0.14 (random) {+/-}0.10 (systematic) mag and the extinction of E(V-I)=0.06 mag were determined for NGC 3319. This galaxy is the last galaxy observed for the HST H_o_ Key Project.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540#1</TD>
            <TD>2011-09-14T19:00:22Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/523/540</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/523/540</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/523/540 [2]</TD>
            <TD>VI photometry of new Cepheids in NGC 3319 (Sakai+, 1999)</TD>
            <TD>The distance to NGC 3319 has been determined from Cepheid variable stars as part of the Hubble Space Telescope Key Project on the Extragalactic Distance Scale. Thirteen and four epochs of observations, using filters F555W (V) and F814W (I), respectively, were made with the Wide Field Planetary Camera 2. Thirty-three Cepheid variables between periods of 8 and 47 days were discovered. Adopting a Large Magellanic Cloud distance modulus of 18.50{+/-}0.10 mag and extinction of E(V-I)=0.13 mag, a true reddening-corrected distance modulus (based on an analysis employing the ALLFRAME software package) of 30.78 {+/-}0.14 (random) {+/-}0.10 (systematic) mag and the extinction of E(V-I)=0.06 mag were determined for NGC 3319. This galaxy is the last galaxy observed for the HST H_o_ Key Project.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540#2</TD>
            <TD>2011-09-14T19:00:22Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/523/540&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/523/540</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/523/540 [1]</TD>
            <TD>VI photometry of new Cepheids in NGC 3319 (Sakai+, 1999)</TD>
            <TD>The distance to NGC 3319 has been determined from Cepheid variable stars as part of the Hubble Space Telescope Key Project on the Extragalactic Distance Scale. Thirteen and four epochs of observations, using filters F555W (V) and F814W (I), respectively, were made with the Wide Field Planetary Camera 2. Thirty-three Cepheid variables between periods of 8 and 47 days were discovered. Adopting a Large Magellanic Cloud distance modulus of 18.50{+/-}0.10 mag and extinction of E(V-I)=0.13 mag, a true reddening-corrected distance modulus (based on an analysis employing the ALLFRAME software package) of 30.78 {+/-}0.14 (random) {+/-}0.10 (systematic) mag and the extinction of E(V-I)=0.06 mag were determined for NGC 3319. This galaxy is the last galaxy observed for the HST H_o_ Key Project.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540#1</TD>
            <TD>2011-09-14T19:00:22Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/523/540</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/523/540</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/523/540 [2]</TD>
            <TD>VI photometry of new Cepheids in NGC 3319 (Sakai+, 1999)</TD>
            <TD>The distance to NGC 3319 has been determined from Cepheid variable stars as part of the Hubble Space Telescope Key Project on the Extragalactic Distance Scale. Thirteen and four epochs of observations, using filters F555W (V) and F814W (I), respectively, were made with the Wide Field Planetary Camera 2. Thirty-three Cepheid variables between periods of 8 and 47 days were discovered. Adopting a Large Magellanic Cloud distance modulus of 18.50{+/-}0.10 mag and extinction of E(V-I)=0.13 mag, a true reddening-corrected distance modulus (based on an analysis employing the ALLFRAME software package) of 30.78 {+/-}0.14 (random) {+/-}0.10 (systematic) mag and the extinction of E(V-I)=0.06 mag were determined for NGC 3319. This galaxy is the last galaxy observed for the HST H_o_ Key Project.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540#2</TD>
            <TD>2011-09-14T19:00:22Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/523/540&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/523/540</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/523/540 [1]</TD>
            <TD>VI photometry of new Cepheids in NGC 3319 (Sakai+, 1999)</TD>
            <TD>The distance to NGC 3319 has been determined from Cepheid variable stars as part of the Hubble Space Telescope Key Project on the Extragalactic Distance Scale. Thirteen and four epochs of observations, using filters F555W (V) and F814W (I), respectively, were made with the Wide Field Planetary Camera 2. Thirty-three Cepheid variables between periods of 8 and 47 days were discovered. Adopting a Large Magellanic Cloud distance modulus of 18.50{+/-}0.10 mag and extinction of E(V-I)=0.13 mag, a true reddening-corrected distance modulus (based on an analysis employing the ALLFRAME software package) of 30.78 {+/-}0.14 (random) {+/-}0.10 (systematic) mag and the extinction of E(V-I)=0.06 mag were determined for NGC 3319. This galaxy is the last galaxy observed for the HST H_o_ Key Project.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540#1</TD>
            <TD>2011-09-14T19:00:22Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/523/540</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/523/540</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/523/540 [2]</TD>
            <TD>VI photometry of new Cepheids in NGC 3319 (Sakai+, 1999)</TD>
            <TD>The distance to NGC 3319 has been determined from Cepheid variable stars as part of the Hubble Space Telescope Key Project on the Extragalactic Distance Scale. Thirteen and four epochs of observations, using filters F555W (V) and F814W (I), respectively, were made with the Wide Field Planetary Camera 2. Thirty-three Cepheid variables between periods of 8 and 47 days were discovered. Adopting a Large Magellanic Cloud distance modulus of 18.50{+/-}0.10 mag and extinction of E(V-I)=0.13 mag, a true reddening-corrected distance modulus (based on an analysis employing the ALLFRAME software package) of 30.78 {+/-}0.14 (random) {+/-}0.10 (systematic) mag and the extinction of E(V-I)=0.06 mag were determined for NGC 3319. This galaxy is the last galaxy observed for the HST H_o_ Key Project.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540#2</TD>
            <TD>2011-09-14T19:00:22Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/523/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/523/540&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/523/540</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/401 [1]</TD>
            <TD>HI survey of polar ring galaxies. II. (Huchtmeier 1997)</TD>
            <TD>We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401#1</TD>
            <TD>2011-09-14T18:49:26Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/401</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/401</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/401 [2]</TD>
            <TD>HI survey of polar ring galaxies. II. (Huchtmeier 1997)</TD>
            <TD>We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401#2</TD>
            <TD>2011-09-14T18:49:26Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/401&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/319/401 [table1]</TD>
            <TD>HI survey of polar ring galaxies. II. (Huchtmeier 1997)</TD>
            <TD>We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401#table1</TD>
            <TD>2011-09-14T18:49:26Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/319/401&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/401</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/401 [1]</TD>
            <TD>HI survey of polar ring galaxies. II. (Huchtmeier 1997)</TD>
            <TD>We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401#1</TD>
            <TD>2011-09-14T18:49:26Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/401</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/401</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/401 [2]</TD>
            <TD>HI survey of polar ring galaxies. II. (Huchtmeier 1997)</TD>
            <TD>We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401#2</TD>
            <TD>2011-09-14T18:49:26Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/401&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/401</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/319/401 [table1]</TD>
            <TD>HI survey of polar ring galaxies. II. (Huchtmeier 1997)</TD>
            <TD>We present the results of a neutral hydrogen survey conducted with the 100-m radiotelescope at Effelsberg of 44 northern objects in the polar-ring galaxy atlas of Whitmore et al. (1990AJ....100.1489W). These observations were performed to complement the Green Bank observations of polar-ring galaxies (Paper I, 1994AJ....107...99R). We detected 29 of these above our detection limit of a few mJy. The relative content of neutral hydrogen (M_HI_/L_B_) of the early-type galaxies (E, S0) in this sample is significantly higher than for galaxies of the same morphological types from comparison samples, i.e. for elliptical galaxies M_HI_/L_B_=0.17+/-0.09 and for S0 galaxies M_HI_/L_B_=0.75+/-0.13 which is about 6 times the mean value from the comparison samples for the same morphological types.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401#table1</TD>
            <TD>2011-09-14T18:49:26Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/401</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/319/401&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/401</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/95/1 [1]</TD>
            <TD>Atlas of Quasar Energy Distributions (Elvis+ 1994)</TD>
            <TD>We present an atlas of the spectral energy distributions (SEDs) of normal, non-blazar, quasars over the whole available range (radio to 10 keV X-rays) of the electromagnetic spectrum. The primary (UVSX) sample includes 47 quasars for which the spectral energy distributions include X-ray spectral indices and UV data. Of these, 29 are radio quiet, and 18 are radio loud. The SEDs are presented both in figures and in tabular form, with additional tabular material published on CD-ROM. Previously unpublished observational data for a second set of quasars excluded from the primary sample are also tabulated. The effects of host galaxy starlight contamination and foreground extinction on the UVSX sample are considered and the sample is used to investigate the range of SED properties. Of course, the properties we derive are influenced strongly by the selection effects induced by quasar discovery techniques. We derive the mean energy distribution (MED) for radio-loud and radio-quiet objects and present the bolometric corrections derived from it. We note, however, that the dispersion about this mean is large (~one decade for both the infrared and ultraviolet components when the MED is normalized at the near-infrared inflection). At least part of the dispersion in the ultraviolet may be due to time variability, but this is unlikely to be important in the infrared. The existence of such a large dispersion indicates that the MED reflects only some of the properties of quasars and so should be used only with caution.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/1#1</TD>
            <TD>2011-09-14T18:50:18Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/95/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/95/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/95/1 [2]</TD>
            <TD>Atlas of Quasar Energy Distributions (Elvis+ 1994)</TD>
            <TD>We present an atlas of the spectral energy distributions (SEDs) of normal, non-blazar, quasars over the whole available range (radio to 10 keV X-rays) of the electromagnetic spectrum. The primary (UVSX) sample includes 47 quasars for which the spectral energy distributions include X-ray spectral indices and UV data. Of these, 29 are radio quiet, and 18 are radio loud. The SEDs are presented both in figures and in tabular form, with additional tabular material published on CD-ROM. Previously unpublished observational data for a second set of quasars excluded from the primary sample are also tabulated. The effects of host galaxy starlight contamination and foreground extinction on the UVSX sample are considered and the sample is used to investigate the range of SED properties. Of course, the properties we derive are influenced strongly by the selection effects induced by quasar discovery techniques. We derive the mean energy distribution (MED) for radio-loud and radio-quiet objects and present the bolometric corrections derived from it. We note, however, that the dispersion about this mean is large (~one decade for both the infrared and ultraviolet components when the MED is normalized at the near-infrared inflection). At least part of the dispersion in the ultraviolet may be due to time variability, but this is unlikely to be important in the infrared. The existence of such a large dispersion indicates that the MED reflects only some of the properties of quasars and so should be used only with caution.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/1#2</TD>
            <TD>2011-09-14T18:50:18Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/95/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/95/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/95/1 [1]</TD>
            <TD>Atlas of Quasar Energy Distributions (Elvis+ 1994)</TD>
            <TD>We present an atlas of the spectral energy distributions (SEDs) of normal, non-blazar, quasars over the whole available range (radio to 10 keV X-rays) of the electromagnetic spectrum. The primary (UVSX) sample includes 47 quasars for which the spectral energy distributions include X-ray spectral indices and UV data. Of these, 29 are radio quiet, and 18 are radio loud. The SEDs are presented both in figures and in tabular form, with additional tabular material published on CD-ROM. Previously unpublished observational data for a second set of quasars excluded from the primary sample are also tabulated. The effects of host galaxy starlight contamination and foreground extinction on the UVSX sample are considered and the sample is used to investigate the range of SED properties. Of course, the properties we derive are influenced strongly by the selection effects induced by quasar discovery techniques. We derive the mean energy distribution (MED) for radio-loud and radio-quiet objects and present the bolometric corrections derived from it. We note, however, that the dispersion about this mean is large (~one decade for both the infrared and ultraviolet components when the MED is normalized at the near-infrared inflection). At least part of the dispersion in the ultraviolet may be due to time variability, but this is unlikely to be important in the infrared. The existence of such a large dispersion indicates that the MED reflects only some of the properties of quasars and so should be used only with caution.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/1#1</TD>
            <TD>2011-09-14T18:50:18Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/95/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/95/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/95/1 [2]</TD>
            <TD>Atlas of Quasar Energy Distributions (Elvis+ 1994)</TD>
            <TD>We present an atlas of the spectral energy distributions (SEDs) of normal, non-blazar, quasars over the whole available range (radio to 10 keV X-rays) of the electromagnetic spectrum. The primary (UVSX) sample includes 47 quasars for which the spectral energy distributions include X-ray spectral indices and UV data. Of these, 29 are radio quiet, and 18 are radio loud. The SEDs are presented both in figures and in tabular form, with additional tabular material published on CD-ROM. Previously unpublished observational data for a second set of quasars excluded from the primary sample are also tabulated. The effects of host galaxy starlight contamination and foreground extinction on the UVSX sample are considered and the sample is used to investigate the range of SED properties. Of course, the properties we derive are influenced strongly by the selection effects induced by quasar discovery techniques. We derive the mean energy distribution (MED) for radio-loud and radio-quiet objects and present the bolometric corrections derived from it. We note, however, that the dispersion about this mean is large (~one decade for both the infrared and ultraviolet components when the MED is normalized at the near-infrared inflection). At least part of the dispersion in the ultraviolet may be due to time variability, but this is unlikely to be important in the infrared. The existence of such a large dispersion indicates that the MED reflects only some of the properties of quasars and so should be used only with caution.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#UV#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/1#2</TD>
            <TD>2011-09-14T18:50:18Z</TD>
            <TD>#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Feb-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/95/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/95/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/95/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/131/295 [1]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#1</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/131/295</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/131/295 [2]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#2</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/131/295&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/131/295 [table4]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#table4</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/131/295&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/131/295 [table2]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#table2</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/131/295&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/131/295 [1]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#1</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/131/295</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/131/295 [2]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#2</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/131/295&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/131/295 [table4]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#table4</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/131/295&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/131/295 [table2]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#table2</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/131/295&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/131/295 [1]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#1</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/131/295</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/131/295 [2]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#2</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/131/295&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/131/295 [table4]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#table4</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/131/295&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/131/295 [table2]</TD>
            <TD>Spectral survey of Case emission-line galaxies (Ugryumov+ 1998)</TD>
            <TD>The results of the follow-up spectroscopy of 178 emission-line galaxy (ELG) candidates from the Case objective-prism survey and nine Markarian galaxies with the 6m telescope are described. Only the candidates classified in the Case survey as those with emission lines were observed with the aim to form a statistical sample of blue compact galaxies (BCGs) with strong emission lines in the zone RA: 8h-16h, and DE: =+29deg-+38deg. We present the redshifts, equivalent widths and flux ratios for the strongest lines and the spectrum type for most of the galaxies with detected emission lines. A significant fraction (about 23%) of the observed Case galaxies do not show emission lines in blue. Preliminary analysis of the data is presented and the properties of the observed ELGs are compared with those of other known samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295#table2</TD>
            <TD>2011-09-14T19:00:45Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/295</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/131/295&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/295</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/102 [1]</TD>
            <TD>NGC 5548 BR photometry (Tyson+ 1998)</TD>
            <TD>Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102#1</TD>
            <TD>2011-09-14T18:52:53Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/102 [2]</TD>
            <TD>NGC 5548 BR photometry (Tyson+ 1998)</TD>
            <TD>Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102#2</TD>
            <TD>2011-09-14T18:52:53Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/102 [table1]</TD>
            <TD>NGC 5548 BR photometry (Tyson+ 1998)</TD>
            <TD>Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102#table1</TD>
            <TD>2011-09-14T18:52:53Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/80/479 [1]</TD>
            <TD>Nearby galaxy flows (Tully+, 1992)</TD>
            <TD>Supporting material for an article in the main journal is presented. One table gives measured galaxy distances used to construct a map of observed peculiar velocities, and another table gives a grid of the distribution of light used to construct a map of expected peculiar velocities. A preferred model was developed which gave a best fit between these maps, and this model has been used to generate output kinematic distances which are recorded here for groups and individual galaxies with V_0_&lt;3000km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/80/479#1</TD>
            <TD>2011-09-14T19:00:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/80/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/80/479</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/80/479</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/80/479 [2]</TD>
            <TD>Nearby galaxy flows (Tully+, 1992)</TD>
            <TD>Supporting material for an article in the main journal is presented. One table gives measured galaxy distances used to construct a map of observed peculiar velocities, and another table gives a grid of the distribution of light used to construct a map of expected peculiar velocities. A preferred model was developed which gave a best fit between these maps, and this model has been used to generate output kinematic distances which are recorded here for groups and individual galaxies with V_0_&lt;3000km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/80/479#2</TD>
            <TD>2011-09-14T19:00:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/80/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/80/479&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/80/479</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/80/479 [1]</TD>
            <TD>Nearby galaxy flows (Tully+, 1992)</TD>
            <TD>Supporting material for an article in the main journal is presented. One table gives measured galaxy distances used to construct a map of observed peculiar velocities, and another table gives a grid of the distribution of light used to construct a map of expected peculiar velocities. A preferred model was developed which gave a best fit between these maps, and this model has been used to generate output kinematic distances which are recorded here for groups and individual galaxies with V_0_&lt;3000km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/80/479#1</TD>
            <TD>2011-09-14T19:00:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/80/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/80/479</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/80/479</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/80/479 [2]</TD>
            <TD>Nearby galaxy flows (Tully+, 1992)</TD>
            <TD>Supporting material for an article in the main journal is presented. One table gives measured galaxy distances used to construct a map of observed peculiar velocities, and another table gives a grid of the distribution of light used to construct a map of expected peculiar velocities. A preferred model was developed which gave a best fit between these maps, and this model has been used to generate output kinematic distances which are recorded here for groups and individual galaxies with V_0_&lt;3000km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/80/479#2</TD>
            <TD>2011-09-14T19:00:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/80/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/80/479&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/80/479</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/274/1107 [1]</TD>
            <TD>Morphological classifications of APM galaxies (Naim+ 1995)</TD>
            <TD>We investigate the consistency of visual morphological classifications of galaxies by comparing classifications for 831 galaxies from six independent observers. The galaxies were classified on laser print copy images or on computer screen using scans made with the Automated Plate Measuring (APM) machine. Classifications are compared using the Revised Hubble numerical type index T. We find that individual observers agree with one another with rms combined dispersions of between 1.3 and 2.3 type units, typically about 1.8 units. The dispersions tend to decrease slightly with increasing angular diameter and, in some cases, with increasing axial ratio (b/a). The agreement between independent observers is reasonably good but the scatter is non-negligible. In spite of the scatter, the Revised Hubble T system can be used to train an automated galaxy classifier, e.g. an artificial neural network, to handle the large number of galaxy images that are being compiled in the APM and other surveys.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107#1</TD>
            <TD>2011-09-14T19:00:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/274/1107</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1107</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/274/1107 [2]</TD>
            <TD>Morphological classifications of APM galaxies (Naim+ 1995)</TD>
            <TD>We investigate the consistency of visual morphological classifications of galaxies by comparing classifications for 831 galaxies from six independent observers. The galaxies were classified on laser print copy images or on computer screen using scans made with the Automated Plate Measuring (APM) machine. Classifications are compared using the Revised Hubble numerical type index T. We find that individual observers agree with one another with rms combined dispersions of between 1.3 and 2.3 type units, typically about 1.8 units. The dispersions tend to decrease slightly with increasing angular diameter and, in some cases, with increasing axial ratio (b/a). The agreement between independent observers is reasonably good but the scatter is non-negligible. In spite of the scatter, the Revised Hubble T system can be used to train an automated galaxy classifier, e.g. an artificial neural network, to handle the large number of galaxy images that are being compiled in the APM and other surveys.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107#2</TD>
            <TD>2011-09-14T19:00:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/274/1107&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1107</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/274/1107 [1]</TD>
            <TD>Morphological classifications of APM galaxies (Naim+ 1995)</TD>
            <TD>We investigate the consistency of visual morphological classifications of galaxies by comparing classifications for 831 galaxies from six independent observers. The galaxies were classified on laser print copy images or on computer screen using scans made with the Automated Plate Measuring (APM) machine. Classifications are compared using the Revised Hubble numerical type index T. We find that individual observers agree with one another with rms combined dispersions of between 1.3 and 2.3 type units, typically about 1.8 units. The dispersions tend to decrease slightly with increasing angular diameter and, in some cases, with increasing axial ratio (b/a). The agreement between independent observers is reasonably good but the scatter is non-negligible. In spite of the scatter, the Revised Hubble T system can be used to train an automated galaxy classifier, e.g. an artificial neural network, to handle the large number of galaxy images that are being compiled in the APM and other surveys.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107#1</TD>
            <TD>2011-09-14T19:00:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/274/1107</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1107</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/274/1107 [2]</TD>
            <TD>Morphological classifications of APM galaxies (Naim+ 1995)</TD>
            <TD>We investigate the consistency of visual morphological classifications of galaxies by comparing classifications for 831 galaxies from six independent observers. The galaxies were classified on laser print copy images or on computer screen using scans made with the Automated Plate Measuring (APM) machine. Classifications are compared using the Revised Hubble numerical type index T. We find that individual observers agree with one another with rms combined dispersions of between 1.3 and 2.3 type units, typically about 1.8 units. The dispersions tend to decrease slightly with increasing angular diameter and, in some cases, with increasing axial ratio (b/a). The agreement between independent observers is reasonably good but the scatter is non-negligible. In spite of the scatter, the Revised Hubble T system can be used to train an automated galaxy classifier, e.g. an artificial neural network, to handle the large number of galaxy images that are being compiled in the APM and other surveys.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107#2</TD>
            <TD>2011-09-14T19:00:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/274/1107&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1107</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/274/1107 [1]</TD>
            <TD>Morphological classifications of APM galaxies (Naim+ 1995)</TD>
            <TD>We investigate the consistency of visual morphological classifications of galaxies by comparing classifications for 831 galaxies from six independent observers. The galaxies were classified on laser print copy images or on computer screen using scans made with the Automated Plate Measuring (APM) machine. Classifications are compared using the Revised Hubble numerical type index T. We find that individual observers agree with one another with rms combined dispersions of between 1.3 and 2.3 type units, typically about 1.8 units. The dispersions tend to decrease slightly with increasing angular diameter and, in some cases, with increasing axial ratio (b/a). The agreement between independent observers is reasonably good but the scatter is non-negligible. In spite of the scatter, the Revised Hubble T system can be used to train an automated galaxy classifier, e.g. an artificial neural network, to handle the large number of galaxy images that are being compiled in the APM and other surveys.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107#1</TD>
            <TD>2011-09-14T19:00:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/274/1107</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1107</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/274/1107 [2]</TD>
            <TD>Morphological classifications of APM galaxies (Naim+ 1995)</TD>
            <TD>We investigate the consistency of visual morphological classifications of galaxies by comparing classifications for 831 galaxies from six independent observers. The galaxies were classified on laser print copy images or on computer screen using scans made with the Automated Plate Measuring (APM) machine. Classifications are compared using the Revised Hubble numerical type index T. We find that individual observers agree with one another with rms combined dispersions of between 1.3 and 2.3 type units, typically about 1.8 units. The dispersions tend to decrease slightly with increasing angular diameter and, in some cases, with increasing axial ratio (b/a). The agreement between independent observers is reasonably good but the scatter is non-negligible. In spite of the scatter, the Revised Hubble T system can be used to train an automated galaxy classifier, e.g. an artificial neural network, to handle the large number of galaxy images that are being compiled in the APM and other surveys.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107#2</TD>
            <TD>2011-09-14T19:00:58Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1107</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/274/1107&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1107</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AcA/48/455 [1]</TD>
            <TD>Globular Clusters in M31 and M33 (Mochejska+, 1998)</TD>
            <TD>We have used the data from the DIRECT project to search for new globular cluster candidates in the M31 and M33 galaxies. We have found 67 new objects in M31 and 35 in M33 and confirmed 38 and 16 previously discovered ones. A VI and BVI photometry has been obtained for all clusters in M31 and M33, respectively. Luminosity functions have been constructed for the clusters in each galaxy and compared with that of the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455#1</TD>
            <TD>2011-09-14T19:01:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AcA/48/455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/48/455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AcA/48/455 [2]</TD>
            <TD>Globular Clusters in M31 and M33 (Mochejska+, 1998)</TD>
            <TD>We have used the data from the DIRECT project to search for new globular cluster candidates in the M31 and M33 galaxies. We have found 67 new objects in M31 and 35 in M33 and confirmed 38 and 16 previously discovered ones. A VI and BVI photometry has been obtained for all clusters in M31 and M33, respectively. Luminosity functions have been constructed for the clusters in each galaxy and compared with that of the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455#2</TD>
            <TD>2011-09-14T19:01:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AcA/48/455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/48/455</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/366/68 [1]</TD>
            <TD>Spectrophotometric indices from galaxy bulges (Prugniel+, 2001)</TD>
            <TD>We have measured Mg_2_, Fe5270 and Fe5335 spectrophotometric indices (LICK system) in the bulge of 89 galaxies, mostly spirals from the Heraudeau sample. The indices are reduced to a null velocity dispersion and normalized to an aperture of 0.2h^-1^kpc. The mean errors are 0.009 mag on Mg_2_, and 0.3{AA} on the iron indices. These measurements almost double the amount of similar data already available on spiral galaxies. Our data confirm the existence of the relation between Mg_2_ and sigma_0_, the central stellar velocity dispersion; and we find an even tighter relation between Mg_2_ and Vmaxrot, the maximum rotational velocity of the galaxy, deduced from HI observations. For the most massive bulges these correlations may be interpreted as a mass-metallicity relation. However, the presence of young stellar populations, traced by the detection of [OIII]{lambda}500.7nm emission, provides a clear evidence that age effects play a role. Since the contribution of the young population is anti-correlated with the mass of the galaxy, it continues the Mg_2_ vs. sigma_0_ relation toward the low sigma_0_ and globally increases its slope. We present also evidence for a new positive correlation between Fe indices and sigma_0_ and for a significant correlation between the line strength indices and the total or disk luminosity. We propose to model the whole sequence of bulges within the following framework: Bulges are composed of a primary population formed prior to the disk during the initial collapse and a secondary population formed along the evolution. The whole family of bulges can be classified in three classes: (A) The bulges dominated by a young population are generally small, have ionized gas, low velocity dispersion and low line strengths. (B) The bulges dominated by the primary population lie along the mass metallicity sequence defined for elliptical galaxies. (C) The bulges where the secondary population is significant are less Mg-overabundant than B-type bulges and deviate from the Mg_2_ vs. sigma_0_ relation of elliptical galaxies. The original data are available in Hypercat: http://www-obs.univ-lyon1.fr/hypercat The tables of measurements and the extracted 1D spectra are also available in the present archive set.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68#1</TD>
            <TD>2011-09-14T19:46:49Z</TD>
            <TD>#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/366/68</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/68</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/366/68 [2]</TD>
            <TD>Spectrophotometric indices from galaxy bulges (Prugniel+, 2001)</TD>
            <TD>We have measured Mg_2_, Fe5270 and Fe5335 spectrophotometric indices (LICK system) in the bulge of 89 galaxies, mostly spirals from the Heraudeau sample. The indices are reduced to a null velocity dispersion and normalized to an aperture of 0.2h^-1^kpc. The mean errors are 0.009 mag on Mg_2_, and 0.3{AA} on the iron indices. These measurements almost double the amount of similar data already available on spiral galaxies. Our data confirm the existence of the relation between Mg_2_ and sigma_0_, the central stellar velocity dispersion; and we find an even tighter relation between Mg_2_ and Vmaxrot, the maximum rotational velocity of the galaxy, deduced from HI observations. For the most massive bulges these correlations may be interpreted as a mass-metallicity relation. However, the presence of young stellar populations, traced by the detection of [OIII]{lambda}500.7nm emission, provides a clear evidence that age effects play a role. Since the contribution of the young population is anti-correlated with the mass of the galaxy, it continues the Mg_2_ vs. sigma_0_ relation toward the low sigma_0_ and globally increases its slope. We present also evidence for a new positive correlation between Fe indices and sigma_0_ and for a significant correlation between the line strength indices and the total or disk luminosity. We propose to model the whole sequence of bulges within the following framework: Bulges are composed of a primary population formed prior to the disk during the initial collapse and a secondary population formed along the evolution. The whole family of bulges can be classified in three classes: (A) The bulges dominated by a young population are generally small, have ionized gas, low velocity dispersion and low line strengths. (B) The bulges dominated by the primary population lie along the mass metallicity sequence defined for elliptical galaxies. (C) The bulges where the secondary population is significant are less Mg-overabundant than B-type bulges and deviate from the Mg_2_ vs. sigma_0_ relation of elliptical galaxies. The original data are available in Hypercat: http://www-obs.univ-lyon1.fr/hypercat The tables of measurements and the extracted 1D spectra are also available in the present archive set.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68#2</TD>
            <TD>2011-09-14T19:46:49Z</TD>
            <TD>#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/366/68&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/68</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/102 [1]</TD>
            <TD>NGC 5548 BR photometry (Tyson+ 1998)</TD>
            <TD>Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102#1</TD>
            <TD>2011-09-14T18:52:53Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/102 [2]</TD>
            <TD>NGC 5548 BR photometry (Tyson+ 1998)</TD>
            <TD>Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102#2</TD>
            <TD>2011-09-14T18:52:53Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/102 [table1]</TD>
            <TD>NGC 5548 BR photometry (Tyson+ 1998)</TD>
            <TD>Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102#table1</TD>
            <TD>2011-09-14T18:52:53Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/366/68 [1]</TD>
            <TD>Spectrophotometric indices from galaxy bulges (Prugniel+, 2001)</TD>
            <TD>We have measured Mg_2_, Fe5270 and Fe5335 spectrophotometric indices (LICK system) in the bulge of 89 galaxies, mostly spirals from the Heraudeau sample. The indices are reduced to a null velocity dispersion and normalized to an aperture of 0.2h^-1^kpc. The mean errors are 0.009 mag on Mg_2_, and 0.3{AA} on the iron indices. These measurements almost double the amount of similar data already available on spiral galaxies. Our data confirm the existence of the relation between Mg_2_ and sigma_0_, the central stellar velocity dispersion; and we find an even tighter relation between Mg_2_ and Vmaxrot, the maximum rotational velocity of the galaxy, deduced from HI observations. For the most massive bulges these correlations may be interpreted as a mass-metallicity relation. However, the presence of young stellar populations, traced by the detection of [OIII]{lambda}500.7nm emission, provides a clear evidence that age effects play a role. Since the contribution of the young population is anti-correlated with the mass of the galaxy, it continues the Mg_2_ vs. sigma_0_ relation toward the low sigma_0_ and globally increases its slope. We present also evidence for a new positive correlation between Fe indices and sigma_0_ and for a significant correlation between the line strength indices and the total or disk luminosity. We propose to model the whole sequence of bulges within the following framework: Bulges are composed of a primary population formed prior to the disk during the initial collapse and a secondary population formed along the evolution. The whole family of bulges can be classified in three classes: (A) The bulges dominated by a young population are generally small, have ionized gas, low velocity dispersion and low line strengths. (B) The bulges dominated by the primary population lie along the mass metallicity sequence defined for elliptical galaxies. (C) The bulges where the secondary population is significant are less Mg-overabundant than B-type bulges and deviate from the Mg_2_ vs. sigma_0_ relation of elliptical galaxies. The original data are available in Hypercat: http://www-obs.univ-lyon1.fr/hypercat The tables of measurements and the extracted 1D spectra are also available in the present archive set.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68#1</TD>
            <TD>2011-09-14T19:46:49Z</TD>
            <TD>#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/366/68</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/68</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/366/68 [2]</TD>
            <TD>Spectrophotometric indices from galaxy bulges (Prugniel+, 2001)</TD>
            <TD>We have measured Mg_2_, Fe5270 and Fe5335 spectrophotometric indices (LICK system) in the bulge of 89 galaxies, mostly spirals from the Heraudeau sample. The indices are reduced to a null velocity dispersion and normalized to an aperture of 0.2h^-1^kpc. The mean errors are 0.009 mag on Mg_2_, and 0.3{AA} on the iron indices. These measurements almost double the amount of similar data already available on spiral galaxies. Our data confirm the existence of the relation between Mg_2_ and sigma_0_, the central stellar velocity dispersion; and we find an even tighter relation between Mg_2_ and Vmaxrot, the maximum rotational velocity of the galaxy, deduced from HI observations. For the most massive bulges these correlations may be interpreted as a mass-metallicity relation. However, the presence of young stellar populations, traced by the detection of [OIII]{lambda}500.7nm emission, provides a clear evidence that age effects play a role. Since the contribution of the young population is anti-correlated with the mass of the galaxy, it continues the Mg_2_ vs. sigma_0_ relation toward the low sigma_0_ and globally increases its slope. We present also evidence for a new positive correlation between Fe indices and sigma_0_ and for a significant correlation between the line strength indices and the total or disk luminosity. We propose to model the whole sequence of bulges within the following framework: Bulges are composed of a primary population formed prior to the disk during the initial collapse and a secondary population formed along the evolution. The whole family of bulges can be classified in three classes: (A) The bulges dominated by a young population are generally small, have ionized gas, low velocity dispersion and low line strengths. (B) The bulges dominated by the primary population lie along the mass metallicity sequence defined for elliptical galaxies. (C) The bulges where the secondary population is significant are less Mg-overabundant than B-type bulges and deviate from the Mg_2_ vs. sigma_0_ relation of elliptical galaxies. The original data are available in Hypercat: http://www-obs.univ-lyon1.fr/hypercat The tables of measurements and the extracted 1D spectra are also available in the present archive set.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68#2</TD>
            <TD>2011-09-14T19:46:49Z</TD>
            <TD>#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/366/68&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/68</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/102 [1]</TD>
            <TD>NGC 5548 BR photometry (Tyson+ 1998)</TD>
            <TD>Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102#1</TD>
            <TD>2011-09-14T18:52:53Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/102 [2]</TD>
            <TD>NGC 5548 BR photometry (Tyson+ 1998)</TD>
            <TD>Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102#2</TD>
            <TD>2011-09-14T18:52:53Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/102 [table1]</TD>
            <TD>NGC 5548 BR photometry (Tyson+ 1998)</TD>
            <TD>Deep Hubble Space Telescope Wide Field Camera (WFC-1) imaging of a region 3.7' east of the V=13mag Seyfert galaxy NGC 5548 in the F555W and F785LP bands, and deep ground-based V and I imaging, show a new extended, blue, low surface brightness structure, apparently a remnant of a tidal interaction associated with NGC 5548. If this straight, low surface brightness (V~27-28mag/arcsec^2^) tidal tail is associated with NGC 5548, it extends at least 80kpc from it and has an absolute magnitude of M_V~-16.4 (H_0_=65km/s/Mpc). Previous imaging surveys of Seyfert galaxies would have missed such low surface brightness tails. Morphologically similar to some brighter tails seen in other interacting systems and in simulations of merging galaxies, this faint tail is a useful diagnostic of an earlier interaction and of the progenitors' halo-to-disk mass ratios. Luminous ripples and a brighter tail wrapped around the galaxy are seen in the inner 1-10kpc region. Unresolved blue objects in the long tail have the colors and absolute magnitudes of young globular clusters. Taken together, the two tails and other features suggest that two spirals merged less than ~1Gyr ago. The inner luminosity profile of NGC 5548 is a good fit to a de Vaucouleurs profile with r_eff_=5.8kpc. Recent simulations of merged galaxies with high-mass halos fail to form lasting tidal tails, suggesting that the NGC 5548 progenitor spirals had modest halo masses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102#table1</TD>
            <TD>2011-09-14T18:52:53Z</TD>
            <TD>#Photometry#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AcA/48/455 [1]</TD>
            <TD>Globular Clusters in M31 and M33 (Mochejska+, 1998)</TD>
            <TD>We have used the data from the DIRECT project to search for new globular cluster candidates in the M31 and M33 galaxies. We have found 67 new objects in M31 and 35 in M33 and confirmed 38 and 16 previously discovered ones. A VI and BVI photometry has been obtained for all clusters in M31 and M33, respectively. Luminosity functions have been constructed for the clusters in each galaxy and compared with that of the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455#1</TD>
            <TD>2011-09-14T19:01:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AcA/48/455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/48/455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AcA/48/455 [2]</TD>
            <TD>Globular Clusters in M31 and M33 (Mochejska+, 1998)</TD>
            <TD>We have used the data from the DIRECT project to search for new globular cluster candidates in the M31 and M33 galaxies. We have found 67 new objects in M31 and 35 in M33 and confirmed 38 and 16 previously discovered ones. A VI and BVI photometry has been obtained for all clusters in M31 and M33, respectively. Luminosity functions have been constructed for the clusters in each galaxy and compared with that of the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455#2</TD>
            <TD>2011-09-14T19:01:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AcA/48/455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/48/455</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/259/233 [1]</TD>
            <TD>Cluster SC2008-57(A3667) (Sodre+ 1992)</TD>
            <TD>We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233#1</TD>
            <TD>2011-09-14T18:37:53Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Photometry#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1993</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/259/233</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/259/233</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/259/233 [2]</TD>
            <TD>Cluster SC2008-57(A3667) (Sodre+ 1992)</TD>
            <TD>We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233#2</TD>
            <TD>2011-09-14T18:37:53Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Photometry#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1993</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/259/233&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/259/233</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/259/233 [table3]</TD>
            <TD>Cluster SC2008-57(A3667) (Sodre+ 1992)</TD>
            <TD>We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233#table3</TD>
            <TD>2011-09-14T18:37:53Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Photometry#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1993</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/259/233&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/259/233</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/259/233 [1]</TD>
            <TD>Cluster SC2008-57(A3667) (Sodre+ 1992)</TD>
            <TD>We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233#1</TD>
            <TD>2011-09-14T18:37:53Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Photometry#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1993</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/259/233</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/259/233</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/259/233 [2]</TD>
            <TD>Cluster SC2008-57(A3667) (Sodre+ 1992)</TD>
            <TD>We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233#2</TD>
            <TD>2011-09-14T18:37:53Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Photometry#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1993</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/259/233&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/259/233</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/259/233 [table3]</TD>
            <TD>Cluster SC2008-57(A3667) (Sodre+ 1992)</TD>
            <TD>We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233#table3</TD>
            <TD>2011-09-14T18:37:53Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Photometry#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1993</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/259/233&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/259/233</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/259/233 [1]</TD>
            <TD>Cluster SC2008-57(A3667) (Sodre+ 1992)</TD>
            <TD>We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233#1</TD>
            <TD>2011-09-14T18:37:53Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Photometry#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1993</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/259/233</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/259/233</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/259/233 [2]</TD>
            <TD>Cluster SC2008-57(A3667) (Sodre+ 1992)</TD>
            <TD>We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233#2</TD>
            <TD>2011-09-14T18:37:53Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Photometry#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1993</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/259/233&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/259/233</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/259/233 [table3]</TD>
            <TD>Cluster SC2008-57(A3667) (Sodre+ 1992)</TD>
            <TD>We present the results of photometric and spectroscopic observations of the cluster of galaxies SC2008-57 (A3667). The observations have resulted in a catalogue with positions and magnitudes for 203 galaxies, complete at b_25 = 18.0, and radial velocities for 128 galaxies, 91 per cent complete at b_25 = 17.5. The cluster can be classified as type L because its galaxy distribution is highly flattened. It shows two strong concentrations: a main concentration, centred on the cluster brightest galaxy (a D galaxy) and coincident with the peak of X-ray emission, and a substructure around the second brightest galaxy (also a D galaxy). Most of the galaxies in this substructure seem to be bound to the second-brightest galaxy, forming a dynamical subunit inside the cluster. The extreme flattening of the cluster may at least partially be due to the presence of the substructure. The cluster also shows evidence for luminosity segregation, with the brightest galaxies being preferentially found in high galaxy density regions. Most of the luminosity segregation, however, is produced by galaxies associated with the two clumps around the D galaxies, suggesting that dynamical friction is effective in subclusters with low velocity dispersions and may be associated with the formation of D galaxies. The velocity dispersion of SC2008-57 is high, about 1200 km/s, but consistent with the observed X-ray luminosity. The cluster mass, derived using several estimators, is about 2.6 x 10^15 M_solar. Both the cluster mass and velocity dispersion may be overestimates due to the presence of the substructure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233#table3</TD>
            <TD>2011-09-14T18:37:53Z</TD>
            <TD>#Positional_Data#Clusters_of_galaxies#Photometry#Spectroscopy#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Nov-1993</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/259/233</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/259/233&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/259/233</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/105/1465 [1]</TD>
            <TD>Distant OB Stars in the Galaxy (Reed 1993)</TD>
            <TD>Distances and reddenings have been computed from UBVbeta photometry for 1044 stars in the Stephenson and Sanduleak (1971) "Catalog of Luminous Stars in the Southern Milky Way".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465#1</TD>
            <TD>2011-09-14T18:38:12Z</TD>
            <TD>#Photometry:narrow-band#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/105/1465</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/105/1465</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/105/1465 [2]</TD>
            <TD>Distant OB Stars in the Galaxy (Reed 1993)</TD>
            <TD>Distances and reddenings have been computed from UBVbeta photometry for 1044 stars in the Stephenson and Sanduleak (1971) "Catalog of Luminous Stars in the Southern Milky Way".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465#2</TD>
            <TD>2011-09-14T18:38:12Z</TD>
            <TD>#Photometry:narrow-band#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/105/1465&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/105/1465</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/146 [1]</TD>
            <TD>UGC 6456 HST photometry (Lynds+ 1998)</TD>
            <TD>Photometry on the UVI system has been performed on the resolved stellar content of the blue compact dwarf galaxy UGC 6456 using Wide Field Planetary Camera 2 (WFPC2) images obtained with the Hubble Space Telescope. The resulting color-magnitude diagram (CMD) goes to about V=27.5 and reveals not only a young population of blue main-sequence stars and blue and red supergiants, but also an older evolved population of red giants and a fairly well represented asymptotic giant branch. The distance to the galaxy is estimated from the tip of the red giant branch to be 4.5Mpc, placing it about 1.5Mpc farther away than the major members of the M81 Group, with which it is usually associated. The youngest stars are generally associated with H ii regions shown on our Halpha image and are largely confined to the 745pc field of our PC images. A comparison of their distribution in the CMD with theoretical isochrones suggests ages from 4 to 10Myr. The population of older stars is found throughout all WFPC2 camera fields and seems to show an elliptical distribution with an aspect ratio of about 2.4 and an exponential falloff in surface density with distance from a center of symmetry that is not far from the centroid of the youngest stars. Theoretical modeling of the CMD at a metallicity of Z=0.001 suggests star formation in the age interval 1-2Gyr, a strong burst in the interval 600-800Myr, and a lower rate of star formation up to the present. The evidence is compatible with a scenario beginning with the formation of a population of low-metallicity stars, enriching a major residual of prestellar material that subsequently fueled an active episode of star formation. That burst of star formation must have been particularly spectacular and may be related to the activity we now see in the distant blue dwarf galaxies revealed in deep imaging.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/146#1</TD>
            <TD>2011-09-14T18:52:54Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/146</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/146</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/146</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/146 [2]</TD>
            <TD>UGC 6456 HST photometry (Lynds+ 1998)</TD>
            <TD>Photometry on the UVI system has been performed on the resolved stellar content of the blue compact dwarf galaxy UGC 6456 using Wide Field Planetary Camera 2 (WFPC2) images obtained with the Hubble Space Telescope. The resulting color-magnitude diagram (CMD) goes to about V=27.5 and reveals not only a young population of blue main-sequence stars and blue and red supergiants, but also an older evolved population of red giants and a fairly well represented asymptotic giant branch. The distance to the galaxy is estimated from the tip of the red giant branch to be 4.5Mpc, placing it about 1.5Mpc farther away than the major members of the M81 Group, with which it is usually associated. The youngest stars are generally associated with H ii regions shown on our Halpha image and are largely confined to the 745pc field of our PC images. A comparison of their distribution in the CMD with theoretical isochrones suggests ages from 4 to 10Myr. The population of older stars is found throughout all WFPC2 camera fields and seems to show an elliptical distribution with an aspect ratio of about 2.4 and an exponential falloff in surface density with distance from a center of symmetry that is not far from the centroid of the youngest stars. Theoretical modeling of the CMD at a metallicity of Z=0.001 suggests star formation in the age interval 1-2Gyr, a strong burst in the interval 600-800Myr, and a lower rate of star formation up to the present. The evidence is compatible with a scenario beginning with the formation of a population of low-metallicity stars, enriching a major residual of prestellar material that subsequently fueled an active episode of star formation. That burst of star formation must have been particularly spectacular and may be related to the activity we now see in the distant blue dwarf galaxies revealed in deep imaging.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/146#2</TD>
            <TD>2011-09-14T18:52:54Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/146</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/146&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/146</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/105/1465 [1]</TD>
            <TD>Distant OB Stars in the Galaxy (Reed 1993)</TD>
            <TD>Distances and reddenings have been computed from UBVbeta photometry for 1044 stars in the Stephenson and Sanduleak (1971) "Catalog of Luminous Stars in the Southern Milky Way".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465#1</TD>
            <TD>2011-09-14T18:38:12Z</TD>
            <TD>#Photometry:narrow-band#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/105/1465</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/105/1465</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/105/1465 [2]</TD>
            <TD>Distant OB Stars in the Galaxy (Reed 1993)</TD>
            <TD>Distances and reddenings have been computed from UBVbeta photometry for 1044 stars in the Stephenson and Sanduleak (1971) "Catalog of Luminous Stars in the Southern Milky Way".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465#2</TD>
            <TD>2011-09-14T18:38:12Z</TD>
            <TD>#Photometry:narrow-band#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/105/1465&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/105/1465</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/105/1465 [1]</TD>
            <TD>Distant OB Stars in the Galaxy (Reed 1993)</TD>
            <TD>Distances and reddenings have been computed from UBVbeta photometry for 1044 stars in the Stephenson and Sanduleak (1971) "Catalog of Luminous Stars in the Southern Milky Way".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465#1</TD>
            <TD>2011-09-14T18:38:12Z</TD>
            <TD>#Photometry:narrow-band#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/105/1465</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/105/1465</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/105/1465 [2]</TD>
            <TD>Distant OB Stars in the Galaxy (Reed 1993)</TD>
            <TD>Distances and reddenings have been computed from UBVbeta photometry for 1044 stars in the Stephenson and Sanduleak (1971) "Catalog of Luminous Stars in the Southern Milky Way".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465#2</TD>
            <TD>2011-09-14T18:38:12Z</TD>
            <TD>#Photometry:narrow-band#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jan-1995</TD>
            <TD>ivo://CDS.VizieR/J/PASP/105/1465</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/105/1465&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/105/1465</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/146 [1]</TD>
            <TD>UGC 6456 HST photometry (Lynds+ 1998)</TD>
            <TD>Photometry on the UVI system has been performed on the resolved stellar content of the blue compact dwarf galaxy UGC 6456 using Wide Field Planetary Camera 2 (WFPC2) images obtained with the Hubble Space Telescope. The resulting color-magnitude diagram (CMD) goes to about V=27.5 and reveals not only a young population of blue main-sequence stars and blue and red supergiants, but also an older evolved population of red giants and a fairly well represented asymptotic giant branch. The distance to the galaxy is estimated from the tip of the red giant branch to be 4.5Mpc, placing it about 1.5Mpc farther away than the major members of the M81 Group, with which it is usually associated. The youngest stars are generally associated with H ii regions shown on our Halpha image and are largely confined to the 745pc field of our PC images. A comparison of their distribution in the CMD with theoretical isochrones suggests ages from 4 to 10Myr. The population of older stars is found throughout all WFPC2 camera fields and seems to show an elliptical distribution with an aspect ratio of about 2.4 and an exponential falloff in surface density with distance from a center of symmetry that is not far from the centroid of the youngest stars. Theoretical modeling of the CMD at a metallicity of Z=0.001 suggests star formation in the age interval 1-2Gyr, a strong burst in the interval 600-800Myr, and a lower rate of star formation up to the present. The evidence is compatible with a scenario beginning with the formation of a population of low-metallicity stars, enriching a major residual of prestellar material that subsequently fueled an active episode of star formation. That burst of star formation must have been particularly spectacular and may be related to the activity we now see in the distant blue dwarf galaxies revealed in deep imaging.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/146#1</TD>
            <TD>2011-09-14T18:52:54Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/146</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/146</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/146</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/146 [2]</TD>
            <TD>UGC 6456 HST photometry (Lynds+ 1998)</TD>
            <TD>Photometry on the UVI system has been performed on the resolved stellar content of the blue compact dwarf galaxy UGC 6456 using Wide Field Planetary Camera 2 (WFPC2) images obtained with the Hubble Space Telescope. The resulting color-magnitude diagram (CMD) goes to about V=27.5 and reveals not only a young population of blue main-sequence stars and blue and red supergiants, but also an older evolved population of red giants and a fairly well represented asymptotic giant branch. The distance to the galaxy is estimated from the tip of the red giant branch to be 4.5Mpc, placing it about 1.5Mpc farther away than the major members of the M81 Group, with which it is usually associated. The youngest stars are generally associated with H ii regions shown on our Halpha image and are largely confined to the 745pc field of our PC images. A comparison of their distribution in the CMD with theoretical isochrones suggests ages from 4 to 10Myr. The population of older stars is found throughout all WFPC2 camera fields and seems to show an elliptical distribution with an aspect ratio of about 2.4 and an exponential falloff in surface density with distance from a center of symmetry that is not far from the centroid of the youngest stars. Theoretical modeling of the CMD at a metallicity of Z=0.001 suggests star formation in the age interval 1-2Gyr, a strong burst in the interval 600-800Myr, and a lower rate of star formation up to the present. The evidence is compatible with a scenario beginning with the formation of a population of low-metallicity stars, enriching a major residual of prestellar material that subsequently fueled an active episode of star formation. That burst of star formation must have been particularly spectacular and may be related to the activity we now see in the distant blue dwarf galaxies revealed in deep imaging.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/146#2</TD>
            <TD>2011-09-14T18:52:54Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/146</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/146&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/146</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/560/566 [1]</TD>
            <TD>K-band galaxy luminosity function from 2MASS (Kochanek+, 2001)</TD>
            <TD>We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with {mu}_Ks_=20mag/arcsec^2^ isophotal magnitudes 7&lt;K_20_&lt;11.25mag spread over 2.12sr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566#1</TD>
            <TD>2011-09-14T19:46:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/560/566</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/566</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/560/566 [2]</TD>
            <TD>K-band galaxy luminosity function from 2MASS (Kochanek+, 2001)</TD>
            <TD>We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with {mu}_Ks_=20mag/arcsec^2^ isophotal magnitudes 7&lt;K_20_&lt;11.25mag spread over 2.12sr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566#2</TD>
            <TD>2011-09-14T19:46:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/560/566&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/566</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/560/566 [table1]</TD>
            <TD>K-band galaxy luminosity function from 2MASS (Kochanek+, 2001)</TD>
            <TD>We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with {mu}_Ks_=20mag/arcsec^2^ isophotal magnitudes 7&lt;K_20_&lt;11.25mag spread over 2.12sr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566#table1</TD>
            <TD>2011-09-14T19:46:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/560/566&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/566</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AcA/48/455 [1]</TD>
            <TD>Globular Clusters in M31 and M33 (Mochejska+, 1998)</TD>
            <TD>We have used the data from the DIRECT project to search for new globular cluster candidates in the M31 and M33 galaxies. We have found 67 new objects in M31 and 35 in M33 and confirmed 38 and 16 previously discovered ones. A VI and BVI photometry has been obtained for all clusters in M31 and M33, respectively. Luminosity functions have been constructed for the clusters in each galaxy and compared with that of the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455#1</TD>
            <TD>2011-09-14T19:01:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AcA/48/455</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/48/455</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AcA/48/455 [2]</TD>
            <TD>Globular Clusters in M31 and M33 (Mochejska+, 1998)</TD>
            <TD>We have used the data from the DIRECT project to search for new globular cluster candidates in the M31 and M33 galaxies. We have found 67 new objects in M31 and 35 in M33 and confirmed 38 and 16 previously discovered ones. A VI and BVI photometry has been obtained for all clusters in M31 and M33, respectively. Luminosity functions have been constructed for the clusters in each galaxy and compared with that of the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455#2</TD>
            <TD>2011-09-14T19:01:00Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/AcA/48/455</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AcA/48/455&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AcA/48/455</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VI/31 [1]</TD>
            <TD>Plate Centers, Epochs Lick/Mt. John Sky Survey (Lick Obs. 1965)</TD>
            <TD>The "Lick Observatory Sky Atlas" (Lick Observatory, 1965) is a set of plates for 166 fields of 18 by 18 degrees, covering the sky from the north pole down to -30 degrees of declination. "The Mount John University Observatory Photographic Sky Survey" (Doughty et al., 1972) covers 142 similar fields from -15 degrees of declination down to the south pole. In the region of overlap, the fields are the same for the two surveys. Fields 1-46 of the Mount John survey cover the part of the sky (-45 degrees of declination to the south pole) not in the Lick survey; in a special limited edition published in 1972, this part is called the "Canterbury Sky Atlas" (Australia). The overlap between fields is 3 degrees. The plate scale is approximately 232 arc seconds per millimeter. The limiting magnitude is approximately 16. Neither survey is intended for astrometry or photometry; the Lick survey was originally done to obtain galaxy statistics (Shane and Wirtanen 1967). An excellent summary of several photographic sky surveys is given by Ingrao and Kasparian (1967). T. A. Nagy (1980) generated the dataset described, and also gathered most of the material used in the writing of this document.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VI/31#1</TD>
            <TD>2011-09-14T18:38:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VI/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VI/31</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/31</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VI/31 [2]</TD>
            <TD>Plate Centers, Epochs Lick/Mt. John Sky Survey (Lick Obs. 1965)</TD>
            <TD>The "Lick Observatory Sky Atlas" (Lick Observatory, 1965) is a set of plates for 166 fields of 18 by 18 degrees, covering the sky from the north pole down to -30 degrees of declination. "The Mount John University Observatory Photographic Sky Survey" (Doughty et al., 1972) covers 142 similar fields from -15 degrees of declination down to the south pole. In the region of overlap, the fields are the same for the two surveys. Fields 1-46 of the Mount John survey cover the part of the sky (-45 degrees of declination to the south pole) not in the Lick survey; in a special limited edition published in 1972, this part is called the "Canterbury Sky Atlas" (Australia). The overlap between fields is 3 degrees. The plate scale is approximately 232 arc seconds per millimeter. The limiting magnitude is approximately 16. Neither survey is intended for astrometry or photometry; the Lick survey was originally done to obtain galaxy statistics (Shane and Wirtanen 1967). An excellent summary of several photographic sky surveys is given by Ingrao and Kasparian (1967). T. A. Nagy (1980) generated the dataset described, and also gathered most of the material used in the writing of this document.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VI/31#2</TD>
            <TD>2011-09-14T18:38:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VI/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VI/31&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/31</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VI/31 [data]</TD>
            <TD>Plate Centers, Epochs Lick/Mt. John Sky Survey (Lick Obs. 1965)</TD>
            <TD>The "Lick Observatory Sky Atlas" (Lick Observatory, 1965) is a set of plates for 166 fields of 18 by 18 degrees, covering the sky from the north pole down to -30 degrees of declination. "The Mount John University Observatory Photographic Sky Survey" (Doughty et al., 1972) covers 142 similar fields from -15 degrees of declination down to the south pole. In the region of overlap, the fields are the same for the two surveys. Fields 1-46 of the Mount John survey cover the part of the sky (-45 degrees of declination to the south pole) not in the Lick survey; in a special limited edition published in 1972, this part is called the "Canterbury Sky Atlas" (Australia). The overlap between fields is 3 degrees. The plate scale is approximately 232 arc seconds per millimeter. The limiting magnitude is approximately 16. Neither survey is intended for astrometry or photometry; the Lick survey was originally done to obtain galaxy statistics (Shane and Wirtanen 1967). An excellent summary of several photographic sky surveys is given by Ingrao and Kasparian (1967). T. A. Nagy (1980) generated the dataset described, and also gathered most of the material used in the writing of this document.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VI/31#data</TD>
            <TD>2011-09-14T18:38:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VI/31</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VI/31&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/31</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/560/566 [1]</TD>
            <TD>K-band galaxy luminosity function from 2MASS (Kochanek+, 2001)</TD>
            <TD>We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with {mu}_Ks_=20mag/arcsec^2^ isophotal magnitudes 7&lt;K_20_&lt;11.25mag spread over 2.12sr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566#1</TD>
            <TD>2011-09-14T19:46:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/560/566</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/566</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/560/566 [2]</TD>
            <TD>K-band galaxy luminosity function from 2MASS (Kochanek+, 2001)</TD>
            <TD>We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with {mu}_Ks_=20mag/arcsec^2^ isophotal magnitudes 7&lt;K_20_&lt;11.25mag spread over 2.12sr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566#2</TD>
            <TD>2011-09-14T19:46:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/560/566&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/566</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/560/566 [table1]</TD>
            <TD>K-band galaxy luminosity function from 2MASS (Kochanek+, 2001)</TD>
            <TD>We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with {mu}_Ks_=20mag/arcsec^2^ isophotal magnitudes 7&lt;K_20_&lt;11.25mag spread over 2.12sr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566#table1</TD>
            <TD>2011-09-14T19:46:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/560/566&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/566</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/1722 [1]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#1</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/1722</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/1722 [2]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#2</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/1722&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/1722 [table2]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#table2</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/1722&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/1722 [table1]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#table1</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/1722&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/23/409 [1]</TD>
            <TD>Spectrophotometry of Mrk 509 (Chuvaev+, 1997)</TD>
            <TD>Variability of the continuum, H{beta}, H{gamma} and HeII(4686{AA}) fluxes of the Seyfert I galaxy Mrk 509 is studied using spectra obtained on the 2.6-m telescope of the Crimean Astrophysical observatory from 1971-1993. All the measurements of fluxes are in the relative units normalized to the flux of [OIII](5007{AA}) taken equal to 100. The flux in the line [OIII](5007{AA}) is estimated in the interval of (5.7-7.6)*10^-13^erg/cm^2^/s=(5.7-7.6)*10^-16^W/m2. The variability amplitude in the continuum is higher than in the hydrogen lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/23/409#1</TD>
            <TD>2011-09-14T18:54:13Z</TD>
            <TD>#Photometry:narrow-band#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1999</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/23/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/23/409</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/23/409</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/23/409 [2]</TD>
            <TD>Spectrophotometry of Mrk 509 (Chuvaev+, 1997)</TD>
            <TD>Variability of the continuum, H{beta}, H{gamma} and HeII(4686{AA}) fluxes of the Seyfert I galaxy Mrk 509 is studied using spectra obtained on the 2.6-m telescope of the Crimean Astrophysical observatory from 1971-1993. All the measurements of fluxes are in the relative units normalized to the flux of [OIII](5007{AA}) taken equal to 100. The flux in the line [OIII](5007{AA}) is estimated in the interval of (5.7-7.6)*10^-13^erg/cm^2^/s=(5.7-7.6)*10^-16^W/m2. The variability amplitude in the continuum is higher than in the hydrogen lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/23/409#2</TD>
            <TD>2011-09-14T18:54:13Z</TD>
            <TD>#Photometry:narrow-band#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1999</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/23/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/23/409&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/23/409</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/560/566 [1]</TD>
            <TD>K-band galaxy luminosity function from 2MASS (Kochanek+, 2001)</TD>
            <TD>We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with {mu}_Ks_=20mag/arcsec^2^ isophotal magnitudes 7&lt;K_20_&lt;11.25mag spread over 2.12sr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566#1</TD>
            <TD>2011-09-14T19:46:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/560/566</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/566</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/560/566 [2]</TD>
            <TD>K-band galaxy luminosity function from 2MASS (Kochanek+, 2001)</TD>
            <TD>We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with {mu}_Ks_=20mag/arcsec^2^ isophotal magnitudes 7&lt;K_20_&lt;11.25mag spread over 2.12sr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566#2</TD>
            <TD>2011-09-14T19:46:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/560/566&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/566</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/560/566 [table1]</TD>
            <TD>K-band galaxy luminosity function from 2MASS (Kochanek+, 2001)</TD>
            <TD>We measured the K-band luminosity function using a complete sample of 4192 morphologically typed 2MASS galaxies with {mu}_Ks_=20mag/arcsec^2^ isophotal magnitudes 7&lt;K_20_&lt;11.25mag spread over 2.12sr.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566#table1</TD>
            <TD>2011-09-14T19:46:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/566</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/560/566&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/566</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/23/409 [1]</TD>
            <TD>Spectrophotometry of Mrk 509 (Chuvaev+, 1997)</TD>
            <TD>Variability of the continuum, H{beta}, H{gamma} and HeII(4686{AA}) fluxes of the Seyfert I galaxy Mrk 509 is studied using spectra obtained on the 2.6-m telescope of the Crimean Astrophysical observatory from 1971-1993. All the measurements of fluxes are in the relative units normalized to the flux of [OIII](5007{AA}) taken equal to 100. The flux in the line [OIII](5007{AA}) is estimated in the interval of (5.7-7.6)*10^-13^erg/cm^2^/s=(5.7-7.6)*10^-16^W/m2. The variability amplitude in the continuum is higher than in the hydrogen lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/23/409#1</TD>
            <TD>2011-09-14T18:54:13Z</TD>
            <TD>#Photometry:narrow-band#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1999</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/23/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/23/409</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/23/409</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/23/409 [2]</TD>
            <TD>Spectrophotometry of Mrk 509 (Chuvaev+, 1997)</TD>
            <TD>Variability of the continuum, H{beta}, H{gamma} and HeII(4686{AA}) fluxes of the Seyfert I galaxy Mrk 509 is studied using spectra obtained on the 2.6-m telescope of the Crimean Astrophysical observatory from 1971-1993. All the measurements of fluxes are in the relative units normalized to the flux of [OIII](5007{AA}) taken equal to 100. The flux in the line [OIII](5007{AA}) is estimated in the interval of (5.7-7.6)*10^-13^erg/cm^2^/s=(5.7-7.6)*10^-16^W/m2. The variability amplitude in the continuum is higher than in the hydrogen lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/23/409#2</TD>
            <TD>2011-09-14T18:54:13Z</TD>
            <TD>#Photometry:narrow-band#Seyfert_Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-1999</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/23/409</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/23/409&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/23/409</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/1722 [1]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#1</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/1722</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/1722 [2]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#2</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/108/1722&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/1722 [table2]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#table2</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/1722&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/1722 [table1]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/73/359 [1]</TD>
            <TD>1.49 GHz atlas of the IRAS bright galaxies (Condon+, 1990)</TD>
            <TD>This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359#1</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/73/359 [2]</TD>
            <TD>1.49 GHz atlas of the IRAS bright galaxies (Condon+, 1990)</TD>
            <TD>This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359#2</TD>
            <TD>2011-09-14T18:55:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359</TD>
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            <TD>J/ApJS/73/359 [iras1490]</TD>
            <TD>1.49 GHz atlas of the IRAS bright galaxies (Condon+, 1990)</TD>
            <TD>This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359#iras1490</TD>
            <TD>2011-09-14T18:55:00Z</TD>
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            <TD>01-Apr-1999</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/359</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/108/1722 [1]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#1</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
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            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/108/1722</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/108/1722 [2]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#2</TD>
            <TD>2011-09-14T19:01:15Z</TD>
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            <TD>#Research#</TD>
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            <TD>J/AJ/108/1722 [table2]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#table2</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/1722&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/108/1722 [table1]</TD>
            <TD>Blue horizontal branch stars (Kinman+ 1994)</TD>
            <TD>A complete sample of blue horizontal branch (BHB) stars in the magnitude range 13.0&lt;V&lt;16.5 is isolated in two Galactic fields that have previously been searched for RR Lyrae variables: SA 57 in the Northern Polar Cap and the Lick Astrograph field RR 7 in the Anticenter (l=183{deg}, b=+37{deg}). These BHB stars are a subset of the AF stars found in the Case Low-Dispersion Northern Survey; lists of these AF stars were made available by the late Nick Sanduleak. The completeness of the sample was confirmed by reference to the photometric survey of SA 57 by Stobie &amp; Ishida (1987AJ93..... 624S) that is complete to fainter than V=18. In the color range 0.00&lt;(B-V)_0_&lt;+0.20, we can distinguish the BHB stars among these AF stars by comparing them both with well known local field horizontal branch (FHB) stars and also the BHB members of the halo globular clusters M3 and M92. The criteria for this comparison include (1) a (u-B)_K_ color index (derived from photoelectric observations using the Stromgren u filter and the Johnson B and V filters) that measures the size of the Balmer jump, (2) a spectrophotometric index A that measures the steepness of the Balmer jump, and (3) a parameter D_0.2_ that is the mean width of the H{gamma} and H{delta} Balmer lines measured at 20 percent of the continuum level. These criteria give consistent results in separating BHB stars from higher gravity main sequence AF stars in the color range 0.00&lt;(B-V)_0_&lt;+0.20. All three photometric and spectrophotometric criteria were measured for 35 stars in the SA 57 field and 37 stars in the RR 7 field that are in the color range (B-V)_0_&lt;+0.23 and in the magnitude range 13.0&lt;V&lt;16.5. For a small number of additional stars only (u-B)_K_ was obtained. Among the AF stars that are fainter than B=13 and bluer than (B-V)_0_=+0.23, about half of those in the SA 57 field and about one third of those in the lower latitude RR 7 field are BHB stars. Isoabundance contours were located empirically in plots of the pseudoequivalent width versus (B-V)_0_ for the lines of Mg II A4481{AA}, Ca II A3933 {AA} and Fe I A4272{AA}. Solar abundances were defined by the data from main sequence stars in the Pleiades and Coma open clusters. Data from the BHB stars in M3 and M92 defined the [Fe/H]=1.5 and -2.2 isoabundance contours, respectively. Metallicities of all stars were estimated by interpolating the measured pseudoequivalent widths in these diagrams at the observed (B-V)_0_. The distribution of [Fe/H] found for the BHB stars in this way is very similar to that which we found for the RR Lyrae stars in the same fields using the Preston AS method. The space densities of these BHB stars were analyzed both separately and together with earlier observations of field BHB stars given by Arnold &amp; Gilmore (1992MNRAS.257..225A), Sommer-Larsen &amp; Christensen (1986MNRAS.219..537S), and Preston et al. (1991ApJ...375..121P). This analysis supports a two-component model for the halo of our Galaxy that is similar in many respects to that proposed by Hartwick [The Galaxy (Reidel, Dordrecht 1987)] although our discussion refers only to the region outside the solar circle. For Z&gt;=35kpc, a classical spherical halo dominates which follows a R_gal_^-3.5^ space-density law and which has a HB morphology like that of the globular cluster M3 (i.e., approximately equal numbers of BHB and RR Lyrae stars). Closer to the galactic plane, there is an additional component with a much flatter galactic distribution (scale height ~2.2kpc near the Sun). The stars of the two components do not have significantly different metallicity distributions but do have slightly different distributions of the A parameter which measures the steepness of the Balmer jump; this is the only physical criterion (independent of spatial or kinematic considerations) which distinguishes between the two components. If present estimates of the local RR Lyrae star space density are correct, then the ratio of BHB stars to RR Lyrae stars is higher in the flatter halo component. The flat component would then have a bluer HB morphology (which could be interpreted as making it older) than the spherical component. In the solar neighborhood about 80 percent of the BHB stars come from the flat component and about 20 percent from the spherical component. More than half of the AF stars with V&gt;13.0 and (B-V)_0_&lt;+0.23 are not BHB stars but have surface gravities that are more like those expected for main sequence stars. Their measured metallicities lie in the range -0.2&lt;[Fe/H]&lt;-2.3. The more metal-poor of these stars are probably similar to the blue metal-poor stars that have been discussed by Preston et al. (1994AJ....108..538P) which, while they probably include globular cluster blue stragglers as a subset, must also comprise stars of other types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722#table1</TD>
            <TD>2011-09-14T19:01:15Z</TD>
            <TD>#Abundances#Stars#Photometry:wide-band#Photometry:intermediate-band#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/108/1722</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/108/1722&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/108/1722</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1626 [1]</TD>
            <TD>Spiral and lenticular galaxy brightness profiles (Baggett+, 1998)</TD>
            <TD>We present one of the largest homogeneous sets of spiral and lenticular galaxy brightness profile decompositions completed to date. The 659 galaxies in our sample have been fitted with a de Vaucouleurs law for the bulge component and an inner-truncated exponential for the disk component. Of the 659 galaxies in the sample, 620 were successfully fitted with the chosen fitting functions. The fits are generally well defined, with more than 90% having rms deviations from the observed profile of less than 0.35mag. We find no correlations of fitting quality, as measured by these rms residuals, with either morphological type or inclination. Similarly, the estimated errors of the fitted coefficients show no significant trends with type or inclination. These decompositions form a useful basis for the study of the light distributions of spiral and lenticular galaxies. The object base is sufficiently large that well-defined samples of galaxies can be selected from it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626#1</TD>
            <TD>2011-09-14T19:01:30Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1626</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1626</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1626 [2]</TD>
            <TD>Spiral and lenticular galaxy brightness profiles (Baggett+, 1998)</TD>
            <TD>We present one of the largest homogeneous sets of spiral and lenticular galaxy brightness profile decompositions completed to date. The 659 galaxies in our sample have been fitted with a de Vaucouleurs law for the bulge component and an inner-truncated exponential for the disk component. Of the 659 galaxies in the sample, 620 were successfully fitted with the chosen fitting functions. The fits are generally well defined, with more than 90% having rms deviations from the observed profile of less than 0.35mag. We find no correlations of fitting quality, as measured by these rms residuals, with either morphological type or inclination. Similarly, the estimated errors of the fitted coefficients show no significant trends with type or inclination. These decompositions form a useful basis for the study of the light distributions of spiral and lenticular galaxies. The object base is sufficiently large that well-defined samples of galaxies can be selected from it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626#2</TD>
            <TD>2011-09-14T19:01:30Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1626&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1626</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1626 [1]</TD>
            <TD>Spiral and lenticular galaxy brightness profiles (Baggett+, 1998)</TD>
            <TD>We present one of the largest homogeneous sets of spiral and lenticular galaxy brightness profile decompositions completed to date. The 659 galaxies in our sample have been fitted with a de Vaucouleurs law for the bulge component and an inner-truncated exponential for the disk component. Of the 659 galaxies in the sample, 620 were successfully fitted with the chosen fitting functions. The fits are generally well defined, with more than 90% having rms deviations from the observed profile of less than 0.35mag. We find no correlations of fitting quality, as measured by these rms residuals, with either morphological type or inclination. Similarly, the estimated errors of the fitted coefficients show no significant trends with type or inclination. These decompositions form a useful basis for the study of the light distributions of spiral and lenticular galaxies. The object base is sufficiently large that well-defined samples of galaxies can be selected from it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626#1</TD>
            <TD>2011-09-14T19:01:30Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1626</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1626</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1626 [2]</TD>
            <TD>Spiral and lenticular galaxy brightness profiles (Baggett+, 1998)</TD>
            <TD>We present one of the largest homogeneous sets of spiral and lenticular galaxy brightness profile decompositions completed to date. The 659 galaxies in our sample have been fitted with a de Vaucouleurs law for the bulge component and an inner-truncated exponential for the disk component. Of the 659 galaxies in the sample, 620 were successfully fitted with the chosen fitting functions. The fits are generally well defined, with more than 90% having rms deviations from the observed profile of less than 0.35mag. We find no correlations of fitting quality, as measured by these rms residuals, with either morphological type or inclination. Similarly, the estimated errors of the fitted coefficients show no significant trends with type or inclination. These decompositions form a useful basis for the study of the light distributions of spiral and lenticular galaxies. The object base is sufficiently large that well-defined samples of galaxies can be selected from it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626#2</TD>
            <TD>2011-09-14T19:01:30Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1626&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1626</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/73/359 [1]</TD>
            <TD>1.49 GHz atlas of the IRAS bright galaxies (Condon+, 1990)</TD>
            <TD>This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359#1</TD>
            <TD>2011-09-14T18:55:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/73/359</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/359</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/73/359 [2]</TD>
            <TD>1.49 GHz atlas of the IRAS bright galaxies (Condon+, 1990)</TD>
            <TD>This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359#2</TD>
            <TD>2011-09-14T18:55:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/73/359&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/359</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/73/359 [iras1490]</TD>
            <TD>1.49 GHz atlas of the IRAS bright galaxies (Condon+, 1990)</TD>
            <TD>This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359#iras1490</TD>
            <TD>2011-09-14T18:55:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/73/359&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/359</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/445/79 [1]</TD>
            <TD>Nearby early-type gal. with ionized gas. II. (Annibali+, 2006)</TD>
            <TD>Rampazzo et al., 2005, Cat. &lt;J/A+A/433/497&gt; (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. &lt;J/ApJS/116/1&gt;; Worthey &amp; Ottaviani, 1997, Cat. &lt;J/ApJS/111/377&gt;), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79#1</TD>
            <TD>2011-09-14T20:01:34Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/445/79</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/79</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/445/79 [2]</TD>
            <TD>Nearby early-type gal. with ionized gas. II. (Annibali+, 2006)</TD>
            <TD>Rampazzo et al., 2005, Cat. &lt;J/A+A/433/497&gt; (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. &lt;J/ApJS/116/1&gt;; Worthey &amp; Ottaviani, 1997, Cat. &lt;J/ApJS/111/377&gt;), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79#2</TD>
            <TD>2011-09-14T20:01:34Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/445/79&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/445/79 [table1]</TD>
            <TD>Nearby early-type gal. with ionized gas. II. (Annibali+, 2006)</TD>
            <TD>Rampazzo et al., 2005, Cat. &lt;J/A+A/433/497&gt; (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. &lt;J/ApJS/116/1&gt;; Worthey &amp; Ottaviani, 1997, Cat. &lt;J/ApJS/111/377&gt;), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79#table1</TD>
            <TD>2011-09-14T20:01:34Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/445/79&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/79</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/1626 [1]</TD>
            <TD>Spiral and lenticular galaxy brightness profiles (Baggett+, 1998)</TD>
            <TD>We present one of the largest homogeneous sets of spiral and lenticular galaxy brightness profile decompositions completed to date. The 659 galaxies in our sample have been fitted with a de Vaucouleurs law for the bulge component and an inner-truncated exponential for the disk component. Of the 659 galaxies in the sample, 620 were successfully fitted with the chosen fitting functions. The fits are generally well defined, with more than 90% having rms deviations from the observed profile of less than 0.35mag. We find no correlations of fitting quality, as measured by these rms residuals, with either morphological type or inclination. Similarly, the estimated errors of the fitted coefficients show no significant trends with type or inclination. These decompositions form a useful basis for the study of the light distributions of spiral and lenticular galaxies. The object base is sufficiently large that well-defined samples of galaxies can be selected from it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626#1</TD>
            <TD>2011-09-14T19:01:30Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/1626</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1626</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/1626 [2]</TD>
            <TD>Spiral and lenticular galaxy brightness profiles (Baggett+, 1998)</TD>
            <TD>We present one of the largest homogeneous sets of spiral and lenticular galaxy brightness profile decompositions completed to date. The 659 galaxies in our sample have been fitted with a de Vaucouleurs law for the bulge component and an inner-truncated exponential for the disk component. Of the 659 galaxies in the sample, 620 were successfully fitted with the chosen fitting functions. The fits are generally well defined, with more than 90% having rms deviations from the observed profile of less than 0.35mag. We find no correlations of fitting quality, as measured by these rms residuals, with either morphological type or inclination. Similarly, the estimated errors of the fitted coefficients show no significant trends with type or inclination. These decompositions form a useful basis for the study of the light distributions of spiral and lenticular galaxies. The object base is sufficiently large that well-defined samples of galaxies can be selected from it.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626#2</TD>
            <TD>2011-09-14T19:01:30Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/1626</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/1626&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/1626</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/73/359 [1]</TD>
            <TD>1.49 GHz atlas of the IRAS bright galaxies (Condon+, 1990)</TD>
            <TD>This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359#1</TD>
            <TD>2011-09-14T18:55:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/73/359</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/359</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/73/359 [2]</TD>
            <TD>1.49 GHz atlas of the IRAS bright galaxies (Condon+, 1990)</TD>
            <TD>This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359#2</TD>
            <TD>2011-09-14T18:55:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/73/359&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/359</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/73/359 [iras1490]</TD>
            <TD>1.49 GHz atlas of the IRAS bright galaxies (Condon+, 1990)</TD>
            <TD>This catalog contains 1.49 GHz VLA observations of sources from the IRAS Bright Galaxy Sample. The original IRAS Bright Galaxy Sample (Soifer et al., 1987ApJ...320..238S) comprises 324 extragalactic objects with 60 micron flux densities above 5.4 Jy. It is the infrared analog of the radio 3CR or optical Shapley-Ames samples. Recalibration of the IRAS flux densities led to a revised Bright Galaxy Sample (Soifer et al., 1989AJ.....98..766S) containing 313 sources stronger than 5.24 Jy at 60 microns. Only one source from these samples was not detected (NGC1377) at 1.49 GHz. For most sources, multiple observations were conducted with different synthesized beam areas. Thus, for a given galaxy there may be several rows in the table reporting data at different angular resolution or reporting different radio components of the object. A low-resolution observation was used to yield an accurate total flux density and a high-resolution observation was used to resolve the brightest components clearly. These observations were originally presented in Condon, et al., (1990ApJS...73..359C).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359#iras1490</TD>
            <TD>2011-09-14T18:55:00Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/73/359</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/73/359&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/73/359</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/445/79 [1]</TD>
            <TD>Nearby early-type gal. with ionized gas. II. (Annibali+, 2006)</TD>
            <TD>Rampazzo et al., 2005, Cat. &lt;J/A+A/433/497&gt; (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. &lt;J/ApJS/116/1&gt;; Worthey &amp; Ottaviani, 1997, Cat. &lt;J/ApJS/111/377&gt;), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79#1</TD>
            <TD>2011-09-14T20:01:34Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/445/79</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/79</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/445/79 [2]</TD>
            <TD>Nearby early-type gal. with ionized gas. II. (Annibali+, 2006)</TD>
            <TD>Rampazzo et al., 2005, Cat. &lt;J/A+A/433/497&gt; (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. &lt;J/ApJS/116/1&gt;; Worthey &amp; Ottaviani, 1997, Cat. &lt;J/ApJS/111/377&gt;), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79#2</TD>
            <TD>2011-09-14T20:01:34Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/445/79&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/445/79 [table1]</TD>
            <TD>Nearby early-type gal. with ionized gas. II. (Annibali+, 2006)</TD>
            <TD>Rampazzo et al., 2005, Cat. &lt;J/A+A/433/497&gt; (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. &lt;J/ApJS/116/1&gt;; Worthey &amp; Ottaviani, 1997, Cat. &lt;J/ApJS/111/377&gt;), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79#table1</TD>
            <TD>2011-09-14T20:01:34Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/445/79&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/79</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/41 [1]</TD>
            <TD>SMC X-ray sources ROSAT PSPC catalogue (Haberl+, 2000)</TD>
            <TD>We present a catalogue of 517 discrete X-ray sources in a 6{deg}x6{deg} field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, Cat. &lt;J/A+AS/139/277&gt;). We followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. For 158 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in ROSAT PSPC observations; most of them with luminosities below 10^36^erg/s suggesting that the fraction of high luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy. Seventeen X-ray sources are associated with SNRs found in earlier work and we suggest here two additional extended sources as SNR candidates. Three very soft sources are newly classified as SSSs from which one is identified with the symbiotic star LIN 358 in the SMC.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41#1</TD>
            <TD>2011-09-14T19:01:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/41</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/41</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/41 [2]</TD>
            <TD>SMC X-ray sources ROSAT PSPC catalogue (Haberl+, 2000)</TD>
            <TD>We present a catalogue of 517 discrete X-ray sources in a 6{deg}x6{deg} field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, Cat. &lt;J/A+AS/139/277&gt;). We followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. For 158 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in ROSAT PSPC observations; most of them with luminosities below 10^36^erg/s suggesting that the fraction of high luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy. Seventeen X-ray sources are associated with SNRs found in earlier work and we suggest here two additional extended sources as SNR candidates. Three very soft sources are newly classified as SSSs from which one is identified with the symbiotic star LIN 358 in the SMC.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41#2</TD>
            <TD>2011-09-14T19:01:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/41&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/41</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/41 [1]</TD>
            <TD>SMC X-ray sources ROSAT PSPC catalogue (Haberl+, 2000)</TD>
            <TD>We present a catalogue of 517 discrete X-ray sources in a 6{deg}x6{deg} field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, Cat. &lt;J/A+AS/139/277&gt;). We followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. For 158 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in ROSAT PSPC observations; most of them with luminosities below 10^36^erg/s suggesting that the fraction of high luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy. Seventeen X-ray sources are associated with SNRs found in earlier work and we suggest here two additional extended sources as SNR candidates. Three very soft sources are newly classified as SSSs from which one is identified with the symbiotic star LIN 358 in the SMC.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41#1</TD>
            <TD>2011-09-14T19:01:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/41</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/41</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/41 [2]</TD>
            <TD>SMC X-ray sources ROSAT PSPC catalogue (Haberl+, 2000)</TD>
            <TD>We present a catalogue of 517 discrete X-ray sources in a 6{deg}x6{deg} field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, Cat. &lt;J/A+AS/139/277&gt;). We followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. For 158 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in ROSAT PSPC observations; most of them with luminosities below 10^36^erg/s suggesting that the fraction of high luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy. Seventeen X-ray sources are associated with SNRs found in earlier work and we suggest here two additional extended sources as SNR candidates. Three very soft sources are newly classified as SSSs from which one is identified with the symbiotic star LIN 358 in the SMC.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41#2</TD>
            <TD>2011-09-14T19:01:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/41&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/41</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/137/419 [1]</TD>
            <TD>Dynamics of blue compact galaxies I. The data (Oestlin + 1999)</TD>
            <TD>Observations of six luminous blue compact galaxies (BCGs) and two star forming companion galaxies were carried out with the CIGALE scanning Fabry-Perot interferometer attached to the ESO 3.6m telescope on La Silla. The observations were made in the H-alpha emission line which is prominent in BCGs. A velocity sampling of 5km/s and a pixel size of 0.9arcseconds were used. In this paper we present the observations and the data together with the velocity fields and the derived rotation curves. In addition we provide rough estimates of the total dynamical mass and of the ionised gas mass for each galaxy. All galaxies display rotation, but while the companion galaxies have regular velocity fields, those of the BCGs are complex and appear perturbed. This is the most extensive study to date of the optical velocity fields of BCGs. The interpretation of these results will be presented in a forthcoming paper (Paper II).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/419#1</TD>
            <TD>2011-09-14T18:56:05Z</TD>
            <TD>#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/137/419</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/419</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/137/419 [2]</TD>
            <TD>Dynamics of blue compact galaxies I. The data (Oestlin + 1999)</TD>
            <TD>Observations of six luminous blue compact galaxies (BCGs) and two star forming companion galaxies were carried out with the CIGALE scanning Fabry-Perot interferometer attached to the ESO 3.6m telescope on La Silla. The observations were made in the H-alpha emission line which is prominent in BCGs. A velocity sampling of 5km/s and a pixel size of 0.9arcseconds were used. In this paper we present the observations and the data together with the velocity fields and the derived rotation curves. In addition we provide rough estimates of the total dynamical mass and of the ionised gas mass for each galaxy. All galaxies display rotation, but while the companion galaxies have regular velocity fields, those of the BCGs are complex and appear perturbed. This is the most extensive study to date of the optical velocity fields of BCGs. The interpretation of these results will be presented in a forthcoming paper (Paper II).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/419#2</TD>
            <TD>2011-09-14T18:56:05Z</TD>
            <TD>#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/137/419&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/419</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/41 [1]</TD>
            <TD>SMC X-ray sources ROSAT PSPC catalogue (Haberl+, 2000)</TD>
            <TD>We present a catalogue of 517 discrete X-ray sources in a 6{deg}x6{deg} field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, Cat. &lt;J/A+AS/139/277&gt;). We followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. For 158 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in ROSAT PSPC observations; most of them with luminosities below 10^36^erg/s suggesting that the fraction of high luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy. Seventeen X-ray sources are associated with SNRs found in earlier work and we suggest here two additional extended sources as SNR candidates. Three very soft sources are newly classified as SSSs from which one is identified with the symbiotic star LIN 358 in the SMC.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41#1</TD>
            <TD>2011-09-14T19:01:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/41</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/41</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/41 [2]</TD>
            <TD>SMC X-ray sources ROSAT PSPC catalogue (Haberl+, 2000)</TD>
            <TD>We present a catalogue of 517 discrete X-ray sources in a 6{deg}x6{deg} field covering the Small Magellanic Cloud (SMC). The catalogue was derived from the pointed ROSAT PSPC observations performed between October 1991 and May 1994 and is complementary to the Large Magellanic Cloud (LMC) catalogue published by Haberl &amp; Pietsch (1999, Cat. &lt;J/A+AS/139/277&gt;). We followed the same identification scheme and used, among other information, X-ray hardness ratios and spatial extent to classify unknown sources as candidates for active galactic nuclei (AGN), foreground stars, supernova remnants (SNRs), supersoft sources (SSSs) and X-ray binaries. For 158 sources a likely source type is given, from which 46 sources are suggested as background AGN (including candidates resulting from a comparison of X-ray and radio images). Nearly all of the X-ray binaries known in the SMC were detected in ROSAT PSPC observations; most of them with luminosities below 10^36^erg/s suggesting that the fraction of high luminosity X-ray binary systems in the Magellanic Clouds (MCs) is not significantly larger than in our galaxy. Seventeen X-ray sources are associated with SNRs found in earlier work and we suggest here two additional extended sources as SNR candidates. Three very soft sources are newly classified as SSSs from which one is identified with the symbiotic star LIN 358 in the SMC.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41#2</TD>
            <TD>2011-09-14T19:01:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/41</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/41&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/41</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/137/419 [1]</TD>
            <TD>Dynamics of blue compact galaxies I. The data (Oestlin + 1999)</TD>
            <TD>Observations of six luminous blue compact galaxies (BCGs) and two star forming companion galaxies were carried out with the CIGALE scanning Fabry-Perot interferometer attached to the ESO 3.6m telescope on La Silla. The observations were made in the H-alpha emission line which is prominent in BCGs. A velocity sampling of 5km/s and a pixel size of 0.9arcseconds were used. In this paper we present the observations and the data together with the velocity fields and the derived rotation curves. In addition we provide rough estimates of the total dynamical mass and of the ionised gas mass for each galaxy. All galaxies display rotation, but while the companion galaxies have regular velocity fields, those of the BCGs are complex and appear perturbed. This is the most extensive study to date of the optical velocity fields of BCGs. The interpretation of these results will be presented in a forthcoming paper (Paper II).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/419#1</TD>
            <TD>2011-09-14T18:56:05Z</TD>
            <TD>#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/137/419</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/419</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/137/419 [2]</TD>
            <TD>Dynamics of blue compact galaxies I. The data (Oestlin + 1999)</TD>
            <TD>Observations of six luminous blue compact galaxies (BCGs) and two star forming companion galaxies were carried out with the CIGALE scanning Fabry-Perot interferometer attached to the ESO 3.6m telescope on La Silla. The observations were made in the H-alpha emission line which is prominent in BCGs. A velocity sampling of 5km/s and a pixel size of 0.9arcseconds were used. In this paper we present the observations and the data together with the velocity fields and the derived rotation curves. In addition we provide rough estimates of the total dynamical mass and of the ionised gas mass for each galaxy. All galaxies display rotation, but while the companion galaxies have regular velocity fields, those of the BCGs are complex and appear perturbed. This is the most extensive study to date of the optical velocity fields of BCGs. The interpretation of these results will be presented in a forthcoming paper (Paper II).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/419#2</TD>
            <TD>2011-09-14T18:56:05Z</TD>
            <TD>#Galaxies#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/419</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/137/419&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/419</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/445/79 [1]</TD>
            <TD>Nearby early-type gal. with ionized gas. II. (Annibali+, 2006)</TD>
            <TD>Rampazzo et al., 2005, Cat. &lt;J/A+A/433/497&gt; (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. &lt;J/ApJS/116/1&gt;; Worthey &amp; Ottaviani, 1997, Cat. &lt;J/ApJS/111/377&gt;), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79#1</TD>
            <TD>2011-09-14T20:01:34Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/445/79</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/79</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/445/79 [2]</TD>
            <TD>Nearby early-type gal. with ionized gas. II. (Annibali+, 2006)</TD>
            <TD>Rampazzo et al., 2005, Cat. &lt;J/A+A/433/497&gt; (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. &lt;J/ApJS/116/1&gt;; Worthey &amp; Ottaviani, 1997, Cat. &lt;J/ApJS/111/377&gt;), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79#2</TD>
            <TD>2011-09-14T20:01:34Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/445/79&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/79</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/445/79 [table1]</TD>
            <TD>Nearby early-type gal. with ionized gas. II. (Annibali+, 2006)</TD>
            <TD>Rampazzo et al., 2005, Cat. &lt;J/A+A/433/497&gt; (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. &lt;J/ApJS/116/1&gt;; Worthey &amp; Ottaviani, 1997, Cat. &lt;J/ApJS/111/377&gt;), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79#table1</TD>
            <TD>2011-09-14T20:01:34Z</TD>
            <TD>#Equivalent_widths#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jan-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/445/79</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/445/79&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/445/79</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/1562 [1]</TD>
            <TD>gri photometry of 48 galaxy clusters (Margoniner+, 2000)</TD>
            <TD>We obtained CCD images of 48 clusters in four runs between 1997 March and 1998 November. All data were taken with the Tek 2K-3 detector at the Cassegrain focus of the 0.9 m telescope at the Cerro Tololo Inter-American Observatory (CTIO). The CCD has 2048x2048 pixels, each pixel covering 0.396'', corresponding to a field of approximately 13.5x13.5 or about 0.5-6.7 Mpc at z=0.03-0.38 (H_0_ = 67 km.s^-1^.Mpc^-1^). We observed 44 Abell clusters and four cluster candidates detected in POSS-II (Second Palomar Sky Survey; Gal et al. 2000AJ....119...12G) photographic plates. The images were taken through the g, r and i filters of the Thuan &amp; Gunn (1976PASP...88..543T) photometric system, with effective wavelengths and widths of 5118 and 900 {AA} for g, 6798 and 1000 {AA} for r, and 8100 and 1500 {AA} for i. The exposure times varied between 15-60 minutes in the g band, 10-20 minutes in the r band, and 10-15 minutes in the i band.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562#1</TD>
            <TD>2011-09-14T19:01:59Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/1562</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/1562</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/1562 [2]</TD>
            <TD>gri photometry of 48 galaxy clusters (Margoniner+, 2000)</TD>
            <TD>We obtained CCD images of 48 clusters in four runs between 1997 March and 1998 November. All data were taken with the Tek 2K-3 detector at the Cassegrain focus of the 0.9 m telescope at the Cerro Tololo Inter-American Observatory (CTIO). The CCD has 2048x2048 pixels, each pixel covering 0.396'', corresponding to a field of approximately 13.5x13.5 or about 0.5-6.7 Mpc at z=0.03-0.38 (H_0_ = 67 km.s^-1^.Mpc^-1^). We observed 44 Abell clusters and four cluster candidates detected in POSS-II (Second Palomar Sky Survey; Gal et al. 2000AJ....119...12G) photographic plates. The images were taken through the g, r and i filters of the Thuan &amp; Gunn (1976PASP...88..543T) photometric system, with effective wavelengths and widths of 5118 and 900 {AA} for g, 6798 and 1000 {AA} for r, and 8100 and 1500 {AA} for i. The exposure times varied between 15-60 minutes in the g band, 10-20 minutes in the r band, and 10-15 minutes in the i band.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562#2</TD>
            <TD>2011-09-14T19:01:59Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/1562&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/1562</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/303/661 [1]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#1</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/303/661</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/303/661 [2]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#2</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/303/661&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/303/661 [table2]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#table2</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/303/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/303/661 [table1]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#table1</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/303/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/634/977 [1]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#1</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/634/977</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/634/977 [2]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#2</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/634/977&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/634/977 [table2]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#table2</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/634/977&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/634/977 [members]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#members</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/634/977&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/1562 [1]</TD>
            <TD>gri photometry of 48 galaxy clusters (Margoniner+, 2000)</TD>
            <TD>We obtained CCD images of 48 clusters in four runs between 1997 March and 1998 November. All data were taken with the Tek 2K-3 detector at the Cassegrain focus of the 0.9 m telescope at the Cerro Tololo Inter-American Observatory (CTIO). The CCD has 2048x2048 pixels, each pixel covering 0.396'', corresponding to a field of approximately 13.5x13.5 or about 0.5-6.7 Mpc at z=0.03-0.38 (H_0_ = 67 km.s^-1^.Mpc^-1^). We observed 44 Abell clusters and four cluster candidates detected in POSS-II (Second Palomar Sky Survey; Gal et al. 2000AJ....119...12G) photographic plates. The images were taken through the g, r and i filters of the Thuan &amp; Gunn (1976PASP...88..543T) photometric system, with effective wavelengths and widths of 5118 and 900 {AA} for g, 6798 and 1000 {AA} for r, and 8100 and 1500 {AA} for i. The exposure times varied between 15-60 minutes in the g band, 10-20 minutes in the r band, and 10-15 minutes in the i band.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562#1</TD>
            <TD>2011-09-14T19:01:59Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/1562</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/1562</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/1562 [2]</TD>
            <TD>gri photometry of 48 galaxy clusters (Margoniner+, 2000)</TD>
            <TD>We obtained CCD images of 48 clusters in four runs between 1997 March and 1998 November. All data were taken with the Tek 2K-3 detector at the Cassegrain focus of the 0.9 m telescope at the Cerro Tololo Inter-American Observatory (CTIO). The CCD has 2048x2048 pixels, each pixel covering 0.396'', corresponding to a field of approximately 13.5x13.5 or about 0.5-6.7 Mpc at z=0.03-0.38 (H_0_ = 67 km.s^-1^.Mpc^-1^). We observed 44 Abell clusters and four cluster candidates detected in POSS-II (Second Palomar Sky Survey; Gal et al. 2000AJ....119...12G) photographic plates. The images were taken through the g, r and i filters of the Thuan &amp; Gunn (1976PASP...88..543T) photometric system, with effective wavelengths and widths of 5118 and 900 {AA} for g, 6798 and 1000 {AA} for r, and 8100 and 1500 {AA} for i. The exposure times varied between 15-60 minutes in the g band, 10-20 minutes in the r band, and 10-15 minutes in the i band.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562#2</TD>
            <TD>2011-09-14T19:01:59Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/1562&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/1562</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/303/661 [1]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#1</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/303/661</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/303/661 [2]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#2</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/303/661&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/303/661 [table2]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#table2</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/303/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/303/661 [table1]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#table1</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/303/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/1562 [1]</TD>
            <TD>gri photometry of 48 galaxy clusters (Margoniner+, 2000)</TD>
            <TD>We obtained CCD images of 48 clusters in four runs between 1997 March and 1998 November. All data were taken with the Tek 2K-3 detector at the Cassegrain focus of the 0.9 m telescope at the Cerro Tololo Inter-American Observatory (CTIO). The CCD has 2048x2048 pixels, each pixel covering 0.396'', corresponding to a field of approximately 13.5x13.5 or about 0.5-6.7 Mpc at z=0.03-0.38 (H_0_ = 67 km.s^-1^.Mpc^-1^). We observed 44 Abell clusters and four cluster candidates detected in POSS-II (Second Palomar Sky Survey; Gal et al. 2000AJ....119...12G) photographic plates. The images were taken through the g, r and i filters of the Thuan &amp; Gunn (1976PASP...88..543T) photometric system, with effective wavelengths and widths of 5118 and 900 {AA} for g, 6798 and 1000 {AA} for r, and 8100 and 1500 {AA} for i. The exposure times varied between 15-60 minutes in the g band, 10-20 minutes in the r band, and 10-15 minutes in the i band.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562#1</TD>
            <TD>2011-09-14T19:01:59Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/1562</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/1562</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/1562 [2]</TD>
            <TD>gri photometry of 48 galaxy clusters (Margoniner+, 2000)</TD>
            <TD>We obtained CCD images of 48 clusters in four runs between 1997 March and 1998 November. All data were taken with the Tek 2K-3 detector at the Cassegrain focus of the 0.9 m telescope at the Cerro Tololo Inter-American Observatory (CTIO). The CCD has 2048x2048 pixels, each pixel covering 0.396'', corresponding to a field of approximately 13.5x13.5 or about 0.5-6.7 Mpc at z=0.03-0.38 (H_0_ = 67 km.s^-1^.Mpc^-1^). We observed 44 Abell clusters and four cluster candidates detected in POSS-II (Second Palomar Sky Survey; Gal et al. 2000AJ....119...12G) photographic plates. The images were taken through the g, r and i filters of the Thuan &amp; Gunn (1976PASP...88..543T) photometric system, with effective wavelengths and widths of 5118 and 900 {AA} for g, 6798 and 1000 {AA} for r, and 8100 and 1500 {AA} for i. The exposure times varied between 15-60 minutes in the g band, 10-20 minutes in the r band, and 10-15 minutes in the i band.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562#2</TD>
            <TD>2011-09-14T19:01:59Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/1562</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/1562&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/1562</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/357/437 [1]</TD>
            <TD>Photometry of young star groupings in spirals (Battinelli+, 2000)</TD>
            <TD>We present multiband photometric observations of three spiral galaxies selected in a sample suited for the study of young stellar groupings and their relationship with the parent galaxy and the galactic environment. Star forming regions have been identified using an objective technique based on a multivariate statistical analysis. Maps of young star groupings are given for each galaxy. The luminosity functions of the young star group populations show a remarkable similarity with a slope in the range -1.52 to -1.33. The size distributions peak around the classical 100pc value of the Local Group associations for two out of the three galaxies. NGC 1058 shows smaller associations (peak at ~50pc). The total number of young groups per unit B absolute luminosity of the galaxy is significantly greater in UGC 12732. The activity of star formation is in all three galaxies clearly stronger in the central regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/437#1</TD>
            <TD>2011-09-14T19:02:08Z</TD>
            <TD>#Galaxies#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/437</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/357/437</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/437</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/357/437 [2]</TD>
            <TD>Photometry of young star groupings in spirals (Battinelli+, 2000)</TD>
            <TD>We present multiband photometric observations of three spiral galaxies selected in a sample suited for the study of young stellar groupings and their relationship with the parent galaxy and the galactic environment. Star forming regions have been identified using an objective technique based on a multivariate statistical analysis. Maps of young star groupings are given for each galaxy. The luminosity functions of the young star group populations show a remarkable similarity with a slope in the range -1.52 to -1.33. The size distributions peak around the classical 100pc value of the Local Group associations for two out of the three galaxies. NGC 1058 shows smaller associations (peak at ~50pc). The total number of young groups per unit B absolute luminosity of the galaxy is significantly greater in UGC 12732. The activity of star formation is in all three galaxies clearly stronger in the central regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/437#2</TD>
            <TD>2011-09-14T19:02:08Z</TD>
            <TD>#Galaxies#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/437</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/357/437&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/437</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/357/437 [1]</TD>
            <TD>Photometry of young star groupings in spirals (Battinelli+, 2000)</TD>
            <TD>We present multiband photometric observations of three spiral galaxies selected in a sample suited for the study of young stellar groupings and their relationship with the parent galaxy and the galactic environment. Star forming regions have been identified using an objective technique based on a multivariate statistical analysis. Maps of young star groupings are given for each galaxy. The luminosity functions of the young star group populations show a remarkable similarity with a slope in the range -1.52 to -1.33. The size distributions peak around the classical 100pc value of the Local Group associations for two out of the three galaxies. NGC 1058 shows smaller associations (peak at ~50pc). The total number of young groups per unit B absolute luminosity of the galaxy is significantly greater in UGC 12732. The activity of star formation is in all three galaxies clearly stronger in the central regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/437#1</TD>
            <TD>2011-09-14T19:02:08Z</TD>
            <TD>#Galaxies#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/437</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/357/437</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/437</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/357/437 [2]</TD>
            <TD>Photometry of young star groupings in spirals (Battinelli+, 2000)</TD>
            <TD>We present multiband photometric observations of three spiral galaxies selected in a sample suited for the study of young stellar groupings and their relationship with the parent galaxy and the galactic environment. Star forming regions have been identified using an objective technique based on a multivariate statistical analysis. Maps of young star groupings are given for each galaxy. The luminosity functions of the young star group populations show a remarkable similarity with a slope in the range -1.52 to -1.33. The size distributions peak around the classical 100pc value of the Local Group associations for two out of the three galaxies. NGC 1058 shows smaller associations (peak at ~50pc). The total number of young groups per unit B absolute luminosity of the galaxy is significantly greater in UGC 12732. The activity of star formation is in all three galaxies clearly stronger in the central regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/437#2</TD>
            <TD>2011-09-14T19:02:08Z</TD>
            <TD>#Galaxies#YSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/357/437</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/357/437&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/357/437</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/81/807 [1]</TD>
            <TD>Deprojection of the r^1/4^ law tables (Young, 1976)</TD>
            <TD>A spherical galaxy with reduced surface brightness, J=B({alpha})/B_e_, obeying the r^1/4^ law, logJ=-3.3307 ({alpha}^1/4^-1), where {alpha} is the reduced radius, {alpha}=r/r_e_ (r_e_ is the effective radius), is deprojected to find the corresponding space density, mass, mean density, force, potential, escape velocity, and potential energy at each point in the galaxy. Numerical tabulations to five significant figures are given for 124 points in the range 10^-6^&lt;=R/r_e_&lt;=260. In addition the projected surface brightness B({alpha}) and integrated luminosity within {alpha} are tabulated for the range 10^-6^&lt;={alpha}=r/r_e_&lt;=260. Conversion factors to cgs units and to M_{sun}_, pc, km/s, L_{sun}_ units are given. Asymptotic expansions for the space density {rho}(s) in the ranges s=&lt;10^-4^ and s&gt;=10^-1^ are derived, and it is demonstrated that the projection of the expansion for s&lt;=10^-1^ is almost indistinguishable from the r^1/4^ law itself, apart from a small excess of luminosity in the central regions. Formulae and numerical tables of the luminosity distribution are given for use in galaxy photometry. Relations between the total galactic mass M_T_, the effective radius r_e_, the velocity dispersion {sigma}_v_, the central density {rho}_c_ and the mass M_N_ and radius R_N_ of the nucleus are derived. Here the "nucleus" is defined as the region within which stars having a velocity equal to the mean velocity dispersion in space, {sigma}_v_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/81/807#1</TD>
            <TD>2011-09-14T19:02:16Z</TD>
            <TD>#Galaxies#Models#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/81/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/81/807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/81/807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/81/807 [2]</TD>
            <TD>Deprojection of the r^1/4^ law tables (Young, 1976)</TD>
            <TD>A spherical galaxy with reduced surface brightness, J=B({alpha})/B_e_, obeying the r^1/4^ law, logJ=-3.3307 ({alpha}^1/4^-1), where {alpha} is the reduced radius, {alpha}=r/r_e_ (r_e_ is the effective radius), is deprojected to find the corresponding space density, mass, mean density, force, potential, escape velocity, and potential energy at each point in the galaxy. Numerical tabulations to five significant figures are given for 124 points in the range 10^-6^&lt;=R/r_e_&lt;=260. In addition the projected surface brightness B({alpha}) and integrated luminosity within {alpha} are tabulated for the range 10^-6^&lt;={alpha}=r/r_e_&lt;=260. Conversion factors to cgs units and to M_{sun}_, pc, km/s, L_{sun}_ units are given. Asymptotic expansions for the space density {rho}(s) in the ranges s=&lt;10^-4^ and s&gt;=10^-1^ are derived, and it is demonstrated that the projection of the expansion for s&lt;=10^-1^ is almost indistinguishable from the r^1/4^ law itself, apart from a small excess of luminosity in the central regions. Formulae and numerical tables of the luminosity distribution are given for use in galaxy photometry. Relations between the total galactic mass M_T_, the effective radius r_e_, the velocity dispersion {sigma}_v_, the central density {rho}_c_ and the mass M_N_ and radius R_N_ of the nucleus are derived. Here the "nucleus" is defined as the region within which stars having a velocity equal to the mean velocity dispersion in space, {sigma}_v_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/81/807#2</TD>
            <TD>2011-09-14T19:02:16Z</TD>
            <TD>#Galaxies#Models#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/81/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/81/807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/81/807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/81/807 [1]</TD>
            <TD>Deprojection of the r^1/4^ law tables (Young, 1976)</TD>
            <TD>A spherical galaxy with reduced surface brightness, J=B({alpha})/B_e_, obeying the r^1/4^ law, logJ=-3.3307 ({alpha}^1/4^-1), where {alpha} is the reduced radius, {alpha}=r/r_e_ (r_e_ is the effective radius), is deprojected to find the corresponding space density, mass, mean density, force, potential, escape velocity, and potential energy at each point in the galaxy. Numerical tabulations to five significant figures are given for 124 points in the range 10^-6^&lt;=R/r_e_&lt;=260. In addition the projected surface brightness B({alpha}) and integrated luminosity within {alpha} are tabulated for the range 10^-6^&lt;={alpha}=r/r_e_&lt;=260. Conversion factors to cgs units and to M_{sun}_, pc, km/s, L_{sun}_ units are given. Asymptotic expansions for the space density {rho}(s) in the ranges s=&lt;10^-4^ and s&gt;=10^-1^ are derived, and it is demonstrated that the projection of the expansion for s&lt;=10^-1^ is almost indistinguishable from the r^1/4^ law itself, apart from a small excess of luminosity in the central regions. Formulae and numerical tables of the luminosity distribution are given for use in galaxy photometry. Relations between the total galactic mass M_T_, the effective radius r_e_, the velocity dispersion {sigma}_v_, the central density {rho}_c_ and the mass M_N_ and radius R_N_ of the nucleus are derived. Here the "nucleus" is defined as the region within which stars having a velocity equal to the mean velocity dispersion in space, {sigma}_v_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/81/807#1</TD>
            <TD>2011-09-14T19:02:16Z</TD>
            <TD>#Galaxies#Models#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/81/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/81/807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/81/807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/81/807 [2]</TD>
            <TD>Deprojection of the r^1/4^ law tables (Young, 1976)</TD>
            <TD>A spherical galaxy with reduced surface brightness, J=B({alpha})/B_e_, obeying the r^1/4^ law, logJ=-3.3307 ({alpha}^1/4^-1), where {alpha} is the reduced radius, {alpha}=r/r_e_ (r_e_ is the effective radius), is deprojected to find the corresponding space density, mass, mean density, force, potential, escape velocity, and potential energy at each point in the galaxy. Numerical tabulations to five significant figures are given for 124 points in the range 10^-6^&lt;=R/r_e_&lt;=260. In addition the projected surface brightness B({alpha}) and integrated luminosity within {alpha} are tabulated for the range 10^-6^&lt;={alpha}=r/r_e_&lt;=260. Conversion factors to cgs units and to M_{sun}_, pc, km/s, L_{sun}_ units are given. Asymptotic expansions for the space density {rho}(s) in the ranges s=&lt;10^-4^ and s&gt;=10^-1^ are derived, and it is demonstrated that the projection of the expansion for s&lt;=10^-1^ is almost indistinguishable from the r^1/4^ law itself, apart from a small excess of luminosity in the central regions. Formulae and numerical tables of the luminosity distribution are given for use in galaxy photometry. Relations between the total galactic mass M_T_, the effective radius r_e_, the velocity dispersion {sigma}_v_, the central density {rho}_c_ and the mass M_N_ and radius R_N_ of the nucleus are derived. Here the "nucleus" is defined as the region within which stars having a velocity equal to the mean velocity dispersion in space, {sigma}_v_.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/81/807#2</TD>
            <TD>2011-09-14T19:02:16Z</TD>
            <TD>#Galaxies#Models#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/81/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/81/807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/81/807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VI/31 [1]</TD>
            <TD>Plate Centers, Epochs Lick/Mt. John Sky Survey (Lick Obs. 1965)</TD>
            <TD>The "Lick Observatory Sky Atlas" (Lick Observatory, 1965) is a set of plates for 166 fields of 18 by 18 degrees, covering the sky from the north pole down to -30 degrees of declination. "The Mount John University Observatory Photographic Sky Survey" (Doughty et al., 1972) covers 142 similar fields from -15 degrees of declination down to the south pole. In the region of overlap, the fields are the same for the two surveys. Fields 1-46 of the Mount John survey cover the part of the sky (-45 degrees of declination to the south pole) not in the Lick survey; in a special limited edition published in 1972, this part is called the "Canterbury Sky Atlas" (Australia). The overlap between fields is 3 degrees. The plate scale is approximately 232 arc seconds per millimeter. The limiting magnitude is approximately 16. Neither survey is intended for astrometry or photometry; the Lick survey was originally done to obtain galaxy statistics (Shane and Wirtanen 1967). An excellent summary of several photographic sky surveys is given by Ingrao and Kasparian (1967). T. A. Nagy (1980) generated the dataset described, and also gathered most of the material used in the writing of this document.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VI/31#1</TD>
            <TD>2011-09-14T18:38:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VI/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VI/31</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/31</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VI/31 [2]</TD>
            <TD>Plate Centers, Epochs Lick/Mt. John Sky Survey (Lick Obs. 1965)</TD>
            <TD>The "Lick Observatory Sky Atlas" (Lick Observatory, 1965) is a set of plates for 166 fields of 18 by 18 degrees, covering the sky from the north pole down to -30 degrees of declination. "The Mount John University Observatory Photographic Sky Survey" (Doughty et al., 1972) covers 142 similar fields from -15 degrees of declination down to the south pole. In the region of overlap, the fields are the same for the two surveys. Fields 1-46 of the Mount John survey cover the part of the sky (-45 degrees of declination to the south pole) not in the Lick survey; in a special limited edition published in 1972, this part is called the "Canterbury Sky Atlas" (Australia). The overlap between fields is 3 degrees. The plate scale is approximately 232 arc seconds per millimeter. The limiting magnitude is approximately 16. Neither survey is intended for astrometry or photometry; the Lick survey was originally done to obtain galaxy statistics (Shane and Wirtanen 1967). An excellent summary of several photographic sky surveys is given by Ingrao and Kasparian (1967). T. A. Nagy (1980) generated the dataset described, and also gathered most of the material used in the writing of this document.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VI/31#2</TD>
            <TD>2011-09-14T18:38:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VI/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VI/31&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/31</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VI/31 [data]</TD>
            <TD>Plate Centers, Epochs Lick/Mt. John Sky Survey (Lick Obs. 1965)</TD>
            <TD>The "Lick Observatory Sky Atlas" (Lick Observatory, 1965) is a set of plates for 166 fields of 18 by 18 degrees, covering the sky from the north pole down to -30 degrees of declination. "The Mount John University Observatory Photographic Sky Survey" (Doughty et al., 1972) covers 142 similar fields from -15 degrees of declination down to the south pole. In the region of overlap, the fields are the same for the two surveys. Fields 1-46 of the Mount John survey cover the part of the sky (-45 degrees of declination to the south pole) not in the Lick survey; in a special limited edition published in 1972, this part is called the "Canterbury Sky Atlas" (Australia). The overlap between fields is 3 degrees. The plate scale is approximately 232 arc seconds per millimeter. The limiting magnitude is approximately 16. Neither survey is intended for astrometry or photometry; the Lick survey was originally done to obtain galaxy statistics (Shane and Wirtanen 1967). An excellent summary of several photographic sky surveys is given by Ingrao and Kasparian (1967). T. A. Nagy (1980) generated the dataset described, and also gathered most of the material used in the writing of this document.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VI/31#data</TD>
            <TD>2011-09-14T18:38:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VI/31</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VI/31&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/31</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/358/819 [1]</TD>
            <TD>BVR photometry of tidal dwarf candidates (Weilbacher+, 2000)</TD>
            <TD>The table gives the colors from the optical photometry of all objects marked on the identification charts in the tails of 10 interacting systems, among them several tidal dwarf galaxy candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/358/819#1</TD>
            <TD>2011-09-14T19:02:20Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/358/819</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/358/819</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/358/819</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/358/819 [2]</TD>
            <TD>BVR photometry of tidal dwarf candidates (Weilbacher+, 2000)</TD>
            <TD>The table gives the colors from the optical photometry of all objects marked on the identification charts in the tails of 10 interacting systems, among them several tidal dwarf galaxy candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/358/819#2</TD>
            <TD>2011-09-14T19:02:20Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/358/819</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/358/819&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/358/819</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/358/819 [1]</TD>
            <TD>BVR photometry of tidal dwarf candidates (Weilbacher+, 2000)</TD>
            <TD>The table gives the colors from the optical photometry of all objects marked on the identification charts in the tails of 10 interacting systems, among them several tidal dwarf galaxy candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/358/819#1</TD>
            <TD>2011-09-14T19:02:20Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/358/819</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/358/819</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/358/819</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/358/819 [2]</TD>
            <TD>BVR photometry of tidal dwarf candidates (Weilbacher+, 2000)</TD>
            <TD>The table gives the colors from the optical photometry of all objects marked on the identification charts in the tails of 10 interacting systems, among them several tidal dwarf galaxy candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/358/819#2</TD>
            <TD>2011-09-14T19:02:20Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/358/819</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/358/819&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/358/819</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/359/597 [1]</TD>
            <TD>Photometry of SX Phe stars in globular clusters (Rodriguez+, 2000)</TD>
            <TD>We present for the first time a catalogue of SX Phe-type pulsating variables in globular clusters. In addition, SX Phe variables discovered in the Carina dwarf galaxy and other ones probably belonging to the Sagittarius dwarf galaxy are included. This catalogue is intended to be an up-dated list of all the SX Phe stars, in globular clusters and galaxies, known until now, covering information published up to January, 2000. In summary, 149 variables are presented in our list for SX Phe-type variables belonging to 18 globular clusters and 2 galaxies. Some relevant distributions are also shown. The analysis of metal abundances and mean periods shows that both parameters are correlated in the sense that the periods of the variables are longer as the metallicity of the stellar system is higher.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597#1</TD>
            <TD>2011-09-14T19:03:04Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/359/597</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/597</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/359/597 [2]</TD>
            <TD>Photometry of SX Phe stars in globular clusters (Rodriguez+, 2000)</TD>
            <TD>We present for the first time a catalogue of SX Phe-type pulsating variables in globular clusters. In addition, SX Phe variables discovered in the Carina dwarf galaxy and other ones probably belonging to the Sagittarius dwarf galaxy are included. This catalogue is intended to be an up-dated list of all the SX Phe stars, in globular clusters and galaxies, known until now, covering information published up to January, 2000. In summary, 149 variables are presented in our list for SX Phe-type variables belonging to 18 globular clusters and 2 galaxies. Some relevant distributions are also shown. The analysis of metal abundances and mean periods shows that both parameters are correlated in the sense that the periods of the variables are longer as the metallicity of the stellar system is higher.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597#2</TD>
            <TD>2011-09-14T19:03:04Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/359/597&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/597</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/359/597 [1]</TD>
            <TD>Photometry of SX Phe stars in globular clusters (Rodriguez+, 2000)</TD>
            <TD>We present for the first time a catalogue of SX Phe-type pulsating variables in globular clusters. In addition, SX Phe variables discovered in the Carina dwarf galaxy and other ones probably belonging to the Sagittarius dwarf galaxy are included. This catalogue is intended to be an up-dated list of all the SX Phe stars, in globular clusters and galaxies, known until now, covering information published up to January, 2000. In summary, 149 variables are presented in our list for SX Phe-type variables belonging to 18 globular clusters and 2 galaxies. Some relevant distributions are also shown. The analysis of metal abundances and mean periods shows that both parameters are correlated in the sense that the periods of the variables are longer as the metallicity of the stellar system is higher.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597#1</TD>
            <TD>2011-09-14T19:03:04Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/359/597</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/597</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/359/597 [2]</TD>
            <TD>Photometry of SX Phe stars in globular clusters (Rodriguez+, 2000)</TD>
            <TD>We present for the first time a catalogue of SX Phe-type pulsating variables in globular clusters. In addition, SX Phe variables discovered in the Carina dwarf galaxy and other ones probably belonging to the Sagittarius dwarf galaxy are included. This catalogue is intended to be an up-dated list of all the SX Phe stars, in globular clusters and galaxies, known until now, covering information published up to January, 2000. In summary, 149 variables are presented in our list for SX Phe-type variables belonging to 18 globular clusters and 2 galaxies. Some relevant distributions are also shown. The analysis of metal abundances and mean periods shows that both parameters are correlated in the sense that the periods of the variables are longer as the metallicity of the stellar system is higher.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597#2</TD>
            <TD>2011-09-14T19:03:04Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/359/597&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/597</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VI/31 [1]</TD>
            <TD>Plate Centers, Epochs Lick/Mt. John Sky Survey (Lick Obs. 1965)</TD>
            <TD>The "Lick Observatory Sky Atlas" (Lick Observatory, 1965) is a set of plates for 166 fields of 18 by 18 degrees, covering the sky from the north pole down to -30 degrees of declination. "The Mount John University Observatory Photographic Sky Survey" (Doughty et al., 1972) covers 142 similar fields from -15 degrees of declination down to the south pole. In the region of overlap, the fields are the same for the two surveys. Fields 1-46 of the Mount John survey cover the part of the sky (-45 degrees of declination to the south pole) not in the Lick survey; in a special limited edition published in 1972, this part is called the "Canterbury Sky Atlas" (Australia). The overlap between fields is 3 degrees. The plate scale is approximately 232 arc seconds per millimeter. The limiting magnitude is approximately 16. Neither survey is intended for astrometry or photometry; the Lick survey was originally done to obtain galaxy statistics (Shane and Wirtanen 1967). An excellent summary of several photographic sky surveys is given by Ingrao and Kasparian (1967). T. A. Nagy (1980) generated the dataset described, and also gathered most of the material used in the writing of this document.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VI/31#1</TD>
            <TD>2011-09-14T18:38:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VI/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VI/31</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/31</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VI/31 [2]</TD>
            <TD>Plate Centers, Epochs Lick/Mt. John Sky Survey (Lick Obs. 1965)</TD>
            <TD>The "Lick Observatory Sky Atlas" (Lick Observatory, 1965) is a set of plates for 166 fields of 18 by 18 degrees, covering the sky from the north pole down to -30 degrees of declination. "The Mount John University Observatory Photographic Sky Survey" (Doughty et al., 1972) covers 142 similar fields from -15 degrees of declination down to the south pole. In the region of overlap, the fields are the same for the two surveys. Fields 1-46 of the Mount John survey cover the part of the sky (-45 degrees of declination to the south pole) not in the Lick survey; in a special limited edition published in 1972, this part is called the "Canterbury Sky Atlas" (Australia). The overlap between fields is 3 degrees. The plate scale is approximately 232 arc seconds per millimeter. The limiting magnitude is approximately 16. Neither survey is intended for astrometry or photometry; the Lick survey was originally done to obtain galaxy statistics (Shane and Wirtanen 1967). An excellent summary of several photographic sky surveys is given by Ingrao and Kasparian (1967). T. A. Nagy (1980) generated the dataset described, and also gathered most of the material used in the writing of this document.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VI/31#2</TD>
            <TD>2011-09-14T18:38:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VI/31</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VI/31&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/31</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VI/31 [data]</TD>
            <TD>Plate Centers, Epochs Lick/Mt. John Sky Survey (Lick Obs. 1965)</TD>
            <TD>The "Lick Observatory Sky Atlas" (Lick Observatory, 1965) is a set of plates for 166 fields of 18 by 18 degrees, covering the sky from the north pole down to -30 degrees of declination. "The Mount John University Observatory Photographic Sky Survey" (Doughty et al., 1972) covers 142 similar fields from -15 degrees of declination down to the south pole. In the region of overlap, the fields are the same for the two surveys. Fields 1-46 of the Mount John survey cover the part of the sky (-45 degrees of declination to the south pole) not in the Lick survey; in a special limited edition published in 1972, this part is called the "Canterbury Sky Atlas" (Australia). The overlap between fields is 3 degrees. The plate scale is approximately 232 arc seconds per millimeter. The limiting magnitude is approximately 16. Neither survey is intended for astrometry or photometry; the Lick survey was originally done to obtain galaxy statistics (Shane and Wirtanen 1967). An excellent summary of several photographic sky surveys is given by Ingrao and Kasparian (1967). T. A. Nagy (1980) generated the dataset described, and also gathered most of the material used in the writing of this document.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VI/31#data</TD>
            <TD>2011-09-14T18:38:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Aug-1995</TD>
            <TD>ivo://CDS.VizieR/VI/31</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VI/31&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/31</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/359/597 [1]</TD>
            <TD>Photometry of SX Phe stars in globular clusters (Rodriguez+, 2000)</TD>
            <TD>We present for the first time a catalogue of SX Phe-type pulsating variables in globular clusters. In addition, SX Phe variables discovered in the Carina dwarf galaxy and other ones probably belonging to the Sagittarius dwarf galaxy are included. This catalogue is intended to be an up-dated list of all the SX Phe stars, in globular clusters and galaxies, known until now, covering information published up to January, 2000. In summary, 149 variables are presented in our list for SX Phe-type variables belonging to 18 globular clusters and 2 galaxies. Some relevant distributions are also shown. The analysis of metal abundances and mean periods shows that both parameters are correlated in the sense that the periods of the variables are longer as the metallicity of the stellar system is higher.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597#1</TD>
            <TD>2011-09-14T19:03:04Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/359/597</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/597</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/359/597 [2]</TD>
            <TD>Photometry of SX Phe stars in globular clusters (Rodriguez+, 2000)</TD>
            <TD>We present for the first time a catalogue of SX Phe-type pulsating variables in globular clusters. In addition, SX Phe variables discovered in the Carina dwarf galaxy and other ones probably belonging to the Sagittarius dwarf galaxy are included. This catalogue is intended to be an up-dated list of all the SX Phe stars, in globular clusters and galaxies, known until now, covering information published up to January, 2000. In summary, 149 variables are presented in our list for SX Phe-type variables belonging to 18 globular clusters and 2 galaxies. Some relevant distributions are also shown. The analysis of metal abundances and mean periods shows that both parameters are correlated in the sense that the periods of the variables are longer as the metallicity of the stellar system is higher.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597#2</TD>
            <TD>2011-09-14T19:03:04Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>19-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/359/597</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/359/597&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/359/597</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/296/839 [1]</TD>
            <TD>Phoenix Deep Survey: 1.4-GHz source counts (Hopkins+, 1998)</TD>
            <TD>We present the first results from the Phoenix Deep Survey, a multiwavelength survey of a 2 deg diameter region. Observations in the radio continuum at 1.4 GHz carried out with the Australia Telescope Compact Array are described. The catalogue of over 1000 radio sources compiled from these observations is analyzed, and the source counts are presented. We model the observational source counts using a two-population model and published luminosity functions for these populations. Upon invoking luminosity and density evolution, we find that a luminosity evolution model best fits the radio observations, consistent with earlier work. The redshift distribution of the two galaxy populations investigated is also modeled and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839#1</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/296/839</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/839</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/296/839 [2]</TD>
            <TD>Phoenix Deep Survey: 1.4-GHz source counts (Hopkins+, 1998)</TD>
            <TD>We present the first results from the Phoenix Deep Survey, a multiwavelength survey of a 2 deg diameter region. Observations in the radio continuum at 1.4 GHz carried out with the Australia Telescope Compact Array are described. The catalogue of over 1000 radio sources compiled from these observations is analyzed, and the source counts are presented. We model the observational source counts using a two-population model and published luminosity functions for these populations. Upon invoking luminosity and density evolution, we find that a luminosity evolution model best fits the radio observations, consistent with earlier work. The redshift distribution of the two galaxy populations investigated is also modeled and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839#2</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/296/839&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/839</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/296/839 [pdf]</TD>
            <TD>Phoenix Deep Survey: 1.4-GHz source counts (Hopkins+, 1998)</TD>
            <TD>We present the first results from the Phoenix Deep Survey, a multiwavelength survey of a 2 deg diameter region. Observations in the radio continuum at 1.4 GHz carried out with the Australia Telescope Compact Array are described. The catalogue of over 1000 radio sources compiled from these observations is analyzed, and the source counts are presented. We model the observational source counts using a two-population model and published luminosity functions for these populations. Upon invoking luminosity and density evolution, we find that a luminosity evolution model best fits the radio observations, consistent with earlier work. The redshift distribution of the two galaxy populations investigated is also modeled and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839#pdf</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/296/839&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/839</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/296/839 [1]</TD>
            <TD>Phoenix Deep Survey: 1.4-GHz source counts (Hopkins+, 1998)</TD>
            <TD>We present the first results from the Phoenix Deep Survey, a multiwavelength survey of a 2 deg diameter region. Observations in the radio continuum at 1.4 GHz carried out with the Australia Telescope Compact Array are described. The catalogue of over 1000 radio sources compiled from these observations is analyzed, and the source counts are presented. We model the observational source counts using a two-population model and published luminosity functions for these populations. Upon invoking luminosity and density evolution, we find that a luminosity evolution model best fits the radio observations, consistent with earlier work. The redshift distribution of the two galaxy populations investigated is also modeled and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839#1</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/296/839</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/839</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/296/839 [2]</TD>
            <TD>Phoenix Deep Survey: 1.4-GHz source counts (Hopkins+, 1998)</TD>
            <TD>We present the first results from the Phoenix Deep Survey, a multiwavelength survey of a 2 deg diameter region. Observations in the radio continuum at 1.4 GHz carried out with the Australia Telescope Compact Array are described. The catalogue of over 1000 radio sources compiled from these observations is analyzed, and the source counts are presented. We model the observational source counts using a two-population model and published luminosity functions for these populations. Upon invoking luminosity and density evolution, we find that a luminosity evolution model best fits the radio observations, consistent with earlier work. The redshift distribution of the two galaxy populations investigated is also modeled and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839#2</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/296/839&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/839</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/296/839 [pdf]</TD>
            <TD>Phoenix Deep Survey: 1.4-GHz source counts (Hopkins+, 1998)</TD>
            <TD>We present the first results from the Phoenix Deep Survey, a multiwavelength survey of a 2 deg diameter region. Observations in the radio continuum at 1.4 GHz carried out with the Australia Telescope Compact Array are described. The catalogue of over 1000 radio sources compiled from these observations is analyzed, and the source counts are presented. We model the observational source counts using a two-population model and published luminosity functions for these populations. Upon invoking luminosity and density evolution, we find that a luminosity evolution model best fits the radio observations, consistent with earlier work. The redshift distribution of the two galaxy populations investigated is also modeled and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839#pdf</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/296/839&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/839</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/296/839 [1]</TD>
            <TD>Phoenix Deep Survey: 1.4-GHz source counts (Hopkins+, 1998)</TD>
            <TD>We present the first results from the Phoenix Deep Survey, a multiwavelength survey of a 2 deg diameter region. Observations in the radio continuum at 1.4 GHz carried out with the Australia Telescope Compact Array are described. The catalogue of over 1000 radio sources compiled from these observations is analyzed, and the source counts are presented. We model the observational source counts using a two-population model and published luminosity functions for these populations. Upon invoking luminosity and density evolution, we find that a luminosity evolution model best fits the radio observations, consistent with earlier work. The redshift distribution of the two galaxy populations investigated is also modeled and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839#1</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/296/839</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/839</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/296/839 [2]</TD>
            <TD>Phoenix Deep Survey: 1.4-GHz source counts (Hopkins+, 1998)</TD>
            <TD>We present the first results from the Phoenix Deep Survey, a multiwavelength survey of a 2 deg diameter region. Observations in the radio continuum at 1.4 GHz carried out with the Australia Telescope Compact Array are described. The catalogue of over 1000 radio sources compiled from these observations is analyzed, and the source counts are presented. We model the observational source counts using a two-population model and published luminosity functions for these populations. Upon invoking luminosity and density evolution, we find that a luminosity evolution model best fits the radio observations, consistent with earlier work. The redshift distribution of the two galaxy populations investigated is also modeled and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839#2</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/296/839&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/839</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/296/839 [pdf]</TD>
            <TD>Phoenix Deep Survey: 1.4-GHz source counts (Hopkins+, 1998)</TD>
            <TD>We present the first results from the Phoenix Deep Survey, a multiwavelength survey of a 2 deg diameter region. Observations in the radio continuum at 1.4 GHz carried out with the Australia Telescope Compact Array are described. The catalogue of over 1000 radio sources compiled from these observations is analyzed, and the source counts are presented. We model the observational source counts using a two-population model and published luminosity functions for these populations. Upon invoking luminosity and density evolution, we find that a luminosity evolution model best fits the radio observations, consistent with earlier work. The redshift distribution of the two galaxy populations investigated is also modeled and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839#pdf</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/839</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/296/839&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/839</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/534/114 [1]</TD>
            <TD>RASSCALS: X-ray and optical study (Mahdavi+, 2000)</TD>
            <TD>We describe the ROSAT All-Sky Survey Center for Astrophysics Loose Systems (RASSCALS), the largest X-ray and optical survey of low-mass galaxy groups to date. We draw 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z_=15.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114#1</TD>
            <TD>2011-09-14T19:04:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/534/114</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/534/114</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/534/114 [2]</TD>
            <TD>RASSCALS: X-ray and optical study (Mahdavi+, 2000)</TD>
            <TD>We describe the ROSAT All-Sky Survey Center for Astrophysics Loose Systems (RASSCALS), the largest X-ray and optical survey of low-mass galaxy groups to date. We draw 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z_=15.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114#2</TD>
            <TD>2011-09-14T19:04:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/534/114&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/534/114</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/534/114 [table2]</TD>
            <TD>RASSCALS: X-ray and optical study (Mahdavi+, 2000)</TD>
            <TD>We describe the ROSAT All-Sky Survey Center for Astrophysics Loose Systems (RASSCALS), the largest X-ray and optical survey of low-mass galaxy groups to date. We draw 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z_=15.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114#table2</TD>
            <TD>2011-09-14T19:04:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/534/114&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/534/114</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/534/114 [1]</TD>
            <TD>RASSCALS: X-ray and optical study (Mahdavi+, 2000)</TD>
            <TD>We describe the ROSAT All-Sky Survey Center for Astrophysics Loose Systems (RASSCALS), the largest X-ray and optical survey of low-mass galaxy groups to date. We draw 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z_=15.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114#1</TD>
            <TD>2011-09-14T19:04:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/534/114</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/534/114</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/534/114 [2]</TD>
            <TD>RASSCALS: X-ray and optical study (Mahdavi+, 2000)</TD>
            <TD>We describe the ROSAT All-Sky Survey Center for Astrophysics Loose Systems (RASSCALS), the largest X-ray and optical survey of low-mass galaxy groups to date. We draw 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z_=15.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114#2</TD>
            <TD>2011-09-14T19:04:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/534/114&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/534/114</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/534/114 [table2]</TD>
            <TD>RASSCALS: X-ray and optical study (Mahdavi+, 2000)</TD>
            <TD>We describe the ROSAT All-Sky Survey Center for Astrophysics Loose Systems (RASSCALS), the largest X-ray and optical survey of low-mass galaxy groups to date. We draw 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z_=15.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114#table2</TD>
            <TD>2011-09-14T19:04:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/534/114&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/534/114</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/534/114 [1]</TD>
            <TD>RASSCALS: X-ray and optical study (Mahdavi+, 2000)</TD>
            <TD>We describe the ROSAT All-Sky Survey Center for Astrophysics Loose Systems (RASSCALS), the largest X-ray and optical survey of low-mass galaxy groups to date. We draw 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z_=15.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114#1</TD>
            <TD>2011-09-14T19:04:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/534/114</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/534/114</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/534/114 [2]</TD>
            <TD>RASSCALS: X-ray and optical study (Mahdavi+, 2000)</TD>
            <TD>We describe the ROSAT All-Sky Survey Center for Astrophysics Loose Systems (RASSCALS), the largest X-ray and optical survey of low-mass galaxy groups to date. We draw 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z_=15.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114#2</TD>
            <TD>2011-09-14T19:04:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/534/114&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/534/114</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/534/114 [table2]</TD>
            <TD>RASSCALS: X-ray and optical study (Mahdavi+, 2000)</TD>
            <TD>We describe the ROSAT All-Sky Survey Center for Astrophysics Loose Systems (RASSCALS), the largest X-ray and optical survey of low-mass galaxy groups to date. We draw 260 groups from the combined Center for Astrophysics and Southern Sky Redshift Surveys, covering one-quarter of the sky to a limiting Zwicky magnitude of m_z_=15.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114#table2</TD>
            <TD>2011-09-14T19:04:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/534/114</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/534/114&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/534/114</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/172 [1]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/VII/172#1</TD>
            <TD>2011-09-14T18:39:00Z</TD>
            <TD>#Galaxies#Galaxies:Markarian#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/VII/172</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/172</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/172</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/172 [2]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/VII/172#2</TD>
            <TD>2011-09-14T18:39:00Z</TD>
            <TD>#Galaxies#Galaxies:Markarian#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/VII/172</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/172&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/172</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/172 [table6]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/VII/172#table6</TD>
            <TD>2011-09-14T18:39:00Z</TD>
            <TD>#Galaxies#Galaxies:Markarian#</TD>
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            <TD>20-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/VII/172</TD>
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/172&amp;</TD>
            <TD>180</TD>
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            <TD>Catalog</TD>
            <TD>VII/172 [table7]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/VII/172#table7</TD>
            <TD>2011-09-14T18:39:00Z</TD>
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            <TD>20-Oct-1997</TD>
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            <TD>180</TD>
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            <TD>Web Page</TD>
            <TD>J/A+AS/94/327 [1]</TD>
            <TD>Nearby clusters of galaxies. I. (Trevese+, 1992)</TD>
            <TD>A study of the properties of nearby clusters of galaxies has been undertaken. This paper describes the data, derived from automated scans of photographic plates. Different methods for the evaluation of cluster center, ellipticity and orientation are compared and errors are estimated by Monte Carlo simulations. We present the results of the analysis of 1256 galaxies brighter than m_3_+3 in eight Abell clusters. We find that different methods give consistent estimates of ellipticity and orientation, provided the radial dependence of these quantities is taken into account. We also find that central densities are consistent with isothermal fits if the center is selected as the baricenter of the cluster. For each galaxy, rectangular coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide identification maps and contour maps of galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/94/327#1</TD>
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            <TD>21-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/94/327</TD>
            <TD />
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            <TD />
            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/94/327</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/94/327</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/94/327 [2]</TD>
            <TD>Nearby clusters of galaxies. I. (Trevese+, 1992)</TD>
            <TD>A study of the properties of nearby clusters of galaxies has been undertaken. This paper describes the data, derived from automated scans of photographic plates. Different methods for the evaluation of cluster center, ellipticity and orientation are compared and errors are estimated by Monte Carlo simulations. We present the results of the analysis of 1256 galaxies brighter than m_3_+3 in eight Abell clusters. We find that different methods give consistent estimates of ellipticity and orientation, provided the radial dependence of these quantities is taken into account. We also find that central densities are consistent with isothermal fits if the center is selected as the baricenter of the cluster. For each galaxy, rectangular coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide identification maps and contour maps of galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/94/327#2</TD>
            <TD>2011-09-14T19:04:11Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
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            <TD>21-Nov-1994</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/94/327</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>VII/172 [1]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/VII/172#1</TD>
            <TD>2011-09-14T18:39:00Z</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/172</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/172 [2]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
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            <TD>Catalog</TD>
            <TD>VII/172 [table6]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/VII/172#table6</TD>
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            <TD>Catalog</TD>
            <TD>VII/172 [table7]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
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            <TD>20-Oct-1997</TD>
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            <TD />
            <TD>ParamHTTP</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/94/327 [1]</TD>
            <TD>Nearby clusters of galaxies. I. (Trevese+, 1992)</TD>
            <TD>A study of the properties of nearby clusters of galaxies has been undertaken. This paper describes the data, derived from automated scans of photographic plates. Different methods for the evaluation of cluster center, ellipticity and orientation are compared and errors are estimated by Monte Carlo simulations. We present the results of the analysis of 1256 galaxies brighter than m_3_+3 in eight Abell clusters. We find that different methods give consistent estimates of ellipticity and orientation, provided the radial dependence of these quantities is taken into account. We also find that central densities are consistent with isothermal fits if the center is selected as the baricenter of the cluster. For each galaxy, rectangular coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide identification maps and contour maps of galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS.VizieR/J/A+AS/94/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/94/327</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/94/327</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/94/327 [2]</TD>
            <TD>Nearby clusters of galaxies. I. (Trevese+, 1992)</TD>
            <TD>A study of the properties of nearby clusters of galaxies has been undertaken. This paper describes the data, derived from automated scans of photographic plates. Different methods for the evaluation of cluster center, ellipticity and orientation are compared and errors are estimated by Monte Carlo simulations. We present the results of the analysis of 1256 galaxies brighter than m_3_+3 in eight Abell clusters. We find that different methods give consistent estimates of ellipticity and orientation, provided the radial dependence of these quantities is taken into account. We also find that central densities are consistent with isothermal fits if the center is selected as the baricenter of the cluster. For each galaxy, rectangular coordinates, magnitude, size, ellipticity and orientation are given. For each cluster we provide identification maps and contour maps of galaxy surface density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/94/327#2</TD>
            <TD>2011-09-14T19:04:11Z</TD>
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            <TD>21-Nov-1994</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>VII/172 [1]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/VII/172#1</TD>
            <TD>2011-09-14T18:39:00Z</TD>
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            <TD>20-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/VII/172</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/172</TD>
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            <TD>ivo://CDS</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/172 [2]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
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            <TD>ParamHTTP</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>VII/172 [table6]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/VII/172#table6</TD>
            <TD>2011-09-14T18:39:00Z</TD>
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            <TD>#Research#</TD>
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            <TD>20-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/VII/172</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/172&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/172</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/172 [table7]</TD>
            <TD>First Byurakan Survey (FBS) (Markarian+, 1989)</TD>
            <TD>A Catalogue of galaxies with UV-continuum (Markarian galaxies) detected during the First Byurakan Survey (FBS) is presented. The purpose of the Survey was to search for peculiar faint extragalactic objects with UV-excess radiation and to study them. The procedure of observations and processings, the Survey areas, the object selection and classification criteria and also several selection effects are described. The Catalogue contains the following initial data on all the objects: the precise coordinates, visual magnitudes, angular sizes, redshifts and classification types. The observational results of slit spectra, UBV-photometry, IR-photometry (IRAS data), morphology and some other data are also included into the Catalogue. While compiling the Catalogue the authors introduced some necessary corrections in the data of the earlier published lists on galaxies with UV-continuum. In addition we included the objects with numbers 1501-1515. In most cases they are well-known Seyfert galaxies omitted by the authors in the lists, but detected on the plates. 41 objects from our lists are not included into the Catalogue, since they are either stars of our Galaxy or star projections on the galaxies. The Catalogue presents the largest homogeneous sample of AGN of different types on the northern sky for bright objects (&lt;16.0). Up to the middle of 1987 the redshifts were measured for 1459 out of 1469 objects of the Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/VII/172#table7</TD>
            <TD>2011-09-14T18:39:00Z</TD>
            <TD>#Galaxies#Galaxies:Markarian#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/VII/172</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/172&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/172</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/539/136 [1]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#1</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/539/136</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/539/136 [2]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#2</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/539/136&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/539/136 [table2]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#table2</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/539/136&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/539/136 [table1]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#table1</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/539/136&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/175 [1]</TD>
            <TD>Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)</TD>
            <TD>We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaAy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/175#1</TD>
            <TD>2011-09-14T18:39:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VII/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/175</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/175</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/175 [2]</TD>
            <TD>Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)</TD>
            <TD>We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaAy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/175#2</TD>
            <TD>2011-09-14T18:39:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VII/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/175&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/175</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/175 [table3]</TD>
            <TD>Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)</TD>
            <TD>We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaAy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/175#table3</TD>
            <TD>2011-09-14T18:39:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VII/175</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/175&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/175</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/539/136 [1]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#1</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/539/136</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/539/136 [2]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#2</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/539/136&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/539/136 [table2]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#table2</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/539/136&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/539/136 [table1]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#table1</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/539/136&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/175 [1]</TD>
            <TD>Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)</TD>
            <TD>We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaAy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/175#1</TD>
            <TD>2011-09-14T18:39:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VII/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/175</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/175</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/175 [2]</TD>
            <TD>Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)</TD>
            <TD>We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaAy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/175#2</TD>
            <TD>2011-09-14T18:39:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VII/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/175&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/175</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/175 [table3]</TD>
            <TD>Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)</TD>
            <TD>We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaAy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/175#table3</TD>
            <TD>2011-09-14T18:39:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VII/175</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/175&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/175</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/539/136 [1]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#1</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/539/136</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/539/136 [2]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#2</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/539/136&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/539/136 [table2]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#table2</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/539/136&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/539/136 [table1]</TD>
            <TD>Properties of poor groups of galaxies. III. (Zabludoff+, 2000)</TD>
            <TD>The form of the galaxy luminosity function (GLF) in poor groups - regions of intermediate galaxy density that are common environments for galaxies - is not well understood. Multiobject spectroscopy and wide-field CCD imaging now allow us to measure the GLF of bound group members directly (i.e., without statistical background subtraction) and to compare the group GLF with the GLFs of the field and of rich clusters. We use R-band images in 1.5x1.5degree^2^ mosaics to obtain photometry for galaxies in the fields of six nearby (2800&lt;cz&lt;7700km/s) poor groups for which we have extensive spectroscopic data, including 328 new galaxy velocities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136#table1</TD>
            <TD>2011-09-14T19:04:16Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>29-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/539/136</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/539/136&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/539/136</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/118/1671 [1]</TD>
            <TD>Fornax cluster 4 VI photometry (Buonanno+, 1999)</TD>
            <TD>Using observations from the Hubble Space Telescope archive, color-magnitude diagrams (CMDs) have been constructed for globular cluster 4 in the Fornax dwarf spheroidal galaxy and its surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1671#1</TD>
            <TD>2011-09-14T19:04:24Z</TD>
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            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1671</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/118/1671</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1671</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/118/1671 [2]</TD>
            <TD>Fornax cluster 4 VI photometry (Buonanno+, 1999)</TD>
            <TD>Using observations from the Hubble Space Telescope archive, color-magnitude diagrams (CMDs) have been constructed for globular cluster 4 in the Fornax dwarf spheroidal galaxy and its surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1671#2</TD>
            <TD>2011-09-14T19:04:24Z</TD>
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            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1671</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/118/1671&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1671</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/118/1671 [1]</TD>
            <TD>Fornax cluster 4 VI photometry (Buonanno+, 1999)</TD>
            <TD>Using observations from the Hubble Space Telescope archive, color-magnitude diagrams (CMDs) have been constructed for globular cluster 4 in the Fornax dwarf spheroidal galaxy and its surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1671#1</TD>
            <TD>2011-09-14T19:04:24Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1671</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/118/1671</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1671</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/118/1671 [2]</TD>
            <TD>Fornax cluster 4 VI photometry (Buonanno+, 1999)</TD>
            <TD>Using observations from the Hubble Space Telescope archive, color-magnitude diagrams (CMDs) have been constructed for globular cluster 4 in the Fornax dwarf spheroidal galaxy and its surrounding field.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1671#2</TD>
            <TD>2011-09-14T19:04:24Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Nov-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/1671</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/118/1671&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/1671</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/1335 [1]</TD>
            <TD>Hubble Deep Field observations (Williams+ 1996)</TD>
            <TD>The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335#1</TD>
            <TD>2011-09-14T19:04:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/1335</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1335</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/1335 [2]</TD>
            <TD>Hubble Deep Field observations (Williams+ 1996)</TD>
            <TD>The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335#2</TD>
            <TD>2011-09-14T19:04:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/1335&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1335</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/1335 [table7]</TD>
            <TD>Hubble Deep Field observations (Williams+ 1996)</TD>
            <TD>The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335#table7</TD>
            <TD>2011-09-14T19:04:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/1335&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1335</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/1335 [1]</TD>
            <TD>Hubble Deep Field observations (Williams+ 1996)</TD>
            <TD>The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335#1</TD>
            <TD>2011-09-14T19:04:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/1335</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1335</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/1335 [2]</TD>
            <TD>Hubble Deep Field observations (Williams+ 1996)</TD>
            <TD>The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335#2</TD>
            <TD>2011-09-14T19:04:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/1335&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1335</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/1335 [table7]</TD>
            <TD>Hubble Deep Field observations (Williams+ 1996)</TD>
            <TD>The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335#table7</TD>
            <TD>2011-09-14T19:04:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/1335&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1335</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/1335 [1]</TD>
            <TD>Hubble Deep Field observations (Williams+ 1996)</TD>
            <TD>The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335#1</TD>
            <TD>2011-09-14T19:04:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/1335</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1335</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/1335 [2]</TD>
            <TD>Hubble Deep Field observations (Williams+ 1996)</TD>
            <TD>The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335#2</TD>
            <TD>2011-09-14T19:04:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/1335&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1335</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/112/1335 [table7]</TD>
            <TD>Hubble Deep Field observations (Williams+ 1996)</TD>
            <TD>The Hubble Deep Field (HDF) is a Director's Discretionary program on HST in Cycle 5 to image an undistinguished field at high Galactic latitude in four passbands as deeply as reasonably possible. These images provide the most detailed view to date of distant field galaxies and are likely to be important for a wide range of studies in galaxy evolution and cosmology. In order to optimize observing in the time available, a field in the northern continuous viewing zone was selected and images were taken for ten consecutive days, or approximately 150 orbits. Shorter 1-2 orbit images were obtained of the fields immediately adjacent to the primary HDF in order to facilitate spectroscopic follow-up by ground- based telescopes. The observations were made from 1995 December 18-30, and both raw and reduced data have been put in the public domain as a community service. We present a summary of the criteria for selecting the field, the rationale behind the filter selection and observing times in each band, and the strategies for planning the observations to maximize the exposure time while avoiding Earth-scattered light. Data reduction procedures are outlined, and images of the combined frames in each band are presented. Objects detected in these images are listed in a catalog with their basic photometric parameters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335#table7</TD>
            <TD>2011-09-14T19:04:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1335</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/112/1335&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1335</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/129/475 [1]</TD>
            <TD>The CNOC2 survey. I. (Yee+, 2000)</TD>
            <TD>The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475#1</TD>
            <TD>2011-09-14T19:07:10Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/129/475</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/129/475</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/129/475 [2]</TD>
            <TD>The CNOC2 survey. I. (Yee+, 2000)</TD>
            <TD>The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475#2</TD>
            <TD>2011-09-14T19:07:10Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/129/475&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/129/475</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/129/475 [cnoc0223]</TD>
            <TD>The CNOC2 survey. I. (Yee+, 2000)</TD>
            <TD>The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475#cnoc0223</TD>
            <TD>2011-09-14T19:07:10Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/129/475&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/129/475</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/129/475 [1]</TD>
            <TD>The CNOC2 survey. I. (Yee+, 2000)</TD>
            <TD>The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475#1</TD>
            <TD>2011-09-14T19:07:10Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/129/475</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/129/475</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/129/475 [2]</TD>
            <TD>The CNOC2 survey. I. (Yee+, 2000)</TD>
            <TD>The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475#2</TD>
            <TD>2011-09-14T19:07:10Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/129/475&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/129/475</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/129/475 [cnoc0223]</TD>
            <TD>The CNOC2 survey. I. (Yee+, 2000)</TD>
            <TD>The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475#cnoc0223</TD>
            <TD>2011-09-14T19:07:10Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/129/475&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/129/475</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/129/475 [1]</TD>
            <TD>The CNOC2 survey. I. (Yee+, 2000)</TD>
            <TD>The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475#1</TD>
            <TD>2011-09-14T19:07:10Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/129/475</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/129/475</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/129/475 [2]</TD>
            <TD>The CNOC2 survey. I. (Yee+, 2000)</TD>
            <TD>The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475#2</TD>
            <TD>2011-09-14T19:07:10Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/129/475&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/129/475</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/129/475 [cnoc0223]</TD>
            <TD>The CNOC2 survey. I. (Yee+, 2000)</TD>
            <TD>The Canadian Network for Observational Cosmology Field Galaxy Redshift Survey (CNOC2) obtained spectroscopic redshifts for about 6200 galaxies to a nominal limit of R=21.5. The survey area of about 1.5 square degrees was spread over four patches on the sky. This catalog presents photometry and redshifts for all galaxies in the CNOC2 0223+00 Patch (area of 1409 square arcminutes). A future paper will provide catalogs for the other three patches.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475#cnoc0223</TD>
            <TD>2011-09-14T19:07:10Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/129/475</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/129/475&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/129/475</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/546/694 [1]</TD>
            <TD>NICMOS star formation history (Thompson +, 2001)</TD>
            <TD>We present the results of an extensive analysis of the star formation rates determined from the NICMOS deep images of the northern Hubble Deep Field. We use SED template fitting photometric techniques to determine both the redshift and the extinction for each galaxy in our field. Measurement of the individual extinctions provides a correction for star formation hidden by dust obscuration. We determine star formation rates for each galaxy based on the 1500{AA} UV flux and add the rates in redshift bins of width 1.0 centered on integer redshift values.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694#1</TD>
            <TD>2011-09-14T19:08:24Z</TD>
            <TD>#Extinction#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/546/694</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/546/694</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/546/694 [2]</TD>
            <TD>NICMOS star formation history (Thompson +, 2001)</TD>
            <TD>We present the results of an extensive analysis of the star formation rates determined from the NICMOS deep images of the northern Hubble Deep Field. We use SED template fitting photometric techniques to determine both the redshift and the extinction for each galaxy in our field. Measurement of the individual extinctions provides a correction for star formation hidden by dust obscuration. We determine star formation rates for each galaxy based on the 1500{AA} UV flux and add the rates in redshift bins of width 1.0 centered on integer redshift values.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694#2</TD>
            <TD>2011-09-14T19:08:24Z</TD>
            <TD>#Extinction#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/546/694&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/546/694</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/546/694 [table1]</TD>
            <TD>NICMOS star formation history (Thompson +, 2001)</TD>
            <TD>We present the results of an extensive analysis of the star formation rates determined from the NICMOS deep images of the northern Hubble Deep Field. We use SED template fitting photometric techniques to determine both the redshift and the extinction for each galaxy in our field. Measurement of the individual extinctions provides a correction for star formation hidden by dust obscuration. We determine star formation rates for each galaxy based on the 1500{AA} UV flux and add the rates in redshift bins of width 1.0 centered on integer redshift values.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694#table1</TD>
            <TD>2011-09-14T19:08:24Z</TD>
            <TD>#Extinction#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/546/694&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/546/694</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/546/694 [1]</TD>
            <TD>NICMOS star formation history (Thompson +, 2001)</TD>
            <TD>We present the results of an extensive analysis of the star formation rates determined from the NICMOS deep images of the northern Hubble Deep Field. We use SED template fitting photometric techniques to determine both the redshift and the extinction for each galaxy in our field. Measurement of the individual extinctions provides a correction for star formation hidden by dust obscuration. We determine star formation rates for each galaxy based on the 1500{AA} UV flux and add the rates in redshift bins of width 1.0 centered on integer redshift values.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694#1</TD>
            <TD>2011-09-14T19:08:24Z</TD>
            <TD>#Extinction#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/546/694</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/546/694</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/546/694 [2]</TD>
            <TD>NICMOS star formation history (Thompson +, 2001)</TD>
            <TD>We present the results of an extensive analysis of the star formation rates determined from the NICMOS deep images of the northern Hubble Deep Field. We use SED template fitting photometric techniques to determine both the redshift and the extinction for each galaxy in our field. Measurement of the individual extinctions provides a correction for star formation hidden by dust obscuration. We determine star formation rates for each galaxy based on the 1500{AA} UV flux and add the rates in redshift bins of width 1.0 centered on integer redshift values.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694#2</TD>
            <TD>2011-09-14T19:08:24Z</TD>
            <TD>#Extinction#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/546/694&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/546/694</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/546/694 [table1]</TD>
            <TD>NICMOS star formation history (Thompson +, 2001)</TD>
            <TD>We present the results of an extensive analysis of the star formation rates determined from the NICMOS deep images of the northern Hubble Deep Field. We use SED template fitting photometric techniques to determine both the redshift and the extinction for each galaxy in our field. Measurement of the individual extinctions provides a correction for star formation hidden by dust obscuration. We determine star formation rates for each galaxy based on the 1500{AA} UV flux and add the rates in redshift bins of width 1.0 centered on integer redshift values.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694#table1</TD>
            <TD>2011-09-14T19:08:24Z</TD>
            <TD>#Extinction#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/546/694&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/546/694</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/546/694 [1]</TD>
            <TD>NICMOS star formation history (Thompson +, 2001)</TD>
            <TD>We present the results of an extensive analysis of the star formation rates determined from the NICMOS deep images of the northern Hubble Deep Field. We use SED template fitting photometric techniques to determine both the redshift and the extinction for each galaxy in our field. Measurement of the individual extinctions provides a correction for star formation hidden by dust obscuration. We determine star formation rates for each galaxy based on the 1500{AA} UV flux and add the rates in redshift bins of width 1.0 centered on integer redshift values.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694#1</TD>
            <TD>2011-09-14T19:08:24Z</TD>
            <TD>#Extinction#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/546/694</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/546/694</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/546/694 [2]</TD>
            <TD>NICMOS star formation history (Thompson +, 2001)</TD>
            <TD>We present the results of an extensive analysis of the star formation rates determined from the NICMOS deep images of the northern Hubble Deep Field. We use SED template fitting photometric techniques to determine both the redshift and the extinction for each galaxy in our field. Measurement of the individual extinctions provides a correction for star formation hidden by dust obscuration. We determine star formation rates for each galaxy based on the 1500{AA} UV flux and add the rates in redshift bins of width 1.0 centered on integer redshift values.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694#2</TD>
            <TD>2011-09-14T19:08:24Z</TD>
            <TD>#Extinction#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/546/694&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/546/694</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/546/694 [table1]</TD>
            <TD>NICMOS star formation history (Thompson +, 2001)</TD>
            <TD>We present the results of an extensive analysis of the star formation rates determined from the NICMOS deep images of the northern Hubble Deep Field. We use SED template fitting photometric techniques to determine both the redshift and the extinction for each galaxy in our field. Measurement of the individual extinctions provides a correction for star formation hidden by dust obscuration. We determine star formation rates for each galaxy based on the 1500{AA} UV flux and add the rates in redshift bins of width 1.0 centered on integer redshift values.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694#table1</TD>
            <TD>2011-09-14T19:08:24Z</TD>
            <TD>#Extinction#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Mar-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/546/694</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/546/694&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/546/694</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/634/977 [1]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#1</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/634/977</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/634/977 [2]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#2</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/634/977&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/634/977 [table2]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#table2</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/634/977&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/634/977 [members]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#members</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/634/977&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/303/661 [1]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#1</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/303/661</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/303/661 [2]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#2</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/303/661&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/303/661 [table2]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#table2</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/303/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/303/661 [table1]</TD>
            <TD>Star-forming galaxies in the Coma Cluster (Donas+, 1995)</TD>
            <TD>In a field of 1deg radius centered in the Coma cluster of galaxies, UV ({lambda}=2000 A) observations with a 40-cm balloon-borne imaging telescope (FOCA) have provided a list of 442 UV sources brighter than m_UV_=18, which are identified in the Godwin (1983) catalogue. 254 are identified as galaxies, 178 as star-like objects and 10 as galaxy-star pairs, unresolved in the UV image.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661#table1</TD>
            <TD>2011-09-14T18:56:18Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-May-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+A/303/661</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/303/661&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/303/661</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/549/820 [1]</TD>
            <TD>H{alpha} flux of ACCG 114 galaxies (Couch+, 2001)</TD>
            <TD>We present the results of a wide-field survey for H{alpha}-emitting galaxies in the cluster AC 114 at z=0.32. Spectra centered on H{alpha} at the cluster redshift have been obtained for 586 galaxies to I_tot_~22 out to a radius of ~h_50_^-1^Mpc. At most, only ~10% of these were found to be H{alpha}-emitting cluster members. These objects are predominantly blue and of late-type spiral morphology, consistent with them hosting star formation. However, ~65% of the cluster members classified morphologically as spirals (with HST) have no detectable H{alpha} emission; star formation and morphological evolution in cluster galaxies appear to be largely decoupled. Changes in the H{alpha} detection rate and the strength of H{alpha} emission with environment (as traced by local galaxy density) are found to be weak within the region studied. Star formation within the cluster members is also found to be strongly and uniformly suppressed with the rates inferred from the H{alpha} emission not exceeding 4M_{sun}_/yr, and AC 114's H{alpha} luminosity function being an order of magnitude below that observed for field galaxies at the same redshift. None of the galaxies detected have the high star formation rates associated with "starburst" galaxies; however, this may still be reconcilable with the known (8%+/-3%) fraction of "post-starburst" galaxies within AC 114, given the poorly determined but short lifetimes of starbursts and the possibility that much of the associated star formation is obscured by dust.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820#1</TD>
            <TD>2011-09-14T19:08:32Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/549/820</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/820</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/549/820 [2]</TD>
            <TD>H{alpha} flux of ACCG 114 galaxies (Couch+, 2001)</TD>
            <TD>We present the results of a wide-field survey for H{alpha}-emitting galaxies in the cluster AC 114 at z=0.32. Spectra centered on H{alpha} at the cluster redshift have been obtained for 586 galaxies to I_tot_~22 out to a radius of ~h_50_^-1^Mpc. At most, only ~10% of these were found to be H{alpha}-emitting cluster members. These objects are predominantly blue and of late-type spiral morphology, consistent with them hosting star formation. However, ~65% of the cluster members classified morphologically as spirals (with HST) have no detectable H{alpha} emission; star formation and morphological evolution in cluster galaxies appear to be largely decoupled. Changes in the H{alpha} detection rate and the strength of H{alpha} emission with environment (as traced by local galaxy density) are found to be weak within the region studied. Star formation within the cluster members is also found to be strongly and uniformly suppressed with the rates inferred from the H{alpha} emission not exceeding 4M_{sun}_/yr, and AC 114's H{alpha} luminosity function being an order of magnitude below that observed for field galaxies at the same redshift. None of the galaxies detected have the high star formation rates associated with "starburst" galaxies; however, this may still be reconcilable with the known (8%+/-3%) fraction of "post-starburst" galaxies within AC 114, given the poorly determined but short lifetimes of starbursts and the possibility that much of the associated star formation is obscured by dust.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820#2</TD>
            <TD>2011-09-14T19:08:32Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>17-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/549/820&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/820</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/549/820 [table1]</TD>
            <TD>H{alpha} flux of ACCG 114 galaxies (Couch+, 2001)</TD>
            <TD>We present the results of a wide-field survey for H{alpha}-emitting galaxies in the cluster AC 114 at z=0.32. Spectra centered on H{alpha} at the cluster redshift have been obtained for 586 galaxies to I_tot_~22 out to a radius of ~h_50_^-1^Mpc. At most, only ~10% of these were found to be H{alpha}-emitting cluster members. These objects are predominantly blue and of late-type spiral morphology, consistent with them hosting star formation. However, ~65% of the cluster members classified morphologically as spirals (with HST) have no detectable H{alpha} emission; star formation and morphological evolution in cluster galaxies appear to be largely decoupled. Changes in the H{alpha} detection rate and the strength of H{alpha} emission with environment (as traced by local galaxy density) are found to be weak within the region studied. Star formation within the cluster members is also found to be strongly and uniformly suppressed with the rates inferred from the H{alpha} emission not exceeding 4M_{sun}_/yr, and AC 114's H{alpha} luminosity function being an order of magnitude below that observed for field galaxies at the same redshift. None of the galaxies detected have the high star formation rates associated with "starburst" galaxies; however, this may still be reconcilable with the known (8%+/-3%) fraction of "post-starburst" galaxies within AC 114, given the poorly determined but short lifetimes of starbursts and the possibility that much of the associated star formation is obscured by dust.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820#table1</TD>
            <TD>2011-09-14T19:08:32Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/549/820&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/820</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/634/977 [1]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#1</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/634/977</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/634/977 [2]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#2</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/634/977&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/634/977 [table2]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#table2</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/634/977&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/634/977 [members]</TD>
            <TD>Redshifts in Cl 0024+16 members (Moran+, 2005)</TD>
            <TD>We report results from a panoramic spectroscopic survey of 955 objects in the field of the rich cluster Cl 0024+1654 (z~0.4), complementing the HST imaging presented in the first paper in this series. Combining with previous work, we compile a catalog of 1394 unique redshifts in the field of this cluster (1334 in Table 2), including 486 cluster members spread across an area 10Mpc in diameter. Our new spectroscopic sample includes over 200 high-quality spectra of cluster members. We examine the properties of a large sample of 104 cluster early-type galaxies as a function of cluster radius and local density, using them as sensitive tracers of the various physical processes that may be responsible for galaxy evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977#members</TD>
            <TD>2011-09-14T20:01:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Oct-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/977</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/634/977&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/977</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/549/820 [1]</TD>
            <TD>H{alpha} flux of ACCG 114 galaxies (Couch+, 2001)</TD>
            <TD>We present the results of a wide-field survey for H{alpha}-emitting galaxies in the cluster AC 114 at z=0.32. Spectra centered on H{alpha} at the cluster redshift have been obtained for 586 galaxies to I_tot_~22 out to a radius of ~h_50_^-1^Mpc. At most, only ~10% of these were found to be H{alpha}-emitting cluster members. These objects are predominantly blue and of late-type spiral morphology, consistent with them hosting star formation. However, ~65% of the cluster members classified morphologically as spirals (with HST) have no detectable H{alpha} emission; star formation and morphological evolution in cluster galaxies appear to be largely decoupled. Changes in the H{alpha} detection rate and the strength of H{alpha} emission with environment (as traced by local galaxy density) are found to be weak within the region studied. Star formation within the cluster members is also found to be strongly and uniformly suppressed with the rates inferred from the H{alpha} emission not exceeding 4M_{sun}_/yr, and AC 114's H{alpha} luminosity function being an order of magnitude below that observed for field galaxies at the same redshift. None of the galaxies detected have the high star formation rates associated with "starburst" galaxies; however, this may still be reconcilable with the known (8%+/-3%) fraction of "post-starburst" galaxies within AC 114, given the poorly determined but short lifetimes of starbursts and the possibility that much of the associated star formation is obscured by dust.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820#1</TD>
            <TD>2011-09-14T19:08:32Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/549/820</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/820</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/549/820 [2]</TD>
            <TD>H{alpha} flux of ACCG 114 galaxies (Couch+, 2001)</TD>
            <TD>We present the results of a wide-field survey for H{alpha}-emitting galaxies in the cluster AC 114 at z=0.32. Spectra centered on H{alpha} at the cluster redshift have been obtained for 586 galaxies to I_tot_~22 out to a radius of ~h_50_^-1^Mpc. At most, only ~10% of these were found to be H{alpha}-emitting cluster members. These objects are predominantly blue and of late-type spiral morphology, consistent with them hosting star formation. However, ~65% of the cluster members classified morphologically as spirals (with HST) have no detectable H{alpha} emission; star formation and morphological evolution in cluster galaxies appear to be largely decoupled. Changes in the H{alpha} detection rate and the strength of H{alpha} emission with environment (as traced by local galaxy density) are found to be weak within the region studied. Star formation within the cluster members is also found to be strongly and uniformly suppressed with the rates inferred from the H{alpha} emission not exceeding 4M_{sun}_/yr, and AC 114's H{alpha} luminosity function being an order of magnitude below that observed for field galaxies at the same redshift. None of the galaxies detected have the high star formation rates associated with "starburst" galaxies; however, this may still be reconcilable with the known (8%+/-3%) fraction of "post-starburst" galaxies within AC 114, given the poorly determined but short lifetimes of starbursts and the possibility that much of the associated star formation is obscured by dust.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820#2</TD>
            <TD>2011-09-14T19:08:32Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/549/820&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/820</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/549/820 [table1]</TD>
            <TD>H{alpha} flux of ACCG 114 galaxies (Couch+, 2001)</TD>
            <TD>We present the results of a wide-field survey for H{alpha}-emitting galaxies in the cluster AC 114 at z=0.32. Spectra centered on H{alpha} at the cluster redshift have been obtained for 586 galaxies to I_tot_~22 out to a radius of ~h_50_^-1^Mpc. At most, only ~10% of these were found to be H{alpha}-emitting cluster members. These objects are predominantly blue and of late-type spiral morphology, consistent with them hosting star formation. However, ~65% of the cluster members classified morphologically as spirals (with HST) have no detectable H{alpha} emission; star formation and morphological evolution in cluster galaxies appear to be largely decoupled. Changes in the H{alpha} detection rate and the strength of H{alpha} emission with environment (as traced by local galaxy density) are found to be weak within the region studied. Star formation within the cluster members is also found to be strongly and uniformly suppressed with the rates inferred from the H{alpha} emission not exceeding 4M_{sun}_/yr, and AC 114's H{alpha} luminosity function being an order of magnitude below that observed for field galaxies at the same redshift. None of the galaxies detected have the high star formation rates associated with "starburst" galaxies; however, this may still be reconcilable with the known (8%+/-3%) fraction of "post-starburst" galaxies within AC 114, given the poorly determined but short lifetimes of starbursts and the possibility that much of the associated star formation is obscured by dust.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820#table1</TD>
            <TD>2011-09-14T19:08:32Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/549/820&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/820</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/139/393 [1]</TD>
            <TD>Young Massive Star Clusters. II. (Larsen, 1999)</TD>
            <TD>Table 4 lists photometric data for Young Massive Star Clusters identified in a sample of 21 nearby galaxies. The photometric data have been corrected for Galactic foreground extinction. Each cluster is identified by the abbreviated NGC number of its host galaxy and an object number: nxxx-yyy is object number yyy in the galaxy NGC xxx. Effective cluster radii have been obtained by modeling the cluster images as MOFFAT15 functions convolved with the point-spread function measured on the CCD images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393#1</TD>
            <TD>2011-09-14T18:57:04Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/139/393</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/139/393</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/139/393 [2]</TD>
            <TD>Young Massive Star Clusters. II. (Larsen, 1999)</TD>
            <TD>Table 4 lists photometric data for Young Massive Star Clusters identified in a sample of 21 nearby galaxies. The photometric data have been corrected for Galactic foreground extinction. Each cluster is identified by the abbreviated NGC number of its host galaxy and an object number: nxxx-yyy is object number yyy in the galaxy NGC xxx. Effective cluster radii have been obtained by modeling the cluster images as MOFFAT15 functions convolved with the point-spread function measured on the CCD images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393#2</TD>
            <TD>2011-09-14T18:57:04Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/139/393&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/139/393</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/549/820 [1]</TD>
            <TD>H{alpha} flux of ACCG 114 galaxies (Couch+, 2001)</TD>
            <TD>We present the results of a wide-field survey for H{alpha}-emitting galaxies in the cluster AC 114 at z=0.32. Spectra centered on H{alpha} at the cluster redshift have been obtained for 586 galaxies to I_tot_~22 out to a radius of ~h_50_^-1^Mpc. At most, only ~10% of these were found to be H{alpha}-emitting cluster members. These objects are predominantly blue and of late-type spiral morphology, consistent with them hosting star formation. However, ~65% of the cluster members classified morphologically as spirals (with HST) have no detectable H{alpha} emission; star formation and morphological evolution in cluster galaxies appear to be largely decoupled. Changes in the H{alpha} detection rate and the strength of H{alpha} emission with environment (as traced by local galaxy density) are found to be weak within the region studied. Star formation within the cluster members is also found to be strongly and uniformly suppressed with the rates inferred from the H{alpha} emission not exceeding 4M_{sun}_/yr, and AC 114's H{alpha} luminosity function being an order of magnitude below that observed for field galaxies at the same redshift. None of the galaxies detected have the high star formation rates associated with "starburst" galaxies; however, this may still be reconcilable with the known (8%+/-3%) fraction of "post-starburst" galaxies within AC 114, given the poorly determined but short lifetimes of starbursts and the possibility that much of the associated star formation is obscured by dust.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820#1</TD>
            <TD>2011-09-14T19:08:32Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/549/820</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/820</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/549/820 [2]</TD>
            <TD>H{alpha} flux of ACCG 114 galaxies (Couch+, 2001)</TD>
            <TD>We present the results of a wide-field survey for H{alpha}-emitting galaxies in the cluster AC 114 at z=0.32. Spectra centered on H{alpha} at the cluster redshift have been obtained for 586 galaxies to I_tot_~22 out to a radius of ~h_50_^-1^Mpc. At most, only ~10% of these were found to be H{alpha}-emitting cluster members. These objects are predominantly blue and of late-type spiral morphology, consistent with them hosting star formation. However, ~65% of the cluster members classified morphologically as spirals (with HST) have no detectable H{alpha} emission; star formation and morphological evolution in cluster galaxies appear to be largely decoupled. Changes in the H{alpha} detection rate and the strength of H{alpha} emission with environment (as traced by local galaxy density) are found to be weak within the region studied. Star formation within the cluster members is also found to be strongly and uniformly suppressed with the rates inferred from the H{alpha} emission not exceeding 4M_{sun}_/yr, and AC 114's H{alpha} luminosity function being an order of magnitude below that observed for field galaxies at the same redshift. None of the galaxies detected have the high star formation rates associated with "starburst" galaxies; however, this may still be reconcilable with the known (8%+/-3%) fraction of "post-starburst" galaxies within AC 114, given the poorly determined but short lifetimes of starbursts and the possibility that much of the associated star formation is obscured by dust.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820#2</TD>
            <TD>2011-09-14T19:08:32Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/549/820&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/820</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/549/820 [table1]</TD>
            <TD>H{alpha} flux of ACCG 114 galaxies (Couch+, 2001)</TD>
            <TD>We present the results of a wide-field survey for H{alpha}-emitting galaxies in the cluster AC 114 at z=0.32. Spectra centered on H{alpha} at the cluster redshift have been obtained for 586 galaxies to I_tot_~22 out to a radius of ~h_50_^-1^Mpc. At most, only ~10% of these were found to be H{alpha}-emitting cluster members. These objects are predominantly blue and of late-type spiral morphology, consistent with them hosting star formation. However, ~65% of the cluster members classified morphologically as spirals (with HST) have no detectable H{alpha} emission; star formation and morphological evolution in cluster galaxies appear to be largely decoupled. Changes in the H{alpha} detection rate and the strength of H{alpha} emission with environment (as traced by local galaxy density) are found to be weak within the region studied. Star formation within the cluster members is also found to be strongly and uniformly suppressed with the rates inferred from the H{alpha} emission not exceeding 4M_{sun}_/yr, and AC 114's H{alpha} luminosity function being an order of magnitude below that observed for field galaxies at the same redshift. None of the galaxies detected have the high star formation rates associated with "starburst" galaxies; however, this may still be reconcilable with the known (8%+/-3%) fraction of "post-starburst" galaxies within AC 114, given the poorly determined but short lifetimes of starbursts and the possibility that much of the associated star formation is obscured by dust.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820#table1</TD>
            <TD>2011-09-14T19:08:32Z</TD>
            <TD>#Photometry:narrow-band#Clusters_of_galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/820</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/549/820&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/820</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/580/774 [1]</TD>
            <TD>X-ray cluster of galaxies behind the Milky way (Ebeling+, 2002)</TD>
            <TD>We report on the design and status of the Clusters in the Zone of Avoidance (CIZA) project, the first systematic X-ray search for clusters of galaxies behind the Milky Way. Our project, Clusters in the Zone of Avoidance (CIZA), uses X-ray data from the RASS for the initial cluster candidate selection and subsequent optical and NIR observations to confirm or refute the cluster nature of all selected candidates. We demonstrate that an X-ray survey can find galaxy clusters at low Galactic latitude where optical searches are inefficient because of massive obscuration and extinction problems. We discuss the rationale for such a survey in the context of large-scale structure studies and describe in detail the combined X-ray/optical/NIR approach used by CIZA to identify clusters of galaxies at |b|&lt;20{deg}, a region of the sky that has traditionally been excluded from earlier cluster catalogs. So far, CIZA has identified and spectroscopically confirmed 137 galaxy clusters in what used to be the zone of avoidance; additional clusters have been confirmed in imaging observations and await spectroscopic observation. We present a catalog of the 73 X-ray brightest CIZA clusters, 53 (73%) of which are new discoveries.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774#1</TD>
            <TD>2011-09-14T20:01:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/580/774</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/580/774</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/580/774 [2]</TD>
            <TD>X-ray cluster of galaxies behind the Milky way (Ebeling+, 2002)</TD>
            <TD>We report on the design and status of the Clusters in the Zone of Avoidance (CIZA) project, the first systematic X-ray search for clusters of galaxies behind the Milky Way. Our project, Clusters in the Zone of Avoidance (CIZA), uses X-ray data from the RASS for the initial cluster candidate selection and subsequent optical and NIR observations to confirm or refute the cluster nature of all selected candidates. We demonstrate that an X-ray survey can find galaxy clusters at low Galactic latitude where optical searches are inefficient because of massive obscuration and extinction problems. We discuss the rationale for such a survey in the context of large-scale structure studies and describe in detail the combined X-ray/optical/NIR approach used by CIZA to identify clusters of galaxies at |b|&lt;20{deg}, a region of the sky that has traditionally been excluded from earlier cluster catalogs. So far, CIZA has identified and spectroscopically confirmed 137 galaxy clusters in what used to be the zone of avoidance; additional clusters have been confirmed in imaging observations and await spectroscopic observation. We present a catalog of the 73 X-ray brightest CIZA clusters, 53 (73%) of which are new discoveries.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774#2</TD>
            <TD>2011-09-14T20:01:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/580/774&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/580/774</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/580/774 [table1]</TD>
            <TD>X-ray cluster of galaxies behind the Milky way (Ebeling+, 2002)</TD>
            <TD>We report on the design and status of the Clusters in the Zone of Avoidance (CIZA) project, the first systematic X-ray search for clusters of galaxies behind the Milky Way. Our project, Clusters in the Zone of Avoidance (CIZA), uses X-ray data from the RASS for the initial cluster candidate selection and subsequent optical and NIR observations to confirm or refute the cluster nature of all selected candidates. We demonstrate that an X-ray survey can find galaxy clusters at low Galactic latitude where optical searches are inefficient because of massive obscuration and extinction problems. We discuss the rationale for such a survey in the context of large-scale structure studies and describe in detail the combined X-ray/optical/NIR approach used by CIZA to identify clusters of galaxies at |b|&lt;20{deg}, a region of the sky that has traditionally been excluded from earlier cluster catalogs. So far, CIZA has identified and spectroscopically confirmed 137 galaxy clusters in what used to be the zone of avoidance; additional clusters have been confirmed in imaging observations and await spectroscopic observation. We present a catalog of the 73 X-ray brightest CIZA clusters, 53 (73%) of which are new discoveries.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774#table1</TD>
            <TD>2011-09-14T20:01:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/580/774&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/580/774</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/549/172 [1]</TD>
            <TD>X-ray-detected, poor groups galaxy populations (Tran+, 2001)</TD>
            <TD>We determine the quantitative morphology and star formation properties of galaxies in six nearby X-ray-detected, poor groups using multiobject spectroscopy and wide-field R imaging. The mean recessional velocities of the galaxy groups range from 2843 to 7558km/s. Each group has 1538 confirmed members ranging in luminosity from dwarfs to giants (-13.7&gt;=M_R_-5logh&gt;=-21.9). We measure structural parameters for each galaxy by fitting a PSF-convolved, two-component model to their surface brightness profiles. To compare the samples directly, we fade, smooth, and rebin each galaxy image so that we effectively observe each galaxy at the same redshift (9000km/s) and physical resolution (0.87h^-1^kpc). The structural parameters are combined with [O II] measurements to test for correlations between morphological characteristics and current star formation in these galaxies. We compare results for the groups to a sample of field galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/172#1</TD>
            <TD>2011-09-14T19:08:51Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/172</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/549/172</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/172</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/549/172 [2]</TD>
            <TD>X-ray-detected, poor groups galaxy populations (Tran+, 2001)</TD>
            <TD>We determine the quantitative morphology and star formation properties of galaxies in six nearby X-ray-detected, poor groups using multiobject spectroscopy and wide-field R imaging. The mean recessional velocities of the galaxy groups range from 2843 to 7558km/s. Each group has 1538 confirmed members ranging in luminosity from dwarfs to giants (-13.7&gt;=M_R_-5logh&gt;=-21.9). We measure structural parameters for each galaxy by fitting a PSF-convolved, two-component model to their surface brightness profiles. To compare the samples directly, we fade, smooth, and rebin each galaxy image so that we effectively observe each galaxy at the same redshift (9000km/s) and physical resolution (0.87h^-1^kpc). The structural parameters are combined with [O II] measurements to test for correlations between morphological characteristics and current star formation in these galaxies. We compare results for the groups to a sample of field galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/172#2</TD>
            <TD>2011-09-14T19:08:51Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/172</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/549/172&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/172</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/139/393 [1]</TD>
            <TD>Young Massive Star Clusters. II. (Larsen, 1999)</TD>
            <TD>Table 4 lists photometric data for Young Massive Star Clusters identified in a sample of 21 nearby galaxies. The photometric data have been corrected for Galactic foreground extinction. Each cluster is identified by the abbreviated NGC number of its host galaxy and an object number: nxxx-yyy is object number yyy in the galaxy NGC xxx. Effective cluster radii have been obtained by modeling the cluster images as MOFFAT15 functions convolved with the point-spread function measured on the CCD images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393#1</TD>
            <TD>2011-09-14T18:57:04Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/139/393</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/139/393</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/139/393 [2]</TD>
            <TD>Young Massive Star Clusters. II. (Larsen, 1999)</TD>
            <TD>Table 4 lists photometric data for Young Massive Star Clusters identified in a sample of 21 nearby galaxies. The photometric data have been corrected for Galactic foreground extinction. Each cluster is identified by the abbreviated NGC number of its host galaxy and an object number: nxxx-yyy is object number yyy in the galaxy NGC xxx. Effective cluster radii have been obtained by modeling the cluster images as MOFFAT15 functions convolved with the point-spread function measured on the CCD images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393#2</TD>
            <TD>2011-09-14T18:57:04Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/139/393&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/139/393</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/580/774 [1]</TD>
            <TD>X-ray cluster of galaxies behind the Milky way (Ebeling+, 2002)</TD>
            <TD>We report on the design and status of the Clusters in the Zone of Avoidance (CIZA) project, the first systematic X-ray search for clusters of galaxies behind the Milky Way. Our project, Clusters in the Zone of Avoidance (CIZA), uses X-ray data from the RASS for the initial cluster candidate selection and subsequent optical and NIR observations to confirm or refute the cluster nature of all selected candidates. We demonstrate that an X-ray survey can find galaxy clusters at low Galactic latitude where optical searches are inefficient because of massive obscuration and extinction problems. We discuss the rationale for such a survey in the context of large-scale structure studies and describe in detail the combined X-ray/optical/NIR approach used by CIZA to identify clusters of galaxies at |b|&lt;20{deg}, a region of the sky that has traditionally been excluded from earlier cluster catalogs. So far, CIZA has identified and spectroscopically confirmed 137 galaxy clusters in what used to be the zone of avoidance; additional clusters have been confirmed in imaging observations and await spectroscopic observation. We present a catalog of the 73 X-ray brightest CIZA clusters, 53 (73%) of which are new discoveries.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774#1</TD>
            <TD>2011-09-14T20:01:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/580/774</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/580/774</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/580/774 [2]</TD>
            <TD>X-ray cluster of galaxies behind the Milky way (Ebeling+, 2002)</TD>
            <TD>We report on the design and status of the Clusters in the Zone of Avoidance (CIZA) project, the first systematic X-ray search for clusters of galaxies behind the Milky Way. Our project, Clusters in the Zone of Avoidance (CIZA), uses X-ray data from the RASS for the initial cluster candidate selection and subsequent optical and NIR observations to confirm or refute the cluster nature of all selected candidates. We demonstrate that an X-ray survey can find galaxy clusters at low Galactic latitude where optical searches are inefficient because of massive obscuration and extinction problems. We discuss the rationale for such a survey in the context of large-scale structure studies and describe in detail the combined X-ray/optical/NIR approach used by CIZA to identify clusters of galaxies at |b|&lt;20{deg}, a region of the sky that has traditionally been excluded from earlier cluster catalogs. So far, CIZA has identified and spectroscopically confirmed 137 galaxy clusters in what used to be the zone of avoidance; additional clusters have been confirmed in imaging observations and await spectroscopic observation. We present a catalog of the 73 X-ray brightest CIZA clusters, 53 (73%) of which are new discoveries.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774#2</TD>
            <TD>2011-09-14T20:01:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/580/774&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/580/774</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/580/774 [table1]</TD>
            <TD>X-ray cluster of galaxies behind the Milky way (Ebeling+, 2002)</TD>
            <TD>We report on the design and status of the Clusters in the Zone of Avoidance (CIZA) project, the first systematic X-ray search for clusters of galaxies behind the Milky Way. Our project, Clusters in the Zone of Avoidance (CIZA), uses X-ray data from the RASS for the initial cluster candidate selection and subsequent optical and NIR observations to confirm or refute the cluster nature of all selected candidates. We demonstrate that an X-ray survey can find galaxy clusters at low Galactic latitude where optical searches are inefficient because of massive obscuration and extinction problems. We discuss the rationale for such a survey in the context of large-scale structure studies and describe in detail the combined X-ray/optical/NIR approach used by CIZA to identify clusters of galaxies at |b|&lt;20{deg}, a region of the sky that has traditionally been excluded from earlier cluster catalogs. So far, CIZA has identified and spectroscopically confirmed 137 galaxy clusters in what used to be the zone of avoidance; additional clusters have been confirmed in imaging observations and await spectroscopic observation. We present a catalog of the 73 X-ray brightest CIZA clusters, 53 (73%) of which are new discoveries.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774#table1</TD>
            <TD>2011-09-14T20:01:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/580/774&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/580/774</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/549/172 [1]</TD>
            <TD>X-ray-detected, poor groups galaxy populations (Tran+, 2001)</TD>
            <TD>We determine the quantitative morphology and star formation properties of galaxies in six nearby X-ray-detected, poor groups using multiobject spectroscopy and wide-field R imaging. The mean recessional velocities of the galaxy groups range from 2843 to 7558km/s. Each group has 1538 confirmed members ranging in luminosity from dwarfs to giants (-13.7&gt;=M_R_-5logh&gt;=-21.9). We measure structural parameters for each galaxy by fitting a PSF-convolved, two-component model to their surface brightness profiles. To compare the samples directly, we fade, smooth, and rebin each galaxy image so that we effectively observe each galaxy at the same redshift (9000km/s) and physical resolution (0.87h^-1^kpc). The structural parameters are combined with [O II] measurements to test for correlations between morphological characteristics and current star formation in these galaxies. We compare results for the groups to a sample of field galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/172#1</TD>
            <TD>2011-09-14T19:08:51Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/172</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/549/172</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/172</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/549/172 [2]</TD>
            <TD>X-ray-detected, poor groups galaxy populations (Tran+, 2001)</TD>
            <TD>We determine the quantitative morphology and star formation properties of galaxies in six nearby X-ray-detected, poor groups using multiobject spectroscopy and wide-field R imaging. The mean recessional velocities of the galaxy groups range from 2843 to 7558km/s. Each group has 1538 confirmed members ranging in luminosity from dwarfs to giants (-13.7&gt;=M_R_-5logh&gt;=-21.9). We measure structural parameters for each galaxy by fitting a PSF-convolved, two-component model to their surface brightness profiles. To compare the samples directly, we fade, smooth, and rebin each galaxy image so that we effectively observe each galaxy at the same redshift (9000km/s) and physical resolution (0.87h^-1^kpc). The structural parameters are combined with [O II] measurements to test for correlations between morphological characteristics and current star formation in these galaxies. We compare results for the groups to a sample of field galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/172#2</TD>
            <TD>2011-09-14T19:08:51Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/549/172</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/549/172&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/549/172</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/139/393 [1]</TD>
            <TD>Young Massive Star Clusters. II. (Larsen, 1999)</TD>
            <TD>Table 4 lists photometric data for Young Massive Star Clusters identified in a sample of 21 nearby galaxies. The photometric data have been corrected for Galactic foreground extinction. Each cluster is identified by the abbreviated NGC number of its host galaxy and an object number: nxxx-yyy is object number yyy in the galaxy NGC xxx. Effective cluster radii have been obtained by modeling the cluster images as MOFFAT15 functions convolved with the point-spread function measured on the CCD images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393#1</TD>
            <TD>2011-09-14T18:57:04Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/139/393</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/139/393</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/139/393 [2]</TD>
            <TD>Young Massive Star Clusters. II. (Larsen, 1999)</TD>
            <TD>Table 4 lists photometric data for Young Massive Star Clusters identified in a sample of 21 nearby galaxies. The photometric data have been corrected for Galactic foreground extinction. Each cluster is identified by the abbreviated NGC number of its host galaxy and an object number: nxxx-yyy is object number yyy in the galaxy NGC xxx. Effective cluster radii have been obtained by modeling the cluster images as MOFFAT15 functions convolved with the point-spread function measured on the CCD images.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393#2</TD>
            <TD>2011-09-14T18:57:04Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jul-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/139/393</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/139/393&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/139/393</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/27/83 [1]</TD>
            <TD>Nuclear activity of NGC 4151 in 1989-2000 (Doroshenko+, 2001)</TD>
            <TD>Broadband UBVRI observations of the nucleus of the Seyfert galaxy NGC 4151 from 1989 until 2000 at three astronomical observatories: the Crimean Station of the Sternberg astronomical institute, The Special Astronomical observatory in the Caucasus and the Maidanac observatory of the Ulugbek Astronomical institute in Uzbekistan. All data have been reduced to a single system and are given for an A=27.5" aperture.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/83#1</TD>
            <TD>2011-09-14T19:08:53Z</TD>
            <TD>#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/27/83</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/83</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/27/83 [2]</TD>
            <TD>Nuclear activity of NGC 4151 in 1989-2000 (Doroshenko+, 2001)</TD>
            <TD>Broadband UBVRI observations of the nucleus of the Seyfert galaxy NGC 4151 from 1989 until 2000 at three astronomical observatories: the Crimean Station of the Sternberg astronomical institute, The Special Astronomical observatory in the Caucasus and the Maidanac observatory of the Ulugbek Astronomical institute in Uzbekistan. All data have been reduced to a single system and are given for an A=27.5" aperture.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/83#2</TD>
            <TD>2011-09-14T19:08:53Z</TD>
            <TD>#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/27/83&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/83</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/580/774 [1]</TD>
            <TD>X-ray cluster of galaxies behind the Milky way (Ebeling+, 2002)</TD>
            <TD>We report on the design and status of the Clusters in the Zone of Avoidance (CIZA) project, the first systematic X-ray search for clusters of galaxies behind the Milky Way. Our project, Clusters in the Zone of Avoidance (CIZA), uses X-ray data from the RASS for the initial cluster candidate selection and subsequent optical and NIR observations to confirm or refute the cluster nature of all selected candidates. We demonstrate that an X-ray survey can find galaxy clusters at low Galactic latitude where optical searches are inefficient because of massive obscuration and extinction problems. We discuss the rationale for such a survey in the context of large-scale structure studies and describe in detail the combined X-ray/optical/NIR approach used by CIZA to identify clusters of galaxies at |b|&lt;20{deg}, a region of the sky that has traditionally been excluded from earlier cluster catalogs. So far, CIZA has identified and spectroscopically confirmed 137 galaxy clusters in what used to be the zone of avoidance; additional clusters have been confirmed in imaging observations and await spectroscopic observation. We present a catalog of the 73 X-ray brightest CIZA clusters, 53 (73%) of which are new discoveries.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774#1</TD>
            <TD>2011-09-14T20:01:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/580/774</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/580/774</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/580/774 [2]</TD>
            <TD>X-ray cluster of galaxies behind the Milky way (Ebeling+, 2002)</TD>
            <TD>We report on the design and status of the Clusters in the Zone of Avoidance (CIZA) project, the first systematic X-ray search for clusters of galaxies behind the Milky Way. Our project, Clusters in the Zone of Avoidance (CIZA), uses X-ray data from the RASS for the initial cluster candidate selection and subsequent optical and NIR observations to confirm or refute the cluster nature of all selected candidates. We demonstrate that an X-ray survey can find galaxy clusters at low Galactic latitude where optical searches are inefficient because of massive obscuration and extinction problems. We discuss the rationale for such a survey in the context of large-scale structure studies and describe in detail the combined X-ray/optical/NIR approach used by CIZA to identify clusters of galaxies at |b|&lt;20{deg}, a region of the sky that has traditionally been excluded from earlier cluster catalogs. So far, CIZA has identified and spectroscopically confirmed 137 galaxy clusters in what used to be the zone of avoidance; additional clusters have been confirmed in imaging observations and await spectroscopic observation. We present a catalog of the 73 X-ray brightest CIZA clusters, 53 (73%) of which are new discoveries.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774#2</TD>
            <TD>2011-09-14T20:01:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/580/774&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/580/774</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/580/774 [table1]</TD>
            <TD>X-ray cluster of galaxies behind the Milky way (Ebeling+, 2002)</TD>
            <TD>We report on the design and status of the Clusters in the Zone of Avoidance (CIZA) project, the first systematic X-ray search for clusters of galaxies behind the Milky Way. Our project, Clusters in the Zone of Avoidance (CIZA), uses X-ray data from the RASS for the initial cluster candidate selection and subsequent optical and NIR observations to confirm or refute the cluster nature of all selected candidates. We demonstrate that an X-ray survey can find galaxy clusters at low Galactic latitude where optical searches are inefficient because of massive obscuration and extinction problems. We discuss the rationale for such a survey in the context of large-scale structure studies and describe in detail the combined X-ray/optical/NIR approach used by CIZA to identify clusters of galaxies at |b|&lt;20{deg}, a region of the sky that has traditionally been excluded from earlier cluster catalogs. So far, CIZA has identified and spectroscopically confirmed 137 galaxy clusters in what used to be the zone of avoidance; additional clusters have been confirmed in imaging observations and await spectroscopic observation. We present a catalog of the 73 X-ray brightest CIZA clusters, 53 (73%) of which are new discoveries.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774#table1</TD>
            <TD>2011-09-14T20:01:50Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/580/774</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/580/774&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/580/774</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/27/83 [1]</TD>
            <TD>Nuclear activity of NGC 4151 in 1989-2000 (Doroshenko+, 2001)</TD>
            <TD>Broadband UBVRI observations of the nucleus of the Seyfert galaxy NGC 4151 from 1989 until 2000 at three astronomical observatories: the Crimean Station of the Sternberg astronomical institute, The Special Astronomical observatory in the Caucasus and the Maidanac observatory of the Ulugbek Astronomical institute in Uzbekistan. All data have been reduced to a single system and are given for an A=27.5" aperture.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/83#1</TD>
            <TD>2011-09-14T19:08:53Z</TD>
            <TD>#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/27/83</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/83</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/27/83 [2]</TD>
            <TD>Nuclear activity of NGC 4151 in 1989-2000 (Doroshenko+, 2001)</TD>
            <TD>Broadband UBVRI observations of the nucleus of the Seyfert galaxy NGC 4151 from 1989 until 2000 at three astronomical observatories: the Crimean Station of the Sternberg astronomical institute, The Special Astronomical observatory in the Caucasus and the Maidanac observatory of the Ulugbek Astronomical institute in Uzbekistan. All data have been reduced to a single system and are given for an A=27.5" aperture.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/83#2</TD>
            <TD>2011-09-14T19:08:53Z</TD>
            <TD>#Seyfert_Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/27/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/27/83&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/27/83</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/1803 [1]</TD>
            <TD>Large Scale Structure (Marzke+ 1996)</TD>
            <TD>We have extended the CfA Redshift Survey to low galactic latitudes to investigate the relation between the Great Wall in the North Galactic Cap and the Perseus-Pisces chain in the South Galactic Cap. We present redshifts for 2020 galaxies in the Catalogue of Galaxies and of Clusters of Galaxies (Zwicky et al. 1961-68, CGCG, Cat. &lt;VII/4&gt;) in the following regions: 4h&lt;=RA&lt;=8h, 17h&lt;=Dec.&lt;=20h, 0deg&lt;=Dec.&lt;=45deg. In these regions, the redshift catalogue includes 1664 galaxies with B(0)&lt;=15.5 (of which 820 are newly measured) and is 97% complete. We also include redshifts for an additional 356 galaxies in these regions with B(0)&gt;15.5; of these, 148 were previously unmeasured. The CGCG samples the galaxy distribution down to b_(II)_~10deg. In this paper, we discuss the acquisition and reduction of the spectra, and we examine the qualitative features of the redshift distribution. The Great Wall and the Perseus-Pisces chain are not simply connected across the Zone of Avoidance. These structures, which at first appear to be coherent on scales of ~100h^-1^Mpc or more, actually form the boundaries of neighboring voids of considerably smaller scale, approximately 50h^-1^Mpc. The structures delineated by our optically-selected sample are qualitatively similar to those detected by the far-infrared-selected IRAS 1.2 Jansky Survey (Fisher et al., 1995ApJS..100...69F). Although the IRAS survey probes more deeply into the Zone of Avoidance, our optically-selected survey provides better sampling of structures at b_(II)&gt;=10deg. (Copyright) 1996 American Astronomical Society.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803#1</TD>
            <TD>2011-09-14T18:57:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/1803</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1803</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/1803 [2]</TD>
            <TD>Large Scale Structure (Marzke+ 1996)</TD>
            <TD>We have extended the CfA Redshift Survey to low galactic latitudes to investigate the relation between the Great Wall in the North Galactic Cap and the Perseus-Pisces chain in the South Galactic Cap. We present redshifts for 2020 galaxies in the Catalogue of Galaxies and of Clusters of Galaxies (Zwicky et al. 1961-68, CGCG, Cat. &lt;VII/4&gt;) in the following regions: 4h&lt;=RA&lt;=8h, 17h&lt;=Dec.&lt;=20h, 0deg&lt;=Dec.&lt;=45deg. In these regions, the redshift catalogue includes 1664 galaxies with B(0)&lt;=15.5 (of which 820 are newly measured) and is 97% complete. We also include redshifts for an additional 356 galaxies in these regions with B(0)&gt;15.5; of these, 148 were previously unmeasured. The CGCG samples the galaxy distribution down to b_(II)_~10deg. In this paper, we discuss the acquisition and reduction of the spectra, and we examine the qualitative features of the redshift distribution. The Great Wall and the Perseus-Pisces chain are not simply connected across the Zone of Avoidance. These structures, which at first appear to be coherent on scales of ~100h^-1^Mpc or more, actually form the boundaries of neighboring voids of considerably smaller scale, approximately 50h^-1^Mpc. The structures delineated by our optically-selected sample are qualitatively similar to those detected by the far-infrared-selected IRAS 1.2 Jansky Survey (Fisher et al., 1995ApJS..100...69F). Although the IRAS survey probes more deeply into the Zone of Avoidance, our optically-selected survey provides better sampling of structures at b_(II)&gt;=10deg. (Copyright) 1996 American Astronomical Society.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803#2</TD>
            <TD>2011-09-14T18:57:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/1803&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1803</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/807 [1]</TD>
            <TD>Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)</TD>
            <TD>We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges ({gamma}-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identifed as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807#1</TD>
            <TD>2011-09-14T20:16:11Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/807 [2]</TD>
            <TD>Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)</TD>
            <TD>We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges ({gamma}-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identifed as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807#2</TD>
            <TD>2011-09-14T20:16:11Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/807</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/807 [lmxb]</TD>
            <TD>Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)</TD>
            <TD>We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges ({gamma}-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identifed as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807#lmxb</TD>
            <TD>2011-09-14T20:16:11Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/807&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/175 [1]</TD>
            <TD>Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)</TD>
            <TD>We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaAy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/175#1</TD>
            <TD>2011-09-14T18:39:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VII/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/175</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/175</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/175 [2]</TD>
            <TD>Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)</TD>
            <TD>We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaAy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/175#2</TD>
            <TD>2011-09-14T18:39:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VII/175</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/175&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/175</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/175 [table3]</TD>
            <TD>Edinburgh-Durham Southern Galaxy Cat. - Cluster Cat. (Lumsden+ 1992)</TD>
            <TD>We present the Edinburgh-Durham Cluster Catalogue (EDCC). This is the first machine-based, objectively selected sample of clusters of galaxies. It consists of 737 clusters or groups of all richnesses, over 0.5 sr of sky, centred on the South Galactic Pole (SGP). The primary galaAy data set for the cluster survey is the Edinburgh-Durham Southern Galaxy Catalogue (EDSGC). The EDCC was constructed using an automatic peak-finding algorithm and is complete to m_10_(b_j_) = 18.75. In a comparison with the Abell clusters in the same region, we detect 80 per cent of their rich clusters nominally brighter than our completion limit in addition to many new systems. This suggests that the EDCC is 90 per cent complete for Abell-type clusters. We also conclude that the Abell magnitude system is biased towards bright magnitudes for most of their clusters, and that their richness estimates are prone to a larger uncertainty than they suggest. The EDCC therefore supersedes the Abell catalogue as a data base for statistical studies of cluster properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/175#table3</TD>
            <TD>2011-09-14T18:39:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Mar-1994</TD>
            <TD>ivo://CDS.VizieR/VII/175</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/175&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/175</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/374/394 [1]</TD>
            <TD>Gas and stars kinematics in disc galaxies (Vega Beltran+ 2001)</TD>
            <TD>Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion (V_g_&gt;V_*_ and {sigma}_g_&lt;{sigma}_*_), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions (V_g_=~V_*_ and {sigma}_g_=~{sigma}_*_). Incorporating the early-type disc galaxies studied by Bertola et al. (1995ApJ...448L..13B), Fisher (1997, Cat. &lt;J/AJ/113/950&gt;) and Corsini et al. (1999, Cat. &lt;J/A+A/342/671&gt;), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of {sigma}_*_ measured at R_e_/4 turns out to be strongly correlated with the galaxy morphological type, while {sigma}_g_ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394#1</TD>
            <TD>2011-09-14T19:09:40Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/374/394</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/394</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/374/394 [2]</TD>
            <TD>Gas and stars kinematics in disc galaxies (Vega Beltran+ 2001)</TD>
            <TD>Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion (V_g_&gt;V_*_ and {sigma}_g_&lt;{sigma}_*_), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions (V_g_=~V_*_ and {sigma}_g_=~{sigma}_*_). Incorporating the early-type disc galaxies studied by Bertola et al. (1995ApJ...448L..13B), Fisher (1997, Cat. &lt;J/AJ/113/950&gt;) and Corsini et al. (1999, Cat. &lt;J/A+A/342/671&gt;), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of {sigma}_*_ measured at R_e_/4 turns out to be strongly correlated with the galaxy morphological type, while {sigma}_g_ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394#2</TD>
            <TD>2011-09-14T19:09:40Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/374/394&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/394</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/374/394 [galaxies]</TD>
            <TD>Gas and stars kinematics in disc galaxies (Vega Beltran+ 2001)</TD>
            <TD>Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion (V_g_&gt;V_*_ and {sigma}_g_&lt;{sigma}_*_), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions (V_g_=~V_*_ and {sigma}_g_=~{sigma}_*_). Incorporating the early-type disc galaxies studied by Bertola et al. (1995ApJ...448L..13B), Fisher (1997, Cat. &lt;J/AJ/113/950&gt;) and Corsini et al. (1999, Cat. &lt;J/A+A/342/671&gt;), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of {sigma}_*_ measured at R_e_/4 turns out to be strongly correlated with the galaxy morphological type, while {sigma}_g_ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394#galaxies</TD>
            <TD>2011-09-14T19:09:40Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/374/394&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/394</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/807 [1]</TD>
            <TD>Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)</TD>
            <TD>We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges ({gamma}-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identifed as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807#1</TD>
            <TD>2011-09-14T20:16:11Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/807 [2]</TD>
            <TD>Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)</TD>
            <TD>We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges ({gamma}-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identifed as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807#2</TD>
            <TD>2011-09-14T20:16:11Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/807</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/807 [lmxb]</TD>
            <TD>Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)</TD>
            <TD>We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges ({gamma}-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identifed as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807#lmxb</TD>
            <TD>2011-09-14T20:16:11Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/807&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/101 [1]</TD>
            <TD>Galaxies in the "zone of avoidance". V. (Seeberger+ 1998)</TD>
            <TD>As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}&lt;=l&lt;=110{deg}, -10{deg}&lt;=b&lt;=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101#1</TD>
            <TD>2011-09-14T18:39:47Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/101 [2]</TD>
            <TD>Galaxies in the "zone of avoidance". V. (Seeberger+ 1998)</TD>
            <TD>As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}&lt;=l&lt;=110{deg}, -10{deg}&lt;=b&lt;=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101#2</TD>
            <TD>2011-09-14T18:39:47Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/101 [table2]</TD>
            <TD>Galaxies in the "zone of avoidance". V. (Seeberger+ 1998)</TD>
            <TD>As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}&lt;=l&lt;=110{deg}, -10{deg}&lt;=b&lt;=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101#table2</TD>
            <TD>2011-09-14T18:39:47Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/374/394 [1]</TD>
            <TD>Gas and stars kinematics in disc galaxies (Vega Beltran+ 2001)</TD>
            <TD>Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion (V_g_&gt;V_*_ and {sigma}_g_&lt;{sigma}_*_), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions (V_g_=~V_*_ and {sigma}_g_=~{sigma}_*_). Incorporating the early-type disc galaxies studied by Bertola et al. (1995ApJ...448L..13B), Fisher (1997, Cat. &lt;J/AJ/113/950&gt;) and Corsini et al. (1999, Cat. &lt;J/A+A/342/671&gt;), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of {sigma}_*_ measured at R_e_/4 turns out to be strongly correlated with the galaxy morphological type, while {sigma}_g_ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394#1</TD>
            <TD>2011-09-14T19:09:40Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/374/394</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/394</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/374/394 [2]</TD>
            <TD>Gas and stars kinematics in disc galaxies (Vega Beltran+ 2001)</TD>
            <TD>Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion (V_g_&gt;V_*_ and {sigma}_g_&lt;{sigma}_*_), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions (V_g_=~V_*_ and {sigma}_g_=~{sigma}_*_). Incorporating the early-type disc galaxies studied by Bertola et al. (1995ApJ...448L..13B), Fisher (1997, Cat. &lt;J/AJ/113/950&gt;) and Corsini et al. (1999, Cat. &lt;J/A+A/342/671&gt;), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of {sigma}_*_ measured at R_e_/4 turns out to be strongly correlated with the galaxy morphological type, while {sigma}_g_ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394#2</TD>
            <TD>2011-09-14T19:09:40Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/374/394&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/394</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/374/394 [galaxies]</TD>
            <TD>Gas and stars kinematics in disc galaxies (Vega Beltran+ 2001)</TD>
            <TD>Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion (V_g_&gt;V_*_ and {sigma}_g_&lt;{sigma}_*_), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions (V_g_=~V_*_ and {sigma}_g_=~{sigma}_*_). Incorporating the early-type disc galaxies studied by Bertola et al. (1995ApJ...448L..13B), Fisher (1997, Cat. &lt;J/AJ/113/950&gt;) and Corsini et al. (1999, Cat. &lt;J/A+A/342/671&gt;), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of {sigma}_*_ measured at R_e_/4 turns out to be strongly correlated with the galaxy morphological type, while {sigma}_g_ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394#galaxies</TD>
            <TD>2011-09-14T19:09:40Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/374/394&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/394</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/374/394 [1]</TD>
            <TD>Gas and stars kinematics in disc galaxies (Vega Beltran+ 2001)</TD>
            <TD>Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion (V_g_&gt;V_*_ and {sigma}_g_&lt;{sigma}_*_), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions (V_g_=~V_*_ and {sigma}_g_=~{sigma}_*_). Incorporating the early-type disc galaxies studied by Bertola et al. (1995ApJ...448L..13B), Fisher (1997, Cat. &lt;J/AJ/113/950&gt;) and Corsini et al. (1999, Cat. &lt;J/A+A/342/671&gt;), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of {sigma}_*_ measured at R_e_/4 turns out to be strongly correlated with the galaxy morphological type, while {sigma}_g_ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394#1</TD>
            <TD>2011-09-14T19:09:40Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/374/394</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/394</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/374/394 [2]</TD>
            <TD>Gas and stars kinematics in disc galaxies (Vega Beltran+ 2001)</TD>
            <TD>Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion (V_g_&gt;V_*_ and {sigma}_g_&lt;{sigma}_*_), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions (V_g_=~V_*_ and {sigma}_g_=~{sigma}_*_). Incorporating the early-type disc galaxies studied by Bertola et al. (1995ApJ...448L..13B), Fisher (1997, Cat. &lt;J/AJ/113/950&gt;) and Corsini et al. (1999, Cat. &lt;J/A+A/342/671&gt;), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of {sigma}_*_ measured at R_e_/4 turns out to be strongly correlated with the galaxy morphological type, while {sigma}_g_ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394#2</TD>
            <TD>2011-09-14T19:09:40Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/374/394&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/394</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/374/394 [galaxies]</TD>
            <TD>Gas and stars kinematics in disc galaxies (Vega Beltran+ 2001)</TD>
            <TD>Ionized gas and stellar kinematical parameters have been measured along the major axis of 20 nearby disc galaxies. We discuss the properties of each sample galaxy, distinguishing between those characterized by regular or peculiar kinematics. In early-type disc galaxies, ionized gas tends to rotate faster than stars and to have a lower velocity dispersion (V_g_&gt;V_*_ and {sigma}_g_&lt;{sigma}_*_), whereas in late-type spirals, gas and stars show almost the same rotation velocities and velocity dispersions (V_g_=~V_*_ and {sigma}_g_=~{sigma}_*_). Incorporating the early-type disc galaxies studied by Bertola et al. (1995ApJ...448L..13B), Fisher (1997, Cat. &lt;J/AJ/113/950&gt;) and Corsini et al. (1999, Cat. &lt;J/A+A/342/671&gt;), we have compiled a sample of some 40 galaxies for which the major-axis radial profiles of both the stellar and gaseous components have been measured. The value of {sigma}_*_ measured at R_e_/4 turns out to be strongly correlated with the galaxy morphological type, while {sigma}_g_ is not and sometimes takes values above the range expected from thermal motions or small-scale turbulence.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394#galaxies</TD>
            <TD>2011-09-14T19:09:40Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/374/394</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/374/394&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/374/394</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/120/2269 [1]</TD>
            <TD>Wide-Angle-Tailed radio galaxies redshifts (Pinkney+, 2000)</TD>
            <TD>We present new redshifts and positions for 635 galaxies in nine rich clusters containing wide-angle tailed (WAT) radio galaxies. Combined with existing data, we now have a sample of 18 WAT-containing clusters with more than 10 redshifts. This sample contains a substantial portion of the WAT clusters in the VLA 20 cm survey of Abell clusters, including 75% of WAT clusters in the complete survey (z&lt;=0.09), and 20% of WAT clusters with z&gt;0.09. It is a representative sample, which should not contain biases other than selection by radio morphology. We graphically present the new data using histograms and sky maps. A semiautomated procedure is used to search for emission lines in the spectra in order to add and verify galaxy redshifts. We find that the average apparent fraction of emission-line galaxies is about 9% in both the clusters and the field. We investigate the magnitude completeness of our redshift surveys with CCD data for a test case, Abell 690. This case indicates that our galaxy target lists are deeper than the detection limit of a typical MX exposure, and they are 82% complete down to R=19.0. The importance of the uniformity of the placement of fibers on targets is posited, and we evaluate this in our data sets. We find some cases of nonuniformities which may influence dynamical analyses. A second paper will use this database to look for correlations between the WAT radio morphology and the cluster's dynamical state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269#1</TD>
            <TD>2011-09-14T19:10:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/120/2269</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2269</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/120/2269 [2]</TD>
            <TD>Wide-Angle-Tailed radio galaxies redshifts (Pinkney+, 2000)</TD>
            <TD>We present new redshifts and positions for 635 galaxies in nine rich clusters containing wide-angle tailed (WAT) radio galaxies. Combined with existing data, we now have a sample of 18 WAT-containing clusters with more than 10 redshifts. This sample contains a substantial portion of the WAT clusters in the VLA 20 cm survey of Abell clusters, including 75% of WAT clusters in the complete survey (z&lt;=0.09), and 20% of WAT clusters with z&gt;0.09. It is a representative sample, which should not contain biases other than selection by radio morphology. We graphically present the new data using histograms and sky maps. A semiautomated procedure is used to search for emission lines in the spectra in order to add and verify galaxy redshifts. We find that the average apparent fraction of emission-line galaxies is about 9% in both the clusters and the field. We investigate the magnitude completeness of our redshift surveys with CCD data for a test case, Abell 690. This case indicates that our galaxy target lists are deeper than the detection limit of a typical MX exposure, and they are 82% complete down to R=19.0. The importance of the uniformity of the placement of fibers on targets is posited, and we evaluate this in our data sets. We find some cases of nonuniformities which may influence dynamical analyses. A second paper will use this database to look for correlations between the WAT radio morphology and the cluster's dynamical state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269#2</TD>
            <TD>2011-09-14T19:10:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/120/2269&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2269</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/120/2269 [table3]</TD>
            <TD>Wide-Angle-Tailed radio galaxies redshifts (Pinkney+, 2000)</TD>
            <TD>We present new redshifts and positions for 635 galaxies in nine rich clusters containing wide-angle tailed (WAT) radio galaxies. Combined with existing data, we now have a sample of 18 WAT-containing clusters with more than 10 redshifts. This sample contains a substantial portion of the WAT clusters in the VLA 20 cm survey of Abell clusters, including 75% of WAT clusters in the complete survey (z&lt;=0.09), and 20% of WAT clusters with z&gt;0.09. It is a representative sample, which should not contain biases other than selection by radio morphology. We graphically present the new data using histograms and sky maps. A semiautomated procedure is used to search for emission lines in the spectra in order to add and verify galaxy redshifts. We find that the average apparent fraction of emission-line galaxies is about 9% in both the clusters and the field. We investigate the magnitude completeness of our redshift surveys with CCD data for a test case, Abell 690. This case indicates that our galaxy target lists are deeper than the detection limit of a typical MX exposure, and they are 82% complete down to R=19.0. The importance of the uniformity of the placement of fibers on targets is posited, and we evaluate this in our data sets. We find some cases of nonuniformities which may influence dynamical analyses. A second paper will use this database to look for correlations between the WAT radio morphology and the cluster's dynamical state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269#table3</TD>
            <TD>2011-09-14T19:10:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/120/2269&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2269</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/120/2269 [1]</TD>
            <TD>Wide-Angle-Tailed radio galaxies redshifts (Pinkney+, 2000)</TD>
            <TD>We present new redshifts and positions for 635 galaxies in nine rich clusters containing wide-angle tailed (WAT) radio galaxies. Combined with existing data, we now have a sample of 18 WAT-containing clusters with more than 10 redshifts. This sample contains a substantial portion of the WAT clusters in the VLA 20 cm survey of Abell clusters, including 75% of WAT clusters in the complete survey (z&lt;=0.09), and 20% of WAT clusters with z&gt;0.09. It is a representative sample, which should not contain biases other than selection by radio morphology. We graphically present the new data using histograms and sky maps. A semiautomated procedure is used to search for emission lines in the spectra in order to add and verify galaxy redshifts. We find that the average apparent fraction of emission-line galaxies is about 9% in both the clusters and the field. We investigate the magnitude completeness of our redshift surveys with CCD data for a test case, Abell 690. This case indicates that our galaxy target lists are deeper than the detection limit of a typical MX exposure, and they are 82% complete down to R=19.0. The importance of the uniformity of the placement of fibers on targets is posited, and we evaluate this in our data sets. We find some cases of nonuniformities which may influence dynamical analyses. A second paper will use this database to look for correlations between the WAT radio morphology and the cluster's dynamical state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269#1</TD>
            <TD>2011-09-14T19:10:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/120/2269</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2269</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/120/2269 [2]</TD>
            <TD>Wide-Angle-Tailed radio galaxies redshifts (Pinkney+, 2000)</TD>
            <TD>We present new redshifts and positions for 635 galaxies in nine rich clusters containing wide-angle tailed (WAT) radio galaxies. Combined with existing data, we now have a sample of 18 WAT-containing clusters with more than 10 redshifts. This sample contains a substantial portion of the WAT clusters in the VLA 20 cm survey of Abell clusters, including 75% of WAT clusters in the complete survey (z&lt;=0.09), and 20% of WAT clusters with z&gt;0.09. It is a representative sample, which should not contain biases other than selection by radio morphology. We graphically present the new data using histograms and sky maps. A semiautomated procedure is used to search for emission lines in the spectra in order to add and verify galaxy redshifts. We find that the average apparent fraction of emission-line galaxies is about 9% in both the clusters and the field. We investigate the magnitude completeness of our redshift surveys with CCD data for a test case, Abell 690. This case indicates that our galaxy target lists are deeper than the detection limit of a typical MX exposure, and they are 82% complete down to R=19.0. The importance of the uniformity of the placement of fibers on targets is posited, and we evaluate this in our data sets. We find some cases of nonuniformities which may influence dynamical analyses. A second paper will use this database to look for correlations between the WAT radio morphology and the cluster's dynamical state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269#2</TD>
            <TD>2011-09-14T19:10:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/120/2269&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2269</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/120/2269 [table3]</TD>
            <TD>Wide-Angle-Tailed radio galaxies redshifts (Pinkney+, 2000)</TD>
            <TD>We present new redshifts and positions for 635 galaxies in nine rich clusters containing wide-angle tailed (WAT) radio galaxies. Combined with existing data, we now have a sample of 18 WAT-containing clusters with more than 10 redshifts. This sample contains a substantial portion of the WAT clusters in the VLA 20 cm survey of Abell clusters, including 75% of WAT clusters in the complete survey (z&lt;=0.09), and 20% of WAT clusters with z&gt;0.09. It is a representative sample, which should not contain biases other than selection by radio morphology. We graphically present the new data using histograms and sky maps. A semiautomated procedure is used to search for emission lines in the spectra in order to add and verify galaxy redshifts. We find that the average apparent fraction of emission-line galaxies is about 9% in both the clusters and the field. We investigate the magnitude completeness of our redshift surveys with CCD data for a test case, Abell 690. This case indicates that our galaxy target lists are deeper than the detection limit of a typical MX exposure, and they are 82% complete down to R=19.0. The importance of the uniformity of the placement of fibers on targets is posited, and we evaluate this in our data sets. We find some cases of nonuniformities which may influence dynamical analyses. A second paper will use this database to look for correlations between the WAT radio morphology and the cluster's dynamical state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269#table3</TD>
            <TD>2011-09-14T19:10:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/120/2269&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2269</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/120/2269 [1]</TD>
            <TD>Wide-Angle-Tailed radio galaxies redshifts (Pinkney+, 2000)</TD>
            <TD>We present new redshifts and positions for 635 galaxies in nine rich clusters containing wide-angle tailed (WAT) radio galaxies. Combined with existing data, we now have a sample of 18 WAT-containing clusters with more than 10 redshifts. This sample contains a substantial portion of the WAT clusters in the VLA 20 cm survey of Abell clusters, including 75% of WAT clusters in the complete survey (z&lt;=0.09), and 20% of WAT clusters with z&gt;0.09. It is a representative sample, which should not contain biases other than selection by radio morphology. We graphically present the new data using histograms and sky maps. A semiautomated procedure is used to search for emission lines in the spectra in order to add and verify galaxy redshifts. We find that the average apparent fraction of emission-line galaxies is about 9% in both the clusters and the field. We investigate the magnitude completeness of our redshift surveys with CCD data for a test case, Abell 690. This case indicates that our galaxy target lists are deeper than the detection limit of a typical MX exposure, and they are 82% complete down to R=19.0. The importance of the uniformity of the placement of fibers on targets is posited, and we evaluate this in our data sets. We find some cases of nonuniformities which may influence dynamical analyses. A second paper will use this database to look for correlations between the WAT radio morphology and the cluster's dynamical state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269#1</TD>
            <TD>2011-09-14T19:10:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/120/2269</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2269</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/120/2269 [2]</TD>
            <TD>Wide-Angle-Tailed radio galaxies redshifts (Pinkney+, 2000)</TD>
            <TD>We present new redshifts and positions for 635 galaxies in nine rich clusters containing wide-angle tailed (WAT) radio galaxies. Combined with existing data, we now have a sample of 18 WAT-containing clusters with more than 10 redshifts. This sample contains a substantial portion of the WAT clusters in the VLA 20 cm survey of Abell clusters, including 75% of WAT clusters in the complete survey (z&lt;=0.09), and 20% of WAT clusters with z&gt;0.09. It is a representative sample, which should not contain biases other than selection by radio morphology. We graphically present the new data using histograms and sky maps. A semiautomated procedure is used to search for emission lines in the spectra in order to add and verify galaxy redshifts. We find that the average apparent fraction of emission-line galaxies is about 9% in both the clusters and the field. We investigate the magnitude completeness of our redshift surveys with CCD data for a test case, Abell 690. This case indicates that our galaxy target lists are deeper than the detection limit of a typical MX exposure, and they are 82% complete down to R=19.0. The importance of the uniformity of the placement of fibers on targets is posited, and we evaluate this in our data sets. We find some cases of nonuniformities which may influence dynamical analyses. A second paper will use this database to look for correlations between the WAT radio morphology and the cluster's dynamical state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269#2</TD>
            <TD>2011-09-14T19:10:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/120/2269&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2269</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/120/2269 [table3]</TD>
            <TD>Wide-Angle-Tailed radio galaxies redshifts (Pinkney+, 2000)</TD>
            <TD>We present new redshifts and positions for 635 galaxies in nine rich clusters containing wide-angle tailed (WAT) radio galaxies. Combined with existing data, we now have a sample of 18 WAT-containing clusters with more than 10 redshifts. This sample contains a substantial portion of the WAT clusters in the VLA 20 cm survey of Abell clusters, including 75% of WAT clusters in the complete survey (z&lt;=0.09), and 20% of WAT clusters with z&gt;0.09. It is a representative sample, which should not contain biases other than selection by radio morphology. We graphically present the new data using histograms and sky maps. A semiautomated procedure is used to search for emission lines in the spectra in order to add and verify galaxy redshifts. We find that the average apparent fraction of emission-line galaxies is about 9% in both the clusters and the field. We investigate the magnitude completeness of our redshift surveys with CCD data for a test case, Abell 690. This case indicates that our galaxy target lists are deeper than the detection limit of a typical MX exposure, and they are 82% complete down to R=19.0. The importance of the uniformity of the placement of fibers on targets is posited, and we evaluate this in our data sets. We find some cases of nonuniformities which may influence dynamical analyses. A second paper will use this database to look for correlations between the WAT radio morphology and the cluster's dynamical state.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269#table3</TD>
            <TD>2011-09-14T19:10:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
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            <TD>12-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2269</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/120/2269&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2269</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/379/21 [1]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#1</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/379/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/379/21 [2]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#2</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/379/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/379/21 [table2]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#table2</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/379/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/379/21 [table1]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#table1</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/379/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/379/21 [1]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#1</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/379/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/379/21 [2]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#2</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/379/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/379/21 [table2]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#table2</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/379/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/379/21 [table1]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#table1</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/379/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/379/21 [1]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#1</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/379/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/379/21 [2]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#2</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/379/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/379/21 [table2]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#table2</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/379/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/379/21 [table1]</TD>
            <TD>Radio-optically selected galaxy clusters I. (Zanichelli+, 2001)</TD>
            <TD>The radiosource catalogs have been extracted from 31 NRAO VLA Sky Survey maps (NVSS, Condon et al., 1988AJ....115.1693C) over approximately 550 square degrees of sky in the region of the South Galactic Pole. File table1.dat contains the catalog of 13340 pointlike sources. For each source are given: Right Ascension and Declination, source name (if applicable), peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected. The name is specified for (1) pointlike sources that are detected in a multiple system (name = DSnnnn or TSnnnn) (2) sources initially classified as components of a double system, which has been considered spurious on the basis of the distance between components (name = Cnnnn or DCnnnn). File table2.dat contains the catalog of 2662 double radiosources. For each source the following parameters are given both for the barycentre and the two components: Right Ascension and Declination, source name, peak flux, flux rms from the fit, error on source position as estimated by the fitting algorithm, distance between the components of the double system, x and y pixel of the position where the peak has been detected on the map (starting position for the fit), control flags coming from the extraction algorithm, and name of the radio map where the source has been detected.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21#table1</TD>
            <TD>2011-09-14T19:11:59Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/379/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/379/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/379/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/380/578 [1]</TD>
            <TD>Equiv. widths of 13 horizontal branch stars (Tautvaisiene+, 2001)</TD>
            <TD>High-resolution spectra of 13 core helium-burning stars in the thick disk of the Galaxy have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 22 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0, 1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. Abundances in the investigated stars suggest that carbon is depleted by about 0.3dex, nitrogen is enhanced by more than 0.4dex and oxygen is unaltered. The 12C/13C ratios are lowered and lie between values 3 and 7 which is in agreement with "cool bottom processing" predictions (Boothroyd &amp; Sackmann, 1999ApJ...510..232B). The C/N ratios in the investigated stars are lowered to values between 0.7 and 1.2 which is less than present day theoretical predictions and call for further studies of stellar mixing processes. Abundance ratios of O, Mg, Eu and other heavy chemical elements to iron in the investigated stars show a pattern characteristic of thick disk stars. The results provide evidence that the thick disk population has a distinct chemical history from the thin disk. The onset of the bulk of SN Ia is suggested to appear at [Fe/H]~-0.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578#1</TD>
            <TD>2011-09-14T19:12:15Z</TD>
            <TD>#Abundances#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/380/578</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/578</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/380/578 [2]</TD>
            <TD>Equiv. widths of 13 horizontal branch stars (Tautvaisiene+, 2001)</TD>
            <TD>High-resolution spectra of 13 core helium-burning stars in the thick disk of the Galaxy have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 22 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0, 1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. Abundances in the investigated stars suggest that carbon is depleted by about 0.3dex, nitrogen is enhanced by more than 0.4dex and oxygen is unaltered. The 12C/13C ratios are lowered and lie between values 3 and 7 which is in agreement with "cool bottom processing" predictions (Boothroyd &amp; Sackmann, 1999ApJ...510..232B). The C/N ratios in the investigated stars are lowered to values between 0.7 and 1.2 which is less than present day theoretical predictions and call for further studies of stellar mixing processes. Abundance ratios of O, Mg, Eu and other heavy chemical elements to iron in the investigated stars show a pattern characteristic of thick disk stars. The results provide evidence that the thick disk population has a distinct chemical history from the thin disk. The onset of the bulk of SN Ia is suggested to appear at [Fe/H]~-0.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578#2</TD>
            <TD>2011-09-14T19:12:15Z</TD>
            <TD>#Abundances#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/380/578&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/578</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/380/578 [stars]</TD>
            <TD>Equiv. widths of 13 horizontal branch stars (Tautvaisiene+, 2001)</TD>
            <TD>High-resolution spectra of 13 core helium-burning stars in the thick disk of the Galaxy have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 22 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0, 1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. Abundances in the investigated stars suggest that carbon is depleted by about 0.3dex, nitrogen is enhanced by more than 0.4dex and oxygen is unaltered. The 12C/13C ratios are lowered and lie between values 3 and 7 which is in agreement with "cool bottom processing" predictions (Boothroyd &amp; Sackmann, 1999ApJ...510..232B). The C/N ratios in the investigated stars are lowered to values between 0.7 and 1.2 which is less than present day theoretical predictions and call for further studies of stellar mixing processes. Abundance ratios of O, Mg, Eu and other heavy chemical elements to iron in the investigated stars show a pattern characteristic of thick disk stars. The results provide evidence that the thick disk population has a distinct chemical history from the thin disk. The onset of the bulk of SN Ia is suggested to appear at [Fe/H]~-0.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578#stars</TD>
            <TD>2011-09-14T19:12:15Z</TD>
            <TD>#Abundances#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/380/578&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/578</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/380/578 [1]</TD>
            <TD>Equiv. widths of 13 horizontal branch stars (Tautvaisiene+, 2001)</TD>
            <TD>High-resolution spectra of 13 core helium-burning stars in the thick disk of the Galaxy have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 22 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0, 1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. Abundances in the investigated stars suggest that carbon is depleted by about 0.3dex, nitrogen is enhanced by more than 0.4dex and oxygen is unaltered. The 12C/13C ratios are lowered and lie between values 3 and 7 which is in agreement with "cool bottom processing" predictions (Boothroyd &amp; Sackmann, 1999ApJ...510..232B). The C/N ratios in the investigated stars are lowered to values between 0.7 and 1.2 which is less than present day theoretical predictions and call for further studies of stellar mixing processes. Abundance ratios of O, Mg, Eu and other heavy chemical elements to iron in the investigated stars show a pattern characteristic of thick disk stars. The results provide evidence that the thick disk population has a distinct chemical history from the thin disk. The onset of the bulk of SN Ia is suggested to appear at [Fe/H]~-0.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578#1</TD>
            <TD>2011-09-14T19:12:15Z</TD>
            <TD>#Abundances#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/380/578</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/578</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/380/578 [2]</TD>
            <TD>Equiv. widths of 13 horizontal branch stars (Tautvaisiene+, 2001)</TD>
            <TD>High-resolution spectra of 13 core helium-burning stars in the thick disk of the Galaxy have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 22 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0, 1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. Abundances in the investigated stars suggest that carbon is depleted by about 0.3dex, nitrogen is enhanced by more than 0.4dex and oxygen is unaltered. The 12C/13C ratios are lowered and lie between values 3 and 7 which is in agreement with "cool bottom processing" predictions (Boothroyd &amp; Sackmann, 1999ApJ...510..232B). The C/N ratios in the investigated stars are lowered to values between 0.7 and 1.2 which is less than present day theoretical predictions and call for further studies of stellar mixing processes. Abundance ratios of O, Mg, Eu and other heavy chemical elements to iron in the investigated stars show a pattern characteristic of thick disk stars. The results provide evidence that the thick disk population has a distinct chemical history from the thin disk. The onset of the bulk of SN Ia is suggested to appear at [Fe/H]~-0.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578#2</TD>
            <TD>2011-09-14T19:12:15Z</TD>
            <TD>#Abundances#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/380/578&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/578</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/380/578 [stars]</TD>
            <TD>Equiv. widths of 13 horizontal branch stars (Tautvaisiene+, 2001)</TD>
            <TD>High-resolution spectra of 13 core helium-burning stars in the thick disk of the Galaxy have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 22 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0, 1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. Abundances in the investigated stars suggest that carbon is depleted by about 0.3dex, nitrogen is enhanced by more than 0.4dex and oxygen is unaltered. The 12C/13C ratios are lowered and lie between values 3 and 7 which is in agreement with "cool bottom processing" predictions (Boothroyd &amp; Sackmann, 1999ApJ...510..232B). The C/N ratios in the investigated stars are lowered to values between 0.7 and 1.2 which is less than present day theoretical predictions and call for further studies of stellar mixing processes. Abundance ratios of O, Mg, Eu and other heavy chemical elements to iron in the investigated stars show a pattern characteristic of thick disk stars. The results provide evidence that the thick disk population has a distinct chemical history from the thin disk. The onset of the bulk of SN Ia is suggested to appear at [Fe/H]~-0.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578#stars</TD>
            <TD>2011-09-14T19:12:15Z</TD>
            <TD>#Abundances#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/380/578&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/578</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/380/578 [1]</TD>
            <TD>Equiv. widths of 13 horizontal branch stars (Tautvaisiene+, 2001)</TD>
            <TD>High-resolution spectra of 13 core helium-burning stars in the thick disk of the Galaxy have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 22 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0, 1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. Abundances in the investigated stars suggest that carbon is depleted by about 0.3dex, nitrogen is enhanced by more than 0.4dex and oxygen is unaltered. The 12C/13C ratios are lowered and lie between values 3 and 7 which is in agreement with "cool bottom processing" predictions (Boothroyd &amp; Sackmann, 1999ApJ...510..232B). The C/N ratios in the investigated stars are lowered to values between 0.7 and 1.2 which is less than present day theoretical predictions and call for further studies of stellar mixing processes. Abundance ratios of O, Mg, Eu and other heavy chemical elements to iron in the investigated stars show a pattern characteristic of thick disk stars. The results provide evidence that the thick disk population has a distinct chemical history from the thin disk. The onset of the bulk of SN Ia is suggested to appear at [Fe/H]~-0.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578#1</TD>
            <TD>2011-09-14T19:12:15Z</TD>
            <TD>#Abundances#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/380/578</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/578</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/380/578 [2]</TD>
            <TD>Equiv. widths of 13 horizontal branch stars (Tautvaisiene+, 2001)</TD>
            <TD>High-resolution spectra of 13 core helium-burning stars in the thick disk of the Galaxy have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 22 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0, 1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. Abundances in the investigated stars suggest that carbon is depleted by about 0.3dex, nitrogen is enhanced by more than 0.4dex and oxygen is unaltered. The 12C/13C ratios are lowered and lie between values 3 and 7 which is in agreement with "cool bottom processing" predictions (Boothroyd &amp; Sackmann, 1999ApJ...510..232B). The C/N ratios in the investigated stars are lowered to values between 0.7 and 1.2 which is less than present day theoretical predictions and call for further studies of stellar mixing processes. Abundance ratios of O, Mg, Eu and other heavy chemical elements to iron in the investigated stars show a pattern characteristic of thick disk stars. The results provide evidence that the thick disk population has a distinct chemical history from the thin disk. The onset of the bulk of SN Ia is suggested to appear at [Fe/H]~-0.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578#2</TD>
            <TD>2011-09-14T19:12:15Z</TD>
            <TD>#Abundances#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/380/578&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/578</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/380/578 [stars]</TD>
            <TD>Equiv. widths of 13 horizontal branch stars (Tautvaisiene+, 2001)</TD>
            <TD>High-resolution spectra of 13 core helium-burning stars in the thick disk of the Galaxy have been obtained with the SOFIN spectrograph on the Nordic Optical Telescope to investigate abundances of up to 22 chemical elements. Abundances of carbon were studied using the C_2_ Swan (0, 1) band head at 5635.5{AA}. The wavelength interval 7980-8130{AA} with strong CN features was analysed in order to determine nitrogen abundances and 12C/13C isotope ratios. The oxygen abundances were determined from the [O I] line at 6300{AA}. Abundances in the investigated stars suggest that carbon is depleted by about 0.3dex, nitrogen is enhanced by more than 0.4dex and oxygen is unaltered. The 12C/13C ratios are lowered and lie between values 3 and 7 which is in agreement with "cool bottom processing" predictions (Boothroyd &amp; Sackmann, 1999ApJ...510..232B). The C/N ratios in the investigated stars are lowered to values between 0.7 and 1.2 which is less than present day theoretical predictions and call for further studies of stellar mixing processes. Abundance ratios of O, Mg, Eu and other heavy chemical elements to iron in the investigated stars show a pattern characteristic of thick disk stars. The results provide evidence that the thick disk population has a distinct chemical history from the thin disk. The onset of the bulk of SN Ia is suggested to appear at [Fe/H]~-0.6dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578#stars</TD>
            <TD>2011-09-14T19:12:15Z</TD>
            <TD>#Abundances#Stars:peculiar#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/578</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/380/578&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/578</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/807 [1]</TD>
            <TD>Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)</TD>
            <TD>We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges ({gamma}-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identifed as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807#1</TD>
            <TD>2011-09-14T20:16:11Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/807 [2]</TD>
            <TD>Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)</TD>
            <TD>We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges ({gamma}-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identifed as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807#2</TD>
            <TD>2011-09-14T20:16:11Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/807</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/807 [lmxb]</TD>
            <TD>Catalogue of Galactic low-mass X-ray binaries (Liu+, 2007)</TD>
            <TD>We present a new edition of the catalogue of the low-mass X-ray binaries in the Galaxy and the Magellanic Clouds. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 187 low-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges ({gamma}-rays, UV, optical, IR, and radio). Some sources, however, are only tentatively identifed as low-mass X-ray binaries on the basis of their X-ray properties similar to the known low-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the low-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2006 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807#lmxb</TD>
            <TD>2011-09-14T20:16:11Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Jun-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/807</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/807&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/1803 [1]</TD>
            <TD>Large Scale Structure (Marzke+ 1996)</TD>
            <TD>We have extended the CfA Redshift Survey to low galactic latitudes to investigate the relation between the Great Wall in the North Galactic Cap and the Perseus-Pisces chain in the South Galactic Cap. We present redshifts for 2020 galaxies in the Catalogue of Galaxies and of Clusters of Galaxies (Zwicky et al. 1961-68, CGCG, Cat. &lt;VII/4&gt;) in the following regions: 4h&lt;=RA&lt;=8h, 17h&lt;=Dec.&lt;=20h, 0deg&lt;=Dec.&lt;=45deg. In these regions, the redshift catalogue includes 1664 galaxies with B(0)&lt;=15.5 (of which 820 are newly measured) and is 97% complete. We also include redshifts for an additional 356 galaxies in these regions with B(0)&gt;15.5; of these, 148 were previously unmeasured. The CGCG samples the galaxy distribution down to b_(II)_~10deg. In this paper, we discuss the acquisition and reduction of the spectra, and we examine the qualitative features of the redshift distribution. The Great Wall and the Perseus-Pisces chain are not simply connected across the Zone of Avoidance. These structures, which at first appear to be coherent on scales of ~100h^-1^Mpc or more, actually form the boundaries of neighboring voids of considerably smaller scale, approximately 50h^-1^Mpc. The structures delineated by our optically-selected sample are qualitatively similar to those detected by the far-infrared-selected IRAS 1.2 Jansky Survey (Fisher et al., 1995ApJS..100...69F). Although the IRAS survey probes more deeply into the Zone of Avoidance, our optically-selected survey provides better sampling of structures at b_(II)&gt;=10deg. (Copyright) 1996 American Astronomical Society.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803#1</TD>
            <TD>2011-09-14T18:57:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/1803</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1803</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/1803 [2]</TD>
            <TD>Large Scale Structure (Marzke+ 1996)</TD>
            <TD>We have extended the CfA Redshift Survey to low galactic latitudes to investigate the relation between the Great Wall in the North Galactic Cap and the Perseus-Pisces chain in the South Galactic Cap. We present redshifts for 2020 galaxies in the Catalogue of Galaxies and of Clusters of Galaxies (Zwicky et al. 1961-68, CGCG, Cat. &lt;VII/4&gt;) in the following regions: 4h&lt;=RA&lt;=8h, 17h&lt;=Dec.&lt;=20h, 0deg&lt;=Dec.&lt;=45deg. In these regions, the redshift catalogue includes 1664 galaxies with B(0)&lt;=15.5 (of which 820 are newly measured) and is 97% complete. We also include redshifts for an additional 356 galaxies in these regions with B(0)&gt;15.5; of these, 148 were previously unmeasured. The CGCG samples the galaxy distribution down to b_(II)_~10deg. In this paper, we discuss the acquisition and reduction of the spectra, and we examine the qualitative features of the redshift distribution. The Great Wall and the Perseus-Pisces chain are not simply connected across the Zone of Avoidance. These structures, which at first appear to be coherent on scales of ~100h^-1^Mpc or more, actually form the boundaries of neighboring voids of considerably smaller scale, approximately 50h^-1^Mpc. The structures delineated by our optically-selected sample are qualitatively similar to those detected by the far-infrared-selected IRAS 1.2 Jansky Survey (Fisher et al., 1995ApJS..100...69F). Although the IRAS survey probes more deeply into the Zone of Avoidance, our optically-selected survey provides better sampling of structures at b_(II)&gt;=10deg. (Copyright) 1996 American Astronomical Society.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803#2</TD>
            <TD>2011-09-14T18:57:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/1803&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1803</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/312/540 [1]</TD>
            <TD>Redshift survey of intercluster galaxies (Bardelli+, 2000)</TD>
            <TD>We present the results of a redshift survey of intercluster galaxies in the central region of the Shapley Concentration supercluster, aimed at determining the distribution of galaxies in between obvious overdensities. Our sample is formed by 442 new redshifts, mainly in the b_J_ magnitude range 17-18.8. Adding the data from our redshift surveys on the A3558 and A3528 complexes, which are close to the geometrical centre of this supercluster, we obtain a total sample of ~2000 radial velocities. The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of their ({alpha}, {delta} position, and it can be fitted by a plane in the three dimensional space ({alpha}, {delta}, v): the distribution of the galaxy distances around the best-fitting plane is described by a Gaussian with dispersion 3.8h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540#1</TD>
            <TD>2011-09-14T19:12:32Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/312/540</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/540</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/312/540 [2]</TD>
            <TD>Redshift survey of intercluster galaxies (Bardelli+, 2000)</TD>
            <TD>We present the results of a redshift survey of intercluster galaxies in the central region of the Shapley Concentration supercluster, aimed at determining the distribution of galaxies in between obvious overdensities. Our sample is formed by 442 new redshifts, mainly in the b_J_ magnitude range 17-18.8. Adding the data from our redshift surveys on the A3558 and A3528 complexes, which are close to the geometrical centre of this supercluster, we obtain a total sample of ~2000 radial velocities. The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of their ({alpha}, {delta} position, and it can be fitted by a plane in the three dimensional space ({alpha}, {delta}, v): the distribution of the galaxy distances around the best-fitting plane is described by a Gaussian with dispersion 3.8h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540#2</TD>
            <TD>2011-09-14T19:12:32Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/312/540&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/540</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/312/540 [table2]</TD>
            <TD>Redshift survey of intercluster galaxies (Bardelli+, 2000)</TD>
            <TD>We present the results of a redshift survey of intercluster galaxies in the central region of the Shapley Concentration supercluster, aimed at determining the distribution of galaxies in between obvious overdensities. Our sample is formed by 442 new redshifts, mainly in the b_J_ magnitude range 17-18.8. Adding the data from our redshift surveys on the A3558 and A3528 complexes, which are close to the geometrical centre of this supercluster, we obtain a total sample of ~2000 radial velocities. The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of their ({alpha}, {delta} position, and it can be fitted by a plane in the three dimensional space ({alpha}, {delta}, v): the distribution of the galaxy distances around the best-fitting plane is described by a Gaussian with dispersion 3.8h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540#table2</TD>
            <TD>2011-09-14T19:12:32Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/312/540&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/540</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/464/495 [1]</TD>
            <TD>UBVI photometry of NGC 45 star clusters (Mora+, 2007)</TD>
            <TD>Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495#1</TD>
            <TD>2011-09-14T20:16:20Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/464/495</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/495</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/464/495 [2]</TD>
            <TD>UBVI photometry of NGC 45 star clusters (Mora+, 2007)</TD>
            <TD>Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495#2</TD>
            <TD>2011-09-14T20:16:20Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/464/495&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/495</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/495 [tables]</TD>
            <TD>UBVI photometry of NGC 45 star clusters (Mora+, 2007)</TD>
            <TD>Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495#tables</TD>
            <TD>2011-09-14T20:16:20Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/495&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/495</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/1803 [1]</TD>
            <TD>Large Scale Structure (Marzke+ 1996)</TD>
            <TD>We have extended the CfA Redshift Survey to low galactic latitudes to investigate the relation between the Great Wall in the North Galactic Cap and the Perseus-Pisces chain in the South Galactic Cap. We present redshifts for 2020 galaxies in the Catalogue of Galaxies and of Clusters of Galaxies (Zwicky et al. 1961-68, CGCG, Cat. &lt;VII/4&gt;) in the following regions: 4h&lt;=RA&lt;=8h, 17h&lt;=Dec.&lt;=20h, 0deg&lt;=Dec.&lt;=45deg. In these regions, the redshift catalogue includes 1664 galaxies with B(0)&lt;=15.5 (of which 820 are newly measured) and is 97% complete. We also include redshifts for an additional 356 galaxies in these regions with B(0)&gt;15.5; of these, 148 were previously unmeasured. The CGCG samples the galaxy distribution down to b_(II)_~10deg. In this paper, we discuss the acquisition and reduction of the spectra, and we examine the qualitative features of the redshift distribution. The Great Wall and the Perseus-Pisces chain are not simply connected across the Zone of Avoidance. These structures, which at first appear to be coherent on scales of ~100h^-1^Mpc or more, actually form the boundaries of neighboring voids of considerably smaller scale, approximately 50h^-1^Mpc. The structures delineated by our optically-selected sample are qualitatively similar to those detected by the far-infrared-selected IRAS 1.2 Jansky Survey (Fisher et al., 1995ApJS..100...69F). Although the IRAS survey probes more deeply into the Zone of Avoidance, our optically-selected survey provides better sampling of structures at b_(II)&gt;=10deg. (Copyright) 1996 American Astronomical Society.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803#1</TD>
            <TD>2011-09-14T18:57:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/1803</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1803</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/1803 [2]</TD>
            <TD>Large Scale Structure (Marzke+ 1996)</TD>
            <TD>We have extended the CfA Redshift Survey to low galactic latitudes to investigate the relation between the Great Wall in the North Galactic Cap and the Perseus-Pisces chain in the South Galactic Cap. We present redshifts for 2020 galaxies in the Catalogue of Galaxies and of Clusters of Galaxies (Zwicky et al. 1961-68, CGCG, Cat. &lt;VII/4&gt;) in the following regions: 4h&lt;=RA&lt;=8h, 17h&lt;=Dec.&lt;=20h, 0deg&lt;=Dec.&lt;=45deg. In these regions, the redshift catalogue includes 1664 galaxies with B(0)&lt;=15.5 (of which 820 are newly measured) and is 97% complete. We also include redshifts for an additional 356 galaxies in these regions with B(0)&gt;15.5; of these, 148 were previously unmeasured. The CGCG samples the galaxy distribution down to b_(II)_~10deg. In this paper, we discuss the acquisition and reduction of the spectra, and we examine the qualitative features of the redshift distribution. The Great Wall and the Perseus-Pisces chain are not simply connected across the Zone of Avoidance. These structures, which at first appear to be coherent on scales of ~100h^-1^Mpc or more, actually form the boundaries of neighboring voids of considerably smaller scale, approximately 50h^-1^Mpc. The structures delineated by our optically-selected sample are qualitatively similar to those detected by the far-infrared-selected IRAS 1.2 Jansky Survey (Fisher et al., 1995ApJS..100...69F). Although the IRAS survey probes more deeply into the Zone of Avoidance, our optically-selected survey provides better sampling of structures at b_(II)&gt;=10deg. (Copyright) 1996 American Astronomical Society.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803#2</TD>
            <TD>2011-09-14T18:57:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/1803</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/1803&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/1803</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/464/495 [1]</TD>
            <TD>UBVI photometry of NGC 45 star clusters (Mora+, 2007)</TD>
            <TD>Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495#1</TD>
            <TD>2011-09-14T20:16:20Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/464/495</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/495</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/464/495 [2]</TD>
            <TD>UBVI photometry of NGC 45 star clusters (Mora+, 2007)</TD>
            <TD>Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495#2</TD>
            <TD>2011-09-14T20:16:20Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/464/495&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/495</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/495 [tables]</TD>
            <TD>UBVI photometry of NGC 45 star clusters (Mora+, 2007)</TD>
            <TD>Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495#tables</TD>
            <TD>2011-09-14T20:16:20Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/495&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/495</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/312/540 [1]</TD>
            <TD>Redshift survey of intercluster galaxies (Bardelli+, 2000)</TD>
            <TD>We present the results of a redshift survey of intercluster galaxies in the central region of the Shapley Concentration supercluster, aimed at determining the distribution of galaxies in between obvious overdensities. Our sample is formed by 442 new redshifts, mainly in the b_J_ magnitude range 17-18.8. Adding the data from our redshift surveys on the A3558 and A3528 complexes, which are close to the geometrical centre of this supercluster, we obtain a total sample of ~2000 radial velocities. The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of their ({alpha}, {delta} position, and it can be fitted by a plane in the three dimensional space ({alpha}, {delta}, v): the distribution of the galaxy distances around the best-fitting plane is described by a Gaussian with dispersion 3.8h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540#1</TD>
            <TD>2011-09-14T19:12:32Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/312/540</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/540</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/312/540 [2]</TD>
            <TD>Redshift survey of intercluster galaxies (Bardelli+, 2000)</TD>
            <TD>We present the results of a redshift survey of intercluster galaxies in the central region of the Shapley Concentration supercluster, aimed at determining the distribution of galaxies in between obvious overdensities. Our sample is formed by 442 new redshifts, mainly in the b_J_ magnitude range 17-18.8. Adding the data from our redshift surveys on the A3558 and A3528 complexes, which are close to the geometrical centre of this supercluster, we obtain a total sample of ~2000 radial velocities. The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of their ({alpha}, {delta} position, and it can be fitted by a plane in the three dimensional space ({alpha}, {delta}, v): the distribution of the galaxy distances around the best-fitting plane is described by a Gaussian with dispersion 3.8h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540#2</TD>
            <TD>2011-09-14T19:12:32Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/312/540&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/540</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/312/540 [table2]</TD>
            <TD>Redshift survey of intercluster galaxies (Bardelli+, 2000)</TD>
            <TD>We present the results of a redshift survey of intercluster galaxies in the central region of the Shapley Concentration supercluster, aimed at determining the distribution of galaxies in between obvious overdensities. Our sample is formed by 442 new redshifts, mainly in the b_J_ magnitude range 17-18.8. Adding the data from our redshift surveys on the A3558 and A3528 complexes, which are close to the geometrical centre of this supercluster, we obtain a total sample of ~2000 radial velocities. The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of their ({alpha}, {delta} position, and it can be fitted by a plane in the three dimensional space ({alpha}, {delta}, v): the distribution of the galaxy distances around the best-fitting plane is described by a Gaussian with dispersion 3.8h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540#table2</TD>
            <TD>2011-09-14T19:12:32Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/312/540&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/540</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/92/787 [1]</TD>
            <TD>Outer galaxy VLA survey (Fich 1986)</TD>
            <TD>The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787#1</TD>
            <TD>2011-09-14T18:57:57Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/92/787</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/92/787</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/92/787 [2]</TD>
            <TD>Outer galaxy VLA survey (Fich 1986)</TD>
            <TD>The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787#2</TD>
            <TD>2011-09-14T18:57:57Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/92/787&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/92/787</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/92/787 [table1]</TD>
            <TD>Outer galaxy VLA survey (Fich 1986)</TD>
            <TD>The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787#table1</TD>
            <TD>2011-09-14T18:57:57Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/92/787&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/92/787</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/464/495 [1]</TD>
            <TD>UBVI photometry of NGC 45 star clusters (Mora+, 2007)</TD>
            <TD>Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495#1</TD>
            <TD>2011-09-14T20:16:20Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/464/495</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/495</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/464/495 [2]</TD>
            <TD>UBVI photometry of NGC 45 star clusters (Mora+, 2007)</TD>
            <TD>Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495#2</TD>
            <TD>2011-09-14T20:16:20Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/464/495&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/495</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/464/495 [tables]</TD>
            <TD>UBVI photometry of NGC 45 star clusters (Mora+, 2007)</TD>
            <TD>Star clusters are present in almost all types of galaxies. Here we investigate the star cluster population in the low-luminosity, unperturbed spiral galaxy NGC 45, which is located in the nearby Sculptor group. Both the old (globular) and young star-cluster populations are studied. Previous ground-based observations have suggested that NGC 45 has few if any "massive" young star clusters. We aim to study the population of lower-mass "open" star clusters and also identify old globular clusters that could not be distinguished from foreground stars in the ground-based data. Star clusters were identified using UBVI imaging from the Advanced Camera for Surveys (ACS) and the Wide Field Planetary Camera 2 (WFPC2) on board the Hubble Space Telescope. From broad band colors and comparison with simple stellar population (SSP) models assuming a fixed metallicity, we derived the age, mass, and extinction. We also measured the radius for each star cluster candidate.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495#tables</TD>
            <TD>2011-09-14T20:16:20Z</TD>
            <TD>#Associations#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/464/495</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/464/495&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/464/495</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/92/787 [1]</TD>
            <TD>Outer galaxy VLA survey (Fich 1986)</TD>
            <TD>The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787#1</TD>
            <TD>2011-09-14T18:57:57Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/92/787</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/92/787</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/92/787 [2]</TD>
            <TD>Outer galaxy VLA survey (Fich 1986)</TD>
            <TD>The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787#2</TD>
            <TD>2011-09-14T18:57:57Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/92/787&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/92/787</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/92/787 [table1]</TD>
            <TD>Outer galaxy VLA survey (Fich 1986)</TD>
            <TD>The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787#table1</TD>
            <TD>2011-09-14T18:57:57Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/92/787&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/92/787</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/312/540 [1]</TD>
            <TD>Redshift survey of intercluster galaxies (Bardelli+, 2000)</TD>
            <TD>We present the results of a redshift survey of intercluster galaxies in the central region of the Shapley Concentration supercluster, aimed at determining the distribution of galaxies in between obvious overdensities. Our sample is formed by 442 new redshifts, mainly in the b_J_ magnitude range 17-18.8. Adding the data from our redshift surveys on the A3558 and A3528 complexes, which are close to the geometrical centre of this supercluster, we obtain a total sample of ~2000 radial velocities. The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of their ({alpha}, {delta} position, and it can be fitted by a plane in the three dimensional space ({alpha}, {delta}, v): the distribution of the galaxy distances around the best-fitting plane is described by a Gaussian with dispersion 3.8h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540#1</TD>
            <TD>2011-09-14T19:12:32Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/312/540</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/540</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/312/540 [2]</TD>
            <TD>Redshift survey of intercluster galaxies (Bardelli+, 2000)</TD>
            <TD>We present the results of a redshift survey of intercluster galaxies in the central region of the Shapley Concentration supercluster, aimed at determining the distribution of galaxies in between obvious overdensities. Our sample is formed by 442 new redshifts, mainly in the b_J_ magnitude range 17-18.8. Adding the data from our redshift surveys on the A3558 and A3528 complexes, which are close to the geometrical centre of this supercluster, we obtain a total sample of ~2000 radial velocities. The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of their ({alpha}, {delta} position, and it can be fitted by a plane in the three dimensional space ({alpha}, {delta}, v): the distribution of the galaxy distances around the best-fitting plane is described by a Gaussian with dispersion 3.8h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540#2</TD>
            <TD>2011-09-14T19:12:32Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/312/540&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/540</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/312/540 [table2]</TD>
            <TD>Redshift survey of intercluster galaxies (Bardelli+, 2000)</TD>
            <TD>We present the results of a redshift survey of intercluster galaxies in the central region of the Shapley Concentration supercluster, aimed at determining the distribution of galaxies in between obvious overdensities. Our sample is formed by 442 new redshifts, mainly in the b_J_ magnitude range 17-18.8. Adding the data from our redshift surveys on the A3558 and A3528 complexes, which are close to the geometrical centre of this supercluster, we obtain a total sample of ~2000 radial velocities. The average velocity of the observed intercluster galaxies in the Shapley Concentration appears to be a function of their ({alpha}, {delta} position, and it can be fitted by a plane in the three dimensional space ({alpha}, {delta}, v): the distribution of the galaxy distances around the best-fitting plane is described by a Gaussian with dispersion 3.8h^-1^Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540#table2</TD>
            <TD>2011-09-14T19:12:32Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/312/540</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/312/540&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/312/540</TD>
          </TR>
          <TR>
            <TD>Spectra</TD>
            <TD>ZCOSMOS DR2 SSA</TD>
            <TD>SSA Service for zCOSMOS Bright Spectroscopic Observations DR2</TD>
            <TD>SSA service on zCOSMOS Data Release DR2. The global COSMOS project is aimed at understanding the evolution of galaxies and active galactic nuclei, and in particular the role of the galactic environment in that evolution. It is built around observations of a single equatorial 1.7 deg2 field corresponding to transverse dimensions of 100 x 100 Mpc2. The zCOSMOS redshift survey is a major project (ESO Large Program 175.A-0839) that is using 600 hours of observing time with the VIMOS spectrograph on the VLT UT3, spread over five observing seasons (2005-2009). It consists of two parts (see Lilly et al., 2007, for details): the first, "zCOSMOS-bright", obtains spectra of about 20,000 galaxies selected to have Iab &lt; 22.5 across the full 1.7 deg2 of the COSMOS field. The zCOSMOS-bright sample was designed to yield a high and fairly uniform sampling rate (about 70%), with a high success rate in measuring redshifts (approaching 100% at 0.5 &lt; z &lt; 0.8), and with sufficient velocity accuracy (about 100 km/s) to efficiently map the environments of galaxies down to the scale of galaxy groups out to redshifts z ~ 1. The zCOSMOS-bright sample was designed to yield a high and fairly uniform sampling rate (about 70%), with a high success rate in measuring redshifts (approaching 100% at 0.5 &lt; z &lt; 0.8), and with sufficient velocity accuracy (about 100 km/s) to efficiently map the environments of galaxies down to the scale of galaxy groups out to redshifts z ~ 1. The second part, the "zCOSMOS-deep", will consist of about 10,000 spectra of higher redshift galaxies, colour-selected to have redshifts in the 1.4 &lt; z &lt; 3.0 range, and lying in the central 1 deg2 region of the COSMOS field. After the first two zCOSMOS observing seasons in 2005 and 2006, about a half of the zCOSMOS-bright observations had been completed, yielding a total of over 10,500 spectra from which redshift measurements have been made. This sample, the so-called "10k-sample" (Lilly et al., 2008, The Messenger, vol. 134, p. 35-40 ), is the one released here (DR2).</TD>
            <TD>German Astrophysical Virtual Observatory</TD>
            <TD>#Optical#</TD>
            <TD>ivo://www.g-vo.org/ssa.service.zcosmos_bright_dr2#1</TD>
            <TD>2009-06-17T20:24:43Z</TD>
            <TD>##</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>DR2</TD>
            <TD>ivo://www.g-vo.org/ssa.service.zcosmos_bright_dr2</TD>
            <TD>SimpleSpectralAccess</TD>
            <TD>ivo://ivoa.net/std/SSA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://www.g-vo.org/ssampe_102/SSA?archiveid=ZCOSMOS_BRIGHT_DR2&amp;</TD>
            <TD>360.0</TD>
            <TD>300</TD>
            <TD>ivo://www.g-vo.org/GAVO</TD>
            <TD>http://www.g-vo.org/ssampe_102/SSA?request=Help</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/92/787 [1]</TD>
            <TD>Outer galaxy VLA survey (Fich 1986)</TD>
            <TD>The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787#1</TD>
            <TD>2011-09-14T18:57:57Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/92/787</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/92/787</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/92/787 [2]</TD>
            <TD>Outer galaxy VLA survey (Fich 1986)</TD>
            <TD>The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787#2</TD>
            <TD>2011-09-14T18:57:57Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/92/787&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/92/787</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/92/787 [table1]</TD>
            <TD>Outer galaxy VLA survey (Fich 1986)</TD>
            <TD>The VLA has been used to make a "snapshot" survey of all radio continuum sources stronger than 0.3Jy at 21cm, smaller than 2arcmin, and in the area in the sky defined by l=93{deg} to 163{deg}, b=-4{deg} to +4{deg}. These objects were observed at 6 cm with a resolution of 4 arcsec and a sensitivity of 1mJy. A second set of observations were carried out to determine the spectral indices of all objects not resolved in the 6 cm survey. These objects were observed at a wavelength of 2cm with resolution and sensitivity similar to the 6cm survey. The purpose of this study was to identify objects within the disk of the outer parts of our galaxy. It is shown that the current lists of identified H II regions in this area are better than ~70% complete for H II regions in the Perseus arm or closer. The only supernova remnants remaining to be discovered in this field are either extremely young, and therefore possibly radio quiet, or they are among those objects too extended to be observed at the VLA in this survey (i.e., greater than 2arcmin in diameter).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787#table1</TD>
            <TD>2011-09-14T18:57:57Z</TD>
            <TD>#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/92/787</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/92/787&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/92/787</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/1383 [1]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#1</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/1383</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/1383 [2]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#2</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1c]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1c</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1b]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1b</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1d]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1d</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1a]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1a</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1e]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1e</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/95 [1]</TD>
            <TD>Stellar Component of the Galaxy, AFGL IR Survey (Grasdalen+ 1983)</TD>
            <TD>Measurements at 2.3, 3.6, 4.9, 8.7, 10, 11.4, 12.6, 19, and 23 {mu}m are included in this catalog based on observations by the Wyoming Infrared Observatory. The sources included are those from the AFGL survey with the 4mu magnitude brighter than +1.3, the 11mu magnitude brighter than -1.5, or the 20mu magnitude brighter than -4, which lie between 20 and 40 minutes in each hour of right ascension.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/95#1</TD>
            <TD>2011-09-14T18:58:27Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-MAY-1996</TD>
            <TD>ivo://CDS.VizieR/II/95</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/95</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/95</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/95 [2]</TD>
            <TD>Stellar Component of the Galaxy, AFGL IR Survey (Grasdalen+ 1983)</TD>
            <TD>Measurements at 2.3, 3.6, 4.9, 8.7, 10, 11.4, 12.6, 19, and 23 {mu}m are included in this catalog based on observations by the Wyoming Infrared Observatory. The sources included are those from the AFGL survey with the 4mu magnitude brighter than +1.3, the 11mu magnitude brighter than -1.5, or the 20mu magnitude brighter than -4, which lie between 20 and 40 minutes in each hour of right ascension.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/95#2</TD>
            <TD>2011-09-14T18:58:27Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-MAY-1996</TD>
            <TD>ivo://CDS.VizieR/II/95</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/95&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/95</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/1397 [1]</TD>
            <TD>Radio study of double-double radio galaxy 3C293 (Joshi+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397#1</TD>
            <TD>2012-04-04T08:05:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/1397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/1397 [2]</TD>
            <TD>Radio study of double-double radio galaxy 3C293 (Joshi+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397#2</TD>
            <TD>2012-04-04T08:05:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/1397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/1397 [tablea1]</TD>
            <TD>Radio study of double-double radio galaxy 3C293 (Joshi+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397#tablea1</TD>
            <TD>2012-04-04T08:05:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/1397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1397</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/1383 [1]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#1</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/1383</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/1383 [2]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#2</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1c]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1c</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1b]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1b</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1d]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1d</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1a]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1a</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1e]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1e</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/95 [1]</TD>
            <TD>Stellar Component of the Galaxy, AFGL IR Survey (Grasdalen+ 1983)</TD>
            <TD>Measurements at 2.3, 3.6, 4.9, 8.7, 10, 11.4, 12.6, 19, and 23 {mu}m are included in this catalog based on observations by the Wyoming Infrared Observatory. The sources included are those from the AFGL survey with the 4mu magnitude brighter than +1.3, the 11mu magnitude brighter than -1.5, or the 20mu magnitude brighter than -4, which lie between 20 and 40 minutes in each hour of right ascension.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/95#1</TD>
            <TD>2011-09-14T18:58:27Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-MAY-1996</TD>
            <TD>ivo://CDS.VizieR/II/95</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/95</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/95</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/95 [2]</TD>
            <TD>Stellar Component of the Galaxy, AFGL IR Survey (Grasdalen+ 1983)</TD>
            <TD>Measurements at 2.3, 3.6, 4.9, 8.7, 10, 11.4, 12.6, 19, and 23 {mu}m are included in this catalog based on observations by the Wyoming Infrared Observatory. The sources included are those from the AFGL survey with the 4mu magnitude brighter than +1.3, the 11mu magnitude brighter than -1.5, or the 20mu magnitude brighter than -4, which lie between 20 and 40 minutes in each hour of right ascension.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/95#2</TD>
            <TD>2011-09-14T18:58:27Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-MAY-1996</TD>
            <TD>ivo://CDS.VizieR/II/95</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/95&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/95</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/1397 [1]</TD>
            <TD>Radio study of double-double radio galaxy 3C293 (Joshi+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397#1</TD>
            <TD>2012-04-04T08:05:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/1397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/1397 [2]</TD>
            <TD>Radio study of double-double radio galaxy 3C293 (Joshi+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397#2</TD>
            <TD>2012-04-04T08:05:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/1397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/1397 [tablea1]</TD>
            <TD>Radio study of double-double radio galaxy 3C293 (Joshi+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397#tablea1</TD>
            <TD>2012-04-04T08:05:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/1397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1397</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/1383 [1]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#1</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/1383</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/1383 [2]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#2</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1c]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1c</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1b]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1b</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1d]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1d</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1a]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1a</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1383 [table1e]</TD>
            <TD>DIRECT BVI photometry in M31 (Mochejska+, 2001)</TD>
            <TD>DIRECT is a project to directly obtain the distances to two important galaxies in the cosmological distance ladder, M31 and M33, using detached eclipsing binaries and Cepheids. As part of our search for these variables, we have obtained photometry and positions for thousands of stellar objects within the monitored fields, covering an area of 557.8arcmin^2^. Here we present the equatorial coordinates and BVI photometry for 26,712 stars in the M31 galaxy, along the eastern arm and in the vicinity of the star-forming region NGC 206.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383#table1e</TD>
            <TD>2011-09-14T19:13:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1383</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1383&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1383</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/1397 [1]</TD>
            <TD>Radio study of double-double radio galaxy 3C293 (Joshi+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397#1</TD>
            <TD>2012-04-04T08:05:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/1397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/1397 [2]</TD>
            <TD>Radio study of double-double radio galaxy 3C293 (Joshi+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397#2</TD>
            <TD>2012-04-04T08:05:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/1397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/1397 [tablea1]</TD>
            <TD>Radio study of double-double radio galaxy 3C293 (Joshi+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397#tablea1</TD>
            <TD>2012-04-04T08:05:45Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/1397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/1397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/1397</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/95 [1]</TD>
            <TD>Stellar Component of the Galaxy, AFGL IR Survey (Grasdalen+ 1983)</TD>
            <TD>Measurements at 2.3, 3.6, 4.9, 8.7, 10, 11.4, 12.6, 19, and 23 {mu}m are included in this catalog based on observations by the Wyoming Infrared Observatory. The sources included are those from the AFGL survey with the 4mu magnitude brighter than +1.3, the 11mu magnitude brighter than -1.5, or the 20mu magnitude brighter than -4, which lie between 20 and 40 minutes in each hour of right ascension.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/95#1</TD>
            <TD>2011-09-14T18:58:27Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-MAY-1996</TD>
            <TD>ivo://CDS.VizieR/II/95</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/95</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/95</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/95 [2]</TD>
            <TD>Stellar Component of the Galaxy, AFGL IR Survey (Grasdalen+ 1983)</TD>
            <TD>Measurements at 2.3, 3.6, 4.9, 8.7, 10, 11.4, 12.6, 19, and 23 {mu}m are included in this catalog based on observations by the Wyoming Infrared Observatory. The sources included are those from the AFGL survey with the 4mu magnitude brighter than +1.3, the 11mu magnitude brighter than -1.5, or the 20mu magnitude brighter than -4, which lie between 20 and 40 minutes in each hour of right ascension.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/95#2</TD>
            <TD>2011-09-14T18:58:27Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-MAY-1996</TD>
            <TD>ivo://CDS.VizieR/II/95</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/95&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/95</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/389 [1]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#1</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/389</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/389 [2]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#2</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/389&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/389 [table2]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#table2</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/389 [clusters]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#clusters</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/3410 [1]</TD>
            <TD>FUV excess in early-type galaxies (Carter+, 2011)</TD>
            <TD>We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410#1</TD>
            <TD>2012-04-19T15:14:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/3410</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3410</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/3410 [2]</TD>
            <TD>FUV excess in early-type galaxies (Carter+, 2011)</TD>
            <TD>We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410#2</TD>
            <TD>2012-04-19T15:14:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/3410&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3410</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/3410 [galaxies]</TD>
            <TD>FUV excess in early-type galaxies (Carter+, 2011)</TD>
            <TD>We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410#galaxies</TD>
            <TD>2012-04-19T15:14:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/3410&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3410</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/137/293 [1]</TD>
            <TD>ZOAG galaxies in 115{deg}&lt;l&lt;157{deg} (Weinberger+, 1999)</TD>
            <TD>A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293#1</TD>
            <TD>2011-09-14T18:58:44Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/137/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/137/293 [2]</TD>
            <TD>ZOAG galaxies in 115{deg}&lt;l&lt;157{deg} (Weinberger+, 1999)</TD>
            <TD>A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293#2</TD>
            <TD>2011-09-14T18:58:44Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/137/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/137/293 [table2]</TD>
            <TD>ZOAG galaxies in 115{deg}&lt;l&lt;157{deg} (Weinberger+, 1999)</TD>
            <TD>A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293#table2</TD>
            <TD>2011-09-14T18:58:44Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/137/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/293</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/389 [1]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#1</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/389</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/389 [2]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#2</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/389&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/389 [table2]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#table2</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/389 [clusters]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#clusters</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/3410 [1]</TD>
            <TD>FUV excess in early-type galaxies (Carter+, 2011)</TD>
            <TD>We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410#1</TD>
            <TD>2012-04-19T15:14:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/3410</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3410</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/3410 [2]</TD>
            <TD>FUV excess in early-type galaxies (Carter+, 2011)</TD>
            <TD>We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410#2</TD>
            <TD>2012-04-19T15:14:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/3410&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3410</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/3410 [galaxies]</TD>
            <TD>FUV excess in early-type galaxies (Carter+, 2011)</TD>
            <TD>We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410#galaxies</TD>
            <TD>2012-04-19T15:14:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/3410&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3410</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/137/293 [1]</TD>
            <TD>ZOAG galaxies in 115{deg}&lt;l&lt;157{deg} (Weinberger+, 1999)</TD>
            <TD>A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293#1</TD>
            <TD>2011-09-14T18:58:44Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/137/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/137/293 [2]</TD>
            <TD>ZOAG galaxies in 115{deg}&lt;l&lt;157{deg} (Weinberger+, 1999)</TD>
            <TD>A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293#2</TD>
            <TD>2011-09-14T18:58:44Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/137/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/137/293 [table2]</TD>
            <TD>ZOAG galaxies in 115{deg}&lt;l&lt;157{deg} (Weinberger+, 1999)</TD>
            <TD>A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293#table2</TD>
            <TD>2011-09-14T18:58:44Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/137/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/293</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/389 [1]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#1</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/389</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/389 [2]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#2</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/389&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/389 [table2]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#table2</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/389 [clusters]</TD>
            <TD>CCD R photometry of 17 clusters of galaxies (Kopylov+, 2002)</TD>
            <TD>Photometric parameters for 210 early-type galaxies in the central regions for 17 clusters around the Giant Void are presented. Galaxies in the following clusters have been observed: A1298, A1361, A1427, A1468, A1542, A1551, A1609, A1637, A1666, A1691, A1700, A1739, A1793, A1823, A1834, A1885, and A1894. For each galaxy equatorial coordinates, total magnitudes in R_c_ (Kron-Cousins) band, effective radius, surface brightness and mean surface brightness are given. The derivation of the effective parameters takes the seeing into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389#clusters</TD>
            <TD>2011-09-14T19:13:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/389</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/414/3410 [1]</TD>
            <TD>FUV excess in early-type galaxies (Carter+, 2011)</TD>
            <TD>We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410#1</TD>
            <TD>2012-04-19T15:14:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/414/3410</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3410</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/414/3410 [2]</TD>
            <TD>FUV excess in early-type galaxies (Carter+, 2011)</TD>
            <TD>We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410#2</TD>
            <TD>2012-04-19T15:14:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/414/3410&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3410</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/414/3410 [galaxies]</TD>
            <TD>FUV excess in early-type galaxies (Carter+, 2011)</TD>
            <TD>We present surface photometry of a sample of 52 galaxies from the GALaxy Evolution eXplorer (GALEX) and Two-Micron All-Sky Survey (2MASS) data archives. These include 32 normal elliptical galaxies, 10 ellipticals with weak LINER or other nuclear activity and 10 star-forming ellipticals or early-type spirals. We examine the spatial distribution of the far-ultraviolet excess in these galaxies, and its correlation with dynamical and stellar population properties of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410#galaxies</TD>
            <TD>2012-04-19T15:14:21Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Feb-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/414/3410</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/414/3410&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/414/3410</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/137/293 [1]</TD>
            <TD>ZOAG galaxies in 115{deg}&lt;l&lt;157{deg} (Weinberger+, 1999)</TD>
            <TD>A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293#1</TD>
            <TD>2011-09-14T18:58:44Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/137/293</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/293</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/137/293 [2]</TD>
            <TD>ZOAG galaxies in 115{deg}&lt;l&lt;157{deg} (Weinberger+, 1999)</TD>
            <TD>A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293#2</TD>
            <TD>2011-09-14T18:58:44Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/137/293&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/293</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/137/293 [table2]</TD>
            <TD>ZOAG galaxies in 115{deg}&lt;l&lt;157{deg} (Weinberger+, 1999)</TD>
            <TD>A systematic search by microscope for non-stellar objects on 19 POSS II R film copies has led to the detection of 3455 objects. The vast majority are obscured galaxies, most of which are new. We present coordinates and optical diameters of these galaxy candidates, list coincidences with objects in optical and infrared catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293#table2</TD>
            <TD>2011-09-14T18:58:44Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/137/293</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/137/293&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/137/293</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/21 [1]</TD>
            <TD>Catalogue of Reflection Nebulae (Van den Bergh, 1966)</TD>
            <TD>A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/21#1</TD>
            <TD>2011-09-14T19:15:02Z</TD>
            <TD>#Positional_Data#Nebulae#Spectral_Classification#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/21 [2]</TD>
            <TD>Catalogue of Reflection Nebulae (Van den Bergh, 1966)</TD>
            <TD>A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/21#2</TD>
            <TD>2011-09-14T19:15:02Z</TD>
            <TD>#Positional_Data#Nebulae#Spectral_Classification#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/21 [catalog]</TD>
            <TD>Catalogue of Reflection Nebulae (Van den Bergh, 1966)</TD>
            <TD>A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/21#catalog</TD>
            <TD>2011-09-14T19:15:02Z</TD>
            <TD>#Positional_Data#Nebulae#Spectral_Classification#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/178/339 [1]</TD>
            <TD>ChaMP extended stellar survey (ChESS) (Covey+, 2008)</TD>
            <TD>We present 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS-DR6). We use morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create our catalog, the ChaMP Extended Stellar Survey (ChESS), from a sample of 2121 matched ChaMP/SDSS sources. Our cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in our final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. We present new spectral classifications and H{alpha} measurements for an additional 79 stars. The catalog is dominated by main-sequence stars; we estimate the fraction of giants in ChESS is ~10%. We identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. Future papers will present analyses of source variability and comparisons of this catalog to models of stellar activity in the Galactic disk.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339#1</TD>
            <TD>2011-09-14T20:35:48Z</TD>
            <TD>#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/178/339</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/339</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/178/339 [2]</TD>
            <TD>ChaMP extended stellar survey (ChESS) (Covey+, 2008)</TD>
            <TD>We present 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS-DR6). We use morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create our catalog, the ChaMP Extended Stellar Survey (ChESS), from a sample of 2121 matched ChaMP/SDSS sources. Our cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in our final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. We present new spectral classifications and H{alpha} measurements for an additional 79 stars. The catalog is dominated by main-sequence stars; we estimate the fraction of giants in ChESS is ~10%. We identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. Future papers will present analyses of source variability and comparisons of this catalog to models of stellar activity in the Galactic disk.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339#2</TD>
            <TD>2011-09-14T20:35:48Z</TD>
            <TD>#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/178/339&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/339</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/339 [table3]</TD>
            <TD>ChaMP extended stellar survey (ChESS) (Covey+, 2008)</TD>
            <TD>We present 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS-DR6). We use morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create our catalog, the ChaMP Extended Stellar Survey (ChESS), from a sample of 2121 matched ChaMP/SDSS sources. Our cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in our final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. We present new spectral classifications and H{alpha} measurements for an additional 79 stars. The catalog is dominated by main-sequence stars; we estimate the fraction of giants in ChESS is ~10%. We identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. Future papers will present analyses of source variability and comparisons of this catalog to models of stellar activity in the Galactic disk.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339#table3</TD>
            <TD>2011-09-14T20:35:48Z</TD>
            <TD>#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/339&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/339</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/75 [1]</TD>
            <TD>BR photometry in Coma, A2199 &amp; AWM5 clusters (Conselice+, 1999)</TD>
            <TD>We present the results of a study on galaxy interactions, tides, and other processes that produce luminous fine-scale substructures in the galaxy clusters: Coma, Perseus, Abell 2199, AWM 3, and AWM 5. All unusual structures in these clusters can be categorized into seven morphologies: interacting galaxies, multiple galaxies (noninteracting), distorted galaxies, tailed galaxies, line galaxies, dwarf galaxy groups, and galaxy aggregates. The various morphologies are described, and a catalog is presented, of 248 objects in these five clusters along with color, and positional information obtained from CCD images taken with the WIYN 3.5 m telescope in broadband B and R filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75#1</TD>
            <TD>2011-09-14T18:59:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/75</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/75</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/75 [2]</TD>
            <TD>BR photometry in Coma, A2199 &amp; AWM5 clusters (Conselice+, 1999)</TD>
            <TD>We present the results of a study on galaxy interactions, tides, and other processes that produce luminous fine-scale substructures in the galaxy clusters: Coma, Perseus, Abell 2199, AWM 3, and AWM 5. All unusual structures in these clusters can be categorized into seven morphologies: interacting galaxies, multiple galaxies (noninteracting), distorted galaxies, tailed galaxies, line galaxies, dwarf galaxy groups, and galaxy aggregates. The various morphologies are described, and a catalog is presented, of 248 objects in these five clusters along with color, and positional information obtained from CCD images taken with the WIYN 3.5 m telescope in broadband B and R filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75#2</TD>
            <TD>2011-09-14T18:59:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/75&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/75</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/21 [1]</TD>
            <TD>Catalogue of Reflection Nebulae (Van den Bergh, 1966)</TD>
            <TD>A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/21#1</TD>
            <TD>2011-09-14T19:15:02Z</TD>
            <TD>#Positional_Data#Nebulae#Spectral_Classification#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/21 [2]</TD>
            <TD>Catalogue of Reflection Nebulae (Van den Bergh, 1966)</TD>
            <TD>A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/21#2</TD>
            <TD>2011-09-14T19:15:02Z</TD>
            <TD>#Positional_Data#Nebulae#Spectral_Classification#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/21 [catalog]</TD>
            <TD>Catalogue of Reflection Nebulae (Van den Bergh, 1966)</TD>
            <TD>A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/21#catalog</TD>
            <TD>2011-09-14T19:15:02Z</TD>
            <TD>#Positional_Data#Nebulae#Spectral_Classification#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/178/339 [1]</TD>
            <TD>ChaMP extended stellar survey (ChESS) (Covey+, 2008)</TD>
            <TD>We present 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS-DR6). We use morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create our catalog, the ChaMP Extended Stellar Survey (ChESS), from a sample of 2121 matched ChaMP/SDSS sources. Our cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in our final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. We present new spectral classifications and H{alpha} measurements for an additional 79 stars. The catalog is dominated by main-sequence stars; we estimate the fraction of giants in ChESS is ~10%. We identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. Future papers will present analyses of source variability and comparisons of this catalog to models of stellar activity in the Galactic disk.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339#1</TD>
            <TD>2011-09-14T20:35:48Z</TD>
            <TD>#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/178/339</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/339</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/178/339 [2]</TD>
            <TD>ChaMP extended stellar survey (ChESS) (Covey+, 2008)</TD>
            <TD>We present 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS-DR6). We use morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create our catalog, the ChaMP Extended Stellar Survey (ChESS), from a sample of 2121 matched ChaMP/SDSS sources. Our cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in our final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. We present new spectral classifications and H{alpha} measurements for an additional 79 stars. The catalog is dominated by main-sequence stars; we estimate the fraction of giants in ChESS is ~10%. We identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. Future papers will present analyses of source variability and comparisons of this catalog to models of stellar activity in the Galactic disk.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339#2</TD>
            <TD>2011-09-14T20:35:48Z</TD>
            <TD>#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/178/339&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/339</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/339 [table3]</TD>
            <TD>ChaMP extended stellar survey (ChESS) (Covey+, 2008)</TD>
            <TD>We present 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS-DR6). We use morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create our catalog, the ChaMP Extended Stellar Survey (ChESS), from a sample of 2121 matched ChaMP/SDSS sources. Our cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in our final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. We present new spectral classifications and H{alpha} measurements for an additional 79 stars. The catalog is dominated by main-sequence stars; we estimate the fraction of giants in ChESS is ~10%. We identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. Future papers will present analyses of source variability and comparisons of this catalog to models of stellar activity in the Galactic disk.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339#table3</TD>
            <TD>2011-09-14T20:35:48Z</TD>
            <TD>#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/339&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/339</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/75 [1]</TD>
            <TD>BR photometry in Coma, A2199 &amp; AWM5 clusters (Conselice+, 1999)</TD>
            <TD>We present the results of a study on galaxy interactions, tides, and other processes that produce luminous fine-scale substructures in the galaxy clusters: Coma, Perseus, Abell 2199, AWM 3, and AWM 5. All unusual structures in these clusters can be categorized into seven morphologies: interacting galaxies, multiple galaxies (noninteracting), distorted galaxies, tailed galaxies, line galaxies, dwarf galaxy groups, and galaxy aggregates. The various morphologies are described, and a catalog is presented, of 248 objects in these five clusters along with color, and positional information obtained from CCD images taken with the WIYN 3.5 m telescope in broadband B and R filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75#1</TD>
            <TD>2011-09-14T18:59:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/75</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/75</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/75 [2]</TD>
            <TD>BR photometry in Coma, A2199 &amp; AWM5 clusters (Conselice+, 1999)</TD>
            <TD>We present the results of a study on galaxy interactions, tides, and other processes that produce luminous fine-scale substructures in the galaxy clusters: Coma, Perseus, Abell 2199, AWM 3, and AWM 5. All unusual structures in these clusters can be categorized into seven morphologies: interacting galaxies, multiple galaxies (noninteracting), distorted galaxies, tailed galaxies, line galaxies, dwarf galaxy groups, and galaxy aggregates. The various morphologies are described, and a catalog is presented, of 248 objects in these five clusters along with color, and positional information obtained from CCD images taken with the WIYN 3.5 m telescope in broadband B and R filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75#2</TD>
            <TD>2011-09-14T18:59:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/75&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/75</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/178/339 [1]</TD>
            <TD>ChaMP extended stellar survey (ChESS) (Covey+, 2008)</TD>
            <TD>We present 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS-DR6). We use morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create our catalog, the ChaMP Extended Stellar Survey (ChESS), from a sample of 2121 matched ChaMP/SDSS sources. Our cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in our final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. We present new spectral classifications and H{alpha} measurements for an additional 79 stars. The catalog is dominated by main-sequence stars; we estimate the fraction of giants in ChESS is ~10%. We identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. Future papers will present analyses of source variability and comparisons of this catalog to models of stellar activity in the Galactic disk.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339#1</TD>
            <TD>2011-09-14T20:35:48Z</TD>
            <TD>#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/178/339</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/339</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/178/339 [2]</TD>
            <TD>ChaMP extended stellar survey (ChESS) (Covey+, 2008)</TD>
            <TD>We present 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS-DR6). We use morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create our catalog, the ChaMP Extended Stellar Survey (ChESS), from a sample of 2121 matched ChaMP/SDSS sources. Our cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in our final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. We present new spectral classifications and H{alpha} measurements for an additional 79 stars. The catalog is dominated by main-sequence stars; we estimate the fraction of giants in ChESS is ~10%. We identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. Future papers will present analyses of source variability and comparisons of this catalog to models of stellar activity in the Galactic disk.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339#2</TD>
            <TD>2011-09-14T20:35:48Z</TD>
            <TD>#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/178/339&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/339</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/339 [table3]</TD>
            <TD>ChaMP extended stellar survey (ChESS) (Covey+, 2008)</TD>
            <TD>We present 348 X-ray-emitting stars identified from correlating the Extended Chandra Multiwavelength Project (ChaMP), a wide-area serendipitous survey based on archival X-ray images, with the Sloan Digital Sky Survey (SDSS-DR6). We use morphological star/galaxy separation, matching to an SDSS quasar catalog, an optical color-magnitude cut, and X-ray data-quality tests to create our catalog, the ChaMP Extended Stellar Survey (ChESS), from a sample of 2121 matched ChaMP/SDSS sources. Our cuts retain 92% of the spectroscopically confirmed stars in the original sample while excluding 99.6% of the 684 spectroscopically confirmed extragalactic sources. Fewer than 3% of the sources in our final catalog are previously identified stellar X-ray emitters. For 42 catalog members, spectroscopic classifications are available in the literature. We present new spectral classifications and H{alpha} measurements for an additional 79 stars. The catalog is dominated by main-sequence stars; we estimate the fraction of giants in ChESS is ~10%. We identify seven giant stars (including a possible Cepheid and an RR Lyrae star) as ChaMP sources, as well as three cataclysmic variables. Future papers will present analyses of source variability and comparisons of this catalog to models of stellar activity in the Galactic disk.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339#table3</TD>
            <TD>2011-09-14T20:35:48Z</TD>
            <TD>#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/339</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/339&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/339</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/21 [1]</TD>
            <TD>Catalogue of Reflection Nebulae (Van den Bergh, 1966)</TD>
            <TD>A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/21#1</TD>
            <TD>2011-09-14T19:15:02Z</TD>
            <TD>#Positional_Data#Nebulae#Spectral_Classification#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/21 [2]</TD>
            <TD>Catalogue of Reflection Nebulae (Van den Bergh, 1966)</TD>
            <TD>A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/21#2</TD>
            <TD>2011-09-14T19:15:02Z</TD>
            <TD>#Positional_Data#Nebulae#Spectral_Classification#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/21 [catalog]</TD>
            <TD>Catalogue of Reflection Nebulae (Van den Bergh, 1966)</TD>
            <TD>A catalogue is given of all BD and CD stars north of -33deg which are surrounded by reflection nebulosity visible on both the blue and red prints of the Palomar Sky Survey. The nearer reflection nebulae lie predominantly along Gould's Belt, whereas the more distant ones are concentrated to the galactic plane. The data outline 13 associations of reflection nebulae, some of which coincide with known OB or T associations. Attention is drawn to the fact that most reflection nebulae are illuminated by the integrated light of the Milky Way. The integrated radiation will be more intense above and below the galactic plane then in the galactic plane where the nuclear bulge of the Galaxy and most of the disk are obscured by interstellar absorption.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/21#catalog</TD>
            <TD>2011-09-14T19:15:02Z</TD>
            <TD>#Positional_Data#Nebulae#Spectral_Classification#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Apr-1998</TD>
            <TD>ivo://CDS.VizieR/VII/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/495/379 [1]</TD>
            <TD>Optical radial velocities in A85 (Bravo-Alfaro+, 2009)</TD>
            <TD>We obtained position and optical magnitude data for galaxies in the A 85/87/89 complex from the SuperCOSMOS Science Archive, available from the Royal Observatory of Edinburgh, http://surveys.roe.ac.uk/ssa/index.html . The area covers a region of 50 arcmin radius around the center of A 85, taken as the position of its cD galaxy, MCG-02-02-086, which also coincides with the peak of the X-ray emission of the cluster. Magnitudes in b_J_ and r_F_ bands came from the digitization of UKST Survey plates (IIIa-J + GG395 and IIIa-F + OG590, respectively) by the SuperCOSMOS machine, using 10um size pixels (0.67").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379#1</TD>
            <TD>2011-09-14T20:36:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/495/379</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/379</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/495/379 [2]</TD>
            <TD>Optical radial velocities in A85 (Bravo-Alfaro+, 2009)</TD>
            <TD>We obtained position and optical magnitude data for galaxies in the A 85/87/89 complex from the SuperCOSMOS Science Archive, available from the Royal Observatory of Edinburgh, http://surveys.roe.ac.uk/ssa/index.html . The area covers a region of 50 arcmin radius around the center of A 85, taken as the position of its cD galaxy, MCG-02-02-086, which also coincides with the peak of the X-ray emission of the cluster. Magnitudes in b_J_ and r_F_ bands came from the digitization of UKST Survey plates (IIIa-J + GG395 and IIIa-F + OG590, respectively) by the SuperCOSMOS machine, using 10um size pixels (0.67").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379#2</TD>
            <TD>2011-09-14T20:36:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/495/379&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/379</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/495/379 [table1]</TD>
            <TD>Optical radial velocities in A85 (Bravo-Alfaro+, 2009)</TD>
            <TD>We obtained position and optical magnitude data for galaxies in the A 85/87/89 complex from the SuperCOSMOS Science Archive, available from the Royal Observatory of Edinburgh, http://surveys.roe.ac.uk/ssa/index.html . The area covers a region of 50 arcmin radius around the center of A 85, taken as the position of its cD galaxy, MCG-02-02-086, which also coincides with the peak of the X-ray emission of the cluster. Magnitudes in b_J_ and r_F_ bands came from the digitization of UKST Survey plates (IIIa-J + GG395 and IIIa-F + OG590, respectively) by the SuperCOSMOS machine, using 10um size pixels (0.67").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379#table1</TD>
            <TD>2011-09-14T20:36:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/495/379&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/379</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/75 [1]</TD>
            <TD>BR photometry in Coma, A2199 &amp; AWM5 clusters (Conselice+, 1999)</TD>
            <TD>We present the results of a study on galaxy interactions, tides, and other processes that produce luminous fine-scale substructures in the galaxy clusters: Coma, Perseus, Abell 2199, AWM 3, and AWM 5. All unusual structures in these clusters can be categorized into seven morphologies: interacting galaxies, multiple galaxies (noninteracting), distorted galaxies, tailed galaxies, line galaxies, dwarf galaxy groups, and galaxy aggregates. The various morphologies are described, and a catalog is presented, of 248 objects in these five clusters along with color, and positional information obtained from CCD images taken with the WIYN 3.5 m telescope in broadband B and R filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75#1</TD>
            <TD>2011-09-14T18:59:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/75</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/75</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/75 [2]</TD>
            <TD>BR photometry in Coma, A2199 &amp; AWM5 clusters (Conselice+, 1999)</TD>
            <TD>We present the results of a study on galaxy interactions, tides, and other processes that produce luminous fine-scale substructures in the galaxy clusters: Coma, Perseus, Abell 2199, AWM 3, and AWM 5. All unusual structures in these clusters can be categorized into seven morphologies: interacting galaxies, multiple galaxies (noninteracting), distorted galaxies, tailed galaxies, line galaxies, dwarf galaxy groups, and galaxy aggregates. The various morphologies are described, and a catalog is presented, of 248 objects in these five clusters along with color, and positional information obtained from CCD images taken with the WIYN 3.5 m telescope in broadband B and R filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75#2</TD>
            <TD>2011-09-14T18:59:15Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/75</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/75&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/75</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/495/379 [1]</TD>
            <TD>Optical radial velocities in A85 (Bravo-Alfaro+, 2009)</TD>
            <TD>We obtained position and optical magnitude data for galaxies in the A 85/87/89 complex from the SuperCOSMOS Science Archive, available from the Royal Observatory of Edinburgh, http://surveys.roe.ac.uk/ssa/index.html . The area covers a region of 50 arcmin radius around the center of A 85, taken as the position of its cD galaxy, MCG-02-02-086, which also coincides with the peak of the X-ray emission of the cluster. Magnitudes in b_J_ and r_F_ bands came from the digitization of UKST Survey plates (IIIa-J + GG395 and IIIa-F + OG590, respectively) by the SuperCOSMOS machine, using 10um size pixels (0.67").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379#1</TD>
            <TD>2011-09-14T20:36:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/495/379</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/379</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/495/379 [2]</TD>
            <TD>Optical radial velocities in A85 (Bravo-Alfaro+, 2009)</TD>
            <TD>We obtained position and optical magnitude data for galaxies in the A 85/87/89 complex from the SuperCOSMOS Science Archive, available from the Royal Observatory of Edinburgh, http://surveys.roe.ac.uk/ssa/index.html . The area covers a region of 50 arcmin radius around the center of A 85, taken as the position of its cD galaxy, MCG-02-02-086, which also coincides with the peak of the X-ray emission of the cluster. Magnitudes in b_J_ and r_F_ bands came from the digitization of UKST Survey plates (IIIa-J + GG395 and IIIa-F + OG590, respectively) by the SuperCOSMOS machine, using 10um size pixels (0.67").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379#2</TD>
            <TD>2011-09-14T20:36:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/495/379&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/379</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/495/379 [table1]</TD>
            <TD>Optical radial velocities in A85 (Bravo-Alfaro+, 2009)</TD>
            <TD>We obtained position and optical magnitude data for galaxies in the A 85/87/89 complex from the SuperCOSMOS Science Archive, available from the Royal Observatory of Edinburgh, http://surveys.roe.ac.uk/ssa/index.html . The area covers a region of 50 arcmin radius around the center of A 85, taken as the position of its cD galaxy, MCG-02-02-086, which also coincides with the peak of the X-ray emission of the cluster. Magnitudes in b_J_ and r_F_ bands came from the digitization of UKST Survey plates (IIIa-J + GG395 and IIIa-F + OG590, respectively) by the SuperCOSMOS machine, using 10um size pixels (0.67").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379#table1</TD>
            <TD>2011-09-14T20:36:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/495/379&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/379</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/495/379 [1]</TD>
            <TD>Optical radial velocities in A85 (Bravo-Alfaro+, 2009)</TD>
            <TD>We obtained position and optical magnitude data for galaxies in the A 85/87/89 complex from the SuperCOSMOS Science Archive, available from the Royal Observatory of Edinburgh, http://surveys.roe.ac.uk/ssa/index.html . The area covers a region of 50 arcmin radius around the center of A 85, taken as the position of its cD galaxy, MCG-02-02-086, which also coincides with the peak of the X-ray emission of the cluster. Magnitudes in b_J_ and r_F_ bands came from the digitization of UKST Survey plates (IIIa-J + GG395 and IIIa-F + OG590, respectively) by the SuperCOSMOS machine, using 10um size pixels (0.67").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379#1</TD>
            <TD>2011-09-14T20:36:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/495/379</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/379</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/495/379 [2]</TD>
            <TD>Optical radial velocities in A85 (Bravo-Alfaro+, 2009)</TD>
            <TD>We obtained position and optical magnitude data for galaxies in the A 85/87/89 complex from the SuperCOSMOS Science Archive, available from the Royal Observatory of Edinburgh, http://surveys.roe.ac.uk/ssa/index.html . The area covers a region of 50 arcmin radius around the center of A 85, taken as the position of its cD galaxy, MCG-02-02-086, which also coincides with the peak of the X-ray emission of the cluster. Magnitudes in b_J_ and r_F_ bands came from the digitization of UKST Survey plates (IIIa-J + GG395 and IIIa-F + OG590, respectively) by the SuperCOSMOS machine, using 10um size pixels (0.67").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379#2</TD>
            <TD>2011-09-14T20:36:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/495/379&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/379</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/495/379 [table1]</TD>
            <TD>Optical radial velocities in A85 (Bravo-Alfaro+, 2009)</TD>
            <TD>We obtained position and optical magnitude data for galaxies in the A 85/87/89 complex from the SuperCOSMOS Science Archive, available from the Royal Observatory of Edinburgh, http://surveys.roe.ac.uk/ssa/index.html . The area covers a region of 50 arcmin radius around the center of A 85, taken as the position of its cD galaxy, MCG-02-02-086, which also coincides with the peak of the X-ray emission of the cluster. Magnitudes in b_J_ and r_F_ bands came from the digitization of UKST Survey plates (IIIa-J + GG395 and IIIa-F + OG590, respectively) by the SuperCOSMOS machine, using 10um size pixels (0.67").</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379#table1</TD>
            <TD>2011-09-14T20:36:13Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/495/379</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/495/379&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/495/379</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/381/420 [1]</TD>
            <TD>Group of Galaxies in the SSRS2 catalog (Adami+, 2002)</TD>
            <TD>We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog (Southern Sky Redshift Survey, Da Costa et al., Cat. J/AJ/116/1). The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420#1</TD>
            <TD>2011-09-14T19:15:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/381/420</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/381/420</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/381/420 [2]</TD>
            <TD>Group of Galaxies in the SSRS2 catalog (Adami+, 2002)</TD>
            <TD>We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog (Southern Sky Redshift Survey, Da Costa et al., Cat. J/AJ/116/1). The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420#2</TD>
            <TD>2011-09-14T19:15:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/381/420&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/381/420</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/381/420 [tables]</TD>
            <TD>Group of Galaxies in the SSRS2 catalog (Adami+, 2002)</TD>
            <TD>We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog (Southern Sky Redshift Survey, Da Costa et al., Cat. J/AJ/116/1). The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420#tables</TD>
            <TD>2011-09-14T19:15:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/381/420&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/381/420</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/502/91 [1]</TD>
            <TD>Proper motions of stars near SgrA* (Schoedel+, 2009)</TD>
            <TD>We used multi-epoch adaptive optics assisted near-infrared observations of the central parsec of the Galaxy obtained with NACO/CONICA at the ESO VLT. Stellar positions were measured via PSF fitting in the individual images and transformed into a common reference frame via suitable sets of reference stars. We measured the proper motions of more than 6000 stars within about 1pc projected distance of the supermassive black hole Sagittarius A*. The table contains for each measured star its projected distance from Sagittarius A*, its offsets in right ascension and declination from Sagittarius A* along with the corresponding uncertainties, its proper motion and the corresponding uncertainty in right ascension and declination, the Ks-band magnitude and the corresponding uncertainty, and its classification as early type in case such a classification exists.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91#1</TD>
            <TD>2011-09-14T20:36:39Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/502/91</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/91</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/502/91 [2]</TD>
            <TD>Proper motions of stars near SgrA* (Schoedel+, 2009)</TD>
            <TD>We used multi-epoch adaptive optics assisted near-infrared observations of the central parsec of the Galaxy obtained with NACO/CONICA at the ESO VLT. Stellar positions were measured via PSF fitting in the individual images and transformed into a common reference frame via suitable sets of reference stars. We measured the proper motions of more than 6000 stars within about 1pc projected distance of the supermassive black hole Sagittarius A*. The table contains for each measured star its projected distance from Sagittarius A*, its offsets in right ascension and declination from Sagittarius A* along with the corresponding uncertainties, its proper motion and the corresponding uncertainty in right ascension and declination, the Ks-band magnitude and the corresponding uncertainty, and its classification as early type in case such a classification exists.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91#2</TD>
            <TD>2011-09-14T20:36:39Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/502/91&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/502/91 [tableb1]</TD>
            <TD>Proper motions of stars near SgrA* (Schoedel+, 2009)</TD>
            <TD>We used multi-epoch adaptive optics assisted near-infrared observations of the central parsec of the Galaxy obtained with NACO/CONICA at the ESO VLT. Stellar positions were measured via PSF fitting in the individual images and transformed into a common reference frame via suitable sets of reference stars. We measured the proper motions of more than 6000 stars within about 1pc projected distance of the supermassive black hole Sagittarius A*. The table contains for each measured star its projected distance from Sagittarius A*, its offsets in right ascension and declination from Sagittarius A* along with the corresponding uncertainties, its proper motion and the corresponding uncertainty in right ascension and declination, the Ks-band magnitude and the corresponding uncertainty, and its classification as early type in case such a classification exists.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91#tableb1</TD>
            <TD>2011-09-14T20:36:39Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/502/91&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/91</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/84/1305 [1]</TD>
            <TD>UBV photometry in NGC 6528 (van den Bergh+, 1979)</TD>
            <TD>On the basis of its color-magnitude diagram NGC 6528 is one of the two most metal-rich globular clusters that have so far been found in the Galaxy. Such a conclusion is consistent with Morgan's metallic line-strength classification of the integrated spectrum of this cluster. The reddening of NGC 6528 is estimated to be E(B-V)=0.52+/-0.07, from which R=6.1kpc and Z=-0.4kpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/84/1305#1</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/84/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/84/1305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/84/1305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/84/1305 [2]</TD>
            <TD>UBV photometry in NGC 6528 (van den Bergh+, 1979)</TD>
            <TD>On the basis of its color-magnitude diagram NGC 6528 is one of the two most metal-rich globular clusters that have so far been found in the Galaxy. Such a conclusion is consistent with Morgan's metallic line-strength classification of the integrated spectrum of this cluster. The reddening of NGC 6528 is estimated to be E(B-V)=0.52+/-0.07, from which R=6.1kpc and Z=-0.4kpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/84/1305#2</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/84/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/84/1305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/84/1305</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/502/91 [1]</TD>
            <TD>Proper motions of stars near SgrA* (Schoedel+, 2009)</TD>
            <TD>We used multi-epoch adaptive optics assisted near-infrared observations of the central parsec of the Galaxy obtained with NACO/CONICA at the ESO VLT. Stellar positions were measured via PSF fitting in the individual images and transformed into a common reference frame via suitable sets of reference stars. We measured the proper motions of more than 6000 stars within about 1pc projected distance of the supermassive black hole Sagittarius A*. The table contains for each measured star its projected distance from Sagittarius A*, its offsets in right ascension and declination from Sagittarius A* along with the corresponding uncertainties, its proper motion and the corresponding uncertainty in right ascension and declination, the Ks-band magnitude and the corresponding uncertainty, and its classification as early type in case such a classification exists.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91#1</TD>
            <TD>2011-09-14T20:36:39Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/502/91</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/91</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/502/91 [2]</TD>
            <TD>Proper motions of stars near SgrA* (Schoedel+, 2009)</TD>
            <TD>We used multi-epoch adaptive optics assisted near-infrared observations of the central parsec of the Galaxy obtained with NACO/CONICA at the ESO VLT. Stellar positions were measured via PSF fitting in the individual images and transformed into a common reference frame via suitable sets of reference stars. We measured the proper motions of more than 6000 stars within about 1pc projected distance of the supermassive black hole Sagittarius A*. The table contains for each measured star its projected distance from Sagittarius A*, its offsets in right ascension and declination from Sagittarius A* along with the corresponding uncertainties, its proper motion and the corresponding uncertainty in right ascension and declination, the Ks-band magnitude and the corresponding uncertainty, and its classification as early type in case such a classification exists.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91#2</TD>
            <TD>2011-09-14T20:36:39Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/502/91&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/502/91 [tableb1]</TD>
            <TD>Proper motions of stars near SgrA* (Schoedel+, 2009)</TD>
            <TD>We used multi-epoch adaptive optics assisted near-infrared observations of the central parsec of the Galaxy obtained with NACO/CONICA at the ESO VLT. Stellar positions were measured via PSF fitting in the individual images and transformed into a common reference frame via suitable sets of reference stars. We measured the proper motions of more than 6000 stars within about 1pc projected distance of the supermassive black hole Sagittarius A*. The table contains for each measured star its projected distance from Sagittarius A*, its offsets in right ascension and declination from Sagittarius A* along with the corresponding uncertainties, its proper motion and the corresponding uncertainty in right ascension and declination, the Ks-band magnitude and the corresponding uncertainty, and its classification as early type in case such a classification exists.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91#tableb1</TD>
            <TD>2011-09-14T20:36:39Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/502/91&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/91</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/381/420 [1]</TD>
            <TD>Group of Galaxies in the SSRS2 catalog (Adami+, 2002)</TD>
            <TD>We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog (Southern Sky Redshift Survey, Da Costa et al., Cat. J/AJ/116/1). The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420#1</TD>
            <TD>2011-09-14T19:15:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/381/420</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/381/420</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/381/420 [2]</TD>
            <TD>Group of Galaxies in the SSRS2 catalog (Adami+, 2002)</TD>
            <TD>We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog (Southern Sky Redshift Survey, Da Costa et al., Cat. J/AJ/116/1). The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420#2</TD>
            <TD>2011-09-14T19:15:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/381/420&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/381/420</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/381/420 [tables]</TD>
            <TD>Group of Galaxies in the SSRS2 catalog (Adami+, 2002)</TD>
            <TD>We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog (Southern Sky Redshift Survey, Da Costa et al., Cat. J/AJ/116/1). The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420#tables</TD>
            <TD>2011-09-14T19:15:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/381/420&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/381/420</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/502/91 [1]</TD>
            <TD>Proper motions of stars near SgrA* (Schoedel+, 2009)</TD>
            <TD>We used multi-epoch adaptive optics assisted near-infrared observations of the central parsec of the Galaxy obtained with NACO/CONICA at the ESO VLT. Stellar positions were measured via PSF fitting in the individual images and transformed into a common reference frame via suitable sets of reference stars. We measured the proper motions of more than 6000 stars within about 1pc projected distance of the supermassive black hole Sagittarius A*. The table contains for each measured star its projected distance from Sagittarius A*, its offsets in right ascension and declination from Sagittarius A* along with the corresponding uncertainties, its proper motion and the corresponding uncertainty in right ascension and declination, the Ks-band magnitude and the corresponding uncertainty, and its classification as early type in case such a classification exists.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91#1</TD>
            <TD>2011-09-14T20:36:39Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/502/91</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/91</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/502/91 [2]</TD>
            <TD>Proper motions of stars near SgrA* (Schoedel+, 2009)</TD>
            <TD>We used multi-epoch adaptive optics assisted near-infrared observations of the central parsec of the Galaxy obtained with NACO/CONICA at the ESO VLT. Stellar positions were measured via PSF fitting in the individual images and transformed into a common reference frame via suitable sets of reference stars. We measured the proper motions of more than 6000 stars within about 1pc projected distance of the supermassive black hole Sagittarius A*. The table contains for each measured star its projected distance from Sagittarius A*, its offsets in right ascension and declination from Sagittarius A* along with the corresponding uncertainties, its proper motion and the corresponding uncertainty in right ascension and declination, the Ks-band magnitude and the corresponding uncertainty, and its classification as early type in case such a classification exists.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91#2</TD>
            <TD>2011-09-14T20:36:39Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/502/91&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/91</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/502/91 [tableb1]</TD>
            <TD>Proper motions of stars near SgrA* (Schoedel+, 2009)</TD>
            <TD>We used multi-epoch adaptive optics assisted near-infrared observations of the central parsec of the Galaxy obtained with NACO/CONICA at the ESO VLT. Stellar positions were measured via PSF fitting in the individual images and transformed into a common reference frame via suitable sets of reference stars. We measured the proper motions of more than 6000 stars within about 1pc projected distance of the supermassive black hole Sagittarius A*. The table contains for each measured star its projected distance from Sagittarius A*, its offsets in right ascension and declination from Sagittarius A* along with the corresponding uncertainties, its proper motion and the corresponding uncertainty in right ascension and declination, the Ks-band magnitude and the corresponding uncertainty, and its classification as early type in case such a classification exists.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91#tableb1</TD>
            <TD>2011-09-14T20:36:39Z</TD>
            <TD>#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/91</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/502/91&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/91</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/84/1305 [1]</TD>
            <TD>UBV photometry in NGC 6528 (van den Bergh+, 1979)</TD>
            <TD>On the basis of its color-magnitude diagram NGC 6528 is one of the two most metal-rich globular clusters that have so far been found in the Galaxy. Such a conclusion is consistent with Morgan's metallic line-strength classification of the integrated spectrum of this cluster. The reddening of NGC 6528 is estimated to be E(B-V)=0.52+/-0.07, from which R=6.1kpc and Z=-0.4kpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/84/1305#1</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/84/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/84/1305</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/84/1305</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/84/1305 [2]</TD>
            <TD>UBV photometry in NGC 6528 (van den Bergh+, 1979)</TD>
            <TD>On the basis of its color-magnitude diagram NGC 6528 is one of the two most metal-rich globular clusters that have so far been found in the Galaxy. Such a conclusion is consistent with Morgan's metallic line-strength classification of the integrated spectrum of this cluster. The reddening of NGC 6528 is estimated to be E(B-V)=0.52+/-0.07, from which R=6.1kpc and Z=-0.4kpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/84/1305#2</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/84/1305</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/84/1305&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/84/1305</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/381/420 [1]</TD>
            <TD>Group of Galaxies in the SSRS2 catalog (Adami+, 2002)</TD>
            <TD>We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog (Southern Sky Redshift Survey, Da Costa et al., Cat. J/AJ/116/1). The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420#1</TD>
            <TD>2011-09-14T19:15:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/381/420</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/381/420</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/381/420 [2]</TD>
            <TD>Group of Galaxies in the SSRS2 catalog (Adami+, 2002)</TD>
            <TD>We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog (Southern Sky Redshift Survey, Da Costa et al., Cat. J/AJ/116/1). The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420#2</TD>
            <TD>2011-09-14T19:15:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/381/420&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/381/420</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/381/420 [tables]</TD>
            <TD>Group of Galaxies in the SSRS2 catalog (Adami+, 2002)</TD>
            <TD>We present an automated method to detect populations of groups in galaxy redshift catalogs. This method uses both analysis of the redshift distribution along lines of sight in fixed cells to detect elementary structures and a friend-of-friend algorithm to merge these elementary structures into physical structures. We apply this method to the SSRS2 galaxy redshift catalog (Southern Sky Redshift Survey, Da Costa et al., Cat. J/AJ/116/1). The groups detected with our method are similar to group catalogs detected with pure friend-of-friend algorithms.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420#tables</TD>
            <TD>2011-09-14T19:15:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/381/420</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/381/420&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/381/420</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/2981 [1]</TD>
            <TD>Northern Optical Cluster Survey. III. (Gal+, 2009)</TD>
            <TD>We present the complete galaxy cluster catalog from the Northern Sky Optical Cluster Survey, a new, objectively defined catalog of candidate galaxy clusters at z&lt;~0.25 drawn from the Digitized Second Palomar Observatory Sky Survey (DPOSS). The data presented here cover the Southern Galactic Cap, as well as the less well-calibrated regions of the Northern Galactic Cap. In addition, due to improvements in our cluster finder and measurement methods, we provide an updated catalog for the well-calibrated Northern Galactic Cap region previously published in Paper II (Cat. J/AJ/125/2064). The complete survey covers 11411deg^2^, with over 15000 candidate clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981#1</TD>
            <TD>2011-09-14T20:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/2981</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/2981</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/2981 [2]</TD>
            <TD>Northern Optical Cluster Survey. III. (Gal+, 2009)</TD>
            <TD>We present the complete galaxy cluster catalog from the Northern Sky Optical Cluster Survey, a new, objectively defined catalog of candidate galaxy clusters at z&lt;~0.25 drawn from the Digitized Second Palomar Observatory Sky Survey (DPOSS). The data presented here cover the Southern Galactic Cap, as well as the less well-calibrated regions of the Northern Galactic Cap. In addition, due to improvements in our cluster finder and measurement methods, we provide an updated catalog for the well-calibrated Northern Galactic Cap region previously published in Paper II (Cat. J/AJ/125/2064). The complete survey covers 11411deg^2^, with over 15000 candidate clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981#2</TD>
            <TD>2011-09-14T20:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/2981&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/2981</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/2981 [table1]</TD>
            <TD>Northern Optical Cluster Survey. III. (Gal+, 2009)</TD>
            <TD>We present the complete galaxy cluster catalog from the Northern Sky Optical Cluster Survey, a new, objectively defined catalog of candidate galaxy clusters at z&lt;~0.25 drawn from the Digitized Second Palomar Observatory Sky Survey (DPOSS). The data presented here cover the Southern Galactic Cap, as well as the less well-calibrated regions of the Northern Galactic Cap. In addition, due to improvements in our cluster finder and measurement methods, we provide an updated catalog for the well-calibrated Northern Galactic Cap region previously published in Paper II (Cat. J/AJ/125/2064). The complete survey covers 11411deg^2^, with over 15000 candidate clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981#table1</TD>
            <TD>2011-09-14T20:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/2981&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/2981</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/314/493 [1]</TD>
            <TD>Boo Void survey (Kirshner+, 1987)</TD>
            <TD>In an earlier paper we inferred, from the distribution of galaxy redshifts in three small fields ~30{deg} apart, the existence of a 10^6^Mpc^3^ void in the distribution of galaxies in the constellation of Bootes. In this paper, we describe a redshift survey undertaken to test that hypothesis. Galaxies were selected by eye from 283 small fields distributed between the three original fields, and redshifts were measured for 239 of them. We confirm the existence of a large, roughly spherical void, of radius 62Mpc, centered at {alpha}=14h50, {delta}=+46{deg}, v=15500km/s. The low density of this region is of high statistical significance and does not appear easily reconcilable with any of the popular models for the growth of structure in the universe. This void does contain some unusual galaxies characterized by strong, high-excitation emission spectra, but not in sufficient numbers to compensate for the absence of more usual objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493#1</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/314/493</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/314/493</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/314/493 [2]</TD>
            <TD>Boo Void survey (Kirshner+, 1987)</TD>
            <TD>In an earlier paper we inferred, from the distribution of galaxy redshifts in three small fields ~30{deg} apart, the existence of a 10^6^Mpc^3^ void in the distribution of galaxies in the constellation of Bootes. In this paper, we describe a redshift survey undertaken to test that hypothesis. Galaxies were selected by eye from 283 small fields distributed between the three original fields, and redshifts were measured for 239 of them. We confirm the existence of a large, roughly spherical void, of radius 62Mpc, centered at {alpha}=14h50, {delta}=+46{deg}, v=15500km/s. The low density of this region is of high statistical significance and does not appear easily reconcilable with any of the popular models for the growth of structure in the universe. This void does contain some unusual galaxies characterized by strong, high-excitation emission spectra, but not in sufficient numbers to compensate for the absence of more usual objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493#2</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/314/493&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/314/493</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/390/511 [1]</TD>
            <TD>Millimetre observations of carbon stars. II. (Groenewegen+, 2002)</TD>
            <TD>Dust- and gas mass loss rates and distances are determined for a sample of about 330 infra-red carbon stars that probe a distance up to about 5.5kpc. The dependence of the dust- and gas mass loss rates, and the expansion velocity upon galactic longitude (l) are studied. It is found that the expansion velocity significantly depends on l, but that the absolute bolometric magnitude, the dust mass loss rate and the gas-to-dust ratio depend on l marginally, if at all, and the gas mass loss rate does not depend on l. Beyond the solar circle, the expansion velocity (as well as the luminosity, dust-to-gas ratio, dust mass loss rate) is lower than inside the solar circle, as expected from the overall gradient in metallicity content of the Galaxy. Combining the average expansion velocity inside and beyond the solar circle with the theoretically predicted relation between expansion velocity and gas-to-dust ratio, we find that the metallicity gradient in the solar neighbourhood is about -0.034dex/kpc, well within the quoted range of values in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511#1</TD>
            <TD>2011-09-14T19:16:21Z</TD>
            <TD>#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/390/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/390/511 [2]</TD>
            <TD>Millimetre observations of carbon stars. II. (Groenewegen+, 2002)</TD>
            <TD>Dust- and gas mass loss rates and distances are determined for a sample of about 330 infra-red carbon stars that probe a distance up to about 5.5kpc. The dependence of the dust- and gas mass loss rates, and the expansion velocity upon galactic longitude (l) are studied. It is found that the expansion velocity significantly depends on l, but that the absolute bolometric magnitude, the dust mass loss rate and the gas-to-dust ratio depend on l marginally, if at all, and the gas mass loss rate does not depend on l. Beyond the solar circle, the expansion velocity (as well as the luminosity, dust-to-gas ratio, dust mass loss rate) is lower than inside the solar circle, as expected from the overall gradient in metallicity content of the Galaxy. Combining the average expansion velocity inside and beyond the solar circle with the theoretically predicted relation between expansion velocity and gas-to-dust ratio, we find that the metallicity gradient in the solar neighbourhood is about -0.034dex/kpc, well within the quoted range of values in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511#2</TD>
            <TD>2011-09-14T19:16:21Z</TD>
            <TD>#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/390/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/390/511 [table1]</TD>
            <TD>Millimetre observations of carbon stars. II. (Groenewegen+, 2002)</TD>
            <TD>Dust- and gas mass loss rates and distances are determined for a sample of about 330 infra-red carbon stars that probe a distance up to about 5.5kpc. The dependence of the dust- and gas mass loss rates, and the expansion velocity upon galactic longitude (l) are studied. It is found that the expansion velocity significantly depends on l, but that the absolute bolometric magnitude, the dust mass loss rate and the gas-to-dust ratio depend on l marginally, if at all, and the gas mass loss rate does not depend on l. Beyond the solar circle, the expansion velocity (as well as the luminosity, dust-to-gas ratio, dust mass loss rate) is lower than inside the solar circle, as expected from the overall gradient in metallicity content of the Galaxy. Combining the average expansion velocity inside and beyond the solar circle with the theoretically predicted relation between expansion velocity and gas-to-dust ratio, we find that the metallicity gradient in the solar neighbourhood is about -0.034dex/kpc, well within the quoted range of values in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511#table1</TD>
            <TD>2011-09-14T19:16:21Z</TD>
            <TD>#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/390/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/2981 [1]</TD>
            <TD>Northern Optical Cluster Survey. III. (Gal+, 2009)</TD>
            <TD>We present the complete galaxy cluster catalog from the Northern Sky Optical Cluster Survey, a new, objectively defined catalog of candidate galaxy clusters at z&lt;~0.25 drawn from the Digitized Second Palomar Observatory Sky Survey (DPOSS). The data presented here cover the Southern Galactic Cap, as well as the less well-calibrated regions of the Northern Galactic Cap. In addition, due to improvements in our cluster finder and measurement methods, we provide an updated catalog for the well-calibrated Northern Galactic Cap region previously published in Paper II (Cat. J/AJ/125/2064). The complete survey covers 11411deg^2^, with over 15000 candidate clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981#1</TD>
            <TD>2011-09-14T20:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/2981</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/2981</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/2981 [2]</TD>
            <TD>Northern Optical Cluster Survey. III. (Gal+, 2009)</TD>
            <TD>We present the complete galaxy cluster catalog from the Northern Sky Optical Cluster Survey, a new, objectively defined catalog of candidate galaxy clusters at z&lt;~0.25 drawn from the Digitized Second Palomar Observatory Sky Survey (DPOSS). The data presented here cover the Southern Galactic Cap, as well as the less well-calibrated regions of the Northern Galactic Cap. In addition, due to improvements in our cluster finder and measurement methods, we provide an updated catalog for the well-calibrated Northern Galactic Cap region previously published in Paper II (Cat. J/AJ/125/2064). The complete survey covers 11411deg^2^, with over 15000 candidate clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981#2</TD>
            <TD>2011-09-14T20:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/2981&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/2981</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/2981 [table1]</TD>
            <TD>Northern Optical Cluster Survey. III. (Gal+, 2009)</TD>
            <TD>We present the complete galaxy cluster catalog from the Northern Sky Optical Cluster Survey, a new, objectively defined catalog of candidate galaxy clusters at z&lt;~0.25 drawn from the Digitized Second Palomar Observatory Sky Survey (DPOSS). The data presented here cover the Southern Galactic Cap, as well as the less well-calibrated regions of the Northern Galactic Cap. In addition, due to improvements in our cluster finder and measurement methods, we provide an updated catalog for the well-calibrated Northern Galactic Cap region previously published in Paper II (Cat. J/AJ/125/2064). The complete survey covers 11411deg^2^, with over 15000 candidate clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981#table1</TD>
            <TD>2011-09-14T20:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/2981&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/2981</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/314/493 [1]</TD>
            <TD>Boo Void survey (Kirshner+, 1987)</TD>
            <TD>In an earlier paper we inferred, from the distribution of galaxy redshifts in three small fields ~30{deg} apart, the existence of a 10^6^Mpc^3^ void in the distribution of galaxies in the constellation of Bootes. In this paper, we describe a redshift survey undertaken to test that hypothesis. Galaxies were selected by eye from 283 small fields distributed between the three original fields, and redshifts were measured for 239 of them. We confirm the existence of a large, roughly spherical void, of radius 62Mpc, centered at {alpha}=14h50, {delta}=+46{deg}, v=15500km/s. The low density of this region is of high statistical significance and does not appear easily reconcilable with any of the popular models for the growth of structure in the universe. This void does contain some unusual galaxies characterized by strong, high-excitation emission spectra, but not in sufficient numbers to compensate for the absence of more usual objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493#1</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/314/493</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/314/493</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/314/493 [2]</TD>
            <TD>Boo Void survey (Kirshner+, 1987)</TD>
            <TD>In an earlier paper we inferred, from the distribution of galaxy redshifts in three small fields ~30{deg} apart, the existence of a 10^6^Mpc^3^ void in the distribution of galaxies in the constellation of Bootes. In this paper, we describe a redshift survey undertaken to test that hypothesis. Galaxies were selected by eye from 283 small fields distributed between the three original fields, and redshifts were measured for 239 of them. We confirm the existence of a large, roughly spherical void, of radius 62Mpc, centered at {alpha}=14h50, {delta}=+46{deg}, v=15500km/s. The low density of this region is of high statistical significance and does not appear easily reconcilable with any of the popular models for the growth of structure in the universe. This void does contain some unusual galaxies characterized by strong, high-excitation emission spectra, but not in sufficient numbers to compensate for the absence of more usual objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493#2</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/314/493&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/314/493</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/137/2981 [1]</TD>
            <TD>Northern Optical Cluster Survey. III. (Gal+, 2009)</TD>
            <TD>We present the complete galaxy cluster catalog from the Northern Sky Optical Cluster Survey, a new, objectively defined catalog of candidate galaxy clusters at z&lt;~0.25 drawn from the Digitized Second Palomar Observatory Sky Survey (DPOSS). The data presented here cover the Southern Galactic Cap, as well as the less well-calibrated regions of the Northern Galactic Cap. In addition, due to improvements in our cluster finder and measurement methods, we provide an updated catalog for the well-calibrated Northern Galactic Cap region previously published in Paper II (Cat. J/AJ/125/2064). The complete survey covers 11411deg^2^, with over 15000 candidate clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981#1</TD>
            <TD>2011-09-14T20:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/137/2981</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/2981</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/137/2981 [2]</TD>
            <TD>Northern Optical Cluster Survey. III. (Gal+, 2009)</TD>
            <TD>We present the complete galaxy cluster catalog from the Northern Sky Optical Cluster Survey, a new, objectively defined catalog of candidate galaxy clusters at z&lt;~0.25 drawn from the Digitized Second Palomar Observatory Sky Survey (DPOSS). The data presented here cover the Southern Galactic Cap, as well as the less well-calibrated regions of the Northern Galactic Cap. In addition, due to improvements in our cluster finder and measurement methods, we provide an updated catalog for the well-calibrated Northern Galactic Cap region previously published in Paper II (Cat. J/AJ/125/2064). The complete survey covers 11411deg^2^, with over 15000 candidate clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981#2</TD>
            <TD>2011-09-14T20:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/137/2981&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/2981</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/137/2981 [table1]</TD>
            <TD>Northern Optical Cluster Survey. III. (Gal+, 2009)</TD>
            <TD>We present the complete galaxy cluster catalog from the Northern Sky Optical Cluster Survey, a new, objectively defined catalog of candidate galaxy clusters at z&lt;~0.25 drawn from the Digitized Second Palomar Observatory Sky Survey (DPOSS). The data presented here cover the Southern Galactic Cap, as well as the less well-calibrated regions of the Northern Galactic Cap. In addition, due to improvements in our cluster finder and measurement methods, we provide an updated catalog for the well-calibrated Northern Galactic Cap region previously published in Paper II (Cat. J/AJ/125/2064). The complete survey covers 11411deg^2^, with over 15000 candidate clusters.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981#table1</TD>
            <TD>2011-09-14T20:36:45Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/137/2981</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/137/2981&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/137/2981</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/390/511 [1]</TD>
            <TD>Millimetre observations of carbon stars. II. (Groenewegen+, 2002)</TD>
            <TD>Dust- and gas mass loss rates and distances are determined for a sample of about 330 infra-red carbon stars that probe a distance up to about 5.5kpc. The dependence of the dust- and gas mass loss rates, and the expansion velocity upon galactic longitude (l) are studied. It is found that the expansion velocity significantly depends on l, but that the absolute bolometric magnitude, the dust mass loss rate and the gas-to-dust ratio depend on l marginally, if at all, and the gas mass loss rate does not depend on l. Beyond the solar circle, the expansion velocity (as well as the luminosity, dust-to-gas ratio, dust mass loss rate) is lower than inside the solar circle, as expected from the overall gradient in metallicity content of the Galaxy. Combining the average expansion velocity inside and beyond the solar circle with the theoretically predicted relation between expansion velocity and gas-to-dust ratio, we find that the metallicity gradient in the solar neighbourhood is about -0.034dex/kpc, well within the quoted range of values in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511#1</TD>
            <TD>2011-09-14T19:16:21Z</TD>
            <TD>#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/390/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/390/511 [2]</TD>
            <TD>Millimetre observations of carbon stars. II. (Groenewegen+, 2002)</TD>
            <TD>Dust- and gas mass loss rates and distances are determined for a sample of about 330 infra-red carbon stars that probe a distance up to about 5.5kpc. The dependence of the dust- and gas mass loss rates, and the expansion velocity upon galactic longitude (l) are studied. It is found that the expansion velocity significantly depends on l, but that the absolute bolometric magnitude, the dust mass loss rate and the gas-to-dust ratio depend on l marginally, if at all, and the gas mass loss rate does not depend on l. Beyond the solar circle, the expansion velocity (as well as the luminosity, dust-to-gas ratio, dust mass loss rate) is lower than inside the solar circle, as expected from the overall gradient in metallicity content of the Galaxy. Combining the average expansion velocity inside and beyond the solar circle with the theoretically predicted relation between expansion velocity and gas-to-dust ratio, we find that the metallicity gradient in the solar neighbourhood is about -0.034dex/kpc, well within the quoted range of values in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511#2</TD>
            <TD>2011-09-14T19:16:21Z</TD>
            <TD>#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/390/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/390/511 [table1]</TD>
            <TD>Millimetre observations of carbon stars. II. (Groenewegen+, 2002)</TD>
            <TD>Dust- and gas mass loss rates and distances are determined for a sample of about 330 infra-red carbon stars that probe a distance up to about 5.5kpc. The dependence of the dust- and gas mass loss rates, and the expansion velocity upon galactic longitude (l) are studied. It is found that the expansion velocity significantly depends on l, but that the absolute bolometric magnitude, the dust mass loss rate and the gas-to-dust ratio depend on l marginally, if at all, and the gas mass loss rate does not depend on l. Beyond the solar circle, the expansion velocity (as well as the luminosity, dust-to-gas ratio, dust mass loss rate) is lower than inside the solar circle, as expected from the overall gradient in metallicity content of the Galaxy. Combining the average expansion velocity inside and beyond the solar circle with the theoretically predicted relation between expansion velocity and gas-to-dust ratio, we find that the metallicity gradient in the solar neighbourhood is about -0.034dex/kpc, well within the quoted range of values in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511#table1</TD>
            <TD>2011-09-14T19:16:21Z</TD>
            <TD>#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/390/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/314/493 [1]</TD>
            <TD>Boo Void survey (Kirshner+, 1987)</TD>
            <TD>In an earlier paper we inferred, from the distribution of galaxy redshifts in three small fields ~30{deg} apart, the existence of a 10^6^Mpc^3^ void in the distribution of galaxies in the constellation of Bootes. In this paper, we describe a redshift survey undertaken to test that hypothesis. Galaxies were selected by eye from 283 small fields distributed between the three original fields, and redshifts were measured for 239 of them. We confirm the existence of a large, roughly spherical void, of radius 62Mpc, centered at {alpha}=14h50, {delta}=+46{deg}, v=15500km/s. The low density of this region is of high statistical significance and does not appear easily reconcilable with any of the popular models for the growth of structure in the universe. This void does contain some unusual galaxies characterized by strong, high-excitation emission spectra, but not in sufficient numbers to compensate for the absence of more usual objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493#1</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/314/493</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/314/493</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/314/493 [2]</TD>
            <TD>Boo Void survey (Kirshner+, 1987)</TD>
            <TD>In an earlier paper we inferred, from the distribution of galaxy redshifts in three small fields ~30{deg} apart, the existence of a 10^6^Mpc^3^ void in the distribution of galaxies in the constellation of Bootes. In this paper, we describe a redshift survey undertaken to test that hypothesis. Galaxies were selected by eye from 283 small fields distributed between the three original fields, and redshifts were measured for 239 of them. We confirm the existence of a large, roughly spherical void, of radius 62Mpc, centered at {alpha}=14h50, {delta}=+46{deg}, v=15500km/s. The low density of this region is of high statistical significance and does not appear easily reconcilable with any of the popular models for the growth of structure in the universe. This void does contain some unusual galaxies characterized by strong, high-excitation emission spectra, but not in sufficient numbers to compensate for the absence of more usual objects.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493#2</TD>
            <TD>2011-09-14T18:59:16Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/314/493</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/314/493&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/314/493</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/168/19 [1]</TD>
            <TD>Chandra sources in 5 galaxy clusters (Martel+, 2007)</TD>
            <TD>All five clusters of the sample were observed as part of the ACS GTO programs 9290 and 9919 in Cycles 11 and 12. Chandra observations were made for RX J0152-1357 was observed on 2000 Sep 8, RX J0849+4452 on 2000 May 3-4, RDCS J0910+5422 on 2001 Apr 24 and 28, MS 1054-0321 on 2000 Apr 21, and RDCS J1252-2927 on 2003 Mar 18 and 20.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19#1</TD>
            <TD>2011-09-14T20:36:52Z</TD>
            <TD>#AGN#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/168/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/168/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/168/19 [2]</TD>
            <TD>Chandra sources in 5 galaxy clusters (Martel+, 2007)</TD>
            <TD>All five clusters of the sample were observed as part of the ACS GTO programs 9290 and 9919 in Cycles 11 and 12. Chandra observations were made for RX J0152-1357 was observed on 2000 Sep 8, RX J0849+4452 on 2000 May 3-4, RDCS J0910+5422 on 2001 Apr 24 and 28, MS 1054-0321 on 2000 Apr 21, and RDCS J1252-2927 on 2003 Mar 18 and 20.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19#2</TD>
            <TD>2011-09-14T20:36:52Z</TD>
            <TD>#AGN#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/168/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/168/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/168/19 [tables]</TD>
            <TD>Chandra sources in 5 galaxy clusters (Martel+, 2007)</TD>
            <TD>All five clusters of the sample were observed as part of the ACS GTO programs 9290 and 9919 in Cycles 11 and 12. Chandra observations were made for RX J0152-1357 was observed on 2000 Sep 8, RX J0849+4452 on 2000 May 3-4, RDCS J0910+5422 on 2001 Apr 24 and 28, MS 1054-0321 on 2000 Apr 21, and RDCS J1252-2927 on 2003 Mar 18 and 20.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19#tables</TD>
            <TD>2011-09-14T20:36:52Z</TD>
            <TD>#AGN#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/168/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/168/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/390/511 [1]</TD>
            <TD>Millimetre observations of carbon stars. II. (Groenewegen+, 2002)</TD>
            <TD>Dust- and gas mass loss rates and distances are determined for a sample of about 330 infra-red carbon stars that probe a distance up to about 5.5kpc. The dependence of the dust- and gas mass loss rates, and the expansion velocity upon galactic longitude (l) are studied. It is found that the expansion velocity significantly depends on l, but that the absolute bolometric magnitude, the dust mass loss rate and the gas-to-dust ratio depend on l marginally, if at all, and the gas mass loss rate does not depend on l. Beyond the solar circle, the expansion velocity (as well as the luminosity, dust-to-gas ratio, dust mass loss rate) is lower than inside the solar circle, as expected from the overall gradient in metallicity content of the Galaxy. Combining the average expansion velocity inside and beyond the solar circle with the theoretically predicted relation between expansion velocity and gas-to-dust ratio, we find that the metallicity gradient in the solar neighbourhood is about -0.034dex/kpc, well within the quoted range of values in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511#1</TD>
            <TD>2011-09-14T19:16:21Z</TD>
            <TD>#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/390/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/390/511 [2]</TD>
            <TD>Millimetre observations of carbon stars. II. (Groenewegen+, 2002)</TD>
            <TD>Dust- and gas mass loss rates and distances are determined for a sample of about 330 infra-red carbon stars that probe a distance up to about 5.5kpc. The dependence of the dust- and gas mass loss rates, and the expansion velocity upon galactic longitude (l) are studied. It is found that the expansion velocity significantly depends on l, but that the absolute bolometric magnitude, the dust mass loss rate and the gas-to-dust ratio depend on l marginally, if at all, and the gas mass loss rate does not depend on l. Beyond the solar circle, the expansion velocity (as well as the luminosity, dust-to-gas ratio, dust mass loss rate) is lower than inside the solar circle, as expected from the overall gradient in metallicity content of the Galaxy. Combining the average expansion velocity inside and beyond the solar circle with the theoretically predicted relation between expansion velocity and gas-to-dust ratio, we find that the metallicity gradient in the solar neighbourhood is about -0.034dex/kpc, well within the quoted range of values in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511#2</TD>
            <TD>2011-09-14T19:16:21Z</TD>
            <TD>#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/390/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/390/511 [table1]</TD>
            <TD>Millimetre observations of carbon stars. II. (Groenewegen+, 2002)</TD>
            <TD>Dust- and gas mass loss rates and distances are determined for a sample of about 330 infra-red carbon stars that probe a distance up to about 5.5kpc. The dependence of the dust- and gas mass loss rates, and the expansion velocity upon galactic longitude (l) are studied. It is found that the expansion velocity significantly depends on l, but that the absolute bolometric magnitude, the dust mass loss rate and the gas-to-dust ratio depend on l marginally, if at all, and the gas mass loss rate does not depend on l. Beyond the solar circle, the expansion velocity (as well as the luminosity, dust-to-gas ratio, dust mass loss rate) is lower than inside the solar circle, as expected from the overall gradient in metallicity content of the Galaxy. Combining the average expansion velocity inside and beyond the solar circle with the theoretically predicted relation between expansion velocity and gas-to-dust ratio, we find that the metallicity gradient in the solar neighbourhood is about -0.034dex/kpc, well within the quoted range of values in the literature.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511#table1</TD>
            <TD>2011-09-14T19:16:21Z</TD>
            <TD>#Velocities#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/390/511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/168/19 [1]</TD>
            <TD>Chandra sources in 5 galaxy clusters (Martel+, 2007)</TD>
            <TD>All five clusters of the sample were observed as part of the ACS GTO programs 9290 and 9919 in Cycles 11 and 12. Chandra observations were made for RX J0152-1357 was observed on 2000 Sep 8, RX J0849+4452 on 2000 May 3-4, RDCS J0910+5422 on 2001 Apr 24 and 28, MS 1054-0321 on 2000 Apr 21, and RDCS J1252-2927 on 2003 Mar 18 and 20.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19#1</TD>
            <TD>2011-09-14T20:36:52Z</TD>
            <TD>#AGN#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/168/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/168/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/168/19 [2]</TD>
            <TD>Chandra sources in 5 galaxy clusters (Martel+, 2007)</TD>
            <TD>All five clusters of the sample were observed as part of the ACS GTO programs 9290 and 9919 in Cycles 11 and 12. Chandra observations were made for RX J0152-1357 was observed on 2000 Sep 8, RX J0849+4452 on 2000 May 3-4, RDCS J0910+5422 on 2001 Apr 24 and 28, MS 1054-0321 on 2000 Apr 21, and RDCS J1252-2927 on 2003 Mar 18 and 20.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19#2</TD>
            <TD>2011-09-14T20:36:52Z</TD>
            <TD>#AGN#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/168/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/168/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/168/19 [tables]</TD>
            <TD>Chandra sources in 5 galaxy clusters (Martel+, 2007)</TD>
            <TD>All five clusters of the sample were observed as part of the ACS GTO programs 9290 and 9919 in Cycles 11 and 12. Chandra observations were made for RX J0152-1357 was observed on 2000 Sep 8, RX J0849+4452 on 2000 May 3-4, RDCS J0910+5422 on 2001 Apr 24 and 28, MS 1054-0321 on 2000 Apr 21, and RDCS J1252-2927 on 2003 Mar 18 and 20.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19#tables</TD>
            <TD>2011-09-14T20:36:52Z</TD>
            <TD>#AGN#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/168/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/168/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/65 [1]</TD>
            <TD>Galaxies morphology and IR photometry III. (Gavazzi+, 2000)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 558 galaxies in the Coma Supercluster and in the Virgo cluster. This data set, obtained with the Arcetri NICMOS3 camera ARNICA mounted on the Gornergrat Infrared Telescope, is aimed at complementing, with observations of mostly early-type objects, our NIR survey of spiral galaxies in these regions, presented in previous papers of this series. Magnitudes at the optical radius, total magnitudes, isophotal radii and light concentration indices are derived. We confirm the existence of a positive correlation between the near-infrared concentration index and the galaxy H-band luminosity</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65#1</TD>
            <TD>2011-09-14T18:59:45Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/65 [2]</TD>
            <TD>Galaxies morphology and IR photometry III. (Gavazzi+, 2000)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 558 galaxies in the Coma Supercluster and in the Virgo cluster. This data set, obtained with the Arcetri NICMOS3 camera ARNICA mounted on the Gornergrat Infrared Telescope, is aimed at complementing, with observations of mostly early-type objects, our NIR survey of spiral galaxies in these regions, presented in previous papers of this series. Magnitudes at the optical radius, total magnitudes, isophotal radii and light concentration indices are derived. We confirm the existence of a positive correlation between the near-infrared concentration index and the galaxy H-band luminosity</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65#2</TD>
            <TD>2011-09-14T18:59:45Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/168/19 [1]</TD>
            <TD>Chandra sources in 5 galaxy clusters (Martel+, 2007)</TD>
            <TD>All five clusters of the sample were observed as part of the ACS GTO programs 9290 and 9919 in Cycles 11 and 12. Chandra observations were made for RX J0152-1357 was observed on 2000 Sep 8, RX J0849+4452 on 2000 May 3-4, RDCS J0910+5422 on 2001 Apr 24 and 28, MS 1054-0321 on 2000 Apr 21, and RDCS J1252-2927 on 2003 Mar 18 and 20.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19#1</TD>
            <TD>2011-09-14T20:36:52Z</TD>
            <TD>#AGN#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/168/19</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/168/19</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/168/19 [2]</TD>
            <TD>Chandra sources in 5 galaxy clusters (Martel+, 2007)</TD>
            <TD>All five clusters of the sample were observed as part of the ACS GTO programs 9290 and 9919 in Cycles 11 and 12. Chandra observations were made for RX J0152-1357 was observed on 2000 Sep 8, RX J0849+4452 on 2000 May 3-4, RDCS J0910+5422 on 2001 Apr 24 and 28, MS 1054-0321 on 2000 Apr 21, and RDCS J1252-2927 on 2003 Mar 18 and 20.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19#2</TD>
            <TD>2011-09-14T20:36:52Z</TD>
            <TD>#AGN#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/168/19&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/168/19</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/168/19 [tables]</TD>
            <TD>Chandra sources in 5 galaxy clusters (Martel+, 2007)</TD>
            <TD>All five clusters of the sample were observed as part of the ACS GTO programs 9290 and 9919 in Cycles 11 and 12. Chandra observations were made for RX J0152-1357 was observed on 2000 Sep 8, RX J0849+4452 on 2000 May 3-4, RDCS J0910+5422 on 2001 Apr 24 and 28, MS 1054-0321 on 2000 Apr 21, and RDCS J1252-2927 on 2003 Mar 18 and 20.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19#tables</TD>
            <TD>2011-09-14T20:36:52Z</TD>
            <TD>#AGN#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/168/19</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/168/19&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/168/19</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/389/795 [1]</TD>
            <TD>Vertical structure of edge-on galaxies (Bizyaev+, 2002)</TD>
            <TD>To analyze the vertical structure of edge-on galaxies, we have used images of a large uniform sample of flat galaxies that have been taken during the 2MASS all-sky survey. The photometric parameters, such as the radial scale length, the vertical scale height, and the deprojected central surface brightness of galactic disks have been obtained. We find a strong correlation between the central surface brightness and the ratio of the vertical scale height to the vertical scale length: the thinner the galaxy, the lower the central surface brightness of its disk. The vertical scale height does not increase systematically with the distance from the galaxy center in the frames of this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795#1</TD>
            <TD>2011-09-14T19:16:51Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/389/795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/389/795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/389/795 [2]</TD>
            <TD>Vertical structure of edge-on galaxies (Bizyaev+, 2002)</TD>
            <TD>To analyze the vertical structure of edge-on galaxies, we have used images of a large uniform sample of flat galaxies that have been taken during the 2MASS all-sky survey. The photometric parameters, such as the radial scale length, the vertical scale height, and the deprojected central surface brightness of galactic disks have been obtained. We find a strong correlation between the central surface brightness and the ratio of the vertical scale height to the vertical scale length: the thinner the galaxy, the lower the central surface brightness of its disk. The vertical scale height does not increase systematically with the distance from the galaxy center in the frames of this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795#2</TD>
            <TD>2011-09-14T19:16:51Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/389/795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/389/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/389/795 [table1]</TD>
            <TD>Vertical structure of edge-on galaxies (Bizyaev+, 2002)</TD>
            <TD>To analyze the vertical structure of edge-on galaxies, we have used images of a large uniform sample of flat galaxies that have been taken during the 2MASS all-sky survey. The photometric parameters, such as the radial scale length, the vertical scale height, and the deprojected central surface brightness of galactic disks have been obtained. We find a strong correlation between the central surface brightness and the ratio of the vertical scale height to the vertical scale length: the thinner the galaxy, the lower the central surface brightness of its disk. The vertical scale height does not increase systematically with the distance from the galaxy center in the frames of this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795#table1</TD>
            <TD>2011-09-14T19:16:51Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/389/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/389/795</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/660/239 [1]</TD>
            <TD>MaxBCG catalog of 13823 galaxy clusters from SDSS (Koester+, 2007)</TD>
            <TD>Data for this study are drawn from the Sloan Digital Sky Survey a combined imaging and spectroscopic survey of 104deg^2^ in the north Galactic cap and a smaller region in the south. The imaging survey was carried out using a specially designed 2.5m telescope in drift-scan mode in five SDSS filters (u, g, r, i, and z) to a limiting magnitude of r&lt;22.5. The maxBCG galaxy cluster selection algorithm applied to the input galaxy catalog is described in more detail in a companion paper (Koester et al., 2007ApJ...660..221K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239#1</TD>
            <TD>2011-09-14T20:42:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/660/239</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/239</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/660/239 [2]</TD>
            <TD>MaxBCG catalog of 13823 galaxy clusters from SDSS (Koester+, 2007)</TD>
            <TD>Data for this study are drawn from the Sloan Digital Sky Survey a combined imaging and spectroscopic survey of 104deg^2^ in the north Galactic cap and a smaller region in the south. The imaging survey was carried out using a specially designed 2.5m telescope in drift-scan mode in five SDSS filters (u, g, r, i, and z) to a limiting magnitude of r&lt;22.5. The maxBCG galaxy cluster selection algorithm applied to the input galaxy catalog is described in more detail in a companion paper (Koester et al., 2007ApJ...660..221K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239#2</TD>
            <TD>2011-09-14T20:42:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/660/239&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/239</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/660/239 [table1]</TD>
            <TD>MaxBCG catalog of 13823 galaxy clusters from SDSS (Koester+, 2007)</TD>
            <TD>Data for this study are drawn from the Sloan Digital Sky Survey a combined imaging and spectroscopic survey of 104deg^2^ in the north Galactic cap and a smaller region in the south. The imaging survey was carried out using a specially designed 2.5m telescope in drift-scan mode in five SDSS filters (u, g, r, i, and z) to a limiting magnitude of r&lt;22.5. The maxBCG galaxy cluster selection algorithm applied to the input galaxy catalog is described in more detail in a companion paper (Koester et al., 2007ApJ...660..221K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239#table1</TD>
            <TD>2011-09-14T20:42:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/660/239&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/239</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/660/239 [1]</TD>
            <TD>MaxBCG catalog of 13823 galaxy clusters from SDSS (Koester+, 2007)</TD>
            <TD>Data for this study are drawn from the Sloan Digital Sky Survey a combined imaging and spectroscopic survey of 104deg^2^ in the north Galactic cap and a smaller region in the south. The imaging survey was carried out using a specially designed 2.5m telescope in drift-scan mode in five SDSS filters (u, g, r, i, and z) to a limiting magnitude of r&lt;22.5. The maxBCG galaxy cluster selection algorithm applied to the input galaxy catalog is described in more detail in a companion paper (Koester et al., 2007ApJ...660..221K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239#1</TD>
            <TD>2011-09-14T20:42:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/660/239</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/239</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/660/239 [2]</TD>
            <TD>MaxBCG catalog of 13823 galaxy clusters from SDSS (Koester+, 2007)</TD>
            <TD>Data for this study are drawn from the Sloan Digital Sky Survey a combined imaging and spectroscopic survey of 104deg^2^ in the north Galactic cap and a smaller region in the south. The imaging survey was carried out using a specially designed 2.5m telescope in drift-scan mode in five SDSS filters (u, g, r, i, and z) to a limiting magnitude of r&lt;22.5. The maxBCG galaxy cluster selection algorithm applied to the input galaxy catalog is described in more detail in a companion paper (Koester et al., 2007ApJ...660..221K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239#2</TD>
            <TD>2011-09-14T20:42:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/660/239&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/239</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/660/239 [table1]</TD>
            <TD>MaxBCG catalog of 13823 galaxy clusters from SDSS (Koester+, 2007)</TD>
            <TD>Data for this study are drawn from the Sloan Digital Sky Survey a combined imaging and spectroscopic survey of 104deg^2^ in the north Galactic cap and a smaller region in the south. The imaging survey was carried out using a specially designed 2.5m telescope in drift-scan mode in five SDSS filters (u, g, r, i, and z) to a limiting magnitude of r&lt;22.5. The maxBCG galaxy cluster selection algorithm applied to the input galaxy catalog is described in more detail in a companion paper (Koester et al., 2007ApJ...660..221K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239#table1</TD>
            <TD>2011-09-14T20:42:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/660/239&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/239</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/65 [1]</TD>
            <TD>Galaxies morphology and IR photometry III. (Gavazzi+, 2000)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 558 galaxies in the Coma Supercluster and in the Virgo cluster. This data set, obtained with the Arcetri NICMOS3 camera ARNICA mounted on the Gornergrat Infrared Telescope, is aimed at complementing, with observations of mostly early-type objects, our NIR survey of spiral galaxies in these regions, presented in previous papers of this series. Magnitudes at the optical radius, total magnitudes, isophotal radii and light concentration indices are derived. We confirm the existence of a positive correlation between the near-infrared concentration index and the galaxy H-band luminosity</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65#1</TD>
            <TD>2011-09-14T18:59:45Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/65 [2]</TD>
            <TD>Galaxies morphology and IR photometry III. (Gavazzi+, 2000)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 558 galaxies in the Coma Supercluster and in the Virgo cluster. This data set, obtained with the Arcetri NICMOS3 camera ARNICA mounted on the Gornergrat Infrared Telescope, is aimed at complementing, with observations of mostly early-type objects, our NIR survey of spiral galaxies in these regions, presented in previous papers of this series. Magnitudes at the optical radius, total magnitudes, isophotal radii and light concentration indices are derived. We confirm the existence of a positive correlation between the near-infrared concentration index and the galaxy H-band luminosity</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65#2</TD>
            <TD>2011-09-14T18:59:45Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/660/239 [1]</TD>
            <TD>MaxBCG catalog of 13823 galaxy clusters from SDSS (Koester+, 2007)</TD>
            <TD>Data for this study are drawn from the Sloan Digital Sky Survey a combined imaging and spectroscopic survey of 104deg^2^ in the north Galactic cap and a smaller region in the south. The imaging survey was carried out using a specially designed 2.5m telescope in drift-scan mode in five SDSS filters (u, g, r, i, and z) to a limiting magnitude of r&lt;22.5. The maxBCG galaxy cluster selection algorithm applied to the input galaxy catalog is described in more detail in a companion paper (Koester et al., 2007ApJ...660..221K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239#1</TD>
            <TD>2011-09-14T20:42:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/660/239</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/239</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/660/239 [2]</TD>
            <TD>MaxBCG catalog of 13823 galaxy clusters from SDSS (Koester+, 2007)</TD>
            <TD>Data for this study are drawn from the Sloan Digital Sky Survey a combined imaging and spectroscopic survey of 104deg^2^ in the north Galactic cap and a smaller region in the south. The imaging survey was carried out using a specially designed 2.5m telescope in drift-scan mode in five SDSS filters (u, g, r, i, and z) to a limiting magnitude of r&lt;22.5. The maxBCG galaxy cluster selection algorithm applied to the input galaxy catalog is described in more detail in a companion paper (Koester et al., 2007ApJ...660..221K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239#2</TD>
            <TD>2011-09-14T20:42:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/660/239&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/239</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/660/239 [table1]</TD>
            <TD>MaxBCG catalog of 13823 galaxy clusters from SDSS (Koester+, 2007)</TD>
            <TD>Data for this study are drawn from the Sloan Digital Sky Survey a combined imaging and spectroscopic survey of 104deg^2^ in the north Galactic cap and a smaller region in the south. The imaging survey was carried out using a specially designed 2.5m telescope in drift-scan mode in five SDSS filters (u, g, r, i, and z) to a limiting magnitude of r&lt;22.5. The maxBCG galaxy cluster selection algorithm applied to the input galaxy catalog is described in more detail in a companion paper (Koester et al., 2007ApJ...660..221K).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239#table1</TD>
            <TD>2011-09-14T20:42:41Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/239</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/660/239&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/239</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/389/795 [1]</TD>
            <TD>Vertical structure of edge-on galaxies (Bizyaev+, 2002)</TD>
            <TD>To analyze the vertical structure of edge-on galaxies, we have used images of a large uniform sample of flat galaxies that have been taken during the 2MASS all-sky survey. The photometric parameters, such as the radial scale length, the vertical scale height, and the deprojected central surface brightness of galactic disks have been obtained. We find a strong correlation between the central surface brightness and the ratio of the vertical scale height to the vertical scale length: the thinner the galaxy, the lower the central surface brightness of its disk. The vertical scale height does not increase systematically with the distance from the galaxy center in the frames of this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795#1</TD>
            <TD>2011-09-14T19:16:51Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/389/795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/389/795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/389/795 [2]</TD>
            <TD>Vertical structure of edge-on galaxies (Bizyaev+, 2002)</TD>
            <TD>To analyze the vertical structure of edge-on galaxies, we have used images of a large uniform sample of flat galaxies that have been taken during the 2MASS all-sky survey. The photometric parameters, such as the radial scale length, the vertical scale height, and the deprojected central surface brightness of galactic disks have been obtained. We find a strong correlation between the central surface brightness and the ratio of the vertical scale height to the vertical scale length: the thinner the galaxy, the lower the central surface brightness of its disk. The vertical scale height does not increase systematically with the distance from the galaxy center in the frames of this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795#2</TD>
            <TD>2011-09-14T19:16:51Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/389/795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/389/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/389/795 [table1]</TD>
            <TD>Vertical structure of edge-on galaxies (Bizyaev+, 2002)</TD>
            <TD>To analyze the vertical structure of edge-on galaxies, we have used images of a large uniform sample of flat galaxies that have been taken during the 2MASS all-sky survey. The photometric parameters, such as the radial scale length, the vertical scale height, and the deprojected central surface brightness of galactic disks have been obtained. We find a strong correlation between the central surface brightness and the ratio of the vertical scale height to the vertical scale length: the thinner the galaxy, the lower the central surface brightness of its disk. The vertical scale height does not increase systematically with the distance from the galaxy center in the frames of this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795#table1</TD>
            <TD>2011-09-14T19:16:51Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/389/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/389/795</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/65 [1]</TD>
            <TD>Galaxies morphology and IR photometry III. (Gavazzi+, 2000)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 558 galaxies in the Coma Supercluster and in the Virgo cluster. This data set, obtained with the Arcetri NICMOS3 camera ARNICA mounted on the Gornergrat Infrared Telescope, is aimed at complementing, with observations of mostly early-type objects, our NIR survey of spiral galaxies in these regions, presented in previous papers of this series. Magnitudes at the optical radius, total magnitudes, isophotal radii and light concentration indices are derived. We confirm the existence of a positive correlation between the near-infrared concentration index and the galaxy H-band luminosity</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65#1</TD>
            <TD>2011-09-14T18:59:45Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/65 [2]</TD>
            <TD>Galaxies morphology and IR photometry III. (Gavazzi+, 2000)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 558 galaxies in the Coma Supercluster and in the Virgo cluster. This data set, obtained with the Arcetri NICMOS3 camera ARNICA mounted on the Gornergrat Infrared Telescope, is aimed at complementing, with observations of mostly early-type objects, our NIR survey of spiral galaxies in these regions, presented in previous papers of this series. Magnitudes at the optical radius, total magnitudes, isophotal radii and light concentration indices are derived. We confirm the existence of a positive correlation between the near-infrared concentration index and the galaxy H-band luminosity</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65#2</TD>
            <TD>2011-09-14T18:59:45Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/538 [1]</TD>
            <TD>XUV-Disk galaxies in the Local Universe (Thilker+, 2007)</TD>
            <TD>GALEX obtained FUV and NUV direct imaging observations of our sample targets during primary mission surveys, principally the Nearby Galaxy Survey (NGS; Bianchi et al. 2003, in The Local Group as an Astrophysical Laboratory, ed. M. Livio &amp; T. Brown (Baltimore: STScI), 10) and Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). Second-generation Digitial Sky Survey (DSS-II) imaging data were used for compared GALEX imagery to the visible morphology of targets. We obtained Sloan Digital Sky Survey (SDSS) DR5 ugriz imagery of confirmed XUV-disk objects whenever possible. 2MASS Large Galaxy Atlas (LGA; Jarrett et al., 2003AJ....125..525J) was our preferred source for K_s_ data.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538#1</TD>
            <TD>2011-09-14T20:45:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/538</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/538</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/538 [2]</TD>
            <TD>XUV-Disk galaxies in the Local Universe (Thilker+, 2007)</TD>
            <TD>GALEX obtained FUV and NUV direct imaging observations of our sample targets during primary mission surveys, principally the Nearby Galaxy Survey (NGS; Bianchi et al. 2003, in The Local Group as an Astrophysical Laboratory, ed. M. Livio &amp; T. Brown (Baltimore: STScI), 10) and Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). Second-generation Digitial Sky Survey (DSS-II) imaging data were used for compared GALEX imagery to the visible morphology of targets. We obtained Sloan Digital Sky Survey (SDSS) DR5 ugriz imagery of confirmed XUV-disk objects whenever possible. 2MASS Large Galaxy Atlas (LGA; Jarrett et al., 2003AJ....125..525J) was our preferred source for K_s_ data.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538#2</TD>
            <TD>2011-09-14T20:45:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/538&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/538</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/173/538 [table1]</TD>
            <TD>XUV-Disk galaxies in the Local Universe (Thilker+, 2007)</TD>
            <TD>GALEX obtained FUV and NUV direct imaging observations of our sample targets during primary mission surveys, principally the Nearby Galaxy Survey (NGS; Bianchi et al. 2003, in The Local Group as an Astrophysical Laboratory, ed. M. Livio &amp; T. Brown (Baltimore: STScI), 10) and Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). Second-generation Digitial Sky Survey (DSS-II) imaging data were used for compared GALEX imagery to the visible morphology of targets. We obtained Sloan Digital Sky Survey (SDSS) DR5 ugriz imagery of confirmed XUV-disk objects whenever possible. 2MASS Large Galaxy Atlas (LGA; Jarrett et al., 2003AJ....125..525J) was our preferred source for K_s_ data.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538#table1</TD>
            <TD>2011-09-14T20:45:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/173/538&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/538</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/389/795 [1]</TD>
            <TD>Vertical structure of edge-on galaxies (Bizyaev+, 2002)</TD>
            <TD>To analyze the vertical structure of edge-on galaxies, we have used images of a large uniform sample of flat galaxies that have been taken during the 2MASS all-sky survey. The photometric parameters, such as the radial scale length, the vertical scale height, and the deprojected central surface brightness of galactic disks have been obtained. We find a strong correlation between the central surface brightness and the ratio of the vertical scale height to the vertical scale length: the thinner the galaxy, the lower the central surface brightness of its disk. The vertical scale height does not increase systematically with the distance from the galaxy center in the frames of this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795#1</TD>
            <TD>2011-09-14T19:16:51Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/389/795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/389/795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/389/795 [2]</TD>
            <TD>Vertical structure of edge-on galaxies (Bizyaev+, 2002)</TD>
            <TD>To analyze the vertical structure of edge-on galaxies, we have used images of a large uniform sample of flat galaxies that have been taken during the 2MASS all-sky survey. The photometric parameters, such as the radial scale length, the vertical scale height, and the deprojected central surface brightness of galactic disks have been obtained. We find a strong correlation between the central surface brightness and the ratio of the vertical scale height to the vertical scale length: the thinner the galaxy, the lower the central surface brightness of its disk. The vertical scale height does not increase systematically with the distance from the galaxy center in the frames of this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795#2</TD>
            <TD>2011-09-14T19:16:51Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/389/795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/389/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/389/795 [table1]</TD>
            <TD>Vertical structure of edge-on galaxies (Bizyaev+, 2002)</TD>
            <TD>To analyze the vertical structure of edge-on galaxies, we have used images of a large uniform sample of flat galaxies that have been taken during the 2MASS all-sky survey. The photometric parameters, such as the radial scale length, the vertical scale height, and the deprojected central surface brightness of galactic disks have been obtained. We find a strong correlation between the central surface brightness and the ratio of the vertical scale height to the vertical scale length: the thinner the galaxy, the lower the central surface brightness of its disk. The vertical scale height does not increase systematically with the distance from the galaxy center in the frames of this sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795#table1</TD>
            <TD>2011-09-14T19:16:51Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/389/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/389/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/389/795</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/116/203 [1]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#1</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/116/203</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/116/203 [2]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#2</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/116/203&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/116/203 [table1]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#table1</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/116/203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/116/203 [table2]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#table2</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/116/203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/538 [1]</TD>
            <TD>XUV-Disk galaxies in the Local Universe (Thilker+, 2007)</TD>
            <TD>GALEX obtained FUV and NUV direct imaging observations of our sample targets during primary mission surveys, principally the Nearby Galaxy Survey (NGS; Bianchi et al. 2003, in The Local Group as an Astrophysical Laboratory, ed. M. Livio &amp; T. Brown (Baltimore: STScI), 10) and Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). Second-generation Digitial Sky Survey (DSS-II) imaging data were used for compared GALEX imagery to the visible morphology of targets. We obtained Sloan Digital Sky Survey (SDSS) DR5 ugriz imagery of confirmed XUV-disk objects whenever possible. 2MASS Large Galaxy Atlas (LGA; Jarrett et al., 2003AJ....125..525J) was our preferred source for K_s_ data.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538#1</TD>
            <TD>2011-09-14T20:45:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/538</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/538</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/538 [2]</TD>
            <TD>XUV-Disk galaxies in the Local Universe (Thilker+, 2007)</TD>
            <TD>GALEX obtained FUV and NUV direct imaging observations of our sample targets during primary mission surveys, principally the Nearby Galaxy Survey (NGS; Bianchi et al. 2003, in The Local Group as an Astrophysical Laboratory, ed. M. Livio &amp; T. Brown (Baltimore: STScI), 10) and Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). Second-generation Digitial Sky Survey (DSS-II) imaging data were used for compared GALEX imagery to the visible morphology of targets. We obtained Sloan Digital Sky Survey (SDSS) DR5 ugriz imagery of confirmed XUV-disk objects whenever possible. 2MASS Large Galaxy Atlas (LGA; Jarrett et al., 2003AJ....125..525J) was our preferred source for K_s_ data.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538#2</TD>
            <TD>2011-09-14T20:45:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/538&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/538</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/173/538 [table1]</TD>
            <TD>XUV-Disk galaxies in the Local Universe (Thilker+, 2007)</TD>
            <TD>GALEX obtained FUV and NUV direct imaging observations of our sample targets during primary mission surveys, principally the Nearby Galaxy Survey (NGS; Bianchi et al. 2003, in The Local Group as an Astrophysical Laboratory, ed. M. Livio &amp; T. Brown (Baltimore: STScI), 10) and Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). Second-generation Digitial Sky Survey (DSS-II) imaging data were used for compared GALEX imagery to the visible morphology of targets. We obtained Sloan Digital Sky Survey (SDSS) DR5 ugriz imagery of confirmed XUV-disk objects whenever possible. 2MASS Large Galaxy Atlas (LGA; Jarrett et al., 2003AJ....125..525J) was our preferred source for K_s_ data.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538#table1</TD>
            <TD>2011-09-14T20:45:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/173/538&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/538</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/392/741 [1]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#1</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/392/741</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/392/741 [2]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#2</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/392/741&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table8]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table8</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table5]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table5</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table4]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table4</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table6]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table6</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table3]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table3</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table7]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table7</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/116/203 [1]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#1</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/116/203</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/116/203 [2]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#2</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/116/203&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/116/203 [table1]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#table1</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/116/203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/116/203 [table2]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#table2</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/116/203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/538 [1]</TD>
            <TD>XUV-Disk galaxies in the Local Universe (Thilker+, 2007)</TD>
            <TD>GALEX obtained FUV and NUV direct imaging observations of our sample targets during primary mission surveys, principally the Nearby Galaxy Survey (NGS; Bianchi et al. 2003, in The Local Group as an Astrophysical Laboratory, ed. M. Livio &amp; T. Brown (Baltimore: STScI), 10) and Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). Second-generation Digitial Sky Survey (DSS-II) imaging data were used for compared GALEX imagery to the visible morphology of targets. We obtained Sloan Digital Sky Survey (SDSS) DR5 ugriz imagery of confirmed XUV-disk objects whenever possible. 2MASS Large Galaxy Atlas (LGA; Jarrett et al., 2003AJ....125..525J) was our preferred source for K_s_ data.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538#1</TD>
            <TD>2011-09-14T20:45:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/538</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/538</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/538 [2]</TD>
            <TD>XUV-Disk galaxies in the Local Universe (Thilker+, 2007)</TD>
            <TD>GALEX obtained FUV and NUV direct imaging observations of our sample targets during primary mission surveys, principally the Nearby Galaxy Survey (NGS; Bianchi et al. 2003, in The Local Group as an Astrophysical Laboratory, ed. M. Livio &amp; T. Brown (Baltimore: STScI), 10) and Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). Second-generation Digitial Sky Survey (DSS-II) imaging data were used for compared GALEX imagery to the visible morphology of targets. We obtained Sloan Digital Sky Survey (SDSS) DR5 ugriz imagery of confirmed XUV-disk objects whenever possible. 2MASS Large Galaxy Atlas (LGA; Jarrett et al., 2003AJ....125..525J) was our preferred source for K_s_ data.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538#2</TD>
            <TD>2011-09-14T20:45:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/538&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/538</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/173/538 [table1]</TD>
            <TD>XUV-Disk galaxies in the Local Universe (Thilker+, 2007)</TD>
            <TD>GALEX obtained FUV and NUV direct imaging observations of our sample targets during primary mission surveys, principally the Nearby Galaxy Survey (NGS; Bianchi et al. 2003, in The Local Group as an Astrophysical Laboratory, ed. M. Livio &amp; T. Brown (Baltimore: STScI), 10) and Medium Imaging Survey (MIS; Martin et al., 2005ApJ...619L...1M). Second-generation Digitial Sky Survey (DSS-II) imaging data were used for compared GALEX imagery to the visible morphology of targets. We obtained Sloan Digital Sky Survey (SDSS) DR5 ugriz imagery of confirmed XUV-disk objects whenever possible. 2MASS Large Galaxy Atlas (LGA; Jarrett et al., 2003AJ....125..525J) was our preferred source for K_s_ data.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538#table1</TD>
            <TD>2011-09-14T20:45:56Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/538</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/173/538&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/538</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/392/741 [1]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#1</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/392/741</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/392/741 [2]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#2</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/392/741&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table8]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table8</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table5]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table5</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table4]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table4</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table6]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table6</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table3]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table3</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table7]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table7</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/116/203 [1]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#1</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/116/203</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/116/203 [2]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#2</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/116/203&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/116/203 [table1]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#table1</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/116/203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/116/203 [table2]</TD>
            <TD>The redshift catalogue for galaxy clusters (Stein+, 1996)</TD>
            <TD>An extensive redshift survey has been conducted on a sample of 15 nearby (0.01&lt;~z&lt;~0.05) clusters of galaxies. A total number of 860 redshifts were determined by fitting of emission-lines and/or cross-correlation techniques. Of this sample, 735 galaxies are within 0.2-0.8Mpc (H_0_=50km/s/Mpc) of the center of clusters. Approximate morphological types are available for most of the galaxies. A comparison of the present redshifts with published data allows an extensive error analysis. The agreement is excellent with the most modern data, showing a zero point error of 5km/s and an overall consistency of the measurements and their uncertainties. We estimate our redshifts to have mean random errors around 30km/s. A population analysis of the clusters will be given in a forthcoming paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203#table2</TD>
            <TD>2011-09-14T19:00:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/203</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/116/203&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/203</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/178/280 [1]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#1</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/178/280</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/178/280 [2]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#2</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/178/280&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/280 [table1]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#table1</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/280&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/280 [table4]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#table4</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
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            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/280&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/392/741 [1]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#1</TD>
            <TD>2011-09-14T19:16:53Z</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/392/741</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/392/741 [2]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#2</TD>
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            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/392/741&amp;</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table8]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table8</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table5]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table5</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table4]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table4</TD>
            <TD>2011-09-14T19:16:53Z</TD>
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            <TD>#Catalog#</TD>
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            <TD>10-Jun-2002</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table6]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table6</TD>
            <TD>2011-09-14T19:16:53Z</TD>
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            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table3]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table3</TD>
            <TD>2011-09-14T19:16:53Z</TD>
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            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/741 [table7]</TD>
            <TD>Stellar Catalogue in the Chandra DFS (Groenewegen+ 2002)</TD>
            <TD>Five and seven passband colour catalogues in the direction of the Chandra Deep Field South are constructed, from previously published single passband catalogues. A method to perform Star-Galaxy separation is presented. Additionally, methods are presented to pick-up QSO and compact galaxies, which are also point sources. The tables present the final 5 and 7 passband catalogues for the objects considered as stars (tables 3 and 4), QSOs (tables 5 and 6) and compact galaxies (tables 7 and 8). All tables contain: the name of the object, Right Ascension and Declination, magnitudes and error for, respectively, 5 or 7 passbands. The last column(s) lists the assigned spectral type for the stellar catalogues, photometric redshift for the QSO catalogues, and galaxy type and photometric redshift for the compact galaxies catalogues.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741#table7</TD>
            <TD>2011-09-14T19:16:53Z</TD>
            <TD>#Galaxies#Photometry:wide-band#QSOs#Stars:white_dwarf#</TD>
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            <TD />
            <TD>10-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/741</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/741&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/741</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/120/521 [1]</TD>
            <TD>Galaxies morphology and IR photometry II. (Gavazzi+ 1996)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, &lt;J/A+AS/120/489&gt;) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. &lt;GCPD/59&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521#1</TD>
            <TD>2011-09-14T19:00:33Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>31-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/120/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/120/521 [2]</TD>
            <TD>Galaxies morphology and IR photometry II. (Gavazzi+ 1996)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, &lt;J/A+AS/120/489&gt;) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. &lt;GCPD/59&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521#2</TD>
            <TD>2011-09-14T19:00:33Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/120/521&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/521</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/120/521 [table1]</TD>
            <TD>Galaxies morphology and IR photometry II. (Gavazzi+ 1996)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, &lt;J/A+AS/120/489&gt;) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. &lt;GCPD/59&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521#table1</TD>
            <TD>2011-09-14T19:00:33Z</TD>
            <TD>#Photometry:surface#</TD>
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            <TD>31-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/120/521&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/178/280 [1]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#1</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/178/280</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/178/280 [2]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#2</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/178/280&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/280 [table1]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#table1</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
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            <TD>#Research#</TD>
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            <TD>20-Jul-2009</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/280&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/280 [table4]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#table4</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/280&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/234 [1]</TD>
            <TD>M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002)</TD>
            <TD>We present first results from a spectroscopic survey designed to examine the metallicity and kinematics of individual red giant branch stars in the outer halo of the Andromeda spiral galaxy (M31). This study is based on multislit spectroscopy with the Keck II 10m telescope and Low Resolution Imaging Spectrograph of the Ca II near-infrared triplet in 99 M31 halo candidates in a field at R=19kpc on the southeast minor axis with brightnesses from 20&lt;I&lt;22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234#1</TD>
            <TD>2011-09-14T19:17:16Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/234</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/234</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/234 [2]</TD>
            <TD>M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002)</TD>
            <TD>We present first results from a spectroscopic survey designed to examine the metallicity and kinematics of individual red giant branch stars in the outer halo of the Andromeda spiral galaxy (M31). This study is based on multislit spectroscopy with the Keck II 10m telescope and Low Resolution Imaging Spectrograph of the Ca II near-infrared triplet in 99 M31 halo candidates in a field at R=19kpc on the southeast minor axis with brightnesses from 20&lt;I&lt;22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234#2</TD>
            <TD>2011-09-14T19:17:16Z</TD>
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            <TD>09-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/234&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/234</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/234 [table1]</TD>
            <TD>M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002)</TD>
            <TD>We present first results from a spectroscopic survey designed to examine the metallicity and kinematics of individual red giant branch stars in the outer halo of the Andromeda spiral galaxy (M31). This study is based on multislit spectroscopy with the Keck II 10m telescope and Low Resolution Imaging Spectrograph of the Ca II near-infrared triplet in 99 M31 halo candidates in a field at R=19kpc on the southeast minor axis with brightnesses from 20&lt;I&lt;22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234#table1</TD>
            <TD>2011-09-14T19:17:16Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Photometry:wide-band#</TD>
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            <TD>#Research#</TD>
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            <TD>09-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/234&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/234</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/178/280 [1]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#1</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/178/280</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/178/280 [2]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#2</TD>
            <TD>2011-09-14T20:46:22Z</TD>
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            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/178/280&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/280 [table1]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#table1</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
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            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/280&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/178/280 [table4]</TD>
            <TD>Compendium of ISO far-IR extragalactic data (Brauher+, 2008)</TD>
            <TD>Far-infrared line and continuum fluxes are presented for a sample of 227 galaxies observed with the Long Wavelength Spectrometer on the Infrared Space Observatory (ISO, Kessler et al., 1996A&amp;A...315L..27K). The galaxy sample includes normal star-forming systems, starbursts, and active galactic nuclei covering a wide range of colors and morphologies. The data set spans some 1300 line fluxes, 600 line upper limits, and 800 continuum fluxes. Several fine-structure emission lines are detected that arise in either photodissociation or HII regions: [OIII] 52um, [NIII] 57um, [OI] 63um, [OIII] 88um, [NII] 122um, [OI] 145um, and [CII] 158um. Molecular lines such as OH at 53, 79, 84, 119, and 163um, and H_2_O at 58, 66, 75, 101, and 108um are also detected in some galaxies. In addition to those lines emitted by the target galaxies, serendipitous detections of Milky Way [CII] 158um and an unidentified line near 74um in NGC 1068 are also reported. Finally, continuum fluxes at 52, 57, 63, 88, 122, 145, 158, and 170um are derived for a subset of galaxies in which the far-infrared emission is contained within the ~75" ISO LWS beam. The statistics of this large database of continuum and line fluxes, including trends in line ratios with the far-infrared color and infrared-to-optical ratio, are explored.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280#table4</TD>
            <TD>2011-09-14T20:46:22Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/178/280</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/178/280&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/178/280</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/120/521 [1]</TD>
            <TD>Galaxies morphology and IR photometry II. (Gavazzi+ 1996)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, &lt;J/A+AS/120/489&gt;) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. &lt;GCPD/59&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521#1</TD>
            <TD>2011-09-14T19:00:33Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/120/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/120/521 [2]</TD>
            <TD>Galaxies morphology and IR photometry II. (Gavazzi+ 1996)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, &lt;J/A+AS/120/489&gt;) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. &lt;GCPD/59&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521#2</TD>
            <TD>2011-09-14T19:00:33Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/120/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/521</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/120/521 [table1]</TD>
            <TD>Galaxies morphology and IR photometry II. (Gavazzi+ 1996)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, &lt;J/A+AS/120/489&gt;) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. &lt;GCPD/59&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521#table1</TD>
            <TD>2011-09-14T19:00:33Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/120/521&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/234 [1]</TD>
            <TD>M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002)</TD>
            <TD>We present first results from a spectroscopic survey designed to examine the metallicity and kinematics of individual red giant branch stars in the outer halo of the Andromeda spiral galaxy (M31). This study is based on multislit spectroscopy with the Keck II 10m telescope and Low Resolution Imaging Spectrograph of the Ca II near-infrared triplet in 99 M31 halo candidates in a field at R=19kpc on the southeast minor axis with brightnesses from 20&lt;I&lt;22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234#1</TD>
            <TD>2011-09-14T19:17:16Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/234</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/234</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/234 [2]</TD>
            <TD>M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002)</TD>
            <TD>We present first results from a spectroscopic survey designed to examine the metallicity and kinematics of individual red giant branch stars in the outer halo of the Andromeda spiral galaxy (M31). This study is based on multislit spectroscopy with the Keck II 10m telescope and Low Resolution Imaging Spectrograph of the Ca II near-infrared triplet in 99 M31 halo candidates in a field at R=19kpc on the southeast minor axis with brightnesses from 20&lt;I&lt;22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234#2</TD>
            <TD>2011-09-14T19:17:16Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/234&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/234</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/234 [table1]</TD>
            <TD>M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002)</TD>
            <TD>We present first results from a spectroscopic survey designed to examine the metallicity and kinematics of individual red giant branch stars in the outer halo of the Andromeda spiral galaxy (M31). This study is based on multislit spectroscopy with the Keck II 10m telescope and Low Resolution Imaging Spectrograph of the Ca II near-infrared triplet in 99 M31 halo candidates in a field at R=19kpc on the southeast minor axis with brightnesses from 20&lt;I&lt;22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234#table1</TD>
            <TD>2011-09-14T19:17:16Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/234&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/234</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/120/521 [1]</TD>
            <TD>Galaxies morphology and IR photometry II. (Gavazzi+ 1996)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, &lt;J/A+AS/120/489&gt;) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. &lt;GCPD/59&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521#1</TD>
            <TD>2011-09-14T19:00:33Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/120/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/120/521 [2]</TD>
            <TD>Galaxies morphology and IR photometry II. (Gavazzi+ 1996)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, &lt;J/A+AS/120/489&gt;) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. &lt;GCPD/59&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521#2</TD>
            <TD>2011-09-14T19:00:33Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/120/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/521</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/120/521 [table1]</TD>
            <TD>Galaxies morphology and IR photometry II. (Gavazzi+ 1996)</TD>
            <TD>We present near-infrared H-band (1.65{mu}m) surface photometry of 297 galaxies (mostly) in the Coma Supercluster obtained with the Arcetri NICMOS3 camera, ARNICA, mounted on the Gornergrat Infrared Telescope. Magnitudes and diameters within the 21.5mag/arcsec^2^ isophote, concentration indices, and total H magnitudes are derived. Combining these observations with those obtained similarly using the Calar Alto telescopes (Paper I, &lt;J/A+AS/120/489&gt;) we find a strong positive correlation between the near-infrared concentration index and the galaxy H-band luminosity, and we analyze the consequent dependence of near-infrared growth-curves on H-band luminosity. For a description of the H band photometric system, see e.g. &lt;GCPD/59&gt;</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521#table1</TD>
            <TD>2011-09-14T19:00:33Z</TD>
            <TD>#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/120/521</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/120/521&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/120/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/664/226 [1]</TD>
            <TD>Nuker law parameters of early-type galaxies (Lauer+, 2007)</TD>
            <TD>We combine several HST investigations on the central structure of early-type galaxies to generate a large sample of surface photometry. The studies selected were those that used the "Nuker law" to characterize the inner light distributions of the galaxies. The sample comprises WFPC1 and WFPC2 V-band observations published earlier by our group, R-band WFPC2 photometry of Rest et al. (2001AJ....121.2431R), NICMOS H-band photometry by Ravindranath et al. (2001AJ....122..653R) and Quillen et al. (2000ApJS..128...85Q), and the brightest cluster galaxy WFPC2 I-band photometry of Laine et al. (2003, Cat. J/AJ/125/478).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226#1</TD>
            <TD>2011-09-14T20:47:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/664/226</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/664/226</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/664/226 [2]</TD>
            <TD>Nuker law parameters of early-type galaxies (Lauer+, 2007)</TD>
            <TD>We combine several HST investigations on the central structure of early-type galaxies to generate a large sample of surface photometry. The studies selected were those that used the "Nuker law" to characterize the inner light distributions of the galaxies. The sample comprises WFPC1 and WFPC2 V-band observations published earlier by our group, R-band WFPC2 photometry of Rest et al. (2001AJ....121.2431R), NICMOS H-band photometry by Ravindranath et al. (2001AJ....122..653R) and Quillen et al. (2000ApJS..128...85Q), and the brightest cluster galaxy WFPC2 I-band photometry of Laine et al. (2003, Cat. J/AJ/125/478).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226#2</TD>
            <TD>2011-09-14T20:47:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/664/226&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/664/226</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/664/226 [tables]</TD>
            <TD>Nuker law parameters of early-type galaxies (Lauer+, 2007)</TD>
            <TD>We combine several HST investigations on the central structure of early-type galaxies to generate a large sample of surface photometry. The studies selected were those that used the "Nuker law" to characterize the inner light distributions of the galaxies. The sample comprises WFPC1 and WFPC2 V-band observations published earlier by our group, R-band WFPC2 photometry of Rest et al. (2001AJ....121.2431R), NICMOS H-band photometry by Ravindranath et al. (2001AJ....122..653R) and Quillen et al. (2000ApJS..128...85Q), and the brightest cluster galaxy WFPC2 I-band photometry of Laine et al. (2003, Cat. J/AJ/125/478).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226#tables</TD>
            <TD>2011-09-14T20:47:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/664/226&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/664/226</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/234 [1]</TD>
            <TD>M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002)</TD>
            <TD>We present first results from a spectroscopic survey designed to examine the metallicity and kinematics of individual red giant branch stars in the outer halo of the Andromeda spiral galaxy (M31). This study is based on multislit spectroscopy with the Keck II 10m telescope and Low Resolution Imaging Spectrograph of the Ca II near-infrared triplet in 99 M31 halo candidates in a field at R=19kpc on the southeast minor axis with brightnesses from 20&lt;I&lt;22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234#1</TD>
            <TD>2011-09-14T19:17:16Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/234</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/234</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/234 [2]</TD>
            <TD>M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002)</TD>
            <TD>We present first results from a spectroscopic survey designed to examine the metallicity and kinematics of individual red giant branch stars in the outer halo of the Andromeda spiral galaxy (M31). This study is based on multislit spectroscopy with the Keck II 10m telescope and Low Resolution Imaging Spectrograph of the Ca II near-infrared triplet in 99 M31 halo candidates in a field at R=19kpc on the southeast minor axis with brightnesses from 20&lt;I&lt;22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234#2</TD>
            <TD>2011-09-14T19:17:16Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/234&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/234</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/234 [table1]</TD>
            <TD>M31 outer halo UBVRI photometry and metallicity (Reitzel+, 2002)</TD>
            <TD>We present first results from a spectroscopic survey designed to examine the metallicity and kinematics of individual red giant branch stars in the outer halo of the Andromeda spiral galaxy (M31). This study is based on multislit spectroscopy with the Keck II 10m telescope and Low Resolution Imaging Spectrograph of the Ca II near-infrared triplet in 99 M31 halo candidates in a field at R=19kpc on the southeast minor axis with brightnesses from 20&lt;I&lt;22.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234#table1</TD>
            <TD>2011-09-14T19:17:16Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/234</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/234&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/234</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/94/461 [1]</TD>
            <TD>The Hawai K-band survey. III. (Songaila+ 1994)</TD>
            <TD>We present spectra and multicolor (B,I,K) data for near-infrared (K) selected spatially complete magnitude limited (K&lt;20) galaxy samples from the Hawaii Survey. The redshift identification of the sample of 298 galaxies is substantially complete to a B magnitude of 26 and an I magnitude of 22.5, and identification of observed galaxies ranges from nearly 100% completeness at K&lt;18 to ~70% completeness at K=19-20. We note that many of the unidentified objects appear to be red (I-K) objects which are flat in the optical and spectroscopically featureless. Strengths of spectral-line features and breaks are tabulated for the 262 galaxies with reasonably secure redshifts. The measured redshifts nearly all fall at z&lt;1, with the exception of a compact absorption-line object at z=2.35. At K&gt;=18, the redshift distribution is well fitted by a model with no luminosity evolution, implying that from the K-band Hubble diagram, the Hubble constant can vary at most by 10% over the redshift range from z~0.025 to 0.25, and that positive luminosity evolution at any significant level between z=0 and z=1 is ruled out. However, the evolution of both the emission-line strengths and the 4000{AA} break indicates that galaxies were undergoing significantly more star formation at z=1 than at the present time.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/94/461#1</TD>
            <TD>2011-09-14T19:00:47Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/94/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/94/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/94/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/94/461 [2]</TD>
            <TD>The Hawai K-band survey. III. (Songaila+ 1994)</TD>
            <TD>We present spectra and multicolor (B,I,K) data for near-infrared (K) selected spatially complete magnitude limited (K&lt;20) galaxy samples from the Hawaii Survey. The redshift identification of the sample of 298 galaxies is substantially complete to a B magnitude of 26 and an I magnitude of 22.5, and identification of observed galaxies ranges from nearly 100% completeness at K&lt;18 to ~70% completeness at K=19-20. We note that many of the unidentified objects appear to be red (I-K) objects which are flat in the optical and spectroscopically featureless. Strengths of spectral-line features and breaks are tabulated for the 262 galaxies with reasonably secure redshifts. The measured redshifts nearly all fall at z&lt;1, with the exception of a compact absorption-line object at z=2.35. At K&gt;=18, the redshift distribution is well fitted by a model with no luminosity evolution, implying that from the K-band Hubble diagram, the Hubble constant can vary at most by 10% over the redshift range from z~0.025 to 0.25, and that positive luminosity evolution at any significant level between z=0 and z=1 is ruled out. However, the evolution of both the emission-line strengths and the 4000{AA} break indicates that galaxies were undergoing significantly more star formation at z=1 than at the present time.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/94/461#2</TD>
            <TD>2011-09-14T19:00:47Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/94/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/94/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/94/461</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/664/226 [1]</TD>
            <TD>Nuker law parameters of early-type galaxies (Lauer+, 2007)</TD>
            <TD>We combine several HST investigations on the central structure of early-type galaxies to generate a large sample of surface photometry. The studies selected were those that used the "Nuker law" to characterize the inner light distributions of the galaxies. The sample comprises WFPC1 and WFPC2 V-band observations published earlier by our group, R-band WFPC2 photometry of Rest et al. (2001AJ....121.2431R), NICMOS H-band photometry by Ravindranath et al. (2001AJ....122..653R) and Quillen et al. (2000ApJS..128...85Q), and the brightest cluster galaxy WFPC2 I-band photometry of Laine et al. (2003, Cat. J/AJ/125/478).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226#1</TD>
            <TD>2011-09-14T20:47:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/664/226</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/664/226</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/664/226 [2]</TD>
            <TD>Nuker law parameters of early-type galaxies (Lauer+, 2007)</TD>
            <TD>We combine several HST investigations on the central structure of early-type galaxies to generate a large sample of surface photometry. The studies selected were those that used the "Nuker law" to characterize the inner light distributions of the galaxies. The sample comprises WFPC1 and WFPC2 V-band observations published earlier by our group, R-band WFPC2 photometry of Rest et al. (2001AJ....121.2431R), NICMOS H-band photometry by Ravindranath et al. (2001AJ....122..653R) and Quillen et al. (2000ApJS..128...85Q), and the brightest cluster galaxy WFPC2 I-band photometry of Laine et al. (2003, Cat. J/AJ/125/478).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226#2</TD>
            <TD>2011-09-14T20:47:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/664/226&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/664/226</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/664/226 [tables]</TD>
            <TD>Nuker law parameters of early-type galaxies (Lauer+, 2007)</TD>
            <TD>We combine several HST investigations on the central structure of early-type galaxies to generate a large sample of surface photometry. The studies selected were those that used the "Nuker law" to characterize the inner light distributions of the galaxies. The sample comprises WFPC1 and WFPC2 V-band observations published earlier by our group, R-band WFPC2 photometry of Rest et al. (2001AJ....121.2431R), NICMOS H-band photometry by Ravindranath et al. (2001AJ....122..653R) and Quillen et al. (2000ApJS..128...85Q), and the brightest cluster galaxy WFPC2 I-band photometry of Laine et al. (2003, Cat. J/AJ/125/478).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226#tables</TD>
            <TD>2011-09-14T20:47:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/664/226&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/664/226</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/565/208 [1]</TD>
            <TD>Galaxy pairs in the CNOC2 Redshift Survey (Patton+, 2002)</TD>
            <TD>We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12&lt;=z&lt;=0.55 and R_C_&lt;=21.5. We identify 88 galaxies in close (5&lt;=rp&lt;=20h^-1^kpc) dynamical ({Delta}&lt;=500km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208#1</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/565/208</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/565/208</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/565/208 [2]</TD>
            <TD>Galaxy pairs in the CNOC2 Redshift Survey (Patton+, 2002)</TD>
            <TD>We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12&lt;=z&lt;=0.55 and R_C_&lt;=21.5. We identify 88 galaxies in close (5&lt;=rp&lt;=20h^-1^kpc) dynamical ({Delta}&lt;=500km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208#2</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/565/208&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/565/208</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/565/208 [table1]</TD>
            <TD>Galaxy pairs in the CNOC2 Redshift Survey (Patton+, 2002)</TD>
            <TD>We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12&lt;=z&lt;=0.55 and R_C_&lt;=21.5. We identify 88 galaxies in close (5&lt;=rp&lt;=20h^-1^kpc) dynamical ({Delta}&lt;=500km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208#table1</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/565/208&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/565/208</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/94/461 [1]</TD>
            <TD>The Hawai K-band survey. III. (Songaila+ 1994)</TD>
            <TD>We present spectra and multicolor (B,I,K) data for near-infrared (K) selected spatially complete magnitude limited (K&lt;20) galaxy samples from the Hawaii Survey. The redshift identification of the sample of 298 galaxies is substantially complete to a B magnitude of 26 and an I magnitude of 22.5, and identification of observed galaxies ranges from nearly 100% completeness at K&lt;18 to ~70% completeness at K=19-20. We note that many of the unidentified objects appear to be red (I-K) objects which are flat in the optical and spectroscopically featureless. Strengths of spectral-line features and breaks are tabulated for the 262 galaxies with reasonably secure redshifts. The measured redshifts nearly all fall at z&lt;1, with the exception of a compact absorption-line object at z=2.35. At K&gt;=18, the redshift distribution is well fitted by a model with no luminosity evolution, implying that from the K-band Hubble diagram, the Hubble constant can vary at most by 10% over the redshift range from z~0.025 to 0.25, and that positive luminosity evolution at any significant level between z=0 and z=1 is ruled out. However, the evolution of both the emission-line strengths and the 4000{AA} break indicates that galaxies were undergoing significantly more star formation at z=1 than at the present time.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/94/461#1</TD>
            <TD>2011-09-14T19:00:47Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/94/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/94/461</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/94/461</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/94/461 [2]</TD>
            <TD>The Hawai K-band survey. III. (Songaila+ 1994)</TD>
            <TD>We present spectra and multicolor (B,I,K) data for near-infrared (K) selected spatially complete magnitude limited (K&lt;20) galaxy samples from the Hawaii Survey. The redshift identification of the sample of 298 galaxies is substantially complete to a B magnitude of 26 and an I magnitude of 22.5, and identification of observed galaxies ranges from nearly 100% completeness at K&lt;18 to ~70% completeness at K=19-20. We note that many of the unidentified objects appear to be red (I-K) objects which are flat in the optical and spectroscopically featureless. Strengths of spectral-line features and breaks are tabulated for the 262 galaxies with reasonably secure redshifts. The measured redshifts nearly all fall at z&lt;1, with the exception of a compact absorption-line object at z=2.35. At K&gt;=18, the redshift distribution is well fitted by a model with no luminosity evolution, implying that from the K-band Hubble diagram, the Hubble constant can vary at most by 10% over the redshift range from z~0.025 to 0.25, and that positive luminosity evolution at any significant level between z=0 and z=1 is ruled out. However, the evolution of both the emission-line strengths and the 4000{AA} break indicates that galaxies were undergoing significantly more star formation at z=1 than at the present time.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/94/461#2</TD>
            <TD>2011-09-14T19:00:47Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jul-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/94/461</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/94/461&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/94/461</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/664/226 [1]</TD>
            <TD>Nuker law parameters of early-type galaxies (Lauer+, 2007)</TD>
            <TD>We combine several HST investigations on the central structure of early-type galaxies to generate a large sample of surface photometry. The studies selected were those that used the "Nuker law" to characterize the inner light distributions of the galaxies. The sample comprises WFPC1 and WFPC2 V-band observations published earlier by our group, R-band WFPC2 photometry of Rest et al. (2001AJ....121.2431R), NICMOS H-band photometry by Ravindranath et al. (2001AJ....122..653R) and Quillen et al. (2000ApJS..128...85Q), and the brightest cluster galaxy WFPC2 I-band photometry of Laine et al. (2003, Cat. J/AJ/125/478).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226#1</TD>
            <TD>2011-09-14T20:47:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/664/226</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/664/226</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/664/226 [2]</TD>
            <TD>Nuker law parameters of early-type galaxies (Lauer+, 2007)</TD>
            <TD>We combine several HST investigations on the central structure of early-type galaxies to generate a large sample of surface photometry. The studies selected were those that used the "Nuker law" to characterize the inner light distributions of the galaxies. The sample comprises WFPC1 and WFPC2 V-band observations published earlier by our group, R-band WFPC2 photometry of Rest et al. (2001AJ....121.2431R), NICMOS H-band photometry by Ravindranath et al. (2001AJ....122..653R) and Quillen et al. (2000ApJS..128...85Q), and the brightest cluster galaxy WFPC2 I-band photometry of Laine et al. (2003, Cat. J/AJ/125/478).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226#2</TD>
            <TD>2011-09-14T20:47:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/664/226&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/664/226</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/664/226 [tables]</TD>
            <TD>Nuker law parameters of early-type galaxies (Lauer+, 2007)</TD>
            <TD>We combine several HST investigations on the central structure of early-type galaxies to generate a large sample of surface photometry. The studies selected were those that used the "Nuker law" to characterize the inner light distributions of the galaxies. The sample comprises WFPC1 and WFPC2 V-band observations published earlier by our group, R-band WFPC2 photometry of Rest et al. (2001AJ....121.2431R), NICMOS H-band photometry by Ravindranath et al. (2001AJ....122..653R) and Quillen et al. (2000ApJS..128...85Q), and the brightest cluster galaxy WFPC2 I-band photometry of Laine et al. (2003, Cat. J/AJ/125/478).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226#tables</TD>
            <TD>2011-09-14T20:47:02Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Aug-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/664/226</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/664/226&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/664/226</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/565/208 [1]</TD>
            <TD>Galaxy pairs in the CNOC2 Redshift Survey (Patton+, 2002)</TD>
            <TD>We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12&lt;=z&lt;=0.55 and R_C_&lt;=21.5. We identify 88 galaxies in close (5&lt;=rp&lt;=20h^-1^kpc) dynamical ({Delta}&lt;=500km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208#1</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/565/208</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/565/208</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/565/208 [2]</TD>
            <TD>Galaxy pairs in the CNOC2 Redshift Survey (Patton+, 2002)</TD>
            <TD>We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12&lt;=z&lt;=0.55 and R_C_&lt;=21.5. We identify 88 galaxies in close (5&lt;=rp&lt;=20h^-1^kpc) dynamical ({Delta}&lt;=500km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208#2</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/565/208&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/565/208</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/565/208 [table1]</TD>
            <TD>Galaxy pairs in the CNOC2 Redshift Survey (Patton+, 2002)</TD>
            <TD>We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12&lt;=z&lt;=0.55 and R_C_&lt;=21.5. We identify 88 galaxies in close (5&lt;=rp&lt;=20h^-1^kpc) dynamical ({Delta}&lt;=500km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208#table1</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/565/208&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/565/208</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/662/15 [1]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#1</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/662/15</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/662/15 [2]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#2</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/662/15&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/662/15 [sample1]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#sample1</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/662/15&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/662/15 [sample2]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#sample2</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/662/15&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/76/83 [1]</TD>
            <TD>Galaxies in and near the cluster A1185 (Botashev+ 1999)</TD>
            <TD>Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are presented. Coordinates have been obtained for 115 galaxies that are either cluster members or field galaxies in the direction of A1185. Radio spectra for a number of galaxies in this cluster have been derived using observations on the RATAN-600 radio telescope at 2.7,3.9,7.6, and 31 cm, together with data published in other study. At the cluster center some of the galaxies have either flat or inverted spectra.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83#1</TD>
            <TD>2011-09-14T19:02:44Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/76/83</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/76/83</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/76/83 [2]</TD>
            <TD>Galaxies in and near the cluster A1185 (Botashev+ 1999)</TD>
            <TD>Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are presented. Coordinates have been obtained for 115 galaxies that are either cluster members or field galaxies in the direction of A1185. Radio spectra for a number of galaxies in this cluster have been derived using observations on the RATAN-600 radio telescope at 2.7,3.9,7.6, and 31 cm, together with data published in other study. At the cluster center some of the galaxies have either flat or inverted spectra.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83#2</TD>
            <TD>2011-09-14T19:02:44Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/76/83&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/76/83</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/662/15 [1]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#1</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/662/15</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/662/15 [2]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#2</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/662/15&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/662/15 [sample1]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#sample1</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/662/15&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/662/15 [sample2]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#sample2</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/662/15&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/565/208 [1]</TD>
            <TD>Galaxy pairs in the CNOC2 Redshift Survey (Patton+, 2002)</TD>
            <TD>We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12&lt;=z&lt;=0.55 and R_C_&lt;=21.5. We identify 88 galaxies in close (5&lt;=rp&lt;=20h^-1^kpc) dynamical ({Delta}&lt;=500km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208#1</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/565/208</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/565/208</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/565/208 [2]</TD>
            <TD>Galaxy pairs in the CNOC2 Redshift Survey (Patton+, 2002)</TD>
            <TD>We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12&lt;=z&lt;=0.55 and R_C_&lt;=21.5. We identify 88 galaxies in close (5&lt;=rp&lt;=20h^-1^kpc) dynamical ({Delta}&lt;=500km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208#2</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/565/208&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/565/208</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/565/208 [table1]</TD>
            <TD>Galaxy pairs in the CNOC2 Redshift Survey (Patton+, 2002)</TD>
            <TD>We investigate redshift evolution in the galaxy merger and accretion rates, using a well-defined sample of 4184 galaxies with 0.12&lt;=z&lt;=0.55 and R_C_&lt;=21.5. We identify 88 galaxies in close (5&lt;=rp&lt;=20h^-1^kpc) dynamical ({Delta}&lt;=500km/s) pairs. These galaxies are used to compute global pair statistics, after accounting for selection effects resulting from the flux limit, k-corrections, luminosity evolution, and spectroscopic incompleteness.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208#table1</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/565/208</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/565/208&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/565/208</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/219 [1]</TD>
            <TD>Revised Flat Galaxy Catalogue (RFGC) (Karachentsev+, 1999)</TD>
            <TD>The Flat Galaxy Catalog (FGC) is the result of a systematic search for disk-like edge-on galaxies with a diameter larger than a=40arcsec and major-to-minor axis ratio a/b&gt;7 from Palomar Observatory and ESO/SERC surveys; it contained 4455 objects covering about 56% of the whole sky (Karachentsev et al., 1993AN....314...97K, see Cat. &lt;VII/162&gt;). The main reasons for preparing a new, improved and supplemented catalogue version were the following: - a possibility of remeasuring the coordinates of flat galaxies with a higher accuracy using the Digital Sky Survey; - the inclusion the data about "red" galaxy diameters which were absent earlier; - a reduction the diameters measured on the J and R films of the ESO/SERC to the diameter system of the POSS-I (near to a_25_ system) that eliminated the difference in photometric depth between two parts of the catalogue (Kudrya et al. 1997PAZh...23...15K); - a calculation of total apparent magnitudes (with a standard error about 0.25mag) for all flat galaxies basing on angular diameters, surface brightnesses, and other parameter data (Kudrya et al. 1997PAZh...23..730K); - a possibility to determine the Galaxy absorption values in the region of each flat galaxy placing using new IR data (Schlegel et al. 1998ApJ...500..525S). - a necessity to remove the faults noted during the work with the FGC data. The structural differences between old and new catalogue versions are: - both the parts, FGC and FGCE, have been joined in the RFGC (Revised Flat Galaxy Catalogue) where the galaxies are ranged according to their Right Ascensions for the epoch J2000.0; - the Addendum have been omitted; - the Notes describing concrete object characteristics have been included in the main corpus of the catalogue, some details were omitted; - the lists of identification of the FGC and the FGCE galaxies have been omitted because these data are accessible now due to different galaxy databases (NED, LEDA etc).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/219#1</TD>
            <TD>2011-09-14T19:17:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/VII/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/219</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/219</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/219 [2]</TD>
            <TD>Revised Flat Galaxy Catalogue (RFGC) (Karachentsev+, 1999)</TD>
            <TD>The Flat Galaxy Catalog (FGC) is the result of a systematic search for disk-like edge-on galaxies with a diameter larger than a=40arcsec and major-to-minor axis ratio a/b&gt;7 from Palomar Observatory and ESO/SERC surveys; it contained 4455 objects covering about 56% of the whole sky (Karachentsev et al., 1993AN....314...97K, see Cat. &lt;VII/162&gt;). The main reasons for preparing a new, improved and supplemented catalogue version were the following: - a possibility of remeasuring the coordinates of flat galaxies with a higher accuracy using the Digital Sky Survey; - the inclusion the data about "red" galaxy diameters which were absent earlier; - a reduction the diameters measured on the J and R films of the ESO/SERC to the diameter system of the POSS-I (near to a_25_ system) that eliminated the difference in photometric depth between two parts of the catalogue (Kudrya et al. 1997PAZh...23...15K); - a calculation of total apparent magnitudes (with a standard error about 0.25mag) for all flat galaxies basing on angular diameters, surface brightnesses, and other parameter data (Kudrya et al. 1997PAZh...23..730K); - a possibility to determine the Galaxy absorption values in the region of each flat galaxy placing using new IR data (Schlegel et al. 1998ApJ...500..525S). - a necessity to remove the faults noted during the work with the FGC data. The structural differences between old and new catalogue versions are: - both the parts, FGC and FGCE, have been joined in the RFGC (Revised Flat Galaxy Catalogue) where the galaxies are ranged according to their Right Ascensions for the epoch J2000.0; - the Addendum have been omitted; - the Notes describing concrete object characteristics have been included in the main corpus of the catalogue, some details were omitted; - the lists of identification of the FGC and the FGCE galaxies have been omitted because these data are accessible now due to different galaxy databases (NED, LEDA etc).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/219#2</TD>
            <TD>2011-09-14T19:17:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/VII/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/219&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/219 [rfgc]</TD>
            <TD>Revised Flat Galaxy Catalogue (RFGC) (Karachentsev+, 1999)</TD>
            <TD>The Flat Galaxy Catalog (FGC) is the result of a systematic search for disk-like edge-on galaxies with a diameter larger than a=40arcsec and major-to-minor axis ratio a/b&gt;7 from Palomar Observatory and ESO/SERC surveys; it contained 4455 objects covering about 56% of the whole sky (Karachentsev et al., 1993AN....314...97K, see Cat. &lt;VII/162&gt;). The main reasons for preparing a new, improved and supplemented catalogue version were the following: - a possibility of remeasuring the coordinates of flat galaxies with a higher accuracy using the Digital Sky Survey; - the inclusion the data about "red" galaxy diameters which were absent earlier; - a reduction the diameters measured on the J and R films of the ESO/SERC to the diameter system of the POSS-I (near to a_25_ system) that eliminated the difference in photometric depth between two parts of the catalogue (Kudrya et al. 1997PAZh...23...15K); - a calculation of total apparent magnitudes (with a standard error about 0.25mag) for all flat galaxies basing on angular diameters, surface brightnesses, and other parameter data (Kudrya et al. 1997PAZh...23..730K); - a possibility to determine the Galaxy absorption values in the region of each flat galaxy placing using new IR data (Schlegel et al. 1998ApJ...500..525S). - a necessity to remove the faults noted during the work with the FGC data. The structural differences between old and new catalogue versions are: - both the parts, FGC and FGCE, have been joined in the RFGC (Revised Flat Galaxy Catalogue) where the galaxies are ranged according to their Right Ascensions for the epoch J2000.0; - the Addendum have been omitted; - the Notes describing concrete object characteristics have been included in the main corpus of the catalogue, some details were omitted; - the lists of identification of the FGC and the FGCE galaxies have been omitted because these data are accessible now due to different galaxy databases (NED, LEDA etc).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/219#rfgc</TD>
            <TD>2011-09-14T19:17:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/VII/219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/219</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/219 [1]</TD>
            <TD>Revised Flat Galaxy Catalogue (RFGC) (Karachentsev+, 1999)</TD>
            <TD>The Flat Galaxy Catalog (FGC) is the result of a systematic search for disk-like edge-on galaxies with a diameter larger than a=40arcsec and major-to-minor axis ratio a/b&gt;7 from Palomar Observatory and ESO/SERC surveys; it contained 4455 objects covering about 56% of the whole sky (Karachentsev et al., 1993AN....314...97K, see Cat. &lt;VII/162&gt;). The main reasons for preparing a new, improved and supplemented catalogue version were the following: - a possibility of remeasuring the coordinates of flat galaxies with a higher accuracy using the Digital Sky Survey; - the inclusion the data about "red" galaxy diameters which were absent earlier; - a reduction the diameters measured on the J and R films of the ESO/SERC to the diameter system of the POSS-I (near to a_25_ system) that eliminated the difference in photometric depth between two parts of the catalogue (Kudrya et al. 1997PAZh...23...15K); - a calculation of total apparent magnitudes (with a standard error about 0.25mag) for all flat galaxies basing on angular diameters, surface brightnesses, and other parameter data (Kudrya et al. 1997PAZh...23..730K); - a possibility to determine the Galaxy absorption values in the region of each flat galaxy placing using new IR data (Schlegel et al. 1998ApJ...500..525S). - a necessity to remove the faults noted during the work with the FGC data. The structural differences between old and new catalogue versions are: - both the parts, FGC and FGCE, have been joined in the RFGC (Revised Flat Galaxy Catalogue) where the galaxies are ranged according to their Right Ascensions for the epoch J2000.0; - the Addendum have been omitted; - the Notes describing concrete object characteristics have been included in the main corpus of the catalogue, some details were omitted; - the lists of identification of the FGC and the FGCE galaxies have been omitted because these data are accessible now due to different galaxy databases (NED, LEDA etc).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/219#1</TD>
            <TD>2011-09-14T19:17:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/VII/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/219</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/219</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/219 [2]</TD>
            <TD>Revised Flat Galaxy Catalogue (RFGC) (Karachentsev+, 1999)</TD>
            <TD>The Flat Galaxy Catalog (FGC) is the result of a systematic search for disk-like edge-on galaxies with a diameter larger than a=40arcsec and major-to-minor axis ratio a/b&gt;7 from Palomar Observatory and ESO/SERC surveys; it contained 4455 objects covering about 56% of the whole sky (Karachentsev et al., 1993AN....314...97K, see Cat. &lt;VII/162&gt;). The main reasons for preparing a new, improved and supplemented catalogue version were the following: - a possibility of remeasuring the coordinates of flat galaxies with a higher accuracy using the Digital Sky Survey; - the inclusion the data about "red" galaxy diameters which were absent earlier; - a reduction the diameters measured on the J and R films of the ESO/SERC to the diameter system of the POSS-I (near to a_25_ system) that eliminated the difference in photometric depth between two parts of the catalogue (Kudrya et al. 1997PAZh...23...15K); - a calculation of total apparent magnitudes (with a standard error about 0.25mag) for all flat galaxies basing on angular diameters, surface brightnesses, and other parameter data (Kudrya et al. 1997PAZh...23..730K); - a possibility to determine the Galaxy absorption values in the region of each flat galaxy placing using new IR data (Schlegel et al. 1998ApJ...500..525S). - a necessity to remove the faults noted during the work with the FGC data. The structural differences between old and new catalogue versions are: - both the parts, FGC and FGCE, have been joined in the RFGC (Revised Flat Galaxy Catalogue) where the galaxies are ranged according to their Right Ascensions for the epoch J2000.0; - the Addendum have been omitted; - the Notes describing concrete object characteristics have been included in the main corpus of the catalogue, some details were omitted; - the lists of identification of the FGC and the FGCE galaxies have been omitted because these data are accessible now due to different galaxy databases (NED, LEDA etc).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/219#2</TD>
            <TD>2011-09-14T19:17:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/VII/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/219&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/219 [rfgc]</TD>
            <TD>Revised Flat Galaxy Catalogue (RFGC) (Karachentsev+, 1999)</TD>
            <TD>The Flat Galaxy Catalog (FGC) is the result of a systematic search for disk-like edge-on galaxies with a diameter larger than a=40arcsec and major-to-minor axis ratio a/b&gt;7 from Palomar Observatory and ESO/SERC surveys; it contained 4455 objects covering about 56% of the whole sky (Karachentsev et al., 1993AN....314...97K, see Cat. &lt;VII/162&gt;). The main reasons for preparing a new, improved and supplemented catalogue version were the following: - a possibility of remeasuring the coordinates of flat galaxies with a higher accuracy using the Digital Sky Survey; - the inclusion the data about "red" galaxy diameters which were absent earlier; - a reduction the diameters measured on the J and R films of the ESO/SERC to the diameter system of the POSS-I (near to a_25_ system) that eliminated the difference in photometric depth between two parts of the catalogue (Kudrya et al. 1997PAZh...23...15K); - a calculation of total apparent magnitudes (with a standard error about 0.25mag) for all flat galaxies basing on angular diameters, surface brightnesses, and other parameter data (Kudrya et al. 1997PAZh...23..730K); - a possibility to determine the Galaxy absorption values in the region of each flat galaxy placing using new IR data (Schlegel et al. 1998ApJ...500..525S). - a necessity to remove the faults noted during the work with the FGC data. The structural differences between old and new catalogue versions are: - both the parts, FGC and FGCE, have been joined in the RFGC (Revised Flat Galaxy Catalogue) where the galaxies are ranged according to their Right Ascensions for the epoch J2000.0; - the Addendum have been omitted; - the Notes describing concrete object characteristics have been included in the main corpus of the catalogue, some details were omitted; - the lists of identification of the FGC and the FGCE galaxies have been omitted because these data are accessible now due to different galaxy databases (NED, LEDA etc).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/219#rfgc</TD>
            <TD>2011-09-14T19:17:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/VII/219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/219</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/101 [1]</TD>
            <TD>Galaxies in the "zone of avoidance". V. (Seeberger+ 1998)</TD>
            <TD>As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}&lt;=l&lt;=110{deg}, -10{deg}&lt;=b&lt;=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101#1</TD>
            <TD>2011-09-14T18:39:47Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/101 [2]</TD>
            <TD>Galaxies in the "zone of avoidance". V. (Seeberger+ 1998)</TD>
            <TD>As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}&lt;=l&lt;=110{deg}, -10{deg}&lt;=b&lt;=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101#2</TD>
            <TD>2011-09-14T18:39:47Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/101 [table2]</TD>
            <TD>Galaxies in the "zone of avoidance". V. (Seeberger+ 1998)</TD>
            <TD>As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}&lt;=l&lt;=110{deg}, -10{deg}&lt;=b&lt;=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101#table2</TD>
            <TD>2011-09-14T18:39:47Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/101 [1]</TD>
            <TD>Galaxies in the "zone of avoidance". V. (Seeberger+ 1998)</TD>
            <TD>As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}&lt;=l&lt;=110{deg}, -10{deg}&lt;=b&lt;=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101#1</TD>
            <TD>2011-09-14T18:39:47Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/101</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/101</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/101 [2]</TD>
            <TD>Galaxies in the "zone of avoidance". V. (Seeberger+ 1998)</TD>
            <TD>As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}&lt;=l&lt;=110{deg}, -10{deg}&lt;=b&lt;=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101#2</TD>
            <TD>2011-09-14T18:39:47Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/101&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/101</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/101 [table2]</TD>
            <TD>Galaxies in the "zone of avoidance". V. (Seeberger+ 1998)</TD>
            <TD>As the fifth part in our series of papers on galaxies in the "zone of avoidance" (ZOA) of the Milky Way we present 1346 new galaxy candidates discovered during a systematic search on Palomar Observatory Sky Survey (POSSI-E) red-sensitive prints. The region searched comprises 400 square degrees at 90{deg}&lt;=l&lt;=110{deg}, -10{deg}&lt;=b&lt;=+10{deg}. We list galactic and equatorial coordinates, maximum optical diameters and diameters of the core, if visible, both for the red- and blue-sensitive POSS prints. An asymmetric distribution of the galaxies with respect to the galactic equator is found and can most probably be attributed to the galactic warp. We also present radial velocities for 14 galaxies measured for the first time which are located in the region where a branch of the Pisces Perseus Supercluster is approaching the ZOA from the south (l=~90{deg}, b=~-10{deg}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101#table2</TD>
            <TD>2011-09-14T18:39:47Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/101</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/101&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/101</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/219 [1]</TD>
            <TD>Revised Flat Galaxy Catalogue (RFGC) (Karachentsev+, 1999)</TD>
            <TD>The Flat Galaxy Catalog (FGC) is the result of a systematic search for disk-like edge-on galaxies with a diameter larger than a=40arcsec and major-to-minor axis ratio a/b&gt;7 from Palomar Observatory and ESO/SERC surveys; it contained 4455 objects covering about 56% of the whole sky (Karachentsev et al., 1993AN....314...97K, see Cat. &lt;VII/162&gt;). The main reasons for preparing a new, improved and supplemented catalogue version were the following: - a possibility of remeasuring the coordinates of flat galaxies with a higher accuracy using the Digital Sky Survey; - the inclusion the data about "red" galaxy diameters which were absent earlier; - a reduction the diameters measured on the J and R films of the ESO/SERC to the diameter system of the POSS-I (near to a_25_ system) that eliminated the difference in photometric depth between two parts of the catalogue (Kudrya et al. 1997PAZh...23...15K); - a calculation of total apparent magnitudes (with a standard error about 0.25mag) for all flat galaxies basing on angular diameters, surface brightnesses, and other parameter data (Kudrya et al. 1997PAZh...23..730K); - a possibility to determine the Galaxy absorption values in the region of each flat galaxy placing using new IR data (Schlegel et al. 1998ApJ...500..525S). - a necessity to remove the faults noted during the work with the FGC data. The structural differences between old and new catalogue versions are: - both the parts, FGC and FGCE, have been joined in the RFGC (Revised Flat Galaxy Catalogue) where the galaxies are ranged according to their Right Ascensions for the epoch J2000.0; - the Addendum have been omitted; - the Notes describing concrete object characteristics have been included in the main corpus of the catalogue, some details were omitted; - the lists of identification of the FGC and the FGCE galaxies have been omitted because these data are accessible now due to different galaxy databases (NED, LEDA etc).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/219#1</TD>
            <TD>2011-09-14T19:17:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/VII/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/219</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/219</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/219 [2]</TD>
            <TD>Revised Flat Galaxy Catalogue (RFGC) (Karachentsev+, 1999)</TD>
            <TD>The Flat Galaxy Catalog (FGC) is the result of a systematic search for disk-like edge-on galaxies with a diameter larger than a=40arcsec and major-to-minor axis ratio a/b&gt;7 from Palomar Observatory and ESO/SERC surveys; it contained 4455 objects covering about 56% of the whole sky (Karachentsev et al., 1993AN....314...97K, see Cat. &lt;VII/162&gt;). The main reasons for preparing a new, improved and supplemented catalogue version were the following: - a possibility of remeasuring the coordinates of flat galaxies with a higher accuracy using the Digital Sky Survey; - the inclusion the data about "red" galaxy diameters which were absent earlier; - a reduction the diameters measured on the J and R films of the ESO/SERC to the diameter system of the POSS-I (near to a_25_ system) that eliminated the difference in photometric depth between two parts of the catalogue (Kudrya et al. 1997PAZh...23...15K); - a calculation of total apparent magnitudes (with a standard error about 0.25mag) for all flat galaxies basing on angular diameters, surface brightnesses, and other parameter data (Kudrya et al. 1997PAZh...23..730K); - a possibility to determine the Galaxy absorption values in the region of each flat galaxy placing using new IR data (Schlegel et al. 1998ApJ...500..525S). - a necessity to remove the faults noted during the work with the FGC data. The structural differences between old and new catalogue versions are: - both the parts, FGC and FGCE, have been joined in the RFGC (Revised Flat Galaxy Catalogue) where the galaxies are ranged according to their Right Ascensions for the epoch J2000.0; - the Addendum have been omitted; - the Notes describing concrete object characteristics have been included in the main corpus of the catalogue, some details were omitted; - the lists of identification of the FGC and the FGCE galaxies have been omitted because these data are accessible now due to different galaxy databases (NED, LEDA etc).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/219#2</TD>
            <TD>2011-09-14T19:17:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/VII/219</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/219&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/219</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/219 [rfgc]</TD>
            <TD>Revised Flat Galaxy Catalogue (RFGC) (Karachentsev+, 1999)</TD>
            <TD>The Flat Galaxy Catalog (FGC) is the result of a systematic search for disk-like edge-on galaxies with a diameter larger than a=40arcsec and major-to-minor axis ratio a/b&gt;7 from Palomar Observatory and ESO/SERC surveys; it contained 4455 objects covering about 56% of the whole sky (Karachentsev et al., 1993AN....314...97K, see Cat. &lt;VII/162&gt;). The main reasons for preparing a new, improved and supplemented catalogue version were the following: - a possibility of remeasuring the coordinates of flat galaxies with a higher accuracy using the Digital Sky Survey; - the inclusion the data about "red" galaxy diameters which were absent earlier; - a reduction the diameters measured on the J and R films of the ESO/SERC to the diameter system of the POSS-I (near to a_25_ system) that eliminated the difference in photometric depth between two parts of the catalogue (Kudrya et al. 1997PAZh...23...15K); - a calculation of total apparent magnitudes (with a standard error about 0.25mag) for all flat galaxies basing on angular diameters, surface brightnesses, and other parameter data (Kudrya et al. 1997PAZh...23..730K); - a possibility to determine the Galaxy absorption values in the region of each flat galaxy placing using new IR data (Schlegel et al. 1998ApJ...500..525S). - a necessity to remove the faults noted during the work with the FGC data. The structural differences between old and new catalogue versions are: - both the parts, FGC and FGCE, have been joined in the RFGC (Revised Flat Galaxy Catalogue) where the galaxies are ranged according to their Right Ascensions for the epoch J2000.0; - the Addendum have been omitted; - the Notes describing concrete object characteristics have been included in the main corpus of the catalogue, some details were omitted; - the lists of identification of the FGC and the FGCE galaxies have been omitted because these data are accessible now due to different galaxy databases (NED, LEDA etc).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/219#rfgc</TD>
            <TD>2011-09-14T19:17:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/VII/219</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/219&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/219</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/99/501 [1]</TD>
            <TD>Spiral galaxies rotation curves (Persic+ 1995)</TD>
            <TD>We present the rotation curves of 967 southern spiral galaxies, obtained by deprojecting and folding the raw H{alpha} data originally published by Mathewson, Ford, &amp; Buchhorn (1992ApJS...81..413M). For 900 objects, we also present, in figures and tables, the rotation curves smoothed on scales corresponding to 5%-20% of the optical size; of these, 80 meet objective excellence criteria and are suitable for individual detailed mass modeling, while 820, individually less compelling mainly because of the moderate statistics and/or limited extension, are suitable for statistical studies. The remaining 67 curves suffer from severe asymmetries, small statistics, and large internal scatter that may largely limit their use in galaxy structure studies. The deprojected folded curves, the smoothed curves, and various related quantities are available via anonymous ftp at galileo.sissa.it in the directory /users/ftp/pub/psrot.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/501#1</TD>
            <TD>2011-09-14T18:41:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/99/501</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/99/501</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/99/501 [2]</TD>
            <TD>Spiral galaxies rotation curves (Persic+ 1995)</TD>
            <TD>We present the rotation curves of 967 southern spiral galaxies, obtained by deprojecting and folding the raw H{alpha} data originally published by Mathewson, Ford, &amp; Buchhorn (1992ApJS...81..413M). For 900 objects, we also present, in figures and tables, the rotation curves smoothed on scales corresponding to 5%-20% of the optical size; of these, 80 meet objective excellence criteria and are suitable for individual detailed mass modeling, while 820, individually less compelling mainly because of the moderate statistics and/or limited extension, are suitable for statistical studies. The remaining 67 curves suffer from severe asymmetries, small statistics, and large internal scatter that may largely limit their use in galaxy structure studies. The deprojected folded curves, the smoothed curves, and various related quantities are available via anonymous ftp at galileo.sissa.it in the directory /users/ftp/pub/psrot.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/501#2</TD>
            <TD>2011-09-14T18:41:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/99/501&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/99/501</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/76/83 [1]</TD>
            <TD>Galaxies in and near the cluster A1185 (Botashev+ 1999)</TD>
            <TD>Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are presented. Coordinates have been obtained for 115 galaxies that are either cluster members or field galaxies in the direction of A1185. Radio spectra for a number of galaxies in this cluster have been derived using observations on the RATAN-600 radio telescope at 2.7,3.9,7.6, and 31 cm, together with data published in other study. At the cluster center some of the galaxies have either flat or inverted spectra.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83#1</TD>
            <TD>2011-09-14T19:02:44Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/76/83</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/76/83</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/76/83 [2]</TD>
            <TD>Galaxies in and near the cluster A1185 (Botashev+ 1999)</TD>
            <TD>Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are presented. Coordinates have been obtained for 115 galaxies that are either cluster members or field galaxies in the direction of A1185. Radio spectra for a number of galaxies in this cluster have been derived using observations on the RATAN-600 radio telescope at 2.7,3.9,7.6, and 31 cm, together with data published in other study. At the cluster center some of the galaxies have either flat or inverted spectra.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83#2</TD>
            <TD>2011-09-14T19:02:44Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/76/83&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/76/83</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/333/423 [1]</TD>
            <TD>Luminosity function of the Virgo Cluster (Trentham+, 2002)</TD>
            <TD>We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes M_B_=-22 and -11 from wide-field charge-coupled device (CCD) imaging data. The data used here were taken on various observing runs during Spring 1999 and Spring 2000 as part of the INT Wide Field Survey (WFS; http://www.ast.cam.ac.uk/wfcsur ; McMahon et al., 2001NewAR..45...97M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423#1</TD>
            <TD>2011-09-14T19:18:20Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/333/423</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/423</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/333/423 [2]</TD>
            <TD>Luminosity function of the Virgo Cluster (Trentham+, 2002)</TD>
            <TD>We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes M_B_=-22 and -11 from wide-field charge-coupled device (CCD) imaging data. The data used here were taken on various observing runs during Spring 1999 and Spring 2000 as part of the INT Wide Field Survey (WFS; http://www.ast.cam.ac.uk/wfcsur ; McMahon et al., 2001NewAR..45...97M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423#2</TD>
            <TD>2011-09-14T19:18:20Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/333/423&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/333/423 [table2]</TD>
            <TD>Luminosity function of the Virgo Cluster (Trentham+, 2002)</TD>
            <TD>We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes M_B_=-22 and -11 from wide-field charge-coupled device (CCD) imaging data. The data used here were taken on various observing runs during Spring 1999 and Spring 2000 as part of the INT Wide Field Survey (WFS; http://www.ast.cam.ac.uk/wfcsur ; McMahon et al., 2001NewAR..45...97M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423#table2</TD>
            <TD>2011-09-14T19:18:20Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/333/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/423</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/99/501 [1]</TD>
            <TD>Spiral galaxies rotation curves (Persic+ 1995)</TD>
            <TD>We present the rotation curves of 967 southern spiral galaxies, obtained by deprojecting and folding the raw H{alpha} data originally published by Mathewson, Ford, &amp; Buchhorn (1992ApJS...81..413M). For 900 objects, we also present, in figures and tables, the rotation curves smoothed on scales corresponding to 5%-20% of the optical size; of these, 80 meet objective excellence criteria and are suitable for individual detailed mass modeling, while 820, individually less compelling mainly because of the moderate statistics and/or limited extension, are suitable for statistical studies. The remaining 67 curves suffer from severe asymmetries, small statistics, and large internal scatter that may largely limit their use in galaxy structure studies. The deprojected folded curves, the smoothed curves, and various related quantities are available via anonymous ftp at galileo.sissa.it in the directory /users/ftp/pub/psrot.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/501#1</TD>
            <TD>2011-09-14T18:41:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/99/501</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/99/501</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/99/501 [2]</TD>
            <TD>Spiral galaxies rotation curves (Persic+ 1995)</TD>
            <TD>We present the rotation curves of 967 southern spiral galaxies, obtained by deprojecting and folding the raw H{alpha} data originally published by Mathewson, Ford, &amp; Buchhorn (1992ApJS...81..413M). For 900 objects, we also present, in figures and tables, the rotation curves smoothed on scales corresponding to 5%-20% of the optical size; of these, 80 meet objective excellence criteria and are suitable for individual detailed mass modeling, while 820, individually less compelling mainly because of the moderate statistics and/or limited extension, are suitable for statistical studies. The remaining 67 curves suffer from severe asymmetries, small statistics, and large internal scatter that may largely limit their use in galaxy structure studies. The deprojected folded curves, the smoothed curves, and various related quantities are available via anonymous ftp at galileo.sissa.it in the directory /users/ftp/pub/psrot.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/501#2</TD>
            <TD>2011-09-14T18:41:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/99/501</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/99/501&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/99/501</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/333/423 [1]</TD>
            <TD>Luminosity function of the Virgo Cluster (Trentham+, 2002)</TD>
            <TD>We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes M_B_=-22 and -11 from wide-field charge-coupled device (CCD) imaging data. The data used here were taken on various observing runs during Spring 1999 and Spring 2000 as part of the INT Wide Field Survey (WFS; http://www.ast.cam.ac.uk/wfcsur ; McMahon et al., 2001NewAR..45...97M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423#1</TD>
            <TD>2011-09-14T19:18:20Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/333/423</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/423</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/333/423 [2]</TD>
            <TD>Luminosity function of the Virgo Cluster (Trentham+, 2002)</TD>
            <TD>We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes M_B_=-22 and -11 from wide-field charge-coupled device (CCD) imaging data. The data used here were taken on various observing runs during Spring 1999 and Spring 2000 as part of the INT Wide Field Survey (WFS; http://www.ast.cam.ac.uk/wfcsur ; McMahon et al., 2001NewAR..45...97M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423#2</TD>
            <TD>2011-09-14T19:18:20Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/333/423&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/333/423 [table2]</TD>
            <TD>Luminosity function of the Virgo Cluster (Trentham+, 2002)</TD>
            <TD>We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes M_B_=-22 and -11 from wide-field charge-coupled device (CCD) imaging data. The data used here were taken on various observing runs during Spring 1999 and Spring 2000 as part of the INT Wide Field Survey (WFS; http://www.ast.cam.ac.uk/wfcsur ; McMahon et al., 2001NewAR..45...97M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423#table2</TD>
            <TD>2011-09-14T19:18:20Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/333/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/423</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/662/15 [1]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#1</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/662/15</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/662/15 [2]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#2</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/662/15&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/662/15 [sample1]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#sample1</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/662/15&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/662/15 [sample2]</TD>
            <TD>Abundances in extragalactic HII regions (Izotov+, 2007)</TD>
            <TD>++++Lrecl of file 'sample2.dat' (70) indicates 30 extra blanks (trim!) %B We determine Yp and dY/dZ independently for two different samples. The HeBCD sample is composed of 93 different observations of 86 HII regions in 77 galaxies. This sample is essentially the same as the one described in Izotov &amp; Thuan (2004, Cat. &lt;J/ApJ/602/200&gt;), except that two close pairs of HII regions in the spiral galaxy M1011 have been added. These four HII regions were observed with the 6.5m MMT on the night of 2004 February 20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15#sample2</TD>
            <TD>2011-09-14T20:47:58Z</TD>
            <TD>#Abundances#Equivalent_widths#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Apr-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/662/15</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/662/15&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/662/15</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/291/261 [1]</TD>
            <TD>Methanol maser of IRAS-selected sources (Walsh+ 1997)</TD>
            <TD>A survey of ultracompact (UC) HII regions has been carried out by searching for 6.669-GHz methanol maser emission from a sample of 535 IRAS-selected candidates. A total of 201 candidates exhibit methanol emission. These sources have been used, in conjunction with previously identified UC HII regions, to provide a base for further studies of such regions. Estimates of distances have indicated that the identified UC HII regions tend to have some Galactic structure but it is not clear whether they lie in or between the spiral arms of the Galaxy. The regions are tightly constrained to the plane of the Galaxy. Comparison of identified regions and IRAS sources selected by Wood &amp; Churchwell indicates that there there is some degree of contamination, which could be due to an older phase in the life on an UC HII region where methanol maser emission is not apparent. Luminosities and spectral types have been derived for many of the regions. The maximum number of maser spots observed seems to increase with increasing peak maser luminosity, which indicates that the maser emission is more dependent on the abundance of methanol than the availability of far-infrared radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261#1</TD>
            <TD>2011-09-14T18:41:02Z</TD>
            <TD>#HII_regions#Masers#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/291/261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/291/261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/291/261 [2]</TD>
            <TD>Methanol maser of IRAS-selected sources (Walsh+ 1997)</TD>
            <TD>A survey of ultracompact (UC) HII regions has been carried out by searching for 6.669-GHz methanol maser emission from a sample of 535 IRAS-selected candidates. A total of 201 candidates exhibit methanol emission. These sources have been used, in conjunction with previously identified UC HII regions, to provide a base for further studies of such regions. Estimates of distances have indicated that the identified UC HII regions tend to have some Galactic structure but it is not clear whether they lie in or between the spiral arms of the Galaxy. The regions are tightly constrained to the plane of the Galaxy. Comparison of identified regions and IRAS sources selected by Wood &amp; Churchwell indicates that there there is some degree of contamination, which could be due to an older phase in the life on an UC HII region where methanol maser emission is not apparent. Luminosities and spectral types have been derived for many of the regions. The maximum number of maser spots observed seems to increase with increasing peak maser luminosity, which indicates that the maser emission is more dependent on the abundance of methanol than the availability of far-infrared radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261#2</TD>
            <TD>2011-09-14T18:41:02Z</TD>
            <TD>#HII_regions#Masers#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/291/261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/291/261</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/333/423 [1]</TD>
            <TD>Luminosity function of the Virgo Cluster (Trentham+, 2002)</TD>
            <TD>We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes M_B_=-22 and -11 from wide-field charge-coupled device (CCD) imaging data. The data used here were taken on various observing runs during Spring 1999 and Spring 2000 as part of the INT Wide Field Survey (WFS; http://www.ast.cam.ac.uk/wfcsur ; McMahon et al., 2001NewAR..45...97M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423#1</TD>
            <TD>2011-09-14T19:18:20Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/333/423</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/423</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/333/423 [2]</TD>
            <TD>Luminosity function of the Virgo Cluster (Trentham+, 2002)</TD>
            <TD>We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes M_B_=-22 and -11 from wide-field charge-coupled device (CCD) imaging data. The data used here were taken on various observing runs during Spring 1999 and Spring 2000 as part of the INT Wide Field Survey (WFS; http://www.ast.cam.ac.uk/wfcsur ; McMahon et al., 2001NewAR..45...97M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423#2</TD>
            <TD>2011-09-14T19:18:20Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/333/423&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/423</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/333/423 [table2]</TD>
            <TD>Luminosity function of the Virgo Cluster (Trentham+, 2002)</TD>
            <TD>We measure the galaxy luminosity function (LF) for the Virgo Cluster between blue magnitudes M_B_=-22 and -11 from wide-field charge-coupled device (CCD) imaging data. The data used here were taken on various observing runs during Spring 1999 and Spring 2000 as part of the INT Wide Field Survey (WFS; http://www.ast.cam.ac.uk/wfcsur ; McMahon et al., 2001NewAR..45...97M).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423#table2</TD>
            <TD>2011-09-14T19:18:20Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/333/423</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/333/423&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/333/423</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/76/83 [1]</TD>
            <TD>Galaxies in and near the cluster A1185 (Botashev+ 1999)</TD>
            <TD>Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are presented. Coordinates have been obtained for 115 galaxies that are either cluster members or field galaxies in the direction of A1185. Radio spectra for a number of galaxies in this cluster have been derived using observations on the RATAN-600 radio telescope at 2.7,3.9,7.6, and 31 cm, together with data published in other study. At the cluster center some of the galaxies have either flat or inverted spectra.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83#1</TD>
            <TD>2011-09-14T19:02:44Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/76/83</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/76/83</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/76/83 [2]</TD>
            <TD>Galaxies in and near the cluster A1185 (Botashev+ 1999)</TD>
            <TD>Results of optical, radio, and submillimeter studies of the nearby galaxy cluster A1185 are presented. Coordinates have been obtained for 115 galaxies that are either cluster members or field galaxies in the direction of A1185. Radio spectra for a number of galaxies in this cluster have been derived using observations on the RATAN-600 radio telescope at 2.7,3.9,7.6, and 31 cm, together with data published in other study. At the cluster center some of the galaxies have either flat or inverted spectra.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83#2</TD>
            <TD>2011-09-14T19:02:44Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jul-2000</TD>
            <TD>ivo://CDS.VizieR/J/AZh/76/83</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/76/83&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/76/83</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/195 [1]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1996)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 146 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: April 1, 1996</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/195#1</TD>
            <TD>2011-09-14T19:18:26Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/195</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/195</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/195 [2]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1996)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 146 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: April 1, 1996</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/195#2</TD>
            <TD>2011-09-14T19:18:26Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/195&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/195 [catalog]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1996)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 146 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: April 1, 1996</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/195#catalog</TD>
            <TD>2011-09-14T19:18:26Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/195</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/195&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/195</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/330/453 [1]</TD>
            <TD>Sagittarius Dwarf Galaxy VI photometry (Marconi+, 1998)</TD>
            <TD>We present V,I deep CCD photometry for three fields of the dwarf galaxy in Sagittarius (Sgr), located at l=5.6{deg}, b=-14.1{deg}. One of the fields is centered on the globular cluster NGC 6715 (M54), which lies in one of the dense clumps of the Sgr galaxy. Comparing the CMD of Sgr with those of globular clusters which are believed to be kinematically associated with the dwarf galaxy (Da Costa &amp; Armandroff, 1995AJ....109.2533D), we conclude that the stellar population of Sgr presents a spread in metallicity of -0.71&lt;=[Fe/H]&lt;=-1.58, and that the dominant population (=~10Gyr old) is extremely similar to the star content of the associated globular cluster Terzan 7. The estimated distance to Sgr is d=~24.55Kpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/453#1</TD>
            <TD>2011-09-14T19:04:22Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/453</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/330/453</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/330/453</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/330/453 [2]</TD>
            <TD>Sagittarius Dwarf Galaxy VI photometry (Marconi+, 1998)</TD>
            <TD>We present V,I deep CCD photometry for three fields of the dwarf galaxy in Sagittarius (Sgr), located at l=5.6{deg}, b=-14.1{deg}. One of the fields is centered on the globular cluster NGC 6715 (M54), which lies in one of the dense clumps of the Sgr galaxy. Comparing the CMD of Sgr with those of globular clusters which are believed to be kinematically associated with the dwarf galaxy (Da Costa &amp; Armandroff, 1995AJ....109.2533D), we conclude that the stellar population of Sgr presents a spread in metallicity of -0.71&lt;=[Fe/H]&lt;=-1.58, and that the dominant population (=~10Gyr old) is extremely similar to the star content of the associated globular cluster Terzan 7. The estimated distance to Sgr is d=~24.55Kpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/453#2</TD>
            <TD>2011-09-14T19:04:22Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/453</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/330/453&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/330/453</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/494 [1]</TD>
            <TD>NGC 5128 globular clusters UBVRICMT1 phot. &amp; RV (Woodley+, 2007)</TD>
            <TD>A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC 5128 is presented. From a spectroscopically confirmed sample of 340 globular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC 5128.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494#1</TD>
            <TD>2011-09-14T20:49:26Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/494</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/494</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/494 [2]</TD>
            <TD>NGC 5128 globular clusters UBVRICMT1 phot. &amp; RV (Woodley+, 2007)</TD>
            <TD>A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC 5128 is presented. From a spectroscopically confirmed sample of 340 globular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC 5128.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494#2</TD>
            <TD>2011-09-14T20:49:26Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/494&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/494</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/494 [table1]</TD>
            <TD>NGC 5128 globular clusters UBVRICMT1 phot. &amp; RV (Woodley+, 2007)</TD>
            <TD>A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC 5128 is presented. From a spectroscopically confirmed sample of 340 globular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC 5128.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494#table1</TD>
            <TD>2011-09-14T20:49:26Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/494&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/494</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/195 [1]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1996)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 146 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: April 1, 1996</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/195#1</TD>
            <TD>2011-09-14T19:18:26Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/195</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/195</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/195 [2]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1996)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 146 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: April 1, 1996</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/195#2</TD>
            <TD>2011-09-14T19:18:26Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/195&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/195 [catalog]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1996)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 146 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: April 1, 1996</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/195#catalog</TD>
            <TD>2011-09-14T19:18:26Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/195</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/195&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/195</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/330/453 [1]</TD>
            <TD>Sagittarius Dwarf Galaxy VI photometry (Marconi+, 1998)</TD>
            <TD>We present V,I deep CCD photometry for three fields of the dwarf galaxy in Sagittarius (Sgr), located at l=5.6{deg}, b=-14.1{deg}. One of the fields is centered on the globular cluster NGC 6715 (M54), which lies in one of the dense clumps of the Sgr galaxy. Comparing the CMD of Sgr with those of globular clusters which are believed to be kinematically associated with the dwarf galaxy (Da Costa &amp; Armandroff, 1995AJ....109.2533D), we conclude that the stellar population of Sgr presents a spread in metallicity of -0.71&lt;=[Fe/H]&lt;=-1.58, and that the dominant population (=~10Gyr old) is extremely similar to the star content of the associated globular cluster Terzan 7. The estimated distance to Sgr is d=~24.55Kpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/453#1</TD>
            <TD>2011-09-14T19:04:22Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/453</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/330/453</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/330/453</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/330/453 [2]</TD>
            <TD>Sagittarius Dwarf Galaxy VI photometry (Marconi+, 1998)</TD>
            <TD>We present V,I deep CCD photometry for three fields of the dwarf galaxy in Sagittarius (Sgr), located at l=5.6{deg}, b=-14.1{deg}. One of the fields is centered on the globular cluster NGC 6715 (M54), which lies in one of the dense clumps of the Sgr galaxy. Comparing the CMD of Sgr with those of globular clusters which are believed to be kinematically associated with the dwarf galaxy (Da Costa &amp; Armandroff, 1995AJ....109.2533D), we conclude that the stellar population of Sgr presents a spread in metallicity of -0.71&lt;=[Fe/H]&lt;=-1.58, and that the dominant population (=~10Gyr old) is extremely similar to the star content of the associated globular cluster Terzan 7. The estimated distance to Sgr is d=~24.55Kpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/453#2</TD>
            <TD>2011-09-14T19:04:22Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/330/453</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/330/453&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/330/453</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/494 [1]</TD>
            <TD>NGC 5128 globular clusters UBVRICMT1 phot. &amp; RV (Woodley+, 2007)</TD>
            <TD>A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC 5128 is presented. From a spectroscopically confirmed sample of 340 globular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC 5128.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494#1</TD>
            <TD>2011-09-14T20:49:26Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/494</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/494</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/494 [2]</TD>
            <TD>NGC 5128 globular clusters UBVRICMT1 phot. &amp; RV (Woodley+, 2007)</TD>
            <TD>A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC 5128 is presented. From a spectroscopically confirmed sample of 340 globular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC 5128.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494#2</TD>
            <TD>2011-09-14T20:49:26Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/494&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/494</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/494 [table1]</TD>
            <TD>NGC 5128 globular clusters UBVRICMT1 phot. &amp; RV (Woodley+, 2007)</TD>
            <TD>A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC 5128 is presented. From a spectroscopically confirmed sample of 340 globular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC 5128.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494#table1</TD>
            <TD>2011-09-14T20:49:26Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/494&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/494</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/195 [1]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1996)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 146 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: April 1, 1996</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/195#1</TD>
            <TD>2011-09-14T19:18:26Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/195</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/195</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/195 [2]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1996)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 146 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: April 1, 1996</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/195#2</TD>
            <TD>2011-09-14T19:18:26Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/195</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/195&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/195</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/195 [catalog]</TD>
            <TD>Globular Clusters in the Milky Way (Harris, 1996)</TD>
            <TD>This catalog compiled by William E. Harris contains basic parameters on distances, velocities, metallicities, luminosities, colors, and dynamical parameters for 146 objects regarded as globular clusters in the Milky Way galaxy. A complete list of source references is given in the companion file "sources". The original files are also accessible through WorldWideWeb, at URL http://www.physics.mcmaster.ca/Globular.html This version corresponds to revision: April 1, 1996</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/195#catalog</TD>
            <TD>2011-09-14T19:18:26Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/VII/195</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/195&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/195</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/90/2221 [1]</TD>
            <TD>UMi dwarf galaxy BV photometry (Olszewski+, 1985)</TD>
            <TD>We have constructed a color-magnitude diagram of the Ursa Minor dwarf spheroidal to m_V_=24.8mag from charged-coupled device (CCD) observations with the Kitt Peak 4 m telescope. The main-sequence turnoff is easily visible. Fits to evolutionary isochrones and the globular M92 indicate that Ursa Minor has an age and metal abundance very similar to that of the latter cluster. No evidence for stars younger than about 16 billion years is seen, with the possible exception of approximately 20 stars believed to be blue stragglers. Ursa Minor is therefore an extreme-age galaxy, unlike superficially similar objects such as the Carina dwarf. Indeed, Ursa Minor may be the only outer-halo spheroidal whose stellar content lives up to the classical ideals of a Population II system. A distance modulus of (m-M)_0_=19.0mag is derived from a sliding fit to the M92 ridge lines. However, this modulus is uncertain by ~0.1mag, for the horizontal branch in our color-magnitude diagram is poorly populated. The ratio of blue stragglers to anomalous Cepheids in Ursa Minor is estimated to be ~100, a number that may provide an important constraint on binary models for the origin of these stars. A surprising result of our study is the discovery of clumpiness in the distribution of stars. This finding may give more weight to the idea that dwarf spheroidal galaxies were previously dwarf irregular galaxies, although clearly, if so, Ursa Minor must have lost its gaseous content very soon after formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/2221#1</TD>
            <TD>2011-09-14T19:04:36Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/2221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/90/2221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/2221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/90/2221 [2]</TD>
            <TD>UMi dwarf galaxy BV photometry (Olszewski+, 1985)</TD>
            <TD>We have constructed a color-magnitude diagram of the Ursa Minor dwarf spheroidal to m_V_=24.8mag from charged-coupled device (CCD) observations with the Kitt Peak 4 m telescope. The main-sequence turnoff is easily visible. Fits to evolutionary isochrones and the globular M92 indicate that Ursa Minor has an age and metal abundance very similar to that of the latter cluster. No evidence for stars younger than about 16 billion years is seen, with the possible exception of approximately 20 stars believed to be blue stragglers. Ursa Minor is therefore an extreme-age galaxy, unlike superficially similar objects such as the Carina dwarf. Indeed, Ursa Minor may be the only outer-halo spheroidal whose stellar content lives up to the classical ideals of a Population II system. A distance modulus of (m-M)_0_=19.0mag is derived from a sliding fit to the M92 ridge lines. However, this modulus is uncertain by ~0.1mag, for the horizontal branch in our color-magnitude diagram is poorly populated. The ratio of blue stragglers to anomalous Cepheids in Ursa Minor is estimated to be ~100, a number that may provide an important constraint on binary models for the origin of these stars. A surprising result of our study is the discovery of clumpiness in the distribution of stars. This finding may give more weight to the idea that dwarf spheroidal galaxies were previously dwarf irregular galaxies, although clearly, if so, Ursa Minor must have lost its gaseous content very soon after formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/2221#2</TD>
            <TD>2011-09-14T19:04:36Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/2221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/90/2221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/2221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/134/494 [1]</TD>
            <TD>NGC 5128 globular clusters UBVRICMT1 phot. &amp; RV (Woodley+, 2007)</TD>
            <TD>A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC 5128 is presented. From a spectroscopically confirmed sample of 340 globular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC 5128.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494#1</TD>
            <TD>2011-09-14T20:49:26Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/134/494</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/494</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/134/494 [2]</TD>
            <TD>NGC 5128 globular clusters UBVRICMT1 phot. &amp; RV (Woodley+, 2007)</TD>
            <TD>A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC 5128 is presented. From a spectroscopically confirmed sample of 340 globular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC 5128.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494#2</TD>
            <TD>2011-09-14T20:49:26Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/134/494&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/494</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/134/494 [table1]</TD>
            <TD>NGC 5128 globular clusters UBVRICMT1 phot. &amp; RV (Woodley+, 2007)</TD>
            <TD>A new kinematic and dynamic study of the halo of the giant elliptical galaxy NGC 5128 is presented. From a spectroscopically confirmed sample of 340 globular clusters and 780 planetary nebulae, the rotation amplitude, rotation axis, velocity dispersion, and total dynamical mass are determined for the halo of NGC 5128.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494#table1</TD>
            <TD>2011-09-14T20:49:26Z</TD>
            <TD>#Globular_Clusters#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/134/494</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/134/494&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/134/494</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/123 [1]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#1</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/123</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/123 [2]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#2</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/123&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/123 [table2]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#table2</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/123 [table1]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#table1</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/90/2221 [1]</TD>
            <TD>UMi dwarf galaxy BV photometry (Olszewski+, 1985)</TD>
            <TD>We have constructed a color-magnitude diagram of the Ursa Minor dwarf spheroidal to m_V_=24.8mag from charged-coupled device (CCD) observations with the Kitt Peak 4 m telescope. The main-sequence turnoff is easily visible. Fits to evolutionary isochrones and the globular M92 indicate that Ursa Minor has an age and metal abundance very similar to that of the latter cluster. No evidence for stars younger than about 16 billion years is seen, with the possible exception of approximately 20 stars believed to be blue stragglers. Ursa Minor is therefore an extreme-age galaxy, unlike superficially similar objects such as the Carina dwarf. Indeed, Ursa Minor may be the only outer-halo spheroidal whose stellar content lives up to the classical ideals of a Population II system. A distance modulus of (m-M)_0_=19.0mag is derived from a sliding fit to the M92 ridge lines. However, this modulus is uncertain by ~0.1mag, for the horizontal branch in our color-magnitude diagram is poorly populated. The ratio of blue stragglers to anomalous Cepheids in Ursa Minor is estimated to be ~100, a number that may provide an important constraint on binary models for the origin of these stars. A surprising result of our study is the discovery of clumpiness in the distribution of stars. This finding may give more weight to the idea that dwarf spheroidal galaxies were previously dwarf irregular galaxies, although clearly, if so, Ursa Minor must have lost its gaseous content very soon after formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/2221#1</TD>
            <TD>2011-09-14T19:04:36Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/2221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/90/2221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/2221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/90/2221 [2]</TD>
            <TD>UMi dwarf galaxy BV photometry (Olszewski+, 1985)</TD>
            <TD>We have constructed a color-magnitude diagram of the Ursa Minor dwarf spheroidal to m_V_=24.8mag from charged-coupled device (CCD) observations with the Kitt Peak 4 m telescope. The main-sequence turnoff is easily visible. Fits to evolutionary isochrones and the globular M92 indicate that Ursa Minor has an age and metal abundance very similar to that of the latter cluster. No evidence for stars younger than about 16 billion years is seen, with the possible exception of approximately 20 stars believed to be blue stragglers. Ursa Minor is therefore an extreme-age galaxy, unlike superficially similar objects such as the Carina dwarf. Indeed, Ursa Minor may be the only outer-halo spheroidal whose stellar content lives up to the classical ideals of a Population II system. A distance modulus of (m-M)_0_=19.0mag is derived from a sliding fit to the M92 ridge lines. However, this modulus is uncertain by ~0.1mag, for the horizontal branch in our color-magnitude diagram is poorly populated. The ratio of blue stragglers to anomalous Cepheids in Ursa Minor is estimated to be ~100, a number that may provide an important constraint on binary models for the origin of these stars. A surprising result of our study is the discovery of clumpiness in the distribution of stars. This finding may give more weight to the idea that dwarf spheroidal galaxies were previously dwarf irregular galaxies, although clearly, if so, Ursa Minor must have lost its gaseous content very soon after formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/2221#2</TD>
            <TD>2011-09-14T19:04:36Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/90/2221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/90/2221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/90/2221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/168 [1]</TD>
            <TD>Kinematics of red giant and RR Lyrae stars (Chiba+ 1998)</TD>
            <TD>++++Lrecl of file 'table1.dat' (127) indicates 2 extra blanks (trim!) %B The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]&lt;=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]&lt;=-1.6, is characterized by a lack of systemic rotation [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e&lt;0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]&lt;=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6&lt;[Fe/H]&lt;=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|&lt;1kpc. This disk component appears to constitute only 10% for -1.6&lt;[Fe/H]&lt;=-1 and 20% for -1.4&lt;[Fe/H]&lt;=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168#1</TD>
            <TD>2011-09-14T20:53:06Z</TD>
            <TD>#Stars#Proper_Motions#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/168</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/168</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/168 [2]</TD>
            <TD>Kinematics of red giant and RR Lyrae stars (Chiba+ 1998)</TD>
            <TD>++++Lrecl of file 'table1.dat' (127) indicates 2 extra blanks (trim!) %B The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]&lt;=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]&lt;=-1.6, is characterized by a lack of systemic rotation [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e&lt;0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]&lt;=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6&lt;[Fe/H]&lt;=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|&lt;1kpc. This disk component appears to constitute only 10% for -1.6&lt;[Fe/H]&lt;=-1 and 20% for -1.4&lt;[Fe/H]&lt;=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168#2</TD>
            <TD>2011-09-14T20:53:06Z</TD>
            <TD>#Stars#Proper_Motions#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/168&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/168</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/168 [table1]</TD>
            <TD>Kinematics of red giant and RR Lyrae stars (Chiba+ 1998)</TD>
            <TD>++++Lrecl of file 'table1.dat' (127) indicates 2 extra blanks (trim!) %B The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]&lt;=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]&lt;=-1.6, is characterized by a lack of systemic rotation [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e&lt;0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]&lt;=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6&lt;[Fe/H]&lt;=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|&lt;1kpc. This disk component appears to constitute only 10% for -1.6&lt;[Fe/H]&lt;=-1 and 20% for -1.4&lt;[Fe/H]&lt;=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168#table1</TD>
            <TD>2011-09-14T20:53:06Z</TD>
            <TD>#Stars#Proper_Motions#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/168&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/168</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/113 [1]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#1</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/113 [2]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#2</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/113 [table5]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#table5</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/113 [table4]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#table4</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/113 [table3]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#table3</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/123 [1]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#1</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/123</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/123 [2]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#2</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/123&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/123 [table2]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#table2</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/123 [table1]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#table1</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/168 [1]</TD>
            <TD>Kinematics of red giant and RR Lyrae stars (Chiba+ 1998)</TD>
            <TD>++++Lrecl of file 'table1.dat' (127) indicates 2 extra blanks (trim!) %B The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]&lt;=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]&lt;=-1.6, is characterized by a lack of systemic rotation [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e&lt;0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]&lt;=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6&lt;[Fe/H]&lt;=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|&lt;1kpc. This disk component appears to constitute only 10% for -1.6&lt;[Fe/H]&lt;=-1 and 20% for -1.4&lt;[Fe/H]&lt;=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168#1</TD>
            <TD>2011-09-14T20:53:06Z</TD>
            <TD>#Stars#Proper_Motions#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/168</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/168</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/168 [2]</TD>
            <TD>Kinematics of red giant and RR Lyrae stars (Chiba+ 1998)</TD>
            <TD>++++Lrecl of file 'table1.dat' (127) indicates 2 extra blanks (trim!) %B The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]&lt;=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]&lt;=-1.6, is characterized by a lack of systemic rotation [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e&lt;0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]&lt;=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6&lt;[Fe/H]&lt;=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|&lt;1kpc. This disk component appears to constitute only 10% for -1.6&lt;[Fe/H]&lt;=-1 and 20% for -1.4&lt;[Fe/H]&lt;=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168#2</TD>
            <TD>2011-09-14T20:53:06Z</TD>
            <TD>#Stars#Proper_Motions#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/168&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/168</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/168 [table1]</TD>
            <TD>Kinematics of red giant and RR Lyrae stars (Chiba+ 1998)</TD>
            <TD>++++Lrecl of file 'table1.dat' (127) indicates 2 extra blanks (trim!) %B The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]&lt;=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]&lt;=-1.6, is characterized by a lack of systemic rotation [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e&lt;0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]&lt;=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6&lt;[Fe/H]&lt;=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|&lt;1kpc. This disk component appears to constitute only 10% for -1.6&lt;[Fe/H]&lt;=-1 and 20% for -1.4&lt;[Fe/H]&lt;=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168#table1</TD>
            <TD>2011-09-14T20:53:06Z</TD>
            <TD>#Stars#Proper_Motions#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/168&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/168</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/113 [1]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#1</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/113 [2]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#2</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/113 [table5]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#table5</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/113 [table4]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#table4</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/113 [table3]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#table3</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/123 [1]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#1</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/123</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/123 [2]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#2</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/123&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/123 [table2]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#table2</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/123 [table1]</TD>
            <TD>Galaxies behind Southern Milky Way (Kraan-Korteweg 2000)</TD>
            <TD>A deep optical galaxy search in the southern Milky Way - aimed at reducing the width of the Zone of Avoidance - revealed 3279 galaxy candidates on the IIIaJ film copies of the ESO/SRC survey above the diameter limit of D greater than approximately 0.2 arcmin. Only 112 (3.4%) were previously catalogued. The surveyed region (266&lt;l&lt;296 and -10&lt;b&lt;+8) lies in the extension of the Hydra and Antlia clusters. Optical properties of the unveiled galaxies such as positions, diameters, magnitudes, morphological types are given in Table 1. Cross-identifications with the IRAS PSC (Cat. &lt;II/125&gt;) are given in Table 2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123#table1</TD>
            <TD>2011-09-14T19:18:41Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/123</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/113 [1]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#1</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/113</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/113 [2]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#2</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/113 [table5]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#table5</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/113 [table4]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#table4</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/113 [table3]</TD>
            <TD>Coma extensive H photometry (Andreon+, 2000)</TD>
            <TD>We present extensive and accurate photometry in the near-infrared H band (about 1.62{mu}m) of a complete sample of objects in an area of about 400arcmin^2^ toward the Coma cluster of galaxies. The sample, including about 300 objects, is complete down to H~17mag, the exact value depending on the type of magnitude (isophotal, aperture, Kron) and the particular region studied. This is six magnitudes below the characteristic magnitude of galaxies, well into the dwarfs' regime at the distance of the Coma cluster. For each object (star or galaxy) we provide aperture magnitudes computed within five different apertures, the magnitude within the 22mag/arcsec^2^ isophote, the Kron magnitude and radius, magnitude errors, as well as the coordinates, the isophotal area, and a stellarity index. Photometric errors are 0.2mag at the completness limit. This sample is meant to be the zero-redshift reference for evolutionary studies of galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113#table3</TD>
            <TD>2011-09-14T19:04:52Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/113</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/113&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/113</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/168 [1]</TD>
            <TD>Kinematics of red giant and RR Lyrae stars (Chiba+ 1998)</TD>
            <TD>++++Lrecl of file 'table1.dat' (127) indicates 2 extra blanks (trim!) %B The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]&lt;=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]&lt;=-1.6, is characterized by a lack of systemic rotation [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e&lt;0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]&lt;=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6&lt;[Fe/H]&lt;=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|&lt;1kpc. This disk component appears to constitute only 10% for -1.6&lt;[Fe/H]&lt;=-1 and 20% for -1.4&lt;[Fe/H]&lt;=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168#1</TD>
            <TD>2011-09-14T20:53:06Z</TD>
            <TD>#Stars#Proper_Motions#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/168</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/168</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/168 [2]</TD>
            <TD>Kinematics of red giant and RR Lyrae stars (Chiba+ 1998)</TD>
            <TD>++++Lrecl of file 'table1.dat' (127) indicates 2 extra blanks (trim!) %B The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]&lt;=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]&lt;=-1.6, is characterized by a lack of systemic rotation [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e&lt;0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]&lt;=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6&lt;[Fe/H]&lt;=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|&lt;1kpc. This disk component appears to constitute only 10% for -1.6&lt;[Fe/H]&lt;=-1 and 20% for -1.4&lt;[Fe/H]&lt;=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168#2</TD>
            <TD>2011-09-14T20:53:06Z</TD>
            <TD>#Stars#Proper_Motions#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/168&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/168</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/168 [table1]</TD>
            <TD>Kinematics of red giant and RR Lyrae stars (Chiba+ 1998)</TD>
            <TD>++++Lrecl of file 'table1.dat' (127) indicates 2 extra blanks (trim!) %B The kinematics of 122 red giant and 124 RR Lyrae stars in the solar neighborhood are studied using accurate measurements of their proper motions obtained by the Hipparcos astrometry satellite, combined with their published photometric distances, metal abundances, and radial velocities. A majority of these sample stars have metal abundances of [Fe/H]&lt;=-1 and thus represent the old stellar populations in the Galaxy. The halo component, with [Fe/H]&lt;=-1.6, is characterized by a lack of systemic rotation [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(16+/-18, -217+/-21, -10+/-12)km/s] and a radially elongated velocity ellipsoid [(&lt;U&gt;, &lt;V&gt;, &lt;W&gt;)=(161+/-10, 115+/-7, 108+/-7)km/s]. About 16% of such metal-poor stars have low orbital eccentricities (e&lt;0.4), and we see no evidence of a correlation between [Fe/H] and e. Based on the model for the e-distribution of orbits, we show that this fraction of low-e stars for [Fe/H]&lt;=-1.6 is explained by the halo component alone, without introducing the extra disk component claimed by recent workers. This is also supported by the absence of a significant change in the e-distribution with height from the Galactic plane. In the intermediate-metallicity range (-1.6&lt;[Fe/H]&lt;=-1), we find that stars with disklike kinematics have only modest effects on the distributions of rotational velocities and e for the sample at |z|&lt;1kpc. This disk component appears to constitute only 10% for -1.6&lt;[Fe/H]&lt;=-1 and 20% for -1.4&lt;[Fe/H]&lt;=-1. It is also verified that this metal-weak disk has a mean rotation of ~195km/s and a vertical extent of 1 kpc, which is consistent with the thick disk's dominating at [Fe/H]=-0.6 to -1. We find no metallicity gradient in the halo, whereas there is an indication of a metallicity gradient in the metal-weak tail of the thick disk. The implications of these results for the early evolution of the Galaxy are also presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168#table1</TD>
            <TD>2011-09-14T20:53:06Z</TD>
            <TD>#Stars#Proper_Motions#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/168</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/168&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/168</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/392/395 [1]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#1</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/392/395</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/392/395 [2]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#2</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/392/395&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/395 [cdfsk]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#cdfsk</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/395&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/395 [0055k]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#0055k</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/395&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/347 [1]</TD>
            <TD>BVRI photometry of NGC 6789 (Drozdovsky+, 2000)</TD>
            <TD>Results of the DAOPHOT/ALLSTAR photometry of the resolved stars in the nearby blue compact dwarf galaxy NGC 6789. Based on observations made with the 2.5m Nordic (La Palma, Spain) telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/347#1</TD>
            <TD>2011-09-14T19:05:45Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/347 [2]</TD>
            <TD>BVRI photometry of NGC 6789 (Drozdovsky+, 2000)</TD>
            <TD>Results of the DAOPHOT/ALLSTAR photometry of the resolved stars in the nearby blue compact dwarf galaxy NGC 6789. Based on observations made with the 2.5m Nordic (La Palma, Spain) telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/347#2</TD>
            <TD>2011-09-14T19:05:45Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/347</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/179/306 [1]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#1</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/179/306</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/179/306 [2]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#2</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/179/306&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/179/306 [table2]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#table2</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/179/306&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/179/306 [table5]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#table5</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/179/306&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/392/395 [1]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#1</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/392/395</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/392/395 [2]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#2</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/392/395&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/395 [cdfsk]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#cdfsk</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/395&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/395 [0055k]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#0055k</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/395&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/142/347 [1]</TD>
            <TD>BVRI photometry of NGC 6789 (Drozdovsky+, 2000)</TD>
            <TD>Results of the DAOPHOT/ALLSTAR photometry of the resolved stars in the nearby blue compact dwarf galaxy NGC 6789. Based on observations made with the 2.5m Nordic (La Palma, Spain) telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/347#1</TD>
            <TD>2011-09-14T19:05:45Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/142/347</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/347</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/142/347 [2]</TD>
            <TD>BVRI photometry of NGC 6789 (Drozdovsky+, 2000)</TD>
            <TD>Results of the DAOPHOT/ALLSTAR photometry of the resolved stars in the nearby blue compact dwarf galaxy NGC 6789. Based on observations made with the 2.5m Nordic (La Palma, Spain) telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/347#2</TD>
            <TD>2011-09-14T19:05:45Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/142/347</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/142/347&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/142/347</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/369/57 [1]</TD>
            <TD>Monitoring Mkn 279 in BVRI and H{beta} fluxes (Santos-Lleo+, 2001)</TD>
            <TD>Mid-infrared images of the Seyfert 1 galaxy Mrk 279 obtained with the ISO satellite are presented together with the results of a one-year monitoring campaign of the 2.5-11.7{mu}m spectrum. Contemporaneous optical photometric and spectrophotometric observations are also presented. The galaxy appears as a point-like source at the resolution of the ISOCAM instrument (4-5"). The 2.5-11.7{mu}m average spectrum of the nucleus in Mrk 279 shows a strong power law continuum with {alpha}=-0.80+/-0.05 (F_{nu}_{prop.to}{nu}^{alpha}^) and weak PAH emission features. The Mrk 279 spectral energy distribution shows a mid-IR bump, which extends from 2 to 15-20{mu}m. The mid-IR bump is consistent with thermal emission from dust grains at a distance of &gt;100 light-days. No significant variations of the mid-IR flux have been detected during our observing campaign, consistent with the relatively low amplitude (~10% rms) of the optical variability during the campaign. The time delay for H{beta} line emission in response to the optical continuum variations is {tau}=16.7^+5.3^_-5.6_days, consistent with previous measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/369/57#1</TD>
            <TD>2011-09-14T19:07:30Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/369/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/369/57</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/369/57</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/369/57 [2]</TD>
            <TD>Monitoring Mkn 279 in BVRI and H{beta} fluxes (Santos-Lleo+, 2001)</TD>
            <TD>Mid-infrared images of the Seyfert 1 galaxy Mrk 279 obtained with the ISO satellite are presented together with the results of a one-year monitoring campaign of the 2.5-11.7{mu}m spectrum. Contemporaneous optical photometric and spectrophotometric observations are also presented. The galaxy appears as a point-like source at the resolution of the ISOCAM instrument (4-5"). The 2.5-11.7{mu}m average spectrum of the nucleus in Mrk 279 shows a strong power law continuum with {alpha}=-0.80+/-0.05 (F_{nu}_{prop.to}{nu}^{alpha}^) and weak PAH emission features. The Mrk 279 spectral energy distribution shows a mid-IR bump, which extends from 2 to 15-20{mu}m. The mid-IR bump is consistent with thermal emission from dust grains at a distance of &gt;100 light-days. No significant variations of the mid-IR flux have been detected during our observing campaign, consistent with the relatively low amplitude (~10% rms) of the optical variability during the campaign. The time delay for H{beta} line emission in response to the optical continuum variations is {tau}=16.7^+5.3^_-5.6_days, consistent with previous measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/369/57#2</TD>
            <TD>2011-09-14T19:07:30Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/369/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/369/57&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/369/57</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/392/395 [1]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#1</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/392/395</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/392/395 [2]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#2</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/392/395&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/395 [cdfsk]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#cdfsk</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/395&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/395 [0055k]</TD>
            <TD>Ks-band magnitudes of the K20 sample (Cimatti+, 2002)</TD>
            <TD>Ks-band "total" magnitudes of the K20 sample galaxies. For each galaxy, the ID name, equatorial coordinates (J2000), total magnitudes and magnitude errors (1{sigma}) are given. A magnitude error equal to 0.30 magnitudes means that the object was deblended. The magnitudes are not corrected for Galactic extinction. According to the maps of Schlegel et al. (1998ApJ...500..525S), the extinction are A_K_=0.007mag and A_K_=0.003mag in the 0055-269 and in the CDFS fields respectively. The coordinates given in these tables were obtained by applying rigid offsets using USNO stars present in the fields, but no corrections for distorsions were applied because of the small number of suitable stars in each field. Thus, the precision of such coordinates is about +/-0.4" both in RA and in Dec, yielding a total uncertainty in the position of about 0.6" (1{sigma}).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395#0055k</TD>
            <TD>2011-09-14T19:19:06Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/395</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/395&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/395</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/179/306 [1]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#1</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/179/306</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/179/306 [2]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#2</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/179/306&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/179/306 [table2]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#table2</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/179/306&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/179/306 [table5]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#table5</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/179/306&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/369/57 [1]</TD>
            <TD>Monitoring Mkn 279 in BVRI and H{beta} fluxes (Santos-Lleo+, 2001)</TD>
            <TD>Mid-infrared images of the Seyfert 1 galaxy Mrk 279 obtained with the ISO satellite are presented together with the results of a one-year monitoring campaign of the 2.5-11.7{mu}m spectrum. Contemporaneous optical photometric and spectrophotometric observations are also presented. The galaxy appears as a point-like source at the resolution of the ISOCAM instrument (4-5"). The 2.5-11.7{mu}m average spectrum of the nucleus in Mrk 279 shows a strong power law continuum with {alpha}=-0.80+/-0.05 (F_{nu}_{prop.to}{nu}^{alpha}^) and weak PAH emission features. The Mrk 279 spectral energy distribution shows a mid-IR bump, which extends from 2 to 15-20{mu}m. The mid-IR bump is consistent with thermal emission from dust grains at a distance of &gt;100 light-days. No significant variations of the mid-IR flux have been detected during our observing campaign, consistent with the relatively low amplitude (~10% rms) of the optical variability during the campaign. The time delay for H{beta} line emission in response to the optical continuum variations is {tau}=16.7^+5.3^_-5.6_days, consistent with previous measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/369/57#1</TD>
            <TD>2011-09-14T19:07:30Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/369/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/369/57</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/369/57</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/369/57 [2]</TD>
            <TD>Monitoring Mkn 279 in BVRI and H{beta} fluxes (Santos-Lleo+, 2001)</TD>
            <TD>Mid-infrared images of the Seyfert 1 galaxy Mrk 279 obtained with the ISO satellite are presented together with the results of a one-year monitoring campaign of the 2.5-11.7{mu}m spectrum. Contemporaneous optical photometric and spectrophotometric observations are also presented. The galaxy appears as a point-like source at the resolution of the ISOCAM instrument (4-5"). The 2.5-11.7{mu}m average spectrum of the nucleus in Mrk 279 shows a strong power law continuum with {alpha}=-0.80+/-0.05 (F_{nu}_{prop.to}{nu}^{alpha}^) and weak PAH emission features. The Mrk 279 spectral energy distribution shows a mid-IR bump, which extends from 2 to 15-20{mu}m. The mid-IR bump is consistent with thermal emission from dust grains at a distance of &gt;100 light-days. No significant variations of the mid-IR flux have been detected during our observing campaign, consistent with the relatively low amplitude (~10% rms) of the optical variability during the campaign. The time delay for H{beta} line emission in response to the optical continuum variations is {tau}=16.7^+5.3^_-5.6_days, consistent with previous measurements.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/369/57#2</TD>
            <TD>2011-09-14T19:07:30Z</TD>
            <TD>#Seyfert_Galaxies#Spectroscopy#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/369/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/369/57&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/369/57</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/338/508 [1]</TD>
            <TD>Photometry+spectroscopy of UCM galaxies (Perez-Gonzalez+, 2003)</TD>
            <TD>Photometric and spectroscopic parameters for 191 galaxies in the UCM Survey of emission-line galaxies Lists I and II (Cats. &lt;J/ApJS/95/387&gt; and &lt;J/ApJS/105/343&gt;). For each galaxy, the table gives: redshift, BrJKs magnitudes and errors inside 3 disk-scale circular apertures (measured in r), H{alpha} equivalent widths and errors, aperture sizes in kpc, H{alpha}/H{beta} ratio (corrected for stellar absorption), Galactic extinction, morphological type, spectroscopic type, and absolute Ks-band magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508#1</TD>
            <TD>2011-09-14T19:19:17Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/338/508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/338/508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/338/508 [2]</TD>
            <TD>Photometry+spectroscopy of UCM galaxies (Perez-Gonzalez+, 2003)</TD>
            <TD>Photometric and spectroscopic parameters for 191 galaxies in the UCM Survey of emission-line galaxies Lists I and II (Cats. &lt;J/ApJS/95/387&gt; and &lt;J/ApJS/105/343&gt;). For each galaxy, the table gives: redshift, BrJKs magnitudes and errors inside 3 disk-scale circular apertures (measured in r), H{alpha} equivalent widths and errors, aperture sizes in kpc, H{alpha}/H{beta} ratio (corrected for stellar absorption), Galactic extinction, morphological type, spectroscopic type, and absolute Ks-band magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508#2</TD>
            <TD>2011-09-14T19:19:17Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/338/508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/338/508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/338/508 [table2]</TD>
            <TD>Photometry+spectroscopy of UCM galaxies (Perez-Gonzalez+, 2003)</TD>
            <TD>Photometric and spectroscopic parameters for 191 galaxies in the UCM Survey of emission-line galaxies Lists I and II (Cats. &lt;J/ApJS/95/387&gt; and &lt;J/ApJS/105/343&gt;). For each galaxy, the table gives: redshift, BrJKs magnitudes and errors inside 3 disk-scale circular apertures (measured in r), H{alpha} equivalent widths and errors, aperture sizes in kpc, H{alpha}/H{beta} ratio (corrected for stellar absorption), Galactic extinction, morphological type, spectroscopic type, and absolute Ks-band magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508#table2</TD>
            <TD>2011-09-14T19:19:17Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/338/508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/338/508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/179/306 [1]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#1</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/179/306</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/179/306 [2]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#2</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/179/306&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/179/306 [table2]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#table2</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/179/306&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/179/306 [table5]</TD>
            <TD>Radio galaxy morphologies (Russell+, 2008)</TD>
            <TD>We begin by correlating the positions from the FIRST catalog with the HST WFPC2 Archive. We excise 300x300 pixel "postage stamp" images from the astrometrically corrected and stacked WFPC2 mosaics centered on each FIRST source position.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306#table5</TD>
            <TD>2011-09-14T20:53:27Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/179/306</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/179/306&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/179/306</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/338/508 [1]</TD>
            <TD>Photometry+spectroscopy of UCM galaxies (Perez-Gonzalez+, 2003)</TD>
            <TD>Photometric and spectroscopic parameters for 191 galaxies in the UCM Survey of emission-line galaxies Lists I and II (Cats. &lt;J/ApJS/95/387&gt; and &lt;J/ApJS/105/343&gt;). For each galaxy, the table gives: redshift, BrJKs magnitudes and errors inside 3 disk-scale circular apertures (measured in r), H{alpha} equivalent widths and errors, aperture sizes in kpc, H{alpha}/H{beta} ratio (corrected for stellar absorption), Galactic extinction, morphological type, spectroscopic type, and absolute Ks-band magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508#1</TD>
            <TD>2011-09-14T19:19:17Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/338/508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/338/508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/338/508 [2]</TD>
            <TD>Photometry+spectroscopy of UCM galaxies (Perez-Gonzalez+, 2003)</TD>
            <TD>Photometric and spectroscopic parameters for 191 galaxies in the UCM Survey of emission-line galaxies Lists I and II (Cats. &lt;J/ApJS/95/387&gt; and &lt;J/ApJS/105/343&gt;). For each galaxy, the table gives: redshift, BrJKs magnitudes and errors inside 3 disk-scale circular apertures (measured in r), H{alpha} equivalent widths and errors, aperture sizes in kpc, H{alpha}/H{beta} ratio (corrected for stellar absorption), Galactic extinction, morphological type, spectroscopic type, and absolute Ks-band magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508#2</TD>
            <TD>2011-09-14T19:19:17Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/338/508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/338/508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/338/508 [table2]</TD>
            <TD>Photometry+spectroscopy of UCM galaxies (Perez-Gonzalez+, 2003)</TD>
            <TD>Photometric and spectroscopic parameters for 191 galaxies in the UCM Survey of emission-line galaxies Lists I and II (Cats. &lt;J/ApJS/95/387&gt; and &lt;J/ApJS/105/343&gt;). For each galaxy, the table gives: redshift, BrJKs magnitudes and errors inside 3 disk-scale circular apertures (measured in r), H{alpha} equivalent widths and errors, aperture sizes in kpc, H{alpha}/H{beta} ratio (corrected for stellar absorption), Galactic extinction, morphological type, spectroscopic type, and absolute Ks-band magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508#table2</TD>
            <TD>2011-09-14T19:19:17Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/338/508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/338/508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/669/959 [1]</TD>
            <TD>Warm molecular hydrogen in SINGS galaxy sample (Roussel+, 2007)</TD>
            <TD>The SINGS sample (Kennicutt et al., 2003PASP..115..928K), comprising 75 galaxies, is intended to be a valuable representative set of local galaxies that are not ultraluminous, and whose moderate distances ensure that the properties of the interstellar medium can be studied at relatively small spatial scales (a few hundreds of parsecs at the shortest wavelengths). To estimate flux densities of the dust continuum and of the aromatic bands (also referred to as the emission from PAHs, or polycyclic aromatic hydrocarbons), we used images in the 3.6 and 7.9um bands of the IRAC camera and scan maps in the three bands of the MIPS instrument at effective wavelengths of 24, 71, and 156um. The targets were observed in mapping mode with the IRS instrument, at low spectral resolution between 5 and 38um, with the SL and LL slits (resolution ~60-130), and at high spectral resolution between 10 and 37um, with the SH and LH slits (rsolution ~600).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959#1</TD>
            <TD>2011-09-14T20:54:33Z</TD>
            <TD>#Galaxies#Interstellar_Medium#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/669/959</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/669/959</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/669/959 [2]</TD>
            <TD>Warm molecular hydrogen in SINGS galaxy sample (Roussel+, 2007)</TD>
            <TD>The SINGS sample (Kennicutt et al., 2003PASP..115..928K), comprising 75 galaxies, is intended to be a valuable representative set of local galaxies that are not ultraluminous, and whose moderate distances ensure that the properties of the interstellar medium can be studied at relatively small spatial scales (a few hundreds of parsecs at the shortest wavelengths). To estimate flux densities of the dust continuum and of the aromatic bands (also referred to as the emission from PAHs, or polycyclic aromatic hydrocarbons), we used images in the 3.6 and 7.9um bands of the IRAC camera and scan maps in the three bands of the MIPS instrument at effective wavelengths of 24, 71, and 156um. The targets were observed in mapping mode with the IRS instrument, at low spectral resolution between 5 and 38um, with the SL and LL slits (resolution ~60-130), and at high spectral resolution between 10 and 37um, with the SH and LH slits (rsolution ~600).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959#2</TD>
            <TD>2011-09-14T20:54:33Z</TD>
            <TD>#Galaxies#Interstellar_Medium#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/669/959&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/669/959</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/669/959 [galaxies]</TD>
            <TD>Warm molecular hydrogen in SINGS galaxy sample (Roussel+, 2007)</TD>
            <TD>The SINGS sample (Kennicutt et al., 2003PASP..115..928K), comprising 75 galaxies, is intended to be a valuable representative set of local galaxies that are not ultraluminous, and whose moderate distances ensure that the properties of the interstellar medium can be studied at relatively small spatial scales (a few hundreds of parsecs at the shortest wavelengths). To estimate flux densities of the dust continuum and of the aromatic bands (also referred to as the emission from PAHs, or polycyclic aromatic hydrocarbons), we used images in the 3.6 and 7.9um bands of the IRAC camera and scan maps in the three bands of the MIPS instrument at effective wavelengths of 24, 71, and 156um. The targets were observed in mapping mode with the IRS instrument, at low spectral resolution between 5 and 38um, with the SL and LL slits (resolution ~60-130), and at high spectral resolution between 10 and 37um, with the SH and LH slits (rsolution ~600).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959#galaxies</TD>
            <TD>2011-09-14T20:54:33Z</TD>
            <TD>#Galaxies#Interstellar_Medium#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/669/959&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/669/959</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/338/508 [1]</TD>
            <TD>Photometry+spectroscopy of UCM galaxies (Perez-Gonzalez+, 2003)</TD>
            <TD>Photometric and spectroscopic parameters for 191 galaxies in the UCM Survey of emission-line galaxies Lists I and II (Cats. &lt;J/ApJS/95/387&gt; and &lt;J/ApJS/105/343&gt;). For each galaxy, the table gives: redshift, BrJKs magnitudes and errors inside 3 disk-scale circular apertures (measured in r), H{alpha} equivalent widths and errors, aperture sizes in kpc, H{alpha}/H{beta} ratio (corrected for stellar absorption), Galactic extinction, morphological type, spectroscopic type, and absolute Ks-band magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508#1</TD>
            <TD>2011-09-14T19:19:17Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/338/508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/338/508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/338/508 [2]</TD>
            <TD>Photometry+spectroscopy of UCM galaxies (Perez-Gonzalez+, 2003)</TD>
            <TD>Photometric and spectroscopic parameters for 191 galaxies in the UCM Survey of emission-line galaxies Lists I and II (Cats. &lt;J/ApJS/95/387&gt; and &lt;J/ApJS/105/343&gt;). For each galaxy, the table gives: redshift, BrJKs magnitudes and errors inside 3 disk-scale circular apertures (measured in r), H{alpha} equivalent widths and errors, aperture sizes in kpc, H{alpha}/H{beta} ratio (corrected for stellar absorption), Galactic extinction, morphological type, spectroscopic type, and absolute Ks-band magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508#2</TD>
            <TD>2011-09-14T19:19:17Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/338/508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/338/508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/338/508 [table2]</TD>
            <TD>Photometry+spectroscopy of UCM galaxies (Perez-Gonzalez+, 2003)</TD>
            <TD>Photometric and spectroscopic parameters for 191 galaxies in the UCM Survey of emission-line galaxies Lists I and II (Cats. &lt;J/ApJS/95/387&gt; and &lt;J/ApJS/105/343&gt;). For each galaxy, the table gives: redshift, BrJKs magnitudes and errors inside 3 disk-scale circular apertures (measured in r), H{alpha} equivalent widths and errors, aperture sizes in kpc, H{alpha}/H{beta} ratio (corrected for stellar absorption), Galactic extinction, morphological type, spectroscopic type, and absolute Ks-band magnitude.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508#table2</TD>
            <TD>2011-09-14T19:19:17Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/338/508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/338/508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/338/508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/400/877 [1]</TD>
            <TD>White dwarfs 3D kinematics from SPY project (Pauli+, 2003)</TD>
            <TD>We present kinematics of a sample of 107 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for a distinction of thin disk, thick disk, and halo populations. This is the first homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations such as the halo and the thick disk. Studies of white dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project are combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters are computed. We calculate individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership are deduced from a sample of F and G stars taken from the literature for which chemical criteria can be used to distinguish between thin disk, thick disk and halo. Candidates for thick disk and halo members are selected in a first step from the classical U-V-velocity diagram. Our final assignment of population membership is based on orbits and position in the J_z_-eccentricity diagram. We find four halo and twelve thick disk white dwarfs. We also present a systematic study of the effects of ignoring the radial velocity in kinematic investigations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877#1</TD>
            <TD>2011-09-14T19:20:20Z</TD>
            <TD>#Stars#Proper_Motions#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/400/877</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/877</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/400/877 [2]</TD>
            <TD>White dwarfs 3D kinematics from SPY project (Pauli+, 2003)</TD>
            <TD>We present kinematics of a sample of 107 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for a distinction of thin disk, thick disk, and halo populations. This is the first homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations such as the halo and the thick disk. Studies of white dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project are combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters are computed. We calculate individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership are deduced from a sample of F and G stars taken from the literature for which chemical criteria can be used to distinguish between thin disk, thick disk and halo. Candidates for thick disk and halo members are selected in a first step from the classical U-V-velocity diagram. Our final assignment of population membership is based on orbits and position in the J_z_-eccentricity diagram. We find four halo and twelve thick disk white dwarfs. We also present a systematic study of the effects of ignoring the radial velocity in kinematic investigations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877#2</TD>
            <TD>2011-09-14T19:20:20Z</TD>
            <TD>#Stars#Proper_Motions#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/400/877&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/877</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/400/877 [table1]</TD>
            <TD>White dwarfs 3D kinematics from SPY project (Pauli+, 2003)</TD>
            <TD>We present kinematics of a sample of 107 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for a distinction of thin disk, thick disk, and halo populations. This is the first homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations such as the halo and the thick disk. Studies of white dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project are combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters are computed. We calculate individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership are deduced from a sample of F and G stars taken from the literature for which chemical criteria can be used to distinguish between thin disk, thick disk and halo. Candidates for thick disk and halo members are selected in a first step from the classical U-V-velocity diagram. Our final assignment of population membership is based on orbits and position in the J_z_-eccentricity diagram. We find four halo and twelve thick disk white dwarfs. We also present a systematic study of the effects of ignoring the radial velocity in kinematic investigations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877#table1</TD>
            <TD>2011-09-14T19:20:20Z</TD>
            <TD>#Stars#Proper_Motions#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/400/877&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/877</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/400/877 [1]</TD>
            <TD>White dwarfs 3D kinematics from SPY project (Pauli+, 2003)</TD>
            <TD>We present kinematics of a sample of 107 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for a distinction of thin disk, thick disk, and halo populations. This is the first homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations such as the halo and the thick disk. Studies of white dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project are combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters are computed. We calculate individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership are deduced from a sample of F and G stars taken from the literature for which chemical criteria can be used to distinguish between thin disk, thick disk and halo. Candidates for thick disk and halo members are selected in a first step from the classical U-V-velocity diagram. Our final assignment of population membership is based on orbits and position in the J_z_-eccentricity diagram. We find four halo and twelve thick disk white dwarfs. We also present a systematic study of the effects of ignoring the radial velocity in kinematic investigations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877#1</TD>
            <TD>2011-09-14T19:20:20Z</TD>
            <TD>#Stars#Proper_Motions#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/400/877</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/877</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/400/877 [2]</TD>
            <TD>White dwarfs 3D kinematics from SPY project (Pauli+, 2003)</TD>
            <TD>We present kinematics of a sample of 107 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for a distinction of thin disk, thick disk, and halo populations. This is the first homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations such as the halo and the thick disk. Studies of white dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project are combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters are computed. We calculate individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership are deduced from a sample of F and G stars taken from the literature for which chemical criteria can be used to distinguish between thin disk, thick disk and halo. Candidates for thick disk and halo members are selected in a first step from the classical U-V-velocity diagram. Our final assignment of population membership is based on orbits and position in the J_z_-eccentricity diagram. We find four halo and twelve thick disk white dwarfs. We also present a systematic study of the effects of ignoring the radial velocity in kinematic investigations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877#2</TD>
            <TD>2011-09-14T19:20:20Z</TD>
            <TD>#Stars#Proper_Motions#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/400/877&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/877</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/400/877 [table1]</TD>
            <TD>White dwarfs 3D kinematics from SPY project (Pauli+, 2003)</TD>
            <TD>We present kinematics of a sample of 107 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for a distinction of thin disk, thick disk, and halo populations. This is the first homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations such as the halo and the thick disk. Studies of white dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project are combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters are computed. We calculate individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership are deduced from a sample of F and G stars taken from the literature for which chemical criteria can be used to distinguish between thin disk, thick disk and halo. Candidates for thick disk and halo members are selected in a first step from the classical U-V-velocity diagram. Our final assignment of population membership is based on orbits and position in the J_z_-eccentricity diagram. We find four halo and twelve thick disk white dwarfs. We also present a systematic study of the effects of ignoring the radial velocity in kinematic investigations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877#table1</TD>
            <TD>2011-09-14T19:20:20Z</TD>
            <TD>#Stars#Proper_Motions#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/400/877&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/877</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/400/877 [1]</TD>
            <TD>White dwarfs 3D kinematics from SPY project (Pauli+, 2003)</TD>
            <TD>We present kinematics of a sample of 107 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for a distinction of thin disk, thick disk, and halo populations. This is the first homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations such as the halo and the thick disk. Studies of white dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project are combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters are computed. We calculate individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership are deduced from a sample of F and G stars taken from the literature for which chemical criteria can be used to distinguish between thin disk, thick disk and halo. Candidates for thick disk and halo members are selected in a first step from the classical U-V-velocity diagram. Our final assignment of population membership is based on orbits and position in the J_z_-eccentricity diagram. We find four halo and twelve thick disk white dwarfs. We also present a systematic study of the effects of ignoring the radial velocity in kinematic investigations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877#1</TD>
            <TD>2011-09-14T19:20:20Z</TD>
            <TD>#Stars#Proper_Motions#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>20-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/400/877</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/877</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/400/877 [2]</TD>
            <TD>White dwarfs 3D kinematics from SPY project (Pauli+, 2003)</TD>
            <TD>We present kinematics of a sample of 107 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for a distinction of thin disk, thick disk, and halo populations. This is the first homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations such as the halo and the thick disk. Studies of white dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project are combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters are computed. We calculate individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership are deduced from a sample of F and G stars taken from the literature for which chemical criteria can be used to distinguish between thin disk, thick disk and halo. Candidates for thick disk and halo members are selected in a first step from the classical U-V-velocity diagram. Our final assignment of population membership is based on orbits and position in the J_z_-eccentricity diagram. We find four halo and twelve thick disk white dwarfs. We also present a systematic study of the effects of ignoring the radial velocity in kinematic investigations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877#2</TD>
            <TD>2011-09-14T19:20:20Z</TD>
            <TD>#Stars#Proper_Motions#Velocities#Stars:white_dwarf#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>20-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/400/877&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/877</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/400/877 [table1]</TD>
            <TD>White dwarfs 3D kinematics from SPY project (Pauli+, 2003)</TD>
            <TD>We present kinematics of a sample of 107 DA white dwarfs from the SPY project (ESO SN Ia Progenitor surveY) and discuss kinematic criteria for a distinction of thin disk, thick disk, and halo populations. This is the first homogeneous sample of white dwarfs for which 3D space motions have been determined. Since the percentage of old stars among white dwarfs is higher than among main-sequence stars, they are presumably valuable tools in studies of old populations such as the halo and the thick disk. Studies of white dwarf kinematics can help to determine the fraction of the total mass of our Galaxy contained in the form of thick disk and halo white dwarfs, an issue which is still under discussion. Radial velocities and spectroscopic distances obtained by the SPY project are combined with our measurements of proper motions to derive 3D space motions. Galactic orbits and further kinematic parameters are computed. We calculate individual errors of kinematic parameters by means of a Monte Carlo error propagation code. Our kinematic criteria for assigning population membership are deduced from a sample of F and G stars taken from the literature for which chemical criteria can be used to distinguish between thin disk, thick disk and halo. Candidates for thick disk and halo members are selected in a first step from the classical U-V-velocity diagram. Our final assignment of population membership is based on orbits and position in the J_z_-eccentricity diagram. We find four halo and twelve thick disk white dwarfs. We also present a systematic study of the effects of ignoring the radial velocity in kinematic investigations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877#table1</TD>
            <TD>2011-09-14T19:20:20Z</TD>
            <TD>#Stars#Proper_Motions#Velocities#Stars:white_dwarf#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>20-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/877</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/400/877&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/877</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1216 [1]</TD>
            <TD>Redshifts in A3128/A3125 (Rose+, 2002)</TD>
            <TD>Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20ks Chandra ACIS-I image of the central 16'x16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216#1</TD>
            <TD>2011-09-14T19:20:43Z</TD>
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            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1216</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1216</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1216 [2]</TD>
            <TD>Redshifts in A3128/A3125 (Rose+, 2002)</TD>
            <TD>Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20ks Chandra ACIS-I image of the central 16'x16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216#2</TD>
            <TD>2011-09-14T19:20:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1216&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1216</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1216 [table1]</TD>
            <TD>Redshifts in A3128/A3125 (Rose+, 2002)</TD>
            <TD>Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20ks Chandra ACIS-I image of the central 16'x16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216#table1</TD>
            <TD>2011-09-14T19:20:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1216&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1216</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1216 [1]</TD>
            <TD>Redshifts in A3128/A3125 (Rose+, 2002)</TD>
            <TD>Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20ks Chandra ACIS-I image of the central 16'x16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216#1</TD>
            <TD>2011-09-14T19:20:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1216</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1216</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1216 [2]</TD>
            <TD>Redshifts in A3128/A3125 (Rose+, 2002)</TD>
            <TD>Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20ks Chandra ACIS-I image of the central 16'x16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216#2</TD>
            <TD>2011-09-14T19:20:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1216&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1216</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1216 [table1]</TD>
            <TD>Redshifts in A3128/A3125 (Rose+, 2002)</TD>
            <TD>Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20ks Chandra ACIS-I image of the central 16'x16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216#table1</TD>
            <TD>2011-09-14T19:20:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1216&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1216</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1216 [1]</TD>
            <TD>Redshifts in A3128/A3125 (Rose+, 2002)</TD>
            <TD>Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20ks Chandra ACIS-I image of the central 16'x16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216#1</TD>
            <TD>2011-09-14T19:20:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1216</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1216</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1216 [2]</TD>
            <TD>Redshifts in A3128/A3125 (Rose+, 2002)</TD>
            <TD>Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20ks Chandra ACIS-I image of the central 16'x16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216#2</TD>
            <TD>2011-09-14T19:20:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1216&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1216</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1216 [table1]</TD>
            <TD>Redshifts in A3128/A3125 (Rose+, 2002)</TD>
            <TD>Multifiber spectroscopy has been obtained for 335 galaxies in the field of the double cluster A3128/A3125, using the 2dF multifiber positioner on the Anglo-Australian Telescope. When combined with previously published results, a total of 532 objects in the double cluster now have known redshifts. We have also obtained a 20ks Chandra ACIS-I image of the central 16'x16' of A3128 and radio imaging of the cluster with the Molonglo Observatory Synthesis Telescope and the Australia Telescope Compact Array. The spatial/kinematic distribution of redshifts in the field of A3128/A3125, when combined with the Chandra ACIS-I image of A3128, reveals a variety of substructures present in the galaxy distribution and in the hot intracluster medium (ICM).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216#table1</TD>
            <TD>2011-09-14T19:20:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1216</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1216&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1216</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2206 [1]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#1</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/2206</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2206 [2]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#2</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2206 [table4]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#table4</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2206 [table6]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#table6</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2206 [table5]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#table5</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2206 [1]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#1</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/2206</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2206 [2]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#2</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2206 [table4]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#table4</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2206 [table6]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#table6</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2206 [table5]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#table5</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2206 [1]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#1</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/2206</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2206 [2]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#2</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2206 [table4]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#table4</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2206 [table6]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#table6</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2206 [table5]</TD>
            <TD>BRI photometry of 3 QSO fields (Prochaska+, 2002)</TD>
            <TD>This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L&lt;L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206#table5</TD>
            <TD>2011-09-14T19:20:49Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2206</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2206&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2206</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/391/887 [1]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#1</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/391/887</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/391/887 [2]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#2</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/391/887&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/887 [table2]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#table2</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/887&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/887 [table1]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#table1</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/887&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/391/887 [1]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#1</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/391/887</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/391/887 [2]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#2</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/391/887&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/887 [table2]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#table2</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/887&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/887 [table1]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#table1</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/887&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/391/887 [1]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#1</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/391/887</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/391/887 [2]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#2</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/391/887&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/887 [table2]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#table2</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/887&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/391/887 [table1]</TD>
            <TD>Redshifts in the Hydra/Antlia Extension (Kraan-Korteweg+, 2002)</TD>
            <TD>As part of our program to map the large-scale distribution of galaxies behind the Milky Way, we used the Parkes 210 ft (64m) radio telescope for pointed HI observations of a sample of low surface-brightness (due to heavy obscuration) spiral galaxies selected from the deep optical Zone of Avoidance (ZOA) galaxy catalog in the Hydra/Antlia region (Kraan-Korteweg, 2000, Cat. &lt;J/A+AS/141/123&gt;). Searching a simultaneous velocity range of either 300 to 5500km/s or 300 to 10500km/s to an rms level of typically 2-4mJy resulted in detections in 61 of the 139 pointings, leading to a total of 66 detections (an additional detection was made in a reference position, and two other pointings revealed two and four independent signals respectively). Except for 2 strong HI emitters identified in the shallow Zone of Avoidance HI survey (Henning et al., 2000AJ....119.2686H), all HI detections are new.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887#table1</TD>
            <TD>2011-09-14T19:24:30Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/391/887</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/391/887&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/391/887</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/669/959 [1]</TD>
            <TD>Warm molecular hydrogen in SINGS galaxy sample (Roussel+, 2007)</TD>
            <TD>The SINGS sample (Kennicutt et al., 2003PASP..115..928K), comprising 75 galaxies, is intended to be a valuable representative set of local galaxies that are not ultraluminous, and whose moderate distances ensure that the properties of the interstellar medium can be studied at relatively small spatial scales (a few hundreds of parsecs at the shortest wavelengths). To estimate flux densities of the dust continuum and of the aromatic bands (also referred to as the emission from PAHs, or polycyclic aromatic hydrocarbons), we used images in the 3.6 and 7.9um bands of the IRAC camera and scan maps in the three bands of the MIPS instrument at effective wavelengths of 24, 71, and 156um. The targets were observed in mapping mode with the IRS instrument, at low spectral resolution between 5 and 38um, with the SL and LL slits (resolution ~60-130), and at high spectral resolution between 10 and 37um, with the SH and LH slits (rsolution ~600).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959#1</TD>
            <TD>2011-09-14T20:54:33Z</TD>
            <TD>#Galaxies#Interstellar_Medium#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/669/959</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/669/959</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/669/959 [2]</TD>
            <TD>Warm molecular hydrogen in SINGS galaxy sample (Roussel+, 2007)</TD>
            <TD>The SINGS sample (Kennicutt et al., 2003PASP..115..928K), comprising 75 galaxies, is intended to be a valuable representative set of local galaxies that are not ultraluminous, and whose moderate distances ensure that the properties of the interstellar medium can be studied at relatively small spatial scales (a few hundreds of parsecs at the shortest wavelengths). To estimate flux densities of the dust continuum and of the aromatic bands (also referred to as the emission from PAHs, or polycyclic aromatic hydrocarbons), we used images in the 3.6 and 7.9um bands of the IRAC camera and scan maps in the three bands of the MIPS instrument at effective wavelengths of 24, 71, and 156um. The targets were observed in mapping mode with the IRS instrument, at low spectral resolution between 5 and 38um, with the SL and LL slits (resolution ~60-130), and at high spectral resolution between 10 and 37um, with the SH and LH slits (rsolution ~600).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959#2</TD>
            <TD>2011-09-14T20:54:33Z</TD>
            <TD>#Galaxies#Interstellar_Medium#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/669/959&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/669/959</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/669/959 [galaxies]</TD>
            <TD>Warm molecular hydrogen in SINGS galaxy sample (Roussel+, 2007)</TD>
            <TD>The SINGS sample (Kennicutt et al., 2003PASP..115..928K), comprising 75 galaxies, is intended to be a valuable representative set of local galaxies that are not ultraluminous, and whose moderate distances ensure that the properties of the interstellar medium can be studied at relatively small spatial scales (a few hundreds of parsecs at the shortest wavelengths). To estimate flux densities of the dust continuum and of the aromatic bands (also referred to as the emission from PAHs, or polycyclic aromatic hydrocarbons), we used images in the 3.6 and 7.9um bands of the IRAC camera and scan maps in the three bands of the MIPS instrument at effective wavelengths of 24, 71, and 156um. The targets were observed in mapping mode with the IRS instrument, at low spectral resolution between 5 and 38um, with the SL and LL slits (resolution ~60-130), and at high spectral resolution between 10 and 37um, with the SH and LH slits (rsolution ~600).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959#galaxies</TD>
            <TD>2011-09-14T20:54:33Z</TD>
            <TD>#Galaxies#Interstellar_Medium#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/669/959&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/669/959</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/393/389 [1]</TD>
            <TD>H{alpha} in HII regions in spiral galaxies (Marquez+, 2002)</TD>
            <TD>In this paper we study long slit spectra in the region of H{alpha} emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected H II regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/H{alpha} ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/H{alpha} ratios measured for disk H II regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of H{alpha} equivalent width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389#1</TD>
            <TD>2011-09-14T19:24:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/393/389</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/389</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/393/389 [2]</TD>
            <TD>H{alpha} in HII regions in spiral galaxies (Marquez+, 2002)</TD>
            <TD>In this paper we study long slit spectra in the region of H{alpha} emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected H II regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/H{alpha} ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/H{alpha} ratios measured for disk H II regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of H{alpha} equivalent width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389#2</TD>
            <TD>2011-09-14T19:24:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/393/389&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/393/389 [table5]</TD>
            <TD>H{alpha} in HII regions in spiral galaxies (Marquez+, 2002)</TD>
            <TD>In this paper we study long slit spectra in the region of H{alpha} emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected H II regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/H{alpha} ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/H{alpha} ratios measured for disk H II regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of H{alpha} equivalent width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389#table5</TD>
            <TD>2011-09-14T19:24:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/393/389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/389</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>III/204 [1]</TD>
            <TD>Stellar radial velocities bibliographic catalog (Malaroda+, 2000)</TD>
            <TD>We present a bibliographic catalogue of stellar radial velocities with 13359 entries for stars in the Galaxy and the Magellanic Clouds, obtained from the issues of several journals published in the period 1991-1994. We have tried to follow the structure of previous compilations although we have relied on data retrieved from the SIMBAD database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/204#1</TD>
            <TD>2011-09-14T19:07:32Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2000</TD>
            <TD>ivo://CDS.VizieR/III/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=III/204</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/204</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>III/204 [2]</TD>
            <TD>Stellar radial velocities bibliographic catalog (Malaroda+, 2000)</TD>
            <TD>We present a bibliographic catalogue of stellar radial velocities with 13359 entries for stars in the Galaxy and the Magellanic Clouds, obtained from the issues of several journals published in the period 1991-1994. We have tried to follow the structure of previous compilations although we have relied on data retrieved from the SIMBAD database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/204#2</TD>
            <TD>2011-09-14T19:07:32Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2000</TD>
            <TD>ivo://CDS.VizieR/III/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=III/204&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/204</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/393/389 [1]</TD>
            <TD>H{alpha} in HII regions in spiral galaxies (Marquez+, 2002)</TD>
            <TD>In this paper we study long slit spectra in the region of H{alpha} emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected H II regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/H{alpha} ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/H{alpha} ratios measured for disk H II regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of H{alpha} equivalent width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389#1</TD>
            <TD>2011-09-14T19:24:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/393/389</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/389</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/393/389 [2]</TD>
            <TD>H{alpha} in HII regions in spiral galaxies (Marquez+, 2002)</TD>
            <TD>In this paper we study long slit spectra in the region of H{alpha} emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected H II regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/H{alpha} ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/H{alpha} ratios measured for disk H II regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of H{alpha} equivalent width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389#2</TD>
            <TD>2011-09-14T19:24:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/393/389&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/393/389 [table5]</TD>
            <TD>H{alpha} in HII regions in spiral galaxies (Marquez+, 2002)</TD>
            <TD>In this paper we study long slit spectra in the region of H{alpha} emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected H II regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/H{alpha} ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/H{alpha} ratios measured for disk H II regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of H{alpha} equivalent width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389#table5</TD>
            <TD>2011-09-14T19:24:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/393/389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/389</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/393/389 [1]</TD>
            <TD>H{alpha} in HII regions in spiral galaxies (Marquez+, 2002)</TD>
            <TD>In this paper we study long slit spectra in the region of H{alpha} emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected H II regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/H{alpha} ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/H{alpha} ratios measured for disk H II regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of H{alpha} equivalent width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389#1</TD>
            <TD>2011-09-14T19:24:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/393/389</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/389</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/393/389 [2]</TD>
            <TD>H{alpha} in HII regions in spiral galaxies (Marquez+, 2002)</TD>
            <TD>In this paper we study long slit spectra in the region of H{alpha} emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected H II regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/H{alpha} ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/H{alpha} ratios measured for disk H II regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of H{alpha} equivalent width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389#2</TD>
            <TD>2011-09-14T19:24:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/393/389&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/393/389 [table5]</TD>
            <TD>H{alpha} in HII regions in spiral galaxies (Marquez+, 2002)</TD>
            <TD>In this paper we study long slit spectra in the region of H{alpha} emission line of a sample of 111 spiral galaxies with recognizable and well defined spiral morphology and with a well determined environmental status, ranging from isolation to non-disruptive interaction with satellites or companions. The form and properties of the rotation curves are considered as a function of the isolation degree, morphological type and luminosity. The line ratios are used to estimate the metallicity of all the detected H II regions, thus producing a composite metallicity profile for different types of spirals. We have found that isolated galaxies tend to be of later types and lower luminosity than the interacting galaxies. The outer parts of the rotation curves of isolated galaxies tend to be flatter than in interacting galaxies, but they show similar relations between global parameters. The scatter of the Tully-Fisher relation defined by isolated galaxies is significantly lower than that of interacting galaxies. The [NII]/H{alpha} ratios, used as a metallicity indicator, show a clear trend between Z and morphological type, t, with earlier spirals showing higher ratios; this trend is tighter when instead of t the gradient of the inner rotation curve, G, is used; no trend is found with the change in interaction status. The Z-gradient of the disks depends on the type, being almost flat for early spirals, and increasing for later types. The [NII]/H{alpha} ratios measured for disk H II regions of interacting galaxies are higher than for normal/isolated objects, even if all the galaxy families present similar distributions of H{alpha} equivalent width.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389#table5</TD>
            <TD>2011-09-14T19:24:39Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Equivalent_widths#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jul-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/393/389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/389</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/669/959 [1]</TD>
            <TD>Warm molecular hydrogen in SINGS galaxy sample (Roussel+, 2007)</TD>
            <TD>The SINGS sample (Kennicutt et al., 2003PASP..115..928K), comprising 75 galaxies, is intended to be a valuable representative set of local galaxies that are not ultraluminous, and whose moderate distances ensure that the properties of the interstellar medium can be studied at relatively small spatial scales (a few hundreds of parsecs at the shortest wavelengths). To estimate flux densities of the dust continuum and of the aromatic bands (also referred to as the emission from PAHs, or polycyclic aromatic hydrocarbons), we used images in the 3.6 and 7.9um bands of the IRAC camera and scan maps in the three bands of the MIPS instrument at effective wavelengths of 24, 71, and 156um. The targets were observed in mapping mode with the IRS instrument, at low spectral resolution between 5 and 38um, with the SL and LL slits (resolution ~60-130), and at high spectral resolution between 10 and 37um, with the SH and LH slits (rsolution ~600).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959#1</TD>
            <TD>2011-09-14T20:54:33Z</TD>
            <TD>#Galaxies#Interstellar_Medium#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/669/959</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/669/959</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/669/959 [2]</TD>
            <TD>Warm molecular hydrogen in SINGS galaxy sample (Roussel+, 2007)</TD>
            <TD>The SINGS sample (Kennicutt et al., 2003PASP..115..928K), comprising 75 galaxies, is intended to be a valuable representative set of local galaxies that are not ultraluminous, and whose moderate distances ensure that the properties of the interstellar medium can be studied at relatively small spatial scales (a few hundreds of parsecs at the shortest wavelengths). To estimate flux densities of the dust continuum and of the aromatic bands (also referred to as the emission from PAHs, or polycyclic aromatic hydrocarbons), we used images in the 3.6 and 7.9um bands of the IRAC camera and scan maps in the three bands of the MIPS instrument at effective wavelengths of 24, 71, and 156um. The targets were observed in mapping mode with the IRS instrument, at low spectral resolution between 5 and 38um, with the SL and LL slits (resolution ~60-130), and at high spectral resolution between 10 and 37um, with the SH and LH slits (rsolution ~600).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959#2</TD>
            <TD>2011-09-14T20:54:33Z</TD>
            <TD>#Galaxies#Interstellar_Medium#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/669/959&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/669/959</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/669/959 [galaxies]</TD>
            <TD>Warm molecular hydrogen in SINGS galaxy sample (Roussel+, 2007)</TD>
            <TD>The SINGS sample (Kennicutt et al., 2003PASP..115..928K), comprising 75 galaxies, is intended to be a valuable representative set of local galaxies that are not ultraluminous, and whose moderate distances ensure that the properties of the interstellar medium can be studied at relatively small spatial scales (a few hundreds of parsecs at the shortest wavelengths). To estimate flux densities of the dust continuum and of the aromatic bands (also referred to as the emission from PAHs, or polycyclic aromatic hydrocarbons), we used images in the 3.6 and 7.9um bands of the IRAC camera and scan maps in the three bands of the MIPS instrument at effective wavelengths of 24, 71, and 156um. The targets were observed in mapping mode with the IRS instrument, at low spectral resolution between 5 and 38um, with the SL and LL slits (resolution ~60-130), and at high spectral resolution between 10 and 37um, with the SH and LH slits (rsolution ~600).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959#galaxies</TD>
            <TD>2011-09-14T20:54:33Z</TD>
            <TD>#Galaxies#Interstellar_Medium#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/669/959</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/669/959&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/669/959</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/412/633 [1]</TD>
            <TD>Catalog of high and low SB disk galaxies (Zavala+, 2003)</TD>
            <TD>Photometric parameters, velocity line-widths, HI integral fluxes and other quantities are presented for a sample of 78 high and low SB disk galaxies (including The Galaxy and Andromeda) compiled mainly from the works by de Jong (1996A&amp;A...313...45D, 1996, Cat. &lt;J/A+A/313/377&gt;), Verheijen (1997, Ph. D. Thesis, Groningen University) and Verheijen &amp; Sancisi (2001, Cat. &lt;J/A+A/370/765&gt;), Bell et al. (2000MNRAS.312..470B), and the LEDA (&lt;http://leda.univ-lyon1.fr/&gt;) catalog. All the data were uniformely corrected by us.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633#1</TD>
            <TD>2011-09-14T19:25:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/412/633</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/412/633</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/412/633 [2]</TD>
            <TD>Catalog of high and low SB disk galaxies (Zavala+, 2003)</TD>
            <TD>Photometric parameters, velocity line-widths, HI integral fluxes and other quantities are presented for a sample of 78 high and low SB disk galaxies (including The Galaxy and Andromeda) compiled mainly from the works by de Jong (1996A&amp;A...313...45D, 1996, Cat. &lt;J/A+A/313/377&gt;), Verheijen (1997, Ph. D. Thesis, Groningen University) and Verheijen &amp; Sancisi (2001, Cat. &lt;J/A+A/370/765&gt;), Bell et al. (2000MNRAS.312..470B), and the LEDA (&lt;http://leda.univ-lyon1.fr/&gt;) catalog. All the data were uniformely corrected by us.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633#2</TD>
            <TD>2011-09-14T19:25:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/412/633&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/412/633</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/412/633 [table1]</TD>
            <TD>Catalog of high and low SB disk galaxies (Zavala+, 2003)</TD>
            <TD>Photometric parameters, velocity line-widths, HI integral fluxes and other quantities are presented for a sample of 78 high and low SB disk galaxies (including The Galaxy and Andromeda) compiled mainly from the works by de Jong (1996A&amp;A...313...45D, 1996, Cat. &lt;J/A+A/313/377&gt;), Verheijen (1997, Ph. D. Thesis, Groningen University) and Verheijen &amp; Sancisi (2001, Cat. &lt;J/A+A/370/765&gt;), Bell et al. (2000MNRAS.312..470B), and the LEDA (&lt;http://leda.univ-lyon1.fr/&gt;) catalog. All the data were uniformely corrected by us.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633#table1</TD>
            <TD>2011-09-14T19:25:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/412/633&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/412/633</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>III/204 [1]</TD>
            <TD>Stellar radial velocities bibliographic catalog (Malaroda+, 2000)</TD>
            <TD>We present a bibliographic catalogue of stellar radial velocities with 13359 entries for stars in the Galaxy and the Magellanic Clouds, obtained from the issues of several journals published in the period 1991-1994. We have tried to follow the structure of previous compilations although we have relied on data retrieved from the SIMBAD database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/204#1</TD>
            <TD>2011-09-14T19:07:32Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2000</TD>
            <TD>ivo://CDS.VizieR/III/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=III/204</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/204</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>III/204 [2]</TD>
            <TD>Stellar radial velocities bibliographic catalog (Malaroda+, 2000)</TD>
            <TD>We present a bibliographic catalogue of stellar radial velocities with 13359 entries for stars in the Galaxy and the Magellanic Clouds, obtained from the issues of several journals published in the period 1991-1994. We have tried to follow the structure of previous compilations although we have relied on data retrieved from the SIMBAD database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/204#2</TD>
            <TD>2011-09-14T19:07:32Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2000</TD>
            <TD>ivo://CDS.VizieR/III/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=III/204&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/204</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/412/633 [1]</TD>
            <TD>Catalog of high and low SB disk galaxies (Zavala+, 2003)</TD>
            <TD>Photometric parameters, velocity line-widths, HI integral fluxes and other quantities are presented for a sample of 78 high and low SB disk galaxies (including The Galaxy and Andromeda) compiled mainly from the works by de Jong (1996A&amp;A...313...45D, 1996, Cat. &lt;J/A+A/313/377&gt;), Verheijen (1997, Ph. D. Thesis, Groningen University) and Verheijen &amp; Sancisi (2001, Cat. &lt;J/A+A/370/765&gt;), Bell et al. (2000MNRAS.312..470B), and the LEDA (&lt;http://leda.univ-lyon1.fr/&gt;) catalog. All the data were uniformely corrected by us.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633#1</TD>
            <TD>2011-09-14T19:25:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/412/633</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/412/633</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/412/633 [2]</TD>
            <TD>Catalog of high and low SB disk galaxies (Zavala+, 2003)</TD>
            <TD>Photometric parameters, velocity line-widths, HI integral fluxes and other quantities are presented for a sample of 78 high and low SB disk galaxies (including The Galaxy and Andromeda) compiled mainly from the works by de Jong (1996A&amp;A...313...45D, 1996, Cat. &lt;J/A+A/313/377&gt;), Verheijen (1997, Ph. D. Thesis, Groningen University) and Verheijen &amp; Sancisi (2001, Cat. &lt;J/A+A/370/765&gt;), Bell et al. (2000MNRAS.312..470B), and the LEDA (&lt;http://leda.univ-lyon1.fr/&gt;) catalog. All the data were uniformely corrected by us.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633#2</TD>
            <TD>2011-09-14T19:25:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/412/633&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/412/633</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/412/633 [table1]</TD>
            <TD>Catalog of high and low SB disk galaxies (Zavala+, 2003)</TD>
            <TD>Photometric parameters, velocity line-widths, HI integral fluxes and other quantities are presented for a sample of 78 high and low SB disk galaxies (including The Galaxy and Andromeda) compiled mainly from the works by de Jong (1996A&amp;A...313...45D, 1996, Cat. &lt;J/A+A/313/377&gt;), Verheijen (1997, Ph. D. Thesis, Groningen University) and Verheijen &amp; Sancisi (2001, Cat. &lt;J/A+A/370/765&gt;), Bell et al. (2000MNRAS.312..470B), and the LEDA (&lt;http://leda.univ-lyon1.fr/&gt;) catalog. All the data were uniformely corrected by us.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633#table1</TD>
            <TD>2011-09-14T19:25:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/412/633&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/412/633</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/313/469 [1]</TD>
            <TD>Streaming motions of galaxy clusters. I. (Smith+, 2000)</TD>
            <TD>++++Lrecl of file 'table3.dat' (94) indicates 1 extra blanks (trim!) %B The present paper is the first in a series presenting results of the "Streaming Motions of Abell Cluster" (SMAC) project. We present new spectroscopic data for 532 early-type galaxies, predominantly Abell cluster members with cz&lt;12000km/s. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, {sigma}, and magnesium line-strength indices, Mg_2_ and Mgb. The median estimated error, per measurement, in {sigma} is 5 per cent. The Mg_2_ line-strength data have median errors of 0.009mag. The observed scatter between repeat measurements is largely accounted for by photon-counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469#1</TD>
            <TD>2011-09-14T20:54:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/313/469</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/313/469</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/313/469 [2]</TD>
            <TD>Streaming motions of galaxy clusters. I. (Smith+, 2000)</TD>
            <TD>++++Lrecl of file 'table3.dat' (94) indicates 1 extra blanks (trim!) %B The present paper is the first in a series presenting results of the "Streaming Motions of Abell Cluster" (SMAC) project. We present new spectroscopic data for 532 early-type galaxies, predominantly Abell cluster members with cz&lt;12000km/s. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, {sigma}, and magnesium line-strength indices, Mg_2_ and Mgb. The median estimated error, per measurement, in {sigma} is 5 per cent. The Mg_2_ line-strength data have median errors of 0.009mag. The observed scatter between repeat measurements is largely accounted for by photon-counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469#2</TD>
            <TD>2011-09-14T20:54:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/313/469&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/313/469</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/313/469 [table3]</TD>
            <TD>Streaming motions of galaxy clusters. I. (Smith+, 2000)</TD>
            <TD>++++Lrecl of file 'table3.dat' (94) indicates 1 extra blanks (trim!) %B The present paper is the first in a series presenting results of the "Streaming Motions of Abell Cluster" (SMAC) project. We present new spectroscopic data for 532 early-type galaxies, predominantly Abell cluster members with cz&lt;12000km/s. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, {sigma}, and magnesium line-strength indices, Mg_2_ and Mgb. The median estimated error, per measurement, in {sigma} is 5 per cent. The Mg_2_ line-strength data have median errors of 0.009mag. The observed scatter between repeat measurements is largely accounted for by photon-counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469#table3</TD>
            <TD>2011-09-14T20:54:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/313/469&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/313/469</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/412/633 [1]</TD>
            <TD>Catalog of high and low SB disk galaxies (Zavala+, 2003)</TD>
            <TD>Photometric parameters, velocity line-widths, HI integral fluxes and other quantities are presented for a sample of 78 high and low SB disk galaxies (including The Galaxy and Andromeda) compiled mainly from the works by de Jong (1996A&amp;A...313...45D, 1996, Cat. &lt;J/A+A/313/377&gt;), Verheijen (1997, Ph. D. Thesis, Groningen University) and Verheijen &amp; Sancisi (2001, Cat. &lt;J/A+A/370/765&gt;), Bell et al. (2000MNRAS.312..470B), and the LEDA (&lt;http://leda.univ-lyon1.fr/&gt;) catalog. All the data were uniformely corrected by us.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633#1</TD>
            <TD>2011-09-14T19:25:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/412/633</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/412/633</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/412/633 [2]</TD>
            <TD>Catalog of high and low SB disk galaxies (Zavala+, 2003)</TD>
            <TD>Photometric parameters, velocity line-widths, HI integral fluxes and other quantities are presented for a sample of 78 high and low SB disk galaxies (including The Galaxy and Andromeda) compiled mainly from the works by de Jong (1996A&amp;A...313...45D, 1996, Cat. &lt;J/A+A/313/377&gt;), Verheijen (1997, Ph. D. Thesis, Groningen University) and Verheijen &amp; Sancisi (2001, Cat. &lt;J/A+A/370/765&gt;), Bell et al. (2000MNRAS.312..470B), and the LEDA (&lt;http://leda.univ-lyon1.fr/&gt;) catalog. All the data were uniformely corrected by us.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633#2</TD>
            <TD>2011-09-14T19:25:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/412/633&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/412/633</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/412/633 [table1]</TD>
            <TD>Catalog of high and low SB disk galaxies (Zavala+, 2003)</TD>
            <TD>Photometric parameters, velocity line-widths, HI integral fluxes and other quantities are presented for a sample of 78 high and low SB disk galaxies (including The Galaxy and Andromeda) compiled mainly from the works by de Jong (1996A&amp;A...313...45D, 1996, Cat. &lt;J/A+A/313/377&gt;), Verheijen (1997, Ph. D. Thesis, Groningen University) and Verheijen &amp; Sancisi (2001, Cat. &lt;J/A+A/370/765&gt;), Bell et al. (2000MNRAS.312..470B), and the LEDA (&lt;http://leda.univ-lyon1.fr/&gt;) catalog. All the data were uniformely corrected by us.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633#table1</TD>
            <TD>2011-09-14T19:25:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/412/633</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/412/633&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/412/633</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/313/469 [1]</TD>
            <TD>Streaming motions of galaxy clusters. I. (Smith+, 2000)</TD>
            <TD>++++Lrecl of file 'table3.dat' (94) indicates 1 extra blanks (trim!) %B The present paper is the first in a series presenting results of the "Streaming Motions of Abell Cluster" (SMAC) project. We present new spectroscopic data for 532 early-type galaxies, predominantly Abell cluster members with cz&lt;12000km/s. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, {sigma}, and magnesium line-strength indices, Mg_2_ and Mgb. The median estimated error, per measurement, in {sigma} is 5 per cent. The Mg_2_ line-strength data have median errors of 0.009mag. The observed scatter between repeat measurements is largely accounted for by photon-counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469#1</TD>
            <TD>2011-09-14T20:54:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/313/469</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/313/469</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/313/469 [2]</TD>
            <TD>Streaming motions of galaxy clusters. I. (Smith+, 2000)</TD>
            <TD>++++Lrecl of file 'table3.dat' (94) indicates 1 extra blanks (trim!) %B The present paper is the first in a series presenting results of the "Streaming Motions of Abell Cluster" (SMAC) project. We present new spectroscopic data for 532 early-type galaxies, predominantly Abell cluster members with cz&lt;12000km/s. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, {sigma}, and magnesium line-strength indices, Mg_2_ and Mgb. The median estimated error, per measurement, in {sigma} is 5 per cent. The Mg_2_ line-strength data have median errors of 0.009mag. The observed scatter between repeat measurements is largely accounted for by photon-counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469#2</TD>
            <TD>2011-09-14T20:54:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/313/469&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/313/469</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/313/469 [table3]</TD>
            <TD>Streaming motions of galaxy clusters. I. (Smith+, 2000)</TD>
            <TD>++++Lrecl of file 'table3.dat' (94) indicates 1 extra blanks (trim!) %B The present paper is the first in a series presenting results of the "Streaming Motions of Abell Cluster" (SMAC) project. We present new spectroscopic data for 532 early-type galaxies, predominantly Abell cluster members with cz&lt;12000km/s. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, {sigma}, and magnesium line-strength indices, Mg_2_ and Mgb. The median estimated error, per measurement, in {sigma} is 5 per cent. The Mg_2_ line-strength data have median errors of 0.009mag. The observed scatter between repeat measurements is largely accounted for by photon-counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469#table3</TD>
            <TD>2011-09-14T20:54:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/313/469&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/313/469</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/414/23 [1]</TD>
            <TD>CCD H{alpha} and R photometry of 334 galaxies (James+, 2004)</TD>
            <TD>H{alpha} plus [NII] and R-band CCD photometry and derived parameters are presented for the full sample of 334 spiral and irregular galaxies. Galaxy distances are derived using a Virgo-infall corrected model which is described in the paper, and star formation rates are derived from H{alpha} plus [NII] fluxes using the conversion defined by Kennicutt et al. (1994ApJ...435...22K). The entries are arranged within five bins in recession velocity, and in order of increasing Right Ascension within these bins.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23#1</TD>
            <TD>2011-09-14T19:26:14Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/414/23</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/23</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/414/23 [2]</TD>
            <TD>CCD H{alpha} and R photometry of 334 galaxies (James+, 2004)</TD>
            <TD>H{alpha} plus [NII] and R-band CCD photometry and derived parameters are presented for the full sample of 334 spiral and irregular galaxies. Galaxy distances are derived using a Virgo-infall corrected model which is described in the paper, and star formation rates are derived from H{alpha} plus [NII] fluxes using the conversion defined by Kennicutt et al. (1994ApJ...435...22K). The entries are arranged within five bins in recession velocity, and in order of increasing Right Ascension within these bins.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23#2</TD>
            <TD>2011-09-14T19:26:14Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/414/23&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/23</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/414/23 [table3]</TD>
            <TD>CCD H{alpha} and R photometry of 334 galaxies (James+, 2004)</TD>
            <TD>H{alpha} plus [NII] and R-band CCD photometry and derived parameters are presented for the full sample of 334 spiral and irregular galaxies. Galaxy distances are derived using a Virgo-infall corrected model which is described in the paper, and star formation rates are derived from H{alpha} plus [NII] fluxes using the conversion defined by Kennicutt et al. (1994ApJ...435...22K). The entries are arranged within five bins in recession velocity, and in order of increasing Right Ascension within these bins.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23#table3</TD>
            <TD>2011-09-14T19:26:14Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/414/23&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/23</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>III/204 [1]</TD>
            <TD>Stellar radial velocities bibliographic catalog (Malaroda+, 2000)</TD>
            <TD>We present a bibliographic catalogue of stellar radial velocities with 13359 entries for stars in the Galaxy and the Magellanic Clouds, obtained from the issues of several journals published in the period 1991-1994. We have tried to follow the structure of previous compilations although we have relied on data retrieved from the SIMBAD database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/204#1</TD>
            <TD>2011-09-14T19:07:32Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2000</TD>
            <TD>ivo://CDS.VizieR/III/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=III/204</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/204</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>III/204 [2]</TD>
            <TD>Stellar radial velocities bibliographic catalog (Malaroda+, 2000)</TD>
            <TD>We present a bibliographic catalogue of stellar radial velocities with 13359 entries for stars in the Galaxy and the Magellanic Clouds, obtained from the issues of several journals published in the period 1991-1994. We have tried to follow the structure of previous compilations although we have relied on data retrieved from the SIMBAD database.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/III/204#2</TD>
            <TD>2011-09-14T19:07:32Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-May-2000</TD>
            <TD>ivo://CDS.VizieR/III/204</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=III/204&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?III/204</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/313/469 [1]</TD>
            <TD>Streaming motions of galaxy clusters. I. (Smith+, 2000)</TD>
            <TD>++++Lrecl of file 'table3.dat' (94) indicates 1 extra blanks (trim!) %B The present paper is the first in a series presenting results of the "Streaming Motions of Abell Cluster" (SMAC) project. We present new spectroscopic data for 532 early-type galaxies, predominantly Abell cluster members with cz&lt;12000km/s. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, {sigma}, and magnesium line-strength indices, Mg_2_ and Mgb. The median estimated error, per measurement, in {sigma} is 5 per cent. The Mg_2_ line-strength data have median errors of 0.009mag. The observed scatter between repeat measurements is largely accounted for by photon-counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469#1</TD>
            <TD>2011-09-14T20:54:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/313/469</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/313/469</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/313/469 [2]</TD>
            <TD>Streaming motions of galaxy clusters. I. (Smith+, 2000)</TD>
            <TD>++++Lrecl of file 'table3.dat' (94) indicates 1 extra blanks (trim!) %B The present paper is the first in a series presenting results of the "Streaming Motions of Abell Cluster" (SMAC) project. We present new spectroscopic data for 532 early-type galaxies, predominantly Abell cluster members with cz&lt;12000km/s. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, {sigma}, and magnesium line-strength indices, Mg_2_ and Mgb. The median estimated error, per measurement, in {sigma} is 5 per cent. The Mg_2_ line-strength data have median errors of 0.009mag. The observed scatter between repeat measurements is largely accounted for by photon-counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469#2</TD>
            <TD>2011-09-14T20:54:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/313/469&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/313/469</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/313/469 [table3]</TD>
            <TD>Streaming motions of galaxy clusters. I. (Smith+, 2000)</TD>
            <TD>++++Lrecl of file 'table3.dat' (94) indicates 1 extra blanks (trim!) %B The present paper is the first in a series presenting results of the "Streaming Motions of Abell Cluster" (SMAC) project. We present new spectroscopic data for 532 early-type galaxies, predominantly Abell cluster members with cz&lt;12000km/s. We tabulate 919 individual measurements, from six observing runs, for recession velocity, cz, central velocity dispersion, {sigma}, and magnesium line-strength indices, Mg_2_ and Mgb. The median estimated error, per measurement, in {sigma} is 5 per cent. The Mg_2_ line-strength data have median errors of 0.009mag. The observed scatter between repeat measurements is largely accounted for by photon-counting errors. These data will be employed in forthcoming papers, where they will form part of a merged and standardized catalogue of Fundamental Plane data for use in cluster distance estimates and peculiar velocity analyses.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469#table3</TD>
            <TD>2011-09-14T20:54:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/313/469</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/313/469&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/313/469</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/414/23 [1]</TD>
            <TD>CCD H{alpha} and R photometry of 334 galaxies (James+, 2004)</TD>
            <TD>H{alpha} plus [NII] and R-band CCD photometry and derived parameters are presented for the full sample of 334 spiral and irregular galaxies. Galaxy distances are derived using a Virgo-infall corrected model which is described in the paper, and star formation rates are derived from H{alpha} plus [NII] fluxes using the conversion defined by Kennicutt et al. (1994ApJ...435...22K). The entries are arranged within five bins in recession velocity, and in order of increasing Right Ascension within these bins.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23#1</TD>
            <TD>2011-09-14T19:26:14Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/414/23</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/23</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/414/23 [2]</TD>
            <TD>CCD H{alpha} and R photometry of 334 galaxies (James+, 2004)</TD>
            <TD>H{alpha} plus [NII] and R-band CCD photometry and derived parameters are presented for the full sample of 334 spiral and irregular galaxies. Galaxy distances are derived using a Virgo-infall corrected model which is described in the paper, and star formation rates are derived from H{alpha} plus [NII] fluxes using the conversion defined by Kennicutt et al. (1994ApJ...435...22K). The entries are arranged within five bins in recession velocity, and in order of increasing Right Ascension within these bins.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23#2</TD>
            <TD>2011-09-14T19:26:14Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/414/23&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/23</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/414/23 [table3]</TD>
            <TD>CCD H{alpha} and R photometry of 334 galaxies (James+, 2004)</TD>
            <TD>H{alpha} plus [NII] and R-band CCD photometry and derived parameters are presented for the full sample of 334 spiral and irregular galaxies. Galaxy distances are derived using a Virgo-infall corrected model which is described in the paper, and star formation rates are derived from H{alpha} plus [NII] fluxes using the conversion defined by Kennicutt et al. (1994ApJ...435...22K). The entries are arranged within five bins in recession velocity, and in order of increasing Right Ascension within these bins.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23#table3</TD>
            <TD>2011-09-14T19:26:14Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/414/23&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/23</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/122/51 [1]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#1</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/122/51</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/122/51 [2]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#2</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/51 [table2]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#table2</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/51 [table4b]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#table4b</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/51 [table4a]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#table4a</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/414/23 [1]</TD>
            <TD>CCD H{alpha} and R photometry of 334 galaxies (James+, 2004)</TD>
            <TD>H{alpha} plus [NII] and R-band CCD photometry and derived parameters are presented for the full sample of 334 spiral and irregular galaxies. Galaxy distances are derived using a Virgo-infall corrected model which is described in the paper, and star formation rates are derived from H{alpha} plus [NII] fluxes using the conversion defined by Kennicutt et al. (1994ApJ...435...22K). The entries are arranged within five bins in recession velocity, and in order of increasing Right Ascension within these bins.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23#1</TD>
            <TD>2011-09-14T19:26:14Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/414/23</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/23</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/414/23 [2]</TD>
            <TD>CCD H{alpha} and R photometry of 334 galaxies (James+, 2004)</TD>
            <TD>H{alpha} plus [NII] and R-band CCD photometry and derived parameters are presented for the full sample of 334 spiral and irregular galaxies. Galaxy distances are derived using a Virgo-infall corrected model which is described in the paper, and star formation rates are derived from H{alpha} plus [NII] fluxes using the conversion defined by Kennicutt et al. (1994ApJ...435...22K). The entries are arranged within five bins in recession velocity, and in order of increasing Right Ascension within these bins.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23#2</TD>
            <TD>2011-09-14T19:26:14Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/414/23&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/23</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/414/23 [table3]</TD>
            <TD>CCD H{alpha} and R photometry of 334 galaxies (James+, 2004)</TD>
            <TD>H{alpha} plus [NII] and R-band CCD photometry and derived parameters are presented for the full sample of 334 spiral and irregular galaxies. Galaxy distances are derived using a Virgo-infall corrected model which is described in the paper, and star formation rates are derived from H{alpha} plus [NII] fluxes using the conversion defined by Kennicutt et al. (1994ApJ...435...22K). The entries are arranged within five bins in recession velocity, and in order of increasing Right Ascension within these bins.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23#table3</TD>
            <TD>2011-09-14T19:26:14Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/23</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/414/23&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/23</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/690/1181 [1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/690/1181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/690/1181 [2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/690/1181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/690/1181 [table1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#table1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/690/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/690/1181 [table2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#table2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/690/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/594/154 [1]</TD>
            <TD>160 square degree ROSAT survey (Mullis+, 2003)</TD>
            <TD>We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z_median_=0.25, and the median X-ray luminosity is L_X,median_=4.2x10^43^h_50_^2^erg/s (0.5-2.0keV). This is the largest high-redshift sample of X-ray-selected clusters published to date. There are 73 objects at z&gt;0.3 and 22 objects at z&gt;0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4x10^-13^erg/cm^2^/s. We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154#1</TD>
            <TD>2011-09-14T19:26:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/594/154</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/594/154</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/594/154 [2]</TD>
            <TD>160 square degree ROSAT survey (Mullis+, 2003)</TD>
            <TD>We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z_median_=0.25, and the median X-ray luminosity is L_X,median_=4.2x10^43^h_50_^2^erg/s (0.5-2.0keV). This is the largest high-redshift sample of X-ray-selected clusters published to date. There are 73 objects at z&gt;0.3 and 22 objects at z&gt;0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4x10^-13^erg/cm^2^/s. We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154#2</TD>
            <TD>2011-09-14T19:26:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/594/154&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/594/154</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/594/154 [table4]</TD>
            <TD>160 square degree ROSAT survey (Mullis+, 2003)</TD>
            <TD>We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z_median_=0.25, and the median X-ray luminosity is L_X,median_=4.2x10^43^h_50_^2^erg/s (0.5-2.0keV). This is the largest high-redshift sample of X-ray-selected clusters published to date. There are 73 objects at z&gt;0.3 and 22 objects at z&gt;0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4x10^-13^erg/cm^2^/s. We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154#table4</TD>
            <TD>2011-09-14T19:26:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/594/154&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/594/154</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/122/51 [1]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#1</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/122/51</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/122/51 [2]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#2</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/51 [table2]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#table2</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/51 [table4b]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#table4b</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/51 [table4a]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#table4a</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/690/1181 [1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/690/1181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/690/1181 [2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/690/1181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/690/1181 [table1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#table1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/690/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/690/1181 [table2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#table2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/690/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/594/154 [1]</TD>
            <TD>160 square degree ROSAT survey (Mullis+, 2003)</TD>
            <TD>We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z_median_=0.25, and the median X-ray luminosity is L_X,median_=4.2x10^43^h_50_^2^erg/s (0.5-2.0keV). This is the largest high-redshift sample of X-ray-selected clusters published to date. There are 73 objects at z&gt;0.3 and 22 objects at z&gt;0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4x10^-13^erg/cm^2^/s. We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154#1</TD>
            <TD>2011-09-14T19:26:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/594/154</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/594/154</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/594/154 [2]</TD>
            <TD>160 square degree ROSAT survey (Mullis+, 2003)</TD>
            <TD>We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z_median_=0.25, and the median X-ray luminosity is L_X,median_=4.2x10^43^h_50_^2^erg/s (0.5-2.0keV). This is the largest high-redshift sample of X-ray-selected clusters published to date. There are 73 objects at z&gt;0.3 and 22 objects at z&gt;0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4x10^-13^erg/cm^2^/s. We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154#2</TD>
            <TD>2011-09-14T19:26:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/594/154&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/594/154</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/594/154 [table4]</TD>
            <TD>160 square degree ROSAT survey (Mullis+, 2003)</TD>
            <TD>We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z_median_=0.25, and the median X-ray luminosity is L_X,median_=4.2x10^43^h_50_^2^erg/s (0.5-2.0keV). This is the largest high-redshift sample of X-ray-selected clusters published to date. There are 73 objects at z&gt;0.3 and 22 objects at z&gt;0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4x10^-13^erg/cm^2^/s. We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154#table4</TD>
            <TD>2011-09-14T19:26:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/594/154&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/594/154</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/690/1181 [1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/690/1181</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/690/1181 [2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/690/1181&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/690/1181 [table1]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#table1</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/690/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/690/1181 [table2]</TD>
            <TD>UV-bright quasars (Syphers+, 2009)</TD>
            <TD>Investigations of HeII Ly{alpha} (304{AA} rest-frame) absorption toward a half-dozen quasars at z~3-4 have demonstrated the great potential of helium studies of the intergalactic medium, but the current critically small sample size of clean sightlines for the HeII Gunn-Peterson test limits confidence in cosmological inferences, and a larger sample is required. Although the unobscured quasar sightlines to high redshift are extremely rare, the Sloan Digital Sky Survey (SDSS) DR6 provides thousands of z&gt;2.8 quasars. We have cross-correlated these SDSS quasars with the Galaxy Evolution Explorer (GALEX) GR2/GR3 to establish a catalog of 200 higher-confidence (~70% secure) cases of quasars at z=2.8-5.1 potentially having surviving far-UV (rest-frame) flux. We also catalog another 112 likely far-UV-bright quasars from GALEX cross-correlation with other (non-SDSS) quasar compilations. Reconnaissance UV prism observations with the Hubble Space Telescope (HST) of 24 of our SDSS/GALEX candidates confirm 12 as detected in the far-UV, with at least nine having flux extending to very near the HeII break; with refinements our success rate is even higher. Our SDSS/GALEX selection approach is thereby confirmed to be an order of magnitude more efficient than previous HeII quasar searches, more than doubles the number of spectroscopically confirmed clean sightlines to high redshift, and provides a resource list of hundreds of high-confidence sightlines for upcoming HeII and other far-UV studies from the HST. Our reconnaissance HST prism spectra suggest some far-UV diversity, confirming the need to obtain a large sample of independent quasar sightlines across a broad redshift range to assess such issues as the epoch(s) of helium reionization, while averaging over individual-object pathology and/or cosmic variance.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181#table2</TD>
            <TD>2011-09-14T20:56:48Z</TD>
            <TD>#Photometry#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/690/1181</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/690/1181&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/690/1181</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/122/51 [1]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#1</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/122/51</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/122/51 [2]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#2</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/51 [table2]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#table2</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/51 [table4b]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#table4b</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/122/51 [table4a]</TD>
            <TD>Spectroscopic catalog of 10 rich galaxy clusters (Dressler+ 1999)</TD>
            <TD>We present spectroscopic observations of galaxies in the fields of 10 distant clusters for which we have previously presented deep imaging with WFPC2 on board the Hubble Space Telescope. The clusters span the redshift range z=0.37-0.56 and are the subject of a detailed ground- and space-based study to investigate the evolution of galaxies as a function of environment and epoch. The data presented here include positions, photometry, redshifts, spectral line strengths, and classifications for 657 galaxies in the fields of the 10 clusters. The catalog is composed of 424 cluster members across the 10 clusters and 233 field galaxies, with detailed morphological information from our WFPC2 images for 204 of the cluster galaxies and 71 in the field. We illustrate some basic properties of the catalog, including correlations between the morphological and spectral properties of our large sample of cluster galaxies. A direct comparison of the spectral properties of the high-redshift cluster and field populations suggests that the phenomenon of strong Balmer lines in otherwise passive galaxies (commonly called E + A but renamed here as the k + a class) shows an order-of-magnitude increase in the rich cluster environment compared with a more modest increase in the field population. This suggests that the process or processes involved in producing k + a galaxies are either substantially more effective in the cluster environment or that this environment prolongs the visibility of this phase. A more detailed analysis and modeling of these data is presented in Poggianti et al. (1999ApJ...518..576P).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51#table4a</TD>
            <TD>2011-09-14T19:07:47Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/122/51</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/122/51&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/122/51</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/594/154 [1]</TD>
            <TD>160 square degree ROSAT survey (Mullis+, 2003)</TD>
            <TD>We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z_median_=0.25, and the median X-ray luminosity is L_X,median_=4.2x10^43^h_50_^2^erg/s (0.5-2.0keV). This is the largest high-redshift sample of X-ray-selected clusters published to date. There are 73 objects at z&gt;0.3 and 22 objects at z&gt;0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4x10^-13^erg/cm^2^/s. We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154#1</TD>
            <TD>2011-09-14T19:26:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/594/154</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/594/154</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/594/154 [2]</TD>
            <TD>160 square degree ROSAT survey (Mullis+, 2003)</TD>
            <TD>We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z_median_=0.25, and the median X-ray luminosity is L_X,median_=4.2x10^43^h_50_^2^erg/s (0.5-2.0keV). This is the largest high-redshift sample of X-ray-selected clusters published to date. There are 73 objects at z&gt;0.3 and 22 objects at z&gt;0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4x10^-13^erg/cm^2^/s. We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154#2</TD>
            <TD>2011-09-14T19:26:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/594/154&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/594/154</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/594/154 [table4]</TD>
            <TD>160 square degree ROSAT survey (Mullis+, 2003)</TD>
            <TD>We present the revised catalog of galaxy clusters detected as extended X-ray sources in the 160 Square Degree ROSAT Survey, including spectroscopic redshifts and X-ray luminosities for 200 of the 201 members. The median redshift is z_median_=0.25, and the median X-ray luminosity is L_X,median_=4.2x10^43^h_50_^2^erg/s (0.5-2.0keV). This is the largest high-redshift sample of X-ray-selected clusters published to date. There are 73 objects at z&gt;0.3 and 22 objects at z&gt;0.5 drawn from a statistically complete flux-limited survey with a median object flux of 1.4x10^-13^erg/cm^2^/s. We describe the optical follow-up of these clusters with an emphasis on our spectroscopy, which has yielded 155 cluster redshifts, 110 of which are presented here for the first time. These measurements, combined with 45 from the literature and other sources, provide near-complete spectroscopic coverage for our survey. We discuss the final optical identifications for the extended X-ray sources in the survey region and compare our results to similar X-ray cluster searches.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154#table4</TD>
            <TD>2011-09-14T19:26:21Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/594/154</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/594/154&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/594/154</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/674/857 [1]</TD>
            <TD>Radial velocities and CT1 magnitudes in M60 galaxy (Lee+, 2008)</TD>
            <TD>We used the Multi-Object Spectrograph (MOS) at the CFHT during two observing runs in 2002 February and 2003 May to obtain spectra of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857#1</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/674/857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/674/857 [2]</TD>
            <TD>Radial velocities and CT1 magnitudes in M60 galaxy (Lee+, 2008)</TD>
            <TD>We used the Multi-Object Spectrograph (MOS) at the CFHT during two observing runs in 2002 February and 2003 May to obtain spectra of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857#2</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/674/857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/674/857 [table4]</TD>
            <TD>Radial velocities and CT1 magnitudes in M60 galaxy (Lee+, 2008)</TD>
            <TD>We used the Multi-Object Spectrograph (MOS) at the CFHT during two observing runs in 2002 February and 2003 May to obtain spectra of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857#table4</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/674/857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/364/517 [1]</TD>
            <TD>HDF-N spiral and irregular galaxies (Rodighiero+, 2000)</TD>
            <TD>We analyze a morphologically-selected complete sample of 52 late-type (spiral and irregular) galaxies in the Hubble Deep Field North with total K-magnitudes brighter than K=20.47 and typical redshifts z~0.5 to 1.4. This sample exploits in particular the ultimate imaging quality achieved by HST in this field, allowing us to clearly disentangle the early- from late-type galaxy morphologies, based on accurate profiles of the surface brightness distributions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517#1</TD>
            <TD>2011-09-14T19:08:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/364/517</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/364/517</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/364/517 [2]</TD>
            <TD>HDF-N spiral and irregular galaxies (Rodighiero+, 2000)</TD>
            <TD>We analyze a morphologically-selected complete sample of 52 late-type (spiral and irregular) galaxies in the Hubble Deep Field North with total K-magnitudes brighter than K=20.47 and typical redshifts z~0.5 to 1.4. This sample exploits in particular the ultimate imaging quality achieved by HST in this field, allowing us to clearly disentangle the early- from late-type galaxy morphologies, based on accurate profiles of the surface brightness distributions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517#2</TD>
            <TD>2011-09-14T19:08:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/364/517&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/364/517</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/364/517 [table1]</TD>
            <TD>HDF-N spiral and irregular galaxies (Rodighiero+, 2000)</TD>
            <TD>We analyze a morphologically-selected complete sample of 52 late-type (spiral and irregular) galaxies in the Hubble Deep Field North with total K-magnitudes brighter than K=20.47 and typical redshifts z~0.5 to 1.4. This sample exploits in particular the ultimate imaging quality achieved by HST in this field, allowing us to clearly disentangle the early- from late-type galaxy morphologies, based on accurate profiles of the surface brightness distributions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517#table1</TD>
            <TD>2011-09-14T19:08:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/364/517&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/364/517</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/415/9 [1]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#1</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/415/9</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/415/9 [2]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#2</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/415/9&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/415/9 [table2]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#table2</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/415/9&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/415/9 [table1]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#table1</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/415/9&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/674/857 [1]</TD>
            <TD>Radial velocities and CT1 magnitudes in M60 galaxy (Lee+, 2008)</TD>
            <TD>We used the Multi-Object Spectrograph (MOS) at the CFHT during two observing runs in 2002 February and 2003 May to obtain spectra of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857#1</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/674/857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/674/857 [2]</TD>
            <TD>Radial velocities and CT1 magnitudes in M60 galaxy (Lee+, 2008)</TD>
            <TD>We used the Multi-Object Spectrograph (MOS) at the CFHT during two observing runs in 2002 February and 2003 May to obtain spectra of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857#2</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/674/857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/674/857 [table4]</TD>
            <TD>Radial velocities and CT1 magnitudes in M60 galaxy (Lee+, 2008)</TD>
            <TD>We used the Multi-Object Spectrograph (MOS) at the CFHT during two observing runs in 2002 February and 2003 May to obtain spectra of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857#table4</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/674/857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/364/517 [1]</TD>
            <TD>HDF-N spiral and irregular galaxies (Rodighiero+, 2000)</TD>
            <TD>We analyze a morphologically-selected complete sample of 52 late-type (spiral and irregular) galaxies in the Hubble Deep Field North with total K-magnitudes brighter than K=20.47 and typical redshifts z~0.5 to 1.4. This sample exploits in particular the ultimate imaging quality achieved by HST in this field, allowing us to clearly disentangle the early- from late-type galaxy morphologies, based on accurate profiles of the surface brightness distributions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517#1</TD>
            <TD>2011-09-14T19:08:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/364/517</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/364/517</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/364/517 [2]</TD>
            <TD>HDF-N spiral and irregular galaxies (Rodighiero+, 2000)</TD>
            <TD>We analyze a morphologically-selected complete sample of 52 late-type (spiral and irregular) galaxies in the Hubble Deep Field North with total K-magnitudes brighter than K=20.47 and typical redshifts z~0.5 to 1.4. This sample exploits in particular the ultimate imaging quality achieved by HST in this field, allowing us to clearly disentangle the early- from late-type galaxy morphologies, based on accurate profiles of the surface brightness distributions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517#2</TD>
            <TD>2011-09-14T19:08:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/364/517&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/364/517</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/364/517 [table1]</TD>
            <TD>HDF-N spiral and irregular galaxies (Rodighiero+, 2000)</TD>
            <TD>We analyze a morphologically-selected complete sample of 52 late-type (spiral and irregular) galaxies in the Hubble Deep Field North with total K-magnitudes brighter than K=20.47 and typical redshifts z~0.5 to 1.4. This sample exploits in particular the ultimate imaging quality achieved by HST in this field, allowing us to clearly disentangle the early- from late-type galaxy morphologies, based on accurate profiles of the surface brightness distributions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517#table1</TD>
            <TD>2011-09-14T19:08:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/364/517&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/364/517</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/415/9 [1]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#1</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/415/9</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/415/9 [2]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#2</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/415/9&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/415/9 [table2]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#table2</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/415/9&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/415/9 [table1]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#table1</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/415/9&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/674/857 [1]</TD>
            <TD>Radial velocities and CT1 magnitudes in M60 galaxy (Lee+, 2008)</TD>
            <TD>We used the Multi-Object Spectrograph (MOS) at the CFHT during two observing runs in 2002 February and 2003 May to obtain spectra of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857#1</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/674/857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/674/857 [2]</TD>
            <TD>Radial velocities and CT1 magnitudes in M60 galaxy (Lee+, 2008)</TD>
            <TD>We used the Multi-Object Spectrograph (MOS) at the CFHT during two observing runs in 2002 February and 2003 May to obtain spectra of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857#2</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/674/857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/674/857 [table4]</TD>
            <TD>Radial velocities and CT1 magnitudes in M60 galaxy (Lee+, 2008)</TD>
            <TD>We used the Multi-Object Spectrograph (MOS) at the CFHT during two observing runs in 2002 February and 2003 May to obtain spectra of the targets.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857#table4</TD>
            <TD>2011-09-14T20:57:46Z</TD>
            <TD>#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/674/857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/674/857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/674/857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/415/9 [1]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#1</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/415/9</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/415/9 [2]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#2</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/415/9&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/415/9 [table2]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#table2</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/415/9&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/415/9 [table1]</TD>
            <TD>Redshifts behind the Southern Milky Way (Woudt+, 2004)</TD>
            <TD>As part of our efforts to unveil extragalactic large-scale structures behind the southern Milky Way, we here present redshifts for 764 galaxies in the Hydra/Antlia, Crux and Great Attractor region (266{deg}&lt;=l&lt;=338{deg}, |b|&lt;=10{deg}), obtained with the Meudon-ESO Fibre Object Spectrograph (MEFOS) at the 3.6-m telescope of ESO. The observations are part of a redshift survey of partially obscured galaxies recorded in the course of a deep optical galaxy search behind the southern Milky Way (Kraan-Korteweg 2000, Cat. &lt;J/A+AS/141/123&gt;; Woudt &amp; Kraan-Korteweg 2001, Cat. &lt;J/A+A/380/441&gt;). A total of 947 galaxies have been observed, a small percentage of the spectra (N=109, 11.5%) were contaminated by foreground stars, and 74 galaxies (7.8%) were too faint to allow a reliable redshift determination. With MEFOS we obtained spectra down to the faintest galaxies of our optical galaxy survey, and hence probe large-scale structures out to larger distances (v&lt;=30000km/s) than our other redshift follow-ups using the 1.9-m telescope at the South African Astronomical Observatory (Kraan-Korteweg et al., 1995, Cat. &lt;J/A+A/297/617&gt;; Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) and the 64-m Parkes radio telescope (Kraan-Korteweg et al., 2002, Cat. &lt;J/A+A/391/887&gt;). The most distinct large-scale structures revealed in the southern Zone of Avoidance are discussed in context to known structures adjacent to the Milky Way.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9#table1</TD>
            <TD>2011-09-14T19:26:46Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/9</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/415/9&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/9</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/364/517 [1]</TD>
            <TD>HDF-N spiral and irregular galaxies (Rodighiero+, 2000)</TD>
            <TD>We analyze a morphologically-selected complete sample of 52 late-type (spiral and irregular) galaxies in the Hubble Deep Field North with total K-magnitudes brighter than K=20.47 and typical redshifts z~0.5 to 1.4. This sample exploits in particular the ultimate imaging quality achieved by HST in this field, allowing us to clearly disentangle the early- from late-type galaxy morphologies, based on accurate profiles of the surface brightness distributions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517#1</TD>
            <TD>2011-09-14T19:08:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/364/517</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/364/517</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/364/517 [2]</TD>
            <TD>HDF-N spiral and irregular galaxies (Rodighiero+, 2000)</TD>
            <TD>We analyze a morphologically-selected complete sample of 52 late-type (spiral and irregular) galaxies in the Hubble Deep Field North with total K-magnitudes brighter than K=20.47 and typical redshifts z~0.5 to 1.4. This sample exploits in particular the ultimate imaging quality achieved by HST in this field, allowing us to clearly disentangle the early- from late-type galaxy morphologies, based on accurate profiles of the surface brightness distributions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517#2</TD>
            <TD>2011-09-14T19:08:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/364/517&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/364/517</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/364/517 [table1]</TD>
            <TD>HDF-N spiral and irregular galaxies (Rodighiero+, 2000)</TD>
            <TD>We analyze a morphologically-selected complete sample of 52 late-type (spiral and irregular) galaxies in the Hubble Deep Field North with total K-magnitudes brighter than K=20.47 and typical redshifts z~0.5 to 1.4. This sample exploits in particular the ultimate imaging quality achieved by HST in this field, allowing us to clearly disentangle the early- from late-type galaxy morphologies, based on accurate profiles of the surface brightness distributions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517#table1</TD>
            <TD>2011-09-14T19:08:01Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/364/517</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/364/517&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/364/517</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/442/137 [1]</TD>
            <TD>HI observations of WHISP disk galaxies (Noordermeer+, 2005)</TD>
            <TD>All galaxies presented here were selected from the WHISP survey (Kamphuis et al., 1996, Cat. &lt;J/A+AS/116/15&gt;; van der Hulst et al., 2001, in Gas and Galaxy Evolution, ASP Conf. Ser. 240, 451).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137#1</TD>
            <TD>2011-09-14T20:57:54Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/442/137</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/137</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/442/137 [2]</TD>
            <TD>HI observations of WHISP disk galaxies (Noordermeer+, 2005)</TD>
            <TD>All galaxies presented here were selected from the WHISP survey (Kamphuis et al., 1996, Cat. &lt;J/A+AS/116/15&gt;; van der Hulst et al., 2001, in Gas and Galaxy Evolution, ASP Conf. Ser. 240, 451).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137#2</TD>
            <TD>2011-09-14T20:57:54Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/442/137&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/137</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/442/137 [whisp]</TD>
            <TD>HI observations of WHISP disk galaxies (Noordermeer+, 2005)</TD>
            <TD>All galaxies presented here were selected from the WHISP survey (Kamphuis et al., 1996, Cat. &lt;J/A+AS/116/15&gt;; van der Hulst et al., 2001, in Gas and Galaxy Evolution, ASP Conf. Ser. 240, 451).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137#whisp</TD>
            <TD>2011-09-14T20:57:54Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/442/137&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/137</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1954 [1]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#1</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1954</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1954 [2]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#2</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1954&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1954 [table3]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#table3</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1954&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1954 [table2]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#table2</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1954&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/366/508 [1]</TD>
            <TD>S Dor variables (van Genderen+, 2001)</TD>
            <TD>The goal in writing this paper is five fold: (1) to summarize the scientific achievements in the 20th century on S Dor variables (or LBVs); (2) to present an inventory of these variables in the Galaxy and the Magellanic Clouds with a description of their physical state and instability properties; (3) to emphasize the photometric achievements of the various types of instabilities. Generally this seems to be a neglected item resulting in a number of misunderstandings continuously wandering through literature; (4) to investigate the structure of the S Dor-area on the HR-diagram; (5) to estimate the total numbers of S Dor variables in the three stellar systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508#1</TD>
            <TD>2011-09-14T19:08:02Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/366/508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/366/508 [2]</TD>
            <TD>S Dor variables (van Genderen+, 2001)</TD>
            <TD>The goal in writing this paper is five fold: (1) to summarize the scientific achievements in the 20th century on S Dor variables (or LBVs); (2) to present an inventory of these variables in the Galaxy and the Magellanic Clouds with a description of their physical state and instability properties; (3) to emphasize the photometric achievements of the various types of instabilities. Generally this seems to be a neglected item resulting in a number of misunderstandings continuously wandering through literature; (4) to investigate the structure of the S Dor-area on the HR-diagram; (5) to estimate the total numbers of S Dor variables in the three stellar systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508#2</TD>
            <TD>2011-09-14T19:08:02Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/366/508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/508 [stars]</TD>
            <TD>S Dor variables (van Genderen+, 2001)</TD>
            <TD>The goal in writing this paper is five fold: (1) to summarize the scientific achievements in the 20th century on S Dor variables (or LBVs); (2) to present an inventory of these variables in the Galaxy and the Magellanic Clouds with a description of their physical state and instability properties; (3) to emphasize the photometric achievements of the various types of instabilities. Generally this seems to be a neglected item resulting in a number of misunderstandings continuously wandering through literature; (4) to investigate the structure of the S Dor-area on the HR-diagram; (5) to estimate the total numbers of S Dor variables in the three stellar systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508#stars</TD>
            <TD>2011-09-14T19:08:02Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1954 [1]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#1</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1954</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1954 [2]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#2</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1954&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1954 [table3]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#table3</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1954&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1954 [table2]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#table2</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1954&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/442/137 [1]</TD>
            <TD>HI observations of WHISP disk galaxies (Noordermeer+, 2005)</TD>
            <TD>All galaxies presented here were selected from the WHISP survey (Kamphuis et al., 1996, Cat. &lt;J/A+AS/116/15&gt;; van der Hulst et al., 2001, in Gas and Galaxy Evolution, ASP Conf. Ser. 240, 451).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137#1</TD>
            <TD>2011-09-14T20:57:54Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/442/137</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/137</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/442/137 [2]</TD>
            <TD>HI observations of WHISP disk galaxies (Noordermeer+, 2005)</TD>
            <TD>All galaxies presented here were selected from the WHISP survey (Kamphuis et al., 1996, Cat. &lt;J/A+AS/116/15&gt;; van der Hulst et al., 2001, in Gas and Galaxy Evolution, ASP Conf. Ser. 240, 451).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137#2</TD>
            <TD>2011-09-14T20:57:54Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/442/137&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/137</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/442/137 [whisp]</TD>
            <TD>HI observations of WHISP disk galaxies (Noordermeer+, 2005)</TD>
            <TD>All galaxies presented here were selected from the WHISP survey (Kamphuis et al., 1996, Cat. &lt;J/A+AS/116/15&gt;; van der Hulst et al., 2001, in Gas and Galaxy Evolution, ASP Conf. Ser. 240, 451).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137#whisp</TD>
            <TD>2011-09-14T20:57:54Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/442/137&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/137</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/366/508 [1]</TD>
            <TD>S Dor variables (van Genderen+, 2001)</TD>
            <TD>The goal in writing this paper is five fold: (1) to summarize the scientific achievements in the 20th century on S Dor variables (or LBVs); (2) to present an inventory of these variables in the Galaxy and the Magellanic Clouds with a description of their physical state and instability properties; (3) to emphasize the photometric achievements of the various types of instabilities. Generally this seems to be a neglected item resulting in a number of misunderstandings continuously wandering through literature; (4) to investigate the structure of the S Dor-area on the HR-diagram; (5) to estimate the total numbers of S Dor variables in the three stellar systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508#1</TD>
            <TD>2011-09-14T19:08:02Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/366/508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/366/508 [2]</TD>
            <TD>S Dor variables (van Genderen+, 2001)</TD>
            <TD>The goal in writing this paper is five fold: (1) to summarize the scientific achievements in the 20th century on S Dor variables (or LBVs); (2) to present an inventory of these variables in the Galaxy and the Magellanic Clouds with a description of their physical state and instability properties; (3) to emphasize the photometric achievements of the various types of instabilities. Generally this seems to be a neglected item resulting in a number of misunderstandings continuously wandering through literature; (4) to investigate the structure of the S Dor-area on the HR-diagram; (5) to estimate the total numbers of S Dor variables in the three stellar systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508#2</TD>
            <TD>2011-09-14T19:08:02Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/366/508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/508 [stars]</TD>
            <TD>S Dor variables (van Genderen+, 2001)</TD>
            <TD>The goal in writing this paper is five fold: (1) to summarize the scientific achievements in the 20th century on S Dor variables (or LBVs); (2) to present an inventory of these variables in the Galaxy and the Magellanic Clouds with a description of their physical state and instability properties; (3) to emphasize the photometric achievements of the various types of instabilities. Generally this seems to be a neglected item resulting in a number of misunderstandings continuously wandering through literature; (4) to investigate the structure of the S Dor-area on the HR-diagram; (5) to estimate the total numbers of S Dor variables in the three stellar systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508#stars</TD>
            <TD>2011-09-14T19:08:02Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1954 [1]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#1</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1954</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1954 [2]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#2</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1954&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1954 [table3]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#table3</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1954&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1954 [table2]</TD>
            <TD>1000 brightest HIPASS galaxies catalog (Ryan-Weber+, 2002)</TD>
            <TD>The HI Parkes All-Sky Survey (HIPASS) is a blind 21cm survey for extragalactic neutral hydrogen, covering the whole southern sky. The HIPASS Bright Galaxy Catalog (BGC) is a subset of HIPASS and contains the 1000 HI brightest (peak flux density) galaxies. Here we present the 138 HIPASS BGC galaxies that had no redshift measured prior to the Parkes multibeam HI surveys. Of the 138 galaxies, 87 are newly catalogued. Newly catalogued is defined as having no optical (or infrared) counterpart in the NASA/IPAC Extragalactic Database. Using the Digitized Sky Survey, we identify optical counterparts for almost half of the newly catalogued galaxies, which are typically of irregular or Magellanic morphological type. Several HI sources appear to be associated with compact groups or pairs of galaxies rather than an individual galaxy. The majority (57) of the newly catalogued galaxies lie within 10{deg} of the Galactic plane and are missing from optical surveys as a result of confusion with stars or dust extinction. This sample also includes newly catalogued galaxies first discovered by Henning et al. in the HI shallow survey of the zone of avoidance. The other 30 newly catalogued galaxies escaped detection because of their low surface brightness or optical compactness. Only one of these, HIPASS J0546-68, has no obvious optical counterpart, as it is obscured by the Large Magellanic Cloud. We find that the newly catalogued galaxies with |b|&gt;10{deg} are generally lower in HI mass and narrower in velocity width compared with the total HIPASS BGC. In contrast, newly catalogued galaxies behind the Milky Way are found to be statistically similar to the entire HIPASS BGC. In addition to these galaxies, the HIPASS BGC contains four previously unknown HI clouds. Description:</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954#table2</TD>
            <TD>2011-09-14T19:26:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1954</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1954&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1954</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/442/137 [1]</TD>
            <TD>HI observations of WHISP disk galaxies (Noordermeer+, 2005)</TD>
            <TD>All galaxies presented here were selected from the WHISP survey (Kamphuis et al., 1996, Cat. &lt;J/A+AS/116/15&gt;; van der Hulst et al., 2001, in Gas and Galaxy Evolution, ASP Conf. Ser. 240, 451).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137#1</TD>
            <TD>2011-09-14T20:57:54Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/442/137</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/137</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/442/137 [2]</TD>
            <TD>HI observations of WHISP disk galaxies (Noordermeer+, 2005)</TD>
            <TD>All galaxies presented here were selected from the WHISP survey (Kamphuis et al., 1996, Cat. &lt;J/A+AS/116/15&gt;; van der Hulst et al., 2001, in Gas and Galaxy Evolution, ASP Conf. Ser. 240, 451).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137#2</TD>
            <TD>2011-09-14T20:57:54Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/442/137&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/137</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/442/137 [whisp]</TD>
            <TD>HI observations of WHISP disk galaxies (Noordermeer+, 2005)</TD>
            <TD>All galaxies presented here were selected from the WHISP survey (Kamphuis et al., 1996, Cat. &lt;J/A+AS/116/15&gt;; van der Hulst et al., 2001, in Gas and Galaxy Evolution, ASP Conf. Ser. 240, 451).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137#whisp</TD>
            <TD>2011-09-14T20:57:54Z</TD>
            <TD>#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/442/137</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/442/137&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/442/137</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/366/508 [1]</TD>
            <TD>S Dor variables (van Genderen+, 2001)</TD>
            <TD>The goal in writing this paper is five fold: (1) to summarize the scientific achievements in the 20th century on S Dor variables (or LBVs); (2) to present an inventory of these variables in the Galaxy and the Magellanic Clouds with a description of their physical state and instability properties; (3) to emphasize the photometric achievements of the various types of instabilities. Generally this seems to be a neglected item resulting in a number of misunderstandings continuously wandering through literature; (4) to investigate the structure of the S Dor-area on the HR-diagram; (5) to estimate the total numbers of S Dor variables in the three stellar systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508#1</TD>
            <TD>2011-09-14T19:08:02Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/366/508</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/508</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/366/508 [2]</TD>
            <TD>S Dor variables (van Genderen+, 2001)</TD>
            <TD>The goal in writing this paper is five fold: (1) to summarize the scientific achievements in the 20th century on S Dor variables (or LBVs); (2) to present an inventory of these variables in the Galaxy and the Magellanic Clouds with a description of their physical state and instability properties; (3) to emphasize the photometric achievements of the various types of instabilities. Generally this seems to be a neglected item resulting in a number of misunderstandings continuously wandering through literature; (4) to investigate the structure of the S Dor-area on the HR-diagram; (5) to estimate the total numbers of S Dor variables in the three stellar systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508#2</TD>
            <TD>2011-09-14T19:08:02Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/366/508&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/508</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/366/508 [stars]</TD>
            <TD>S Dor variables (van Genderen+, 2001)</TD>
            <TD>The goal in writing this paper is five fold: (1) to summarize the scientific achievements in the 20th century on S Dor variables (or LBVs); (2) to present an inventory of these variables in the Galaxy and the Magellanic Clouds with a description of their physical state and instability properties; (3) to emphasize the photometric achievements of the various types of instabilities. Generally this seems to be a neglected item resulting in a number of misunderstandings continuously wandering through literature; (4) to investigate the structure of the S Dor-area on the HR-diagram; (5) to estimate the total numbers of S Dor variables in the three stellar systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508#stars</TD>
            <TD>2011-09-14T19:08:02Z</TD>
            <TD>#Stars#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/366/508</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/366/508&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/366/508</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/659/1241 [1]</TD>
            <TD>Stellar variability in Galactic Center (Rafelski+, 2007)</TD>
            <TD>++++Lrecl of file 'table2.dat' (90) increased to 92 %B K-band ({lambda}_0_=2.2um, {DELTA}{lambda}=0.4um) speckle imaging observations of the Galaxy's central stellar cluster were obtained with the W.M. Keck I 10m telescope using the facility near-infrared camera (NIRC). Observations taken from 1995 to 2004 have been described in detail elsewhere (Ghez et al., 1998ApJ...509..678G, 2000Natur.407..349G, 2005ApJ...620..744G; Lu et al., 2005ApJ...625L..51L), and new observations on 2005 April 24-25 were conducted in a similar manner, resulting in diffraction-limited images.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241#1</TD>
            <TD>2011-09-14T21:01:22Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/659/1241</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1241</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/659/1241 [2]</TD>
            <TD>Stellar variability in Galactic Center (Rafelski+, 2007)</TD>
            <TD>++++Lrecl of file 'table2.dat' (90) increased to 92 %B K-band ({lambda}_0_=2.2um, {DELTA}{lambda}=0.4um) speckle imaging observations of the Galaxy's central stellar cluster were obtained with the W.M. Keck I 10m telescope using the facility near-infrared camera (NIRC). Observations taken from 1995 to 2004 have been described in detail elsewhere (Ghez et al., 1998ApJ...509..678G, 2000Natur.407..349G, 2005ApJ...620..744G; Lu et al., 2005ApJ...625L..51L), and new observations on 2005 April 24-25 were conducted in a similar manner, resulting in diffraction-limited images.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241#2</TD>
            <TD>2011-09-14T21:01:22Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/659/1241&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1241</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/659/1241 [GCstars]</TD>
            <TD>Stellar variability in Galactic Center (Rafelski+, 2007)</TD>
            <TD>++++Lrecl of file 'table2.dat' (90) increased to 92 %B K-band ({lambda}_0_=2.2um, {DELTA}{lambda}=0.4um) speckle imaging observations of the Galaxy's central stellar cluster were obtained with the W.M. Keck I 10m telescope using the facility near-infrared camera (NIRC). Observations taken from 1995 to 2004 have been described in detail elsewhere (Ghez et al., 1998ApJ...509..678G, 2000Natur.407..349G, 2005ApJ...620..744G; Lu et al., 2005ApJ...625L..51L), and new observations on 2005 April 24-25 were conducted in a similar manner, resulting in diffraction-limited images.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241#GCstars</TD>
            <TD>2011-09-14T21:01:22Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/659/1241&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1241</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/414/905 [1]</TD>
            <TD>H-band photometry in Pisces-Perseus disk galaxies (Hunt+, 2004)</TD>
            <TD>We present the results of the photometric deconvolution of the sample galaxies. The given surface brightnesses are corrected to face-on assuming full transparency. No correction is applied for internal extinction. Magnitudes and surface brightnesses are corrected for extinction within our Galaxy and for redshift dimming.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905#1</TD>
            <TD>2011-09-14T19:27:03Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/414/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/414/905 [2]</TD>
            <TD>H-band photometry in Pisces-Perseus disk galaxies (Hunt+, 2004)</TD>
            <TD>We present the results of the photometric deconvolution of the sample galaxies. The given surface brightnesses are corrected to face-on assuming full transparency. No correction is applied for internal extinction. Magnitudes and surface brightnesses are corrected for extinction within our Galaxy and for redshift dimming.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905#2</TD>
            <TD>2011-09-14T19:27:03Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/414/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/414/905 [table1]</TD>
            <TD>H-band photometry in Pisces-Perseus disk galaxies (Hunt+, 2004)</TD>
            <TD>We present the results of the photometric deconvolution of the sample galaxies. The given surface brightnesses are corrected to face-on assuming full transparency. No correction is applied for internal extinction. Magnitudes and surface brightnesses are corrected for extinction within our Galaxy and for redshift dimming.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905#table1</TD>
            <TD>2011-09-14T19:27:03Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/414/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/659/1241 [1]</TD>
            <TD>Stellar variability in Galactic Center (Rafelski+, 2007)</TD>
            <TD>++++Lrecl of file 'table2.dat' (90) increased to 92 %B K-band ({lambda}_0_=2.2um, {DELTA}{lambda}=0.4um) speckle imaging observations of the Galaxy's central stellar cluster were obtained with the W.M. Keck I 10m telescope using the facility near-infrared camera (NIRC). Observations taken from 1995 to 2004 have been described in detail elsewhere (Ghez et al., 1998ApJ...509..678G, 2000Natur.407..349G, 2005ApJ...620..744G; Lu et al., 2005ApJ...625L..51L), and new observations on 2005 April 24-25 were conducted in a similar manner, resulting in diffraction-limited images.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241#1</TD>
            <TD>2011-09-14T21:01:22Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/659/1241</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1241</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/659/1241 [2]</TD>
            <TD>Stellar variability in Galactic Center (Rafelski+, 2007)</TD>
            <TD>++++Lrecl of file 'table2.dat' (90) increased to 92 %B K-band ({lambda}_0_=2.2um, {DELTA}{lambda}=0.4um) speckle imaging observations of the Galaxy's central stellar cluster were obtained with the W.M. Keck I 10m telescope using the facility near-infrared camera (NIRC). Observations taken from 1995 to 2004 have been described in detail elsewhere (Ghez et al., 1998ApJ...509..678G, 2000Natur.407..349G, 2005ApJ...620..744G; Lu et al., 2005ApJ...625L..51L), and new observations on 2005 April 24-25 were conducted in a similar manner, resulting in diffraction-limited images.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241#2</TD>
            <TD>2011-09-14T21:01:22Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/659/1241&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1241</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/659/1241 [GCstars]</TD>
            <TD>Stellar variability in Galactic Center (Rafelski+, 2007)</TD>
            <TD>++++Lrecl of file 'table2.dat' (90) increased to 92 %B K-band ({lambda}_0_=2.2um, {DELTA}{lambda}=0.4um) speckle imaging observations of the Galaxy's central stellar cluster were obtained with the W.M. Keck I 10m telescope using the facility near-infrared camera (NIRC). Observations taken from 1995 to 2004 have been described in detail elsewhere (Ghez et al., 1998ApJ...509..678G, 2000Natur.407..349G, 2005ApJ...620..744G; Lu et al., 2005ApJ...625L..51L), and new observations on 2005 April 24-25 were conducted in a similar manner, resulting in diffraction-limited images.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241#GCstars</TD>
            <TD>2011-09-14T21:01:22Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/659/1241&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1241</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/414/905 [1]</TD>
            <TD>H-band photometry in Pisces-Perseus disk galaxies (Hunt+, 2004)</TD>
            <TD>We present the results of the photometric deconvolution of the sample galaxies. The given surface brightnesses are corrected to face-on assuming full transparency. No correction is applied for internal extinction. Magnitudes and surface brightnesses are corrected for extinction within our Galaxy and for redshift dimming.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905#1</TD>
            <TD>2011-09-14T19:27:03Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/414/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/414/905 [2]</TD>
            <TD>H-band photometry in Pisces-Perseus disk galaxies (Hunt+, 2004)</TD>
            <TD>We present the results of the photometric deconvolution of the sample galaxies. The given surface brightnesses are corrected to face-on assuming full transparency. No correction is applied for internal extinction. Magnitudes and surface brightnesses are corrected for extinction within our Galaxy and for redshift dimming.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905#2</TD>
            <TD>2011-09-14T19:27:03Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/414/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/414/905 [table1]</TD>
            <TD>H-band photometry in Pisces-Perseus disk galaxies (Hunt+, 2004)</TD>
            <TD>We present the results of the photometric deconvolution of the sample galaxies. The given surface brightnesses are corrected to face-on assuming full transparency. No correction is applied for internal extinction. Magnitudes and surface brightnesses are corrected for extinction within our Galaxy and for redshift dimming.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905#table1</TD>
            <TD>2011-09-14T19:27:03Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/414/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/372/364 [1]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#1</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/372/364</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/372/364 [2]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#2</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/372/364&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table12]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table12</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table9]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table9</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table8]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table8</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table10]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table10</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table7]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table7</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table11]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table11</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/659/1241 [1]</TD>
            <TD>Stellar variability in Galactic Center (Rafelski+, 2007)</TD>
            <TD>++++Lrecl of file 'table2.dat' (90) increased to 92 %B K-band ({lambda}_0_=2.2um, {DELTA}{lambda}=0.4um) speckle imaging observations of the Galaxy's central stellar cluster were obtained with the W.M. Keck I 10m telescope using the facility near-infrared camera (NIRC). Observations taken from 1995 to 2004 have been described in detail elsewhere (Ghez et al., 1998ApJ...509..678G, 2000Natur.407..349G, 2005ApJ...620..744G; Lu et al., 2005ApJ...625L..51L), and new observations on 2005 April 24-25 were conducted in a similar manner, resulting in diffraction-limited images.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241#1</TD>
            <TD>2011-09-14T21:01:22Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/659/1241</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1241</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/659/1241 [2]</TD>
            <TD>Stellar variability in Galactic Center (Rafelski+, 2007)</TD>
            <TD>++++Lrecl of file 'table2.dat' (90) increased to 92 %B K-band ({lambda}_0_=2.2um, {DELTA}{lambda}=0.4um) speckle imaging observations of the Galaxy's central stellar cluster were obtained with the W.M. Keck I 10m telescope using the facility near-infrared camera (NIRC). Observations taken from 1995 to 2004 have been described in detail elsewhere (Ghez et al., 1998ApJ...509..678G, 2000Natur.407..349G, 2005ApJ...620..744G; Lu et al., 2005ApJ...625L..51L), and new observations on 2005 April 24-25 were conducted in a similar manner, resulting in diffraction-limited images.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241#2</TD>
            <TD>2011-09-14T21:01:22Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/659/1241&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1241</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/659/1241 [GCstars]</TD>
            <TD>Stellar variability in Galactic Center (Rafelski+, 2007)</TD>
            <TD>++++Lrecl of file 'table2.dat' (90) increased to 92 %B K-band ({lambda}_0_=2.2um, {DELTA}{lambda}=0.4um) speckle imaging observations of the Galaxy's central stellar cluster were obtained with the W.M. Keck I 10m telescope using the facility near-infrared camera (NIRC). Observations taken from 1995 to 2004 have been described in detail elsewhere (Ghez et al., 1998ApJ...509..678G, 2000Natur.407..349G, 2005ApJ...620..744G; Lu et al., 2005ApJ...625L..51L), and new observations on 2005 April 24-25 were conducted in a similar manner, resulting in diffraction-limited images.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241#GCstars</TD>
            <TD>2011-09-14T21:01:22Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/659/1241</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/659/1241&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/659/1241</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/414/905 [1]</TD>
            <TD>H-band photometry in Pisces-Perseus disk galaxies (Hunt+, 2004)</TD>
            <TD>We present the results of the photometric deconvolution of the sample galaxies. The given surface brightnesses are corrected to face-on assuming full transparency. No correction is applied for internal extinction. Magnitudes and surface brightnesses are corrected for extinction within our Galaxy and for redshift dimming.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905#1</TD>
            <TD>2011-09-14T19:27:03Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/414/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/414/905 [2]</TD>
            <TD>H-band photometry in Pisces-Perseus disk galaxies (Hunt+, 2004)</TD>
            <TD>We present the results of the photometric deconvolution of the sample galaxies. The given surface brightnesses are corrected to face-on assuming full transparency. No correction is applied for internal extinction. Magnitudes and surface brightnesses are corrected for extinction within our Galaxy and for redshift dimming.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905#2</TD>
            <TD>2011-09-14T19:27:03Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/414/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/414/905 [table1]</TD>
            <TD>H-band photometry in Pisces-Perseus disk galaxies (Hunt+, 2004)</TD>
            <TD>We present the results of the photometric deconvolution of the sample galaxies. The given surface brightnesses are corrected to face-on assuming full transparency. No correction is applied for internal extinction. Magnitudes and surface brightnesses are corrected for extinction within our Galaxy and for redshift dimming.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905#table1</TD>
            <TD>2011-09-14T19:27:03Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/414/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/414/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/414/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/372/364 [1]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#1</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/372/364</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/372/364 [2]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#2</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/372/364&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table12]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table12</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table9]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table9</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table8]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table8</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table10]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table10</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table7]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table7</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table11]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table11</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/197/21 [1]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)</TD>
            <TD>All the images for CGS were taken with the du Pont 2.5m telescope, during the period 2003 February to 2006 June, spread over 69 nights and nine observing runs. Table 2 gives a log of the observations. Each galaxy was imaged in the Johnson B and V and Kron-Cousins R and I filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21#1</TD>
            <TD>2012-02-20T16:04:40Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/197/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/197/21 [2]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)</TD>
            <TD>All the images for CGS were taken with the du Pont 2.5m telescope, during the period 2003 February to 2006 June, spread over 69 nights and nine observing runs. Table 2 gives a log of the observations. Each galaxy was imaged in the Johnson B and V and Kron-Cousins R and I filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21#2</TD>
            <TD>2012-02-20T16:04:40Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/197/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/197/21 [cgs]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)</TD>
            <TD>All the images for CGS were taken with the du Pont 2.5m telescope, during the period 2003 February to 2006 June, spread over 69 nights and nine observing runs. Table 2 gives a log of the observations. Each galaxy was imaged in the Johnson B and V and Kron-Cousins R and I filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21#cgs</TD>
            <TD>2012-02-20T16:04:40Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/197/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/416/111 [1]</TD>
            <TD>C stars in Wolf-Lundmark-Melotte galaxy (Battinelli+, 2004)</TD>
            <TD>We list the apparent I magnitude, (R-I) and (CN-TiO) colour indices of 149 carbon stars identified in WLM. The observations were obtained with the CFH12K camera attached to the CFHT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111#1</TD>
            <TD>2011-09-14T19:27:05Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/416/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/416/111 [2]</TD>
            <TD>C stars in Wolf-Lundmark-Melotte galaxy (Battinelli+, 2004)</TD>
            <TD>We list the apparent I magnitude, (R-I) and (CN-TiO) colour indices of 149 carbon stars identified in WLM. The observations were obtained with the CFH12K camera attached to the CFHT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111#2</TD>
            <TD>2011-09-14T19:27:05Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/416/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/416/111 [table2]</TD>
            <TD>C stars in Wolf-Lundmark-Melotte galaxy (Battinelli+, 2004)</TD>
            <TD>We list the apparent I magnitude, (R-I) and (CN-TiO) colour indices of 149 carbon stars identified in WLM. The observations were obtained with the CFH12K camera attached to the CFHT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111#table2</TD>
            <TD>2011-09-14T19:27:05Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/416/111&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/111</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/197/21 [1]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)</TD>
            <TD>All the images for CGS were taken with the du Pont 2.5m telescope, during the period 2003 February to 2006 June, spread over 69 nights and nine observing runs. Table 2 gives a log of the observations. Each galaxy was imaged in the Johnson B and V and Kron-Cousins R and I filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21#1</TD>
            <TD>2012-02-20T16:04:40Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/197/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/197/21 [2]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)</TD>
            <TD>All the images for CGS were taken with the du Pont 2.5m telescope, during the period 2003 February to 2006 June, spread over 69 nights and nine observing runs. Table 2 gives a log of the observations. Each galaxy was imaged in the Johnson B and V and Kron-Cousins R and I filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21#2</TD>
            <TD>2012-02-20T16:04:40Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/197/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/197/21 [cgs]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)</TD>
            <TD>All the images for CGS were taken with the du Pont 2.5m telescope, during the period 2003 February to 2006 June, spread over 69 nights and nine observing runs. Table 2 gives a log of the observations. Each galaxy was imaged in the Johnson B and V and Kron-Cousins R and I filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21#cgs</TD>
            <TD>2012-02-20T16:04:40Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/197/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/372/364 [1]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#1</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/372/364</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/372/364 [2]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#2</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/372/364&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table12]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table12</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table9]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table9</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table8]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table8</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table10]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table10</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table7]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table7</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/372/364 [table11]</TD>
            <TD>ISO FIRBACK Source Catalog at 170um (Dole+, 2001)</TD>
            <TD>The FIRBACK (Far Infrared BACKground) survey is one of the deepest imaging surveys carried out at 170{mu}m with ISOPHOT onboard ISO, and is aimed at the study of the structure of the Cosmic Far Infrared Background. This paper provides the analysis of resolved sources. After a validated process of data reduction and calibration, we perform intensive simulations to optimize the source extraction, measure the confusion noise ({sigma}_c_=45mJy), and give the photometric and astrometric accuracies. 196 galaxies with flux S&gt;3{sigma}_c_ are detected in the area of 3.89 square degrees. Counts of sources with flux S&gt;4{sigma}_c_ present a steep slope of 3.3+/-0.6 on a differential ``logN-logS'' plot between 180 and 500mJy. As a consequence, the confusion level is high and will impact dramatically on future IR deep surveys. This strong evolution, compared with a slope of 2.5 from Euclidian geometry, is in line with models implying a strongly evolving Luminous Infrared Galaxy population. The resolved sources account for less than 10% of the Cosmic Infrared Background at 170{mu}m, which is expected to be resolved into sources in the 1 to 10mJy range.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364#table11</TD>
            <TD>2011-09-14T19:08:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-May-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/372/364</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/372/364&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/372/364</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/416/111 [1]</TD>
            <TD>C stars in Wolf-Lundmark-Melotte galaxy (Battinelli+, 2004)</TD>
            <TD>We list the apparent I magnitude, (R-I) and (CN-TiO) colour indices of 149 carbon stars identified in WLM. The observations were obtained with the CFH12K camera attached to the CFHT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111#1</TD>
            <TD>2011-09-14T19:27:05Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/416/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/416/111 [2]</TD>
            <TD>C stars in Wolf-Lundmark-Melotte galaxy (Battinelli+, 2004)</TD>
            <TD>We list the apparent I magnitude, (R-I) and (CN-TiO) colour indices of 149 carbon stars identified in WLM. The observations were obtained with the CFH12K camera attached to the CFHT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111#2</TD>
            <TD>2011-09-14T19:27:05Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/416/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/416/111 [table2]</TD>
            <TD>C stars in Wolf-Lundmark-Melotte galaxy (Battinelli+, 2004)</TD>
            <TD>We list the apparent I magnitude, (R-I) and (CN-TiO) colour indices of 149 carbon stars identified in WLM. The observations were obtained with the CFH12K camera attached to the CFHT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111#table2</TD>
            <TD>2011-09-14T19:27:05Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/416/111&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/111</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/197/21 [1]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)</TD>
            <TD>All the images for CGS were taken with the du Pont 2.5m telescope, during the period 2003 February to 2006 June, spread over 69 nights and nine observing runs. Table 2 gives a log of the observations. Each galaxy was imaged in the Johnson B and V and Kron-Cousins R and I filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21#1</TD>
            <TD>2012-02-20T16:04:40Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/197/21</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/21</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/197/21 [2]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)</TD>
            <TD>All the images for CGS were taken with the du Pont 2.5m telescope, during the period 2003 February to 2006 June, spread over 69 nights and nine observing runs. Table 2 gives a log of the observations. Each galaxy was imaged in the Johnson B and V and Kron-Cousins R and I filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21#2</TD>
            <TD>2012-02-20T16:04:40Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/197/21&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/21</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/197/21 [cgs]</TD>
            <TD>The Carnegie-Irvine Galaxy Survey (CGS). I. (Ho+, 2011)</TD>
            <TD>All the images for CGS were taken with the du Pont 2.5m telescope, during the period 2003 February to 2006 June, spread over 69 nights and nine observing runs. Table 2 gives a log of the observations. Each galaxy was imaged in the Johnson B and V and Kron-Cousins R and I filters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21#cgs</TD>
            <TD>2012-02-20T16:04:40Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/197/21</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/197/21&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/197/21</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/335/85 [1]</TD>
            <TD>HST photometry of ESO 338-IG04 globular clusters (Oestlin+, 1998)</TD>
            <TD>Multicolour images of the starbursting metal poor blue compact galaxy ESO 338-IG04 have been obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope. In the images we find numerous point-like sources concentrated towards the main body of the galaxy, which we identify as globular cluster candidates. We show that these objects are physically associated with the galaxy and that they are spatially extended. Given their high intrinsic luminosities, these objects cannot be individual stars. Using photometric evolution models we show that the objects constitute a rich population of massive star clusters with ages ranging from a few Myr to 10Gyr, and masses ranging from 10^4^ to more than 10^7^M_{sun}_. There are peaks in the age distribution of the clusters: one with objects &lt;=30Myr, one at ~100Myr, one at ~600Myr, one to two at 2.5-5Gyr and one at ~10Gyr. The youngest objects are predominantly found in the crowded starburst region. They have properties which agree with what is expected for young globular clusters, although it cannot be excluded that some of them may be dissolved or disrupted. For objects older than a few times 10Myr, the only plausible explanation is that these are globular clusters. The galaxy presently appears to be involved in a merger, which is the probable cause of the present globular cluster formation. The presence of a numerous intermediate age (2.5 to 5Gyr) population of globular clusters, suggests that a previous merger might have occurred. As the starburst fades, this galaxy will become very rich in globular clusters. Transforming all objects to an age comparable to that of Milky Way globular clusters reveals a luminosity function similar to the Galactic. We suggest that this galaxy is the result of a merger between a dwarf elliptical and a gas rich dwarf. The possibility of dating the globular clusters offers an efficient way of studying the history of violent star formation in this and similar galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/85#1</TD>
            <TD>2011-09-14T19:09:21Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/335/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/335/85 [2]</TD>
            <TD>HST photometry of ESO 338-IG04 globular clusters (Oestlin+, 1998)</TD>
            <TD>Multicolour images of the starbursting metal poor blue compact galaxy ESO 338-IG04 have been obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope. In the images we find numerous point-like sources concentrated towards the main body of the galaxy, which we identify as globular cluster candidates. We show that these objects are physically associated with the galaxy and that they are spatially extended. Given their high intrinsic luminosities, these objects cannot be individual stars. Using photometric evolution models we show that the objects constitute a rich population of massive star clusters with ages ranging from a few Myr to 10Gyr, and masses ranging from 10^4^ to more than 10^7^M_{sun}_. There are peaks in the age distribution of the clusters: one with objects &lt;=30Myr, one at ~100Myr, one at ~600Myr, one to two at 2.5-5Gyr and one at ~10Gyr. The youngest objects are predominantly found in the crowded starburst region. They have properties which agree with what is expected for young globular clusters, although it cannot be excluded that some of them may be dissolved or disrupted. For objects older than a few times 10Myr, the only plausible explanation is that these are globular clusters. The galaxy presently appears to be involved in a merger, which is the probable cause of the present globular cluster formation. The presence of a numerous intermediate age (2.5 to 5Gyr) population of globular clusters, suggests that a previous merger might have occurred. As the starburst fades, this galaxy will become very rich in globular clusters. Transforming all objects to an age comparable to that of Milky Way globular clusters reveals a luminosity function similar to the Galactic. We suggest that this galaxy is the result of a merger between a dwarf elliptical and a gas rich dwarf. The possibility of dating the globular clusters offers an efficient way of studying the history of violent star formation in this and similar galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/85#2</TD>
            <TD>2011-09-14T19:09:21Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/335/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/416/111 [1]</TD>
            <TD>C stars in Wolf-Lundmark-Melotte galaxy (Battinelli+, 2004)</TD>
            <TD>We list the apparent I magnitude, (R-I) and (CN-TiO) colour indices of 149 carbon stars identified in WLM. The observations were obtained with the CFH12K camera attached to the CFHT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111#1</TD>
            <TD>2011-09-14T19:27:05Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/416/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/416/111 [2]</TD>
            <TD>C stars in Wolf-Lundmark-Melotte galaxy (Battinelli+, 2004)</TD>
            <TD>We list the apparent I magnitude, (R-I) and (CN-TiO) colour indices of 149 carbon stars identified in WLM. The observations were obtained with the CFH12K camera attached to the CFHT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111#2</TD>
            <TD>2011-09-14T19:27:05Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/416/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/416/111 [table2]</TD>
            <TD>C stars in Wolf-Lundmark-Melotte galaxy (Battinelli+, 2004)</TD>
            <TD>We list the apparent I magnitude, (R-I) and (CN-TiO) colour indices of 149 carbon stars identified in WLM. The observations were obtained with the CFH12K camera attached to the CFHT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111#table2</TD>
            <TD>2011-09-14T19:27:05Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/111</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/416/111&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/111</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/538/A100 [1]</TD>
            <TD>Abundances of Carina red giant branch (Lemasle+, 2012)</TD>
            <TD>We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R~20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100#1</TD>
            <TD>2012-02-09T12:56:39Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/538/A100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/538/A100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/538/A100 [2]</TD>
            <TD>Abundances of Carina red giant branch (Lemasle+, 2012)</TD>
            <TD>We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R~20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100#2</TD>
            <TD>2012-02-09T12:56:39Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/538/A100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/538/A100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/538/A100 [table3]</TD>
            <TD>Abundances of Carina red giant branch (Lemasle+, 2012)</TD>
            <TD>We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R~20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100#table3</TD>
            <TD>2012-02-09T12:56:39Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/538/A100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/538/A100</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/335/85 [1]</TD>
            <TD>HST photometry of ESO 338-IG04 globular clusters (Oestlin+, 1998)</TD>
            <TD>Multicolour images of the starbursting metal poor blue compact galaxy ESO 338-IG04 have been obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope. In the images we find numerous point-like sources concentrated towards the main body of the galaxy, which we identify as globular cluster candidates. We show that these objects are physically associated with the galaxy and that they are spatially extended. Given their high intrinsic luminosities, these objects cannot be individual stars. Using photometric evolution models we show that the objects constitute a rich population of massive star clusters with ages ranging from a few Myr to 10Gyr, and masses ranging from 10^4^ to more than 10^7^M_{sun}_. There are peaks in the age distribution of the clusters: one with objects &lt;=30Myr, one at ~100Myr, one at ~600Myr, one to two at 2.5-5Gyr and one at ~10Gyr. The youngest objects are predominantly found in the crowded starburst region. They have properties which agree with what is expected for young globular clusters, although it cannot be excluded that some of them may be dissolved or disrupted. For objects older than a few times 10Myr, the only plausible explanation is that these are globular clusters. The galaxy presently appears to be involved in a merger, which is the probable cause of the present globular cluster formation. The presence of a numerous intermediate age (2.5 to 5Gyr) population of globular clusters, suggests that a previous merger might have occurred. As the starburst fades, this galaxy will become very rich in globular clusters. Transforming all objects to an age comparable to that of Milky Way globular clusters reveals a luminosity function similar to the Galactic. We suggest that this galaxy is the result of a merger between a dwarf elliptical and a gas rich dwarf. The possibility of dating the globular clusters offers an efficient way of studying the history of violent star formation in this and similar galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/85#1</TD>
            <TD>2011-09-14T19:09:21Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/335/85</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/85</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/335/85 [2]</TD>
            <TD>HST photometry of ESO 338-IG04 globular clusters (Oestlin+, 1998)</TD>
            <TD>Multicolour images of the starbursting metal poor blue compact galaxy ESO 338-IG04 have been obtained with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope. In the images we find numerous point-like sources concentrated towards the main body of the galaxy, which we identify as globular cluster candidates. We show that these objects are physically associated with the galaxy and that they are spatially extended. Given their high intrinsic luminosities, these objects cannot be individual stars. Using photometric evolution models we show that the objects constitute a rich population of massive star clusters with ages ranging from a few Myr to 10Gyr, and masses ranging from 10^4^ to more than 10^7^M_{sun}_. There are peaks in the age distribution of the clusters: one with objects &lt;=30Myr, one at ~100Myr, one at ~600Myr, one to two at 2.5-5Gyr and one at ~10Gyr. The youngest objects are predominantly found in the crowded starburst region. They have properties which agree with what is expected for young globular clusters, although it cannot be excluded that some of them may be dissolved or disrupted. For objects older than a few times 10Myr, the only plausible explanation is that these are globular clusters. The galaxy presently appears to be involved in a merger, which is the probable cause of the present globular cluster formation. The presence of a numerous intermediate age (2.5 to 5Gyr) population of globular clusters, suggests that a previous merger might have occurred. As the starburst fades, this galaxy will become very rich in globular clusters. Transforming all objects to an age comparable to that of Milky Way globular clusters reveals a luminosity function similar to the Galactic. We suggest that this galaxy is the result of a merger between a dwarf elliptical and a gas rich dwarf. The possibility of dating the globular clusters offers an efficient way of studying the history of violent star formation in this and similar galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/85#2</TD>
            <TD>2011-09-14T19:09:21Z</TD>
            <TD>#Globular_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jun-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/335/85</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/335/85&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/335/85</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/420/147 [1]</TD>
            <TD>Velocity in 6 spiral galaxies (Blais-ouellette+, 2004)</TD>
            <TD>H{alpha} rotation curves for 6 spiral galaxies are presented. The galaxies are UGC 2259, NGC 2403, NGC 6946, NGC 5055, NGC 2841, NGC 5985. For each galaxy each row of the table describes the data at a given distance from the galactic center.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/147#1</TD>
            <TD>2011-09-14T19:28:44Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/420/147</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/147</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/420/147 [2]</TD>
            <TD>Velocity in 6 spiral galaxies (Blais-ouellette+, 2004)</TD>
            <TD>H{alpha} rotation curves for 6 spiral galaxies are presented. The galaxies are UGC 2259, NGC 2403, NGC 6946, NGC 5055, NGC 2841, NGC 5985. For each galaxy each row of the table describes the data at a given distance from the galactic center.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/147#2</TD>
            <TD>2011-09-14T19:28:44Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/420/147&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/147</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/538/A100 [1]</TD>
            <TD>Abundances of Carina red giant branch (Lemasle+, 2012)</TD>
            <TD>We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R~20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100#1</TD>
            <TD>2012-02-09T12:56:39Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/538/A100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/538/A100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/538/A100 [2]</TD>
            <TD>Abundances of Carina red giant branch (Lemasle+, 2012)</TD>
            <TD>We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R~20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100#2</TD>
            <TD>2012-02-09T12:56:39Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/538/A100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/538/A100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/538/A100 [table3]</TD>
            <TD>Abundances of Carina red giant branch (Lemasle+, 2012)</TD>
            <TD>We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R~20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100#table3</TD>
            <TD>2012-02-09T12:56:39Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/538/A100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/538/A100</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/279/567 [1]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#1</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/279/567</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/279/567 [2]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#2</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/279/567&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/279/567 [table4]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#table4</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/279/567&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/279/567 [table3]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#table3</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/279/567&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/420/147 [1]</TD>
            <TD>Velocity in 6 spiral galaxies (Blais-ouellette+, 2004)</TD>
            <TD>H{alpha} rotation curves for 6 spiral galaxies are presented. The galaxies are UGC 2259, NGC 2403, NGC 6946, NGC 5055, NGC 2841, NGC 5985. For each galaxy each row of the table describes the data at a given distance from the galactic center.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/147#1</TD>
            <TD>2011-09-14T19:28:44Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/420/147</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/147</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/420/147 [2]</TD>
            <TD>Velocity in 6 spiral galaxies (Blais-ouellette+, 2004)</TD>
            <TD>H{alpha} rotation curves for 6 spiral galaxies are presented. The galaxies are UGC 2259, NGC 2403, NGC 6946, NGC 5055, NGC 2841, NGC 5985. For each galaxy each row of the table describes the data at a given distance from the galactic center.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/147#2</TD>
            <TD>2011-09-14T19:28:44Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/420/147</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/420/147&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/420/147</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/538/A100 [1]</TD>
            <TD>Abundances of Carina red giant branch (Lemasle+, 2012)</TD>
            <TD>We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R~20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100#1</TD>
            <TD>2012-02-09T12:56:39Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/538/A100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/538/A100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/538/A100 [2]</TD>
            <TD>Abundances of Carina red giant branch (Lemasle+, 2012)</TD>
            <TD>We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R~20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100#2</TD>
            <TD>2012-02-09T12:56:39Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/538/A100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/538/A100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/538/A100 [table3]</TD>
            <TD>Abundances of Carina red giant branch (Lemasle+, 2012)</TD>
            <TD>We use the VLT-FLAMES multi-fibre spectrograph in high-resolution mode (R~20000) to measure the abundances of several chemical elements, including Fe, Mg, Ca and Ba, in a sample of 35 individual Red Giant Branch stars in the Carina dwarf spheroidal galaxy. We also combine these abundances with photometry to derive age estimates for these stars. This allows us to determine which of two distinct star formation episodes the stars in our sample belong to, and thus to define the relationship between star formation and chemical enrichment during these two episodes.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100#table3</TD>
            <TD>2012-02-09T12:56:39Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/538/A100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/538/A100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/538/A100</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/279/567 [1]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#1</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/279/567</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/279/567 [2]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#2</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/279/567&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/279/567 [table4]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#table4</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/279/567&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/279/567 [table3]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#table3</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/279/567&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/777 [1]</TD>
            <TD>BVRI photometry of Sagittarius dwarf irregular galaxy (Lee+, 2000)</TD>
            <TD>We present deep BVRI CCD photometry of the stars in the dwarf irregular galaxy SagDIG, obtained on the photometric night of 1994 October 8 (UT) using the University of Hawaii 2.2 m telescope at Mauna Kea.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/777#1</TD>
            <TD>2011-09-14T19:29:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/777</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/777</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/777</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/777 [2]</TD>
            <TD>BVRI photometry of Sagittarius dwarf irregular galaxy (Lee+, 2000)</TD>
            <TD>We present deep BVRI CCD photometry of the stars in the dwarf irregular galaxy SagDIG, obtained on the photometric night of 1994 October 8 (UT) using the University of Hawaii 2.2 m telescope at Mauna Kea.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/777#2</TD>
            <TD>2011-09-14T19:29:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/777</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/777&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/777</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/777 [1]</TD>
            <TD>BVRI photometry of Sagittarius dwarf irregular galaxy (Lee+, 2000)</TD>
            <TD>We present deep BVRI CCD photometry of the stars in the dwarf irregular galaxy SagDIG, obtained on the photometric night of 1994 October 8 (UT) using the University of Hawaii 2.2 m telescope at Mauna Kea.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/777#1</TD>
            <TD>2011-09-14T19:29:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/777</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/777</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/777</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/777 [2]</TD>
            <TD>BVRI photometry of Sagittarius dwarf irregular galaxy (Lee+, 2000)</TD>
            <TD>We present deep BVRI CCD photometry of the stars in the dwarf irregular galaxy SagDIG, obtained on the photometric night of 1994 October 8 (UT) using the University of Hawaii 2.2 m telescope at Mauna Kea.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/777#2</TD>
            <TD>2011-09-14T19:29:10Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/777</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/777&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/777</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/279/567 [1]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#1</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/279/567</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/279/567 [2]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#2</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/279/567&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/279/567 [table4]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#table4</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/279/567&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/279/567 [table3]</TD>
            <TD>Abundances of non-type I PNe in LMC (Freitas Pacheco+ 1993)</TD>
            <TD>Spectroscopic observations, plasma diagnostics and chemical composition of 15 non-type I planetary nebulae (PNe) in the Large Magellanic Cloud (LMC) are reported. Abundances of He, O, N, S, and Ar are determined and compared with recently obtained data for nebulae both in the Magellanic Clouds and in the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567#table3</TD>
            <TD>2011-09-14T19:09:35Z</TD>
            <TD>#Abundances#Spectroscopy#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Jul-1993</TD>
            <TD>ivo://CDS.VizieR/J/A+A/279/567</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/279/567&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/279/567</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/281/799 [1]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#1</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/281/799</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/281/799 [2]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#2</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/281/799&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/281/799 [table34]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#table34</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/281/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/281/799 [table2]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#table2</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/281/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/291/261 [1]</TD>
            <TD>Methanol maser of IRAS-selected sources (Walsh+ 1997)</TD>
            <TD>A survey of ultracompact (UC) HII regions has been carried out by searching for 6.669-GHz methanol maser emission from a sample of 535 IRAS-selected candidates. A total of 201 candidates exhibit methanol emission. These sources have been used, in conjunction with previously identified UC HII regions, to provide a base for further studies of such regions. Estimates of distances have indicated that the identified UC HII regions tend to have some Galactic structure but it is not clear whether they lie in or between the spiral arms of the Galaxy. The regions are tightly constrained to the plane of the Galaxy. Comparison of identified regions and IRAS sources selected by Wood &amp; Churchwell indicates that there there is some degree of contamination, which could be due to an older phase in the life on an UC HII region where methanol maser emission is not apparent. Luminosities and spectral types have been derived for many of the regions. The maximum number of maser spots observed seems to increase with increasing peak maser luminosity, which indicates that the maser emission is more dependent on the abundance of methanol than the availability of far-infrared radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261#1</TD>
            <TD>2011-09-14T18:41:02Z</TD>
            <TD>#HII_regions#Masers#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/291/261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/291/261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/291/261 [2]</TD>
            <TD>Methanol maser of IRAS-selected sources (Walsh+ 1997)</TD>
            <TD>A survey of ultracompact (UC) HII regions has been carried out by searching for 6.669-GHz methanol maser emission from a sample of 535 IRAS-selected candidates. A total of 201 candidates exhibit methanol emission. These sources have been used, in conjunction with previously identified UC HII regions, to provide a base for further studies of such regions. Estimates of distances have indicated that the identified UC HII regions tend to have some Galactic structure but it is not clear whether they lie in or between the spiral arms of the Galaxy. The regions are tightly constrained to the plane of the Galaxy. Comparison of identified regions and IRAS sources selected by Wood &amp; Churchwell indicates that there there is some degree of contamination, which could be due to an older phase in the life on an UC HII region where methanol maser emission is not apparent. Luminosities and spectral types have been derived for many of the regions. The maximum number of maser spots observed seems to increase with increasing peak maser luminosity, which indicates that the maser emission is more dependent on the abundance of methanol than the availability of far-infrared radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261#2</TD>
            <TD>2011-09-14T18:41:02Z</TD>
            <TD>#HII_regions#Masers#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/291/261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/291/261</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/2341 [1]</TD>
            <TD>UBVRI photometry in Sextans A (Van Dyk+ 1998)</TD>
            <TD>We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341#1</TD>
            <TD>2011-09-14T18:48:50Z</TD>
            <TD>#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/2341</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2341</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/2341 [2]</TD>
            <TD>UBVRI photometry in Sextans A (Van Dyk+ 1998)</TD>
            <TD>We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341#2</TD>
            <TD>2011-09-14T18:48:50Z</TD>
            <TD>#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/2341&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2341</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/2341 [sextansa]</TD>
            <TD>UBVRI photometry in Sextans A (Van Dyk+ 1998)</TD>
            <TD>We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341#sextansa</TD>
            <TD>2011-09-14T18:48:50Z</TD>
            <TD>#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/2341&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2341</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/281/799 [1]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#1</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/281/799</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/281/799 [2]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#2</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/281/799&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/281/799 [table34]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#table34</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/281/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/281/799 [table2]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#table2</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/281/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/291/261 [1]</TD>
            <TD>Methanol maser of IRAS-selected sources (Walsh+ 1997)</TD>
            <TD>A survey of ultracompact (UC) HII regions has been carried out by searching for 6.669-GHz methanol maser emission from a sample of 535 IRAS-selected candidates. A total of 201 candidates exhibit methanol emission. These sources have been used, in conjunction with previously identified UC HII regions, to provide a base for further studies of such regions. Estimates of distances have indicated that the identified UC HII regions tend to have some Galactic structure but it is not clear whether they lie in or between the spiral arms of the Galaxy. The regions are tightly constrained to the plane of the Galaxy. Comparison of identified regions and IRAS sources selected by Wood &amp; Churchwell indicates that there there is some degree of contamination, which could be due to an older phase in the life on an UC HII region where methanol maser emission is not apparent. Luminosities and spectral types have been derived for many of the regions. The maximum number of maser spots observed seems to increase with increasing peak maser luminosity, which indicates that the maser emission is more dependent on the abundance of methanol than the availability of far-infrared radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261#1</TD>
            <TD>2011-09-14T18:41:02Z</TD>
            <TD>#HII_regions#Masers#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/291/261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/291/261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/291/261 [2]</TD>
            <TD>Methanol maser of IRAS-selected sources (Walsh+ 1997)</TD>
            <TD>A survey of ultracompact (UC) HII regions has been carried out by searching for 6.669-GHz methanol maser emission from a sample of 535 IRAS-selected candidates. A total of 201 candidates exhibit methanol emission. These sources have been used, in conjunction with previously identified UC HII regions, to provide a base for further studies of such regions. Estimates of distances have indicated that the identified UC HII regions tend to have some Galactic structure but it is not clear whether they lie in or between the spiral arms of the Galaxy. The regions are tightly constrained to the plane of the Galaxy. Comparison of identified regions and IRAS sources selected by Wood &amp; Churchwell indicates that there there is some degree of contamination, which could be due to an older phase in the life on an UC HII region where methanol maser emission is not apparent. Luminosities and spectral types have been derived for many of the regions. The maximum number of maser spots observed seems to increase with increasing peak maser luminosity, which indicates that the maser emission is more dependent on the abundance of methanol than the availability of far-infrared radiation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261#2</TD>
            <TD>2011-09-14T18:41:02Z</TD>
            <TD>#HII_regions#Masers#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/291/261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/291/261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/291/261</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/281/799 [1]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#1</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/281/799</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/281/799 [2]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#2</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/281/799&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/281/799 [table34]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#table34</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/281/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/281/799 [table2]</TD>
            <TD>XBACs, the sample (Ebeling+, 1996)</TD>
            <TD>We present an essentially complete, all-sky, X-ray flux-limited sample of 242 Abell clusters of galaxies (six of which are double) compiled from ROSAT All-Sky Survey data. Our sample is uncontaminated in the sense that systems featuring prominent X-ray point sources such as AGN or foreground stars have been removed. The sample is limited to high Galactic latitudes (|b|&gt;=20{deg}), the nominal redshift range of the ACO catalogue of z&lt;=0.2, and X-ray fluxes above 5.0x10^-12^erg/cm^2^/s in the 0.1-2.4keV band. Owing to the X-ray flux limit, our sample consists, at intermediate and high redshifts, exclusively of very X-ray-luminous clusters. Since the latter tend to be also optically rich, the sample is not affected by the optical selection effects and, in particular, not by the volume incompleteness known to be present in the Abell and ACO catalogues for richness class 0 and 1 clusters. Our sample is the largest X-ray flux-limited sample of galaxy clusters compiled to date and will allow investigations of unprecedented statistical quality into the properties and distribution of rich clusters in the local Universe.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799#table2</TD>
            <TD>2011-09-14T19:29:20Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/281/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/281/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/281/799</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/570/100 [1]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#1</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/570/100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/570/100 [2]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#2</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/570/100 [table4]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#table4</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/570/100 [table3]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#table3</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/570/100 [table5]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#table5</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/2341 [1]</TD>
            <TD>UBVRI photometry in Sextans A (Van Dyk+ 1998)</TD>
            <TD>We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341#1</TD>
            <TD>2011-09-14T18:48:50Z</TD>
            <TD>#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/2341</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2341</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/2341 [2]</TD>
            <TD>UBVRI photometry in Sextans A (Van Dyk+ 1998)</TD>
            <TD>We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341#2</TD>
            <TD>2011-09-14T18:48:50Z</TD>
            <TD>#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/2341&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2341</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/2341 [sextansa]</TD>
            <TD>UBVRI photometry in Sextans A (Van Dyk+ 1998)</TD>
            <TD>We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341#sextansa</TD>
            <TD>2011-09-14T18:48:50Z</TD>
            <TD>#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/2341&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2341</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/2381 [1]</TD>
            <TD>UBRI photometry of radio galaxies (Brown+, 2001)</TD>
            <TD>We describe a new estimate of the radio galaxy 1.4 GHz luminosity function and its evolution at intermediate redshifts (z~0.4). Photometric redshifts and color selection have been used to select B_J_&lt;23.5 early-type galaxies from the Panoramic Deep Fields, a multicolor survey of two 25deg^2^ fields. Approximately 230 radio galaxies have then been selected by matching early-type galaxies with NVSS radio sources brighter than 5mJy. Estimates of the 1.4GHz luminosity function of radio galaxies measure significant evolution over the observed redshift range. For an {Omega}_M_=1 cosmology the evolution of the radio power is consistent with luminosity evolution where P(z)~P(0)(1+z)^K_L_^ and 3&lt;K_L_&lt;5. The observed evolution is similar to that observed for UVX and X-ray selected active galactic nuclei and is consistent with the same physical process being responsible for the optical and radio luminosity evolution of active galactic nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381#1</TD>
            <TD>2011-09-14T19:11:23Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/2381</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2381</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/2381 [2]</TD>
            <TD>UBRI photometry of radio galaxies (Brown+, 2001)</TD>
            <TD>We describe a new estimate of the radio galaxy 1.4 GHz luminosity function and its evolution at intermediate redshifts (z~0.4). Photometric redshifts and color selection have been used to select B_J_&lt;23.5 early-type galaxies from the Panoramic Deep Fields, a multicolor survey of two 25deg^2^ fields. Approximately 230 radio galaxies have then been selected by matching early-type galaxies with NVSS radio sources brighter than 5mJy. Estimates of the 1.4GHz luminosity function of radio galaxies measure significant evolution over the observed redshift range. For an {Omega}_M_=1 cosmology the evolution of the radio power is consistent with luminosity evolution where P(z)~P(0)(1+z)^K_L_^ and 3&lt;K_L_&lt;5. The observed evolution is similar to that observed for UVX and X-ray selected active galactic nuclei and is consistent with the same physical process being responsible for the optical and radio luminosity evolution of active galactic nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381#2</TD>
            <TD>2011-09-14T19:11:23Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/2381&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2381</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2381 [table2]</TD>
            <TD>UBRI photometry of radio galaxies (Brown+, 2001)</TD>
            <TD>We describe a new estimate of the radio galaxy 1.4 GHz luminosity function and its evolution at intermediate redshifts (z~0.4). Photometric redshifts and color selection have been used to select B_J_&lt;23.5 early-type galaxies from the Panoramic Deep Fields, a multicolor survey of two 25deg^2^ fields. Approximately 230 radio galaxies have then been selected by matching early-type galaxies with NVSS radio sources brighter than 5mJy. Estimates of the 1.4GHz luminosity function of radio galaxies measure significant evolution over the observed redshift range. For an {Omega}_M_=1 cosmology the evolution of the radio power is consistent with luminosity evolution where P(z)~P(0)(1+z)^K_L_^ and 3&lt;K_L_&lt;5. The observed evolution is similar to that observed for UVX and X-ray selected active galactic nuclei and is consistent with the same physical process being responsible for the optical and radio luminosity evolution of active galactic nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381#table2</TD>
            <TD>2011-09-14T19:11:23Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2381&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2381</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/570/100 [1]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#1</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/570/100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/570/100 [2]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#2</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/570/100 [table4]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#table4</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/570/100 [table3]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#table3</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/570/100 [table5]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#table5</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/570/100 [1]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#1</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/570/100</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/570/100 [2]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#2</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/570/100 [table4]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#table4</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/570/100 [table3]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#table3</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/570/100 [table5]</TD>
            <TD>BeppoSAX HELLAS survey. V. (La Franca+, 2002)</TD>
            <TD>We present optical spectroscopic identifications of hard X-ray (5-10keV) selected sources belonging to the High-Energy Large-Area Survey sample obtained with BeppoSAX down to a 5-10keV flux limit of F(5-10kev)~3x10^-14^erg/cm^2^/s. The sample consists of 118 sources. There are 25 sources that have been identified through correlations with catalogs of known sources. A spectroscopic identification for 49 more has been searched for with the telescope. The results of 13 fields were empty down to R=21. There were 37 sources identified as type 1 active galactic nuclei (AGNs) and nine as type 2 AGNs. The remaining sources are five narrow emission-line galaxies, six clusters, two BL Lac objects, one radio galaxy, and one star.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100#table5</TD>
            <TD>2011-09-14T19:29:54Z</TD>
            <TD>#AGN#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/570/100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/570/100&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/570/100</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/422/925 [1]</TD>
            <TD>Profile variability in lines of NGC 5548 (Shapovalova+ 2004)</TD>
            <TD>Between 1996 and 2002, we have carried out a spectral monitoring program for the Seyfert galaxy NGC 5548 with the 6m and 1m telescopes of SAO (Russia) and with the 2.1m telescope of Guillermo Haro Observatory (GHO) at Cananea, Mexico. High quality spectra with S/N&gt;50 in the continuum near H{alpha} and H{beta} were obtained, covering the spectral range ~(4000-7500){AA} with a (4.5 to 15){AA}-resolution. We found that both the flux in the lines and the continuum gradually decreased, reaching minimum values during May-June 2002. In the minimum state, the wings of H{beta} and H{alpha} became extremely weak, corresponding to a Sy1.8 type, not to a Sy1, as observed previously when the nucleus was brighter. The line profiles were decomposed into variable and constant components. The variable broad component is well correlated with the continuum variation. It consists of a double peaked structure with radial velocities ~+/-1000 km/s relative to the narrow component. A constant component, whose presence is independent of the continuum flux variations, shows only narrow emission lines. The mean, rms, and the averaged over years, observed and difference line profiles of H{beta} and H{alpha} reveal the same double peaked structure. The relative intensity of these peaks changes with time. During 1996, the red peak was the brightest, while in 1998-2002, the blue peak became the brighter one. Their radial velocities vary in the ~(500-1200) km/s range. In 2000-2002 a distinct third peak appeared in the red wing of H{alpha} and H{beta} line profiles. The radial velocity of this feature decreased between 2000 and 2002: from the observed profiles, from ~+(2500-2600) km/s to ~+2000 km/s and is clearly seen on the difference profiles. The fluxes of the various parts of the line profiles are well correlated with each other and also with the continuum flux. The blue and red parts of the line profiles at the same radial velocities vary in an almost identical manner. Shape changes of the different parts of the broad line are not correlated with continuum variations and, apparently, are not related to reverberation effects. Changes of the integral Balmer decrement are, on average, anticorrelated with the continuum flux variations. This is probably due to an increasing role of collisional excitation as the ionizing flux decreases. The behaviour of the Balmer decrement of the various parts of the line profiles was different in 1996-2000 as compared with the 2001 behaviour. Our results favour the formation of the broad Balmer lines in a turbulent accretion disc with large and moving "optically thick" inhomogeneities, capable of reprocessing the central source continuum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/925#1</TD>
            <TD>2011-09-14T19:30:02Z</TD>
            <TD>#AGN#Spectroscopy#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/925</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/422/925</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/925</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/422/925 [2]</TD>
            <TD>Profile variability in lines of NGC 5548 (Shapovalova+ 2004)</TD>
            <TD>Between 1996 and 2002, we have carried out a spectral monitoring program for the Seyfert galaxy NGC 5548 with the 6m and 1m telescopes of SAO (Russia) and with the 2.1m telescope of Guillermo Haro Observatory (GHO) at Cananea, Mexico. High quality spectra with S/N&gt;50 in the continuum near H{alpha} and H{beta} were obtained, covering the spectral range ~(4000-7500){AA} with a (4.5 to 15){AA}-resolution. We found that both the flux in the lines and the continuum gradually decreased, reaching minimum values during May-June 2002. In the minimum state, the wings of H{beta} and H{alpha} became extremely weak, corresponding to a Sy1.8 type, not to a Sy1, as observed previously when the nucleus was brighter. The line profiles were decomposed into variable and constant components. The variable broad component is well correlated with the continuum variation. It consists of a double peaked structure with radial velocities ~+/-1000 km/s relative to the narrow component. A constant component, whose presence is independent of the continuum flux variations, shows only narrow emission lines. The mean, rms, and the averaged over years, observed and difference line profiles of H{beta} and H{alpha} reveal the same double peaked structure. The relative intensity of these peaks changes with time. During 1996, the red peak was the brightest, while in 1998-2002, the blue peak became the brighter one. Their radial velocities vary in the ~(500-1200) km/s range. In 2000-2002 a distinct third peak appeared in the red wing of H{alpha} and H{beta} line profiles. The radial velocity of this feature decreased between 2000 and 2002: from the observed profiles, from ~+(2500-2600) km/s to ~+2000 km/s and is clearly seen on the difference profiles. The fluxes of the various parts of the line profiles are well correlated with each other and also with the continuum flux. The blue and red parts of the line profiles at the same radial velocities vary in an almost identical manner. Shape changes of the different parts of the broad line are not correlated with continuum variations and, apparently, are not related to reverberation effects. Changes of the integral Balmer decrement are, on average, anticorrelated with the continuum flux variations. This is probably due to an increasing role of collisional excitation as the ionizing flux decreases. The behaviour of the Balmer decrement of the various parts of the line profiles was different in 1996-2000 as compared with the 2001 behaviour. Our results favour the formation of the broad Balmer lines in a turbulent accretion disc with large and moving "optically thick" inhomogeneities, capable of reprocessing the central source continuum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/925#2</TD>
            <TD>2011-09-14T19:30:02Z</TD>
            <TD>#AGN#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/925</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/422/925&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/925</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/116/2341 [1]</TD>
            <TD>UBVRI photometry in Sextans A (Van Dyk+ 1998)</TD>
            <TD>We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341#1</TD>
            <TD>2011-09-14T18:48:50Z</TD>
            <TD>#Stars#Galaxies#Photometry:wide-band#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/116/2341</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2341</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/116/2341 [2]</TD>
            <TD>UBVRI photometry in Sextans A (Van Dyk+ 1998)</TD>
            <TD>We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341#2</TD>
            <TD>2011-09-14T18:48:50Z</TD>
            <TD>#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/116/2341&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2341</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/116/2341 [sextansa]</TD>
            <TD>UBVRI photometry in Sextans A (Van Dyk+ 1998)</TD>
            <TD>We investigate the relationship between the spatial distributions of stellar populations and of neutral and ionized gas in the Local Group dwarf irregular galaxy Sextans A. We have resolved various populations of stars via deep UBV(RI)_C imaging over an area with diameter 5.3 arcmin. We arrive at 2525 stars detected in V and at least one other band. We provide here the magnitudes, colors, and absolute positions for the stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341#sextansa</TD>
            <TD>2011-09-14T18:48:50Z</TD>
            <TD>#Stars#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/116/2341</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/116/2341&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/116/2341</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/422/925 [1]</TD>
            <TD>Profile variability in lines of NGC 5548 (Shapovalova+ 2004)</TD>
            <TD>Between 1996 and 2002, we have carried out a spectral monitoring program for the Seyfert galaxy NGC 5548 with the 6m and 1m telescopes of SAO (Russia) and with the 2.1m telescope of Guillermo Haro Observatory (GHO) at Cananea, Mexico. High quality spectra with S/N&gt;50 in the continuum near H{alpha} and H{beta} were obtained, covering the spectral range ~(4000-7500){AA} with a (4.5 to 15){AA}-resolution. We found that both the flux in the lines and the continuum gradually decreased, reaching minimum values during May-June 2002. In the minimum state, the wings of H{beta} and H{alpha} became extremely weak, corresponding to a Sy1.8 type, not to a Sy1, as observed previously when the nucleus was brighter. The line profiles were decomposed into variable and constant components. The variable broad component is well correlated with the continuum variation. It consists of a double peaked structure with radial velocities ~+/-1000 km/s relative to the narrow component. A constant component, whose presence is independent of the continuum flux variations, shows only narrow emission lines. The mean, rms, and the averaged over years, observed and difference line profiles of H{beta} and H{alpha} reveal the same double peaked structure. The relative intensity of these peaks changes with time. During 1996, the red peak was the brightest, while in 1998-2002, the blue peak became the brighter one. Their radial velocities vary in the ~(500-1200) km/s range. In 2000-2002 a distinct third peak appeared in the red wing of H{alpha} and H{beta} line profiles. The radial velocity of this feature decreased between 2000 and 2002: from the observed profiles, from ~+(2500-2600) km/s to ~+2000 km/s and is clearly seen on the difference profiles. The fluxes of the various parts of the line profiles are well correlated with each other and also with the continuum flux. The blue and red parts of the line profiles at the same radial velocities vary in an almost identical manner. Shape changes of the different parts of the broad line are not correlated with continuum variations and, apparently, are not related to reverberation effects. Changes of the integral Balmer decrement are, on average, anticorrelated with the continuum flux variations. This is probably due to an increasing role of collisional excitation as the ionizing flux decreases. The behaviour of the Balmer decrement of the various parts of the line profiles was different in 1996-2000 as compared with the 2001 behaviour. Our results favour the formation of the broad Balmer lines in a turbulent accretion disc with large and moving "optically thick" inhomogeneities, capable of reprocessing the central source continuum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/925#1</TD>
            <TD>2011-09-14T19:30:02Z</TD>
            <TD>#AGN#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/925</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/422/925</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/925</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/422/925 [2]</TD>
            <TD>Profile variability in lines of NGC 5548 (Shapovalova+ 2004)</TD>
            <TD>Between 1996 and 2002, we have carried out a spectral monitoring program for the Seyfert galaxy NGC 5548 with the 6m and 1m telescopes of SAO (Russia) and with the 2.1m telescope of Guillermo Haro Observatory (GHO) at Cananea, Mexico. High quality spectra with S/N&gt;50 in the continuum near H{alpha} and H{beta} were obtained, covering the spectral range ~(4000-7500){AA} with a (4.5 to 15){AA}-resolution. We found that both the flux in the lines and the continuum gradually decreased, reaching minimum values during May-June 2002. In the minimum state, the wings of H{beta} and H{alpha} became extremely weak, corresponding to a Sy1.8 type, not to a Sy1, as observed previously when the nucleus was brighter. The line profiles were decomposed into variable and constant components. The variable broad component is well correlated with the continuum variation. It consists of a double peaked structure with radial velocities ~+/-1000 km/s relative to the narrow component. A constant component, whose presence is independent of the continuum flux variations, shows only narrow emission lines. The mean, rms, and the averaged over years, observed and difference line profiles of H{beta} and H{alpha} reveal the same double peaked structure. The relative intensity of these peaks changes with time. During 1996, the red peak was the brightest, while in 1998-2002, the blue peak became the brighter one. Their radial velocities vary in the ~(500-1200) km/s range. In 2000-2002 a distinct third peak appeared in the red wing of H{alpha} and H{beta} line profiles. The radial velocity of this feature decreased between 2000 and 2002: from the observed profiles, from ~+(2500-2600) km/s to ~+2000 km/s and is clearly seen on the difference profiles. The fluxes of the various parts of the line profiles are well correlated with each other and also with the continuum flux. The blue and red parts of the line profiles at the same radial velocities vary in an almost identical manner. Shape changes of the different parts of the broad line are not correlated with continuum variations and, apparently, are not related to reverberation effects. Changes of the integral Balmer decrement are, on average, anticorrelated with the continuum flux variations. This is probably due to an increasing role of collisional excitation as the ionizing flux decreases. The behaviour of the Balmer decrement of the various parts of the line profiles was different in 1996-2000 as compared with the 2001 behaviour. Our results favour the formation of the broad Balmer lines in a turbulent accretion disc with large and moving "optically thick" inhomogeneities, capable of reprocessing the central source continuum.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/925#2</TD>
            <TD>2011-09-14T19:30:02Z</TD>
            <TD>#AGN#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/925</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/422/925&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/925</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/2381 [1]</TD>
            <TD>UBRI photometry of radio galaxies (Brown+, 2001)</TD>
            <TD>We describe a new estimate of the radio galaxy 1.4 GHz luminosity function and its evolution at intermediate redshifts (z~0.4). Photometric redshifts and color selection have been used to select B_J_&lt;23.5 early-type galaxies from the Panoramic Deep Fields, a multicolor survey of two 25deg^2^ fields. Approximately 230 radio galaxies have then been selected by matching early-type galaxies with NVSS radio sources brighter than 5mJy. Estimates of the 1.4GHz luminosity function of radio galaxies measure significant evolution over the observed redshift range. For an {Omega}_M_=1 cosmology the evolution of the radio power is consistent with luminosity evolution where P(z)~P(0)(1+z)^K_L_^ and 3&lt;K_L_&lt;5. The observed evolution is similar to that observed for UVX and X-ray selected active galactic nuclei and is consistent with the same physical process being responsible for the optical and radio luminosity evolution of active galactic nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381#1</TD>
            <TD>2011-09-14T19:11:23Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/2381</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2381</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/2381 [2]</TD>
            <TD>UBRI photometry of radio galaxies (Brown+, 2001)</TD>
            <TD>We describe a new estimate of the radio galaxy 1.4 GHz luminosity function and its evolution at intermediate redshifts (z~0.4). Photometric redshifts and color selection have been used to select B_J_&lt;23.5 early-type galaxies from the Panoramic Deep Fields, a multicolor survey of two 25deg^2^ fields. Approximately 230 radio galaxies have then been selected by matching early-type galaxies with NVSS radio sources brighter than 5mJy. Estimates of the 1.4GHz luminosity function of radio galaxies measure significant evolution over the observed redshift range. For an {Omega}_M_=1 cosmology the evolution of the radio power is consistent with luminosity evolution where P(z)~P(0)(1+z)^K_L_^ and 3&lt;K_L_&lt;5. The observed evolution is similar to that observed for UVX and X-ray selected active galactic nuclei and is consistent with the same physical process being responsible for the optical and radio luminosity evolution of active galactic nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381#2</TD>
            <TD>2011-09-14T19:11:23Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/2381&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2381</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2381 [table2]</TD>
            <TD>UBRI photometry of radio galaxies (Brown+, 2001)</TD>
            <TD>We describe a new estimate of the radio galaxy 1.4 GHz luminosity function and its evolution at intermediate redshifts (z~0.4). Photometric redshifts and color selection have been used to select B_J_&lt;23.5 early-type galaxies from the Panoramic Deep Fields, a multicolor survey of two 25deg^2^ fields. Approximately 230 radio galaxies have then been selected by matching early-type galaxies with NVSS radio sources brighter than 5mJy. Estimates of the 1.4GHz luminosity function of radio galaxies measure significant evolution over the observed redshift range. For an {Omega}_M_=1 cosmology the evolution of the radio power is consistent with luminosity evolution where P(z)~P(0)(1+z)^K_L_^ and 3&lt;K_L_&lt;5. The observed evolution is similar to that observed for UVX and X-ray selected active galactic nuclei and is consistent with the same physical process being responsible for the optical and radio luminosity evolution of active galactic nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381#table2</TD>
            <TD>2011-09-14T19:11:23Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2381&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2381</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/345/747 [1]</TD>
            <TD>RR Lyrae in 4 Fornax globular clusters (Mackey+, 2003)</TD>
            <TD>We have surveyed four of the globular clusters in the Fornax dwarf galaxy (clusters 1, 2, 3 and 5) for RR Lyrae stars, using archival F555W and F814W Hubble Space Telescope observations. We identify 197 new RR Lyrae stars in these four clusters, and 13 additional candidate horizontal-branch variable stars. Although somewhat restricted by our short observational baseline, we derive periods and light curves for all of the stars in the sample, and calculate photometric parameters such as mean magnitudes and colours. This is the first time that RR Lyrae stars in the Fornax globular clusters have been quantitatively identified and measured.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/345/747#1</TD>
            <TD>2011-09-14T19:30:54Z</TD>
            <TD>#Globular_Clusters#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/345/747</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/345/747</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/345/747</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/345/747 [2]</TD>
            <TD>RR Lyrae in 4 Fornax globular clusters (Mackey+, 2003)</TD>
            <TD>We have surveyed four of the globular clusters in the Fornax dwarf galaxy (clusters 1, 2, 3 and 5) for RR Lyrae stars, using archival F555W and F814W Hubble Space Telescope observations. We identify 197 new RR Lyrae stars in these four clusters, and 13 additional candidate horizontal-branch variable stars. Although somewhat restricted by our short observational baseline, we derive periods and light curves for all of the stars in the sample, and calculate photometric parameters such as mean magnitudes and colours. This is the first time that RR Lyrae stars in the Fornax globular clusters have been quantitatively identified and measured.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/345/747#2</TD>
            <TD>2011-09-14T19:30:54Z</TD>
            <TD>#Globular_Clusters#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/345/747</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/345/747&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/345/747</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/67 [1]</TD>
            <TD>HI observations of dwarf galaxies in voids (Huchtmeier+ 1997)</TD>
            <TD>We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2&lt;=logL_B_&lt;=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67#1</TD>
            <TD>2011-09-14T18:49:28Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/67</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/67</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/67 [2]</TD>
            <TD>HI observations of dwarf galaxies in voids (Huchtmeier+ 1997)</TD>
            <TD>We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2&lt;=logL_B_&lt;=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67#2</TD>
            <TD>2011-09-14T18:49:28Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/67&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/319/67 [table1]</TD>
            <TD>HI observations of dwarf galaxies in voids (Huchtmeier+ 1997)</TD>
            <TD>We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2&lt;=logL_B_&lt;=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67#table1</TD>
            <TD>2011-09-14T18:49:28Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/319/67&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/67</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/2381 [1]</TD>
            <TD>UBRI photometry of radio galaxies (Brown+, 2001)</TD>
            <TD>We describe a new estimate of the radio galaxy 1.4 GHz luminosity function and its evolution at intermediate redshifts (z~0.4). Photometric redshifts and color selection have been used to select B_J_&lt;23.5 early-type galaxies from the Panoramic Deep Fields, a multicolor survey of two 25deg^2^ fields. Approximately 230 radio galaxies have then been selected by matching early-type galaxies with NVSS radio sources brighter than 5mJy. Estimates of the 1.4GHz luminosity function of radio galaxies measure significant evolution over the observed redshift range. For an {Omega}_M_=1 cosmology the evolution of the radio power is consistent with luminosity evolution where P(z)~P(0)(1+z)^K_L_^ and 3&lt;K_L_&lt;5. The observed evolution is similar to that observed for UVX and X-ray selected active galactic nuclei and is consistent with the same physical process being responsible for the optical and radio luminosity evolution of active galactic nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381#1</TD>
            <TD>2011-09-14T19:11:23Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/2381</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2381</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/2381 [2]</TD>
            <TD>UBRI photometry of radio galaxies (Brown+, 2001)</TD>
            <TD>We describe a new estimate of the radio galaxy 1.4 GHz luminosity function and its evolution at intermediate redshifts (z~0.4). Photometric redshifts and color selection have been used to select B_J_&lt;23.5 early-type galaxies from the Panoramic Deep Fields, a multicolor survey of two 25deg^2^ fields. Approximately 230 radio galaxies have then been selected by matching early-type galaxies with NVSS radio sources brighter than 5mJy. Estimates of the 1.4GHz luminosity function of radio galaxies measure significant evolution over the observed redshift range. For an {Omega}_M_=1 cosmology the evolution of the radio power is consistent with luminosity evolution where P(z)~P(0)(1+z)^K_L_^ and 3&lt;K_L_&lt;5. The observed evolution is similar to that observed for UVX and X-ray selected active galactic nuclei and is consistent with the same physical process being responsible for the optical and radio luminosity evolution of active galactic nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381#2</TD>
            <TD>2011-09-14T19:11:23Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/2381&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2381</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2381 [table2]</TD>
            <TD>UBRI photometry of radio galaxies (Brown+, 2001)</TD>
            <TD>We describe a new estimate of the radio galaxy 1.4 GHz luminosity function and its evolution at intermediate redshifts (z~0.4). Photometric redshifts and color selection have been used to select B_J_&lt;23.5 early-type galaxies from the Panoramic Deep Fields, a multicolor survey of two 25deg^2^ fields. Approximately 230 radio galaxies have then been selected by matching early-type galaxies with NVSS radio sources brighter than 5mJy. Estimates of the 1.4GHz luminosity function of radio galaxies measure significant evolution over the observed redshift range. For an {Omega}_M_=1 cosmology the evolution of the radio power is consistent with luminosity evolution where P(z)~P(0)(1+z)^K_L_^ and 3&lt;K_L_&lt;5. The observed evolution is similar to that observed for UVX and X-ray selected active galactic nuclei and is consistent with the same physical process being responsible for the optical and radio luminosity evolution of active galactic nuclei.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381#table2</TD>
            <TD>2011-09-14T19:11:23Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2381</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2381&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2381</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/345/747 [1]</TD>
            <TD>RR Lyrae in 4 Fornax globular clusters (Mackey+, 2003)</TD>
            <TD>We have surveyed four of the globular clusters in the Fornax dwarf galaxy (clusters 1, 2, 3 and 5) for RR Lyrae stars, using archival F555W and F814W Hubble Space Telescope observations. We identify 197 new RR Lyrae stars in these four clusters, and 13 additional candidate horizontal-branch variable stars. Although somewhat restricted by our short observational baseline, we derive periods and light curves for all of the stars in the sample, and calculate photometric parameters such as mean magnitudes and colours. This is the first time that RR Lyrae stars in the Fornax globular clusters have been quantitatively identified and measured.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/345/747#1</TD>
            <TD>2011-09-14T19:30:54Z</TD>
            <TD>#Globular_Clusters#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/345/747</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/345/747</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/345/747</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/345/747 [2]</TD>
            <TD>RR Lyrae in 4 Fornax globular clusters (Mackey+, 2003)</TD>
            <TD>We have surveyed four of the globular clusters in the Fornax dwarf galaxy (clusters 1, 2, 3 and 5) for RR Lyrae stars, using archival F555W and F814W Hubble Space Telescope observations. We identify 197 new RR Lyrae stars in these four clusters, and 13 additional candidate horizontal-branch variable stars. Although somewhat restricted by our short observational baseline, we derive periods and light curves for all of the stars in the sample, and calculate photometric parameters such as mean magnitudes and colours. This is the first time that RR Lyrae stars in the Fornax globular clusters have been quantitatively identified and measured.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/345/747#2</TD>
            <TD>2011-09-14T19:30:54Z</TD>
            <TD>#Globular_Clusters#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/345/747</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/345/747&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/345/747</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/67 [1]</TD>
            <TD>HI observations of dwarf galaxies in voids (Huchtmeier+ 1997)</TD>
            <TD>We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2&lt;=logL_B_&lt;=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67#1</TD>
            <TD>2011-09-14T18:49:28Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/67</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/67</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/67 [2]</TD>
            <TD>HI observations of dwarf galaxies in voids (Huchtmeier+ 1997)</TD>
            <TD>We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2&lt;=logL_B_&lt;=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67#2</TD>
            <TD>2011-09-14T18:49:28Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/67&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/319/67 [table1]</TD>
            <TD>HI observations of dwarf galaxies in voids (Huchtmeier+ 1997)</TD>
            <TD>We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2&lt;=logL_B_&lt;=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67#table1</TD>
            <TD>2011-09-14T18:49:28Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/319/67&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/67</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/2895 [1]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#1</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/2895</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/2895 [2]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#2</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table8]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table8</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table6b]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table6b</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table6a]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table6a</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table7a]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table7a</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table1]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table1</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table7b]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table7b</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/319/67 [1]</TD>
            <TD>HI observations of dwarf galaxies in voids (Huchtmeier+ 1997)</TD>
            <TD>We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2&lt;=logL_B_&lt;=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67#1</TD>
            <TD>2011-09-14T18:49:28Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/319/67</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/67</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/319/67 [2]</TD>
            <TD>HI observations of dwarf galaxies in voids (Huchtmeier+ 1997)</TD>
            <TD>We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2&lt;=logL_B_&lt;=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67#2</TD>
            <TD>2011-09-14T18:49:28Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/319/67&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/319/67 [table1]</TD>
            <TD>HI observations of dwarf galaxies in voids (Huchtmeier+ 1997)</TD>
            <TD>We report HI-observations of a sample of 43 optically selected galaxies from the Heidelberg-void project. Only emission-line galaxies have been selected. The HI-detection rate was 67%. The observed sample is a mix in late-type morphology objects with a spread in luminosity. They were compared to other samples with similar selection effects and mixtures. The detected galaxies have a high HI content and their M_HI_/L_B_ values are systematically higher than expected from a local field comparison sample. Especially, for the 10 dwarfs in our sample (8.2&lt;=logL_B_&lt;=9.2) which appear to be highly isolated, a mean M_HI_/L_B_=1.8 was derived which is higher than for all comparison samples, including those with the same restricted luminosity range. We discuss a trend in our data between the relative HI-content and the surrounding galaxy density holding from very high densities (Virgo-cluster) to the very isolated objects at the rims of the voids. We also present HI observations of 7 HII-galaxies of the University of Michigan (UM) sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67#table1</TD>
            <TD>2011-09-14T18:49:28Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+A/319/67</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/319/67&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/319/67</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/240 [1]</TD>
            <TD>Millennium Galaxy Catalogue (Liske+, 2003)</TD>
            <TD>The Millennium Galaxy Catalogue (MGC) is a 37.5deg^2^, medium-deep, B-band imaging survey along the celestial equator, taken with the Wide Field Camera on the Isaac Newton Telescope. The survey region is contained within the regions of both the Two Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey Early Data Release (SDSS-EDR). The survey has a uniform isophotal detection limit of 26mag.arcsec^-2^ and it provides a robust, well-defined catalogue of stars and galaxies in the range 16&lt;=B_MGC_&lt;24 mag. Here we describe the survey strategy, the photometric and astrometric calibration, source detection and analysis, and present the galaxy number counts that connect the bright and faint galaxy populations within a single survey. We argue that these counts represent the state of the art and use them to constrain the normalizations ({phi}*) of a number of recent estimates of the local galaxy luminosity function. We find that the 2dFGRS, SDSS Commissioning Data (CD), ESO Slice Project, Century Survey, Durham/UKST, Mt Stromlo/APM, SSRS2 and NOG luminosity functions require a revision of their published {phi}* values by factors of 1.05+/-0.05, 0.76+/-0.10, 1.02+/-0.22, 1.02+/-0.16, 1.16+/-0.28, 1.75+/-0.37, 1.40+/-0.26 and 1.01+/-0.39, respectively. After renormalizing the galaxy luminosity functions we find a mean local b_J_ luminosity density of 1.986+/-0.031x10^8^h L_{sun}_.Mpc^-3^</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/240#1</TD>
            <TD>2011-09-14T19:31:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2004</TD>
            <TD>ivo://CDS.VizieR/VII/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/240</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/240</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/240 [2]</TD>
            <TD>Millennium Galaxy Catalogue (Liske+, 2003)</TD>
            <TD>The Millennium Galaxy Catalogue (MGC) is a 37.5deg^2^, medium-deep, B-band imaging survey along the celestial equator, taken with the Wide Field Camera on the Isaac Newton Telescope. The survey region is contained within the regions of both the Two Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey Early Data Release (SDSS-EDR). The survey has a uniform isophotal detection limit of 26mag.arcsec^-2^ and it provides a robust, well-defined catalogue of stars and galaxies in the range 16&lt;=B_MGC_&lt;24 mag. Here we describe the survey strategy, the photometric and astrometric calibration, source detection and analysis, and present the galaxy number counts that connect the bright and faint galaxy populations within a single survey. We argue that these counts represent the state of the art and use them to constrain the normalizations ({phi}*) of a number of recent estimates of the local galaxy luminosity function. We find that the 2dFGRS, SDSS Commissioning Data (CD), ESO Slice Project, Century Survey, Durham/UKST, Mt Stromlo/APM, SSRS2 and NOG luminosity functions require a revision of their published {phi}* values by factors of 1.05+/-0.05, 0.76+/-0.10, 1.02+/-0.22, 1.02+/-0.16, 1.16+/-0.28, 1.75+/-0.37, 1.40+/-0.26 and 1.01+/-0.39, respectively. After renormalizing the galaxy luminosity functions we find a mean local b_J_ luminosity density of 1.986+/-0.031x10^8^h L_{sun}_.Mpc^-3^</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/240#2</TD>
            <TD>2011-09-14T19:31:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2004</TD>
            <TD>ivo://CDS.VizieR/VII/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/240&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/240 [mgczcat]</TD>
            <TD>Millennium Galaxy Catalogue (Liske+, 2003)</TD>
            <TD>The Millennium Galaxy Catalogue (MGC) is a 37.5deg^2^, medium-deep, B-band imaging survey along the celestial equator, taken with the Wide Field Camera on the Isaac Newton Telescope. The survey region is contained within the regions of both the Two Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey Early Data Release (SDSS-EDR). The survey has a uniform isophotal detection limit of 26mag.arcsec^-2^ and it provides a robust, well-defined catalogue of stars and galaxies in the range 16&lt;=B_MGC_&lt;24 mag. Here we describe the survey strategy, the photometric and astrometric calibration, source detection and analysis, and present the galaxy number counts that connect the bright and faint galaxy populations within a single survey. We argue that these counts represent the state of the art and use them to constrain the normalizations ({phi}*) of a number of recent estimates of the local galaxy luminosity function. We find that the 2dFGRS, SDSS Commissioning Data (CD), ESO Slice Project, Century Survey, Durham/UKST, Mt Stromlo/APM, SSRS2 and NOG luminosity functions require a revision of their published {phi}* values by factors of 1.05+/-0.05, 0.76+/-0.10, 1.02+/-0.22, 1.02+/-0.16, 1.16+/-0.28, 1.75+/-0.37, 1.40+/-0.26 and 1.01+/-0.39, respectively. After renormalizing the galaxy luminosity functions we find a mean local b_J_ luminosity density of 1.986+/-0.031x10^8^h L_{sun}_.Mpc^-3^</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/240#mgczcat</TD>
            <TD>2011-09-14T19:31:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2004</TD>
            <TD>ivo://CDS.VizieR/VII/240</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/240&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/240</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/2895 [1]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#1</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/2895</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/2895 [2]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#2</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table8]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table8</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table6b]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table6b</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table6a]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table6a</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table7a]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table7a</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table1]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table1</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table7b]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table7b</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/116/429 [1]</TD>
            <TD>Classification of Coma early galaxies (Andreon+ 1996)</TD>
            <TD>We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429#1</TD>
            <TD>2011-09-14T18:49:48Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/116/429</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/429</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/116/429 [2]</TD>
            <TD>Classification of Coma early galaxies (Andreon+ 1996)</TD>
            <TD>We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429#2</TD>
            <TD>2011-09-14T18:49:48Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/116/429&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/429</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/116/429 [table4]</TD>
            <TD>Classification of Coma early galaxies (Andreon+ 1996)</TD>
            <TD>We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429#table4</TD>
            <TD>2011-09-14T18:49:48Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/116/429&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/429</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/240 [1]</TD>
            <TD>Millennium Galaxy Catalogue (Liske+, 2003)</TD>
            <TD>The Millennium Galaxy Catalogue (MGC) is a 37.5deg^2^, medium-deep, B-band imaging survey along the celestial equator, taken with the Wide Field Camera on the Isaac Newton Telescope. The survey region is contained within the regions of both the Two Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey Early Data Release (SDSS-EDR). The survey has a uniform isophotal detection limit of 26mag.arcsec^-2^ and it provides a robust, well-defined catalogue of stars and galaxies in the range 16&lt;=B_MGC_&lt;24 mag. Here we describe the survey strategy, the photometric and astrometric calibration, source detection and analysis, and present the galaxy number counts that connect the bright and faint galaxy populations within a single survey. We argue that these counts represent the state of the art and use them to constrain the normalizations ({phi}*) of a number of recent estimates of the local galaxy luminosity function. We find that the 2dFGRS, SDSS Commissioning Data (CD), ESO Slice Project, Century Survey, Durham/UKST, Mt Stromlo/APM, SSRS2 and NOG luminosity functions require a revision of their published {phi}* values by factors of 1.05+/-0.05, 0.76+/-0.10, 1.02+/-0.22, 1.02+/-0.16, 1.16+/-0.28, 1.75+/-0.37, 1.40+/-0.26 and 1.01+/-0.39, respectively. After renormalizing the galaxy luminosity functions we find a mean local b_J_ luminosity density of 1.986+/-0.031x10^8^h L_{sun}_.Mpc^-3^</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/240#1</TD>
            <TD>2011-09-14T19:31:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2004</TD>
            <TD>ivo://CDS.VizieR/VII/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/240</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/240</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/240 [2]</TD>
            <TD>Millennium Galaxy Catalogue (Liske+, 2003)</TD>
            <TD>The Millennium Galaxy Catalogue (MGC) is a 37.5deg^2^, medium-deep, B-band imaging survey along the celestial equator, taken with the Wide Field Camera on the Isaac Newton Telescope. The survey region is contained within the regions of both the Two Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey Early Data Release (SDSS-EDR). The survey has a uniform isophotal detection limit of 26mag.arcsec^-2^ and it provides a robust, well-defined catalogue of stars and galaxies in the range 16&lt;=B_MGC_&lt;24 mag. Here we describe the survey strategy, the photometric and astrometric calibration, source detection and analysis, and present the galaxy number counts that connect the bright and faint galaxy populations within a single survey. We argue that these counts represent the state of the art and use them to constrain the normalizations ({phi}*) of a number of recent estimates of the local galaxy luminosity function. We find that the 2dFGRS, SDSS Commissioning Data (CD), ESO Slice Project, Century Survey, Durham/UKST, Mt Stromlo/APM, SSRS2 and NOG luminosity functions require a revision of their published {phi}* values by factors of 1.05+/-0.05, 0.76+/-0.10, 1.02+/-0.22, 1.02+/-0.16, 1.16+/-0.28, 1.75+/-0.37, 1.40+/-0.26 and 1.01+/-0.39, respectively. After renormalizing the galaxy luminosity functions we find a mean local b_J_ luminosity density of 1.986+/-0.031x10^8^h L_{sun}_.Mpc^-3^</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/240#2</TD>
            <TD>2011-09-14T19:31:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2004</TD>
            <TD>ivo://CDS.VizieR/VII/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/240&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/240 [mgczcat]</TD>
            <TD>Millennium Galaxy Catalogue (Liske+, 2003)</TD>
            <TD>The Millennium Galaxy Catalogue (MGC) is a 37.5deg^2^, medium-deep, B-band imaging survey along the celestial equator, taken with the Wide Field Camera on the Isaac Newton Telescope. The survey region is contained within the regions of both the Two Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey Early Data Release (SDSS-EDR). The survey has a uniform isophotal detection limit of 26mag.arcsec^-2^ and it provides a robust, well-defined catalogue of stars and galaxies in the range 16&lt;=B_MGC_&lt;24 mag. Here we describe the survey strategy, the photometric and astrometric calibration, source detection and analysis, and present the galaxy number counts that connect the bright and faint galaxy populations within a single survey. We argue that these counts represent the state of the art and use them to constrain the normalizations ({phi}*) of a number of recent estimates of the local galaxy luminosity function. We find that the 2dFGRS, SDSS Commissioning Data (CD), ESO Slice Project, Century Survey, Durham/UKST, Mt Stromlo/APM, SSRS2 and NOG luminosity functions require a revision of their published {phi}* values by factors of 1.05+/-0.05, 0.76+/-0.10, 1.02+/-0.22, 1.02+/-0.16, 1.16+/-0.28, 1.75+/-0.37, 1.40+/-0.26 and 1.01+/-0.39, respectively. After renormalizing the galaxy luminosity functions we find a mean local b_J_ luminosity density of 1.986+/-0.031x10^8^h L_{sun}_.Mpc^-3^</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/240#mgczcat</TD>
            <TD>2011-09-14T19:31:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2004</TD>
            <TD>ivo://CDS.VizieR/VII/240</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/240&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/240</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/240 [1]</TD>
            <TD>Millennium Galaxy Catalogue (Liske+, 2003)</TD>
            <TD>The Millennium Galaxy Catalogue (MGC) is a 37.5deg^2^, medium-deep, B-band imaging survey along the celestial equator, taken with the Wide Field Camera on the Isaac Newton Telescope. The survey region is contained within the regions of both the Two Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey Early Data Release (SDSS-EDR). The survey has a uniform isophotal detection limit of 26mag.arcsec^-2^ and it provides a robust, well-defined catalogue of stars and galaxies in the range 16&lt;=B_MGC_&lt;24 mag. Here we describe the survey strategy, the photometric and astrometric calibration, source detection and analysis, and present the galaxy number counts that connect the bright and faint galaxy populations within a single survey. We argue that these counts represent the state of the art and use them to constrain the normalizations ({phi}*) of a number of recent estimates of the local galaxy luminosity function. We find that the 2dFGRS, SDSS Commissioning Data (CD), ESO Slice Project, Century Survey, Durham/UKST, Mt Stromlo/APM, SSRS2 and NOG luminosity functions require a revision of their published {phi}* values by factors of 1.05+/-0.05, 0.76+/-0.10, 1.02+/-0.22, 1.02+/-0.16, 1.16+/-0.28, 1.75+/-0.37, 1.40+/-0.26 and 1.01+/-0.39, respectively. After renormalizing the galaxy luminosity functions we find a mean local b_J_ luminosity density of 1.986+/-0.031x10^8^h L_{sun}_.Mpc^-3^</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/240#1</TD>
            <TD>2011-09-14T19:31:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2004</TD>
            <TD>ivo://CDS.VizieR/VII/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/240</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/240</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/240 [2]</TD>
            <TD>Millennium Galaxy Catalogue (Liske+, 2003)</TD>
            <TD>The Millennium Galaxy Catalogue (MGC) is a 37.5deg^2^, medium-deep, B-band imaging survey along the celestial equator, taken with the Wide Field Camera on the Isaac Newton Telescope. The survey region is contained within the regions of both the Two Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey Early Data Release (SDSS-EDR). The survey has a uniform isophotal detection limit of 26mag.arcsec^-2^ and it provides a robust, well-defined catalogue of stars and galaxies in the range 16&lt;=B_MGC_&lt;24 mag. Here we describe the survey strategy, the photometric and astrometric calibration, source detection and analysis, and present the galaxy number counts that connect the bright and faint galaxy populations within a single survey. We argue that these counts represent the state of the art and use them to constrain the normalizations ({phi}*) of a number of recent estimates of the local galaxy luminosity function. We find that the 2dFGRS, SDSS Commissioning Data (CD), ESO Slice Project, Century Survey, Durham/UKST, Mt Stromlo/APM, SSRS2 and NOG luminosity functions require a revision of their published {phi}* values by factors of 1.05+/-0.05, 0.76+/-0.10, 1.02+/-0.22, 1.02+/-0.16, 1.16+/-0.28, 1.75+/-0.37, 1.40+/-0.26 and 1.01+/-0.39, respectively. After renormalizing the galaxy luminosity functions we find a mean local b_J_ luminosity density of 1.986+/-0.031x10^8^h L_{sun}_.Mpc^-3^</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/240#2</TD>
            <TD>2011-09-14T19:31:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2004</TD>
            <TD>ivo://CDS.VizieR/VII/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/240&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/240 [mgczcat]</TD>
            <TD>Millennium Galaxy Catalogue (Liske+, 2003)</TD>
            <TD>The Millennium Galaxy Catalogue (MGC) is a 37.5deg^2^, medium-deep, B-band imaging survey along the celestial equator, taken with the Wide Field Camera on the Isaac Newton Telescope. The survey region is contained within the regions of both the Two Degree Field Galaxy Redshift Survey (2dFGRS) and the Sloan Digital Sky Survey Early Data Release (SDSS-EDR). The survey has a uniform isophotal detection limit of 26mag.arcsec^-2^ and it provides a robust, well-defined catalogue of stars and galaxies in the range 16&lt;=B_MGC_&lt;24 mag. Here we describe the survey strategy, the photometric and astrometric calibration, source detection and analysis, and present the galaxy number counts that connect the bright and faint galaxy populations within a single survey. We argue that these counts represent the state of the art and use them to constrain the normalizations ({phi}*) of a number of recent estimates of the local galaxy luminosity function. We find that the 2dFGRS, SDSS Commissioning Data (CD), ESO Slice Project, Century Survey, Durham/UKST, Mt Stromlo/APM, SSRS2 and NOG luminosity functions require a revision of their published {phi}* values by factors of 1.05+/-0.05, 0.76+/-0.10, 1.02+/-0.22, 1.02+/-0.16, 1.16+/-0.28, 1.75+/-0.37, 1.40+/-0.26 and 1.01+/-0.39, respectively. After renormalizing the galaxy luminosity functions we find a mean local b_J_ luminosity density of 1.986+/-0.031x10^8^h L_{sun}_.Mpc^-3^</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/240#mgczcat</TD>
            <TD>2011-09-14T19:31:41Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-May-2004</TD>
            <TD>ivo://CDS.VizieR/VII/240</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/240&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/240</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/318 [1]</TD>
            <TD>BV photometry of Andromeda II variables (Pritzl+, 2004)</TD>
            <TD>Observations of And II were taken by the HST Wide Field Planetary Camera 2 (WFPC2) as part of the GO program 6514 on 1997 August 29 and 1997 September 3, using the same orientation. Three 1200s integrations through the F555W filter and seven 1300s integrations through the F450W filter were taken during the first set of observations. Identical exposure times were used for the second set of observations, but there were four F555W and eight F450W integrations. The images were offset from the center of the dSph galaxy in order to avoid bright foreground stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318#1</TD>
            <TD>2011-09-14T19:31:57Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/318</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/318</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/318 [2]</TD>
            <TD>BV photometry of Andromeda II variables (Pritzl+, 2004)</TD>
            <TD>Observations of And II were taken by the HST Wide Field Planetary Camera 2 (WFPC2) as part of the GO program 6514 on 1997 August 29 and 1997 September 3, using the same orientation. Three 1200s integrations through the F555W filter and seven 1300s integrations through the F450W filter were taken during the first set of observations. Identical exposure times were used for the second set of observations, but there were four F555W and eight F450W integrations. The images were offset from the center of the dSph galaxy in order to avoid bright foreground stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318#2</TD>
            <TD>2011-09-14T19:31:57Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/318&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/318</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/318 [table2]</TD>
            <TD>BV photometry of Andromeda II variables (Pritzl+, 2004)</TD>
            <TD>Observations of And II were taken by the HST Wide Field Planetary Camera 2 (WFPC2) as part of the GO program 6514 on 1997 August 29 and 1997 September 3, using the same orientation. Three 1200s integrations through the F555W filter and seven 1300s integrations through the F450W filter were taken during the first set of observations. Identical exposure times were used for the second set of observations, but there were four F555W and eight F450W integrations. The images were offset from the center of the dSph galaxy in order to avoid bright foreground stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318#table2</TD>
            <TD>2011-09-14T19:31:57Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/318&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/318</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/318 [1]</TD>
            <TD>BV photometry of Andromeda II variables (Pritzl+, 2004)</TD>
            <TD>Observations of And II were taken by the HST Wide Field Planetary Camera 2 (WFPC2) as part of the GO program 6514 on 1997 August 29 and 1997 September 3, using the same orientation. Three 1200s integrations through the F555W filter and seven 1300s integrations through the F450W filter were taken during the first set of observations. Identical exposure times were used for the second set of observations, but there were four F555W and eight F450W integrations. The images were offset from the center of the dSph galaxy in order to avoid bright foreground stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318#1</TD>
            <TD>2011-09-14T19:31:57Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/318</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/318</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/318 [2]</TD>
            <TD>BV photometry of Andromeda II variables (Pritzl+, 2004)</TD>
            <TD>Observations of And II were taken by the HST Wide Field Planetary Camera 2 (WFPC2) as part of the GO program 6514 on 1997 August 29 and 1997 September 3, using the same orientation. Three 1200s integrations through the F555W filter and seven 1300s integrations through the F450W filter were taken during the first set of observations. Identical exposure times were used for the second set of observations, but there were four F555W and eight F450W integrations. The images were offset from the center of the dSph galaxy in order to avoid bright foreground stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318#2</TD>
            <TD>2011-09-14T19:31:57Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/318&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/318</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/318 [table2]</TD>
            <TD>BV photometry of Andromeda II variables (Pritzl+, 2004)</TD>
            <TD>Observations of And II were taken by the HST Wide Field Planetary Camera 2 (WFPC2) as part of the GO program 6514 on 1997 August 29 and 1997 September 3, using the same orientation. Three 1200s integrations through the F555W filter and seven 1300s integrations through the F450W filter were taken during the first set of observations. Identical exposure times were used for the second set of observations, but there were four F555W and eight F450W integrations. The images were offset from the center of the dSph galaxy in order to avoid bright foreground stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318#table2</TD>
            <TD>2011-09-14T19:31:57Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/318&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/318</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/318 [1]</TD>
            <TD>BV photometry of Andromeda II variables (Pritzl+, 2004)</TD>
            <TD>Observations of And II were taken by the HST Wide Field Planetary Camera 2 (WFPC2) as part of the GO program 6514 on 1997 August 29 and 1997 September 3, using the same orientation. Three 1200s integrations through the F555W filter and seven 1300s integrations through the F450W filter were taken during the first set of observations. Identical exposure times were used for the second set of observations, but there were four F555W and eight F450W integrations. The images were offset from the center of the dSph galaxy in order to avoid bright foreground stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318#1</TD>
            <TD>2011-09-14T19:31:57Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/318</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/318</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/318 [2]</TD>
            <TD>BV photometry of Andromeda II variables (Pritzl+, 2004)</TD>
            <TD>Observations of And II were taken by the HST Wide Field Planetary Camera 2 (WFPC2) as part of the GO program 6514 on 1997 August 29 and 1997 September 3, using the same orientation. Three 1200s integrations through the F555W filter and seven 1300s integrations through the F450W filter were taken during the first set of observations. Identical exposure times were used for the second set of observations, but there were four F555W and eight F450W integrations. The images were offset from the center of the dSph galaxy in order to avoid bright foreground stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318#2</TD>
            <TD>2011-09-14T19:31:57Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/318&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/318</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/127/318 [table2]</TD>
            <TD>BV photometry of Andromeda II variables (Pritzl+, 2004)</TD>
            <TD>Observations of And II were taken by the HST Wide Field Planetary Camera 2 (WFPC2) as part of the GO program 6514 on 1997 August 29 and 1997 September 3, using the same orientation. Three 1200s integrations through the F555W filter and seven 1300s integrations through the F450W filter were taken during the first set of observations. Identical exposure times were used for the second set of observations, but there were four F555W and eight F450W integrations. The images were offset from the center of the dSph galaxy in order to avoid bright foreground stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318#table2</TD>
            <TD>2011-09-14T19:31:57Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/318</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/127/318&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/318</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1513 [1]</TD>
            <TD>Lick indices on M67 members (Schiavon+, 2004)</TD>
            <TD>We construct an integrated spectrum of the intermediate-age, solar-metallicity Galactic cluster M67, from individual spectroscopic observations of bona fide cluster members. The spectrum so obtained is used as a template to test our stellar population synthesis models, in an age and metallicity regime where such models remain largely untested. As a result, we demonstrate that our models predict a spectroscopic age of 3.5+/-0.5Gyr for M67, which is the same age we obtain from fitting isochrones to the color-magnitude diagram of the cluster. Full consistency is reached when using either H{beta}, H{gamma}, or H{delta} as the age indicator. We also check if the models, when applied to the cluster integrated spectrum, predict elemental abundances in agreement with the known detailed abundance pattern of the cluster. The models also pass the latter test, by predicting the abundances of iron, magnesium, carbon, and nitrogen in agreement with detailed abundance analyses of cluster stars to within 0.1dex. Encouraged by the high degree of consistency of our models, we apply them to the study of the integrated spectrum of the central 3" of the compact elliptical galaxy M32.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513#1</TD>
            <TD>2011-09-14T19:32:55Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1513</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1513</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1513 [2]</TD>
            <TD>Lick indices on M67 members (Schiavon+, 2004)</TD>
            <TD>We construct an integrated spectrum of the intermediate-age, solar-metallicity Galactic cluster M67, from individual spectroscopic observations of bona fide cluster members. The spectrum so obtained is used as a template to test our stellar population synthesis models, in an age and metallicity regime where such models remain largely untested. As a result, we demonstrate that our models predict a spectroscopic age of 3.5+/-0.5Gyr for M67, which is the same age we obtain from fitting isochrones to the color-magnitude diagram of the cluster. Full consistency is reached when using either H{beta}, H{gamma}, or H{delta} as the age indicator. We also check if the models, when applied to the cluster integrated spectrum, predict elemental abundances in agreement with the known detailed abundance pattern of the cluster. The models also pass the latter test, by predicting the abundances of iron, magnesium, carbon, and nitrogen in agreement with detailed abundance analyses of cluster stars to within 0.1dex. Encouraged by the high degree of consistency of our models, we apply them to the study of the integrated spectrum of the central 3" of the compact elliptical galaxy M32.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513#2</TD>
            <TD>2011-09-14T19:32:55Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1513&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1513</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/116 [1]</TD>
            <TD>Southern Galaxy Catalogue (SGC) (Corwin+ 1985)</TD>
            <TD>The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D&gt;1.52.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/116#1</TD>
            <TD>2011-09-14T18:41:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1994</TD>
            <TD>ivo://CDS.VizieR/VII/116</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/116</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/116</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/116 [2]</TD>
            <TD>Southern Galaxy Catalogue (SGC) (Corwin+ 1985)</TD>
            <TD>The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D&gt;1.52.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/116#2</TD>
            <TD>2011-09-14T18:41:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1994</TD>
            <TD>ivo://CDS.VizieR/VII/116</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/116&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/116</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/116 [catalog]</TD>
            <TD>Southern Galaxy Catalogue (SGC) (Corwin+ 1985)</TD>
            <TD>The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D&gt;1.52.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/116#catalog</TD>
            <TD>2011-09-14T18:41:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1994</TD>
            <TD>ivo://CDS.VizieR/VII/116</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/116&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/116</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1513 [1]</TD>
            <TD>Lick indices on M67 members (Schiavon+, 2004)</TD>
            <TD>We construct an integrated spectrum of the intermediate-age, solar-metallicity Galactic cluster M67, from individual spectroscopic observations of bona fide cluster members. The spectrum so obtained is used as a template to test our stellar population synthesis models, in an age and metallicity regime where such models remain largely untested. As a result, we demonstrate that our models predict a spectroscopic age of 3.5+/-0.5Gyr for M67, which is the same age we obtain from fitting isochrones to the color-magnitude diagram of the cluster. Full consistency is reached when using either H{beta}, H{gamma}, or H{delta} as the age indicator. We also check if the models, when applied to the cluster integrated spectrum, predict elemental abundances in agreement with the known detailed abundance pattern of the cluster. The models also pass the latter test, by predicting the abundances of iron, magnesium, carbon, and nitrogen in agreement with detailed abundance analyses of cluster stars to within 0.1dex. Encouraged by the high degree of consistency of our models, we apply them to the study of the integrated spectrum of the central 3" of the compact elliptical galaxy M32.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513#1</TD>
            <TD>2011-09-14T19:32:55Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1513</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1513</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1513 [2]</TD>
            <TD>Lick indices on M67 members (Schiavon+, 2004)</TD>
            <TD>We construct an integrated spectrum of the intermediate-age, solar-metallicity Galactic cluster M67, from individual spectroscopic observations of bona fide cluster members. The spectrum so obtained is used as a template to test our stellar population synthesis models, in an age and metallicity regime where such models remain largely untested. As a result, we demonstrate that our models predict a spectroscopic age of 3.5+/-0.5Gyr for M67, which is the same age we obtain from fitting isochrones to the color-magnitude diagram of the cluster. Full consistency is reached when using either H{beta}, H{gamma}, or H{delta} as the age indicator. We also check if the models, when applied to the cluster integrated spectrum, predict elemental abundances in agreement with the known detailed abundance pattern of the cluster. The models also pass the latter test, by predicting the abundances of iron, magnesium, carbon, and nitrogen in agreement with detailed abundance analyses of cluster stars to within 0.1dex. Encouraged by the high degree of consistency of our models, we apply them to the study of the integrated spectrum of the central 3" of the compact elliptical galaxy M32.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513#2</TD>
            <TD>2011-09-14T19:32:55Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1513&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1513</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/116 [1]</TD>
            <TD>Southern Galaxy Catalogue (SGC) (Corwin+ 1985)</TD>
            <TD>The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D&gt;1.52.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/116#1</TD>
            <TD>2011-09-14T18:41:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1994</TD>
            <TD>ivo://CDS.VizieR/VII/116</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/116</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/116</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/116 [2]</TD>
            <TD>Southern Galaxy Catalogue (SGC) (Corwin+ 1985)</TD>
            <TD>The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D&gt;1.52.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/116#2</TD>
            <TD>2011-09-14T18:41:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1994</TD>
            <TD>ivo://CDS.VizieR/VII/116</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/116&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/116</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/116 [catalog]</TD>
            <TD>Southern Galaxy Catalogue (SGC) (Corwin+ 1985)</TD>
            <TD>The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D&gt;1.52.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/116#catalog</TD>
            <TD>2011-09-14T18:41:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1994</TD>
            <TD>ivo://CDS.VizieR/VII/116</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/116&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/116</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1513 [1]</TD>
            <TD>Lick indices on M67 members (Schiavon+, 2004)</TD>
            <TD>We construct an integrated spectrum of the intermediate-age, solar-metallicity Galactic cluster M67, from individual spectroscopic observations of bona fide cluster members. The spectrum so obtained is used as a template to test our stellar population synthesis models, in an age and metallicity regime where such models remain largely untested. As a result, we demonstrate that our models predict a spectroscopic age of 3.5+/-0.5Gyr for M67, which is the same age we obtain from fitting isochrones to the color-magnitude diagram of the cluster. Full consistency is reached when using either H{beta}, H{gamma}, or H{delta} as the age indicator. We also check if the models, when applied to the cluster integrated spectrum, predict elemental abundances in agreement with the known detailed abundance pattern of the cluster. The models also pass the latter test, by predicting the abundances of iron, magnesium, carbon, and nitrogen in agreement with detailed abundance analyses of cluster stars to within 0.1dex. Encouraged by the high degree of consistency of our models, we apply them to the study of the integrated spectrum of the central 3" of the compact elliptical galaxy M32.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513#1</TD>
            <TD>2011-09-14T19:32:55Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1513</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1513</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1513 [2]</TD>
            <TD>Lick indices on M67 members (Schiavon+, 2004)</TD>
            <TD>We construct an integrated spectrum of the intermediate-age, solar-metallicity Galactic cluster M67, from individual spectroscopic observations of bona fide cluster members. The spectrum so obtained is used as a template to test our stellar population synthesis models, in an age and metallicity regime where such models remain largely untested. As a result, we demonstrate that our models predict a spectroscopic age of 3.5+/-0.5Gyr for M67, which is the same age we obtain from fitting isochrones to the color-magnitude diagram of the cluster. Full consistency is reached when using either H{beta}, H{gamma}, or H{delta} as the age indicator. We also check if the models, when applied to the cluster integrated spectrum, predict elemental abundances in agreement with the known detailed abundance pattern of the cluster. The models also pass the latter test, by predicting the abundances of iron, magnesium, carbon, and nitrogen in agreement with detailed abundance analyses of cluster stars to within 0.1dex. Encouraged by the high degree of consistency of our models, we apply them to the study of the integrated spectrum of the central 3" of the compact elliptical galaxy M32.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513#2</TD>
            <TD>2011-09-14T19:32:55Z</TD>
            <TD>#Open_Clusters#Photometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1513</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1513&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1513</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/116 [1]</TD>
            <TD>Southern Galaxy Catalogue (SGC) (Corwin+ 1985)</TD>
            <TD>The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D&gt;1.52.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/116#1</TD>
            <TD>2011-09-14T18:41:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1994</TD>
            <TD>ivo://CDS.VizieR/VII/116</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/116</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/116</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/116 [2]</TD>
            <TD>Southern Galaxy Catalogue (SGC) (Corwin+ 1985)</TD>
            <TD>The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D&gt;1.52.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/116#2</TD>
            <TD>2011-09-14T18:41:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1994</TD>
            <TD>ivo://CDS.VizieR/VII/116</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/116&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/116</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/116 [catalog]</TD>
            <TD>Southern Galaxy Catalogue (SGC) (Corwin+ 1985)</TD>
            <TD>The "Southern Galaxy Catalogue" provides a finding list of galaxies larger than about 1.5 to 2 arc minutes, south of declination -17 degrees. It includes, as far as possible, precise positions, morphological types, luminosity classifications, and diameters. It is essentially complete for log D&gt;1.52.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/116#catalog</TD>
            <TD>2011-09-14T18:41:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-1994</TD>
            <TD>ivo://CDS.VizieR/VII/116</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/116&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/116</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/330/1 [1]</TD>
            <TD>HST observations of Extremely Red Objects (Smith+, 2002)</TD>
            <TD>We present the results of a survey for extremely red objects (EROs) undertaken in the fields of 10 massive galaxy cluster lenses at z~0.2, combining sensitive, high-resolution Hubble Space Telescope imaging with deep, half-arcsecond K-band imaging from UKIRT. We detect 60 EROs with (R-K)&gt;=5.3, of which 26 have (R-K)&gt;=6.0 in a total image-plane survey area of 49arcmin2 down to K=20.6, including one multiply imaged ERO.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1#1</TD>
            <TD>2011-09-14T19:33:26Z</TD>
            <TD>#Galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/330/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/330/1 [2]</TD>
            <TD>HST observations of Extremely Red Objects (Smith+, 2002)</TD>
            <TD>We present the results of a survey for extremely red objects (EROs) undertaken in the fields of 10 massive galaxy cluster lenses at z~0.2, combining sensitive, high-resolution Hubble Space Telescope imaging with deep, half-arcsecond K-band imaging from UKIRT. We detect 60 EROs with (R-K)&gt;=5.3, of which 26 have (R-K)&gt;=6.0 in a total image-plane survey area of 49arcmin2 down to K=20.6, including one multiply imaged ERO.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1#2</TD>
            <TD>2011-09-14T19:33:26Z</TD>
            <TD>#Galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/330/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/2895 [1]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#1</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/2895</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/2895 [2]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#2</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table8]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table8</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table6b]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table6b</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table6a]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table6a</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table7a]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table7a</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table1]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table1</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2895 [table7b]</TD>
            <TD>HDF-N Caltech faint galaxy redshift survey. XIII. (Cohen 2001)</TD>
            <TD>We introduce a new empirical function for modeling the spectral energy distributions (SEDs) of galaxies. We apply it to a sample of 590 galaxies in the region of the Hubble Deep Field (HDF) with z&lt;1.5 using multicolor photometry with wide wavelength coverage combined with spectroscopic redshifts from our 93% complete R-selected redshift survey there.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895#table7b</TD>
            <TD>2011-09-14T19:11:24Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2895</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2895&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2895</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/521 [1]</TD>
            <TD>Very luminous IRAS galaxies spectra. (Wu+ 1998)</TD>
            <TD>This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)&gt;=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag&lt;=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. &lt;II/174&gt;). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521#1</TD>
            <TD>2011-09-14T18:42:07Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/521 [2]</TD>
            <TD>Very luminous IRAS galaxies spectra. (Wu+ 1998)</TD>
            <TD>This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)&gt;=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag&lt;=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. &lt;II/174&gt;). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521#2</TD>
            <TD>2011-09-14T18:42:07Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/521</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/521 [table2]</TD>
            <TD>Very luminous IRAS galaxies spectra. (Wu+ 1998)</TD>
            <TD>This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)&gt;=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag&lt;=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. &lt;II/174&gt;). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521#table2</TD>
            <TD>2011-09-14T18:42:07Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/521&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/330/1 [1]</TD>
            <TD>HST observations of Extremely Red Objects (Smith+, 2002)</TD>
            <TD>We present the results of a survey for extremely red objects (EROs) undertaken in the fields of 10 massive galaxy cluster lenses at z~0.2, combining sensitive, high-resolution Hubble Space Telescope imaging with deep, half-arcsecond K-band imaging from UKIRT. We detect 60 EROs with (R-K)&gt;=5.3, of which 26 have (R-K)&gt;=6.0 in a total image-plane survey area of 49arcmin2 down to K=20.6, including one multiply imaged ERO.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1#1</TD>
            <TD>2011-09-14T19:33:26Z</TD>
            <TD>#Galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/330/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/330/1 [2]</TD>
            <TD>HST observations of Extremely Red Objects (Smith+, 2002)</TD>
            <TD>We present the results of a survey for extremely red objects (EROs) undertaken in the fields of 10 massive galaxy cluster lenses at z~0.2, combining sensitive, high-resolution Hubble Space Telescope imaging with deep, half-arcsecond K-band imaging from UKIRT. We detect 60 EROs with (R-K)&gt;=5.3, of which 26 have (R-K)&gt;=6.0 in a total image-plane survey area of 49arcmin2 down to K=20.6, including one multiply imaged ERO.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1#2</TD>
            <TD>2011-09-14T19:33:26Z</TD>
            <TD>#Galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/330/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/377/428 [1]</TD>
            <TD>Abell 970 galaxies radial velocities (Sodre+, 2001)</TD>
            <TD>We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428#1</TD>
            <TD>2011-09-14T19:11:38Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/377/428</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/428</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/377/428 [2]</TD>
            <TD>Abell 970 galaxies radial velocities (Sodre+, 2001)</TD>
            <TD>We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428#2</TD>
            <TD>2011-09-14T19:11:38Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/377/428&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/428</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/377/428 [table1]</TD>
            <TD>Abell 970 galaxies radial velocities (Sodre+, 2001)</TD>
            <TD>We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428#table1</TD>
            <TD>2011-09-14T19:11:38Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/377/428&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/428</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/330/1 [1]</TD>
            <TD>HST observations of Extremely Red Objects (Smith+, 2002)</TD>
            <TD>We present the results of a survey for extremely red objects (EROs) undertaken in the fields of 10 massive galaxy cluster lenses at z~0.2, combining sensitive, high-resolution Hubble Space Telescope imaging with deep, half-arcsecond K-band imaging from UKIRT. We detect 60 EROs with (R-K)&gt;=5.3, of which 26 have (R-K)&gt;=6.0 in a total image-plane survey area of 49arcmin2 down to K=20.6, including one multiply imaged ERO.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1#1</TD>
            <TD>2011-09-14T19:33:26Z</TD>
            <TD>#Galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/330/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/330/1 [2]</TD>
            <TD>HST observations of Extremely Red Objects (Smith+, 2002)</TD>
            <TD>We present the results of a survey for extremely red objects (EROs) undertaken in the fields of 10 massive galaxy cluster lenses at z~0.2, combining sensitive, high-resolution Hubble Space Telescope imaging with deep, half-arcsecond K-band imaging from UKIRT. We detect 60 EROs with (R-K)&gt;=5.3, of which 26 have (R-K)&gt;=6.0 in a total image-plane survey area of 49arcmin2 down to K=20.6, including one multiply imaged ERO.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1#2</TD>
            <TD>2011-09-14T19:33:26Z</TD>
            <TD>#Galaxies#Gravitational_lensing#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/330/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/330/1&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/330/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/521 [1]</TD>
            <TD>Very luminous IRAS galaxies spectra. (Wu+ 1998)</TD>
            <TD>This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)&gt;=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag&lt;=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. &lt;II/174&gt;). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521#1</TD>
            <TD>2011-09-14T18:42:07Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/521 [2]</TD>
            <TD>Very luminous IRAS galaxies spectra. (Wu+ 1998)</TD>
            <TD>This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)&gt;=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag&lt;=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. &lt;II/174&gt;). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521#2</TD>
            <TD>2011-09-14T18:42:07Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/521</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/521 [table2]</TD>
            <TD>Very luminous IRAS galaxies spectra. (Wu+ 1998)</TD>
            <TD>This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)&gt;=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag&lt;=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. &lt;II/174&gt;). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521#table2</TD>
            <TD>2011-09-14T18:42:07Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/521&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/116/429 [1]</TD>
            <TD>Classification of Coma early galaxies (Andreon+ 1996)</TD>
            <TD>We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429#1</TD>
            <TD>2011-09-14T18:49:48Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/116/429</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/429</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/116/429 [2]</TD>
            <TD>Classification of Coma early galaxies (Andreon+ 1996)</TD>
            <TD>We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429#2</TD>
            <TD>2011-09-14T18:49:48Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/116/429&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/429</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/116/429 [table4]</TD>
            <TD>Classification of Coma early galaxies (Andreon+ 1996)</TD>
            <TD>We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429#table4</TD>
            <TD>2011-09-14T18:49:48Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/116/429&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/429</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/146/209 [1]</TD>
            <TD>STIS emission-line galaxies observations (Teplitz+, 2003)</TD>
            <TD>In the first 3 years of operation the Space Telescope Imaging Spectrograph (STIS) obtained slitless spectra of ~2500 fields in parallel to prime Hubble Space Telescope (HST) observations as part of the STIS parallel survey (SPS). The archive contains ~300 fields at high Galactic latitude (|b|&gt;30{deg}) with spectroscopic exposure times greater than 3000s. This sample contains 219 fields (excluding special regions and requiring a consistent grating angle) observed between 1997 June 6 and 2000 September 21, with a total survey area of ~160-arcmin^2^. At this depth, the SPS detects an average of one emission-line galaxy per three fields. We present the analysis of these data and the identification of 131 low- to intermediate-redshift galaxies detected by optical emission lines. The sample contains 78 objects with emission lines that we infer to be redshifted [O II] {lambda}3727 emission at 0.43&lt;z&lt;1.7. The comoving number density of these objects is comparable to that of H{alpha}-emitting galaxies in the NICMOS parallel observations. One quasar and three probable Seyfert galaxies are detected. Many of the emission-line objects show morphologies suggestive of mergers or interactions. The reduced data are available upon request from the authors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209#1</TD>
            <TD>2011-09-14T19:33:33Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/146/209</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/146/209</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/146/209 [2]</TD>
            <TD>STIS emission-line galaxies observations (Teplitz+, 2003)</TD>
            <TD>In the first 3 years of operation the Space Telescope Imaging Spectrograph (STIS) obtained slitless spectra of ~2500 fields in parallel to prime Hubble Space Telescope (HST) observations as part of the STIS parallel survey (SPS). The archive contains ~300 fields at high Galactic latitude (|b|&gt;30{deg}) with spectroscopic exposure times greater than 3000s. This sample contains 219 fields (excluding special regions and requiring a consistent grating angle) observed between 1997 June 6 and 2000 September 21, with a total survey area of ~160-arcmin^2^. At this depth, the SPS detects an average of one emission-line galaxy per three fields. We present the analysis of these data and the identification of 131 low- to intermediate-redshift galaxies detected by optical emission lines. The sample contains 78 objects with emission lines that we infer to be redshifted [O II] {lambda}3727 emission at 0.43&lt;z&lt;1.7. The comoving number density of these objects is comparable to that of H{alpha}-emitting galaxies in the NICMOS parallel observations. One quasar and three probable Seyfert galaxies are detected. Many of the emission-line objects show morphologies suggestive of mergers or interactions. The reduced data are available upon request from the authors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209#2</TD>
            <TD>2011-09-14T19:33:33Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>16-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/146/209&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/146/209</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/116/429 [1]</TD>
            <TD>Classification of Coma early galaxies (Andreon+ 1996)</TD>
            <TD>We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429#1</TD>
            <TD>2011-09-14T18:49:48Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/116/429</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/429</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/116/429 [2]</TD>
            <TD>Classification of Coma early galaxies (Andreon+ 1996)</TD>
            <TD>We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429#2</TD>
            <TD>2011-09-14T18:49:48Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/116/429&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/429</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/116/429 [table4]</TD>
            <TD>Classification of Coma early galaxies (Andreon+ 1996)</TD>
            <TD>We present the results of an isophotal shape analysis of three samples of galaxies in the Coma cluster. Quantitative morphology, together with structural and photometric parameters, is given for each galaxy. Special emphasis has been placed on the detailed classification of early-type galaxies. The three samples are: i) a sample of 97 early-type galaxies brighter than m_B_=17.00 falling within one degree from the center of the Coma cluster; these galaxies were observed with CCD cameras, mostly in good to excellent resolution conditions; ii) a magnitude complete sample of 107 galaxies of all morphological types down to m_B_=17.00 falling in a circular region of 50arcmin diameter, slightly offcentered to the North-West of the cluster center; the images for this and the next sample come from digitized photographic plates; iii) a complete comparison sample of 26 galaxies of all morphological types down to m_R_=16.05 (or m_B_=~17.5), also in a region of 50arcmin diameter, but centered 2.6degrees West of the cluster center. The reliability of our morphological classifications and structural parameters of galaxies, down to the adopted magnitude limits, is assessed by comparing the results on those galaxies for which we had images taken with different instrumentation and/or seeing conditions, and by comparing our results with similar data from other observers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429#table4</TD>
            <TD>2011-09-14T18:49:48Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/116/429</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/116/429&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/116/429</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/127/521 [1]</TD>
            <TD>Very luminous IRAS galaxies spectra. (Wu+ 1998)</TD>
            <TD>This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)&gt;=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag&lt;=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. &lt;II/174&gt;). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521#1</TD>
            <TD>2011-09-14T18:42:07Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/127/521</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/521</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/127/521 [2]</TD>
            <TD>Very luminous IRAS galaxies spectra. (Wu+ 1998)</TD>
            <TD>This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)&gt;=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag&lt;=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. &lt;II/174&gt;). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521#2</TD>
            <TD>2011-09-14T18:42:07Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/127/521&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/521</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/127/521 [table2]</TD>
            <TD>Very luminous IRAS galaxies spectra. (Wu+ 1998)</TD>
            <TD>This paper presents the results of spectral observations for the largest complete sample of very luminous IRAS galaxies obtained to date. The sample consists of those 73 objects for which log(L_IR_/L_sun_)&gt;=11.5 (H0=50 km/s/Mpc, q0=0.5) and mag&lt;=15.5, and was extracted from the 2Jy IRAS redshift catalog (Cat. &lt;II/174&gt;). All spectra were obtained using 2.16m telescope of Beijing Astronomical Observatory during the years 1994-1996. A total of 123 galaxy spectra were obtained with spectral ranges of 4400A to 7100A and 3500A to 8100A at resolutions of 11.2A and 9.3A respectively. In addition to the 73 spectra for sample galaxies, we also present spectra for ten non-sample galaxies and a further 40 for the companions of sample galaxies. The data presented include nuclear spectrum and the parameters describing the emission lines, absorption lines and continua as well as DSS images and environmental parameters.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521#table2</TD>
            <TD>2011-09-14T18:42:07Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/127/521</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/127/521&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/127/521</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/124/1 [1]</TD>
            <TD>The Centaurus Cluster Catalogue (Jerjen+ 1997)</TD>
            <TD>The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1#1</TD>
            <TD>2011-09-14T18:49:56Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/124/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/124/1 [2]</TD>
            <TD>The Centaurus Cluster Catalogue (Jerjen+ 1997)</TD>
            <TD>The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1#2</TD>
            <TD>2011-09-14T18:49:56Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/124/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/124/1 [table6]</TD>
            <TD>The Centaurus Cluster Catalogue (Jerjen+ 1997)</TD>
            <TD>The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1#table6</TD>
            <TD>2011-09-14T18:49:56Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/124/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/146/209 [1]</TD>
            <TD>STIS emission-line galaxies observations (Teplitz+, 2003)</TD>
            <TD>In the first 3 years of operation the Space Telescope Imaging Spectrograph (STIS) obtained slitless spectra of ~2500 fields in parallel to prime Hubble Space Telescope (HST) observations as part of the STIS parallel survey (SPS). The archive contains ~300 fields at high Galactic latitude (|b|&gt;30{deg}) with spectroscopic exposure times greater than 3000s. This sample contains 219 fields (excluding special regions and requiring a consistent grating angle) observed between 1997 June 6 and 2000 September 21, with a total survey area of ~160-arcmin^2^. At this depth, the SPS detects an average of one emission-line galaxy per three fields. We present the analysis of these data and the identification of 131 low- to intermediate-redshift galaxies detected by optical emission lines. The sample contains 78 objects with emission lines that we infer to be redshifted [O II] {lambda}3727 emission at 0.43&lt;z&lt;1.7. The comoving number density of these objects is comparable to that of H{alpha}-emitting galaxies in the NICMOS parallel observations. One quasar and three probable Seyfert galaxies are detected. Many of the emission-line objects show morphologies suggestive of mergers or interactions. The reduced data are available upon request from the authors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209#1</TD>
            <TD>2011-09-14T19:33:33Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/146/209</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/146/209</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/146/209 [2]</TD>
            <TD>STIS emission-line galaxies observations (Teplitz+, 2003)</TD>
            <TD>In the first 3 years of operation the Space Telescope Imaging Spectrograph (STIS) obtained slitless spectra of ~2500 fields in parallel to prime Hubble Space Telescope (HST) observations as part of the STIS parallel survey (SPS). The archive contains ~300 fields at high Galactic latitude (|b|&gt;30{deg}) with spectroscopic exposure times greater than 3000s. This sample contains 219 fields (excluding special regions and requiring a consistent grating angle) observed between 1997 June 6 and 2000 September 21, with a total survey area of ~160-arcmin^2^. At this depth, the SPS detects an average of one emission-line galaxy per three fields. We present the analysis of these data and the identification of 131 low- to intermediate-redshift galaxies detected by optical emission lines. The sample contains 78 objects with emission lines that we infer to be redshifted [O II] {lambda}3727 emission at 0.43&lt;z&lt;1.7. The comoving number density of these objects is comparable to that of H{alpha}-emitting galaxies in the NICMOS parallel observations. One quasar and three probable Seyfert galaxies are detected. Many of the emission-line objects show morphologies suggestive of mergers or interactions. The reduced data are available upon request from the authors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209#2</TD>
            <TD>2011-09-14T19:33:33Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/146/209&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/146/209</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/124/1 [1]</TD>
            <TD>The Centaurus Cluster Catalogue (Jerjen+ 1997)</TD>
            <TD>The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1#1</TD>
            <TD>2011-09-14T18:49:56Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/124/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/124/1 [2]</TD>
            <TD>The Centaurus Cluster Catalogue (Jerjen+ 1997)</TD>
            <TD>The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1#2</TD>
            <TD>2011-09-14T18:49:56Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/124/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/124/1 [table6]</TD>
            <TD>The Centaurus Cluster Catalogue (Jerjen+ 1997)</TD>
            <TD>The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1#table6</TD>
            <TD>2011-09-14T18:49:56Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/124/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/114/565 [1]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#1</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/114/565</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/114/565 [2]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#2</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/114/565&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/565 [table2]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#table2</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/565&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/565 [table1]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#table1</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/565&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/124/1 [1]</TD>
            <TD>The Centaurus Cluster Catalogue (Jerjen+ 1997)</TD>
            <TD>The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1#1</TD>
            <TD>2011-09-14T18:49:56Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/124/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/124/1 [2]</TD>
            <TD>The Centaurus Cluster Catalogue (Jerjen+ 1997)</TD>
            <TD>The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1#2</TD>
            <TD>2011-09-14T18:49:56Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/124/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/124/1 [table6]</TD>
            <TD>The Centaurus Cluster Catalogue (Jerjen+ 1997)</TD>
            <TD>The central region of the Centaurus cluster was surveyed on a film copy of a high-resolution photographic Las Campanas duPont plate. A large number of cluster galaxy candidates were identified down to a limiting magnitude of 21.5 in B. Between cluster members and background objects were distinguished by applying morphological criteria. Following the morphological classification of each member, the images of all 296 cluster galaxies on a SERC deep-blue sky survey plate were digitized, processed and analysed with the image processing package MIDAS. We established total apparent B-magnitude and other structure parameters for each cluster galaxy which are listed in the Centaurus Cluster Catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1#table6</TD>
            <TD>2011-09-14T18:49:56Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Nov-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/124/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/124/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/124/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/114/565 [1]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#1</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/114/565</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/114/565 [2]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#2</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/114/565&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/565 [table2]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#table2</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/565&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/565 [table1]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#table1</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/565&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/145 [1]</TD>
            <TD>Nearby Galaxies Catalogue (NBG) (Tully 1988)</TD>
            <TD>This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/145#1</TD>
            <TD>2011-09-14T18:52:46Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/145</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/145</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/145</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/145 [2]</TD>
            <TD>Nearby Galaxies Catalogue (NBG) (Tully 1988)</TD>
            <TD>This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/145#2</TD>
            <TD>2011-09-14T18:52:46Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/145</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/145&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/145</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/145 [catalog]</TD>
            <TD>Nearby Galaxies Catalogue (NBG) (Tully 1988)</TD>
            <TD>This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/145#catalog</TD>
            <TD>2011-09-14T18:52:46Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/145</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/145&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/145</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/146/209 [1]</TD>
            <TD>STIS emission-line galaxies observations (Teplitz+, 2003)</TD>
            <TD>In the first 3 years of operation the Space Telescope Imaging Spectrograph (STIS) obtained slitless spectra of ~2500 fields in parallel to prime Hubble Space Telescope (HST) observations as part of the STIS parallel survey (SPS). The archive contains ~300 fields at high Galactic latitude (|b|&gt;30{deg}) with spectroscopic exposure times greater than 3000s. This sample contains 219 fields (excluding special regions and requiring a consistent grating angle) observed between 1997 June 6 and 2000 September 21, with a total survey area of ~160-arcmin^2^. At this depth, the SPS detects an average of one emission-line galaxy per three fields. We present the analysis of these data and the identification of 131 low- to intermediate-redshift galaxies detected by optical emission lines. The sample contains 78 objects with emission lines that we infer to be redshifted [O II] {lambda}3727 emission at 0.43&lt;z&lt;1.7. The comoving number density of these objects is comparable to that of H{alpha}-emitting galaxies in the NICMOS parallel observations. One quasar and three probable Seyfert galaxies are detected. Many of the emission-line objects show morphologies suggestive of mergers or interactions. The reduced data are available upon request from the authors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209#1</TD>
            <TD>2011-09-14T19:33:33Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/146/209</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/146/209</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/146/209 [2]</TD>
            <TD>STIS emission-line galaxies observations (Teplitz+, 2003)</TD>
            <TD>In the first 3 years of operation the Space Telescope Imaging Spectrograph (STIS) obtained slitless spectra of ~2500 fields in parallel to prime Hubble Space Telescope (HST) observations as part of the STIS parallel survey (SPS). The archive contains ~300 fields at high Galactic latitude (|b|&gt;30{deg}) with spectroscopic exposure times greater than 3000s. This sample contains 219 fields (excluding special regions and requiring a consistent grating angle) observed between 1997 June 6 and 2000 September 21, with a total survey area of ~160-arcmin^2^. At this depth, the SPS detects an average of one emission-line galaxy per three fields. We present the analysis of these data and the identification of 131 low- to intermediate-redshift galaxies detected by optical emission lines. The sample contains 78 objects with emission lines that we infer to be redshifted [O II] {lambda}3727 emission at 0.43&lt;z&lt;1.7. The comoving number density of these objects is comparable to that of H{alpha}-emitting galaxies in the NICMOS parallel observations. One quasar and three probable Seyfert galaxies are detected. Many of the emission-line objects show morphologies suggestive of mergers or interactions. The reduced data are available upon request from the authors.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209#2</TD>
            <TD>2011-09-14T19:33:33Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/146/209</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/146/209&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/146/209</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/145 [1]</TD>
            <TD>Nearby Galaxies Catalogue (NBG) (Tully 1988)</TD>
            <TD>This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/145#1</TD>
            <TD>2011-09-14T18:52:46Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/145</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/145</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/145</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/145 [2]</TD>
            <TD>Nearby Galaxies Catalogue (NBG) (Tully 1988)</TD>
            <TD>This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/145#2</TD>
            <TD>2011-09-14T18:52:46Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/145</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/145&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/145</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/145 [catalog]</TD>
            <TD>Nearby Galaxies Catalogue (NBG) (Tully 1988)</TD>
            <TD>This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/145#catalog</TD>
            <TD>2011-09-14T18:52:46Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/145</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/145&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/145</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/342/738 [1]</TD>
            <TD>HI Jodrell All Sky Survey (Lang+, 2003)</TD>
            <TD>Details are presented of the H I Jodrell All Sky Survey (HIJASS). HIJASS is a blind neutral hydrogen (H I) survey of the northern sky ({delta}&gt;22{deg}), being conducted using the multibeam receiver on the Lovell Telescope (full width at half-maximum beamwidth 12-arcmin) at Jodrell Bank. HIJASS covers the velocity range -3500 to 10000 km/s, with a velocity resolution of 18.1km/s and spatial positional accuracy of ~2.5arcmin. Thus far about 1115 deg^2^ of sky have been surveyed. The average rms noise during the early part of the survey was around 16mJy/beam Following the first phase of the Lovell Telescope upgrade (in 2001), the rms noise is now around 13mJy/beam. We describe the methods of detecting galaxies within the HIJASS data and of measuring their H I parameters. The properties of the resulting H I-selected sample of galaxies are described. Of the 222 sources so far confirmed, 170 (77 per cent) are clearly associated with a previously catalogued galaxy. A further 23 sources (10 per cent) lie close (within 6 arcmin) to a previously catalogued galaxy for which no previous redshift exists. A further 29 sources (13 per cent) do not appear to be associated with any previously catalogued galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738#1</TD>
            <TD>2011-09-14T19:36:13Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/342/738</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/342/738</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/342/738 [2]</TD>
            <TD>HI Jodrell All Sky Survey (Lang+, 2003)</TD>
            <TD>Details are presented of the H I Jodrell All Sky Survey (HIJASS). HIJASS is a blind neutral hydrogen (H I) survey of the northern sky ({delta}&gt;22{deg}), being conducted using the multibeam receiver on the Lovell Telescope (full width at half-maximum beamwidth 12-arcmin) at Jodrell Bank. HIJASS covers the velocity range -3500 to 10000 km/s, with a velocity resolution of 18.1km/s and spatial positional accuracy of ~2.5arcmin. Thus far about 1115 deg^2^ of sky have been surveyed. The average rms noise during the early part of the survey was around 16mJy/beam Following the first phase of the Lovell Telescope upgrade (in 2001), the rms noise is now around 13mJy/beam. We describe the methods of detecting galaxies within the HIJASS data and of measuring their H I parameters. The properties of the resulting H I-selected sample of galaxies are described. Of the 222 sources so far confirmed, 170 (77 per cent) are clearly associated with a previously catalogued galaxy. A further 23 sources (10 per cent) lie close (within 6 arcmin) to a previously catalogued galaxy for which no previous redshift exists. A further 29 sources (13 per cent) do not appear to be associated with any previously catalogued galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738#2</TD>
            <TD>2011-09-14T19:36:13Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/342/738&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/342/738</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/145 [1]</TD>
            <TD>Nearby Galaxies Catalogue (NBG) (Tully 1988)</TD>
            <TD>This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/145#1</TD>
            <TD>2011-09-14T18:52:46Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/145</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/145</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/145</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/145 [2]</TD>
            <TD>Nearby Galaxies Catalogue (NBG) (Tully 1988)</TD>
            <TD>This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/145#2</TD>
            <TD>2011-09-14T18:52:46Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/145</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/145&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/145</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/145 [catalog]</TD>
            <TD>Nearby Galaxies Catalogue (NBG) (Tully 1988)</TD>
            <TD>This compendium is a companion to the Nearby Galaxies Atlas (ref. 29; hereafter NBG Atlas). Data has been accumulated on 2367 galaxies with systemic velocities less than 3000 kilometers/second. Any galaxy was admitted to the catalog if it had a known velocity in 1978 that satisfied the specified limit of 3000 kilometers/second, or if it was subsequently observed to have a suitable velocity in surveys of the entire sky by the author and collaborators (ref. 6, 11, 22). There are many sources of velocities, so this catalog could potentially be quite heterogeneous. However, two sources dominate. One of these is the magnitude-limited Shapley-Ames sample, which assures the inclusion of all galaxies brighter than 12th magnitude in the blue passband (ref. 25). There are 1053 Shapley-Ames galaxies within the velocity limit. The other source was already mentioned: the all-sky survey in the neutral hydrogen line by the author and collaborators. This survey was undertaken after a complete reinspection of photographic atlases of the sky. This survey was insensitive to gas-deficient systems and has severe incompletion problems at velocities beyond 2000 kilometers/second (discussed in ref. 11). However, the virtue of our survey is homogeneous coverage across the unobscured part of the sky. The neutral hydrogen survey provides 1515 velocities to the catalog. There is some overlap between the two principal sources. It is this cumulative sample that is mapped in the NBG Atlas. There are three parts to the catalog. The first and by far the largest section (catalog) provides information about each of the 2367 galaxies. One element of that information is a group affiliation, and in a second section (groups) there is a reordered listing that clarifies the composition of each group. The final, very short section (clusters) identifies the rich clusters of galaxies that delineate the supercluster complexes mapped in the last two plates of the NBG Atlas. The text of the atlas is written at a level that can be appreciated by a wide audience. The material in this catalog and the following description are of a more technical nature. This catalog is intended for an audience of professional and motivated amateur astronomers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/145#catalog</TD>
            <TD>2011-09-14T18:52:46Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/VII/145</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/145&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/145</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/114/565 [1]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#1</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/114/565</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/114/565 [2]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#2</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/114/565&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/565 [table2]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#table2</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/565&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/114/565 [table1]</TD>
            <TD>Radial velocities in clusters of galaxies. (Proust+, 1995)</TD>
            <TD>We have obtained 65 new redshifts in 4 Abell galaxy as well as 15 velocities of galaxies observed through the galactic plane, at ESO and OHP. Data on individual galaxies are presented, and the accuracy of the determined velocities are discussed as well as some properties of the clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565#table1</TD>
            <TD>2011-09-14T18:42:36Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/114/565</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/114/565&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/114/565</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/161 [1]</TD>
            <TD>Nearby Galaxies (Schmidt+ 1993)</TD>
            <TD>The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt &amp; Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/161#1</TD>
            <TD>2011-09-14T18:52:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/VII/161</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/161</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/161</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/161 [2]</TD>
            <TD>Nearby Galaxies (Schmidt+ 1993)</TD>
            <TD>The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt &amp; Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/161#2</TD>
            <TD>2011-09-14T18:52:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/VII/161</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/161&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/161</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/161 [catalog]</TD>
            <TD>Nearby Galaxies (Schmidt+ 1993)</TD>
            <TD>The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt &amp; Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/161#catalog</TD>
            <TD>2011-09-14T18:52:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/VII/161</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/161&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/161</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/342/738 [1]</TD>
            <TD>HI Jodrell All Sky Survey (Lang+, 2003)</TD>
            <TD>Details are presented of the H I Jodrell All Sky Survey (HIJASS). HIJASS is a blind neutral hydrogen (H I) survey of the northern sky ({delta}&gt;22{deg}), being conducted using the multibeam receiver on the Lovell Telescope (full width at half-maximum beamwidth 12-arcmin) at Jodrell Bank. HIJASS covers the velocity range -3500 to 10000 km/s, with a velocity resolution of 18.1km/s and spatial positional accuracy of ~2.5arcmin. Thus far about 1115 deg^2^ of sky have been surveyed. The average rms noise during the early part of the survey was around 16mJy/beam Following the first phase of the Lovell Telescope upgrade (in 2001), the rms noise is now around 13mJy/beam. We describe the methods of detecting galaxies within the HIJASS data and of measuring their H I parameters. The properties of the resulting H I-selected sample of galaxies are described. Of the 222 sources so far confirmed, 170 (77 per cent) are clearly associated with a previously catalogued galaxy. A further 23 sources (10 per cent) lie close (within 6 arcmin) to a previously catalogued galaxy for which no previous redshift exists. A further 29 sources (13 per cent) do not appear to be associated with any previously catalogued galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738#1</TD>
            <TD>2011-09-14T19:36:13Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/342/738</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/342/738</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/342/738 [2]</TD>
            <TD>HI Jodrell All Sky Survey (Lang+, 2003)</TD>
            <TD>Details are presented of the H I Jodrell All Sky Survey (HIJASS). HIJASS is a blind neutral hydrogen (H I) survey of the northern sky ({delta}&gt;22{deg}), being conducted using the multibeam receiver on the Lovell Telescope (full width at half-maximum beamwidth 12-arcmin) at Jodrell Bank. HIJASS covers the velocity range -3500 to 10000 km/s, with a velocity resolution of 18.1km/s and spatial positional accuracy of ~2.5arcmin. Thus far about 1115 deg^2^ of sky have been surveyed. The average rms noise during the early part of the survey was around 16mJy/beam Following the first phase of the Lovell Telescope upgrade (in 2001), the rms noise is now around 13mJy/beam. We describe the methods of detecting galaxies within the HIJASS data and of measuring their H I parameters. The properties of the resulting H I-selected sample of galaxies are described. Of the 222 sources so far confirmed, 170 (77 per cent) are clearly associated with a previously catalogued galaxy. A further 23 sources (10 per cent) lie close (within 6 arcmin) to a previously catalogued galaxy for which no previous redshift exists. A further 29 sources (13 per cent) do not appear to be associated with any previously catalogued galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738#2</TD>
            <TD>2011-09-14T19:36:13Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/342/738&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/342/738</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/161 [1]</TD>
            <TD>Nearby Galaxies (Schmidt+ 1993)</TD>
            <TD>The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt &amp; Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/161#1</TD>
            <TD>2011-09-14T18:52:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/VII/161</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/161</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/161</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/161 [2]</TD>
            <TD>Nearby Galaxies (Schmidt+ 1993)</TD>
            <TD>The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt &amp; Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/161#2</TD>
            <TD>2011-09-14T18:52:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/VII/161</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/161&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/161</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/161 [catalog]</TD>
            <TD>Nearby Galaxies (Schmidt+ 1993)</TD>
            <TD>The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt &amp; Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/161#catalog</TD>
            <TD>2011-09-14T18:52:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/VII/161</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/161&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/161</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/342/738 [1]</TD>
            <TD>HI Jodrell All Sky Survey (Lang+, 2003)</TD>
            <TD>Details are presented of the H I Jodrell All Sky Survey (HIJASS). HIJASS is a blind neutral hydrogen (H I) survey of the northern sky ({delta}&gt;22{deg}), being conducted using the multibeam receiver on the Lovell Telescope (full width at half-maximum beamwidth 12-arcmin) at Jodrell Bank. HIJASS covers the velocity range -3500 to 10000 km/s, with a velocity resolution of 18.1km/s and spatial positional accuracy of ~2.5arcmin. Thus far about 1115 deg^2^ of sky have been surveyed. The average rms noise during the early part of the survey was around 16mJy/beam Following the first phase of the Lovell Telescope upgrade (in 2001), the rms noise is now around 13mJy/beam. We describe the methods of detecting galaxies within the HIJASS data and of measuring their H I parameters. The properties of the resulting H I-selected sample of galaxies are described. Of the 222 sources so far confirmed, 170 (77 per cent) are clearly associated with a previously catalogued galaxy. A further 23 sources (10 per cent) lie close (within 6 arcmin) to a previously catalogued galaxy for which no previous redshift exists. A further 29 sources (13 per cent) do not appear to be associated with any previously catalogued galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738#1</TD>
            <TD>2011-09-14T19:36:13Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/342/738</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/342/738</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/342/738 [2]</TD>
            <TD>HI Jodrell All Sky Survey (Lang+, 2003)</TD>
            <TD>Details are presented of the H I Jodrell All Sky Survey (HIJASS). HIJASS is a blind neutral hydrogen (H I) survey of the northern sky ({delta}&gt;22{deg}), being conducted using the multibeam receiver on the Lovell Telescope (full width at half-maximum beamwidth 12-arcmin) at Jodrell Bank. HIJASS covers the velocity range -3500 to 10000 km/s, with a velocity resolution of 18.1km/s and spatial positional accuracy of ~2.5arcmin. Thus far about 1115 deg^2^ of sky have been surveyed. The average rms noise during the early part of the survey was around 16mJy/beam Following the first phase of the Lovell Telescope upgrade (in 2001), the rms noise is now around 13mJy/beam. We describe the methods of detecting galaxies within the HIJASS data and of measuring their H I parameters. The properties of the resulting H I-selected sample of galaxies are described. Of the 222 sources so far confirmed, 170 (77 per cent) are clearly associated with a previously catalogued galaxy. A further 23 sources (10 per cent) lie close (within 6 arcmin) to a previously catalogued galaxy for which no previous redshift exists. A further 29 sources (13 per cent) do not appear to be associated with any previously catalogued galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738#2</TD>
            <TD>2011-09-14T19:36:13Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/342/738</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/342/738&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/342/738</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/161 [1]</TD>
            <TD>Nearby Galaxies (Schmidt+ 1993)</TD>
            <TD>The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt &amp; Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/161#1</TD>
            <TD>2011-09-14T18:52:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/VII/161</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/161</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/161</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/161 [2]</TD>
            <TD>Nearby Galaxies (Schmidt+ 1993)</TD>
            <TD>The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt &amp; Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/161#2</TD>
            <TD>2011-09-14T18:52:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/VII/161</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/161&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/161</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/161 [catalog]</TD>
            <TD>Nearby Galaxies (Schmidt+ 1993)</TD>
            <TD>The sample contains the galaxies with a velocity less than 500km/s with respect to the centroid of the Local Group. The inclusion of a galaxy into the catalog depends on its redshift as in the catalogue of Kraan-Korteweg and Tammann (1979) or on the fact that the objects are known to be certain or probable member of nearby groups. The galaxies in this catalogue form the Local Group, but one third of the galaxies does not seem to belong to any group. For a detailed explanation of the astrophysical meaning of the columns, please refer in any case to the explanation given in Schmidt and Boller (1992). Concerning the references, the basic list of references is given in Schmidt &amp; Boller (1992). The dust masses of six dwarf irregular galaxies (LGS3, U3974, A0818+71, U8091, D210, U12613) are taken from Young et al. (1989). Additional data for several galaxies, especially on the apparent magnitudes as well as on the profile width of the 21 cm line at the level 50 per cent of the maximum value, are taken from a recent preprint by Karachentsev (1993).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/161#catalog</TD>
            <TD>2011-09-14T18:52:48Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/VII/161</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/161&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/161</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/56 [1]</TD>
            <TD>HII regions in NGC 6814 (Knapen+, 1993)</TD>
            <TD>We present a new Halpha image of high quality of the grand-design galaxy NGC 6814, and describe statistical properties of the HII region population. We have determined positions, angular sizes, and calibrated fluxes of 735 individual HII regions. We construct luminosity functions (LFs) for the complete sample, separately for arm and interarm regions, and for HII regions within and outside the limiting radius corresponding to the bright optical disk. The slope of the LF for the complete sample agrees well with values published for other Sbc and Sc galaxies. LFs for HII regions in the arms, in the interarm regions, in the inner part, and in the outer part of the galaxy all have the same slopes. We show and discuss the diameter distribution of the HII regions, both for the complete sample and for the separate arm, interarm, inner, and outer disk samples. There is no evidence for a different population of HII regions in the spiral arms, nor is there evidence for the existence of a significant population of density-bounded HII regions. We discuss implications for massive star forming processes in this galaxy, and discuss possible differences from other grand-design spirals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/56#1</TD>
            <TD>2011-09-14T18:53:22Z</TD>
            <TD>#Positional_Data#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/56</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/56</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/56</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/56 [2]</TD>
            <TD>HII regions in NGC 6814 (Knapen+, 1993)</TD>
            <TD>We present a new Halpha image of high quality of the grand-design galaxy NGC 6814, and describe statistical properties of the HII region population. We have determined positions, angular sizes, and calibrated fluxes of 735 individual HII regions. We construct luminosity functions (LFs) for the complete sample, separately for arm and interarm regions, and for HII regions within and outside the limiting radius corresponding to the bright optical disk. The slope of the LF for the complete sample agrees well with values published for other Sbc and Sc galaxies. LFs for HII regions in the arms, in the interarm regions, in the inner part, and in the outer part of the galaxy all have the same slopes. We show and discuss the diameter distribution of the HII regions, both for the complete sample and for the separate arm, interarm, inner, and outer disk samples. There is no evidence for a different population of HII regions in the spiral arms, nor is there evidence for the existence of a significant population of density-bounded HII regions. We discuss implications for massive star forming processes in this galaxy, and discuss possible differences from other grand-design spirals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/56#2</TD>
            <TD>2011-09-14T18:53:22Z</TD>
            <TD>#Positional_Data#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/56</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/56&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/56</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/432/381 [1]</TD>
            <TD>VLT spectroscopic survey of RX J0152.7-1357 (Demarco+, 2005)</TD>
            <TD>Spectroscopic catalogs of cluster members and field galaxies in the field of RX J0152.7-1357. The spectroscopic data have been obtained with VLT/FORS under seeing conditions of &lt;0.8". For cluster members, the following information is given: equatorial coordinates (J2000), redshift and error in redshift, emission line flag indicating presence of emission features in galaxy spectra, most prominent spectral features and spectroscopic type as defined in Dressler et al. (1999, Cat. &lt;J/ApJS/122/51&gt;). For field galaxies only equatorial coordinates (J2000), redshift and error in redshift are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381#1</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
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            <TD>25-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/432/381</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/432/381</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/432/381 [2]</TD>
            <TD>VLT spectroscopic survey of RX J0152.7-1357 (Demarco+, 2005)</TD>
            <TD>Spectroscopic catalogs of cluster members and field galaxies in the field of RX J0152.7-1357. The spectroscopic data have been obtained with VLT/FORS under seeing conditions of &lt;0.8". For cluster members, the following information is given: equatorial coordinates (J2000), redshift and error in redshift, emission line flag indicating presence of emission features in galaxy spectra, most prominent spectral features and spectroscopic type as defined in Dressler et al. (1999, Cat. &lt;J/ApJS/122/51&gt;). For field galaxies only equatorial coordinates (J2000), redshift and error in redshift are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381#2</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/432/381&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/432/381</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/106/56 [1]</TD>
            <TD>HII regions in NGC 6814 (Knapen+, 1993)</TD>
            <TD>We present a new Halpha image of high quality of the grand-design galaxy NGC 6814, and describe statistical properties of the HII region population. We have determined positions, angular sizes, and calibrated fluxes of 735 individual HII regions. We construct luminosity functions (LFs) for the complete sample, separately for arm and interarm regions, and for HII regions within and outside the limiting radius corresponding to the bright optical disk. The slope of the LF for the complete sample agrees well with values published for other Sbc and Sc galaxies. LFs for HII regions in the arms, in the interarm regions, in the inner part, and in the outer part of the galaxy all have the same slopes. We show and discuss the diameter distribution of the HII regions, both for the complete sample and for the separate arm, interarm, inner, and outer disk samples. There is no evidence for a different population of HII regions in the spiral arms, nor is there evidence for the existence of a significant population of density-bounded HII regions. We discuss implications for massive star forming processes in this galaxy, and discuss possible differences from other grand-design spirals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/56#1</TD>
            <TD>2011-09-14T18:53:22Z</TD>
            <TD>#Positional_Data#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/56</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/106/56</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/56</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/106/56 [2]</TD>
            <TD>HII regions in NGC 6814 (Knapen+, 1993)</TD>
            <TD>We present a new Halpha image of high quality of the grand-design galaxy NGC 6814, and describe statistical properties of the HII region population. We have determined positions, angular sizes, and calibrated fluxes of 735 individual HII regions. We construct luminosity functions (LFs) for the complete sample, separately for arm and interarm regions, and for HII regions within and outside the limiting radius corresponding to the bright optical disk. The slope of the LF for the complete sample agrees well with values published for other Sbc and Sc galaxies. LFs for HII regions in the arms, in the interarm regions, in the inner part, and in the outer part of the galaxy all have the same slopes. We show and discuss the diameter distribution of the HII regions, both for the complete sample and for the separate arm, interarm, inner, and outer disk samples. There is no evidence for a different population of HII regions in the spiral arms, nor is there evidence for the existence of a significant population of density-bounded HII regions. We discuss implications for massive star forming processes in this galaxy, and discuss possible differences from other grand-design spirals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/56#2</TD>
            <TD>2011-09-14T18:53:22Z</TD>
            <TD>#Positional_Data#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/106/56</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/106/56&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/106/56</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/126/503 [1]</TD>
            <TD>Southern spiral galaxies scaleheights (Ma+ 1997)</TD>
            <TD>Based on Peng's method (1988A&amp;A...206...18P), we obtain scaleheights of 486 southern spiral galaxies, the images of which are taken from the Digitized Sky Survey at Xinglong Station of Beijing Astronomical Observatory. The fitted spiral arms of 70 galaxies are compared with their images to get their optimum inclinations. The scaleheights of other 416 ones are listed in Table 1 in Appendix. After compiling and analyzing the data, we find some statistical correlations. The most interesting results are that a flatter galaxy is bluer and looks brighter, and galaxies become flatter along the Hubble sequence Sab-Scd.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/503#1</TD>
            <TD>2011-09-14T18:42:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/503</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/126/503</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/503</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/126/503 [2]</TD>
            <TD>Southern spiral galaxies scaleheights (Ma+ 1997)</TD>
            <TD>Based on Peng's method (1988A&amp;A...206...18P), we obtain scaleheights of 486 southern spiral galaxies, the images of which are taken from the Digitized Sky Survey at Xinglong Station of Beijing Astronomical Observatory. The fitted spiral arms of 70 galaxies are compared with their images to get their optimum inclinations. The scaleheights of other 416 ones are listed in Table 1 in Appendix. After compiling and analyzing the data, we find some statistical correlations. The most interesting results are that a flatter galaxy is bluer and looks brighter, and galaxies become flatter along the Hubble sequence Sab-Scd.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/503#2</TD>
            <TD>2011-09-14T18:42:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/503</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/126/503&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/503</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/453/616 [1]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#1</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/453/616</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/453/616 [2]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#2</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/453/616&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/453/616 [table2]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#table2</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/453/616&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/453/616 [table1]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#table1</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/453/616&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/432/381 [1]</TD>
            <TD>VLT spectroscopic survey of RX J0152.7-1357 (Demarco+, 2005)</TD>
            <TD>Spectroscopic catalogs of cluster members and field galaxies in the field of RX J0152.7-1357. The spectroscopic data have been obtained with VLT/FORS under seeing conditions of &lt;0.8". For cluster members, the following information is given: equatorial coordinates (J2000), redshift and error in redshift, emission line flag indicating presence of emission features in galaxy spectra, most prominent spectral features and spectroscopic type as defined in Dressler et al. (1999, Cat. &lt;J/ApJS/122/51&gt;). For field galaxies only equatorial coordinates (J2000), redshift and error in redshift are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381#1</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/432/381 [2]</TD>
            <TD>VLT spectroscopic survey of RX J0152.7-1357 (Demarco+, 2005)</TD>
            <TD>Spectroscopic catalogs of cluster members and field galaxies in the field of RX J0152.7-1357. The spectroscopic data have been obtained with VLT/FORS under seeing conditions of &lt;0.8". For cluster members, the following information is given: equatorial coordinates (J2000), redshift and error in redshift, emission line flag indicating presence of emission features in galaxy spectra, most prominent spectral features and spectroscopic type as defined in Dressler et al. (1999, Cat. &lt;J/ApJS/122/51&gt;). For field galaxies only equatorial coordinates (J2000), redshift and error in redshift are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381#2</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>25-Nov-2004</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJ/453/616 [1]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#1</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
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            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/453/616</TD>
            <TD />
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            <TD>ivo://CDS</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/453/616 [2]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#2</TD>
            <TD>2011-09-14T18:53:28Z</TD>
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            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/453/616&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/453/616 [table2]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#table2</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/453/616&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/453/616 [table1]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#table1</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/453/616&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/126/503 [1]</TD>
            <TD>Southern spiral galaxies scaleheights (Ma+ 1997)</TD>
            <TD>Based on Peng's method (1988A&amp;A...206...18P), we obtain scaleheights of 486 southern spiral galaxies, the images of which are taken from the Digitized Sky Survey at Xinglong Station of Beijing Astronomical Observatory. The fitted spiral arms of 70 galaxies are compared with their images to get their optimum inclinations. The scaleheights of other 416 ones are listed in Table 1 in Appendix. After compiling and analyzing the data, we find some statistical correlations. The most interesting results are that a flatter galaxy is bluer and looks brighter, and galaxies become flatter along the Hubble sequence Sab-Scd.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/503#1</TD>
            <TD>2011-09-14T18:42:37Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
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            <TD>ivo://CDS.VizieR/J/A+AS/126/503</TD>
            <TD />
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/503</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/126/503 [2]</TD>
            <TD>Southern spiral galaxies scaleheights (Ma+ 1997)</TD>
            <TD>Based on Peng's method (1988A&amp;A...206...18P), we obtain scaleheights of 486 southern spiral galaxies, the images of which are taken from the Digitized Sky Survey at Xinglong Station of Beijing Astronomical Observatory. The fitted spiral arms of 70 galaxies are compared with their images to get their optimum inclinations. The scaleheights of other 416 ones are listed in Table 1 in Appendix. After compiling and analyzing the data, we find some statistical correlations. The most interesting results are that a flatter galaxy is bluer and looks brighter, and galaxies become flatter along the Hubble sequence Sab-Scd.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/503#2</TD>
            <TD>2011-09-14T18:42:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>09-May-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/126/503</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/126/503</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/432/381 [1]</TD>
            <TD>VLT spectroscopic survey of RX J0152.7-1357 (Demarco+, 2005)</TD>
            <TD>Spectroscopic catalogs of cluster members and field galaxies in the field of RX J0152.7-1357. The spectroscopic data have been obtained with VLT/FORS under seeing conditions of &lt;0.8". For cluster members, the following information is given: equatorial coordinates (J2000), redshift and error in redshift, emission line flag indicating presence of emission features in galaxy spectra, most prominent spectral features and spectroscopic type as defined in Dressler et al. (1999, Cat. &lt;J/ApJS/122/51&gt;). For field galaxies only equatorial coordinates (J2000), redshift and error in redshift are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381#1</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/432/381</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/432/381</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/432/381 [2]</TD>
            <TD>VLT spectroscopic survey of RX J0152.7-1357 (Demarco+, 2005)</TD>
            <TD>Spectroscopic catalogs of cluster members and field galaxies in the field of RX J0152.7-1357. The spectroscopic data have been obtained with VLT/FORS under seeing conditions of &lt;0.8". For cluster members, the following information is given: equatorial coordinates (J2000), redshift and error in redshift, emission line flag indicating presence of emission features in galaxy spectra, most prominent spectral features and spectroscopic type as defined in Dressler et al. (1999, Cat. &lt;J/ApJS/122/51&gt;). For field galaxies only equatorial coordinates (J2000), redshift and error in redshift are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381#2</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/432/381</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/432/381&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/432/381</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/453/616 [1]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#1</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/453/616</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/453/616 [2]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#2</TD>
            <TD>2011-09-14T18:53:28Z</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/453/616&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/453/616 [table2]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#table2</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/453/616&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/453/616 [table1]</TD>
            <TD>JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)</TD>
            <TD>Aperture photometry from our own observations and the literature is presented for the 12 um galaxies in the near-infrared J, H, and K bands and, in some cases, in the L band. These data are corrected to "total" near-infrared magnitudes (with a typical uncertainty of 0.3mag) for a direct comparison with our IRAS fluxes which apply to the entire galaxy. The corrected data are used to derive integrated total near-infrared and far-infrared luminosities. We then combine these with blue photometry and an estimate of the flux contribution from cold dust at wavelengths longward of 100um to derive the first bolometric luminosities for a large sample of galaxies. The presence of nonstellar radiation at 2-3um correlates very well with nonstellar IRAS colors. This enables us to identify a universal Seyfert nuclear continuum from near- to far-infrared wavelengths. Thus, there is a sequence of infrared colors which runs from a pure "normal galaxy" to a pure Seyfert/quasar nucleus. Seyfert 2 galaxies fall close to this same sequence, although only a few extreme narrow-line Seyfert galaxies have quasar-like colors, and these show strong evidence of harboring an obscured broad-line region. A corollary is that the host galaxies of Seyfert nuclei have normal near- to far-infrared spectra on average. Starburst galaxies lie significantly off the sequence, having a relative excess of 60um emission probably as a result of stochastically heated dust grains. We use these correlations to identify several combinations of infrared colors which discriminate between Seyfert 1 and 2 galaxies, LINERs, and ultraluminous starbursts. In the infrared, Seyfert 2 galaxies are much more like Seyfert 1s than they are like starbursts, presumably because both kinds of Seyferts are heated by a single central source, rather than a distributed region of star formation. Moreover, combining the [25-2.2um] color with the [60-12um] color, it appears that Seyfert 1 galaxies are segregated from Seyfert 2 galaxies and starburst galaxies in a well-defined region characterized by the hottest colors, corresponding to the flattest spectral slopes. Virtually no Seyfert 2 galaxy is present in such a region. To reconcile this with the "unified scheme" for Seyfert 1 and 2 galaxies would therefore require that the higher frequency radiation from the nuclei of Seyfert 2 galaxies to be absorbed by intervening dust and re-emitted at lower frequencies. We find that bolometric luminosity is most closely proportional to 12um luminosity. The 60 and 25um luminosities rise faster than linearly with bolometric luminosity, while the optical flux rises less than linearly with bolometric luminosity. This result is a confirmation of the observation that more luminous disk galaxies have relatively more dust-enshrouded stars. Increases in the dust content shifts luminosity from the optical to 25-60um, while leaving a "pivot point" in the mid-IR essentially unchanged. Thus, 12um selection is the closest available approximation to selection by a limiting bolometric flux, which is approximately 14 times nu.L_nu at 12um for non-Seyfert galaxies. It follows that future deep surveys in the mid-infrared, at wavelengths of 8-12um, will simultaneously provide complete samples to different bolometric flux levels of normal and active galaxies, which will not suffer the strong selection effects present both in the optical-UV and far-infrared.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616#table1</TD>
            <TD>2011-09-14T18:53:28Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jan-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/453/616</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/453/616&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/453/616</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/351/265 [1]</TD>
            <TD>Cluster galaxy circular velocity function (Desai+, 2004)</TD>
            <TD>We present galaxy circular velocity functions (GCVFs) for 34 low-redshift (z&lt;~0.15) clusters identified in the Sloan Digital Sky Survey (SDSS, Cat. &lt;J/AJ/123/567&gt;), for 15 clusters drawn from dark matter simulations of hierarchical structure growth in a {LAMBDA}CDM cosmology, and for ~22000 SDSS field galaxies. We find that the simulations successfully reproduce the shape, amplitude and scatter in the observed distribution of cluster galaxy circular velocities. The power-law slope of the observed cluster GCVF is ~-2.4, independent of cluster velocity dispersion. The average slope of the simulated GCVFs is somewhat steeper, although formally consistent given the errors. We find that the effects of baryons on galaxy rotation curves is to flatten the simulated cluster GCVF into better agreement with observations. The cumulative GCVFs of the simulated clusters are very similar across a wide range of cluster masses, provided individual subhalo circular velocities are scaled by the circular velocities of the parent cluster. The scatter is consistent with that measured in the cumulative, scaled observed cluster GCVF. Finally, the observed field GCVF deviates significantly from a power law, being flatter than the cluster GCVF at circular velocities less than 200km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265#1</TD>
            <TD>2011-09-14T19:37:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/351/265</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/351/265</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/351/265 [2]</TD>
            <TD>Cluster galaxy circular velocity function (Desai+, 2004)</TD>
            <TD>We present galaxy circular velocity functions (GCVFs) for 34 low-redshift (z&lt;~0.15) clusters identified in the Sloan Digital Sky Survey (SDSS, Cat. &lt;J/AJ/123/567&gt;), for 15 clusters drawn from dark matter simulations of hierarchical structure growth in a {LAMBDA}CDM cosmology, and for ~22000 SDSS field galaxies. We find that the simulations successfully reproduce the shape, amplitude and scatter in the observed distribution of cluster galaxy circular velocities. The power-law slope of the observed cluster GCVF is ~-2.4, independent of cluster velocity dispersion. The average slope of the simulated GCVFs is somewhat steeper, although formally consistent given the errors. We find that the effects of baryons on galaxy rotation curves is to flatten the simulated cluster GCVF into better agreement with observations. The cumulative GCVFs of the simulated clusters are very similar across a wide range of cluster masses, provided individual subhalo circular velocities are scaled by the circular velocities of the parent cluster. The scatter is consistent with that measured in the cumulative, scaled observed cluster GCVF. Finally, the observed field GCVF deviates significantly from a power law, being flatter than the cluster GCVF at circular velocities less than 200km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265#2</TD>
            <TD>2011-09-14T19:37:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/351/265&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/351/265</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/351/265 [1]</TD>
            <TD>Cluster galaxy circular velocity function (Desai+, 2004)</TD>
            <TD>We present galaxy circular velocity functions (GCVFs) for 34 low-redshift (z&lt;~0.15) clusters identified in the Sloan Digital Sky Survey (SDSS, Cat. &lt;J/AJ/123/567&gt;), for 15 clusters drawn from dark matter simulations of hierarchical structure growth in a {LAMBDA}CDM cosmology, and for ~22000 SDSS field galaxies. We find that the simulations successfully reproduce the shape, amplitude and scatter in the observed distribution of cluster galaxy circular velocities. The power-law slope of the observed cluster GCVF is ~-2.4, independent of cluster velocity dispersion. The average slope of the simulated GCVFs is somewhat steeper, although formally consistent given the errors. We find that the effects of baryons on galaxy rotation curves is to flatten the simulated cluster GCVF into better agreement with observations. The cumulative GCVFs of the simulated clusters are very similar across a wide range of cluster masses, provided individual subhalo circular velocities are scaled by the circular velocities of the parent cluster. The scatter is consistent with that measured in the cumulative, scaled observed cluster GCVF. Finally, the observed field GCVF deviates significantly from a power law, being flatter than the cluster GCVF at circular velocities less than 200km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265#1</TD>
            <TD>2011-09-14T19:37:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/351/265</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/351/265</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/351/265 [2]</TD>
            <TD>Cluster galaxy circular velocity function (Desai+, 2004)</TD>
            <TD>We present galaxy circular velocity functions (GCVFs) for 34 low-redshift (z&lt;~0.15) clusters identified in the Sloan Digital Sky Survey (SDSS, Cat. &lt;J/AJ/123/567&gt;), for 15 clusters drawn from dark matter simulations of hierarchical structure growth in a {LAMBDA}CDM cosmology, and for ~22000 SDSS field galaxies. We find that the simulations successfully reproduce the shape, amplitude and scatter in the observed distribution of cluster galaxy circular velocities. The power-law slope of the observed cluster GCVF is ~-2.4, independent of cluster velocity dispersion. The average slope of the simulated GCVFs is somewhat steeper, although formally consistent given the errors. We find that the effects of baryons on galaxy rotation curves is to flatten the simulated cluster GCVF into better agreement with observations. The cumulative GCVFs of the simulated clusters are very similar across a wide range of cluster masses, provided individual subhalo circular velocities are scaled by the circular velocities of the parent cluster. The scatter is consistent with that measured in the cumulative, scaled observed cluster GCVF. Finally, the observed field GCVF deviates significantly from a power law, being flatter than the cluster GCVF at circular velocities less than 200km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265#2</TD>
            <TD>2011-09-14T19:37:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/351/265&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/351/265</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/351/265 [1]</TD>
            <TD>Cluster galaxy circular velocity function (Desai+, 2004)</TD>
            <TD>We present galaxy circular velocity functions (GCVFs) for 34 low-redshift (z&lt;~0.15) clusters identified in the Sloan Digital Sky Survey (SDSS, Cat. &lt;J/AJ/123/567&gt;), for 15 clusters drawn from dark matter simulations of hierarchical structure growth in a {LAMBDA}CDM cosmology, and for ~22000 SDSS field galaxies. We find that the simulations successfully reproduce the shape, amplitude and scatter in the observed distribution of cluster galaxy circular velocities. The power-law slope of the observed cluster GCVF is ~-2.4, independent of cluster velocity dispersion. The average slope of the simulated GCVFs is somewhat steeper, although formally consistent given the errors. We find that the effects of baryons on galaxy rotation curves is to flatten the simulated cluster GCVF into better agreement with observations. The cumulative GCVFs of the simulated clusters are very similar across a wide range of cluster masses, provided individual subhalo circular velocities are scaled by the circular velocities of the parent cluster. The scatter is consistent with that measured in the cumulative, scaled observed cluster GCVF. Finally, the observed field GCVF deviates significantly from a power law, being flatter than the cluster GCVF at circular velocities less than 200km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265#1</TD>
            <TD>2011-09-14T19:37:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/351/265</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/351/265</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/351/265 [2]</TD>
            <TD>Cluster galaxy circular velocity function (Desai+, 2004)</TD>
            <TD>We present galaxy circular velocity functions (GCVFs) for 34 low-redshift (z&lt;~0.15) clusters identified in the Sloan Digital Sky Survey (SDSS, Cat. &lt;J/AJ/123/567&gt;), for 15 clusters drawn from dark matter simulations of hierarchical structure growth in a {LAMBDA}CDM cosmology, and for ~22000 SDSS field galaxies. We find that the simulations successfully reproduce the shape, amplitude and scatter in the observed distribution of cluster galaxy circular velocities. The power-law slope of the observed cluster GCVF is ~-2.4, independent of cluster velocity dispersion. The average slope of the simulated GCVFs is somewhat steeper, although formally consistent given the errors. We find that the effects of baryons on galaxy rotation curves is to flatten the simulated cluster GCVF into better agreement with observations. The cumulative GCVFs of the simulated clusters are very similar across a wide range of cluster masses, provided individual subhalo circular velocities are scaled by the circular velocities of the parent cluster. The scatter is consistent with that measured in the cumulative, scaled observed cluster GCVF. Finally, the observed field GCVF deviates significantly from a power law, being flatter than the cluster GCVF at circular velocities less than 200km/s.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265#2</TD>
            <TD>2011-09-14T19:37:58Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/351/265</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/351/265&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/351/265</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/149/327 [1]</TD>
            <TD>JKs photometry of local universe galaxies (Grauer+, 2003)</TD>
            <TD>This paper presents empirical results from a deep imaging survey of galaxies in the local universe at the J and Ks wavelengths. Three hundred ninety-one images have been obtained and calibrated using the same camera and filter set with the Steward Observatory 1.6m Kuiper Telescope on Mount Bigelow and the 2.3m Bok Telescope on Kitt Peak. The limiting magnitude is typically 22mag/arcsec at J and 21mag/arcsec at Ks. The central surface brightness, apparent magnitudes, sizes, scale lengths, and inclinations are tabulated from measurements made using these data. The purpose of this paper is to provide basic near-infrared data on a variety of galaxy types.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327#1</TD>
            <TD>2011-09-14T19:38:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/149/327</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/149/327</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/149/327 [2]</TD>
            <TD>JKs photometry of local universe galaxies (Grauer+, 2003)</TD>
            <TD>This paper presents empirical results from a deep imaging survey of galaxies in the local universe at the J and Ks wavelengths. Three hundred ninety-one images have been obtained and calibrated using the same camera and filter set with the Steward Observatory 1.6m Kuiper Telescope on Mount Bigelow and the 2.3m Bok Telescope on Kitt Peak. The limiting magnitude is typically 22mag/arcsec at J and 21mag/arcsec at Ks. The central surface brightness, apparent magnitudes, sizes, scale lengths, and inclinations are tabulated from measurements made using these data. The purpose of this paper is to provide basic near-infrared data on a variety of galaxy types.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327#2</TD>
            <TD>2011-09-14T19:38:11Z</TD>
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            <TD />
            <TD>19-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/149/327&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/149/327</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/149/327 [1]</TD>
            <TD>JKs photometry of local universe galaxies (Grauer+, 2003)</TD>
            <TD>This paper presents empirical results from a deep imaging survey of galaxies in the local universe at the J and Ks wavelengths. Three hundred ninety-one images have been obtained and calibrated using the same camera and filter set with the Steward Observatory 1.6m Kuiper Telescope on Mount Bigelow and the 2.3m Bok Telescope on Kitt Peak. The limiting magnitude is typically 22mag/arcsec at J and 21mag/arcsec at Ks. The central surface brightness, apparent magnitudes, sizes, scale lengths, and inclinations are tabulated from measurements made using these data. The purpose of this paper is to provide basic near-infrared data on a variety of galaxy types.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327#1</TD>
            <TD>2011-09-14T19:38:11Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/149/327</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/149/327</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/149/327 [2]</TD>
            <TD>JKs photometry of local universe galaxies (Grauer+, 2003)</TD>
            <TD>This paper presents empirical results from a deep imaging survey of galaxies in the local universe at the J and Ks wavelengths. Three hundred ninety-one images have been obtained and calibrated using the same camera and filter set with the Steward Observatory 1.6m Kuiper Telescope on Mount Bigelow and the 2.3m Bok Telescope on Kitt Peak. The limiting magnitude is typically 22mag/arcsec at J and 21mag/arcsec at Ks. The central surface brightness, apparent magnitudes, sizes, scale lengths, and inclinations are tabulated from measurements made using these data. The purpose of this paper is to provide basic near-infrared data on a variety of galaxy types.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327#2</TD>
            <TD>2011-09-14T19:38:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/149/327&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/149/327</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/149/327 [1]</TD>
            <TD>JKs photometry of local universe galaxies (Grauer+, 2003)</TD>
            <TD>This paper presents empirical results from a deep imaging survey of galaxies in the local universe at the J and Ks wavelengths. Three hundred ninety-one images have been obtained and calibrated using the same camera and filter set with the Steward Observatory 1.6m Kuiper Telescope on Mount Bigelow and the 2.3m Bok Telescope on Kitt Peak. The limiting magnitude is typically 22mag/arcsec at J and 21mag/arcsec at Ks. The central surface brightness, apparent magnitudes, sizes, scale lengths, and inclinations are tabulated from measurements made using these data. The purpose of this paper is to provide basic near-infrared data on a variety of galaxy types.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327#1</TD>
            <TD>2011-09-14T19:38:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/149/327</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/149/327</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/149/327 [2]</TD>
            <TD>JKs photometry of local universe galaxies (Grauer+, 2003)</TD>
            <TD>This paper presents empirical results from a deep imaging survey of galaxies in the local universe at the J and Ks wavelengths. Three hundred ninety-one images have been obtained and calibrated using the same camera and filter set with the Steward Observatory 1.6m Kuiper Telescope on Mount Bigelow and the 2.3m Bok Telescope on Kitt Peak. The limiting magnitude is typically 22mag/arcsec at J and 21mag/arcsec at Ks. The central surface brightness, apparent magnitudes, sizes, scale lengths, and inclinations are tabulated from measurements made using these data. The purpose of this paper is to provide basic near-infrared data on a variety of galaxy types.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327#2</TD>
            <TD>2011-09-14T19:38:11Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/149/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/149/327&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/149/327</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/435/65 [1]</TD>
            <TD>UBVI photometry of NGC 6872 clusters population (Bastian+, 2005)</TD>
            <TD>Photometric and derived properties for the star cluster candidates in the interacting galaxy NGC 6872. The table provides the ID, position, photometry and errors, the reduced chi-squared of the best fitting model, the extinction, age, and mass of the best fitting model, and the absolute magnitude of the source correcting for the distance and reddening.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65#1</TD>
            <TD>2011-09-14T19:38:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/435/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/435/65 [2]</TD>
            <TD>UBVI photometry of NGC 6872 clusters population (Bastian+, 2005)</TD>
            <TD>Photometric and derived properties for the star cluster candidates in the interacting galaxy NGC 6872. The table provides the ID, position, photometry and errors, the reduced chi-squared of the best fitting model, the extinction, age, and mass of the best fitting model, and the absolute magnitude of the source correcting for the distance and reddening.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65#2</TD>
            <TD>2011-09-14T19:38:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/435/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/435/65 [1]</TD>
            <TD>UBVI photometry of NGC 6872 clusters population (Bastian+, 2005)</TD>
            <TD>Photometric and derived properties for the star cluster candidates in the interacting galaxy NGC 6872. The table provides the ID, position, photometry and errors, the reduced chi-squared of the best fitting model, the extinction, age, and mass of the best fitting model, and the absolute magnitude of the source correcting for the distance and reddening.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65#1</TD>
            <TD>2011-09-14T19:38:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/435/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/435/65 [2]</TD>
            <TD>UBVI photometry of NGC 6872 clusters population (Bastian+, 2005)</TD>
            <TD>Photometric and derived properties for the star cluster candidates in the interacting galaxy NGC 6872. The table provides the ID, position, photometry and errors, the reduced chi-squared of the best fitting model, the extinction, age, and mass of the best fitting model, and the absolute magnitude of the source correcting for the distance and reddening.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65#2</TD>
            <TD>2011-09-14T19:38:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/435/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/377/428 [1]</TD>
            <TD>Abell 970 galaxies radial velocities (Sodre+, 2001)</TD>
            <TD>We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428#1</TD>
            <TD>2011-09-14T19:11:38Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/377/428</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/428</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/377/428 [2]</TD>
            <TD>Abell 970 galaxies radial velocities (Sodre+, 2001)</TD>
            <TD>We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428#2</TD>
            <TD>2011-09-14T19:11:38Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/377/428&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/428</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/377/428 [table1]</TD>
            <TD>Abell 970 galaxies radial velocities (Sodre+, 2001)</TD>
            <TD>We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428#table1</TD>
            <TD>2011-09-14T19:11:38Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/377/428&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/428</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/435/65 [1]</TD>
            <TD>UBVI photometry of NGC 6872 clusters population (Bastian+, 2005)</TD>
            <TD>Photometric and derived properties for the star cluster candidates in the interacting galaxy NGC 6872. The table provides the ID, position, photometry and errors, the reduced chi-squared of the best fitting model, the extinction, age, and mass of the best fitting model, and the absolute magnitude of the source correcting for the distance and reddening.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65#1</TD>
            <TD>2011-09-14T19:38:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/435/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/435/65 [2]</TD>
            <TD>UBVI photometry of NGC 6872 clusters population (Bastian+, 2005)</TD>
            <TD>Photometric and derived properties for the star cluster candidates in the interacting galaxy NGC 6872. The table provides the ID, position, photometry and errors, the reduced chi-squared of the best fitting model, the extinction, age, and mass of the best fitting model, and the absolute magnitude of the source correcting for the distance and reddening.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65#2</TD>
            <TD>2011-09-14T19:38:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/435/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/435/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/435/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/489 [1]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#1</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/489</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/489 [2]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#2</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc346]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc346</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc2004]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc2004</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc1948]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc1948</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc2100]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc2100</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc1818]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc1818</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc330]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc330</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/377/428 [1]</TD>
            <TD>Abell 970 galaxies radial velocities (Sodre+, 2001)</TD>
            <TD>We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428#1</TD>
            <TD>2011-09-14T19:11:38Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/377/428</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/428</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/377/428 [2]</TD>
            <TD>Abell 970 galaxies radial velocities (Sodre+, 2001)</TD>
            <TD>We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428#2</TD>
            <TD>2011-09-14T19:11:38Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/377/428&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/428</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/377/428 [table1]</TD>
            <TD>Abell 970 galaxies radial velocities (Sodre+, 2001)</TD>
            <TD>We present a dynamical analysis of the galaxy cluster Abell 970 based on a new set of radial velocities measured at ESO, Pic du Midi and Haute-Provence observatories. Our analysis indicates that this cluster has a substructure and is out of dynamical equilibrium. This conclusion is also supported by differences in the positions of the peaks of the surface density distribution and X-ray emission, as well as by the evidence of a large-scale velocity gradient in the cluster. We also found a discrepancy between the masses inferred with the virial theorem and those inferred with the X-ray emission, which is expected if the galaxies and the gas inside the cluster are not in hydrostatic equilibrium. Abell 970 has a modest cooling flow, as is expected if it is out of equilibrium. We propose that cooling flows may have an intermittent behaviour, with phases of massive cooling flows being followed by phases without significant cooling flows after the accretion of a galaxy group massive enough to disrupt the dynamical equilibrium in the centre of the clusters. A massive cooling flow will be established again, after a new equilibrium is achieved.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428#table1</TD>
            <TD>2011-09-14T19:11:38Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/377/428</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/377/428&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/377/428</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/103 [1]</TD>
            <TD>86GHz SiO maser survey in the Inner Galaxy (Messineo+, 2004)</TD>
            <TD>A catalogue of infrared photometry from DENIS (bulge PSC), 2MASS (all sky data release), ISOGAL (PSC 1.0), MSX (PSC 1.2) and IRAS (PSC 2.0) is presented for a sample of stars which we previously searched for SiO maser emission. The identification source numbers (e.g #99) are taken from Table 2 (86GHz SiO maser detections) and Table 3 (non-detections) in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;). The number of targeted positions searched for SiO maser emission in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;) is 441. As three positions showed a double 86GHz SiO maser detection, the line identification number goes up to 444. For two of these three positions, we were able to identify two distinct possible infrared counterparts within the IRAM beam.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103#1</TD>
            <TD>2011-09-14T19:38:30Z</TD>
            <TD>#Stars#Masers#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/103</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/103</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/103 [2]</TD>
            <TD>86GHz SiO maser survey in the Inner Galaxy (Messineo+, 2004)</TD>
            <TD>A catalogue of infrared photometry from DENIS (bulge PSC), 2MASS (all sky data release), ISOGAL (PSC 1.0), MSX (PSC 1.2) and IRAS (PSC 2.0) is presented for a sample of stars which we previously searched for SiO maser emission. The identification source numbers (e.g #99) are taken from Table 2 (86GHz SiO maser detections) and Table 3 (non-detections) in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;). The number of targeted positions searched for SiO maser emission in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;) is 441. As three positions showed a double 86GHz SiO maser detection, the line identification number goes up to 444. For two of these three positions, we were able to identify two distinct possible infrared counterparts within the IRAM beam.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103#2</TD>
            <TD>2011-09-14T19:38:30Z</TD>
            <TD>#Stars#Masers#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/103&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/103</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/489 [1]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#1</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/489</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/489 [2]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#2</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc346]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc346</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc2004]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc2004</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc1948]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc1948</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc2100]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc2100</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc1818]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc1818</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc330]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc330</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/140/89 [1]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#1</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/140/89</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/140/89 [2]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#2</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/140/89&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/140/89 [table1]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#table1</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/140/89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/140/89 [table2]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#table2</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/140/89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/103 [1]</TD>
            <TD>86GHz SiO maser survey in the Inner Galaxy (Messineo+, 2004)</TD>
            <TD>A catalogue of infrared photometry from DENIS (bulge PSC), 2MASS (all sky data release), ISOGAL (PSC 1.0), MSX (PSC 1.2) and IRAS (PSC 2.0) is presented for a sample of stars which we previously searched for SiO maser emission. The identification source numbers (e.g #99) are taken from Table 2 (86GHz SiO maser detections) and Table 3 (non-detections) in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;). The number of targeted positions searched for SiO maser emission in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;) is 441. As three positions showed a double 86GHz SiO maser detection, the line identification number goes up to 444. For two of these three positions, we were able to identify two distinct possible infrared counterparts within the IRAM beam.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103#1</TD>
            <TD>2011-09-14T19:38:30Z</TD>
            <TD>#Stars#Masers#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/103</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/103</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/103 [2]</TD>
            <TD>86GHz SiO maser survey in the Inner Galaxy (Messineo+, 2004)</TD>
            <TD>A catalogue of infrared photometry from DENIS (bulge PSC), 2MASS (all sky data release), ISOGAL (PSC 1.0), MSX (PSC 1.2) and IRAS (PSC 2.0) is presented for a sample of stars which we previously searched for SiO maser emission. The identification source numbers (e.g #99) are taken from Table 2 (86GHz SiO maser detections) and Table 3 (non-detections) in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;). The number of targeted positions searched for SiO maser emission in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;) is 441. As three positions showed a double 86GHz SiO maser detection, the line identification number goes up to 444. For two of these three positions, we were able to identify two distinct possible infrared counterparts within the IRAM beam.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103#2</TD>
            <TD>2011-09-14T19:38:30Z</TD>
            <TD>#Stars#Masers#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/103&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/103</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/134/489 [1]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#1</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/134/489</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/134/489 [2]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#2</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc346]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc346</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc2004]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc2004</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc1948]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc1948</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc2100]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc2100</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc1818]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc1818</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/134/489 [ngc330]</TD>
            <TD>Be stars in MC young clusters (Keller+ 1999)</TD>
            <TD>We present the results of a search for Be stars in six fields centered on the young clusters NGC 330 and NGC 346 in the SMC, and NGC 1818, NGC 1948, NGC 2004 and NGC 2100 in the LMC. Be stars were identified by differencing R band and narrow-band H{alpha} CCD images. Our comparatively large images provide substantial Be star populations both within the clusters and in their surrounding fields. Magnitudes, positions and finding charts are given for the 224 Be stars found. The fraction of Be stars to normal B stars within each cluster is found to vary significantly although the average ratio is similar to the average Be to B star ratio found in the Galaxy. In some clusters, the Be star population is weighted to magnitudes near the main sequence turn-off. The Be stars are redder in V-I than normal main-sequence stars of similar magnitude and the redness increases with increasing H{alpha} emission strength.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489#ngc330</TD>
            <TD>2011-09-14T18:53:38Z</TD>
            <TD>#Open_Clusters#Photometry#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/134/489</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/134/489&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/134/489</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/103 [1]</TD>
            <TD>86GHz SiO maser survey in the Inner Galaxy (Messineo+, 2004)</TD>
            <TD>A catalogue of infrared photometry from DENIS (bulge PSC), 2MASS (all sky data release), ISOGAL (PSC 1.0), MSX (PSC 1.2) and IRAS (PSC 2.0) is presented for a sample of stars which we previously searched for SiO maser emission. The identification source numbers (e.g #99) are taken from Table 2 (86GHz SiO maser detections) and Table 3 (non-detections) in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;). The number of targeted positions searched for SiO maser emission in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;) is 441. As three positions showed a double 86GHz SiO maser detection, the line identification number goes up to 444. For two of these three positions, we were able to identify two distinct possible infrared counterparts within the IRAM beam.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103#1</TD>
            <TD>2011-09-14T19:38:30Z</TD>
            <TD>#Stars#Masers#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/103</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/103</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/103 [2]</TD>
            <TD>86GHz SiO maser survey in the Inner Galaxy (Messineo+, 2004)</TD>
            <TD>A catalogue of infrared photometry from DENIS (bulge PSC), 2MASS (all sky data release), ISOGAL (PSC 1.0), MSX (PSC 1.2) and IRAS (PSC 2.0) is presented for a sample of stars which we previously searched for SiO maser emission. The identification source numbers (e.g #99) are taken from Table 2 (86GHz SiO maser detections) and Table 3 (non-detections) in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;). The number of targeted positions searched for SiO maser emission in Messineo et al. (2002, Cat. &lt;J/A+A/393/115&gt;) is 441. As three positions showed a double 86GHz SiO maser detection, the line identification number goes up to 444. For two of these three positions, we were able to identify two distinct possible infrared counterparts within the IRAM beam.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103#2</TD>
            <TD>2011-09-14T19:38:30Z</TD>
            <TD>#Stars#Masers#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/103&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/103</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/140/89 [1]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#1</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/140/89</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/140/89 [2]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#2</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/140/89&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/140/89 [table1]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#table1</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/140/89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/140/89 [table2]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#table2</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/140/89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/331/949 [1]</TD>
            <TD>Wolf-Rayet and O-star runaways kinematics (Moffat+ 1998)</TD>
            <TD>Reliable systemic radial velocities are almost impossible to secure for Wolf-Rayet stars, difficult for O stars. Therefore, to study the motions - both systematic in the Galaxy and peculiar - of these two related types of hot, luminous star, we have examined the Hipparcos proper motions of some 70 stars of each type. We find that (a) both groups follow Galactic rotation in the same way, (b) both have a similar fraction of ``runaways'', (c) mean kinetic ages based on displacement and motion away from the Galactic plane tend to slightly favour the cluster ejection over the the binary supernova hypothesis for their formation, and (d) those with significant peculiar supersonic motion relative to the ambient ISM, tend to form bow shocks in the direction of the motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949#1</TD>
            <TD>2011-09-14T18:54:50Z</TD>
            <TD>#Proper_Motions#Velocities#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/331/949</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/331/949</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/331/949 [2]</TD>
            <TD>Wolf-Rayet and O-star runaways kinematics (Moffat+ 1998)</TD>
            <TD>Reliable systemic radial velocities are almost impossible to secure for Wolf-Rayet stars, difficult for O stars. Therefore, to study the motions - both systematic in the Galaxy and peculiar - of these two related types of hot, luminous star, we have examined the Hipparcos proper motions of some 70 stars of each type. We find that (a) both groups follow Galactic rotation in the same way, (b) both have a similar fraction of ``runaways'', (c) mean kinetic ages based on displacement and motion away from the Galactic plane tend to slightly favour the cluster ejection over the the binary supernova hypothesis for their formation, and (d) those with significant peculiar supersonic motion relative to the ambient ISM, tend to form bow shocks in the direction of the motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949#2</TD>
            <TD>2011-09-14T18:54:50Z</TD>
            <TD>#Proper_Motions#Velocities#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/331/949&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/331/949</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/1607 [1]</TD>
            <TD>IRAS Revised Bright Galaxy Sample (Sanders+, 2003)</TD>
            <TD>IRAS flux densities, redshifts, and infrared luminosities are reported for all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a complete flux-limited survey of all extragalactic objects with total 60{mu}m flux density greater than 5.24Jy, covering the entire sky surveyed by IRAS at Galactic latitudes |b|&gt;5{deg}. The RBGS includes 629 objects, with median and mean sample redshifts of 0.0082 and 0.0126, respectively, and a maximum redshift of 0.0876. The RBGS supersedes the previous two-part IRAS Bright Galaxy Samples (BGS1+BGS2) which were compiled before the final (Pass 3) calibration of the IRAS Level 1 Archive in 1990 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607#1</TD>
            <TD>2011-09-14T19:38:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/1607</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1607</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/1607 [2]</TD>
            <TD>IRAS Revised Bright Galaxy Sample (Sanders+, 2003)</TD>
            <TD>IRAS flux densities, redshifts, and infrared luminosities are reported for all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a complete flux-limited survey of all extragalactic objects with total 60{mu}m flux density greater than 5.24Jy, covering the entire sky surveyed by IRAS at Galactic latitudes |b|&gt;5{deg}. The RBGS includes 629 objects, with median and mean sample redshifts of 0.0082 and 0.0126, respectively, and a maximum redshift of 0.0876. The RBGS supersedes the previous two-part IRAS Bright Galaxy Samples (BGS1+BGS2) which were compiled before the final (Pass 3) calibration of the IRAS Level 1 Archive in 1990 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607#2</TD>
            <TD>2011-09-14T19:38:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/1607&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1607</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/140/89 [1]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#1</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/140/89</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/140/89 [2]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#2</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/140/89&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/140/89 [table1]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#table1</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/140/89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/140/89 [table2]</TD>
            <TD>Galaxy coordinates. II (Paturel, 1999)</TD>
            <TD>Table 1: Control sample. For each galaxy the new J2000.0 equatorial coordinates are given first. The second coordinates are those extracted from the LEDA database (http://www-obs.univ-lyon1.fr). This sample of 1522 galaxies was used to check the method of measurement. Table 2: This table presents the full sample of new measurements of accurate coordinates. It contains 17615 measurements for 17298 galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89#table2</TD>
            <TD>2011-09-14T19:12:58Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/140/89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/89</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/1607 [1]</TD>
            <TD>IRAS Revised Bright Galaxy Sample (Sanders+, 2003)</TD>
            <TD>IRAS flux densities, redshifts, and infrared luminosities are reported for all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a complete flux-limited survey of all extragalactic objects with total 60{mu}m flux density greater than 5.24Jy, covering the entire sky surveyed by IRAS at Galactic latitudes |b|&gt;5{deg}. The RBGS includes 629 objects, with median and mean sample redshifts of 0.0082 and 0.0126, respectively, and a maximum redshift of 0.0876. The RBGS supersedes the previous two-part IRAS Bright Galaxy Samples (BGS1+BGS2) which were compiled before the final (Pass 3) calibration of the IRAS Level 1 Archive in 1990 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607#1</TD>
            <TD>2011-09-14T19:38:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/1607</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1607</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/1607 [2]</TD>
            <TD>IRAS Revised Bright Galaxy Sample (Sanders+, 2003)</TD>
            <TD>IRAS flux densities, redshifts, and infrared luminosities are reported for all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a complete flux-limited survey of all extragalactic objects with total 60{mu}m flux density greater than 5.24Jy, covering the entire sky surveyed by IRAS at Galactic latitudes |b|&gt;5{deg}. The RBGS includes 629 objects, with median and mean sample redshifts of 0.0082 and 0.0126, respectively, and a maximum redshift of 0.0876. The RBGS supersedes the previous two-part IRAS Bright Galaxy Samples (BGS1+BGS2) which were compiled before the final (Pass 3) calibration of the IRAS Level 1 Archive in 1990 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607#2</TD>
            <TD>2011-09-14T19:38:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/1607&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1607</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/38 [1]</TD>
            <TD>BVRI photometry of Abell 2443 (Trujillo+, 2001)</TD>
            <TD>We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sersic r^1/n^ bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into account the effects of seeing on the structural parameters and considers ellipticity as an active parameter, we avoid systematic errors arising from assumptions of circular symmetry. Of the sample galaxies, 76% were classified with these models, while the rest were morphologically peculiar. For the spiral galaxies, the relation between n and B/D is consistent with the trend observed in nearby field galaxy samples. The Sersic index n (which can be considered as a concentration index) of the elliptical galaxies is correlated with the local surface density of the cluster. Monte Carlo simulations were used to check the reliability of the method and determine the magnitude selection criteria. Observations were obtained on 1998 August 19 at the 2.5 m Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos on La Palma. The prime-focus CCD camera was used with pixel scale of 0.11"/pix, and the seeing ranged from FWHM 0.88" to 1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38#1</TD>
            <TD>2011-09-14T19:13:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/38</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/38</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/38 [2]</TD>
            <TD>BVRI photometry of Abell 2443 (Trujillo+, 2001)</TD>
            <TD>We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sersic r^1/n^ bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into account the effects of seeing on the structural parameters and considers ellipticity as an active parameter, we avoid systematic errors arising from assumptions of circular symmetry. Of the sample galaxies, 76% were classified with these models, while the rest were morphologically peculiar. For the spiral galaxies, the relation between n and B/D is consistent with the trend observed in nearby field galaxy samples. The Sersic index n (which can be considered as a concentration index) of the elliptical galaxies is correlated with the local surface density of the cluster. Monte Carlo simulations were used to check the reliability of the method and determine the magnitude selection criteria. Observations were obtained on 1998 August 19 at the 2.5 m Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos on La Palma. The prime-focus CCD camera was used with pixel scale of 0.11"/pix, and the seeing ranged from FWHM 0.88" to 1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38#2</TD>
            <TD>2011-09-14T19:13:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/38&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/38</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/38 [table3]</TD>
            <TD>BVRI photometry of Abell 2443 (Trujillo+, 2001)</TD>
            <TD>We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sersic r^1/n^ bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into account the effects of seeing on the structural parameters and considers ellipticity as an active parameter, we avoid systematic errors arising from assumptions of circular symmetry. Of the sample galaxies, 76% were classified with these models, while the rest were morphologically peculiar. For the spiral galaxies, the relation between n and B/D is consistent with the trend observed in nearby field galaxy samples. The Sersic index n (which can be considered as a concentration index) of the elliptical galaxies is correlated with the local surface density of the cluster. Monte Carlo simulations were used to check the reliability of the method and determine the magnitude selection criteria. Observations were obtained on 1998 August 19 at the 2.5 m Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos on La Palma. The prime-focus CCD camera was used with pixel scale of 0.11"/pix, and the seeing ranged from FWHM 0.88" to 1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38#table3</TD>
            <TD>2011-09-14T19:13:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/38&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/38</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/331/949 [1]</TD>
            <TD>Wolf-Rayet and O-star runaways kinematics (Moffat+ 1998)</TD>
            <TD>Reliable systemic radial velocities are almost impossible to secure for Wolf-Rayet stars, difficult for O stars. Therefore, to study the motions - both systematic in the Galaxy and peculiar - of these two related types of hot, luminous star, we have examined the Hipparcos proper motions of some 70 stars of each type. We find that (a) both groups follow Galactic rotation in the same way, (b) both have a similar fraction of ``runaways'', (c) mean kinetic ages based on displacement and motion away from the Galactic plane tend to slightly favour the cluster ejection over the the binary supernova hypothesis for their formation, and (d) those with significant peculiar supersonic motion relative to the ambient ISM, tend to form bow shocks in the direction of the motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949#1</TD>
            <TD>2011-09-14T18:54:50Z</TD>
            <TD>#Proper_Motions#Velocities#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/331/949</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/331/949</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/331/949 [2]</TD>
            <TD>Wolf-Rayet and O-star runaways kinematics (Moffat+ 1998)</TD>
            <TD>Reliable systemic radial velocities are almost impossible to secure for Wolf-Rayet stars, difficult for O stars. Therefore, to study the motions - both systematic in the Galaxy and peculiar - of these two related types of hot, luminous star, we have examined the Hipparcos proper motions of some 70 stars of each type. We find that (a) both groups follow Galactic rotation in the same way, (b) both have a similar fraction of ``runaways'', (c) mean kinetic ages based on displacement and motion away from the Galactic plane tend to slightly favour the cluster ejection over the the binary supernova hypothesis for their formation, and (d) those with significant peculiar supersonic motion relative to the ambient ISM, tend to form bow shocks in the direction of the motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949#2</TD>
            <TD>2011-09-14T18:54:50Z</TD>
            <TD>#Proper_Motions#Velocities#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/331/949&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/331/949</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/1607 [1]</TD>
            <TD>IRAS Revised Bright Galaxy Sample (Sanders+, 2003)</TD>
            <TD>IRAS flux densities, redshifts, and infrared luminosities are reported for all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a complete flux-limited survey of all extragalactic objects with total 60{mu}m flux density greater than 5.24Jy, covering the entire sky surveyed by IRAS at Galactic latitudes |b|&gt;5{deg}. The RBGS includes 629 objects, with median and mean sample redshifts of 0.0082 and 0.0126, respectively, and a maximum redshift of 0.0876. The RBGS supersedes the previous two-part IRAS Bright Galaxy Samples (BGS1+BGS2) which were compiled before the final (Pass 3) calibration of the IRAS Level 1 Archive in 1990 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607#1</TD>
            <TD>2011-09-14T19:38:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/1607</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1607</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/1607 [2]</TD>
            <TD>IRAS Revised Bright Galaxy Sample (Sanders+, 2003)</TD>
            <TD>IRAS flux densities, redshifts, and infrared luminosities are reported for all sources identified in the IRAS Revised Bright Galaxy Sample (RBGS), a complete flux-limited survey of all extragalactic objects with total 60{mu}m flux density greater than 5.24Jy, covering the entire sky surveyed by IRAS at Galactic latitudes |b|&gt;5{deg}. The RBGS includes 629 objects, with median and mean sample redshifts of 0.0082 and 0.0126, respectively, and a maximum redshift of 0.0876. The RBGS supersedes the previous two-part IRAS Bright Galaxy Samples (BGS1+BGS2) which were compiled before the final (Pass 3) calibration of the IRAS Level 1 Archive in 1990 May.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607#2</TD>
            <TD>2011-09-14T19:38:51Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1607</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/1607&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1607</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/38 [1]</TD>
            <TD>BVRI photometry of Abell 2443 (Trujillo+, 2001)</TD>
            <TD>We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sersic r^1/n^ bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into account the effects of seeing on the structural parameters and considers ellipticity as an active parameter, we avoid systematic errors arising from assumptions of circular symmetry. Of the sample galaxies, 76% were classified with these models, while the rest were morphologically peculiar. For the spiral galaxies, the relation between n and B/D is consistent with the trend observed in nearby field galaxy samples. The Sersic index n (which can be considered as a concentration index) of the elliptical galaxies is correlated with the local surface density of the cluster. Monte Carlo simulations were used to check the reliability of the method and determine the magnitude selection criteria. Observations were obtained on 1998 August 19 at the 2.5 m Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos on La Palma. The prime-focus CCD camera was used with pixel scale of 0.11"/pix, and the seeing ranged from FWHM 0.88" to 1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38#1</TD>
            <TD>2011-09-14T19:13:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/38</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/38</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/38 [2]</TD>
            <TD>BVRI photometry of Abell 2443 (Trujillo+, 2001)</TD>
            <TD>We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sersic r^1/n^ bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into account the effects of seeing on the structural parameters and considers ellipticity as an active parameter, we avoid systematic errors arising from assumptions of circular symmetry. Of the sample galaxies, 76% were classified with these models, while the rest were morphologically peculiar. For the spiral galaxies, the relation between n and B/D is consistent with the trend observed in nearby field galaxy samples. The Sersic index n (which can be considered as a concentration index) of the elliptical galaxies is correlated with the local surface density of the cluster. Monte Carlo simulations were used to check the reliability of the method and determine the magnitude selection criteria. Observations were obtained on 1998 August 19 at the 2.5 m Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos on La Palma. The prime-focus CCD camera was used with pixel scale of 0.11"/pix, and the seeing ranged from FWHM 0.88" to 1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38#2</TD>
            <TD>2011-09-14T19:13:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/38&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/38</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/38 [table3]</TD>
            <TD>BVRI photometry of Abell 2443 (Trujillo+, 2001)</TD>
            <TD>We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sersic r^1/n^ bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into account the effects of seeing on the structural parameters and considers ellipticity as an active parameter, we avoid systematic errors arising from assumptions of circular symmetry. Of the sample galaxies, 76% were classified with these models, while the rest were morphologically peculiar. For the spiral galaxies, the relation between n and B/D is consistent with the trend observed in nearby field galaxy samples. The Sersic index n (which can be considered as a concentration index) of the elliptical galaxies is correlated with the local surface density of the cluster. Monte Carlo simulations were used to check the reliability of the method and determine the magnitude selection criteria. Observations were obtained on 1998 August 19 at the 2.5 m Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos on La Palma. The prime-focus CCD camera was used with pixel scale of 0.11"/pix, and the seeing ranged from FWHM 0.88" to 1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38#table3</TD>
            <TD>2011-09-14T19:13:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/38&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/38</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/331/949 [1]</TD>
            <TD>Wolf-Rayet and O-star runaways kinematics (Moffat+ 1998)</TD>
            <TD>Reliable systemic radial velocities are almost impossible to secure for Wolf-Rayet stars, difficult for O stars. Therefore, to study the motions - both systematic in the Galaxy and peculiar - of these two related types of hot, luminous star, we have examined the Hipparcos proper motions of some 70 stars of each type. We find that (a) both groups follow Galactic rotation in the same way, (b) both have a similar fraction of ``runaways'', (c) mean kinetic ages based on displacement and motion away from the Galactic plane tend to slightly favour the cluster ejection over the the binary supernova hypothesis for their formation, and (d) those with significant peculiar supersonic motion relative to the ambient ISM, tend to form bow shocks in the direction of the motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949#1</TD>
            <TD>2011-09-14T18:54:50Z</TD>
            <TD>#Proper_Motions#Velocities#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/331/949</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/331/949</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/331/949 [2]</TD>
            <TD>Wolf-Rayet and O-star runaways kinematics (Moffat+ 1998)</TD>
            <TD>Reliable systemic radial velocities are almost impossible to secure for Wolf-Rayet stars, difficult for O stars. Therefore, to study the motions - both systematic in the Galaxy and peculiar - of these two related types of hot, luminous star, we have examined the Hipparcos proper motions of some 70 stars of each type. We find that (a) both groups follow Galactic rotation in the same way, (b) both have a similar fraction of ``runaways'', (c) mean kinetic ages based on displacement and motion away from the Galactic plane tend to slightly favour the cluster ejection over the the binary supernova hypothesis for their formation, and (d) those with significant peculiar supersonic motion relative to the ambient ISM, tend to form bow shocks in the direction of the motion.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949#2</TD>
            <TD>2011-09-14T18:54:50Z</TD>
            <TD>#Proper_Motions#Velocities#Stars:early-type#Stars:WR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+A/331/949</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/331/949&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/331/949</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/609/564 [1]</TD>
            <TD>Blazar counterparts for 3EG sources (Sowards-Emmerd+, 2004)</TD>
            <TD>Supplementing existing survey data with Very Large Array (VLA) observations, we have extended {gamma}-ray counterpart identifications down to decl.=-40{deg} using our "figure-of-merit" approach. We find blazar counterparts for 70% of EGRET sources above decl.=-40{deg} away from the Galaxy. Spectroscopic confirmation is in progress, and spectra for 24 sources are presented here. We find evidence that increased exposure in the bulge region allowed EGRET to detect relatively faint blazars; a clear excess of nonblazar objects in this region, however, argues for an additional (new) source class.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564#1</TD>
            <TD>2011-09-14T19:39:33Z</TD>
            <TD>#AGN#BL_Lac_objects#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/609/564</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/609/564</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/609/564 [2]</TD>
            <TD>Blazar counterparts for 3EG sources (Sowards-Emmerd+, 2004)</TD>
            <TD>Supplementing existing survey data with Very Large Array (VLA) observations, we have extended {gamma}-ray counterpart identifications down to decl.=-40{deg} using our "figure-of-merit" approach. We find blazar counterparts for 70% of EGRET sources above decl.=-40{deg} away from the Galaxy. Spectroscopic confirmation is in progress, and spectra for 24 sources are presented here. We find evidence that increased exposure in the bulge region allowed EGRET to detect relatively faint blazars; a clear excess of nonblazar objects in this region, however, argues for an additional (new) source class.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564#2</TD>
            <TD>2011-09-14T19:39:33Z</TD>
            <TD>#AGN#BL_Lac_objects#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/609/564&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/609/564</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/609/564 [table1]</TD>
            <TD>Blazar counterparts for 3EG sources (Sowards-Emmerd+, 2004)</TD>
            <TD>Supplementing existing survey data with Very Large Array (VLA) observations, we have extended {gamma}-ray counterpart identifications down to decl.=-40{deg} using our "figure-of-merit" approach. We find blazar counterparts for 70% of EGRET sources above decl.=-40{deg} away from the Galaxy. Spectroscopic confirmation is in progress, and spectra for 24 sources are presented here. We find evidence that increased exposure in the bulge region allowed EGRET to detect relatively faint blazars; a clear excess of nonblazar objects in this region, however, argues for an additional (new) source class.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564#table1</TD>
            <TD>2011-09-14T19:39:33Z</TD>
            <TD>#AGN#BL_Lac_objects#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/609/564&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/609/564</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/38 [1]</TD>
            <TD>BVRI photometry of Abell 2443 (Trujillo+, 2001)</TD>
            <TD>We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sersic r^1/n^ bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into account the effects of seeing on the structural parameters and considers ellipticity as an active parameter, we avoid systematic errors arising from assumptions of circular symmetry. Of the sample galaxies, 76% were classified with these models, while the rest were morphologically peculiar. For the spiral galaxies, the relation between n and B/D is consistent with the trend observed in nearby field galaxy samples. The Sersic index n (which can be considered as a concentration index) of the elliptical galaxies is correlated with the local surface density of the cluster. Monte Carlo simulations were used to check the reliability of the method and determine the magnitude selection criteria. Observations were obtained on 1998 August 19 at the 2.5 m Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos on La Palma. The prime-focus CCD camera was used with pixel scale of 0.11"/pix, and the seeing ranged from FWHM 0.88" to 1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38#1</TD>
            <TD>2011-09-14T19:13:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/38</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/38</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/38 [2]</TD>
            <TD>BVRI photometry of Abell 2443 (Trujillo+, 2001)</TD>
            <TD>We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sersic r^1/n^ bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into account the effects of seeing on the structural parameters and considers ellipticity as an active parameter, we avoid systematic errors arising from assumptions of circular symmetry. Of the sample galaxies, 76% were classified with these models, while the rest were morphologically peculiar. For the spiral galaxies, the relation between n and B/D is consistent with the trend observed in nearby field galaxy samples. The Sersic index n (which can be considered as a concentration index) of the elliptical galaxies is correlated with the local surface density of the cluster. Monte Carlo simulations were used to check the reliability of the method and determine the magnitude selection criteria. Observations were obtained on 1998 August 19 at the 2.5 m Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos on La Palma. The prime-focus CCD camera was used with pixel scale of 0.11"/pix, and the seeing ranged from FWHM 0.88" to 1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38#2</TD>
            <TD>2011-09-14T19:13:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/38&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/38</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/38 [table3]</TD>
            <TD>BVRI photometry of Abell 2443 (Trujillo+, 2001)</TD>
            <TD>We present broadband photometry and provide a quantitative analysis of the structure of galaxies in the inner region of the Abell Cluster 2443 (z~0.1). The galaxy parameters have been derived by fitting a two-component model (Sersic r^1/n^ bulge and exponential disk) to a magnitude-limited sample. Using a new method of analysis that takes into account the effects of seeing on the structural parameters and considers ellipticity as an active parameter, we avoid systematic errors arising from assumptions of circular symmetry. Of the sample galaxies, 76% were classified with these models, while the rest were morphologically peculiar. For the spiral galaxies, the relation between n and B/D is consistent with the trend observed in nearby field galaxy samples. The Sersic index n (which can be considered as a concentration index) of the elliptical galaxies is correlated with the local surface density of the cluster. Monte Carlo simulations were used to check the reliability of the method and determine the magnitude selection criteria. Observations were obtained on 1998 August 19 at the 2.5 m Nordic Optical Telescope (NOT) at the Observatorio del Roque de los Muchachos on La Palma. The prime-focus CCD camera was used with pixel scale of 0.11"/pix, and the seeing ranged from FWHM 0.88" to 1".</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38#table3</TD>
            <TD>2011-09-14T19:13:31Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/38</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/38&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/38</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/118/329 [1]</TD>
            <TD>MOST supernova remnant catalogue (MSC) (Whiteoak+ 1996)</TD>
            <TD>A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}&lt;=l&lt;=355{deg}, |b|&lt;~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329#1</TD>
            <TD>2011-09-14T18:55:21Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/118/329</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/329</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/118/329 [2]</TD>
            <TD>MOST supernova remnant catalogue (MSC) (Whiteoak+ 1996)</TD>
            <TD>A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}&lt;=l&lt;=355{deg}, |b|&lt;~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329#2</TD>
            <TD>2011-09-14T18:55:21Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/118/329&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/329</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/329 [msc]</TD>
            <TD>MOST supernova remnant catalogue (MSC) (Whiteoak+ 1996)</TD>
            <TD>A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}&lt;=l&lt;=355{deg}, |b|&lt;~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329#msc</TD>
            <TD>2011-09-14T18:55:21Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/329&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/329</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/609/564 [1]</TD>
            <TD>Blazar counterparts for 3EG sources (Sowards-Emmerd+, 2004)</TD>
            <TD>Supplementing existing survey data with Very Large Array (VLA) observations, we have extended {gamma}-ray counterpart identifications down to decl.=-40{deg} using our "figure-of-merit" approach. We find blazar counterparts for 70% of EGRET sources above decl.=-40{deg} away from the Galaxy. Spectroscopic confirmation is in progress, and spectra for 24 sources are presented here. We find evidence that increased exposure in the bulge region allowed EGRET to detect relatively faint blazars; a clear excess of nonblazar objects in this region, however, argues for an additional (new) source class.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564#1</TD>
            <TD>2011-09-14T19:39:33Z</TD>
            <TD>#AGN#BL_Lac_objects#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/609/564</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/609/564</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/609/564 [2]</TD>
            <TD>Blazar counterparts for 3EG sources (Sowards-Emmerd+, 2004)</TD>
            <TD>Supplementing existing survey data with Very Large Array (VLA) observations, we have extended {gamma}-ray counterpart identifications down to decl.=-40{deg} using our "figure-of-merit" approach. We find blazar counterparts for 70% of EGRET sources above decl.=-40{deg} away from the Galaxy. Spectroscopic confirmation is in progress, and spectra for 24 sources are presented here. We find evidence that increased exposure in the bulge region allowed EGRET to detect relatively faint blazars; a clear excess of nonblazar objects in this region, however, argues for an additional (new) source class.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564#2</TD>
            <TD>2011-09-14T19:39:33Z</TD>
            <TD>#AGN#BL_Lac_objects#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/609/564&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/609/564</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/609/564 [table1]</TD>
            <TD>Blazar counterparts for 3EG sources (Sowards-Emmerd+, 2004)</TD>
            <TD>Supplementing existing survey data with Very Large Array (VLA) observations, we have extended {gamma}-ray counterpart identifications down to decl.=-40{deg} using our "figure-of-merit" approach. We find blazar counterparts for 70% of EGRET sources above decl.=-40{deg} away from the Galaxy. Spectroscopic confirmation is in progress, and spectra for 24 sources are presented here. We find evidence that increased exposure in the bulge region allowed EGRET to detect relatively faint blazars; a clear excess of nonblazar objects in this region, however, argues for an additional (new) source class.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564#table1</TD>
            <TD>2011-09-14T19:39:33Z</TD>
            <TD>#AGN#BL_Lac_objects#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/609/564&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/609/564</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/118/329 [1]</TD>
            <TD>MOST supernova remnant catalogue (MSC) (Whiteoak+ 1996)</TD>
            <TD>A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}&lt;=l&lt;=355{deg}, |b|&lt;~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329#1</TD>
            <TD>2011-09-14T18:55:21Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/118/329</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/329</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/118/329 [2]</TD>
            <TD>MOST supernova remnant catalogue (MSC) (Whiteoak+ 1996)</TD>
            <TD>A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}&lt;=l&lt;=355{deg}, |b|&lt;~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329#2</TD>
            <TD>2011-09-14T18:55:21Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/118/329&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/329</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/329 [msc]</TD>
            <TD>MOST supernova remnant catalogue (MSC) (Whiteoak+ 1996)</TD>
            <TD>A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}&lt;=l&lt;=355{deg}, |b|&lt;~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329#msc</TD>
            <TD>2011-09-14T18:55:21Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/329&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/329</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/609/564 [1]</TD>
            <TD>Blazar counterparts for 3EG sources (Sowards-Emmerd+, 2004)</TD>
            <TD>Supplementing existing survey data with Very Large Array (VLA) observations, we have extended {gamma}-ray counterpart identifications down to decl.=-40{deg} using our "figure-of-merit" approach. We find blazar counterparts for 70% of EGRET sources above decl.=-40{deg} away from the Galaxy. Spectroscopic confirmation is in progress, and spectra for 24 sources are presented here. We find evidence that increased exposure in the bulge region allowed EGRET to detect relatively faint blazars; a clear excess of nonblazar objects in this region, however, argues for an additional (new) source class.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564#1</TD>
            <TD>2011-09-14T19:39:33Z</TD>
            <TD>#AGN#BL_Lac_objects#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/609/564</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/609/564</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/609/564 [2]</TD>
            <TD>Blazar counterparts for 3EG sources (Sowards-Emmerd+, 2004)</TD>
            <TD>Supplementing existing survey data with Very Large Array (VLA) observations, we have extended {gamma}-ray counterpart identifications down to decl.=-40{deg} using our "figure-of-merit" approach. We find blazar counterparts for 70% of EGRET sources above decl.=-40{deg} away from the Galaxy. Spectroscopic confirmation is in progress, and spectra for 24 sources are presented here. We find evidence that increased exposure in the bulge region allowed EGRET to detect relatively faint blazars; a clear excess of nonblazar objects in this region, however, argues for an additional (new) source class.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564#2</TD>
            <TD>2011-09-14T19:39:33Z</TD>
            <TD>#AGN#BL_Lac_objects#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/609/564&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/609/564</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/609/564 [table1]</TD>
            <TD>Blazar counterparts for 3EG sources (Sowards-Emmerd+, 2004)</TD>
            <TD>Supplementing existing survey data with Very Large Array (VLA) observations, we have extended {gamma}-ray counterpart identifications down to decl.=-40{deg} using our "figure-of-merit" approach. We find blazar counterparts for 70% of EGRET sources above decl.=-40{deg} away from the Galaxy. Spectroscopic confirmation is in progress, and spectra for 24 sources are presented here. We find evidence that increased exposure in the bulge region allowed EGRET to detect relatively faint blazars; a clear excess of nonblazar objects in this region, however, argues for an additional (new) source class.</TD>
            <TD>CDS</TD>
            <TD>#Gamma-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564#table1</TD>
            <TD>2011-09-14T19:39:33Z</TD>
            <TD>#AGN#BL_Lac_objects#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/609/564</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/609/564&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/609/564</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/137/117 [1]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#1</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/137/117</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/137/117 [2]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#2</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/137/117&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/137/117 [table2]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#table2</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/137/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/137/117 [table1]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#table1</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/137/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/118/329 [1]</TD>
            <TD>MOST supernova remnant catalogue (MSC) (Whiteoak+ 1996)</TD>
            <TD>A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}&lt;=l&lt;=355{deg}, |b|&lt;~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329#1</TD>
            <TD>2011-09-14T18:55:21Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/118/329</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/329</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/118/329 [2]</TD>
            <TD>MOST supernova remnant catalogue (MSC) (Whiteoak+ 1996)</TD>
            <TD>A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}&lt;=l&lt;=355{deg}, |b|&lt;~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329#2</TD>
            <TD>2011-09-14T18:55:21Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/118/329&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/329</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/329 [msc]</TD>
            <TD>MOST supernova remnant catalogue (MSC) (Whiteoak+ 1996)</TD>
            <TD>A catalogue of supernova remnants in the southern Galaxy within the area 245{deg}&lt;=l&lt;=355{deg}, |b|&lt;~1.5{deg} has been produced from observations made at 0.843GHz with a resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329#msc</TD>
            <TD>2011-09-14T18:55:21Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/329</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/329&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/329</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/305/259 [1]</TD>
            <TD>EFAR galaxies redshifts &amp; velocity dispersions (Wegner+, 1999)</TD>
            <TD>We present the spectroscopic data for the galaxies studied in the EFAR project, which is designed to measure the properties and peculiar motions of early-type galaxies in two distant regions. We have obtained 1319 spectra of 714 early-type galaxies over 33 observing runs on 10 different telescopes. We describe the observations and data reductions used to measure redshifts, velocity dispersions and the Mgb and Mg_2_ Lick linestrength indices. Detailed simulations and intercomparison of the large number of repeat observations lead to reliable error estimates for all quantities. The measurements from different observing runs are calibrated to a common zero-point or scale before being combined, yielding a total of 706 redshifts, 676 velocity dispersions, 676 Mgb linestrengths and 582 Mg_2_ linestrengths. The median estimated errors in the combined measurements are {Delta}cz=20km/s, {Delta}sigma/sigma=9.1%, {Delta}Mgb/Mgb=7.2% and {Delta}Mg_2_=0.015mag. Comparison of our measurements with published data sets shows no systematic errors in the redshifts or velocity dispersions, and only small zero-point corrections to bring our linestrengths on to the standard Lick system. We have assigned galaxies to physical clusters by examining the line-of-sight velocity distributions based on EFAR and ZCAT redshifts, together with the projected distributions on the sky. We derive mean redshifts and velocity dispersions for these clusters, which will be used in estimating distances and peculiar velocities and to test for trends in the galaxy population with cluster mass. The spectroscopic parameters presented here for 706 galaxies combine high-quality data, uniform reduction and measurement procedures, and detailed error analysis. They form the largest single set of velocity dispersions and linestrengths for early-type galaxies published to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/305/259#1</TD>
            <TD>2011-09-14T18:56:29Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/305/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/305/259</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/305/259</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/305/259 [2]</TD>
            <TD>EFAR galaxies redshifts &amp; velocity dispersions (Wegner+, 1999)</TD>
            <TD>We present the spectroscopic data for the galaxies studied in the EFAR project, which is designed to measure the properties and peculiar motions of early-type galaxies in two distant regions. We have obtained 1319 spectra of 714 early-type galaxies over 33 observing runs on 10 different telescopes. We describe the observations and data reductions used to measure redshifts, velocity dispersions and the Mgb and Mg_2_ Lick linestrength indices. Detailed simulations and intercomparison of the large number of repeat observations lead to reliable error estimates for all quantities. The measurements from different observing runs are calibrated to a common zero-point or scale before being combined, yielding a total of 706 redshifts, 676 velocity dispersions, 676 Mgb linestrengths and 582 Mg_2_ linestrengths. The median estimated errors in the combined measurements are {Delta}cz=20km/s, {Delta}sigma/sigma=9.1%, {Delta}Mgb/Mgb=7.2% and {Delta}Mg_2_=0.015mag. Comparison of our measurements with published data sets shows no systematic errors in the redshifts or velocity dispersions, and only small zero-point corrections to bring our linestrengths on to the standard Lick system. We have assigned galaxies to physical clusters by examining the line-of-sight velocity distributions based on EFAR and ZCAT redshifts, together with the projected distributions on the sky. We derive mean redshifts and velocity dispersions for these clusters, which will be used in estimating distances and peculiar velocities and to test for trends in the galaxy population with cluster mass. The spectroscopic parameters presented here for 706 galaxies combine high-quality data, uniform reduction and measurement procedures, and detailed error analysis. They form the largest single set of velocity dispersions and linestrengths for early-type galaxies published to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/305/259#2</TD>
            <TD>2011-09-14T18:56:29Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/305/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/305/259&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/305/259</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/142/153 [1]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#1</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/142/153</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/142/153 [2]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#2</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jiv-h]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jiv-h</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jvrb-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jvrb-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [hjir-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#hjir-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jirb-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jirb-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jr-h]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jr-h</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
            <TD>9999</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [hjrg-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#hjrg-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [hjiv-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#hjiv-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/305/259 [1]</TD>
            <TD>EFAR galaxies redshifts &amp; velocity dispersions (Wegner+, 1999)</TD>
            <TD>We present the spectroscopic data for the galaxies studied in the EFAR project, which is designed to measure the properties and peculiar motions of early-type galaxies in two distant regions. We have obtained 1319 spectra of 714 early-type galaxies over 33 observing runs on 10 different telescopes. We describe the observations and data reductions used to measure redshifts, velocity dispersions and the Mgb and Mg_2_ Lick linestrength indices. Detailed simulations and intercomparison of the large number of repeat observations lead to reliable error estimates for all quantities. The measurements from different observing runs are calibrated to a common zero-point or scale before being combined, yielding a total of 706 redshifts, 676 velocity dispersions, 676 Mgb linestrengths and 582 Mg_2_ linestrengths. The median estimated errors in the combined measurements are {Delta}cz=20km/s, {Delta}sigma/sigma=9.1%, {Delta}Mgb/Mgb=7.2% and {Delta}Mg_2_=0.015mag. Comparison of our measurements with published data sets shows no systematic errors in the redshifts or velocity dispersions, and only small zero-point corrections to bring our linestrengths on to the standard Lick system. We have assigned galaxies to physical clusters by examining the line-of-sight velocity distributions based on EFAR and ZCAT redshifts, together with the projected distributions on the sky. We derive mean redshifts and velocity dispersions for these clusters, which will be used in estimating distances and peculiar velocities and to test for trends in the galaxy population with cluster mass. The spectroscopic parameters presented here for 706 galaxies combine high-quality data, uniform reduction and measurement procedures, and detailed error analysis. They form the largest single set of velocity dispersions and linestrengths for early-type galaxies published to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/305/259#1</TD>
            <TD>2011-09-14T18:56:29Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/305/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/305/259</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/305/259</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/305/259 [2]</TD>
            <TD>EFAR galaxies redshifts &amp; velocity dispersions (Wegner+, 1999)</TD>
            <TD>We present the spectroscopic data for the galaxies studied in the EFAR project, which is designed to measure the properties and peculiar motions of early-type galaxies in two distant regions. We have obtained 1319 spectra of 714 early-type galaxies over 33 observing runs on 10 different telescopes. We describe the observations and data reductions used to measure redshifts, velocity dispersions and the Mgb and Mg_2_ Lick linestrength indices. Detailed simulations and intercomparison of the large number of repeat observations lead to reliable error estimates for all quantities. The measurements from different observing runs are calibrated to a common zero-point or scale before being combined, yielding a total of 706 redshifts, 676 velocity dispersions, 676 Mgb linestrengths and 582 Mg_2_ linestrengths. The median estimated errors in the combined measurements are {Delta}cz=20km/s, {Delta}sigma/sigma=9.1%, {Delta}Mgb/Mgb=7.2% and {Delta}Mg_2_=0.015mag. Comparison of our measurements with published data sets shows no systematic errors in the redshifts or velocity dispersions, and only small zero-point corrections to bring our linestrengths on to the standard Lick system. We have assigned galaxies to physical clusters by examining the line-of-sight velocity distributions based on EFAR and ZCAT redshifts, together with the projected distributions on the sky. We derive mean redshifts and velocity dispersions for these clusters, which will be used in estimating distances and peculiar velocities and to test for trends in the galaxy population with cluster mass. The spectroscopic parameters presented here for 706 galaxies combine high-quality data, uniform reduction and measurement procedures, and detailed error analysis. They form the largest single set of velocity dispersions and linestrengths for early-type galaxies published to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/305/259#2</TD>
            <TD>2011-09-14T18:56:29Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/305/259</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/305/259&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/305/259</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/137/117 [1]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#1</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/137/117</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/137/117 [2]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#2</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/137/117&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/137/117 [table2]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#table2</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/137/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/137/117 [table1]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#table1</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/137/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/142/153 [1]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#1</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/142/153</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/142/153 [2]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#2</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jiv-h]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jiv-h</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jvrb-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jvrb-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [hjir-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#hjir-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jirb-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jirb-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jr-h]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jr-h</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [hjrg-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#hjrg-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [hjiv-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#hjiv-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/71/189 [1]</TD>
            <TD>Gas Kinematics from Halpha line in NGC 4151 (Sergeev, 1994)</TD>
            <TD>The nucleus spectra of the Seyfert galaxy NGC 4151 obtained in 1988-1991 were analyzed in order to study the profile variability of the Ha line resulting from ionizing continuum flux variations. At the time of this galaxy monitoring, the response of the integral flux of the Ha line was almost linear and the average profile shape did not change by more than 5%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/71/189#1</TD>
            <TD>2011-09-14T18:56:51Z</TD>
            <TD>#AGN#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AZh/71/189</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/71/189</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/71/189</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/71/189 [2]</TD>
            <TD>Gas Kinematics from Halpha line in NGC 4151 (Sergeev, 1994)</TD>
            <TD>The nucleus spectra of the Seyfert galaxy NGC 4151 obtained in 1988-1991 were analyzed in order to study the profile variability of the Ha line resulting from ionizing continuum flux variations. At the time of this galaxy monitoring, the response of the integral flux of the Ha line was almost linear and the average profile shape did not change by more than 5%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/71/189#2</TD>
            <TD>2011-09-14T18:56:51Z</TD>
            <TD>#AGN#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AZh/71/189</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/71/189&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/71/189</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/137/117 [1]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#1</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/137/117</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/137/117 [2]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#2</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/137/117&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/137/117 [table2]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#table2</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/137/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/137/117 [table1]</TD>
            <TD>Las Campanas Distant Cluster Survey (LCDCS) (Gonzales+, 2001)</TD>
            <TD>We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3&lt;~z&lt;~1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. The survey data were obtained in 1995 March under photometric conditions using the Las Campanas 1 m telescope, the Great Circle Camera, and the Tek No. 5 CCD. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, {sigma}, is used to estimate the limiting velocity dispersion of the survey as a function of redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117#table1</TD>
            <TD>2011-09-14T19:13:32Z</TD>
            <TD>#Clusters_of_galaxies#Extinction#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/137/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/137/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/137/117</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/142/153 [1]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#1</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/142/153</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/142/153 [2]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#2</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jiv-h]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jiv-h</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jvrb-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jvrb-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [hjir-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#hjir-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jirb-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jirb-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [jr-h]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#jr-h</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [hjrg-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#hjrg-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/142/153 [hjiv-k]</TD>
            <TD>Distant galaxy clusters photometry (Stanford+, 2002)</TD>
            <TD>We present optical and near-infrared photometry of 45 clusters of galaxies at 0.1&lt;z&lt;1.3. Galaxy catalogs in each cluster were defined at the longest wavelength available, generally the K band, down to approximately 2mag below M*. We include finding chart images of the band used for catalog definition. The photometry has been used in previously published papers to examine the origin and evolution of galaxies in distant clusters. Beginning in 1991, we sought to make use of the advent of relatively large format near-IR detectors to study the galaxy populations of distant clusters. We collected imaging data in both the near-IR and the optical on a large sample of clusters drawn from several samples. These data were analyzed and detailed results were presented on the evolution of early-type galaxies at moderate redshifts in Stanford, Eisenhardt, &amp; Dickinson (1995ApJ...450..512S, 1998ApJ...492..461S), on the evolution of the K-band luminosity function in De Propris et al. (1999AJ....118..719D), on the Butcher-Oemler effect in K-selected galaxy samples in De Propris et al. (2003, ApJ, submitted), and on the evolution of early-type galaxies in high-redshift clusters in Holden et al. (2003, ApJ, in press). So far the photometry for these various studies has been published for only two clusters, Abell 370 and Abell 851 in Stanford et al. (1995ApJ...450..512S). In this paper, we present the photometry on the other 43 clusters used in our published work on distant clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153#hjiv-k</TD>
            <TD>2011-09-14T19:39:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/142/153</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/142/153&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/142/153</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/71/189 [1]</TD>
            <TD>Gas Kinematics from Halpha line in NGC 4151 (Sergeev, 1994)</TD>
            <TD>The nucleus spectra of the Seyfert galaxy NGC 4151 obtained in 1988-1991 were analyzed in order to study the profile variability of the Ha line resulting from ionizing continuum flux variations. At the time of this galaxy monitoring, the response of the integral flux of the Ha line was almost linear and the average profile shape did not change by more than 5%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/71/189#1</TD>
            <TD>2011-09-14T18:56:51Z</TD>
            <TD>#AGN#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AZh/71/189</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/71/189</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/71/189</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/71/189 [2]</TD>
            <TD>Gas Kinematics from Halpha line in NGC 4151 (Sergeev, 1994)</TD>
            <TD>The nucleus spectra of the Seyfert galaxy NGC 4151 obtained in 1988-1991 were analyzed in order to study the profile variability of the Ha line resulting from ionizing continuum flux variations. At the time of this galaxy monitoring, the response of the integral flux of the Ha line was almost linear and the average profile shape did not change by more than 5%.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/71/189#2</TD>
            <TD>2011-09-14T18:56:51Z</TD>
            <TD>#AGN#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Dec-1996</TD>
            <TD>ivo://CDS.VizieR/J/AZh/71/189</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/71/189&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/71/189</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/588 [1]</TD>
            <TD>Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)</TD>
            <TD>The Las Campanas Observatory and Anglo-Australian Telescope Rich Cluster Survey (LARCS) is a panoramic imaging and spectroscopic survey of an X-ray luminosity-selected sample of 21 clusters of galaxies at 0.97&lt;z&lt;0.16. Charge-coupled device (CCD) imaging was obtained in B and R of typically 2{deg} wide regions centred on the 21 clusters, and the galaxy sample selected from the imaging is being used for an on-going spectroscopic survey of the clusters with the 2dF spectrograph on the Anglo-Australian Telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588#1</TD>
            <TD>2011-09-14T19:13:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/588</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/588</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/588 [2]</TD>
            <TD>Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)</TD>
            <TD>The Las Campanas Observatory and Anglo-Australian Telescope Rich Cluster Survey (LARCS) is a panoramic imaging and spectroscopic survey of an X-ray luminosity-selected sample of 21 clusters of galaxies at 0.97&lt;z&lt;0.16. Charge-coupled device (CCD) imaging was obtained in B and R of typically 2{deg} wide regions centred on the 21 clusters, and the galaxy sample selected from the imaging is being used for an on-going spectroscopic survey of the clusters with the 2dF spectrograph on the Anglo-Australian Telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588#2</TD>
            <TD>2011-09-14T19:13:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/588&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/588</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/588 [table1]</TD>
            <TD>Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)</TD>
            <TD>The Las Campanas Observatory and Anglo-Australian Telescope Rich Cluster Survey (LARCS) is a panoramic imaging and spectroscopic survey of an X-ray luminosity-selected sample of 21 clusters of galaxies at 0.97&lt;z&lt;0.16. Charge-coupled device (CCD) imaging was obtained in B and R of typically 2{deg} wide regions centred on the 21 clusters, and the galaxy sample selected from the imaging is being used for an on-going spectroscopic survey of the clusters with the 2dF spectrograph on the Anglo-Australian Telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588#table1</TD>
            <TD>2011-09-14T19:13:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/588&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/588</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/588 [1]</TD>
            <TD>Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)</TD>
            <TD>The Las Campanas Observatory and Anglo-Australian Telescope Rich Cluster Survey (LARCS) is a panoramic imaging and spectroscopic survey of an X-ray luminosity-selected sample of 21 clusters of galaxies at 0.97&lt;z&lt;0.16. Charge-coupled device (CCD) imaging was obtained in B and R of typically 2{deg} wide regions centred on the 21 clusters, and the galaxy sample selected from the imaging is being used for an on-going spectroscopic survey of the clusters with the 2dF spectrograph on the Anglo-Australian Telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588#1</TD>
            <TD>2011-09-14T19:13:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/588</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/588</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/588 [2]</TD>
            <TD>Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)</TD>
            <TD>The Las Campanas Observatory and Anglo-Australian Telescope Rich Cluster Survey (LARCS) is a panoramic imaging and spectroscopic survey of an X-ray luminosity-selected sample of 21 clusters of galaxies at 0.97&lt;z&lt;0.16. Charge-coupled device (CCD) imaging was obtained in B and R of typically 2{deg} wide regions centred on the 21 clusters, and the galaxy sample selected from the imaging is being used for an on-going spectroscopic survey of the clusters with the 2dF spectrograph on the Anglo-Australian Telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588#2</TD>
            <TD>2011-09-14T19:13:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/588&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/588</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/588 [table1]</TD>
            <TD>Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)</TD>
            <TD>The Las Campanas Observatory and Anglo-Australian Telescope Rich Cluster Survey (LARCS) is a panoramic imaging and spectroscopic survey of an X-ray luminosity-selected sample of 21 clusters of galaxies at 0.97&lt;z&lt;0.16. Charge-coupled device (CCD) imaging was obtained in B and R of typically 2{deg} wide regions centred on the 21 clusters, and the galaxy sample selected from the imaging is being used for an on-going spectroscopic survey of the clusters with the 2dF spectrograph on the Anglo-Australian Telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588#table1</TD>
            <TD>2011-09-14T19:13:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/588&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/588</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/38/351 [1]</TD>
            <TD>M31 planetary nebulae (Ford+, 1978)</TD>
            <TD>Finding charts and equatorial coordinates are presented for 311 planetary nebulae and for nearby reference stars in the Andromeda galaxy (M31). The standard deviation of the coordinates relative to the AGK3 is smaller than 1.0". The standard deviation of the coordinates relative to the reference stars is smaller than 0.5".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351#1</TD>
            <TD>2011-09-14T19:40:34Z</TD>
            <TD>#AGN#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/38/351</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/38/351</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/38/351 [2]</TD>
            <TD>M31 planetary nebulae (Ford+, 1978)</TD>
            <TD>Finding charts and equatorial coordinates are presented for 311 planetary nebulae and for nearby reference stars in the Andromeda galaxy (M31). The standard deviation of the coordinates relative to the AGK3 is smaller than 1.0". The standard deviation of the coordinates relative to the reference stars is smaller than 0.5".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351#2</TD>
            <TD>2011-09-14T19:40:34Z</TD>
            <TD>#AGN#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/38/351&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/38/351</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/500/554 [1]</TD>
            <TD>COBE DIRBE IR photometry (Odenwald+ 1998)</TD>
            <TD>A comparison of the COBE Diffuse Infrared Background Experiment (DIRBE) all-sky survey with the locations of known galaxies in the IRAS Catalog of Extragalactic Objects and the Center for Astrophysics Catalog of Galaxies led to the detection of as many as 57 galaxies. In this paper, we present the photometric data for these galaxies and an analysisof the seven galaxiesthat were detected at {lambda}&gt;100{mu}m. Estimates of the ratio of the mass of the cold dust (CD) component detected at T_d_=20-30K to a very cold dust (VCD) component with T_d_~10-15K suggest that between 2%-100% of the cirrus-like CD mass can also exist in many of these galaxies as VCD. In one galaxy, M33, the DIRBE photometry at 240{mu}m suggests as much as 26 times as much VCD may be present as compared to the cirrus-like component. Further submillimeter measurements of this galaxy are required to verify such a large population of VCD. We also present 10 galaxies that were detected in the sky region not previously surveyed by IRAS and that can be used to construct a flux-limited all-sky catalog of galaxies brighter than 1000Jy with a modest completeness limit of about 65%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554#1</TD>
            <TD>2011-09-14T18:58:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/500/554</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/554</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/500/554 [2]</TD>
            <TD>COBE DIRBE IR photometry (Odenwald+ 1998)</TD>
            <TD>A comparison of the COBE Diffuse Infrared Background Experiment (DIRBE) all-sky survey with the locations of known galaxies in the IRAS Catalog of Extragalactic Objects and the Center for Astrophysics Catalog of Galaxies led to the detection of as many as 57 galaxies. In this paper, we present the photometric data for these galaxies and an analysisof the seven galaxiesthat were detected at {lambda}&gt;100{mu}m. Estimates of the ratio of the mass of the cold dust (CD) component detected at T_d_=20-30K to a very cold dust (VCD) component with T_d_~10-15K suggest that between 2%-100% of the cirrus-like CD mass can also exist in many of these galaxies as VCD. In one galaxy, M33, the DIRBE photometry at 240{mu}m suggests as much as 26 times as much VCD may be present as compared to the cirrus-like component. Further submillimeter measurements of this galaxy are required to verify such a large population of VCD. We also present 10 galaxies that were detected in the sky region not previously surveyed by IRAS and that can be used to construct a flux-limited all-sky catalog of galaxies brighter than 1000Jy with a modest completeness limit of about 65%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554#2</TD>
            <TD>2011-09-14T18:58:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/500/554&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/554</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/327/588 [1]</TD>
            <TD>Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)</TD>
            <TD>The Las Campanas Observatory and Anglo-Australian Telescope Rich Cluster Survey (LARCS) is a panoramic imaging and spectroscopic survey of an X-ray luminosity-selected sample of 21 clusters of galaxies at 0.97&lt;z&lt;0.16. Charge-coupled device (CCD) imaging was obtained in B and R of typically 2{deg} wide regions centred on the 21 clusters, and the galaxy sample selected from the imaging is being used for an on-going spectroscopic survey of the clusters with the 2dF spectrograph on the Anglo-Australian Telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588#1</TD>
            <TD>2011-09-14T19:13:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/327/588</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/588</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/327/588 [2]</TD>
            <TD>Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)</TD>
            <TD>The Las Campanas Observatory and Anglo-Australian Telescope Rich Cluster Survey (LARCS) is a panoramic imaging and spectroscopic survey of an X-ray luminosity-selected sample of 21 clusters of galaxies at 0.97&lt;z&lt;0.16. Charge-coupled device (CCD) imaging was obtained in B and R of typically 2{deg} wide regions centred on the 21 clusters, and the galaxy sample selected from the imaging is being used for an on-going spectroscopic survey of the clusters with the 2dF spectrograph on the Anglo-Australian Telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588#2</TD>
            <TD>2011-09-14T19:13:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/327/588&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/588</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/327/588 [table1]</TD>
            <TD>Las Campanas/AAT Rich Cluster Survey - I (Pimbblet+, 2001)</TD>
            <TD>The Las Campanas Observatory and Anglo-Australian Telescope Rich Cluster Survey (LARCS) is a panoramic imaging and spectroscopic survey of an X-ray luminosity-selected sample of 21 clusters of galaxies at 0.97&lt;z&lt;0.16. Charge-coupled device (CCD) imaging was obtained in B and R of typically 2{deg} wide regions centred on the 21 clusters, and the galaxy sample selected from the imaging is being used for an on-going spectroscopic survey of the clusters with the 2dF spectrograph on the Anglo-Australian Telescope.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588#table1</TD>
            <TD>2011-09-14T19:13:33Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/327/588</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/327/588&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/327/588</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/38/351 [1]</TD>
            <TD>M31 planetary nebulae (Ford+, 1978)</TD>
            <TD>Finding charts and equatorial coordinates are presented for 311 planetary nebulae and for nearby reference stars in the Andromeda galaxy (M31). The standard deviation of the coordinates relative to the AGK3 is smaller than 1.0". The standard deviation of the coordinates relative to the reference stars is smaller than 0.5".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351#1</TD>
            <TD>2011-09-14T19:40:34Z</TD>
            <TD>#AGN#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/38/351</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/38/351</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/38/351 [2]</TD>
            <TD>M31 planetary nebulae (Ford+, 1978)</TD>
            <TD>Finding charts and equatorial coordinates are presented for 311 planetary nebulae and for nearby reference stars in the Andromeda galaxy (M31). The standard deviation of the coordinates relative to the AGK3 is smaller than 1.0". The standard deviation of the coordinates relative to the reference stars is smaller than 0.5".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351#2</TD>
            <TD>2011-09-14T19:40:34Z</TD>
            <TD>#AGN#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/38/351&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/38/351</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/500/554 [1]</TD>
            <TD>COBE DIRBE IR photometry (Odenwald+ 1998)</TD>
            <TD>A comparison of the COBE Diffuse Infrared Background Experiment (DIRBE) all-sky survey with the locations of known galaxies in the IRAS Catalog of Extragalactic Objects and the Center for Astrophysics Catalog of Galaxies led to the detection of as many as 57 galaxies. In this paper, we present the photometric data for these galaxies and an analysisof the seven galaxiesthat were detected at {lambda}&gt;100{mu}m. Estimates of the ratio of the mass of the cold dust (CD) component detected at T_d_=20-30K to a very cold dust (VCD) component with T_d_~10-15K suggest that between 2%-100% of the cirrus-like CD mass can also exist in many of these galaxies as VCD. In one galaxy, M33, the DIRBE photometry at 240{mu}m suggests as much as 26 times as much VCD may be present as compared to the cirrus-like component. Further submillimeter measurements of this galaxy are required to verify such a large population of VCD. We also present 10 galaxies that were detected in the sky region not previously surveyed by IRAS and that can be used to construct a flux-limited all-sky catalog of galaxies brighter than 1000Jy with a modest completeness limit of about 65%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554#1</TD>
            <TD>2011-09-14T18:58:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/500/554</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/554</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/500/554 [2]</TD>
            <TD>COBE DIRBE IR photometry (Odenwald+ 1998)</TD>
            <TD>A comparison of the COBE Diffuse Infrared Background Experiment (DIRBE) all-sky survey with the locations of known galaxies in the IRAS Catalog of Extragalactic Objects and the Center for Astrophysics Catalog of Galaxies led to the detection of as many as 57 galaxies. In this paper, we present the photometric data for these galaxies and an analysisof the seven galaxiesthat were detected at {lambda}&gt;100{mu}m. Estimates of the ratio of the mass of the cold dust (CD) component detected at T_d_=20-30K to a very cold dust (VCD) component with T_d_~10-15K suggest that between 2%-100% of the cirrus-like CD mass can also exist in many of these galaxies as VCD. In one galaxy, M33, the DIRBE photometry at 240{mu}m suggests as much as 26 times as much VCD may be present as compared to the cirrus-like component. Further submillimeter measurements of this galaxy are required to verify such a large population of VCD. We also present 10 galaxies that were detected in the sky region not previously surveyed by IRAS and that can be used to construct a flux-limited all-sky catalog of galaxies brighter than 1000Jy with a modest completeness limit of about 65%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554#2</TD>
            <TD>2011-09-14T18:58:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/500/554&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/554</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/301/881 [1]</TD>
            <TD>The ROSAT brightest cluster sample - I. (Ebeling+, 1998)</TD>
            <TD>We present a 90 per cent flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere ({delta}&gt;=0{deg}), at high Galactic latitudes (|b|&gt;= 20{deg}), with measured redshifts z&lt;=0.3 and fluxes higher than 4.4x10^-12^erg/cm^2^/s in the 0.112.4 keV band. The sample, called the ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky Survey data and is the largest X-ray-selected cluster sample compiled to date. In addition to Abell clusters, which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes are computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15 per cent (mean 1{sigma} error).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881#1</TD>
            <TD>2011-09-14T19:13:47Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/301/881</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/301/881</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/301/881 [2]</TD>
            <TD>The ROSAT brightest cluster sample - I. (Ebeling+, 1998)</TD>
            <TD>We present a 90 per cent flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere ({delta}&gt;=0{deg}), at high Galactic latitudes (|b|&gt;= 20{deg}), with measured redshifts z&lt;=0.3 and fluxes higher than 4.4x10^-12^erg/cm^2^/s in the 0.112.4 keV band. The sample, called the ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky Survey data and is the largest X-ray-selected cluster sample compiled to date. In addition to Abell clusters, which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes are computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15 per cent (mean 1{sigma} error).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881#2</TD>
            <TD>2011-09-14T19:13:47Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/301/881&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/301/881</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/301/881 [table3]</TD>
            <TD>The ROSAT brightest cluster sample - I. (Ebeling+, 1998)</TD>
            <TD>We present a 90 per cent flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere ({delta}&gt;=0{deg}), at high Galactic latitudes (|b|&gt;= 20{deg}), with measured redshifts z&lt;=0.3 and fluxes higher than 4.4x10^-12^erg/cm^2^/s in the 0.112.4 keV band. The sample, called the ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky Survey data and is the largest X-ray-selected cluster sample compiled to date. In addition to Abell clusters, which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes are computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15 per cent (mean 1{sigma} error).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881#table3</TD>
            <TD>2011-09-14T19:13:47Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/301/881&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/301/881</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/38/351 [1]</TD>
            <TD>M31 planetary nebulae (Ford+, 1978)</TD>
            <TD>Finding charts and equatorial coordinates are presented for 311 planetary nebulae and for nearby reference stars in the Andromeda galaxy (M31). The standard deviation of the coordinates relative to the AGK3 is smaller than 1.0". The standard deviation of the coordinates relative to the reference stars is smaller than 0.5".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351#1</TD>
            <TD>2011-09-14T19:40:34Z</TD>
            <TD>#AGN#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/38/351</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/38/351</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/38/351 [2]</TD>
            <TD>M31 planetary nebulae (Ford+, 1978)</TD>
            <TD>Finding charts and equatorial coordinates are presented for 311 planetary nebulae and for nearby reference stars in the Andromeda galaxy (M31). The standard deviation of the coordinates relative to the AGK3 is smaller than 1.0". The standard deviation of the coordinates relative to the reference stars is smaller than 0.5".</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351#2</TD>
            <TD>2011-09-14T19:40:34Z</TD>
            <TD>#AGN#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/38/351</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/38/351&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/38/351</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/500/554 [1]</TD>
            <TD>COBE DIRBE IR photometry (Odenwald+ 1998)</TD>
            <TD>A comparison of the COBE Diffuse Infrared Background Experiment (DIRBE) all-sky survey with the locations of known galaxies in the IRAS Catalog of Extragalactic Objects and the Center for Astrophysics Catalog of Galaxies led to the detection of as many as 57 galaxies. In this paper, we present the photometric data for these galaxies and an analysisof the seven galaxiesthat were detected at {lambda}&gt;100{mu}m. Estimates of the ratio of the mass of the cold dust (CD) component detected at T_d_=20-30K to a very cold dust (VCD) component with T_d_~10-15K suggest that between 2%-100% of the cirrus-like CD mass can also exist in many of these galaxies as VCD. In one galaxy, M33, the DIRBE photometry at 240{mu}m suggests as much as 26 times as much VCD may be present as compared to the cirrus-like component. Further submillimeter measurements of this galaxy are required to verify such a large population of VCD. We also present 10 galaxies that were detected in the sky region not previously surveyed by IRAS and that can be used to construct a flux-limited all-sky catalog of galaxies brighter than 1000Jy with a modest completeness limit of about 65%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554#1</TD>
            <TD>2011-09-14T18:58:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/500/554</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/554</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/500/554 [2]</TD>
            <TD>COBE DIRBE IR photometry (Odenwald+ 1998)</TD>
            <TD>A comparison of the COBE Diffuse Infrared Background Experiment (DIRBE) all-sky survey with the locations of known galaxies in the IRAS Catalog of Extragalactic Objects and the Center for Astrophysics Catalog of Galaxies led to the detection of as many as 57 galaxies. In this paper, we present the photometric data for these galaxies and an analysisof the seven galaxiesthat were detected at {lambda}&gt;100{mu}m. Estimates of the ratio of the mass of the cold dust (CD) component detected at T_d_=20-30K to a very cold dust (VCD) component with T_d_~10-15K suggest that between 2%-100% of the cirrus-like CD mass can also exist in many of these galaxies as VCD. In one galaxy, M33, the DIRBE photometry at 240{mu}m suggests as much as 26 times as much VCD may be present as compared to the cirrus-like component. Further submillimeter measurements of this galaxy are required to verify such a large population of VCD. We also present 10 galaxies that were detected in the sky region not previously surveyed by IRAS and that can be used to construct a flux-limited all-sky catalog of galaxies brighter than 1000Jy with a modest completeness limit of about 65%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554#2</TD>
            <TD>2011-09-14T18:58:33Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/500/554</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/500/554&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/500/554</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/301/881 [1]</TD>
            <TD>The ROSAT brightest cluster sample - I. (Ebeling+, 1998)</TD>
            <TD>We present a 90 per cent flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere ({delta}&gt;=0{deg}), at high Galactic latitudes (|b|&gt;= 20{deg}), with measured redshifts z&lt;=0.3 and fluxes higher than 4.4x10^-12^erg/cm^2^/s in the 0.112.4 keV band. The sample, called the ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky Survey data and is the largest X-ray-selected cluster sample compiled to date. In addition to Abell clusters, which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes are computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15 per cent (mean 1{sigma} error).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881#1</TD>
            <TD>2011-09-14T19:13:47Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/301/881</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/301/881</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/301/881 [2]</TD>
            <TD>The ROSAT brightest cluster sample - I. (Ebeling+, 1998)</TD>
            <TD>We present a 90 per cent flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere ({delta}&gt;=0{deg}), at high Galactic latitudes (|b|&gt;= 20{deg}), with measured redshifts z&lt;=0.3 and fluxes higher than 4.4x10^-12^erg/cm^2^/s in the 0.112.4 keV band. The sample, called the ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky Survey data and is the largest X-ray-selected cluster sample compiled to date. In addition to Abell clusters, which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes are computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15 per cent (mean 1{sigma} error).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881#2</TD>
            <TD>2011-09-14T19:13:47Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/301/881&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/301/881</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/301/881 [table3]</TD>
            <TD>The ROSAT brightest cluster sample - I. (Ebeling+, 1998)</TD>
            <TD>We present a 90 per cent flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere ({delta}&gt;=0{deg}), at high Galactic latitudes (|b|&gt;= 20{deg}), with measured redshifts z&lt;=0.3 and fluxes higher than 4.4x10^-12^erg/cm^2^/s in the 0.112.4 keV band. The sample, called the ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky Survey data and is the largest X-ray-selected cluster sample compiled to date. In addition to Abell clusters, which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes are computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15 per cent (mean 1{sigma} error).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881#table3</TD>
            <TD>2011-09-14T19:13:47Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/301/881&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/301/881</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/1 [1]</TD>
            <TD>Morphologies of distant galaxies II (Abraham+ 1996)</TD>
            <TD>The morphological properties of high-redshift galaxies are investigated using a sample of 507 objects (I&lt;22.0mag) from the Hubble Space Telescope (HST) Medium Deep Survey. Independent visual morphological classifications for each galaxy are used to quantify the statistical uncertainties in the galaxy classifications. Visual classifications are found to agree well for I&lt;21mag. Fainter than I=21mag significant disagreements are seen in the independent visual classifications of late-type systems with T&gt;7, merging systems, and peculiar galaxies. The classifications of these systems are shown to be somewhat subjective. Objective classifications based upon measurements of central concentration and asymmetry for the Medium Deep Survey sample are presented. These classifications are calibrated using measurements of structural parameters for an artificially redshifted sample of local objects. Morphologically segregated number counts using both sets of visual classifications and objective classifications support the conclusion that the observed galaxy counts agree with no-evolution predictions for the elliptical and spiral populations, as reported in Glazebrook et al. (1995MNRAS.275L..19G). A major conclusion is that the large overdensity of merging/ peculiar/ irregular galaxies relative to the predictions of no-evolution models (reported by Glazebrook et al. 1995MNRAS.275L..19G) is confirmed. However, the shape of the faint-end (I&gt;21.0mag) number count relation for peculiar objects is sensitive to the large systematic uncertainties inherent in the visual classification of these objects. Despite this caveat, the frequency of objects showing clear evidence for tidal interactions (e.g., tidal tails) in the HST sample is at least 50% larger than it is among nearby galaxies, at the 2{sigma} level. Relatively few "chain galaxies" are seen among the sample of peculiar objects, suggesting that these systems do not form a large component of the peculiar galaxy population at I&lt;22mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1#1</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/1 [2]</TD>
            <TD>Morphologies of distant galaxies II (Abraham+ 1996)</TD>
            <TD>The morphological properties of high-redshift galaxies are investigated using a sample of 507 objects (I&lt;22.0mag) from the Hubble Space Telescope (HST) Medium Deep Survey. Independent visual morphological classifications for each galaxy are used to quantify the statistical uncertainties in the galaxy classifications. Visual classifications are found to agree well for I&lt;21mag. Fainter than I=21mag significant disagreements are seen in the independent visual classifications of late-type systems with T&gt;7, merging systems, and peculiar galaxies. The classifications of these systems are shown to be somewhat subjective. Objective classifications based upon measurements of central concentration and asymmetry for the Medium Deep Survey sample are presented. These classifications are calibrated using measurements of structural parameters for an artificially redshifted sample of local objects. Morphologically segregated number counts using both sets of visual classifications and objective classifications support the conclusion that the observed galaxy counts agree with no-evolution predictions for the elliptical and spiral populations, as reported in Glazebrook et al. (1995MNRAS.275L..19G). A major conclusion is that the large overdensity of merging/ peculiar/ irregular galaxies relative to the predictions of no-evolution models (reported by Glazebrook et al. 1995MNRAS.275L..19G) is confirmed. However, the shape of the faint-end (I&gt;21.0mag) number count relation for peculiar objects is sensitive to the large systematic uncertainties inherent in the visual classification of these objects. Despite this caveat, the frequency of objects showing clear evidence for tidal interactions (e.g., tidal tails) in the HST sample is at least 50% larger than it is among nearby galaxies, at the 2{sigma} level. Relatively few "chain galaxies" are seen among the sample of peculiar objects, suggesting that these systems do not form a large component of the peculiar galaxy population at I&lt;22mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1#2</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/140/327 [1]</TD>
            <TD>Fundamental plane galaxies redshifts (Mueller+, 1999)</TD>
            <TD>Radial velocities and central velocity dispersions are derived for 238 E/S0 galaxies from medium-resolution spectroscopy. New spectroscopic data have been obtained as part of a study of the Fundamental Plane distances and peculiar motions of early-type galaxies in three selected directions of the South Equatorial Strip, undertaken in order to investigate the reality of large-scale streaming motion; results of this study have been reported in Mueller et al. (1998ApJ...507L.105M). The new APM South Equatorial Strip Catalog (-17.5deg&lt;{delta}&lt;+2.5deg) (Raychaudhury &amp; Lynden-Bell, 2000) was used to select the sample of field galaxies in three directions: (1) 15h10-16h10; (2) 20h30-21h50; (3) 00h10-01h30. The spectra obtained have a median S/N per {AA} of 23, an instrumental resolution (FWHM) of ~4{AA}, and the spectrograph resolution (dispersion) is ~100km/s. The Fourier cross-correlation method was used to derive the radial velocities and velocity dispersions. The velocity dispersions have been corrected for the size of the aperture and for the galaxy effective radius. Comparisons of the derived radial velocities with data from the literature show that our values are accurate to 40km/s. A comparison with results from Jorgensen et al. (1995MNRAS.276.1341J) shows that the derived central velocity dispersion have an rms scatter of 0.036 in log{sigma}. There is no offset relative to the velocity dispersions of Davies et al. (1987ApJS...64..581D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327#1</TD>
            <TD>2011-09-14T18:59:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/140/327</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/327</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/140/327 [2]</TD>
            <TD>Fundamental plane galaxies redshifts (Mueller+, 1999)</TD>
            <TD>Radial velocities and central velocity dispersions are derived for 238 E/S0 galaxies from medium-resolution spectroscopy. New spectroscopic data have been obtained as part of a study of the Fundamental Plane distances and peculiar motions of early-type galaxies in three selected directions of the South Equatorial Strip, undertaken in order to investigate the reality of large-scale streaming motion; results of this study have been reported in Mueller et al. (1998ApJ...507L.105M). The new APM South Equatorial Strip Catalog (-17.5deg&lt;{delta}&lt;+2.5deg) (Raychaudhury &amp; Lynden-Bell, 2000) was used to select the sample of field galaxies in three directions: (1) 15h10-16h10; (2) 20h30-21h50; (3) 00h10-01h30. The spectra obtained have a median S/N per {AA} of 23, an instrumental resolution (FWHM) of ~4{AA}, and the spectrograph resolution (dispersion) is ~100km/s. The Fourier cross-correlation method was used to derive the radial velocities and velocity dispersions. The velocity dispersions have been corrected for the size of the aperture and for the galaxy effective radius. Comparisons of the derived radial velocities with data from the literature show that our values are accurate to 40km/s. A comparison with results from Jorgensen et al. (1995MNRAS.276.1341J) shows that the derived central velocity dispersion have an rms scatter of 0.036 in log{sigma}. There is no offset relative to the velocity dispersions of Davies et al. (1987ApJS...64..581D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327#2</TD>
            <TD>2011-09-14T18:59:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/140/327&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/327</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/301/881 [1]</TD>
            <TD>The ROSAT brightest cluster sample - I. (Ebeling+, 1998)</TD>
            <TD>We present a 90 per cent flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere ({delta}&gt;=0{deg}), at high Galactic latitudes (|b|&gt;= 20{deg}), with measured redshifts z&lt;=0.3 and fluxes higher than 4.4x10^-12^erg/cm^2^/s in the 0.112.4 keV band. The sample, called the ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky Survey data and is the largest X-ray-selected cluster sample compiled to date. In addition to Abell clusters, which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes are computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15 per cent (mean 1{sigma} error).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881#1</TD>
            <TD>2011-09-14T19:13:47Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/301/881</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/301/881</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/301/881 [2]</TD>
            <TD>The ROSAT brightest cluster sample - I. (Ebeling+, 1998)</TD>
            <TD>We present a 90 per cent flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere ({delta}&gt;=0{deg}), at high Galactic latitudes (|b|&gt;= 20{deg}), with measured redshifts z&lt;=0.3 and fluxes higher than 4.4x10^-12^erg/cm^2^/s in the 0.112.4 keV band. The sample, called the ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky Survey data and is the largest X-ray-selected cluster sample compiled to date. In addition to Abell clusters, which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes are computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15 per cent (mean 1{sigma} error).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881#2</TD>
            <TD>2011-09-14T19:13:47Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/301/881&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/301/881</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/301/881 [table3]</TD>
            <TD>The ROSAT brightest cluster sample - I. (Ebeling+, 1998)</TD>
            <TD>We present a 90 per cent flux-complete sample of the 201 X-ray-brightest clusters of galaxies in the northern hemisphere ({delta}&gt;=0{deg}), at high Galactic latitudes (|b|&gt;= 20{deg}), with measured redshifts z&lt;=0.3 and fluxes higher than 4.4x10^-12^erg/cm^2^/s in the 0.112.4 keV band. The sample, called the ROSAT Brightest Cluster Sample (BCS), is selected from ROSAT All-Sky Survey data and is the largest X-ray-selected cluster sample compiled to date. In addition to Abell clusters, which form the bulk of the sample, the BCS also contains the X-ray-brightest Zwicky clusters and other clusters selected from their X-ray properties alone. Effort has been made to ensure the highest possible completeness of the sample and the smallest possible contamination by non-cluster X-ray sources. X-ray fluxes are computed using an algorithm tailored for the detection and characterization of X-ray emission from galaxy clusters. These fluxes are accurate to better than 15 per cent (mean 1{sigma} error).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881#table3</TD>
            <TD>2011-09-14T19:13:47Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/301/881</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/301/881&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/301/881</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/1 [1]</TD>
            <TD>Morphologies of distant galaxies II (Abraham+ 1996)</TD>
            <TD>The morphological properties of high-redshift galaxies are investigated using a sample of 507 objects (I&lt;22.0mag) from the Hubble Space Telescope (HST) Medium Deep Survey. Independent visual morphological classifications for each galaxy are used to quantify the statistical uncertainties in the galaxy classifications. Visual classifications are found to agree well for I&lt;21mag. Fainter than I=21mag significant disagreements are seen in the independent visual classifications of late-type systems with T&gt;7, merging systems, and peculiar galaxies. The classifications of these systems are shown to be somewhat subjective. Objective classifications based upon measurements of central concentration and asymmetry for the Medium Deep Survey sample are presented. These classifications are calibrated using measurements of structural parameters for an artificially redshifted sample of local objects. Morphologically segregated number counts using both sets of visual classifications and objective classifications support the conclusion that the observed galaxy counts agree with no-evolution predictions for the elliptical and spiral populations, as reported in Glazebrook et al. (1995MNRAS.275L..19G). A major conclusion is that the large overdensity of merging/ peculiar/ irregular galaxies relative to the predictions of no-evolution models (reported by Glazebrook et al. 1995MNRAS.275L..19G) is confirmed. However, the shape of the faint-end (I&gt;21.0mag) number count relation for peculiar objects is sensitive to the large systematic uncertainties inherent in the visual classification of these objects. Despite this caveat, the frequency of objects showing clear evidence for tidal interactions (e.g., tidal tails) in the HST sample is at least 50% larger than it is among nearby galaxies, at the 2{sigma} level. Relatively few "chain galaxies" are seen among the sample of peculiar objects, suggesting that these systems do not form a large component of the peculiar galaxy population at I&lt;22mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1#1</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/1 [2]</TD>
            <TD>Morphologies of distant galaxies II (Abraham+ 1996)</TD>
            <TD>The morphological properties of high-redshift galaxies are investigated using a sample of 507 objects (I&lt;22.0mag) from the Hubble Space Telescope (HST) Medium Deep Survey. Independent visual morphological classifications for each galaxy are used to quantify the statistical uncertainties in the galaxy classifications. Visual classifications are found to agree well for I&lt;21mag. Fainter than I=21mag significant disagreements are seen in the independent visual classifications of late-type systems with T&gt;7, merging systems, and peculiar galaxies. The classifications of these systems are shown to be somewhat subjective. Objective classifications based upon measurements of central concentration and asymmetry for the Medium Deep Survey sample are presented. These classifications are calibrated using measurements of structural parameters for an artificially redshifted sample of local objects. Morphologically segregated number counts using both sets of visual classifications and objective classifications support the conclusion that the observed galaxy counts agree with no-evolution predictions for the elliptical and spiral populations, as reported in Glazebrook et al. (1995MNRAS.275L..19G). A major conclusion is that the large overdensity of merging/ peculiar/ irregular galaxies relative to the predictions of no-evolution models (reported by Glazebrook et al. 1995MNRAS.275L..19G) is confirmed. However, the shape of the faint-end (I&gt;21.0mag) number count relation for peculiar objects is sensitive to the large systematic uncertainties inherent in the visual classification of these objects. Despite this caveat, the frequency of objects showing clear evidence for tidal interactions (e.g., tidal tails) in the HST sample is at least 50% larger than it is among nearby galaxies, at the 2{sigma} level. Relatively few "chain galaxies" are seen among the sample of peculiar objects, suggesting that these systems do not form a large component of the peculiar galaxy population at I&lt;22mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1#2</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/140/327 [1]</TD>
            <TD>Fundamental plane galaxies redshifts (Mueller+, 1999)</TD>
            <TD>Radial velocities and central velocity dispersions are derived for 238 E/S0 galaxies from medium-resolution spectroscopy. New spectroscopic data have been obtained as part of a study of the Fundamental Plane distances and peculiar motions of early-type galaxies in three selected directions of the South Equatorial Strip, undertaken in order to investigate the reality of large-scale streaming motion; results of this study have been reported in Mueller et al. (1998ApJ...507L.105M). The new APM South Equatorial Strip Catalog (-17.5deg&lt;{delta}&lt;+2.5deg) (Raychaudhury &amp; Lynden-Bell, 2000) was used to select the sample of field galaxies in three directions: (1) 15h10-16h10; (2) 20h30-21h50; (3) 00h10-01h30. The spectra obtained have a median S/N per {AA} of 23, an instrumental resolution (FWHM) of ~4{AA}, and the spectrograph resolution (dispersion) is ~100km/s. The Fourier cross-correlation method was used to derive the radial velocities and velocity dispersions. The velocity dispersions have been corrected for the size of the aperture and for the galaxy effective radius. Comparisons of the derived radial velocities with data from the literature show that our values are accurate to 40km/s. A comparison with results from Jorgensen et al. (1995MNRAS.276.1341J) shows that the derived central velocity dispersion have an rms scatter of 0.036 in log{sigma}. There is no offset relative to the velocity dispersions of Davies et al. (1987ApJS...64..581D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327#1</TD>
            <TD>2011-09-14T18:59:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/140/327</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/327</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/140/327 [2]</TD>
            <TD>Fundamental plane galaxies redshifts (Mueller+, 1999)</TD>
            <TD>Radial velocities and central velocity dispersions are derived for 238 E/S0 galaxies from medium-resolution spectroscopy. New spectroscopic data have been obtained as part of a study of the Fundamental Plane distances and peculiar motions of early-type galaxies in three selected directions of the South Equatorial Strip, undertaken in order to investigate the reality of large-scale streaming motion; results of this study have been reported in Mueller et al. (1998ApJ...507L.105M). The new APM South Equatorial Strip Catalog (-17.5deg&lt;{delta}&lt;+2.5deg) (Raychaudhury &amp; Lynden-Bell, 2000) was used to select the sample of field galaxies in three directions: (1) 15h10-16h10; (2) 20h30-21h50; (3) 00h10-01h30. The spectra obtained have a median S/N per {AA} of 23, an instrumental resolution (FWHM) of ~4{AA}, and the spectrograph resolution (dispersion) is ~100km/s. The Fourier cross-correlation method was used to derive the radial velocities and velocity dispersions. The velocity dispersions have been corrected for the size of the aperture and for the galaxy effective radius. Comparisons of the derived radial velocities with data from the literature show that our values are accurate to 40km/s. A comparison with results from Jorgensen et al. (1995MNRAS.276.1341J) shows that the derived central velocity dispersion have an rms scatter of 0.036 in log{sigma}. There is no offset relative to the velocity dispersions of Davies et al. (1987ApJS...64..581D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327#2</TD>
            <TD>2011-09-14T18:59:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/140/327&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/327</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/513 [1]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#1</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/513</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/513 [2]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#2</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/513&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/513 [table2]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#table2</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/513&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/513 [table1]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#table1</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/513&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/107/1 [1]</TD>
            <TD>Morphologies of distant galaxies II (Abraham+ 1996)</TD>
            <TD>The morphological properties of high-redshift galaxies are investigated using a sample of 507 objects (I&lt;22.0mag) from the Hubble Space Telescope (HST) Medium Deep Survey. Independent visual morphological classifications for each galaxy are used to quantify the statistical uncertainties in the galaxy classifications. Visual classifications are found to agree well for I&lt;21mag. Fainter than I=21mag significant disagreements are seen in the independent visual classifications of late-type systems with T&gt;7, merging systems, and peculiar galaxies. The classifications of these systems are shown to be somewhat subjective. Objective classifications based upon measurements of central concentration and asymmetry for the Medium Deep Survey sample are presented. These classifications are calibrated using measurements of structural parameters for an artificially redshifted sample of local objects. Morphologically segregated number counts using both sets of visual classifications and objective classifications support the conclusion that the observed galaxy counts agree with no-evolution predictions for the elliptical and spiral populations, as reported in Glazebrook et al. (1995MNRAS.275L..19G). A major conclusion is that the large overdensity of merging/ peculiar/ irregular galaxies relative to the predictions of no-evolution models (reported by Glazebrook et al. 1995MNRAS.275L..19G) is confirmed. However, the shape of the faint-end (I&gt;21.0mag) number count relation for peculiar objects is sensitive to the large systematic uncertainties inherent in the visual classification of these objects. Despite this caveat, the frequency of objects showing clear evidence for tidal interactions (e.g., tidal tails) in the HST sample is at least 50% larger than it is among nearby galaxies, at the 2{sigma} level. Relatively few "chain galaxies" are seen among the sample of peculiar objects, suggesting that these systems do not form a large component of the peculiar galaxy population at I&lt;22mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1#1</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/107/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/107/1 [2]</TD>
            <TD>Morphologies of distant galaxies II (Abraham+ 1996)</TD>
            <TD>The morphological properties of high-redshift galaxies are investigated using a sample of 507 objects (I&lt;22.0mag) from the Hubble Space Telescope (HST) Medium Deep Survey. Independent visual morphological classifications for each galaxy are used to quantify the statistical uncertainties in the galaxy classifications. Visual classifications are found to agree well for I&lt;21mag. Fainter than I=21mag significant disagreements are seen in the independent visual classifications of late-type systems with T&gt;7, merging systems, and peculiar galaxies. The classifications of these systems are shown to be somewhat subjective. Objective classifications based upon measurements of central concentration and asymmetry for the Medium Deep Survey sample are presented. These classifications are calibrated using measurements of structural parameters for an artificially redshifted sample of local objects. Morphologically segregated number counts using both sets of visual classifications and objective classifications support the conclusion that the observed galaxy counts agree with no-evolution predictions for the elliptical and spiral populations, as reported in Glazebrook et al. (1995MNRAS.275L..19G). A major conclusion is that the large overdensity of merging/ peculiar/ irregular galaxies relative to the predictions of no-evolution models (reported by Glazebrook et al. 1995MNRAS.275L..19G) is confirmed. However, the shape of the faint-end (I&gt;21.0mag) number count relation for peculiar objects is sensitive to the large systematic uncertainties inherent in the visual classification of these objects. Despite this caveat, the frequency of objects showing clear evidence for tidal interactions (e.g., tidal tails) in the HST sample is at least 50% larger than it is among nearby galaxies, at the 2{sigma} level. Relatively few "chain galaxies" are seen among the sample of peculiar objects, suggesting that these systems do not form a large component of the peculiar galaxy population at I&lt;22mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1#2</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Aug-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/107/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/107/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/107/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/140/327 [1]</TD>
            <TD>Fundamental plane galaxies redshifts (Mueller+, 1999)</TD>
            <TD>Radial velocities and central velocity dispersions are derived for 238 E/S0 galaxies from medium-resolution spectroscopy. New spectroscopic data have been obtained as part of a study of the Fundamental Plane distances and peculiar motions of early-type galaxies in three selected directions of the South Equatorial Strip, undertaken in order to investigate the reality of large-scale streaming motion; results of this study have been reported in Mueller et al. (1998ApJ...507L.105M). The new APM South Equatorial Strip Catalog (-17.5deg&lt;{delta}&lt;+2.5deg) (Raychaudhury &amp; Lynden-Bell, 2000) was used to select the sample of field galaxies in three directions: (1) 15h10-16h10; (2) 20h30-21h50; (3) 00h10-01h30. The spectra obtained have a median S/N per {AA} of 23, an instrumental resolution (FWHM) of ~4{AA}, and the spectrograph resolution (dispersion) is ~100km/s. The Fourier cross-correlation method was used to derive the radial velocities and velocity dispersions. The velocity dispersions have been corrected for the size of the aperture and for the galaxy effective radius. Comparisons of the derived radial velocities with data from the literature show that our values are accurate to 40km/s. A comparison with results from Jorgensen et al. (1995MNRAS.276.1341J) shows that the derived central velocity dispersion have an rms scatter of 0.036 in log{sigma}. There is no offset relative to the velocity dispersions of Davies et al. (1987ApJS...64..581D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327#1</TD>
            <TD>2011-09-14T18:59:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/140/327</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/327</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/140/327 [2]</TD>
            <TD>Fundamental plane galaxies redshifts (Mueller+, 1999)</TD>
            <TD>Radial velocities and central velocity dispersions are derived for 238 E/S0 galaxies from medium-resolution spectroscopy. New spectroscopic data have been obtained as part of a study of the Fundamental Plane distances and peculiar motions of early-type galaxies in three selected directions of the South Equatorial Strip, undertaken in order to investigate the reality of large-scale streaming motion; results of this study have been reported in Mueller et al. (1998ApJ...507L.105M). The new APM South Equatorial Strip Catalog (-17.5deg&lt;{delta}&lt;+2.5deg) (Raychaudhury &amp; Lynden-Bell, 2000) was used to select the sample of field galaxies in three directions: (1) 15h10-16h10; (2) 20h30-21h50; (3) 00h10-01h30. The spectra obtained have a median S/N per {AA} of 23, an instrumental resolution (FWHM) of ~4{AA}, and the spectrograph resolution (dispersion) is ~100km/s. The Fourier cross-correlation method was used to derive the radial velocities and velocity dispersions. The velocity dispersions have been corrected for the size of the aperture and for the galaxy effective radius. Comparisons of the derived radial velocities with data from the literature show that our values are accurate to 40km/s. A comparison with results from Jorgensen et al. (1995MNRAS.276.1341J) shows that the derived central velocity dispersion have an rms scatter of 0.036 in log{sigma}. There is no offset relative to the velocity dispersions of Davies et al. (1987ApJS...64..581D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327#2</TD>
            <TD>2011-09-14T18:59:43Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Feb-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/140/327</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/140/327&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/140/327</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/513 [1]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#1</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/513</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/513 [2]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#2</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/513&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/513 [table2]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#table2</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/513&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/513 [table1]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#table1</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/513&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1338 [1]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#1</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1338</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1338 [2]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#2</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1338&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1338 [table6]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#table6</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1338&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1338 [table11]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#table11</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1338&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/513 [1]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#1</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/513</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/513 [2]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#2</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/513&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/513 [table2]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#table2</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/513&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/513 [table1]</TD>
            <TD>Galaxy warps in the HDF North and South (Reshetnikov+, 2002)</TD>
            <TD>We present a statistical study of the presence of galaxy warps in the Hubble deep fields. Among a complete sample of 45 edge-on galaxies above a diameter of 1.3", we find 5 galaxies to be certainly warped and 6 galaxies as good candidates. In addition, 4 galaxies reveal a characteristic U-warp. Compared to statistical studies of local warps, and taking into account the strong bias against observing the outer parts of galaxies at high redshift, these numbers point towards a very high frequency of warps at z~1: almost all galaxy discs might be warped. Furthermore, the amplitude of warps are stronger than for local warps. This is easily interpreted in terms of higher galaxy interactions and matter accretion in the past. This result supports these two mechanisms as the best candidates for the origin of early warps. The mean observed axis ratio of our sample of edge-on galaxies is significantly larger in the high-z sample than is found for samples of local spiral galaxies. This might be due to disk thickening due to more frequent galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513#table1</TD>
            <TD>2011-09-14T19:14:50Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/513</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/513&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/513</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/519/1 [1]</TD>
            <TD>Lyman-break galaxies at z {&gt;~} 4 (Steidel+, 1999)</TD>
            <TD>We present initial results of a survey for star-forming galaxies in the redshift range 3.8{&lt;~}z{&lt;~}4.5. This sample consists of a photometric catalog of 244 galaxies culled from a total solid angle of 0.23 deg^2^ to an apparent magnitude of I_AB_=25.0. Spectroscopic redshifts in the range 3.61{&lt;~}z{&lt;~}4.81 have been obtained for 48 of these galaxies; their median redshift is &lt;z&gt;=4.13. Selecting these galaxies in a manner entirely analogous to our large survey for Lyman-break galaxies at smaller redshift (2.7{&lt;~}z{&lt;~}3.4) allows a relatively clean differential comparison between the populations and integrated luminosity density at these two cosmic epochs. Over the same range of UV luminosity, the spectroscopic properties of the galaxy samples at z{~}4 and z{~}3 are indistinguishable, as are the luminosity function shapes and the total integrated UV luminosity densities [{rho}_UV_(z=3)/{rho}_UV_(z=4)=1.1{+/_}0.3].</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1#1</TD>
            <TD>2011-09-14T19:00:19Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/519/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/519/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/519/1 [2]</TD>
            <TD>Lyman-break galaxies at z {&gt;~} 4 (Steidel+, 1999)</TD>
            <TD>We present initial results of a survey for star-forming galaxies in the redshift range 3.8{&lt;~}z{&lt;~}4.5. This sample consists of a photometric catalog of 244 galaxies culled from a total solid angle of 0.23 deg^2^ to an apparent magnitude of I_AB_=25.0. Spectroscopic redshifts in the range 3.61{&lt;~}z{&lt;~}4.81 have been obtained for 48 of these galaxies; their median redshift is &lt;z&gt;=4.13. Selecting these galaxies in a manner entirely analogous to our large survey for Lyman-break galaxies at smaller redshift (2.7{&lt;~}z{&lt;~}3.4) allows a relatively clean differential comparison between the populations and integrated luminosity density at these two cosmic epochs. Over the same range of UV luminosity, the spectroscopic properties of the galaxy samples at z{~}4 and z{~}3 are indistinguishable, as are the luminosity function shapes and the total integrated UV luminosity densities [{rho}_UV_(z=3)/{rho}_UV_(z=4)=1.1{+/_}0.3].</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1#2</TD>
            <TD>2011-09-14T19:00:19Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/519/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/519/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1338 [1]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#1</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1338</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1338 [2]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#2</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1338&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1338 [table6]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#table6</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1338&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1338 [table11]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#table11</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1338&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/60 [1]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#1</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/60</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/60 [2]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#2</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/60&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table3]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table3</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table2]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table2</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table4]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table4</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table1]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table1</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/519/1 [1]</TD>
            <TD>Lyman-break galaxies at z {&gt;~} 4 (Steidel+, 1999)</TD>
            <TD>We present initial results of a survey for star-forming galaxies in the redshift range 3.8{&lt;~}z{&lt;~}4.5. This sample consists of a photometric catalog of 244 galaxies culled from a total solid angle of 0.23 deg^2^ to an apparent magnitude of I_AB_=25.0. Spectroscopic redshifts in the range 3.61{&lt;~}z{&lt;~}4.81 have been obtained for 48 of these galaxies; their median redshift is &lt;z&gt;=4.13. Selecting these galaxies in a manner entirely analogous to our large survey for Lyman-break galaxies at smaller redshift (2.7{&lt;~}z{&lt;~}3.4) allows a relatively clean differential comparison between the populations and integrated luminosity density at these two cosmic epochs. Over the same range of UV luminosity, the spectroscopic properties of the galaxy samples at z{~}4 and z{~}3 are indistinguishable, as are the luminosity function shapes and the total integrated UV luminosity densities [{rho}_UV_(z=3)/{rho}_UV_(z=4)=1.1{+/_}0.3].</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1#1</TD>
            <TD>2011-09-14T19:00:19Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/519/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/519/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/519/1 [2]</TD>
            <TD>Lyman-break galaxies at z {&gt;~} 4 (Steidel+, 1999)</TD>
            <TD>We present initial results of a survey for star-forming galaxies in the redshift range 3.8{&lt;~}z{&lt;~}4.5. This sample consists of a photometric catalog of 244 galaxies culled from a total solid angle of 0.23 deg^2^ to an apparent magnitude of I_AB_=25.0. Spectroscopic redshifts in the range 3.61{&lt;~}z{&lt;~}4.81 have been obtained for 48 of these galaxies; their median redshift is &lt;z&gt;=4.13. Selecting these galaxies in a manner entirely analogous to our large survey for Lyman-break galaxies at smaller redshift (2.7{&lt;~}z{&lt;~}3.4) allows a relatively clean differential comparison between the populations and integrated luminosity density at these two cosmic epochs. Over the same range of UV luminosity, the spectroscopic properties of the galaxy samples at z{~}4 and z{~}3 are indistinguishable, as are the luminosity function shapes and the total integrated UV luminosity densities [{rho}_UV_(z=3)/{rho}_UV_(z=4)=1.1{+/_}0.3].</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1#2</TD>
            <TD>2011-09-14T19:00:19Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/519/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/519/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1338 [1]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#1</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1338</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1338 [2]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#2</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1338&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1338 [table6]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#table6</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1338&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1338 [table11]</TD>
            <TD>UV-selected stars in Tau and Upper Sco (Findeisen+, 2010)</TD>
            <TD>We have carried out a Galaxy Evolution Explorer (GALEX) Cycle 1 guest investigator program covering 56deg^2^ near the Taurus T association and 12deg^2^ along the northern edge of the Upper Scorpius OB association. We combined photometry in the GALEX far-ultraviolet and near-ultraviolet bands with data from the Two Micron All Sky Survey to identify candidate young (&lt;~100Myr old) stars as those with an ultraviolet excess relative to older main-sequence stars. Follow-up spectroscopy of a partial sample of these candidates suggests five new members of Taurus, with 8-20 expected from additional observations, and five new members of Upper Scorpius, with three to six expected from additional observations.</TD>
            <TD>CDS</TD>
            <TD>#UV#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338#table11</TD>
            <TD>2012-09-11T14:05:48Z</TD>
            <TD>#Associations#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1338</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1338&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1338</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/60 [1]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#1</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/60</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/60 [2]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#2</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/60&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table3]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table3</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table2]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table2</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table4]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table4</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table1]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table1</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/519/1 [1]</TD>
            <TD>Lyman-break galaxies at z {&gt;~} 4 (Steidel+, 1999)</TD>
            <TD>We present initial results of a survey for star-forming galaxies in the redshift range 3.8{&lt;~}z{&lt;~}4.5. This sample consists of a photometric catalog of 244 galaxies culled from a total solid angle of 0.23 deg^2^ to an apparent magnitude of I_AB_=25.0. Spectroscopic redshifts in the range 3.61{&lt;~}z{&lt;~}4.81 have been obtained for 48 of these galaxies; their median redshift is &lt;z&gt;=4.13. Selecting these galaxies in a manner entirely analogous to our large survey for Lyman-break galaxies at smaller redshift (2.7{&lt;~}z{&lt;~}3.4) allows a relatively clean differential comparison between the populations and integrated luminosity density at these two cosmic epochs. Over the same range of UV luminosity, the spectroscopic properties of the galaxy samples at z{~}4 and z{~}3 are indistinguishable, as are the luminosity function shapes and the total integrated UV luminosity densities [{rho}_UV_(z=3)/{rho}_UV_(z=4)=1.1{+/_}0.3].</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1#1</TD>
            <TD>2011-09-14T19:00:19Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/519/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/519/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/519/1 [2]</TD>
            <TD>Lyman-break galaxies at z {&gt;~} 4 (Steidel+, 1999)</TD>
            <TD>We present initial results of a survey for star-forming galaxies in the redshift range 3.8{&lt;~}z{&lt;~}4.5. This sample consists of a photometric catalog of 244 galaxies culled from a total solid angle of 0.23 deg^2^ to an apparent magnitude of I_AB_=25.0. Spectroscopic redshifts in the range 3.61{&lt;~}z{&lt;~}4.81 have been obtained for 48 of these galaxies; their median redshift is &lt;z&gt;=4.13. Selecting these galaxies in a manner entirely analogous to our large survey for Lyman-break galaxies at smaller redshift (2.7{&lt;~}z{&lt;~}3.4) allows a relatively clean differential comparison between the populations and integrated luminosity density at these two cosmic epochs. Over the same range of UV luminosity, the spectroscopic properties of the galaxy samples at z{~}4 and z{~}3 are indistinguishable, as are the luminosity function shapes and the total integrated UV luminosity densities [{rho}_UV_(z=3)/{rho}_UV_(z=4)=1.1{+/_}0.3].</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1#2</TD>
            <TD>2011-09-14T19:00:19Z</TD>
            <TD>#Photometry#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/519/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/519/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/519/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/547/A65 [1]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#1</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/547/A65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/547/A65 [2]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#2</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/547/A65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/547/A65 [galaxies]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#galaxies</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/547/A65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/547/A65 [table1]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#table1</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/547/A65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/60 [1]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#1</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/60</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/60 [2]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#2</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/60&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table3]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table3</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table2]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table2</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table4]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table4</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/382/60 [table1]</TD>
            <TD>BVR photometry in Abell 1689 (Duc+, 2002)</TD>
            <TD>At a redshift of 0.18, Abell 1689 is so far the most distant cluster of galaxies for which substantial mid-infrared (MIR) data have been published. Its mapping with the ISOCAM camera onboard the ISO satellite allowed the detection of 30 cluster members at 6.75{mu}m (LW2 filter) and 16 cluster members at 15{mu}m (LW3 filter) within a clustercentric radius of 0.5Mpc (Fadda et al., 2000A&amp;A...361..827F, Paper I). We present here the follow-up optical photometric and spectroscopic observations which were used to study the individual properties of the galaxy members of A1689. We confirm the high fraction of blue galaxies initially reported in this rich cluster by Butcher &amp; Oemler (1984ApJ...285..426B), that was challenged by some subsequent studies. We discuss the spectral and morphological properties of all cluster members in our spectroscopic sample, and of the MIR-detected galaxies in particular.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60#table1</TD>
            <TD>2011-09-14T19:14:51Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/60</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/382/60&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/60</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/236/207 [1]</TD>
            <TD>Galaxy redshift catalogue (Metcalfe+, 1989)</TD>
            <TD>We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207#1</TD>
            <TD>2011-09-14T19:00:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/236/207</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/236/207</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/236/207 [2]</TD>
            <TD>Galaxy redshift catalogue (Metcalfe+, 1989)</TD>
            <TD>We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207#2</TD>
            <TD>2011-09-14T19:00:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/236/207&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/236/207</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/236/207 [table5]</TD>
            <TD>Galaxy redshift catalogue (Metcalfe+, 1989)</TD>
            <TD>We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207#table5</TD>
            <TD>2011-09-14T19:00:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/236/207&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/236/207</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/547/A65 [1]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#1</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/547/A65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/547/A65 [2]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#2</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/547/A65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/547/A65 [galaxies]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#galaxies</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/547/A65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/547/A65 [table1]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#table1</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/547/A65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/386/140 [1]</TD>
            <TD>HI survey of polar ring galaxies. IV. (van Driel+, 2002)</TD>
            <TD>A total of 33 polar ring galaxies and polar ring galaxy candidates were observed in the 21-cm HI line with the 64-m Parkes radio telescope. The objects, selected by their optical morphology, are all south of declination -39{deg} and in only 5 of them had been reported previously. HI line emission was detected towards 18 objects, though in 3 cases the detection may be confused by another galaxy in the telescope beam, and one is a marginal detection. Eight objects were detected for the first time in HI, of which 5 did not have previously known redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140#1</TD>
            <TD>2011-09-14T19:15:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/386/140</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/386/140</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/386/140 [2]</TD>
            <TD>HI survey of polar ring galaxies. IV. (van Driel+, 2002)</TD>
            <TD>A total of 33 polar ring galaxies and polar ring galaxy candidates were observed in the 21-cm HI line with the 64-m Parkes radio telescope. The objects, selected by their optical morphology, are all south of declination -39{deg} and in only 5 of them had been reported previously. HI line emission was detected towards 18 objects, though in 3 cases the detection may be confused by another galaxy in the telescope beam, and one is a marginal detection. Eight objects were detected for the first time in HI, of which 5 did not have previously known redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140#2</TD>
            <TD>2011-09-14T19:15:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/386/140&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/386/140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/386/140 [table1]</TD>
            <TD>HI survey of polar ring galaxies. IV. (van Driel+, 2002)</TD>
            <TD>A total of 33 polar ring galaxies and polar ring galaxy candidates were observed in the 21-cm HI line with the 64-m Parkes radio telescope. The objects, selected by their optical morphology, are all south of declination -39{deg} and in only 5 of them had been reported previously. HI line emission was detected towards 18 objects, though in 3 cases the detection may be confused by another galaxy in the telescope beam, and one is a marginal detection. Eight objects were detected for the first time in HI, of which 5 did not have previously known redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140#table1</TD>
            <TD>2011-09-14T19:15:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/386/140&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/386/140</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/547/A65 [1]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#1</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/547/A65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/547/A65 [2]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#2</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/547/A65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/547/A65 [galaxies]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#galaxies</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/547/A65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/547/A65 [table1]</TD>
            <TD>Extended stellar objects in galaxies (Bruens+, 2012)</TD>
            <TD>The table contains the catalog of the 813 EOs presented in this paper. For each EO, a running number, the designation of EO in this paper (name of galaxy + EO + number), an alternative name or designation in a previous paper, the effective radius of the EO, the absolute V-band luminosity of the EO, the projected distance to the host galaxy (for the Milky Way the galactocentric distance is used), and the references to the publications are given in the catalog.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65#table1</TD>
            <TD>2012-10-31T09:24:52Z</TD>
            <TD>#Associations#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/547/A65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/547/A65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/547/A65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/236/207 [1]</TD>
            <TD>Galaxy redshift catalogue (Metcalfe+, 1989)</TD>
            <TD>We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207#1</TD>
            <TD>2011-09-14T19:00:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/236/207</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/236/207</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/236/207 [2]</TD>
            <TD>Galaxy redshift catalogue (Metcalfe+, 1989)</TD>
            <TD>We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207#2</TD>
            <TD>2011-09-14T19:00:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/236/207&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/236/207</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/236/207 [table5]</TD>
            <TD>Galaxy redshift catalogue (Metcalfe+, 1989)</TD>
            <TD>We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207#table5</TD>
            <TD>2011-09-14T19:00:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/236/207&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/236/207</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/386/140 [1]</TD>
            <TD>HI survey of polar ring galaxies. IV. (van Driel+, 2002)</TD>
            <TD>A total of 33 polar ring galaxies and polar ring galaxy candidates were observed in the 21-cm HI line with the 64-m Parkes radio telescope. The objects, selected by their optical morphology, are all south of declination -39{deg} and in only 5 of them had been reported previously. HI line emission was detected towards 18 objects, though in 3 cases the detection may be confused by another galaxy in the telescope beam, and one is a marginal detection. Eight objects were detected for the first time in HI, of which 5 did not have previously known redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140#1</TD>
            <TD>2011-09-14T19:15:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/386/140</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/386/140</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/386/140 [2]</TD>
            <TD>HI survey of polar ring galaxies. IV. (van Driel+, 2002)</TD>
            <TD>A total of 33 polar ring galaxies and polar ring galaxy candidates were observed in the 21-cm HI line with the 64-m Parkes radio telescope. The objects, selected by their optical morphology, are all south of declination -39{deg} and in only 5 of them had been reported previously. HI line emission was detected towards 18 objects, though in 3 cases the detection may be confused by another galaxy in the telescope beam, and one is a marginal detection. Eight objects were detected for the first time in HI, of which 5 did not have previously known redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140#2</TD>
            <TD>2011-09-14T19:15:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/386/140&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/386/140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/386/140 [table1]</TD>
            <TD>HI survey of polar ring galaxies. IV. (van Driel+, 2002)</TD>
            <TD>A total of 33 polar ring galaxies and polar ring galaxy candidates were observed in the 21-cm HI line with the 64-m Parkes radio telescope. The objects, selected by their optical morphology, are all south of declination -39{deg} and in only 5 of them had been reported previously. HI line emission was detected towards 18 objects, though in 3 cases the detection may be confused by another galaxy in the telescope beam, and one is a marginal detection. Eight objects were detected for the first time in HI, of which 5 did not have previously known redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140#table1</TD>
            <TD>2011-09-14T19:15:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/386/140&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/386/140</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/712/1259 [1]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#1</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/712/1259</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/712/1259 [2]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#2</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/712/1259&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/712/1259 [table4]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#table4</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/712/1259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/712/1259 [table5]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#table5</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/712/1259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/236/207 [1]</TD>
            <TD>Galaxy redshift catalogue (Metcalfe+, 1989)</TD>
            <TD>We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207#1</TD>
            <TD>2011-09-14T19:00:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/236/207</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/236/207</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/236/207 [2]</TD>
            <TD>Galaxy redshift catalogue (Metcalfe+, 1989)</TD>
            <TD>We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207#2</TD>
            <TD>2011-09-14T19:00:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/236/207&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/236/207</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/236/207 [table5]</TD>
            <TD>Galaxy redshift catalogue (Metcalfe+, 1989)</TD>
            <TD>We present redshifts and blue magnitudes for a sample of 264 'field' galaxies virtually complete to a limiting magnitude of bj~=16.80mag. The galaxies were selected by sampling one galaxy in every three in order of apparent magnitude on each of nine high-latitude UK Schmidt (UKST) fields. Photometric data were provided by COSMOS machine measures of UKST plates, zero-pointed with CCD photometry. The spectral data came from observations with the 1.9-m telescope at the South African Astronomical Observatory (SAAO), and the resulting radial velocities have a precision of ~+/-130km/s. This survey augments substantially the Durham/AAT redshift survey. In this paper we discuss the observational techniques and reduction procedures.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207#table5</TD>
            <TD>2011-09-14T19:00:59Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Oct-1996</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/236/207</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/236/207&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/236/207</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/386/140 [1]</TD>
            <TD>HI survey of polar ring galaxies. IV. (van Driel+, 2002)</TD>
            <TD>A total of 33 polar ring galaxies and polar ring galaxy candidates were observed in the 21-cm HI line with the 64-m Parkes radio telescope. The objects, selected by their optical morphology, are all south of declination -39{deg} and in only 5 of them had been reported previously. HI line emission was detected towards 18 objects, though in 3 cases the detection may be confused by another galaxy in the telescope beam, and one is a marginal detection. Eight objects were detected for the first time in HI, of which 5 did not have previously known redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140#1</TD>
            <TD>2011-09-14T19:15:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/386/140</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/386/140</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/386/140 [2]</TD>
            <TD>HI survey of polar ring galaxies. IV. (van Driel+, 2002)</TD>
            <TD>A total of 33 polar ring galaxies and polar ring galaxy candidates were observed in the 21-cm HI line with the 64-m Parkes radio telescope. The objects, selected by their optical morphology, are all south of declination -39{deg} and in only 5 of them had been reported previously. HI line emission was detected towards 18 objects, though in 3 cases the detection may be confused by another galaxy in the telescope beam, and one is a marginal detection. Eight objects were detected for the first time in HI, of which 5 did not have previously known redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140#2</TD>
            <TD>2011-09-14T19:15:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/386/140&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/386/140</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/386/140 [table1]</TD>
            <TD>HI survey of polar ring galaxies. IV. (van Driel+, 2002)</TD>
            <TD>A total of 33 polar ring galaxies and polar ring galaxy candidates were observed in the 21-cm HI line with the 64-m Parkes radio telescope. The objects, selected by their optical morphology, are all south of declination -39{deg} and in only 5 of them had been reported previously. HI line emission was detected towards 18 objects, though in 3 cases the detection may be confused by another galaxy in the telescope beam, and one is a marginal detection. Eight objects were detected for the first time in HI, of which 5 did not have previously known redshifts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140#table1</TD>
            <TD>2011-09-14T19:15:05Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/386/140</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/386/140&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/386/140</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/712/1259 [1]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#1</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/712/1259</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/712/1259 [2]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#2</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/712/1259&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/712/1259 [table4]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#table4</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/712/1259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/712/1259 [table5]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#table5</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/712/1259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/2757 [1]</TD>
            <TD>Surface photometry of NGC 5907 (Zheng+, 1999)</TD>
            <TD>Intrigued by the initial report of an extended luminosity distribution perpendicular to the disk of the edge-on Sc galaxy NGC 5907, we have obtained very deep exposures of this galaxy with a Schmidt telescope, large-format CCD, and intermediate-band filters centered at 6660 {AA} and 8020 {AA}. These two filters, part of a 15-filter set, are custom designed to avoid the brightest (and most variable) night skylines. As a result, our images are able to go deeper with lower sky noise than those taken with broadband filters at similar effective wavelengths: e.g., 0.6 e^-^ arcsec^-2^ s^-1^ for our observations versus 7.4 e^-^ arcsec^-2^ s-1 for the R-band measures of Morrison et al. (1994AJ....108.1191M). In our assessment of both random and systematic errors, we show that the flux level where the errors of observation reach 1 mag arcsec^-2^ are 29.00 mag arcsec^-2^ in the 6660 {AA} image (corresponding to 28.7 in the R band) and 27.4 mag arcsec^-2^ in the 8020 {AA} image (essentially on the I-band system)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2757#1</TD>
            <TD>2011-09-14T19:01:08Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2757</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/2757</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2757</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/2757 [2]</TD>
            <TD>Surface photometry of NGC 5907 (Zheng+, 1999)</TD>
            <TD>Intrigued by the initial report of an extended luminosity distribution perpendicular to the disk of the edge-on Sc galaxy NGC 5907, we have obtained very deep exposures of this galaxy with a Schmidt telescope, large-format CCD, and intermediate-band filters centered at 6660 {AA} and 8020 {AA}. These two filters, part of a 15-filter set, are custom designed to avoid the brightest (and most variable) night skylines. As a result, our images are able to go deeper with lower sky noise than those taken with broadband filters at similar effective wavelengths: e.g., 0.6 e^-^ arcsec^-2^ s^-1^ for our observations versus 7.4 e^-^ arcsec^-2^ s-1 for the R-band measures of Morrison et al. (1994AJ....108.1191M). In our assessment of both random and systematic errors, we show that the flux level where the errors of observation reach 1 mag arcsec^-2^ are 29.00 mag arcsec^-2^ in the 6660 {AA} image (corresponding to 28.7 in the R band) and 27.4 mag arcsec^-2^ in the 8020 {AA} image (essentially on the I-band system)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2757#2</TD>
            <TD>2011-09-14T19:01:08Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2757</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/2757&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2757</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/559/606 [1]</TD>
            <TD>Star formation in spectroscopic survey (Carter+, 2001)</TD>
            <TD>The 15R-North galaxy redshift survey is a uniform spectroscopic survey (S/N~10) covering the range 3650-7400{AA} for 3149 galaxies with median redshift 0.05. The sample is 90% complete to R=15.4. The median slit covering fraction is 24% of the galaxy, apparently sufficient to minimize the effects of aperture bias on the EW(H{alpha}). Forty-nine percent of the galaxies in the survey have one or more emission lines detected at &gt;=2{sigma}. In agreement with previous surveys, the fraction of absorption-line galaxies increases steeply with galaxy luminosity. We use H{beta}, [O III], H{alpha}, and [N II] to discriminate between star-forming galaxies and AGNs. At least 20% of the galaxies are star-forming, at least 17% have AGN-like emission, and 12% have unclassifiable emission. The data for the entire survey will appear in Geller et al. 2002, in preparation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606#1</TD>
            <TD>2011-09-14T19:15:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/559/606</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/559/606</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/559/606 [2]</TD>
            <TD>Star formation in spectroscopic survey (Carter+, 2001)</TD>
            <TD>The 15R-North galaxy redshift survey is a uniform spectroscopic survey (S/N~10) covering the range 3650-7400{AA} for 3149 galaxies with median redshift 0.05. The sample is 90% complete to R=15.4. The median slit covering fraction is 24% of the galaxy, apparently sufficient to minimize the effects of aperture bias on the EW(H{alpha}). Forty-nine percent of the galaxies in the survey have one or more emission lines detected at &gt;=2{sigma}. In agreement with previous surveys, the fraction of absorption-line galaxies increases steeply with galaxy luminosity. We use H{beta}, [O III], H{alpha}, and [N II] to discriminate between star-forming galaxies and AGNs. At least 20% of the galaxies are star-forming, at least 17% have AGN-like emission, and 12% have unclassifiable emission. The data for the entire survey will appear in Geller et al. 2002, in preparation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606#2</TD>
            <TD>2011-09-14T19:15:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/559/606&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/559/606</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/559/606 [table3]</TD>
            <TD>Star formation in spectroscopic survey (Carter+, 2001)</TD>
            <TD>The 15R-North galaxy redshift survey is a uniform spectroscopic survey (S/N~10) covering the range 3650-7400{AA} for 3149 galaxies with median redshift 0.05. The sample is 90% complete to R=15.4. The median slit covering fraction is 24% of the galaxy, apparently sufficient to minimize the effects of aperture bias on the EW(H{alpha}). Forty-nine percent of the galaxies in the survey have one or more emission lines detected at &gt;=2{sigma}. In agreement with previous surveys, the fraction of absorption-line galaxies increases steeply with galaxy luminosity. We use H{beta}, [O III], H{alpha}, and [N II] to discriminate between star-forming galaxies and AGNs. At least 20% of the galaxies are star-forming, at least 17% have AGN-like emission, and 12% have unclassifiable emission. The data for the entire survey will appear in Geller et al. 2002, in preparation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606#table3</TD>
            <TD>2011-09-14T19:15:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/559/606&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/559/606</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/712/1259 [1]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#1</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/712/1259</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/712/1259 [2]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#2</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/712/1259&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/712/1259 [table4]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#table4</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/712/1259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/712/1259 [table5]</TD>
            <TD>LCID project. II. Variables in IC1613 (Bernard+, 2010)</TD>
            <TD>This work is based on observations obtained with the ACS onboard the HST of a field located about 5' west of the center of IC 1613. 24 HST orbits were devoted to this galaxy. These were collected over about 2.4 consecutive days between 2006 August 28 and 30 in F475W and F814W.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259#table5</TD>
            <TD>2012-11-06T13:16:28Z</TD>
            <TD>#Binaries:eclipsing#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/712/1259</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/712/1259&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/712/1259</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/2757 [1]</TD>
            <TD>Surface photometry of NGC 5907 (Zheng+, 1999)</TD>
            <TD>Intrigued by the initial report of an extended luminosity distribution perpendicular to the disk of the edge-on Sc galaxy NGC 5907, we have obtained very deep exposures of this galaxy with a Schmidt telescope, large-format CCD, and intermediate-band filters centered at 6660 {AA} and 8020 {AA}. These two filters, part of a 15-filter set, are custom designed to avoid the brightest (and most variable) night skylines. As a result, our images are able to go deeper with lower sky noise than those taken with broadband filters at similar effective wavelengths: e.g., 0.6 e^-^ arcsec^-2^ s^-1^ for our observations versus 7.4 e^-^ arcsec^-2^ s-1 for the R-band measures of Morrison et al. (1994AJ....108.1191M). In our assessment of both random and systematic errors, we show that the flux level where the errors of observation reach 1 mag arcsec^-2^ are 29.00 mag arcsec^-2^ in the 6660 {AA} image (corresponding to 28.7 in the R band) and 27.4 mag arcsec^-2^ in the 8020 {AA} image (essentially on the I-band system)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2757#1</TD>
            <TD>2011-09-14T19:01:08Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2757</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/2757</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2757</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/2757 [2]</TD>
            <TD>Surface photometry of NGC 5907 (Zheng+, 1999)</TD>
            <TD>Intrigued by the initial report of an extended luminosity distribution perpendicular to the disk of the edge-on Sc galaxy NGC 5907, we have obtained very deep exposures of this galaxy with a Schmidt telescope, large-format CCD, and intermediate-band filters centered at 6660 {AA} and 8020 {AA}. These two filters, part of a 15-filter set, are custom designed to avoid the brightest (and most variable) night skylines. As a result, our images are able to go deeper with lower sky noise than those taken with broadband filters at similar effective wavelengths: e.g., 0.6 e^-^ arcsec^-2^ s^-1^ for our observations versus 7.4 e^-^ arcsec^-2^ s-1 for the R-band measures of Morrison et al. (1994AJ....108.1191M). In our assessment of both random and systematic errors, we show that the flux level where the errors of observation reach 1 mag arcsec^-2^ are 29.00 mag arcsec^-2^ in the 6660 {AA} image (corresponding to 28.7 in the R band) and 27.4 mag arcsec^-2^ in the 8020 {AA} image (essentially on the I-band system)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2757#2</TD>
            <TD>2011-09-14T19:01:08Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Apr-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/2757</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/2757&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/2757</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/559/606 [1]</TD>
            <TD>Star formation in spectroscopic survey (Carter+, 2001)</TD>
            <TD>The 15R-North galaxy redshift survey is a uniform spectroscopic survey (S/N~10) covering the range 3650-7400{AA} for 3149 galaxies with median redshift 0.05. The sample is 90% complete to R=15.4. The median slit covering fraction is 24% of the galaxy, apparently sufficient to minimize the effects of aperture bias on the EW(H{alpha}). Forty-nine percent of the galaxies in the survey have one or more emission lines detected at &gt;=2{sigma}. In agreement with previous surveys, the fraction of absorption-line galaxies increases steeply with galaxy luminosity. We use H{beta}, [O III], H{alpha}, and [N II] to discriminate between star-forming galaxies and AGNs. At least 20% of the galaxies are star-forming, at least 17% have AGN-like emission, and 12% have unclassifiable emission. The data for the entire survey will appear in Geller et al. 2002, in preparation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606#1</TD>
            <TD>2011-09-14T19:15:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/559/606</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/559/606</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/559/606 [2]</TD>
            <TD>Star formation in spectroscopic survey (Carter+, 2001)</TD>
            <TD>The 15R-North galaxy redshift survey is a uniform spectroscopic survey (S/N~10) covering the range 3650-7400{AA} for 3149 galaxies with median redshift 0.05. The sample is 90% complete to R=15.4. The median slit covering fraction is 24% of the galaxy, apparently sufficient to minimize the effects of aperture bias on the EW(H{alpha}). Forty-nine percent of the galaxies in the survey have one or more emission lines detected at &gt;=2{sigma}. In agreement with previous surveys, the fraction of absorption-line galaxies increases steeply with galaxy luminosity. We use H{beta}, [O III], H{alpha}, and [N II] to discriminate between star-forming galaxies and AGNs. At least 20% of the galaxies are star-forming, at least 17% have AGN-like emission, and 12% have unclassifiable emission. The data for the entire survey will appear in Geller et al. 2002, in preparation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606#2</TD>
            <TD>2011-09-14T19:15:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/559/606&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/559/606</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/559/606 [table3]</TD>
            <TD>Star formation in spectroscopic survey (Carter+, 2001)</TD>
            <TD>The 15R-North galaxy redshift survey is a uniform spectroscopic survey (S/N~10) covering the range 3650-7400{AA} for 3149 galaxies with median redshift 0.05. The sample is 90% complete to R=15.4. The median slit covering fraction is 24% of the galaxy, apparently sufficient to minimize the effects of aperture bias on the EW(H{alpha}). Forty-nine percent of the galaxies in the survey have one or more emission lines detected at &gt;=2{sigma}. In agreement with previous surveys, the fraction of absorption-line galaxies increases steeply with galaxy luminosity. We use H{beta}, [O III], H{alpha}, and [N II] to discriminate between star-forming galaxies and AGNs. At least 20% of the galaxies are star-forming, at least 17% have AGN-like emission, and 12% have unclassifiable emission. The data for the entire survey will appear in Geller et al. 2002, in preparation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606#table3</TD>
            <TD>2011-09-14T19:15:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/559/606&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/559/606</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/89/674 [1]</TD>
            <TD>Open clusters non-stationarity parameter (Danilov+, 2012)</TD>
            <TD>{alpha}_0_ - is the mean value of a virial factor, {delta}{alpha}-is the amplitude of virial factor oscillations, {nu}={rho}_c_/{rho}_0_-is the density contrast ({rho}_c_ - is the mean density of a cluster core, {rho}_0_ - is the cluster centre density), N_K_/N - is the ratio of the stars number in a cluster received by King's distribution and by stellar counts, P_1_-is the period of cluster core oscillations, P_2_ - is the period of cluster oscillations, {delta}R_1_/R_10_-is the relative amplitude of core radius oscillations, {lambda}={sigma}/{sigma}_iz_, {sigma}_iz_^2^ - is the velocity dispersion of an isolated virialized cluster, {sigma}^2^, {sigma}_1_^2^, {sigma}_2_^2^ - are the velocity dispersions of nonisolated nonsteady clusters with spherical halo; with ellipsoidal halo elongated to the centre of Galaxy; with ellipsoidal halo elongated to the direction of cluster motion correspondingly. Errors of values {alpha}_0_, {delta}{alpha}, {delta}R_1_/R_10_, P_1_ have been estimated by the assumption of the normal distribution of the values M (the mass of a cluster), R_2_ (the radius of a cluster), {xi} (the ratio of core radius to halo radius), {mu} (the ratio of core mass to halo mass). Assuming a deviation of one of the four values equal to zero we receive four sections of 1{sigma}-errors ellipsoid. These sections are the spheres of radius 2^0.5^. Taking points on each sphere with the step 0.25*{pi} on angular coordinates we receive 96 points on a surface of the 1{sigma}-errors ellipsoid. The values {alpha}_0_, {delta}{alpha}, {delta}R_1_/R_10_, P_1_ were calculated in the 96 points. The centre of the ellipsoidal was used for calculation of the mean values. The errors of the values were computed as root-mean-squire deviations of 96 values from the same mean values. The errors of the others values of the catalog were computed by the errors calculation rule of indirect measuring.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/89/674#1</TD>
            <TD>2012-12-11T07:10:03Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/AZh/89/674</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/89/674</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/89/674</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/89/674 [2]</TD>
            <TD>Open clusters non-stationarity parameter (Danilov+, 2012)</TD>
            <TD>{alpha}_0_ - is the mean value of a virial factor, {delta}{alpha}-is the amplitude of virial factor oscillations, {nu}={rho}_c_/{rho}_0_-is the density contrast ({rho}_c_ - is the mean density of a cluster core, {rho}_0_ - is the cluster centre density), N_K_/N - is the ratio of the stars number in a cluster received by King's distribution and by stellar counts, P_1_-is the period of cluster core oscillations, P_2_ - is the period of cluster oscillations, {delta}R_1_/R_10_-is the relative amplitude of core radius oscillations, {lambda}={sigma}/{sigma}_iz_, {sigma}_iz_^2^ - is the velocity dispersion of an isolated virialized cluster, {sigma}^2^, {sigma}_1_^2^, {sigma}_2_^2^ - are the velocity dispersions of nonisolated nonsteady clusters with spherical halo; with ellipsoidal halo elongated to the centre of Galaxy; with ellipsoidal halo elongated to the direction of cluster motion correspondingly. Errors of values {alpha}_0_, {delta}{alpha}, {delta}R_1_/R_10_, P_1_ have been estimated by the assumption of the normal distribution of the values M (the mass of a cluster), R_2_ (the radius of a cluster), {xi} (the ratio of core radius to halo radius), {mu} (the ratio of core mass to halo mass). Assuming a deviation of one of the four values equal to zero we receive four sections of 1{sigma}-errors ellipsoid. These sections are the spheres of radius 2^0.5^. Taking points on each sphere with the step 0.25*{pi} on angular coordinates we receive 96 points on a surface of the 1{sigma}-errors ellipsoid. The values {alpha}_0_, {delta}{alpha}, {delta}R_1_/R_10_, P_1_ were calculated in the 96 points. The centre of the ellipsoidal was used for calculation of the mean values. The errors of the values were computed as root-mean-squire deviations of 96 values from the same mean values. The errors of the others values of the catalog were computed by the errors calculation rule of indirect measuring.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/89/674#2</TD>
            <TD>2012-12-11T07:10:03Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/AZh/89/674</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/89/674&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/89/674</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/1095 [1]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#1</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/1095</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/1095 [2]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#2</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/1095&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/1095 [table4]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#table4</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/1095&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/1095 [table2]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#table2</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/1095&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/89/674 [1]</TD>
            <TD>Open clusters non-stationarity parameter (Danilov+, 2012)</TD>
            <TD>{alpha}_0_ - is the mean value of a virial factor, {delta}{alpha}-is the amplitude of virial factor oscillations, {nu}={rho}_c_/{rho}_0_-is the density contrast ({rho}_c_ - is the mean density of a cluster core, {rho}_0_ - is the cluster centre density), N_K_/N - is the ratio of the stars number in a cluster received by King's distribution and by stellar counts, P_1_-is the period of cluster core oscillations, P_2_ - is the period of cluster oscillations, {delta}R_1_/R_10_-is the relative amplitude of core radius oscillations, {lambda}={sigma}/{sigma}_iz_, {sigma}_iz_^2^ - is the velocity dispersion of an isolated virialized cluster, {sigma}^2^, {sigma}_1_^2^, {sigma}_2_^2^ - are the velocity dispersions of nonisolated nonsteady clusters with spherical halo; with ellipsoidal halo elongated to the centre of Galaxy; with ellipsoidal halo elongated to the direction of cluster motion correspondingly. Errors of values {alpha}_0_, {delta}{alpha}, {delta}R_1_/R_10_, P_1_ have been estimated by the assumption of the normal distribution of the values M (the mass of a cluster), R_2_ (the radius of a cluster), {xi} (the ratio of core radius to halo radius), {mu} (the ratio of core mass to halo mass). Assuming a deviation of one of the four values equal to zero we receive four sections of 1{sigma}-errors ellipsoid. These sections are the spheres of radius 2^0.5^. Taking points on each sphere with the step 0.25*{pi} on angular coordinates we receive 96 points on a surface of the 1{sigma}-errors ellipsoid. The values {alpha}_0_, {delta}{alpha}, {delta}R_1_/R_10_, P_1_ were calculated in the 96 points. The centre of the ellipsoidal was used for calculation of the mean values. The errors of the values were computed as root-mean-squire deviations of 96 values from the same mean values. The errors of the others values of the catalog were computed by the errors calculation rule of indirect measuring.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/89/674#1</TD>
            <TD>2012-12-11T07:10:03Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/AZh/89/674</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/89/674</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/89/674</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/89/674 [2]</TD>
            <TD>Open clusters non-stationarity parameter (Danilov+, 2012)</TD>
            <TD>{alpha}_0_ - is the mean value of a virial factor, {delta}{alpha}-is the amplitude of virial factor oscillations, {nu}={rho}_c_/{rho}_0_-is the density contrast ({rho}_c_ - is the mean density of a cluster core, {rho}_0_ - is the cluster centre density), N_K_/N - is the ratio of the stars number in a cluster received by King's distribution and by stellar counts, P_1_-is the period of cluster core oscillations, P_2_ - is the period of cluster oscillations, {delta}R_1_/R_10_-is the relative amplitude of core radius oscillations, {lambda}={sigma}/{sigma}_iz_, {sigma}_iz_^2^ - is the velocity dispersion of an isolated virialized cluster, {sigma}^2^, {sigma}_1_^2^, {sigma}_2_^2^ - are the velocity dispersions of nonisolated nonsteady clusters with spherical halo; with ellipsoidal halo elongated to the centre of Galaxy; with ellipsoidal halo elongated to the direction of cluster motion correspondingly. Errors of values {alpha}_0_, {delta}{alpha}, {delta}R_1_/R_10_, P_1_ have been estimated by the assumption of the normal distribution of the values M (the mass of a cluster), R_2_ (the radius of a cluster), {xi} (the ratio of core radius to halo radius), {mu} (the ratio of core mass to halo mass). Assuming a deviation of one of the four values equal to zero we receive four sections of 1{sigma}-errors ellipsoid. These sections are the spheres of radius 2^0.5^. Taking points on each sphere with the step 0.25*{pi} on angular coordinates we receive 96 points on a surface of the 1{sigma}-errors ellipsoid. The values {alpha}_0_, {delta}{alpha}, {delta}R_1_/R_10_, P_1_ were calculated in the 96 points. The centre of the ellipsoidal was used for calculation of the mean values. The errors of the values were computed as root-mean-squire deviations of 96 values from the same mean values. The errors of the others values of the catalog were computed by the errors calculation rule of indirect measuring.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AZh/89/674#2</TD>
            <TD>2012-12-11T07:10:03Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Dec-2012</TD>
            <TD>ivo://CDS.VizieR/J/AZh/89/674</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/89/674&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/89/674</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/559/606 [1]</TD>
            <TD>Star formation in spectroscopic survey (Carter+, 2001)</TD>
            <TD>The 15R-North galaxy redshift survey is a uniform spectroscopic survey (S/N~10) covering the range 3650-7400{AA} for 3149 galaxies with median redshift 0.05. The sample is 90% complete to R=15.4. The median slit covering fraction is 24% of the galaxy, apparently sufficient to minimize the effects of aperture bias on the EW(H{alpha}). Forty-nine percent of the galaxies in the survey have one or more emission lines detected at &gt;=2{sigma}. In agreement with previous surveys, the fraction of absorption-line galaxies increases steeply with galaxy luminosity. We use H{beta}, [O III], H{alpha}, and [N II] to discriminate between star-forming galaxies and AGNs. At least 20% of the galaxies are star-forming, at least 17% have AGN-like emission, and 12% have unclassifiable emission. The data for the entire survey will appear in Geller et al. 2002, in preparation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606#1</TD>
            <TD>2011-09-14T19:15:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/559/606</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/559/606</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/559/606 [2]</TD>
            <TD>Star formation in spectroscopic survey (Carter+, 2001)</TD>
            <TD>The 15R-North galaxy redshift survey is a uniform spectroscopic survey (S/N~10) covering the range 3650-7400{AA} for 3149 galaxies with median redshift 0.05. The sample is 90% complete to R=15.4. The median slit covering fraction is 24% of the galaxy, apparently sufficient to minimize the effects of aperture bias on the EW(H{alpha}). Forty-nine percent of the galaxies in the survey have one or more emission lines detected at &gt;=2{sigma}. In agreement with previous surveys, the fraction of absorption-line galaxies increases steeply with galaxy luminosity. We use H{beta}, [O III], H{alpha}, and [N II] to discriminate between star-forming galaxies and AGNs. At least 20% of the galaxies are star-forming, at least 17% have AGN-like emission, and 12% have unclassifiable emission. The data for the entire survey will appear in Geller et al. 2002, in preparation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606#2</TD>
            <TD>2011-09-14T19:15:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/559/606&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/559/606</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/559/606 [table3]</TD>
            <TD>Star formation in spectroscopic survey (Carter+, 2001)</TD>
            <TD>The 15R-North galaxy redshift survey is a uniform spectroscopic survey (S/N~10) covering the range 3650-7400{AA} for 3149 galaxies with median redshift 0.05. The sample is 90% complete to R=15.4. The median slit covering fraction is 24% of the galaxy, apparently sufficient to minimize the effects of aperture bias on the EW(H{alpha}). Forty-nine percent of the galaxies in the survey have one or more emission lines detected at &gt;=2{sigma}. In agreement with previous surveys, the fraction of absorption-line galaxies increases steeply with galaxy luminosity. We use H{beta}, [O III], H{alpha}, and [N II] to discriminate between star-forming galaxies and AGNs. At least 20% of the galaxies are star-forming, at least 17% have AGN-like emission, and 12% have unclassifiable emission. The data for the entire survey will appear in Geller et al. 2002, in preparation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606#table3</TD>
            <TD>2011-09-14T19:15:38Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/559/606</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/559/606&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/559/606</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/1095 [1]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#1</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/1095</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/1095 [2]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#2</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/1095&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/1095 [table4]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#table4</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/1095&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/1095 [table2]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#table2</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/1095&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/731/120 [1]</TD>
            <TD>Intrinsic SN Ia light curves (Mandel+, 2011)</TD>
            <TD>We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_&lt;~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_&gt;~1, low values of R_V_&lt;2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120#1</TD>
            <TD>2012-12-14T12:19:56Z</TD>
            <TD>#Photometry#Extinction#Models#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/731/120</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/731/120</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/731/120 [2]</TD>
            <TD>Intrinsic SN Ia light curves (Mandel+, 2011)</TD>
            <TD>We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_&lt;~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_&gt;~1, low values of R_V_&lt;2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120#2</TD>
            <TD>2012-12-14T12:19:56Z</TD>
            <TD>#Photometry#Extinction#Models#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/731/120&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/731/120</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/731/120 [sncat]</TD>
            <TD>Intrinsic SN Ia light curves (Mandel+, 2011)</TD>
            <TD>We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_&lt;~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_&gt;~1, low values of R_V_&lt;2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120#sncat</TD>
            <TD>2012-12-14T12:19:56Z</TD>
            <TD>#Photometry#Extinction#Models#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/731/120&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/731/120</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/731/120 [1]</TD>
            <TD>Intrinsic SN Ia light curves (Mandel+, 2011)</TD>
            <TD>We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_&lt;~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_&gt;~1, low values of R_V_&lt;2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120#1</TD>
            <TD>2012-12-14T12:19:56Z</TD>
            <TD>#Photometry#Extinction#Models#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/731/120</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/731/120</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/731/120 [2]</TD>
            <TD>Intrinsic SN Ia light curves (Mandel+, 2011)</TD>
            <TD>We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_&lt;~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_&gt;~1, low values of R_V_&lt;2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120#2</TD>
            <TD>2012-12-14T12:19:56Z</TD>
            <TD>#Photometry#Extinction#Models#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/731/120&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/731/120</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/731/120 [sncat]</TD>
            <TD>Intrinsic SN Ia light curves (Mandel+, 2011)</TD>
            <TD>We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_&lt;~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_&gt;~1, low values of R_V_&lt;2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120#sncat</TD>
            <TD>2012-12-14T12:19:56Z</TD>
            <TD>#Photometry#Extinction#Models#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/731/120&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/731/120</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/731/120 [1]</TD>
            <TD>Intrinsic SN Ia light curves (Mandel+, 2011)</TD>
            <TD>We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_&lt;~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_&gt;~1, low values of R_V_&lt;2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120#1</TD>
            <TD>2012-12-14T12:19:56Z</TD>
            <TD>#Photometry#Extinction#Models#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/731/120</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/731/120</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/731/120 [2]</TD>
            <TD>Intrinsic SN Ia light curves (Mandel+, 2011)</TD>
            <TD>We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_&lt;~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_&gt;~1, low values of R_V_&lt;2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120#2</TD>
            <TD>2012-12-14T12:19:56Z</TD>
            <TD>#Photometry#Extinction#Models#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/731/120&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/731/120</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/731/120 [sncat]</TD>
            <TD>Intrinsic SN Ia light curves (Mandel+, 2011)</TD>
            <TD>We have constructed a comprehensive statistical model for Type Ia supernova (SN Ia) light curves spanning optical through near-infrared (NIR) data. A hierarchical framework coherently models multiple random and uncertain effects, including intrinsic supernova (SN) light curve covariances, dust extinction and reddening, and distances. An improved BayeSN Markov Chain Monte Carlo code computes probabilistic inferences for the hierarchical model by sampling the global probability density of parameters describing individual SNe and the population. We have applied this hierarchical model to optical and NIR data of 127 SNe Ia from PAIRITEL, CfA3, Carnegie Supernova Project, and the literature. We find an apparent population correlation between the host galaxy extinction AV and the ratio of total-to-selective dust absorption RV. For SNe with low dust extinction, A_V_&lt;~0.4, we find R_V_~2.5-2.9, while at high extinctions, A_V_&gt;~1, low values of R_V_&lt;2 are favored. The NIR luminosities are excellent standard candles and are less sensitive to dust extinction. They exhibit low correlation with optical peak luminosities, and thus provide independent information on distances. The combination of NIR and optical data constrains the dust extinction and improves the predictive precision of individual SN Ia distances by about 60%. Using cross-validation, we estimate an rms distance modulus prediction error of 0.11mag for SNe with optical and NIR data versus 0.15mag for SNe with optical data alone. Continued study of SNe Ia in the NIR is important for improving their utility as precise and accurate cosmological distance indicators.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120#sncat</TD>
            <TD>2012-12-14T12:19:56Z</TD>
            <TD>#Photometry#Extinction#Models#Redshifts#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Oct-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/731/120</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/731/120&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/731/120</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/546/A64 [1]</TD>
            <TD>H and K-band stacked spectra of U/LIRGs (Piqueras Lopez+, 2012)</TD>
            <TD>H- and K-band stacked spectra of the U/LIRG sample, divided into three subsets with log(L_IR_\L_{sun}_)&lt;11.35 (low infra-red luminosity), 11.35&lt;=log(L_IR_\L_{sun}_)&lt;12 (intermediate infra-red luminosity), and log(L_IR_\L_{sun}_)&gt;=12 (high infra-red luminosity). The spectra are normalised to a linear fit of the continuum measured within the intervals [1.600, 1.610]um and [1.690, 1.700]um for the H-band and [2.080, 2.115]um and [2.172, 2.204]um for the K-band. The spectra of each galaxy in each luminosity bin are derotated, rebinned, stacked, and convolved to a resolution of 10{AA} (FWHM) to achieve a homogeneous resolution. See the text for further details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A64#1</TD>
            <TD>2012-12-29T09:04:46Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A64</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/546/A64</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A64</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/546/A64 [2]</TD>
            <TD>H and K-band stacked spectra of U/LIRGs (Piqueras Lopez+, 2012)</TD>
            <TD>H- and K-band stacked spectra of the U/LIRG sample, divided into three subsets with log(L_IR_\L_{sun}_)&lt;11.35 (low infra-red luminosity), 11.35&lt;=log(L_IR_\L_{sun}_)&lt;12 (intermediate infra-red luminosity), and log(L_IR_\L_{sun}_)&gt;=12 (high infra-red luminosity). The spectra are normalised to a linear fit of the continuum measured within the intervals [1.600, 1.610]um and [1.690, 1.700]um for the H-band and [2.080, 2.115]um and [2.172, 2.204]um for the K-band. The spectra of each galaxy in each luminosity bin are derotated, rebinned, stacked, and convolved to a resolution of 10{AA} (FWHM) to achieve a homogeneous resolution. See the text for further details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A64#2</TD>
            <TD>2012-12-29T09:04:46Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A64</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/546/A64&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A64</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/546/A64 [1]</TD>
            <TD>H and K-band stacked spectra of U/LIRGs (Piqueras Lopez+, 2012)</TD>
            <TD>H- and K-band stacked spectra of the U/LIRG sample, divided into three subsets with log(L_IR_\L_{sun}_)&lt;11.35 (low infra-red luminosity), 11.35&lt;=log(L_IR_\L_{sun}_)&lt;12 (intermediate infra-red luminosity), and log(L_IR_\L_{sun}_)&gt;=12 (high infra-red luminosity). The spectra are normalised to a linear fit of the continuum measured within the intervals [1.600, 1.610]um and [1.690, 1.700]um for the H-band and [2.080, 2.115]um and [2.172, 2.204]um for the K-band. The spectra of each galaxy in each luminosity bin are derotated, rebinned, stacked, and convolved to a resolution of 10{AA} (FWHM) to achieve a homogeneous resolution. See the text for further details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A64#1</TD>
            <TD>2012-12-29T09:04:46Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A64</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/546/A64</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A64</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/546/A64 [2]</TD>
            <TD>H and K-band stacked spectra of U/LIRGs (Piqueras Lopez+, 2012)</TD>
            <TD>H- and K-band stacked spectra of the U/LIRG sample, divided into three subsets with log(L_IR_\L_{sun}_)&lt;11.35 (low infra-red luminosity), 11.35&lt;=log(L_IR_\L_{sun}_)&lt;12 (intermediate infra-red luminosity), and log(L_IR_\L_{sun}_)&gt;=12 (high infra-red luminosity). The spectra are normalised to a linear fit of the continuum measured within the intervals [1.600, 1.610]um and [1.690, 1.700]um for the H-band and [2.080, 2.115]um and [2.172, 2.204]um for the K-band. The spectra of each galaxy in each luminosity bin are derotated, rebinned, stacked, and convolved to a resolution of 10{AA} (FWHM) to achieve a homogeneous resolution. See the text for further details.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A64#2</TD>
            <TD>2012-12-29T09:04:46Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A64</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/546/A64&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A64</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/vsx [1]</TD>
            <TD>AAVSO International Variable Star Index VSX (Watson+, 2006-2012)</TD>
            <TD>This file contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the AAVSO International Variable Star Index (VSX; http://www.aavso.org/vsx). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/vsx#1</TD>
            <TD>2013-01-06T07:49:13Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-2013</TD>
            <TD>ivo://CDS.VizieR/B/vsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/vsx</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/vsx</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/vsx [2]</TD>
            <TD>AAVSO International Variable Star Index VSX (Watson+, 2006-2012)</TD>
            <TD>This file contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the AAVSO International Variable Star Index (VSX; http://www.aavso.org/vsx). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/vsx#2</TD>
            <TD>2013-01-06T07:49:13Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-2013</TD>
            <TD>ivo://CDS.VizieR/B/vsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/vsx&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/vsx</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/vsx [vsx]</TD>
            <TD>AAVSO International Variable Star Index VSX (Watson+, 2006-2012)</TD>
            <TD>This file contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the AAVSO International Variable Star Index (VSX; http://www.aavso.org/vsx). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/vsx#vsx</TD>
            <TD>2013-01-06T07:49:13Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-2013</TD>
            <TD>ivo://CDS.VizieR/B/vsx</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/vsx&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/vsx</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/vsx [1]</TD>
            <TD>AAVSO International Variable Star Index VSX (Watson+, 2006-2012)</TD>
            <TD>This file contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the AAVSO International Variable Star Index (VSX; http://www.aavso.org/vsx). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/vsx#1</TD>
            <TD>2013-01-06T07:49:13Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-2013</TD>
            <TD>ivo://CDS.VizieR/B/vsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/vsx</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/vsx</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/vsx [2]</TD>
            <TD>AAVSO International Variable Star Index VSX (Watson+, 2006-2012)</TD>
            <TD>This file contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the AAVSO International Variable Star Index (VSX; http://www.aavso.org/vsx). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/vsx#2</TD>
            <TD>2013-01-06T07:49:13Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-2013</TD>
            <TD>ivo://CDS.VizieR/B/vsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/vsx&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/vsx</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/vsx [vsx]</TD>
            <TD>AAVSO International Variable Star Index VSX (Watson+, 2006-2012)</TD>
            <TD>This file contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the AAVSO International Variable Star Index (VSX; http://www.aavso.org/vsx). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/vsx#vsx</TD>
            <TD>2013-01-06T07:49:13Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-2013</TD>
            <TD>ivo://CDS.VizieR/B/vsx</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/vsx&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/vsx</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/vsx [1]</TD>
            <TD>AAVSO International Variable Star Index VSX (Watson+, 2006-2012)</TD>
            <TD>This file contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the AAVSO International Variable Star Index (VSX; http://www.aavso.org/vsx). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/vsx#1</TD>
            <TD>2013-01-06T07:49:13Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-2013</TD>
            <TD>ivo://CDS.VizieR/B/vsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/vsx</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/vsx</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/vsx [2]</TD>
            <TD>AAVSO International Variable Star Index VSX (Watson+, 2006-2012)</TD>
            <TD>This file contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the AAVSO International Variable Star Index (VSX; http://www.aavso.org/vsx). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/vsx#2</TD>
            <TD>2013-01-06T07:49:13Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-2013</TD>
            <TD>ivo://CDS.VizieR/B/vsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/vsx&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/vsx</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/vsx [vsx]</TD>
            <TD>AAVSO International Variable Star Index VSX (Watson+, 2006-2012)</TD>
            <TD>This file contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the AAVSO International Variable Star Index (VSX; http://www.aavso.org/vsx). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/B/vsx#vsx</TD>
            <TD>2013-01-06T07:49:13Z</TD>
            <TD>#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jan-2013</TD>
            <TD>ivo://CDS.VizieR/B/vsx</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/vsx&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/vsx</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/723/1119 [1]</TD>
            <TD>Optical properties of radio galaxies at z&lt;0.3 (Lin+, 2010)</TD>
            <TD>Extended extragalactic radio sources have traditionally been classified into Fanaroff &amp; Riley (FR) I and II types, based on the ratio r_s_ of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source (r_s_~S/T). In this paper, we examine the distribution of various physical properties as a function of r_s_ of 1040 luminous (L&gt;~L*) extended radio galaxies (RGs) at z&lt;0.3 selected with well-defined criteria from the SDSS (Strauss et al. 2002AJ....124.1810S), NVSS (Condon et al. 1998, Cat. VIII/65), and FIRST (Becker et al. 1995+, Cat. VIII/71) surveys. About 2/3 of the RGs are lobe dominated (LD) and 1/3 have prominent jets. If we follow the original definition of the FR types, i.e., a division based solely on r_s_, FRI and FRII RGs overlap in their host galaxy properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119#1</TD>
            <TD>2013-01-07T12:28:07Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/723/1119</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/723/1119</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/723/1119 [2]</TD>
            <TD>Optical properties of radio galaxies at z&lt;0.3 (Lin+, 2010)</TD>
            <TD>Extended extragalactic radio sources have traditionally been classified into Fanaroff &amp; Riley (FR) I and II types, based on the ratio r_s_ of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source (r_s_~S/T). In this paper, we examine the distribution of various physical properties as a function of r_s_ of 1040 luminous (L&gt;~L*) extended radio galaxies (RGs) at z&lt;0.3 selected with well-defined criteria from the SDSS (Strauss et al. 2002AJ....124.1810S), NVSS (Condon et al. 1998, Cat. VIII/65), and FIRST (Becker et al. 1995+, Cat. VIII/71) surveys. About 2/3 of the RGs are lobe dominated (LD) and 1/3 have prominent jets. If we follow the original definition of the FR types, i.e., a division based solely on r_s_, FRI and FRII RGs overlap in their host galaxy properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119#2</TD>
            <TD>2013-01-07T12:28:07Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/723/1119&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/723/1119</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/723/1119 [table4]</TD>
            <TD>Optical properties of radio galaxies at z&lt;0.3 (Lin+, 2010)</TD>
            <TD>Extended extragalactic radio sources have traditionally been classified into Fanaroff &amp; Riley (FR) I and II types, based on the ratio r_s_ of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source (r_s_~S/T). In this paper, we examine the distribution of various physical properties as a function of r_s_ of 1040 luminous (L&gt;~L*) extended radio galaxies (RGs) at z&lt;0.3 selected with well-defined criteria from the SDSS (Strauss et al. 2002AJ....124.1810S), NVSS (Condon et al. 1998, Cat. VIII/65), and FIRST (Becker et al. 1995+, Cat. VIII/71) surveys. About 2/3 of the RGs are lobe dominated (LD) and 1/3 have prominent jets. If we follow the original definition of the FR types, i.e., a division based solely on r_s_, FRI and FRII RGs overlap in their host galaxy properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119#table4</TD>
            <TD>2013-01-07T12:28:07Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/723/1119&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/723/1119</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/723/1119 [1]</TD>
            <TD>Optical properties of radio galaxies at z&lt;0.3 (Lin+, 2010)</TD>
            <TD>Extended extragalactic radio sources have traditionally been classified into Fanaroff &amp; Riley (FR) I and II types, based on the ratio r_s_ of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source (r_s_~S/T). In this paper, we examine the distribution of various physical properties as a function of r_s_ of 1040 luminous (L&gt;~L*) extended radio galaxies (RGs) at z&lt;0.3 selected with well-defined criteria from the SDSS (Strauss et al. 2002AJ....124.1810S), NVSS (Condon et al. 1998, Cat. VIII/65), and FIRST (Becker et al. 1995+, Cat. VIII/71) surveys. About 2/3 of the RGs are lobe dominated (LD) and 1/3 have prominent jets. If we follow the original definition of the FR types, i.e., a division based solely on r_s_, FRI and FRII RGs overlap in their host galaxy properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119#1</TD>
            <TD>2013-01-07T12:28:07Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/723/1119</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/723/1119</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/723/1119 [2]</TD>
            <TD>Optical properties of radio galaxies at z&lt;0.3 (Lin+, 2010)</TD>
            <TD>Extended extragalactic radio sources have traditionally been classified into Fanaroff &amp; Riley (FR) I and II types, based on the ratio r_s_ of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source (r_s_~S/T). In this paper, we examine the distribution of various physical properties as a function of r_s_ of 1040 luminous (L&gt;~L*) extended radio galaxies (RGs) at z&lt;0.3 selected with well-defined criteria from the SDSS (Strauss et al. 2002AJ....124.1810S), NVSS (Condon et al. 1998, Cat. VIII/65), and FIRST (Becker et al. 1995+, Cat. VIII/71) surveys. About 2/3 of the RGs are lobe dominated (LD) and 1/3 have prominent jets. If we follow the original definition of the FR types, i.e., a division based solely on r_s_, FRI and FRII RGs overlap in their host galaxy properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119#2</TD>
            <TD>2013-01-07T12:28:07Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/723/1119&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/723/1119</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/723/1119 [table4]</TD>
            <TD>Optical properties of radio galaxies at z&lt;0.3 (Lin+, 2010)</TD>
            <TD>Extended extragalactic radio sources have traditionally been classified into Fanaroff &amp; Riley (FR) I and II types, based on the ratio r_s_ of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source (r_s_~S/T). In this paper, we examine the distribution of various physical properties as a function of r_s_ of 1040 luminous (L&gt;~L*) extended radio galaxies (RGs) at z&lt;0.3 selected with well-defined criteria from the SDSS (Strauss et al. 2002AJ....124.1810S), NVSS (Condon et al. 1998, Cat. VIII/65), and FIRST (Becker et al. 1995+, Cat. VIII/71) surveys. About 2/3 of the RGs are lobe dominated (LD) and 1/3 have prominent jets. If we follow the original definition of the FR types, i.e., a division based solely on r_s_, FRI and FRII RGs overlap in their host galaxy properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119#table4</TD>
            <TD>2013-01-07T12:28:07Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/723/1119&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/723/1119</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/723/1119 [1]</TD>
            <TD>Optical properties of radio galaxies at z&lt;0.3 (Lin+, 2010)</TD>
            <TD>Extended extragalactic radio sources have traditionally been classified into Fanaroff &amp; Riley (FR) I and II types, based on the ratio r_s_ of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source (r_s_~S/T). In this paper, we examine the distribution of various physical properties as a function of r_s_ of 1040 luminous (L&gt;~L*) extended radio galaxies (RGs) at z&lt;0.3 selected with well-defined criteria from the SDSS (Strauss et al. 2002AJ....124.1810S), NVSS (Condon et al. 1998, Cat. VIII/65), and FIRST (Becker et al. 1995+, Cat. VIII/71) surveys. About 2/3 of the RGs are lobe dominated (LD) and 1/3 have prominent jets. If we follow the original definition of the FR types, i.e., a division based solely on r_s_, FRI and FRII RGs overlap in their host galaxy properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119#1</TD>
            <TD>2013-01-07T12:28:07Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/723/1119</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/723/1119</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/723/1119 [2]</TD>
            <TD>Optical properties of radio galaxies at z&lt;0.3 (Lin+, 2010)</TD>
            <TD>Extended extragalactic radio sources have traditionally been classified into Fanaroff &amp; Riley (FR) I and II types, based on the ratio r_s_ of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source (r_s_~S/T). In this paper, we examine the distribution of various physical properties as a function of r_s_ of 1040 luminous (L&gt;~L*) extended radio galaxies (RGs) at z&lt;0.3 selected with well-defined criteria from the SDSS (Strauss et al. 2002AJ....124.1810S), NVSS (Condon et al. 1998, Cat. VIII/65), and FIRST (Becker et al. 1995+, Cat. VIII/71) surveys. About 2/3 of the RGs are lobe dominated (LD) and 1/3 have prominent jets. If we follow the original definition of the FR types, i.e., a division based solely on r_s_, FRI and FRII RGs overlap in their host galaxy properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119#2</TD>
            <TD>2013-01-07T12:28:07Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/723/1119&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/723/1119</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/723/1119 [table4]</TD>
            <TD>Optical properties of radio galaxies at z&lt;0.3 (Lin+, 2010)</TD>
            <TD>Extended extragalactic radio sources have traditionally been classified into Fanaroff &amp; Riley (FR) I and II types, based on the ratio r_s_ of the separation S between the brightest regions on either sides of the host galaxy and the total size T of the radio source (r_s_~S/T). In this paper, we examine the distribution of various physical properties as a function of r_s_ of 1040 luminous (L&gt;~L*) extended radio galaxies (RGs) at z&lt;0.3 selected with well-defined criteria from the SDSS (Strauss et al. 2002AJ....124.1810S), NVSS (Condon et al. 1998, Cat. VIII/65), and FIRST (Becker et al. 1995+, Cat. VIII/71) surveys. About 2/3 of the RGs are lobe dominated (LD) and 1/3 have prominent jets. If we follow the original definition of the FR types, i.e., a division based solely on r_s_, FRI and FRII RGs overlap in their host galaxy properties.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119#table4</TD>
            <TD>2013-01-07T12:28:07Z</TD>
            <TD>#AGN#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/723/1119</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/723/1119&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/723/1119</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/734/68 [1]</TD>
            <TD>High redshift galaxy clusters in deep fields (Wen+, 2011)</TD>
            <TD>The CFHT survey is carried out with the 3.6m CFHT in the u', g', r', i', and z' bands for three imaging sub-surveys: the CFHT Deep Survey, the CFHT Wide Survey, and the CFHT Very Wide Survey. The photo-z data of the deep and wide fields have been published and used in previous works (see references in Section 1.1). The CFHT wide survey covers 35deg^2^ in three deep fields (W1, W3, W4). The CFHT Deep survey covers 3.2deg^2^ in four deep fields (D1, D2, D3, D4). COSMOS is formed from a field of 2deg^2^ by many observations from X-ray to radio (XMM, Galaxy Evolution Explorer, Hubble Space Telescope, CFHT, United Kingdom Infrared Telescope, Subaru, Spitzer, and Very Large Array). Spitzer SWIRE provides photometry (Lonsdale et al. 2003PASP..115..897L) in the IRAC bands of 3.6um, 4.5um, 5.8um, and 8.0um and MIPS bands of 24um, 70um, and 160um for six regions (ELAIS-N1, ELAIS-N2, Lockman Hole, XMM, ELAIS-S1, and the Chandra Deep Field South (CDFS)). The photometries in optical bands u, g, r, i, and z (the band only here, not the redshift) are available from the SWIRE photometry program and from McMahon et al. (2001NewAR..45...97M) and Pierre et al. (2007, Cat. J/MNRAS/382/279). Detailed parameters for the four fields are given in Table 1, including the field size, magnitude limit, number of bands for photometry, and the accuracy of photo-z : -------------------------------------------------------------------------------- Name Field l_mage_z No.r_zph NCl NnewCl Nhz Nnewhz (deg^2^) Bands -------------------------------------------------------------------------------- CFHT Wide 35.0i'&lt;22.5 0.038 5 1 631 285 24 19 CFHT Deep 3.2i'&lt;240.029 5 1,220255 53 29 COSMOS 2.0i^+^&lt;25 0.012 30 3 187 127 43 38 SWIRE 33.0r&lt;24 0.035 5-12 4 737 674116 106 -------------------------------------------------------------------------------- References for photo-z: (1) Coupon et al. 2009A&amp;A...500..981C; (2) Ilbert et al. 2006A&amp;A...457..841I; (3) Ilbert et al. 2009ApJ...690.1236I; (4) Rowan-Robinson et al. (2008, Cat. II/290). Here, high-z (hz) means z&gt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68#1</TD>
            <TD>2013-02-06T12:34:11Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/734/68</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/734/68</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/734/68 [2]</TD>
            <TD>High redshift galaxy clusters in deep fields (Wen+, 2011)</TD>
            <TD>The CFHT survey is carried out with the 3.6m CFHT in the u', g', r', i', and z' bands for three imaging sub-surveys: the CFHT Deep Survey, the CFHT Wide Survey, and the CFHT Very Wide Survey. The photo-z data of the deep and wide fields have been published and used in previous works (see references in Section 1.1). The CFHT wide survey covers 35deg^2^ in three deep fields (W1, W3, W4). The CFHT Deep survey covers 3.2deg^2^ in four deep fields (D1, D2, D3, D4). COSMOS is formed from a field of 2deg^2^ by many observations from X-ray to radio (XMM, Galaxy Evolution Explorer, Hubble Space Telescope, CFHT, United Kingdom Infrared Telescope, Subaru, Spitzer, and Very Large Array). Spitzer SWIRE provides photometry (Lonsdale et al. 2003PASP..115..897L) in the IRAC bands of 3.6um, 4.5um, 5.8um, and 8.0um and MIPS bands of 24um, 70um, and 160um for six regions (ELAIS-N1, ELAIS-N2, Lockman Hole, XMM, ELAIS-S1, and the Chandra Deep Field South (CDFS)). The photometries in optical bands u, g, r, i, and z (the band only here, not the redshift) are available from the SWIRE photometry program and from McMahon et al. (2001NewAR..45...97M) and Pierre et al. (2007, Cat. J/MNRAS/382/279). Detailed parameters for the four fields are given in Table 1, including the field size, magnitude limit, number of bands for photometry, and the accuracy of photo-z : -------------------------------------------------------------------------------- Name Field l_mage_z No.r_zph NCl NnewCl Nhz Nnewhz (deg^2^) Bands -------------------------------------------------------------------------------- CFHT Wide 35.0i'&lt;22.5 0.038 5 1 631 285 24 19 CFHT Deep 3.2i'&lt;240.029 5 1,220255 53 29 COSMOS 2.0i^+^&lt;25 0.012 30 3 187 127 43 38 SWIRE 33.0r&lt;24 0.035 5-12 4 737 674116 106 -------------------------------------------------------------------------------- References for photo-z: (1) Coupon et al. 2009A&amp;A...500..981C; (2) Ilbert et al. 2006A&amp;A...457..841I; (3) Ilbert et al. 2009ApJ...690.1236I; (4) Rowan-Robinson et al. (2008, Cat. II/290). Here, high-z (hz) means z&gt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68#2</TD>
            <TD>2013-02-06T12:34:11Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/734/68&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/734/68</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/734/68 [table2]</TD>
            <TD>High redshift galaxy clusters in deep fields (Wen+, 2011)</TD>
            <TD>The CFHT survey is carried out with the 3.6m CFHT in the u', g', r', i', and z' bands for three imaging sub-surveys: the CFHT Deep Survey, the CFHT Wide Survey, and the CFHT Very Wide Survey. The photo-z data of the deep and wide fields have been published and used in previous works (see references in Section 1.1). The CFHT wide survey covers 35deg^2^ in three deep fields (W1, W3, W4). The CFHT Deep survey covers 3.2deg^2^ in four deep fields (D1, D2, D3, D4). COSMOS is formed from a field of 2deg^2^ by many observations from X-ray to radio (XMM, Galaxy Evolution Explorer, Hubble Space Telescope, CFHT, United Kingdom Infrared Telescope, Subaru, Spitzer, and Very Large Array). Spitzer SWIRE provides photometry (Lonsdale et al. 2003PASP..115..897L) in the IRAC bands of 3.6um, 4.5um, 5.8um, and 8.0um and MIPS bands of 24um, 70um, and 160um for six regions (ELAIS-N1, ELAIS-N2, Lockman Hole, XMM, ELAIS-S1, and the Chandra Deep Field South (CDFS)). The photometries in optical bands u, g, r, i, and z (the band only here, not the redshift) are available from the SWIRE photometry program and from McMahon et al. (2001NewAR..45...97M) and Pierre et al. (2007, Cat. J/MNRAS/382/279). Detailed parameters for the four fields are given in Table 1, including the field size, magnitude limit, number of bands for photometry, and the accuracy of photo-z : -------------------------------------------------------------------------------- Name Field l_mage_z No.r_zph NCl NnewCl Nhz Nnewhz (deg^2^) Bands -------------------------------------------------------------------------------- CFHT Wide 35.0i'&lt;22.5 0.038 5 1 631 285 24 19 CFHT Deep 3.2i'&lt;240.029 5 1,220255 53 29 COSMOS 2.0i^+^&lt;25 0.012 30 3 187 127 43 38 SWIRE 33.0r&lt;24 0.035 5-12 4 737 674116 106 -------------------------------------------------------------------------------- References for photo-z: (1) Coupon et al. 2009A&amp;A...500..981C; (2) Ilbert et al. 2006A&amp;A...457..841I; (3) Ilbert et al. 2009ApJ...690.1236I; (4) Rowan-Robinson et al. (2008, Cat. II/290). Here, high-z (hz) means z&gt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68#table2</TD>
            <TD>2013-02-06T12:34:11Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/734/68&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/734/68</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/109/1095 [1]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#1</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/109/1095</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/109/1095 [2]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#2</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/109/1095&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/1095 [table4]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#table4</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/1095&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/109/1095 [table2]</TD>
            <TD>Thick Disk Chemical Abundance Distribution (Gilmore+ 1995)</TD>
            <TD>We present a determination of the thick disk iron abundance distribution obtained from an in situ sample of F/G stars. These stars are faint, 15&lt;=V=&lt;18, selected on the basis of color, being a subset of the larger survey of Gilmore and Wyse designed to determine the properties of the stellar populations several kiloparsecs from the Sun. The fields studied in the present paper probe the iron abundance distribution of the stellar populations of the galaxy at 500-3000pc above the plane, at the solar Galactocentric distance. The derived chemical abundance distributions are consistent with no metallicity gradients in the thick disk over this range of vertical distance, and with an iron abundance distribution for the thick disk that has a peak at -0.7dex. The lack of a vertical gradient argues against slow, dissipational settling as a mechanism for the formation of the thick disk. The photometric and metallicity data support a turn-off of the thick disk that is comparable in age to the metal-rich globular clusters, or &gt;=12Gyr, and are consistent with a spread to older ages.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095#table2</TD>
            <TD>2011-09-14T19:01:16Z</TD>
            <TD>#Photometry#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jun-1996</TD>
            <TD>ivo://CDS.VizieR/J/AJ/109/1095</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/109/1095&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/109/1095</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/111/438 [1]</TD>
            <TD>Updated Zwicky catalog (UZC) (Falco+, 1999)</TD>
            <TD>The Zwicky Catalog of galaxies (ZC), with m_Zw_&lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing (1) coordinates with ~&lt;2" errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7257 galaxies in the CfA2 redshift survey not previously published; for another 5625 CfA redshifts we list the remeasured or uniformly rereduced value. Among our new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438#1</TD>
            <TD>2011-09-14T19:16:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/111/438</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/111/438</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/111/438 [2]</TD>
            <TD>Updated Zwicky catalog (UZC) (Falco+, 1999)</TD>
            <TD>The Zwicky Catalog of galaxies (ZC), with m_Zw_&lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing (1) coordinates with ~&lt;2" errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7257 galaxies in the CfA2 redshift survey not previously published; for another 5625 CfA redshifts we list the remeasured or uniformly rereduced value. Among our new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438#2</TD>
            <TD>2011-09-14T19:16:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/111/438&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/111/438</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/111/438 [catalog]</TD>
            <TD>Updated Zwicky catalog (UZC) (Falco+, 1999)</TD>
            <TD>The Zwicky Catalog of galaxies (ZC), with m_Zw_&lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing (1) coordinates with ~&lt;2" errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7257 galaxies in the CfA2 redshift survey not previously published; for another 5625 CfA redshifts we list the remeasured or uniformly rereduced value. Among our new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438#catalog</TD>
            <TD>2011-09-14T19:16:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/111/438&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/111/438</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/734/68 [1]</TD>
            <TD>High redshift galaxy clusters in deep fields (Wen+, 2011)</TD>
            <TD>The CFHT survey is carried out with the 3.6m CFHT in the u', g', r', i', and z' bands for three imaging sub-surveys: the CFHT Deep Survey, the CFHT Wide Survey, and the CFHT Very Wide Survey. The photo-z data of the deep and wide fields have been published and used in previous works (see references in Section 1.1). The CFHT wide survey covers 35deg^2^ in three deep fields (W1, W3, W4). The CFHT Deep survey covers 3.2deg^2^ in four deep fields (D1, D2, D3, D4). COSMOS is formed from a field of 2deg^2^ by many observations from X-ray to radio (XMM, Galaxy Evolution Explorer, Hubble Space Telescope, CFHT, United Kingdom Infrared Telescope, Subaru, Spitzer, and Very Large Array). Spitzer SWIRE provides photometry (Lonsdale et al. 2003PASP..115..897L) in the IRAC bands of 3.6um, 4.5um, 5.8um, and 8.0um and MIPS bands of 24um, 70um, and 160um for six regions (ELAIS-N1, ELAIS-N2, Lockman Hole, XMM, ELAIS-S1, and the Chandra Deep Field South (CDFS)). The photometries in optical bands u, g, r, i, and z (the band only here, not the redshift) are available from the SWIRE photometry program and from McMahon et al. (2001NewAR..45...97M) and Pierre et al. (2007, Cat. J/MNRAS/382/279). Detailed parameters for the four fields are given in Table 1, including the field size, magnitude limit, number of bands for photometry, and the accuracy of photo-z : -------------------------------------------------------------------------------- Name Field l_mage_z No.r_zph NCl NnewCl Nhz Nnewhz (deg^2^) Bands -------------------------------------------------------------------------------- CFHT Wide 35.0i'&lt;22.5 0.038 5 1 631 285 24 19 CFHT Deep 3.2i'&lt;240.029 5 1,220255 53 29 COSMOS 2.0i^+^&lt;25 0.012 30 3 187 127 43 38 SWIRE 33.0r&lt;24 0.035 5-12 4 737 674116 106 -------------------------------------------------------------------------------- References for photo-z: (1) Coupon et al. 2009A&amp;A...500..981C; (2) Ilbert et al. 2006A&amp;A...457..841I; (3) Ilbert et al. 2009ApJ...690.1236I; (4) Rowan-Robinson et al. (2008, Cat. II/290). Here, high-z (hz) means z&gt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68#1</TD>
            <TD>2013-02-06T12:34:11Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/734/68</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/734/68</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/734/68 [2]</TD>
            <TD>High redshift galaxy clusters in deep fields (Wen+, 2011)</TD>
            <TD>The CFHT survey is carried out with the 3.6m CFHT in the u', g', r', i', and z' bands for three imaging sub-surveys: the CFHT Deep Survey, the CFHT Wide Survey, and the CFHT Very Wide Survey. The photo-z data of the deep and wide fields have been published and used in previous works (see references in Section 1.1). The CFHT wide survey covers 35deg^2^ in three deep fields (W1, W3, W4). The CFHT Deep survey covers 3.2deg^2^ in four deep fields (D1, D2, D3, D4). COSMOS is formed from a field of 2deg^2^ by many observations from X-ray to radio (XMM, Galaxy Evolution Explorer, Hubble Space Telescope, CFHT, United Kingdom Infrared Telescope, Subaru, Spitzer, and Very Large Array). Spitzer SWIRE provides photometry (Lonsdale et al. 2003PASP..115..897L) in the IRAC bands of 3.6um, 4.5um, 5.8um, and 8.0um and MIPS bands of 24um, 70um, and 160um for six regions (ELAIS-N1, ELAIS-N2, Lockman Hole, XMM, ELAIS-S1, and the Chandra Deep Field South (CDFS)). The photometries in optical bands u, g, r, i, and z (the band only here, not the redshift) are available from the SWIRE photometry program and from McMahon et al. (2001NewAR..45...97M) and Pierre et al. (2007, Cat. J/MNRAS/382/279). Detailed parameters for the four fields are given in Table 1, including the field size, magnitude limit, number of bands for photometry, and the accuracy of photo-z : -------------------------------------------------------------------------------- Name Field l_mage_z No.r_zph NCl NnewCl Nhz Nnewhz (deg^2^) Bands -------------------------------------------------------------------------------- CFHT Wide 35.0i'&lt;22.5 0.038 5 1 631 285 24 19 CFHT Deep 3.2i'&lt;240.029 5 1,220255 53 29 COSMOS 2.0i^+^&lt;25 0.012 30 3 187 127 43 38 SWIRE 33.0r&lt;24 0.035 5-12 4 737 674116 106 -------------------------------------------------------------------------------- References for photo-z: (1) Coupon et al. 2009A&amp;A...500..981C; (2) Ilbert et al. 2006A&amp;A...457..841I; (3) Ilbert et al. 2009ApJ...690.1236I; (4) Rowan-Robinson et al. (2008, Cat. II/290). Here, high-z (hz) means z&gt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68#2</TD>
            <TD>2013-02-06T12:34:11Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/734/68&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/734/68</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/734/68 [table2]</TD>
            <TD>High redshift galaxy clusters in deep fields (Wen+, 2011)</TD>
            <TD>The CFHT survey is carried out with the 3.6m CFHT in the u', g', r', i', and z' bands for three imaging sub-surveys: the CFHT Deep Survey, the CFHT Wide Survey, and the CFHT Very Wide Survey. The photo-z data of the deep and wide fields have been published and used in previous works (see references in Section 1.1). The CFHT wide survey covers 35deg^2^ in three deep fields (W1, W3, W4). The CFHT Deep survey covers 3.2deg^2^ in four deep fields (D1, D2, D3, D4). COSMOS is formed from a field of 2deg^2^ by many observations from X-ray to radio (XMM, Galaxy Evolution Explorer, Hubble Space Telescope, CFHT, United Kingdom Infrared Telescope, Subaru, Spitzer, and Very Large Array). Spitzer SWIRE provides photometry (Lonsdale et al. 2003PASP..115..897L) in the IRAC bands of 3.6um, 4.5um, 5.8um, and 8.0um and MIPS bands of 24um, 70um, and 160um for six regions (ELAIS-N1, ELAIS-N2, Lockman Hole, XMM, ELAIS-S1, and the Chandra Deep Field South (CDFS)). The photometries in optical bands u, g, r, i, and z (the band only here, not the redshift) are available from the SWIRE photometry program and from McMahon et al. (2001NewAR..45...97M) and Pierre et al. (2007, Cat. J/MNRAS/382/279). Detailed parameters for the four fields are given in Table 1, including the field size, magnitude limit, number of bands for photometry, and the accuracy of photo-z : -------------------------------------------------------------------------------- Name Field l_mage_z No.r_zph NCl NnewCl Nhz Nnewhz (deg^2^) Bands -------------------------------------------------------------------------------- CFHT Wide 35.0i'&lt;22.5 0.038 5 1 631 285 24 19 CFHT Deep 3.2i'&lt;240.029 5 1,220255 53 29 COSMOS 2.0i^+^&lt;25 0.012 30 3 187 127 43 38 SWIRE 33.0r&lt;24 0.035 5-12 4 737 674116 106 -------------------------------------------------------------------------------- References for photo-z: (1) Coupon et al. 2009A&amp;A...500..981C; (2) Ilbert et al. 2006A&amp;A...457..841I; (3) Ilbert et al. 2009ApJ...690.1236I; (4) Rowan-Robinson et al. (2008, Cat. II/290). Here, high-z (hz) means z&gt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68#table2</TD>
            <TD>2013-02-06T12:34:11Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/734/68&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/734/68</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/118/2014 [1]</TD>
            <TD>Nearby poor clusters of galaxies catalog (White+, 1999)</TD>
            <TD>A catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3{deg} declination is presented. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^4/3^. These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. The information on individual galaxies includes redshifts and cross-references to other galaxy catalogs. The entries for the clusters include redshift (where available) and cross-references to other group and cluster catalogs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014#1</TD>
            <TD>2011-09-14T19:01:25Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/118/2014</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/2014</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/118/2014 [2]</TD>
            <TD>Nearby poor clusters of galaxies catalog (White+, 1999)</TD>
            <TD>A catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3{deg} declination is presented. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^4/3^. These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. The information on individual galaxies includes redshifts and cross-references to other galaxy catalogs. The entries for the clusters include redshift (where available) and cross-references to other group and cluster catalogs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014#2</TD>
            <TD>2011-09-14T19:01:25Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/118/2014&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/2014</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/734/68 [1]</TD>
            <TD>High redshift galaxy clusters in deep fields (Wen+, 2011)</TD>
            <TD>The CFHT survey is carried out with the 3.6m CFHT in the u', g', r', i', and z' bands for three imaging sub-surveys: the CFHT Deep Survey, the CFHT Wide Survey, and the CFHT Very Wide Survey. The photo-z data of the deep and wide fields have been published and used in previous works (see references in Section 1.1). The CFHT wide survey covers 35deg^2^ in three deep fields (W1, W3, W4). The CFHT Deep survey covers 3.2deg^2^ in four deep fields (D1, D2, D3, D4). COSMOS is formed from a field of 2deg^2^ by many observations from X-ray to radio (XMM, Galaxy Evolution Explorer, Hubble Space Telescope, CFHT, United Kingdom Infrared Telescope, Subaru, Spitzer, and Very Large Array). Spitzer SWIRE provides photometry (Lonsdale et al. 2003PASP..115..897L) in the IRAC bands of 3.6um, 4.5um, 5.8um, and 8.0um and MIPS bands of 24um, 70um, and 160um for six regions (ELAIS-N1, ELAIS-N2, Lockman Hole, XMM, ELAIS-S1, and the Chandra Deep Field South (CDFS)). The photometries in optical bands u, g, r, i, and z (the band only here, not the redshift) are available from the SWIRE photometry program and from McMahon et al. (2001NewAR..45...97M) and Pierre et al. (2007, Cat. J/MNRAS/382/279). Detailed parameters for the four fields are given in Table 1, including the field size, magnitude limit, number of bands for photometry, and the accuracy of photo-z : -------------------------------------------------------------------------------- Name Field l_mage_z No.r_zph NCl NnewCl Nhz Nnewhz (deg^2^) Bands -------------------------------------------------------------------------------- CFHT Wide 35.0i'&lt;22.5 0.038 5 1 631 285 24 19 CFHT Deep 3.2i'&lt;240.029 5 1,220255 53 29 COSMOS 2.0i^+^&lt;25 0.012 30 3 187 127 43 38 SWIRE 33.0r&lt;24 0.035 5-12 4 737 674116 106 -------------------------------------------------------------------------------- References for photo-z: (1) Coupon et al. 2009A&amp;A...500..981C; (2) Ilbert et al. 2006A&amp;A...457..841I; (3) Ilbert et al. 2009ApJ...690.1236I; (4) Rowan-Robinson et al. (2008, Cat. II/290). Here, high-z (hz) means z&gt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68#1</TD>
            <TD>2013-02-06T12:34:11Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/734/68</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/734/68</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/734/68 [2]</TD>
            <TD>High redshift galaxy clusters in deep fields (Wen+, 2011)</TD>
            <TD>The CFHT survey is carried out with the 3.6m CFHT in the u', g', r', i', and z' bands for three imaging sub-surveys: the CFHT Deep Survey, the CFHT Wide Survey, and the CFHT Very Wide Survey. The photo-z data of the deep and wide fields have been published and used in previous works (see references in Section 1.1). The CFHT wide survey covers 35deg^2^ in three deep fields (W1, W3, W4). The CFHT Deep survey covers 3.2deg^2^ in four deep fields (D1, D2, D3, D4). COSMOS is formed from a field of 2deg^2^ by many observations from X-ray to radio (XMM, Galaxy Evolution Explorer, Hubble Space Telescope, CFHT, United Kingdom Infrared Telescope, Subaru, Spitzer, and Very Large Array). Spitzer SWIRE provides photometry (Lonsdale et al. 2003PASP..115..897L) in the IRAC bands of 3.6um, 4.5um, 5.8um, and 8.0um and MIPS bands of 24um, 70um, and 160um for six regions (ELAIS-N1, ELAIS-N2, Lockman Hole, XMM, ELAIS-S1, and the Chandra Deep Field South (CDFS)). The photometries in optical bands u, g, r, i, and z (the band only here, not the redshift) are available from the SWIRE photometry program and from McMahon et al. (2001NewAR..45...97M) and Pierre et al. (2007, Cat. J/MNRAS/382/279). Detailed parameters for the four fields are given in Table 1, including the field size, magnitude limit, number of bands for photometry, and the accuracy of photo-z : -------------------------------------------------------------------------------- Name Field l_mage_z No.r_zph NCl NnewCl Nhz Nnewhz (deg^2^) Bands -------------------------------------------------------------------------------- CFHT Wide 35.0i'&lt;22.5 0.038 5 1 631 285 24 19 CFHT Deep 3.2i'&lt;240.029 5 1,220255 53 29 COSMOS 2.0i^+^&lt;25 0.012 30 3 187 127 43 38 SWIRE 33.0r&lt;24 0.035 5-12 4 737 674116 106 -------------------------------------------------------------------------------- References for photo-z: (1) Coupon et al. 2009A&amp;A...500..981C; (2) Ilbert et al. 2006A&amp;A...457..841I; (3) Ilbert et al. 2009ApJ...690.1236I; (4) Rowan-Robinson et al. (2008, Cat. II/290). Here, high-z (hz) means z&gt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68#2</TD>
            <TD>2013-02-06T12:34:11Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/734/68&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/734/68</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/734/68 [table2]</TD>
            <TD>High redshift galaxy clusters in deep fields (Wen+, 2011)</TD>
            <TD>The CFHT survey is carried out with the 3.6m CFHT in the u', g', r', i', and z' bands for three imaging sub-surveys: the CFHT Deep Survey, the CFHT Wide Survey, and the CFHT Very Wide Survey. The photo-z data of the deep and wide fields have been published and used in previous works (see references in Section 1.1). The CFHT wide survey covers 35deg^2^ in three deep fields (W1, W3, W4). The CFHT Deep survey covers 3.2deg^2^ in four deep fields (D1, D2, D3, D4). COSMOS is formed from a field of 2deg^2^ by many observations from X-ray to radio (XMM, Galaxy Evolution Explorer, Hubble Space Telescope, CFHT, United Kingdom Infrared Telescope, Subaru, Spitzer, and Very Large Array). Spitzer SWIRE provides photometry (Lonsdale et al. 2003PASP..115..897L) in the IRAC bands of 3.6um, 4.5um, 5.8um, and 8.0um and MIPS bands of 24um, 70um, and 160um for six regions (ELAIS-N1, ELAIS-N2, Lockman Hole, XMM, ELAIS-S1, and the Chandra Deep Field South (CDFS)). The photometries in optical bands u, g, r, i, and z (the band only here, not the redshift) are available from the SWIRE photometry program and from McMahon et al. (2001NewAR..45...97M) and Pierre et al. (2007, Cat. J/MNRAS/382/279). Detailed parameters for the four fields are given in Table 1, including the field size, magnitude limit, number of bands for photometry, and the accuracy of photo-z : -------------------------------------------------------------------------------- Name Field l_mage_z No.r_zph NCl NnewCl Nhz Nnewhz (deg^2^) Bands -------------------------------------------------------------------------------- CFHT Wide 35.0i'&lt;22.5 0.038 5 1 631 285 24 19 CFHT Deep 3.2i'&lt;240.029 5 1,220255 53 29 COSMOS 2.0i^+^&lt;25 0.012 30 3 187 127 43 38 SWIRE 33.0r&lt;24 0.035 5-12 4 737 674116 106 -------------------------------------------------------------------------------- References for photo-z: (1) Coupon et al. 2009A&amp;A...500..981C; (2) Ilbert et al. 2006A&amp;A...457..841I; (3) Ilbert et al. 2009ApJ...690.1236I; (4) Rowan-Robinson et al. (2008, Cat. II/290). Here, high-z (hz) means z&gt;=1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68#table2</TD>
            <TD>2013-02-06T12:34:11Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/734/68</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/734/68&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/734/68</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/111/438 [1]</TD>
            <TD>Updated Zwicky catalog (UZC) (Falco+, 1999)</TD>
            <TD>The Zwicky Catalog of galaxies (ZC), with m_Zw_&lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing (1) coordinates with ~&lt;2" errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7257 galaxies in the CfA2 redshift survey not previously published; for another 5625 CfA redshifts we list the remeasured or uniformly rereduced value. Among our new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438#1</TD>
            <TD>2011-09-14T19:16:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/111/438</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/111/438</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/111/438 [2]</TD>
            <TD>Updated Zwicky catalog (UZC) (Falco+, 1999)</TD>
            <TD>The Zwicky Catalog of galaxies (ZC), with m_Zw_&lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing (1) coordinates with ~&lt;2" errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7257 galaxies in the CfA2 redshift survey not previously published; for another 5625 CfA redshifts we list the remeasured or uniformly rereduced value. Among our new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438#2</TD>
            <TD>2011-09-14T19:16:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/111/438&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/111/438</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/111/438 [catalog]</TD>
            <TD>Updated Zwicky catalog (UZC) (Falco+, 1999)</TD>
            <TD>The Zwicky Catalog of galaxies (ZC), with m_Zw_&lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing (1) coordinates with ~&lt;2" errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7257 galaxies in the CfA2 redshift survey not previously published; for another 5625 CfA redshifts we list the remeasured or uniformly rereduced value. Among our new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438#catalog</TD>
            <TD>2011-09-14T19:16:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/111/438&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/111/438</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/118/2014 [1]</TD>
            <TD>Nearby poor clusters of galaxies catalog (White+, 1999)</TD>
            <TD>A catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3{deg} declination is presented. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^4/3^. These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. The information on individual galaxies includes redshifts and cross-references to other galaxy catalogs. The entries for the clusters include redshift (where available) and cross-references to other group and cluster catalogs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014#1</TD>
            <TD>2011-09-14T19:01:25Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/118/2014</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/2014</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/118/2014 [2]</TD>
            <TD>Nearby poor clusters of galaxies catalog (White+, 1999)</TD>
            <TD>A catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3{deg} declination is presented. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^4/3^. These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. The information on individual galaxies includes redshifts and cross-references to other galaxy catalogs. The entries for the clusters include redshift (where available) and cross-references to other group and cluster catalogs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014#2</TD>
            <TD>2011-09-14T19:01:25Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/118/2014&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/2014</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/111/438 [1]</TD>
            <TD>Updated Zwicky catalog (UZC) (Falco+, 1999)</TD>
            <TD>The Zwicky Catalog of galaxies (ZC), with m_Zw_&lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing (1) coordinates with ~&lt;2" errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7257 galaxies in the CfA2 redshift survey not previously published; for another 5625 CfA redshifts we list the remeasured or uniformly rereduced value. Among our new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438#1</TD>
            <TD>2011-09-14T19:16:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/111/438</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/111/438</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/111/438 [2]</TD>
            <TD>Updated Zwicky catalog (UZC) (Falco+, 1999)</TD>
            <TD>The Zwicky Catalog of galaxies (ZC), with m_Zw_&lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing (1) coordinates with ~&lt;2" errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7257 galaxies in the CfA2 redshift survey not previously published; for another 5625 CfA redshifts we list the remeasured or uniformly rereduced value. Among our new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438#2</TD>
            <TD>2011-09-14T19:16:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/111/438&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/111/438</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/111/438 [catalog]</TD>
            <TD>Updated Zwicky catalog (UZC) (Falco+, 1999)</TD>
            <TD>The Zwicky Catalog of galaxies (ZC), with m_Zw_&lt;=15.5, has been the basis for the Center for Astrophysics (CfA) redshift surveys. To date, analyses of the ZC and redshift surveys based on it have relied on heterogeneous sets of galaxy coordinates and redshifts. Here we correct some of the inadequacies of previous catalogs by providing (1) coordinates with ~&lt;2" errors for all of the 19,369 catalog galaxies, (2) homogeneously estimated redshifts for the majority (98%) of the data taken at the CfA (14,632 spectra), and (3) an estimate of the remaining "blunder" rate for both the CfA redshifts and for those compiled from the literature. For the reanalyzed CfA data we include a calibrated, uniformly determined error and an indication of the presence of emission lines in each spectrum. We provide redshifts for 7257 galaxies in the CfA2 redshift survey not previously published; for another 5625 CfA redshifts we list the remeasured or uniformly rereduced value. Among our new measurements, 1807 are members of UZC "multiplets" associated with the original Zwicky catalog position in the coordinate range where the catalog is 98% complete.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438#catalog</TD>
            <TD>2011-09-14T19:16:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/PASP/111/438</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/111/438&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/111/438</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/118/2014 [1]</TD>
            <TD>Nearby poor clusters of galaxies catalog (White+, 1999)</TD>
            <TD>A catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3{deg} declination is presented. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^4/3^. These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. The information on individual galaxies includes redshifts and cross-references to other galaxy catalogs. The entries for the clusters include redshift (where available) and cross-references to other group and cluster catalogs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014#1</TD>
            <TD>2011-09-14T19:01:25Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/118/2014</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/2014</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/118/2014 [2]</TD>
            <TD>Nearby poor clusters of galaxies catalog (White+, 1999)</TD>
            <TD>A catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3{deg} declination is presented. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^4/3^. These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. The information on individual galaxies includes redshifts and cross-references to other galaxy catalogs. The entries for the clusters include redshift (where available) and cross-references to other group and cluster catalogs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014#2</TD>
            <TD>2011-09-14T19:01:25Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/118/2014</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/118/2014&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/118/2014</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1411 [1]</TD>
            <TD>UBVIHalpha photometry of NGC 4314 star clusters (Benedict+, 2002)</TD>
            <TD>Using Hubble Space Telescope (HST) WFPC2 images, we have obtained U, B, V, I, and H{alpha} photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner inner Lindblad resonance (IILR). The blue colors and H{alpha} emission for most of these clusters imply very young ages of 115 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30Myr. By estimating the masses of stars in the clusters and comparing with the H{alpha} luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411#1</TD>
            <TD>2011-09-14T19:17:12Z</TD>
            <TD>#Photometry:narrow-band#Globular_Clusters#Open_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1411</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1411</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1411 [2]</TD>
            <TD>UBVIHalpha photometry of NGC 4314 star clusters (Benedict+, 2002)</TD>
            <TD>Using Hubble Space Telescope (HST) WFPC2 images, we have obtained U, B, V, I, and H{alpha} photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner inner Lindblad resonance (IILR). The blue colors and H{alpha} emission for most of these clusters imply very young ages of 115 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30Myr. By estimating the masses of stars in the clusters and comparing with the H{alpha} luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411#2</TD>
            <TD>2011-09-14T19:17:12Z</TD>
            <TD>#Photometry:narrow-band#Globular_Clusters#Open_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1411&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1411</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1411 [table2]</TD>
            <TD>UBVIHalpha photometry of NGC 4314 star clusters (Benedict+, 2002)</TD>
            <TD>Using Hubble Space Telescope (HST) WFPC2 images, we have obtained U, B, V, I, and H{alpha} photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner inner Lindblad resonance (IILR). The blue colors and H{alpha} emission for most of these clusters imply very young ages of 115 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30Myr. By estimating the masses of stars in the clusters and comparing with the H{alpha} luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411#table2</TD>
            <TD>2011-09-14T19:17:12Z</TD>
            <TD>#Photometry:narrow-band#Globular_Clusters#Open_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1411&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1411</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/44 [1]</TD>
            <TD>Redshifts in AWM 7 galaxy cluster (Koranyi+, 2000)</TD>
            <TD>We have measured 492 redshifts (311 new) in the direction of the poor cluster AWM 7 and have identified 179 cluster members (73 new).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44#1</TD>
            <TD>2011-09-14T19:02:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/44</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/44</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/44 [2]</TD>
            <TD>Redshifts in AWM 7 galaxy cluster (Koranyi+, 2000)</TD>
            <TD>We have measured 492 redshifts (311 new) in the direction of the poor cluster AWM 7 and have identified 179 cluster members (73 new).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44#2</TD>
            <TD>2011-09-14T19:02:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/44&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/44</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1411 [1]</TD>
            <TD>UBVIHalpha photometry of NGC 4314 star clusters (Benedict+, 2002)</TD>
            <TD>Using Hubble Space Telescope (HST) WFPC2 images, we have obtained U, B, V, I, and H{alpha} photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner inner Lindblad resonance (IILR). The blue colors and H{alpha} emission for most of these clusters imply very young ages of 115 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30Myr. By estimating the masses of stars in the clusters and comparing with the H{alpha} luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411#1</TD>
            <TD>2011-09-14T19:17:12Z</TD>
            <TD>#Photometry:narrow-band#Globular_Clusters#Open_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1411</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1411</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1411 [2]</TD>
            <TD>UBVIHalpha photometry of NGC 4314 star clusters (Benedict+, 2002)</TD>
            <TD>Using Hubble Space Telescope (HST) WFPC2 images, we have obtained U, B, V, I, and H{alpha} photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner inner Lindblad resonance (IILR). The blue colors and H{alpha} emission for most of these clusters imply very young ages of 115 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30Myr. By estimating the masses of stars in the clusters and comparing with the H{alpha} luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411#2</TD>
            <TD>2011-09-14T19:17:12Z</TD>
            <TD>#Photometry:narrow-band#Globular_Clusters#Open_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1411&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1411</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1411 [table2]</TD>
            <TD>UBVIHalpha photometry of NGC 4314 star clusters (Benedict+, 2002)</TD>
            <TD>Using Hubble Space Telescope (HST) WFPC2 images, we have obtained U, B, V, I, and H{alpha} photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner inner Lindblad resonance (IILR). The blue colors and H{alpha} emission for most of these clusters imply very young ages of 115 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30Myr. By estimating the masses of stars in the clusters and comparing with the H{alpha} luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411#table2</TD>
            <TD>2011-09-14T19:17:12Z</TD>
            <TD>#Photometry:narrow-band#Globular_Clusters#Open_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1411&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1411</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/44 [1]</TD>
            <TD>Redshifts in AWM 7 galaxy cluster (Koranyi+, 2000)</TD>
            <TD>We have measured 492 redshifts (311 new) in the direction of the poor cluster AWM 7 and have identified 179 cluster members (73 new).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44#1</TD>
            <TD>2011-09-14T19:02:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/44</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/44</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/44 [2]</TD>
            <TD>Redshifts in AWM 7 galaxy cluster (Koranyi+, 2000)</TD>
            <TD>We have measured 492 redshifts (311 new) in the direction of the poor cluster AWM 7 and have identified 179 cluster members (73 new).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44#2</TD>
            <TD>2011-09-14T19:02:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/44&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/44</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1411 [1]</TD>
            <TD>UBVIHalpha photometry of NGC 4314 star clusters (Benedict+, 2002)</TD>
            <TD>Using Hubble Space Telescope (HST) WFPC2 images, we have obtained U, B, V, I, and H{alpha} photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner inner Lindblad resonance (IILR). The blue colors and H{alpha} emission for most of these clusters imply very young ages of 115 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30Myr. By estimating the masses of stars in the clusters and comparing with the H{alpha} luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411#1</TD>
            <TD>2011-09-14T19:17:12Z</TD>
            <TD>#Photometry:narrow-band#Globular_Clusters#Open_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1411</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1411</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1411 [2]</TD>
            <TD>UBVIHalpha photometry of NGC 4314 star clusters (Benedict+, 2002)</TD>
            <TD>Using Hubble Space Telescope (HST) WFPC2 images, we have obtained U, B, V, I, and H{alpha} photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner inner Lindblad resonance (IILR). The blue colors and H{alpha} emission for most of these clusters imply very young ages of 115 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30Myr. By estimating the masses of stars in the clusters and comparing with the H{alpha} luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411#2</TD>
            <TD>2011-09-14T19:17:12Z</TD>
            <TD>#Photometry:narrow-band#Globular_Clusters#Open_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1411&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1411</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1411 [table2]</TD>
            <TD>UBVIHalpha photometry of NGC 4314 star clusters (Benedict+, 2002)</TD>
            <TD>Using Hubble Space Telescope (HST) WFPC2 images, we have obtained U, B, V, I, and H{alpha} photometry for 76 star clusters in the nuclear star-forming ring of the barred spiral galaxy NGC 4314. These clusters are likely associated with an inner inner Lindblad resonance (IILR). The blue colors and H{alpha} emission for most of these clusters imply very young ages of 115 Myr. Age estimates based on several reddening-free parameters indicate that the present epoch of star formation has lasted at least 30Myr. By estimating the masses of stars in the clusters and comparing with the H{alpha} luminosity, we conclude that a significant fraction of ongoing star formation in the nuclear ring of NGC 4314 occurs in clusters. The cluster masses identify these as young open clusters, not young globular clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411#table2</TD>
            <TD>2011-09-14T19:17:12Z</TD>
            <TD>#Photometry:narrow-band#Globular_Clusters#Open_Clusters#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1411</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1411&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1411</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/3154 [1]</TD>
            <TD>RV light curves of variable stars in Leo A (Dolphin+, 2002)</TD>
            <TD>We present the results of a search for short-period variable stars in Leo A. We have found 92 candidate variables, including eight candidate RR Lyrae stars. From the RR Lyrae stars, we measure a distance modulus of (m-M)0=24.51+/-0.12, or 0.80+/-0.04Mpc. This discovery of RR Lyrae stars confirms for the first time the presence of an ancient (older than ~11Gyr) population in Leo A, accounting for at least 0.1% of the galaxy's V luminosity. We have also discovered a halo of old (more than ~2Gyr) stars surrounding Leo A, with a scale length roughly 50% larger than that of the dominant young population. We also report the discovery of a large population of Cepheids in Leo A. The median absolute magnitude of our Cepheid sample is M_V_=-1.1, fainter than 96% of SMC and 99% of LMC Cepheids. Their periods are also unusual, with three Cepheids that are deduced to be pulsating in the fundamental mode having periods of under 1 day. Upon examination, these characteristics of the Leo A Cepheid population appear to be a natural extension of the classical Cepheid period-luminosity relations to low metallicity, rather than being indicative of a large population of "anomalous" Cepheids. We demonstrate that the periods and luminosities are consistent with the expected values of low-metallicity blue helium-burning stars (BHeB's), which populate the instability strip at lower luminosities than do higher metallicity BHeB's. Observations of Leo A were obtained at the WIYN 3.5 m telescope on the nights of 20-22 December 2000, using the MIMO camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/3154#1</TD>
            <TD>2011-09-14T19:17:14Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/3154</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/3154</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/3154</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/3154 [2]</TD>
            <TD>RV light curves of variable stars in Leo A (Dolphin+, 2002)</TD>
            <TD>We present the results of a search for short-period variable stars in Leo A. We have found 92 candidate variables, including eight candidate RR Lyrae stars. From the RR Lyrae stars, we measure a distance modulus of (m-M)0=24.51+/-0.12, or 0.80+/-0.04Mpc. This discovery of RR Lyrae stars confirms for the first time the presence of an ancient (older than ~11Gyr) population in Leo A, accounting for at least 0.1% of the galaxy's V luminosity. We have also discovered a halo of old (more than ~2Gyr) stars surrounding Leo A, with a scale length roughly 50% larger than that of the dominant young population. We also report the discovery of a large population of Cepheids in Leo A. The median absolute magnitude of our Cepheid sample is M_V_=-1.1, fainter than 96% of SMC and 99% of LMC Cepheids. Their periods are also unusual, with three Cepheids that are deduced to be pulsating in the fundamental mode having periods of under 1 day. Upon examination, these characteristics of the Leo A Cepheid population appear to be a natural extension of the classical Cepheid period-luminosity relations to low metallicity, rather than being indicative of a large population of "anomalous" Cepheids. We demonstrate that the periods and luminosities are consistent with the expected values of low-metallicity blue helium-burning stars (BHeB's), which populate the instability strip at lower luminosities than do higher metallicity BHeB's. Observations of Leo A were obtained at the WIYN 3.5 m telescope on the nights of 20-22 December 2000, using the MIMO camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/3154#2</TD>
            <TD>2011-09-14T19:17:14Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/3154</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/3154&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/3154</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/44 [1]</TD>
            <TD>Redshifts in AWM 7 galaxy cluster (Koranyi+, 2000)</TD>
            <TD>We have measured 492 redshifts (311 new) in the direction of the poor cluster AWM 7 and have identified 179 cluster members (73 new).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44#1</TD>
            <TD>2011-09-14T19:02:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/44</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/44</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/44 [2]</TD>
            <TD>Redshifts in AWM 7 galaxy cluster (Koranyi+, 2000)</TD>
            <TD>We have measured 492 redshifts (311 new) in the direction of the poor cluster AWM 7 and have identified 179 cluster members (73 new).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44#2</TD>
            <TD>2011-09-14T19:02:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/44</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/44&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/44</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/3154 [1]</TD>
            <TD>RV light curves of variable stars in Leo A (Dolphin+, 2002)</TD>
            <TD>We present the results of a search for short-period variable stars in Leo A. We have found 92 candidate variables, including eight candidate RR Lyrae stars. From the RR Lyrae stars, we measure a distance modulus of (m-M)0=24.51+/-0.12, or 0.80+/-0.04Mpc. This discovery of RR Lyrae stars confirms for the first time the presence of an ancient (older than ~11Gyr) population in Leo A, accounting for at least 0.1% of the galaxy's V luminosity. We have also discovered a halo of old (more than ~2Gyr) stars surrounding Leo A, with a scale length roughly 50% larger than that of the dominant young population. We also report the discovery of a large population of Cepheids in Leo A. The median absolute magnitude of our Cepheid sample is M_V_=-1.1, fainter than 96% of SMC and 99% of LMC Cepheids. Their periods are also unusual, with three Cepheids that are deduced to be pulsating in the fundamental mode having periods of under 1 day. Upon examination, these characteristics of the Leo A Cepheid population appear to be a natural extension of the classical Cepheid period-luminosity relations to low metallicity, rather than being indicative of a large population of "anomalous" Cepheids. We demonstrate that the periods and luminosities are consistent with the expected values of low-metallicity blue helium-burning stars (BHeB's), which populate the instability strip at lower luminosities than do higher metallicity BHeB's. Observations of Leo A were obtained at the WIYN 3.5 m telescope on the nights of 20-22 December 2000, using the MIMO camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/3154#1</TD>
            <TD>2011-09-14T19:17:14Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/3154</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/3154</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/3154</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/3154 [2]</TD>
            <TD>RV light curves of variable stars in Leo A (Dolphin+, 2002)</TD>
            <TD>We present the results of a search for short-period variable stars in Leo A. We have found 92 candidate variables, including eight candidate RR Lyrae stars. From the RR Lyrae stars, we measure a distance modulus of (m-M)0=24.51+/-0.12, or 0.80+/-0.04Mpc. This discovery of RR Lyrae stars confirms for the first time the presence of an ancient (older than ~11Gyr) population in Leo A, accounting for at least 0.1% of the galaxy's V luminosity. We have also discovered a halo of old (more than ~2Gyr) stars surrounding Leo A, with a scale length roughly 50% larger than that of the dominant young population. We also report the discovery of a large population of Cepheids in Leo A. The median absolute magnitude of our Cepheid sample is M_V_=-1.1, fainter than 96% of SMC and 99% of LMC Cepheids. Their periods are also unusual, with three Cepheids that are deduced to be pulsating in the fundamental mode having periods of under 1 day. Upon examination, these characteristics of the Leo A Cepheid population appear to be a natural extension of the classical Cepheid period-luminosity relations to low metallicity, rather than being indicative of a large population of "anomalous" Cepheids. We demonstrate that the periods and luminosities are consistent with the expected values of low-metallicity blue helium-burning stars (BHeB's), which populate the instability strip at lower luminosities than do higher metallicity BHeB's. Observations of Leo A were obtained at the WIYN 3.5 m telescope on the nights of 20-22 December 2000, using the MIMO camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/3154#2</TD>
            <TD>2011-09-14T19:17:14Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/3154</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/3154&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/3154</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/124/127 [1]</TD>
            <TD>Near IR Imaging of Early-Type Galaxies (Pahre, 1999)</TD>
            <TD>An imaging survey of 341 nearby early-type galaxies in the near-infrared K-band atmospheric window (2.2{micron}) is described. The galaxies primarily reside in 13 nearby rich clusters (85%), while some additional galaxies are drawn from loose groups (12%) and the general field (3%). Surface photometry was measured for the entire sample. Detailed corrections were derived from an extensive grid of seeing-convolved r^1/4^ models and then applied to the isophotal surface brightness, aperture magnitude, and ellipticity profiles. Global photometric parameters were derived from this seeing-corrected photometry. More than 25% of the sample has been observed at least twice, and these repeat measurements demonstrate the small internal uncertainties on the derived global photometric parameters. Extensive comparisons with aperture photometry from the literature demonstrate that the photometric system is fully consistent with other photometric systems to &lt;=0.01mag and confirm the estimates of internal random uncertainties. Additional global parameters are drawn from the literature in a homogeneous manner in order to construct a large catalog of galaxy properties: 95% of the galaxies have a velocity dispersion, 69% have a Mg_2_ index, 80% have an optical r_eff_ and {mu}_eff_, 82% have a D_n_, and 81% have a derived optical - infrared color measurement. This large data set provides excellent source material for investigations of the physical origins of the global scaling relations of early-type galaxies, velocity fields in the local universe, and comparisons to higher redshift early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/124/127#1</TD>
            <TD>2011-09-14T19:02:58Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/124/127</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/124/127</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/124/127</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/124/127 [2]</TD>
            <TD>Near IR Imaging of Early-Type Galaxies (Pahre, 1999)</TD>
            <TD>An imaging survey of 341 nearby early-type galaxies in the near-infrared K-band atmospheric window (2.2{micron}) is described. The galaxies primarily reside in 13 nearby rich clusters (85%), while some additional galaxies are drawn from loose groups (12%) and the general field (3%). Surface photometry was measured for the entire sample. Detailed corrections were derived from an extensive grid of seeing-convolved r^1/4^ models and then applied to the isophotal surface brightness, aperture magnitude, and ellipticity profiles. Global photometric parameters were derived from this seeing-corrected photometry. More than 25% of the sample has been observed at least twice, and these repeat measurements demonstrate the small internal uncertainties on the derived global photometric parameters. Extensive comparisons with aperture photometry from the literature demonstrate that the photometric system is fully consistent with other photometric systems to &lt;=0.01mag and confirm the estimates of internal random uncertainties. Additional global parameters are drawn from the literature in a homogeneous manner in order to construct a large catalog of galaxy properties: 95% of the galaxies have a velocity dispersion, 69% have a Mg_2_ index, 80% have an optical r_eff_ and {mu}_eff_, 82% have a D_n_, and 81% have a derived optical - infrared color measurement. This large data set provides excellent source material for investigations of the physical origins of the global scaling relations of early-type galaxies, velocity fields in the local universe, and comparisons to higher redshift early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/124/127#2</TD>
            <TD>2011-09-14T19:02:58Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/124/127</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/124/127&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/124/127</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/393/439 [1]</TD>
            <TD>Catalogue of galaxies towards Abell 496 (Durret+, 2002)</TD>
            <TD>We have derived the galaxy luminosity function (GLF) in the cluster of galaxies Abell 496 from a wide field image in the I band. A single Schechter function reproduces quite well the GLF in the 17&lt;=I_AB_&lt;=22 (-19.5&lt;=M_I_&lt;=eq-14.5) magnitude interval, and the power law index of this function is found to be somewhat steeper in the outer regions than in the inner regions. This result agrees with the idea that faint galaxies are more abundant in the outer regions of clusters, while in the denser inner regions they have partly been accreted by larger galaxies or have been dimmed or even disrupted by tidal interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439#1</TD>
            <TD>2011-09-14T19:18:01Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/393/439</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/439</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/393/439 [2]</TD>
            <TD>Catalogue of galaxies towards Abell 496 (Durret+, 2002)</TD>
            <TD>We have derived the galaxy luminosity function (GLF) in the cluster of galaxies Abell 496 from a wide field image in the I band. A single Schechter function reproduces quite well the GLF in the 17&lt;=I_AB_&lt;=22 (-19.5&lt;=M_I_&lt;=eq-14.5) magnitude interval, and the power law index of this function is found to be somewhat steeper in the outer regions than in the inner regions. This result agrees with the idea that faint galaxies are more abundant in the outer regions of clusters, while in the denser inner regions they have partly been accreted by larger galaxies or have been dimmed or even disrupted by tidal interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439#2</TD>
            <TD>2011-09-14T19:18:01Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/393/439&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/439</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/393/439 [catalog]</TD>
            <TD>Catalogue of galaxies towards Abell 496 (Durret+, 2002)</TD>
            <TD>We have derived the galaxy luminosity function (GLF) in the cluster of galaxies Abell 496 from a wide field image in the I band. A single Schechter function reproduces quite well the GLF in the 17&lt;=I_AB_&lt;=22 (-19.5&lt;=M_I_&lt;=eq-14.5) magnitude interval, and the power law index of this function is found to be somewhat steeper in the outer regions than in the inner regions. This result agrees with the idea that faint galaxies are more abundant in the outer regions of clusters, while in the denser inner regions they have partly been accreted by larger galaxies or have been dimmed or even disrupted by tidal interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439#catalog</TD>
            <TD>2011-09-14T19:18:01Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/393/439&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/439</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/124/127 [1]</TD>
            <TD>Near IR Imaging of Early-Type Galaxies (Pahre, 1999)</TD>
            <TD>An imaging survey of 341 nearby early-type galaxies in the near-infrared K-band atmospheric window (2.2{micron}) is described. The galaxies primarily reside in 13 nearby rich clusters (85%), while some additional galaxies are drawn from loose groups (12%) and the general field (3%). Surface photometry was measured for the entire sample. Detailed corrections were derived from an extensive grid of seeing-convolved r^1/4^ models and then applied to the isophotal surface brightness, aperture magnitude, and ellipticity profiles. Global photometric parameters were derived from this seeing-corrected photometry. More than 25% of the sample has been observed at least twice, and these repeat measurements demonstrate the small internal uncertainties on the derived global photometric parameters. Extensive comparisons with aperture photometry from the literature demonstrate that the photometric system is fully consistent with other photometric systems to &lt;=0.01mag and confirm the estimates of internal random uncertainties. Additional global parameters are drawn from the literature in a homogeneous manner in order to construct a large catalog of galaxy properties: 95% of the galaxies have a velocity dispersion, 69% have a Mg_2_ index, 80% have an optical r_eff_ and {mu}_eff_, 82% have a D_n_, and 81% have a derived optical - infrared color measurement. This large data set provides excellent source material for investigations of the physical origins of the global scaling relations of early-type galaxies, velocity fields in the local universe, and comparisons to higher redshift early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/124/127#1</TD>
            <TD>2011-09-14T19:02:58Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/124/127</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/124/127</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/124/127</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/124/127 [2]</TD>
            <TD>Near IR Imaging of Early-Type Galaxies (Pahre, 1999)</TD>
            <TD>An imaging survey of 341 nearby early-type galaxies in the near-infrared K-band atmospheric window (2.2{micron}) is described. The galaxies primarily reside in 13 nearby rich clusters (85%), while some additional galaxies are drawn from loose groups (12%) and the general field (3%). Surface photometry was measured for the entire sample. Detailed corrections were derived from an extensive grid of seeing-convolved r^1/4^ models and then applied to the isophotal surface brightness, aperture magnitude, and ellipticity profiles. Global photometric parameters were derived from this seeing-corrected photometry. More than 25% of the sample has been observed at least twice, and these repeat measurements demonstrate the small internal uncertainties on the derived global photometric parameters. Extensive comparisons with aperture photometry from the literature demonstrate that the photometric system is fully consistent with other photometric systems to &lt;=0.01mag and confirm the estimates of internal random uncertainties. Additional global parameters are drawn from the literature in a homogeneous manner in order to construct a large catalog of galaxy properties: 95% of the galaxies have a velocity dispersion, 69% have a Mg_2_ index, 80% have an optical r_eff_ and {mu}_eff_, 82% have a D_n_, and 81% have a derived optical - infrared color measurement. This large data set provides excellent source material for investigations of the physical origins of the global scaling relations of early-type galaxies, velocity fields in the local universe, and comparisons to higher redshift early-type galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/124/127#2</TD>
            <TD>2011-09-14T19:02:58Z</TD>
            <TD>#Galaxies#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/124/127</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/124/127&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/124/127</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/393/439 [1]</TD>
            <TD>Catalogue of galaxies towards Abell 496 (Durret+, 2002)</TD>
            <TD>We have derived the galaxy luminosity function (GLF) in the cluster of galaxies Abell 496 from a wide field image in the I band. A single Schechter function reproduces quite well the GLF in the 17&lt;=I_AB_&lt;=22 (-19.5&lt;=M_I_&lt;=eq-14.5) magnitude interval, and the power law index of this function is found to be somewhat steeper in the outer regions than in the inner regions. This result agrees with the idea that faint galaxies are more abundant in the outer regions of clusters, while in the denser inner regions they have partly been accreted by larger galaxies or have been dimmed or even disrupted by tidal interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439#1</TD>
            <TD>2011-09-14T19:18:01Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/393/439</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/439</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/393/439 [2]</TD>
            <TD>Catalogue of galaxies towards Abell 496 (Durret+, 2002)</TD>
            <TD>We have derived the galaxy luminosity function (GLF) in the cluster of galaxies Abell 496 from a wide field image in the I band. A single Schechter function reproduces quite well the GLF in the 17&lt;=I_AB_&lt;=22 (-19.5&lt;=M_I_&lt;=eq-14.5) magnitude interval, and the power law index of this function is found to be somewhat steeper in the outer regions than in the inner regions. This result agrees with the idea that faint galaxies are more abundant in the outer regions of clusters, while in the denser inner regions they have partly been accreted by larger galaxies or have been dimmed or even disrupted by tidal interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439#2</TD>
            <TD>2011-09-14T19:18:01Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/393/439&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/439</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/393/439 [catalog]</TD>
            <TD>Catalogue of galaxies towards Abell 496 (Durret+, 2002)</TD>
            <TD>We have derived the galaxy luminosity function (GLF) in the cluster of galaxies Abell 496 from a wide field image in the I band. A single Schechter function reproduces quite well the GLF in the 17&lt;=I_AB_&lt;=22 (-19.5&lt;=M_I_&lt;=eq-14.5) magnitude interval, and the power law index of this function is found to be somewhat steeper in the outer regions than in the inner regions. This result agrees with the idea that faint galaxies are more abundant in the outer regions of clusters, while in the denser inner regions they have partly been accreted by larger galaxies or have been dimmed or even disrupted by tidal interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439#catalog</TD>
            <TD>2011-09-14T19:18:01Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/393/439&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/439</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/360/439 [1]</TD>
            <TD>Stellar and ionized gas kinematics in NGC 4672 (Sarzi+, 2000)</TD>
            <TD>We report the case of the early-type disk galaxy NGC 4672 as a new example of a galaxy characterized by the orthogonal geometrical decoupling between bulge and disk. The morphological features of this galaxy are discussed as well as the velocity curves and velocity dispersion profiles of stars and ionized gas along both its major and minor axis. We conclude that NGC 4672 has structural (i.e. a bulge elongated perpendicularly to the disk) and kinematical (i.e. a stellar core rotating perpendicularly to the disk) properties similar to those of the Sa NGC 4698. The presence of the isolated core suggests that the disk component is the end result of the acquisition of external material in polar orbits around a pre-existing oblate spheroid as in the case of the ring component of AM 2020-504, the prototype of polar ring ellipticals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/360/439#1</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/360/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/360/439</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/360/439</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/360/439 [2]</TD>
            <TD>Stellar and ionized gas kinematics in NGC 4672 (Sarzi+, 2000)</TD>
            <TD>We report the case of the early-type disk galaxy NGC 4672 as a new example of a galaxy characterized by the orthogonal geometrical decoupling between bulge and disk. The morphological features of this galaxy are discussed as well as the velocity curves and velocity dispersion profiles of stars and ionized gas along both its major and minor axis. We conclude that NGC 4672 has structural (i.e. a bulge elongated perpendicularly to the disk) and kinematical (i.e. a stellar core rotating perpendicularly to the disk) properties similar to those of the Sa NGC 4698. The presence of the isolated core suggests that the disk component is the end result of the acquisition of external material in polar orbits around a pre-existing oblate spheroid as in the case of the ring component of AM 2020-504, the prototype of polar ring ellipticals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/360/439#2</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/360/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/360/439&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/360/439</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/393/439 [1]</TD>
            <TD>Catalogue of galaxies towards Abell 496 (Durret+, 2002)</TD>
            <TD>We have derived the galaxy luminosity function (GLF) in the cluster of galaxies Abell 496 from a wide field image in the I band. A single Schechter function reproduces quite well the GLF in the 17&lt;=I_AB_&lt;=22 (-19.5&lt;=M_I_&lt;=eq-14.5) magnitude interval, and the power law index of this function is found to be somewhat steeper in the outer regions than in the inner regions. This result agrees with the idea that faint galaxies are more abundant in the outer regions of clusters, while in the denser inner regions they have partly been accreted by larger galaxies or have been dimmed or even disrupted by tidal interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439#1</TD>
            <TD>2011-09-14T19:18:01Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/393/439</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/439</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/393/439 [2]</TD>
            <TD>Catalogue of galaxies towards Abell 496 (Durret+, 2002)</TD>
            <TD>We have derived the galaxy luminosity function (GLF) in the cluster of galaxies Abell 496 from a wide field image in the I band. A single Schechter function reproduces quite well the GLF in the 17&lt;=I_AB_&lt;=22 (-19.5&lt;=M_I_&lt;=eq-14.5) magnitude interval, and the power law index of this function is found to be somewhat steeper in the outer regions than in the inner regions. This result agrees with the idea that faint galaxies are more abundant in the outer regions of clusters, while in the denser inner regions they have partly been accreted by larger galaxies or have been dimmed or even disrupted by tidal interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439#2</TD>
            <TD>2011-09-14T19:18:01Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/393/439&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/439</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/393/439 [catalog]</TD>
            <TD>Catalogue of galaxies towards Abell 496 (Durret+, 2002)</TD>
            <TD>We have derived the galaxy luminosity function (GLF) in the cluster of galaxies Abell 496 from a wide field image in the I band. A single Schechter function reproduces quite well the GLF in the 17&lt;=I_AB_&lt;=22 (-19.5&lt;=M_I_&lt;=eq-14.5) magnitude interval, and the power law index of this function is found to be somewhat steeper in the outer regions than in the inner regions. This result agrees with the idea that faint galaxies are more abundant in the outer regions of clusters, while in the denser inner regions they have partly been accreted by larger galaxies or have been dimmed or even disrupted by tidal interactions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439#catalog</TD>
            <TD>2011-09-14T19:18:01Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/393/439</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/393/439&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/393/439</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/360/439 [1]</TD>
            <TD>Stellar and ionized gas kinematics in NGC 4672 (Sarzi+, 2000)</TD>
            <TD>We report the case of the early-type disk galaxy NGC 4672 as a new example of a galaxy characterized by the orthogonal geometrical decoupling between bulge and disk. The morphological features of this galaxy are discussed as well as the velocity curves and velocity dispersion profiles of stars and ionized gas along both its major and minor axis. We conclude that NGC 4672 has structural (i.e. a bulge elongated perpendicularly to the disk) and kinematical (i.e. a stellar core rotating perpendicularly to the disk) properties similar to those of the Sa NGC 4698. The presence of the isolated core suggests that the disk component is the end result of the acquisition of external material in polar orbits around a pre-existing oblate spheroid as in the case of the ring component of AM 2020-504, the prototype of polar ring ellipticals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/360/439#1</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/360/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/360/439</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/360/439</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/360/439 [2]</TD>
            <TD>Stellar and ionized gas kinematics in NGC 4672 (Sarzi+, 2000)</TD>
            <TD>We report the case of the early-type disk galaxy NGC 4672 as a new example of a galaxy characterized by the orthogonal geometrical decoupling between bulge and disk. The morphological features of this galaxy are discussed as well as the velocity curves and velocity dispersion profiles of stars and ionized gas along both its major and minor axis. We conclude that NGC 4672 has structural (i.e. a bulge elongated perpendicularly to the disk) and kinematical (i.e. a stellar core rotating perpendicularly to the disk) properties similar to those of the Sa NGC 4698. The presence of the isolated core suggests that the disk component is the end result of the acquisition of external material in polar orbits around a pre-existing oblate spheroid as in the case of the ring component of AM 2020-504, the prototype of polar ring ellipticals.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/360/439#2</TD>
            <TD>2011-09-14T19:03:23Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/360/439</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/360/439&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/360/439</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/114/820 [1]</TD>
            <TD>Supernovae host galaxies classification (van den Bergh+, 2002)</TD>
            <TD>Classifications on the DDO system are given for the host galaxies of 177 supernovae (SNe) that have been discovered since 1997 during the course of the Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope. Whereas SNe Ia occur in all galaxy types, it is found, at a high level of statistical confidence, that SNe Ib, Ic, and II are strongly concentrated in late-type galaxies. However, attention is drawn to a possible exception provided by SN 2001I. This SN IIn occurred in the E2 galaxy UGC 2836, which was not expected to harbor a massive young supernova progenitor.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820#1</TD>
            <TD>2011-09-14T19:18:30Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/114/820</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/820</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/114/820 [2]</TD>
            <TD>Supernovae host galaxies classification (van den Bergh+, 2002)</TD>
            <TD>Classifications on the DDO system are given for the host galaxies of 177 supernovae (SNe) that have been discovered since 1997 during the course of the Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope. Whereas SNe Ia occur in all galaxy types, it is found, at a high level of statistical confidence, that SNe Ib, Ic, and II are strongly concentrated in late-type galaxies. However, attention is drawn to a possible exception provided by SN 2001I. This SN IIn occurred in the E2 galaxy UGC 2836, which was not expected to harbor a massive young supernova progenitor.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820#2</TD>
            <TD>2011-09-14T19:18:30Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/114/820&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/820</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/114/820 [table1]</TD>
            <TD>Supernovae host galaxies classification (van den Bergh+, 2002)</TD>
            <TD>Classifications on the DDO system are given for the host galaxies of 177 supernovae (SNe) that have been discovered since 1997 during the course of the Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope. Whereas SNe Ia occur in all galaxy types, it is found, at a high level of statistical confidence, that SNe Ib, Ic, and II are strongly concentrated in late-type galaxies. However, attention is drawn to a possible exception provided by SN 2001I. This SN IIn occurred in the E2 galaxy UGC 2836, which was not expected to harbor a massive young supernova progenitor.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820#table1</TD>
            <TD>2011-09-14T19:18:30Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/114/820&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/820</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/120/1306 [1]</TD>
            <TD>NGC 628 H II regions (Lelievre+, 2000)</TD>
            <TD>Employing deep H{alpha} narrowband imagery, we identified and measured the fluxes of 137 small H II regions in the extreme outer disk (R&gt;=R_25_) of the nearly face-on, Sc I galaxy NGC 628. A majority of these H II regions are located in two faint, outer spiral arms visible in H I maps. The faintest H II regions that could be measured have fluxes of only a few times 10^-16^ergs/cm^2^/s, which correspond to luminosities of 10^36^ergs/s, or a fraction of the Orion Nebula luminosity. The most distant object detected is at R~27kpc from the galaxy center. The massive star formation rate, as measured from the azimuthally averaged H{alpha} flux, is consistent with a monotonic decrease as far as R~1.3R_25_ (20kpc), where there is a sharp drop. The Schmidt law for the whole disk of NGC 628 corresponds to a relatively steep power law with n=2.9+/-0.2, but it "fails" below {Sigma}gas&lt;=4M_{sun}_/pc^2^; the index depends strongly on the CO data used. We derived the luminosity function (LF) of 598 H II regions over the whole disk, and we compared the shapes of the cumulative LFs between R&gt;=R_25_ and R&lt;R_25_; the LF of the outer regions is significantly steeper than that of the inner regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/1306#1</TD>
            <TD>2011-09-14T19:03:54Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/1306</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/120/1306</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/1306</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/120/1306 [2]</TD>
            <TD>NGC 628 H II regions (Lelievre+, 2000)</TD>
            <TD>Employing deep H{alpha} narrowband imagery, we identified and measured the fluxes of 137 small H II regions in the extreme outer disk (R&gt;=R_25_) of the nearly face-on, Sc I galaxy NGC 628. A majority of these H II regions are located in two faint, outer spiral arms visible in H I maps. The faintest H II regions that could be measured have fluxes of only a few times 10^-16^ergs/cm^2^/s, which correspond to luminosities of 10^36^ergs/s, or a fraction of the Orion Nebula luminosity. The most distant object detected is at R~27kpc from the galaxy center. The massive star formation rate, as measured from the azimuthally averaged H{alpha} flux, is consistent with a monotonic decrease as far as R~1.3R_25_ (20kpc), where there is a sharp drop. The Schmidt law for the whole disk of NGC 628 corresponds to a relatively steep power law with n=2.9+/-0.2, but it "fails" below {Sigma}gas&lt;=4M_{sun}_/pc^2^; the index depends strongly on the CO data used. We derived the luminosity function (LF) of 598 H II regions over the whole disk, and we compared the shapes of the cumulative LFs between R&gt;=R_25_ and R&lt;R_25_; the LF of the outer regions is significantly steeper than that of the inner regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/1306#2</TD>
            <TD>2011-09-14T19:03:54Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/1306</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/120/1306&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/1306</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/120/1306 [1]</TD>
            <TD>NGC 628 H II regions (Lelievre+, 2000)</TD>
            <TD>Employing deep H{alpha} narrowband imagery, we identified and measured the fluxes of 137 small H II regions in the extreme outer disk (R&gt;=R_25_) of the nearly face-on, Sc I galaxy NGC 628. A majority of these H II regions are located in two faint, outer spiral arms visible in H I maps. The faintest H II regions that could be measured have fluxes of only a few times 10^-16^ergs/cm^2^/s, which correspond to luminosities of 10^36^ergs/s, or a fraction of the Orion Nebula luminosity. The most distant object detected is at R~27kpc from the galaxy center. The massive star formation rate, as measured from the azimuthally averaged H{alpha} flux, is consistent with a monotonic decrease as far as R~1.3R_25_ (20kpc), where there is a sharp drop. The Schmidt law for the whole disk of NGC 628 corresponds to a relatively steep power law with n=2.9+/-0.2, but it "fails" below {Sigma}gas&lt;=4M_{sun}_/pc^2^; the index depends strongly on the CO data used. We derived the luminosity function (LF) of 598 H II regions over the whole disk, and we compared the shapes of the cumulative LFs between R&gt;=R_25_ and R&lt;R_25_; the LF of the outer regions is significantly steeper than that of the inner regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/1306#1</TD>
            <TD>2011-09-14T19:03:54Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/1306</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/120/1306</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/1306</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/120/1306 [2]</TD>
            <TD>NGC 628 H II regions (Lelievre+, 2000)</TD>
            <TD>Employing deep H{alpha} narrowband imagery, we identified and measured the fluxes of 137 small H II regions in the extreme outer disk (R&gt;=R_25_) of the nearly face-on, Sc I galaxy NGC 628. A majority of these H II regions are located in two faint, outer spiral arms visible in H I maps. The faintest H II regions that could be measured have fluxes of only a few times 10^-16^ergs/cm^2^/s, which correspond to luminosities of 10^36^ergs/s, or a fraction of the Orion Nebula luminosity. The most distant object detected is at R~27kpc from the galaxy center. The massive star formation rate, as measured from the azimuthally averaged H{alpha} flux, is consistent with a monotonic decrease as far as R~1.3R_25_ (20kpc), where there is a sharp drop. The Schmidt law for the whole disk of NGC 628 corresponds to a relatively steep power law with n=2.9+/-0.2, but it "fails" below {Sigma}gas&lt;=4M_{sun}_/pc^2^; the index depends strongly on the CO data used. We derived the luminosity function (LF) of 598 H II regions over the whole disk, and we compared the shapes of the cumulative LFs between R&gt;=R_25_ and R&lt;R_25_; the LF of the outer regions is significantly steeper than that of the inner regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/1306#2</TD>
            <TD>2011-09-14T19:03:54Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Sep-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/1306</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/120/1306&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/1306</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/310/715 [1]</TD>
            <TD>Tucana dwarf galaxy VI photometry (Castellani+, 1996)</TD>
            <TD>We present deep CCD photometry for the dwarf galaxy in Tucana (l=323, b=-47.4). The data indicate that the galaxy is dominated by an intermediate/old stellar population with metallicity similar to that of the galactic globular clusters NGC 6752 and NGC 7089 (M2) (we find [Fe/H]=~-1.56). The distance modulus we derived, (m-M)_V_=~24.72+/-0.2, makes clear that this galaxy belongs to the Local Gro up. Tucana is clearly different from other dwarf galaxies, such as Leo I (Lee et al., 1993AJ....106.1420L), or Phoenix (Ortolani and Gratton, 1988PASP..100.1405O), because there is no evidence of a young stellar population (t&lt;=5Gyrs) We suggest that the Tucana Galaxy is a genuine dwarf spheroidal in which no recent burst of star formation occurred.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/715#1</TD>
            <TD>2011-09-14T19:04:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/310/715</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/310/715</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/310/715 [2]</TD>
            <TD>Tucana dwarf galaxy VI photometry (Castellani+, 1996)</TD>
            <TD>We present deep CCD photometry for the dwarf galaxy in Tucana (l=323, b=-47.4). The data indicate that the galaxy is dominated by an intermediate/old stellar population with metallicity similar to that of the galactic globular clusters NGC 6752 and NGC 7089 (M2) (we find [Fe/H]=~-1.56). The distance modulus we derived, (m-M)_V_=~24.72+/-0.2, makes clear that this galaxy belongs to the Local Gro up. Tucana is clearly different from other dwarf galaxies, such as Leo I (Lee et al., 1993AJ....106.1420L), or Phoenix (Ortolani and Gratton, 1988PASP..100.1405O), because there is no evidence of a young stellar population (t&lt;=5Gyrs) We suggest that the Tucana Galaxy is a genuine dwarf spheroidal in which no recent burst of star formation occurred.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/715#2</TD>
            <TD>2011-09-14T19:04:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/310/715&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/310/715</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/310/715 [1]</TD>
            <TD>Tucana dwarf galaxy VI photometry (Castellani+, 1996)</TD>
            <TD>We present deep CCD photometry for the dwarf galaxy in Tucana (l=323, b=-47.4). The data indicate that the galaxy is dominated by an intermediate/old stellar population with metallicity similar to that of the galactic globular clusters NGC 6752 and NGC 7089 (M2) (we find [Fe/H]=~-1.56). The distance modulus we derived, (m-M)_V_=~24.72+/-0.2, makes clear that this galaxy belongs to the Local Gro up. Tucana is clearly different from other dwarf galaxies, such as Leo I (Lee et al., 1993AJ....106.1420L), or Phoenix (Ortolani and Gratton, 1988PASP..100.1405O), because there is no evidence of a young stellar population (t&lt;=5Gyrs) We suggest that the Tucana Galaxy is a genuine dwarf spheroidal in which no recent burst of star formation occurred.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/715#1</TD>
            <TD>2011-09-14T19:04:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/310/715</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/310/715</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/310/715 [2]</TD>
            <TD>Tucana dwarf galaxy VI photometry (Castellani+, 1996)</TD>
            <TD>We present deep CCD photometry for the dwarf galaxy in Tucana (l=323, b=-47.4). The data indicate that the galaxy is dominated by an intermediate/old stellar population with metallicity similar to that of the galactic globular clusters NGC 6752 and NGC 7089 (M2) (we find [Fe/H]=~-1.56). The distance modulus we derived, (m-M)_V_=~24.72+/-0.2, makes clear that this galaxy belongs to the Local Gro up. Tucana is clearly different from other dwarf galaxies, such as Leo I (Lee et al., 1993AJ....106.1420L), or Phoenix (Ortolani and Gratton, 1988PASP..100.1405O), because there is no evidence of a young stellar population (t&lt;=5Gyrs) We suggest that the Tucana Galaxy is a genuine dwarf spheroidal in which no recent burst of star formation occurred.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/715#2</TD>
            <TD>2011-09-14T19:04:23Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+A/310/715</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/310/715&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/310/715</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/114/820 [1]</TD>
            <TD>Supernovae host galaxies classification (van den Bergh+, 2002)</TD>
            <TD>Classifications on the DDO system are given for the host galaxies of 177 supernovae (SNe) that have been discovered since 1997 during the course of the Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope. Whereas SNe Ia occur in all galaxy types, it is found, at a high level of statistical confidence, that SNe Ib, Ic, and II are strongly concentrated in late-type galaxies. However, attention is drawn to a possible exception provided by SN 2001I. This SN IIn occurred in the E2 galaxy UGC 2836, which was not expected to harbor a massive young supernova progenitor.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820#1</TD>
            <TD>2011-09-14T19:18:30Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/114/820</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/820</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/114/820 [2]</TD>
            <TD>Supernovae host galaxies classification (van den Bergh+, 2002)</TD>
            <TD>Classifications on the DDO system are given for the host galaxies of 177 supernovae (SNe) that have been discovered since 1997 during the course of the Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope. Whereas SNe Ia occur in all galaxy types, it is found, at a high level of statistical confidence, that SNe Ib, Ic, and II are strongly concentrated in late-type galaxies. However, attention is drawn to a possible exception provided by SN 2001I. This SN IIn occurred in the E2 galaxy UGC 2836, which was not expected to harbor a massive young supernova progenitor.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820#2</TD>
            <TD>2011-09-14T19:18:30Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/114/820&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/820</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/114/820 [table1]</TD>
            <TD>Supernovae host galaxies classification (van den Bergh+, 2002)</TD>
            <TD>Classifications on the DDO system are given for the host galaxies of 177 supernovae (SNe) that have been discovered since 1997 during the course of the Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope. Whereas SNe Ia occur in all galaxy types, it is found, at a high level of statistical confidence, that SNe Ib, Ic, and II are strongly concentrated in late-type galaxies. However, attention is drawn to a possible exception provided by SN 2001I. This SN IIn occurred in the E2 galaxy UGC 2836, which was not expected to harbor a massive young supernova progenitor.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820#table1</TD>
            <TD>2011-09-14T19:18:30Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/114/820&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/820</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/145/111 [1]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#1</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/145/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/145/111 [2]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#2</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/145/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/145/111 [colour]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#colour</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/145/111&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/145/111 [ubvimag]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#ubvimag</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/145/111&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PASP/114/820 [1]</TD>
            <TD>Supernovae host galaxies classification (van den Bergh+, 2002)</TD>
            <TD>Classifications on the DDO system are given for the host galaxies of 177 supernovae (SNe) that have been discovered since 1997 during the course of the Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope. Whereas SNe Ia occur in all galaxy types, it is found, at a high level of statistical confidence, that SNe Ib, Ic, and II are strongly concentrated in late-type galaxies. However, attention is drawn to a possible exception provided by SN 2001I. This SN IIn occurred in the E2 galaxy UGC 2836, which was not expected to harbor a massive young supernova progenitor.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820#1</TD>
            <TD>2011-09-14T19:18:30Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PASP/114/820</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/820</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PASP/114/820 [2]</TD>
            <TD>Supernovae host galaxies classification (van den Bergh+, 2002)</TD>
            <TD>Classifications on the DDO system are given for the host galaxies of 177 supernovae (SNe) that have been discovered since 1997 during the course of the Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope. Whereas SNe Ia occur in all galaxy types, it is found, at a high level of statistical confidence, that SNe Ib, Ic, and II are strongly concentrated in late-type galaxies. However, attention is drawn to a possible exception provided by SN 2001I. This SN IIn occurred in the E2 galaxy UGC 2836, which was not expected to harbor a massive young supernova progenitor.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820#2</TD>
            <TD>2011-09-14T19:18:30Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PASP/114/820&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/820</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PASP/114/820 [table1]</TD>
            <TD>Supernovae host galaxies classification (van den Bergh+, 2002)</TD>
            <TD>Classifications on the DDO system are given for the host galaxies of 177 supernovae (SNe) that have been discovered since 1997 during the course of the Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope. Whereas SNe Ia occur in all galaxy types, it is found, at a high level of statistical confidence, that SNe Ib, Ic, and II are strongly concentrated in late-type galaxies. However, attention is drawn to a possible exception provided by SN 2001I. This SN IIn occurred in the E2 galaxy UGC 2836, which was not expected to harbor a massive young supernova progenitor.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820#table1</TD>
            <TD>2011-09-14T19:18:30Z</TD>
            <TD>#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/PASP/114/820</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PASP/114/820&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PASP/114/820</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/avo.rad [1]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#1</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/avo.rad</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/avo.rad [2]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#2</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/avo.rad&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/avo.rad [wsrt]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#wsrt</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/avo.rad&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/avo.rad [catalog]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#catalog</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/avo.rad&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/avo.rad [1]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#1</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/avo.rad</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/avo.rad [2]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#2</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/avo.rad&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/avo.rad [wsrt]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#wsrt</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/avo.rad&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/avo.rad [catalog]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#catalog</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/avo.rad&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/145/111 [1]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#1</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/145/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/145/111 [2]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#2</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/145/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/145/111 [colour]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#colour</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/145/111&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/145/111 [ubvimag]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#ubvimag</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/145/111&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>B/avo.rad [1]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#1</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=B/avo.rad</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>B/avo.rad [2]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#2</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=B/avo.rad&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/avo.rad [wsrt]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#wsrt</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/avo.rad&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>B/avo.rad [catalog]</TD>
            <TD>MERLIN+VLA images of HDF/HFF sources (Muxlow+, 2003)</TD>
            <TD>18 days of MERLIN data and 42 hours of A-array VLA data at 1.4 GHz have been combined to image a 10 arcminute field centred on the Hubble Deep Field. This area includes both the Hubble Deep and Flanking Fields. A complete sample of 92 sources with flux densities above 40{mu}Jy have been detected using the VLA data, and imaged with the MERLIN+VLA combination at resolutions of 0.2, 0.3 and 0.5 arcsecond. These are the most sensitive 1.4 GHz images yet made, with rms noise levels of 3.3{mu}Jy/beam in the 0.2 arcsecond images. Virtually all the objects are resolved by the MERLIN+VLA combination images showing that they have angular sizes in the range 0.2 to 3 arcseconds, typically smaller than the sizes of the optical galaxy images. In addition to the imaging of 92 sources found with the VLA alone, the central 3 arcminutes, which encloses the HDF, has been separately imaged with the MERLIN+VLA combination at the full 3.3{mu}Jy/beam sensitivity to search for compact sources fainter than 40{mu}Jy. No additional sources were found that were not previously detected by the VLA, indicating that such sources are heavily resolved with MERLIN and hence must have typical angular sizes &gt;0.5 arcseconds. In addition to the images, high quality astrometry is an equally important product of this work allowing reliable source identification in a crowded field. Radio sources associated with compact galaxies have been used to align both the HST WFPC2 frames and a CFHT optical field to the ICRF. The HST optical field has been aligned to better than 50 mas in the Deep Field itself, and to ~150 mas in the outer parts of the Flanking Fields. The proportion of starburst systems is found to increase with decreasing source strength. At fluxes below 100{mu}Jy in excess of 70% of the {mu}Jy sources are found to be starburst type systems associated with major disc galaxies in the redshift range 0.3 - 1.3. Some 40% of the brighter sources are found to be intermediate luminosity AGN systems identified with galxies in a similar redshift range. Around 85% of the sources are identified with galaxies brighter than I=25mag. The remaining 15% are associated with optically faint systems close to or beyond the HDF limit; many of these may be dust-shrouded starburst galaxies at high redshift (z&gt;3). Approaching half the sources in the 10 arcminute field are detected in X-rays by the Chandra Satellite. The X-ray detection rate appears to be uncorrelated with the radio source classification.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad#catalog</TD>
            <TD>2011-09-14T19:18:45Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/B/avo.rad</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=B/avo.rad&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?B/avo.rad</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/145/111 [1]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#1</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/145/111</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/145/111 [2]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#2</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/145/111&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/145/111 [colour]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#colour</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/145/111&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/145/111 [ubvimag]</TD>
            <TD>HDF-South catalogue of galaxies (Volonteri+, 2000)</TD>
            <TD>We present a catalogue of galaxies in the HDF-S, created using the public version 1 images of the WFPC2 data. We created a catalogue with 4 pass-band (I(814), V(606), B(450), U(300). In V(606), B(450), U(300) and I(814), for each galaxy the catalogue gives photometric parameters. For the I(814), we estimated also the colours and for I(814)&lt;26, the petrosian radius, the mean surface brightness within the petrosian radius, light concentration indexes, that is C_eta_ and C_abr_, and the asymmetry index as computed by Abraham software.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111#ubvimag</TD>
            <TD>2011-09-14T19:04:56Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-May-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/145/111</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/145/111&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/145/111</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/390/863 [1]</TD>
            <TD>CCD R Photometry of WHISP Dwarf Galaxies (Swaters, 2002)</TD>
            <TD>R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B-band observations are given as well.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863#1</TD>
            <TD>2011-09-14T19:18:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/390/863</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/863</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/390/863 [2]</TD>
            <TD>CCD R Photometry of WHISP Dwarf Galaxies (Swaters, 2002)</TD>
            <TD>R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B-band observations are given as well.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863#2</TD>
            <TD>2011-09-14T19:18:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/390/863&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/863</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/390/863 [tablea1]</TD>
            <TD>CCD R Photometry of WHISP Dwarf Galaxies (Swaters, 2002)</TD>
            <TD>R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B-band observations are given as well.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863#tablea1</TD>
            <TD>2011-09-14T19:18:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/390/863&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/863</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/120/2747 [1]</TD>
            <TD>HDF-South WFPC2 observations (Casertano+, 2000)</TD>
            <TD>The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z&gt;2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747#1</TD>
            <TD>2011-09-14T19:07:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/120/2747</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2747</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/120/2747 [2]</TD>
            <TD>HDF-South WFPC2 observations (Casertano+, 2000)</TD>
            <TD>The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z&gt;2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747#2</TD>
            <TD>2011-09-14T19:07:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/120/2747&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2747</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/120/2747 [table6]</TD>
            <TD>HDF-South WFPC2 observations (Casertano+, 2000)</TD>
            <TD>The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z&gt;2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747#table6</TD>
            <TD>2011-09-14T19:07:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/120/2747&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2747</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/120/2747 [1]</TD>
            <TD>HDF-South WFPC2 observations (Casertano+, 2000)</TD>
            <TD>The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z&gt;2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747#1</TD>
            <TD>2011-09-14T19:07:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/120/2747</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2747</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/120/2747 [2]</TD>
            <TD>HDF-South WFPC2 observations (Casertano+, 2000)</TD>
            <TD>The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z&gt;2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747#2</TD>
            <TD>2011-09-14T19:07:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/120/2747&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2747</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/120/2747 [table6]</TD>
            <TD>HDF-South WFPC2 observations (Casertano+, 2000)</TD>
            <TD>The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z&gt;2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747#table6</TD>
            <TD>2011-09-14T19:07:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/120/2747&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2747</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/390/863 [1]</TD>
            <TD>CCD R Photometry of WHISP Dwarf Galaxies (Swaters, 2002)</TD>
            <TD>R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B-band observations are given as well.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863#1</TD>
            <TD>2011-09-14T19:18:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/390/863</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/863</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/390/863 [2]</TD>
            <TD>CCD R Photometry of WHISP Dwarf Galaxies (Swaters, 2002)</TD>
            <TD>R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B-band observations are given as well.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863#2</TD>
            <TD>2011-09-14T19:18:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/390/863&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/863</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/390/863 [tablea1]</TD>
            <TD>CCD R Photometry of WHISP Dwarf Galaxies (Swaters, 2002)</TD>
            <TD>R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B-band observations are given as well.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863#tablea1</TD>
            <TD>2011-09-14T19:18:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/390/863&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/863</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/120/2747 [1]</TD>
            <TD>HDF-South WFPC2 observations (Casertano+, 2000)</TD>
            <TD>The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z&gt;2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747#1</TD>
            <TD>2011-09-14T19:07:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/120/2747</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2747</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/120/2747 [2]</TD>
            <TD>HDF-South WFPC2 observations (Casertano+, 2000)</TD>
            <TD>The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z&gt;2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747#2</TD>
            <TD>2011-09-14T19:07:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/120/2747&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2747</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/120/2747 [table6]</TD>
            <TD>HDF-South WFPC2 observations (Casertano+, 2000)</TD>
            <TD>The Hubble Deep Field South (HDF-S) observations targeted a high Galactic latitude field near QSO J2233-606. We present Wide Field Planetary Camera 2 observations of the field in four wide bandpasses centered at roughly 300, 450, 606, and 814 nm. Observations, data reduction procedures, and noise properties of the final images are discussed in detail. A catalog of sources is presented, and the number counts and color distributions of the galaxies are compared with a new catalog of the original Hubble Deep Field (HDF-N) that has been constructed in an identical manner. The two fields are qualitatively similar, with the galaxy number counts for the two fields agreeing to within 20%. The HDF-S has more candidate Lyman break galaxies at z&gt;2 than the HDF-N. The star formation rate per unit volume computed from the HDF-S, based on the UV luminosity of high-redshift candidates, is a factor of 1.9 higher than from the HDF-N at z~2.7, and a factor of 1.3 higher at z~4.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747#table6</TD>
            <TD>2011-09-14T19:07:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Feb-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/120/2747</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/120/2747&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/120/2747</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/390/863 [1]</TD>
            <TD>CCD R Photometry of WHISP Dwarf Galaxies (Swaters, 2002)</TD>
            <TD>R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B-band observations are given as well.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863#1</TD>
            <TD>2011-09-14T19:18:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/390/863</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/863</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/390/863 [2]</TD>
            <TD>CCD R Photometry of WHISP Dwarf Galaxies (Swaters, 2002)</TD>
            <TD>R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B-band observations are given as well.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863#2</TD>
            <TD>2011-09-14T19:18:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/390/863&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/863</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/390/863 [tablea1]</TD>
            <TD>CCD R Photometry of WHISP Dwarf Galaxies (Swaters, 2002)</TD>
            <TD>R-band photometric and isophotal parameters for 171 late-type dwarf galaxies. For each galaxy the date of observation, seeing, adopted distance, equatorial coordinates, apparent magnitudes, central surface brightnesses, isophotal diameters and fractional light radii are given. For 46 galaxies, photometric and isophotal parameters derived from B-band observations are given as well.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863#tablea1</TD>
            <TD>2011-09-14T19:18:49Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/390/863</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/390/863&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/390/863</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/131/185 [1]</TD>
            <TD>The FIRST sample of ultraluminous IR galaxies (Stanford+, 2000)</TD>
            <TD>We present a new sample of distant ultraluminous infrared galaxies. The sample was selected from a positional cross-correlation of the IRAS Faint Source Catalog (Cat. &lt;II/156&gt;) with the FIRST database. Objects from this set were selected for spectroscopy by virtue of following the well-known star-forming galaxy correlation between 1.4 GHz and 60 {mu}m flux, and by being optically faint on the POSS. Optical identification and spectroscopy were obtained for 108 targets at the Lick Observatory 3 m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185#1</TD>
            <TD>2011-09-14T19:08:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/131/185</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/131/185</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/131/185 [2]</TD>
            <TD>The FIRST sample of ultraluminous IR galaxies (Stanford+, 2000)</TD>
            <TD>We present a new sample of distant ultraluminous infrared galaxies. The sample was selected from a positional cross-correlation of the IRAS Faint Source Catalog (Cat. &lt;II/156&gt;) with the FIRST database. Objects from this set were selected for spectroscopy by virtue of following the well-known star-forming galaxy correlation between 1.4 GHz and 60 {mu}m flux, and by being optically faint on the POSS. Optical identification and spectroscopy were obtained for 108 targets at the Lick Observatory 3 m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185#2</TD>
            <TD>2011-09-14T19:08:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/131/185&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/131/185</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/131/185 [table1]</TD>
            <TD>The FIRST sample of ultraluminous IR galaxies (Stanford+, 2000)</TD>
            <TD>We present a new sample of distant ultraluminous infrared galaxies. The sample was selected from a positional cross-correlation of the IRAS Faint Source Catalog (Cat. &lt;II/156&gt;) with the FIRST database. Objects from this set were selected for spectroscopy by virtue of following the well-known star-forming galaxy correlation between 1.4 GHz and 60 {mu}m flux, and by being optically faint on the POSS. Optical identification and spectroscopy were obtained for 108 targets at the Lick Observatory 3 m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185#table1</TD>
            <TD>2011-09-14T19:08:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/131/185&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/131/185</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/397/431 [1]</TD>
            <TD>Redshifts of ABCG209 galaxies (Mercurio+, 2003)</TD>
            <TD>We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, {sigma}_v_=1250-1400km/s, on the whole observed area (1h^-1^Mpc from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15^h^-1^M_{sun}_ within the virial radius, assuming the dynamical equilibrium. The data were collected at the ESO New Technology Telescope (NTT) with the ESO Multi Mode Instrument (EMMI) in October 2001.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431#1</TD>
            <TD>2011-09-14T19:20:30Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/397/431</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/431</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/397/431 [2]</TD>
            <TD>Redshifts of ABCG209 galaxies (Mercurio+, 2003)</TD>
            <TD>We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, {sigma}_v_=1250-1400km/s, on the whole observed area (1h^-1^Mpc from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15^h^-1^M_{sun}_ within the virial radius, assuming the dynamical equilibrium. The data were collected at the ESO New Technology Telescope (NTT) with the ESO Multi Mode Instrument (EMMI) in October 2001.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431#2</TD>
            <TD>2011-09-14T19:20:30Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/397/431&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/431</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/397/431 [table1]</TD>
            <TD>Redshifts of ABCG209 galaxies (Mercurio+, 2003)</TD>
            <TD>We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, {sigma}_v_=1250-1400km/s, on the whole observed area (1h^-1^Mpc from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15^h^-1^M_{sun}_ within the virial radius, assuming the dynamical equilibrium. The data were collected at the ESO New Technology Telescope (NTT) with the ESO Multi Mode Instrument (EMMI) in October 2001.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431#table1</TD>
            <TD>2011-09-14T19:20:30Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/397/431&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/431</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/131/185 [1]</TD>
            <TD>The FIRST sample of ultraluminous IR galaxies (Stanford+, 2000)</TD>
            <TD>We present a new sample of distant ultraluminous infrared galaxies. The sample was selected from a positional cross-correlation of the IRAS Faint Source Catalog (Cat. &lt;II/156&gt;) with the FIRST database. Objects from this set were selected for spectroscopy by virtue of following the well-known star-forming galaxy correlation between 1.4 GHz and 60 {mu}m flux, and by being optically faint on the POSS. Optical identification and spectroscopy were obtained for 108 targets at the Lick Observatory 3 m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185#1</TD>
            <TD>2011-09-14T19:08:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/131/185</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/131/185</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/131/185 [2]</TD>
            <TD>The FIRST sample of ultraluminous IR galaxies (Stanford+, 2000)</TD>
            <TD>We present a new sample of distant ultraluminous infrared galaxies. The sample was selected from a positional cross-correlation of the IRAS Faint Source Catalog (Cat. &lt;II/156&gt;) with the FIRST database. Objects from this set were selected for spectroscopy by virtue of following the well-known star-forming galaxy correlation between 1.4 GHz and 60 {mu}m flux, and by being optically faint on the POSS. Optical identification and spectroscopy were obtained for 108 targets at the Lick Observatory 3 m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185#2</TD>
            <TD>2011-09-14T19:08:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/131/185&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/131/185</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/131/185 [table1]</TD>
            <TD>The FIRST sample of ultraluminous IR galaxies (Stanford+, 2000)</TD>
            <TD>We present a new sample of distant ultraluminous infrared galaxies. The sample was selected from a positional cross-correlation of the IRAS Faint Source Catalog (Cat. &lt;II/156&gt;) with the FIRST database. Objects from this set were selected for spectroscopy by virtue of following the well-known star-forming galaxy correlation between 1.4 GHz and 60 {mu}m flux, and by being optically faint on the POSS. Optical identification and spectroscopy were obtained for 108 targets at the Lick Observatory 3 m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185#table1</TD>
            <TD>2011-09-14T19:08:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/131/185&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/131/185</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/397/431 [1]</TD>
            <TD>Redshifts of ABCG209 galaxies (Mercurio+, 2003)</TD>
            <TD>We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, {sigma}_v_=1250-1400km/s, on the whole observed area (1h^-1^Mpc from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15^h^-1^M_{sun}_ within the virial radius, assuming the dynamical equilibrium. The data were collected at the ESO New Technology Telescope (NTT) with the ESO Multi Mode Instrument (EMMI) in October 2001.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431#1</TD>
            <TD>2011-09-14T19:20:30Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/397/431</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/431</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/397/431 [2]</TD>
            <TD>Redshifts of ABCG209 galaxies (Mercurio+, 2003)</TD>
            <TD>We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, {sigma}_v_=1250-1400km/s, on the whole observed area (1h^-1^Mpc from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15^h^-1^M_{sun}_ within the virial radius, assuming the dynamical equilibrium. The data were collected at the ESO New Technology Telescope (NTT) with the ESO Multi Mode Instrument (EMMI) in October 2001.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431#2</TD>
            <TD>2011-09-14T19:20:30Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/397/431&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/431</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/397/431 [table1]</TD>
            <TD>Redshifts of ABCG209 galaxies (Mercurio+, 2003)</TD>
            <TD>We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, {sigma}_v_=1250-1400km/s, on the whole observed area (1h^-1^Mpc from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15^h^-1^M_{sun}_ within the virial radius, assuming the dynamical equilibrium. The data were collected at the ESO New Technology Telescope (NTT) with the ESO Multi Mode Instrument (EMMI) in October 2001.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431#table1</TD>
            <TD>2011-09-14T19:20:30Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/397/431&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/431</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/131/185 [1]</TD>
            <TD>The FIRST sample of ultraluminous IR galaxies (Stanford+, 2000)</TD>
            <TD>We present a new sample of distant ultraluminous infrared galaxies. The sample was selected from a positional cross-correlation of the IRAS Faint Source Catalog (Cat. &lt;II/156&gt;) with the FIRST database. Objects from this set were selected for spectroscopy by virtue of following the well-known star-forming galaxy correlation between 1.4 GHz and 60 {mu}m flux, and by being optically faint on the POSS. Optical identification and spectroscopy were obtained for 108 targets at the Lick Observatory 3 m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185#1</TD>
            <TD>2011-09-14T19:08:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/131/185</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/131/185</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/131/185 [2]</TD>
            <TD>The FIRST sample of ultraluminous IR galaxies (Stanford+, 2000)</TD>
            <TD>We present a new sample of distant ultraluminous infrared galaxies. The sample was selected from a positional cross-correlation of the IRAS Faint Source Catalog (Cat. &lt;II/156&gt;) with the FIRST database. Objects from this set were selected for spectroscopy by virtue of following the well-known star-forming galaxy correlation between 1.4 GHz and 60 {mu}m flux, and by being optically faint on the POSS. Optical identification and spectroscopy were obtained for 108 targets at the Lick Observatory 3 m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185#2</TD>
            <TD>2011-09-14T19:08:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/131/185&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/131/185</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/131/185 [table1]</TD>
            <TD>The FIRST sample of ultraluminous IR galaxies (Stanford+, 2000)</TD>
            <TD>We present a new sample of distant ultraluminous infrared galaxies. The sample was selected from a positional cross-correlation of the IRAS Faint Source Catalog (Cat. &lt;II/156&gt;) with the FIRST database. Objects from this set were selected for spectroscopy by virtue of following the well-known star-forming galaxy correlation between 1.4 GHz and 60 {mu}m flux, and by being optically faint on the POSS. Optical identification and spectroscopy were obtained for 108 targets at the Lick Observatory 3 m telescope.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185#table1</TD>
            <TD>2011-09-14T19:08:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/131/185</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/131/185&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/131/185</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/397/431 [1]</TD>
            <TD>Redshifts of ABCG209 galaxies (Mercurio+, 2003)</TD>
            <TD>We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, {sigma}_v_=1250-1400km/s, on the whole observed area (1h^-1^Mpc from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15^h^-1^M_{sun}_ within the virial radius, assuming the dynamical equilibrium. The data were collected at the ESO New Technology Telescope (NTT) with the ESO Multi Mode Instrument (EMMI) in October 2001.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431#1</TD>
            <TD>2011-09-14T19:20:30Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/397/431</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/431</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/397/431 [2]</TD>
            <TD>Redshifts of ABCG209 galaxies (Mercurio+, 2003)</TD>
            <TD>We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, {sigma}_v_=1250-1400km/s, on the whole observed area (1h^-1^Mpc from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15^h^-1^M_{sun}_ within the virial radius, assuming the dynamical equilibrium. The data were collected at the ESO New Technology Telescope (NTT) with the ESO Multi Mode Instrument (EMMI) in October 2001.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431#2</TD>
            <TD>2011-09-14T19:20:30Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/397/431&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/431</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/397/431 [table1]</TD>
            <TD>Redshifts of ABCG209 galaxies (Mercurio+, 2003)</TD>
            <TD>We study the internal dynamics of the rich galaxy cluster ABGC 209 on the basis of new spectroscopic and photometric data. The distribution in redshift shows that ABCG 209 is a well isolated peak of 112 detected member galaxies at z=0.209, characterised by a high value of the line-of-sight velocity dispersion, {sigma}_v_=1250-1400km/s, on the whole observed area (1h^-1^Mpc from the cluster center), that leads to a virial mass of M=1.6-2.2x10^15^h^-1^M_{sun}_ within the virial radius, assuming the dynamical equilibrium. The data were collected at the ESO New Technology Telescope (NTT) with the ESO Multi Mode Instrument (EMMI) in October 2001.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431#table1</TD>
            <TD>2011-09-14T19:20:30Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/431</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/397/431&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/431</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/133/77 [1]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#1</TD>
            <TD>2011-09-14T19:08:14Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/133/77</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/133/77 [2]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#2</TD>
            <TD>2011-09-14T19:08:14Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/133/77&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/133/77 [table4]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#table4</TD>
            <TD>2011-09-14T19:08:14Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/133/77&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/133/77 [table3]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#table3</TD>
            <TD>2011-09-14T19:08:14Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/133/77&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/133/77 [table1]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#table1</TD>
            <TD>2011-09-14T19:08:14Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/133/77&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1464 [1]</TD>
            <TD>Variable stars in Andromeda VI (Pritzl+, 2002)</TD>
            <TD>We have surveyed Andromeda VI, a dwarf spheroidal galaxy companion to M31, for variable stars by using F450W and F555W observations obtained with the Hubble Space Telescope on 1999 October 25 and 1999 October 27 (WFPC2 instrument). A total of 118 variables were found, including 111 RR Lyrae stars, six anomalous Cepheids, and one variable that we were unable to classify. We find that the Andromeda VI anomalous Cepheids have properties consistent with those of anomalous Cepheids in other dwarf spheroidal galaxies. We revise the existing period-luminosity relations for these variables. Further, using these and other available data, we show that there is no clear difference between fundamental and first-overtone anomalous Cepheids in a period-amplitude diagram at shorter periods, unlike the RR Lyrae stars. For the Andromeda VI RR Lyrae stars, we find that they lie close to the Oosterhoff type I Galactic globular clusters in the period-amplitude diagram, although the mean period of the RRab stars, &lt;P_ab_&gt;=0.588days, is slightly longer than that of the typical Oosterhoff type I cluster. The mean V magnitude of the RR Lyrae stars in Andromeda VI is 25.29+/-0.03, resulting in a distance 815+/-25kpc on the Lee, Demarque, &amp; Zinn (1990ApJ...350..155L) distance scale. This is consistent with the distance derived from the I magnitude of the tip of the red giant branch. Similarly, the properties of the RR Lyrae stars indicate a mean abundance for Andromeda VI that is consistent with that derived from the mean red giant branch color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464#1</TD>
            <TD>2011-09-14T19:21:18Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1464</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1464</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1464 [2]</TD>
            <TD>Variable stars in Andromeda VI (Pritzl+, 2002)</TD>
            <TD>We have surveyed Andromeda VI, a dwarf spheroidal galaxy companion to M31, for variable stars by using F450W and F555W observations obtained with the Hubble Space Telescope on 1999 October 25 and 1999 October 27 (WFPC2 instrument). A total of 118 variables were found, including 111 RR Lyrae stars, six anomalous Cepheids, and one variable that we were unable to classify. We find that the Andromeda VI anomalous Cepheids have properties consistent with those of anomalous Cepheids in other dwarf spheroidal galaxies. We revise the existing period-luminosity relations for these variables. Further, using these and other available data, we show that there is no clear difference between fundamental and first-overtone anomalous Cepheids in a period-amplitude diagram at shorter periods, unlike the RR Lyrae stars. For the Andromeda VI RR Lyrae stars, we find that they lie close to the Oosterhoff type I Galactic globular clusters in the period-amplitude diagram, although the mean period of the RRab stars, &lt;P_ab_&gt;=0.588days, is slightly longer than that of the typical Oosterhoff type I cluster. The mean V magnitude of the RR Lyrae stars in Andromeda VI is 25.29+/-0.03, resulting in a distance 815+/-25kpc on the Lee, Demarque, &amp; Zinn (1990ApJ...350..155L) distance scale. This is consistent with the distance derived from the I magnitude of the tip of the red giant branch. Similarly, the properties of the RR Lyrae stars indicate a mean abundance for Andromeda VI that is consistent with that derived from the mean red giant branch color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464#2</TD>
            <TD>2011-09-14T19:21:18Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1464&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1464</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1464 [table1]</TD>
            <TD>Variable stars in Andromeda VI (Pritzl+, 2002)</TD>
            <TD>We have surveyed Andromeda VI, a dwarf spheroidal galaxy companion to M31, for variable stars by using F450W and F555W observations obtained with the Hubble Space Telescope on 1999 October 25 and 1999 October 27 (WFPC2 instrument). A total of 118 variables were found, including 111 RR Lyrae stars, six anomalous Cepheids, and one variable that we were unable to classify. We find that the Andromeda VI anomalous Cepheids have properties consistent with those of anomalous Cepheids in other dwarf spheroidal galaxies. We revise the existing period-luminosity relations for these variables. Further, using these and other available data, we show that there is no clear difference between fundamental and first-overtone anomalous Cepheids in a period-amplitude diagram at shorter periods, unlike the RR Lyrae stars. For the Andromeda VI RR Lyrae stars, we find that they lie close to the Oosterhoff type I Galactic globular clusters in the period-amplitude diagram, although the mean period of the RRab stars, &lt;P_ab_&gt;=0.588days, is slightly longer than that of the typical Oosterhoff type I cluster. The mean V magnitude of the RR Lyrae stars in Andromeda VI is 25.29+/-0.03, resulting in a distance 815+/-25kpc on the Lee, Demarque, &amp; Zinn (1990ApJ...350..155L) distance scale. This is consistent with the distance derived from the I magnitude of the tip of the red giant branch. Similarly, the properties of the RR Lyrae stars indicate a mean abundance for Andromeda VI that is consistent with that derived from the mean red giant branch color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464#table1</TD>
            <TD>2011-09-14T19:21:18Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1464&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1464</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/133/77 [1]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
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            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/133/77</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJS/133/77 [2]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#2</TD>
            <TD>2011-09-14T19:08:14Z</TD>
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            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/133/77&amp;</TD>
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          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/133/77 [table4]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
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            <TD>2011-09-14T19:08:14Z</TD>
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            <TD>#Catalog#</TD>
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            <TD>24-Apr-2001</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/133/77 [table3]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#table3</TD>
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            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/133/77&amp;</TD>
            <TD>180</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/133/77 [table1]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1464 [1]</TD>
            <TD>Variable stars in Andromeda VI (Pritzl+, 2002)</TD>
            <TD>We have surveyed Andromeda VI, a dwarf spheroidal galaxy companion to M31, for variable stars by using F450W and F555W observations obtained with the Hubble Space Telescope on 1999 October 25 and 1999 October 27 (WFPC2 instrument). A total of 118 variables were found, including 111 RR Lyrae stars, six anomalous Cepheids, and one variable that we were unable to classify. We find that the Andromeda VI anomalous Cepheids have properties consistent with those of anomalous Cepheids in other dwarf spheroidal galaxies. We revise the existing period-luminosity relations for these variables. Further, using these and other available data, we show that there is no clear difference between fundamental and first-overtone anomalous Cepheids in a period-amplitude diagram at shorter periods, unlike the RR Lyrae stars. For the Andromeda VI RR Lyrae stars, we find that they lie close to the Oosterhoff type I Galactic globular clusters in the period-amplitude diagram, although the mean period of the RRab stars, &lt;P_ab_&gt;=0.588days, is slightly longer than that of the typical Oosterhoff type I cluster. The mean V magnitude of the RR Lyrae stars in Andromeda VI is 25.29+/-0.03, resulting in a distance 815+/-25kpc on the Lee, Demarque, &amp; Zinn (1990ApJ...350..155L) distance scale. This is consistent with the distance derived from the I magnitude of the tip of the red giant branch. Similarly, the properties of the RR Lyrae stars indicate a mean abundance for Andromeda VI that is consistent with that derived from the mean red giant branch color.</TD>
            <TD>CDS</TD>
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            <TD>08-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1464</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1464</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1464 [2]</TD>
            <TD>Variable stars in Andromeda VI (Pritzl+, 2002)</TD>
            <TD>We have surveyed Andromeda VI, a dwarf spheroidal galaxy companion to M31, for variable stars by using F450W and F555W observations obtained with the Hubble Space Telescope on 1999 October 25 and 1999 October 27 (WFPC2 instrument). A total of 118 variables were found, including 111 RR Lyrae stars, six anomalous Cepheids, and one variable that we were unable to classify. We find that the Andromeda VI anomalous Cepheids have properties consistent with those of anomalous Cepheids in other dwarf spheroidal galaxies. We revise the existing period-luminosity relations for these variables. Further, using these and other available data, we show that there is no clear difference between fundamental and first-overtone anomalous Cepheids in a period-amplitude diagram at shorter periods, unlike the RR Lyrae stars. For the Andromeda VI RR Lyrae stars, we find that they lie close to the Oosterhoff type I Galactic globular clusters in the period-amplitude diagram, although the mean period of the RRab stars, &lt;P_ab_&gt;=0.588days, is slightly longer than that of the typical Oosterhoff type I cluster. The mean V magnitude of the RR Lyrae stars in Andromeda VI is 25.29+/-0.03, resulting in a distance 815+/-25kpc on the Lee, Demarque, &amp; Zinn (1990ApJ...350..155L) distance scale. This is consistent with the distance derived from the I magnitude of the tip of the red giant branch. Similarly, the properties of the RR Lyrae stars indicate a mean abundance for Andromeda VI that is consistent with that derived from the mean red giant branch color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464#2</TD>
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            <TD />
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            <TD>ivo://CDS.VizieR/J/AJ/124/1464</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1464 [table1]</TD>
            <TD>Variable stars in Andromeda VI (Pritzl+, 2002)</TD>
            <TD>We have surveyed Andromeda VI, a dwarf spheroidal galaxy companion to M31, for variable stars by using F450W and F555W observations obtained with the Hubble Space Telescope on 1999 October 25 and 1999 October 27 (WFPC2 instrument). A total of 118 variables were found, including 111 RR Lyrae stars, six anomalous Cepheids, and one variable that we were unable to classify. We find that the Andromeda VI anomalous Cepheids have properties consistent with those of anomalous Cepheids in other dwarf spheroidal galaxies. We revise the existing period-luminosity relations for these variables. Further, using these and other available data, we show that there is no clear difference between fundamental and first-overtone anomalous Cepheids in a period-amplitude diagram at shorter periods, unlike the RR Lyrae stars. For the Andromeda VI RR Lyrae stars, we find that they lie close to the Oosterhoff type I Galactic globular clusters in the period-amplitude diagram, although the mean period of the RRab stars, &lt;P_ab_&gt;=0.588days, is slightly longer than that of the typical Oosterhoff type I cluster. The mean V magnitude of the RR Lyrae stars in Andromeda VI is 25.29+/-0.03, resulting in a distance 815+/-25kpc on the Lee, Demarque, &amp; Zinn (1990ApJ...350..155L) distance scale. This is consistent with the distance derived from the I magnitude of the tip of the red giant branch. Similarly, the properties of the RR Lyrae stars indicate a mean abundance for Andromeda VI that is consistent with that derived from the mean red giant branch color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464#table1</TD>
            <TD>2011-09-14T19:21:18Z</TD>
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            <TD>08-Nov-2002</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJS/133/77 [1]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
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            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
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            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/133/77</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/133/77 [2]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#2</TD>
            <TD>2011-09-14T19:08:14Z</TD>
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            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD />
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/133/77 [table4]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#table4</TD>
            <TD>2011-09-14T19:08:14Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/133/77&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/133/77 [table3]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#table3</TD>
            <TD>2011-09-14T19:08:14Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/133/77&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/133/77 [table1]</TD>
            <TD>VLA radio continuum survey of Seyfert galaxies (Ho+, 2001)</TD>
            <TD>We have used the Very Large Array (VLA) to conduct a survey for radio continuum emission in the sample of 52 Seyfert nuclei selected from the optical spectroscopic galaxy catalog of Ho, Filippenko, &amp; Sargent (1995, Cat. &lt;J/ApJS/98/477&gt;. This Seyfert sample is the most complete and least biased available, and, as such, it will be useful for a variety of statistical analyses. Here we present the observations, measurements, and an atlas of radio maps. The observations were made at 6 cm in the B array and at 20 cm in the A array, yielding matched angular resolutions of ~1". We detected 44 objects (85%) at 6 cm and 37 objects (71%) at 20 cm above a 3{sigma} threshold of 0.12mJy/beam. The sources have a wide range of radio powers (P~10^19^-10^25^W/Hz), spectral indices ({alpha}^20^_6_~+0.5 to 1), and linear sizes (L~few tens pc - 15kpc). The morphology of the radio emission is predominantly that of a compact core, either unresolved or slightly resolved, occasionally accompanied by elongated, jetlike features. Linearly polarized emission was detected at 6 cm in 12 sources, nine of which were also detected at 20 cm.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77#table1</TD>
            <TD>2011-09-14T19:08:14Z</TD>
            <TD>#Galaxies#Seyfert_Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Apr-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/133/77</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/133/77&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/133/77</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/1464 [1]</TD>
            <TD>Variable stars in Andromeda VI (Pritzl+, 2002)</TD>
            <TD>We have surveyed Andromeda VI, a dwarf spheroidal galaxy companion to M31, for variable stars by using F450W and F555W observations obtained with the Hubble Space Telescope on 1999 October 25 and 1999 October 27 (WFPC2 instrument). A total of 118 variables were found, including 111 RR Lyrae stars, six anomalous Cepheids, and one variable that we were unable to classify. We find that the Andromeda VI anomalous Cepheids have properties consistent with those of anomalous Cepheids in other dwarf spheroidal galaxies. We revise the existing period-luminosity relations for these variables. Further, using these and other available data, we show that there is no clear difference between fundamental and first-overtone anomalous Cepheids in a period-amplitude diagram at shorter periods, unlike the RR Lyrae stars. For the Andromeda VI RR Lyrae stars, we find that they lie close to the Oosterhoff type I Galactic globular clusters in the period-amplitude diagram, although the mean period of the RRab stars, &lt;P_ab_&gt;=0.588days, is slightly longer than that of the typical Oosterhoff type I cluster. The mean V magnitude of the RR Lyrae stars in Andromeda VI is 25.29+/-0.03, resulting in a distance 815+/-25kpc on the Lee, Demarque, &amp; Zinn (1990ApJ...350..155L) distance scale. This is consistent with the distance derived from the I magnitude of the tip of the red giant branch. Similarly, the properties of the RR Lyrae stars indicate a mean abundance for Andromeda VI that is consistent with that derived from the mean red giant branch color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464#1</TD>
            <TD>2011-09-14T19:21:18Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/1464</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1464</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/1464 [2]</TD>
            <TD>Variable stars in Andromeda VI (Pritzl+, 2002)</TD>
            <TD>We have surveyed Andromeda VI, a dwarf spheroidal galaxy companion to M31, for variable stars by using F450W and F555W observations obtained with the Hubble Space Telescope on 1999 October 25 and 1999 October 27 (WFPC2 instrument). A total of 118 variables were found, including 111 RR Lyrae stars, six anomalous Cepheids, and one variable that we were unable to classify. We find that the Andromeda VI anomalous Cepheids have properties consistent with those of anomalous Cepheids in other dwarf spheroidal galaxies. We revise the existing period-luminosity relations for these variables. Further, using these and other available data, we show that there is no clear difference between fundamental and first-overtone anomalous Cepheids in a period-amplitude diagram at shorter periods, unlike the RR Lyrae stars. For the Andromeda VI RR Lyrae stars, we find that they lie close to the Oosterhoff type I Galactic globular clusters in the period-amplitude diagram, although the mean period of the RRab stars, &lt;P_ab_&gt;=0.588days, is slightly longer than that of the typical Oosterhoff type I cluster. The mean V magnitude of the RR Lyrae stars in Andromeda VI is 25.29+/-0.03, resulting in a distance 815+/-25kpc on the Lee, Demarque, &amp; Zinn (1990ApJ...350..155L) distance scale. This is consistent with the distance derived from the I magnitude of the tip of the red giant branch. Similarly, the properties of the RR Lyrae stars indicate a mean abundance for Andromeda VI that is consistent with that derived from the mean red giant branch color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464#2</TD>
            <TD>2011-09-14T19:21:18Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/1464&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1464</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/1464 [table1]</TD>
            <TD>Variable stars in Andromeda VI (Pritzl+, 2002)</TD>
            <TD>We have surveyed Andromeda VI, a dwarf spheroidal galaxy companion to M31, for variable stars by using F450W and F555W observations obtained with the Hubble Space Telescope on 1999 October 25 and 1999 October 27 (WFPC2 instrument). A total of 118 variables were found, including 111 RR Lyrae stars, six anomalous Cepheids, and one variable that we were unable to classify. We find that the Andromeda VI anomalous Cepheids have properties consistent with those of anomalous Cepheids in other dwarf spheroidal galaxies. We revise the existing period-luminosity relations for these variables. Further, using these and other available data, we show that there is no clear difference between fundamental and first-overtone anomalous Cepheids in a period-amplitude diagram at shorter periods, unlike the RR Lyrae stars. For the Andromeda VI RR Lyrae stars, we find that they lie close to the Oosterhoff type I Galactic globular clusters in the period-amplitude diagram, although the mean period of the RRab stars, &lt;P_ab_&gt;=0.588days, is slightly longer than that of the typical Oosterhoff type I cluster. The mean V magnitude of the RR Lyrae stars in Andromeda VI is 25.29+/-0.03, resulting in a distance 815+/-25kpc on the Lee, Demarque, &amp; Zinn (1990ApJ...350..155L) distance scale. This is consistent with the distance derived from the I magnitude of the tip of the red giant branch. Similarly, the properties of the RR Lyrae stars indicate a mean abundance for Andromeda VI that is consistent with that derived from the mean red giant branch color.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464#table1</TD>
            <TD>2011-09-14T19:21:18Z</TD>
            <TD>#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Nov-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/1464</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/1464&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/1464</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/361/491 [1]</TD>
            <TD>NGC 3109 X-ray sources (Kahabka+, 2000)</TD>
            <TD>We established the catalog of X-ray point sources in the field of the Magellanic-type spiral galaxy NGC 3109 (DDO 236) from two ROSAT PSPC observations. Of the 91 X-ray sources 26 are contained within the HI extent of NGC 3109 as derived by Jobin &amp; Carignan (1990AJ....100..648J) with the VLA. For 10 of these we can determine accurate hardness ratios {delta}HR2&lt;=0.2. We find 3 candidate AGN, 2 candidate X-ray binaries and one source which may belong to either class. We also find 2 candidate foreground stars. In a field of 8'x8' observed with the NTT in the I-b and and centered on the nucleus of NGC 3109 we determine candidates for optical counterparts in the X-ray error circle of 7 ROSAT PSPC sources. We apply a spectral fit to the ROSAT spectrum of the X-ray brightest absorbed candidate AGN behind NGC 3109, RX J1003.2-2607. Assuming a galactic foreground hydrogen column density of 4.3x10^20^cm^-2^ we derive from the X-ray spectral fit, assuming reduced metallicities (~0.2 solar), a hydrogen column density due to NGC 3109 of 11+/-^7^_5_x10^20^cm^-2^. This value is slightly larger than the hydrogen column density derived from the 21-cm observations of ~8x10^20^cm^-2^. We estimate that the molecular mass fraction of the gas is not larger than ~60%.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491#1</TD>
            <TD>2011-09-14T19:08:37Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/361/491</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/361/491</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/361/491 [2]</TD>
            <TD>NGC 3109 X-ray sources (Kahabka+, 2000)</TD>
            <TD>We established the catalog of X-ray point sources in the field of the Magellanic-type spiral galaxy NGC 3109 (DDO 236) from two ROSAT PSPC observations. Of the 91 X-ray sources 26 are contained within the HI extent of NGC 3109 as derived by Jobin &amp; Carignan (1990AJ....100..648J) with the VLA. For 10 of these we can determine accurate hardness ratios {delta}HR2&lt;=0.2. We find 3 candidate AGN, 2 candidate X-ray binaries and one source which may belong to either class. We also find 2 candidate foreground stars. In a field of 8'x8' observed with the NTT in the I-b and and centered on the nucleus of NGC 3109 we determine candidates for optical counterparts in the X-ray error circle of 7 ROSAT PSPC sources. We apply a spectral fit to the ROSAT spectrum of the X-ray brightest absorbed candidate AGN behind NGC 3109, RX J1003.2-2607. Assuming a galactic foreground hydrogen column density of 4.3x10^20^cm^-2^ we derive from the X-ray spectral fit, assuming reduced metallicities (~0.2 solar), a hydrogen column density due to NGC 3109 of 11+/-^7^_5_x10^20^cm^-2^. This value is slightly larger than the hydrogen column density derived from the 21-cm observations of ~8x10^20^cm^-2^. We estimate that the molecular mass fraction of the gas is not larger than ~60%.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491#2</TD>
            <TD>2011-09-14T19:08:37Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/361/491&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/361/491</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/361/491 [table6]</TD>
            <TD>NGC 3109 X-ray sources (Kahabka+, 2000)</TD>
            <TD>We established the catalog of X-ray point sources in the field of the Magellanic-type spiral galaxy NGC 3109 (DDO 236) from two ROSAT PSPC observations. Of the 91 X-ray sources 26 are contained within the HI extent of NGC 3109 as derived by Jobin &amp; Carignan (1990AJ....100..648J) with the VLA. For 10 of these we can determine accurate hardness ratios {delta}HR2&lt;=0.2. We find 3 candidate AGN, 2 candidate X-ray binaries and one source which may belong to either class. We also find 2 candidate foreground stars. In a field of 8'x8' observed with the NTT in the I-b and and centered on the nucleus of NGC 3109 we determine candidates for optical counterparts in the X-ray error circle of 7 ROSAT PSPC sources. We apply a spectral fit to the ROSAT spectrum of the X-ray brightest absorbed candidate AGN behind NGC 3109, RX J1003.2-2607. Assuming a galactic foreground hydrogen column density of 4.3x10^20^cm^-2^ we derive from the X-ray spectral fit, assuming reduced metallicities (~0.2 solar), a hydrogen column density due to NGC 3109 of 11+/-^7^_5_x10^20^cm^-2^. This value is slightly larger than the hydrogen column density derived from the 21-cm observations of ~8x10^20^cm^-2^. We estimate that the molecular mass fraction of the gas is not larger than ~60%.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491#table6</TD>
            <TD>2011-09-14T19:08:37Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/361/491&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/361/491</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/339/652 [1]</TD>
            <TD>The FLASH Redshift Survey (Kaldare+ 2003)</TD>
            <TD>The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue consists of 4613 galaxies brighter than b_J_= 16.7 (corrected for Galactic extinction) over a 700-deg^2^ region of sky in the general direction of the Local Group motion. The survey region is a 70x10{deg} strip spanning the sky from the Shapley Supercluster to the Hydra cluster, and contains 3141 galaxies with measured redshifts. Designed to explore the effect of the galaxy concentrations in this direction (in particular the Supergalactic plane and the Shapley Supercluster) upon the Local Group motion, the 68 per cent completeness allows us to sample the large-scale structure better than similar sparsely-sampled surveys. The survey region does not overlap with the areas covered by ongoing wide-angle (Sloan or 2dF) complete redshift surveys. In this paper, the first in a series, we describe the observation and data reduction procedures, the analysis for the redshift errors and survey completeness, and present the survey data. Note that there are some minor change/improvements over the example table published in MNRAS: 1. R.A./Dec. is now J2000 rather than B1950. 2. l/b are now given to 3 decimal places rather than 1 decimal place. 3. Some additional redshifts from NED and ZCAT have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652#1</TD>
            <TD>2011-09-14T19:21:54Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/339/652</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/652</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/339/652 [2]</TD>
            <TD>The FLASH Redshift Survey (Kaldare+ 2003)</TD>
            <TD>The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue consists of 4613 galaxies brighter than b_J_= 16.7 (corrected for Galactic extinction) over a 700-deg^2^ region of sky in the general direction of the Local Group motion. The survey region is a 70x10{deg} strip spanning the sky from the Shapley Supercluster to the Hydra cluster, and contains 3141 galaxies with measured redshifts. Designed to explore the effect of the galaxy concentrations in this direction (in particular the Supergalactic plane and the Shapley Supercluster) upon the Local Group motion, the 68 per cent completeness allows us to sample the large-scale structure better than similar sparsely-sampled surveys. The survey region does not overlap with the areas covered by ongoing wide-angle (Sloan or 2dF) complete redshift surveys. In this paper, the first in a series, we describe the observation and data reduction procedures, the analysis for the redshift errors and survey completeness, and present the survey data. Note that there are some minor change/improvements over the example table published in MNRAS: 1. R.A./Dec. is now J2000 rather than B1950. 2. l/b are now given to 3 decimal places rather than 1 decimal place. 3. Some additional redshifts from NED and ZCAT have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652#2</TD>
            <TD>2011-09-14T19:21:54Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/339/652&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/652</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/339/652 [catalog]</TD>
            <TD>The FLASH Redshift Survey (Kaldare+ 2003)</TD>
            <TD>The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue consists of 4613 galaxies brighter than b_J_= 16.7 (corrected for Galactic extinction) over a 700-deg^2^ region of sky in the general direction of the Local Group motion. The survey region is a 70x10{deg} strip spanning the sky from the Shapley Supercluster to the Hydra cluster, and contains 3141 galaxies with measured redshifts. Designed to explore the effect of the galaxy concentrations in this direction (in particular the Supergalactic plane and the Shapley Supercluster) upon the Local Group motion, the 68 per cent completeness allows us to sample the large-scale structure better than similar sparsely-sampled surveys. The survey region does not overlap with the areas covered by ongoing wide-angle (Sloan or 2dF) complete redshift surveys. In this paper, the first in a series, we describe the observation and data reduction procedures, the analysis for the redshift errors and survey completeness, and present the survey data. Note that there are some minor change/improvements over the example table published in MNRAS: 1. R.A./Dec. is now J2000 rather than B1950. 2. l/b are now given to 3 decimal places rather than 1 decimal place. 3. Some additional redshifts from NED and ZCAT have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652#catalog</TD>
            <TD>2011-09-14T19:21:54Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/339/652&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/652</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/361/491 [1]</TD>
            <TD>NGC 3109 X-ray sources (Kahabka+, 2000)</TD>
            <TD>We established the catalog of X-ray point sources in the field of the Magellanic-type spiral galaxy NGC 3109 (DDO 236) from two ROSAT PSPC observations. Of the 91 X-ray sources 26 are contained within the HI extent of NGC 3109 as derived by Jobin &amp; Carignan (1990AJ....100..648J) with the VLA. For 10 of these we can determine accurate hardness ratios {delta}HR2&lt;=0.2. We find 3 candidate AGN, 2 candidate X-ray binaries and one source which may belong to either class. We also find 2 candidate foreground stars. In a field of 8'x8' observed with the NTT in the I-b and and centered on the nucleus of NGC 3109 we determine candidates for optical counterparts in the X-ray error circle of 7 ROSAT PSPC sources. We apply a spectral fit to the ROSAT spectrum of the X-ray brightest absorbed candidate AGN behind NGC 3109, RX J1003.2-2607. Assuming a galactic foreground hydrogen column density of 4.3x10^20^cm^-2^ we derive from the X-ray spectral fit, assuming reduced metallicities (~0.2 solar), a hydrogen column density due to NGC 3109 of 11+/-^7^_5_x10^20^cm^-2^. This value is slightly larger than the hydrogen column density derived from the 21-cm observations of ~8x10^20^cm^-2^. We estimate that the molecular mass fraction of the gas is not larger than ~60%.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491#1</TD>
            <TD>2011-09-14T19:08:37Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>31-Jan-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/361/491</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/361/491</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/361/491 [2]</TD>
            <TD>NGC 3109 X-ray sources (Kahabka+, 2000)</TD>
            <TD>We established the catalog of X-ray point sources in the field of the Magellanic-type spiral galaxy NGC 3109 (DDO 236) from two ROSAT PSPC observations. Of the 91 X-ray sources 26 are contained within the HI extent of NGC 3109 as derived by Jobin &amp; Carignan (1990AJ....100..648J) with the VLA. For 10 of these we can determine accurate hardness ratios {delta}HR2&lt;=0.2. We find 3 candidate AGN, 2 candidate X-ray binaries and one source which may belong to either class. We also find 2 candidate foreground stars. In a field of 8'x8' observed with the NTT in the I-b and and centered on the nucleus of NGC 3109 we determine candidates for optical counterparts in the X-ray error circle of 7 ROSAT PSPC sources. We apply a spectral fit to the ROSAT spectrum of the X-ray brightest absorbed candidate AGN behind NGC 3109, RX J1003.2-2607. Assuming a galactic foreground hydrogen column density of 4.3x10^20^cm^-2^ we derive from the X-ray spectral fit, assuming reduced metallicities (~0.2 solar), a hydrogen column density due to NGC 3109 of 11+/-^7^_5_x10^20^cm^-2^. This value is slightly larger than the hydrogen column density derived from the 21-cm observations of ~8x10^20^cm^-2^. We estimate that the molecular mass fraction of the gas is not larger than ~60%.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491#2</TD>
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            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/361/491&amp;</TD>
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            <TD>Catalog</TD>
            <TD>J/A+A/361/491 [table6]</TD>
            <TD>NGC 3109 X-ray sources (Kahabka+, 2000)</TD>
            <TD>We established the catalog of X-ray point sources in the field of the Magellanic-type spiral galaxy NGC 3109 (DDO 236) from two ROSAT PSPC observations. Of the 91 X-ray sources 26 are contained within the HI extent of NGC 3109 as derived by Jobin &amp; Carignan (1990AJ....100..648J) with the VLA. For 10 of these we can determine accurate hardness ratios {delta}HR2&lt;=0.2. We find 3 candidate AGN, 2 candidate X-ray binaries and one source which may belong to either class. We also find 2 candidate foreground stars. In a field of 8'x8' observed with the NTT in the I-b and and centered on the nucleus of NGC 3109 we determine candidates for optical counterparts in the X-ray error circle of 7 ROSAT PSPC sources. We apply a spectral fit to the ROSAT spectrum of the X-ray brightest absorbed candidate AGN behind NGC 3109, RX J1003.2-2607. Assuming a galactic foreground hydrogen column density of 4.3x10^20^cm^-2^ we derive from the X-ray spectral fit, assuming reduced metallicities (~0.2 solar), a hydrogen column density due to NGC 3109 of 11+/-^7^_5_x10^20^cm^-2^. This value is slightly larger than the hydrogen column density derived from the 21-cm observations of ~8x10^20^cm^-2^. We estimate that the molecular mass fraction of the gas is not larger than ~60%.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491#table6</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/361/491&amp;</TD>
            <TD>180</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/339/652 [1]</TD>
            <TD>The FLASH Redshift Survey (Kaldare+ 2003)</TD>
            <TD>The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue consists of 4613 galaxies brighter than b_J_= 16.7 (corrected for Galactic extinction) over a 700-deg^2^ region of sky in the general direction of the Local Group motion. The survey region is a 70x10{deg} strip spanning the sky from the Shapley Supercluster to the Hydra cluster, and contains 3141 galaxies with measured redshifts. Designed to explore the effect of the galaxy concentrations in this direction (in particular the Supergalactic plane and the Shapley Supercluster) upon the Local Group motion, the 68 per cent completeness allows us to sample the large-scale structure better than similar sparsely-sampled surveys. The survey region does not overlap with the areas covered by ongoing wide-angle (Sloan or 2dF) complete redshift surveys. In this paper, the first in a series, we describe the observation and data reduction procedures, the analysis for the redshift errors and survey completeness, and present the survey data. Note that there are some minor change/improvements over the example table published in MNRAS: 1. R.A./Dec. is now J2000 rather than B1950. 2. l/b are now given to 3 decimal places rather than 1 decimal place. 3. Some additional redshifts from NED and ZCAT have been included.</TD>
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            <TD>08-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/339/652</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/652</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/339/652 [2]</TD>
            <TD>The FLASH Redshift Survey (Kaldare+ 2003)</TD>
            <TD>The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue consists of 4613 galaxies brighter than b_J_= 16.7 (corrected for Galactic extinction) over a 700-deg^2^ region of sky in the general direction of the Local Group motion. The survey region is a 70x10{deg} strip spanning the sky from the Shapley Supercluster to the Hydra cluster, and contains 3141 galaxies with measured redshifts. Designed to explore the effect of the galaxy concentrations in this direction (in particular the Supergalactic plane and the Shapley Supercluster) upon the Local Group motion, the 68 per cent completeness allows us to sample the large-scale structure better than similar sparsely-sampled surveys. The survey region does not overlap with the areas covered by ongoing wide-angle (Sloan or 2dF) complete redshift surveys. In this paper, the first in a series, we describe the observation and data reduction procedures, the analysis for the redshift errors and survey completeness, and present the survey data. Note that there are some minor change/improvements over the example table published in MNRAS: 1. R.A./Dec. is now J2000 rather than B1950. 2. l/b are now given to 3 decimal places rather than 1 decimal place. 3. Some additional redshifts from NED and ZCAT have been included.</TD>
            <TD>CDS</TD>
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            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/339/652&amp;</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/339/652 [catalog]</TD>
            <TD>The FLASH Redshift Survey (Kaldare+ 2003)</TD>
            <TD>The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue consists of 4613 galaxies brighter than b_J_= 16.7 (corrected for Galactic extinction) over a 700-deg^2^ region of sky in the general direction of the Local Group motion. The survey region is a 70x10{deg} strip spanning the sky from the Shapley Supercluster to the Hydra cluster, and contains 3141 galaxies with measured redshifts. Designed to explore the effect of the galaxy concentrations in this direction (in particular the Supergalactic plane and the Shapley Supercluster) upon the Local Group motion, the 68 per cent completeness allows us to sample the large-scale structure better than similar sparsely-sampled surveys. The survey region does not overlap with the areas covered by ongoing wide-angle (Sloan or 2dF) complete redshift surveys. In this paper, the first in a series, we describe the observation and data reduction procedures, the analysis for the redshift errors and survey completeness, and present the survey data. Note that there are some minor change/improvements over the example table published in MNRAS: 1. R.A./Dec. is now J2000 rather than B1950. 2. l/b are now given to 3 decimal places rather than 1 decimal place. 3. Some additional redshifts from NED and ZCAT have been included.</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/339/652&amp;</TD>
            <TD>180</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/652</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/361/491 [1]</TD>
            <TD>NGC 3109 X-ray sources (Kahabka+, 2000)</TD>
            <TD>We established the catalog of X-ray point sources in the field of the Magellanic-type spiral galaxy NGC 3109 (DDO 236) from two ROSAT PSPC observations. Of the 91 X-ray sources 26 are contained within the HI extent of NGC 3109 as derived by Jobin &amp; Carignan (1990AJ....100..648J) with the VLA. For 10 of these we can determine accurate hardness ratios {delta}HR2&lt;=0.2. We find 3 candidate AGN, 2 candidate X-ray binaries and one source which may belong to either class. We also find 2 candidate foreground stars. In a field of 8'x8' observed with the NTT in the I-b and and centered on the nucleus of NGC 3109 we determine candidates for optical counterparts in the X-ray error circle of 7 ROSAT PSPC sources. We apply a spectral fit to the ROSAT spectrum of the X-ray brightest absorbed candidate AGN behind NGC 3109, RX J1003.2-2607. Assuming a galactic foreground hydrogen column density of 4.3x10^20^cm^-2^ we derive from the X-ray spectral fit, assuming reduced metallicities (~0.2 solar), a hydrogen column density due to NGC 3109 of 11+/-^7^_5_x10^20^cm^-2^. This value is slightly larger than the hydrogen column density derived from the 21-cm observations of ~8x10^20^cm^-2^. We estimate that the molecular mass fraction of the gas is not larger than ~60%.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/361/491</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/361/491</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/361/491 [2]</TD>
            <TD>NGC 3109 X-ray sources (Kahabka+, 2000)</TD>
            <TD>We established the catalog of X-ray point sources in the field of the Magellanic-type spiral galaxy NGC 3109 (DDO 236) from two ROSAT PSPC observations. Of the 91 X-ray sources 26 are contained within the HI extent of NGC 3109 as derived by Jobin &amp; Carignan (1990AJ....100..648J) with the VLA. For 10 of these we can determine accurate hardness ratios {delta}HR2&lt;=0.2. We find 3 candidate AGN, 2 candidate X-ray binaries and one source which may belong to either class. We also find 2 candidate foreground stars. In a field of 8'x8' observed with the NTT in the I-b and and centered on the nucleus of NGC 3109 we determine candidates for optical counterparts in the X-ray error circle of 7 ROSAT PSPC sources. We apply a spectral fit to the ROSAT spectrum of the X-ray brightest absorbed candidate AGN behind NGC 3109, RX J1003.2-2607. Assuming a galactic foreground hydrogen column density of 4.3x10^20^cm^-2^ we derive from the X-ray spectral fit, assuming reduced metallicities (~0.2 solar), a hydrogen column density due to NGC 3109 of 11+/-^7^_5_x10^20^cm^-2^. This value is slightly larger than the hydrogen column density derived from the 21-cm observations of ~8x10^20^cm^-2^. We estimate that the molecular mass fraction of the gas is not larger than ~60%.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491#2</TD>
            <TD>2011-09-14T19:08:37Z</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/361/491</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/361/491&amp;</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/361/491</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/361/491 [table6]</TD>
            <TD>NGC 3109 X-ray sources (Kahabka+, 2000)</TD>
            <TD>We established the catalog of X-ray point sources in the field of the Magellanic-type spiral galaxy NGC 3109 (DDO 236) from two ROSAT PSPC observations. Of the 91 X-ray sources 26 are contained within the HI extent of NGC 3109 as derived by Jobin &amp; Carignan (1990AJ....100..648J) with the VLA. For 10 of these we can determine accurate hardness ratios {delta}HR2&lt;=0.2. We find 3 candidate AGN, 2 candidate X-ray binaries and one source which may belong to either class. We also find 2 candidate foreground stars. In a field of 8'x8' observed with the NTT in the I-b and and centered on the nucleus of NGC 3109 we determine candidates for optical counterparts in the X-ray error circle of 7 ROSAT PSPC sources. We apply a spectral fit to the ROSAT spectrum of the X-ray brightest absorbed candidate AGN behind NGC 3109, RX J1003.2-2607. Assuming a galactic foreground hydrogen column density of 4.3x10^20^cm^-2^ we derive from the X-ray spectral fit, assuming reduced metallicities (~0.2 solar), a hydrogen column density due to NGC 3109 of 11+/-^7^_5_x10^20^cm^-2^. This value is slightly larger than the hydrogen column density derived from the 21-cm observations of ~8x10^20^cm^-2^. We estimate that the molecular mass fraction of the gas is not larger than ~60%.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/361/491#table6</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/339/652 [1]</TD>
            <TD>The FLASH Redshift Survey (Kaldare+ 2003)</TD>
            <TD>The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue consists of 4613 galaxies brighter than b_J_= 16.7 (corrected for Galactic extinction) over a 700-deg^2^ region of sky in the general direction of the Local Group motion. The survey region is a 70x10{deg} strip spanning the sky from the Shapley Supercluster to the Hydra cluster, and contains 3141 galaxies with measured redshifts. Designed to explore the effect of the galaxy concentrations in this direction (in particular the Supergalactic plane and the Shapley Supercluster) upon the Local Group motion, the 68 per cent completeness allows us to sample the large-scale structure better than similar sparsely-sampled surveys. The survey region does not overlap with the areas covered by ongoing wide-angle (Sloan or 2dF) complete redshift surveys. In this paper, the first in a series, we describe the observation and data reduction procedures, the analysis for the redshift errors and survey completeness, and present the survey data. Note that there are some minor change/improvements over the example table published in MNRAS: 1. R.A./Dec. is now J2000 rather than B1950. 2. l/b are now given to 3 decimal places rather than 1 decimal place. 3. Some additional redshifts from NED and ZCAT have been included.</TD>
            <TD>CDS</TD>
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            <TD>08-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/339/652</TD>
            <TD />
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/652</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/339/652 [2]</TD>
            <TD>The FLASH Redshift Survey (Kaldare+ 2003)</TD>
            <TD>The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue consists of 4613 galaxies brighter than b_J_= 16.7 (corrected for Galactic extinction) over a 700-deg^2^ region of sky in the general direction of the Local Group motion. The survey region is a 70x10{deg} strip spanning the sky from the Shapley Supercluster to the Hydra cluster, and contains 3141 galaxies with measured redshifts. Designed to explore the effect of the galaxy concentrations in this direction (in particular the Supergalactic plane and the Shapley Supercluster) upon the Local Group motion, the 68 per cent completeness allows us to sample the large-scale structure better than similar sparsely-sampled surveys. The survey region does not overlap with the areas covered by ongoing wide-angle (Sloan or 2dF) complete redshift surveys. In this paper, the first in a series, we describe the observation and data reduction procedures, the analysis for the redshift errors and survey completeness, and present the survey data. Note that there are some minor change/improvements over the example table published in MNRAS: 1. R.A./Dec. is now J2000 rather than B1950. 2. l/b are now given to 3 decimal places rather than 1 decimal place. 3. Some additional redshifts from NED and ZCAT have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T19:21:54Z</TD>
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            <TD>08-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/339/652&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/652</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/339/652 [catalog]</TD>
            <TD>The FLASH Redshift Survey (Kaldare+ 2003)</TD>
            <TD>The FLAIR Shapley-Hydra (FLASH) redshift survey catalogue consists of 4613 galaxies brighter than b_J_= 16.7 (corrected for Galactic extinction) over a 700-deg^2^ region of sky in the general direction of the Local Group motion. The survey region is a 70x10{deg} strip spanning the sky from the Shapley Supercluster to the Hydra cluster, and contains 3141 galaxies with measured redshifts. Designed to explore the effect of the galaxy concentrations in this direction (in particular the Supergalactic plane and the Shapley Supercluster) upon the Local Group motion, the 68 per cent completeness allows us to sample the large-scale structure better than similar sparsely-sampled surveys. The survey region does not overlap with the areas covered by ongoing wide-angle (Sloan or 2dF) complete redshift surveys. In this paper, the first in a series, we describe the observation and data reduction procedures, the analysis for the redshift errors and survey completeness, and present the survey data. Note that there are some minor change/improvements over the example table published in MNRAS: 1. R.A./Dec. is now J2000 rather than B1950. 2. l/b are now given to 3 decimal places rather than 1 decimal place. 3. Some additional redshifts from NED and ZCAT have been included.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T19:21:54Z</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>08-Apr-2003</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/339/652</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/339/652&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/339/652</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/118/65 [1]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#1</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/118/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/118/65 [2]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#2</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/118/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/65 [table5]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#table5</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/65 [table4]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#table4</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/125/1817 [1]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#1</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/125/1817</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/125/1817 [2]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#2</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
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            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3b]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3b</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2c]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2c</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3c]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3c</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2b]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2b</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3d]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3d</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2a]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2a</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2d]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2d</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3a]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3a</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/118/65 [1]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#1</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/118/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/118/65 [2]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#2</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/118/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/65 [table5]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#table5</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/65 [table4]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#table4</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/125/1817 [1]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#1</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/125/1817</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/125/1817 [2]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#2</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3b]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3b</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2c]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2c</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3c]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3c</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2b]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2b</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3d]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3d</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2a]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2a</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2d]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2d</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3a]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3a</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/118/65 [1]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#1</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/118/65</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/118/65 [2]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#2</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/118/65&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/65 [table5]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#table5</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/118/65 [table4]</TD>
            <TD>BRI &amp; redshifts in Cl0939+472 &amp; Cl0016+161 (Belloni+, 1996)</TD>
            <TD>We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65#table4</TD>
            <TD>2011-09-14T19:09:00Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/118/65</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/118/65&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/118/65</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/125/1817 [1]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#1</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/125/1817</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/125/1817 [2]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#2</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3b]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3b</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2c]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2c</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3c]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3c</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2b]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2b</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3d]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3d</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2a]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2a</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table2d]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table2d</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/125/1817 [table3a]</TD>
            <TD>SDSS Early-Type Galaxies Catalog (Bernardi+, 2003)</TD>
            <TD>A sample of nearly 9000 early-type galaxies, in the redshift range 0.01&lt;=z&lt;=0.3, was selected from the Sloan Digital Sky Survey (SDSS) using morphological and spectral criteria. The paper describes how the sample was selected, presents examples of images and seeing-corrected fits to the observed surface brightness profiles, describes our method for estimating K-corrections, and shows that the SDSS spectra are of sufficiently high quality to measure velocity dispersions accurately. It also provides catalogs of the measured photometric and spectroscopic parameters. In related papers, these data are used to study how early-type galaxy observables, including luminosity, effective radius, surface brightness, color, and velocity dispersion, are correlated with one another.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817#table3a</TD>
            <TD>2011-09-14T19:23:49Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/125/1817</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/125/1817&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/125/1817</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/504/27 [1]</TD>
            <TD>The L_X_-T Relation for Nearby Clusters (Markevitch, 1998)</TD>
            <TD>The X-ray luminosity-temperature relation for nearby T ~= 3.5-10 keV clusters is rederived using new ASCA temperatures and ROSAT luminosities. Both quantities are derived by directly excluding the cooling flow regions. This correction results in a greatly reduced scatter in the L_X_-T relation; cooling flow clusters are similar to others outside the small cooling flow regions. For a fit of the form L_bol_ {prop.to} T^{alpha}^, we obtain {alpha} = 2.64 +/- 0.27 (90%) and a residual rms scatter in log L_bol_ of 0.10. The derived relation can be directly compared to theoretical predictions that do not include radiative cooling. It also provides an accurate reference point for future evolution searches and comparison to cooler clusters. The new temperatures and L_X_-T relation together with a newly selected cluster sample are used to update the temperature function at z ~ 0.05. The resulting function is generally higher and flatter than, although within the errors of, the previous estimates by Edge and coworkers and Henry and Arnaud (as rederived by Eke and coworkers). For a qualitative estimate of constraints that the new data place on the density fluctuation spectrum, we apply the Press-Schechter formalism for {Omega}_0_ = 1 and 0.3. For {Omega}_0_ = 1, assuming cluster isothermality, the temperature function implies {sigma}_8_ = 0.55 +/- 0.03, while taking into account the observed cluster temperature profiles, {sigma}_8_ = 0.51 +/- 0.03, consistent with the previously derived range. The dependence of {sigma}_8_ on {Omega}_0_ is different from the earlier results because of our treatment of the slope of the fluctuation spectrum, n, as a free parameter. For the considered values of {Omega}_0_, n = -(2.0-2.3) +/- 0.3, somewhat steeper than that derived from the earlier temperature function data, in agreement with the local slope of the galaxy fluctuation spectrum from the Automatic Plate Measuring Facility (APM) survey, and significantly steeper than the standard cold dark matter prediction.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27#1</TD>
            <TD>2011-09-14T19:09:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/504/27</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/504/27</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/504/27 [2]</TD>
            <TD>The L_X_-T Relation for Nearby Clusters (Markevitch, 1998)</TD>
            <TD>The X-ray luminosity-temperature relation for nearby T ~= 3.5-10 keV clusters is rederived using new ASCA temperatures and ROSAT luminosities. Both quantities are derived by directly excluding the cooling flow regions. This correction results in a greatly reduced scatter in the L_X_-T relation; cooling flow clusters are similar to others outside the small cooling flow regions. For a fit of the form L_bol_ {prop.to} T^{alpha}^, we obtain {alpha} = 2.64 +/- 0.27 (90%) and a residual rms scatter in log L_bol_ of 0.10. The derived relation can be directly compared to theoretical predictions that do not include radiative cooling. It also provides an accurate reference point for future evolution searches and comparison to cooler clusters. The new temperatures and L_X_-T relation together with a newly selected cluster sample are used to update the temperature function at z ~ 0.05. The resulting function is generally higher and flatter than, although within the errors of, the previous estimates by Edge and coworkers and Henry and Arnaud (as rederived by Eke and coworkers). For a qualitative estimate of constraints that the new data place on the density fluctuation spectrum, we apply the Press-Schechter formalism for {Omega}_0_ = 1 and 0.3. For {Omega}_0_ = 1, assuming cluster isothermality, the temperature function implies {sigma}_8_ = 0.55 +/- 0.03, while taking into account the observed cluster temperature profiles, {sigma}_8_ = 0.51 +/- 0.03, consistent with the previously derived range. The dependence of {sigma}_8_ on {Omega}_0_ is different from the earlier results because of our treatment of the slope of the fluctuation spectrum, n, as a free parameter. For the considered values of {Omega}_0_, n = -(2.0-2.3) +/- 0.3, somewhat steeper than that derived from the earlier temperature function data, in agreement with the local slope of the galaxy fluctuation spectrum from the Automatic Plate Measuring Facility (APM) survey, and significantly steeper than the standard cold dark matter prediction.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27#2</TD>
            <TD>2011-09-14T19:09:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/504/27&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/504/27</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/504/27 [table1]</TD>
            <TD>The L_X_-T Relation for Nearby Clusters (Markevitch, 1998)</TD>
            <TD>The X-ray luminosity-temperature relation for nearby T ~= 3.5-10 keV clusters is rederived using new ASCA temperatures and ROSAT luminosities. Both quantities are derived by directly excluding the cooling flow regions. This correction results in a greatly reduced scatter in the L_X_-T relation; cooling flow clusters are similar to others outside the small cooling flow regions. For a fit of the form L_bol_ {prop.to} T^{alpha}^, we obtain {alpha} = 2.64 +/- 0.27 (90%) and a residual rms scatter in log L_bol_ of 0.10. The derived relation can be directly compared to theoretical predictions that do not include radiative cooling. It also provides an accurate reference point for future evolution searches and comparison to cooler clusters. The new temperatures and L_X_-T relation together with a newly selected cluster sample are used to update the temperature function at z ~ 0.05. The resulting function is generally higher and flatter than, although within the errors of, the previous estimates by Edge and coworkers and Henry and Arnaud (as rederived by Eke and coworkers). For a qualitative estimate of constraints that the new data place on the density fluctuation spectrum, we apply the Press-Schechter formalism for {Omega}_0_ = 1 and 0.3. For {Omega}_0_ = 1, assuming cluster isothermality, the temperature function implies {sigma}_8_ = 0.55 +/- 0.03, while taking into account the observed cluster temperature profiles, {sigma}_8_ = 0.51 +/- 0.03, consistent with the previously derived range. The dependence of {sigma}_8_ on {Omega}_0_ is different from the earlier results because of our treatment of the slope of the fluctuation spectrum, n, as a free parameter. For the considered values of {Omega}_0_, n = -(2.0-2.3) +/- 0.3, somewhat steeper than that derived from the earlier temperature function data, in agreement with the local slope of the galaxy fluctuation spectrum from the Automatic Plate Measuring Facility (APM) survey, and significantly steeper than the standard cold dark matter prediction.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27#table1</TD>
            <TD>2011-09-14T19:09:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/504/27&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/504/27</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/120/247 [1]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#1</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/120/247</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/120/247 [2]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#2</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/120/247&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/120/247 [table4]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#table4</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/120/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/120/247 [table1]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#table1</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/120/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/504/27 [1]</TD>
            <TD>The L_X_-T Relation for Nearby Clusters (Markevitch, 1998)</TD>
            <TD>The X-ray luminosity-temperature relation for nearby T ~= 3.5-10 keV clusters is rederived using new ASCA temperatures and ROSAT luminosities. Both quantities are derived by directly excluding the cooling flow regions. This correction results in a greatly reduced scatter in the L_X_-T relation; cooling flow clusters are similar to others outside the small cooling flow regions. For a fit of the form L_bol_ {prop.to} T^{alpha}^, we obtain {alpha} = 2.64 +/- 0.27 (90%) and a residual rms scatter in log L_bol_ of 0.10. The derived relation can be directly compared to theoretical predictions that do not include radiative cooling. It also provides an accurate reference point for future evolution searches and comparison to cooler clusters. The new temperatures and L_X_-T relation together with a newly selected cluster sample are used to update the temperature function at z ~ 0.05. The resulting function is generally higher and flatter than, although within the errors of, the previous estimates by Edge and coworkers and Henry and Arnaud (as rederived by Eke and coworkers). For a qualitative estimate of constraints that the new data place on the density fluctuation spectrum, we apply the Press-Schechter formalism for {Omega}_0_ = 1 and 0.3. For {Omega}_0_ = 1, assuming cluster isothermality, the temperature function implies {sigma}_8_ = 0.55 +/- 0.03, while taking into account the observed cluster temperature profiles, {sigma}_8_ = 0.51 +/- 0.03, consistent with the previously derived range. The dependence of {sigma}_8_ on {Omega}_0_ is different from the earlier results because of our treatment of the slope of the fluctuation spectrum, n, as a free parameter. For the considered values of {Omega}_0_, n = -(2.0-2.3) +/- 0.3, somewhat steeper than that derived from the earlier temperature function data, in agreement with the local slope of the galaxy fluctuation spectrum from the Automatic Plate Measuring Facility (APM) survey, and significantly steeper than the standard cold dark matter prediction.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27#1</TD>
            <TD>2011-09-14T19:09:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/504/27</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/504/27</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/504/27 [2]</TD>
            <TD>The L_X_-T Relation for Nearby Clusters (Markevitch, 1998)</TD>
            <TD>The X-ray luminosity-temperature relation for nearby T ~= 3.5-10 keV clusters is rederived using new ASCA temperatures and ROSAT luminosities. Both quantities are derived by directly excluding the cooling flow regions. This correction results in a greatly reduced scatter in the L_X_-T relation; cooling flow clusters are similar to others outside the small cooling flow regions. For a fit of the form L_bol_ {prop.to} T^{alpha}^, we obtain {alpha} = 2.64 +/- 0.27 (90%) and a residual rms scatter in log L_bol_ of 0.10. The derived relation can be directly compared to theoretical predictions that do not include radiative cooling. It also provides an accurate reference point for future evolution searches and comparison to cooler clusters. The new temperatures and L_X_-T relation together with a newly selected cluster sample are used to update the temperature function at z ~ 0.05. The resulting function is generally higher and flatter than, although within the errors of, the previous estimates by Edge and coworkers and Henry and Arnaud (as rederived by Eke and coworkers). For a qualitative estimate of constraints that the new data place on the density fluctuation spectrum, we apply the Press-Schechter formalism for {Omega}_0_ = 1 and 0.3. For {Omega}_0_ = 1, assuming cluster isothermality, the temperature function implies {sigma}_8_ = 0.55 +/- 0.03, while taking into account the observed cluster temperature profiles, {sigma}_8_ = 0.51 +/- 0.03, consistent with the previously derived range. The dependence of {sigma}_8_ on {Omega}_0_ is different from the earlier results because of our treatment of the slope of the fluctuation spectrum, n, as a free parameter. For the considered values of {Omega}_0_, n = -(2.0-2.3) +/- 0.3, somewhat steeper than that derived from the earlier temperature function data, in agreement with the local slope of the galaxy fluctuation spectrum from the Automatic Plate Measuring Facility (APM) survey, and significantly steeper than the standard cold dark matter prediction.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27#2</TD>
            <TD>2011-09-14T19:09:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/504/27&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/504/27</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/504/27 [table1]</TD>
            <TD>The L_X_-T Relation for Nearby Clusters (Markevitch, 1998)</TD>
            <TD>The X-ray luminosity-temperature relation for nearby T ~= 3.5-10 keV clusters is rederived using new ASCA temperatures and ROSAT luminosities. Both quantities are derived by directly excluding the cooling flow regions. This correction results in a greatly reduced scatter in the L_X_-T relation; cooling flow clusters are similar to others outside the small cooling flow regions. For a fit of the form L_bol_ {prop.to} T^{alpha}^, we obtain {alpha} = 2.64 +/- 0.27 (90%) and a residual rms scatter in log L_bol_ of 0.10. The derived relation can be directly compared to theoretical predictions that do not include radiative cooling. It also provides an accurate reference point for future evolution searches and comparison to cooler clusters. The new temperatures and L_X_-T relation together with a newly selected cluster sample are used to update the temperature function at z ~ 0.05. The resulting function is generally higher and flatter than, although within the errors of, the previous estimates by Edge and coworkers and Henry and Arnaud (as rederived by Eke and coworkers). For a qualitative estimate of constraints that the new data place on the density fluctuation spectrum, we apply the Press-Schechter formalism for {Omega}_0_ = 1 and 0.3. For {Omega}_0_ = 1, assuming cluster isothermality, the temperature function implies {sigma}_8_ = 0.55 +/- 0.03, while taking into account the observed cluster temperature profiles, {sigma}_8_ = 0.51 +/- 0.03, consistent with the previously derived range. The dependence of {sigma}_8_ on {Omega}_0_ is different from the earlier results because of our treatment of the slope of the fluctuation spectrum, n, as a free parameter. For the considered values of {Omega}_0_, n = -(2.0-2.3) +/- 0.3, somewhat steeper than that derived from the earlier temperature function data, in agreement with the local slope of the galaxy fluctuation spectrum from the Automatic Plate Measuring Facility (APM) survey, and significantly steeper than the standard cold dark matter prediction.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27#table1</TD>
            <TD>2011-09-14T19:09:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/504/27&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/504/27</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/120/247 [1]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#1</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/120/247</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/120/247 [2]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#2</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/120/247&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/120/247 [table4]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#table4</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/120/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/120/247 [table1]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#table1</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/120/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/504/27 [1]</TD>
            <TD>The L_X_-T Relation for Nearby Clusters (Markevitch, 1998)</TD>
            <TD>The X-ray luminosity-temperature relation for nearby T ~= 3.5-10 keV clusters is rederived using new ASCA temperatures and ROSAT luminosities. Both quantities are derived by directly excluding the cooling flow regions. This correction results in a greatly reduced scatter in the L_X_-T relation; cooling flow clusters are similar to others outside the small cooling flow regions. For a fit of the form L_bol_ {prop.to} T^{alpha}^, we obtain {alpha} = 2.64 +/- 0.27 (90%) and a residual rms scatter in log L_bol_ of 0.10. The derived relation can be directly compared to theoretical predictions that do not include radiative cooling. It also provides an accurate reference point for future evolution searches and comparison to cooler clusters. The new temperatures and L_X_-T relation together with a newly selected cluster sample are used to update the temperature function at z ~ 0.05. The resulting function is generally higher and flatter than, although within the errors of, the previous estimates by Edge and coworkers and Henry and Arnaud (as rederived by Eke and coworkers). For a qualitative estimate of constraints that the new data place on the density fluctuation spectrum, we apply the Press-Schechter formalism for {Omega}_0_ = 1 and 0.3. For {Omega}_0_ = 1, assuming cluster isothermality, the temperature function implies {sigma}_8_ = 0.55 +/- 0.03, while taking into account the observed cluster temperature profiles, {sigma}_8_ = 0.51 +/- 0.03, consistent with the previously derived range. The dependence of {sigma}_8_ on {Omega}_0_ is different from the earlier results because of our treatment of the slope of the fluctuation spectrum, n, as a free parameter. For the considered values of {Omega}_0_, n = -(2.0-2.3) +/- 0.3, somewhat steeper than that derived from the earlier temperature function data, in agreement with the local slope of the galaxy fluctuation spectrum from the Automatic Plate Measuring Facility (APM) survey, and significantly steeper than the standard cold dark matter prediction.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27#1</TD>
            <TD>2011-09-14T19:09:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/504/27</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/504/27</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/504/27 [2]</TD>
            <TD>The L_X_-T Relation for Nearby Clusters (Markevitch, 1998)</TD>
            <TD>The X-ray luminosity-temperature relation for nearby T ~= 3.5-10 keV clusters is rederived using new ASCA temperatures and ROSAT luminosities. Both quantities are derived by directly excluding the cooling flow regions. This correction results in a greatly reduced scatter in the L_X_-T relation; cooling flow clusters are similar to others outside the small cooling flow regions. For a fit of the form L_bol_ {prop.to} T^{alpha}^, we obtain {alpha} = 2.64 +/- 0.27 (90%) and a residual rms scatter in log L_bol_ of 0.10. The derived relation can be directly compared to theoretical predictions that do not include radiative cooling. It also provides an accurate reference point for future evolution searches and comparison to cooler clusters. The new temperatures and L_X_-T relation together with a newly selected cluster sample are used to update the temperature function at z ~ 0.05. The resulting function is generally higher and flatter than, although within the errors of, the previous estimates by Edge and coworkers and Henry and Arnaud (as rederived by Eke and coworkers). For a qualitative estimate of constraints that the new data place on the density fluctuation spectrum, we apply the Press-Schechter formalism for {Omega}_0_ = 1 and 0.3. For {Omega}_0_ = 1, assuming cluster isothermality, the temperature function implies {sigma}_8_ = 0.55 +/- 0.03, while taking into account the observed cluster temperature profiles, {sigma}_8_ = 0.51 +/- 0.03, consistent with the previously derived range. The dependence of {sigma}_8_ on {Omega}_0_ is different from the earlier results because of our treatment of the slope of the fluctuation spectrum, n, as a free parameter. For the considered values of {Omega}_0_, n = -(2.0-2.3) +/- 0.3, somewhat steeper than that derived from the earlier temperature function data, in agreement with the local slope of the galaxy fluctuation spectrum from the Automatic Plate Measuring Facility (APM) survey, and significantly steeper than the standard cold dark matter prediction.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27#2</TD>
            <TD>2011-09-14T19:09:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/504/27&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/504/27</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/504/27 [table1]</TD>
            <TD>The L_X_-T Relation for Nearby Clusters (Markevitch, 1998)</TD>
            <TD>The X-ray luminosity-temperature relation for nearby T ~= 3.5-10 keV clusters is rederived using new ASCA temperatures and ROSAT luminosities. Both quantities are derived by directly excluding the cooling flow regions. This correction results in a greatly reduced scatter in the L_X_-T relation; cooling flow clusters are similar to others outside the small cooling flow regions. For a fit of the form L_bol_ {prop.to} T^{alpha}^, we obtain {alpha} = 2.64 +/- 0.27 (90%) and a residual rms scatter in log L_bol_ of 0.10. The derived relation can be directly compared to theoretical predictions that do not include radiative cooling. It also provides an accurate reference point for future evolution searches and comparison to cooler clusters. The new temperatures and L_X_-T relation together with a newly selected cluster sample are used to update the temperature function at z ~ 0.05. The resulting function is generally higher and flatter than, although within the errors of, the previous estimates by Edge and coworkers and Henry and Arnaud (as rederived by Eke and coworkers). For a qualitative estimate of constraints that the new data place on the density fluctuation spectrum, we apply the Press-Schechter formalism for {Omega}_0_ = 1 and 0.3. For {Omega}_0_ = 1, assuming cluster isothermality, the temperature function implies {sigma}_8_ = 0.55 +/- 0.03, while taking into account the observed cluster temperature profiles, {sigma}_8_ = 0.51 +/- 0.03, consistent with the previously derived range. The dependence of {sigma}_8_ on {Omega}_0_ is different from the earlier results because of our treatment of the slope of the fluctuation spectrum, n, as a free parameter. For the considered values of {Omega}_0_, n = -(2.0-2.3) +/- 0.3, somewhat steeper than that derived from the earlier temperature function data, in agreement with the local slope of the galaxy fluctuation spectrum from the Automatic Plate Measuring Facility (APM) survey, and significantly steeper than the standard cold dark matter prediction.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27#table1</TD>
            <TD>2011-09-14T19:09:53Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Jul-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/504/27</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/504/27&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/504/27</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/120/247 [1]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#1</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/120/247</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/120/247 [2]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#2</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/120/247&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/120/247 [table4]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#table4</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/120/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/120/247 [table1]</TD>
            <TD>Supernova remnants in M33 (Gordon+, 1999)</TD>
            <TD>Using radio data to identify and optical data to confirm, we have established the largest and most complete sample of extragalactic radio-bright supernova remnants (SNRs) in the nearby spiral galaxy M33. We have identified 53 radio SNRs, doubling the size of the earlier survey by Duric et al. (1993A&amp;AS...99..217D).</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247#table1</TD>
            <TD>2011-09-14T19:23:53Z</TD>
            <TD>#SuperNovae_Remnants#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/120/247</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/120/247&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/120/247</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/2020 [1]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#1</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/2020</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/2020 [2]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#2</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/2020&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2020 [table3]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#table3</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2020&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2020 [table1]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#table1</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2020&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/3061 [1]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#1</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/3061</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/3061 [2]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#2</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/3061 [table3]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#table3</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/3061 [table2]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#table2</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/3061 [table1]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#table1</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/2020 [1]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#1</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/2020</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/2020 [2]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#2</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/2020&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2020 [table3]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#table3</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2020&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2020 [table1]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#table1</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2020&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/3061 [1]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#1</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/3061</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/3061 [2]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#2</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/3061 [table3]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#table3</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/3061 [table2]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#table2</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/3061 [table1]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#table1</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/121/2020 [1]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#1</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/121/2020</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/121/2020 [2]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#2</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/121/2020&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2020 [table3]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#table3</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2020&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/121/2020 [table1]</TD>
            <TD>CTIO and WFPC2 photometry in NGC 6822 (Bianchi+, 2001)</TD>
            <TD>We investigate the massive star population of NGC 6822 with ground-based UBV photometry covering the whole of the galaxy and HST WFPC2 photometry with filters F255W, F336W, F439W, and F555W of two fields containing very rich and crowded OB associations. The four-band WFPC2 photometry is used to derive Teff and E(B-V). H-R diagrams are constructed for the OB associations included in our fields. These show that 10Myr old populations are present in OB 9 and OB 6, while more recent star formation have occurred in OB 8, OB 13, OB 15, and OB 7. Two particularly interesting H II regions, Hubble V and Hubble X, are included in our fields. The luminous massive stars that power these bright H II regions (H{alpha} luminosity several times that of the Orion nebula), could be resolved even in their dense cores thanks to the HST spatial resolution. Our data reveal very young (a few million years), apparently coeval populations, with several massive star candidates.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020#table1</TD>
            <TD>2011-09-14T19:11:21Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/AJ/121/2020</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/121/2020&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/121/2020</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/3061 [1]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#1</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/3061</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/3061 [2]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#2</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/3061 [table3]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#table3</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/3061 [table2]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#table2</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/3061 [table1]</TD>
            <TD>uz,vz,bz,yz photometry in Coma cluster (Odell+, 2002)</TD>
            <TD>The Coma Cluster (Abell 1656) is roughly 89' in radius, with three dominant galaxies (NGC 4889, 4874, and 4839) forming the core of three separate cluster components. The first two of these, only 7' apart, seem to be the relic central galaxies of previous groups that have recently merged into the current cluster. An additional subcluster, centered on the third galaxy, NGC 4839, 40' to the southwest, seems to be falling into the central region or has just passed through the main body of the cluster, perhaps triggering new star formation. Each section of the Coma Cluster was observed with the Kuiper 1.55m telescope of the Steward Observatory on Mount Bigelow, Arizona. Data was taken with the LPL Focal Reducer and 2K CCD chip (binned to 1K), which yielded 0.65"/pix or a field size of 10.8'. We centered one field on NGC 4889 (2000 April 24) and the other on the central giant NGC 4874 (2000 May 10-11). Our results are restricted to these central regions and therefore are not necessarily typical for the whole cluster. The total April exposure time for the uz filter was 11700s, the vz filter 9600s, the bz filter 3000s, and the yz filter 3000s. Each set of exposures was divided in frames of 600-1200s to reduce the influence of cosmic rays and irregularities of pixels on the chip. For the May observing run, the total exposure times were 7200s in each of yz and bz and 9600s in vz. Weather conditions restricted the uz filter to 2400s, and therefore it is of lower quality. Calibration was obtained through a number of spectrophotometric standards measured on each night. The region around NGC 4839 was observed with the 4 m Mayall telescope of the National Optical Astronomy Observatory (NOAO) on Kitt Peak, Arizona (2001 June 27-28). The Prime Focus T2KB CCD camera produces a 14' field with 0.42"/pix. The total exposure of 1800s in each filter consists of three 300s exposures each night.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061#table1</TD>
            <TD>2011-09-14T19:24:08Z</TD>
            <TD>#Abundances#Photometry:narrow-band#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/3061</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/3061&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/3061</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/551/973 [1]</TD>
            <TD>Variables near SN 1991T in NGC 4527 (Saha+, 2001)</TD>
            <TD>Repeated imaging observations have been made of NGC 4527 with the Hubble Space Telescope between 1999 April and June, over an interval of 69 days. Images were obtained on 12 epochs in the F555W band and on five epochs in the F814W band. The galaxy hosted the Type Ia supernova SN 1991T, which showed relatively unusual behaviour by having both an abnormal spectrum near light maximum, and a slower declining light curve than the prototypical Branch-normal SNe Ia. A total of 86 variables that are putative Cepheids have been found, with periods ranging from 7.4 days to over 70 days.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/973#1</TD>
            <TD>2011-09-14T19:11:35Z</TD>
            <TD>#Photometry#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/973</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/551/973</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/973</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/551/973 [2]</TD>
            <TD>Variables near SN 1991T in NGC 4527 (Saha+, 2001)</TD>
            <TD>Repeated imaging observations have been made of NGC 4527 with the Hubble Space Telescope between 1999 April and June, over an interval of 69 days. Images were obtained on 12 epochs in the F555W band and on five epochs in the F814W band. The galaxy hosted the Type Ia supernova SN 1991T, which showed relatively unusual behaviour by having both an abnormal spectrum near light maximum, and a slower declining light curve than the prototypical Branch-normal SNe Ia. A total of 86 variables that are putative Cepheids have been found, with periods ranging from 7.4 days to over 70 days.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/973#2</TD>
            <TD>2011-09-14T19:11:35Z</TD>
            <TD>#Photometry#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/973</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/551/973&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/973</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/237 [1]</TD>
            <TD>HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)</TD>
            <TD>We present the new catalog of principal galaxies (PGC2003). It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than ~18B-mag. In order to provide the best possible identification for each galaxy we give: accurate coordinates (typical accuracy better than 2 arcsec), diameter, axis ratio and position angle. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25B-mag/arcsec^2^, using a new method, the EPIDEMIC method. In order to provide the best designation for each galaxy, we collected the names from 50 catalogues. The compatibility of the spelling is tested against NED and SIMBAD, and, as far as possible we used a spelling compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, we propose some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, http://leda.univ-lyon1.fr/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/237#1</TD>
            <TD>2011-09-14T19:24:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/VII/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/237 [2]</TD>
            <TD>HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)</TD>
            <TD>We present the new catalog of principal galaxies (PGC2003). It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than ~18B-mag. In order to provide the best possible identification for each galaxy we give: accurate coordinates (typical accuracy better than 2 arcsec), diameter, axis ratio and position angle. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25B-mag/arcsec^2^, using a new method, the EPIDEMIC method. In order to provide the best designation for each galaxy, we collected the names from 50 catalogues. The compatibility of the spelling is tested against NED and SIMBAD, and, as far as possible we used a spelling compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, we propose some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, http://leda.univ-lyon1.fr/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/237#2</TD>
            <TD>2011-09-14T19:24:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/VII/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/237 [pgc]</TD>
            <TD>HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)</TD>
            <TD>We present the new catalog of principal galaxies (PGC2003). It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than ~18B-mag. In order to provide the best possible identification for each galaxy we give: accurate coordinates (typical accuracy better than 2 arcsec), diameter, axis ratio and position angle. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25B-mag/arcsec^2^, using a new method, the EPIDEMIC method. In order to provide the best designation for each galaxy, we collected the names from 50 catalogues. The compatibility of the spelling is tested against NED and SIMBAD, and, as far as possible we used a spelling compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, we propose some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, http://leda.univ-lyon1.fr/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/237#pgc</TD>
            <TD>2011-09-14T19:24:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/VII/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/551/973 [1]</TD>
            <TD>Variables near SN 1991T in NGC 4527 (Saha+, 2001)</TD>
            <TD>Repeated imaging observations have been made of NGC 4527 with the Hubble Space Telescope between 1999 April and June, over an interval of 69 days. Images were obtained on 12 epochs in the F555W band and on five epochs in the F814W band. The galaxy hosted the Type Ia supernova SN 1991T, which showed relatively unusual behaviour by having both an abnormal spectrum near light maximum, and a slower declining light curve than the prototypical Branch-normal SNe Ia. A total of 86 variables that are putative Cepheids have been found, with periods ranging from 7.4 days to over 70 days.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/973#1</TD>
            <TD>2011-09-14T19:11:35Z</TD>
            <TD>#Photometry#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/973</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/551/973</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/973</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/551/973 [2]</TD>
            <TD>Variables near SN 1991T in NGC 4527 (Saha+, 2001)</TD>
            <TD>Repeated imaging observations have been made of NGC 4527 with the Hubble Space Telescope between 1999 April and June, over an interval of 69 days. Images were obtained on 12 epochs in the F555W band and on five epochs in the F814W band. The galaxy hosted the Type Ia supernova SN 1991T, which showed relatively unusual behaviour by having both an abnormal spectrum near light maximum, and a slower declining light curve than the prototypical Branch-normal SNe Ia. A total of 86 variables that are putative Cepheids have been found, with periods ranging from 7.4 days to over 70 days.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/973#2</TD>
            <TD>2011-09-14T19:11:35Z</TD>
            <TD>#Photometry#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/551/973</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/551/973&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/551/973</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/237 [1]</TD>
            <TD>HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)</TD>
            <TD>We present the new catalog of principal galaxies (PGC2003). It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than ~18B-mag. In order to provide the best possible identification for each galaxy we give: accurate coordinates (typical accuracy better than 2 arcsec), diameter, axis ratio and position angle. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25B-mag/arcsec^2^, using a new method, the EPIDEMIC method. In order to provide the best designation for each galaxy, we collected the names from 50 catalogues. The compatibility of the spelling is tested against NED and SIMBAD, and, as far as possible we used a spelling compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, we propose some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, http://leda.univ-lyon1.fr/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/237#1</TD>
            <TD>2011-09-14T19:24:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/VII/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/237 [2]</TD>
            <TD>HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)</TD>
            <TD>We present the new catalog of principal galaxies (PGC2003). It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than ~18B-mag. In order to provide the best possible identification for each galaxy we give: accurate coordinates (typical accuracy better than 2 arcsec), diameter, axis ratio and position angle. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25B-mag/arcsec^2^, using a new method, the EPIDEMIC method. In order to provide the best designation for each galaxy, we collected the names from 50 catalogues. The compatibility of the spelling is tested against NED and SIMBAD, and, as far as possible we used a spelling compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, we propose some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, http://leda.univ-lyon1.fr/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/237#2</TD>
            <TD>2011-09-14T19:24:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/VII/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/237 [pgc]</TD>
            <TD>HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)</TD>
            <TD>We present the new catalog of principal galaxies (PGC2003). It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than ~18B-mag. In order to provide the best possible identification for each galaxy we give: accurate coordinates (typical accuracy better than 2 arcsec), diameter, axis ratio and position angle. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25B-mag/arcsec^2^, using a new method, the EPIDEMIC method. In order to provide the best designation for each galaxy, we collected the names from 50 catalogues. The compatibility of the spelling is tested against NED and SIMBAD, and, as far as possible we used a spelling compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, we propose some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, http://leda.univ-lyon1.fr/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/237#pgc</TD>
            <TD>2011-09-14T19:24:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/VII/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/502/558 [1]</TD>
            <TD>Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)</TD>
            <TD>We present a catalog of 203 clusters of galaxies serendipitously detected in 647 ROSAT PSPC high Galactic latitude pointings covering 158deg^2^. This is one of the largest X-ray-selected cluster samples, comparable in size only to the ROSAT All-Sky Survey sample of nearby clusters (Ebeling et al., 1997ApJ...479L.101E). We detect clusters in the inner 175 of the ROSAT PSPC field of view using the spatial extent of their X-ray emission. Fluxes of detected clusters range from 1.6x10^-14^ to 8x10^-12^ergs/s/cm^2^ in the 0.52keV energy band. X-ray luminosities range from 10^42^ergs/s, corresponding to very poor groups, to ~5x10^44^ergs/s, corresponding to rich clusters. The cluster redshifts range from z=0.015 to z&gt;0.5. The catalog lists X-ray fluxes, core radii, and spectroscopic redshifts for 73 clusters and photometric redshifts for the remainder.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558#1</TD>
            <TD>2011-09-14T19:12:24Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/502/558</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/502/558</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/502/558 [2]</TD>
            <TD>Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)</TD>
            <TD>We present a catalog of 203 clusters of galaxies serendipitously detected in 647 ROSAT PSPC high Galactic latitude pointings covering 158deg^2^. This is one of the largest X-ray-selected cluster samples, comparable in size only to the ROSAT All-Sky Survey sample of nearby clusters (Ebeling et al., 1997ApJ...479L.101E). We detect clusters in the inner 175 of the ROSAT PSPC field of view using the spatial extent of their X-ray emission. Fluxes of detected clusters range from 1.6x10^-14^ to 8x10^-12^ergs/s/cm^2^ in the 0.52keV energy band. X-ray luminosities range from 10^42^ergs/s, corresponding to very poor groups, to ~5x10^44^ergs/s, corresponding to rich clusters. The cluster redshifts range from z=0.015 to z&gt;0.5. The catalog lists X-ray fluxes, core radii, and spectroscopic redshifts for 73 clusters and photometric redshifts for the remainder.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558#2</TD>
            <TD>2011-09-14T19:12:24Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/502/558&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/502/558</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/502/558 [table3]</TD>
            <TD>Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)</TD>
            <TD>We present a catalog of 203 clusters of galaxies serendipitously detected in 647 ROSAT PSPC high Galactic latitude pointings covering 158deg^2^. This is one of the largest X-ray-selected cluster samples, comparable in size only to the ROSAT All-Sky Survey sample of nearby clusters (Ebeling et al., 1997ApJ...479L.101E). We detect clusters in the inner 175 of the ROSAT PSPC field of view using the spatial extent of their X-ray emission. Fluxes of detected clusters range from 1.6x10^-14^ to 8x10^-12^ergs/s/cm^2^ in the 0.52keV energy band. X-ray luminosities range from 10^42^ergs/s, corresponding to very poor groups, to ~5x10^44^ergs/s, corresponding to rich clusters. The cluster redshifts range from z=0.015 to z&gt;0.5. The catalog lists X-ray fluxes, core radii, and spectroscopic redshifts for 73 clusters and photometric redshifts for the remainder.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558#table3</TD>
            <TD>2011-09-14T19:12:24Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/502/558&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/502/558</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/237 [1]</TD>
            <TD>HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)</TD>
            <TD>We present the new catalog of principal galaxies (PGC2003). It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than ~18B-mag. In order to provide the best possible identification for each galaxy we give: accurate coordinates (typical accuracy better than 2 arcsec), diameter, axis ratio and position angle. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25B-mag/arcsec^2^, using a new method, the EPIDEMIC method. In order to provide the best designation for each galaxy, we collected the names from 50 catalogues. The compatibility of the spelling is tested against NED and SIMBAD, and, as far as possible we used a spelling compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, we propose some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, http://leda.univ-lyon1.fr/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/237#1</TD>
            <TD>2011-09-14T19:24:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/VII/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/237</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/237</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/237 [2]</TD>
            <TD>HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)</TD>
            <TD>We present the new catalog of principal galaxies (PGC2003). It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than ~18B-mag. In order to provide the best possible identification for each galaxy we give: accurate coordinates (typical accuracy better than 2 arcsec), diameter, axis ratio and position angle. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25B-mag/arcsec^2^, using a new method, the EPIDEMIC method. In order to provide the best designation for each galaxy, we collected the names from 50 catalogues. The compatibility of the spelling is tested against NED and SIMBAD, and, as far as possible we used a spelling compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, we propose some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, http://leda.univ-lyon1.fr/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/237#2</TD>
            <TD>2011-09-14T19:24:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/VII/237</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/237&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/237</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/237 [pgc]</TD>
            <TD>HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)</TD>
            <TD>We present the new catalog of principal galaxies (PGC2003). It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than ~18B-mag. In order to provide the best possible identification for each galaxy we give: accurate coordinates (typical accuracy better than 2 arcsec), diameter, axis ratio and position angle. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25B-mag/arcsec^2^, using a new method, the EPIDEMIC method. In order to provide the best designation for each galaxy, we collected the names from 50 catalogues. The compatibility of the spelling is tested against NED and SIMBAD, and, as far as possible we used a spelling compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, we propose some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, http://leda.univ-lyon1.fr/ .</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/237#pgc</TD>
            <TD>2011-09-14T19:24:40Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/VII/237</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/237&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/237</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/502/558 [1]</TD>
            <TD>Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)</TD>
            <TD>We present a catalog of 203 clusters of galaxies serendipitously detected in 647 ROSAT PSPC high Galactic latitude pointings covering 158deg^2^. This is one of the largest X-ray-selected cluster samples, comparable in size only to the ROSAT All-Sky Survey sample of nearby clusters (Ebeling et al., 1997ApJ...479L.101E). We detect clusters in the inner 175 of the ROSAT PSPC field of view using the spatial extent of their X-ray emission. Fluxes of detected clusters range from 1.6x10^-14^ to 8x10^-12^ergs/s/cm^2^ in the 0.52keV energy band. X-ray luminosities range from 10^42^ergs/s, corresponding to very poor groups, to ~5x10^44^ergs/s, corresponding to rich clusters. The cluster redshifts range from z=0.015 to z&gt;0.5. The catalog lists X-ray fluxes, core radii, and spectroscopic redshifts for 73 clusters and photometric redshifts for the remainder.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558#1</TD>
            <TD>2011-09-14T19:12:24Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/502/558</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/502/558</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/502/558 [2]</TD>
            <TD>Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)</TD>
            <TD>We present a catalog of 203 clusters of galaxies serendipitously detected in 647 ROSAT PSPC high Galactic latitude pointings covering 158deg^2^. This is one of the largest X-ray-selected cluster samples, comparable in size only to the ROSAT All-Sky Survey sample of nearby clusters (Ebeling et al., 1997ApJ...479L.101E). We detect clusters in the inner 175 of the ROSAT PSPC field of view using the spatial extent of their X-ray emission. Fluxes of detected clusters range from 1.6x10^-14^ to 8x10^-12^ergs/s/cm^2^ in the 0.52keV energy band. X-ray luminosities range from 10^42^ergs/s, corresponding to very poor groups, to ~5x10^44^ergs/s, corresponding to rich clusters. The cluster redshifts range from z=0.015 to z&gt;0.5. The catalog lists X-ray fluxes, core radii, and spectroscopic redshifts for 73 clusters and photometric redshifts for the remainder.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558#2</TD>
            <TD>2011-09-14T19:12:24Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/502/558&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/502/558</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/502/558 [table3]</TD>
            <TD>Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)</TD>
            <TD>We present a catalog of 203 clusters of galaxies serendipitously detected in 647 ROSAT PSPC high Galactic latitude pointings covering 158deg^2^. This is one of the largest X-ray-selected cluster samples, comparable in size only to the ROSAT All-Sky Survey sample of nearby clusters (Ebeling et al., 1997ApJ...479L.101E). We detect clusters in the inner 175 of the ROSAT PSPC field of view using the spatial extent of their X-ray emission. Fluxes of detected clusters range from 1.6x10^-14^ to 8x10^-12^ergs/s/cm^2^ in the 0.52keV energy band. X-ray luminosities range from 10^42^ergs/s, corresponding to very poor groups, to ~5x10^44^ergs/s, corresponding to rich clusters. The cluster redshifts range from z=0.015 to z&gt;0.5. The catalog lists X-ray fluxes, core radii, and spectroscopic redshifts for 73 clusters and photometric redshifts for the remainder.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558#table3</TD>
            <TD>2011-09-14T19:12:24Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/502/558&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/502/558</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/413/771 [1]</TD>
            <TD>Galaxies in the Tycho-2 catalogue (Metz+, 2004)</TD>
            <TD>We have identified galaxies in the Tycho-2 Catalogue (Cat. &lt;I/259&gt;) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. &lt;VII/119&gt;) and the Tycho-2 positions of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771#1</TD>
            <TD>2011-09-14T19:26:09Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/413/771</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/413/771</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/413/771 [2]</TD>
            <TD>Galaxies in the Tycho-2 catalogue (Metz+, 2004)</TD>
            <TD>We have identified galaxies in the Tycho-2 Catalogue (Cat. &lt;I/259&gt;) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. &lt;VII/119&gt;) and the Tycho-2 positions of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771#2</TD>
            <TD>2011-09-14T19:26:09Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/413/771&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/413/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/413/771 [table]</TD>
            <TD>Galaxies in the Tycho-2 catalogue (Metz+, 2004)</TD>
            <TD>We have identified galaxies in the Tycho-2 Catalogue (Cat. &lt;I/259&gt;) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. &lt;VII/119&gt;) and the Tycho-2 positions of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771#table</TD>
            <TD>2011-09-14T19:26:09Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/413/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/413/771</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/502/558 [1]</TD>
            <TD>Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)</TD>
            <TD>We present a catalog of 203 clusters of galaxies serendipitously detected in 647 ROSAT PSPC high Galactic latitude pointings covering 158deg^2^. This is one of the largest X-ray-selected cluster samples, comparable in size only to the ROSAT All-Sky Survey sample of nearby clusters (Ebeling et al., 1997ApJ...479L.101E). We detect clusters in the inner 175 of the ROSAT PSPC field of view using the spatial extent of their X-ray emission. Fluxes of detected clusters range from 1.6x10^-14^ to 8x10^-12^ergs/s/cm^2^ in the 0.52keV energy band. X-ray luminosities range from 10^42^ergs/s, corresponding to very poor groups, to ~5x10^44^ergs/s, corresponding to rich clusters. The cluster redshifts range from z=0.015 to z&gt;0.5. The catalog lists X-ray fluxes, core radii, and spectroscopic redshifts for 73 clusters and photometric redshifts for the remainder.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558#1</TD>
            <TD>2011-09-14T19:12:24Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/502/558</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/502/558</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/502/558 [2]</TD>
            <TD>Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)</TD>
            <TD>We present a catalog of 203 clusters of galaxies serendipitously detected in 647 ROSAT PSPC high Galactic latitude pointings covering 158deg^2^. This is one of the largest X-ray-selected cluster samples, comparable in size only to the ROSAT All-Sky Survey sample of nearby clusters (Ebeling et al., 1997ApJ...479L.101E). We detect clusters in the inner 175 of the ROSAT PSPC field of view using the spatial extent of their X-ray emission. Fluxes of detected clusters range from 1.6x10^-14^ to 8x10^-12^ergs/s/cm^2^ in the 0.52keV energy band. X-ray luminosities range from 10^42^ergs/s, corresponding to very poor groups, to ~5x10^44^ergs/s, corresponding to rich clusters. The cluster redshifts range from z=0.015 to z&gt;0.5. The catalog lists X-ray fluxes, core radii, and spectroscopic redshifts for 73 clusters and photometric redshifts for the remainder.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558#2</TD>
            <TD>2011-09-14T19:12:24Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/502/558&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/502/558</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/502/558 [table3]</TD>
            <TD>Catalog of ROSAT galaxy clusters (Vikhlinin+ 1998)</TD>
            <TD>We present a catalog of 203 clusters of galaxies serendipitously detected in 647 ROSAT PSPC high Galactic latitude pointings covering 158deg^2^. This is one of the largest X-ray-selected cluster samples, comparable in size only to the ROSAT All-Sky Survey sample of nearby clusters (Ebeling et al., 1997ApJ...479L.101E). We detect clusters in the inner 175 of the ROSAT PSPC field of view using the spatial extent of their X-ray emission. Fluxes of detected clusters range from 1.6x10^-14^ to 8x10^-12^ergs/s/cm^2^ in the 0.52keV energy band. X-ray luminosities range from 10^42^ergs/s, corresponding to very poor groups, to ~5x10^44^ergs/s, corresponding to rich clusters. The cluster redshifts range from z=0.015 to z&gt;0.5. The catalog lists X-ray fluxes, core radii, and spectroscopic redshifts for 73 clusters and photometric redshifts for the remainder.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558#table3</TD>
            <TD>2011-09-14T19:12:24Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/502/558</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/502/558&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/502/558</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/413/771 [1]</TD>
            <TD>Galaxies in the Tycho-2 catalogue (Metz+, 2004)</TD>
            <TD>We have identified galaxies in the Tycho-2 Catalogue (Cat. &lt;I/259&gt;) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. &lt;VII/119&gt;) and the Tycho-2 positions of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771#1</TD>
            <TD>2011-09-14T19:26:09Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/413/771</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/413/771</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/413/771 [2]</TD>
            <TD>Galaxies in the Tycho-2 catalogue (Metz+, 2004)</TD>
            <TD>We have identified galaxies in the Tycho-2 Catalogue (Cat. &lt;I/259&gt;) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. &lt;VII/119&gt;) and the Tycho-2 positions of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771#2</TD>
            <TD>2011-09-14T19:26:09Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/413/771&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/413/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/413/771 [table]</TD>
            <TD>Galaxies in the Tycho-2 catalogue (Metz+, 2004)</TD>
            <TD>We have identified galaxies in the Tycho-2 Catalogue (Cat. &lt;I/259&gt;) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. &lt;VII/119&gt;) and the Tycho-2 positions of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771#table</TD>
            <TD>2011-09-14T19:26:09Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/413/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/413/771</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/296/599 [1]</TD>
            <TD>A3558 complex redshifts (Bardelli+, 1998)</TD>
            <TD>The Shapley Concentration is the richest supercluster of clusters in the nearby Universe, and its core is a remarkable complex formed by the ACO clusters A3558, A3562 and A3556, and by the two minor groups SC 1327-312 and SC 1329-314. This structure has been studied in various wavelength bands, revealing that it is probably dynamically very active. In this paper we present 174 new galaxy redshifts in this cluster complex, which are added to the sample of 540 already existing velocities. The spectroscopic observations were performed at the 3.6m ESO telescope at La Silla, equiped with the OPTOPUS multifibre spectrograph, on the nights 1993 February of 21-24.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599#1</TD>
            <TD>2011-09-14T19:12:31Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/296/599</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/599</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/296/599 [2]</TD>
            <TD>A3558 complex redshifts (Bardelli+, 1998)</TD>
            <TD>The Shapley Concentration is the richest supercluster of clusters in the nearby Universe, and its core is a remarkable complex formed by the ACO clusters A3558, A3562 and A3556, and by the two minor groups SC 1327-312 and SC 1329-314. This structure has been studied in various wavelength bands, revealing that it is probably dynamically very active. In this paper we present 174 new galaxy redshifts in this cluster complex, which are added to the sample of 540 already existing velocities. The spectroscopic observations were performed at the 3.6m ESO telescope at La Silla, equiped with the OPTOPUS multifibre spectrograph, on the nights 1993 February of 21-24.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599#2</TD>
            <TD>2011-09-14T19:12:31Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/296/599&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/599</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/296/599 [table2]</TD>
            <TD>A3558 complex redshifts (Bardelli+, 1998)</TD>
            <TD>The Shapley Concentration is the richest supercluster of clusters in the nearby Universe, and its core is a remarkable complex formed by the ACO clusters A3558, A3562 and A3556, and by the two minor groups SC 1327-312 and SC 1329-314. This structure has been studied in various wavelength bands, revealing that it is probably dynamically very active. In this paper we present 174 new galaxy redshifts in this cluster complex, which are added to the sample of 540 already existing velocities. The spectroscopic observations were performed at the 3.6m ESO telescope at La Silla, equiped with the OPTOPUS multifibre spectrograph, on the nights 1993 February of 21-24.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599#table2</TD>
            <TD>2011-09-14T19:12:31Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/296/599&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/599</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/413/771 [1]</TD>
            <TD>Galaxies in the Tycho-2 catalogue (Metz+, 2004)</TD>
            <TD>We have identified galaxies in the Tycho-2 Catalogue (Cat. &lt;I/259&gt;) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. &lt;VII/119&gt;) and the Tycho-2 positions of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771#1</TD>
            <TD>2011-09-14T19:26:09Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/413/771</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/413/771</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/413/771 [2]</TD>
            <TD>Galaxies in the Tycho-2 catalogue (Metz+, 2004)</TD>
            <TD>We have identified galaxies in the Tycho-2 Catalogue (Cat. &lt;I/259&gt;) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. &lt;VII/119&gt;) and the Tycho-2 positions of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771#2</TD>
            <TD>2011-09-14T19:26:09Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/413/771&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/413/771</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/413/771 [table]</TD>
            <TD>Galaxies in the Tycho-2 catalogue (Metz+, 2004)</TD>
            <TD>We have identified galaxies in the Tycho-2 Catalogue (Cat. &lt;I/259&gt;) by a position cross correlation with galaxy catalogues. In the table we give the cross references to the PGC (Cat. &lt;VII/119&gt;) and the Tycho-2 positions of the galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771#table</TD>
            <TD>2011-09-14T19:26:09Z</TD>
            <TD>#Positional_Data#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/413/771</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/413/771&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/413/771</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/296/599 [1]</TD>
            <TD>A3558 complex redshifts (Bardelli+, 1998)</TD>
            <TD>The Shapley Concentration is the richest supercluster of clusters in the nearby Universe, and its core is a remarkable complex formed by the ACO clusters A3558, A3562 and A3556, and by the two minor groups SC 1327-312 and SC 1329-314. This structure has been studied in various wavelength bands, revealing that it is probably dynamically very active. In this paper we present 174 new galaxy redshifts in this cluster complex, which are added to the sample of 540 already existing velocities. The spectroscopic observations were performed at the 3.6m ESO telescope at La Silla, equiped with the OPTOPUS multifibre spectrograph, on the nights 1993 February of 21-24.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599#1</TD>
            <TD>2011-09-14T19:12:31Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/296/599</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/599</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/296/599 [2]</TD>
            <TD>A3558 complex redshifts (Bardelli+, 1998)</TD>
            <TD>The Shapley Concentration is the richest supercluster of clusters in the nearby Universe, and its core is a remarkable complex formed by the ACO clusters A3558, A3562 and A3556, and by the two minor groups SC 1327-312 and SC 1329-314. This structure has been studied in various wavelength bands, revealing that it is probably dynamically very active. In this paper we present 174 new galaxy redshifts in this cluster complex, which are added to the sample of 540 already existing velocities. The spectroscopic observations were performed at the 3.6m ESO telescope at La Silla, equiped with the OPTOPUS multifibre spectrograph, on the nights 1993 February of 21-24.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599#2</TD>
            <TD>2011-09-14T19:12:31Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/296/599&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/599</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/296/599 [table2]</TD>
            <TD>A3558 complex redshifts (Bardelli+, 1998)</TD>
            <TD>The Shapley Concentration is the richest supercluster of clusters in the nearby Universe, and its core is a remarkable complex formed by the ACO clusters A3558, A3562 and A3556, and by the two minor groups SC 1327-312 and SC 1329-314. This structure has been studied in various wavelength bands, revealing that it is probably dynamically very active. In this paper we present 174 new galaxy redshifts in this cluster complex, which are added to the sample of 540 already existing velocities. The spectroscopic observations were performed at the 3.6m ESO telescope at La Silla, equiped with the OPTOPUS multifibre spectrograph, on the nights 1993 February of 21-24.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599#table2</TD>
            <TD>2011-09-14T19:12:31Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/296/599&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/599</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/415/849 [1]</TD>
            <TD>Deprojection of spiral galaxies (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table7a.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849#1</TD>
            <TD>2011-09-14T19:27:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/415/849</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/849</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/415/849 [2]</TD>
            <TD>Deprojection of spiral galaxies (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table7a.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849#2</TD>
            <TD>2011-09-14T19:27:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/415/849&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/849</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/415/849 [table7a]</TD>
            <TD>Deprojection of spiral galaxies (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table7a.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849#table7a</TD>
            <TD>2011-09-14T19:27:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/415/849&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/849</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/296/599 [1]</TD>
            <TD>A3558 complex redshifts (Bardelli+, 1998)</TD>
            <TD>The Shapley Concentration is the richest supercluster of clusters in the nearby Universe, and its core is a remarkable complex formed by the ACO clusters A3558, A3562 and A3556, and by the two minor groups SC 1327-312 and SC 1329-314. This structure has been studied in various wavelength bands, revealing that it is probably dynamically very active. In this paper we present 174 new galaxy redshifts in this cluster complex, which are added to the sample of 540 already existing velocities. The spectroscopic observations were performed at the 3.6m ESO telescope at La Silla, equiped with the OPTOPUS multifibre spectrograph, on the nights 1993 February of 21-24.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599#1</TD>
            <TD>2011-09-14T19:12:31Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/296/599</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/599</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/296/599 [2]</TD>
            <TD>A3558 complex redshifts (Bardelli+, 1998)</TD>
            <TD>The Shapley Concentration is the richest supercluster of clusters in the nearby Universe, and its core is a remarkable complex formed by the ACO clusters A3558, A3562 and A3556, and by the two minor groups SC 1327-312 and SC 1329-314. This structure has been studied in various wavelength bands, revealing that it is probably dynamically very active. In this paper we present 174 new galaxy redshifts in this cluster complex, which are added to the sample of 540 already existing velocities. The spectroscopic observations were performed at the 3.6m ESO telescope at La Silla, equiped with the OPTOPUS multifibre spectrograph, on the nights 1993 February of 21-24.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599#2</TD>
            <TD>2011-09-14T19:12:31Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/296/599&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/599</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/296/599 [table2]</TD>
            <TD>A3558 complex redshifts (Bardelli+, 1998)</TD>
            <TD>The Shapley Concentration is the richest supercluster of clusters in the nearby Universe, and its core is a remarkable complex formed by the ACO clusters A3558, A3562 and A3556, and by the two minor groups SC 1327-312 and SC 1329-314. This structure has been studied in various wavelength bands, revealing that it is probably dynamically very active. In this paper we present 174 new galaxy redshifts in this cluster complex, which are added to the sample of 540 already existing velocities. The spectroscopic observations were performed at the 3.6m ESO telescope at La Silla, equiped with the OPTOPUS multifibre spectrograph, on the nights 1993 February of 21-24.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599#table2</TD>
            <TD>2011-09-14T19:12:31Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Apr-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/296/599</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/296/599&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/296/599</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/415/849 [1]</TD>
            <TD>Deprojection of spiral galaxies (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table7a.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849#1</TD>
            <TD>2011-09-14T19:27:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/415/849</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/849</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/415/849 [2]</TD>
            <TD>Deprojection of spiral galaxies (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table7a.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849#2</TD>
            <TD>2011-09-14T19:27:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/415/849&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/849</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/415/849 [table7a]</TD>
            <TD>Deprojection of spiral galaxies (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table7a.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849#table7a</TD>
            <TD>2011-09-14T19:27:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/415/849&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/849</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/378/30 [1]</TD>
            <TD>ROSAT-BSC galaxy identifications (Zimmermann+, 2001)</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, Cat. &lt;XI/10&gt;) with the Catalogue of Principal Galaxies (PGC, Cat. &lt;VII/119&gt;) 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100". File table1 contains 1124 optical galaxy entries and 904 relevant X-ray candidates/counterparts from the ROSAT All-Sky Survey. Besides a compilation of X-ray and optical parameters for each source, also the results of an identification screening are given. 547 optical/X-ray correlations have been quoted as reliable identifications. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30#1</TD>
            <TD>2011-09-14T19:12:41Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/378/30</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/378/30</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/378/30 [2]</TD>
            <TD>ROSAT-BSC galaxy identifications (Zimmermann+, 2001)</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, Cat. &lt;XI/10&gt;) with the Catalogue of Principal Galaxies (PGC, Cat. &lt;VII/119&gt;) 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100". File table1 contains 1124 optical galaxy entries and 904 relevant X-ray candidates/counterparts from the ROSAT All-Sky Survey. Besides a compilation of X-ray and optical parameters for each source, also the results of an identification screening are given. 547 optical/X-ray correlations have been quoted as reliable identifications. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30#2</TD>
            <TD>2011-09-14T19:12:41Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/378/30&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/378/30</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/378/30 [table1]</TD>
            <TD>ROSAT-BSC galaxy identifications (Zimmermann+, 2001)</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, Cat. &lt;XI/10&gt;) with the Catalogue of Principal Galaxies (PGC, Cat. &lt;VII/119&gt;) 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100". File table1 contains 1124 optical galaxy entries and 904 relevant X-ray candidates/counterparts from the ROSAT All-Sky Survey. Besides a compilation of X-ray and optical parameters for each source, also the results of an identification screening are given. 547 optical/X-ray correlations have been quoted as reliable identifications. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30#table1</TD>
            <TD>2011-09-14T19:12:41Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/378/30&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/378/30</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/415/849 [1]</TD>
            <TD>Deprojection of spiral galaxies (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table7a.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849#1</TD>
            <TD>2011-09-14T19:27:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/415/849</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/849</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/415/849 [2]</TD>
            <TD>Deprojection of spiral galaxies (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table7a.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849#2</TD>
            <TD>2011-09-14T19:27:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/415/849&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/849</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/415/849 [table7a]</TD>
            <TD>Deprojection of spiral galaxies (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table7a.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849#table7a</TD>
            <TD>2011-09-14T19:27:01Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/415/849</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/415/849&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/415/849</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/378/30 [1]</TD>
            <TD>ROSAT-BSC galaxy identifications (Zimmermann+, 2001)</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, Cat. &lt;XI/10&gt;) with the Catalogue of Principal Galaxies (PGC, Cat. &lt;VII/119&gt;) 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100". File table1 contains 1124 optical galaxy entries and 904 relevant X-ray candidates/counterparts from the ROSAT All-Sky Survey. Besides a compilation of X-ray and optical parameters for each source, also the results of an identification screening are given. 547 optical/X-ray correlations have been quoted as reliable identifications. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30#1</TD>
            <TD>2011-09-14T19:12:41Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/378/30</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/378/30</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/378/30 [2]</TD>
            <TD>ROSAT-BSC galaxy identifications (Zimmermann+, 2001)</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, Cat. &lt;XI/10&gt;) with the Catalogue of Principal Galaxies (PGC, Cat. &lt;VII/119&gt;) 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100". File table1 contains 1124 optical galaxy entries and 904 relevant X-ray candidates/counterparts from the ROSAT All-Sky Survey. Besides a compilation of X-ray and optical parameters for each source, also the results of an identification screening are given. 547 optical/X-ray correlations have been quoted as reliable identifications. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30#2</TD>
            <TD>2011-09-14T19:12:41Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/378/30&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/378/30</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/378/30 [table1]</TD>
            <TD>ROSAT-BSC galaxy identifications (Zimmermann+, 2001)</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, Cat. &lt;XI/10&gt;) with the Catalogue of Principal Galaxies (PGC, Cat. &lt;VII/119&gt;) 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100". File table1 contains 1124 optical galaxy entries and 904 relevant X-ray candidates/counterparts from the ROSAT All-Sky Survey. Besides a compilation of X-ray and optical parameters for each source, also the results of an identification screening are given. 547 optical/X-ray correlations have been quoted as reliable identifications. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30#table1</TD>
            <TD>2011-09-14T19:12:41Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/378/30&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/378/30</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/869 [1]</TD>
            <TD>M31-RV evolution (1942-1993) (Boschi+, 2004)</TD>
            <TD>The photometric evolution of M31-RV has been investigated on 1447 plates of the Andromeda galaxy obtained over half a century with the Asiago telescopes. M31-RV is a gigantic stellar explosion that occurred during 1988 in the Bulge of M31 and that was characterized by the appearance for a few months of an M supergiant reaching M_bol_=-10. The 1988 outburst has been positively detected on Asiago plates, and it has been the only such event recorded over the period covered by the plates (1942-1993). In particular, an alleged previous outburst in 1967 is excluded by the more numerous and deeper Asiago plates, with relevant implication for the interpretative models of this unique event.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/869#1</TD>
            <TD>2011-09-14T19:28:22Z</TD>
            <TD>#Novae#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/869</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/869</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/869</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/869 [2]</TD>
            <TD>M31-RV evolution (1942-1993) (Boschi+, 2004)</TD>
            <TD>The photometric evolution of M31-RV has been investigated on 1447 plates of the Andromeda galaxy obtained over half a century with the Asiago telescopes. M31-RV is a gigantic stellar explosion that occurred during 1988 in the Bulge of M31 and that was characterized by the appearance for a few months of an M supergiant reaching M_bol_=-10. The 1988 outburst has been positively detected on Asiago plates, and it has been the only such event recorded over the period covered by the plates (1942-1993). In particular, an alleged previous outburst in 1967 is excluded by the more numerous and deeper Asiago plates, with relevant implication for the interpretative models of this unique event.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/869#2</TD>
            <TD>2011-09-14T19:28:22Z</TD>
            <TD>#Novae#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/869</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/869&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/869</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/378/30 [1]</TD>
            <TD>ROSAT-BSC galaxy identifications (Zimmermann+, 2001)</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, Cat. &lt;XI/10&gt;) with the Catalogue of Principal Galaxies (PGC, Cat. &lt;VII/119&gt;) 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100". File table1 contains 1124 optical galaxy entries and 904 relevant X-ray candidates/counterparts from the ROSAT All-Sky Survey. Besides a compilation of X-ray and optical parameters for each source, also the results of an identification screening are given. 547 optical/X-ray correlations have been quoted as reliable identifications. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30#1</TD>
            <TD>2011-09-14T19:12:41Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/378/30</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/378/30</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/378/30 [2]</TD>
            <TD>ROSAT-BSC galaxy identifications (Zimmermann+, 2001)</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, Cat. &lt;XI/10&gt;) with the Catalogue of Principal Galaxies (PGC, Cat. &lt;VII/119&gt;) 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100". File table1 contains 1124 optical galaxy entries and 904 relevant X-ray candidates/counterparts from the ROSAT All-Sky Survey. Besides a compilation of X-ray and optical parameters for each source, also the results of an identification screening are given. 547 optical/X-ray correlations have been quoted as reliable identifications. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30#2</TD>
            <TD>2011-09-14T19:12:41Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/378/30&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/378/30</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/378/30 [table1]</TD>
            <TD>ROSAT-BSC galaxy identifications (Zimmermann+, 2001)</TD>
            <TD>In a correlation study of the ROSAT All-Sky Survey Bright Source Catalogue (RASS-BSC, Cat. &lt;XI/10&gt;) with the Catalogue of Principal Galaxies (PGC, Cat. &lt;VII/119&gt;) 904 X-ray sources were found that possess possible extragalactic counterparts within a search radius of 100". File table1 contains 1124 optical galaxy entries and 904 relevant X-ray candidates/counterparts from the ROSAT All-Sky Survey. Besides a compilation of X-ray and optical parameters for each source, also the results of an identification screening are given. 547 optical/X-ray correlations have been quoted as reliable identifications. The 904 optical images with X-ray overlay contours (xID_nnn.ps.gz) used in the screening process are added for each user's own judgement.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30#table1</TD>
            <TD>2011-09-14T19:12:41Z</TD>
            <TD>#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Oct-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/378/30</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/378/30&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/378/30</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/869 [1]</TD>
            <TD>M31-RV evolution (1942-1993) (Boschi+, 2004)</TD>
            <TD>The photometric evolution of M31-RV has been investigated on 1447 plates of the Andromeda galaxy obtained over half a century with the Asiago telescopes. M31-RV is a gigantic stellar explosion that occurred during 1988 in the Bulge of M31 and that was characterized by the appearance for a few months of an M supergiant reaching M_bol_=-10. The 1988 outburst has been positively detected on Asiago plates, and it has been the only such event recorded over the period covered by the plates (1942-1993). In particular, an alleged previous outburst in 1967 is excluded by the more numerous and deeper Asiago plates, with relevant implication for the interpretative models of this unique event.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/869#1</TD>
            <TD>2011-09-14T19:28:22Z</TD>
            <TD>#Novae#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/869</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/869</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/869</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/869 [2]</TD>
            <TD>M31-RV evolution (1942-1993) (Boschi+, 2004)</TD>
            <TD>The photometric evolution of M31-RV has been investigated on 1447 plates of the Andromeda galaxy obtained over half a century with the Asiago telescopes. M31-RV is a gigantic stellar explosion that occurred during 1988 in the Bulge of M31 and that was characterized by the appearance for a few months of an M supergiant reaching M_bol_=-10. The 1988 outburst has been positively detected on Asiago plates, and it has been the only such event recorded over the period covered by the plates (1942-1993). In particular, an alleged previous outburst in 1967 is excluded by the more numerous and deeper Asiago plates, with relevant implication for the interpretative models of this unique event.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/869#2</TD>
            <TD>2011-09-14T19:28:22Z</TD>
            <TD>#Novae#Obs_Log#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/869</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/869&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/869</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/554/742 [1]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#1</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/554/742</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/554/742 [2]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#2</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table9]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table9</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table4]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table4</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table8]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table8</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table6]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table6</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table10]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table10</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/885 [1]</TD>
            <TD>The FORS Deep Field Spectroscopic Survey (Noll+, 2004)</TD>
            <TD>We present a catalogue and atlas of low-resolution spectra of a sample of 341 objects with reliable redshifts in the FORS Deep Field (FDF). The sample contains 42 stars, 8 QSOs, and 291 galaxies up to z=5.98 objects are at z&gt;2. For z&gt;1 most objects were selected using photometric redshifts. The limiting I magnitude has been I=24.5 for 2&lt;z&lt;4. All spectra were obtained using the FORS instruments at the ESO VLT and cover the wavelength range 3300-10000{AA}. The grism 150I with a 1" slit width was used, resulting in a spectral resolution element of our spectra of 18-24{AA}, depending on the light distribution in the slit. Most objects were observed several times. Typical exposure times were about 10h for our z&gt;2 objects. The individual spectra were S/N-optimised co-added. The final spectra were flux calibrated, smoothed to the resolution element, and corrected for atmospheric extinction. Moreover, the spectra were corrected for the atmospheric A and B bands. Redshifts and rough object types were derived by cross-correlation of the galaxy spectra with six template spectra, which had been created from high-quality FDF spectroscopic data by an iterative procedure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885#1</TD>
            <TD>2011-09-14T19:28:23Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/885</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/885</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/885 [2]</TD>
            <TD>The FORS Deep Field Spectroscopic Survey (Noll+, 2004)</TD>
            <TD>We present a catalogue and atlas of low-resolution spectra of a sample of 341 objects with reliable redshifts in the FORS Deep Field (FDF). The sample contains 42 stars, 8 QSOs, and 291 galaxies up to z=5.98 objects are at z&gt;2. For z&gt;1 most objects were selected using photometric redshifts. The limiting I magnitude has been I=24.5 for 2&lt;z&lt;4. All spectra were obtained using the FORS instruments at the ESO VLT and cover the wavelength range 3300-10000{AA}. The grism 150I with a 1" slit width was used, resulting in a spectral resolution element of our spectra of 18-24{AA}, depending on the light distribution in the slit. Most objects were observed several times. Typical exposure times were about 10h for our z&gt;2 objects. The individual spectra were S/N-optimised co-added. The final spectra were flux calibrated, smoothed to the resolution element, and corrected for atmospheric extinction. Moreover, the spectra were corrected for the atmospheric A and B bands. Redshifts and rough object types were derived by cross-correlation of the galaxy spectra with six template spectra, which had been created from high-quality FDF spectroscopic data by an iterative procedure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885#2</TD>
            <TD>2011-09-14T19:28:23Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/885&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/885</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/418/885 [table1]</TD>
            <TD>The FORS Deep Field Spectroscopic Survey (Noll+, 2004)</TD>
            <TD>We present a catalogue and atlas of low-resolution spectra of a sample of 341 objects with reliable redshifts in the FORS Deep Field (FDF). The sample contains 42 stars, 8 QSOs, and 291 galaxies up to z=5.98 objects are at z&gt;2. For z&gt;1 most objects were selected using photometric redshifts. The limiting I magnitude has been I=24.5 for 2&lt;z&lt;4. All spectra were obtained using the FORS instruments at the ESO VLT and cover the wavelength range 3300-10000{AA}. The grism 150I with a 1" slit width was used, resulting in a spectral resolution element of our spectra of 18-24{AA}, depending on the light distribution in the slit. Most objects were observed several times. Typical exposure times were about 10h for our z&gt;2 objects. The individual spectra were S/N-optimised co-added. The final spectra were flux calibrated, smoothed to the resolution element, and corrected for atmospheric extinction. Moreover, the spectra were corrected for the atmospheric A and B bands. Redshifts and rough object types were derived by cross-correlation of the galaxy spectra with six template spectra, which had been created from high-quality FDF spectroscopic data by an iterative procedure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885#table1</TD>
            <TD>2011-09-14T19:28:23Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/418/885&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/885</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/554/742 [1]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#1</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/554/742</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/554/742 [2]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#2</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table9]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table9</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table4]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table4</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table8]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table8</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table6]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table6</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table10]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table10</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/885 [1]</TD>
            <TD>The FORS Deep Field Spectroscopic Survey (Noll+, 2004)</TD>
            <TD>We present a catalogue and atlas of low-resolution spectra of a sample of 341 objects with reliable redshifts in the FORS Deep Field (FDF). The sample contains 42 stars, 8 QSOs, and 291 galaxies up to z=5.98 objects are at z&gt;2. For z&gt;1 most objects were selected using photometric redshifts. The limiting I magnitude has been I=24.5 for 2&lt;z&lt;4. All spectra were obtained using the FORS instruments at the ESO VLT and cover the wavelength range 3300-10000{AA}. The grism 150I with a 1" slit width was used, resulting in a spectral resolution element of our spectra of 18-24{AA}, depending on the light distribution in the slit. Most objects were observed several times. Typical exposure times were about 10h for our z&gt;2 objects. The individual spectra were S/N-optimised co-added. The final spectra were flux calibrated, smoothed to the resolution element, and corrected for atmospheric extinction. Moreover, the spectra were corrected for the atmospheric A and B bands. Redshifts and rough object types were derived by cross-correlation of the galaxy spectra with six template spectra, which had been created from high-quality FDF spectroscopic data by an iterative procedure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885#1</TD>
            <TD>2011-09-14T19:28:23Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/885</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/885</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/885 [2]</TD>
            <TD>The FORS Deep Field Spectroscopic Survey (Noll+, 2004)</TD>
            <TD>We present a catalogue and atlas of low-resolution spectra of a sample of 341 objects with reliable redshifts in the FORS Deep Field (FDF). The sample contains 42 stars, 8 QSOs, and 291 galaxies up to z=5.98 objects are at z&gt;2. For z&gt;1 most objects were selected using photometric redshifts. The limiting I magnitude has been I=24.5 for 2&lt;z&lt;4. All spectra were obtained using the FORS instruments at the ESO VLT and cover the wavelength range 3300-10000{AA}. The grism 150I with a 1" slit width was used, resulting in a spectral resolution element of our spectra of 18-24{AA}, depending on the light distribution in the slit. Most objects were observed several times. Typical exposure times were about 10h for our z&gt;2 objects. The individual spectra were S/N-optimised co-added. The final spectra were flux calibrated, smoothed to the resolution element, and corrected for atmospheric extinction. Moreover, the spectra were corrected for the atmospheric A and B bands. Redshifts and rough object types were derived by cross-correlation of the galaxy spectra with six template spectra, which had been created from high-quality FDF spectroscopic data by an iterative procedure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885#2</TD>
            <TD>2011-09-14T19:28:23Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/885&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/885</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/418/885 [table1]</TD>
            <TD>The FORS Deep Field Spectroscopic Survey (Noll+, 2004)</TD>
            <TD>We present a catalogue and atlas of low-resolution spectra of a sample of 341 objects with reliable redshifts in the FORS Deep Field (FDF). The sample contains 42 stars, 8 QSOs, and 291 galaxies up to z=5.98 objects are at z&gt;2. For z&gt;1 most objects were selected using photometric redshifts. The limiting I magnitude has been I=24.5 for 2&lt;z&lt;4. All spectra were obtained using the FORS instruments at the ESO VLT and cover the wavelength range 3300-10000{AA}. The grism 150I with a 1" slit width was used, resulting in a spectral resolution element of our spectra of 18-24{AA}, depending on the light distribution in the slit. Most objects were observed several times. Typical exposure times were about 10h for our z&gt;2 objects. The individual spectra were S/N-optimised co-added. The final spectra were flux calibrated, smoothed to the resolution element, and corrected for atmospheric extinction. Moreover, the spectra were corrected for the atmospheric A and B bands. Redshifts and rough object types were derived by cross-correlation of the galaxy spectra with six template spectra, which had been created from high-quality FDF spectroscopic data by an iterative procedure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885#table1</TD>
            <TD>2011-09-14T19:28:23Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/418/885&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/885</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/554/742 [1]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#1</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/554/742</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/554/742 [2]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#2</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table9]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table9</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table4]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table4</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table8]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table8</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table6]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table6</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/554/742 [table10]</TD>
            <TD>Chandra Deep Survey of the HDF-N (Hornschemeier+, 2001)</TD>
            <TD>A deep X-ray survey of the Hubble Deep Field-North (HDF-N) and its environs is performed using data collected by the Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-Ray Observatory. Currently a 221.9ks exposure is available, the deepest ever presented, and here we give results on X-ray sources located in the 8.6'x8.7' area covered by the Caltech Faint Field Galaxy Redshift Survey (the "Caltech area"). This area has (1) deep photometric coverage in several optical and near-infrared bands; (2) extensive coverage at radio, submillimeter, and mid-infrared wavelengths; and (3) some of the deepest and most complete spectroscopic coverage ever obtained. It is also where the X-ray data have the greatest sensitivity; the minimum detectable fluxes in the 0.5-2keV (soft) and 2-8keV (hard) bands are ~1.3x10^-16^ and ~6.5x10^-16^ergs/cm^2^/s, respectively.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742#table10</TD>
            <TD>2011-09-14T19:12:47Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Sep-2001</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/554/742</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/554/742&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/554/742</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/885 [1]</TD>
            <TD>The FORS Deep Field Spectroscopic Survey (Noll+, 2004)</TD>
            <TD>We present a catalogue and atlas of low-resolution spectra of a sample of 341 objects with reliable redshifts in the FORS Deep Field (FDF). The sample contains 42 stars, 8 QSOs, and 291 galaxies up to z=5.98 objects are at z&gt;2. For z&gt;1 most objects were selected using photometric redshifts. The limiting I magnitude has been I=24.5 for 2&lt;z&lt;4. All spectra were obtained using the FORS instruments at the ESO VLT and cover the wavelength range 3300-10000{AA}. The grism 150I with a 1" slit width was used, resulting in a spectral resolution element of our spectra of 18-24{AA}, depending on the light distribution in the slit. Most objects were observed several times. Typical exposure times were about 10h for our z&gt;2 objects. The individual spectra were S/N-optimised co-added. The final spectra were flux calibrated, smoothed to the resolution element, and corrected for atmospheric extinction. Moreover, the spectra were corrected for the atmospheric A and B bands. Redshifts and rough object types were derived by cross-correlation of the galaxy spectra with six template spectra, which had been created from high-quality FDF spectroscopic data by an iterative procedure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885#1</TD>
            <TD>2011-09-14T19:28:23Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/885</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/885</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/885 [2]</TD>
            <TD>The FORS Deep Field Spectroscopic Survey (Noll+, 2004)</TD>
            <TD>We present a catalogue and atlas of low-resolution spectra of a sample of 341 objects with reliable redshifts in the FORS Deep Field (FDF). The sample contains 42 stars, 8 QSOs, and 291 galaxies up to z=5.98 objects are at z&gt;2. For z&gt;1 most objects were selected using photometric redshifts. The limiting I magnitude has been I=24.5 for 2&lt;z&lt;4. All spectra were obtained using the FORS instruments at the ESO VLT and cover the wavelength range 3300-10000{AA}. The grism 150I with a 1" slit width was used, resulting in a spectral resolution element of our spectra of 18-24{AA}, depending on the light distribution in the slit. Most objects were observed several times. Typical exposure times were about 10h for our z&gt;2 objects. The individual spectra were S/N-optimised co-added. The final spectra were flux calibrated, smoothed to the resolution element, and corrected for atmospheric extinction. Moreover, the spectra were corrected for the atmospheric A and B bands. Redshifts and rough object types were derived by cross-correlation of the galaxy spectra with six template spectra, which had been created from high-quality FDF spectroscopic data by an iterative procedure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885#2</TD>
            <TD>2011-09-14T19:28:23Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/885&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/885</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/418/885 [table1]</TD>
            <TD>The FORS Deep Field Spectroscopic Survey (Noll+, 2004)</TD>
            <TD>We present a catalogue and atlas of low-resolution spectra of a sample of 341 objects with reliable redshifts in the FORS Deep Field (FDF). The sample contains 42 stars, 8 QSOs, and 291 galaxies up to z=5.98 objects are at z&gt;2. For z&gt;1 most objects were selected using photometric redshifts. The limiting I magnitude has been I=24.5 for 2&lt;z&lt;4. All spectra were obtained using the FORS instruments at the ESO VLT and cover the wavelength range 3300-10000{AA}. The grism 150I with a 1" slit width was used, resulting in a spectral resolution element of our spectra of 18-24{AA}, depending on the light distribution in the slit. Most objects were observed several times. Typical exposure times were about 10h for our z&gt;2 objects. The individual spectra were S/N-optimised co-added. The final spectra were flux calibrated, smoothed to the resolution element, and corrected for atmospheric extinction. Moreover, the spectra were corrected for the atmospheric A and B bands. Redshifts and rough object types were derived by cross-correlation of the galaxy spectra with six template spectra, which had been created from high-quality FDF spectroscopic data by an iterative procedure.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885#table1</TD>
            <TD>2011-09-14T19:28:23Z</TD>
            <TD>#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/885</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/418/885&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/885</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/114/2402 [1]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#1</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/114/2402</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/114/2402 [2]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#2</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/114/2402&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/2402 [table7]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#table7</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/2402&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/2402 [table6]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#table6</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/2402&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/419/469 [1]</TD>
            <TD>Abundances in the galaxy HS 0837+4717 (Pustilnik+, 2004)</TD>
            <TD>Spectrophotometric observations of HS 0837+4717 with high S/N ratio were obtained with the MMT on May 1, 1997. HI line observations were carried out in February 1998 with the 300m Nancay radio telescope (NRT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/419/469#1</TD>
            <TD>2011-09-14T19:28:43Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>01-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/419/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/419/469</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/419/469</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/419/469 [2]</TD>
            <TD>Abundances in the galaxy HS 0837+4717 (Pustilnik+, 2004)</TD>
            <TD>Spectrophotometric observations of HS 0837+4717 with high S/N ratio were obtained with the MMT on May 1, 1997. HI line observations were carried out in February 1998 with the 300m Nancay radio telescope (NRT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/419/469#2</TD>
            <TD>2011-09-14T19:28:43Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/419/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/419/469&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/419/469</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/114/2402 [1]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#1</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/114/2402</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/114/2402 [2]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#2</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/114/2402&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/2402 [table7]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#table7</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/2402&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/2402 [table6]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#table6</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/2402&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/419/469 [1]</TD>
            <TD>Abundances in the galaxy HS 0837+4717 (Pustilnik+, 2004)</TD>
            <TD>Spectrophotometric observations of HS 0837+4717 with high S/N ratio were obtained with the MMT on May 1, 1997. HI line observations were carried out in February 1998 with the 300m Nancay radio telescope (NRT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/419/469#1</TD>
            <TD>2011-09-14T19:28:43Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>01-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/419/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/419/469</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/419/469</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/419/469 [2]</TD>
            <TD>Abundances in the galaxy HS 0837+4717 (Pustilnik+, 2004)</TD>
            <TD>Spectrophotometric observations of HS 0837+4717 with high S/N ratio were obtained with the MMT on May 1, 1997. HI line observations were carried out in February 1998 with the 300m Nancay radio telescope (NRT).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/419/469#2</TD>
            <TD>2011-09-14T19:28:43Z</TD>
            <TD>#Abundances#Stars#Equivalent_widths#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/419/469</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/419/469&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/419/469</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/114/2402 [1]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#1</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/114/2402</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/114/2402 [2]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#2</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/114/2402&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/2402 [table7]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#table7</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/2402&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/2402 [table6]</TD>
            <TD>Rotation curves of early-type galaxies (Courteau+, 1997)</TD>
            <TD>Optical long-slit rotation curves have been studied for 304 northern Sb-Sc galaxies from the Courteau-Faber (CF) sample designed for Tully-Fischer (TF) applications; r-band photometry exists also for each galaxy of the sample. The procedure of rotation curve (RC) extraction and construction of optical profiles are analogous to 21cm integrated linewidths. More than 20% of the galaxies were observed twice or more, allowing for a proper determination of systematic errors. Various measures of maximum rotational velocity to be used as input in the TF relation are tested on the basis of their repeatability, minimization of TF scatter, and match with 21cm linewidths. The best measure of TF velocity, V2.2 is given at the location of peak rotational velocity of a pure exponential disk. An alternative measure to V2.2 which makes no assumption about the luminosity profile or shape of the rotation curve is Vhist, the 20% width of the velocity histogram, though the match with 21cm linewidths is not good. The paper shows that optical TF calibrations yield internal scatter comparable to, if not smaller than, the best calibrations based on single-dish 21cm radio linewidths. Tables 6 and 7 contain the values of the parameters fitting the rotation curves of two samples of galaxies: the CF (Courteau-Faber) sample (table6) and the MAT (Mathewson et al., 1992ApJS...81..413M) sample (table7). Two fitting models were used: the ArcTan function (Model 1) where the velocity varies as v(r) = v(0) + K . arctan(R)(R being (r-r_0_)/r_t_) and a multi-parameter function (Model 2) modelling the rotation curve close to a solid-body close to the rotation center, and close to a flat rotation at large distances (see section 5 of the paper).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402#table6</TD>
            <TD>2011-09-14T19:12:56Z</TD>
            <TD>#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-1999</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/2402</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/2402&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/2402</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/141 [1]</TD>
            <TD>Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</TD>
            <TD>This catalog contains 56 spectra: 55 galaxy spectra, and one night sky spectrum, which is included for users wishing to check for low-level spurious features in the galaxy spectra. The file "spectra.dat" contains a summary of the spectra. The user should consult the paper for details of the observations and a discussion of the limitations of the spectrophotometry. The spectra are integrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength of 555nm. An atmospheric extinction correction has been applied to the data, but otherwise they are not corrected for reddening, redshift, etc. The spectral range covered is 365-710 nm and the resolution is 5-8{AA}. Each spectrum consists in 1726 normalized flux values spaced each 2{AA}, stored as a file in the subdirectory "sp". Tests show that the spectrophotometry is accurate to the few percent level over small wavelength regions, and at the 10% level over the entire wavelength range. Although the data are useful for a variety of applications, the user should be forewarned that they may not be suitable for applications requiring precision colors over a long wavelength baseline (e.g., computation of K-corrections, some spectral synthesis applications).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/141#1</TD>
            <TD>2011-09-14T19:29:50Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/VII/141</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/141</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/141</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/141 [2]</TD>
            <TD>Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</TD>
            <TD>This catalog contains 56 spectra: 55 galaxy spectra, and one night sky spectrum, which is included for users wishing to check for low-level spurious features in the galaxy spectra. The file "spectra.dat" contains a summary of the spectra. The user should consult the paper for details of the observations and a discussion of the limitations of the spectrophotometry. The spectra are integrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength of 555nm. An atmospheric extinction correction has been applied to the data, but otherwise they are not corrected for reddening, redshift, etc. The spectral range covered is 365-710 nm and the resolution is 5-8{AA}. Each spectrum consists in 1726 normalized flux values spaced each 2{AA}, stored as a file in the subdirectory "sp". Tests show that the spectrophotometry is accurate to the few percent level over small wavelength regions, and at the 10% level over the entire wavelength range. Although the data are useful for a variety of applications, the user should be forewarned that they may not be suitable for applications requiring precision colors over a long wavelength baseline (e.g., computation of K-corrections, some spectral synthesis applications).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/141#2</TD>
            <TD>2011-09-14T19:29:50Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/VII/141</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/141&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/141</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/141 [spectra]</TD>
            <TD>Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</TD>
            <TD>This catalog contains 56 spectra: 55 galaxy spectra, and one night sky spectrum, which is included for users wishing to check for low-level spurious features in the galaxy spectra. The file "spectra.dat" contains a summary of the spectra. The user should consult the paper for details of the observations and a discussion of the limitations of the spectrophotometry. The spectra are integrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength of 555nm. An atmospheric extinction correction has been applied to the data, but otherwise they are not corrected for reddening, redshift, etc. The spectral range covered is 365-710 nm and the resolution is 5-8{AA}. Each spectrum consists in 1726 normalized flux values spaced each 2{AA}, stored as a file in the subdirectory "sp". Tests show that the spectrophotometry is accurate to the few percent level over small wavelength regions, and at the 10% level over the entire wavelength range. Although the data are useful for a variety of applications, the user should be forewarned that they may not be suitable for applications requiring precision colors over a long wavelength baseline (e.g., computation of K-corrections, some spectral synthesis applications).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/141#spectra</TD>
            <TD>2011-09-14T19:29:50Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/VII/141</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/141&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/141</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/488 [1]</TD>
            <TD>Stellar and ionized gas kinematics in NGC 2855 (Corsini+, 2002)</TD>
            <TD>We present major and minor-axis kinematics of stars and ionized gas as well as narrow and broad-band surface photometry of the Sa spiral NGC 2855. In the nuclear regions of this unbarred and apparently undisturbed spiral galaxy the gas is rotating perpendicularly to the galaxy disk. We suggest that this kinematically-decoupled component is the signature of an acquisition process in the history of this galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/488#1</TD>
            <TD>2011-09-14T19:13:09Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/488</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/488</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/488</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/488 [2]</TD>
            <TD>Stellar and ionized gas kinematics in NGC 2855 (Corsini+, 2002)</TD>
            <TD>We present major and minor-axis kinematics of stars and ionized gas as well as narrow and broad-band surface photometry of the Sa spiral NGC 2855. In the nuclear regions of this unbarred and apparently undisturbed spiral galaxy the gas is rotating perpendicularly to the galaxy disk. We suggest that this kinematically-decoupled component is the signature of an acquisition process in the history of this galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/488#2</TD>
            <TD>2011-09-14T19:13:09Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/488</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/488&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/488</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/141 [1]</TD>
            <TD>Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</TD>
            <TD>This catalog contains 56 spectra: 55 galaxy spectra, and one night sky spectrum, which is included for users wishing to check for low-level spurious features in the galaxy spectra. The file "spectra.dat" contains a summary of the spectra. The user should consult the paper for details of the observations and a discussion of the limitations of the spectrophotometry. The spectra are integrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength of 555nm. An atmospheric extinction correction has been applied to the data, but otherwise they are not corrected for reddening, redshift, etc. The spectral range covered is 365-710 nm and the resolution is 5-8{AA}. Each spectrum consists in 1726 normalized flux values spaced each 2{AA}, stored as a file in the subdirectory "sp". Tests show that the spectrophotometry is accurate to the few percent level over small wavelength regions, and at the 10% level over the entire wavelength range. Although the data are useful for a variety of applications, the user should be forewarned that they may not be suitable for applications requiring precision colors over a long wavelength baseline (e.g., computation of K-corrections, some spectral synthesis applications).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/141#1</TD>
            <TD>2011-09-14T19:29:50Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/VII/141</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/141</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/141</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/141 [2]</TD>
            <TD>Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</TD>
            <TD>This catalog contains 56 spectra: 55 galaxy spectra, and one night sky spectrum, which is included for users wishing to check for low-level spurious features in the galaxy spectra. The file "spectra.dat" contains a summary of the spectra. The user should consult the paper for details of the observations and a discussion of the limitations of the spectrophotometry. The spectra are integrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength of 555nm. An atmospheric extinction correction has been applied to the data, but otherwise they are not corrected for reddening, redshift, etc. The spectral range covered is 365-710 nm and the resolution is 5-8{AA}. Each spectrum consists in 1726 normalized flux values spaced each 2{AA}, stored as a file in the subdirectory "sp". Tests show that the spectrophotometry is accurate to the few percent level over small wavelength regions, and at the 10% level over the entire wavelength range. Although the data are useful for a variety of applications, the user should be forewarned that they may not be suitable for applications requiring precision colors over a long wavelength baseline (e.g., computation of K-corrections, some spectral synthesis applications).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/141#2</TD>
            <TD>2011-09-14T19:29:50Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/VII/141</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/141&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/141</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/141 [spectra]</TD>
            <TD>Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</TD>
            <TD>This catalog contains 56 spectra: 55 galaxy spectra, and one night sky spectrum, which is included for users wishing to check for low-level spurious features in the galaxy spectra. The file "spectra.dat" contains a summary of the spectra. The user should consult the paper for details of the observations and a discussion of the limitations of the spectrophotometry. The spectra are integrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength of 555nm. An atmospheric extinction correction has been applied to the data, but otherwise they are not corrected for reddening, redshift, etc. The spectral range covered is 365-710 nm and the resolution is 5-8{AA}. Each spectrum consists in 1726 normalized flux values spaced each 2{AA}, stored as a file in the subdirectory "sp". Tests show that the spectrophotometry is accurate to the few percent level over small wavelength regions, and at the 10% level over the entire wavelength range. Although the data are useful for a variety of applications, the user should be forewarned that they may not be suitable for applications requiring precision colors over a long wavelength baseline (e.g., computation of K-corrections, some spectral synthesis applications).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/141#spectra</TD>
            <TD>2011-09-14T19:29:50Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/VII/141</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/141&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/141</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/382/488 [1]</TD>
            <TD>Stellar and ionized gas kinematics in NGC 2855 (Corsini+, 2002)</TD>
            <TD>We present major and minor-axis kinematics of stars and ionized gas as well as narrow and broad-band surface photometry of the Sa spiral NGC 2855. In the nuclear regions of this unbarred and apparently undisturbed spiral galaxy the gas is rotating perpendicularly to the galaxy disk. We suggest that this kinematically-decoupled component is the signature of an acquisition process in the history of this galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/488#1</TD>
            <TD>2011-09-14T19:13:09Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/488</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/382/488</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/488</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/382/488 [2]</TD>
            <TD>Stellar and ionized gas kinematics in NGC 2855 (Corsini+, 2002)</TD>
            <TD>We present major and minor-axis kinematics of stars and ionized gas as well as narrow and broad-band surface photometry of the Sa spiral NGC 2855. In the nuclear regions of this unbarred and apparently undisturbed spiral galaxy the gas is rotating perpendicularly to the galaxy disk. We suggest that this kinematically-decoupled component is the signature of an acquisition process in the history of this galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/488#2</TD>
            <TD>2011-09-14T19:13:09Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/382/488</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/382/488&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/382/488</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/141 [1]</TD>
            <TD>Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</TD>
            <TD>This catalog contains 56 spectra: 55 galaxy spectra, and one night sky spectrum, which is included for users wishing to check for low-level spurious features in the galaxy spectra. The file "spectra.dat" contains a summary of the spectra. The user should consult the paper for details of the observations and a discussion of the limitations of the spectrophotometry. The spectra are integrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength of 555nm. An atmospheric extinction correction has been applied to the data, but otherwise they are not corrected for reddening, redshift, etc. The spectral range covered is 365-710 nm and the resolution is 5-8{AA}. Each spectrum consists in 1726 normalized flux values spaced each 2{AA}, stored as a file in the subdirectory "sp". Tests show that the spectrophotometry is accurate to the few percent level over small wavelength regions, and at the 10% level over the entire wavelength range. Although the data are useful for a variety of applications, the user should be forewarned that they may not be suitable for applications requiring precision colors over a long wavelength baseline (e.g., computation of K-corrections, some spectral synthesis applications).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/141#1</TD>
            <TD>2011-09-14T19:29:50Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/VII/141</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/141</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/141</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/141 [2]</TD>
            <TD>Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</TD>
            <TD>This catalog contains 56 spectra: 55 galaxy spectra, and one night sky spectrum, which is included for users wishing to check for low-level spurious features in the galaxy spectra. The file "spectra.dat" contains a summary of the spectra. The user should consult the paper for details of the observations and a discussion of the limitations of the spectrophotometry. The spectra are integrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength of 555nm. An atmospheric extinction correction has been applied to the data, but otherwise they are not corrected for reddening, redshift, etc. The spectral range covered is 365-710 nm and the resolution is 5-8{AA}. Each spectrum consists in 1726 normalized flux values spaced each 2{AA}, stored as a file in the subdirectory "sp". Tests show that the spectrophotometry is accurate to the few percent level over small wavelength regions, and at the 10% level over the entire wavelength range. Although the data are useful for a variety of applications, the user should be forewarned that they may not be suitable for applications requiring precision colors over a long wavelength baseline (e.g., computation of K-corrections, some spectral synthesis applications).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/141#2</TD>
            <TD>2011-09-14T19:29:50Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/VII/141</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/141&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/141</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/141 [spectra]</TD>
            <TD>Spectrophotometric Atlas of Galaxies (Kennicutt Jr. 1992)</TD>
            <TD>This catalog contains 56 spectra: 55 galaxy spectra, and one night sky spectrum, which is included for users wishing to check for low-level spurious features in the galaxy spectra. The file "spectra.dat" contains a summary of the spectra. The user should consult the paper for details of the observations and a discussion of the limitations of the spectrophotometry. The spectra are integrated measurements made with apertures comparable to the diameters of the galaxies. The original spectra have been combined, rebinned to a common wavelength scale, and normalized in flux to unity at a reference wavelength of 555nm. An atmospheric extinction correction has been applied to the data, but otherwise they are not corrected for reddening, redshift, etc. The spectral range covered is 365-710 nm and the resolution is 5-8{AA}. Each spectrum consists in 1726 normalized flux values spaced each 2{AA}, stored as a file in the subdirectory "sp". Tests show that the spectrophotometry is accurate to the few percent level over small wavelength regions, and at the 10% level over the entire wavelength range. Although the data are useful for a variety of applications, the user should be forewarned that they may not be suitable for applications requiring precision colors over a long wavelength baseline (e.g., computation of K-corrections, some spectral synthesis applications).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/141#spectra</TD>
            <TD>2011-09-14T19:29:50Z</TD>
            <TD>#Galaxies#Galaxies:spectra#Spectrophotometry#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Aug-2004</TD>
            <TD>ivo://CDS.VizieR/VII/141</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/141&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/141</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/422/511 [1]</TD>
            <TD>Oxygen abundance in M101 HII regions (Cedres+, 2004)</TD>
            <TD>We present the oxygen abundance determination for 90 HII regions in the inner parts of the grand design galaxy M101. The abundances were derived employing the P method (Pilyugin, 2001A&amp;A...369..594P). A comparison is made with previous determinations using another calibration and direct measurements of electron temperature to derive the oxygen abundance. The results show agreement with the abundances derived from the electron temperature method and also show that the older calibration is not as accurate as the P method.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/511#1</TD>
            <TD>2011-09-14T19:30:09Z</TD>
            <TD>#Abundances#Photometry:narrow-band#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/422/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/422/511 [2]</TD>
            <TD>Oxygen abundance in M101 HII regions (Cedres+, 2004)</TD>
            <TD>We present the oxygen abundance determination for 90 HII regions in the inner parts of the grand design galaxy M101. The abundances were derived employing the P method (Pilyugin, 2001A&amp;A...369..594P). A comparison is made with previous determinations using another calibration and direct measurements of electron temperature to derive the oxygen abundance. The results show agreement with the abundances derived from the electron temperature method and also show that the older calibration is not as accurate as the P method.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/511#2</TD>
            <TD>2011-09-14T19:30:09Z</TD>
            <TD>#Abundances#Photometry:narrow-band#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/422/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/1330 [1]</TD>
            <TD>HST BVI photometry of M 81 star clusters (Chandar+, 2001)</TD>
            <TD>In this paper, we present the discovery of 114 compact star clusters in the nearby spiral galaxy M81 from B-, V-, and I-band Hubble Space Telescope Wide Field Planetary Camera 2 imaging in eight fields, covering a total area of ~40arcmin^2^. The fields sample a variety of environments (both spiral and interarm regions), as well as a range of projected galactocentric distances from 2 to 12kpc. The sample is complete to V~22, deeper by ~1mag than any previous cluster survey in M81. We present details of the separation of clusters from both stellar sources and background galaxies, which has been based solely on structural parameters and morphology and not using any color cuts, as is necessary for ground-based surveys. We present magnitudes and colors of detected clusters. Surface brightness profiles are compared with single-mass King models, giving a range of core radii for the clusters in our sample between 0.2 and 7pc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330#1</TD>
            <TD>2011-09-14T19:13:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/1330</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1330</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/1330 [2]</TD>
            <TD>HST BVI photometry of M 81 star clusters (Chandar+, 2001)</TD>
            <TD>In this paper, we present the discovery of 114 compact star clusters in the nearby spiral galaxy M81 from B-, V-, and I-band Hubble Space Telescope Wide Field Planetary Camera 2 imaging in eight fields, covering a total area of ~40arcmin^2^. The fields sample a variety of environments (both spiral and interarm regions), as well as a range of projected galactocentric distances from 2 to 12kpc. The sample is complete to V~22, deeper by ~1mag than any previous cluster survey in M81. We present details of the separation of clusters from both stellar sources and background galaxies, which has been based solely on structural parameters and morphology and not using any color cuts, as is necessary for ground-based surveys. We present magnitudes and colors of detected clusters. Surface brightness profiles are compared with single-mass King models, giving a range of core radii for the clusters in our sample between 0.2 and 7pc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330#2</TD>
            <TD>2011-09-14T19:13:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/1330&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1330</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1330 [table2]</TD>
            <TD>HST BVI photometry of M 81 star clusters (Chandar+, 2001)</TD>
            <TD>In this paper, we present the discovery of 114 compact star clusters in the nearby spiral galaxy M81 from B-, V-, and I-band Hubble Space Telescope Wide Field Planetary Camera 2 imaging in eight fields, covering a total area of ~40arcmin^2^. The fields sample a variety of environments (both spiral and interarm regions), as well as a range of projected galactocentric distances from 2 to 12kpc. The sample is complete to V~22, deeper by ~1mag than any previous cluster survey in M81. We present details of the separation of clusters from both stellar sources and background galaxies, which has been based solely on structural parameters and morphology and not using any color cuts, as is necessary for ground-based surveys. We present magnitudes and colors of detected clusters. Surface brightness profiles are compared with single-mass King models, giving a range of core radii for the clusters in our sample between 0.2 and 7pc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330#table2</TD>
            <TD>2011-09-14T19:13:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1330&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1330</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/422/511 [1]</TD>
            <TD>Oxygen abundance in M101 HII regions (Cedres+, 2004)</TD>
            <TD>We present the oxygen abundance determination for 90 HII regions in the inner parts of the grand design galaxy M101. The abundances were derived employing the P method (Pilyugin, 2001A&amp;A...369..594P). A comparison is made with previous determinations using another calibration and direct measurements of electron temperature to derive the oxygen abundance. The results show agreement with the abundances derived from the electron temperature method and also show that the older calibration is not as accurate as the P method.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/511#1</TD>
            <TD>2011-09-14T19:30:09Z</TD>
            <TD>#Abundances#Photometry:narrow-band#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/422/511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/422/511 [2]</TD>
            <TD>Oxygen abundance in M101 HII regions (Cedres+, 2004)</TD>
            <TD>We present the oxygen abundance determination for 90 HII regions in the inner parts of the grand design galaxy M101. The abundances were derived employing the P method (Pilyugin, 2001A&amp;A...369..594P). A comparison is made with previous determinations using another calibration and direct measurements of electron temperature to derive the oxygen abundance. The results show agreement with the abundances derived from the electron temperature method and also show that the older calibration is not as accurate as the P method.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/511#2</TD>
            <TD>2011-09-14T19:30:09Z</TD>
            <TD>#Abundances#Photometry:narrow-band#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/422/511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/1330 [1]</TD>
            <TD>HST BVI photometry of M 81 star clusters (Chandar+, 2001)</TD>
            <TD>In this paper, we present the discovery of 114 compact star clusters in the nearby spiral galaxy M81 from B-, V-, and I-band Hubble Space Telescope Wide Field Planetary Camera 2 imaging in eight fields, covering a total area of ~40arcmin^2^. The fields sample a variety of environments (both spiral and interarm regions), as well as a range of projected galactocentric distances from 2 to 12kpc. The sample is complete to V~22, deeper by ~1mag than any previous cluster survey in M81. We present details of the separation of clusters from both stellar sources and background galaxies, which has been based solely on structural parameters and morphology and not using any color cuts, as is necessary for ground-based surveys. We present magnitudes and colors of detected clusters. Surface brightness profiles are compared with single-mass King models, giving a range of core radii for the clusters in our sample between 0.2 and 7pc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330#1</TD>
            <TD>2011-09-14T19:13:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/1330</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1330</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/1330 [2]</TD>
            <TD>HST BVI photometry of M 81 star clusters (Chandar+, 2001)</TD>
            <TD>In this paper, we present the discovery of 114 compact star clusters in the nearby spiral galaxy M81 from B-, V-, and I-band Hubble Space Telescope Wide Field Planetary Camera 2 imaging in eight fields, covering a total area of ~40arcmin^2^. The fields sample a variety of environments (both spiral and interarm regions), as well as a range of projected galactocentric distances from 2 to 12kpc. The sample is complete to V~22, deeper by ~1mag than any previous cluster survey in M81. We present details of the separation of clusters from both stellar sources and background galaxies, which has been based solely on structural parameters and morphology and not using any color cuts, as is necessary for ground-based surveys. We present magnitudes and colors of detected clusters. Surface brightness profiles are compared with single-mass King models, giving a range of core radii for the clusters in our sample between 0.2 and 7pc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330#2</TD>
            <TD>2011-09-14T19:13:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/1330&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1330</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1330 [table2]</TD>
            <TD>HST BVI photometry of M 81 star clusters (Chandar+, 2001)</TD>
            <TD>In this paper, we present the discovery of 114 compact star clusters in the nearby spiral galaxy M81 from B-, V-, and I-band Hubble Space Telescope Wide Field Planetary Camera 2 imaging in eight fields, covering a total area of ~40arcmin^2^. The fields sample a variety of environments (both spiral and interarm regions), as well as a range of projected galactocentric distances from 2 to 12kpc. The sample is complete to V~22, deeper by ~1mag than any previous cluster survey in M81. We present details of the separation of clusters from both stellar sources and background galaxies, which has been based solely on structural parameters and morphology and not using any color cuts, as is necessary for ground-based surveys. We present magnitudes and colors of detected clusters. Surface brightness profiles are compared with single-mass King models, giving a range of core radii for the clusters in our sample between 0.2 and 7pc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330#table2</TD>
            <TD>2011-09-14T19:13:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1330&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1330</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/348/857 [1]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#1</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/348/857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/348/857 [2]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#2</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/348/857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/857 [table2]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#table2</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/857 [table1]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#table1</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/122/1330 [1]</TD>
            <TD>HST BVI photometry of M 81 star clusters (Chandar+, 2001)</TD>
            <TD>In this paper, we present the discovery of 114 compact star clusters in the nearby spiral galaxy M81 from B-, V-, and I-band Hubble Space Telescope Wide Field Planetary Camera 2 imaging in eight fields, covering a total area of ~40arcmin^2^. The fields sample a variety of environments (both spiral and interarm regions), as well as a range of projected galactocentric distances from 2 to 12kpc. The sample is complete to V~22, deeper by ~1mag than any previous cluster survey in M81. We present details of the separation of clusters from both stellar sources and background galaxies, which has been based solely on structural parameters and morphology and not using any color cuts, as is necessary for ground-based surveys. We present magnitudes and colors of detected clusters. Surface brightness profiles are compared with single-mass King models, giving a range of core radii for the clusters in our sample between 0.2 and 7pc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330#1</TD>
            <TD>2011-09-14T19:13:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/122/1330</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1330</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/122/1330 [2]</TD>
            <TD>HST BVI photometry of M 81 star clusters (Chandar+, 2001)</TD>
            <TD>In this paper, we present the discovery of 114 compact star clusters in the nearby spiral galaxy M81 from B-, V-, and I-band Hubble Space Telescope Wide Field Planetary Camera 2 imaging in eight fields, covering a total area of ~40arcmin^2^. The fields sample a variety of environments (both spiral and interarm regions), as well as a range of projected galactocentric distances from 2 to 12kpc. The sample is complete to V~22, deeper by ~1mag than any previous cluster survey in M81. We present details of the separation of clusters from both stellar sources and background galaxies, which has been based solely on structural parameters and morphology and not using any color cuts, as is necessary for ground-based surveys. We present magnitudes and colors of detected clusters. Surface brightness profiles are compared with single-mass King models, giving a range of core radii for the clusters in our sample between 0.2 and 7pc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330#2</TD>
            <TD>2011-09-14T19:13:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/122/1330&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1330</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/122/1330 [table2]</TD>
            <TD>HST BVI photometry of M 81 star clusters (Chandar+, 2001)</TD>
            <TD>In this paper, we present the discovery of 114 compact star clusters in the nearby spiral galaxy M81 from B-, V-, and I-band Hubble Space Telescope Wide Field Planetary Camera 2 imaging in eight fields, covering a total area of ~40arcmin^2^. The fields sample a variety of environments (both spiral and interarm regions), as well as a range of projected galactocentric distances from 2 to 12kpc. The sample is complete to V~22, deeper by ~1mag than any previous cluster survey in M81. We present details of the separation of clusters from both stellar sources and background galaxies, which has been based solely on structural parameters and morphology and not using any color cuts, as is necessary for ground-based surveys. We present magnitudes and colors of detected clusters. Surface brightness profiles are compared with single-mass King models, giving a range of core radii for the clusters in our sample between 0.2 and 7pc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330#table2</TD>
            <TD>2011-09-14T19:13:20Z</TD>
            <TD>#Associations#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/122/1330</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/122/1330&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/122/1330</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/348/857 [1]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#1</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/348/857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/348/857 [2]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#2</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/348/857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/857 [table2]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#table2</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/857 [table1]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#table1</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/727 [1]</TD>
            <TD>M31 globular clusters photometry (Barmby+, 2000)</TD>
            <TD>We present a new catalog of photometric and spectroscopic data on M31 globular clusters (GCs). The catalog includes new optical and near-infrared photometry for a substantial fraction of the 435 clusters and cluster candidates. We use these data to determine the reddening and intrinsic colors of individual clusters, and we find that the extinction laws in the Galaxy and M31 are not significantly different. There are significant (up to 0.2 mag in V-K) offsets between the clusters' intrinsic colors and simple stellar population colors predicted by population synthesis models; we suggest that these are due to systematic errors in the models. The distributions of M31 clusters' metallicities and metallicity-sensitive colors are bimodal, with peaks at [Fe/H]~-1.4 and -0.6. The distribution of V-I is often bimodal in elliptical galaxies' globular cluster systems, but it is not sensitive enough to metallicity to show bimodality in M31 and Galactic cluster systems. The radial distribution and kinematics of the two M31 metallicity groups imply that they are analogs of the Galactic "halo" and "disk/bulge" cluster systems. The globular clusters in M31 have a small radial metallicity gradient, suggesting that some dissipation occurred during the formation of the globular cluster system. The lack of correlation between cluster luminosity and metallicity in M31 GCs shows that self-enrichment is not important in GC formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/727#1</TD>
            <TD>2011-09-14T19:14:17Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/727</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/727</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/727 [2]</TD>
            <TD>M31 globular clusters photometry (Barmby+, 2000)</TD>
            <TD>We present a new catalog of photometric and spectroscopic data on M31 globular clusters (GCs). The catalog includes new optical and near-infrared photometry for a substantial fraction of the 435 clusters and cluster candidates. We use these data to determine the reddening and intrinsic colors of individual clusters, and we find that the extinction laws in the Galaxy and M31 are not significantly different. There are significant (up to 0.2 mag in V-K) offsets between the clusters' intrinsic colors and simple stellar population colors predicted by population synthesis models; we suggest that these are due to systematic errors in the models. The distributions of M31 clusters' metallicities and metallicity-sensitive colors are bimodal, with peaks at [Fe/H]~-1.4 and -0.6. The distribution of V-I is often bimodal in elliptical galaxies' globular cluster systems, but it is not sensitive enough to metallicity to show bimodality in M31 and Galactic cluster systems. The radial distribution and kinematics of the two M31 metallicity groups imply that they are analogs of the Galactic "halo" and "disk/bulge" cluster systems. The globular clusters in M31 have a small radial metallicity gradient, suggesting that some dissipation occurred during the formation of the globular cluster system. The lack of correlation between cluster luminosity and metallicity in M31 GCs shows that self-enrichment is not important in GC formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/727#2</TD>
            <TD>2011-09-14T19:14:17Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/727&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/727</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/348/857 [1]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#1</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/348/857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/348/857 [2]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#2</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/348/857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/857 [table2]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#table2</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/348/857 [table1]</TD>
            <TD>Radio-loud QSOs at z~4 (Holt+, 2004)</TD>
            <TD>Observations of 54 of the 194 candidates were reported in Paper I, Benn et al., 2002MNRAS.329..221B. The 55th object reported there, 1349+38, is actually detected on the Minnesota APS scan of the POSS-I blue plate (i.e. it is not red), and thus does not meet selection criterion (red also in the Minnesota APS (Pennington et al. catalogue of the POSS-I plates, 1993PASP..105..521P). Spectra were obtained of 60 more candidates using the IDS spectrograph on the Isaac Newton Telescope during near-photometric nights (occasional light cirrus) in 2001 May. Some of the 194 candidates were imaged through a Harris R filter with the 1.0-m Jacobus Kapteyn Telescope (JKT) in service time, in order to identify extended objects. Spectra were later obtained of most of these candidates at the Isaac Newton Telescope (INT), but the 'G' (galaxy) classifications of four objects in Table 2 are based on JKT imaging alone. The 13 z&gt;3.6 QSOs with S_1.4GHz_&gt;3mJy were observed at 4.85 and 10GHz, with the Effelsberg radio telescope, during the night of 2002 January 13.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857#table1</TD>
            <TD>2011-09-14T19:30:56Z</TD>
            <TD>#Photometry#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Mar-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/348/857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/348/857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/348/857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/119/727 [1]</TD>
            <TD>M31 globular clusters photometry (Barmby+, 2000)</TD>
            <TD>We present a new catalog of photometric and spectroscopic data on M31 globular clusters (GCs). The catalog includes new optical and near-infrared photometry for a substantial fraction of the 435 clusters and cluster candidates. We use these data to determine the reddening and intrinsic colors of individual clusters, and we find that the extinction laws in the Galaxy and M31 are not significantly different. There are significant (up to 0.2 mag in V-K) offsets between the clusters' intrinsic colors and simple stellar population colors predicted by population synthesis models; we suggest that these are due to systematic errors in the models. The distributions of M31 clusters' metallicities and metallicity-sensitive colors are bimodal, with peaks at [Fe/H]~-1.4 and -0.6. The distribution of V-I is often bimodal in elliptical galaxies' globular cluster systems, but it is not sensitive enough to metallicity to show bimodality in M31 and Galactic cluster systems. The radial distribution and kinematics of the two M31 metallicity groups imply that they are analogs of the Galactic "halo" and "disk/bulge" cluster systems. The globular clusters in M31 have a small radial metallicity gradient, suggesting that some dissipation occurred during the formation of the globular cluster system. The lack of correlation between cluster luminosity and metallicity in M31 GCs shows that self-enrichment is not important in GC formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/727#1</TD>
            <TD>2011-09-14T19:14:17Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/119/727</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/727</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/119/727 [2]</TD>
            <TD>M31 globular clusters photometry (Barmby+, 2000)</TD>
            <TD>We present a new catalog of photometric and spectroscopic data on M31 globular clusters (GCs). The catalog includes new optical and near-infrared photometry for a substantial fraction of the 435 clusters and cluster candidates. We use these data to determine the reddening and intrinsic colors of individual clusters, and we find that the extinction laws in the Galaxy and M31 are not significantly different. There are significant (up to 0.2 mag in V-K) offsets between the clusters' intrinsic colors and simple stellar population colors predicted by population synthesis models; we suggest that these are due to systematic errors in the models. The distributions of M31 clusters' metallicities and metallicity-sensitive colors are bimodal, with peaks at [Fe/H]~-1.4 and -0.6. The distribution of V-I is often bimodal in elliptical galaxies' globular cluster systems, but it is not sensitive enough to metallicity to show bimodality in M31 and Galactic cluster systems. The radial distribution and kinematics of the two M31 metallicity groups imply that they are analogs of the Galactic "halo" and "disk/bulge" cluster systems. The globular clusters in M31 have a small radial metallicity gradient, suggesting that some dissipation occurred during the formation of the globular cluster system. The lack of correlation between cluster luminosity and metallicity in M31 GCs shows that self-enrichment is not important in GC formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/727#2</TD>
            <TD>2011-09-14T19:14:17Z</TD>
            <TD>#Abundances#Globular_Clusters#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Mar-2000</TD>
            <TD>ivo://CDS.VizieR/J/AJ/119/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/119/727&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/119/727</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/383/631 [1]</TD>
            <TD>Catalogue of dust clouds in the Galaxy (Dutra+, 2002)</TD>
            <TD>The file cdn.dat is an unified dust cloud catalogue of the Galaxy. Considering an initial list of approximately 6500 entries we condensed them into a cross-identified all-sky catalogue containing 5004 dust clouds.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631#1</TD>
            <TD>2011-09-14T19:14:22Z</TD>
            <TD>#Nebulae#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/383/631</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/383/631</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/383/631 [2]</TD>
            <TD>Catalogue of dust clouds in the Galaxy (Dutra+, 2002)</TD>
            <TD>The file cdn.dat is an unified dust cloud catalogue of the Galaxy. Considering an initial list of approximately 6500 entries we condensed them into a cross-identified all-sky catalogue containing 5004 dust clouds.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631#2</TD>
            <TD>2011-09-14T19:14:22Z</TD>
            <TD>#Nebulae#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/383/631&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/383/631</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/383/631 [cdn]</TD>
            <TD>Catalogue of dust clouds in the Galaxy (Dutra+, 2002)</TD>
            <TD>The file cdn.dat is an unified dust cloud catalogue of the Galaxy. Considering an initial list of approximately 6500 entries we condensed them into a cross-identified all-sky catalogue containing 5004 dust clouds.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631#cdn</TD>
            <TD>2011-09-14T19:14:22Z</TD>
            <TD>#Nebulae#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/383/631&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/383/631</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/383/631 [1]</TD>
            <TD>Catalogue of dust clouds in the Galaxy (Dutra+, 2002)</TD>
            <TD>The file cdn.dat is an unified dust cloud catalogue of the Galaxy. Considering an initial list of approximately 6500 entries we condensed them into a cross-identified all-sky catalogue containing 5004 dust clouds.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631#1</TD>
            <TD>2011-09-14T19:14:22Z</TD>
            <TD>#Nebulae#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/383/631</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/383/631</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/383/631 [2]</TD>
            <TD>Catalogue of dust clouds in the Galaxy (Dutra+, 2002)</TD>
            <TD>The file cdn.dat is an unified dust cloud catalogue of the Galaxy. Considering an initial list of approximately 6500 entries we condensed them into a cross-identified all-sky catalogue containing 5004 dust clouds.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631#2</TD>
            <TD>2011-09-14T19:14:22Z</TD>
            <TD>#Nebulae#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/383/631&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/383/631</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/383/631 [cdn]</TD>
            <TD>Catalogue of dust clouds in the Galaxy (Dutra+, 2002)</TD>
            <TD>The file cdn.dat is an unified dust cloud catalogue of the Galaxy. Considering an initial list of approximately 6500 entries we condensed them into a cross-identified all-sky catalogue containing 5004 dust clouds.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631#cdn</TD>
            <TD>2011-09-14T19:14:22Z</TD>
            <TD>#Nebulae#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/383/631&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/383/631</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/383/631 [1]</TD>
            <TD>Catalogue of dust clouds in the Galaxy (Dutra+, 2002)</TD>
            <TD>The file cdn.dat is an unified dust cloud catalogue of the Galaxy. Considering an initial list of approximately 6500 entries we condensed them into a cross-identified all-sky catalogue containing 5004 dust clouds.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631#1</TD>
            <TD>2011-09-14T19:14:22Z</TD>
            <TD>#Nebulae#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/383/631</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/383/631</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/383/631 [2]</TD>
            <TD>Catalogue of dust clouds in the Galaxy (Dutra+, 2002)</TD>
            <TD>The file cdn.dat is an unified dust cloud catalogue of the Galaxy. Considering an initial list of approximately 6500 entries we condensed them into a cross-identified all-sky catalogue containing 5004 dust clouds.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631#2</TD>
            <TD>2011-09-14T19:14:22Z</TD>
            <TD>#Nebulae#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/383/631&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/383/631</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/383/631 [cdn]</TD>
            <TD>Catalogue of dust clouds in the Galaxy (Dutra+, 2002)</TD>
            <TD>The file cdn.dat is an unified dust cloud catalogue of the Galaxy. Considering an initial list of approximately 6500 entries we condensed them into a cross-identified all-sky catalogue containing 5004 dust clouds.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631#cdn</TD>
            <TD>2011-09-14T19:14:22Z</TD>
            <TD>#Nebulae#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/383/631</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/383/631&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/383/631</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/387/26 [1]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#1</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/387/26</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/387/26 [2]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#2</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/387/26&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/387/26 [table7]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#table7</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/387/26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/387/26 [table6]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#table6</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/387/26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/387/26 [1]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#1</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/387/26</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/387/26 [2]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#2</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/387/26&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/387/26 [table7]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#table7</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/387/26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/387/26 [table6]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#table6</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/387/26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/387/26 [1]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#1</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/387/26</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/387/26 [2]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#2</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/387/26&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/387/26 [table7]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#table7</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/387/26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/387/26 [table6]</TD>
            <TD>Surface photometry in 7 nearby clusters (Fasano+, 2002)</TD>
            <TD>This is the first paper of a series investigating the scaling relations of early-type galaxies in clusters. Here we illustrate the multi-band imagery and the image reduction and calibration procedures relative to the whole sample of 22 clusters at 0.05&lt;~z&lt;~0.25. We also present detailed surface photometry of 312 early-type galaxies in 7 clusters (A1069, A119, A1983, A2151, A2670, A3125 and DC2103) in the first redshift bin, z=0.025-0.075. We give for each galaxy the complete set of luminosity and geometrical profiles, and a number of global, photometric and morphological parameters. They have been evaluated taking into account the effects of seeing. Internal consistency checks and comparisons with data in the literature confirm the quality of our analysis. These data, together with the spectroscopic ones presented in the second paper of the series, will provide the local calibration of the scaling relations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26#table6</TD>
            <TD>2011-09-14T19:15:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/26</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/387/26&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/26</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/387/1 [1]</TD>
            <TD>DENIS galaxies behind the Milky Way (Vauglin+, 2002)</TD>
            <TD>A search has been undertaken at Lyon Observatory to identify, by eye, galaxy candidates at galactic latitudes lower than +/-15 degrees on the DENIS J and K-band images. This paper presents a list of 2028 objects that were serendipitously detected throughout the DENIS survey. Cross-identification with galaxy entries in the LEDA Database has been performed. Comparison with the second release of the 2MASS survey led to a satisfactory agreement of J band magnitudes (std. dev.=0.3mag). The distribution of galaxy candidates along the Galactic Plane shows a concentration near the galactic longitude l=305deg. As a by product of this inspection of J and K images some interesting galactic objects were found (star clusters and nebulae).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1#1</TD>
            <TD>2011-09-14T19:16:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/387/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/387/1 [2]</TD>
            <TD>DENIS galaxies behind the Milky Way (Vauglin+, 2002)</TD>
            <TD>A search has been undertaken at Lyon Observatory to identify, by eye, galaxy candidates at galactic latitudes lower than +/-15 degrees on the DENIS J and K-band images. This paper presents a list of 2028 objects that were serendipitously detected throughout the DENIS survey. Cross-identification with galaxy entries in the LEDA Database has been performed. Comparison with the second release of the 2MASS survey led to a satisfactory agreement of J band magnitudes (std. dev.=0.3mag). The distribution of galaxy candidates along the Galactic Plane shows a concentration near the galactic longitude l=305deg. As a by product of this inspection of J and K images some interesting galactic objects were found (star clusters and nebulae).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1#2</TD>
            <TD>2011-09-14T19:16:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/387/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/387/1 [catalog]</TD>
            <TD>DENIS galaxies behind the Milky Way (Vauglin+, 2002)</TD>
            <TD>A search has been undertaken at Lyon Observatory to identify, by eye, galaxy candidates at galactic latitudes lower than +/-15 degrees on the DENIS J and K-band images. This paper presents a list of 2028 objects that were serendipitously detected throughout the DENIS survey. Cross-identification with galaxy entries in the LEDA Database has been performed. Comparison with the second release of the 2MASS survey led to a satisfactory agreement of J band magnitudes (std. dev.=0.3mag). The distribution of galaxy candidates along the Galactic Plane shows a concentration near the galactic longitude l=305deg. As a by product of this inspection of J and K images some interesting galactic objects were found (star clusters and nebulae).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1#catalog</TD>
            <TD>2011-09-14T19:16:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/387/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/387/1 [1]</TD>
            <TD>DENIS galaxies behind the Milky Way (Vauglin+, 2002)</TD>
            <TD>A search has been undertaken at Lyon Observatory to identify, by eye, galaxy candidates at galactic latitudes lower than +/-15 degrees on the DENIS J and K-band images. This paper presents a list of 2028 objects that were serendipitously detected throughout the DENIS survey. Cross-identification with galaxy entries in the LEDA Database has been performed. Comparison with the second release of the 2MASS survey led to a satisfactory agreement of J band magnitudes (std. dev.=0.3mag). The distribution of galaxy candidates along the Galactic Plane shows a concentration near the galactic longitude l=305deg. As a by product of this inspection of J and K images some interesting galactic objects were found (star clusters and nebulae).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1#1</TD>
            <TD>2011-09-14T19:16:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/387/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/387/1 [2]</TD>
            <TD>DENIS galaxies behind the Milky Way (Vauglin+, 2002)</TD>
            <TD>A search has been undertaken at Lyon Observatory to identify, by eye, galaxy candidates at galactic latitudes lower than +/-15 degrees on the DENIS J and K-band images. This paper presents a list of 2028 objects that were serendipitously detected throughout the DENIS survey. Cross-identification with galaxy entries in the LEDA Database has been performed. Comparison with the second release of the 2MASS survey led to a satisfactory agreement of J band magnitudes (std. dev.=0.3mag). The distribution of galaxy candidates along the Galactic Plane shows a concentration near the galactic longitude l=305deg. As a by product of this inspection of J and K images some interesting galactic objects were found (star clusters and nebulae).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1#2</TD>
            <TD>2011-09-14T19:16:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/387/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/387/1 [catalog]</TD>
            <TD>DENIS galaxies behind the Milky Way (Vauglin+, 2002)</TD>
            <TD>A search has been undertaken at Lyon Observatory to identify, by eye, galaxy candidates at galactic latitudes lower than +/-15 degrees on the DENIS J and K-band images. This paper presents a list of 2028 objects that were serendipitously detected throughout the DENIS survey. Cross-identification with galaxy entries in the LEDA Database has been performed. Comparison with the second release of the 2MASS survey led to a satisfactory agreement of J band magnitudes (std. dev.=0.3mag). The distribution of galaxy candidates along the Galactic Plane shows a concentration near the galactic longitude l=305deg. As a by product of this inspection of J and K images some interesting galactic objects were found (star clusters and nebulae).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1#catalog</TD>
            <TD>2011-09-14T19:16:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/387/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/6 [1]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#1</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/6 [2]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#2</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/6 [table1]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#table1</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/6 [table9]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#table9</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/387/1 [1]</TD>
            <TD>DENIS galaxies behind the Milky Way (Vauglin+, 2002)</TD>
            <TD>A search has been undertaken at Lyon Observatory to identify, by eye, galaxy candidates at galactic latitudes lower than +/-15 degrees on the DENIS J and K-band images. This paper presents a list of 2028 objects that were serendipitously detected throughout the DENIS survey. Cross-identification with galaxy entries in the LEDA Database has been performed. Comparison with the second release of the 2MASS survey led to a satisfactory agreement of J band magnitudes (std. dev.=0.3mag). The distribution of galaxy candidates along the Galactic Plane shows a concentration near the galactic longitude l=305deg. As a by product of this inspection of J and K images some interesting galactic objects were found (star clusters and nebulae).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1#1</TD>
            <TD>2011-09-14T19:16:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/387/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/387/1 [2]</TD>
            <TD>DENIS galaxies behind the Milky Way (Vauglin+, 2002)</TD>
            <TD>A search has been undertaken at Lyon Observatory to identify, by eye, galaxy candidates at galactic latitudes lower than +/-15 degrees on the DENIS J and K-band images. This paper presents a list of 2028 objects that were serendipitously detected throughout the DENIS survey. Cross-identification with galaxy entries in the LEDA Database has been performed. Comparison with the second release of the 2MASS survey led to a satisfactory agreement of J band magnitudes (std. dev.=0.3mag). The distribution of galaxy candidates along the Galactic Plane shows a concentration near the galactic longitude l=305deg. As a by product of this inspection of J and K images some interesting galactic objects were found (star clusters and nebulae).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1#2</TD>
            <TD>2011-09-14T19:16:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/387/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/1</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/387/1 [catalog]</TD>
            <TD>DENIS galaxies behind the Milky Way (Vauglin+, 2002)</TD>
            <TD>A search has been undertaken at Lyon Observatory to identify, by eye, galaxy candidates at galactic latitudes lower than +/-15 degrees on the DENIS J and K-band images. This paper presents a list of 2028 objects that were serendipitously detected throughout the DENIS survey. Cross-identification with galaxy entries in the LEDA Database has been performed. Comparison with the second release of the 2MASS survey led to a satisfactory agreement of J band magnitudes (std. dev.=0.3mag). The distribution of galaxy candidates along the Galactic Plane shows a concentration near the galactic longitude l=305deg. As a by product of this inspection of J and K images some interesting galactic objects were found (star clusters and nebulae).</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1#catalog</TD>
            <TD>2011-09-14T19:16:37Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/387/1</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/387/1&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/387/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/782 [1]</TD>
            <TD>Bar galaxies and their environments (van den Bergh+, 2002)</TD>
            <TD>The prints of the Palomar Sky Survey, luminosity classifications, and radial velocities were used to assign all northern Shapley-Ames galaxies to either (1) field, (2) group, or (3) cluster environments. This information for 930 galaxies shows no evidence for a dependence of bar frequency on galaxy environment. This suggests that the formation of a bar in a disk galaxy is mainly determined by the properties of the parent galaxy, rather than by the characteristics of its environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/782#1</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/782</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/782</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/782</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/782 [2]</TD>
            <TD>Bar galaxies and their environments (van den Bergh+, 2002)</TD>
            <TD>The prints of the Palomar Sky Survey, luminosity classifications, and radial velocities were used to assign all northern Shapley-Ames galaxies to either (1) field, (2) group, or (3) cluster environments. This information for 930 galaxies shows no evidence for a dependence of bar frequency on galaxy environment. This suggests that the formation of a bar in a disk galaxy is mainly determined by the properties of the parent galaxy, rather than by the characteristics of its environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/782#2</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/782</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/782&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/782</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/329/877 [1]</TD>
            <TD>The CLASS blazar survey. II. (Caccianiga+, 2002)</TD>
            <TD>This paper presents the optical properties of the objects selected in the CLASS blazar survey. Because an optical spectrum is now available for 70 per cent of the 325 sources present in the sample, a spectral classification, based on the appearance of the emission/absorption lines, is possible. A wide variety of optical spectral types is found. Besides `classical' BL Lacs (42), BL Lac candidates (5) and high-power (P_5GHz_&gt;10^26^W/Hz) flat spectrum radio quasars (67), a significant number of `passive' elliptical galaxies (41) is also found. Moreover, 33 broad emission line objects with a low radio power (P(5GHz)&gt;10^26^W/Hz) are discovered, suggesting that at least a fraction (~24-30 per cent) of low-power blazars have a broad line region. Finally, 34 objects showing only narrow emission lines, either as a result of some starburst activity in the host galaxy or as a result of the presence of an active galactic nucleus, appear in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877#1</TD>
            <TD>2011-09-14T19:30:58Z</TD>
            <TD>#BL_Lac_objects#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/329/877</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/877</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/329/877 [2]</TD>
            <TD>The CLASS blazar survey. II. (Caccianiga+, 2002)</TD>
            <TD>This paper presents the optical properties of the objects selected in the CLASS blazar survey. Because an optical spectrum is now available for 70 per cent of the 325 sources present in the sample, a spectral classification, based on the appearance of the emission/absorption lines, is possible. A wide variety of optical spectral types is found. Besides `classical' BL Lacs (42), BL Lac candidates (5) and high-power (P_5GHz_&gt;10^26^W/Hz) flat spectrum radio quasars (67), a significant number of `passive' elliptical galaxies (41) is also found. Moreover, 33 broad emission line objects with a low radio power (P(5GHz)&gt;10^26^W/Hz) are discovered, suggesting that at least a fraction (~24-30 per cent) of low-power blazars have a broad line region. Finally, 34 objects showing only narrow emission lines, either as a result of some starburst activity in the host galaxy or as a result of the presence of an active galactic nucleus, appear in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877#2</TD>
            <TD>2011-09-14T19:30:58Z</TD>
            <TD>#BL_Lac_objects#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/329/877&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/877</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/329/877 [table2]</TD>
            <TD>The CLASS blazar survey. II. (Caccianiga+, 2002)</TD>
            <TD>This paper presents the optical properties of the objects selected in the CLASS blazar survey. Because an optical spectrum is now available for 70 per cent of the 325 sources present in the sample, a spectral classification, based on the appearance of the emission/absorption lines, is possible. A wide variety of optical spectral types is found. Besides `classical' BL Lacs (42), BL Lac candidates (5) and high-power (P_5GHz_&gt;10^26^W/Hz) flat spectrum radio quasars (67), a significant number of `passive' elliptical galaxies (41) is also found. Moreover, 33 broad emission line objects with a low radio power (P(5GHz)&gt;10^26^W/Hz) are discovered, suggesting that at least a fraction (~24-30 per cent) of low-power blazars have a broad line region. Finally, 34 objects showing only narrow emission lines, either as a result of some starburst activity in the host galaxy or as a result of the presence of an active galactic nucleus, appear in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877#table2</TD>
            <TD>2011-09-14T19:30:58Z</TD>
            <TD>#BL_Lac_objects#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/329/877&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/877</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/329/877 [1]</TD>
            <TD>The CLASS blazar survey. II. (Caccianiga+, 2002)</TD>
            <TD>This paper presents the optical properties of the objects selected in the CLASS blazar survey. Because an optical spectrum is now available for 70 per cent of the 325 sources present in the sample, a spectral classification, based on the appearance of the emission/absorption lines, is possible. A wide variety of optical spectral types is found. Besides `classical' BL Lacs (42), BL Lac candidates (5) and high-power (P_5GHz_&gt;10^26^W/Hz) flat spectrum radio quasars (67), a significant number of `passive' elliptical galaxies (41) is also found. Moreover, 33 broad emission line objects with a low radio power (P(5GHz)&gt;10^26^W/Hz) are discovered, suggesting that at least a fraction (~24-30 per cent) of low-power blazars have a broad line region. Finally, 34 objects showing only narrow emission lines, either as a result of some starburst activity in the host galaxy or as a result of the presence of an active galactic nucleus, appear in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877#1</TD>
            <TD>2011-09-14T19:30:58Z</TD>
            <TD>#BL_Lac_objects#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/329/877</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/877</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/329/877 [2]</TD>
            <TD>The CLASS blazar survey. II. (Caccianiga+, 2002)</TD>
            <TD>This paper presents the optical properties of the objects selected in the CLASS blazar survey. Because an optical spectrum is now available for 70 per cent of the 325 sources present in the sample, a spectral classification, based on the appearance of the emission/absorption lines, is possible. A wide variety of optical spectral types is found. Besides `classical' BL Lacs (42), BL Lac candidates (5) and high-power (P_5GHz_&gt;10^26^W/Hz) flat spectrum radio quasars (67), a significant number of `passive' elliptical galaxies (41) is also found. Moreover, 33 broad emission line objects with a low radio power (P(5GHz)&gt;10^26^W/Hz) are discovered, suggesting that at least a fraction (~24-30 per cent) of low-power blazars have a broad line region. Finally, 34 objects showing only narrow emission lines, either as a result of some starburst activity in the host galaxy or as a result of the presence of an active galactic nucleus, appear in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877#2</TD>
            <TD>2011-09-14T19:30:58Z</TD>
            <TD>#BL_Lac_objects#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/329/877&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/877</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/329/877 [table2]</TD>
            <TD>The CLASS blazar survey. II. (Caccianiga+, 2002)</TD>
            <TD>This paper presents the optical properties of the objects selected in the CLASS blazar survey. Because an optical spectrum is now available for 70 per cent of the 325 sources present in the sample, a spectral classification, based on the appearance of the emission/absorption lines, is possible. A wide variety of optical spectral types is found. Besides `classical' BL Lacs (42), BL Lac candidates (5) and high-power (P_5GHz_&gt;10^26^W/Hz) flat spectrum radio quasars (67), a significant number of `passive' elliptical galaxies (41) is also found. Moreover, 33 broad emission line objects with a low radio power (P(5GHz)&gt;10^26^W/Hz) are discovered, suggesting that at least a fraction (~24-30 per cent) of low-power blazars have a broad line region. Finally, 34 objects showing only narrow emission lines, either as a result of some starburst activity in the host galaxy or as a result of the presence of an active galactic nucleus, appear in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877#table2</TD>
            <TD>2011-09-14T19:30:58Z</TD>
            <TD>#BL_Lac_objects#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/329/877&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/877</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/782 [1]</TD>
            <TD>Bar galaxies and their environments (van den Bergh+, 2002)</TD>
            <TD>The prints of the Palomar Sky Survey, luminosity classifications, and radial velocities were used to assign all northern Shapley-Ames galaxies to either (1) field, (2) group, or (3) cluster environments. This information for 930 galaxies shows no evidence for a dependence of bar frequency on galaxy environment. This suggests that the formation of a bar in a disk galaxy is mainly determined by the properties of the parent galaxy, rather than by the characteristics of its environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/782#1</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/782</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/782</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/782</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/782 [2]</TD>
            <TD>Bar galaxies and their environments (van den Bergh+, 2002)</TD>
            <TD>The prints of the Palomar Sky Survey, luminosity classifications, and radial velocities were used to assign all northern Shapley-Ames galaxies to either (1) field, (2) group, or (3) cluster environments. This information for 930 galaxies shows no evidence for a dependence of bar frequency on galaxy environment. This suggests that the formation of a bar in a disk galaxy is mainly determined by the properties of the parent galaxy, rather than by the characteristics of its environment.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/782#2</TD>
            <TD>2011-09-14T19:17:17Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Sep-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/782</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/782&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/782</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/6 [1]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#1</TD>
            <TD>2011-09-14T18:42:38Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/6 [2]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#2</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/6&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/6 [table1]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#table1</TD>
            <TD>2011-09-14T18:42:38Z</TD>
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            <TD>#Research#</TD>
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            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/6 [table9]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#table9</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/392/795 [1]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#1</TD>
            <TD>2011-09-14T19:17:38Z</TD>
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            <TD>#Catalog#</TD>
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            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/392/795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/392/795 [2]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#2</TD>
            <TD>2011-09-14T19:17:38Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/392/795&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table11]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table11</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table4]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table4</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table12]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table12</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table3]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table3</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/6 [1]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#1</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/6 [2]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#2</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/6 [table1]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#table1</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/115/6 [table9]</TD>
            <TD>Hercules supercluster kinematics (Barmby+ 1998)</TD>
            <TD>The Hercules supercluster consists of the Abell clusters A2147, A2151, and A2152. Previous studies of the kinematics have been confounded by the difficulty of correctly assigning galaxies to the individual clusters, which are not well separated. Our study has a total of 468 available velocities for galaxies in the region, 175 of them new. There are 414 galaxies in the supercluster, about 3 times the number used in the previous supercluster study. We verify the existence of the three individual clusters and compute their individual dynamical parameters. We investigate several techniques for assigning galaxy membership to clusters in this crowded field. We use the Kaye's mixture model (Ashman, Bird, &amp; Zepf, 1994AJ....108.2348A) algorithm to separate the galaxies into clusters; we find that A2152 has a higher mean velocity than previous studies have reported. A2147 and A2152 also have lower velocity dispersions: 821^+68^_-55_ and 715^+81^_-61_km/s, respectively. The assignment of galaxies to either A2152 or A2147 requires velocity and position information. We study the kinematics of the supercluster using the two-body formalism of Beers, Geller, &amp; Huchra (1982ApJ...257...23B) and conclude that A2147 and A2151 are probably bound to each other and that the supercluster as a whole may also be bound. The mass of the supercluster, if bound, is (7.6+/-2.0)x10^15^h^-1^M_{sun}_; with the supercluster luminosity, (1.4+/-0.2)x10^13^h^-2^L_{sun}_, this yields {OMEGA}=0.34+/-0.1.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6#table9</TD>
            <TD>2011-09-14T18:42:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/115/6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/329/877 [1]</TD>
            <TD>The CLASS blazar survey. II. (Caccianiga+, 2002)</TD>
            <TD>This paper presents the optical properties of the objects selected in the CLASS blazar survey. Because an optical spectrum is now available for 70 per cent of the 325 sources present in the sample, a spectral classification, based on the appearance of the emission/absorption lines, is possible. A wide variety of optical spectral types is found. Besides `classical' BL Lacs (42), BL Lac candidates (5) and high-power (P_5GHz_&gt;10^26^W/Hz) flat spectrum radio quasars (67), a significant number of `passive' elliptical galaxies (41) is also found. Moreover, 33 broad emission line objects with a low radio power (P(5GHz)&gt;10^26^W/Hz) are discovered, suggesting that at least a fraction (~24-30 per cent) of low-power blazars have a broad line region. Finally, 34 objects showing only narrow emission lines, either as a result of some starburst activity in the host galaxy or as a result of the presence of an active galactic nucleus, appear in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877#1</TD>
            <TD>2011-09-14T19:30:58Z</TD>
            <TD>#BL_Lac_objects#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/329/877</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/877</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/329/877 [2]</TD>
            <TD>The CLASS blazar survey. II. (Caccianiga+, 2002)</TD>
            <TD>This paper presents the optical properties of the objects selected in the CLASS blazar survey. Because an optical spectrum is now available for 70 per cent of the 325 sources present in the sample, a spectral classification, based on the appearance of the emission/absorption lines, is possible. A wide variety of optical spectral types is found. Besides `classical' BL Lacs (42), BL Lac candidates (5) and high-power (P_5GHz_&gt;10^26^W/Hz) flat spectrum radio quasars (67), a significant number of `passive' elliptical galaxies (41) is also found. Moreover, 33 broad emission line objects with a low radio power (P(5GHz)&gt;10^26^W/Hz) are discovered, suggesting that at least a fraction (~24-30 per cent) of low-power blazars have a broad line region. Finally, 34 objects showing only narrow emission lines, either as a result of some starburst activity in the host galaxy or as a result of the presence of an active galactic nucleus, appear in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877#2</TD>
            <TD>2011-09-14T19:30:58Z</TD>
            <TD>#BL_Lac_objects#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/329/877&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/877</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/329/877 [table2]</TD>
            <TD>The CLASS blazar survey. II. (Caccianiga+, 2002)</TD>
            <TD>This paper presents the optical properties of the objects selected in the CLASS blazar survey. Because an optical spectrum is now available for 70 per cent of the 325 sources present in the sample, a spectral classification, based on the appearance of the emission/absorption lines, is possible. A wide variety of optical spectral types is found. Besides `classical' BL Lacs (42), BL Lac candidates (5) and high-power (P_5GHz_&gt;10^26^W/Hz) flat spectrum radio quasars (67), a significant number of `passive' elliptical galaxies (41) is also found. Moreover, 33 broad emission line objects with a low radio power (P(5GHz)&gt;10^26^W/Hz) are discovered, suggesting that at least a fraction (~24-30 per cent) of low-power blazars have a broad line region. Finally, 34 objects showing only narrow emission lines, either as a result of some starburst activity in the host galaxy or as a result of the presence of an active galactic nucleus, appear in the sample.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877#table2</TD>
            <TD>2011-09-14T19:30:58Z</TD>
            <TD>#BL_Lac_objects#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Mar-2002</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/329/877</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/329/877&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/329/877</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/392/795 [1]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#1</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/392/795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/392/795 [2]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#2</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/392/795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table11]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table11</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table4]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table4</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table12]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table12</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table3]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table3</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/150/1 [1]</TD>
            <TD>VV29 and NGC 4676 HST photometry (Benitez+, 2004)</TD>
            <TD>We present the analysis of the faint galaxy population in the Advanced Camera for Surveys (ACS) Early Release Observation fields VV 29 (UGC 10214) and NGC 4676. These observations cover a total area of 26.3arcmin^2^ and have depths close to that of the Hubble Deep Fields in the deepest part of the VV 29 image, with 10{sigma} detection limits for point sources of 27.8, 27.6, and 27.2 AB magnitudes in the g_F475W_, V_F606W_, and I_F814W_ bands, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1#1</TD>
            <TD>2011-09-14T19:32:02Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/150/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/150/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/150/1 [2]</TD>
            <TD>VV29 and NGC 4676 HST photometry (Benitez+, 2004)</TD>
            <TD>We present the analysis of the faint galaxy population in the Advanced Camera for Surveys (ACS) Early Release Observation fields VV 29 (UGC 10214) and NGC 4676. These observations cover a total area of 26.3arcmin^2^ and have depths close to that of the Hubble Deep Fields in the deepest part of the VV 29 image, with 10{sigma} detection limits for point sources of 27.8, 27.6, and 27.2 AB magnitudes in the g_F475W_, V_F606W_, and I_F814W_ bands, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1#2</TD>
            <TD>2011-09-14T19:32:02Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/150/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/150/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/392/795 [1]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#1</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/392/795</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/392/795 [2]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#2</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/392/795&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table11]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table11</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table4]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table4</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table12]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table12</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/392/795 [table3]</TD>
            <TD>Multi-wavelength study of 2 galaxy clusters (Valtchanov+, 2002)</TD>
            <TD>We present results from optical, X-ray and radio observations of two X-ray bright (L_X_~10^45^erg/s) galaxy clusters. Abell 1451 is at redshift z=0.1989 and has line-of-sight velocity dispersion {sigma}_V_=1330km/s as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6-251521 (for short RXJ1314-25) has z=0.2474 and {sigma}_V_=1100km/s from 37 galaxies. There are two distinct galaxy groups with a projected separation of ~700kpc. The velocity histogram is bi-modal with a redshift-space separation of ~1700km/s, and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795#table3</TD>
            <TD>2011-09-14T19:17:38Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/392/795</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/392/795&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/392/795</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/380/441 [1]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#1</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/380/441</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/380/441 [2]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#2</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/380/441&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/380/441 [table3]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#table3</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/380/441&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/380/441 [table1]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#table1</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/380/441&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/99 [1]</TD>
            <TD>Radial Velocities of Galaxies (Palumbo+ 1986)</TD>
            <TD>This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/99#1</TD>
            <TD>2011-09-14T18:42:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/99</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/99</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/99 [2]</TD>
            <TD>Radial Velocities of Galaxies (Palumbo+ 1986)</TD>
            <TD>This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/99#2</TD>
            <TD>2011-09-14T18:42:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/99&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/99 [catalog]</TD>
            <TD>Radial Velocities of Galaxies (Palumbo+ 1986)</TD>
            <TD>This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/99#catalog</TD>
            <TD>2011-09-14T18:42:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/99</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/99 [1]</TD>
            <TD>Radial Velocities of Galaxies (Palumbo+ 1986)</TD>
            <TD>This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/99#1</TD>
            <TD>2011-09-14T18:42:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/99</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/99</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/99 [2]</TD>
            <TD>Radial Velocities of Galaxies (Palumbo+ 1986)</TD>
            <TD>This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/99#2</TD>
            <TD>2011-09-14T18:42:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/99&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/99 [catalog]</TD>
            <TD>Radial Velocities of Galaxies (Palumbo+ 1986)</TD>
            <TD>This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/99#catalog</TD>
            <TD>2011-09-14T18:42:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/99</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/150/1 [1]</TD>
            <TD>VV29 and NGC 4676 HST photometry (Benitez+, 2004)</TD>
            <TD>We present the analysis of the faint galaxy population in the Advanced Camera for Surveys (ACS) Early Release Observation fields VV 29 (UGC 10214) and NGC 4676. These observations cover a total area of 26.3arcmin^2^ and have depths close to that of the Hubble Deep Fields in the deepest part of the VV 29 image, with 10{sigma} detection limits for point sources of 27.8, 27.6, and 27.2 AB magnitudes in the g_F475W_, V_F606W_, and I_F814W_ bands, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1#1</TD>
            <TD>2011-09-14T19:32:02Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/150/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/150/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/150/1 [2]</TD>
            <TD>VV29 and NGC 4676 HST photometry (Benitez+, 2004)</TD>
            <TD>We present the analysis of the faint galaxy population in the Advanced Camera for Surveys (ACS) Early Release Observation fields VV 29 (UGC 10214) and NGC 4676. These observations cover a total area of 26.3arcmin^2^ and have depths close to that of the Hubble Deep Fields in the deepest part of the VV 29 image, with 10{sigma} detection limits for point sources of 27.8, 27.6, and 27.2 AB magnitudes in the g_F475W_, V_F606W_, and I_F814W_ bands, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1#2</TD>
            <TD>2011-09-14T19:32:02Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/150/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/150/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/99 [1]</TD>
            <TD>Radial Velocities of Galaxies (Palumbo+ 1986)</TD>
            <TD>This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/99#1</TD>
            <TD>2011-09-14T18:42:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/99</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/99</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/99 [2]</TD>
            <TD>Radial Velocities of Galaxies (Palumbo+ 1986)</TD>
            <TD>This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/99#2</TD>
            <TD>2011-09-14T18:42:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/99</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/99&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/99</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/99 [catalog]</TD>
            <TD>Radial Velocities of Galaxies (Palumbo+ 1986)</TD>
            <TD>This catalog lists coordinates, names, and radial velocities for 8250 galaxies scattered over the whole sky. Both optical and radio measures are included. The individual values are given as published, with a reference to each, but no unpublished data are included. An attempt was made to obtain the most accurate coordinates for each object rather than relying on the source papers. In addition to the positions and heliocentric velocities, the catalog contains a name of the galaxy, whether the observation is made by radio or optically, the mean error of the velocity, a correction for the galactic motion of the Sun, and comments. This electronic version is a slightly improved version compared to the published one, and contains more names. References and notes are not included, and the user must refer to the printed version to get them.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/99#catalog</TD>
            <TD>2011-09-14T18:42:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-1996</TD>
            <TD>ivo://CDS.VizieR/VII/99</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/99&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/99</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/150/1 [1]</TD>
            <TD>VV29 and NGC 4676 HST photometry (Benitez+, 2004)</TD>
            <TD>We present the analysis of the faint galaxy population in the Advanced Camera for Surveys (ACS) Early Release Observation fields VV 29 (UGC 10214) and NGC 4676. These observations cover a total area of 26.3arcmin^2^ and have depths close to that of the Hubble Deep Fields in the deepest part of the VV 29 image, with 10{sigma} detection limits for point sources of 27.8, 27.6, and 27.2 AB magnitudes in the g_F475W_, V_F606W_, and I_F814W_ bands, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1#1</TD>
            <TD>2011-09-14T19:32:02Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/150/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/150/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/150/1 [2]</TD>
            <TD>VV29 and NGC 4676 HST photometry (Benitez+, 2004)</TD>
            <TD>We present the analysis of the faint galaxy population in the Advanced Camera for Surveys (ACS) Early Release Observation fields VV 29 (UGC 10214) and NGC 4676. These observations cover a total area of 26.3arcmin^2^ and have depths close to that of the Hubble Deep Fields in the deepest part of the VV 29 image, with 10{sigma} detection limits for point sources of 27.8, 27.6, and 27.2 AB magnitudes in the g_F475W_, V_F606W_, and I_F814W_ bands, respectively.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1#2</TD>
            <TD>2011-09-14T19:32:02Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/150/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/150/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/150/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/560/675 [1]</TD>
            <TD>Chandra X-ray point sources in Cen A (Kraft+, 2001)</TD>
            <TD>We present results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, we detect 246 individual point sources above a limiting luminosity of ~2*10^36^ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. We identify eight foreground stars in our observations. We also identify nine of the sources with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view are detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675#1</TD>
            <TD>2011-09-14T19:32:17Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/560/675</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/675</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/560/675 [2]</TD>
            <TD>Chandra X-ray point sources in Cen A (Kraft+, 2001)</TD>
            <TD>We present results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, we detect 246 individual point sources above a limiting luminosity of ~2*10^36^ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. We identify eight foreground stars in our observations. We also identify nine of the sources with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view are detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675#2</TD>
            <TD>2011-09-14T19:32:17Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/560/675&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/675</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/324/435 [1]</TD>
            <TD>Chemical composition of six K supergiants in the SMC (Hill 1997)</TD>
            <TD>A sample of six SMC cool stars (K supergiants) are analysed by high resolution spectroscopy in order to investigate their chemical content, which should reflect that of the current interstellar medium within the SMC. The abundance of Na, Al, {alpha}-elements, Fe peak and heavy elements are derived through an LTE analysis of the lines, compared to a Galactic "standard" (the well-studied K giant Arcturus) and discussed in terms of chemical evolution of the SMC. The following results were obtained: 1. All the stars from this sample are metal deficient ([Fe/H] ranges from -0.59 to -0.89dex). The abundance varies little from star-to-star (0.10dex rms, comparable with the expected error due to uncertainties on the effective parameters of the stars), in agreement with the very small chemical composition variations among the H II regions within the SMC found by Pagel et al. (1978MNRAS.184..569P). 2. Sodium is not strongly enhanced in these stars, and the star-to-star scatter is larger than expected. 3. At variance with metal-poor stars in our Galaxy, the so-called {alpha}-elements do not seem to be enhanced. 4. Nickel displays a noticeable depletion with respect to iron ([Ni/Fe]=~-0.3dex), at variance with what is found in the SMC F supergiants and in Arcturus. 5. Except for PMMR 144, the s and r process elements heavier than Ba are enhanced in all of our stars by =~+0.4dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/435#1</TD>
            <TD>2011-09-14T18:43:25Z</TD>
            <TD>#Abundances#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/435</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/324/435</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/324/435</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/324/435 [2]</TD>
            <TD>Chemical composition of six K supergiants in the SMC (Hill 1997)</TD>
            <TD>A sample of six SMC cool stars (K supergiants) are analysed by high resolution spectroscopy in order to investigate their chemical content, which should reflect that of the current interstellar medium within the SMC. The abundance of Na, Al, {alpha}-elements, Fe peak and heavy elements are derived through an LTE analysis of the lines, compared to a Galactic "standard" (the well-studied K giant Arcturus) and discussed in terms of chemical evolution of the SMC. The following results were obtained: 1. All the stars from this sample are metal deficient ([Fe/H] ranges from -0.59 to -0.89dex). The abundance varies little from star-to-star (0.10dex rms, comparable with the expected error due to uncertainties on the effective parameters of the stars), in agreement with the very small chemical composition variations among the H II regions within the SMC found by Pagel et al. (1978MNRAS.184..569P). 2. Sodium is not strongly enhanced in these stars, and the star-to-star scatter is larger than expected. 3. At variance with metal-poor stars in our Galaxy, the so-called {alpha}-elements do not seem to be enhanced. 4. Nickel displays a noticeable depletion with respect to iron ([Ni/Fe]=~-0.3dex), at variance with what is found in the SMC F supergiants and in Arcturus. 5. Except for PMMR 144, the s and r process elements heavier than Ba are enhanced in all of our stars by =~+0.4dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/435#2</TD>
            <TD>2011-09-14T18:43:25Z</TD>
            <TD>#Abundances#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/435</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/324/435&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/324/435</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/380/441 [1]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#1</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/380/441</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/380/441 [2]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#2</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/380/441&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/380/441 [table3]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#table3</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/380/441&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/380/441 [table1]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#table1</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/380/441&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/324/435 [1]</TD>
            <TD>Chemical composition of six K supergiants in the SMC (Hill 1997)</TD>
            <TD>A sample of six SMC cool stars (K supergiants) are analysed by high resolution spectroscopy in order to investigate their chemical content, which should reflect that of the current interstellar medium within the SMC. The abundance of Na, Al, {alpha}-elements, Fe peak and heavy elements are derived through an LTE analysis of the lines, compared to a Galactic "standard" (the well-studied K giant Arcturus) and discussed in terms of chemical evolution of the SMC. The following results were obtained: 1. All the stars from this sample are metal deficient ([Fe/H] ranges from -0.59 to -0.89dex). The abundance varies little from star-to-star (0.10dex rms, comparable with the expected error due to uncertainties on the effective parameters of the stars), in agreement with the very small chemical composition variations among the H II regions within the SMC found by Pagel et al. (1978MNRAS.184..569P). 2. Sodium is not strongly enhanced in these stars, and the star-to-star scatter is larger than expected. 3. At variance with metal-poor stars in our Galaxy, the so-called {alpha}-elements do not seem to be enhanced. 4. Nickel displays a noticeable depletion with respect to iron ([Ni/Fe]=~-0.3dex), at variance with what is found in the SMC F supergiants and in Arcturus. 5. Except for PMMR 144, the s and r process elements heavier than Ba are enhanced in all of our stars by =~+0.4dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/435#1</TD>
            <TD>2011-09-14T18:43:25Z</TD>
            <TD>#Abundances#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/435</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/324/435</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/324/435</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/324/435 [2]</TD>
            <TD>Chemical composition of six K supergiants in the SMC (Hill 1997)</TD>
            <TD>A sample of six SMC cool stars (K supergiants) are analysed by high resolution spectroscopy in order to investigate their chemical content, which should reflect that of the current interstellar medium within the SMC. The abundance of Na, Al, {alpha}-elements, Fe peak and heavy elements are derived through an LTE analysis of the lines, compared to a Galactic "standard" (the well-studied K giant Arcturus) and discussed in terms of chemical evolution of the SMC. The following results were obtained: 1. All the stars from this sample are metal deficient ([Fe/H] ranges from -0.59 to -0.89dex). The abundance varies little from star-to-star (0.10dex rms, comparable with the expected error due to uncertainties on the effective parameters of the stars), in agreement with the very small chemical composition variations among the H II regions within the SMC found by Pagel et al. (1978MNRAS.184..569P). 2. Sodium is not strongly enhanced in these stars, and the star-to-star scatter is larger than expected. 3. At variance with metal-poor stars in our Galaxy, the so-called {alpha}-elements do not seem to be enhanced. 4. Nickel displays a noticeable depletion with respect to iron ([Ni/Fe]=~-0.3dex), at variance with what is found in the SMC F supergiants and in Arcturus. 5. Except for PMMR 144, the s and r process elements heavier than Ba are enhanced in all of our stars by =~+0.4dex.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/435#2</TD>
            <TD>2011-09-14T18:43:25Z</TD>
            <TD>#Abundances#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+A/324/435</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/324/435&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/324/435</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/560/675 [1]</TD>
            <TD>Chandra X-ray point sources in Cen A (Kraft+, 2001)</TD>
            <TD>We present results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, we detect 246 individual point sources above a limiting luminosity of ~2*10^36^ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. We identify eight foreground stars in our observations. We also identify nine of the sources with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view are detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675#1</TD>
            <TD>2011-09-14T19:32:17Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/560/675</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/675</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/560/675 [2]</TD>
            <TD>Chandra X-ray point sources in Cen A (Kraft+, 2001)</TD>
            <TD>We present results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, we detect 246 individual point sources above a limiting luminosity of ~2*10^36^ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. We identify eight foreground stars in our observations. We also identify nine of the sources with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view are detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675#2</TD>
            <TD>2011-09-14T19:32:17Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/560/675&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/675</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/560/675 [1]</TD>
            <TD>Chandra X-ray point sources in Cen A (Kraft+, 2001)</TD>
            <TD>We present results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, we detect 246 individual point sources above a limiting luminosity of ~2*10^36^ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. We identify eight foreground stars in our observations. We also identify nine of the sources with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view are detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675#1</TD>
            <TD>2011-09-14T19:32:17Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/560/675</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/675</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/560/675 [2]</TD>
            <TD>Chandra X-ray point sources in Cen A (Kraft+, 2001)</TD>
            <TD>We present results from two Chandra X-ray Observatory observations of the X-ray point source population in the nearby radio galaxy Centaurus A (NGC 5128). Using a wavelet decomposition detection algorithm, we detect 246 individual point sources above a limiting luminosity of ~2*10^36^ergs/s, 82 of which are detected in both data sets where the fields of view overlap. Thirty-eight sources were detected in only one observation but were within the field of view of both pointings, implying considerable variability. We identify eight foreground stars in our observations. We also identify nine of the sources with known globular clusters in Centaurus A. All previously observed ROSAT sources within our field of view are detected.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675#2</TD>
            <TD>2011-09-14T19:32:17Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/560/675</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/560/675&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/560/675</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/130/323 [1]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#1</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/130/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/130/323 [2]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#2</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/130/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/323 [table3]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#table3</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/323 [table2]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#table2</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/380/441 [1]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#1</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/380/441</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/380/441 [2]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#2</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/380/441&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/380/441 [table3]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#table3</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/380/441&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/380/441 [table1]</TD>
            <TD>Galaxies behind Southern Milky Way. II. (Woudt+, 2001)</TD>
            <TD>In this second paper of the catalogue series of galaxies behind the southern Milky Way, we report on the deep optical galaxy search in the Crux region (289{deg}&lt;~l&lt;~318{deg} and -10{deg}&lt;~b&lt;~10{deg}) and the Great Attractor region (316{deg}&lt;~l&lt;~338{deg} and -10{deg}&lt;~b&lt;~10{deg}). The galaxy catalogues are presented, a brief description of the galaxy search given, as well as a discussion on the distribution and characteristics of the uncovered galaxies. A total of 8183 galaxies with major diameters D&gt;~0.2 arcmin were identified in this ~850 square degree area: 3759 galaxies in the Crux region and 4423 galaxies in the Great Attractor region. Of the 8183 galaxies, 229 (2.8%) were catalogued before in the optical (3 in radio) and 251 galaxies have a reliable (159), or likely (92) cross-identification in the IRAS Point Source Catalogue (3.1%). A number of prominent overdensities and filaments of galaxies are identified. They are not correlated with the Galactic foreground extinction and hence indicative of extragalactic large-scale structures. Redshifts obtained at the South African Astronomical Observatory (SAAO) for 518 of the newly catalogued galaxies in the Crux and Great Attractor regions (Fairall et al., 1998, Cat. &lt;J/A+AS/127/463&gt;; Woudt et al., 1999, Cat. &lt;J/A+A/352/39&gt;) confirm distinct voids and clusters in the area here surveyed. With this optical galaxy search, we have reduced the width of the optical `Zone of Avoidance' for galaxies with extinction-corrected diameters larger than 1.3' from extinction levels A_B&gt;~1.0mag to A_B&gt;~3.0mag: the remaining optical Zone of Avoidance is now limited by |b|&lt;~3{deg} (see Fig. 16).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441#table1</TD>
            <TD>2011-09-14T19:18:42Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Nov-2001</TD>
            <TD>ivo://CDS.VizieR/J/A+A/380/441</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/380/441&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/380/441</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/130/323 [1]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#1</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/130/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/130/323 [2]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#2</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/130/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/323 [table3]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#table3</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/323 [table2]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#table2</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/600/L99 [1]</TD>
            <TD>Colours of z~6 galaxies in GOODS (Dickinson+, 2004)</TD>
            <TD>We report early results on galaxies at z~6 selected from Hubble Space Telescope imaging for the Great Observatories Origins Deep Survey. Spectroscopy of one object with the Advanced Camera for Surveys grism and from the Keck and Very Large Telescope observatories shows a strong continuum break and asymmetric line emission, identified as Ly{alpha} at z=5.83. We find only five spatially extended candidates with signal-to-noise ratios greater than 10, two of which have spectroscopic confirmation. This is much fewer than would be expected if galaxies at z=6 had the same luminosity function as those at z=3. There are many fainter candidates, but we expect substantial contamination from foreground interlopers and spurious detections. Our best estimates favor a z=6 galaxy population with fainter luminosities, higher space density, and similar comoving ultraviolet emissivity to that at z=3, but this depends critically on counts at fluxes fainter than those reliably probed by the current data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99#1</TD>
            <TD>2011-09-14T19:32:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/600/L99</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/600/L99</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/600/L99 [2]</TD>
            <TD>Colours of z~6 galaxies in GOODS (Dickinson+, 2004)</TD>
            <TD>We report early results on galaxies at z~6 selected from Hubble Space Telescope imaging for the Great Observatories Origins Deep Survey. Spectroscopy of one object with the Advanced Camera for Surveys grism and from the Keck and Very Large Telescope observatories shows a strong continuum break and asymmetric line emission, identified as Ly{alpha} at z=5.83. We find only five spatially extended candidates with signal-to-noise ratios greater than 10, two of which have spectroscopic confirmation. This is much fewer than would be expected if galaxies at z=6 had the same luminosity function as those at z=3. There are many fainter candidates, but we expect substantial contamination from foreground interlopers and spurious detections. Our best estimates favor a z=6 galaxy population with fainter luminosities, higher space density, and similar comoving ultraviolet emissivity to that at z=3, but this depends critically on counts at fluxes fainter than those reliably probed by the current data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99#2</TD>
            <TD>2011-09-14T19:32:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/600/L99&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/600/L99</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/397/177 [1]</TD>
            <TD>IR star clusters and stellar groups catalog (Bica+, 2003)</TD>
            <TD>We compiled a catalogue of infrared star clusters in the Galaxy, which are most of them embedded. It condenses the growing literature information. We also include in the sample infrared stellar groups which are less dense than star clusters, such as those embedded in the dark clouds Taurus-Auriga and Chamaleon I. We provide galactic and equatorial coordinates, angular dimensions, different designations and related objects such as nebulae. A total of 189 infrared clusters and 87 embedded stellar groups are included. A fraction of 25% of the embedded clusters are projected close to each other in pair or triplet systems, indicating that multiplicity plays an important role in star cluster formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177#1</TD>
            <TD>2011-09-14T19:19:07Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/397/177</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/177</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/397/177 [2]</TD>
            <TD>IR star clusters and stellar groups catalog (Bica+, 2003)</TD>
            <TD>We compiled a catalogue of infrared star clusters in the Galaxy, which are most of them embedded. It condenses the growing literature information. We also include in the sample infrared stellar groups which are less dense than star clusters, such as those embedded in the dark clouds Taurus-Auriga and Chamaleon I. We provide galactic and equatorial coordinates, angular dimensions, different designations and related objects such as nebulae. A total of 189 infrared clusters and 87 embedded stellar groups are included. A fraction of 25% of the embedded clusters are projected close to each other in pair or triplet systems, indicating that multiplicity plays an important role in star cluster formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177#2</TD>
            <TD>2011-09-14T19:19:07Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/397/177&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/397/177 [table1]</TD>
            <TD>IR star clusters and stellar groups catalog (Bica+, 2003)</TD>
            <TD>We compiled a catalogue of infrared star clusters in the Galaxy, which are most of them embedded. It condenses the growing literature information. We also include in the sample infrared stellar groups which are less dense than star clusters, such as those embedded in the dark clouds Taurus-Auriga and Chamaleon I. We provide galactic and equatorial coordinates, angular dimensions, different designations and related objects such as nebulae. A total of 189 infrared clusters and 87 embedded stellar groups are included. A fraction of 25% of the embedded clusters are projected close to each other in pair or triplet systems, indicating that multiplicity plays an important role in star cluster formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177#table1</TD>
            <TD>2011-09-14T19:19:07Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/397/177&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/177</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/397/177 [1]</TD>
            <TD>IR star clusters and stellar groups catalog (Bica+, 2003)</TD>
            <TD>We compiled a catalogue of infrared star clusters in the Galaxy, which are most of them embedded. It condenses the growing literature information. We also include in the sample infrared stellar groups which are less dense than star clusters, such as those embedded in the dark clouds Taurus-Auriga and Chamaleon I. We provide galactic and equatorial coordinates, angular dimensions, different designations and related objects such as nebulae. A total of 189 infrared clusters and 87 embedded stellar groups are included. A fraction of 25% of the embedded clusters are projected close to each other in pair or triplet systems, indicating that multiplicity plays an important role in star cluster formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177#1</TD>
            <TD>2011-09-14T19:19:07Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/397/177</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/177</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/397/177 [2]</TD>
            <TD>IR star clusters and stellar groups catalog (Bica+, 2003)</TD>
            <TD>We compiled a catalogue of infrared star clusters in the Galaxy, which are most of them embedded. It condenses the growing literature information. We also include in the sample infrared stellar groups which are less dense than star clusters, such as those embedded in the dark clouds Taurus-Auriga and Chamaleon I. We provide galactic and equatorial coordinates, angular dimensions, different designations and related objects such as nebulae. A total of 189 infrared clusters and 87 embedded stellar groups are included. A fraction of 25% of the embedded clusters are projected close to each other in pair or triplet systems, indicating that multiplicity plays an important role in star cluster formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177#2</TD>
            <TD>2011-09-14T19:19:07Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/397/177&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/397/177 [table1]</TD>
            <TD>IR star clusters and stellar groups catalog (Bica+, 2003)</TD>
            <TD>We compiled a catalogue of infrared star clusters in the Galaxy, which are most of them embedded. It condenses the growing literature information. We also include in the sample infrared stellar groups which are less dense than star clusters, such as those embedded in the dark clouds Taurus-Auriga and Chamaleon I. We provide galactic and equatorial coordinates, angular dimensions, different designations and related objects such as nebulae. A total of 189 infrared clusters and 87 embedded stellar groups are included. A fraction of 25% of the embedded clusters are projected close to each other in pair or triplet systems, indicating that multiplicity plays an important role in star cluster formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177#table1</TD>
            <TD>2011-09-14T19:19:07Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/397/177&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/177</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/397/177 [1]</TD>
            <TD>IR star clusters and stellar groups catalog (Bica+, 2003)</TD>
            <TD>We compiled a catalogue of infrared star clusters in the Galaxy, which are most of them embedded. It condenses the growing literature information. We also include in the sample infrared stellar groups which are less dense than star clusters, such as those embedded in the dark clouds Taurus-Auriga and Chamaleon I. We provide galactic and equatorial coordinates, angular dimensions, different designations and related objects such as nebulae. A total of 189 infrared clusters and 87 embedded stellar groups are included. A fraction of 25% of the embedded clusters are projected close to each other in pair or triplet systems, indicating that multiplicity plays an important role in star cluster formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177#1</TD>
            <TD>2011-09-14T19:19:07Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/397/177</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/177</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/397/177 [2]</TD>
            <TD>IR star clusters and stellar groups catalog (Bica+, 2003)</TD>
            <TD>We compiled a catalogue of infrared star clusters in the Galaxy, which are most of them embedded. It condenses the growing literature information. We also include in the sample infrared stellar groups which are less dense than star clusters, such as those embedded in the dark clouds Taurus-Auriga and Chamaleon I. We provide galactic and equatorial coordinates, angular dimensions, different designations and related objects such as nebulae. A total of 189 infrared clusters and 87 embedded stellar groups are included. A fraction of 25% of the embedded clusters are projected close to each other in pair or triplet systems, indicating that multiplicity plays an important role in star cluster formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177#2</TD>
            <TD>2011-09-14T19:19:07Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/397/177&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/177</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/397/177 [table1]</TD>
            <TD>IR star clusters and stellar groups catalog (Bica+, 2003)</TD>
            <TD>We compiled a catalogue of infrared star clusters in the Galaxy, which are most of them embedded. It condenses the growing literature information. We also include in the sample infrared stellar groups which are less dense than star clusters, such as those embedded in the dark clouds Taurus-Auriga and Chamaleon I. We provide galactic and equatorial coordinates, angular dimensions, different designations and related objects such as nebulae. A total of 189 infrared clusters and 87 embedded stellar groups are included. A fraction of 25% of the embedded clusters are projected close to each other in pair or triplet systems, indicating that multiplicity plays an important role in star cluster formation.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177#table1</TD>
            <TD>2011-09-14T19:19:07Z</TD>
            <TD>#Associations#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/177</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/397/177&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/177</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/399/813 [1]</TD>
            <TD>Multiple merging events in Abell 521 (Ferrari, 2003)</TD>
            <TD>Radial velocity measurements and spectral features of 191 objects in the central region of the galaxy cluster Abell 521, observed through a campaign of multi-object spectroscopy at the ESO 3.6m telescope (3 nights in October 1999, and 2.5 nights in December 2000). The spectral resolution is 1.85nm in October 1999 and 1.25nm in December 2000 (FWHM)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813#1</TD>
            <TD>2011-09-14T19:19:23Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/399/813</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/813</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/399/813 [2]</TD>
            <TD>Multiple merging events in Abell 521 (Ferrari, 2003)</TD>
            <TD>Radial velocity measurements and spectral features of 191 objects in the central region of the galaxy cluster Abell 521, observed through a campaign of multi-object spectroscopy at the ESO 3.6m telescope (3 nights in October 1999, and 2.5 nights in December 2000). The spectral resolution is 1.85nm in October 1999 and 1.25nm in December 2000 (FWHM)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813#2</TD>
            <TD>2011-09-14T19:19:23Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/399/813&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/813</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/813 [table10]</TD>
            <TD>Multiple merging events in Abell 521 (Ferrari, 2003)</TD>
            <TD>Radial velocity measurements and spectral features of 191 objects in the central region of the galaxy cluster Abell 521, observed through a campaign of multi-object spectroscopy at the ESO 3.6m telescope (3 nights in October 1999, and 2.5 nights in December 2000). The spectral resolution is 1.85nm in October 1999 and 1.25nm in December 2000 (FWHM)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813#table10</TD>
            <TD>2011-09-14T19:19:23Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/813&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/813</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/399/813 [1]</TD>
            <TD>Multiple merging events in Abell 521 (Ferrari, 2003)</TD>
            <TD>Radial velocity measurements and spectral features of 191 objects in the central region of the galaxy cluster Abell 521, observed through a campaign of multi-object spectroscopy at the ESO 3.6m telescope (3 nights in October 1999, and 2.5 nights in December 2000). The spectral resolution is 1.85nm in October 1999 and 1.25nm in December 2000 (FWHM)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813#1</TD>
            <TD>2011-09-14T19:19:23Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/399/813</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/813</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/399/813 [2]</TD>
            <TD>Multiple merging events in Abell 521 (Ferrari, 2003)</TD>
            <TD>Radial velocity measurements and spectral features of 191 objects in the central region of the galaxy cluster Abell 521, observed through a campaign of multi-object spectroscopy at the ESO 3.6m telescope (3 nights in October 1999, and 2.5 nights in December 2000). The spectral resolution is 1.85nm in October 1999 and 1.25nm in December 2000 (FWHM)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813#2</TD>
            <TD>2011-09-14T19:19:23Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/399/813&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/813</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/813 [table10]</TD>
            <TD>Multiple merging events in Abell 521 (Ferrari, 2003)</TD>
            <TD>Radial velocity measurements and spectral features of 191 objects in the central region of the galaxy cluster Abell 521, observed through a campaign of multi-object spectroscopy at the ESO 3.6m telescope (3 nights in October 1999, and 2.5 nights in December 2000). The spectral resolution is 1.85nm in October 1999 and 1.25nm in December 2000 (FWHM)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813#table10</TD>
            <TD>2011-09-14T19:19:23Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/813&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/813</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/399/813 [1]</TD>
            <TD>Multiple merging events in Abell 521 (Ferrari, 2003)</TD>
            <TD>Radial velocity measurements and spectral features of 191 objects in the central region of the galaxy cluster Abell 521, observed through a campaign of multi-object spectroscopy at the ESO 3.6m telescope (3 nights in October 1999, and 2.5 nights in December 2000). The spectral resolution is 1.85nm in October 1999 and 1.25nm in December 2000 (FWHM)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813#1</TD>
            <TD>2011-09-14T19:19:23Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/399/813</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/813</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/399/813 [2]</TD>
            <TD>Multiple merging events in Abell 521 (Ferrari, 2003)</TD>
            <TD>Radial velocity measurements and spectral features of 191 objects in the central region of the galaxy cluster Abell 521, observed through a campaign of multi-object spectroscopy at the ESO 3.6m telescope (3 nights in October 1999, and 2.5 nights in December 2000). The spectral resolution is 1.85nm in October 1999 and 1.25nm in December 2000 (FWHM)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813#2</TD>
            <TD>2011-09-14T19:19:23Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/399/813&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/813</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/399/813 [table10]</TD>
            <TD>Multiple merging events in Abell 521 (Ferrari, 2003)</TD>
            <TD>Radial velocity measurements and spectral features of 191 objects in the central region of the galaxy cluster Abell 521, observed through a campaign of multi-object spectroscopy at the ESO 3.6m telescope (3 nights in October 1999, and 2.5 nights in December 2000). The spectral resolution is 1.85nm in October 1999 and 1.25nm in December 2000 (FWHM)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813#table10</TD>
            <TD>2011-09-14T19:19:23Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/399/813</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/399/813&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/399/813</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/2990 [1]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
            <TD>We have imaged eight nearby spiral galaxies with the SPIRIT III infrared telescope on the Midcourse Space Experiment (MSX) satellite in the mid-infrared at 18" resolution at 8.3, 12.1, 14.7, and 21.3{mu}m. Each of the eight shows interesting structure not previously detected with older, lower resolution infrared data sets, such as a resolved nucleus or spiral structure. The MSX data are compared with existing data sets at ultraviolet, optical, and infrared wavelengths, including recent observations from the Infrared Space Observatory. The infrared structures in M83 and NGC 5055 show a striking similarity to the ultraviolet emission but are less similar to the optical emission. Several point sources with no identified counterparts at other wavelengths are found near M31, NGC 4945, M83, and M101. Over 200 previously known objects are also detected at 8{mu}m.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#1</TD>
            <TD>2011-09-14T19:20:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/2990</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/2990</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/2990 [2]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
            <TD>We have imaged eight nearby spiral galaxies with the SPIRIT III infrared telescope on the Midcourse Space Experiment (MSX) satellite in the mid-infrared at 18" resolution at 8.3, 12.1, 14.7, and 21.3{mu}m. Each of the eight shows interesting structure not previously detected with older, lower resolution infrared data sets, such as a resolved nucleus or spiral structure. The MSX data are compared with existing data sets at ultraviolet, optical, and infrared wavelengths, including recent observations from the Infrared Space Observatory. The infrared structures in M83 and NGC 5055 show a striking similarity to the ultraviolet emission but are less similar to the optical emission. Several point sources with no identified counterparts at other wavelengths are found near M31, NGC 4945, M83, and M101. Over 200 previously known objects are also detected at 8{mu}m.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#2</TD>
            <TD>2011-09-14T19:20:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/2990&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/2990</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/2990 [table5]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
            <TD>We have imaged eight nearby spiral galaxies with the SPIRIT III infrared telescope on the Midcourse Space Experiment (MSX) satellite in the mid-infrared at 18" resolution at 8.3, 12.1, 14.7, and 21.3{mu}m. Each of the eight shows interesting structure not previously detected with older, lower resolution infrared data sets, such as a resolved nucleus or spiral structure. The MSX data are compared with existing data sets at ultraviolet, optical, and infrared wavelengths, including recent observations from the Infrared Space Observatory. The infrared structures in M83 and NGC 5055 show a striking similarity to the ultraviolet emission but are less similar to the optical emission. Several point sources with no identified counterparts at other wavelengths are found near M31, NGC 4945, M83, and M101. Over 200 previously known objects are also detected at 8{mu}m.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#table5</TD>
            <TD>2011-09-14T19:20:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/2990&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/2990</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/2990 [table4]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
            <TD>We have imaged eight nearby spiral galaxies with the SPIRIT III infrared telescope on the Midcourse Space Experiment (MSX) satellite in the mid-infrared at 18" resolution at 8.3, 12.1, 14.7, and 21.3{mu}m. Each of the eight shows interesting structure not previously detected with older, lower resolution infrared data sets, such as a resolved nucleus or spiral structure. The MSX data are compared with existing data sets at ultraviolet, optical, and infrared wavelengths, including recent observations from the Infrared Space Observatory. The infrared structures in M83 and NGC 5055 show a striking similarity to the ultraviolet emission but are less similar to the optical emission. Several point sources with no identified counterparts at other wavelengths are found near M31, NGC 4945, M83, and M101. Over 200 previously known objects are also detected at 8{mu}m.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#table4</TD>
            <TD>2011-09-14T19:20:09Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/2990&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/2990</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/2990 [1]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
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            <TD>#Infrared#</TD>
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            <TD>13-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
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            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/2990</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/2990</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/2990 [2]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
            <TD>We have imaged eight nearby spiral galaxies with the SPIRIT III infrared telescope on the Midcourse Space Experiment (MSX) satellite in the mid-infrared at 18" resolution at 8.3, 12.1, 14.7, and 21.3{mu}m. Each of the eight shows interesting structure not previously detected with older, lower resolution infrared data sets, such as a resolved nucleus or spiral structure. The MSX data are compared with existing data sets at ultraviolet, optical, and infrared wavelengths, including recent observations from the Infrared Space Observatory. The infrared structures in M83 and NGC 5055 show a striking similarity to the ultraviolet emission but are less similar to the optical emission. Several point sources with no identified counterparts at other wavelengths are found near M31, NGC 4945, M83, and M101. Over 200 previously known objects are also detected at 8{mu}m.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#2</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/124/2990</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/2990&amp;</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/2990 [table5]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
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            <TD>#Infrared#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/2990&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/124/2990 [table4]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
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            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#table4</TD>
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            <TD>13-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/2990&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/2990</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/124/2990 [1]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
            <TD>We have imaged eight nearby spiral galaxies with the SPIRIT III infrared telescope on the Midcourse Space Experiment (MSX) satellite in the mid-infrared at 18" resolution at 8.3, 12.1, 14.7, and 21.3{mu}m. Each of the eight shows interesting structure not previously detected with older, lower resolution infrared data sets, such as a resolved nucleus or spiral structure. The MSX data are compared with existing data sets at ultraviolet, optical, and infrared wavelengths, including recent observations from the Infrared Space Observatory. The infrared structures in M83 and NGC 5055 show a striking similarity to the ultraviolet emission but are less similar to the optical emission. Several point sources with no identified counterparts at other wavelengths are found near M31, NGC 4945, M83, and M101. Over 200 previously known objects are also detected at 8{mu}m.</TD>
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            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#1</TD>
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            <TD>13-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/124/2990</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/2990</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/124/2990 [2]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
            <TD>We have imaged eight nearby spiral galaxies with the SPIRIT III infrared telescope on the Midcourse Space Experiment (MSX) satellite in the mid-infrared at 18" resolution at 8.3, 12.1, 14.7, and 21.3{mu}m. Each of the eight shows interesting structure not previously detected with older, lower resolution infrared data sets, such as a resolved nucleus or spiral structure. The MSX data are compared with existing data sets at ultraviolet, optical, and infrared wavelengths, including recent observations from the Infrared Space Observatory. The infrared structures in M83 and NGC 5055 show a striking similarity to the ultraviolet emission but are less similar to the optical emission. Several point sources with no identified counterparts at other wavelengths are found near M31, NGC 4945, M83, and M101. Over 200 previously known objects are also detected at 8{mu}m.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#2</TD>
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            <TD>13-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/124/2990&amp;</TD>
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            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/AJ/124/2990 [table5]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
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            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#table5</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/2990&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/124/2990 [table4]</TD>
            <TD>MSX galaxy observations (Kraemer+, 2002)</TD>
            <TD>We have imaged eight nearby spiral galaxies with the SPIRIT III infrared telescope on the Midcourse Space Experiment (MSX) satellite in the mid-infrared at 18" resolution at 8.3, 12.1, 14.7, and 21.3{mu}m. Each of the eight shows interesting structure not previously detected with older, lower resolution infrared data sets, such as a resolved nucleus or spiral structure. The MSX data are compared with existing data sets at ultraviolet, optical, and infrared wavelengths, including recent observations from the Infrared Space Observatory. The infrared structures in M83 and NGC 5055 show a striking similarity to the ultraviolet emission but are less similar to the optical emission. Several point sources with no identified counterparts at other wavelengths are found near M31, NGC 4945, M83, and M101. Over 200 previously known objects are also detected at 8{mu}m.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/124/2990#table4</TD>
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            <TD>13-Jan-2003</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/124/2990&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/124/2990</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/578/114 [1]</TD>
            <TD>Chandra HRC source in M31 (Kaaret, 2002)</TD>
            <TD>We present results from a 47ks observation of the Andromeda galaxy, M31, using the High Resolution Camera of the Chandra X-Ray Observatory. We detect 142 point sources spanning 3 orders of magnitude in luminosity, from L_X_=2x10^35^ to 2x10^38^erg/s in the 0.1-10keV band. The X-ray source location accuracy is better than 1" in the central regions of the galaxy. One source lies within 1.3" of SN 1885 but does not coincide with the UV absorption feature identified as the supernova remnant.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/578/114#1</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/578/114</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/578/114</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/578/114 [2]</TD>
            <TD>Chandra HRC source in M31 (Kaaret, 2002)</TD>
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            <TD>CDS</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/578/114&amp;</TD>
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            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJ/578/114 [table1]</TD>
            <TD>Chandra HRC source in M31 (Kaaret, 2002)</TD>
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            <TD>#X-ray#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/578/114&amp;</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/578/114</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/578/114 [1]</TD>
            <TD>Chandra HRC source in M31 (Kaaret, 2002)</TD>
            <TD>We present results from a 47ks observation of the Andromeda galaxy, M31, using the High Resolution Camera of the Chandra X-Ray Observatory. We detect 142 point sources spanning 3 orders of magnitude in luminosity, from L_X_=2x10^35^ to 2x10^38^erg/s in the 0.1-10keV band. The X-ray source location accuracy is better than 1" in the central regions of the galaxy. One source lies within 1.3" of SN 1885 but does not coincide with the UV absorption feature identified as the supernova remnant.</TD>
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            <TD>#X-ray#</TD>
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            <TD>ivo://CDS.VizieR/J/ApJ/578/114</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/578/114</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/578/114</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/578/114 [2]</TD>
            <TD>Chandra HRC source in M31 (Kaaret, 2002)</TD>
            <TD>We present results from a 47ks observation of the Andromeda galaxy, M31, using the High Resolution Camera of the Chandra X-Ray Observatory. We detect 142 point sources spanning 3 orders of magnitude in luminosity, from L_X_=2x10^35^ to 2x10^38^erg/s in the 0.1-10keV band. The X-ray source location accuracy is better than 1" in the central regions of the galaxy. One source lies within 1.3" of SN 1885 but does not coincide with the UV absorption feature identified as the supernova remnant.</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/578/114 [table1]</TD>
            <TD>Chandra HRC source in M31 (Kaaret, 2002)</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/578/114&amp;</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/578/114</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/578/114 [1]</TD>
            <TD>Chandra HRC source in M31 (Kaaret, 2002)</TD>
            <TD>We present results from a 47ks observation of the Andromeda galaxy, M31, using the High Resolution Camera of the Chandra X-Ray Observatory. We detect 142 point sources spanning 3 orders of magnitude in luminosity, from L_X_=2x10^35^ to 2x10^38^erg/s in the 0.1-10keV band. The X-ray source location accuracy is better than 1" in the central regions of the galaxy. One source lies within 1.3" of SN 1885 but does not coincide with the UV absorption feature identified as the supernova remnant.</TD>
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            <TD>09-Dec-2002</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/578/114</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/578/114</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/578/114 [2]</TD>
            <TD>Chandra HRC source in M31 (Kaaret, 2002)</TD>
            <TD>We present results from a 47ks observation of the Andromeda galaxy, M31, using the High Resolution Camera of the Chandra X-Ray Observatory. We detect 142 point sources spanning 3 orders of magnitude in luminosity, from L_X_=2x10^35^ to 2x10^38^erg/s in the 0.1-10keV band. The X-ray source location accuracy is better than 1" in the central regions of the galaxy. One source lies within 1.3" of SN 1885 but does not coincide with the UV absorption feature identified as the supernova remnant.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/578/114#2</TD>
            <TD>2011-09-14T19:20:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/578/114</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/578/114&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/578/114</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/578/114 [table1]</TD>
            <TD>Chandra HRC source in M31 (Kaaret, 2002)</TD>
            <TD>We present results from a 47ks observation of the Andromeda galaxy, M31, using the High Resolution Camera of the Chandra X-Ray Observatory. We detect 142 point sources spanning 3 orders of magnitude in luminosity, from L_X_=2x10^35^ to 2x10^38^erg/s in the 0.1-10keV band. The X-ray source location accuracy is better than 1" in the central regions of the galaxy. One source lies within 1.3" of SN 1885 but does not coincide with the UV absorption feature identified as the supernova remnant.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/578/114#table1</TD>
            <TD>2011-09-14T19:20:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/578/114</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/578/114&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/578/114</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/400/533 [1]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#1</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/400/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/400/533 [2]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#2</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/400/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/400/533 [table3]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#table3</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/400/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/400/533 [table4]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#table4</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/400/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/400/533 [1]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#1</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/400/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/400/533 [2]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#2</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/400/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/400/533 [table3]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#table3</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/400/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/400/533 [table4]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#table4</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/400/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/400/533 [1]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#1</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/400/533</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/400/533 [2]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#2</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/400/533&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/400/533 [table3]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#table3</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/400/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/400/533 [table4]</TD>
            <TD>New infrared star clusters in southern Milky Way (Dutra+, 2003)</TD>
            <TD>We carried out a 2MASS J, H and Ks survey of infrared star clusters in the Milky Way sector 230{deg}&lt;l&lt;350{deg}. This zone was the least studied in the literature, previously including only 12 infrared clusters or stellar groups with |b|&lt;10{deg}, according to the recent catalogue by Bica et al. (2003, Cat. &lt;J/A+A/397/177&gt;). We concentrated efforts on embedded clusters, which are those expected in the areas of known radio and optical nebulae. The present study provides 179 new infrared clusters and stellar groups, which are interesting targets for detailed future infrared studies. The sample of catalogued infrared clusters and stellar groups in the Galaxy is now increased by 63%.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533#table4</TD>
            <TD>2011-09-14T19:20:27Z</TD>
            <TD>#Open_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Jan-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/400/533</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/400/533&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/400/533</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/397/133 [1]</TD>
            <TD>Star-forming complexes in the Galaxy (Russeil+, 2003)</TD>
            <TD>We have carried out a multiwavelength study of the plane of our Galaxy in order to establish a star-forming-complex catalogue which is as complete as possible. Features observed include H{alpha}, H109{alpha}, CO, the radio continuum and absorption lines. For each complex we have determined the position, the systemic velocity, the kinematic distance and, when possible, the stellar distance and the corresponding uncertainties. All of these parameters were determined as homogeneously as possible, in particular all the stellar distances have been (re)calculated with the same calibration and the kinematic distances with the same mean Galactic rotation curve. Through the complexes with stellar distance determination, a rotation curve has been fitted. It is in good agreement with the one of Brand &amp; Blitz (1993, Cat. &lt;J/A+A/275/67&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133#1</TD>
            <TD>2011-09-14T19:20:40Z</TD>
            <TD>#Stars#HII_regions#Velocities#</TD>
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            <TD />
            <TD>13-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/397/133</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/133</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/397/133 [2]</TD>
            <TD>Star-forming complexes in the Galaxy (Russeil+, 2003)</TD>
            <TD>We have carried out a multiwavelength study of the plane of our Galaxy in order to establish a star-forming-complex catalogue which is as complete as possible. Features observed include H{alpha}, H109{alpha}, CO, the radio continuum and absorption lines. For each complex we have determined the position, the systemic velocity, the kinematic distance and, when possible, the stellar distance and the corresponding uncertainties. All of these parameters were determined as homogeneously as possible, in particular all the stellar distances have been (re)calculated with the same calibration and the kinematic distances with the same mean Galactic rotation curve. Through the complexes with stellar distance determination, a rotation curve has been fitted. It is in good agreement with the one of Brand &amp; Blitz (1993, Cat. &lt;J/A+A/275/67&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133#2</TD>
            <TD>2011-09-14T19:20:40Z</TD>
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            <TD>13-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/397/133&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/133</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/397/133 [1]</TD>
            <TD>Star-forming complexes in the Galaxy (Russeil+, 2003)</TD>
            <TD>We have carried out a multiwavelength study of the plane of our Galaxy in order to establish a star-forming-complex catalogue which is as complete as possible. Features observed include H{alpha}, H109{alpha}, CO, the radio continuum and absorption lines. For each complex we have determined the position, the systemic velocity, the kinematic distance and, when possible, the stellar distance and the corresponding uncertainties. All of these parameters were determined as homogeneously as possible, in particular all the stellar distances have been (re)calculated with the same calibration and the kinematic distances with the same mean Galactic rotation curve. Through the complexes with stellar distance determination, a rotation curve has been fitted. It is in good agreement with the one of Brand &amp; Blitz (1993, Cat. &lt;J/A+A/275/67&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133#1</TD>
            <TD>2011-09-14T19:20:40Z</TD>
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            <TD />
            <TD>13-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/397/133</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/133</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/397/133 [2]</TD>
            <TD>Star-forming complexes in the Galaxy (Russeil+, 2003)</TD>
            <TD>We have carried out a multiwavelength study of the plane of our Galaxy in order to establish a star-forming-complex catalogue which is as complete as possible. Features observed include H{alpha}, H109{alpha}, CO, the radio continuum and absorption lines. For each complex we have determined the position, the systemic velocity, the kinematic distance and, when possible, the stellar distance and the corresponding uncertainties. All of these parameters were determined as homogeneously as possible, in particular all the stellar distances have been (re)calculated with the same calibration and the kinematic distances with the same mean Galactic rotation curve. Through the complexes with stellar distance determination, a rotation curve has been fitted. It is in good agreement with the one of Brand &amp; Blitz (1993, Cat. &lt;J/A+A/275/67&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133#2</TD>
            <TD>2011-09-14T19:20:40Z</TD>
            <TD>#Stars#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>13-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/397/133&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/133</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/397/133 [1]</TD>
            <TD>Star-forming complexes in the Galaxy (Russeil+, 2003)</TD>
            <TD>We have carried out a multiwavelength study of the plane of our Galaxy in order to establish a star-forming-complex catalogue which is as complete as possible. Features observed include H{alpha}, H109{alpha}, CO, the radio continuum and absorption lines. For each complex we have determined the position, the systemic velocity, the kinematic distance and, when possible, the stellar distance and the corresponding uncertainties. All of these parameters were determined as homogeneously as possible, in particular all the stellar distances have been (re)calculated with the same calibration and the kinematic distances with the same mean Galactic rotation curve. Through the complexes with stellar distance determination, a rotation curve has been fitted. It is in good agreement with the one of Brand &amp; Blitz (1993, Cat. &lt;J/A+A/275/67&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133#1</TD>
            <TD>2011-09-14T19:20:40Z</TD>
            <TD>#Stars#HII_regions#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/397/133</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/133</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/397/133 [2]</TD>
            <TD>Star-forming complexes in the Galaxy (Russeil+, 2003)</TD>
            <TD>We have carried out a multiwavelength study of the plane of our Galaxy in order to establish a star-forming-complex catalogue which is as complete as possible. Features observed include H{alpha}, H109{alpha}, CO, the radio continuum and absorption lines. For each complex we have determined the position, the systemic velocity, the kinematic distance and, when possible, the stellar distance and the corresponding uncertainties. All of these parameters were determined as homogeneously as possible, in particular all the stellar distances have been (re)calculated with the same calibration and the kinematic distances with the same mean Galactic rotation curve. Through the complexes with stellar distance determination, a rotation curve has been fitted. It is in good agreement with the one of Brand &amp; Blitz (1993, Cat. &lt;J/A+A/275/67&gt;).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133#2</TD>
            <TD>2011-09-14T19:20:40Z</TD>
            <TD>#Stars#HII_regions#Velocities#</TD>
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            <TD />
            <TD>13-Dec-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+A/397/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/397/133&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/397/133</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1200 [1]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#1</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1200</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1200 [2]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#2</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1200&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1200 [table2]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#table2</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1200&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1200 [table3]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#table3</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1200&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1200 [1]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#1</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1200</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1200 [2]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#2</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1200&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1200 [table2]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#table2</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1200&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1200 [table3]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#table3</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1200&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1200 [1]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#1</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1200</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1200 [2]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#2</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1200&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1200 [table2]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#table2</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1200&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1200 [table3]</TD>
            <TD>Aquarius superclusters. I. (Caretta+, 2002)</TD>
            <TD>We study the distribution of galaxies and galaxy clusters in a 10{deg}x6{deg} field in the Aquarius region. In addition to 63 clusters in the literature, we have found 39 new candidate clusters using a matched-filter technique and a counts-in-cells analysis. From redshift measurements of galaxies in the direction of these cluster candidates, we present new mean redshifts for 31 previously unobserved clusters, while improved mean redshifts are presented for 35 other systems.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200#table3</TD>
            <TD>2011-09-14T19:20:42Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1200</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1200&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1200</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2511 [1]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#1</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/2511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2511 [2]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#2</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/2511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2511 [table2]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#table2</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2511 [table3]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#table3</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2511 [1]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#1</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/2511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2511 [2]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#2</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/2511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2511 [table2]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#table2</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2511 [table3]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#table3</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/2511 [1]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#1</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/2511</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/2511 [2]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#2</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/2511&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2511 [table2]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#table2</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/2511 [table3]</TD>
            <TD>RV photometry of Draco dwarf spheroidal galaxy (Piatek+, 2002)</TD>
            <TD>This article studies the structure of the Draco dwarf spheroidal galaxy, with an emphasis on the question of whether the spatial distribution of its stars has been affected by the tidal interaction with the Milky Way, using R- and V-band CCD photometry for 11 fields that are located in and around the Draco galaxy. 9 fields are in common with Piatek et al. (J/AJ/121/841); two additional fields, N1 and S1, are adjacent to the central C0 field studied by Piatek et al. in the north and south dire ctions, respectively, and extend beyond the tidal boundary along the minor axis. hese additional fields were imaged with the KPNO 0.9 m telescope using the 2048x2048 T2KA CCD chip. The article reports coordinates for the center, a position angle of the major axis, and the ellipticity. It also reports the results of searches for asymmetries in the structure of Draco. These results and searches for a "break" in the radial profile and for the presence of principal sequences of Draco in a color-magnitude diagram for regions more than 50' from the center yield no evidence that tidal forces from the Milky Way have affected the structure of Draco.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511#table3</TD>
            <TD>2011-09-14T19:20:50Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jun-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/2511</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/2511&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/2511</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/BASI/30. [1]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#1</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/BASI/30.911</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/BASI/30. [2]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#2</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table8]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table8</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table7]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table7</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table9]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table9</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table6]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table6</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/BASI/30. [1]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#1</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/BASI/30.911</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/BASI/30. [2]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#2</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table8]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table8</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table7]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table7</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table9]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table9</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table6]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table6</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/BASI/30. [1]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#1</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/BASI/30.911</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/BASI/30. [2]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#2</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table8]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table8</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table7]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table7</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table9]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table9</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/BASI/30. [table6]</TD>
            <TD>BVRI CCD photometry of 4 galaxy clusters (Sharma+, 2002)</TD>
            <TD>We acquired optical imaging observations at the prime focus of the 2.34-m Vainu Bappu Telescope (VBT), at the Vainu Bappu Observatory (VBO), Kavalur, India. The observatory (longitude 78.8{deg}E, latitude 12.5{deg}N, altitude 730m above sea level) is operated by the Indian Institute of Astrophysics, Bangalore. We employed the following filters in our observations: broad-band blue, visual, red and near infra-red (approximating the standard B, V, R and I photometric bands). We chose to transform our instrumental magnitudes to the standard Johnson-Morgan BV and Kron-Cousins R_c_I_c_ broadband systems using the old Galactic cluster M67 for which many studies are available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911#table6</TD>
            <TD>2011-09-14T19:22:40Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2003</TD>
            <TD>ivo://CDS.VizieR/J/other/BASI/30.911</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/BASI/30.911&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/BASI/30.911</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/29/253 [1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#1</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/29/253</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/29/253 [2]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#2</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [table3]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#table3</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [objects1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#objects1</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [table1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#table1</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [objects3]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#objects3</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/29/253 [1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#1</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/29/253</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/29/253 [2]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#2</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [table3]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#table3</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [objects1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#objects1</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [table1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#table1</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [objects3]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#objects3</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/29/253 [1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#1</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/29/253</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/29/253 [2]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#2</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [table3]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#table3</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [objects1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#objects1</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [table1]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#table1</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/29/253 [objects3]</TD>
            <TD>Globular clusters as gravitational lenses (Bukhmastova, 2003)</TD>
            <TD>We argue that globular clusters (GCs) are good candidates for gravitational lenses in explaining quasar-galaxy associations. The catalog of associations (Bukhmastova, 2001, Cat. &lt;J/AZh/78/675&gt;) compiled from the LEDA catalog of galaxies (Paturel, 1997A&amp;AS..124..109P) and from the catalog of quasars (Veron-Cetty and Vero, 1998, see Cat. &lt;VII/235&gt;) is used. Based on the new catalog, we show that one might expect an increased number of GCs around irregular galaxies of types 9 and 10 from the hypothesis that distant compact sources are gravitationally lensed by GCs in the halos of foreground galaxies. The King model is used to determine the central surface densities of 135 GCs in the Milky Way. The distribution of GCs in central surface density was found to be lognormal.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253#objects3</TD>
            <TD>2011-09-14T19:25:47Z</TD>
            <TD>#Globular_Clusters#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Oct-2003</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/29/253</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/29/253&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/29/253</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/416/839 [1]</TD>
            <TD>Radial velocities of A2219 galaxies (Boschin+, 2004)</TD>
            <TD>Spectroscopic redshifts for 132 galaxies in the central region of the galaxy cluster Abell 2219 are presented. For each galaxy equatorial coordinates, total R magnitude and B-R colour (Harris filters), and velocity are given. Where available, we also give a code for the spectral classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839#1</TD>
            <TD>2011-09-14T19:26:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/416/839</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/839</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/416/839 [2]</TD>
            <TD>Radial velocities of A2219 galaxies (Boschin+, 2004)</TD>
            <TD>Spectroscopic redshifts for 132 galaxies in the central region of the galaxy cluster Abell 2219 are presented. For each galaxy equatorial coordinates, total R magnitude and B-R colour (Harris filters), and velocity are given. Where available, we also give a code for the spectral classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839#2</TD>
            <TD>2011-09-14T19:26:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/416/839&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/839</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/416/839 [table1]</TD>
            <TD>Radial velocities of A2219 galaxies (Boschin+, 2004)</TD>
            <TD>Spectroscopic redshifts for 132 galaxies in the central region of the galaxy cluster Abell 2219 are presented. For each galaxy equatorial coordinates, total R magnitude and B-R colour (Harris filters), and velocity are given. Where available, we also give a code for the spectral classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839#table1</TD>
            <TD>2011-09-14T19:26:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/416/839&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/839</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/600/L99 [1]</TD>
            <TD>Colours of z~6 galaxies in GOODS (Dickinson+, 2004)</TD>
            <TD>We report early results on galaxies at z~6 selected from Hubble Space Telescope imaging for the Great Observatories Origins Deep Survey. Spectroscopy of one object with the Advanced Camera for Surveys grism and from the Keck and Very Large Telescope observatories shows a strong continuum break and asymmetric line emission, identified as Ly{alpha} at z=5.83. We find only five spatially extended candidates with signal-to-noise ratios greater than 10, two of which have spectroscopic confirmation. This is much fewer than would be expected if galaxies at z=6 had the same luminosity function as those at z=3. There are many fainter candidates, but we expect substantial contamination from foreground interlopers and spurious detections. Our best estimates favor a z=6 galaxy population with fainter luminosities, higher space density, and similar comoving ultraviolet emissivity to that at z=3, but this depends critically on counts at fluxes fainter than those reliably probed by the current data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99#1</TD>
            <TD>2011-09-14T19:32:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/600/L99</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/600/L99</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/600/L99 [2]</TD>
            <TD>Colours of z~6 galaxies in GOODS (Dickinson+, 2004)</TD>
            <TD>We report early results on galaxies at z~6 selected from Hubble Space Telescope imaging for the Great Observatories Origins Deep Survey. Spectroscopy of one object with the Advanced Camera for Surveys grism and from the Keck and Very Large Telescope observatories shows a strong continuum break and asymmetric line emission, identified as Ly{alpha} at z=5.83. We find only five spatially extended candidates with signal-to-noise ratios greater than 10, two of which have spectroscopic confirmation. This is much fewer than would be expected if galaxies at z=6 had the same luminosity function as those at z=3. There are many fainter candidates, but we expect substantial contamination from foreground interlopers and spurious detections. Our best estimates favor a z=6 galaxy population with fainter luminosities, higher space density, and similar comoving ultraviolet emissivity to that at z=3, but this depends critically on counts at fluxes fainter than those reliably probed by the current data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99#2</TD>
            <TD>2011-09-14T19:32:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/600/L99&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/600/L99</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/416/839 [1]</TD>
            <TD>Radial velocities of A2219 galaxies (Boschin+, 2004)</TD>
            <TD>Spectroscopic redshifts for 132 galaxies in the central region of the galaxy cluster Abell 2219 are presented. For each galaxy equatorial coordinates, total R magnitude and B-R colour (Harris filters), and velocity are given. Where available, we also give a code for the spectral classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839#1</TD>
            <TD>2011-09-14T19:26:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/416/839</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/839</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/416/839 [2]</TD>
            <TD>Radial velocities of A2219 galaxies (Boschin+, 2004)</TD>
            <TD>Spectroscopic redshifts for 132 galaxies in the central region of the galaxy cluster Abell 2219 are presented. For each galaxy equatorial coordinates, total R magnitude and B-R colour (Harris filters), and velocity are given. Where available, we also give a code for the spectral classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839#2</TD>
            <TD>2011-09-14T19:26:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/416/839&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/839</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/416/839 [table1]</TD>
            <TD>Radial velocities of A2219 galaxies (Boschin+, 2004)</TD>
            <TD>Spectroscopic redshifts for 132 galaxies in the central region of the galaxy cluster Abell 2219 are presented. For each galaxy equatorial coordinates, total R magnitude and B-R colour (Harris filters), and velocity are given. Where available, we also give a code for the spectral classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839#table1</TD>
            <TD>2011-09-14T19:26:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/416/839&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/839</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/416/839 [1]</TD>
            <TD>Radial velocities of A2219 galaxies (Boschin+, 2004)</TD>
            <TD>Spectroscopic redshifts for 132 galaxies in the central region of the galaxy cluster Abell 2219 are presented. For each galaxy equatorial coordinates, total R magnitude and B-R colour (Harris filters), and velocity are given. Where available, we also give a code for the spectral classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839#1</TD>
            <TD>2011-09-14T19:26:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/416/839</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/839</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/416/839 [2]</TD>
            <TD>Radial velocities of A2219 galaxies (Boschin+, 2004)</TD>
            <TD>Spectroscopic redshifts for 132 galaxies in the central region of the galaxy cluster Abell 2219 are presented. For each galaxy equatorial coordinates, total R magnitude and B-R colour (Harris filters), and velocity are given. Where available, we also give a code for the spectral classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839#2</TD>
            <TD>2011-09-14T19:26:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/416/839&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/839</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/416/839 [table1]</TD>
            <TD>Radial velocities of A2219 galaxies (Boschin+, 2004)</TD>
            <TD>Spectroscopic redshifts for 132 galaxies in the central region of the galaxy cluster Abell 2219 are presented. For each galaxy equatorial coordinates, total R magnitude and B-R colour (Harris filters), and velocity are given. Where available, we also give a code for the spectral classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839#table1</TD>
            <TD>2011-09-14T19:26:38Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Dec-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/416/839</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/416/839&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/416/839</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/445 [1]</TD>
            <TD>FCOS Ultra Compact Dwarf galaxies radial vel. (Mieske+, 2004)</TD>
            <TD>The relation between the Ultra Compact Dwarf galaxies (hereafter UCDs) recently discovered in the Fornax cluster (Drinkwater et al., 2003Natur.423..519D; Mieske et al., 2002, Cat. &lt;J/A+A/383/823&gt;) and the brightest globular clusters associated with the central galaxy NGC 1399 has been investigated in the spectroscopic Fornax Compact Object Survey FCOS. FCOS was carried out with the 2.5m du Pont telescope at Las Campanas, in the three nights of 2002/12/04 to 2002/12/06. Mieske et al. (2002, Cat. &lt;J/A+A/383/823&gt;) deals with the first part FCOS-1, this paper deals with the larger FCOS-2. The spectral resolution of FCOS was approx. 4{AA}. In the FCOS, 280 unresolved objects with 0&lt;(V-I)&lt;1.5mag in the magnitude space covering UCDs and bright globular clusters (18&lt;V&lt;21mag) were observed spectroscopically, among them 185 in FCOS-2. In the entire FCOS-sample there are five already known UCDs and 54 new Fornax members, 12 from FCOS-1 and 42 from FCOS-2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445#1</TD>
            <TD>2011-09-14T19:29:17Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/445</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/445</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/445 [2]</TD>
            <TD>FCOS Ultra Compact Dwarf galaxies radial vel. (Mieske+, 2004)</TD>
            <TD>The relation between the Ultra Compact Dwarf galaxies (hereafter UCDs) recently discovered in the Fornax cluster (Drinkwater et al., 2003Natur.423..519D; Mieske et al., 2002, Cat. &lt;J/A+A/383/823&gt;) and the brightest globular clusters associated with the central galaxy NGC 1399 has been investigated in the spectroscopic Fornax Compact Object Survey FCOS. FCOS was carried out with the 2.5m du Pont telescope at Las Campanas, in the three nights of 2002/12/04 to 2002/12/06. Mieske et al. (2002, Cat. &lt;J/A+A/383/823&gt;) deals with the first part FCOS-1, this paper deals with the larger FCOS-2. The spectral resolution of FCOS was approx. 4{AA}. In the FCOS, 280 unresolved objects with 0&lt;(V-I)&lt;1.5mag in the magnitude space covering UCDs and bright globular clusters (18&lt;V&lt;21mag) were observed spectroscopically, among them 185 in FCOS-2. In the entire FCOS-sample there are five already known UCDs and 54 new Fornax members, 12 from FCOS-1 and 42 from FCOS-2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445#2</TD>
            <TD>2011-09-14T19:29:17Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/445&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/445</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/418/445 [fcos2]</TD>
            <TD>FCOS Ultra Compact Dwarf galaxies radial vel. (Mieske+, 2004)</TD>
            <TD>The relation between the Ultra Compact Dwarf galaxies (hereafter UCDs) recently discovered in the Fornax cluster (Drinkwater et al., 2003Natur.423..519D; Mieske et al., 2002, Cat. &lt;J/A+A/383/823&gt;) and the brightest globular clusters associated with the central galaxy NGC 1399 has been investigated in the spectroscopic Fornax Compact Object Survey FCOS. FCOS was carried out with the 2.5m du Pont telescope at Las Campanas, in the three nights of 2002/12/04 to 2002/12/06. Mieske et al. (2002, Cat. &lt;J/A+A/383/823&gt;) deals with the first part FCOS-1, this paper deals with the larger FCOS-2. The spectral resolution of FCOS was approx. 4{AA}. In the FCOS, 280 unresolved objects with 0&lt;(V-I)&lt;1.5mag in the magnitude space covering UCDs and bright globular clusters (18&lt;V&lt;21mag) were observed spectroscopically, among them 185 in FCOS-2. In the entire FCOS-sample there are five already known UCDs and 54 new Fornax members, 12 from FCOS-1 and 42 from FCOS-2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445#fcos2</TD>
            <TD>2011-09-14T19:29:17Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/418/445&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/445</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/130/323 [1]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#1</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/130/323</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/130/323 [2]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#2</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/130/323&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/323 [table3]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#table3</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/130/323 [table2]</TD>
            <TD>ESO Slice Project (Vettolani+ 1998)</TD>
            <TD>The ESO Slice Project (ESP) is a galaxy redshift survey in a region near the South Galactic Pole (see Vettolani et al., 1997A&amp;A...325..954V; Zucca et al., 1997A&amp;A...326..477Z). It extends over a strip 22(RA)x1(DEC) square degrees, plus a nearby area of 5x1 square degrees, 5 degrees west of the main strip. The right ascension limits are 22h30m and 01h20m, at a mean declination of -40{deg}15' (B1950). We have covered this region with a regular grid of adjacent circular fields, with a diameter of 32arcmin each, corresponding to the field of view of the multifiber spectrograph OPTOPUS at the 3.6m ESO telescope. The total solid angle of the spectroscopic survey is 23.2 square degrees. The galaxy catalogue has been extracted from the Edinburgh-Durham Southern Galaxy catalogue (Heydon-Dumbleton et al., 1989MNRAS.238..379H) which has been obtained from COSMOS (MacGillivray &amp; Stobie, 1984VA.....27..433M) scans of SERC J survey plates. The number of objects in the photometric ESP sample is 4487. The spectroscopic survey is about 85% complete to the limiting magnitude bJ=19.4, and consists of 3342 galaxies + 1 QSO with redshift determination. The ESP survey is intermediate between shallow, wide angle samples and very deep, one--dimensional pencil beams. Table 2 lists the fields observed with OPTOPUS and their properties: the numbers listed in this table can be used to compute the redshift completeness of each fields, following eq.(2) of the paper. Table 3 provides the catalogue, with galaxies sorted in right ascension. The catalogue with additional information and updates can also be found at the following URL: http://boas5.bo.astro.it/~cappi/esokp.html</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323#table2</TD>
            <TD>2011-09-14T18:43:42Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/130/323</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/130/323&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/130/323</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/131/221 [1]</TD>
            <TD>Abell 3733 radial velocities (Solanes+ 1998)</TD>
            <TD>Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221#1</TD>
            <TD>2011-09-14T18:44:23Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/131/221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/131/221 [2]</TD>
            <TD>Abell 3733 radial velocities (Solanes+ 1998)</TD>
            <TD>Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221#2</TD>
            <TD>2011-09-14T18:44:23Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/131/221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/131/221 [table1]</TD>
            <TD>Abell 3733 radial velocities (Solanes+ 1998)</TD>
            <TD>Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221#table1</TD>
            <TD>2011-09-14T18:44:23Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/131/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/131/221 [1]</TD>
            <TD>Abell 3733 radial velocities (Solanes+ 1998)</TD>
            <TD>Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221#1</TD>
            <TD>2011-09-14T18:44:23Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/131/221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/131/221 [2]</TD>
            <TD>Abell 3733 radial velocities (Solanes+ 1998)</TD>
            <TD>Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221#2</TD>
            <TD>2011-09-14T18:44:23Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/131/221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/131/221 [table1]</TD>
            <TD>Abell 3733 radial velocities (Solanes+ 1998)</TD>
            <TD>Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221#table1</TD>
            <TD>2011-09-14T18:44:23Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/131/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/131/221 [1]</TD>
            <TD>Abell 3733 radial velocities (Solanes+ 1998)</TD>
            <TD>Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221#1</TD>
            <TD>2011-09-14T18:44:23Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/131/221</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/221</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/131/221 [2]</TD>
            <TD>Abell 3733 radial velocities (Solanes+ 1998)</TD>
            <TD>Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221#2</TD>
            <TD>2011-09-14T18:44:23Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/131/221&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/221</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/131/221 [table1]</TD>
            <TD>Abell 3733 radial velocities (Solanes+ 1998)</TD>
            <TD>Cross-correlation and emission-line heliocentric radial velocities for 112 galaxies observed with the MEFOS and OPTOPUS spectrographs in the field of the galaxy cluster A3733. The last column lists the final radial velocities which result form a weighted average of the velocity data in the previous columns.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221#table1</TD>
            <TD>2011-09-14T18:44:23Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Mar-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/131/221</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/131/221&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/131/221</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/445 [1]</TD>
            <TD>FCOS Ultra Compact Dwarf galaxies radial vel. (Mieske+, 2004)</TD>
            <TD>The relation between the Ultra Compact Dwarf galaxies (hereafter UCDs) recently discovered in the Fornax cluster (Drinkwater et al., 2003Natur.423..519D; Mieske et al., 2002, Cat. &lt;J/A+A/383/823&gt;) and the brightest globular clusters associated with the central galaxy NGC 1399 has been investigated in the spectroscopic Fornax Compact Object Survey FCOS. FCOS was carried out with the 2.5m du Pont telescope at Las Campanas, in the three nights of 2002/12/04 to 2002/12/06. Mieske et al. (2002, Cat. &lt;J/A+A/383/823&gt;) deals with the first part FCOS-1, this paper deals with the larger FCOS-2. The spectral resolution of FCOS was approx. 4{AA}. In the FCOS, 280 unresolved objects with 0&lt;(V-I)&lt;1.5mag in the magnitude space covering UCDs and bright globular clusters (18&lt;V&lt;21mag) were observed spectroscopically, among them 185 in FCOS-2. In the entire FCOS-sample there are five already known UCDs and 54 new Fornax members, 12 from FCOS-1 and 42 from FCOS-2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445#1</TD>
            <TD>2011-09-14T19:29:17Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/445</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/445</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/445 [2]</TD>
            <TD>FCOS Ultra Compact Dwarf galaxies radial vel. (Mieske+, 2004)</TD>
            <TD>The relation between the Ultra Compact Dwarf galaxies (hereafter UCDs) recently discovered in the Fornax cluster (Drinkwater et al., 2003Natur.423..519D; Mieske et al., 2002, Cat. &lt;J/A+A/383/823&gt;) and the brightest globular clusters associated with the central galaxy NGC 1399 has been investigated in the spectroscopic Fornax Compact Object Survey FCOS. FCOS was carried out with the 2.5m du Pont telescope at Las Campanas, in the three nights of 2002/12/04 to 2002/12/06. Mieske et al. (2002, Cat. &lt;J/A+A/383/823&gt;) deals with the first part FCOS-1, this paper deals with the larger FCOS-2. The spectral resolution of FCOS was approx. 4{AA}. In the FCOS, 280 unresolved objects with 0&lt;(V-I)&lt;1.5mag in the magnitude space covering UCDs and bright globular clusters (18&lt;V&lt;21mag) were observed spectroscopically, among them 185 in FCOS-2. In the entire FCOS-sample there are five already known UCDs and 54 new Fornax members, 12 from FCOS-1 and 42 from FCOS-2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445#2</TD>
            <TD>2011-09-14T19:29:17Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/445&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/445</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/418/445 [fcos2]</TD>
            <TD>FCOS Ultra Compact Dwarf galaxies radial vel. (Mieske+, 2004)</TD>
            <TD>The relation between the Ultra Compact Dwarf galaxies (hereafter UCDs) recently discovered in the Fornax cluster (Drinkwater et al., 2003Natur.423..519D; Mieske et al., 2002, Cat. &lt;J/A+A/383/823&gt;) and the brightest globular clusters associated with the central galaxy NGC 1399 has been investigated in the spectroscopic Fornax Compact Object Survey FCOS. FCOS was carried out with the 2.5m du Pont telescope at Las Campanas, in the three nights of 2002/12/04 to 2002/12/06. Mieske et al. (2002, Cat. &lt;J/A+A/383/823&gt;) deals with the first part FCOS-1, this paper deals with the larger FCOS-2. The spectral resolution of FCOS was approx. 4{AA}. In the FCOS, 280 unresolved objects with 0&lt;(V-I)&lt;1.5mag in the magnitude space covering UCDs and bright globular clusters (18&lt;V&lt;21mag) were observed spectroscopically, among them 185 in FCOS-2. In the entire FCOS-sample there are five already known UCDs and 54 new Fornax members, 12 from FCOS-1 and 42 from FCOS-2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445#fcos2</TD>
            <TD>2011-09-14T19:29:17Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/418/445&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/445</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/114/122 [1]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#1</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/114/122</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/114/122 [2]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#2</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/114/122&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/122 [table2]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#table2</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/122&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/122 [table1]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#table1</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/122&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/114/122 [1]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#1</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/114/122</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/114/122 [2]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#2</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/114/122&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/122 [table2]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#table2</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/122&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/122 [table1]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#table1</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/122&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/418/445 [1]</TD>
            <TD>FCOS Ultra Compact Dwarf galaxies radial vel. (Mieske+, 2004)</TD>
            <TD>The relation between the Ultra Compact Dwarf galaxies (hereafter UCDs) recently discovered in the Fornax cluster (Drinkwater et al., 2003Natur.423..519D; Mieske et al., 2002, Cat. &lt;J/A+A/383/823&gt;) and the brightest globular clusters associated with the central galaxy NGC 1399 has been investigated in the spectroscopic Fornax Compact Object Survey FCOS. FCOS was carried out with the 2.5m du Pont telescope at Las Campanas, in the three nights of 2002/12/04 to 2002/12/06. Mieske et al. (2002, Cat. &lt;J/A+A/383/823&gt;) deals with the first part FCOS-1, this paper deals with the larger FCOS-2. The spectral resolution of FCOS was approx. 4{AA}. In the FCOS, 280 unresolved objects with 0&lt;(V-I)&lt;1.5mag in the magnitude space covering UCDs and bright globular clusters (18&lt;V&lt;21mag) were observed spectroscopically, among them 185 in FCOS-2. In the entire FCOS-sample there are five already known UCDs and 54 new Fornax members, 12 from FCOS-1 and 42 from FCOS-2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445#1</TD>
            <TD>2011-09-14T19:29:17Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/418/445</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/445</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/418/445 [2]</TD>
            <TD>FCOS Ultra Compact Dwarf galaxies radial vel. (Mieske+, 2004)</TD>
            <TD>The relation between the Ultra Compact Dwarf galaxies (hereafter UCDs) recently discovered in the Fornax cluster (Drinkwater et al., 2003Natur.423..519D; Mieske et al., 2002, Cat. &lt;J/A+A/383/823&gt;) and the brightest globular clusters associated with the central galaxy NGC 1399 has been investigated in the spectroscopic Fornax Compact Object Survey FCOS. FCOS was carried out with the 2.5m du Pont telescope at Las Campanas, in the three nights of 2002/12/04 to 2002/12/06. Mieske et al. (2002, Cat. &lt;J/A+A/383/823&gt;) deals with the first part FCOS-1, this paper deals with the larger FCOS-2. The spectral resolution of FCOS was approx. 4{AA}. In the FCOS, 280 unresolved objects with 0&lt;(V-I)&lt;1.5mag in the magnitude space covering UCDs and bright globular clusters (18&lt;V&lt;21mag) were observed spectroscopically, among them 185 in FCOS-2. In the entire FCOS-sample there are five already known UCDs and 54 new Fornax members, 12 from FCOS-1 and 42 from FCOS-2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445#2</TD>
            <TD>2011-09-14T19:29:17Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/418/445&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/445</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/418/445 [fcos2]</TD>
            <TD>FCOS Ultra Compact Dwarf galaxies radial vel. (Mieske+, 2004)</TD>
            <TD>The relation between the Ultra Compact Dwarf galaxies (hereafter UCDs) recently discovered in the Fornax cluster (Drinkwater et al., 2003Natur.423..519D; Mieske et al., 2002, Cat. &lt;J/A+A/383/823&gt;) and the brightest globular clusters associated with the central galaxy NGC 1399 has been investigated in the spectroscopic Fornax Compact Object Survey FCOS. FCOS was carried out with the 2.5m du Pont telescope at Las Campanas, in the three nights of 2002/12/04 to 2002/12/06. Mieske et al. (2002, Cat. &lt;J/A+A/383/823&gt;) deals with the first part FCOS-1, this paper deals with the larger FCOS-2. The spectral resolution of FCOS was approx. 4{AA}. In the FCOS, 280 unresolved objects with 0&lt;(V-I)&lt;1.5mag in the magnitude space covering UCDs and bright globular clusters (18&lt;V&lt;21mag) were observed spectroscopically, among them 185 in FCOS-2. In the entire FCOS-sample there are five already known UCDs and 54 new Fornax members, 12 from FCOS-1 and 42 from FCOS-2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445#fcos2</TD>
            <TD>2011-09-14T19:29:17Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Jun-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/418/445</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/418/445&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/418/445</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/114/122 [1]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#1</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/114/122</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/114/122 [2]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#2</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/114/122&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/122 [table2]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#table2</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/122&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/114/122 [table1]</TD>
            <TD>Spectroscopy of edge-on spirals (Giovanelli+ 1997)</TD>
            <TD>We present H I line observations of 744 edge-on spiral galaxies, extracted from the Flat Galaxy Catalog of Karachentsev et al. (1993AN....314...97K). Fluxes, systemic velocities and line widths are given for 587 detected galaxies, as well as search parameters for 157 undetected systems. Widths are corrected for instrumental broadening, smoothing, signal-to-noise and profile shape, and an estimate of the error on the width is given. When corrected for turbulent broadening and inclination angle of the disks, the velocity widths presented here can provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122#table1</TD>
            <TD>2011-09-14T18:44:40Z</TD>
            <TD>#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/114/122</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/114/122&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/114/122</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/109/45 [1]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#1</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/109/45</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/109/45 [2]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#2</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/109/45&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/109/45 [table6]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#table6</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/109/45&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/109/45 [table5]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#table5</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/109/45&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/109/45 [1]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#1</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/109/45</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/109/45 [2]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#2</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/109/45&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/109/45 [table6]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#table6</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/109/45&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/109/45 [table5]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#table5</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/109/45&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/421/539 [1]</TD>
            <TD>VLT spectroscopy of Tol 1214-277 &amp; Tol 65 (Izotov+, 2004)</TD>
            <TD>We present VLT spectroscopic observations with different spectral resolutions and different slit orientations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. The oxygen abundances in the brightest HII regions of Tol 1214-277 and Tol 65 are found to be 12+logO/H=7.55+/-0.01 and 7.54+/-0.01, or Z_{sun}_/24. The nitrogen-to-oxygen abundance ratios in the two galaxies are logN/O=-1.64+/-0.03 and -1.60+/-0.02 and lie in the narrow range found for other most metal-deficient BCDs. The helium mass fraction derived in several HII regions in both galaxies is consistent with a high primordial helium mass fraction, Yp~0.244. We confirm the detection of the high-ionization forbidden emission line [FeV]4227 in the spectrum of Tol 1214-277. Additionally, weak [NeIV]4725, [FeVI]5146,5177, and [FeVII]5721,6087 emission lines are detected in the high-resolution spectrum of Tol 1214-277. The detection of these lines implies the presence of hard radiation with photon energy in the range ~4-8Ryd. Emission lines are detected in the spectra of eight galaxies in the fields of Tol 1214-277 and Tol 65. Seven of these galaxies are background objects, while one galaxy has a redshift close to that of Tol 1214-277. Situated at a projected distance of ~14.5kpc from Tol 1214-277, this galaxy is probably a companion of the BCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539#1</TD>
            <TD>2011-09-14T19:29:29Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/421/539</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/539</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/421/539 [2]</TD>
            <TD>VLT spectroscopy of Tol 1214-277 &amp; Tol 65 (Izotov+, 2004)</TD>
            <TD>We present VLT spectroscopic observations with different spectral resolutions and different slit orientations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. The oxygen abundances in the brightest HII regions of Tol 1214-277 and Tol 65 are found to be 12+logO/H=7.55+/-0.01 and 7.54+/-0.01, or Z_{sun}_/24. The nitrogen-to-oxygen abundance ratios in the two galaxies are logN/O=-1.64+/-0.03 and -1.60+/-0.02 and lie in the narrow range found for other most metal-deficient BCDs. The helium mass fraction derived in several HII regions in both galaxies is consistent with a high primordial helium mass fraction, Yp~0.244. We confirm the detection of the high-ionization forbidden emission line [FeV]4227 in the spectrum of Tol 1214-277. Additionally, weak [NeIV]4725, [FeVI]5146,5177, and [FeVII]5721,6087 emission lines are detected in the high-resolution spectrum of Tol 1214-277. The detection of these lines implies the presence of hard radiation with photon energy in the range ~4-8Ryd. Emission lines are detected in the spectra of eight galaxies in the fields of Tol 1214-277 and Tol 65. Seven of these galaxies are background objects, while one galaxy has a redshift close to that of Tol 1214-277. Situated at a projected distance of ~14.5kpc from Tol 1214-277, this galaxy is probably a companion of the BCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539#2</TD>
            <TD>2011-09-14T19:29:29Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/421/539&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/539</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/421/539 [table7]</TD>
            <TD>VLT spectroscopy of Tol 1214-277 &amp; Tol 65 (Izotov+, 2004)</TD>
            <TD>We present VLT spectroscopic observations with different spectral resolutions and different slit orientations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. The oxygen abundances in the brightest HII regions of Tol 1214-277 and Tol 65 are found to be 12+logO/H=7.55+/-0.01 and 7.54+/-0.01, or Z_{sun}_/24. The nitrogen-to-oxygen abundance ratios in the two galaxies are logN/O=-1.64+/-0.03 and -1.60+/-0.02 and lie in the narrow range found for other most metal-deficient BCDs. The helium mass fraction derived in several HII regions in both galaxies is consistent with a high primordial helium mass fraction, Yp~0.244. We confirm the detection of the high-ionization forbidden emission line [FeV]4227 in the spectrum of Tol 1214-277. Additionally, weak [NeIV]4725, [FeVI]5146,5177, and [FeVII]5721,6087 emission lines are detected in the high-resolution spectrum of Tol 1214-277. The detection of these lines implies the presence of hard radiation with photon energy in the range ~4-8Ryd. Emission lines are detected in the spectra of eight galaxies in the fields of Tol 1214-277 and Tol 65. Seven of these galaxies are background objects, while one galaxy has a redshift close to that of Tol 1214-277. Situated at a projected distance of ~14.5kpc from Tol 1214-277, this galaxy is probably a companion of the BCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539#table7</TD>
            <TD>2011-09-14T19:29:29Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/421/539&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/539</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/109/45 [1]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#1</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/109/45</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/109/45 [2]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#2</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/109/45&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/109/45 [table6]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#table6</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/109/45&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/109/45 [table5]</TD>
            <TD>Kitt Peak galaxy redshift survey (Munn+ 1997)</TD>
            <TD>Redshifts, four-band photometry (U B_J_ R_F_ I_N_), and astrometry are presented for faint galaxies in four widely separated fields. We provide the necessary information to enable well-defined, statistically complete subsamples of faint galaxies to be constructed from the master catalog. The redshift survey is 86% and 71% complete to R_F_&lt;=18.5 and R_F&lt;=19, respectively, yielding 328 galaxies with reliable redshifts to R_F_&lt;=19, with a median redshift of 0.142. Adding the galaxies from the fainter statistical sample yields a total of 583 reliable redshifts with a median redshift of 0.202. An additional 156 redshifts in the same fields, but not part of the samples defined here, are also given. Of the 739 galaxy redshifts presented, 212 are for galaxies with R_F_&gt;20.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45#table5</TD>
            <TD>2011-09-14T18:44:53Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/109/45</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/109/45&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/109/45</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/2500 [1]</TD>
            <TD>JHK' photometry of 4 clusters of galaxies (McLean+ 1996)</TD>
            <TD>Deep near-infrared images of four intermediate redshift (z=0.2-0.4) clusters (Abell 370, Abell 963, CL 0024+1654 and CL 0909+4408) have been obtained in the J, H, and K bands using the UCLA Two-Channel IR Camera with a spatial resolution of ~1". The 3'x3' field of view includes over 100 galaxies in each cluster. Photometry has been obtained with 1{sigma} or limiting magnitudes of 21.7 at J, 21.0 at H, and 20.4 at K', and complete to 2 magnitudes fainter than L^*^. Data reduction techniques for flat-fielding object identification, and photometry of faint object crowded fields are discussed. The best method is the subtraction of a running-average sky made from object frames. The photometry is cross referenced to previous catalogs, and infrared color-magnitude diagrams are presented. Comparison of the IR colors of these four clusters to the predictions of the spectral synthesis models of Bruzual and Chariot is discussed. There is a discrepancy between the models and the observations of several tenths of a magnitude in the colors. Photometry has also been obtained for the gravitational lensing arcs in CL 0024+1654, which is consistent with an actively star-forming galaxy at z&gt;1. For a description of the JHK' photometric system, see e.g. &lt;GCPD/09&gt;</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2500#1</TD>
            <TD>2011-09-14T18:45:09Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2500</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/2500</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/2500</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/2500 [2]</TD>
            <TD>JHK' photometry of 4 clusters of galaxies (McLean+ 1996)</TD>
            <TD>Deep near-infrared images of four intermediate redshift (z=0.2-0.4) clusters (Abell 370, Abell 963, CL 0024+1654 and CL 0909+4408) have been obtained in the J, H, and K bands using the UCLA Two-Channel IR Camera with a spatial resolution of ~1". The 3'x3' field of view includes over 100 galaxies in each cluster. Photometry has been obtained with 1{sigma} or limiting magnitudes of 21.7 at J, 21.0 at H, and 20.4 at K', and complete to 2 magnitudes fainter than L^*^. Data reduction techniques for flat-fielding object identification, and photometry of faint object crowded fields are discussed. The best method is the subtraction of a running-average sky made from object frames. The photometry is cross referenced to previous catalogs, and infrared color-magnitude diagrams are presented. Comparison of the IR colors of these four clusters to the predictions of the spectral synthesis models of Bruzual and Chariot is discussed. There is a discrepancy between the models and the observations of several tenths of a magnitude in the colors. Photometry has also been obtained for the gravitational lensing arcs in CL 0024+1654, which is consistent with an actively star-forming galaxy at z&gt;1. For a description of the JHK' photometric system, see e.g. &lt;GCPD/09&gt;</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2500#2</TD>
            <TD>2011-09-14T18:45:09Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2500</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/2500&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/2500</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/112/2500 [1]</TD>
            <TD>JHK' photometry of 4 clusters of galaxies (McLean+ 1996)</TD>
            <TD>Deep near-infrared images of four intermediate redshift (z=0.2-0.4) clusters (Abell 370, Abell 963, CL 0024+1654 and CL 0909+4408) have been obtained in the J, H, and K bands using the UCLA Two-Channel IR Camera with a spatial resolution of ~1". The 3'x3' field of view includes over 100 galaxies in each cluster. Photometry has been obtained with 1{sigma} or limiting magnitudes of 21.7 at J, 21.0 at H, and 20.4 at K', and complete to 2 magnitudes fainter than L^*^. Data reduction techniques for flat-fielding object identification, and photometry of faint object crowded fields are discussed. The best method is the subtraction of a running-average sky made from object frames. The photometry is cross referenced to previous catalogs, and infrared color-magnitude diagrams are presented. Comparison of the IR colors of these four clusters to the predictions of the spectral synthesis models of Bruzual and Chariot is discussed. There is a discrepancy between the models and the observations of several tenths of a magnitude in the colors. Photometry has also been obtained for the gravitational lensing arcs in CL 0024+1654, which is consistent with an actively star-forming galaxy at z&gt;1. For a description of the JHK' photometric system, see e.g. &lt;GCPD/09&gt;</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2500#1</TD>
            <TD>2011-09-14T18:45:09Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2500</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/112/2500</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/2500</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/112/2500 [2]</TD>
            <TD>JHK' photometry of 4 clusters of galaxies (McLean+ 1996)</TD>
            <TD>Deep near-infrared images of four intermediate redshift (z=0.2-0.4) clusters (Abell 370, Abell 963, CL 0024+1654 and CL 0909+4408) have been obtained in the J, H, and K bands using the UCLA Two-Channel IR Camera with a spatial resolution of ~1". The 3'x3' field of view includes over 100 galaxies in each cluster. Photometry has been obtained with 1{sigma} or limiting magnitudes of 21.7 at J, 21.0 at H, and 20.4 at K', and complete to 2 magnitudes fainter than L^*^. Data reduction techniques for flat-fielding object identification, and photometry of faint object crowded fields are discussed. The best method is the subtraction of a running-average sky made from object frames. The photometry is cross referenced to previous catalogs, and infrared color-magnitude diagrams are presented. Comparison of the IR colors of these four clusters to the predictions of the spectral synthesis models of Bruzual and Chariot is discussed. There is a discrepancy between the models and the observations of several tenths of a magnitude in the colors. Photometry has also been obtained for the gravitational lensing arcs in CL 0024+1654, which is consistent with an actively star-forming galaxy at z&gt;1. For a description of the JHK' photometric system, see e.g. &lt;GCPD/09&gt;</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2500#2</TD>
            <TD>2011-09-14T18:45:09Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1997</TD>
            <TD>ivo://CDS.VizieR/J/AJ/112/2500</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/112/2500&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/112/2500</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/421/539 [1]</TD>
            <TD>VLT spectroscopy of Tol 1214-277 &amp; Tol 65 (Izotov+, 2004)</TD>
            <TD>We present VLT spectroscopic observations with different spectral resolutions and different slit orientations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. The oxygen abundances in the brightest HII regions of Tol 1214-277 and Tol 65 are found to be 12+logO/H=7.55+/-0.01 and 7.54+/-0.01, or Z_{sun}_/24. The nitrogen-to-oxygen abundance ratios in the two galaxies are logN/O=-1.64+/-0.03 and -1.60+/-0.02 and lie in the narrow range found for other most metal-deficient BCDs. The helium mass fraction derived in several HII regions in both galaxies is consistent with a high primordial helium mass fraction, Yp~0.244. We confirm the detection of the high-ionization forbidden emission line [FeV]4227 in the spectrum of Tol 1214-277. Additionally, weak [NeIV]4725, [FeVI]5146,5177, and [FeVII]5721,6087 emission lines are detected in the high-resolution spectrum of Tol 1214-277. The detection of these lines implies the presence of hard radiation with photon energy in the range ~4-8Ryd. Emission lines are detected in the spectra of eight galaxies in the fields of Tol 1214-277 and Tol 65. Seven of these galaxies are background objects, while one galaxy has a redshift close to that of Tol 1214-277. Situated at a projected distance of ~14.5kpc from Tol 1214-277, this galaxy is probably a companion of the BCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539#1</TD>
            <TD>2011-09-14T19:29:29Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/421/539</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/539</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/421/539 [2]</TD>
            <TD>VLT spectroscopy of Tol 1214-277 &amp; Tol 65 (Izotov+, 2004)</TD>
            <TD>We present VLT spectroscopic observations with different spectral resolutions and different slit orientations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. The oxygen abundances in the brightest HII regions of Tol 1214-277 and Tol 65 are found to be 12+logO/H=7.55+/-0.01 and 7.54+/-0.01, or Z_{sun}_/24. The nitrogen-to-oxygen abundance ratios in the two galaxies are logN/O=-1.64+/-0.03 and -1.60+/-0.02 and lie in the narrow range found for other most metal-deficient BCDs. The helium mass fraction derived in several HII regions in both galaxies is consistent with a high primordial helium mass fraction, Yp~0.244. We confirm the detection of the high-ionization forbidden emission line [FeV]4227 in the spectrum of Tol 1214-277. Additionally, weak [NeIV]4725, [FeVI]5146,5177, and [FeVII]5721,6087 emission lines are detected in the high-resolution spectrum of Tol 1214-277. The detection of these lines implies the presence of hard radiation with photon energy in the range ~4-8Ryd. Emission lines are detected in the spectra of eight galaxies in the fields of Tol 1214-277 and Tol 65. Seven of these galaxies are background objects, while one galaxy has a redshift close to that of Tol 1214-277. Situated at a projected distance of ~14.5kpc from Tol 1214-277, this galaxy is probably a companion of the BCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539#2</TD>
            <TD>2011-09-14T19:29:29Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/421/539&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/539</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/421/539 [table7]</TD>
            <TD>VLT spectroscopy of Tol 1214-277 &amp; Tol 65 (Izotov+, 2004)</TD>
            <TD>We present VLT spectroscopic observations with different spectral resolutions and different slit orientations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. The oxygen abundances in the brightest HII regions of Tol 1214-277 and Tol 65 are found to be 12+logO/H=7.55+/-0.01 and 7.54+/-0.01, or Z_{sun}_/24. The nitrogen-to-oxygen abundance ratios in the two galaxies are logN/O=-1.64+/-0.03 and -1.60+/-0.02 and lie in the narrow range found for other most metal-deficient BCDs. The helium mass fraction derived in several HII regions in both galaxies is consistent with a high primordial helium mass fraction, Yp~0.244. We confirm the detection of the high-ionization forbidden emission line [FeV]4227 in the spectrum of Tol 1214-277. Additionally, weak [NeIV]4725, [FeVI]5146,5177, and [FeVII]5721,6087 emission lines are detected in the high-resolution spectrum of Tol 1214-277. The detection of these lines implies the presence of hard radiation with photon energy in the range ~4-8Ryd. Emission lines are detected in the spectra of eight galaxies in the fields of Tol 1214-277 and Tol 65. Seven of these galaxies are background objects, while one galaxy has a redshift close to that of Tol 1214-277. Situated at a projected distance of ~14.5kpc from Tol 1214-277, this galaxy is probably a companion of the BCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539#table7</TD>
            <TD>2011-09-14T19:29:29Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/421/539&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/539</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/274/1071 [1]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#1</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/274/1071</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/274/1071 [2]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#2</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table4]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table4</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table3]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table3</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table5]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table5</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table2]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table2</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/274/1071 [1]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#1</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/274/1071</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/274/1071 [2]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#2</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table4]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table4</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table3]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table3</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table5]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table5</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table2]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table2</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/421/539 [1]</TD>
            <TD>VLT spectroscopy of Tol 1214-277 &amp; Tol 65 (Izotov+, 2004)</TD>
            <TD>We present VLT spectroscopic observations with different spectral resolutions and different slit orientations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. The oxygen abundances in the brightest HII regions of Tol 1214-277 and Tol 65 are found to be 12+logO/H=7.55+/-0.01 and 7.54+/-0.01, or Z_{sun}_/24. The nitrogen-to-oxygen abundance ratios in the two galaxies are logN/O=-1.64+/-0.03 and -1.60+/-0.02 and lie in the narrow range found for other most metal-deficient BCDs. The helium mass fraction derived in several HII regions in both galaxies is consistent with a high primordial helium mass fraction, Yp~0.244. We confirm the detection of the high-ionization forbidden emission line [FeV]4227 in the spectrum of Tol 1214-277. Additionally, weak [NeIV]4725, [FeVI]5146,5177, and [FeVII]5721,6087 emission lines are detected in the high-resolution spectrum of Tol 1214-277. The detection of these lines implies the presence of hard radiation with photon energy in the range ~4-8Ryd. Emission lines are detected in the spectra of eight galaxies in the fields of Tol 1214-277 and Tol 65. Seven of these galaxies are background objects, while one galaxy has a redshift close to that of Tol 1214-277. Situated at a projected distance of ~14.5kpc from Tol 1214-277, this galaxy is probably a companion of the BCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539#1</TD>
            <TD>2011-09-14T19:29:29Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/421/539</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/539</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/421/539 [2]</TD>
            <TD>VLT spectroscopy of Tol 1214-277 &amp; Tol 65 (Izotov+, 2004)</TD>
            <TD>We present VLT spectroscopic observations with different spectral resolutions and different slit orientations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. The oxygen abundances in the brightest HII regions of Tol 1214-277 and Tol 65 are found to be 12+logO/H=7.55+/-0.01 and 7.54+/-0.01, or Z_{sun}_/24. The nitrogen-to-oxygen abundance ratios in the two galaxies are logN/O=-1.64+/-0.03 and -1.60+/-0.02 and lie in the narrow range found for other most metal-deficient BCDs. The helium mass fraction derived in several HII regions in both galaxies is consistent with a high primordial helium mass fraction, Yp~0.244. We confirm the detection of the high-ionization forbidden emission line [FeV]4227 in the spectrum of Tol 1214-277. Additionally, weak [NeIV]4725, [FeVI]5146,5177, and [FeVII]5721,6087 emission lines are detected in the high-resolution spectrum of Tol 1214-277. The detection of these lines implies the presence of hard radiation with photon energy in the range ~4-8Ryd. Emission lines are detected in the spectra of eight galaxies in the fields of Tol 1214-277 and Tol 65. Seven of these galaxies are background objects, while one galaxy has a redshift close to that of Tol 1214-277. Situated at a projected distance of ~14.5kpc from Tol 1214-277, this galaxy is probably a companion of the BCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539#2</TD>
            <TD>2011-09-14T19:29:29Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/421/539&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/539</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/421/539 [table7]</TD>
            <TD>VLT spectroscopy of Tol 1214-277 &amp; Tol 65 (Izotov+, 2004)</TD>
            <TD>We present VLT spectroscopic observations with different spectral resolutions and different slit orientations of the two metal-deficient blue compact dwarf (BCD) galaxies Tol 1214-277 and Tol 65. The oxygen abundances in the brightest HII regions of Tol 1214-277 and Tol 65 are found to be 12+logO/H=7.55+/-0.01 and 7.54+/-0.01, or Z_{sun}_/24. The nitrogen-to-oxygen abundance ratios in the two galaxies are logN/O=-1.64+/-0.03 and -1.60+/-0.02 and lie in the narrow range found for other most metal-deficient BCDs. The helium mass fraction derived in several HII regions in both galaxies is consistent with a high primordial helium mass fraction, Yp~0.244. We confirm the detection of the high-ionization forbidden emission line [FeV]4227 in the spectrum of Tol 1214-277. Additionally, weak [NeIV]4725, [FeVI]5146,5177, and [FeVII]5721,6087 emission lines are detected in the high-resolution spectrum of Tol 1214-277. The detection of these lines implies the presence of hard radiation with photon energy in the range ~4-8Ryd. Emission lines are detected in the spectra of eight galaxies in the fields of Tol 1214-277 and Tol 65. Seven of these galaxies are background objects, while one galaxy has a redshift close to that of Tol 1214-277. Situated at a projected distance of ~14.5kpc from Tol 1214-277, this galaxy is probably a companion of the BCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539#table7</TD>
            <TD>2011-09-14T19:29:29Z</TD>
            <TD>#Equivalent_widths#Galaxies:spectra#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/539</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/421/539&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/539</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/274/1071 [1]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#1</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/274/1071</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/274/1071 [2]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#2</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table4]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table4</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table3]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table3</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table5]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table5</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/274/1071 [table2]</TD>
            <TD>Edinburgh-Milano cluster redshift survey (Collins+ 1995)</TD>
            <TD>In this paper, we present the redshifts of the galaxies and galaxy clusters which form the Edinburgh-Milano (EM) cluster redshift survey. A total of 777 galaxy redshifts have been measured in 94 clusters extracted from the digitized Edinburgh-Durham Cluster Catalogue. We also present the radial velocity dispersions for 37 clusters. Observational and data reduction techniques are discussed in detail, together with the strategy adopted to determine the mean redshift of a cluster and to identify and discard plausible phantom clusters. Some 10 per cent of our clusters show heavy contamination, indicating that projection is a serious problem for optically selected, rich clusters. The median velocity dispersion estimated for a subsample of richness R&gt;=1 clusters is 742+/-63km/s. From a simple comparison with {OMEGA}=1 cold dark matter models of structure formation, these results favour a biasing parameter b=1.6-2.0 and are inconsistent with a bias outside of the range b=1.3-2.5.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071#table2</TD>
            <TD>2011-09-14T18:45:40Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Feb-1997</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/274/1071</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/274/1071&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/274/1071</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/586/814 [1]</TD>
            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814#1</TD>
            <TD>2011-09-14T19:30:05Z</TD>
            <TD>#Globular_Clusters#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/586/814</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/586/814</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/586/814 [2]</TD>
            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814#2</TD>
            <TD>2011-09-14T19:30:05Z</TD>
            <TD>#Globular_Clusters#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/586/814&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/586/814</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/586/814 [table2]</TD>
            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814#table2</TD>
            <TD>2011-09-14T19:30:05Z</TD>
            <TD>#Globular_Clusters#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/586/814&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/586/814</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/586/814 [table1]</TD>
            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814#table1</TD>
            <TD>2011-09-14T19:30:05Z</TD>
            <TD>#Globular_Clusters#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/586/814&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/586/814</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/586/814 [table3]</TD>
            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814#table3</TD>
            <TD>2011-09-14T19:30:05Z</TD>
            <TD>#Globular_Clusters#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/586/814&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/586/814</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/405/94 [1]</TD>
            <TD>Far-infrared emission from 5 galaxy clusters (Wise+ 1993)</TD>
            <TD>We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.</TD>
            <TD>CDS</TD>
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            <TD>J/ApJ/405/94 [2]</TD>
            <TD>Far-infrared emission from 5 galaxy clusters (Wise+ 1993)</TD>
            <TD>We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.</TD>
            <TD>CDS</TD>
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            <TD>J/ApJ/405/94 [table3]</TD>
            <TD>Far-infrared emission from 5 galaxy clusters (Wise+ 1993)</TD>
            <TD>We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.</TD>
            <TD>CDS</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJ/586/814 [1]</TD>
            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/ApJ/586/814</TD>
            <TD />
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/586/814</TD>
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            <TD>HTTP Request</TD>
            <TD>J/ApJ/586/814 [2]</TD>
            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
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            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
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            <TD>ParamHTTP</TD>
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            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
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            <TD>#X-ray#Optical#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>ParamHTTP</TD>
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            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJ/586/814 [1]</TD>
            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
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            <TD />
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            <TD />
            <TD>WebBrowser</TD>
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            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
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            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
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            <TD>ivo://CDS.VizieR/J/ApJ/586/814</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJ/586/814 [table3]</TD>
            <TD>NGC 4472 Chandra/HST study (Maccarone+, 2003)</TD>
            <TD>We present the results of a Chandra/Hubble Space Telescope (HST) study of the point sources of the Virgo Cluster giant elliptical galaxy NGC 4472. We identify 144 X-ray point sources outside the nuclear region, 72 of which are located within the HST fields. The optical data show 1102 sources, of which 829 have colors consistent with being globular clusters (with only four in the restricted central 10" region). Thirty matches are found between the two lists - these are likely to be low-mass X-ray binaries (LMXBs) associated with globular clusters, while ~42 of the X-ray sources have no optical counterparts to V&lt;~25 and I&lt;~24, indicating that they are likely to be predominantly LMXBs in the field star population with a small amount of possible contamination from background active galactic nuclei. Thus approximately 40% of the X-ray sources are in globular clusters and 4% of the globular clusters contain X-ray sources.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814#table3</TD>
            <TD>2011-09-14T19:30:05Z</TD>
            <TD>#Globular_Clusters#Stars#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-May-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/586/814</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/586/814&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/586/814</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/2840 [1]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#1</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/2840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/2840 [2]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#2</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/2840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/126/2840 [table6]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#table6</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/126/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/126/2840 [table3]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#table3</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/126/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/2840 [1]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#1</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/2840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/2840 [2]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#2</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/2840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/126/2840 [table6]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#table6</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/126/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/126/2840 [table3]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#table3</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/126/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/2840 [1]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#1</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/2840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/2840 [2]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#2</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/2840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/126/2840 [table6]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#table6</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/126/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/126/2840 [table3]</TD>
            <TD>BVI CCD photometry of Sextans dSph galaxy (Lee+, 2003)</TD>
            <TD>BVI CCD images of the Sextans dSph were obtained at the 3.6m Canada-France-Hawaii Telescope (CFHT) on the nights of UT 2001 February 16-17 using the CFH12K mosaic CCD camera.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840#table3</TD>
            <TD>2011-09-14T19:31:10Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/126/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/2840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/417/499 [1]</TD>
            <TD>Spectrophotometry of Virgo cluster galaxies (Gavazzi+, 2004)</TD>
            <TD>Long-slit spectra of 333 galaxies, obtained during approximately 50 nights distributed in 6 years (1998-2003) using the 1.93m telescope of the Observatoire de Haute Provence (OHP), the ESO 3.6m telescope, the Loiano 1.52m telescope and the San Pedro Martir (SPM) 2.1m telescope are presented. The observations were taken in the "drift-scan" mode, i.e. with the slit, generally parallel to the galaxy major axis, drifting over the optical surface of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499#1</TD>
            <TD>2011-09-14T19:31:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/417/499</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/417/499</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/417/499 [2]</TD>
            <TD>Spectrophotometry of Virgo cluster galaxies (Gavazzi+, 2004)</TD>
            <TD>Long-slit spectra of 333 galaxies, obtained during approximately 50 nights distributed in 6 years (1998-2003) using the 1.93m telescope of the Observatoire de Haute Provence (OHP), the ESO 3.6m telescope, the Loiano 1.52m telescope and the San Pedro Martir (SPM) 2.1m telescope are presented. The observations were taken in the "drift-scan" mode, i.e. with the slit, generally parallel to the galaxy major axis, drifting over the optical surface of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499#2</TD>
            <TD>2011-09-14T19:31:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/417/499&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/417/499</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/417/499 [table6]</TD>
            <TD>Spectrophotometry of Virgo cluster galaxies (Gavazzi+, 2004)</TD>
            <TD>Long-slit spectra of 333 galaxies, obtained during approximately 50 nights distributed in 6 years (1998-2003) using the 1.93m telescope of the Observatoire de Haute Provence (OHP), the ESO 3.6m telescope, the Loiano 1.52m telescope and the San Pedro Martir (SPM) 2.1m telescope are presented. The observations were taken in the "drift-scan" mode, i.e. with the slit, generally parallel to the galaxy major axis, drifting over the optical surface of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499#table6</TD>
            <TD>2011-09-14T19:31:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/417/499&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/417/499</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/417/499 [1]</TD>
            <TD>Spectrophotometry of Virgo cluster galaxies (Gavazzi+, 2004)</TD>
            <TD>Long-slit spectra of 333 galaxies, obtained during approximately 50 nights distributed in 6 years (1998-2003) using the 1.93m telescope of the Observatoire de Haute Provence (OHP), the ESO 3.6m telescope, the Loiano 1.52m telescope and the San Pedro Martir (SPM) 2.1m telescope are presented. The observations were taken in the "drift-scan" mode, i.e. with the slit, generally parallel to the galaxy major axis, drifting over the optical surface of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499#1</TD>
            <TD>2011-09-14T19:31:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/417/499</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/417/499</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/417/499 [2]</TD>
            <TD>Spectrophotometry of Virgo cluster galaxies (Gavazzi+, 2004)</TD>
            <TD>Long-slit spectra of 333 galaxies, obtained during approximately 50 nights distributed in 6 years (1998-2003) using the 1.93m telescope of the Observatoire de Haute Provence (OHP), the ESO 3.6m telescope, the Loiano 1.52m telescope and the San Pedro Martir (SPM) 2.1m telescope are presented. The observations were taken in the "drift-scan" mode, i.e. with the slit, generally parallel to the galaxy major axis, drifting over the optical surface of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499#2</TD>
            <TD>2011-09-14T19:31:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/417/499&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/417/499</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/417/499 [table6]</TD>
            <TD>Spectrophotometry of Virgo cluster galaxies (Gavazzi+, 2004)</TD>
            <TD>Long-slit spectra of 333 galaxies, obtained during approximately 50 nights distributed in 6 years (1998-2003) using the 1.93m telescope of the Observatoire de Haute Provence (OHP), the ESO 3.6m telescope, the Loiano 1.52m telescope and the San Pedro Martir (SPM) 2.1m telescope are presented. The observations were taken in the "drift-scan" mode, i.e. with the slit, generally parallel to the galaxy major axis, drifting over the optical surface of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499#table6</TD>
            <TD>2011-09-14T19:31:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/417/499&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/417/499</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/417/499 [1]</TD>
            <TD>Spectrophotometry of Virgo cluster galaxies (Gavazzi+, 2004)</TD>
            <TD>Long-slit spectra of 333 galaxies, obtained during approximately 50 nights distributed in 6 years (1998-2003) using the 1.93m telescope of the Observatoire de Haute Provence (OHP), the ESO 3.6m telescope, the Loiano 1.52m telescope and the San Pedro Martir (SPM) 2.1m telescope are presented. The observations were taken in the "drift-scan" mode, i.e. with the slit, generally parallel to the galaxy major axis, drifting over the optical surface of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499#1</TD>
            <TD>2011-09-14T19:31:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/417/499</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/417/499</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/417/499 [2]</TD>
            <TD>Spectrophotometry of Virgo cluster galaxies (Gavazzi+, 2004)</TD>
            <TD>Long-slit spectra of 333 galaxies, obtained during approximately 50 nights distributed in 6 years (1998-2003) using the 1.93m telescope of the Observatoire de Haute Provence (OHP), the ESO 3.6m telescope, the Loiano 1.52m telescope and the San Pedro Martir (SPM) 2.1m telescope are presented. The observations were taken in the "drift-scan" mode, i.e. with the slit, generally parallel to the galaxy major axis, drifting over the optical surface of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499#2</TD>
            <TD>2011-09-14T19:31:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/417/499&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/417/499</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/417/499 [table6]</TD>
            <TD>Spectrophotometry of Virgo cluster galaxies (Gavazzi+, 2004)</TD>
            <TD>Long-slit spectra of 333 galaxies, obtained during approximately 50 nights distributed in 6 years (1998-2003) using the 1.93m telescope of the Observatoire de Haute Provence (OHP), the ESO 3.6m telescope, the Loiano 1.52m telescope and the San Pedro Martir (SPM) 2.1m telescope are presented. The observations were taken in the "drift-scan" mode, i.e. with the slit, generally parallel to the galaxy major axis, drifting over the optical surface of the galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499#table6</TD>
            <TD>2011-09-14T19:31:18Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/417/499</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/417/499&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/417/499</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/425/367 [1]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#1</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/425/367</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/425/367 [2]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#2</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/425/367&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [reflex50]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#reflex50</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [reflex]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#reflex</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [reflex70]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#reflex70</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [table9]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#table9</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/425/367 [1]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#1</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/425/367</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/425/367 [2]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#2</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/425/367&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [reflex50]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#reflex50</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [reflex]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#reflex</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [reflex70]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#reflex70</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [table9]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#table9</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/425/367 [1]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#1</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/425/367</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/425/367 [2]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#2</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/425/367&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [reflex50]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#reflex50</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [reflex]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#reflex</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [reflex70]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#reflex70</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/425/367 [table9]</TD>
            <TD>REFLEX Galaxy Cluster Survey catalogue (Boehringer+, 2004)</TD>
            <TD>The following tables provide the catalogue as well as several data files necessary to reproduce the sample preparation. These files are also required for the cosmological modeling of these observations in e.g. the study of the statistics of the large-scale structure of the matter distribution in the Universe and related cosmological tests.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367#table9</TD>
            <TD>2011-09-14T19:31:27Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2004</TD>
            <TD>ivo://CDS.VizieR/J/A+A/425/367</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/425/367&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/425/367</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/112/407 [1]</TD>
            <TD>Variable Stars in the Sculptor dwarf galaxy (Kaluzny+, 1995)</TD>
            <TD>The central area of the Sculptor dwarf galaxy was surveyed for variable stars as a side-program of the OGLE project. Light curves in the V band were obtained for 226 RR Lyr stars and for 3 anomalous cepheids. The data on RR Lyr variables in four nearby dwarf galaxies are summarized and discussed briefly.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407#1</TD>
            <TD>2011-09-14T19:32:22Z</TD>
            <TD>#Positional_Data#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/112/407</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/112/407</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/112/407 [2]</TD>
            <TD>Variable Stars in the Sculptor dwarf galaxy (Kaluzny+, 1995)</TD>
            <TD>The central area of the Sculptor dwarf galaxy was surveyed for variable stars as a side-program of the OGLE project. Light curves in the V band were obtained for 226 RR Lyr stars and for 3 anomalous cepheids. The data on RR Lyr variables in four nearby dwarf galaxies are summarized and discussed briefly.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407#2</TD>
            <TD>2011-09-14T19:32:22Z</TD>
            <TD>#Positional_Data#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/112/407&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/112/407</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/112/407 [1]</TD>
            <TD>Variable Stars in the Sculptor dwarf galaxy (Kaluzny+, 1995)</TD>
            <TD>The central area of the Sculptor dwarf galaxy was surveyed for variable stars as a side-program of the OGLE project. Light curves in the V band were obtained for 226 RR Lyr stars and for 3 anomalous cepheids. The data on RR Lyr variables in four nearby dwarf galaxies are summarized and discussed briefly.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407#1</TD>
            <TD>2011-09-14T19:32:22Z</TD>
            <TD>#Positional_Data#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/112/407</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/112/407</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/112/407 [2]</TD>
            <TD>Variable Stars in the Sculptor dwarf galaxy (Kaluzny+, 1995)</TD>
            <TD>The central area of the Sculptor dwarf galaxy was surveyed for variable stars as a side-program of the OGLE project. Light curves in the V band were obtained for 226 RR Lyr stars and for 3 anomalous cepheids. The data on RR Lyr variables in four nearby dwarf galaxies are summarized and discussed briefly.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407#2</TD>
            <TD>2011-09-14T19:32:22Z</TD>
            <TD>#Positional_Data#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/112/407&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/112/407</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/112/407 [1]</TD>
            <TD>Variable Stars in the Sculptor dwarf galaxy (Kaluzny+, 1995)</TD>
            <TD>The central area of the Sculptor dwarf galaxy was surveyed for variable stars as a side-program of the OGLE project. Light curves in the V band were obtained for 226 RR Lyr stars and for 3 anomalous cepheids. The data on RR Lyr variables in four nearby dwarf galaxies are summarized and discussed briefly.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407#1</TD>
            <TD>2011-09-14T19:32:22Z</TD>
            <TD>#Positional_Data#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/112/407</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/112/407</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/112/407 [2]</TD>
            <TD>Variable Stars in the Sculptor dwarf galaxy (Kaluzny+, 1995)</TD>
            <TD>The central area of the Sculptor dwarf galaxy was surveyed for variable stars as a side-program of the OGLE project. Light curves in the V band were obtained for 226 RR Lyr stars and for 3 anomalous cepheids. The data on RR Lyr variables in four nearby dwarf galaxies are summarized and discussed briefly.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407#2</TD>
            <TD>2011-09-14T19:32:22Z</TD>
            <TD>#Positional_Data#Galaxies#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Apr-1995</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/112/407</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/112/407&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/112/407</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/30/173 [1]</TD>
            <TD>Space velocities of solar neighborhood stars (Borkova+, 2004)</TD>
            <TD>For 77 main-sequence F-G stars in the solar neighborhood with published iron, magnesium, and europium abundances and with the ages we calculated the spatial velocities using Hipparcos data and the galactic orbital elements. A comparison with the orbital elements of the globular clusters that are known to have been accreted by our Galaxy in the past reveals stars of the extragalactic origin. We show that the abundance ratios of r- and {alpha}-elements in all the accreted stars differ sharply from those in the stars that are genetically associated with the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173#1</TD>
            <TD>2011-09-14T19:33:19Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2004</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/30/173</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/30/173</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/30/173 [2]</TD>
            <TD>Space velocities of solar neighborhood stars (Borkova+, 2004)</TD>
            <TD>For 77 main-sequence F-G stars in the solar neighborhood with published iron, magnesium, and europium abundances and with the ages we calculated the spatial velocities using Hipparcos data and the galactic orbital elements. A comparison with the orbital elements of the globular clusters that are known to have been accreted by our Galaxy in the past reveals stars of the extragalactic origin. We show that the abundance ratios of r- and {alpha}-elements in all the accreted stars differ sharply from those in the stars that are genetically associated with the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173#2</TD>
            <TD>2011-09-14T19:33:19Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2004</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/30/173&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/30/173</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/30/173 [1]</TD>
            <TD>Space velocities of solar neighborhood stars (Borkova+, 2004)</TD>
            <TD>For 77 main-sequence F-G stars in the solar neighborhood with published iron, magnesium, and europium abundances and with the ages we calculated the spatial velocities using Hipparcos data and the galactic orbital elements. A comparison with the orbital elements of the globular clusters that are known to have been accreted by our Galaxy in the past reveals stars of the extragalactic origin. We show that the abundance ratios of r- and {alpha}-elements in all the accreted stars differ sharply from those in the stars that are genetically associated with the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173#1</TD>
            <TD>2011-09-14T19:33:19Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2004</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/30/173</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/30/173</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/30/173 [2]</TD>
            <TD>Space velocities of solar neighborhood stars (Borkova+, 2004)</TD>
            <TD>For 77 main-sequence F-G stars in the solar neighborhood with published iron, magnesium, and europium abundances and with the ages we calculated the spatial velocities using Hipparcos data and the galactic orbital elements. A comparison with the orbital elements of the globular clusters that are known to have been accreted by our Galaxy in the past reveals stars of the extragalactic origin. We show that the abundance ratios of r- and {alpha}-elements in all the accreted stars differ sharply from those in the stars that are genetically associated with the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173#2</TD>
            <TD>2011-09-14T19:33:19Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2004</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/30/173&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/30/173</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/30/173 [1]</TD>
            <TD>Space velocities of solar neighborhood stars (Borkova+, 2004)</TD>
            <TD>For 77 main-sequence F-G stars in the solar neighborhood with published iron, magnesium, and europium abundances and with the ages we calculated the spatial velocities using Hipparcos data and the galactic orbital elements. A comparison with the orbital elements of the globular clusters that are known to have been accreted by our Galaxy in the past reveals stars of the extragalactic origin. We show that the abundance ratios of r- and {alpha}-elements in all the accreted stars differ sharply from those in the stars that are genetically associated with the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173#1</TD>
            <TD>2011-09-14T19:33:19Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2004</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/30/173</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/30/173</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/30/173 [2]</TD>
            <TD>Space velocities of solar neighborhood stars (Borkova+, 2004)</TD>
            <TD>For 77 main-sequence F-G stars in the solar neighborhood with published iron, magnesium, and europium abundances and with the ages we calculated the spatial velocities using Hipparcos data and the galactic orbital elements. A comparison with the orbital elements of the globular clusters that are known to have been accreted by our Galaxy in the past reveals stars of the extragalactic origin. We show that the abundance ratios of r- and {alpha}-elements in all the accreted stars differ sharply from those in the stars that are genetically associated with the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173#2</TD>
            <TD>2011-09-14T19:33:19Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Oct-2004</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/30/173</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/30/173&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/30/173</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/404/223 [1]</TD>
            <TD>2MASS IR star clusters in the Galaxy (Bica+, 2003)</TD>
            <TD>We carried out a survey of infrared star clusters and stellar groups on the 2MASS J, H and Ks all-sky release Atlas in the Northern and Equatorial Milky Way (350{deg},l&lt;360{deg}, 0{deg}&lt;l&lt;230{deg}). The search in this zone complements that in the Southern Milky Way (Dutra et al., 2003, Cat. &lt;J/A+A/400/533&gt;). The method concentrates efforts on the directions of known optical and radio nebulae. The present study provides 167 new infrared clusters, stellar groups and candidates. Combining the two studies for the whole Milky Way, 346 infrared clusters, stellar groups and candidates were discovered, whereas 315 objects were previously known. They constitute an important new sample for future detailed studies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223#1</TD>
            <TD>2011-09-14T19:33:25Z</TD>
            <TD>#Associations#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/404/223</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/404/223</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/404/223 [2]</TD>
            <TD>2MASS IR star clusters in the Galaxy (Bica+, 2003)</TD>
            <TD>We carried out a survey of infrared star clusters and stellar groups on the 2MASS J, H and Ks all-sky release Atlas in the Northern and Equatorial Milky Way (350{deg},l&lt;360{deg}, 0{deg}&lt;l&lt;230{deg}). The search in this zone complements that in the Southern Milky Way (Dutra et al., 2003, Cat. &lt;J/A+A/400/533&gt;). The method concentrates efforts on the directions of known optical and radio nebulae. The present study provides 167 new infrared clusters, stellar groups and candidates. Combining the two studies for the whole Milky Way, 346 infrared clusters, stellar groups and candidates were discovered, whereas 315 objects were previously known. They constitute an important new sample for future detailed studies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223#2</TD>
            <TD>2011-09-14T19:33:25Z</TD>
            <TD>#Associations#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/404/223&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/404/223</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/404/223 [1]</TD>
            <TD>2MASS IR star clusters in the Galaxy (Bica+, 2003)</TD>
            <TD>We carried out a survey of infrared star clusters and stellar groups on the 2MASS J, H and Ks all-sky release Atlas in the Northern and Equatorial Milky Way (350{deg},l&lt;360{deg}, 0{deg}&lt;l&lt;230{deg}). The search in this zone complements that in the Southern Milky Way (Dutra et al., 2003, Cat. &lt;J/A+A/400/533&gt;). The method concentrates efforts on the directions of known optical and radio nebulae. The present study provides 167 new infrared clusters, stellar groups and candidates. Combining the two studies for the whole Milky Way, 346 infrared clusters, stellar groups and candidates were discovered, whereas 315 objects were previously known. They constitute an important new sample for future detailed studies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223#1</TD>
            <TD>2011-09-14T19:33:25Z</TD>
            <TD>#Associations#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/404/223</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/404/223</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/404/223 [2]</TD>
            <TD>2MASS IR star clusters in the Galaxy (Bica+, 2003)</TD>
            <TD>We carried out a survey of infrared star clusters and stellar groups on the 2MASS J, H and Ks all-sky release Atlas in the Northern and Equatorial Milky Way (350{deg},l&lt;360{deg}, 0{deg}&lt;l&lt;230{deg}). The search in this zone complements that in the Southern Milky Way (Dutra et al., 2003, Cat. &lt;J/A+A/400/533&gt;). The method concentrates efforts on the directions of known optical and radio nebulae. The present study provides 167 new infrared clusters, stellar groups and candidates. Combining the two studies for the whole Milky Way, 346 infrared clusters, stellar groups and candidates were discovered, whereas 315 objects were previously known. They constitute an important new sample for future detailed studies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223#2</TD>
            <TD>2011-09-14T19:33:25Z</TD>
            <TD>#Associations#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/404/223&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/404/223</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/404/223 [1]</TD>
            <TD>2MASS IR star clusters in the Galaxy (Bica+, 2003)</TD>
            <TD>We carried out a survey of infrared star clusters and stellar groups on the 2MASS J, H and Ks all-sky release Atlas in the Northern and Equatorial Milky Way (350{deg},l&lt;360{deg}, 0{deg}&lt;l&lt;230{deg}). The search in this zone complements that in the Southern Milky Way (Dutra et al., 2003, Cat. &lt;J/A+A/400/533&gt;). The method concentrates efforts on the directions of known optical and radio nebulae. The present study provides 167 new infrared clusters, stellar groups and candidates. Combining the two studies for the whole Milky Way, 346 infrared clusters, stellar groups and candidates were discovered, whereas 315 objects were previously known. They constitute an important new sample for future detailed studies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223#1</TD>
            <TD>2011-09-14T19:33:25Z</TD>
            <TD>#Associations#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/404/223</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/404/223</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/404/223 [2]</TD>
            <TD>2MASS IR star clusters in the Galaxy (Bica+, 2003)</TD>
            <TD>We carried out a survey of infrared star clusters and stellar groups on the 2MASS J, H and Ks all-sky release Atlas in the Northern and Equatorial Milky Way (350{deg},l&lt;360{deg}, 0{deg}&lt;l&lt;230{deg}). The search in this zone complements that in the Southern Milky Way (Dutra et al., 2003, Cat. &lt;J/A+A/400/533&gt;). The method concentrates efforts on the directions of known optical and radio nebulae. The present study provides 167 new infrared clusters, stellar groups and candidates. Combining the two studies for the whole Milky Way, 346 infrared clusters, stellar groups and candidates were discovered, whereas 315 objects were previously known. They constitute an important new sample for future detailed studies.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223#2</TD>
            <TD>2011-09-14T19:33:25Z</TD>
            <TD>#Associations#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/404/223</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/404/223&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/404/223</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/421/595 [1]</TD>
            <TD>Deprojecting spiral galaxies method (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table1.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595#1</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/421/595</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/595</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/421/595 [2]</TD>
            <TD>Deprojecting spiral galaxies method (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table1.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595#2</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/421/595&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/595</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/421/595 [1]</TD>
            <TD>Deprojecting spiral galaxies method (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table1.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595#1</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/421/595</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/595</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/421/595 [2]</TD>
            <TD>Deprojecting spiral galaxies method (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table1.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595#2</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/421/595&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/595</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/421/595 [1]</TD>
            <TD>Deprojecting spiral galaxies method (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table1.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595#1</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/421/595</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/595</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/421/595 [2]</TD>
            <TD>Deprojecting spiral galaxies method (Garcia-Gomez+, 2004)</TD>
            <TD>Deprojection angles of each galaxy using the BAG1 and BAG2 methods plus the deprojection angles found in the literature. The last four columns of table1.dat contain the values adopted for the position angle, its dispersion, the inclination angle and its dispersion in degrees.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595#2</TD>
            <TD>2011-09-14T19:37:23Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Feb-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/421/595</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/421/595&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/421/595</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/2723 [1]</TD>
            <TD>Abundances of 3 supergiants in Sextans A (Kaufer+, 2004)</TD>
            <TD>We present the abundance analyses of three isolated A-type supergiant stars in the dwarf irregular galaxy Sextans A (=DDO 75) from high-resolution spectra obtained with the Ultraviolet-Visual Echelle Spectrograph (UVES) on the Kueyen telescope (UT2) of the ESO Very Large Telescope (VLT). Detailed model atmosphere analyses have been used to determine the stellar atmospheric parameters and the elemental abundances of the stars.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2723#1</TD>
            <TD>2011-09-14T19:38:43Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2723</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/2723</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2723</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/2723 [2]</TD>
            <TD>Abundances of 3 supergiants in Sextans A (Kaufer+, 2004)</TD>
            <TD>We present the abundance analyses of three isolated A-type supergiant stars in the dwarf irregular galaxy Sextans A (=DDO 75) from high-resolution spectra obtained with the Ultraviolet-Visual Echelle Spectrograph (UVES) on the Kueyen telescope (UT2) of the ESO Very Large Telescope (VLT). Detailed model atmosphere analyses have been used to determine the stellar atmospheric parameters and the elemental abundances of the stars.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2723#2</TD>
            <TD>2011-09-14T19:38:43Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2723</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/2723&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2723</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/2723 [1]</TD>
            <TD>Abundances of 3 supergiants in Sextans A (Kaufer+, 2004)</TD>
            <TD>We present the abundance analyses of three isolated A-type supergiant stars in the dwarf irregular galaxy Sextans A (=DDO 75) from high-resolution spectra obtained with the Ultraviolet-Visual Echelle Spectrograph (UVES) on the Kueyen telescope (UT2) of the ESO Very Large Telescope (VLT). Detailed model atmosphere analyses have been used to determine the stellar atmospheric parameters and the elemental abundances of the stars.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2723#1</TD>
            <TD>2011-09-14T19:38:43Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2723</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/2723</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2723</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/2723 [2]</TD>
            <TD>Abundances of 3 supergiants in Sextans A (Kaufer+, 2004)</TD>
            <TD>We present the abundance analyses of three isolated A-type supergiant stars in the dwarf irregular galaxy Sextans A (=DDO 75) from high-resolution spectra obtained with the Ultraviolet-Visual Echelle Spectrograph (UVES) on the Kueyen telescope (UT2) of the ESO Very Large Telescope (VLT). Detailed model atmosphere analyses have been used to determine the stellar atmospheric parameters and the elemental abundances of the stars.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2723#2</TD>
            <TD>2011-09-14T19:38:43Z</TD>
            <TD>#Abundances#Stars#Spectroscopy#Stars:early-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2723</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/2723&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2723</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/479/231 [1]</TD>
            <TD>PNe in M51, M96 &amp; M101 (Feldmeier+ 1997)</TD>
            <TD>We report the results of an [O III]{lambda}5007 survey for planetary nebulae (PNs) in three spiral galaxies: M101 (NGC 5457), M51 (NGC 5194/5l95), and M96 (NGC 3368). By comparing on-band/off-band [O III]{lambda}5007 images with images taken in H{alpha} and broadband R. we identify 65, 64, and 74 PN candidates in each galaxy, respectively. From these data, an adopted M31 distance of 770kpc, and the empirical planetary nebula luminosity function (PNLF), we derive distances to M101, M51, and M96 of 7.7+/-0.5, 8.4+/-0.6, and 9.6+/-0.6Mpc. These observations demonstrate that the PNLF technique can be successfully applied to late-type galaxies and can provide an important overlap between the Population I and Population II distance scales. We also discuss some special problems associated with using the PNLF in spiral galaxies, including the effects of dust and the possible presence of [O III] bright supernova remnants.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231#1</TD>
            <TD>2011-09-14T19:39:08Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/479/231</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/479/231</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/479/231 [2]</TD>
            <TD>PNe in M51, M96 &amp; M101 (Feldmeier+ 1997)</TD>
            <TD>We report the results of an [O III]{lambda}5007 survey for planetary nebulae (PNs) in three spiral galaxies: M101 (NGC 5457), M51 (NGC 5194/5l95), and M96 (NGC 3368). By comparing on-band/off-band [O III]{lambda}5007 images with images taken in H{alpha} and broadband R. we identify 65, 64, and 74 PN candidates in each galaxy, respectively. From these data, an adopted M31 distance of 770kpc, and the empirical planetary nebula luminosity function (PNLF), we derive distances to M101, M51, and M96 of 7.7+/-0.5, 8.4+/-0.6, and 9.6+/-0.6Mpc. These observations demonstrate that the PNLF technique can be successfully applied to late-type galaxies and can provide an important overlap between the Population I and Population II distance scales. We also discuss some special problems associated with using the PNLF in spiral galaxies, including the effects of dust and the possible presence of [O III] bright supernova remnants.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231#2</TD>
            <TD>2011-09-14T19:39:08Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/479/231&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/479/231</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/479/231 [1]</TD>
            <TD>PNe in M51, M96 &amp; M101 (Feldmeier+ 1997)</TD>
            <TD>We report the results of an [O III]{lambda}5007 survey for planetary nebulae (PNs) in three spiral galaxies: M101 (NGC 5457), M51 (NGC 5194/5l95), and M96 (NGC 3368). By comparing on-band/off-band [O III]{lambda}5007 images with images taken in H{alpha} and broadband R. we identify 65, 64, and 74 PN candidates in each galaxy, respectively. From these data, an adopted M31 distance of 770kpc, and the empirical planetary nebula luminosity function (PNLF), we derive distances to M101, M51, and M96 of 7.7+/-0.5, 8.4+/-0.6, and 9.6+/-0.6Mpc. These observations demonstrate that the PNLF technique can be successfully applied to late-type galaxies and can provide an important overlap between the Population I and Population II distance scales. We also discuss some special problems associated with using the PNLF in spiral galaxies, including the effects of dust and the possible presence of [O III] bright supernova remnants.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231#1</TD>
            <TD>2011-09-14T19:39:08Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/479/231</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/479/231</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/479/231 [2]</TD>
            <TD>PNe in M51, M96 &amp; M101 (Feldmeier+ 1997)</TD>
            <TD>We report the results of an [O III]{lambda}5007 survey for planetary nebulae (PNs) in three spiral galaxies: M101 (NGC 5457), M51 (NGC 5194/5l95), and M96 (NGC 3368). By comparing on-band/off-band [O III]{lambda}5007 images with images taken in H{alpha} and broadband R. we identify 65, 64, and 74 PN candidates in each galaxy, respectively. From these data, an adopted M31 distance of 770kpc, and the empirical planetary nebula luminosity function (PNLF), we derive distances to M101, M51, and M96 of 7.7+/-0.5, 8.4+/-0.6, and 9.6+/-0.6Mpc. These observations demonstrate that the PNLF technique can be successfully applied to late-type galaxies and can provide an important overlap between the Population I and Population II distance scales. We also discuss some special problems associated with using the PNLF in spiral galaxies, including the effects of dust and the possible presence of [O III] bright supernova remnants.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231#2</TD>
            <TD>2011-09-14T19:39:08Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
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            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/479/231&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/479/231</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/479/231 [1]</TD>
            <TD>PNe in M51, M96 &amp; M101 (Feldmeier+ 1997)</TD>
            <TD>We report the results of an [O III]{lambda}5007 survey for planetary nebulae (PNs) in three spiral galaxies: M101 (NGC 5457), M51 (NGC 5194/5l95), and M96 (NGC 3368). By comparing on-band/off-band [O III]{lambda}5007 images with images taken in H{alpha} and broadband R. we identify 65, 64, and 74 PN candidates in each galaxy, respectively. From these data, an adopted M31 distance of 770kpc, and the empirical planetary nebula luminosity function (PNLF), we derive distances to M101, M51, and M96 of 7.7+/-0.5, 8.4+/-0.6, and 9.6+/-0.6Mpc. These observations demonstrate that the PNLF technique can be successfully applied to late-type galaxies and can provide an important overlap between the Population I and Population II distance scales. We also discuss some special problems associated with using the PNLF in spiral galaxies, including the effects of dust and the possible presence of [O III] bright supernova remnants.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231#1</TD>
            <TD>2011-09-14T19:39:08Z</TD>
            <TD>#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/479/231</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/479/231</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/479/231 [2]</TD>
            <TD>PNe in M51, M96 &amp; M101 (Feldmeier+ 1997)</TD>
            <TD>We report the results of an [O III]{lambda}5007 survey for planetary nebulae (PNs) in three spiral galaxies: M101 (NGC 5457), M51 (NGC 5194/5l95), and M96 (NGC 3368). By comparing on-band/off-band [O III]{lambda}5007 images with images taken in H{alpha} and broadband R. we identify 65, 64, and 74 PN candidates in each galaxy, respectively. From these data, an adopted M31 distance of 770kpc, and the empirical planetary nebula luminosity function (PNLF), we derive distances to M101, M51, and M96 of 7.7+/-0.5, 8.4+/-0.6, and 9.6+/-0.6Mpc. These observations demonstrate that the PNLF technique can be successfully applied to late-type galaxies and can provide an important overlap between the Population I and Population II distance scales. We also discuss some special problems associated with using the PNLF in spiral galaxies, including the effects of dust and the possible presence of [O III] bright supernova remnants.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231#2</TD>
            <TD>2011-09-14T19:39:08Z</TD>
            <TD>#Planetary_Nebulae#</TD>
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            <TD>07-Oct-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/479/231</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/479/231&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/479/231</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/414/463 [1]</TD>
            <TD>Planetary nebula system of NGC 5128 (Hui+, 1993)</TD>
            <TD>Our PN observations of NGC 5128 took place over three observing seasons. During 1985 and 1986, we took [O III] {lambda}5007{AA} on-band/off-band pictures of selected galaxy fields using the RCA CCD camera at the prime focus of the CTIO 4m telescope. In 1988 a third survey was carried out on the same telescope with a TI CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463#1</TD>
            <TD>2011-09-14T19:40:33Z</TD>
            <TD>#Positional_Data#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/414/463</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/463</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/414/463 [2]</TD>
            <TD>Planetary nebula system of NGC 5128 (Hui+, 1993)</TD>
            <TD>Our PN observations of NGC 5128 took place over three observing seasons. During 1985 and 1986, we took [O III] {lambda}5007{AA} on-band/off-band pictures of selected galaxy fields using the RCA CCD camera at the prime focus of the CTIO 4m telescope. In 1988 a third survey was carried out on the same telescope with a TI CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463#2</TD>
            <TD>2011-09-14T19:40:33Z</TD>
            <TD>#Positional_Data#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/414/463&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/414/463 [table6]</TD>
            <TD>Planetary nebula system of NGC 5128 (Hui+, 1993)</TD>
            <TD>Our PN observations of NGC 5128 took place over three observing seasons. During 1985 and 1986, we took [O III] {lambda}5007{AA} on-band/off-band pictures of selected galaxy fields using the RCA CCD camera at the prime focus of the CTIO 4m telescope. In 1988 a third survey was carried out on the same telescope with a TI CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463#table6</TD>
            <TD>2011-09-14T19:40:33Z</TD>
            <TD>#Positional_Data#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/414/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/463</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/414/463 [1]</TD>
            <TD>Planetary nebula system of NGC 5128 (Hui+, 1993)</TD>
            <TD>Our PN observations of NGC 5128 took place over three observing seasons. During 1985 and 1986, we took [O III] {lambda}5007{AA} on-band/off-band pictures of selected galaxy fields using the RCA CCD camera at the prime focus of the CTIO 4m telescope. In 1988 a third survey was carried out on the same telescope with a TI CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463#1</TD>
            <TD>2011-09-14T19:40:33Z</TD>
            <TD>#Positional_Data#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/414/463</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/463</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/414/463 [2]</TD>
            <TD>Planetary nebula system of NGC 5128 (Hui+, 1993)</TD>
            <TD>Our PN observations of NGC 5128 took place over three observing seasons. During 1985 and 1986, we took [O III] {lambda}5007{AA} on-band/off-band pictures of selected galaxy fields using the RCA CCD camera at the prime focus of the CTIO 4m telescope. In 1988 a third survey was carried out on the same telescope with a TI CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463#2</TD>
            <TD>2011-09-14T19:40:33Z</TD>
            <TD>#Positional_Data#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/414/463&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/414/463 [table6]</TD>
            <TD>Planetary nebula system of NGC 5128 (Hui+, 1993)</TD>
            <TD>Our PN observations of NGC 5128 took place over three observing seasons. During 1985 and 1986, we took [O III] {lambda}5007{AA} on-band/off-band pictures of selected galaxy fields using the RCA CCD camera at the prime focus of the CTIO 4m telescope. In 1988 a third survey was carried out on the same telescope with a TI CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463#table6</TD>
            <TD>2011-09-14T19:40:33Z</TD>
            <TD>#Positional_Data#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/414/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/463</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/414/463 [1]</TD>
            <TD>Planetary nebula system of NGC 5128 (Hui+, 1993)</TD>
            <TD>Our PN observations of NGC 5128 took place over three observing seasons. During 1985 and 1986, we took [O III] {lambda}5007{AA} on-band/off-band pictures of selected galaxy fields using the RCA CCD camera at the prime focus of the CTIO 4m telescope. In 1988 a third survey was carried out on the same telescope with a TI CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463#1</TD>
            <TD>2011-09-14T19:40:33Z</TD>
            <TD>#Positional_Data#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/414/463</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/463</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/414/463 [2]</TD>
            <TD>Planetary nebula system of NGC 5128 (Hui+, 1993)</TD>
            <TD>Our PN observations of NGC 5128 took place over three observing seasons. During 1985 and 1986, we took [O III] {lambda}5007{AA} on-band/off-band pictures of selected galaxy fields using the RCA CCD camera at the prime focus of the CTIO 4m telescope. In 1988 a third survey was carried out on the same telescope with a TI CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463#2</TD>
            <TD>2011-09-14T19:40:33Z</TD>
            <TD>#Positional_Data#Galaxies#Planetary_Nebulae#</TD>
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            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/414/463&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/463</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/414/463 [table6]</TD>
            <TD>Planetary nebula system of NGC 5128 (Hui+, 1993)</TD>
            <TD>Our PN observations of NGC 5128 took place over three observing seasons. During 1985 and 1986, we took [O III] {lambda}5007{AA} on-band/off-band pictures of selected galaxy fields using the RCA CCD camera at the prime focus of the CTIO 4m telescope. In 1988 a third survey was carried out on the same telescope with a TI CCD.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463#table6</TD>
            <TD>2011-09-14T19:40:33Z</TD>
            <TD>#Positional_Data#Galaxies#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jan-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/414/463</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/414/463&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/414/463</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/297/885 [1]</TD>
            <TD>Faint galaxies KIc photometry (Glazebrook+, 1998)</TD>
            <TD>The excess number of blue galaxies at faint magnitudes is a subject of much controversy. Recent Hubble Space Telescope results have revealed a plethora of galaxies with peculiar morphologies tentatively identified as the evolving population. We report the results of optical spectroscopy and near-infrared photometry of a sample of faint HST galaxies from the Medium Deep Survey to ascertain the physical properties of the faint morphological populations. We find four principal results. First, the population of objects classified as 'peculiar' are intrinsically luminous in the optical (M_B_~-19). Secondly these systems tend to be strong sources of [OII] line luminosity. Thirdly the optical-infrared colours of the faint population (a) confirm the presence of a population of compact blue galaxies and (b) show the stellar populations of irregular/peculiar galaxies encompass a wide range in age. Finally a surface-brightness comparison with the local galaxy sample of Freiz et al. (1996AJ....111..174F) shows that these objects are not of anomalously low surface brightness, rather we find that all morphological classes have evolved to a higher surface brightness at higher redshifts (z&gt;0.3).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885#1</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/297/885</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/885</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/297/885 [2]</TD>
            <TD>Faint galaxies KIc photometry (Glazebrook+, 1998)</TD>
            <TD>The excess number of blue galaxies at faint magnitudes is a subject of much controversy. Recent Hubble Space Telescope results have revealed a plethora of galaxies with peculiar morphologies tentatively identified as the evolving population. We report the results of optical spectroscopy and near-infrared photometry of a sample of faint HST galaxies from the Medium Deep Survey to ascertain the physical properties of the faint morphological populations. We find four principal results. First, the population of objects classified as 'peculiar' are intrinsically luminous in the optical (M_B_~-19). Secondly these systems tend to be strong sources of [OII] line luminosity. Thirdly the optical-infrared colours of the faint population (a) confirm the presence of a population of compact blue galaxies and (b) show the stellar populations of irregular/peculiar galaxies encompass a wide range in age. Finally a surface-brightness comparison with the local galaxy sample of Freiz et al. (1996AJ....111..174F) shows that these objects are not of anomalously low surface brightness, rather we find that all morphological classes have evolved to a higher surface brightness at higher redshifts (z&gt;0.3).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885#2</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/297/885&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/885</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/297/885 [1]</TD>
            <TD>Faint galaxies KIc photometry (Glazebrook+, 1998)</TD>
            <TD>The excess number of blue galaxies at faint magnitudes is a subject of much controversy. Recent Hubble Space Telescope results have revealed a plethora of galaxies with peculiar morphologies tentatively identified as the evolving population. We report the results of optical spectroscopy and near-infrared photometry of a sample of faint HST galaxies from the Medium Deep Survey to ascertain the physical properties of the faint morphological populations. We find four principal results. First, the population of objects classified as 'peculiar' are intrinsically luminous in the optical (M_B_~-19). Secondly these systems tend to be strong sources of [OII] line luminosity. Thirdly the optical-infrared colours of the faint population (a) confirm the presence of a population of compact blue galaxies and (b) show the stellar populations of irregular/peculiar galaxies encompass a wide range in age. Finally a surface-brightness comparison with the local galaxy sample of Freiz et al. (1996AJ....111..174F) shows that these objects are not of anomalously low surface brightness, rather we find that all morphological classes have evolved to a higher surface brightness at higher redshifts (z&gt;0.3).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885#1</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/297/885</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/885</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/297/885 [2]</TD>
            <TD>Faint galaxies KIc photometry (Glazebrook+, 1998)</TD>
            <TD>The excess number of blue galaxies at faint magnitudes is a subject of much controversy. Recent Hubble Space Telescope results have revealed a plethora of galaxies with peculiar morphologies tentatively identified as the evolving population. We report the results of optical spectroscopy and near-infrared photometry of a sample of faint HST galaxies from the Medium Deep Survey to ascertain the physical properties of the faint morphological populations. We find four principal results. First, the population of objects classified as 'peculiar' are intrinsically luminous in the optical (M_B_~-19). Secondly these systems tend to be strong sources of [OII] line luminosity. Thirdly the optical-infrared colours of the faint population (a) confirm the presence of a population of compact blue galaxies and (b) show the stellar populations of irregular/peculiar galaxies encompass a wide range in age. Finally a surface-brightness comparison with the local galaxy sample of Freiz et al. (1996AJ....111..174F) shows that these objects are not of anomalously low surface brightness, rather we find that all morphological classes have evolved to a higher surface brightness at higher redshifts (z&gt;0.3).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885#2</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
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            <TD>03-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/297/885&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/885</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/297/885 [1]</TD>
            <TD>Faint galaxies KIc photometry (Glazebrook+, 1998)</TD>
            <TD>The excess number of blue galaxies at faint magnitudes is a subject of much controversy. Recent Hubble Space Telescope results have revealed a plethora of galaxies with peculiar morphologies tentatively identified as the evolving population. We report the results of optical spectroscopy and near-infrared photometry of a sample of faint HST galaxies from the Medium Deep Survey to ascertain the physical properties of the faint morphological populations. We find four principal results. First, the population of objects classified as 'peculiar' are intrinsically luminous in the optical (M_B_~-19). Secondly these systems tend to be strong sources of [OII] line luminosity. Thirdly the optical-infrared colours of the faint population (a) confirm the presence of a population of compact blue galaxies and (b) show the stellar populations of irregular/peculiar galaxies encompass a wide range in age. Finally a surface-brightness comparison with the local galaxy sample of Freiz et al. (1996AJ....111..174F) shows that these objects are not of anomalously low surface brightness, rather we find that all morphological classes have evolved to a higher surface brightness at higher redshifts (z&gt;0.3).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885#1</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/297/885</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/885</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/297/885 [2]</TD>
            <TD>Faint galaxies KIc photometry (Glazebrook+, 1998)</TD>
            <TD>The excess number of blue galaxies at faint magnitudes is a subject of much controversy. Recent Hubble Space Telescope results have revealed a plethora of galaxies with peculiar morphologies tentatively identified as the evolving population. We report the results of optical spectroscopy and near-infrared photometry of a sample of faint HST galaxies from the Medium Deep Survey to ascertain the physical properties of the faint morphological populations. We find four principal results. First, the population of objects classified as 'peculiar' are intrinsically luminous in the optical (M_B_~-19). Secondly these systems tend to be strong sources of [OII] line luminosity. Thirdly the optical-infrared colours of the faint population (a) confirm the presence of a population of compact blue galaxies and (b) show the stellar populations of irregular/peculiar galaxies encompass a wide range in age. Finally a surface-brightness comparison with the local galaxy sample of Freiz et al. (1996AJ....111..174F) shows that these objects are not of anomalously low surface brightness, rather we find that all morphological classes have evolved to a higher surface brightness at higher redshifts (z&gt;0.3).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885#2</TD>
            <TD>2011-09-14T19:40:41Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Dec-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/297/885</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/297/885&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/297/885</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/612/L93 [1]</TD>
            <TD>Candidates of z~5.5-7 galaxies in the HST-UDF (Yan+, 2004)</TD>
            <TD>We report results from our z~5.5-7 galaxy search in the Hubble Space Telescope Ultra Deep Field (UDF). Using the 400 orbit of Advanced Camera for Surveys data, we found 108 plausible 5.5&lt;=z&lt;=6.5 (or z~6 for short) candidates to m_AB_(z_850_)=30.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93#1</TD>
            <TD>2011-09-14T19:41:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/612/L93</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/612/L93</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/612/L93 [2]</TD>
            <TD>Candidates of z~5.5-7 galaxies in the HST-UDF (Yan+, 2004)</TD>
            <TD>We report results from our z~5.5-7 galaxy search in the Hubble Space Telescope Ultra Deep Field (UDF). Using the 400 orbit of Advanced Camera for Surveys data, we found 108 plausible 5.5&lt;=z&lt;=6.5 (or z~6 for short) candidates to m_AB_(z_850_)=30.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93#2</TD>
            <TD>2011-09-14T19:41:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/612/L93&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/612/L93</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/612/L93 [1]</TD>
            <TD>Candidates of z~5.5-7 galaxies in the HST-UDF (Yan+, 2004)</TD>
            <TD>We report results from our z~5.5-7 galaxy search in the Hubble Space Telescope Ultra Deep Field (UDF). Using the 400 orbit of Advanced Camera for Surveys data, we found 108 plausible 5.5&lt;=z&lt;=6.5 (or z~6 for short) candidates to m_AB_(z_850_)=30.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93#1</TD>
            <TD>2011-09-14T19:41:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/612/L93</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/612/L93</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/612/L93 [2]</TD>
            <TD>Candidates of z~5.5-7 galaxies in the HST-UDF (Yan+, 2004)</TD>
            <TD>We report results from our z~5.5-7 galaxy search in the Hubble Space Telescope Ultra Deep Field (UDF). Using the 400 orbit of Advanced Camera for Surveys data, we found 108 plausible 5.5&lt;=z&lt;=6.5 (or z~6 for short) candidates to m_AB_(z_850_)=30.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93#2</TD>
            <TD>2011-09-14T19:41:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/612/L93&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/612/L93</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/612/L93 [1]</TD>
            <TD>Candidates of z~5.5-7 galaxies in the HST-UDF (Yan+, 2004)</TD>
            <TD>We report results from our z~5.5-7 galaxy search in the Hubble Space Telescope Ultra Deep Field (UDF). Using the 400 orbit of Advanced Camera for Surveys data, we found 108 plausible 5.5&lt;=z&lt;=6.5 (or z~6 for short) candidates to m_AB_(z_850_)=30.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93#1</TD>
            <TD>2011-09-14T19:41:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/612/L93</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/612/L93</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/612/L93 [2]</TD>
            <TD>Candidates of z~5.5-7 galaxies in the HST-UDF (Yan+, 2004)</TD>
            <TD>We report results from our z~5.5-7 galaxy search in the Hubble Space Telescope Ultra Deep Field (UDF). Using the 400 orbit of Advanced Camera for Surveys data, we found 108 plausible 5.5&lt;=z&lt;=6.5 (or z~6 for short) candidates to m_AB_(z_850_)=30.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93#2</TD>
            <TD>2011-09-14T19:41:52Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/612/L93</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/612/L93&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/612/L93</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/1 [1]</TD>
            <TD>First Look Survey: NOAO R-band Mosaic (Fadda+, 2004)</TD>
            <TD>We present R-band images covering more than 11 square degrees of sky that were obtained in preparation for the Spitzer Space Telescope First-Look Survey (FLS). The FLS was designed to characterize the mid-infrared sky at depths 2 orders of magnitude deeper than previous surveys. The extragalactic component is the first cosmological survey done with Spitzer. Source catalogs extracted from the R-band images are also presented. The R-band images were obtained using the Mosaic-1 camera on the 4m Mayall Telescope of the Kitt Peak National Observatory. Two relatively large regions of the sky were observed to modest depth: the main FLS extragalactic field (17h18m00s, +59{deg}30'00.0"[J2000]; l=88.3{deg}, b=+34.9{deg}) and the ELAIS-N1 field (16h10m01s, +54{deg}30'36.0"; l=84.2{deg}, b=+44.9{deg}). While both these fields were in early plans for the FLS, only a single deep-pointing test observation was made at the ELAIS-N1 location. The larger Legacy program SWIRE will include this region among its surveyed areas. The data products of our KPNO imaging (images and object catalogs) are made available to the community through the World Wide Web (via the Spitzer Science Center and NOAO Science Archive, http://ssc.spitzer.caltech.edu/fls/). The overall quality of the images is high. The measured positions of sources detected in the images have rms uncertainties in their absolute positions on the order of 0.35" with possible systematic offsets on the order of 0.1", depending on the reference frame of comparison. The relative astrometric accuracy is much better than 1/10 of an arcsecond. Typical delivered image quality in the images is 1.1" full width at half-maximum. The images are relatively deep, since they reach a median 5{sigma} depth limiting magnitude of R=25.5 (Vega) as measured within a 1.35 FWHM aperture, for which the signal-to-noise ratio (S/N) is maximal. Catalogs have been extracted with SExtractor, using thresholds in area and flux for which the number of false detections is below 1% at R=25. Only sources with S/N&gt;3 have been retained in the final catalogs. Comparing the galaxy number counts from our images with those of deeper R-band surveys, we estimate that our observations are 50% complete at R=24.5. These limits in depth are sufficient to identify a substantial fraction of the infrared sources that will be detected by Spitzer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1#1</TD>
            <TD>2011-09-14T19:42:07Z</TD>
            <TD>#Galaxies#</TD>
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            <TD>16-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/1 [2]</TD>
            <TD>First Look Survey: NOAO R-band Mosaic (Fadda+, 2004)</TD>
            <TD>We present R-band images covering more than 11 square degrees of sky that were obtained in preparation for the Spitzer Space Telescope First-Look Survey (FLS). The FLS was designed to characterize the mid-infrared sky at depths 2 orders of magnitude deeper than previous surveys. The extragalactic component is the first cosmological survey done with Spitzer. Source catalogs extracted from the R-band images are also presented. The R-band images were obtained using the Mosaic-1 camera on the 4m Mayall Telescope of the Kitt Peak National Observatory. Two relatively large regions of the sky were observed to modest depth: the main FLS extragalactic field (17h18m00s, +59{deg}30'00.0"[J2000]; l=88.3{deg}, b=+34.9{deg}) and the ELAIS-N1 field (16h10m01s, +54{deg}30'36.0"; l=84.2{deg}, b=+44.9{deg}). While both these fields were in early plans for the FLS, only a single deep-pointing test observation was made at the ELAIS-N1 location. The larger Legacy program SWIRE will include this region among its surveyed areas. The data products of our KPNO imaging (images and object catalogs) are made available to the community through the World Wide Web (via the Spitzer Science Center and NOAO Science Archive, http://ssc.spitzer.caltech.edu/fls/). The overall quality of the images is high. The measured positions of sources detected in the images have rms uncertainties in their absolute positions on the order of 0.35" with possible systematic offsets on the order of 0.1", depending on the reference frame of comparison. The relative astrometric accuracy is much better than 1/10 of an arcsecond. Typical delivered image quality in the images is 1.1" full width at half-maximum. The images are relatively deep, since they reach a median 5{sigma} depth limiting magnitude of R=25.5 (Vega) as measured within a 1.35 FWHM aperture, for which the signal-to-noise ratio (S/N) is maximal. Catalogs have been extracted with SExtractor, using thresholds in area and flux for which the number of false detections is below 1% at R=25. Only sources with S/N&gt;3 have been retained in the final catalogs. Comparing the galaxy number counts from our images with those of deeper R-band surveys, we estimate that our observations are 50% complete at R=24.5. These limits in depth are sufficient to identify a substantial fraction of the infrared sources that will be detected by Spitzer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/1&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/1 [1]</TD>
            <TD>First Look Survey: NOAO R-band Mosaic (Fadda+, 2004)</TD>
            <TD>We present R-band images covering more than 11 square degrees of sky that were obtained in preparation for the Spitzer Space Telescope First-Look Survey (FLS). The FLS was designed to characterize the mid-infrared sky at depths 2 orders of magnitude deeper than previous surveys. The extragalactic component is the first cosmological survey done with Spitzer. Source catalogs extracted from the R-band images are also presented. The R-band images were obtained using the Mosaic-1 camera on the 4m Mayall Telescope of the Kitt Peak National Observatory. Two relatively large regions of the sky were observed to modest depth: the main FLS extragalactic field (17h18m00s, +59{deg}30'00.0"[J2000]; l=88.3{deg}, b=+34.9{deg}) and the ELAIS-N1 field (16h10m01s, +54{deg}30'36.0"; l=84.2{deg}, b=+44.9{deg}). While both these fields were in early plans for the FLS, only a single deep-pointing test observation was made at the ELAIS-N1 location. The larger Legacy program SWIRE will include this region among its surveyed areas. The data products of our KPNO imaging (images and object catalogs) are made available to the community through the World Wide Web (via the Spitzer Science Center and NOAO Science Archive, http://ssc.spitzer.caltech.edu/fls/). The overall quality of the images is high. The measured positions of sources detected in the images have rms uncertainties in their absolute positions on the order of 0.35" with possible systematic offsets on the order of 0.1", depending on the reference frame of comparison. The relative astrometric accuracy is much better than 1/10 of an arcsecond. Typical delivered image quality in the images is 1.1" full width at half-maximum. The images are relatively deep, since they reach a median 5{sigma} depth limiting magnitude of R=25.5 (Vega) as measured within a 1.35 FWHM aperture, for which the signal-to-noise ratio (S/N) is maximal. Catalogs have been extracted with SExtractor, using thresholds in area and flux for which the number of false detections is below 1% at R=25. Only sources with S/N&gt;3 have been retained in the final catalogs. Comparing the galaxy number counts from our images with those of deeper R-band surveys, we estimate that our observations are 50% complete at R=24.5. These limits in depth are sufficient to identify a substantial fraction of the infrared sources that will be detected by Spitzer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/128/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/1 [2]</TD>
            <TD>First Look Survey: NOAO R-band Mosaic (Fadda+, 2004)</TD>
            <TD>We present R-band images covering more than 11 square degrees of sky that were obtained in preparation for the Spitzer Space Telescope First-Look Survey (FLS). The FLS was designed to characterize the mid-infrared sky at depths 2 orders of magnitude deeper than previous surveys. The extragalactic component is the first cosmological survey done with Spitzer. Source catalogs extracted from the R-band images are also presented. The R-band images were obtained using the Mosaic-1 camera on the 4m Mayall Telescope of the Kitt Peak National Observatory. Two relatively large regions of the sky were observed to modest depth: the main FLS extragalactic field (17h18m00s, +59{deg}30'00.0"[J2000]; l=88.3{deg}, b=+34.9{deg}) and the ELAIS-N1 field (16h10m01s, +54{deg}30'36.0"; l=84.2{deg}, b=+44.9{deg}). While both these fields were in early plans for the FLS, only a single deep-pointing test observation was made at the ELAIS-N1 location. The larger Legacy program SWIRE will include this region among its surveyed areas. The data products of our KPNO imaging (images and object catalogs) are made available to the community through the World Wide Web (via the Spitzer Science Center and NOAO Science Archive, http://ssc.spitzer.caltech.edu/fls/). The overall quality of the images is high. The measured positions of sources detected in the images have rms uncertainties in their absolute positions on the order of 0.35" with possible systematic offsets on the order of 0.1", depending on the reference frame of comparison. The relative astrometric accuracy is much better than 1/10 of an arcsecond. Typical delivered image quality in the images is 1.1" full width at half-maximum. The images are relatively deep, since they reach a median 5{sigma} depth limiting magnitude of R=25.5 (Vega) as measured within a 1.35 FWHM aperture, for which the signal-to-noise ratio (S/N) is maximal. Catalogs have been extracted with SExtractor, using thresholds in area and flux for which the number of false detections is below 1% at R=25. Only sources with S/N&gt;3 have been retained in the final catalogs. Comparing the galaxy number counts from our images with those of deeper R-band surveys, we estimate that our observations are 50% complete at R=24.5. These limits in depth are sufficient to identify a substantial fraction of the infrared sources that will be detected by Spitzer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1#2</TD>
            <TD>2011-09-14T19:42:07Z</TD>
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            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/128/1 [1]</TD>
            <TD>First Look Survey: NOAO R-band Mosaic (Fadda+, 2004)</TD>
            <TD>We present R-band images covering more than 11 square degrees of sky that were obtained in preparation for the Spitzer Space Telescope First-Look Survey (FLS). The FLS was designed to characterize the mid-infrared sky at depths 2 orders of magnitude deeper than previous surveys. The extragalactic component is the first cosmological survey done with Spitzer. Source catalogs extracted from the R-band images are also presented. The R-band images were obtained using the Mosaic-1 camera on the 4m Mayall Telescope of the Kitt Peak National Observatory. Two relatively large regions of the sky were observed to modest depth: the main FLS extragalactic field (17h18m00s, +59{deg}30'00.0"[J2000]; l=88.3{deg}, b=+34.9{deg}) and the ELAIS-N1 field (16h10m01s, +54{deg}30'36.0"; l=84.2{deg}, b=+44.9{deg}). While both these fields were in early plans for the FLS, only a single deep-pointing test observation was made at the ELAIS-N1 location. The larger Legacy program SWIRE will include this region among its surveyed areas. The data products of our KPNO imaging (images and object catalogs) are made available to the community through the World Wide Web (via the Spitzer Science Center and NOAO Science Archive, http://ssc.spitzer.caltech.edu/fls/). The overall quality of the images is high. The measured positions of sources detected in the images have rms uncertainties in their absolute positions on the order of 0.35" with possible systematic offsets on the order of 0.1", depending on the reference frame of comparison. The relative astrometric accuracy is much better than 1/10 of an arcsecond. Typical delivered image quality in the images is 1.1" full width at half-maximum. The images are relatively deep, since they reach a median 5{sigma} depth limiting magnitude of R=25.5 (Vega) as measured within a 1.35 FWHM aperture, for which the signal-to-noise ratio (S/N) is maximal. Catalogs have been extracted with SExtractor, using thresholds in area and flux for which the number of false detections is below 1% at R=25. Only sources with S/N&gt;3 have been retained in the final catalogs. Comparing the galaxy number counts from our images with those of deeper R-band surveys, we estimate that our observations are 50% complete at R=24.5. These limits in depth are sufficient to identify a substantial fraction of the infrared sources that will be detected by Spitzer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1#1</TD>
            <TD>2011-09-14T19:42:07Z</TD>
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            <TD>16-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/128/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/128/1 [2]</TD>
            <TD>First Look Survey: NOAO R-band Mosaic (Fadda+, 2004)</TD>
            <TD>We present R-band images covering more than 11 square degrees of sky that were obtained in preparation for the Spitzer Space Telescope First-Look Survey (FLS). The FLS was designed to characterize the mid-infrared sky at depths 2 orders of magnitude deeper than previous surveys. The extragalactic component is the first cosmological survey done with Spitzer. Source catalogs extracted from the R-band images are also presented. The R-band images were obtained using the Mosaic-1 camera on the 4m Mayall Telescope of the Kitt Peak National Observatory. Two relatively large regions of the sky were observed to modest depth: the main FLS extragalactic field (17h18m00s, +59{deg}30'00.0"[J2000]; l=88.3{deg}, b=+34.9{deg}) and the ELAIS-N1 field (16h10m01s, +54{deg}30'36.0"; l=84.2{deg}, b=+44.9{deg}). While both these fields were in early plans for the FLS, only a single deep-pointing test observation was made at the ELAIS-N1 location. The larger Legacy program SWIRE will include this region among its surveyed areas. The data products of our KPNO imaging (images and object catalogs) are made available to the community through the World Wide Web (via the Spitzer Science Center and NOAO Science Archive, http://ssc.spitzer.caltech.edu/fls/). The overall quality of the images is high. The measured positions of sources detected in the images have rms uncertainties in their absolute positions on the order of 0.35" with possible systematic offsets on the order of 0.1", depending on the reference frame of comparison. The relative astrometric accuracy is much better than 1/10 of an arcsecond. Typical delivered image quality in the images is 1.1" full width at half-maximum. The images are relatively deep, since they reach a median 5{sigma} depth limiting magnitude of R=25.5 (Vega) as measured within a 1.35 FWHM aperture, for which the signal-to-noise ratio (S/N) is maximal. Catalogs have been extracted with SExtractor, using thresholds in area and flux for which the number of false detections is below 1% at R=25. Only sources with S/N&gt;3 have been retained in the final catalogs. Comparing the galaxy number counts from our images with those of deeper R-band surveys, we estimate that our observations are 50% complete at R=24.5. These limits in depth are sufficient to identify a substantial fraction of the infrared sources that will be detected by Spitzer.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1#2</TD>
            <TD>2011-09-14T19:42:07Z</TD>
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            <TD>16-Jun-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/128/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/128/1&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/128/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/440/61 [1]</TD>
            <TD>FORS spectroscopy of HDFS galaxies (Rigopoulou+, 2005)</TD>
            <TD>Table 2 : IDs and photometric data for the spectroscopic targets. For each galaxy coordinates (J2000), IDs and U,B,V,R,I,J,H,K photometry is given. Table 3: spectroscopic redshifts for each target together with the detected emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61#1</TD>
            <TD>2011-09-14T19:42:57Z</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/440/61</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/440/61</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/61</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/440/61 [2]</TD>
            <TD>FORS spectroscopy of HDFS galaxies (Rigopoulou+, 2005)</TD>
            <TD>Table 2 : IDs and photometric data for the spectroscopic targets. For each galaxy coordinates (J2000), IDs and U,B,V,R,I,J,H,K photometry is given. Table 3: spectroscopic redshifts for each target together with the detected emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61#2</TD>
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            <TD>12-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/440/61&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/61</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/440/61 [1]</TD>
            <TD>FORS spectroscopy of HDFS galaxies (Rigopoulou+, 2005)</TD>
            <TD>Table 2 : IDs and photometric data for the spectroscopic targets. For each galaxy coordinates (J2000), IDs and U,B,V,R,I,J,H,K photometry is given. Table 3: spectroscopic redshifts for each target together with the detected emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61#1</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/440/61</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/440/61</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/61</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/440/61 [2]</TD>
            <TD>FORS spectroscopy of HDFS galaxies (Rigopoulou+, 2005)</TD>
            <TD>Table 2 : IDs and photometric data for the spectroscopic targets. For each galaxy coordinates (J2000), IDs and U,B,V,R,I,J,H,K photometry is given. Table 3: spectroscopic redshifts for each target together with the detected emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61#2</TD>
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            <TD>12-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/440/61&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/61</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/440/61 [1]</TD>
            <TD>FORS spectroscopy of HDFS galaxies (Rigopoulou+, 2005)</TD>
            <TD>Table 2 : IDs and photometric data for the spectroscopic targets. For each galaxy coordinates (J2000), IDs and U,B,V,R,I,J,H,K photometry is given. Table 3: spectroscopic redshifts for each target together with the detected emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61#1</TD>
            <TD>2011-09-14T19:42:57Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/440/61</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/61</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/440/61 [2]</TD>
            <TD>FORS spectroscopy of HDFS galaxies (Rigopoulou+, 2005)</TD>
            <TD>Table 2 : IDs and photometric data for the spectroscopic targets. For each galaxy coordinates (J2000), IDs and U,B,V,R,I,J,H,K photometry is given. Table 3: spectroscopic redshifts for each target together with the detected emission lines.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61#2</TD>
            <TD>2011-09-14T19:42:57Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/440/61</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/440/61&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/440/61</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/719/1104 [1]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#1</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/719/1104</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/719/1104 [2]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#2</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/719/1104 [table4]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#table4</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/719/1104 [table3]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#table3</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/719/1104 [sfcdata]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#sfcdata</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/719/1104 [1]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#1</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/719/1104</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/719/1104 [2]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#2</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/719/1104 [table4]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#table4</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/719/1104 [table3]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#table3</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/719/1104 [sfcdata]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#sfcdata</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/719/1104 [1]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#1</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/719/1104</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/719/1104 [2]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#2</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/719/1104 [table4]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#table4</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/719/1104 [table3]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#table3</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/719/1104 [sfcdata]</TD>
            <TD>Massive star forming complexes in GLIMPSE (Rahman+, 2010)</TD>
            <TD>In Paper I (Murray &amp; Rahman, 2010, Cat. J/ApJ/709/424), we divided the total flux of the WMAP regions along a given line of sight based on various distance determinations (radio recombination lines, molecular absorption lines, and stellar distances). Using this division, one-third of the Galactic free-free emission arises from 14 discrete WMAP sources. These sources contain more than one-third of the O star population of the Galaxy. Here, we investigate in more detail, using additional radial velocities, the 13 most luminous free-free sources in the Galaxy from Paper I.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104#sfcdata</TD>
            <TD>2012-12-11T13:13:54Z</TD>
            <TD>#HII_regions#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/719/1104</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/719/1104&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/719/1104</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/530/A28 [1]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#1</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/530/A28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/530/A28 [2]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#2</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/530/A28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/530/A28 [targets]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#targets</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/530/A28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/530/A28 [tablea1]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#tablea1</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/530/A28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/530/A28 [1]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#1</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/530/A28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/530/A28 [2]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#2</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/530/A28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/530/A28 [targets]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#targets</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/530/A28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/530/A28 [tablea1]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#tablea1</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/530/A28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/530/A28 [1]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#1</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/530/A28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/530/A28 [2]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#2</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/530/A28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/530/A28 [targets]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#targets</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/530/A28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/530/A28 [tablea1]</TD>
            <TD>Priority targets for the MUCHFUSS project (Geier+, 2011)</TD>
            <TD>The project Massive Unseen Companions to Hot Faint Underluminous Stars from SDSS (MUCHFUSS) aims at finding sdBs with compact companions like supermassive white dwarfs (M&gt;1.0M_{sun}_), neutron stars or black holes. The existence of such systems is predicted by binary evolution theory and recent discoveries indicate that they are likely to exist in our Galaxy. A determination of the orbital parameters is sufficient to put a lower limit on the companion mass by calculating the binary mass function. If this lower limit exceeds the Chandrasekhar mass and no sign of a companion is visible in the spectra, the existence of a massive compact companion is proven without the need for any additional assumptions. We identified about 1100 hot subdwarf stars from the SDSS by colour selection and visual inspection of their spectra. Stars with high velocities have been reobserved and individual SDSS spectra have been analysed. In total 127 radial velocity variable subdwarfs have been discovered. Binaries with high RV shifts and binaries with moderate shifts within short timespans have the highest probability of hosting massive compact companions. Atmospheric parameters of 69 hot subdwarfs in these binary systems have been determined by means of a quantitative spectral analysis. The atmospheric parameter distribution of the selected sample does not differ from previously studied samples of hot subdwarfs. The systems are considered the best candidates to search for massive compact companions by follow-up time resolved spectroscopy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28#tablea1</TD>
            <TD>2013-01-09T09:04:08Z</TD>
            <TD>#Binaries:spectroscopic#Stars#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2011</TD>
            <TD>ivo://CDS.VizieR/J/A+A/530/A28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/530/A28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/530/A28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/405/94 [1]</TD>
            <TD>Far-infrared emission from 5 galaxy clusters (Wise+ 1993)</TD>
            <TD>We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94#1</TD>
            <TD>2011-09-14T18:45:58Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/405/94</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/94</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/405/94 [2]</TD>
            <TD>Far-infrared emission from 5 galaxy clusters (Wise+ 1993)</TD>
            <TD>We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94#2</TD>
            <TD>2011-09-14T18:45:58Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/405/94&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/94</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/405/94 [table3]</TD>
            <TD>Far-infrared emission from 5 galaxy clusters (Wise+ 1993)</TD>
            <TD>We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94#table3</TD>
            <TD>2011-09-14T18:45:58Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/405/94&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/94</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/405/94 [1]</TD>
            <TD>Far-infrared emission from 5 galaxy clusters (Wise+ 1993)</TD>
            <TD>We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94#1</TD>
            <TD>2011-09-14T18:45:58Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/405/94</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/94</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/405/94 [2]</TD>
            <TD>Far-infrared emission from 5 galaxy clusters (Wise+ 1993)</TD>
            <TD>We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94#2</TD>
            <TD>2011-09-14T18:45:58Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/405/94&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/94</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/405/94 [table3]</TD>
            <TD>Far-infrared emission from 5 galaxy clusters (Wise+ 1993)</TD>
            <TD>We have analyzed IRAS image data using a random position, multiple-aperture photometry method to study diffuse far-infrared emission for a sample of 56 clusters of galaxies at 60 and 100um. Five of the clusters in the sample exhibit excess far-infrared emission, but at low levels of significance. For A496 (Perseus) and MKW 1, this emission appears to be associated with a strong point source: in A2344, the observed excess is probably due to a foreground cirrus cloud. Two clusters, A262 and A2670, show evidence for extended diffuse emission. This emission is unlikely to be due to point sources associated with the clusters. In these two clusters, the diffuse emission shows evidence of being extended along the cluster's major axis. Far-infrared maps at 60 and 100um are presented for these five clusters. We find that contamination due to diffuse Galactic cirrus represents the major source of uncertainty in the measurement of far-infrared emission. The mean cluster fluxes for the sample as a whole are 44 and 107mJy for a 4' diameter aperture at 60 and 100um, respectively. The corresponding fluxes for a 10' diameter aperture are 138 and 253mJy at 60 and 100um. Photometry for the entire sample shows statistical evidence for excess emission at 60um associated with clusters in apertures 4' and 10' in diameter. This result is unlikely to be caused by random sampling errors. The flux distributions are analyzed for evidence that excess far-infrared radiation correlates with cluster environmental characteristics. Although we find evidence that poorer X-ray clusters are stronger far-infrared emitters, this result is tentative owing to the small sample sizes involved. The far-infrared luminosities, dust temperatures, and dust masses which these results imply are also presented. Finally, the origin and possible heating mechanism for dust in the intracluster medium is discussed.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94#table3</TD>
            <TD>2011-09-14T18:45:58Z</TD>
            <TD>#Clusters_of_galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Feb-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/405/94</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/405/94&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/405/94</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/196 [1]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#1</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/196</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/196 [2]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#2</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/196&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/196 [south]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#south</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/196&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/196 [north]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#north</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/196&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/196 [1]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#1</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/196</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/196 [2]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#2</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/196&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/196 [south]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#south</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/196&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/196 [north]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#north</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/196&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/196 [1]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#1</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/196</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/196 [2]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#2</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/196&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/196 [south]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#south</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/196&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/196 [north]</TD>
            <TD>Shakhbazian compact groups of galaxies (Stoll+ 1993-97)</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (see cat. &lt;VII/89&gt;). This catalogue provides accurate positions of individual galaxies in the groups; photometrical properties of the Southern sky (delta not greater than +2{deg}30') are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. The catalogue contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: =&gt; No data for groups 001 (there were already published data by other authors), 206 (could not be re-identified) 241 (could not be re-identified) 252 (is identical with 214), 301 (could not be re-identified) 353 (could not be re-identified) =&gt; Group 328 was published twice (in North and South) =&gt; Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/196#north</TD>
            <TD>2011-09-14T18:46:28Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-1998</TD>
            <TD>ivo://CDS.VizieR/VII/196</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/196&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/196</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/338/813 [1]</TD>
            <TD>Galaxy clusters {sigma}-T relationship (Wu+ 1998)</TD>
            <TD>This is a sample of 149 galaxy clusters for which both the X-ray determined temperature T of the intracluster gas and the optical measured velocity dispersion {sigma} of the cluster galaxies have been available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/338/813#1</TD>
            <TD>2011-09-14T18:46:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/338/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/338/813</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/338/813</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/338/813 [2]</TD>
            <TD>Galaxy clusters {sigma}-T relationship (Wu+ 1998)</TD>
            <TD>This is a sample of 149 galaxy clusters for which both the X-ray determined temperature T of the intracluster gas and the optical measured velocity dispersion {sigma} of the cluster galaxies have been available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/338/813#2</TD>
            <TD>2011-09-14T18:46:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/338/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/338/813&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/338/813</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/338/813 [1]</TD>
            <TD>Galaxy clusters {sigma}-T relationship (Wu+ 1998)</TD>
            <TD>This is a sample of 149 galaxy clusters for which both the X-ray determined temperature T of the intracluster gas and the optical measured velocity dispersion {sigma} of the cluster galaxies have been available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/338/813#1</TD>
            <TD>2011-09-14T18:46:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/338/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/338/813</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/338/813</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/338/813 [2]</TD>
            <TD>Galaxy clusters {sigma}-T relationship (Wu+ 1998)</TD>
            <TD>This is a sample of 149 galaxy clusters for which both the X-ray determined temperature T of the intracluster gas and the optical measured velocity dispersion {sigma} of the cluster galaxies have been available.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/338/813#2</TD>
            <TD>2011-09-14T18:46:42Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/338/813</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/338/813&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/338/813</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/339/34 [1]</TD>
            <TD>Bright galaxies from the WENSS minisurvey (de Ruiter+ 1998)</TD>
            <TD>A search for bright galaxies associated with radio sources from the Westerbork Northern Sky Survey (WENSS) minisurvey has been carried out. A galaxy counterpart was found for 402 of almost 10,000 radio sources. Of these a radio and optically complete sample, with a flux density limit at 325MHz of 30mJy and a limiting red magnitude of 16, can be constructed, which contains 119 galaxies. This paper is the first step of a more general study, in which we aim to derive a bright galaxy sample from the entire WENSS survey (which is now available in the public domain) and thus to construct practically definitive local radio luminosity functions of elliptical and spiral galaxies. We briefly describe the WENSS minisurvey, and the steps that are needed for the optical identification of its radio sources. Due to the large numbers of sources involved (over 200,000) completely automated procedures are obviously needed and we discuss these in some detail. It is shown that with modern utilities projects as described here have become quite feasible. Some results (e.g. a preliminary determination of the local radio luminosity function) are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/339/34#1</TD>
            <TD>2011-09-14T18:46:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/339/34</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/339/34</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/339/34</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/339/34 [2]</TD>
            <TD>Bright galaxies from the WENSS minisurvey (de Ruiter+ 1998)</TD>
            <TD>A search for bright galaxies associated with radio sources from the Westerbork Northern Sky Survey (WENSS) minisurvey has been carried out. A galaxy counterpart was found for 402 of almost 10,000 radio sources. Of these a radio and optically complete sample, with a flux density limit at 325MHz of 30mJy and a limiting red magnitude of 16, can be constructed, which contains 119 galaxies. This paper is the first step of a more general study, in which we aim to derive a bright galaxy sample from the entire WENSS survey (which is now available in the public domain) and thus to construct practically definitive local radio luminosity functions of elliptical and spiral galaxies. We briefly describe the WENSS minisurvey, and the steps that are needed for the optical identification of its radio sources. Due to the large numbers of sources involved (over 200,000) completely automated procedures are obviously needed and we discuss these in some detail. It is shown that with modern utilities projects as described here have become quite feasible. Some results (e.g. a preliminary determination of the local radio luminosity function) are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/339/34#2</TD>
            <TD>2011-09-14T18:46:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/339/34</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/339/34&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/339/34</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/339/34 [1]</TD>
            <TD>Bright galaxies from the WENSS minisurvey (de Ruiter+ 1998)</TD>
            <TD>A search for bright galaxies associated with radio sources from the Westerbork Northern Sky Survey (WENSS) minisurvey has been carried out. A galaxy counterpart was found for 402 of almost 10,000 radio sources. Of these a radio and optically complete sample, with a flux density limit at 325MHz of 30mJy and a limiting red magnitude of 16, can be constructed, which contains 119 galaxies. This paper is the first step of a more general study, in which we aim to derive a bright galaxy sample from the entire WENSS survey (which is now available in the public domain) and thus to construct practically definitive local radio luminosity functions of elliptical and spiral galaxies. We briefly describe the WENSS minisurvey, and the steps that are needed for the optical identification of its radio sources. Due to the large numbers of sources involved (over 200,000) completely automated procedures are obviously needed and we discuss these in some detail. It is shown that with modern utilities projects as described here have become quite feasible. Some results (e.g. a preliminary determination of the local radio luminosity function) are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/339/34#1</TD>
            <TD>2011-09-14T18:46:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/339/34</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/339/34</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/339/34</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/339/34 [2]</TD>
            <TD>Bright galaxies from the WENSS minisurvey (de Ruiter+ 1998)</TD>
            <TD>A search for bright galaxies associated with radio sources from the Westerbork Northern Sky Survey (WENSS) minisurvey has been carried out. A galaxy counterpart was found for 402 of almost 10,000 radio sources. Of these a radio and optically complete sample, with a flux density limit at 325MHz of 30mJy and a limiting red magnitude of 16, can be constructed, which contains 119 galaxies. This paper is the first step of a more general study, in which we aim to derive a bright galaxy sample from the entire WENSS survey (which is now available in the public domain) and thus to construct practically definitive local radio luminosity functions of elliptical and spiral galaxies. We briefly describe the WENSS minisurvey, and the steps that are needed for the optical identification of its radio sources. Due to the large numbers of sources involved (over 200,000) completely automated procedures are obviously needed and we discuss these in some detail. It is shown that with modern utilities projects as described here have become quite feasible. Some results (e.g. a preliminary determination of the local radio luminosity function) are presented.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/339/34#2</TD>
            <TD>2011-09-14T18:46:45Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/A+A/339/34</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/339/34&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/339/34</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/104/2078 [1]</TD>
            <TD>cD Galaxy in Abell 2107 (Oegerle+ 1992)</TD>
            <TD>As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078#1</TD>
            <TD>2011-09-14T18:47:48Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/104/2078</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/2078</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/104/2078 [2]</TD>
            <TD>cD Galaxy in Abell 2107 (Oegerle+ 1992)</TD>
            <TD>As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078#2</TD>
            <TD>2011-09-14T18:47:48Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/104/2078&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/2078</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/104/2078 [table1]</TD>
            <TD>cD Galaxy in Abell 2107 (Oegerle+ 1992)</TD>
            <TD>As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078#table1</TD>
            <TD>2011-09-14T18:47:48Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/104/2078&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/2078</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/104/2078 [1]</TD>
            <TD>cD Galaxy in Abell 2107 (Oegerle+ 1992)</TD>
            <TD>As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078#1</TD>
            <TD>2011-09-14T18:47:48Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/104/2078</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/2078</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/104/2078 [2]</TD>
            <TD>cD Galaxy in Abell 2107 (Oegerle+ 1992)</TD>
            <TD>As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078#2</TD>
            <TD>2011-09-14T18:47:48Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/104/2078&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/2078</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/104/2078 [table1]</TD>
            <TD>cD Galaxy in Abell 2107 (Oegerle+ 1992)</TD>
            <TD>As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078#table1</TD>
            <TD>2011-09-14T18:47:48Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/104/2078&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/2078</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/104/2078 [1]</TD>
            <TD>cD Galaxy in Abell 2107 (Oegerle+ 1992)</TD>
            <TD>As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078#1</TD>
            <TD>2011-09-14T18:47:48Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/104/2078</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/2078</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/104/2078 [2]</TD>
            <TD>cD Galaxy in Abell 2107 (Oegerle+ 1992)</TD>
            <TD>As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078#2</TD>
            <TD>2011-09-14T18:47:48Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/104/2078&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/2078</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/104/2078 [table1]</TD>
            <TD>cD Galaxy in Abell 2107 (Oegerle+ 1992)</TD>
            <TD>As part of a program to study the kinematics of cD clusters of galaxies, we have measured the radial velocities of 75 galaxies in the field of Abell 2107. Sixty-eight of these galaxies are cluster members. The mean observed velocity of A2105 is 12335 +/- 86 km/s and the velocity dispersion is 672 [+67,-52] km/s. The cD galaxy has a peculiar velocity of 270 km/s with respect to the cluster mean. The distribution of velocities is well fitted by a Gaussian, but the velocities are spatially correlated. We have investigated simple two-body subcluster models for A2107, which are consistent with the observed data and account for the peculiar velocity of the cD galaxy. Alternatively, the spatial distribution of velocities is also consistent with rotation of a single cluster at the 98% confidence level. However, the pure rotation model fails to explain the peculiar velocity of the cD galaxy, which lies at the center of the cluster.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078#table1</TD>
            <TD>2011-09-14T18:47:48Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-1994</TD>
            <TD>ivo://CDS.VizieR/J/AJ/104/2078</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/104/2078&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/104/2078</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/1840 [1]</TD>
            <TD>BV photometry in Carina dwarf galaxy (Hurley-Keller+ 1998)</TD>
            <TD>We have analyzed deep B and V photometry of the Carina dwarf spheroidal galaxy reaching below the old main-sequence turnoff to V~25. Using simulated color-magnitude diagrams to model a range of star formation scenarios, we have extracted a detailed, global star formation history. Carina experienced three significant episodes of star formation at ~15, 7, and 3Gyr. Contrary to the generic picture of galaxy evolution, however, the bulk of star formation, at least 50%, occurred during the episode 7Gyr ago, which may have lasted as long as 2Gyr. For unknown reasons, Carina formed only 10%-20% of its stars at an ancient epoch and then remained quiescent for more than 4 Gyr. The remainder (~30%) formed relatively recently, only 3Gyr ago. Interest in the local population of dwarf galaxies has increased lately because of their potential importance in the understanding of faint galaxy counts. We surmise that objects like Carina, which exhibits the most extreme episodic behavior of any of the dwarf spheroidal companions to the Galaxy, are capable of contributing to the observed excess of blue galaxies at B~24 only if the star formation occurred instantaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1840#1</TD>
            <TD>2011-09-14T18:48:03Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/1840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/1840 [2]</TD>
            <TD>BV photometry in Carina dwarf galaxy (Hurley-Keller+ 1998)</TD>
            <TD>We have analyzed deep B and V photometry of the Carina dwarf spheroidal galaxy reaching below the old main-sequence turnoff to V~25. Using simulated color-magnitude diagrams to model a range of star formation scenarios, we have extracted a detailed, global star formation history. Carina experienced three significant episodes of star formation at ~15, 7, and 3Gyr. Contrary to the generic picture of galaxy evolution, however, the bulk of star formation, at least 50%, occurred during the episode 7Gyr ago, which may have lasted as long as 2Gyr. For unknown reasons, Carina formed only 10%-20% of its stars at an ancient epoch and then remained quiescent for more than 4 Gyr. The remainder (~30%) formed relatively recently, only 3Gyr ago. Interest in the local population of dwarf galaxies has increased lately because of their potential importance in the understanding of faint galaxy counts. We surmise that objects like Carina, which exhibits the most extreme episodic behavior of any of the dwarf spheroidal companions to the Galaxy, are capable of contributing to the observed excess of blue galaxies at B~24 only if the star formation occurred instantaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1840#2</TD>
            <TD>2011-09-14T18:48:03Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/1840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/115/1840 [1]</TD>
            <TD>BV photometry in Carina dwarf galaxy (Hurley-Keller+ 1998)</TD>
            <TD>We have analyzed deep B and V photometry of the Carina dwarf spheroidal galaxy reaching below the old main-sequence turnoff to V~25. Using simulated color-magnitude diagrams to model a range of star formation scenarios, we have extracted a detailed, global star formation history. Carina experienced three significant episodes of star formation at ~15, 7, and 3Gyr. Contrary to the generic picture of galaxy evolution, however, the bulk of star formation, at least 50%, occurred during the episode 7Gyr ago, which may have lasted as long as 2Gyr. For unknown reasons, Carina formed only 10%-20% of its stars at an ancient epoch and then remained quiescent for more than 4 Gyr. The remainder (~30%) formed relatively recently, only 3Gyr ago. Interest in the local population of dwarf galaxies has increased lately because of their potential importance in the understanding of faint galaxy counts. We surmise that objects like Carina, which exhibits the most extreme episodic behavior of any of the dwarf spheroidal companions to the Galaxy, are capable of contributing to the observed excess of blue galaxies at B~24 only if the star formation occurred instantaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1840#1</TD>
            <TD>2011-09-14T18:48:03Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/115/1840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/115/1840 [2]</TD>
            <TD>BV photometry in Carina dwarf galaxy (Hurley-Keller+ 1998)</TD>
            <TD>We have analyzed deep B and V photometry of the Carina dwarf spheroidal galaxy reaching below the old main-sequence turnoff to V~25. Using simulated color-magnitude diagrams to model a range of star formation scenarios, we have extracted a detailed, global star formation history. Carina experienced three significant episodes of star formation at ~15, 7, and 3Gyr. Contrary to the generic picture of galaxy evolution, however, the bulk of star formation, at least 50%, occurred during the episode 7Gyr ago, which may have lasted as long as 2Gyr. For unknown reasons, Carina formed only 10%-20% of its stars at an ancient epoch and then remained quiescent for more than 4 Gyr. The remainder (~30%) formed relatively recently, only 3Gyr ago. Interest in the local population of dwarf galaxies has increased lately because of their potential importance in the understanding of faint galaxy counts. We surmise that objects like Carina, which exhibits the most extreme episodic behavior of any of the dwarf spheroidal companions to the Galaxy, are capable of contributing to the observed excess of blue galaxies at B~24 only if the star formation occurred instantaneously.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1840#2</TD>
            <TD>2011-09-14T18:48:03Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/AJ/115/1840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/115/1840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/115/1840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/113/1 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. III. (Ellingson+ 1997)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 1621.5+2640 (z=0.4275) and MS 0302.7+1658 (z=0.4245), is presented as part of the Canadian Network for Observation Cosmology (CNOC) Cluster Redshift Survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover strips cantered on each cluster of approximately 23.3'x9.0', and 7.9'x9.0', for MS 1621.5+2640 and MS 0302.7+1658, respectively. Redshifts for 371 galaxies, primarily ranging in magnitude from r=20 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/113/1#1</TD>
            <TD>2011-09-14T18:48:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/113/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/113/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/113/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/113/1 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. III. (Ellingson+ 1997)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 1621.5+2640 (z=0.4275) and MS 0302.7+1658 (z=0.4245), is presented as part of the Canadian Network for Observation Cosmology (CNOC) Cluster Redshift Survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover strips cantered on each cluster of approximately 23.3'x9.0', and 7.9'x9.0', for MS 1621.5+2640 and MS 0302.7+1658, respectively. Redshifts for 371 galaxies, primarily ranging in magnitude from r=20 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/113/1#2</TD>
            <TD>2011-09-14T18:48:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/113/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/113/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/113/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/113/1 [1]</TD>
            <TD>CNOC cluster redshift survey catalogs. III. (Ellingson+ 1997)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 1621.5+2640 (z=0.4275) and MS 0302.7+1658 (z=0.4245), is presented as part of the Canadian Network for Observation Cosmology (CNOC) Cluster Redshift Survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover strips cantered on each cluster of approximately 23.3'x9.0', and 7.9'x9.0', for MS 1621.5+2640 and MS 0302.7+1658, respectively. Redshifts for 371 galaxies, primarily ranging in magnitude from r=20 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/113/1#1</TD>
            <TD>2011-09-14T18:48:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/113/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/113/1</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/113/1</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/113/1 [2]</TD>
            <TD>CNOC cluster redshift survey catalogs. III. (Ellingson+ 1997)</TD>
            <TD>A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 1621.5+2640 (z=0.4275) and MS 0302.7+1658 (z=0.4245), is presented as part of the Canadian Network for Observation Cosmology (CNOC) Cluster Redshift Survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover strips cantered on each cluster of approximately 23.3'x9.0', and 7.9'x9.0', for MS 1621.5+2640 and MS 0302.7+1658, respectively. Redshifts for 371 galaxies, primarily ranging in magnitude from r=20 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/113/1#2</TD>
            <TD>2011-09-14T18:48:05Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Aug-1998</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/113/1</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/113/1&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/113/1</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/600/L99 [1]</TD>
            <TD>Colours of z~6 galaxies in GOODS (Dickinson+, 2004)</TD>
            <TD>We report early results on galaxies at z~6 selected from Hubble Space Telescope imaging for the Great Observatories Origins Deep Survey. Spectroscopy of one object with the Advanced Camera for Surveys grism and from the Keck and Very Large Telescope observatories shows a strong continuum break and asymmetric line emission, identified as Ly{alpha} at z=5.83. We find only five spatially extended candidates with signal-to-noise ratios greater than 10, two of which have spectroscopic confirmation. This is much fewer than would be expected if galaxies at z=6 had the same luminosity function as those at z=3. There are many fainter candidates, but we expect substantial contamination from foreground interlopers and spurious detections. Our best estimates favor a z=6 galaxy population with fainter luminosities, higher space density, and similar comoving ultraviolet emissivity to that at z=3, but this depends critically on counts at fluxes fainter than those reliably probed by the current data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99#1</TD>
            <TD>2011-09-14T19:32:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/600/L99</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/600/L99</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/600/L99 [2]</TD>
            <TD>Colours of z~6 galaxies in GOODS (Dickinson+, 2004)</TD>
            <TD>We report early results on galaxies at z~6 selected from Hubble Space Telescope imaging for the Great Observatories Origins Deep Survey. Spectroscopy of one object with the Advanced Camera for Surveys grism and from the Keck and Very Large Telescope observatories shows a strong continuum break and asymmetric line emission, identified as Ly{alpha} at z=5.83. We find only five spatially extended candidates with signal-to-noise ratios greater than 10, two of which have spectroscopic confirmation. This is much fewer than would be expected if galaxies at z=6 had the same luminosity function as those at z=3. There are many fainter candidates, but we expect substantial contamination from foreground interlopers and spurious detections. Our best estimates favor a z=6 galaxy population with fainter luminosities, higher space density, and similar comoving ultraviolet emissivity to that at z=3, but this depends critically on counts at fluxes fainter than those reliably probed by the current data.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99#2</TD>
            <TD>2011-09-14T19:32:19Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Feb-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/600/L99</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/600/L99&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/600/L99</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/591/53 [1]</TD>
            <TD>I photometry of Cl 0024+16 (Treu+, 2003)</TD>
            <TD>We describe a new wide-field Hubble Space Telescope survey of the galaxy cluster Cl 0024+16 (z~0.4) consisting of a sparsely sampled mosaic of 39 Wide Field Planetary Camera 2 images that extends to a cluster radius of ~5Mpc. Together with extensive ground-based spectroscopy taken from the literature, augmented with over a hundred newly determined redshifts, this unique data set enables us to examine environmental influences on the properties of cluster members from the inner core to well beyond the virial radius (~1.7Mpc). We catalog photometric measures for 22000 objects to I&gt;~25 and assign morphological types for 2181 to I=22.5, of which 195 are spectroscopically confirmed cluster members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53#1</TD>
            <TD>2011-09-14T19:33:21Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/591/53</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/53</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/591/53 [2]</TD>
            <TD>I photometry of Cl 0024+16 (Treu+, 2003)</TD>
            <TD>We describe a new wide-field Hubble Space Telescope survey of the galaxy cluster Cl 0024+16 (z~0.4) consisting of a sparsely sampled mosaic of 39 Wide Field Planetary Camera 2 images that extends to a cluster radius of ~5Mpc. Together with extensive ground-based spectroscopy taken from the literature, augmented with over a hundred newly determined redshifts, this unique data set enables us to examine environmental influences on the properties of cluster members from the inner core to well beyond the virial radius (~1.7Mpc). We catalog photometric measures for 22000 objects to I&gt;~25 and assign morphological types for 2181 to I=22.5, of which 195 are spectroscopically confirmed cluster members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53#2</TD>
            <TD>2011-09-14T19:33:21Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/591/53&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/53</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/591/53 [1]</TD>
            <TD>I photometry of Cl 0024+16 (Treu+, 2003)</TD>
            <TD>We describe a new wide-field Hubble Space Telescope survey of the galaxy cluster Cl 0024+16 (z~0.4) consisting of a sparsely sampled mosaic of 39 Wide Field Planetary Camera 2 images that extends to a cluster radius of ~5Mpc. Together with extensive ground-based spectroscopy taken from the literature, augmented with over a hundred newly determined redshifts, this unique data set enables us to examine environmental influences on the properties of cluster members from the inner core to well beyond the virial radius (~1.7Mpc). We catalog photometric measures for 22000 objects to I&gt;~25 and assign morphological types for 2181 to I=22.5, of which 195 are spectroscopically confirmed cluster members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53#1</TD>
            <TD>2011-09-14T19:33:21Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/591/53</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/53</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/591/53 [2]</TD>
            <TD>I photometry of Cl 0024+16 (Treu+, 2003)</TD>
            <TD>We describe a new wide-field Hubble Space Telescope survey of the galaxy cluster Cl 0024+16 (z~0.4) consisting of a sparsely sampled mosaic of 39 Wide Field Planetary Camera 2 images that extends to a cluster radius of ~5Mpc. Together with extensive ground-based spectroscopy taken from the literature, augmented with over a hundred newly determined redshifts, this unique data set enables us to examine environmental influences on the properties of cluster members from the inner core to well beyond the virial radius (~1.7Mpc). We catalog photometric measures for 22000 objects to I&gt;~25 and assign morphological types for 2181 to I=22.5, of which 195 are spectroscopically confirmed cluster members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53#2</TD>
            <TD>2011-09-14T19:33:21Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/591/53&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/53</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/591/53 [1]</TD>
            <TD>I photometry of Cl 0024+16 (Treu+, 2003)</TD>
            <TD>We describe a new wide-field Hubble Space Telescope survey of the galaxy cluster Cl 0024+16 (z~0.4) consisting of a sparsely sampled mosaic of 39 Wide Field Planetary Camera 2 images that extends to a cluster radius of ~5Mpc. Together with extensive ground-based spectroscopy taken from the literature, augmented with over a hundred newly determined redshifts, this unique data set enables us to examine environmental influences on the properties of cluster members from the inner core to well beyond the virial radius (~1.7Mpc). We catalog photometric measures for 22000 objects to I&gt;~25 and assign morphological types for 2181 to I=22.5, of which 195 are spectroscopically confirmed cluster members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53#1</TD>
            <TD>2011-09-14T19:33:21Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/591/53</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/53</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/591/53 [2]</TD>
            <TD>I photometry of Cl 0024+16 (Treu+, 2003)</TD>
            <TD>We describe a new wide-field Hubble Space Telescope survey of the galaxy cluster Cl 0024+16 (z~0.4) consisting of a sparsely sampled mosaic of 39 Wide Field Planetary Camera 2 images that extends to a cluster radius of ~5Mpc. Together with extensive ground-based spectroscopy taken from the literature, augmented with over a hundred newly determined redshifts, this unique data set enables us to examine environmental influences on the properties of cluster members from the inner core to well beyond the virial radius (~1.7Mpc). We catalog photometric measures for 22000 objects to I&gt;~25 and assign morphological types for 2181 to I=22.5, of which 195 are spectroscopically confirmed cluster members.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53#2</TD>
            <TD>2011-09-14T19:33:21Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/53</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/591/53&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/53</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/350/1485 [1]</TD>
            <TD>2dFGRS: Radio galaxies properties (Magliocchetti+, 2004)</TD>
            <TD>The clustering properties of local, S_1.4GHz_&gt;=1mJy, radio sources are investigated for a sample of 820 objects drawn from the joint use of the Faint Images of the Radio Sky at 20cm (FIRST, &lt;VIII/71&gt;) and 2dF Galaxy Redshift surveys (&lt;VII/223&gt;, &lt;VII/226&gt;). To this aim, we present 271 new b_J_&lt;=19.45mag spectroscopic counterparts of FIRST radio sources to be added to those already introduced in our previous paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/350/1485#1</TD>
            <TD>2011-09-14T19:36:58Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/350/1485</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/350/1485</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/350/1485</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/350/1485 [2]</TD>
            <TD>2dFGRS: Radio galaxies properties (Magliocchetti+, 2004)</TD>
            <TD>The clustering properties of local, S_1.4GHz_&gt;=1mJy, radio sources are investigated for a sample of 820 objects drawn from the joint use of the Faint Images of the Radio Sky at 20cm (FIRST, &lt;VIII/71&gt;) and 2dF Galaxy Redshift surveys (&lt;VII/223&gt;, &lt;VII/226&gt;). To this aim, we present 271 new b_J_&lt;=19.45mag spectroscopic counterparts of FIRST radio sources to be added to those already introduced in our previous paper.</TD>
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            <TD>ivo://CDS.VizieR/J/MNRAS/350/1485</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/350/1485&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/350/1485</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/350/1485 [1]</TD>
            <TD>2dFGRS: Radio galaxies properties (Magliocchetti+, 2004)</TD>
            <TD>The clustering properties of local, S_1.4GHz_&gt;=1mJy, radio sources are investigated for a sample of 820 objects drawn from the joint use of the Faint Images of the Radio Sky at 20cm (FIRST, &lt;VIII/71&gt;) and 2dF Galaxy Redshift surveys (&lt;VII/223&gt;, &lt;VII/226&gt;). To this aim, we present 271 new b_J_&lt;=19.45mag spectroscopic counterparts of FIRST radio sources to be added to those already introduced in our previous paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/350/1485#1</TD>
            <TD>2011-09-14T19:36:58Z</TD>
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            <TD>19-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/350/1485</TD>
            <TD />
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            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/350/1485</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/350/1485</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/350/1485 [2]</TD>
            <TD>2dFGRS: Radio galaxies properties (Magliocchetti+, 2004)</TD>
            <TD>The clustering properties of local, S_1.4GHz_&gt;=1mJy, radio sources are investigated for a sample of 820 objects drawn from the joint use of the Faint Images of the Radio Sky at 20cm (FIRST, &lt;VIII/71&gt;) and 2dF Galaxy Redshift surveys (&lt;VII/223&gt;, &lt;VII/226&gt;). To this aim, we present 271 new b_J_&lt;=19.45mag spectroscopic counterparts of FIRST radio sources to be added to those already introduced in our previous paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/350/1485#2</TD>
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            <TD>ivo://CDS.VizieR/J/MNRAS/350/1485</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/350/1485&amp;</TD>
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            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/350/1485</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/350/1485 [1]</TD>
            <TD>2dFGRS: Radio galaxies properties (Magliocchetti+, 2004)</TD>
            <TD>The clustering properties of local, S_1.4GHz_&gt;=1mJy, radio sources are investigated for a sample of 820 objects drawn from the joint use of the Faint Images of the Radio Sky at 20cm (FIRST, &lt;VIII/71&gt;) and 2dF Galaxy Redshift surveys (&lt;VII/223&gt;, &lt;VII/226&gt;). To this aim, we present 271 new b_J_&lt;=19.45mag spectroscopic counterparts of FIRST radio sources to be added to those already introduced in our previous paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
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            <TD>ivo://CDS.VizieR/J/MNRAS/350/1485</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/350/1485</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/350/1485</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/350/1485 [2]</TD>
            <TD>2dFGRS: Radio galaxies properties (Magliocchetti+, 2004)</TD>
            <TD>The clustering properties of local, S_1.4GHz_&gt;=1mJy, radio sources are investigated for a sample of 820 objects drawn from the joint use of the Faint Images of the Radio Sky at 20cm (FIRST, &lt;VIII/71&gt;) and 2dF Galaxy Redshift surveys (&lt;VII/223&gt;, &lt;VII/226&gt;). To this aim, we present 271 new b_J_&lt;=19.45mag spectroscopic counterparts of FIRST radio sources to be added to those already introduced in our previous paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
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            <TD>19-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/350/1485</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/350/1485&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/350/1485</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/1750 [1]</TD>
            <TD>Seyfert population in SSRS2 (Maia+, 2003)</TD>
            <TD>The magnitude-limited catalog of the Southern Sky Redshift Survey (SSRS2, Cat. &lt;J/AJ/116/1&gt;) is used to characterize the properties of galaxies hosting active galactic nuclei (AGNs). Using emission-line ratios, we identify a total of 162 (3%) Seyfert galaxies out of the parent sample with 5399 galaxies. The sample contains 121 Seyfert 2 galaxies and 41 Seyfert 1 galaxies. The SSRS2 Seyfert galaxies are predominantly in spirals of types Sb and earlier or in galaxies with perturbed appearance as the result of strong interactions or mergers. Seyfert galaxies in this sample are twice as common in barred hosts as the non-Seyfert galaxies. By assigning galaxies to groups using a percolation algorithm, we find that the Seyfert galaxies in the SSRS2 are more likely to be found in binary systems when compared with galaxies in the SSRS2 parent sample. However, there is no statistically significant difference between the Seyfert and SSRS2 parent sample when systems with more than two galaxies are considered. The analysis of the present sample suggests that there is a stronger correlation between the presence of the AGN phenomenon with internal properties of galaxies (morphology, presence of bar, luminosity) than with environmental effects (local galaxy density, group velocity dispersion, nearest neighbor distance).</TD>
            <TD>CDS</TD>
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            <TD>21-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1750</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/1750</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1750</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/1750 [2]</TD>
            <TD>Seyfert population in SSRS2 (Maia+, 2003)</TD>
            <TD>The magnitude-limited catalog of the Southern Sky Redshift Survey (SSRS2, Cat. &lt;J/AJ/116/1&gt;) is used to characterize the properties of galaxies hosting active galactic nuclei (AGNs). Using emission-line ratios, we identify a total of 162 (3%) Seyfert galaxies out of the parent sample with 5399 galaxies. The sample contains 121 Seyfert 2 galaxies and 41 Seyfert 1 galaxies. The SSRS2 Seyfert galaxies are predominantly in spirals of types Sb and earlier or in galaxies with perturbed appearance as the result of strong interactions or mergers. Seyfert galaxies in this sample are twice as common in barred hosts as the non-Seyfert galaxies. By assigning galaxies to groups using a percolation algorithm, we find that the Seyfert galaxies in the SSRS2 are more likely to be found in binary systems when compared with galaxies in the SSRS2 parent sample. However, there is no statistically significant difference between the Seyfert and SSRS2 parent sample when systems with more than two galaxies are considered. The analysis of the present sample suggests that there is a stronger correlation between the presence of the AGN phenomenon with internal properties of galaxies (morphology, presence of bar, luminosity) than with environmental effects (local galaxy density, group velocity dispersion, nearest neighbor distance).</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/126/1750</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/1750&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1750</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/1750 [1]</TD>
            <TD>Seyfert population in SSRS2 (Maia+, 2003)</TD>
            <TD>The magnitude-limited catalog of the Southern Sky Redshift Survey (SSRS2, Cat. &lt;J/AJ/116/1&gt;) is used to characterize the properties of galaxies hosting active galactic nuclei (AGNs). Using emission-line ratios, we identify a total of 162 (3%) Seyfert galaxies out of the parent sample with 5399 galaxies. The sample contains 121 Seyfert 2 galaxies and 41 Seyfert 1 galaxies. The SSRS2 Seyfert galaxies are predominantly in spirals of types Sb and earlier or in galaxies with perturbed appearance as the result of strong interactions or mergers. Seyfert galaxies in this sample are twice as common in barred hosts as the non-Seyfert galaxies. By assigning galaxies to groups using a percolation algorithm, we find that the Seyfert galaxies in the SSRS2 are more likely to be found in binary systems when compared with galaxies in the SSRS2 parent sample. However, there is no statistically significant difference between the Seyfert and SSRS2 parent sample when systems with more than two galaxies are considered. The analysis of the present sample suggests that there is a stronger correlation between the presence of the AGN phenomenon with internal properties of galaxies (morphology, presence of bar, luminosity) than with environmental effects (local galaxy density, group velocity dispersion, nearest neighbor distance).</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/126/1750</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/1750</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/1750 [2]</TD>
            <TD>Seyfert population in SSRS2 (Maia+, 2003)</TD>
            <TD>The magnitude-limited catalog of the Southern Sky Redshift Survey (SSRS2, Cat. &lt;J/AJ/116/1&gt;) is used to characterize the properties of galaxies hosting active galactic nuclei (AGNs). Using emission-line ratios, we identify a total of 162 (3%) Seyfert galaxies out of the parent sample with 5399 galaxies. The sample contains 121 Seyfert 2 galaxies and 41 Seyfert 1 galaxies. The SSRS2 Seyfert galaxies are predominantly in spirals of types Sb and earlier or in galaxies with perturbed appearance as the result of strong interactions or mergers. Seyfert galaxies in this sample are twice as common in barred hosts as the non-Seyfert galaxies. By assigning galaxies to groups using a percolation algorithm, we find that the Seyfert galaxies in the SSRS2 are more likely to be found in binary systems when compared with galaxies in the SSRS2 parent sample. However, there is no statistically significant difference between the Seyfert and SSRS2 parent sample when systems with more than two galaxies are considered. The analysis of the present sample suggests that there is a stronger correlation between the presence of the AGN phenomenon with internal properties of galaxies (morphology, presence of bar, luminosity) than with environmental effects (local galaxy density, group velocity dispersion, nearest neighbor distance).</TD>
            <TD>CDS</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/126/1750</TD>
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/1750&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1750</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/126/1750 [1]</TD>
            <TD>Seyfert population in SSRS2 (Maia+, 2003)</TD>
            <TD>The magnitude-limited catalog of the Southern Sky Redshift Survey (SSRS2, Cat. &lt;J/AJ/116/1&gt;) is used to characterize the properties of galaxies hosting active galactic nuclei (AGNs). Using emission-line ratios, we identify a total of 162 (3%) Seyfert galaxies out of the parent sample with 5399 galaxies. The sample contains 121 Seyfert 2 galaxies and 41 Seyfert 1 galaxies. The SSRS2 Seyfert galaxies are predominantly in spirals of types Sb and earlier or in galaxies with perturbed appearance as the result of strong interactions or mergers. Seyfert galaxies in this sample are twice as common in barred hosts as the non-Seyfert galaxies. By assigning galaxies to groups using a percolation algorithm, we find that the Seyfert galaxies in the SSRS2 are more likely to be found in binary systems when compared with galaxies in the SSRS2 parent sample. However, there is no statistically significant difference between the Seyfert and SSRS2 parent sample when systems with more than two galaxies are considered. The analysis of the present sample suggests that there is a stronger correlation between the presence of the AGN phenomenon with internal properties of galaxies (morphology, presence of bar, luminosity) than with environmental effects (local galaxy density, group velocity dispersion, nearest neighbor distance).</TD>
            <TD>CDS</TD>
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            <TD>21-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/AJ/126/1750</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/126/1750</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1750</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/126/1750 [2]</TD>
            <TD>Seyfert population in SSRS2 (Maia+, 2003)</TD>
            <TD>The magnitude-limited catalog of the Southern Sky Redshift Survey (SSRS2, Cat. &lt;J/AJ/116/1&gt;) is used to characterize the properties of galaxies hosting active galactic nuclei (AGNs). Using emission-line ratios, we identify a total of 162 (3%) Seyfert galaxies out of the parent sample with 5399 galaxies. The sample contains 121 Seyfert 2 galaxies and 41 Seyfert 1 galaxies. The SSRS2 Seyfert galaxies are predominantly in spirals of types Sb and earlier or in galaxies with perturbed appearance as the result of strong interactions or mergers. Seyfert galaxies in this sample are twice as common in barred hosts as the non-Seyfert galaxies. By assigning galaxies to groups using a percolation algorithm, we find that the Seyfert galaxies in the SSRS2 are more likely to be found in binary systems when compared with galaxies in the SSRS2 parent sample. However, there is no statistically significant difference between the Seyfert and SSRS2 parent sample when systems with more than two galaxies are considered. The analysis of the present sample suggests that there is a stronger correlation between the presence of the AGN phenomenon with internal properties of galaxies (morphology, presence of bar, luminosity) than with environmental effects (local galaxy density, group velocity dispersion, nearest neighbor distance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T19:37:11Z</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/126/1750</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/126/1750&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/126/1750</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/411/361 [1]</TD>
            <TD>VI photometry of extra-galactic Cepheids (Kanbur+, 2003)</TD>
            <TD>We present the V and I band mean magnitudes for the extra-galactic Cepheids used in the paper (Table 1 in the paper). Column 1 lists out the names of the target galaxy and the Cepheids, column 2 lists out the period (in log P) as adopted from literature, column 3 and 4 are the derived mean V and I band magnitudes, respectively, from the Fourier techniques described in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/411/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/411/361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/411/361</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/411/361 [2]</TD>
            <TD>VI photometry of extra-galactic Cepheids (Kanbur+, 2003)</TD>
            <TD>We present the V and I band mean magnitudes for the extra-galactic Cepheids used in the paper (Table 1 in the paper). Column 1 lists out the names of the target galaxy and the Cepheids, column 2 lists out the period (in log P) as adopted from literature, column 3 and 4 are the derived mean V and I band magnitudes, respectively, from the Fourier techniques described in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T19:39:56Z</TD>
            <TD>#Stars#Stars:variable#</TD>
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            <TD>15-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/411/361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/411/361</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/411/361 [table1]</TD>
            <TD>VI photometry of extra-galactic Cepheids (Kanbur+, 2003)</TD>
            <TD>We present the V and I band mean magnitudes for the extra-galactic Cepheids used in the paper (Table 1 in the paper). Column 1 lists out the names of the target galaxy and the Cepheids, column 2 lists out the period (in log P) as adopted from literature, column 3 and 4 are the derived mean V and I band magnitudes, respectively, from the Fourier techniques described in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361#table1</TD>
            <TD>2011-09-14T19:39:56Z</TD>
            <TD>#Stars#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/411/361&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/411/361</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/411/361 [1]</TD>
            <TD>VI photometry of extra-galactic Cepheids (Kanbur+, 2003)</TD>
            <TD>We present the V and I band mean magnitudes for the extra-galactic Cepheids used in the paper (Table 1 in the paper). Column 1 lists out the names of the target galaxy and the Cepheids, column 2 lists out the period (in log P) as adopted from literature, column 3 and 4 are the derived mean V and I band magnitudes, respectively, from the Fourier techniques described in the paper.</TD>
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            <TD>2011-09-14T19:39:56Z</TD>
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            <TD>ivo://CDS.VizieR/J/A+A/411/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/411/361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/411/361</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/411/361 [2]</TD>
            <TD>VI photometry of extra-galactic Cepheids (Kanbur+, 2003)</TD>
            <TD>We present the V and I band mean magnitudes for the extra-galactic Cepheids used in the paper (Table 1 in the paper). Column 1 lists out the names of the target galaxy and the Cepheids, column 2 lists out the period (in log P) as adopted from literature, column 3 and 4 are the derived mean V and I band magnitudes, respectively, from the Fourier techniques described in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361#2</TD>
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            <TD>15-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/411/361&amp;</TD>
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            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/411/361</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/411/361 [table1]</TD>
            <TD>VI photometry of extra-galactic Cepheids (Kanbur+, 2003)</TD>
            <TD>We present the V and I band mean magnitudes for the extra-galactic Cepheids used in the paper (Table 1 in the paper). Column 1 lists out the names of the target galaxy and the Cepheids, column 2 lists out the period (in log P) as adopted from literature, column 3 and 4 are the derived mean V and I band magnitudes, respectively, from the Fourier techniques described in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361#table1</TD>
            <TD>2011-09-14T19:39:56Z</TD>
            <TD>#Stars#Stars:variable#</TD>
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            <TD>15-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/411/361&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/411/361</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/411/361 [1]</TD>
            <TD>VI photometry of extra-galactic Cepheids (Kanbur+, 2003)</TD>
            <TD>We present the V and I band mean magnitudes for the extra-galactic Cepheids used in the paper (Table 1 in the paper). Column 1 lists out the names of the target galaxy and the Cepheids, column 2 lists out the period (in log P) as adopted from literature, column 3 and 4 are the derived mean V and I band magnitudes, respectively, from the Fourier techniques described in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361#1</TD>
            <TD>2011-09-14T19:39:56Z</TD>
            <TD>#Stars#Stars:variable#</TD>
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            <TD>15-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/411/361</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/411/361</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/411/361 [2]</TD>
            <TD>VI photometry of extra-galactic Cepheids (Kanbur+, 2003)</TD>
            <TD>We present the V and I band mean magnitudes for the extra-galactic Cepheids used in the paper (Table 1 in the paper). Column 1 lists out the names of the target galaxy and the Cepheids, column 2 lists out the period (in log P) as adopted from literature, column 3 and 4 are the derived mean V and I band magnitudes, respectively, from the Fourier techniques described in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361#2</TD>
            <TD>2011-09-14T19:39:56Z</TD>
            <TD>#Stars#Stars:variable#</TD>
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            <TD>15-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/411/361&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/411/361</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/411/361 [table1]</TD>
            <TD>VI photometry of extra-galactic Cepheids (Kanbur+, 2003)</TD>
            <TD>We present the V and I band mean magnitudes for the extra-galactic Cepheids used in the paper (Table 1 in the paper). Column 1 lists out the names of the target galaxy and the Cepheids, column 2 lists out the period (in log P) as adopted from literature, column 3 and 4 are the derived mean V and I band magnitudes, respectively, from the Fourier techniques described in the paper.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361#table1</TD>
            <TD>2011-09-14T19:39:56Z</TD>
            <TD>#Stars#Stars:variable#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>15-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/411/361</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/411/361&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/411/361</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/292/499 [1]</TD>
            <TD>EFAR photometric data (Saglia+, 1997)</TD>
            <TD>We present R-band CCD photometry for 776 galaxies observed in the EFAR (Elliptical FAR away) project. The photometry is compared with photoelectric data, showing that a common zero-point good to better than 1% and a precision of 0.03mag per zero-point have been achieved. We give the circularly averaged surface brightness profiles and the photometric parameters of the 762 program galaxies, D(n) diameters (at 20.5mag/arcsec^2^), half-luminosity radii Re, total magnitudes m_T_, and average effective surface brightnesses &lt;SBe&gt;. More than 80% of the profiles have a global S/N ratio larger than 300. The extrapolation needed to derive total magnitudes is less than 10% for 80% of the fits. More than 80% of the galaxies have mean effective surface brightness larger than the observed sky brightness. In 90% of the profiles the estimate of the contamination of the sky by the galaxy light is less than 1%. We derive total magnitudes and half-luminosity radii to better than 0.15mag and 25%, respectively, for 90% of our sample. In contrast, external comparisons show that data in the literature can be strongly affected by systematic errors due to large extrapolations, small radial range, sky subtraction errors, seeing effects, and the use of a simple R^1/4^ fit. The resulting errors can easily amount to more than 0.5mag in the total magnitudes and 50% in the half-luminosity radii.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499#1</TD>
            <TD>2011-09-14T19:42:20Z</TD>
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            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/292/499</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/292/499</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/292/499 [2]</TD>
            <TD>EFAR photometric data (Saglia+, 1997)</TD>
            <TD>We present R-band CCD photometry for 776 galaxies observed in the EFAR (Elliptical FAR away) project. The photometry is compared with photoelectric data, showing that a common zero-point good to better than 1% and a precision of 0.03mag per zero-point have been achieved. We give the circularly averaged surface brightness profiles and the photometric parameters of the 762 program galaxies, D(n) diameters (at 20.5mag/arcsec^2^), half-luminosity radii Re, total magnitudes m_T_, and average effective surface brightnesses &lt;SBe&gt;. More than 80% of the profiles have a global S/N ratio larger than 300. The extrapolation needed to derive total magnitudes is less than 10% for 80% of the fits. More than 80% of the galaxies have mean effective surface brightness larger than the observed sky brightness. In 90% of the profiles the estimate of the contamination of the sky by the galaxy light is less than 1%. We derive total magnitudes and half-luminosity radii to better than 0.15mag and 25%, respectively, for 90% of our sample. In contrast, external comparisons show that data in the literature can be strongly affected by systematic errors due to large extrapolations, small radial range, sky subtraction errors, seeing effects, and the use of a simple R^1/4^ fit. The resulting errors can easily amount to more than 0.5mag in the total magnitudes and 50% in the half-luminosity radii.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499#2</TD>
            <TD>2011-09-14T19:42:20Z</TD>
            <TD>#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
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            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/292/499&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/292/499</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/292/499 [table4]</TD>
            <TD>EFAR photometric data (Saglia+, 1997)</TD>
            <TD>We present R-band CCD photometry for 776 galaxies observed in the EFAR (Elliptical FAR away) project. The photometry is compared with photoelectric data, showing that a common zero-point good to better than 1% and a precision of 0.03mag per zero-point have been achieved. We give the circularly averaged surface brightness profiles and the photometric parameters of the 762 program galaxies, D(n) diameters (at 20.5mag/arcsec^2^), half-luminosity radii Re, total magnitudes m_T_, and average effective surface brightnesses &lt;SBe&gt;. More than 80% of the profiles have a global S/N ratio larger than 300. The extrapolation needed to derive total magnitudes is less than 10% for 80% of the fits. More than 80% of the galaxies have mean effective surface brightness larger than the observed sky brightness. In 90% of the profiles the estimate of the contamination of the sky by the galaxy light is less than 1%. We derive total magnitudes and half-luminosity radii to better than 0.15mag and 25%, respectively, for 90% of our sample. In contrast, external comparisons show that data in the literature can be strongly affected by systematic errors due to large extrapolations, small radial range, sky subtraction errors, seeing effects, and the use of a simple R^1/4^ fit. The resulting errors can easily amount to more than 0.5mag in the total magnitudes and 50% in the half-luminosity radii.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499#table4</TD>
            <TD>2011-09-14T19:42:20Z</TD>
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            <TD>04-Oct-1999</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/292/499&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/292/499</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/292/499 [1]</TD>
            <TD>EFAR photometric data (Saglia+, 1997)</TD>
            <TD>We present R-band CCD photometry for 776 galaxies observed in the EFAR (Elliptical FAR away) project. The photometry is compared with photoelectric data, showing that a common zero-point good to better than 1% and a precision of 0.03mag per zero-point have been achieved. We give the circularly averaged surface brightness profiles and the photometric parameters of the 762 program galaxies, D(n) diameters (at 20.5mag/arcsec^2^), half-luminosity radii Re, total magnitudes m_T_, and average effective surface brightnesses &lt;SBe&gt;. More than 80% of the profiles have a global S/N ratio larger than 300. The extrapolation needed to derive total magnitudes is less than 10% for 80% of the fits. More than 80% of the galaxies have mean effective surface brightness larger than the observed sky brightness. In 90% of the profiles the estimate of the contamination of the sky by the galaxy light is less than 1%. We derive total magnitudes and half-luminosity radii to better than 0.15mag and 25%, respectively, for 90% of our sample. In contrast, external comparisons show that data in the literature can be strongly affected by systematic errors due to large extrapolations, small radial range, sky subtraction errors, seeing effects, and the use of a simple R^1/4^ fit. The resulting errors can easily amount to more than 0.5mag in the total magnitudes and 50% in the half-luminosity radii.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499#1</TD>
            <TD>2011-09-14T19:42:20Z</TD>
            <TD>#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
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            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/292/499</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/292/499</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/292/499 [2]</TD>
            <TD>EFAR photometric data (Saglia+, 1997)</TD>
            <TD>We present R-band CCD photometry for 776 galaxies observed in the EFAR (Elliptical FAR away) project. The photometry is compared with photoelectric data, showing that a common zero-point good to better than 1% and a precision of 0.03mag per zero-point have been achieved. We give the circularly averaged surface brightness profiles and the photometric parameters of the 762 program galaxies, D(n) diameters (at 20.5mag/arcsec^2^), half-luminosity radii Re, total magnitudes m_T_, and average effective surface brightnesses &lt;SBe&gt;. More than 80% of the profiles have a global S/N ratio larger than 300. The extrapolation needed to derive total magnitudes is less than 10% for 80% of the fits. More than 80% of the galaxies have mean effective surface brightness larger than the observed sky brightness. In 90% of the profiles the estimate of the contamination of the sky by the galaxy light is less than 1%. We derive total magnitudes and half-luminosity radii to better than 0.15mag and 25%, respectively, for 90% of our sample. In contrast, external comparisons show that data in the literature can be strongly affected by systematic errors due to large extrapolations, small radial range, sky subtraction errors, seeing effects, and the use of a simple R^1/4^ fit. The resulting errors can easily amount to more than 0.5mag in the total magnitudes and 50% in the half-luminosity radii.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499#2</TD>
            <TD>2011-09-14T19:42:20Z</TD>
            <TD>#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/292/499&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/292/499</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/292/499 [table4]</TD>
            <TD>EFAR photometric data (Saglia+, 1997)</TD>
            <TD>We present R-band CCD photometry for 776 galaxies observed in the EFAR (Elliptical FAR away) project. The photometry is compared with photoelectric data, showing that a common zero-point good to better than 1% and a precision of 0.03mag per zero-point have been achieved. We give the circularly averaged surface brightness profiles and the photometric parameters of the 762 program galaxies, D(n) diameters (at 20.5mag/arcsec^2^), half-luminosity radii Re, total magnitudes m_T_, and average effective surface brightnesses &lt;SBe&gt;. More than 80% of the profiles have a global S/N ratio larger than 300. The extrapolation needed to derive total magnitudes is less than 10% for 80% of the fits. More than 80% of the galaxies have mean effective surface brightness larger than the observed sky brightness. In 90% of the profiles the estimate of the contamination of the sky by the galaxy light is less than 1%. We derive total magnitudes and half-luminosity radii to better than 0.15mag and 25%, respectively, for 90% of our sample. In contrast, external comparisons show that data in the literature can be strongly affected by systematic errors due to large extrapolations, small radial range, sky subtraction errors, seeing effects, and the use of a simple R^1/4^ fit. The resulting errors can easily amount to more than 0.5mag in the total magnitudes and 50% in the half-luminosity radii.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499#table4</TD>
            <TD>2011-09-14T19:42:20Z</TD>
            <TD>#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/292/499&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/292/499</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/292/499 [1]</TD>
            <TD>EFAR photometric data (Saglia+, 1997)</TD>
            <TD>We present R-band CCD photometry for 776 galaxies observed in the EFAR (Elliptical FAR away) project. The photometry is compared with photoelectric data, showing that a common zero-point good to better than 1% and a precision of 0.03mag per zero-point have been achieved. We give the circularly averaged surface brightness profiles and the photometric parameters of the 762 program galaxies, D(n) diameters (at 20.5mag/arcsec^2^), half-luminosity radii Re, total magnitudes m_T_, and average effective surface brightnesses &lt;SBe&gt;. More than 80% of the profiles have a global S/N ratio larger than 300. The extrapolation needed to derive total magnitudes is less than 10% for 80% of the fits. More than 80% of the galaxies have mean effective surface brightness larger than the observed sky brightness. In 90% of the profiles the estimate of the contamination of the sky by the galaxy light is less than 1%. We derive total magnitudes and half-luminosity radii to better than 0.15mag and 25%, respectively, for 90% of our sample. In contrast, external comparisons show that data in the literature can be strongly affected by systematic errors due to large extrapolations, small radial range, sky subtraction errors, seeing effects, and the use of a simple R^1/4^ fit. The resulting errors can easily amount to more than 0.5mag in the total magnitudes and 50% in the half-luminosity radii.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499#1</TD>
            <TD>2011-09-14T19:42:20Z</TD>
            <TD>#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/292/499</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/292/499</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/292/499 [2]</TD>
            <TD>EFAR photometric data (Saglia+, 1997)</TD>
            <TD>We present R-band CCD photometry for 776 galaxies observed in the EFAR (Elliptical FAR away) project. The photometry is compared with photoelectric data, showing that a common zero-point good to better than 1% and a precision of 0.03mag per zero-point have been achieved. We give the circularly averaged surface brightness profiles and the photometric parameters of the 762 program galaxies, D(n) diameters (at 20.5mag/arcsec^2^), half-luminosity radii Re, total magnitudes m_T_, and average effective surface brightnesses &lt;SBe&gt;. More than 80% of the profiles have a global S/N ratio larger than 300. The extrapolation needed to derive total magnitudes is less than 10% for 80% of the fits. More than 80% of the galaxies have mean effective surface brightness larger than the observed sky brightness. In 90% of the profiles the estimate of the contamination of the sky by the galaxy light is less than 1%. We derive total magnitudes and half-luminosity radii to better than 0.15mag and 25%, respectively, for 90% of our sample. In contrast, external comparisons show that data in the literature can be strongly affected by systematic errors due to large extrapolations, small radial range, sky subtraction errors, seeing effects, and the use of a simple R^1/4^ fit. The resulting errors can easily amount to more than 0.5mag in the total magnitudes and 50% in the half-luminosity radii.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499#2</TD>
            <TD>2011-09-14T19:42:20Z</TD>
            <TD>#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/292/499&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/292/499</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/292/499 [table4]</TD>
            <TD>EFAR photometric data (Saglia+, 1997)</TD>
            <TD>We present R-band CCD photometry for 776 galaxies observed in the EFAR (Elliptical FAR away) project. The photometry is compared with photoelectric data, showing that a common zero-point good to better than 1% and a precision of 0.03mag per zero-point have been achieved. We give the circularly averaged surface brightness profiles and the photometric parameters of the 762 program galaxies, D(n) diameters (at 20.5mag/arcsec^2^), half-luminosity radii Re, total magnitudes m_T_, and average effective surface brightnesses &lt;SBe&gt;. More than 80% of the profiles have a global S/N ratio larger than 300. The extrapolation needed to derive total magnitudes is less than 10% for 80% of the fits. More than 80% of the galaxies have mean effective surface brightness larger than the observed sky brightness. In 90% of the profiles the estimate of the contamination of the sky by the galaxy light is less than 1%. We derive total magnitudes and half-luminosity radii to better than 0.15mag and 25%, respectively, for 90% of our sample. In contrast, external comparisons show that data in the literature can be strongly affected by systematic errors due to large extrapolations, small radial range, sky subtraction errors, seeing effects, and the use of a simple R^1/4^ fit. The resulting errors can easily amount to more than 0.5mag in the total magnitudes and 50% in the half-luminosity radii.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499#table4</TD>
            <TD>2011-09-14T19:42:20Z</TD>
            <TD>#Photometry#Galaxies:spectra#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Oct-1999</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/292/499</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/292/499&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/292/499</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/682 [1]</TD>
            <TD>Structural properties of S+S galaxies (Hernandez-Toledo+, 2005)</TD>
            <TD>We present a structural analysis of nearby galaxies in spiral-spiral pairs in optical BVRI bands and compare them with the structures of isolated spiral galaxies and galaxies in ongoing mergers. We use these comparisons to determine how galaxy structure changes during galaxy interactions and mergers. We analyze light concentration (C), asymmetry (A), and clumpiness (S) parameters, and use the projections of CAS parameter space to compare these samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682#1</TD>
            <TD>2011-09-14T19:43:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/682</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/682</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/682 [2]</TD>
            <TD>Structural properties of S+S galaxies (Hernandez-Toledo+, 2005)</TD>
            <TD>We present a structural analysis of nearby galaxies in spiral-spiral pairs in optical BVRI bands and compare them with the structures of isolated spiral galaxies and galaxies in ongoing mergers. We use these comparisons to determine how galaxy structure changes during galaxy interactions and mergers. We analyze light concentration (C), asymmetry (A), and clumpiness (S) parameters, and use the projections of CAS parameter space to compare these samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682#2</TD>
            <TD>2011-09-14T19:43:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/682&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/682</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/682 [tables]</TD>
            <TD>Structural properties of S+S galaxies (Hernandez-Toledo+, 2005)</TD>
            <TD>We present a structural analysis of nearby galaxies in spiral-spiral pairs in optical BVRI bands and compare them with the structures of isolated spiral galaxies and galaxies in ongoing mergers. We use these comparisons to determine how galaxy structure changes during galaxy interactions and mergers. We analyze light concentration (C), asymmetry (A), and clumpiness (S) parameters, and use the projections of CAS parameter space to compare these samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682#tables</TD>
            <TD>2011-09-14T19:43:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/682&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/682</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/682 [1]</TD>
            <TD>Structural properties of S+S galaxies (Hernandez-Toledo+, 2005)</TD>
            <TD>We present a structural analysis of nearby galaxies in spiral-spiral pairs in optical BVRI bands and compare them with the structures of isolated spiral galaxies and galaxies in ongoing mergers. We use these comparisons to determine how galaxy structure changes during galaxy interactions and mergers. We analyze light concentration (C), asymmetry (A), and clumpiness (S) parameters, and use the projections of CAS parameter space to compare these samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682#1</TD>
            <TD>2011-09-14T19:43:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/682</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/682</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/682 [2]</TD>
            <TD>Structural properties of S+S galaxies (Hernandez-Toledo+, 2005)</TD>
            <TD>We present a structural analysis of nearby galaxies in spiral-spiral pairs in optical BVRI bands and compare them with the structures of isolated spiral galaxies and galaxies in ongoing mergers. We use these comparisons to determine how galaxy structure changes during galaxy interactions and mergers. We analyze light concentration (C), asymmetry (A), and clumpiness (S) parameters, and use the projections of CAS parameter space to compare these samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682#2</TD>
            <TD>2011-09-14T19:43:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/682&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/682</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/129/682 [tables]</TD>
            <TD>Structural properties of S+S galaxies (Hernandez-Toledo+, 2005)</TD>
            <TD>We present a structural analysis of nearby galaxies in spiral-spiral pairs in optical BVRI bands and compare them with the structures of isolated spiral galaxies and galaxies in ongoing mergers. We use these comparisons to determine how galaxy structure changes during galaxy interactions and mergers. We analyze light concentration (C), asymmetry (A), and clumpiness (S) parameters, and use the projections of CAS parameter space to compare these samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682#tables</TD>
            <TD>2011-09-14T19:43:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/682&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/682</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/129/682 [1]</TD>
            <TD>Structural properties of S+S galaxies (Hernandez-Toledo+, 2005)</TD>
            <TD>We present a structural analysis of nearby galaxies in spiral-spiral pairs in optical BVRI bands and compare them with the structures of isolated spiral galaxies and galaxies in ongoing mergers. We use these comparisons to determine how galaxy structure changes during galaxy interactions and mergers. We analyze light concentration (C), asymmetry (A), and clumpiness (S) parameters, and use the projections of CAS parameter space to compare these samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682#1</TD>
            <TD>2011-09-14T19:43:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>06-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/129/682</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/682</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/129/682 [2]</TD>
            <TD>Structural properties of S+S galaxies (Hernandez-Toledo+, 2005)</TD>
            <TD>We present a structural analysis of nearby galaxies in spiral-spiral pairs in optical BVRI bands and compare them with the structures of isolated spiral galaxies and galaxies in ongoing mergers. We use these comparisons to determine how galaxy structure changes during galaxy interactions and mergers. We analyze light concentration (C), asymmetry (A), and clumpiness (S) parameters, and use the projections of CAS parameter space to compare these samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682#2</TD>
            <TD>2011-09-14T19:43:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
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            <TD />
            <TD>06-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/129/682&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/682</TD>
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          <TR>
            <TD>Catalog</TD>
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            <TD>Structural properties of S+S galaxies (Hernandez-Toledo+, 2005)</TD>
            <TD>We present a structural analysis of nearby galaxies in spiral-spiral pairs in optical BVRI bands and compare them with the structures of isolated spiral galaxies and galaxies in ongoing mergers. We use these comparisons to determine how galaxy structure changes during galaxy interactions and mergers. We analyze light concentration (C), asymmetry (A), and clumpiness (S) parameters, and use the projections of CAS parameter space to compare these samples.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682#tables</TD>
            <TD>2011-09-14T19:43:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/129/682</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/129/682&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/129/682</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/422/907 [1]</TD>
            <TD>Velocities of spiral galaxies in distant clusters (Jaeger+, 2004)</TD>
            <TD>We have conducted an observing campaign with the FORS instruments at the ESO-Very Large Telescope to explore the kinematical properties of spiral galaxies in distant galaxy clusters. Our main goal is to analyse transformation - and interaction processes of disk galaxies within the special environment of clusters as compared to the hierarchical evolution of galaxies in the field. Spatially resolved multi object spectra have been obtained for seven galaxy clusters at 0.3&lt;z&lt;0.6 to measure rotation velocities of cluster members. For three of the clusters, Cl 0303+17, Cl 0413-65, and MS 1008-12, for which we presented results including a Tully-Fisher-diagram in Ziegler et al. (2003ApJ...598L..87Z), we describe here in detail the sample selection, observations, data reduction, and data analysis. Each of them was observed with two setups of the standard MOS-unit of FORS.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907#1</TD>
            <TD>2011-09-14T19:43:27Z</TD>
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            <TD>#Catalog#</TD>
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            <TD />
            <TD>24-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/422/907</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/907</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/422/907 [2]</TD>
            <TD>Velocities of spiral galaxies in distant clusters (Jaeger+, 2004)</TD>
            <TD>We have conducted an observing campaign with the FORS instruments at the ESO-Very Large Telescope to explore the kinematical properties of spiral galaxies in distant galaxy clusters. Our main goal is to analyse transformation - and interaction processes of disk galaxies within the special environment of clusters as compared to the hierarchical evolution of galaxies in the field. Spatially resolved multi object spectra have been obtained for seven galaxy clusters at 0.3&lt;z&lt;0.6 to measure rotation velocities of cluster members. For three of the clusters, Cl 0303+17, Cl 0413-65, and MS 1008-12, for which we presented results including a Tully-Fisher-diagram in Ziegler et al. (2003ApJ...598L..87Z), we describe here in detail the sample selection, observations, data reduction, and data analysis. Each of them was observed with two setups of the standard MOS-unit of FORS.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907#2</TD>
            <TD>2011-09-14T19:43:27Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/422/907&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/907</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/422/907 [1]</TD>
            <TD>Velocities of spiral galaxies in distant clusters (Jaeger+, 2004)</TD>
            <TD>We have conducted an observing campaign with the FORS instruments at the ESO-Very Large Telescope to explore the kinematical properties of spiral galaxies in distant galaxy clusters. Our main goal is to analyse transformation - and interaction processes of disk galaxies within the special environment of clusters as compared to the hierarchical evolution of galaxies in the field. Spatially resolved multi object spectra have been obtained for seven galaxy clusters at 0.3&lt;z&lt;0.6 to measure rotation velocities of cluster members. For three of the clusters, Cl 0303+17, Cl 0413-65, and MS 1008-12, for which we presented results including a Tully-Fisher-diagram in Ziegler et al. (2003ApJ...598L..87Z), we describe here in detail the sample selection, observations, data reduction, and data analysis. Each of them was observed with two setups of the standard MOS-unit of FORS.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>2011-09-14T19:43:27Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/422/907</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/907</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/422/907 [2]</TD>
            <TD>Velocities of spiral galaxies in distant clusters (Jaeger+, 2004)</TD>
            <TD>We have conducted an observing campaign with the FORS instruments at the ESO-Very Large Telescope to explore the kinematical properties of spiral galaxies in distant galaxy clusters. Our main goal is to analyse transformation - and interaction processes of disk galaxies within the special environment of clusters as compared to the hierarchical evolution of galaxies in the field. Spatially resolved multi object spectra have been obtained for seven galaxy clusters at 0.3&lt;z&lt;0.6 to measure rotation velocities of cluster members. For three of the clusters, Cl 0303+17, Cl 0413-65, and MS 1008-12, for which we presented results including a Tully-Fisher-diagram in Ziegler et al. (2003ApJ...598L..87Z), we describe here in detail the sample selection, observations, data reduction, and data analysis. Each of them was observed with two setups of the standard MOS-unit of FORS.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907#2</TD>
            <TD>2011-09-14T19:43:27Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>24-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/422/907&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/907</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/422/907 [1]</TD>
            <TD>Velocities of spiral galaxies in distant clusters (Jaeger+, 2004)</TD>
            <TD>We have conducted an observing campaign with the FORS instruments at the ESO-Very Large Telescope to explore the kinematical properties of spiral galaxies in distant galaxy clusters. Our main goal is to analyse transformation - and interaction processes of disk galaxies within the special environment of clusters as compared to the hierarchical evolution of galaxies in the field. Spatially resolved multi object spectra have been obtained for seven galaxy clusters at 0.3&lt;z&lt;0.6 to measure rotation velocities of cluster members. For three of the clusters, Cl 0303+17, Cl 0413-65, and MS 1008-12, for which we presented results including a Tully-Fisher-diagram in Ziegler et al. (2003ApJ...598L..87Z), we describe here in detail the sample selection, observations, data reduction, and data analysis. Each of them was observed with two setups of the standard MOS-unit of FORS.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907#1</TD>
            <TD>2011-09-14T19:43:27Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/422/907</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/907</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/422/907 [2]</TD>
            <TD>Velocities of spiral galaxies in distant clusters (Jaeger+, 2004)</TD>
            <TD>We have conducted an observing campaign with the FORS instruments at the ESO-Very Large Telescope to explore the kinematical properties of spiral galaxies in distant galaxy clusters. Our main goal is to analyse transformation - and interaction processes of disk galaxies within the special environment of clusters as compared to the hierarchical evolution of galaxies in the field. Spatially resolved multi object spectra have been obtained for seven galaxy clusters at 0.3&lt;z&lt;0.6 to measure rotation velocities of cluster members. For three of the clusters, Cl 0303+17, Cl 0413-65, and MS 1008-12, for which we presented results including a Tully-Fisher-diagram in Ziegler et al. (2003ApJ...598L..87Z), we describe here in detail the sample selection, observations, data reduction, and data analysis. Each of them was observed with two setups of the standard MOS-unit of FORS.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907#2</TD>
            <TD>2011-09-14T19:43:27Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies:spectra#Redshifts#Rotational_Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2005</TD>
            <TD>ivo://CDS.VizieR/J/A+A/422/907</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/422/907&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/422/907</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/721/1368 [1]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#1</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/721/1368</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/721/1368 [2]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#2</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/1368 [table1]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#table1</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/1368 [Xobs]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#Xobs</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/1368 [table5]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#table5</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/721/1368 [1]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#1</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/721/1368</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/721/1368 [2]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#2</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/1368 [table1]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#table1</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/1368 [Xobs]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#Xobs</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/1368 [table5]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#table5</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/721/1368 [1]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#1</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/721/1368</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/721/1368 [2]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#2</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/1368 [table1]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#table1</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/1368 [Xobs]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#Xobs</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/1368 [table5]</TD>
            <TD>X-ray emission from the Sombrero galaxy (Li+, 2010)</TD>
            <TD>Existing Chandra studies of X-ray sources in Sombrero (Di Stefano et al. 2003, Cat. J/ApJ/599/1067; Kundu et al. 2007, Cat. J/ApJ/662/525; Li et al. 2007, Cat. J/MNRAS/376/960) are based on a 19ks ACIS-S observation taken on 2001 May 31 (ObsID 1586; PI: S. Murray). On April 29 and 2008 December 2, we obtained two new Chandra ACIS-I observations (ObsIDs 9532 and 9533; PI: C. Jones), with exposures of 85 and 90ks, respectively. In this work, we utilize data from all three observations. Hubble Space Telescope (HST)/Advance Camera for Surveys (ACS) data in the "science-ready form" were used by Spitler et al. (S06; 2006, Cat. J/AJ/132/1593) to identify GC candidates in a ~600"x400" six-pointing mosaic centered on Sombrero. Three optical bands (BVR) were obtained through the Hubble Heritage Project (PI: K. Noll, PID 9714). S06 used photometric and size selection (GCs are partially resolved on the ACS imaging) to construct a catalog of 659 GC candidates. Owing to the excellent quality of the HST images, the catalog contains all but the faintest 5% of the GCs in this field, with minimal contamination. In particular, objects falling on Sombrero's prominent dust lane are excluded. Here, we use improved photometric measurements for the GC candidates (see discussion in Spitler et al. 2008, Cat. J/MNRAS/389/1150).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368#table5</TD>
            <TD>2012-09-16T07:07:12Z</TD>
            <TD>#Globular_Clusters#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/1368</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/1368&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/1368</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/102/451 [1]</TD>
            <TD>Emission-line stars and PNe in the SMC (Meyssonnier+ 1993)</TD>
            <TD>An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451#1</TD>
            <TD>2012-12-12T13:26:31Z</TD>
            <TD>#Planetary_Nebulae#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/102/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/102/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/102/451 [2]</TD>
            <TD>Emission-line stars and PNe in the SMC (Meyssonnier+ 1993)</TD>
            <TD>An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451#2</TD>
            <TD>2012-12-12T13:26:31Z</TD>
            <TD>#Planetary_Nebulae#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/102/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/102/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/102/451 [table2]</TD>
            <TD>Emission-line stars and PNe in the SMC (Meyssonnier+ 1993)</TD>
            <TD>An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451#table2</TD>
            <TD>2012-12-12T13:26:31Z</TD>
            <TD>#Planetary_Nebulae#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/102/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/102/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/102/451 [1]</TD>
            <TD>Emission-line stars and PNe in the SMC (Meyssonnier+ 1993)</TD>
            <TD>An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451#1</TD>
            <TD>2012-12-12T13:26:31Z</TD>
            <TD>#Planetary_Nebulae#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/102/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/102/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/102/451 [2]</TD>
            <TD>Emission-line stars and PNe in the SMC (Meyssonnier+ 1993)</TD>
            <TD>An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451#2</TD>
            <TD>2012-12-12T13:26:31Z</TD>
            <TD>#Planetary_Nebulae#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/102/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/102/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/102/451 [table2]</TD>
            <TD>Emission-line stars and PNe in the SMC (Meyssonnier+ 1993)</TD>
            <TD>An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451#table2</TD>
            <TD>2012-12-12T13:26:31Z</TD>
            <TD>#Planetary_Nebulae#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/102/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/102/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/102/451 [1]</TD>
            <TD>Emission-line stars and PNe in the SMC (Meyssonnier+ 1993)</TD>
            <TD>An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451#1</TD>
            <TD>2012-12-12T13:26:31Z</TD>
            <TD>#Planetary_Nebulae#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/102/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/102/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/102/451 [2]</TD>
            <TD>Emission-line stars and PNe in the SMC (Meyssonnier+ 1993)</TD>
            <TD>An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451#2</TD>
            <TD>2012-12-12T13:26:31Z</TD>
            <TD>#Planetary_Nebulae#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/102/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/102/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/102/451 [table2]</TD>
            <TD>Emission-line stars and PNe in the SMC (Meyssonnier+ 1993)</TD>
            <TD>An objective-prism survey of the Small Magellanic Cloud (SMC) has been performed through an H-{alpha} + [NII] interference filter, using the 90cm Curtis Schmidt telescope of Cerro Tololo. 1898 emission-line objects have been detected in the main body of this galaxy, almost quadrupling the number of those found in the same region by the previous objective-prism surveys. Among these objects are newly discovered planetary nebulae, compact HII regions and late-type stars. Continuum intensity, as well as the shape and relative strength of the H-{alpha} emission-line have been estimated; coordinates, cross-identifications for the listed objects are provided. The original paper contains in addition finding charts.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451#table2</TD>
            <TD>2012-12-12T13:26:31Z</TD>
            <TD>#Planetary_Nebulae#Stars:Emission#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/102/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/102/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/102/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/546/A2 [1]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#1</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/546/A2</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/546/A2 [2]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#2</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/546/A2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/546/A2 [table1]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#table1</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/546/A2&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/546/A2 [catalog]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#catalog</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/546/A2&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/546/A2 [1]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#1</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/546/A2</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/546/A2 [2]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#2</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/546/A2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/546/A2 [table1]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#table1</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/546/A2&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/546/A2 [catalog]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#catalog</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/546/A2&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/546/A2 [1]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#1</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/546/A2</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/546/A2 [2]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#2</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/546/A2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/546/A2 [table1]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#table1</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/546/A2&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/546/A2 [catalog]</TD>
            <TD>Spectroscopy of HII regions in nearby galaxies (Sanchez+, 2012)</TD>
            <TD>In this work we analyze the spectroscopic properties of a large number of HII regions, ~2600, located in 38 galaxies. The sample of galaxies has been assembled from the face-on spirals in the PINGS survey and a sample described in Marmol-Queralto (2011A&amp;A...534A...8M). All the galaxies were observed using Integral Field Spectroscopy with a similar setup, covering their optical extension up to ~2.4 effective radii within a wavelength range from ~3700 to ~6900{AA}. We develop a new automatic procedure to detect HII regions, based on the contrast of the H{alpha} intensity maps extracted from the datacubes. Once detected, the procedure provides us with the integrated spectra of each individual segmented region. In total, we derive good quality spectroscopic information for ~2600 independent HII regions/complexes. This is by far the largest nearby 2-dimensional spectroscopic survey presented on this kind of regions up-to-date. Even more, our selection criteria and dataset guarantee that we cover the regions in an unbiased way, regarding the spatial sampling. A well-tested automatic decoupling procedure has been applied to remove the underlying stellar population, deriving the main properties (intensity, dispersion and velocity) of the strongest emission lines in the considered wavelength range (covering from [OII]3727 to [SII]6731). A final catalogue of the spectroscopic properties of these regions has been created for each galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2#catalog</TD>
            <TD>2012-12-27T17:34:11Z</TD>
            <TD>#Equivalent_widths#Galaxies#HII_regions#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/546/A2&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A2</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/546/A6 [1]</TD>
            <TD>Metal abundances of galaxy clusters (Andreon, 2012)</TD>
            <TD>This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1&lt;z&lt;1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6#1</TD>
            <TD>2012-12-27T17:47:45Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/546/A6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/546/A6 [2]</TD>
            <TD>Metal abundances of galaxy clusters (Andreon, 2012)</TD>
            <TD>This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1&lt;z&lt;1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6#2</TD>
            <TD>2012-12-27T17:47:45Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/546/A6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/546/A6 [table1]</TD>
            <TD>Metal abundances of galaxy clusters (Andreon, 2012)</TD>
            <TD>This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1&lt;z&lt;1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6#table1</TD>
            <TD>2012-12-27T17:47:45Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/546/A6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/546/A6 [1]</TD>
            <TD>Metal abundances of galaxy clusters (Andreon, 2012)</TD>
            <TD>This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1&lt;z&lt;1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6#1</TD>
            <TD>2012-12-27T17:47:45Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/546/A6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/546/A6 [2]</TD>
            <TD>Metal abundances of galaxy clusters (Andreon, 2012)</TD>
            <TD>This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1&lt;z&lt;1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6#2</TD>
            <TD>2012-12-27T17:47:45Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/546/A6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/546/A6 [table1]</TD>
            <TD>Metal abundances of galaxy clusters (Andreon, 2012)</TD>
            <TD>This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1&lt;z&lt;1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6#table1</TD>
            <TD>2012-12-27T17:47:45Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/546/A6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/546/A6 [1]</TD>
            <TD>Metal abundances of galaxy clusters (Andreon, 2012)</TD>
            <TD>This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1&lt;z&lt;1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6#1</TD>
            <TD>2012-12-27T17:47:45Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/546/A6</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A6</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/546/A6 [2]</TD>
            <TD>Metal abundances of galaxy clusters (Andreon, 2012)</TD>
            <TD>This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1&lt;z&lt;1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6#2</TD>
            <TD>2012-12-27T17:47:45Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/546/A6&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A6</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/546/A6 [table1]</TD>
            <TD>Metal abundances of galaxy clusters (Andreon, 2012)</TD>
            <TD>This work measures the evolution of the iron content in galaxy clusters by a rigorous analysis of the data of 130 clusters at 0.1&lt;z&lt;1.3. This task is made difficult by a) the low signal-to-noise ratio of abundance measurements and the upper limits, b) possible selection effects, c) boundaries in the parameter space, d) non-Gaussian errors, e) the intrinsic variety of the objects studied, and f) abundance systematics. We introduce a Bayesian model to address all these issues at the same time, thus allowing cross-talk (covariance).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6#table1</TD>
            <TD>2012-12-27T17:47:45Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/A+A/546/A6</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/546/A6&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/546/A6</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/193/14 [1]</TD>
            <TD>DEEP3 Galaxy Redshift Survey: GOODS-N field (Cooper+, 2011)</TD>
            <TD>Spectroscopic observations using DEIMOS were completed during April 2009 and 2010, with a nominal spectral coverage of 4600-9800{AA} at a resolution (FWHM) of ~3.5{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14#1</TD>
            <TD>2013-01-03T12:54:32Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/193/14</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/14</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/193/14 [2]</TD>
            <TD>DEEP3 Galaxy Redshift Survey: GOODS-N field (Cooper+, 2011)</TD>
            <TD>Spectroscopic observations using DEIMOS were completed during April 2009 and 2010, with a nominal spectral coverage of 4600-9800{AA} at a resolution (FWHM) of ~3.5{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14#2</TD>
            <TD>2013-01-03T12:54:32Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/193/14&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/14</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/14 [table2]</TD>
            <TD>DEEP3 Galaxy Redshift Survey: GOODS-N field (Cooper+, 2011)</TD>
            <TD>Spectroscopic observations using DEIMOS were completed during April 2009 and 2010, with a nominal spectral coverage of 4600-9800{AA} at a resolution (FWHM) of ~3.5{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14#table2</TD>
            <TD>2013-01-03T12:54:32Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/14&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/14</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/193/14 [1]</TD>
            <TD>DEEP3 Galaxy Redshift Survey: GOODS-N field (Cooper+, 2011)</TD>
            <TD>Spectroscopic observations using DEIMOS were completed during April 2009 and 2010, with a nominal spectral coverage of 4600-9800{AA} at a resolution (FWHM) of ~3.5{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14#1</TD>
            <TD>2013-01-03T12:54:32Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/193/14</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/14</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/193/14 [2]</TD>
            <TD>DEEP3 Galaxy Redshift Survey: GOODS-N field (Cooper+, 2011)</TD>
            <TD>Spectroscopic observations using DEIMOS were completed during April 2009 and 2010, with a nominal spectral coverage of 4600-9800{AA} at a resolution (FWHM) of ~3.5{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14#2</TD>
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            <TD />
            <TD>12-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/193/14&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/14</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/14 [table2]</TD>
            <TD>DEEP3 Galaxy Redshift Survey: GOODS-N field (Cooper+, 2011)</TD>
            <TD>Spectroscopic observations using DEIMOS were completed during April 2009 and 2010, with a nominal spectral coverage of 4600-9800{AA} at a resolution (FWHM) of ~3.5{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14#table2</TD>
            <TD>2013-01-03T12:54:32Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/14&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/14</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/193/14 [1]</TD>
            <TD>DEEP3 Galaxy Redshift Survey: GOODS-N field (Cooper+, 2011)</TD>
            <TD>Spectroscopic observations using DEIMOS were completed during April 2009 and 2010, with a nominal spectral coverage of 4600-9800{AA} at a resolution (FWHM) of ~3.5{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14#1</TD>
            <TD>2013-01-03T12:54:32Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/193/14</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/14</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/193/14 [2]</TD>
            <TD>DEEP3 Galaxy Redshift Survey: GOODS-N field (Cooper+, 2011)</TD>
            <TD>Spectroscopic observations using DEIMOS were completed during April 2009 and 2010, with a nominal spectral coverage of 4600-9800{AA} at a resolution (FWHM) of ~3.5{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14#2</TD>
            <TD>2013-01-03T12:54:32Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
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            <TD />
            <TD>12-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/193/14&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/14</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/14 [table2]</TD>
            <TD>DEEP3 Galaxy Redshift Survey: GOODS-N field (Cooper+, 2011)</TD>
            <TD>Spectroscopic observations using DEIMOS were completed during April 2009 and 2010, with a nominal spectral coverage of 4600-9800{AA} at a resolution (FWHM) of ~3.5{AA}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14#table2</TD>
            <TD>2013-01-03T12:54:32Z</TD>
            <TD>#Galaxies#Spectroscopy#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Apr-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/14</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/14&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/14</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/348/98 [1]</TD>
            <TD>LMC AGB stars IRAS fluxes (Reid+ 1990)</TD>
            <TD>We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_&lt;9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_&lt;-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98#1</TD>
            <TD>2013-01-09T14:05:08Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/348/98</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/348/98</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/348/98 [2]</TD>
            <TD>LMC AGB stars IRAS fluxes (Reid+ 1990)</TD>
            <TD>We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_&lt;9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_&lt;-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98#2</TD>
            <TD>2013-01-09T14:05:08Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/348/98&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/348/98</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/348/98 [table3]</TD>
            <TD>LMC AGB stars IRAS fluxes (Reid+ 1990)</TD>
            <TD>We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_&lt;9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_&lt;-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98#table3</TD>
            <TD>2013-01-09T14:05:08Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/348/98&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/348/98</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/348/98 [1]</TD>
            <TD>LMC AGB stars IRAS fluxes (Reid+ 1990)</TD>
            <TD>We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_&lt;9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_&lt;-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98#1</TD>
            <TD>2013-01-09T14:05:08Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/348/98</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/348/98</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/348/98 [2]</TD>
            <TD>LMC AGB stars IRAS fluxes (Reid+ 1990)</TD>
            <TD>We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_&lt;9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_&lt;-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98#2</TD>
            <TD>2013-01-09T14:05:08Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/348/98&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/348/98</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/348/98 [table3]</TD>
            <TD>LMC AGB stars IRAS fluxes (Reid+ 1990)</TD>
            <TD>We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_&lt;9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_&lt;-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98#table3</TD>
            <TD>2013-01-09T14:05:08Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/348/98&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/348/98</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/348/98 [1]</TD>
            <TD>LMC AGB stars IRAS fluxes (Reid+ 1990)</TD>
            <TD>We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_&lt;9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_&lt;-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98#1</TD>
            <TD>2013-01-09T14:05:08Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/348/98</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/348/98</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/348/98 [2]</TD>
            <TD>LMC AGB stars IRAS fluxes (Reid+ 1990)</TD>
            <TD>We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_&lt;9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_&lt;-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98#2</TD>
            <TD>2013-01-09T14:05:08Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/348/98&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/348/98</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/348/98 [table3]</TD>
            <TD>LMC AGB stars IRAS fluxes (Reid+ 1990)</TD>
            <TD>We present the results of a search for optically obscured asymptotic giant branch (AGB) stars in the Large Magellanic Cloud (LMC), combining data obtained using the IRAS satellite with near-infrared photographic plate material of a 15deg^2^ region in the northern LMC. Of the 156 IRAS sources that are detected either in separate cross-scans or in more than one passband, 63 have [12-25] colors consistent with their being either stellar photospheres or circumstellar dust shells. Seventeen of these we identify with bright (I_c_&lt;9) foreground stars in our own Galaxy, while a further 17 are associated with red supergiants in the LMC. Of the remaining stars, no more than five are likely to be optically visible AGB stars, while the rest have no obvious optical counterpart. This immediately rules out the presence of sufficient high-luminosity "cocoon" stars to explain the observed deficit of several hundred luminous (M_bol_&lt;-6) AGB stars between the predictions of standard models of AGB evolution and the observed luminosity function. It remains possible that most of the unidentified sources are dusty AGB stars, evolving through a phase of enhanced mass loss toward becoming planetary nebulae. We infer bolometric magnitudes as low as M_bol_~-5 for these sources and suggest that this phase can be triggered at low luminosities, truncating AGB evolution and leading to the observed scarcity of asymptotic giant branch stars with bolometric magnitudes brighter than -6.0mag.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98#table3</TD>
            <TD>2013-01-09T14:05:08Z</TD>
            <TD>#Stars#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Sep-1996</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/348/98</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/348/98&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/348/98</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/449/527 [1]</TD>
            <TD>Galaxies in the zone of avoidance (Lu+ 1995)</TD>
            <TD>We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h&lt;RA&lt;10h and 0deg&lt;DE&lt;36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA&lt;3h from structures at RA&gt;4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully &amp; Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527#1</TD>
            <TD>2013-01-09T14:58:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/449/527</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/527</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/449/527 [2]</TD>
            <TD>Galaxies in the zone of avoidance (Lu+ 1995)</TD>
            <TD>We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h&lt;RA&lt;10h and 0deg&lt;DE&lt;36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA&lt;3h from structures at RA&gt;4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully &amp; Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527#2</TD>
            <TD>2013-01-09T14:58:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/449/527&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/527</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/449/527 [table2]</TD>
            <TD>Galaxies in the zone of avoidance (Lu+ 1995)</TD>
            <TD>We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h&lt;RA&lt;10h and 0deg&lt;DE&lt;36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA&lt;3h from structures at RA&gt;4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully &amp; Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527#table2</TD>
            <TD>2013-01-09T14:58:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/449/527&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/527</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/449/527 [1]</TD>
            <TD>Galaxies in the zone of avoidance (Lu+ 1995)</TD>
            <TD>We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h&lt;RA&lt;10h and 0deg&lt;DE&lt;36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA&lt;3h from structures at RA&gt;4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully &amp; Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527#1</TD>
            <TD>2013-01-09T14:58:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/449/527</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/527</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/449/527 [2]</TD>
            <TD>Galaxies in the zone of avoidance (Lu+ 1995)</TD>
            <TD>We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h&lt;RA&lt;10h and 0deg&lt;DE&lt;36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA&lt;3h from structures at RA&gt;4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully &amp; Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527#2</TD>
            <TD>2013-01-09T14:58:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/449/527&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/527</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/449/527 [table2]</TD>
            <TD>Galaxies in the zone of avoidance (Lu+ 1995)</TD>
            <TD>We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h&lt;RA&lt;10h and 0deg&lt;DE&lt;36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA&lt;3h from structures at RA&gt;4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully &amp; Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527#table2</TD>
            <TD>2013-01-09T14:58:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/449/527&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/527</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/449/527 [1]</TD>
            <TD>Galaxies in the zone of avoidance (Lu+ 1995)</TD>
            <TD>We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h&lt;RA&lt;10h and 0deg&lt;DE&lt;36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA&lt;3h from structures at RA&gt;4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully &amp; Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527#1</TD>
            <TD>2013-01-09T14:58:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/449/527</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/527</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/449/527 [2]</TD>
            <TD>Galaxies in the zone of avoidance (Lu+ 1995)</TD>
            <TD>We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h&lt;RA&lt;10h and 0deg&lt;DE&lt;36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA&lt;3h from structures at RA&gt;4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully &amp; Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527#2</TD>
            <TD>2013-01-09T14:58:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/449/527&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/527</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/449/527 [table2]</TD>
            <TD>Galaxies in the zone of avoidance (Lu+ 1995)</TD>
            <TD>We have selected a sample of 876 galaxy candidates from the IRAS Point Source Catalog in the region of 2h&lt;RA&lt;10h and 0deg&lt;DE&lt;36deg, which crosses the Galactic anticenter part of the Zone of Avoidance (ZOA) and includes most of the highly obscured Orion-Taurus complex region. We have identified galaxies among the candidate sources by attempting to detect the 21cm H I line of those sources which were not known to be galaxies at the beginning of the survey. In this manner, we constructed a galaxy sample which is largely free from Galactic reddening. Of the 272 observed candidates, 89 were detected in the H I line up to a heliocentric velocity of v_h_~16,000km/s. The resulting galaxy sample of 717 galaxies is fairly complete (within about 10%) and uniform (within about 4%) in the part of the survey area 10deg away from the Galactic plane and for velocities up to at least 9000km/s. This provides, for the first time, a largely unbiased view on the large-scale structures in much of the survey area. Our main results are the following: (1) Several large voids are identified. In particular, a void between RA~3h and 4h, up to v_h_~6000km/s, separates the Pisces-Perseus supercluster at RA&lt;3h from structures at RA&gt;4h; and a "nearby void" occupies most of our survey area and reaches out to a redshift of nearly 3000km/s. (2) We found no nearby galaxy concentration that could significantly contribute to the "Local Velocity Anomaly" (LVA), but a general excess of galaxies around v_h_~5000km/s in the survey area. (3) The contrast between the "Great Wall" at v_h_~8500km/s and the void in front of it appears to gradually diffuse out after it enters the Zone of Avoidance from the northern Galactic hemisphere. (4) Our data combined with other galaxy surveys in or near the Galactic anticenter part of the ZOA suggest that the main ridge of the Pisces-Perseus supercluster does also not extend to Abell 569, a cluster in the northern Galactic hemisphere, and that the simple gravitational model consisting of the Local Void of Tully &amp; Fisher, our nearby void, and Puppis and Fornax-Eridanus clusters would predict a LVA whose direction is probably too far away from that derived from observations.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527#table2</TD>
            <TD>2013-01-09T14:58:32Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Apr-1997</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/449/527</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/449/527&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/449/527</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/418/2054 [1]</TD>
            <TD>Recession velocities for fossil galaxy groups (Proctor+, 2011)</TD>
            <TD>The Magellan Baade telescope multi-object spectroscopy of five candidate fossil groups selected from the maxBCG catalogue was carried out on the f/2 camera of the IMACS instrument in 2009 February. The Gemini GMOS spectroscopic observations of RX J1256.0+2556 were carried out on Gemini North on 2006 June 24. Observations of RX J1331.5+1108 were carried out on Gemini North on 2005 March 7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054#1</TD>
            <TD>2013-01-27T13:32:49Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/418/2054</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/2054</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/418/2054 [2]</TD>
            <TD>Recession velocities for fossil galaxy groups (Proctor+, 2011)</TD>
            <TD>The Magellan Baade telescope multi-object spectroscopy of five candidate fossil groups selected from the maxBCG catalogue was carried out on the f/2 camera of the IMACS instrument in 2009 February. The Gemini GMOS spectroscopic observations of RX J1256.0+2556 were carried out on Gemini North on 2006 June 24. Observations of RX J1331.5+1108 were carried out on Gemini North on 2005 March 7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054#2</TD>
            <TD>2013-01-27T13:32:49Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/418/2054&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/2054</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/418/2054 [tableb]</TD>
            <TD>Recession velocities for fossil galaxy groups (Proctor+, 2011)</TD>
            <TD>The Magellan Baade telescope multi-object spectroscopy of five candidate fossil groups selected from the maxBCG catalogue was carried out on the f/2 camera of the IMACS instrument in 2009 February. The Gemini GMOS spectroscopic observations of RX J1256.0+2556 were carried out on Gemini North on 2006 June 24. Observations of RX J1331.5+1108 were carried out on Gemini North on 2005 March 7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054#tableb</TD>
            <TD>2013-01-27T13:32:49Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/418/2054&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/2054</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/418/2054 [1]</TD>
            <TD>Recession velocities for fossil galaxy groups (Proctor+, 2011)</TD>
            <TD>The Magellan Baade telescope multi-object spectroscopy of five candidate fossil groups selected from the maxBCG catalogue was carried out on the f/2 camera of the IMACS instrument in 2009 February. The Gemini GMOS spectroscopic observations of RX J1256.0+2556 were carried out on Gemini North on 2006 June 24. Observations of RX J1331.5+1108 were carried out on Gemini North on 2005 March 7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054#1</TD>
            <TD>2013-01-27T13:32:49Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/418/2054</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/2054</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/418/2054 [2]</TD>
            <TD>Recession velocities for fossil galaxy groups (Proctor+, 2011)</TD>
            <TD>The Magellan Baade telescope multi-object spectroscopy of five candidate fossil groups selected from the maxBCG catalogue was carried out on the f/2 camera of the IMACS instrument in 2009 February. The Gemini GMOS spectroscopic observations of RX J1256.0+2556 were carried out on Gemini North on 2006 June 24. Observations of RX J1331.5+1108 were carried out on Gemini North on 2005 March 7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054#2</TD>
            <TD>2013-01-27T13:32:49Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/418/2054&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/2054</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/418/2054 [tableb]</TD>
            <TD>Recession velocities for fossil galaxy groups (Proctor+, 2011)</TD>
            <TD>The Magellan Baade telescope multi-object spectroscopy of five candidate fossil groups selected from the maxBCG catalogue was carried out on the f/2 camera of the IMACS instrument in 2009 February. The Gemini GMOS spectroscopic observations of RX J1256.0+2556 were carried out on Gemini North on 2006 June 24. Observations of RX J1331.5+1108 were carried out on Gemini North on 2005 March 7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054#tableb</TD>
            <TD>2013-01-27T13:32:49Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/418/2054&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/2054</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/418/2054 [1]</TD>
            <TD>Recession velocities for fossil galaxy groups (Proctor+, 2011)</TD>
            <TD>The Magellan Baade telescope multi-object spectroscopy of five candidate fossil groups selected from the maxBCG catalogue was carried out on the f/2 camera of the IMACS instrument in 2009 February. The Gemini GMOS spectroscopic observations of RX J1256.0+2556 were carried out on Gemini North on 2006 June 24. Observations of RX J1331.5+1108 were carried out on Gemini North on 2005 March 7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054#1</TD>
            <TD>2013-01-27T13:32:49Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/418/2054</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/2054</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/418/2054 [2]</TD>
            <TD>Recession velocities for fossil galaxy groups (Proctor+, 2011)</TD>
            <TD>The Magellan Baade telescope multi-object spectroscopy of five candidate fossil groups selected from the maxBCG catalogue was carried out on the f/2 camera of the IMACS instrument in 2009 February. The Gemini GMOS spectroscopic observations of RX J1256.0+2556 were carried out on Gemini North on 2006 June 24. Observations of RX J1331.5+1108 were carried out on Gemini North on 2005 March 7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054#2</TD>
            <TD>2013-01-27T13:32:49Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/418/2054&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/2054</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/418/2054 [tableb]</TD>
            <TD>Recession velocities for fossil galaxy groups (Proctor+, 2011)</TD>
            <TD>The Magellan Baade telescope multi-object spectroscopy of five candidate fossil groups selected from the maxBCG catalogue was carried out on the f/2 camera of the IMACS instrument in 2009 February. The Gemini GMOS spectroscopic observations of RX J1256.0+2556 were carried out on Gemini North on 2006 June 24. Observations of RX J1331.5+1108 were carried out on Gemini North on 2005 March 7.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054#tableb</TD>
            <TD>2013-01-27T13:32:49Z</TD>
            <TD>#Clusters_of_galaxies#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/418/2054</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/418/2054&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/418/2054</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/422/25 [1]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#1</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/422/25</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/422/25 [2]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#2</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/25 [void]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#void</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/25 [table5]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#table5</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/25 [table1]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#table1</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/422/25 [1]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#1</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/422/25</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/422/25 [2]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#2</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/25 [void]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#void</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/25 [table5]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#table5</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/25 [table1]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#table1</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/422/25 [1]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#1</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/422/25</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/422/25 [2]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#2</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/25 [void]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#void</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/25 [table5]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#table5</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/25 [table1]</TD>
            <TD>SDSS DR7 groups, clusters and filaments (Smith+, 2012)</TD>
            <TD>We have developed a multiscale structure identification algorithm for the detection of overdensities in galaxy data that identifies structures having radii within a user-defined range. Our "multiscale probability mapping" technique combines density estimation with a shape statistic to identify local peaks in the density field. This technique takes advantage of a user-defined range of scale sizes, which are used in constructing a coarse-grained map of the underlying fine-grained galaxy distribution, from which overdense structures are then identified. In this study we have compiled a catalogue of groups and clusters at 0.025&lt;z&lt;0.24 based on the Sloan Digital Sky Survey (SDSS), Data Release 7, quantifying their significance and comparing with other catalogues. Most measured velocity dispersions for these structures lie between 50 and 400km/s. A clear trend of increasing velocity dispersion with radius from 0.2 to 1Mpc/h is detected, confirming the lack of a sharp division between groups and clusters. A method for quantifying elongation is also developed to measure the elongation of group and cluster environments. By using our group and cluster catalogue as a coarse-grained representation of the galaxy distribution for structure sizes of &lt;~1Mpc/h, we identify 53 filaments (from an algorithmically derived set of 100 candidates) as elongated unions of groups and clusters at 0.025&lt;z&lt;0.13. These filaments have morphologies that are consistent with previous samples studied.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25#table1</TD>
            <TD>2013-02-07T17:20:02Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/25</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/25&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/25</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/422/89 [1]</TD>
            <TD>Cetus dSph RR Lyrae (Monelli+, 2012)</TD>
            <TD>The analysis of variable stars in the Cetus dSph galaxy presented in this paper is based on data collected in service mode using the VIMOS camera mounted on the VLT (ESO program 081.D-0775, P.I.: E.J. Bernard). The images were acquired during six nights between 2008 July 27 and August 8.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89#1</TD>
            <TD>2013-02-08T17:09:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/422/89</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/89</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/422/89 [2]</TD>
            <TD>Cetus dSph RR Lyrae (Monelli+, 2012)</TD>
            <TD>The analysis of variable stars in the Cetus dSph galaxy presented in this paper is based on data collected in service mode using the VIMOS camera mounted on the VLT (ESO program 081.D-0775, P.I.: E.J. Bernard). The images were acquired during six nights between 2008 July 27 and August 8.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89#2</TD>
            <TD>2013-02-08T17:09:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/422/89&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/89 [table2]</TD>
            <TD>Cetus dSph RR Lyrae (Monelli+, 2012)</TD>
            <TD>The analysis of variable stars in the Cetus dSph galaxy presented in this paper is based on data collected in service mode using the VIMOS camera mounted on the VLT (ESO program 081.D-0775, P.I.: E.J. Bernard). The images were acquired during six nights between 2008 July 27 and August 8.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89#table2</TD>
            <TD>2013-02-08T17:09:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/89</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/422/89 [1]</TD>
            <TD>Cetus dSph RR Lyrae (Monelli+, 2012)</TD>
            <TD>The analysis of variable stars in the Cetus dSph galaxy presented in this paper is based on data collected in service mode using the VIMOS camera mounted on the VLT (ESO program 081.D-0775, P.I.: E.J. Bernard). The images were acquired during six nights between 2008 July 27 and August 8.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89#1</TD>
            <TD>2013-02-08T17:09:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/422/89</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/89</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/422/89 [2]</TD>
            <TD>Cetus dSph RR Lyrae (Monelli+, 2012)</TD>
            <TD>The analysis of variable stars in the Cetus dSph galaxy presented in this paper is based on data collected in service mode using the VIMOS camera mounted on the VLT (ESO program 081.D-0775, P.I.: E.J. Bernard). The images were acquired during six nights between 2008 July 27 and August 8.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89#2</TD>
            <TD>2013-02-08T17:09:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/422/89&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/89 [table2]</TD>
            <TD>Cetus dSph RR Lyrae (Monelli+, 2012)</TD>
            <TD>The analysis of variable stars in the Cetus dSph galaxy presented in this paper is based on data collected in service mode using the VIMOS camera mounted on the VLT (ESO program 081.D-0775, P.I.: E.J. Bernard). The images were acquired during six nights between 2008 July 27 and August 8.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89#table2</TD>
            <TD>2013-02-08T17:09:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/89</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/422/89 [1]</TD>
            <TD>Cetus dSph RR Lyrae (Monelli+, 2012)</TD>
            <TD>The analysis of variable stars in the Cetus dSph galaxy presented in this paper is based on data collected in service mode using the VIMOS camera mounted on the VLT (ESO program 081.D-0775, P.I.: E.J. Bernard). The images were acquired during six nights between 2008 July 27 and August 8.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89#1</TD>
            <TD>2013-02-08T17:09:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/422/89</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/89</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/422/89 [2]</TD>
            <TD>Cetus dSph RR Lyrae (Monelli+, 2012)</TD>
            <TD>The analysis of variable stars in the Cetus dSph galaxy presented in this paper is based on data collected in service mode using the VIMOS camera mounted on the VLT (ESO program 081.D-0775, P.I.: E.J. Bernard). The images were acquired during six nights between 2008 July 27 and August 8.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89#2</TD>
            <TD>2013-02-08T17:09:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/422/89&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/89</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/422/89 [table2]</TD>
            <TD>Cetus dSph RR Lyrae (Monelli+, 2012)</TD>
            <TD>The analysis of variable stars in the Cetus dSph galaxy presented in this paper is based on data collected in service mode using the VIMOS camera mounted on the VLT (ESO program 081.D-0775, P.I.: E.J. Bernard). The images were acquired during six nights between 2008 July 27 and August 8.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89#table2</TD>
            <TD>2013-02-08T17:09:08Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Nov-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/422/89</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/422/89&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/422/89</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/267 [1]</TD>
            <TD>Gravitational Wave Galaxy Catalogue (White+ 2011)</TD>
            <TD />
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/267#1</TD>
            <TD>2012-01-24T13:50:36Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/VII/267</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/267</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/267</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/267 [2]</TD>
            <TD>Gravitational Wave Galaxy Catalogue (White+ 2011)</TD>
            <TD />
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/267#2</TD>
            <TD>2012-01-24T13:50:36Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/VII/267</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/267&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/267</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/267 [gwgc]</TD>
            <TD>Gravitational Wave Galaxy Catalogue (White+ 2011)</TD>
            <TD />
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/267#gwgc</TD>
            <TD>2012-01-24T13:50:36Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/VII/267</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/267&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/267</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/267 [1]</TD>
            <TD>Gravitational Wave Galaxy Catalogue (White+ 2011)</TD>
            <TD />
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/267#1</TD>
            <TD>2012-01-24T13:50:36Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/VII/267</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/267</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/267</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/267 [2]</TD>
            <TD>Gravitational Wave Galaxy Catalogue (White+ 2011)</TD>
            <TD />
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/267#2</TD>
            <TD>2012-01-24T13:50:36Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/VII/267</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/267&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/267</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/267 [gwgc]</TD>
            <TD>Gravitational Wave Galaxy Catalogue (White+ 2011)</TD>
            <TD />
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/267#gwgc</TD>
            <TD>2012-01-24T13:50:36Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/VII/267</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/267&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/267</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VII/267 [1]</TD>
            <TD>Gravitational Wave Galaxy Catalogue (White+ 2011)</TD>
            <TD />
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/267#1</TD>
            <TD>2012-01-24T13:50:36Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/VII/267</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VII/267</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/267</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VII/267 [2]</TD>
            <TD>Gravitational Wave Galaxy Catalogue (White+ 2011)</TD>
            <TD />
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/267#2</TD>
            <TD>2012-01-24T13:50:36Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/VII/267</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VII/267&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/267</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VII/267 [gwgc]</TD>
            <TD>Gravitational Wave Galaxy Catalogue (White+ 2011)</TD>
            <TD />
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/VII/267#gwgc</TD>
            <TD>2012-01-24T13:50:36Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Jan-2012</TD>
            <TD>ivo://CDS.VizieR/VII/267</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VII/267&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VII/267</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [1]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#1</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VIKING DR2 [2]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#2</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/DirectCone?DSACAT=VIKING_DR2&amp;DSATAB=vikingDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [3]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#3</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VIKING DR2 [4]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#4</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [5]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#5</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [6]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#6</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [7]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#7</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [8]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#8</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [9]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#9</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [10]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#10</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VIKING DR2 [11]</TD>
            <TD>VIKING - VISTA Kilo-degree Infrared Galaxy survey Data Release 2</TD>
            <TD>The VIKING survey is the VISTA counterpart to the VST KIDS survey. The KIDS survey will cover 1500 deg^2 in u,g,r,i divided in two stripes (NGP, centred on equator ; SGP, centred on Dec = -30). The matching VISTA survey will cover (almost) all of these stripes in Z,Y,J,H, Ks with ~ 400s exposures per band.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa#11</TD>
            <TD>2012-07-17T15:45:28Z</TD>
            <TD>#Infrared, survey, galaxy, KIDS#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 2</TD>
            <TD>ivo://wfau.roe.ac.uk/vikingDR2-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vikingDR2-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.astro-wise.org/projects/VIKING/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [1]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#1</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VMC DR1 [2]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#2</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/DirectCone?DSACAT=VMC_DR1&amp;DSATAB=vmcDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [3]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#3</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>VMC DR1 [4]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#4</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [5]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#5</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [6]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#6</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [7]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#7</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [8]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#8</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [9]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#9</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [10]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#10</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VMC DR1 [11]</TD>
            <TD>VMC DR1 - VISTA Magellanic System survey</TD>
            <TD>The VMC survey aims to obtain YJKs band photometry across the system down to Ks=20.3 at S/N=10. This sensitivity corresponds to the bottom of the red giant branch field stellar population and allows us to determine the global spatially resolved star formation history with unprecedented quality and to construct a three-dimensional map of the system. A wide-area encompassing the D25 as well as major features delineated by the distribution of stars and HI gas, will both trace the structure of the galaxies and signatures of past and present interactions. Contemporary optical and kinematic observations of comparable sensitivity will provide the community with a superior database for future studies of the system and will give us an excellent insight as to what has happened elsewhere in the Universe.</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa#11</TD>
            <TD>2012-07-17T16:00:21Z</TD>
            <TD>#Infrared, survey, galaxy, Marellanic Cloud#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 1</TD>
            <TD>ivo://wfau.roe.ac.uk/vmcDR1-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/vmcDR1-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://www.star.herts.ac.uk/~mcioni/vmc/</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [1]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#1</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [2]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#2</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [3]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#3</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [4]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#4</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [5]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#5</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [6]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#6</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [7]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#7</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [8]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#8</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [9]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#9</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR4 [10]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#10</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/DirectCone?DSACAT=UKIDSS_DR4&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [11]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#11</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR4 [12]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#12</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [13]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#13</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [14]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#14</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [15]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#15</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [16]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#16</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [17]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#17</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [18]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#18</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR4 [19]</TD>
            <TD>UKIDSS DR4 - UKIRT Infrared Deep Sky Survey Data Release 4</TD>
            <TD>This DSA hosts data release 4 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. The data for the Galactic Plane Survey will not be available until April 22, 2010. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa#19</TD>
            <TD>2012-07-18T12:42:31Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 4</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR4-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR4-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [1]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#1</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [2]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#2</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=lasDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [3]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#3</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [4]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#4</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=dxsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [5]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#5</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [6]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#6</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gcsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [7]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#7</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [8]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#8</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=udsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [9]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#9</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsSource&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>UKIDSS DR5 [10]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#10</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/DirectCone?DSACAT=UKIDSS_DR5&amp;DSATAB=gpsDetection&amp;</TD>
            <TD>1.500000</TD>
            <TD>2000000</TD>
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [11]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#11</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/TAP</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/TAP</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Custom Service</TD>
            <TD>UKIDSS DR5 [12]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#12</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD>CeaCapability</TD>
            <TD>ivo://org.astrogrid/std/CEA/v1.0</TD>
            <TD />
            <TD>CECInterface</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/services/CommonExecutionConnectorService</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [13]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#13</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [14]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#14</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#capabilities</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/capabilities</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [15]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#15</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [16]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#16</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/VOSI#availability</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/availability</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [17]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#17</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#tables</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/tables</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [18]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#18</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://org.astrogrid/std/VOSI/v0.3#ceaApplication</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/VOSI/applications</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>UKIDSS DR5 [19]</TD>
            <TD>UKIDSS DR5 - UKIRT Infrared Deep Sky Survey Data Release 5</TD>
            <TD>This DSA hosts data release 5 of the UKIRT Infrared Deep Sky Survey housed at the Wide Field Astronomy Unit at the Univeristy of Edinburgh. This catalog contains WFCAM data primarily originating from four of the five UKIDSS surveys: Large Area Survey, Galactic Clusters Survey, Deep Extragalactic Survey and the Ultra Deep Survey. (see www.ukidss.org for survey descriptions)</TD>
            <TD>WFAU, Institute for Astronomy, University of Edinburgh</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa#19</TD>
            <TD>2012-07-18T12:43:17Z</TD>
            <TD>#Infrared, survey, galaxy, point source#</TD>
            <TD>#Survey#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>Data Release 5</TD>
            <TD>ivo://wfau.roe.ac.uk/ukidssDR5-dsa</TD>
            <TD />
            <TD>ivo://ivoa.net/std/Delegation</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://wfaudata.roe.ac.uk/ukidssDR5-dsa/delegations</TD>
            <TD />
            <TD />
            <TD>ivo://wfau.roe.ac.uk</TD>
            <TD>http://surveys.roe.ac.uk/wsa</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1807 [1]</TD>
            <TD>SDSS galaxy clusters redshifts (Goto+, 2002)</TD>
            <TD>We describe an automated method, the cut-and-enhance (CE) method, for detecting clusters of galaxies in multicolor optical imaging surveys. This method uses simple color cuts, combined with a density enhancement algorithm, to up-weight pairs of galaxies that are close in both angular separation and color. The method is semiparametric, since it uses minimal assumptions about cluster properties in order to minimize possible biases. No assumptions are made about the shape of clusters, their radial profile, or their luminosity function. The method is successful in finding systems ranging from poor to rich clusters of galaxies, of both regular and irregular shape. We determine the selection function of the CE method via extensive Monte Carlo simulations that use both the real, observed background of galaxies and a randomized background of galaxies. We use position-shuffled and color-shuffled data to perform false-positive tests. We have also visually checked all the clusters detected by the CE method. We apply the CE method to the 350{deg}^2^ of the Sloan Digital Sky Survey (SDSS) commissioning data, taken in 1998 September and 1999 March, and construct an SDSS CE galaxy cluster catalog with an estimated redshift and richness for each cluster. The CE method is compared with other cluster selection methods used on SDSS data such as the matched filter, "maxBCG," and Voronoi tessellation techniques. The CE method can be adopted for cluster selection in any multicolor imaging survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807#1</TD>
            <TD>2012-07-19T08:09:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1807 [2]</TD>
            <TD>SDSS galaxy clusters redshifts (Goto+, 2002)</TD>
            <TD>We describe an automated method, the cut-and-enhance (CE) method, for detecting clusters of galaxies in multicolor optical imaging surveys. This method uses simple color cuts, combined with a density enhancement algorithm, to up-weight pairs of galaxies that are close in both angular separation and color. The method is semiparametric, since it uses minimal assumptions about cluster properties in order to minimize possible biases. No assumptions are made about the shape of clusters, their radial profile, or their luminosity function. The method is successful in finding systems ranging from poor to rich clusters of galaxies, of both regular and irregular shape. We determine the selection function of the CE method via extensive Monte Carlo simulations that use both the real, observed background of galaxies and a randomized background of galaxies. We use position-shuffled and color-shuffled data to perform false-positive tests. We have also visually checked all the clusters detected by the CE method. We apply the CE method to the 350{deg}^2^ of the Sloan Digital Sky Survey (SDSS) commissioning data, taken in 1998 September and 1999 March, and construct an SDSS CE galaxy cluster catalog with an estimated redshift and richness for each cluster. The CE method is compared with other cluster selection methods used on SDSS data such as the matched filter, "maxBCG," and Voronoi tessellation techniques. The CE method can be adopted for cluster selection in any multicolor imaging survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807#2</TD>
            <TD>2012-07-19T08:09:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1807</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1807 [clusters]</TD>
            <TD>SDSS galaxy clusters redshifts (Goto+, 2002)</TD>
            <TD>We describe an automated method, the cut-and-enhance (CE) method, for detecting clusters of galaxies in multicolor optical imaging surveys. This method uses simple color cuts, combined with a density enhancement algorithm, to up-weight pairs of galaxies that are close in both angular separation and color. The method is semiparametric, since it uses minimal assumptions about cluster properties in order to minimize possible biases. No assumptions are made about the shape of clusters, their radial profile, or their luminosity function. The method is successful in finding systems ranging from poor to rich clusters of galaxies, of both regular and irregular shape. We determine the selection function of the CE method via extensive Monte Carlo simulations that use both the real, observed background of galaxies and a randomized background of galaxies. We use position-shuffled and color-shuffled data to perform false-positive tests. We have also visually checked all the clusters detected by the CE method. We apply the CE method to the 350{deg}^2^ of the Sloan Digital Sky Survey (SDSS) commissioning data, taken in 1998 September and 1999 March, and construct an SDSS CE galaxy cluster catalog with an estimated redshift and richness for each cluster. The CE method is compared with other cluster selection methods used on SDSS data such as the matched filter, "maxBCG," and Voronoi tessellation techniques. The CE method can be adopted for cluster selection in any multicolor imaging survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807#clusters</TD>
            <TD>2012-07-19T08:09:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1807&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1807 [1]</TD>
            <TD>SDSS galaxy clusters redshifts (Goto+, 2002)</TD>
            <TD>We describe an automated method, the cut-and-enhance (CE) method, for detecting clusters of galaxies in multicolor optical imaging surveys. This method uses simple color cuts, combined with a density enhancement algorithm, to up-weight pairs of galaxies that are close in both angular separation and color. The method is semiparametric, since it uses minimal assumptions about cluster properties in order to minimize possible biases. No assumptions are made about the shape of clusters, their radial profile, or their luminosity function. The method is successful in finding systems ranging from poor to rich clusters of galaxies, of both regular and irregular shape. We determine the selection function of the CE method via extensive Monte Carlo simulations that use both the real, observed background of galaxies and a randomized background of galaxies. We use position-shuffled and color-shuffled data to perform false-positive tests. We have also visually checked all the clusters detected by the CE method. We apply the CE method to the 350{deg}^2^ of the Sloan Digital Sky Survey (SDSS) commissioning data, taken in 1998 September and 1999 March, and construct an SDSS CE galaxy cluster catalog with an estimated redshift and richness for each cluster. The CE method is compared with other cluster selection methods used on SDSS data such as the matched filter, "maxBCG," and Voronoi tessellation techniques. The CE method can be adopted for cluster selection in any multicolor imaging survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807#1</TD>
            <TD>2012-07-19T08:09:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1807 [2]</TD>
            <TD>SDSS galaxy clusters redshifts (Goto+, 2002)</TD>
            <TD>We describe an automated method, the cut-and-enhance (CE) method, for detecting clusters of galaxies in multicolor optical imaging surveys. This method uses simple color cuts, combined with a density enhancement algorithm, to up-weight pairs of galaxies that are close in both angular separation and color. The method is semiparametric, since it uses minimal assumptions about cluster properties in order to minimize possible biases. No assumptions are made about the shape of clusters, their radial profile, or their luminosity function. The method is successful in finding systems ranging from poor to rich clusters of galaxies, of both regular and irregular shape. We determine the selection function of the CE method via extensive Monte Carlo simulations that use both the real, observed background of galaxies and a randomized background of galaxies. We use position-shuffled and color-shuffled data to perform false-positive tests. We have also visually checked all the clusters detected by the CE method. We apply the CE method to the 350{deg}^2^ of the Sloan Digital Sky Survey (SDSS) commissioning data, taken in 1998 September and 1999 March, and construct an SDSS CE galaxy cluster catalog with an estimated redshift and richness for each cluster. The CE method is compared with other cluster selection methods used on SDSS data such as the matched filter, "maxBCG," and Voronoi tessellation techniques. The CE method can be adopted for cluster selection in any multicolor imaging survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807#2</TD>
            <TD>2012-07-19T08:09:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1807</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1807 [clusters]</TD>
            <TD>SDSS galaxy clusters redshifts (Goto+, 2002)</TD>
            <TD>We describe an automated method, the cut-and-enhance (CE) method, for detecting clusters of galaxies in multicolor optical imaging surveys. This method uses simple color cuts, combined with a density enhancement algorithm, to up-weight pairs of galaxies that are close in both angular separation and color. The method is semiparametric, since it uses minimal assumptions about cluster properties in order to minimize possible biases. No assumptions are made about the shape of clusters, their radial profile, or their luminosity function. The method is successful in finding systems ranging from poor to rich clusters of galaxies, of both regular and irregular shape. We determine the selection function of the CE method via extensive Monte Carlo simulations that use both the real, observed background of galaxies and a randomized background of galaxies. We use position-shuffled and color-shuffled data to perform false-positive tests. We have also visually checked all the clusters detected by the CE method. We apply the CE method to the 350{deg}^2^ of the Sloan Digital Sky Survey (SDSS) commissioning data, taken in 1998 September and 1999 March, and construct an SDSS CE galaxy cluster catalog with an estimated redshift and richness for each cluster. The CE method is compared with other cluster selection methods used on SDSS data such as the matched filter, "maxBCG," and Voronoi tessellation techniques. The CE method can be adopted for cluster selection in any multicolor imaging survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807#clusters</TD>
            <TD>2012-07-19T08:09:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1807&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1807</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/123/1807 [1]</TD>
            <TD>SDSS galaxy clusters redshifts (Goto+, 2002)</TD>
            <TD>We describe an automated method, the cut-and-enhance (CE) method, for detecting clusters of galaxies in multicolor optical imaging surveys. This method uses simple color cuts, combined with a density enhancement algorithm, to up-weight pairs of galaxies that are close in both angular separation and color. The method is semiparametric, since it uses minimal assumptions about cluster properties in order to minimize possible biases. No assumptions are made about the shape of clusters, their radial profile, or their luminosity function. The method is successful in finding systems ranging from poor to rich clusters of galaxies, of both regular and irregular shape. We determine the selection function of the CE method via extensive Monte Carlo simulations that use both the real, observed background of galaxies and a randomized background of galaxies. We use position-shuffled and color-shuffled data to perform false-positive tests. We have also visually checked all the clusters detected by the CE method. We apply the CE method to the 350{deg}^2^ of the Sloan Digital Sky Survey (SDSS) commissioning data, taken in 1998 September and 1999 March, and construct an SDSS CE galaxy cluster catalog with an estimated redshift and richness for each cluster. The CE method is compared with other cluster selection methods used on SDSS data such as the matched filter, "maxBCG," and Voronoi tessellation techniques. The CE method can be adopted for cluster selection in any multicolor imaging survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807#1</TD>
            <TD>2012-07-19T08:09:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/123/1807</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1807</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/123/1807 [2]</TD>
            <TD>SDSS galaxy clusters redshifts (Goto+, 2002)</TD>
            <TD>We describe an automated method, the cut-and-enhance (CE) method, for detecting clusters of galaxies in multicolor optical imaging surveys. This method uses simple color cuts, combined with a density enhancement algorithm, to up-weight pairs of galaxies that are close in both angular separation and color. The method is semiparametric, since it uses minimal assumptions about cluster properties in order to minimize possible biases. No assumptions are made about the shape of clusters, their radial profile, or their luminosity function. The method is successful in finding systems ranging from poor to rich clusters of galaxies, of both regular and irregular shape. We determine the selection function of the CE method via extensive Monte Carlo simulations that use both the real, observed background of galaxies and a randomized background of galaxies. We use position-shuffled and color-shuffled data to perform false-positive tests. We have also visually checked all the clusters detected by the CE method. We apply the CE method to the 350{deg}^2^ of the Sloan Digital Sky Survey (SDSS) commissioning data, taken in 1998 September and 1999 March, and construct an SDSS CE galaxy cluster catalog with an estimated redshift and richness for each cluster. The CE method is compared with other cluster selection methods used on SDSS data such as the matched filter, "maxBCG," and Voronoi tessellation techniques. The CE method can be adopted for cluster selection in any multicolor imaging survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807#2</TD>
            <TD>2012-07-19T08:09:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/123/1807&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1807</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/123/1807 [clusters]</TD>
            <TD>SDSS galaxy clusters redshifts (Goto+, 2002)</TD>
            <TD>We describe an automated method, the cut-and-enhance (CE) method, for detecting clusters of galaxies in multicolor optical imaging surveys. This method uses simple color cuts, combined with a density enhancement algorithm, to up-weight pairs of galaxies that are close in both angular separation and color. The method is semiparametric, since it uses minimal assumptions about cluster properties in order to minimize possible biases. No assumptions are made about the shape of clusters, their radial profile, or their luminosity function. The method is successful in finding systems ranging from poor to rich clusters of galaxies, of both regular and irregular shape. We determine the selection function of the CE method via extensive Monte Carlo simulations that use both the real, observed background of galaxies and a randomized background of galaxies. We use position-shuffled and color-shuffled data to perform false-positive tests. We have also visually checked all the clusters detected by the CE method. We apply the CE method to the 350{deg}^2^ of the Sloan Digital Sky Survey (SDSS) commissioning data, taken in 1998 September and 1999 March, and construct an SDSS CE galaxy cluster catalog with an estimated redshift and richness for each cluster. The CE method is compared with other cluster selection methods used on SDSS data such as the matched filter, "maxBCG," and Voronoi tessellation techniques. The CE method can be adopted for cluster selection in any multicolor imaging survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807#clusters</TD>
            <TD>2012-07-19T08:09:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-May-2002</TD>
            <TD>ivo://CDS.VizieR/J/AJ/123/1807</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/123/1807&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/123/1807</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>WMAPILC5YR [1]</TD>
            <TD>WMAP Five Year Galaxy Removed</TD>
            <TD>These survey represents a combination of the 5-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body. &lt;p&gt; The original data are available at the &lt;http://lambda.gsfc.nasa.gov&gt;LAMBDA archive&lt;/a&gt;. &lt;p&gt; The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the WMAP data. &lt;/p&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/skyview/wmapilc5yr#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/wmapilc5yr</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=wmapilc5yr&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WMAPILC5YR [2]</TD>
            <TD>WMAP Five Year Galaxy Removed</TD>
            <TD>These survey represents a combination of the 5-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body. &lt;p&gt; The original data are available at the &lt;http://lambda.gsfc.nasa.gov&gt;LAMBDA archive&lt;/a&gt;. &lt;p&gt; The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the WMAP data. &lt;/p&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/skyview/wmapilc5yr#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/wmapilc5yr</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>WMAPILC5YR [1]</TD>
            <TD>WMAP Five Year Galaxy Removed</TD>
            <TD>These survey represents a combination of the 5-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body. &lt;p&gt; The original data are available at the &lt;http://lambda.gsfc.nasa.gov&gt;LAMBDA archive&lt;/a&gt;. &lt;p&gt; The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the WMAP data. &lt;/p&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/skyview/wmapilc5yr#1</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/wmapilc5yr</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/vo/sia.pl?survey=wmapilc5yr&amp;</TD>
            <TD />
            <TD>500</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WMAPILC5YR [2]</TD>
            <TD>WMAP Five Year Galaxy Removed</TD>
            <TD>These survey represents a combination of the 5-year data combined in a way that is intended to minimize the contribution from the galaxy. The data measure the temperature deviation from a uniform black body. &lt;p&gt; The original data are available at the &lt;http://lambda.gsfc.nasa.gov&gt;LAMBDA archive&lt;/a&gt;. &lt;p&gt; The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the WMAP data. &lt;/p&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://nasa.heasarc/skyview/wmapilc5yr#2</TD>
            <TD>2011-06-14T00:00:00Z</TD>
            <TD>#surveys#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/skyview/wmapilc5yr</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://skyview.gsfc.nasa.gov/cgi-bin/query.pl?</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://skyview.gsfc.nasa.gov</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/540/A123 [1]</TD>
            <TD>Galaxy clusters from SDSS DR8 (Einasto+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123#1</TD>
            <TD>2012-08-11T16:20:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/540/A123</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A123</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/540/A123 [2]</TD>
            <TD>Galaxy clusters from SDSS DR8 (Einasto+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123#2</TD>
            <TD>2012-08-11T16:20:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/540/A123&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A123 [table3]</TD>
            <TD>Galaxy clusters from SDSS DR8 (Einasto+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123#table3</TD>
            <TD>2012-08-11T16:20:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A123</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/540/A123 [1]</TD>
            <TD>Galaxy clusters from SDSS DR8 (Einasto+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123#1</TD>
            <TD>2012-08-11T16:20:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/540/A123</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A123</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/540/A123 [2]</TD>
            <TD>Galaxy clusters from SDSS DR8 (Einasto+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123#2</TD>
            <TD>2012-08-11T16:20:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/540/A123&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A123 [table3]</TD>
            <TD>Galaxy clusters from SDSS DR8 (Einasto+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123#table3</TD>
            <TD>2012-08-11T16:20:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A123</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/540/A123 [1]</TD>
            <TD>Galaxy clusters from SDSS DR8 (Einasto+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123#1</TD>
            <TD>2012-08-11T16:20:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/540/A123</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A123</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/540/A123 [2]</TD>
            <TD>Galaxy clusters from SDSS DR8 (Einasto+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123#2</TD>
            <TD>2012-08-11T16:20:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/540/A123&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A123</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/540/A123 [table3]</TD>
            <TD>Galaxy clusters from SDSS DR8 (Einasto+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123#table3</TD>
            <TD>2012-08-11T16:20:03Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/A+A/540/A123</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/540/A123&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/540/A123</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/721/369 [1]</TD>
            <TD>PNe in the elliptical galaxy NGC 821 (Teodorescu+, 2010)</TD>
            <TD>The observations were made by one of us (R.H.M.) with the Faint Object Camera and Spectrograph (FOCAS) attached to the Cassegrain focus of the 8.2m Subaru telescope, Mauna Kea, Hawaii, on three nights, 2004 November 7-9. The radial velocities were measured using a slitless method (see Section 2.2) involving images taken through both the on-band filter and an echelle grism. The on-band filter has a central wavelength of 5025{AA}, an FWHM of 60{AA}, a peak transmission of 0.68, and an equivalent width of 40{AA}. We conservatively estimate the calibration errors in FOCAS slitless radial velocities to be of the order of 10km/s. We estimate an rms of about 0.3" for the astrometry of our catalog of PNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369#1</TD>
            <TD>2012-08-22T12:08:36Z</TD>
            <TD>#Stars#Galaxies#Spectroscopy#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/721/369</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/369</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/721/369 [2]</TD>
            <TD>PNe in the elliptical galaxy NGC 821 (Teodorescu+, 2010)</TD>
            <TD>The observations were made by one of us (R.H.M.) with the Faint Object Camera and Spectrograph (FOCAS) attached to the Cassegrain focus of the 8.2m Subaru telescope, Mauna Kea, Hawaii, on three nights, 2004 November 7-9. The radial velocities were measured using a slitless method (see Section 2.2) involving images taken through both the on-band filter and an echelle grism. The on-band filter has a central wavelength of 5025{AA}, an FWHM of 60{AA}, a peak transmission of 0.68, and an equivalent width of 40{AA}. We conservatively estimate the calibration errors in FOCAS slitless radial velocities to be of the order of 10km/s. We estimate an rms of about 0.3" for the astrometry of our catalog of PNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369#2</TD>
            <TD>2012-08-22T12:08:36Z</TD>
            <TD>#Stars#Galaxies#Spectroscopy#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/721/369&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/369</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/369 [table2]</TD>
            <TD>PNe in the elliptical galaxy NGC 821 (Teodorescu+, 2010)</TD>
            <TD>The observations were made by one of us (R.H.M.) with the Faint Object Camera and Spectrograph (FOCAS) attached to the Cassegrain focus of the 8.2m Subaru telescope, Mauna Kea, Hawaii, on three nights, 2004 November 7-9. The radial velocities were measured using a slitless method (see Section 2.2) involving images taken through both the on-band filter and an echelle grism. The on-band filter has a central wavelength of 5025{AA}, an FWHM of 60{AA}, a peak transmission of 0.68, and an equivalent width of 40{AA}. We conservatively estimate the calibration errors in FOCAS slitless radial velocities to be of the order of 10km/s. We estimate an rms of about 0.3" for the astrometry of our catalog of PNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369#table2</TD>
            <TD>2012-08-22T12:08:36Z</TD>
            <TD>#Stars#Galaxies#Spectroscopy#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/369&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/369</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/721/369 [1]</TD>
            <TD>PNe in the elliptical galaxy NGC 821 (Teodorescu+, 2010)</TD>
            <TD>The observations were made by one of us (R.H.M.) with the Faint Object Camera and Spectrograph (FOCAS) attached to the Cassegrain focus of the 8.2m Subaru telescope, Mauna Kea, Hawaii, on three nights, 2004 November 7-9. The radial velocities were measured using a slitless method (see Section 2.2) involving images taken through both the on-band filter and an echelle grism. The on-band filter has a central wavelength of 5025{AA}, an FWHM of 60{AA}, a peak transmission of 0.68, and an equivalent width of 40{AA}. We conservatively estimate the calibration errors in FOCAS slitless radial velocities to be of the order of 10km/s. We estimate an rms of about 0.3" for the astrometry of our catalog of PNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369#1</TD>
            <TD>2012-08-22T12:08:36Z</TD>
            <TD>#Stars#Galaxies#Spectroscopy#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/721/369</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/369</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/721/369 [2]</TD>
            <TD>PNe in the elliptical galaxy NGC 821 (Teodorescu+, 2010)</TD>
            <TD>The observations were made by one of us (R.H.M.) with the Faint Object Camera and Spectrograph (FOCAS) attached to the Cassegrain focus of the 8.2m Subaru telescope, Mauna Kea, Hawaii, on three nights, 2004 November 7-9. The radial velocities were measured using a slitless method (see Section 2.2) involving images taken through both the on-band filter and an echelle grism. The on-band filter has a central wavelength of 5025{AA}, an FWHM of 60{AA}, a peak transmission of 0.68, and an equivalent width of 40{AA}. We conservatively estimate the calibration errors in FOCAS slitless radial velocities to be of the order of 10km/s. We estimate an rms of about 0.3" for the astrometry of our catalog of PNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369#2</TD>
            <TD>2012-08-22T12:08:36Z</TD>
            <TD>#Stars#Galaxies#Spectroscopy#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/721/369&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/369</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/369 [table2]</TD>
            <TD>PNe in the elliptical galaxy NGC 821 (Teodorescu+, 2010)</TD>
            <TD>The observations were made by one of us (R.H.M.) with the Faint Object Camera and Spectrograph (FOCAS) attached to the Cassegrain focus of the 8.2m Subaru telescope, Mauna Kea, Hawaii, on three nights, 2004 November 7-9. The radial velocities were measured using a slitless method (see Section 2.2) involving images taken through both the on-band filter and an echelle grism. The on-band filter has a central wavelength of 5025{AA}, an FWHM of 60{AA}, a peak transmission of 0.68, and an equivalent width of 40{AA}. We conservatively estimate the calibration errors in FOCAS slitless radial velocities to be of the order of 10km/s. We estimate an rms of about 0.3" for the astrometry of our catalog of PNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369#table2</TD>
            <TD>2012-08-22T12:08:36Z</TD>
            <TD>#Stars#Galaxies#Spectroscopy#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/369&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/369</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/721/369 [1]</TD>
            <TD>PNe in the elliptical galaxy NGC 821 (Teodorescu+, 2010)</TD>
            <TD>The observations were made by one of us (R.H.M.) with the Faint Object Camera and Spectrograph (FOCAS) attached to the Cassegrain focus of the 8.2m Subaru telescope, Mauna Kea, Hawaii, on three nights, 2004 November 7-9. The radial velocities were measured using a slitless method (see Section 2.2) involving images taken through both the on-band filter and an echelle grism. The on-band filter has a central wavelength of 5025{AA}, an FWHM of 60{AA}, a peak transmission of 0.68, and an equivalent width of 40{AA}. We conservatively estimate the calibration errors in FOCAS slitless radial velocities to be of the order of 10km/s. We estimate an rms of about 0.3" for the astrometry of our catalog of PNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369#1</TD>
            <TD>2012-08-22T12:08:36Z</TD>
            <TD>#Stars#Galaxies#Spectroscopy#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/721/369</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/369</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/721/369 [2]</TD>
            <TD>PNe in the elliptical galaxy NGC 821 (Teodorescu+, 2010)</TD>
            <TD>The observations were made by one of us (R.H.M.) with the Faint Object Camera and Spectrograph (FOCAS) attached to the Cassegrain focus of the 8.2m Subaru telescope, Mauna Kea, Hawaii, on three nights, 2004 November 7-9. The radial velocities were measured using a slitless method (see Section 2.2) involving images taken through both the on-band filter and an echelle grism. The on-band filter has a central wavelength of 5025{AA}, an FWHM of 60{AA}, a peak transmission of 0.68, and an equivalent width of 40{AA}. We conservatively estimate the calibration errors in FOCAS slitless radial velocities to be of the order of 10km/s. We estimate an rms of about 0.3" for the astrometry of our catalog of PNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369#2</TD>
            <TD>2012-08-22T12:08:36Z</TD>
            <TD>#Stars#Galaxies#Spectroscopy#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/721/369&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/369</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/721/369 [table2]</TD>
            <TD>PNe in the elliptical galaxy NGC 821 (Teodorescu+, 2010)</TD>
            <TD>The observations were made by one of us (R.H.M.) with the Faint Object Camera and Spectrograph (FOCAS) attached to the Cassegrain focus of the 8.2m Subaru telescope, Mauna Kea, Hawaii, on three nights, 2004 November 7-9. The radial velocities were measured using a slitless method (see Section 2.2) involving images taken through both the on-band filter and an echelle grism. The on-band filter has a central wavelength of 5025{AA}, an FWHM of 60{AA}, a peak transmission of 0.68, and an equivalent width of 40{AA}. We conservatively estimate the calibration errors in FOCAS slitless radial velocities to be of the order of 10km/s. We estimate an rms of about 0.3" for the astrometry of our catalog of PNs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369#table2</TD>
            <TD>2012-08-22T12:08:36Z</TD>
            <TD>#Stars#Galaxies#Spectroscopy#Planetary_Nebulae#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/721/369</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/721/369&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/721/369</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/462 [1]</TD>
            <TD>Intermediate-mass star-forming regions (Arvidsson+, 2010)</TD>
            <TD>In an effort to understand the factors that govern the transition from low- to high-mass star formation, for the first time we identify a sample of intermediate-mass star-forming regions (IM SFRs) where stars up to (but not exceeding) ~8M_{sun}_ are being produced. We use IRAS colors and Spitzer Space Telescope mid-IR images, in conjunction with millimeter continuum and ^13^CO maps, to compile a sample of 50 IM SFRs in the inner Galaxy. These are likely to be precursors to Herbig AeBe stars and their associated clusters of low-mass stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462#1</TD>
            <TD>2012-08-22T12:08:59Z</TD>
            <TD>#Associations#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/462</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/462</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/462 [2]</TD>
            <TD>Intermediate-mass star-forming regions (Arvidsson+, 2010)</TD>
            <TD>In an effort to understand the factors that govern the transition from low- to high-mass star formation, for the first time we identify a sample of intermediate-mass star-forming regions (IM SFRs) where stars up to (but not exceeding) ~8M_{sun}_ are being produced. We use IRAS colors and Spitzer Space Telescope mid-IR images, in conjunction with millimeter continuum and ^13^CO maps, to compile a sample of 50 IM SFRs in the inner Galaxy. These are likely to be precursors to Herbig AeBe stars and their associated clusters of low-mass stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462#2</TD>
            <TD>2012-08-22T12:08:59Z</TD>
            <TD>#Associations#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/462&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/462</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/462 [SFRs]</TD>
            <TD>Intermediate-mass star-forming regions (Arvidsson+, 2010)</TD>
            <TD>In an effort to understand the factors that govern the transition from low- to high-mass star formation, for the first time we identify a sample of intermediate-mass star-forming regions (IM SFRs) where stars up to (but not exceeding) ~8M_{sun}_ are being produced. We use IRAS colors and Spitzer Space Telescope mid-IR images, in conjunction with millimeter continuum and ^13^CO maps, to compile a sample of 50 IM SFRs in the inner Galaxy. These are likely to be precursors to Herbig AeBe stars and their associated clusters of low-mass stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462#SFRs</TD>
            <TD>2012-08-22T12:08:59Z</TD>
            <TD>#Associations#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/462&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/462</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/462 [1]</TD>
            <TD>Intermediate-mass star-forming regions (Arvidsson+, 2010)</TD>
            <TD>In an effort to understand the factors that govern the transition from low- to high-mass star formation, for the first time we identify a sample of intermediate-mass star-forming regions (IM SFRs) where stars up to (but not exceeding) ~8M_{sun}_ are being produced. We use IRAS colors and Spitzer Space Telescope mid-IR images, in conjunction with millimeter continuum and ^13^CO maps, to compile a sample of 50 IM SFRs in the inner Galaxy. These are likely to be precursors to Herbig AeBe stars and their associated clusters of low-mass stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462#1</TD>
            <TD>2012-08-22T12:08:59Z</TD>
            <TD>#Associations#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/462</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/462</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/462 [2]</TD>
            <TD>Intermediate-mass star-forming regions (Arvidsson+, 2010)</TD>
            <TD>In an effort to understand the factors that govern the transition from low- to high-mass star formation, for the first time we identify a sample of intermediate-mass star-forming regions (IM SFRs) where stars up to (but not exceeding) ~8M_{sun}_ are being produced. We use IRAS colors and Spitzer Space Telescope mid-IR images, in conjunction with millimeter continuum and ^13^CO maps, to compile a sample of 50 IM SFRs in the inner Galaxy. These are likely to be precursors to Herbig AeBe stars and their associated clusters of low-mass stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462#2</TD>
            <TD>2012-08-22T12:08:59Z</TD>
            <TD>#Associations#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/462&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/462</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/462 [SFRs]</TD>
            <TD>Intermediate-mass star-forming regions (Arvidsson+, 2010)</TD>
            <TD>In an effort to understand the factors that govern the transition from low- to high-mass star formation, for the first time we identify a sample of intermediate-mass star-forming regions (IM SFRs) where stars up to (but not exceeding) ~8M_{sun}_ are being produced. We use IRAS colors and Spitzer Space Telescope mid-IR images, in conjunction with millimeter continuum and ^13^CO maps, to compile a sample of 50 IM SFRs in the inner Galaxy. These are likely to be precursors to Herbig AeBe stars and their associated clusters of low-mass stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462#SFRs</TD>
            <TD>2012-08-22T12:08:59Z</TD>
            <TD>#Associations#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/462&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/462</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/462 [1]</TD>
            <TD>Intermediate-mass star-forming regions (Arvidsson+, 2010)</TD>
            <TD>In an effort to understand the factors that govern the transition from low- to high-mass star formation, for the first time we identify a sample of intermediate-mass star-forming regions (IM SFRs) where stars up to (but not exceeding) ~8M_{sun}_ are being produced. We use IRAS colors and Spitzer Space Telescope mid-IR images, in conjunction with millimeter continuum and ^13^CO maps, to compile a sample of 50 IM SFRs in the inner Galaxy. These are likely to be precursors to Herbig AeBe stars and their associated clusters of low-mass stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462#1</TD>
            <TD>2012-08-22T12:08:59Z</TD>
            <TD>#Associations#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/462</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/462</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/462 [2]</TD>
            <TD>Intermediate-mass star-forming regions (Arvidsson+, 2010)</TD>
            <TD>In an effort to understand the factors that govern the transition from low- to high-mass star formation, for the first time we identify a sample of intermediate-mass star-forming regions (IM SFRs) where stars up to (but not exceeding) ~8M_{sun}_ are being produced. We use IRAS colors and Spitzer Space Telescope mid-IR images, in conjunction with millimeter continuum and ^13^CO maps, to compile a sample of 50 IM SFRs in the inner Galaxy. These are likely to be precursors to Herbig AeBe stars and their associated clusters of low-mass stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462#2</TD>
            <TD>2012-08-22T12:08:59Z</TD>
            <TD>#Associations#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/462&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/462</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/462 [SFRs]</TD>
            <TD>Intermediate-mass star-forming regions (Arvidsson+, 2010)</TD>
            <TD>In an effort to understand the factors that govern the transition from low- to high-mass star formation, for the first time we identify a sample of intermediate-mass star-forming regions (IM SFRs) where stars up to (but not exceeding) ~8M_{sun}_ are being produced. We use IRAS colors and Spitzer Space Telescope mid-IR images, in conjunction with millimeter continuum and ^13^CO maps, to compile a sample of 50 IM SFRs in the inner Galaxy. These are likely to be precursors to Herbig AeBe stars and their associated clusters of low-mass stars.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462#SFRs</TD>
            <TD>2012-08-22T12:08:59Z</TD>
            <TD>#Associations#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>15-Jun-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/462</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/462&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/462</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/200/12 [1]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#1</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/200/12</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/200/12 [2]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#2</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/200/12&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/12 [table1]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#table1</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/12&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/12 [table4]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#table4</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/12&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/200/12 [1]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#1</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/200/12</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/200/12 [2]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#2</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/200/12&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/12 [table1]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#table1</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/12&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/12 [table4]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#table4</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/12&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/200/12 [1]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#1</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/200/12</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/200/12 [2]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#2</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/200/12&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/12 [table1]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#table1</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/12&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/12 [table4]</TD>
            <TD>CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)</TD>
            <TD>The CfA4 sample consists of 5522 light-curve points. All 94 SNe have BVr'i' measurements, while 14 have U and 12 have u'. The CfA4 data were obtained on the 1.2m telescope at the FLWO using the single-chip, four-amplifier CCD KeplerCam. CfA4 data processing followed the same three steps used for CfA3: reduction, calibration, and host-galaxy subtraction (see Hicken et al. 2009, Cat. J/ApJ/700/331 for a more detailed treatment).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12#table4</TD>
            <TD>2012-08-27T15:25:22Z</TD>
            <TD>#Photometry:wide-band#SuperNovae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/12</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/12&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/12</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/1987 [1]</TD>
            <TD>SDSS-GALEX QSO catalog (Hutchings+, 2010)</TD>
            <TD>We discuss a sample of ~60000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5-1.5. We use SDSS spectra of a subsample of ~4500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. We discuss the distributions of redshift, luminosity, and reddening of the 19100 QSOs (~96%) that we estimate to be present in the final sample of 19812 point sources.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987#1</TD>
            <TD>2012-08-29T13:25:43Z</TD>
            <TD>#Photometry#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/1987</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1987</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/1987 [2]</TD>
            <TD>SDSS-GALEX QSO catalog (Hutchings+, 2010)</TD>
            <TD>We discuss a sample of ~60000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5-1.5. We use SDSS spectra of a subsample of ~4500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. We discuss the distributions of redshift, luminosity, and reddening of the 19100 QSOs (~96%) that we estimate to be present in the final sample of 19812 point sources.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987#2</TD>
            <TD>2012-08-29T13:25:43Z</TD>
            <TD>#Photometry#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/1987&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1987</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1987 [table2]</TD>
            <TD>SDSS-GALEX QSO catalog (Hutchings+, 2010)</TD>
            <TD>We discuss a sample of ~60000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5-1.5. We use SDSS spectra of a subsample of ~4500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. We discuss the distributions of redshift, luminosity, and reddening of the 19100 QSOs (~96%) that we estimate to be present in the final sample of 19812 point sources.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987#table2</TD>
            <TD>2012-08-29T13:25:43Z</TD>
            <TD>#Photometry#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1987&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1987</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/1987 [1]</TD>
            <TD>SDSS-GALEX QSO catalog (Hutchings+, 2010)</TD>
            <TD>We discuss a sample of ~60000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5-1.5. We use SDSS spectra of a subsample of ~4500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. We discuss the distributions of redshift, luminosity, and reddening of the 19100 QSOs (~96%) that we estimate to be present in the final sample of 19812 point sources.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987#1</TD>
            <TD>2012-08-29T13:25:43Z</TD>
            <TD>#Photometry#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/1987</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1987</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/1987 [2]</TD>
            <TD>SDSS-GALEX QSO catalog (Hutchings+, 2010)</TD>
            <TD>We discuss a sample of ~60000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5-1.5. We use SDSS spectra of a subsample of ~4500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. We discuss the distributions of redshift, luminosity, and reddening of the 19100 QSOs (~96%) that we estimate to be present in the final sample of 19812 point sources.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987#2</TD>
            <TD>2012-08-29T13:25:43Z</TD>
            <TD>#Photometry#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/1987&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1987</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1987 [table2]</TD>
            <TD>SDSS-GALEX QSO catalog (Hutchings+, 2010)</TD>
            <TD>We discuss a sample of ~60000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5-1.5. We use SDSS spectra of a subsample of ~4500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. We discuss the distributions of redshift, luminosity, and reddening of the 19100 QSOs (~96%) that we estimate to be present in the final sample of 19812 point sources.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987#table2</TD>
            <TD>2012-08-29T13:25:43Z</TD>
            <TD>#Photometry#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1987&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1987</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/140/1987 [1]</TD>
            <TD>SDSS-GALEX QSO catalog (Hutchings+, 2010)</TD>
            <TD>We discuss a sample of ~60000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5-1.5. We use SDSS spectra of a subsample of ~4500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. We discuss the distributions of redshift, luminosity, and reddening of the 19100 QSOs (~96%) that we estimate to be present in the final sample of 19812 point sources.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987#1</TD>
            <TD>2012-08-29T13:25:43Z</TD>
            <TD>#Photometry#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/140/1987</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1987</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/140/1987 [2]</TD>
            <TD>SDSS-GALEX QSO catalog (Hutchings+, 2010)</TD>
            <TD>We discuss a sample of ~60000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5-1.5. We use SDSS spectra of a subsample of ~4500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. We discuss the distributions of redshift, luminosity, and reddening of the 19100 QSOs (~96%) that we estimate to be present in the final sample of 19812 point sources.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987#2</TD>
            <TD>2012-08-29T13:25:43Z</TD>
            <TD>#Photometry#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/140/1987&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1987</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/140/1987 [table2]</TD>
            <TD>SDSS-GALEX QSO catalog (Hutchings+, 2010)</TD>
            <TD>We discuss a sample of ~60000 objects from the combined Sloan Digital Sky Survey-Galaxy Evolution Explorer (SDSS-GALEX) database with UV-optical colors that should isolate QSOs in the redshift range 0.5-1.5. We use SDSS spectra of a subsample of ~4500 to remove stellar and galaxy contaminants in the sample to a very high level, based on the 7-band photometry. We discuss the distributions of redshift, luminosity, and reddening of the 19100 QSOs (~96%) that we estimate to be present in the final sample of 19812 point sources.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987#table2</TD>
            <TD>2012-08-29T13:25:43Z</TD>
            <TD>#Photometry#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jul-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/140/1987</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/140/1987&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/140/1987</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/724/1389 [1]</TD>
            <TD>Mapping the diffuse UV sky with GALEX (Murthy+, 2010)</TD>
            <TD>The launch of the Galaxy Evolution Explorer (GALEX) in 2003 provided a new platform for diffuse UV observations. In the 7 years since its launch, GALEX has obtained over 30000 observations covering 75% of the sky in two ultraviolet bands (far-ultraviolet, FUV: 1350-1750{AA} and near-ultraviolet, NUV: 1750-2850{AA}). The GALEX instrument consists of a Ritchey-Chretien telescope with a diameter of 50cm for the primary mirror. Light from the sky is separated by a dichroic onto two detectors (FUV and NUV) with a spatial resolution of 3"-5" over a 1.25{deg} field of view.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389#1</TD>
            <TD>2012-09-08T11:53:27Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/724/1389</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/1389</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/724/1389 [2]</TD>
            <TD>Mapping the diffuse UV sky with GALEX (Murthy+, 2010)</TD>
            <TD>The launch of the Galaxy Evolution Explorer (GALEX) in 2003 provided a new platform for diffuse UV observations. In the 7 years since its launch, GALEX has obtained over 30000 observations covering 75% of the sky in two ultraviolet bands (far-ultraviolet, FUV: 1350-1750{AA} and near-ultraviolet, NUV: 1750-2850{AA}). The GALEX instrument consists of a Ritchey-Chretien telescope with a diameter of 50cm for the primary mirror. Light from the sky is separated by a dichroic onto two detectors (FUV and NUV) with a spatial resolution of 3"-5" over a 1.25{deg} field of view.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389#2</TD>
            <TD>2012-09-08T11:53:27Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/724/1389&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/1389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/724/1389 [table1]</TD>
            <TD>Mapping the diffuse UV sky with GALEX (Murthy+, 2010)</TD>
            <TD>The launch of the Galaxy Evolution Explorer (GALEX) in 2003 provided a new platform for diffuse UV observations. In the 7 years since its launch, GALEX has obtained over 30000 observations covering 75% of the sky in two ultraviolet bands (far-ultraviolet, FUV: 1350-1750{AA} and near-ultraviolet, NUV: 1750-2850{AA}). The GALEX instrument consists of a Ritchey-Chretien telescope with a diameter of 50cm for the primary mirror. Light from the sky is separated by a dichroic onto two detectors (FUV and NUV) with a spatial resolution of 3"-5" over a 1.25{deg} field of view.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389#table1</TD>
            <TD>2012-09-08T11:53:27Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/724/1389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/1389</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/724/1389 [1]</TD>
            <TD>Mapping the diffuse UV sky with GALEX (Murthy+, 2010)</TD>
            <TD>The launch of the Galaxy Evolution Explorer (GALEX) in 2003 provided a new platform for diffuse UV observations. In the 7 years since its launch, GALEX has obtained over 30000 observations covering 75% of the sky in two ultraviolet bands (far-ultraviolet, FUV: 1350-1750{AA} and near-ultraviolet, NUV: 1750-2850{AA}). The GALEX instrument consists of a Ritchey-Chretien telescope with a diameter of 50cm for the primary mirror. Light from the sky is separated by a dichroic onto two detectors (FUV and NUV) with a spatial resolution of 3"-5" over a 1.25{deg} field of view.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389#1</TD>
            <TD>2012-09-08T11:53:27Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/724/1389</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/1389</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/724/1389 [2]</TD>
            <TD>Mapping the diffuse UV sky with GALEX (Murthy+, 2010)</TD>
            <TD>The launch of the Galaxy Evolution Explorer (GALEX) in 2003 provided a new platform for diffuse UV observations. In the 7 years since its launch, GALEX has obtained over 30000 observations covering 75% of the sky in two ultraviolet bands (far-ultraviolet, FUV: 1350-1750{AA} and near-ultraviolet, NUV: 1750-2850{AA}). The GALEX instrument consists of a Ritchey-Chretien telescope with a diameter of 50cm for the primary mirror. Light from the sky is separated by a dichroic onto two detectors (FUV and NUV) with a spatial resolution of 3"-5" over a 1.25{deg} field of view.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389#2</TD>
            <TD>2012-09-08T11:53:27Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/724/1389&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/1389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/724/1389 [table1]</TD>
            <TD>Mapping the diffuse UV sky with GALEX (Murthy+, 2010)</TD>
            <TD>The launch of the Galaxy Evolution Explorer (GALEX) in 2003 provided a new platform for diffuse UV observations. In the 7 years since its launch, GALEX has obtained over 30000 observations covering 75% of the sky in two ultraviolet bands (far-ultraviolet, FUV: 1350-1750{AA} and near-ultraviolet, NUV: 1750-2850{AA}). The GALEX instrument consists of a Ritchey-Chretien telescope with a diameter of 50cm for the primary mirror. Light from the sky is separated by a dichroic onto two detectors (FUV and NUV) with a spatial resolution of 3"-5" over a 1.25{deg} field of view.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389#table1</TD>
            <TD>2012-09-08T11:53:27Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/724/1389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/1389</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/724/1389 [1]</TD>
            <TD>Mapping the diffuse UV sky with GALEX (Murthy+, 2010)</TD>
            <TD>The launch of the Galaxy Evolution Explorer (GALEX) in 2003 provided a new platform for diffuse UV observations. In the 7 years since its launch, GALEX has obtained over 30000 observations covering 75% of the sky in two ultraviolet bands (far-ultraviolet, FUV: 1350-1750{AA} and near-ultraviolet, NUV: 1750-2850{AA}). The GALEX instrument consists of a Ritchey-Chretien telescope with a diameter of 50cm for the primary mirror. Light from the sky is separated by a dichroic onto two detectors (FUV and NUV) with a spatial resolution of 3"-5" over a 1.25{deg} field of view.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389#1</TD>
            <TD>2012-09-08T11:53:27Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/724/1389</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/1389</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/724/1389 [2]</TD>
            <TD>Mapping the diffuse UV sky with GALEX (Murthy+, 2010)</TD>
            <TD>The launch of the Galaxy Evolution Explorer (GALEX) in 2003 provided a new platform for diffuse UV observations. In the 7 years since its launch, GALEX has obtained over 30000 observations covering 75% of the sky in two ultraviolet bands (far-ultraviolet, FUV: 1350-1750{AA} and near-ultraviolet, NUV: 1750-2850{AA}). The GALEX instrument consists of a Ritchey-Chretien telescope with a diameter of 50cm for the primary mirror. Light from the sky is separated by a dichroic onto two detectors (FUV and NUV) with a spatial resolution of 3"-5" over a 1.25{deg} field of view.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389#2</TD>
            <TD>2012-09-08T11:53:27Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/724/1389&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/1389</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/724/1389 [table1]</TD>
            <TD>Mapping the diffuse UV sky with GALEX (Murthy+, 2010)</TD>
            <TD>The launch of the Galaxy Evolution Explorer (GALEX) in 2003 provided a new platform for diffuse UV observations. In the 7 years since its launch, GALEX has obtained over 30000 observations covering 75% of the sky in two ultraviolet bands (far-ultraviolet, FUV: 1350-1750{AA} and near-ultraviolet, NUV: 1750-2850{AA}). The GALEX instrument consists of a Ritchey-Chretien telescope with a diameter of 50cm for the primary mirror. Light from the sky is separated by a dichroic onto two detectors (FUV and NUV) with a spatial resolution of 3"-5" over a 1.25{deg} field of view.</TD>
            <TD>CDS</TD>
            <TD>#UV#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389#table1</TD>
            <TD>2012-09-08T11:53:27Z</TD>
            <TD>#Interstellar_Medium#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2012</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/724/1389</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/724/1389&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/724/1389</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/25/18 [1]</TD>
            <TD>Spectroscopy of H{alpha} blue stars in M 33 (Sholukhova+, 1999)</TD>
            <TD>Multiobject spectroscopy for 118 blue stars with an H{alpha} excess in the galaxy M 33 from the lists of SS 433 and LBV candidates and other rare types of massive stars is presented. The H{alpha} parameters and the relative intensities of the [NII]6584{AA} and [SII]6716{AA} lines are given. We identified stars with a broad H{alpha} emission line, which is probably emitted in the stellar wind.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18#1</TD>
            <TD>2012-10-24T13:16:43Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-April-2000</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/25/18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/25/18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/25/18 [2]</TD>
            <TD>Spectroscopy of H{alpha} blue stars in M 33 (Sholukhova+, 1999)</TD>
            <TD>Multiobject spectroscopy for 118 blue stars with an H{alpha} excess in the galaxy M 33 from the lists of SS 433 and LBV candidates and other rare types of massive stars is presented. The H{alpha} parameters and the relative intensities of the [NII]6584{AA} and [SII]6716{AA} lines are given. We identified stars with a broad H{alpha} emission line, which is probably emitted in the stellar wind.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18#2</TD>
            <TD>2012-10-24T13:16:43Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-April-2000</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/25/18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/25/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/25/18 [object]</TD>
            <TD>Spectroscopy of H{alpha} blue stars in M 33 (Sholukhova+, 1999)</TD>
            <TD>Multiobject spectroscopy for 118 blue stars with an H{alpha} excess in the galaxy M 33 from the lists of SS 433 and LBV candidates and other rare types of massive stars is presented. The H{alpha} parameters and the relative intensities of the [NII]6584{AA} and [SII]6716{AA} lines are given. We identified stars with a broad H{alpha} emission line, which is probably emitted in the stellar wind.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18#object</TD>
            <TD>2012-10-24T13:16:43Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-April-2000</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/25/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/25/18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/25/18 [1]</TD>
            <TD>Spectroscopy of H{alpha} blue stars in M 33 (Sholukhova+, 1999)</TD>
            <TD>Multiobject spectroscopy for 118 blue stars with an H{alpha} excess in the galaxy M 33 from the lists of SS 433 and LBV candidates and other rare types of massive stars is presented. The H{alpha} parameters and the relative intensities of the [NII]6584{AA} and [SII]6716{AA} lines are given. We identified stars with a broad H{alpha} emission line, which is probably emitted in the stellar wind.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18#1</TD>
            <TD>2012-10-24T13:16:43Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-April-2000</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/25/18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/25/18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/25/18 [2]</TD>
            <TD>Spectroscopy of H{alpha} blue stars in M 33 (Sholukhova+, 1999)</TD>
            <TD>Multiobject spectroscopy for 118 blue stars with an H{alpha} excess in the galaxy M 33 from the lists of SS 433 and LBV candidates and other rare types of massive stars is presented. The H{alpha} parameters and the relative intensities of the [NII]6584{AA} and [SII]6716{AA} lines are given. We identified stars with a broad H{alpha} emission line, which is probably emitted in the stellar wind.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18#2</TD>
            <TD>2012-10-24T13:16:43Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-April-2000</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/25/18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/25/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/25/18 [object]</TD>
            <TD>Spectroscopy of H{alpha} blue stars in M 33 (Sholukhova+, 1999)</TD>
            <TD>Multiobject spectroscopy for 118 blue stars with an H{alpha} excess in the galaxy M 33 from the lists of SS 433 and LBV candidates and other rare types of massive stars is presented. The H{alpha} parameters and the relative intensities of the [NII]6584{AA} and [SII]6716{AA} lines are given. We identified stars with a broad H{alpha} emission line, which is probably emitted in the stellar wind.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18#object</TD>
            <TD>2012-10-24T13:16:43Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-April-2000</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/25/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/25/18</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/25/18 [1]</TD>
            <TD>Spectroscopy of H{alpha} blue stars in M 33 (Sholukhova+, 1999)</TD>
            <TD>Multiobject spectroscopy for 118 blue stars with an H{alpha} excess in the galaxy M 33 from the lists of SS 433 and LBV candidates and other rare types of massive stars is presented. The H{alpha} parameters and the relative intensities of the [NII]6584{AA} and [SII]6716{AA} lines are given. We identified stars with a broad H{alpha} emission line, which is probably emitted in the stellar wind.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18#1</TD>
            <TD>2012-10-24T13:16:43Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-April-2000</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/25/18</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/25/18</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/25/18 [2]</TD>
            <TD>Spectroscopy of H{alpha} blue stars in M 33 (Sholukhova+, 1999)</TD>
            <TD>Multiobject spectroscopy for 118 blue stars with an H{alpha} excess in the galaxy M 33 from the lists of SS 433 and LBV candidates and other rare types of massive stars is presented. The H{alpha} parameters and the relative intensities of the [NII]6584{AA} and [SII]6716{AA} lines are given. We identified stars with a broad H{alpha} emission line, which is probably emitted in the stellar wind.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18#2</TD>
            <TD>2012-10-24T13:16:43Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-April-2000</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/25/18&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/25/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/25/18 [object]</TD>
            <TD>Spectroscopy of H{alpha} blue stars in M 33 (Sholukhova+, 1999)</TD>
            <TD>Multiobject spectroscopy for 118 blue stars with an H{alpha} excess in the galaxy M 33 from the lists of SS 433 and LBV candidates and other rare types of massive stars is presented. The H{alpha} parameters and the relative intensities of the [NII]6584{AA} and [SII]6716{AA} lines are given. We identified stars with a broad H{alpha} emission line, which is probably emitted in the stellar wind.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18#object</TD>
            <TD>2012-10-24T13:16:43Z</TD>
            <TD>#Stars#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-April-2000</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/25/18</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/PAZh/25/18&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/25/18</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>BHROSATOpt. [1]</TD>
            <TD>Byurakan/Hamburg/ROSAT Catalog of Optical IDs</TD>
            <TD>This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog &lt;IX/29&gt;) with galactic latitude |b| &gt;= 30 degrees, declination &gt;= 0 degrees, and ROSAT PSPC count rate CR &gt; 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/bhrfscid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/bhrfscid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=bhrfscid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/bhrfscid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>BHROSATOpt. [2]</TD>
            <TD>Byurakan/Hamburg/ROSAT Catalog of Optical IDs</TD>
            <TD>This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog &lt;IX/29&gt;) with galactic latitude |b| &gt;= 30 degrees, declination &gt;= 0 degrees, and ROSAT PSPC count rate CR &gt; 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/bhrfscid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/bhrfscid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=bhrfscid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/bhrfscid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>BHROSATOpt. [3]</TD>
            <TD>Byurakan/Hamburg/ROSAT Catalog of Optical IDs</TD>
            <TD>This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog &lt;IX/29&gt;) with galactic latitude |b| &gt;= 30 degrees, declination &gt;= 0 degrees, and ROSAT PSPC count rate CR &gt; 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/bhrfscid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/bhrfscid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_bhrfscid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/bhrfscid.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>BHROSATOpt. [1]</TD>
            <TD>Byurakan/Hamburg/ROSAT Catalog of Optical IDs</TD>
            <TD>This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog &lt;IX/29&gt;) with galactic latitude |b| &gt;= 30 degrees, declination &gt;= 0 degrees, and ROSAT PSPC count rate CR &gt; 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/bhrfscid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/bhrfscid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=bhrfscid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/bhrfscid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>BHROSATOpt. [2]</TD>
            <TD>Byurakan/Hamburg/ROSAT Catalog of Optical IDs</TD>
            <TD>This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog &lt;IX/29&gt;) with galactic latitude |b| &gt;= 30 degrees, declination &gt;= 0 degrees, and ROSAT PSPC count rate CR &gt; 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/bhrfscid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/bhrfscid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=bhrfscid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/bhrfscid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>BHROSATOpt. [3]</TD>
            <TD>Byurakan/Hamburg/ROSAT Catalog of Optical IDs</TD>
            <TD>This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog &lt;IX/29&gt;) with galactic latitude |b| &gt;= 30 degrees, declination &gt;= 0 degrees, and ROSAT PSPC count rate CR &gt; 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/bhrfscid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/bhrfscid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_bhrfscid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/bhrfscid.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>BHROSATOpt. [1]</TD>
            <TD>Byurakan/Hamburg/ROSAT Catalog of Optical IDs</TD>
            <TD>This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog &lt;IX/29&gt;) with galactic latitude |b| &gt;= 30 degrees, declination &gt;= 0 degrees, and ROSAT PSPC count rate CR &gt; 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/bhrfscid#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/bhrfscid</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=bhrfscid&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/bhrfscid.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>BHROSATOpt. [2]</TD>
            <TD>Byurakan/Hamburg/ROSAT Catalog of Optical IDs</TD>
            <TD>This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog &lt;IX/29&gt;) with galactic latitude |b| &gt;= 30 degrees, declination &gt;= 0 degrees, and ROSAT PSPC count rate CR &gt; 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/bhrfscid#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/bhrfscid</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=bhrfscid&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/bhrfscid.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>BHROSATOpt. [3]</TD>
            <TD>Byurakan/Hamburg/ROSAT Catalog of Optical IDs</TD>
            <TD>This table contains the Byurakan/Hamburg/ROSAT Catalog (BHRC) of the optical identifications of X-ray sources. The BHRC includes all 2791 X-ray sources from the ROSAT Faint Source Catalog (ROSAT-FSC, CDS Catalog &lt;IX/29&gt;) with galactic latitude |b| &gt;= 30 degrees, declination &gt;= 0 degrees, and ROSAT PSPC count rate CR &gt; 0.04 ct/s. The optical identifications were carried out using the Hamburg Quasar Survey (HQS) digitized spectroscopic plates, the DSS1 and DSS2 (blue, red, and IR) images, the MAPS photometric data, the USNO-B1.0 (for proper motion), the NVSS and FIRST radio, and the IRAS and 2MASS infrared catalogs. From the DSS images, positional, brightness, color, extension, variability, and proper-motion information, the optical-to-X-ray positional offsets were obtained and a morphological classification was made. Available SIMBAD and NED data were also utilized. Cross-correlations were made with AGN, white dwarf, and cataclysmic variable catalogs (322, 8 and 7 associations, respectively). The authors managed to identify 97% of the sources (2696/2791 sources) that are associated with 3202 optical objects. 2248 X-ray sources have a single optical counterpart, 144 have a double or multiple optical counterpart (binaries, galaxy groups, etc.), and 304 have ambiguous identifications (some of the latter might actually be blends of two X-ray sources that were not resolved by ROSAT). The QSOs and AGN represent the largest group of X-ray counterparts (56.2%); bright stars (including late-type stars, but excluding WDs and CVs) are counterparts for 33.2% of the sources, and bright galaxies and groups of galaxies comprise 9.2%. A number of close galaxy pairs (possibly interacting/merging galaxies) are found as counterparts for X-ray sources (3.0%), as well as 1.0% WDs and 0.4% CVs. The BHRC may be used for the selection and study of samples of the various classes of X-ray emitters: the table gives all the available multiwavelength data for the identified sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/bhrfscid#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/bhrfscid</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_bhrfscid&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/bhrfscid.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CfARed.S. [1]</TD>
            <TD>CfA Redshift Survey: South Galactic Cap Data</TD>
            <TD>The Center for Astrophysics (CfA) Redshift Survey South Galactic Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies with blue (Zwicky B(0) type) magnitude &lt;= 15.5 covering the range from 20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination. This sample is complete for all galaxies in the merge of the Zwicky et al. and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these were measured as part of the second CfA Redshift Survey. The data reveal large voids in the foreground and background of the Perseus-Pisces Supercluster. The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter of ~ 5000km/s, and is enclosed by a complex of dense structures. The large structure known as the Perseus-Pisces Supercluster forms the near side of this complex. On the far side of this large void, at a mean velocity of ~ 12000km/s, there is another coherent dense wall. The structures in this survey support the view that galaxies generally lie on surfaces surrounding or nearly surrounding low-density regions or voids.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cfa2s#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cfa2s</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cfa2s&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cfa2s.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CfARed.S. [2]</TD>
            <TD>CfA Redshift Survey: South Galactic Cap Data</TD>
            <TD>The Center for Astrophysics (CfA) Redshift Survey South Galactic Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies with blue (Zwicky B(0) type) magnitude &lt;= 15.5 covering the range from 20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination. This sample is complete for all galaxies in the merge of the Zwicky et al. and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these were measured as part of the second CfA Redshift Survey. The data reveal large voids in the foreground and background of the Perseus-Pisces Supercluster. The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter of ~ 5000km/s, and is enclosed by a complex of dense structures. The large structure known as the Perseus-Pisces Supercluster forms the near side of this complex. On the far side of this large void, at a mean velocity of ~ 12000km/s, there is another coherent dense wall. The structures in this survey support the view that galaxies generally lie on surfaces surrounding or nearly surrounding low-density regions or voids.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cfa2s#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cfa2s</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cfa2s&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cfa2s.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CfARed.S. [3]</TD>
            <TD>CfA Redshift Survey: South Galactic Cap Data</TD>
            <TD>The Center for Astrophysics (CfA) Redshift Survey South Galactic Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies with blue (Zwicky B(0) type) magnitude &lt;= 15.5 covering the range from 20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination. This sample is complete for all galaxies in the merge of the Zwicky et al. and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these were measured as part of the second CfA Redshift Survey. The data reveal large voids in the foreground and background of the Perseus-Pisces Supercluster. The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter of ~ 5000km/s, and is enclosed by a complex of dense structures. The large structure known as the Perseus-Pisces Supercluster forms the near side of this complex. On the far side of this large void, at a mean velocity of ~ 12000km/s, there is another coherent dense wall. The structures in this survey support the view that galaxies generally lie on surfaces surrounding or nearly surrounding low-density regions or voids.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cfa2s#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cfa2s</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cfa2s&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cfa2s.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CfARed.S. [1]</TD>
            <TD>CfA Redshift Survey: South Galactic Cap Data</TD>
            <TD>The Center for Astrophysics (CfA) Redshift Survey South Galactic Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies with blue (Zwicky B(0) type) magnitude &lt;= 15.5 covering the range from 20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination. This sample is complete for all galaxies in the merge of the Zwicky et al. and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these were measured as part of the second CfA Redshift Survey. The data reveal large voids in the foreground and background of the Perseus-Pisces Supercluster. The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter of ~ 5000km/s, and is enclosed by a complex of dense structures. The large structure known as the Perseus-Pisces Supercluster forms the near side of this complex. On the far side of this large void, at a mean velocity of ~ 12000km/s, there is another coherent dense wall. The structures in this survey support the view that galaxies generally lie on surfaces surrounding or nearly surrounding low-density regions or voids.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cfa2s#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cfa2s</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cfa2s&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cfa2s.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CfARed.S. [2]</TD>
            <TD>CfA Redshift Survey: South Galactic Cap Data</TD>
            <TD>The Center for Astrophysics (CfA) Redshift Survey South Galactic Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies with blue (Zwicky B(0) type) magnitude &lt;= 15.5 covering the range from 20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination. This sample is complete for all galaxies in the merge of the Zwicky et al. and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these were measured as part of the second CfA Redshift Survey. The data reveal large voids in the foreground and background of the Perseus-Pisces Supercluster. The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter of ~ 5000km/s, and is enclosed by a complex of dense structures. The large structure known as the Perseus-Pisces Supercluster forms the near side of this complex. On the far side of this large void, at a mean velocity of ~ 12000km/s, there is another coherent dense wall. The structures in this survey support the view that galaxies generally lie on surfaces surrounding or nearly surrounding low-density regions or voids.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cfa2s#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cfa2s</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cfa2s&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cfa2s.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CfARed.S. [3]</TD>
            <TD>CfA Redshift Survey: South Galactic Cap Data</TD>
            <TD>The Center for Astrophysics (CfA) Redshift Survey South Galactic Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies with blue (Zwicky B(0) type) magnitude &lt;= 15.5 covering the range from 20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination. This sample is complete for all galaxies in the merge of the Zwicky et al. and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these were measured as part of the second CfA Redshift Survey. The data reveal large voids in the foreground and background of the Perseus-Pisces Supercluster. The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter of ~ 5000km/s, and is enclosed by a complex of dense structures. The large structure known as the Perseus-Pisces Supercluster forms the near side of this complex. On the far side of this large void, at a mean velocity of ~ 12000km/s, there is another coherent dense wall. The structures in this survey support the view that galaxies generally lie on surfaces surrounding or nearly surrounding low-density regions or voids.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cfa2s#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cfa2s</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cfa2s&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cfa2s.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CfARed.S. [1]</TD>
            <TD>CfA Redshift Survey: South Galactic Cap Data</TD>
            <TD>The Center for Astrophysics (CfA) Redshift Survey South Galactic Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies with blue (Zwicky B(0) type) magnitude &lt;= 15.5 covering the range from 20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination. This sample is complete for all galaxies in the merge of the Zwicky et al. and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these were measured as part of the second CfA Redshift Survey. The data reveal large voids in the foreground and background of the Perseus-Pisces Supercluster. The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter of ~ 5000km/s, and is enclosed by a complex of dense structures. The large structure known as the Perseus-Pisces Supercluster forms the near side of this complex. On the far side of this large void, at a mean velocity of ~ 12000km/s, there is another coherent dense wall. The structures in this survey support the view that galaxies generally lie on surfaces surrounding or nearly surrounding low-density regions or voids.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cfa2s#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cfa2s</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cfa2s&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cfa2s.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CfARed.S. [2]</TD>
            <TD>CfA Redshift Survey: South Galactic Cap Data</TD>
            <TD>The Center for Astrophysics (CfA) Redshift Survey South Galactic Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies with blue (Zwicky B(0) type) magnitude &lt;= 15.5 covering the range from 20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination. This sample is complete for all galaxies in the merge of the Zwicky et al. and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these were measured as part of the second CfA Redshift Survey. The data reveal large voids in the foreground and background of the Perseus-Pisces Supercluster. The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter of ~ 5000km/s, and is enclosed by a complex of dense structures. The large structure known as the Perseus-Pisces Supercluster forms the near side of this complex. On the far side of this large void, at a mean velocity of ~ 12000km/s, there is another coherent dense wall. The structures in this survey support the view that galaxies generally lie on surfaces surrounding or nearly surrounding low-density regions or voids.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cfa2s#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cfa2s</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cfa2s&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cfa2s.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CfARed.S. [3]</TD>
            <TD>CfA Redshift Survey: South Galactic Cap Data</TD>
            <TD>The Center for Astrophysics (CfA) Redshift Survey South Galactic Cap (CFA2S) Catalog contains redshifts for a sample of about 4300 galaxies with blue (Zwicky B(0) type) magnitude &lt;= 15.5 covering the range from 20 h to 4h in right ascension and from -2.5 deg to 90 deg in declination. This sample is complete for all galaxies in the merge of the Zwicky et al. and Nilson catalogs in the south Galactic cap. Redshifts for 2964 of these were measured as part of the second CfA Redshift Survey. The data reveal large voids in the foreground and background of the Perseus-Pisces Supercluster. The largest of these voids lies at a mean velocity ~ 8000km/s, has diameter of ~ 5000km/s, and is enclosed by a complex of dense structures. The large structure known as the Perseus-Pisces Supercluster forms the near side of this complex. On the far side of this large void, at a mean velocity of ~ 12000km/s, there is another coherent dense wall. The structures in this survey support the view that galaxies generally lie on surfaces surrounding or nearly surrounding low-density regions or voids.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cfa2s#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cfa2s</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cfa2s&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cfa2s.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CG [1]</TD>
            <TD>Candidate Galaxies Behind the Milky Way</TD>
            <TD>This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cgmw#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cgmw</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cgmw&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cgmw.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CG [2]</TD>
            <TD>Candidate Galaxies Behind the Milky Way</TD>
            <TD>This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cgmw#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cgmw</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cgmw&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cgmw.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CG [3]</TD>
            <TD>Candidate Galaxies Behind the Milky Way</TD>
            <TD>This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cgmw#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cgmw</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cgmw&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cgmw.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CG [1]</TD>
            <TD>Candidate Galaxies Behind the Milky Way</TD>
            <TD>This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cgmw#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cgmw</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cgmw&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cgmw.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CG [2]</TD>
            <TD>Candidate Galaxies Behind the Milky Way</TD>
            <TD>This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cgmw#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cgmw</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cgmw&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cgmw.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CG [3]</TD>
            <TD>Candidate Galaxies Behind the Milky Way</TD>
            <TD>This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cgmw#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cgmw</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cgmw&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cgmw.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CG [1]</TD>
            <TD>Candidate Galaxies Behind the Milky Way</TD>
            <TD>This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cgmw#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cgmw</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cgmw&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cgmw.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CG [2]</TD>
            <TD>Candidate Galaxies Behind the Milky Way</TD>
            <TD>This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cgmw#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cgmw</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cgmw&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cgmw.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CG [3]</TD>
            <TD>Candidate Galaxies Behind the Milky Way</TD>
            <TD>This catalog gathers the searches for galaxies of apparent size greater than 0.1 mm on film (6.7" in angular size) lieing behind the Milky Way from photographic surveys in the near-infrared. The four volumes (CGMW1, CGMW2, CGMW3, and CGMW4) cover the galactic longitude ranges from -7 to +43 degrees, and from 210 to 250 degrees. The two volumes, CGMW1 and CGMW2, giving about 7000 galaxies behind the Milky Way between l = 210 degrees and 250 degrees, represent a systematic search for galaxies by means of 32 film copies of the UK Schmidt Southern Infrared Atlas on the Milky Way covering about 900 square degrees. In the search galaxies with apparent sizes greater than 0.1mm on film (6.7 arcsec in size) were detected by visual inspection. The material and procedure of search are described as well as the detectability of galaxies in paper I and paper II appended before Vol. 1 and Vol. 2 of the catalog, respectively, which have been published in Publ. Astron. Soc Japan, Vol. 42 (1990) and Vol. 43 (1991). The parameters of catalogued galaxies are also explained in paper I. Cross-identifications with other catalogs are also given. The third volume CGMW3 lists about 5300 galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 800 square degrees around l = 8 to 43 degrees, and b = -17 to +17 degrees. This surveyed region is located between the northern Local void and the Ophiuchus void. The fourth volume CGMW4 lists about 7150 galaxies and galaxy candidates having sizes larger than 0.1 arcminutes that were found in a search of Schmidt atlases covering a Milky Way region of about 260 square degrees around l = -7 to +16 degrees, and b = -19 to -1 degrees, i.e., a field in Sagittarius in the Galactic Center region.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/cgmw#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cgmw</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cgmw&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/cgmw.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHANULXCAT [1]</TD>
            <TD>Chandra Archive Of Galaxies Ultraluminous X-Ray Source Catalog</TD>
            <TD>One hundred fifty-five (the abstract in the paper erroneously states the number to be 154) discrete, non-nuclear, ultraluminous X-ray (ULX) sources, with spectroscopically determined intrinsic X-ray luminosities greater than 10^39 erg/s, have been identified in 82 galaxies that were observed with Chandra's Advanced CCD Imaging Spectrometer (ACIS). Positions, X-ray luminosities, and spectral and timing characteristics of these ULXs are contained in this table. Eighty-three percent of ULX candidates have spectra that can be described as absorbed power laws with mean index Gamma = 1.74 and column density N_H = 2.24 x 10^21 atoms cm^-2, or ~5 times the average Galactic column. About 20% of the ULXs have much steeper indices indicative of a soft, and likely thermal, spectrum. The locations of ULXs in their host galaxies are strongly peaked toward their galaxy centers. The deprojected radial distribution of the ULX candidates is somewhat steeper than an exponential disk, indistinguishable from that of the weaker sources. About 5%-15% of ULX candidates are variable during the Chandra observations (which average 39.5 ks). Comparison of the cumulative X-ray luminosity functions of the ULXs to Chandra Deep Field results suggests ~25% of the sources may be background objects, including 14% of the ULX candidates in the sample of spiral galaxies and 44% of those in elliptical galaxies, implying the elliptical galaxy ULX population is severely compromised by background active galactic nuclei. Correlations with host galaxy properties confirm the number and total X-ray luminosity of the ULXs are associated with recent star formation and with galaxy merging and interactions. The preponderance of ULXs in star-forming galaxies as well as their similarities to less-luminous sources suggest they originate in a young but short-lived population such as the high-mass X-ray binaries, with a smaller contribution (based on spectral slope) from recent supernovae. The number of ULXs in elliptical galaxies scales with host galaxy mass and can be explained most simply as the high-luminosity end of the low-mass X-ray binary population.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanulxcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanulxcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chanulxcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanulxcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHANULXCAT [2]</TD>
            <TD>Chandra Archive Of Galaxies Ultraluminous X-Ray Source Catalog</TD>
            <TD>One hundred fifty-five (the abstract in the paper erroneously states the number to be 154) discrete, non-nuclear, ultraluminous X-ray (ULX) sources, with spectroscopically determined intrinsic X-ray luminosities greater than 10^39 erg/s, have been identified in 82 galaxies that were observed with Chandra's Advanced CCD Imaging Spectrometer (ACIS). Positions, X-ray luminosities, and spectral and timing characteristics of these ULXs are contained in this table. Eighty-three percent of ULX candidates have spectra that can be described as absorbed power laws with mean index Gamma = 1.74 and column density N_H = 2.24 x 10^21 atoms cm^-2, or ~5 times the average Galactic column. About 20% of the ULXs have much steeper indices indicative of a soft, and likely thermal, spectrum. The locations of ULXs in their host galaxies are strongly peaked toward their galaxy centers. The deprojected radial distribution of the ULX candidates is somewhat steeper than an exponential disk, indistinguishable from that of the weaker sources. About 5%-15% of ULX candidates are variable during the Chandra observations (which average 39.5 ks). Comparison of the cumulative X-ray luminosity functions of the ULXs to Chandra Deep Field results suggests ~25% of the sources may be background objects, including 14% of the ULX candidates in the sample of spiral galaxies and 44% of those in elliptical galaxies, implying the elliptical galaxy ULX population is severely compromised by background active galactic nuclei. Correlations with host galaxy properties confirm the number and total X-ray luminosity of the ULXs are associated with recent star formation and with galaxy merging and interactions. The preponderance of ULXs in star-forming galaxies as well as their similarities to less-luminous sources suggest they originate in a young but short-lived population such as the high-mass X-ray binaries, with a smaller contribution (based on spectral slope) from recent supernovae. The number of ULXs in elliptical galaxies scales with host galaxy mass and can be explained most simply as the high-luminosity end of the low-mass X-ray binary population.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanulxcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanulxcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chanulxcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanulxcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHANULXCAT [3]</TD>
            <TD>Chandra Archive Of Galaxies Ultraluminous X-Ray Source Catalog</TD>
            <TD>One hundred fifty-five (the abstract in the paper erroneously states the number to be 154) discrete, non-nuclear, ultraluminous X-ray (ULX) sources, with spectroscopically determined intrinsic X-ray luminosities greater than 10^39 erg/s, have been identified in 82 galaxies that were observed with Chandra's Advanced CCD Imaging Spectrometer (ACIS). Positions, X-ray luminosities, and spectral and timing characteristics of these ULXs are contained in this table. Eighty-three percent of ULX candidates have spectra that can be described as absorbed power laws with mean index Gamma = 1.74 and column density N_H = 2.24 x 10^21 atoms cm^-2, or ~5 times the average Galactic column. About 20% of the ULXs have much steeper indices indicative of a soft, and likely thermal, spectrum. The locations of ULXs in their host galaxies are strongly peaked toward their galaxy centers. The deprojected radial distribution of the ULX candidates is somewhat steeper than an exponential disk, indistinguishable from that of the weaker sources. About 5%-15% of ULX candidates are variable during the Chandra observations (which average 39.5 ks). Comparison of the cumulative X-ray luminosity functions of the ULXs to Chandra Deep Field results suggests ~25% of the sources may be background objects, including 14% of the ULX candidates in the sample of spiral galaxies and 44% of those in elliptical galaxies, implying the elliptical galaxy ULX population is severely compromised by background active galactic nuclei. Correlations with host galaxy properties confirm the number and total X-ray luminosity of the ULXs are associated with recent star formation and with galaxy merging and interactions. The preponderance of ULXs in star-forming galaxies as well as their similarities to less-luminous sources suggest they originate in a young but short-lived population such as the high-mass X-ray binaries, with a smaller contribution (based on spectral slope) from recent supernovae. The number of ULXs in elliptical galaxies scales with host galaxy mass and can be explained most simply as the high-luminosity end of the low-mass X-ray binary population.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanulxcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanulxcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chanulxcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanulxcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHANULXCAT [1]</TD>
            <TD>Chandra Archive Of Galaxies Ultraluminous X-Ray Source Catalog</TD>
            <TD>One hundred fifty-five (the abstract in the paper erroneously states the number to be 154) discrete, non-nuclear, ultraluminous X-ray (ULX) sources, with spectroscopically determined intrinsic X-ray luminosities greater than 10^39 erg/s, have been identified in 82 galaxies that were observed with Chandra's Advanced CCD Imaging Spectrometer (ACIS). Positions, X-ray luminosities, and spectral and timing characteristics of these ULXs are contained in this table. Eighty-three percent of ULX candidates have spectra that can be described as absorbed power laws with mean index Gamma = 1.74 and column density N_H = 2.24 x 10^21 atoms cm^-2, or ~5 times the average Galactic column. About 20% of the ULXs have much steeper indices indicative of a soft, and likely thermal, spectrum. The locations of ULXs in their host galaxies are strongly peaked toward their galaxy centers. The deprojected radial distribution of the ULX candidates is somewhat steeper than an exponential disk, indistinguishable from that of the weaker sources. About 5%-15% of ULX candidates are variable during the Chandra observations (which average 39.5 ks). Comparison of the cumulative X-ray luminosity functions of the ULXs to Chandra Deep Field results suggests ~25% of the sources may be background objects, including 14% of the ULX candidates in the sample of spiral galaxies and 44% of those in elliptical galaxies, implying the elliptical galaxy ULX population is severely compromised by background active galactic nuclei. Correlations with host galaxy properties confirm the number and total X-ray luminosity of the ULXs are associated with recent star formation and with galaxy merging and interactions. The preponderance of ULXs in star-forming galaxies as well as their similarities to less-luminous sources suggest they originate in a young but short-lived population such as the high-mass X-ray binaries, with a smaller contribution (based on spectral slope) from recent supernovae. The number of ULXs in elliptical galaxies scales with host galaxy mass and can be explained most simply as the high-luminosity end of the low-mass X-ray binary population.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanulxcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanulxcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chanulxcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanulxcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHANULXCAT [2]</TD>
            <TD>Chandra Archive Of Galaxies Ultraluminous X-Ray Source Catalog</TD>
            <TD>One hundred fifty-five (the abstract in the paper erroneously states the number to be 154) discrete, non-nuclear, ultraluminous X-ray (ULX) sources, with spectroscopically determined intrinsic X-ray luminosities greater than 10^39 erg/s, have been identified in 82 galaxies that were observed with Chandra's Advanced CCD Imaging Spectrometer (ACIS). Positions, X-ray luminosities, and spectral and timing characteristics of these ULXs are contained in this table. Eighty-three percent of ULX candidates have spectra that can be described as absorbed power laws with mean index Gamma = 1.74 and column density N_H = 2.24 x 10^21 atoms cm^-2, or ~5 times the average Galactic column. About 20% of the ULXs have much steeper indices indicative of a soft, and likely thermal, spectrum. The locations of ULXs in their host galaxies are strongly peaked toward their galaxy centers. The deprojected radial distribution of the ULX candidates is somewhat steeper than an exponential disk, indistinguishable from that of the weaker sources. About 5%-15% of ULX candidates are variable during the Chandra observations (which average 39.5 ks). Comparison of the cumulative X-ray luminosity functions of the ULXs to Chandra Deep Field results suggests ~25% of the sources may be background objects, including 14% of the ULX candidates in the sample of spiral galaxies and 44% of those in elliptical galaxies, implying the elliptical galaxy ULX population is severely compromised by background active galactic nuclei. Correlations with host galaxy properties confirm the number and total X-ray luminosity of the ULXs are associated with recent star formation and with galaxy merging and interactions. The preponderance of ULXs in star-forming galaxies as well as their similarities to less-luminous sources suggest they originate in a young but short-lived population such as the high-mass X-ray binaries, with a smaller contribution (based on spectral slope) from recent supernovae. The number of ULXs in elliptical galaxies scales with host galaxy mass and can be explained most simply as the high-luminosity end of the low-mass X-ray binary population.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanulxcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanulxcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chanulxcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanulxcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHANULXCAT [3]</TD>
            <TD>Chandra Archive Of Galaxies Ultraluminous X-Ray Source Catalog</TD>
            <TD>One hundred fifty-five (the abstract in the paper erroneously states the number to be 154) discrete, non-nuclear, ultraluminous X-ray (ULX) sources, with spectroscopically determined intrinsic X-ray luminosities greater than 10^39 erg/s, have been identified in 82 galaxies that were observed with Chandra's Advanced CCD Imaging Spectrometer (ACIS). Positions, X-ray luminosities, and spectral and timing characteristics of these ULXs are contained in this table. Eighty-three percent of ULX candidates have spectra that can be described as absorbed power laws with mean index Gamma = 1.74 and column density N_H = 2.24 x 10^21 atoms cm^-2, or ~5 times the average Galactic column. About 20% of the ULXs have much steeper indices indicative of a soft, and likely thermal, spectrum. The locations of ULXs in their host galaxies are strongly peaked toward their galaxy centers. The deprojected radial distribution of the ULX candidates is somewhat steeper than an exponential disk, indistinguishable from that of the weaker sources. About 5%-15% of ULX candidates are variable during the Chandra observations (which average 39.5 ks). Comparison of the cumulative X-ray luminosity functions of the ULXs to Chandra Deep Field results suggests ~25% of the sources may be background objects, including 14% of the ULX candidates in the sample of spiral galaxies and 44% of those in elliptical galaxies, implying the elliptical galaxy ULX population is severely compromised by background active galactic nuclei. Correlations with host galaxy properties confirm the number and total X-ray luminosity of the ULXs are associated with recent star formation and with galaxy merging and interactions. The preponderance of ULXs in star-forming galaxies as well as their similarities to less-luminous sources suggest they originate in a young but short-lived population such as the high-mass X-ray binaries, with a smaller contribution (based on spectral slope) from recent supernovae. The number of ULXs in elliptical galaxies scales with host galaxy mass and can be explained most simply as the high-luminosity end of the low-mass X-ray binary population.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanulxcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanulxcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chanulxcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanulxcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHANULXCAT [1]</TD>
            <TD>Chandra Archive Of Galaxies Ultraluminous X-Ray Source Catalog</TD>
            <TD>One hundred fifty-five (the abstract in the paper erroneously states the number to be 154) discrete, non-nuclear, ultraluminous X-ray (ULX) sources, with spectroscopically determined intrinsic X-ray luminosities greater than 10^39 erg/s, have been identified in 82 galaxies that were observed with Chandra's Advanced CCD Imaging Spectrometer (ACIS). Positions, X-ray luminosities, and spectral and timing characteristics of these ULXs are contained in this table. Eighty-three percent of ULX candidates have spectra that can be described as absorbed power laws with mean index Gamma = 1.74 and column density N_H = 2.24 x 10^21 atoms cm^-2, or ~5 times the average Galactic column. About 20% of the ULXs have much steeper indices indicative of a soft, and likely thermal, spectrum. The locations of ULXs in their host galaxies are strongly peaked toward their galaxy centers. The deprojected radial distribution of the ULX candidates is somewhat steeper than an exponential disk, indistinguishable from that of the weaker sources. About 5%-15% of ULX candidates are variable during the Chandra observations (which average 39.5 ks). Comparison of the cumulative X-ray luminosity functions of the ULXs to Chandra Deep Field results suggests ~25% of the sources may be background objects, including 14% of the ULX candidates in the sample of spiral galaxies and 44% of those in elliptical galaxies, implying the elliptical galaxy ULX population is severely compromised by background active galactic nuclei. Correlations with host galaxy properties confirm the number and total X-ray luminosity of the ULXs are associated with recent star formation and with galaxy merging and interactions. The preponderance of ULXs in star-forming galaxies as well as their similarities to less-luminous sources suggest they originate in a young but short-lived population such as the high-mass X-ray binaries, with a smaller contribution (based on spectral slope) from recent supernovae. The number of ULXs in elliptical galaxies scales with host galaxy mass and can be explained most simply as the high-luminosity end of the low-mass X-ray binary population.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanulxcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanulxcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=chanulxcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanulxcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHANULXCAT [2]</TD>
            <TD>Chandra Archive Of Galaxies Ultraluminous X-Ray Source Catalog</TD>
            <TD>One hundred fifty-five (the abstract in the paper erroneously states the number to be 154) discrete, non-nuclear, ultraluminous X-ray (ULX) sources, with spectroscopically determined intrinsic X-ray luminosities greater than 10^39 erg/s, have been identified in 82 galaxies that were observed with Chandra's Advanced CCD Imaging Spectrometer (ACIS). Positions, X-ray luminosities, and spectral and timing characteristics of these ULXs are contained in this table. Eighty-three percent of ULX candidates have spectra that can be described as absorbed power laws with mean index Gamma = 1.74 and column density N_H = 2.24 x 10^21 atoms cm^-2, or ~5 times the average Galactic column. About 20% of the ULXs have much steeper indices indicative of a soft, and likely thermal, spectrum. The locations of ULXs in their host galaxies are strongly peaked toward their galaxy centers. The deprojected radial distribution of the ULX candidates is somewhat steeper than an exponential disk, indistinguishable from that of the weaker sources. About 5%-15% of ULX candidates are variable during the Chandra observations (which average 39.5 ks). Comparison of the cumulative X-ray luminosity functions of the ULXs to Chandra Deep Field results suggests ~25% of the sources may be background objects, including 14% of the ULX candidates in the sample of spiral galaxies and 44% of those in elliptical galaxies, implying the elliptical galaxy ULX population is severely compromised by background active galactic nuclei. Correlations with host galaxy properties confirm the number and total X-ray luminosity of the ULXs are associated with recent star formation and with galaxy merging and interactions. The preponderance of ULXs in star-forming galaxies as well as their similarities to less-luminous sources suggest they originate in a young but short-lived population such as the high-mass X-ray binaries, with a smaller contribution (based on spectral slope) from recent supernovae. The number of ULXs in elliptical galaxies scales with host galaxy mass and can be explained most simply as the high-luminosity end of the low-mass X-ray binary population.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanulxcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanulxcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=chanulxcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanulxcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHANULXCAT [3]</TD>
            <TD>Chandra Archive Of Galaxies Ultraluminous X-Ray Source Catalog</TD>
            <TD>One hundred fifty-five (the abstract in the paper erroneously states the number to be 154) discrete, non-nuclear, ultraluminous X-ray (ULX) sources, with spectroscopically determined intrinsic X-ray luminosities greater than 10^39 erg/s, have been identified in 82 galaxies that were observed with Chandra's Advanced CCD Imaging Spectrometer (ACIS). Positions, X-ray luminosities, and spectral and timing characteristics of these ULXs are contained in this table. Eighty-three percent of ULX candidates have spectra that can be described as absorbed power laws with mean index Gamma = 1.74 and column density N_H = 2.24 x 10^21 atoms cm^-2, or ~5 times the average Galactic column. About 20% of the ULXs have much steeper indices indicative of a soft, and likely thermal, spectrum. The locations of ULXs in their host galaxies are strongly peaked toward their galaxy centers. The deprojected radial distribution of the ULX candidates is somewhat steeper than an exponential disk, indistinguishable from that of the weaker sources. About 5%-15% of ULX candidates are variable during the Chandra observations (which average 39.5 ks). Comparison of the cumulative X-ray luminosity functions of the ULXs to Chandra Deep Field results suggests ~25% of the sources may be background objects, including 14% of the ULX candidates in the sample of spiral galaxies and 44% of those in elliptical galaxies, implying the elliptical galaxy ULX population is severely compromised by background active galactic nuclei. Correlations with host galaxy properties confirm the number and total X-ray luminosity of the ULXs are associated with recent star formation and with galaxy merging and interactions. The preponderance of ULXs in star-forming galaxies as well as their similarities to less-luminous sources suggest they originate in a young but short-lived population such as the high-mass X-ray binaries, with a smaller contribution (based on spectral slope) from recent supernovae. The number of ULXs in elliptical galaxies scales with host galaxy mass and can be explained most simply as the high-luminosity end of the low-mass X-ray binary population.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/chanulxcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/chanulxcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_chanulxcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/chanulxcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>EGRET [1]</TD>
            <TD>CGRO/EGRET Third Source Catalog</TD>
            <TD>The Third EGRET Catalog of High-Energy Gamma-Ray Sources is based on data obtained by the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO) during the period from 1991 April 22 to 1995 October 3, corresponding to GRO Cycles 1, 2, 3, and 4. EGRET is sensitive to photons in the energy range from about 30 MeV to over 20 GeV, the highest energies accessible by the CGRO instruments, and, like COMPTEL, is an imaging instrument. In addition to including more data than the Second EGRET Catalog (2EG, Thompson et al. 1995, ApJS, 101, 259) and its supplement (2EGS, Thompson et al. 1996, ApJS, 107, 227), this catalog uses completely reprocessed data so as to correct a number of mostly minimal errors and problems. The 271 sources (E &gt; 100 MeV) in the catalog include the single 1991 solar flare that was bright enough to detected as a source, the LMC, 5 pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower-confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources that are not yet firmly identified with known objects, although potential identifications have been suggested for a number of these. As already noted, there are 271 distinct sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 5246 entries in the HEASARC's version of the 3rd EGRET Catalog corresponding to the same number of lines in Table 4 of the published version. Thus, there are an average of about 20 entries for every distinct source. Notice that 14 sources reported in the 2nd EGRET Catalog or its supplement do not appear in this 3rd EGRET Catalog: 2EG J0403+3357, 2EG J0426+6618, 2EGS J0500+5902, 2EGS J0552-1026, 2EG J1136-0414, 2EGS J1236-0416, 2EG J1239+0441, 2EG J1314+5151, 2EG J1430+5356, 2EG J1443-6040, 2EG J1631-2845, 2EG J1709-0350, 2EG J1815+2950, and 2EG J2027+1054 due to the fact that the re-analysis of the EGRET data has dropped their statistical significance from just above the catalog threshold to just below it; additional information on these sources is provided in Table 5 of the published version of the 3rd EGRET Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egret3#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egret3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=egret3&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egret3.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>EGRET [2]</TD>
            <TD>CGRO/EGRET Third Source Catalog</TD>
            <TD>The Third EGRET Catalog of High-Energy Gamma-Ray Sources is based on data obtained by the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO) during the period from 1991 April 22 to 1995 October 3, corresponding to GRO Cycles 1, 2, 3, and 4. EGRET is sensitive to photons in the energy range from about 30 MeV to over 20 GeV, the highest energies accessible by the CGRO instruments, and, like COMPTEL, is an imaging instrument. In addition to including more data than the Second EGRET Catalog (2EG, Thompson et al. 1995, ApJS, 101, 259) and its supplement (2EGS, Thompson et al. 1996, ApJS, 107, 227), this catalog uses completely reprocessed data so as to correct a number of mostly minimal errors and problems. The 271 sources (E &gt; 100 MeV) in the catalog include the single 1991 solar flare that was bright enough to detected as a source, the LMC, 5 pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower-confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources that are not yet firmly identified with known objects, although potential identifications have been suggested for a number of these. As already noted, there are 271 distinct sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 5246 entries in the HEASARC's version of the 3rd EGRET Catalog corresponding to the same number of lines in Table 4 of the published version. Thus, there are an average of about 20 entries for every distinct source. Notice that 14 sources reported in the 2nd EGRET Catalog or its supplement do not appear in this 3rd EGRET Catalog: 2EG J0403+3357, 2EG J0426+6618, 2EGS J0500+5902, 2EGS J0552-1026, 2EG J1136-0414, 2EGS J1236-0416, 2EG J1239+0441, 2EG J1314+5151, 2EG J1430+5356, 2EG J1443-6040, 2EG J1631-2845, 2EG J1709-0350, 2EG J1815+2950, and 2EG J2027+1054 due to the fact that the re-analysis of the EGRET data has dropped their statistical significance from just above the catalog threshold to just below it; additional information on these sources is provided in Table 5 of the published version of the 3rd EGRET Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egret3#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egret3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=egret3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egret3.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>EGRET [3]</TD>
            <TD>CGRO/EGRET Third Source Catalog</TD>
            <TD>The Third EGRET Catalog of High-Energy Gamma-Ray Sources is based on data obtained by the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO) during the period from 1991 April 22 to 1995 October 3, corresponding to GRO Cycles 1, 2, 3, and 4. EGRET is sensitive to photons in the energy range from about 30 MeV to over 20 GeV, the highest energies accessible by the CGRO instruments, and, like COMPTEL, is an imaging instrument. In addition to including more data than the Second EGRET Catalog (2EG, Thompson et al. 1995, ApJS, 101, 259) and its supplement (2EGS, Thompson et al. 1996, ApJS, 107, 227), this catalog uses completely reprocessed data so as to correct a number of mostly minimal errors and problems. The 271 sources (E &gt; 100 MeV) in the catalog include the single 1991 solar flare that was bright enough to detected as a source, the LMC, 5 pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower-confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources that are not yet firmly identified with known objects, although potential identifications have been suggested for a number of these. As already noted, there are 271 distinct sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 5246 entries in the HEASARC's version of the 3rd EGRET Catalog corresponding to the same number of lines in Table 4 of the published version. Thus, there are an average of about 20 entries for every distinct source. Notice that 14 sources reported in the 2nd EGRET Catalog or its supplement do not appear in this 3rd EGRET Catalog: 2EG J0403+3357, 2EG J0426+6618, 2EGS J0500+5902, 2EGS J0552-1026, 2EG J1136-0414, 2EGS J1236-0416, 2EG J1239+0441, 2EG J1314+5151, 2EG J1430+5356, 2EG J1443-6040, 2EG J1631-2845, 2EG J1709-0350, 2EG J1815+2950, and 2EG J2027+1054 due to the fact that the re-analysis of the EGRET data has dropped their statistical significance from just above the catalog threshold to just below it; additional information on these sources is provided in Table 5 of the published version of the 3rd EGRET Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egret3#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egret3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_egret3&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egret3.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>EGRET [1]</TD>
            <TD>CGRO/EGRET Third Source Catalog</TD>
            <TD>The Third EGRET Catalog of High-Energy Gamma-Ray Sources is based on data obtained by the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO) during the period from 1991 April 22 to 1995 October 3, corresponding to GRO Cycles 1, 2, 3, and 4. EGRET is sensitive to photons in the energy range from about 30 MeV to over 20 GeV, the highest energies accessible by the CGRO instruments, and, like COMPTEL, is an imaging instrument. In addition to including more data than the Second EGRET Catalog (2EG, Thompson et al. 1995, ApJS, 101, 259) and its supplement (2EGS, Thompson et al. 1996, ApJS, 107, 227), this catalog uses completely reprocessed data so as to correct a number of mostly minimal errors and problems. The 271 sources (E &gt; 100 MeV) in the catalog include the single 1991 solar flare that was bright enough to detected as a source, the LMC, 5 pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower-confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources that are not yet firmly identified with known objects, although potential identifications have been suggested for a number of these. As already noted, there are 271 distinct sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 5246 entries in the HEASARC's version of the 3rd EGRET Catalog corresponding to the same number of lines in Table 4 of the published version. Thus, there are an average of about 20 entries for every distinct source. Notice that 14 sources reported in the 2nd EGRET Catalog or its supplement do not appear in this 3rd EGRET Catalog: 2EG J0403+3357, 2EG J0426+6618, 2EGS J0500+5902, 2EGS J0552-1026, 2EG J1136-0414, 2EGS J1236-0416, 2EG J1239+0441, 2EG J1314+5151, 2EG J1430+5356, 2EG J1443-6040, 2EG J1631-2845, 2EG J1709-0350, 2EG J1815+2950, and 2EG J2027+1054 due to the fact that the re-analysis of the EGRET data has dropped their statistical significance from just above the catalog threshold to just below it; additional information on these sources is provided in Table 5 of the published version of the 3rd EGRET Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egret3#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egret3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=egret3&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egret3.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>EGRET [2]</TD>
            <TD>CGRO/EGRET Third Source Catalog</TD>
            <TD>The Third EGRET Catalog of High-Energy Gamma-Ray Sources is based on data obtained by the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO) during the period from 1991 April 22 to 1995 October 3, corresponding to GRO Cycles 1, 2, 3, and 4. EGRET is sensitive to photons in the energy range from about 30 MeV to over 20 GeV, the highest energies accessible by the CGRO instruments, and, like COMPTEL, is an imaging instrument. In addition to including more data than the Second EGRET Catalog (2EG, Thompson et al. 1995, ApJS, 101, 259) and its supplement (2EGS, Thompson et al. 1996, ApJS, 107, 227), this catalog uses completely reprocessed data so as to correct a number of mostly minimal errors and problems. The 271 sources (E &gt; 100 MeV) in the catalog include the single 1991 solar flare that was bright enough to detected as a source, the LMC, 5 pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower-confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources that are not yet firmly identified with known objects, although potential identifications have been suggested for a number of these. As already noted, there are 271 distinct sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 5246 entries in the HEASARC's version of the 3rd EGRET Catalog corresponding to the same number of lines in Table 4 of the published version. Thus, there are an average of about 20 entries for every distinct source. Notice that 14 sources reported in the 2nd EGRET Catalog or its supplement do not appear in this 3rd EGRET Catalog: 2EG J0403+3357, 2EG J0426+6618, 2EGS J0500+5902, 2EGS J0552-1026, 2EG J1136-0414, 2EGS J1236-0416, 2EG J1239+0441, 2EG J1314+5151, 2EG J1430+5356, 2EG J1443-6040, 2EG J1631-2845, 2EG J1709-0350, 2EG J1815+2950, and 2EG J2027+1054 due to the fact that the re-analysis of the EGRET data has dropped their statistical significance from just above the catalog threshold to just below it; additional information on these sources is provided in Table 5 of the published version of the 3rd EGRET Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egret3#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egret3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=egret3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egret3.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>EGRET [3]</TD>
            <TD>CGRO/EGRET Third Source Catalog</TD>
            <TD>The Third EGRET Catalog of High-Energy Gamma-Ray Sources is based on data obtained by the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO) during the period from 1991 April 22 to 1995 October 3, corresponding to GRO Cycles 1, 2, 3, and 4. EGRET is sensitive to photons in the energy range from about 30 MeV to over 20 GeV, the highest energies accessible by the CGRO instruments, and, like COMPTEL, is an imaging instrument. In addition to including more data than the Second EGRET Catalog (2EG, Thompson et al. 1995, ApJS, 101, 259) and its supplement (2EGS, Thompson et al. 1996, ApJS, 107, 227), this catalog uses completely reprocessed data so as to correct a number of mostly minimal errors and problems. The 271 sources (E &gt; 100 MeV) in the catalog include the single 1991 solar flare that was bright enough to detected as a source, the LMC, 5 pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower-confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources that are not yet firmly identified with known objects, although potential identifications have been suggested for a number of these. As already noted, there are 271 distinct sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 5246 entries in the HEASARC's version of the 3rd EGRET Catalog corresponding to the same number of lines in Table 4 of the published version. Thus, there are an average of about 20 entries for every distinct source. Notice that 14 sources reported in the 2nd EGRET Catalog or its supplement do not appear in this 3rd EGRET Catalog: 2EG J0403+3357, 2EG J0426+6618, 2EGS J0500+5902, 2EGS J0552-1026, 2EG J1136-0414, 2EGS J1236-0416, 2EG J1239+0441, 2EG J1314+5151, 2EG J1430+5356, 2EG J1443-6040, 2EG J1631-2845, 2EG J1709-0350, 2EG J1815+2950, and 2EG J2027+1054 due to the fact that the re-analysis of the EGRET data has dropped their statistical significance from just above the catalog threshold to just below it; additional information on these sources is provided in Table 5 of the published version of the 3rd EGRET Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egret3#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egret3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_egret3&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egret3.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>EGRET [1]</TD>
            <TD>CGRO/EGRET Third Source Catalog</TD>
            <TD>The Third EGRET Catalog of High-Energy Gamma-Ray Sources is based on data obtained by the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO) during the period from 1991 April 22 to 1995 October 3, corresponding to GRO Cycles 1, 2, 3, and 4. EGRET is sensitive to photons in the energy range from about 30 MeV to over 20 GeV, the highest energies accessible by the CGRO instruments, and, like COMPTEL, is an imaging instrument. In addition to including more data than the Second EGRET Catalog (2EG, Thompson et al. 1995, ApJS, 101, 259) and its supplement (2EGS, Thompson et al. 1996, ApJS, 107, 227), this catalog uses completely reprocessed data so as to correct a number of mostly minimal errors and problems. The 271 sources (E &gt; 100 MeV) in the catalog include the single 1991 solar flare that was bright enough to detected as a source, the LMC, 5 pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower-confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources that are not yet firmly identified with known objects, although potential identifications have been suggested for a number of these. As already noted, there are 271 distinct sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 5246 entries in the HEASARC's version of the 3rd EGRET Catalog corresponding to the same number of lines in Table 4 of the published version. Thus, there are an average of about 20 entries for every distinct source. Notice that 14 sources reported in the 2nd EGRET Catalog or its supplement do not appear in this 3rd EGRET Catalog: 2EG J0403+3357, 2EG J0426+6618, 2EGS J0500+5902, 2EGS J0552-1026, 2EG J1136-0414, 2EGS J1236-0416, 2EG J1239+0441, 2EG J1314+5151, 2EG J1430+5356, 2EG J1443-6040, 2EG J1631-2845, 2EG J1709-0350, 2EG J1815+2950, and 2EG J2027+1054 due to the fact that the re-analysis of the EGRET data has dropped their statistical significance from just above the catalog threshold to just below it; additional information on these sources is provided in Table 5 of the published version of the 3rd EGRET Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egret3#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egret3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=egret3&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egret3.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>EGRET [2]</TD>
            <TD>CGRO/EGRET Third Source Catalog</TD>
            <TD>The Third EGRET Catalog of High-Energy Gamma-Ray Sources is based on data obtained by the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO) during the period from 1991 April 22 to 1995 October 3, corresponding to GRO Cycles 1, 2, 3, and 4. EGRET is sensitive to photons in the energy range from about 30 MeV to over 20 GeV, the highest energies accessible by the CGRO instruments, and, like COMPTEL, is an imaging instrument. In addition to including more data than the Second EGRET Catalog (2EG, Thompson et al. 1995, ApJS, 101, 259) and its supplement (2EGS, Thompson et al. 1996, ApJS, 107, 227), this catalog uses completely reprocessed data so as to correct a number of mostly minimal errors and problems. The 271 sources (E &gt; 100 MeV) in the catalog include the single 1991 solar flare that was bright enough to detected as a source, the LMC, 5 pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower-confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources that are not yet firmly identified with known objects, although potential identifications have been suggested for a number of these. As already noted, there are 271 distinct sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 5246 entries in the HEASARC's version of the 3rd EGRET Catalog corresponding to the same number of lines in Table 4 of the published version. Thus, there are an average of about 20 entries for every distinct source. Notice that 14 sources reported in the 2nd EGRET Catalog or its supplement do not appear in this 3rd EGRET Catalog: 2EG J0403+3357, 2EG J0426+6618, 2EGS J0500+5902, 2EGS J0552-1026, 2EG J1136-0414, 2EGS J1236-0416, 2EG J1239+0441, 2EG J1314+5151, 2EG J1430+5356, 2EG J1443-6040, 2EG J1631-2845, 2EG J1709-0350, 2EG J1815+2950, and 2EG J2027+1054 due to the fact that the re-analysis of the EGRET data has dropped their statistical significance from just above the catalog threshold to just below it; additional information on these sources is provided in Table 5 of the published version of the 3rd EGRET Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egret3#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egret3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=egret3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egret3.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>EGRET [3]</TD>
            <TD>CGRO/EGRET Third Source Catalog</TD>
            <TD>The Third EGRET Catalog of High-Energy Gamma-Ray Sources is based on data obtained by the Energetic Gamma-Ray Experiment Telescope (EGRET) on board the Compton Gamma-Ray Observatory (CGRO) during the period from 1991 April 22 to 1995 October 3, corresponding to GRO Cycles 1, 2, 3, and 4. EGRET is sensitive to photons in the energy range from about 30 MeV to over 20 GeV, the highest energies accessible by the CGRO instruments, and, like COMPTEL, is an imaging instrument. In addition to including more data than the Second EGRET Catalog (2EG, Thompson et al. 1995, ApJS, 101, 259) and its supplement (2EGS, Thompson et al. 1996, ApJS, 107, 227), this catalog uses completely reprocessed data so as to correct a number of mostly minimal errors and problems. The 271 sources (E &gt; 100 MeV) in the catalog include the single 1991 solar flare that was bright enough to detected as a source, the LMC, 5 pulsars, one probable radio galaxy detection (Cen A), and 66 high-confidence identifications of blazars (BL Lac objects, flat-spectrum radio quasars, or unidentified flat-spectrum radio sources). In addition, 27 lower-confidence potential blazar identifications are noted. Finally, the catalog contains 170 sources that are not yet firmly identified with known objects, although potential identifications have been suggested for a number of these. As already noted, there are 271 distinct sources in this catalog: since there are multiple measurements for these sources corresponding to the various viewing periods, there are 5246 entries in the HEASARC's version of the 3rd EGRET Catalog corresponding to the same number of lines in Table 4 of the published version. Thus, there are an average of about 20 entries for every distinct source. Notice that 14 sources reported in the 2nd EGRET Catalog or its supplement do not appear in this 3rd EGRET Catalog: 2EG J0403+3357, 2EG J0426+6618, 2EGS J0500+5902, 2EGS J0552-1026, 2EG J1136-0414, 2EGS J1236-0416, 2EG J1239+0441, 2EG J1314+5151, 2EG J1430+5356, 2EG J1443-6040, 2EG J1631-2845, 2EG J1709-0350, 2EG J1815+2950, and 2EG J2027+1054 due to the fact that the re-analysis of the EGRET data has dropped their statistical significance from just above the catalog threshold to just below it; additional information on these sources is provided in Table 5 of the published version of the 3rd EGRET Catalog.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Gamma-ray#</TD>
            <TD>ivo://nasa.heasarc/egret3#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>3</TD>
            <TD />
            <TD>ivo://nasa.heasarc/egret3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_egret3&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/cgro/egret3.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Einstein/Gal [1]</TD>
            <TD>CatalogofGalaxiesObservedbytheEinsteinObservatoryIPC&amp;HRI</TD>
            <TD>This is a catalog of galaxies observed in the X-ray band with the Einstein Observatory imaging instruments, the Imaging Proportional Counter (IPC) and the High Resolution Imager (HRI). The catalog comprises 716 observations of 493 galaxies, including those that were targets of pointed observations, and galaxies from the Revised Shapley-Ames (RSA) Catalog of Bright Galaxies and the Second Revised Catalog (RC2) Catalog of Bright Galaxies that were serendipitously included in Einstein fields, plus X-ray data on 4 other galaxies (LMC, SMC, M 31 = NGC 224, and M 32 = NGC 221) taken from the literature, for a total of 720 entries. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 212 3-sigma upper limits. The other galaxies were either at the edge of the visible field of view or were confused with other X-ray sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/eingalcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/eingalcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=eingalcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/eingalcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Einstein/Gal [2]</TD>
            <TD>CatalogofGalaxiesObservedbytheEinsteinObservatoryIPC&amp;HRI</TD>
            <TD>This is a catalog of galaxies observed in the X-ray band with the Einstein Observatory imaging instruments, the Imaging Proportional Counter (IPC) and the High Resolution Imager (HRI). The catalog comprises 716 observations of 493 galaxies, including those that were targets of pointed observations, and galaxies from the Revised Shapley-Ames (RSA) Catalog of Bright Galaxies and the Second Revised Catalog (RC2) Catalog of Bright Galaxies that were serendipitously included in Einstein fields, plus X-ray data on 4 other galaxies (LMC, SMC, M 31 = NGC 224, and M 32 = NGC 221) taken from the literature, for a total of 720 entries. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 212 3-sigma upper limits. The other galaxies were either at the edge of the visible field of view or were confused with other X-ray sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/eingalcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/eingalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=eingalcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/eingalcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Einstein/Gal [3]</TD>
            <TD>CatalogofGalaxiesObservedbytheEinsteinObservatoryIPC&amp;HRI</TD>
            <TD>This is a catalog of galaxies observed in the X-ray band with the Einstein Observatory imaging instruments, the Imaging Proportional Counter (IPC) and the High Resolution Imager (HRI). The catalog comprises 716 observations of 493 galaxies, including those that were targets of pointed observations, and galaxies from the Revised Shapley-Ames (RSA) Catalog of Bright Galaxies and the Second Revised Catalog (RC2) Catalog of Bright Galaxies that were serendipitously included in Einstein fields, plus X-ray data on 4 other galaxies (LMC, SMC, M 31 = NGC 224, and M 32 = NGC 221) taken from the literature, for a total of 720 entries. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 212 3-sigma upper limits. The other galaxies were either at the edge of the visible field of view or were confused with other X-ray sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/eingalcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/eingalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_eingalcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/eingalcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Einstein/Gal [1]</TD>
            <TD>CatalogofGalaxiesObservedbytheEinsteinObservatoryIPC&amp;HRI</TD>
            <TD>This is a catalog of galaxies observed in the X-ray band with the Einstein Observatory imaging instruments, the Imaging Proportional Counter (IPC) and the High Resolution Imager (HRI). The catalog comprises 716 observations of 493 galaxies, including those that were targets of pointed observations, and galaxies from the Revised Shapley-Ames (RSA) Catalog of Bright Galaxies and the Second Revised Catalog (RC2) Catalog of Bright Galaxies that were serendipitously included in Einstein fields, plus X-ray data on 4 other galaxies (LMC, SMC, M 31 = NGC 224, and M 32 = NGC 221) taken from the literature, for a total of 720 entries. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 212 3-sigma upper limits. The other galaxies were either at the edge of the visible field of view or were confused with other X-ray sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/eingalcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/eingalcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=eingalcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/eingalcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Einstein/Gal [2]</TD>
            <TD>CatalogofGalaxiesObservedbytheEinsteinObservatoryIPC&amp;HRI</TD>
            <TD>This is a catalog of galaxies observed in the X-ray band with the Einstein Observatory imaging instruments, the Imaging Proportional Counter (IPC) and the High Resolution Imager (HRI). The catalog comprises 716 observations of 493 galaxies, including those that were targets of pointed observations, and galaxies from the Revised Shapley-Ames (RSA) Catalog of Bright Galaxies and the Second Revised Catalog (RC2) Catalog of Bright Galaxies that were serendipitously included in Einstein fields, plus X-ray data on 4 other galaxies (LMC, SMC, M 31 = NGC 224, and M 32 = NGC 221) taken from the literature, for a total of 720 entries. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 212 3-sigma upper limits. The other galaxies were either at the edge of the visible field of view or were confused with other X-ray sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/eingalcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/eingalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=eingalcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/eingalcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Einstein/Gal [3]</TD>
            <TD>CatalogofGalaxiesObservedbytheEinsteinObservatoryIPC&amp;HRI</TD>
            <TD>This is a catalog of galaxies observed in the X-ray band with the Einstein Observatory imaging instruments, the Imaging Proportional Counter (IPC) and the High Resolution Imager (HRI). The catalog comprises 716 observations of 493 galaxies, including those that were targets of pointed observations, and galaxies from the Revised Shapley-Ames (RSA) Catalog of Bright Galaxies and the Second Revised Catalog (RC2) Catalog of Bright Galaxies that were serendipitously included in Einstein fields, plus X-ray data on 4 other galaxies (LMC, SMC, M 31 = NGC 224, and M 32 = NGC 221) taken from the literature, for a total of 720 entries. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 212 3-sigma upper limits. The other galaxies were either at the edge of the visible field of view or were confused with other X-ray sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/eingalcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/eingalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_eingalcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/eingalcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Einstein/Gal [1]</TD>
            <TD>CatalogofGalaxiesObservedbytheEinsteinObservatoryIPC&amp;HRI</TD>
            <TD>This is a catalog of galaxies observed in the X-ray band with the Einstein Observatory imaging instruments, the Imaging Proportional Counter (IPC) and the High Resolution Imager (HRI). The catalog comprises 716 observations of 493 galaxies, including those that were targets of pointed observations, and galaxies from the Revised Shapley-Ames (RSA) Catalog of Bright Galaxies and the Second Revised Catalog (RC2) Catalog of Bright Galaxies that were serendipitously included in Einstein fields, plus X-ray data on 4 other galaxies (LMC, SMC, M 31 = NGC 224, and M 32 = NGC 221) taken from the literature, for a total of 720 entries. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 212 3-sigma upper limits. The other galaxies were either at the edge of the visible field of view or were confused with other X-ray sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/eingalcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/eingalcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=eingalcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/eingalcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Einstein/Gal [2]</TD>
            <TD>CatalogofGalaxiesObservedbytheEinsteinObservatoryIPC&amp;HRI</TD>
            <TD>This is a catalog of galaxies observed in the X-ray band with the Einstein Observatory imaging instruments, the Imaging Proportional Counter (IPC) and the High Resolution Imager (HRI). The catalog comprises 716 observations of 493 galaxies, including those that were targets of pointed observations, and galaxies from the Revised Shapley-Ames (RSA) Catalog of Bright Galaxies and the Second Revised Catalog (RC2) Catalog of Bright Galaxies that were serendipitously included in Einstein fields, plus X-ray data on 4 other galaxies (LMC, SMC, M 31 = NGC 224, and M 32 = NGC 221) taken from the literature, for a total of 720 entries. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 212 3-sigma upper limits. The other galaxies were either at the edge of the visible field of view or were confused with other X-ray sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/eingalcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/eingalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=eingalcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/eingalcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Einstein/Gal [3]</TD>
            <TD>CatalogofGalaxiesObservedbytheEinsteinObservatoryIPC&amp;HRI</TD>
            <TD>This is a catalog of galaxies observed in the X-ray band with the Einstein Observatory imaging instruments, the Imaging Proportional Counter (IPC) and the High Resolution Imager (HRI). The catalog comprises 716 observations of 493 galaxies, including those that were targets of pointed observations, and galaxies from the Revised Shapley-Ames (RSA) Catalog of Bright Galaxies and the Second Revised Catalog (RC2) Catalog of Bright Galaxies that were serendipitously included in Einstein fields, plus X-ray data on 4 other galaxies (LMC, SMC, M 31 = NGC 224, and M 32 = NGC 221) taken from the literature, for a total of 720 entries. A total of 450 of these galaxies were imaged well within the instrumental fields, resulting in 238 detections and 212 3-sigma upper limits. The other galaxies were either at the edge of the visible field of view or were confused with other X-ray sources.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/eingalcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/eingalcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_eingalcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/einstein/eingalcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>H&amp;B91 [1]</TD>
            <TD>Hewitt&amp;Burbidge(1991)CatalogofExtragalacticEmission-LineObjects</TD>
            <TD>This is the Hewitt &amp; Burbidge (1991) Optical Catalog of Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects. It contains a total of 935 galaxies which have optical properties similar to QSOs. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z that are &lt;= 0.2, and most have been classified as Seyfert galaxies, N systems, or radio galaxies. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z &gt; 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06. Notice that this catalog does not include star-like objects with emission-line redshifts &gt;= 0.1 (these can be found in the HEASARC QSO database which contains the Revised and Updated Catalog of Quasi-Stellar Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947). Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or starburst galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/exgalemobj#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/exgalemobj</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=exgalemobj&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/exgalemobj.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>H&amp;B91 [2]</TD>
            <TD>Hewitt&amp;Burbidge(1991)CatalogofExtragalacticEmission-LineObjects</TD>
            <TD>This is the Hewitt &amp; Burbidge (1991) Optical Catalog of Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects. It contains a total of 935 galaxies which have optical properties similar to QSOs. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z that are &lt;= 0.2, and most have been classified as Seyfert galaxies, N systems, or radio galaxies. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z &gt; 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06. Notice that this catalog does not include star-like objects with emission-line redshifts &gt;= 0.1 (these can be found in the HEASARC QSO database which contains the Revised and Updated Catalog of Quasi-Stellar Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947). Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or starburst galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/exgalemobj#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/exgalemobj</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=exgalemobj&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/exgalemobj.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>H&amp;B91 [3]</TD>
            <TD>Hewitt&amp;Burbidge(1991)CatalogofExtragalacticEmission-LineObjects</TD>
            <TD>This is the Hewitt &amp; Burbidge (1991) Optical Catalog of Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects. It contains a total of 935 galaxies which have optical properties similar to QSOs. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z that are &lt;= 0.2, and most have been classified as Seyfert galaxies, N systems, or radio galaxies. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z &gt; 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06. Notice that this catalog does not include star-like objects with emission-line redshifts &gt;= 0.1 (these can be found in the HEASARC QSO database which contains the Revised and Updated Catalog of Quasi-Stellar Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947). Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or starburst galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/exgalemobj#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/exgalemobj</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_exgalemobj&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/exgalemobj.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>H&amp;B91 [1]</TD>
            <TD>Hewitt&amp;Burbidge(1991)CatalogofExtragalacticEmission-LineObjects</TD>
            <TD>This is the Hewitt &amp; Burbidge (1991) Optical Catalog of Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects. It contains a total of 935 galaxies which have optical properties similar to QSOs. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z that are &lt;= 0.2, and most have been classified as Seyfert galaxies, N systems, or radio galaxies. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z &gt; 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06. Notice that this catalog does not include star-like objects with emission-line redshifts &gt;= 0.1 (these can be found in the HEASARC QSO database which contains the Revised and Updated Catalog of Quasi-Stellar Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947). Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or starburst galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/exgalemobj#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/exgalemobj</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=exgalemobj&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/exgalemobj.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>H&amp;B91 [2]</TD>
            <TD>Hewitt&amp;Burbidge(1991)CatalogofExtragalacticEmission-LineObjects</TD>
            <TD>This is the Hewitt &amp; Burbidge (1991) Optical Catalog of Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects. It contains a total of 935 galaxies which have optical properties similar to QSOs. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z that are &lt;= 0.2, and most have been classified as Seyfert galaxies, N systems, or radio galaxies. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z &gt; 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06. Notice that this catalog does not include star-like objects with emission-line redshifts &gt;= 0.1 (these can be found in the HEASARC QSO database which contains the Revised and Updated Catalog of Quasi-Stellar Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947). Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or starburst galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/exgalemobj#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/exgalemobj</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=exgalemobj&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/exgalemobj.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>H&amp;B91 [3]</TD>
            <TD>Hewitt&amp;Burbidge(1991)CatalogofExtragalacticEmission-LineObjects</TD>
            <TD>This is the Hewitt &amp; Burbidge (1991) Optical Catalog of Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects. It contains a total of 935 galaxies which have optical properties similar to QSOs. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z that are &lt;= 0.2, and most have been classified as Seyfert galaxies, N systems, or radio galaxies. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z &gt; 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06. Notice that this catalog does not include star-like objects with emission-line redshifts &gt;= 0.1 (these can be found in the HEASARC QSO database which contains the Revised and Updated Catalog of Quasi-Stellar Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947). Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or starburst galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/exgalemobj#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/exgalemobj</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_exgalemobj&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/exgalemobj.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>H&amp;B91 [1]</TD>
            <TD>Hewitt&amp;Burbidge(1991)CatalogofExtragalacticEmission-LineObjects</TD>
            <TD>This is the Hewitt &amp; Burbidge (1991) Optical Catalog of Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects. It contains a total of 935 galaxies which have optical properties similar to QSOs. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z that are &lt;= 0.2, and most have been classified as Seyfert galaxies, N systems, or radio galaxies. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z &gt; 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06. Notice that this catalog does not include star-like objects with emission-line redshifts &gt;= 0.1 (these can be found in the HEASARC QSO database which contains the Revised and Updated Catalog of Quasi-Stellar Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947). Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or starburst galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/exgalemobj#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/exgalemobj</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=exgalemobj&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/exgalemobj.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>H&amp;B91 [2]</TD>
            <TD>Hewitt&amp;Burbidge(1991)CatalogofExtragalacticEmission-LineObjects</TD>
            <TD>This is the Hewitt &amp; Burbidge (1991) Optical Catalog of Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects. It contains a total of 935 galaxies which have optical properties similar to QSOs. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z that are &lt;= 0.2, and most have been classified as Seyfert galaxies, N systems, or radio galaxies. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z &gt; 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06. Notice that this catalog does not include star-like objects with emission-line redshifts &gt;= 0.1 (these can be found in the HEASARC QSO database which contains the Revised and Updated Catalog of Quasi-Stellar Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947). Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or starburst galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/exgalemobj#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/exgalemobj</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=exgalemobj&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/exgalemobj.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>H&amp;B91 [3]</TD>
            <TD>Hewitt&amp;Burbidge(1991)CatalogofExtragalacticEmission-LineObjects</TD>
            <TD>This is the Hewitt &amp; Burbidge (1991) Optical Catalog of Extragalactic Emission-Line Objects Similar to Quasi-Stellar Objects. It contains a total of 935 galaxies which have optical properties similar to QSOs. Most of the objects appear to be nonstellar. The majority, more than 700, have redshifts z that are &lt;= 0.2, and most have been classified as Seyfert galaxies, N systems, or radio galaxies. The redshift distribution peaks at z ~ 0.025, but there are about 200 powerful radio galaxies in the extended tail of the distribution which have z &gt; 0.2. There is a separate and distinct peak in the redshift distribution at z = 0.06. Notice that this catalog does not include star-like objects with emission-line redshifts &gt;= 0.1 (these can be found in the HEASARC QSO database which contains the Revised and Updated Catalog of Quasi-Stellar Objects" of Hewitt, A. and Burbidge, G. 1993, ApJS, Vol. 87, pp. 451-947). Neither does it contain LINERs (sometimes called Seyfert 3 galaxies) or starburst galaxies.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/exgalemobj#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/exgalemobj</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_exgalemobj&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/exgalemobj.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LCRSCAT [1]</TD>
            <TD>Las Campanas Redshift Survey Catalog</TD>
            <TD>The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg&lt;sup&gt;2&lt;/sup&gt; in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s&lt;sup&gt;-1&lt;/sup&gt;. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s&lt;sup&gt;-1&lt;/sup&gt;, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: &lt;a href="http://qold.astro.utoronto.ca/~lin/lcrs.html"&gt;http://qold.astro.utoronto.ca/~lin/lcrs.html&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lcrscat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lcrscat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lcrscat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/lcrscat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LCRSCAT [2]</TD>
            <TD>Las Campanas Redshift Survey Catalog</TD>
            <TD>The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg&lt;sup&gt;2&lt;/sup&gt; in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s&lt;sup&gt;-1&lt;/sup&gt;. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s&lt;sup&gt;-1&lt;/sup&gt;, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: &lt;a href="http://qold.astro.utoronto.ca/~lin/lcrs.html"&gt;http://qold.astro.utoronto.ca/~lin/lcrs.html&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lcrscat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lcrscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lcrscat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/lcrscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LCRSCAT [3]</TD>
            <TD>Las Campanas Redshift Survey Catalog</TD>
            <TD>The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg&lt;sup&gt;2&lt;/sup&gt; in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s&lt;sup&gt;-1&lt;/sup&gt;. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s&lt;sup&gt;-1&lt;/sup&gt;, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: &lt;a href="http://qold.astro.utoronto.ca/~lin/lcrs.html"&gt;http://qold.astro.utoronto.ca/~lin/lcrs.html&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lcrscat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lcrscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lcrscat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/lcrscat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LCRSCAT [1]</TD>
            <TD>Las Campanas Redshift Survey Catalog</TD>
            <TD>The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg&lt;sup&gt;2&lt;/sup&gt; in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s&lt;sup&gt;-1&lt;/sup&gt;. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s&lt;sup&gt;-1&lt;/sup&gt;, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: &lt;a href="http://qold.astro.utoronto.ca/~lin/lcrs.html"&gt;http://qold.astro.utoronto.ca/~lin/lcrs.html&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lcrscat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lcrscat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lcrscat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/lcrscat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LCRSCAT [2]</TD>
            <TD>Las Campanas Redshift Survey Catalog</TD>
            <TD>The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg&lt;sup&gt;2&lt;/sup&gt; in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s&lt;sup&gt;-1&lt;/sup&gt;. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s&lt;sup&gt;-1&lt;/sup&gt;, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: &lt;a href="http://qold.astro.utoronto.ca/~lin/lcrs.html"&gt;http://qold.astro.utoronto.ca/~lin/lcrs.html&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lcrscat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lcrscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lcrscat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/lcrscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LCRSCAT [3]</TD>
            <TD>Las Campanas Redshift Survey Catalog</TD>
            <TD>The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg&lt;sup&gt;2&lt;/sup&gt; in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s&lt;sup&gt;-1&lt;/sup&gt;. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s&lt;sup&gt;-1&lt;/sup&gt;, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: &lt;a href="http://qold.astro.utoronto.ca/~lin/lcrs.html"&gt;http://qold.astro.utoronto.ca/~lin/lcrs.html&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lcrscat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lcrscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lcrscat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/lcrscat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LCRSCAT [1]</TD>
            <TD>Las Campanas Redshift Survey Catalog</TD>
            <TD>The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg&lt;sup&gt;2&lt;/sup&gt; in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s&lt;sup&gt;-1&lt;/sup&gt;. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s&lt;sup&gt;-1&lt;/sup&gt;, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: &lt;a href="http://qold.astro.utoronto.ca/~lin/lcrs.html"&gt;http://qold.astro.utoronto.ca/~lin/lcrs.html&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lcrscat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lcrscat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lcrscat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/lcrscat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LCRSCAT [2]</TD>
            <TD>Las Campanas Redshift Survey Catalog</TD>
            <TD>The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg&lt;sup&gt;2&lt;/sup&gt; in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s&lt;sup&gt;-1&lt;/sup&gt;. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s&lt;sup&gt;-1&lt;/sup&gt;, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: &lt;a href="http://qold.astro.utoronto.ca/~lin/lcrs.html"&gt;http://qold.astro.utoronto.ca/~lin/lcrs.html&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lcrscat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lcrscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lcrscat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/lcrscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LCRSCAT [3]</TD>
            <TD>Las Campanas Redshift Survey Catalog</TD>
            <TD>The Las Campanas Redshift Survey (LCRS) consists of 26,418 redshifts of galaxies selected from a CCD-based catalog obtained in the R band. The survey covers over 700 deg&lt;sup&gt;2&lt;/sup&gt; in six strips, each 1.5 x 80 degrees, three each in the north and south Galactic caps. The median redshift in the survey is about 30,000 km s&lt;sup&gt;-1&lt;/sup&gt;. Essential features of the galaxy selection and redshift measurement methods are described and tabulated in the reference paper. These details are important for subsequent analysis of the LCRS data. Two-dimensional representations of the redshift distributions reveal many repetitions of voids, on the scale of about 5000 km s&lt;sup&gt;-1&lt;/sup&gt;, sharply bounded by large walls of galaxies as seen in nearby surveys. Statistical investigations of the mean galaxy properties and of clustering on the large scale are reported elsewhere. These include studies of the luminosity function, power spectrum in two and three dimensions, correlation function, pairwise velocity distribution, identification of large-scale structures, and a group catalog. This table contains entries for 94959 objects from the LCRS for which photometric data were obtained and which were initially classified as galaxies on the basis of this photometric information, although subsequent spectroscopy indicated that a small fracton of them are actually stars. There are 27021 objects out of this total which have spectroscopic redshift information (either of themselves or of a nearby object). See also the LCRS home pages at: &lt;a href="http://qold.astro.utoronto.ca/~lin/lcrs.html"&gt;http://qold.astro.utoronto.ca/~lin/lcrs.html&lt;/a&gt; .</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/lcrscat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lcrscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lcrscat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/lcrscat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M101CXO [1]</TD>
            <TD>M 101 Chandra X-Ray Point Source Catalog</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M 101. From this rich data set, the authors have created a catalog of the 110 sources from the S3 chip which were detected with a significance of greater than 3-sigma. This detection threshold corresponds to a flux of ~ 10^-16 ergs/cm^2/s and a luminosity of ~ 10^36 ergs/s for a distance to M 101 of 7.2 Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources. The 29 brightest sources have enough flux (greater than 100 counts) to perform at least crude spectral modeling using the HEASARC XSPEC model fitting program. Most of the sources could be satisfactorily fitted with a simple absorbed power-law spectrum model; however, eight of the softest sources were better fitted by an absorbed blackbody model.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m101cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m101cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M101CXO [2]</TD>
            <TD>M 101 Chandra X-Ray Point Source Catalog</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M 101. From this rich data set, the authors have created a catalog of the 110 sources from the S3 chip which were detected with a significance of greater than 3-sigma. This detection threshold corresponds to a flux of ~ 10^-16 ergs/cm^2/s and a luminosity of ~ 10^36 ergs/s for a distance to M 101 of 7.2 Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources. The 29 brightest sources have enough flux (greater than 100 counts) to perform at least crude spectral modeling using the HEASARC XSPEC model fitting program. Most of the sources could be satisfactorily fitted with a simple absorbed power-law spectrum model; however, eight of the softest sources were better fitted by an absorbed blackbody model.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m101cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m101cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M101CXO [3]</TD>
            <TD>M 101 Chandra X-Ray Point Source Catalog</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M 101. From this rich data set, the authors have created a catalog of the 110 sources from the S3 chip which were detected with a significance of greater than 3-sigma. This detection threshold corresponds to a flux of ~ 10^-16 ergs/cm^2/s and a luminosity of ~ 10^36 ergs/s for a distance to M 101 of 7.2 Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources. The 29 brightest sources have enough flux (greater than 100 counts) to perform at least crude spectral modeling using the HEASARC XSPEC model fitting program. Most of the sources could be satisfactorily fitted with a simple absorbed power-law spectrum model; however, eight of the softest sources were better fitted by an absorbed blackbody model.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m101cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m101cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M101CXO [1]</TD>
            <TD>M 101 Chandra X-Ray Point Source Catalog</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M 101. From this rich data set, the authors have created a catalog of the 110 sources from the S3 chip which were detected with a significance of greater than 3-sigma. This detection threshold corresponds to a flux of ~ 10^-16 ergs/cm^2/s and a luminosity of ~ 10^36 ergs/s for a distance to M 101 of 7.2 Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources. The 29 brightest sources have enough flux (greater than 100 counts) to perform at least crude spectral modeling using the HEASARC XSPEC model fitting program. Most of the sources could be satisfactorily fitted with a simple absorbed power-law spectrum model; however, eight of the softest sources were better fitted by an absorbed blackbody model.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m101cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m101cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M101CXO [2]</TD>
            <TD>M 101 Chandra X-Ray Point Source Catalog</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M 101. From this rich data set, the authors have created a catalog of the 110 sources from the S3 chip which were detected with a significance of greater than 3-sigma. This detection threshold corresponds to a flux of ~ 10^-16 ergs/cm^2/s and a luminosity of ~ 10^36 ergs/s for a distance to M 101 of 7.2 Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources. The 29 brightest sources have enough flux (greater than 100 counts) to perform at least crude spectral modeling using the HEASARC XSPEC model fitting program. Most of the sources could be satisfactorily fitted with a simple absorbed power-law spectrum model; however, eight of the softest sources were better fitted by an absorbed blackbody model.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m101cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m101cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M101CXO [3]</TD>
            <TD>M 101 Chandra X-Ray Point Source Catalog</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M 101. From this rich data set, the authors have created a catalog of the 110 sources from the S3 chip which were detected with a significance of greater than 3-sigma. This detection threshold corresponds to a flux of ~ 10^-16 ergs/cm^2/s and a luminosity of ~ 10^36 ergs/s for a distance to M 101 of 7.2 Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources. The 29 brightest sources have enough flux (greater than 100 counts) to perform at least crude spectral modeling using the HEASARC XSPEC model fitting program. Most of the sources could be satisfactorily fitted with a simple absorbed power-law spectrum model; however, eight of the softest sources were better fitted by an absorbed blackbody model.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m101cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m101cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M101CXO [1]</TD>
            <TD>M 101 Chandra X-Ray Point Source Catalog</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M 101. From this rich data set, the authors have created a catalog of the 110 sources from the S3 chip which were detected with a significance of greater than 3-sigma. This detection threshold corresponds to a flux of ~ 10^-16 ergs/cm^2/s and a luminosity of ~ 10^36 ergs/s for a distance to M 101 of 7.2 Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources. The 29 brightest sources have enough flux (greater than 100 counts) to perform at least crude spectral modeling using the HEASARC XSPEC model fitting program. Most of the sources could be satisfactorily fitted with a simple absorbed power-law spectrum model; however, eight of the softest sources were better fitted by an absorbed blackbody model.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m101cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m101cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M101CXO [2]</TD>
            <TD>M 101 Chandra X-Ray Point Source Catalog</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M 101. From this rich data set, the authors have created a catalog of the 110 sources from the S3 chip which were detected with a significance of greater than 3-sigma. This detection threshold corresponds to a flux of ~ 10^-16 ergs/cm^2/s and a luminosity of ~ 10^36 ergs/s for a distance to M 101 of 7.2 Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources. The 29 brightest sources have enough flux (greater than 100 counts) to perform at least crude spectral modeling using the HEASARC XSPEC model fitting program. Most of the sources could be satisfactorily fitted with a simple absorbed power-law spectrum model; however, eight of the softest sources were better fitted by an absorbed blackbody model.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m101cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m101cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M101CXO [3]</TD>
            <TD>M 101 Chandra X-Ray Point Source Catalog</TD>
            <TD>A deep (98.2ks) Chandra Cycle 1 observation has revealed a wealth of discrete X-ray sources as well as diffuse emission in the nearby face-on spiral galaxy M 101. From this rich data set, the authors have created a catalog of the 110 sources from the S3 chip which were detected with a significance of greater than 3-sigma. This detection threshold corresponds to a flux of ~ 10^-16 ergs/cm^2/s and a luminosity of ~ 10^36 ergs/s for a distance to M 101 of 7.2 Mpc. The sources display a distinct correlation with the spiral arms of M101 and include a variety of X-ray binaries, supersoft sources, supernova remnants, and other objects of which only ~27 are likely to be background sources. The 29 brightest sources have enough flux (greater than 100 counts) to perform at least crude spectral modeling using the HEASARC XSPEC model fitting program. Most of the sources could be satisfactorily fitted with a simple absorbed power-law spectrum model; however, eight of the softest sources were better fitted by an absorbed blackbody model.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m101cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m101cxo.html</TD>
          </TR>
          <TR>
            <TD>CatalogService</TD>
            <TD>M31/GC</TD>
            <TD>M31 Globular Cluster Candidates Catalog</TD>
            <TD>This database table contains a list of 288 globular cluster candidates and 132 miscellaneous objects found in a 70 arcminute square field centered on the M 31 (Andromeda) Galaxy.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/m31clustrs</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Star Cluster#</TD>
            <TD>#Catalog#</TD>
            <TD>#University#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m31clustrs</TD>
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/m31clustrs.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M87CXO [1]</TD>
            <TD>M 87 Chandra X-Ray Point Source Catalog</TD>
            <TD>The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M 87 (NGC 4486), the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images - with a total exposure time of 154 ks - are the deepest X-ray observations obtained as of 2004 of M 87. The authors identified 174 X-ray point sources, (contained in this Browse table) of which ~ 150 are likely LMXBs. This LMXB catalog was combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in the authors' catalog, a fraction f_X = 3.6% ? 0.5% contain an LMXB. M 87 (NGC 4486) was observed with the Chandra Advanced CCD Imaging Spectrometer (ACIS) for 121 ks on 2002 July 5-6. In this table, only the S3 chip data are used. The data were processed following the CIAO data reduction threads, including a correction for charge transfer inefficiency (CTI). In addition, the authors used 38 ks of archival ACIS observations of M 87 taken on 2000 July 29. These data were processed in a fashion similar to the 2002 July data, except that no CTI correction was possible because the data were telemetered in graded mode. All reductions were carried out with CIAO, version 2.3, coupled with CALDB, version 2.21. In order to combine the event files into a single image for point-source detection, the authors obtained relative offsets by matching the celestial coordinates of two X-ray point sources. The relative offset was ~ 0.5". The total exposure time of the co-added image, excluding four background flares totaling ~ 2.5 ks, was 154 ks.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m87cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m87cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m87cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m87cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M87CXO [2]</TD>
            <TD>M 87 Chandra X-Ray Point Source Catalog</TD>
            <TD>The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M 87 (NGC 4486), the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images - with a total exposure time of 154 ks - are the deepest X-ray observations obtained as of 2004 of M 87. The authors identified 174 X-ray point sources, (contained in this Browse table) of which ~ 150 are likely LMXBs. This LMXB catalog was combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in the authors' catalog, a fraction f_X = 3.6% ? 0.5% contain an LMXB. M 87 (NGC 4486) was observed with the Chandra Advanced CCD Imaging Spectrometer (ACIS) for 121 ks on 2002 July 5-6. In this table, only the S3 chip data are used. The data were processed following the CIAO data reduction threads, including a correction for charge transfer inefficiency (CTI). In addition, the authors used 38 ks of archival ACIS observations of M 87 taken on 2000 July 29. These data were processed in a fashion similar to the 2002 July data, except that no CTI correction was possible because the data were telemetered in graded mode. All reductions were carried out with CIAO, version 2.3, coupled with CALDB, version 2.21. In order to combine the event files into a single image for point-source detection, the authors obtained relative offsets by matching the celestial coordinates of two X-ray point sources. The relative offset was ~ 0.5". The total exposure time of the co-added image, excluding four background flares totaling ~ 2.5 ks, was 154 ks.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m87cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m87cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m87cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m87cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M87CXO [3]</TD>
            <TD>M 87 Chandra X-Ray Point Source Catalog</TD>
            <TD>The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M 87 (NGC 4486), the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images - with a total exposure time of 154 ks - are the deepest X-ray observations obtained as of 2004 of M 87. The authors identified 174 X-ray point sources, (contained in this Browse table) of which ~ 150 are likely LMXBs. This LMXB catalog was combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in the authors' catalog, a fraction f_X = 3.6% ? 0.5% contain an LMXB. M 87 (NGC 4486) was observed with the Chandra Advanced CCD Imaging Spectrometer (ACIS) for 121 ks on 2002 July 5-6. In this table, only the S3 chip data are used. The data were processed following the CIAO data reduction threads, including a correction for charge transfer inefficiency (CTI). In addition, the authors used 38 ks of archival ACIS observations of M 87 taken on 2000 July 29. These data were processed in a fashion similar to the 2002 July data, except that no CTI correction was possible because the data were telemetered in graded mode. All reductions were carried out with CIAO, version 2.3, coupled with CALDB, version 2.21. In order to combine the event files into a single image for point-source detection, the authors obtained relative offsets by matching the celestial coordinates of two X-ray point sources. The relative offset was ~ 0.5". The total exposure time of the co-added image, excluding four background flares totaling ~ 2.5 ks, was 154 ks.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m87cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m87cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m87cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m87cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M87CXO [1]</TD>
            <TD>M 87 Chandra X-Ray Point Source Catalog</TD>
            <TD>The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M 87 (NGC 4486), the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images - with a total exposure time of 154 ks - are the deepest X-ray observations obtained as of 2004 of M 87. The authors identified 174 X-ray point sources, (contained in this Browse table) of which ~ 150 are likely LMXBs. This LMXB catalog was combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in the authors' catalog, a fraction f_X = 3.6% ? 0.5% contain an LMXB. M 87 (NGC 4486) was observed with the Chandra Advanced CCD Imaging Spectrometer (ACIS) for 121 ks on 2002 July 5-6. In this table, only the S3 chip data are used. The data were processed following the CIAO data reduction threads, including a correction for charge transfer inefficiency (CTI). In addition, the authors used 38 ks of archival ACIS observations of M 87 taken on 2000 July 29. These data were processed in a fashion similar to the 2002 July data, except that no CTI correction was possible because the data were telemetered in graded mode. All reductions were carried out with CIAO, version 2.3, coupled with CALDB, version 2.21. In order to combine the event files into a single image for point-source detection, the authors obtained relative offsets by matching the celestial coordinates of two X-ray point sources. The relative offset was ~ 0.5". The total exposure time of the co-added image, excluding four background flares totaling ~ 2.5 ks, was 154 ks.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m87cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m87cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m87cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m87cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M87CXO [2]</TD>
            <TD>M 87 Chandra X-Ray Point Source Catalog</TD>
            <TD>The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M 87 (NGC 4486), the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images - with a total exposure time of 154 ks - are the deepest X-ray observations obtained as of 2004 of M 87. The authors identified 174 X-ray point sources, (contained in this Browse table) of which ~ 150 are likely LMXBs. This LMXB catalog was combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in the authors' catalog, a fraction f_X = 3.6% ? 0.5% contain an LMXB. M 87 (NGC 4486) was observed with the Chandra Advanced CCD Imaging Spectrometer (ACIS) for 121 ks on 2002 July 5-6. In this table, only the S3 chip data are used. The data were processed following the CIAO data reduction threads, including a correction for charge transfer inefficiency (CTI). In addition, the authors used 38 ks of archival ACIS observations of M 87 taken on 2000 July 29. These data were processed in a fashion similar to the 2002 July data, except that no CTI correction was possible because the data were telemetered in graded mode. All reductions were carried out with CIAO, version 2.3, coupled with CALDB, version 2.21. In order to combine the event files into a single image for point-source detection, the authors obtained relative offsets by matching the celestial coordinates of two X-ray point sources. The relative offset was ~ 0.5". The total exposure time of the co-added image, excluding four background flares totaling ~ 2.5 ks, was 154 ks.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m87cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m87cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m87cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m87cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M87CXO [3]</TD>
            <TD>M 87 Chandra X-Ray Point Source Catalog</TD>
            <TD>The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M 87 (NGC 4486), the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images - with a total exposure time of 154 ks - are the deepest X-ray observations obtained as of 2004 of M 87. The authors identified 174 X-ray point sources, (contained in this Browse table) of which ~ 150 are likely LMXBs. This LMXB catalog was combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in the authors' catalog, a fraction f_X = 3.6% ? 0.5% contain an LMXB. M 87 (NGC 4486) was observed with the Chandra Advanced CCD Imaging Spectrometer (ACIS) for 121 ks on 2002 July 5-6. In this table, only the S3 chip data are used. The data were processed following the CIAO data reduction threads, including a correction for charge transfer inefficiency (CTI). In addition, the authors used 38 ks of archival ACIS observations of M 87 taken on 2000 July 29. These data were processed in a fashion similar to the 2002 July data, except that no CTI correction was possible because the data were telemetered in graded mode. All reductions were carried out with CIAO, version 2.3, coupled with CALDB, version 2.21. In order to combine the event files into a single image for point-source detection, the authors obtained relative offsets by matching the celestial coordinates of two X-ray point sources. The relative offset was ~ 0.5". The total exposure time of the co-added image, excluding four background flares totaling ~ 2.5 ks, was 154 ks.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m87cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m87cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m87cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m87cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M87CXO [1]</TD>
            <TD>M 87 Chandra X-Ray Point Source Catalog</TD>
            <TD>The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M 87 (NGC 4486), the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images - with a total exposure time of 154 ks - are the deepest X-ray observations obtained as of 2004 of M 87. The authors identified 174 X-ray point sources, (contained in this Browse table) of which ~ 150 are likely LMXBs. This LMXB catalog was combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in the authors' catalog, a fraction f_X = 3.6% ? 0.5% contain an LMXB. M 87 (NGC 4486) was observed with the Chandra Advanced CCD Imaging Spectrometer (ACIS) for 121 ks on 2002 July 5-6. In this table, only the S3 chip data are used. The data were processed following the CIAO data reduction threads, including a correction for charge transfer inefficiency (CTI). In addition, the authors used 38 ks of archival ACIS observations of M 87 taken on 2000 July 29. These data were processed in a fashion similar to the 2002 July data, except that no CTI correction was possible because the data were telemetered in graded mode. All reductions were carried out with CIAO, version 2.3, coupled with CALDB, version 2.21. In order to combine the event files into a single image for point-source detection, the authors obtained relative offsets by matching the celestial coordinates of two X-ray point sources. The relative offset was ~ 0.5". The total exposure time of the co-added image, excluding four background flares totaling ~ 2.5 ks, was 154 ks.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m87cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m87cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m87cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m87cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M87CXO [2]</TD>
            <TD>M 87 Chandra X-Ray Point Source Catalog</TD>
            <TD>The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M 87 (NGC 4486), the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images - with a total exposure time of 154 ks - are the deepest X-ray observations obtained as of 2004 of M 87. The authors identified 174 X-ray point sources, (contained in this Browse table) of which ~ 150 are likely LMXBs. This LMXB catalog was combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in the authors' catalog, a fraction f_X = 3.6% ? 0.5% contain an LMXB. M 87 (NGC 4486) was observed with the Chandra Advanced CCD Imaging Spectrometer (ACIS) for 121 ks on 2002 July 5-6. In this table, only the S3 chip data are used. The data were processed following the CIAO data reduction threads, including a correction for charge transfer inefficiency (CTI). In addition, the authors used 38 ks of archival ACIS observations of M 87 taken on 2000 July 29. These data were processed in a fashion similar to the 2002 July data, except that no CTI correction was possible because the data were telemetered in graded mode. All reductions were carried out with CIAO, version 2.3, coupled with CALDB, version 2.21. In order to combine the event files into a single image for point-source detection, the authors obtained relative offsets by matching the celestial coordinates of two X-ray point sources. The relative offset was ~ 0.5". The total exposure time of the co-added image, excluding four background flares totaling ~ 2.5 ks, was 154 ks.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m87cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m87cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m87cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m87cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M87CXO [3]</TD>
            <TD>M 87 Chandra X-Ray Point Source Catalog</TD>
            <TD>The ACIS instrument on board the Chandra X-Ray Observatory has been used to carry out the first systematic study of low-mass X-ray binaries (LMXBs) in M 87 (NGC 4486), the giant elliptical galaxy near the dynamical center of the Virgo Cluster. These images - with a total exposure time of 154 ks - are the deepest X-ray observations obtained as of 2004 of M 87. The authors identified 174 X-ray point sources, (contained in this Browse table) of which ~ 150 are likely LMXBs. This LMXB catalog was combined with deep F475W and F850LP images taken with ACS on the Hubble Space Telescope (HST) (as part of the ACS Virgo Cluster Survey) to examine the connection between LMXBs and globular clusters in M87. Of the 1688 globular clusters in the authors' catalog, a fraction f_X = 3.6% ? 0.5% contain an LMXB. M 87 (NGC 4486) was observed with the Chandra Advanced CCD Imaging Spectrometer (ACIS) for 121 ks on 2002 July 5-6. In this table, only the S3 chip data are used. The data were processed following the CIAO data reduction threads, including a correction for charge transfer inefficiency (CTI). In addition, the authors used 38 ks of archival ACIS observations of M 87 taken on 2000 July 29. These data were processed in a fashion similar to the 2002 July data, except that no CTI correction was possible because the data were telemetered in graded mode. All reductions were carried out with CIAO, version 2.3, coupled with CALDB, version 2.21. In order to combine the event files into a single image for point-source detection, the authors obtained relative offsets by matching the celestial coordinates of two X-ray point sources. The relative offset was ~ 0.5". The total exposure time of the co-added image, excluding four background flares totaling ~ 2.5 ks, was 154 ks.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m87cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m87cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m87cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/m87cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MOSTSNRCAT [1]</TD>
            <TD>Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog</TD>
            <TD>A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees &lt;= galactic longitude l_II &lt;= 355 degrees, galactic latitude |b_II| &lt;~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/mostsnrcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#SNR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mostsnrcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=mostsnrcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/nebula-catalog/mostsnrcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MOSTSNRCAT [2]</TD>
            <TD>Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog</TD>
            <TD>A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees &lt;= galactic longitude l_II &lt;= 355 degrees, galactic latitude |b_II| &lt;~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/mostsnrcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#SNR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mostsnrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=mostsnrcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/nebula-catalog/mostsnrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MOSTSNRCAT [3]</TD>
            <TD>Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog</TD>
            <TD>A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees &lt;= galactic longitude l_II &lt;= 355 degrees, galactic latitude |b_II| &lt;~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/mostsnrcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#SNR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mostsnrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_mostsnrcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/nebula-catalog/mostsnrcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MOSTSNRCAT [1]</TD>
            <TD>Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog</TD>
            <TD>A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees &lt;= galactic longitude l_II &lt;= 355 degrees, galactic latitude |b_II| &lt;~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/mostsnrcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#SNR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mostsnrcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=mostsnrcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/nebula-catalog/mostsnrcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MOSTSNRCAT [2]</TD>
            <TD>Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog</TD>
            <TD>A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees &lt;= galactic longitude l_II &lt;= 355 degrees, galactic latitude |b_II| &lt;~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/mostsnrcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#SNR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mostsnrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=mostsnrcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/nebula-catalog/mostsnrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MOSTSNRCAT [3]</TD>
            <TD>Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog</TD>
            <TD>A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees &lt;= galactic longitude l_II &lt;= 355 degrees, galactic latitude |b_II| &lt;~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/mostsnrcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#SNR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mostsnrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_mostsnrcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/nebula-catalog/mostsnrcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>MOSTSNRCAT [1]</TD>
            <TD>Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog</TD>
            <TD>A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees &lt;= galactic longitude l_II &lt;= 355 degrees, galactic latitude |b_II| &lt;~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/mostsnrcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#SNR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mostsnrcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=mostsnrcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/nebula-catalog/mostsnrcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>MOSTSNRCAT [2]</TD>
            <TD>Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog</TD>
            <TD>A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees &lt;= galactic longitude l_II &lt;= 355 degrees, galactic latitude |b_II| &lt;~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/mostsnrcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#SNR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mostsnrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=mostsnrcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/nebula-catalog/mostsnrcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>MOSTSNRCAT [3]</TD>
            <TD>Molonglo Observatory Synthesis Telescope Supernova Remnant Catalog</TD>
            <TD>A catalog of supernova remnants (SNR) in the southern Galaxy within the Galactic Plane area 245 degrees &lt;= galactic longitude l_II &lt;= 355 degrees, galactic latitude |b_II| &lt;~ 1.5 degrees has been produced from observations made in a series of 650 overlapping fields at 0.843 GHz (35.6 cm) with a spatial resolution of 43" using the Molonglo Observatory Synthesis Telescope (MOST). This table contains information on 57 known SNR (listed in Table MSC.A of the reference paper), 18 SNR newly discovered in this survey (Table MSC.B), 16 possible SNR (Table MSC.C), and 2 reclassified SNR (discussed in Section 3.3 of the reference paper), for a total of 93 SNR.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/mostsnrcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#SNR#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>1</TD>
            <TD />
            <TD>ivo://nasa.heasarc/mostsnrcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_mostsnrcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/nebula-catalog/mostsnrcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC253XMM [1]</TD>
            <TD>NGC 253 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table contains the NGC 253 XMM-Newton x-Ray point source catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc253xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc253xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc253xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc253xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC253XMM [2]</TD>
            <TD>NGC 253 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table contains the NGC 253 XMM-Newton x-Ray point source catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc253xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc253xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc253xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc253xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC253XMM [3]</TD>
            <TD>NGC 253 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table contains the NGC 253 XMM-Newton x-Ray point source catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc253xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc253xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc253xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc253xmm.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC253XMM [1]</TD>
            <TD>NGC 253 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table contains the NGC 253 XMM-Newton x-Ray point source catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc253xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc253xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc253xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc253xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC253XMM [2]</TD>
            <TD>NGC 253 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table contains the NGC 253 XMM-Newton x-Ray point source catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc253xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc253xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc253xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc253xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC253XMM [3]</TD>
            <TD>NGC 253 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table contains the NGC 253 XMM-Newton x-Ray point source catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc253xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc253xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc253xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc253xmm.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC253XMM [1]</TD>
            <TD>NGC 253 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table contains the NGC 253 XMM-Newton x-Ray point source catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc253xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc253xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc253xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc253xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC253XMM [2]</TD>
            <TD>NGC 253 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table contains the NGC 253 XMM-Newton x-Ray point source catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc253xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc253xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc253xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc253xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC253XMM [3]</TD>
            <TD>NGC 253 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>This table contains the NGC 253 XMM-Newton x-Ray point source catalog. NGC 253 is a local, starbursting spiral galaxy with strong X-ray emission from hot gas, as well as many point sources. The authors have conducted a spectral survey of the X-ray population of NGC 253 using a deep XMM-Newton observation. NGC 253 only accounts for ~20 per cent of the XMM-Newton EPIC field of view, allowing them to identify ~ 100 X-ray sources that are unlikely to be associated with NGC 253. Hence, they were able to make a direct estimate of contamination from, for example, foreground stars and background galaxies. X-ray luminosity functions (XLFs) of galaxy populations are often used to characterize their properties. There are several methods for estimating the luminosities of X-ray sources with few photons. The authors have obtained spectral fits for the brightest 140 sources in the 2003 XMM-Newton observation of NGC 253, and compare the best-fitting luminosities of those 69 non-nuclear sources associated with NGC 253 with luminosities derived using other methods. They find the luminosities obtained from these various methods to vary systematically by a factor of up to 3 for the same data; this is largely due to differences in absorption. The authors therefore conclude that assuming Galactic absorption is probably unwise; rather, one should measure the absorption for the population. In addition, they find that standard estimations of the background contribution to the X-ray sources in the field are insufficient, and that the background active galactic nuclei (AGN) may be systematically more luminous than previously expected. However, the excess in their measured AGN XLF with respect to the expected XLF may be due to an as yet unrecognized population associated with NGC253. XMM-Newton observations are susceptible to periods of high background levels, caused by increased flux of solar particles. The authors screened the data from each of the EPIC cameras (MOS1, MOS2 and pn), to remove flaring intervals. This process resulted in ~ 46 ks of good time for the pn and ~ 69 ks for the MOS cameras. The authors combined the cleaned MOS and pn data, and ran the source detection algorithm provided with the XMM-Newton data analysis suite SAS version 7.0. They accepted sources with maximum-likelihood detections &gt; 10 (equivalent to 4 sigma).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc253xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc253xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc253xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/ngc253xmm.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4278CXO [1]</TD>
            <TD>NGC 4278 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table lists some of the properties of the discrete X-ray sources detected in the authors' monitoring program of the globular cluster (GC)-rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D_25 ellipse angular diameter of the galaxy. These 236 sources range in X-ray luminosity L_X from 3.5 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (with 3-sigma upper limit &lt;=1 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) to ~2 x 10&lt;sup&gt;40&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L_X &gt; 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of the sources expected to be background objects from the log N-log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. This HEASARC table contains the master source list (Table 3 of the reference paper) and the X-ray properties of the sources in the co-added observations (Table 4 of the reference paper), but not the X-ray properties of the sources in the 6 individual observations (Tables 5-10 of the reference paper). The details of the six individual pointings used in this study, e.g., the Chandra OBSIDs, dates, exposure times and cleaned exposure times, are given in Table 1 of the reference paper, and repeated here: &lt;pre&gt; Obs. No.OBSID Date Exposure (s) Cleaned Exposure (s) 1 4741 2005 Feb 3 37462.0 37264.5 2 7077 2006 Mar 16 110303.8 107736.7 3 7078 2006 Jul 25 51433.2 48076.2 4 7079 2006 Oct 24 105071.7 102504.6 5 7081 2007 Feb 20 110724.0 107564.5 6 7080 2007 Apr 20 55824.8 54837.5 Total Co-added 470819.5 457984.0 &lt;/pre&gt; Notes. The pointing OBSID 7181 was taken before OBSID 7080, so to maintain the time sequence of the exposures these observation numbers have been labeled as above in the reference paper. The details of the energy bands and X-ray colors used in this study are given in Table 2 of the reference paper, and repeated here: &lt;pre&gt; Band/Color Energy Range/Definition Broad (B) 0.3-8 keV Soft (S) 0.3-2.5 keV Hard (H) 2.5-8 keV Soft 1 (S1) 0.3-0.9 keV Soft 2 (S2) 0.9-2.5 keV Conventional broad (Bc) 0.5-8 keV Conventional soft (Sc) 0.5-2 keV Conventional hard (Hc) 2-8 keV Hardness ratio HR (Hc-Sc)/(Hc+Sc) X-ray color C21 -log(S2) + log(S1) = log(S1/S2) X-ray color C32 -log(H) + log(S2) = log(S2/H) &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4278cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4278cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4278cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4278cxo.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4278CXO [2]</TD>
            <TD>NGC 4278 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table lists some of the properties of the discrete X-ray sources detected in the authors' monitoring program of the globular cluster (GC)-rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D_25 ellipse angular diameter of the galaxy. These 236 sources range in X-ray luminosity L_X from 3.5 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (with 3-sigma upper limit &lt;=1 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) to ~2 x 10&lt;sup&gt;40&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L_X &gt; 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of the sources expected to be background objects from the log N-log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. This HEASARC table contains the master source list (Table 3 of the reference paper) and the X-ray properties of the sources in the co-added observations (Table 4 of the reference paper), but not the X-ray properties of the sources in the 6 individual observations (Tables 5-10 of the reference paper). The details of the six individual pointings used in this study, e.g., the Chandra OBSIDs, dates, exposure times and cleaned exposure times, are given in Table 1 of the reference paper, and repeated here: &lt;pre&gt; Obs. No.OBSID Date Exposure (s) Cleaned Exposure (s) 1 4741 2005 Feb 3 37462.0 37264.5 2 7077 2006 Mar 16 110303.8 107736.7 3 7078 2006 Jul 25 51433.2 48076.2 4 7079 2006 Oct 24 105071.7 102504.6 5 7081 2007 Feb 20 110724.0 107564.5 6 7080 2007 Apr 20 55824.8 54837.5 Total Co-added 470819.5 457984.0 &lt;/pre&gt; Notes. The pointing OBSID 7181 was taken before OBSID 7080, so to maintain the time sequence of the exposures these observation numbers have been labeled as above in the reference paper. The details of the energy bands and X-ray colors used in this study are given in Table 2 of the reference paper, and repeated here: &lt;pre&gt; Band/Color Energy Range/Definition Broad (B) 0.3-8 keV Soft (S) 0.3-2.5 keV Hard (H) 2.5-8 keV Soft 1 (S1) 0.3-0.9 keV Soft 2 (S2) 0.9-2.5 keV Conventional broad (Bc) 0.5-8 keV Conventional soft (Sc) 0.5-2 keV Conventional hard (Hc) 2-8 keV Hardness ratio HR (Hc-Sc)/(Hc+Sc) X-ray color C21 -log(S2) + log(S1) = log(S1/S2) X-ray color C32 -log(H) + log(S2) = log(S2/H) &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4278cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4278cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ngc4278cxo&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4278cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4278CXO [3]</TD>
            <TD>NGC 4278 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table lists some of the properties of the discrete X-ray sources detected in the authors' monitoring program of the globular cluster (GC)-rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D_25 ellipse angular diameter of the galaxy. These 236 sources range in X-ray luminosity L_X from 3.5 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (with 3-sigma upper limit &lt;=1 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) to ~2 x 10&lt;sup&gt;40&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L_X &gt; 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of the sources expected to be background objects from the log N-log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. This HEASARC table contains the master source list (Table 3 of the reference paper) and the X-ray properties of the sources in the co-added observations (Table 4 of the reference paper), but not the X-ray properties of the sources in the 6 individual observations (Tables 5-10 of the reference paper). The details of the six individual pointings used in this study, e.g., the Chandra OBSIDs, dates, exposure times and cleaned exposure times, are given in Table 1 of the reference paper, and repeated here: &lt;pre&gt; Obs. No.OBSID Date Exposure (s) Cleaned Exposure (s) 1 4741 2005 Feb 3 37462.0 37264.5 2 7077 2006 Mar 16 110303.8 107736.7 3 7078 2006 Jul 25 51433.2 48076.2 4 7079 2006 Oct 24 105071.7 102504.6 5 7081 2007 Feb 20 110724.0 107564.5 6 7080 2007 Apr 20 55824.8 54837.5 Total Co-added 470819.5 457984.0 &lt;/pre&gt; Notes. The pointing OBSID 7181 was taken before OBSID 7080, so to maintain the time sequence of the exposures these observation numbers have been labeled as above in the reference paper. The details of the energy bands and X-ray colors used in this study are given in Table 2 of the reference paper, and repeated here: &lt;pre&gt; Band/Color Energy Range/Definition Broad (B) 0.3-8 keV Soft (S) 0.3-2.5 keV Hard (H) 2.5-8 keV Soft 1 (S1) 0.3-0.9 keV Soft 2 (S2) 0.9-2.5 keV Conventional broad (Bc) 0.5-8 keV Conventional soft (Sc) 0.5-2 keV Conventional hard (Hc) 2-8 keV Hardness ratio HR (Hc-Sc)/(Hc+Sc) X-ray color C21 -log(S2) + log(S1) = log(S1/S2) X-ray color C32 -log(H) + log(S2) = log(S2/H) &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4278cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4278cxo</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4278cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4278cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4278CXO [1]</TD>
            <TD>NGC 4278 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table lists some of the properties of the discrete X-ray sources detected in the authors' monitoring program of the globular cluster (GC)-rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D_25 ellipse angular diameter of the galaxy. These 236 sources range in X-ray luminosity L_X from 3.5 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (with 3-sigma upper limit &lt;=1 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) to ~2 x 10&lt;sup&gt;40&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L_X &gt; 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of the sources expected to be background objects from the log N-log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. This HEASARC table contains the master source list (Table 3 of the reference paper) and the X-ray properties of the sources in the co-added observations (Table 4 of the reference paper), but not the X-ray properties of the sources in the 6 individual observations (Tables 5-10 of the reference paper). The details of the six individual pointings used in this study, e.g., the Chandra OBSIDs, dates, exposure times and cleaned exposure times, are given in Table 1 of the reference paper, and repeated here: &lt;pre&gt; Obs. No.OBSID Date Exposure (s) Cleaned Exposure (s) 1 4741 2005 Feb 3 37462.0 37264.5 2 7077 2006 Mar 16 110303.8 107736.7 3 7078 2006 Jul 25 51433.2 48076.2 4 7079 2006 Oct 24 105071.7 102504.6 5 7081 2007 Feb 20 110724.0 107564.5 6 7080 2007 Apr 20 55824.8 54837.5 Total Co-added 470819.5 457984.0 &lt;/pre&gt; Notes. The pointing OBSID 7181 was taken before OBSID 7080, so to maintain the time sequence of the exposures these observation numbers have been labeled as above in the reference paper. The details of the energy bands and X-ray colors used in this study are given in Table 2 of the reference paper, and repeated here: &lt;pre&gt; Band/Color Energy Range/Definition Broad (B) 0.3-8 keV Soft (S) 0.3-2.5 keV Hard (H) 2.5-8 keV Soft 1 (S1) 0.3-0.9 keV Soft 2 (S2) 0.9-2.5 keV Conventional broad (Bc) 0.5-8 keV Conventional soft (Sc) 0.5-2 keV Conventional hard (Hc) 2-8 keV Hardness ratio HR (Hc-Sc)/(Hc+Sc) X-ray color C21 -log(S2) + log(S1) = log(S1/S2) X-ray color C32 -log(H) + log(S2) = log(S2/H) &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4278cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ngc4278cxo</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ngc4278cxo&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4278CXO [2]</TD>
            <TD>NGC 4278 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table lists some of the properties of the discrete X-ray sources detected in the authors' monitoring program of the globular cluster (GC)-rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D_25 ellipse angular diameter of the galaxy. These 236 sources range in X-ray luminosity L_X from 3.5 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (with 3-sigma upper limit &lt;=1 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) to ~2 x 10&lt;sup&gt;40&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L_X &gt; 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of the sources expected to be background objects from the log N-log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. This HEASARC table contains the master source list (Table 3 of the reference paper) and the X-ray properties of the sources in the co-added observations (Table 4 of the reference paper), but not the X-ray properties of the sources in the 6 individual observations (Tables 5-10 of the reference paper). The details of the six individual pointings used in this study, e.g., the Chandra OBSIDs, dates, exposure times and cleaned exposure times, are given in Table 1 of the reference paper, and repeated here: &lt;pre&gt; Obs. No.OBSID Date Exposure (s) Cleaned Exposure (s) 1 4741 2005 Feb 3 37462.0 37264.5 2 7077 2006 Mar 16 110303.8 107736.7 3 7078 2006 Jul 25 51433.2 48076.2 4 7079 2006 Oct 24 105071.7 102504.6 5 7081 2007 Feb 20 110724.0 107564.5 6 7080 2007 Apr 20 55824.8 54837.5 Total Co-added 470819.5 457984.0 &lt;/pre&gt; Notes. The pointing OBSID 7181 was taken before OBSID 7080, so to maintain the time sequence of the exposures these observation numbers have been labeled as above in the reference paper. The details of the energy bands and X-ray colors used in this study are given in Table 2 of the reference paper, and repeated here: &lt;pre&gt; Band/Color Energy Range/Definition Broad (B) 0.3-8 keV Soft (S) 0.3-2.5 keV Hard (H) 2.5-8 keV Soft 1 (S1) 0.3-0.9 keV Soft 2 (S2) 0.9-2.5 keV Conventional broad (Bc) 0.5-8 keV Conventional soft (Sc) 0.5-2 keV Conventional hard (Hc) 2-8 keV Hardness ratio HR (Hc-Sc)/(Hc+Sc) X-ray color C21 -log(S2) + log(S1) = log(S1/S2) X-ray color C32 -log(H) + log(S2) = log(S2/H) &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4278cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD />
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            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4278cxo.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4278CXO [3]</TD>
            <TD>NGC 4278 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table lists some of the properties of the discrete X-ray sources detected in the authors' monitoring program of the globular cluster (GC)-rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D_25 ellipse angular diameter of the galaxy. These 236 sources range in X-ray luminosity L_X from 3.5 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (with 3-sigma upper limit &lt;=1 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) to ~2 x 10&lt;sup&gt;40&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L_X &gt; 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of the sources expected to be background objects from the log N-log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. This HEASARC table contains the master source list (Table 3 of the reference paper) and the X-ray properties of the sources in the co-added observations (Table 4 of the reference paper), but not the X-ray properties of the sources in the 6 individual observations (Tables 5-10 of the reference paper). The details of the six individual pointings used in this study, e.g., the Chandra OBSIDs, dates, exposure times and cleaned exposure times, are given in Table 1 of the reference paper, and repeated here: &lt;pre&gt; Obs. No.OBSID Date Exposure (s) Cleaned Exposure (s) 1 4741 2005 Feb 3 37462.0 37264.5 2 7077 2006 Mar 16 110303.8 107736.7 3 7078 2006 Jul 25 51433.2 48076.2 4 7079 2006 Oct 24 105071.7 102504.6 5 7081 2007 Feb 20 110724.0 107564.5 6 7080 2007 Apr 20 55824.8 54837.5 Total Co-added 470819.5 457984.0 &lt;/pre&gt; Notes. The pointing OBSID 7181 was taken before OBSID 7080, so to maintain the time sequence of the exposures these observation numbers have been labeled as above in the reference paper. The details of the energy bands and X-ray colors used in this study are given in Table 2 of the reference paper, and repeated here: &lt;pre&gt; Band/Color Energy Range/Definition Broad (B) 0.3-8 keV Soft (S) 0.3-2.5 keV Hard (H) 2.5-8 keV Soft 1 (S1) 0.3-0.9 keV Soft 2 (S2) 0.9-2.5 keV Conventional broad (Bc) 0.5-8 keV Conventional soft (Sc) 0.5-2 keV Conventional hard (Hc) 2-8 keV Hardness ratio HR (Hc-Sc)/(Hc+Sc) X-ray color C21 -log(S2) + log(S1) = log(S1/S2) X-ray color C32 -log(H) + log(S2) = log(S2/H) &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4278cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ngc4278cxo&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ngc4278cxo.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NGC4278CXO [1]</TD>
            <TD>NGC 4278 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table lists some of the properties of the discrete X-ray sources detected in the authors' monitoring program of the globular cluster (GC)-rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D_25 ellipse angular diameter of the galaxy. These 236 sources range in X-ray luminosity L_X from 3.5 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (with 3-sigma upper limit &lt;=1 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) to ~2 x 10&lt;sup&gt;40&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L_X &gt; 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of the sources expected to be background objects from the log N-log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. This HEASARC table contains the master source list (Table 3 of the reference paper) and the X-ray properties of the sources in the co-added observations (Table 4 of the reference paper), but not the X-ray properties of the sources in the 6 individual observations (Tables 5-10 of the reference paper). The details of the six individual pointings used in this study, e.g., the Chandra OBSIDs, dates, exposure times and cleaned exposure times, are given in Table 1 of the reference paper, and repeated here: &lt;pre&gt; Obs. No.OBSID Date Exposure (s) Cleaned Exposure (s) 1 4741 2005 Feb 3 37462.0 37264.5 2 7077 2006 Mar 16 110303.8 107736.7 3 7078 2006 Jul 25 51433.2 48076.2 4 7079 2006 Oct 24 105071.7 102504.6 5 7081 2007 Feb 20 110724.0 107564.5 6 7080 2007 Apr 20 55824.8 54837.5 Total Co-added 470819.5 457984.0 &lt;/pre&gt; Notes. The pointing OBSID 7181 was taken before OBSID 7080, so to maintain the time sequence of the exposures these observation numbers have been labeled as above in the reference paper. The details of the energy bands and X-ray colors used in this study are given in Table 2 of the reference paper, and repeated here: &lt;pre&gt; Band/Color Energy Range/Definition Broad (B) 0.3-8 keV Soft (S) 0.3-2.5 keV Hard (H) 2.5-8 keV Soft 1 (S1) 0.3-0.9 keV Soft 2 (S2) 0.9-2.5 keV Conventional broad (Bc) 0.5-8 keV Conventional soft (Sc) 0.5-2 keV Conventional hard (Hc) 2-8 keV Hardness ratio HR (Hc-Sc)/(Hc+Sc) X-ray color C21 -log(S2) + log(S1) = log(S1/S2) X-ray color C32 -log(H) + log(S2) = log(S2/H) &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4278cxo#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NGC4278CXO [2]</TD>
            <TD>NGC 4278 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table lists some of the properties of the discrete X-ray sources detected in the authors' monitoring program of the globular cluster (GC)-rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D_25 ellipse angular diameter of the galaxy. These 236 sources range in X-ray luminosity L_X from 3.5 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (with 3-sigma upper limit &lt;=1 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) to ~2 x 10&lt;sup&gt;40&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L_X &gt; 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of the sources expected to be background objects from the log N-log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. This HEASARC table contains the master source list (Table 3 of the reference paper) and the X-ray properties of the sources in the co-added observations (Table 4 of the reference paper), but not the X-ray properties of the sources in the 6 individual observations (Tables 5-10 of the reference paper). The details of the six individual pointings used in this study, e.g., the Chandra OBSIDs, dates, exposure times and cleaned exposure times, are given in Table 1 of the reference paper, and repeated here: &lt;pre&gt; Obs. No.OBSID Date Exposure (s) Cleaned Exposure (s) 1 4741 2005 Feb 3 37462.0 37264.5 2 7077 2006 Mar 16 110303.8 107736.7 3 7078 2006 Jul 25 51433.2 48076.2 4 7079 2006 Oct 24 105071.7 102504.6 5 7081 2007 Feb 20 110724.0 107564.5 6 7080 2007 Apr 20 55824.8 54837.5 Total Co-added 470819.5 457984.0 &lt;/pre&gt; Notes. The pointing OBSID 7181 was taken before OBSID 7080, so to maintain the time sequence of the exposures these observation numbers have been labeled as above in the reference paper. The details of the energy bands and X-ray colors used in this study are given in Table 2 of the reference paper, and repeated here: &lt;pre&gt; Band/Color Energy Range/Definition Broad (B) 0.3-8 keV Soft (S) 0.3-2.5 keV Hard (H) 2.5-8 keV Soft 1 (S1) 0.3-0.9 keV Soft 2 (S2) 0.9-2.5 keV Conventional broad (Bc) 0.5-8 keV Conventional soft (Sc) 0.5-2 keV Conventional hard (Hc) 2-8 keV Hardness ratio HR (Hc-Sc)/(Hc+Sc) X-ray color C21 -log(S2) + log(S1) = log(S1/S2) X-ray color C32 -log(H) + log(S2) = log(S2/H) &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4278cxo#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NGC4278CXO [3]</TD>
            <TD>NGC 4278 Chandra X-Ray Point Source Catalog</TD>
            <TD>This table lists some of the properties of the discrete X-ray sources detected in the authors' monitoring program of the globular cluster (GC)-rich elliptical galaxy, NGC 4278, observed with Chandra ACIS-S in six separate pointings, resulting in a co-added exposure of 458 ks. From this deep observation, 236 sources have been detected within the region overlapped by all observations, 180 of which lie within the D_25 ellipse angular diameter of the galaxy. These 236 sources range in X-ray luminosity L_X from 3.5 x 10&lt;sup&gt;36&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt; (with 3-sigma upper limit &lt;=1 x 10&lt;sup&gt;37&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;) to ~2 x 10&lt;sup&gt;40&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;, including the central nuclear source which has been classified as a LINER. From optical data, 39 X-ray sources have been determined to be coincident with a GC, these sources tend to have high X-ray luminosity, with 10 of these sources exhibiting L_X &gt; 1 x 10&lt;sup&gt;38&lt;/sup&gt; erg s&lt;sup&gt;-1&lt;/sup&gt;. From X-ray source photometry, it has been determined that the majority of the 236 point sources that have well-constrained colors have values that are consistent with typical low-mass X-ray binary spectra, with 29 of the sources expected to be background objects from the log N-log S relation. There are 103 sources in this population that exhibit long-term variability, indicating that they are accreting compact objects. Three of these sources have been identified as transient candidates, with a further three possible transients. Spectral variations have also been identified in the majority of the source population, where a diverse range of variability has been identified, indicating that there are many different source classes located within this galaxy. This HEASARC table contains the master source list (Table 3 of the reference paper) and the X-ray properties of the sources in the co-added observations (Table 4 of the reference paper), but not the X-ray properties of the sources in the 6 individual observations (Tables 5-10 of the reference paper). The details of the six individual pointings used in this study, e.g., the Chandra OBSIDs, dates, exposure times and cleaned exposure times, are given in Table 1 of the reference paper, and repeated here: &lt;pre&gt; Obs. No.OBSID Date Exposure (s) Cleaned Exposure (s) 1 4741 2005 Feb 3 37462.0 37264.5 2 7077 2006 Mar 16 110303.8 107736.7 3 7078 2006 Jul 25 51433.2 48076.2 4 7079 2006 Oct 24 105071.7 102504.6 5 7081 2007 Feb 20 110724.0 107564.5 6 7080 2007 Apr 20 55824.8 54837.5 Total Co-added 470819.5 457984.0 &lt;/pre&gt; Notes. The pointing OBSID 7181 was taken before OBSID 7080, so to maintain the time sequence of the exposures these observation numbers have been labeled as above in the reference paper. The details of the energy bands and X-ray colors used in this study are given in Table 2 of the reference paper, and repeated here: &lt;pre&gt; Band/Color Energy Range/Definition Broad (B) 0.3-8 keV Soft (S) 0.3-2.5 keV Hard (H) 2.5-8 keV Soft 1 (S1) 0.3-0.9 keV Soft 2 (S2) 0.9-2.5 keV Conventional broad (Bc) 0.5-8 keV Conventional soft (Sc) 0.5-2 keV Conventional hard (Hc) 2-8 keV Hardness ratio HR (Hc-Sc)/(Hc+Sc) X-ray color C21 -log(S2) + log(S1) = log(S1/S2) X-ray color C32 -log(H) + log(S2) = log(S2/H) &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ngc4278cxo#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>NORASGalClus [1]</TD>
            <TD>Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog</TD>
            <TD>In the construction of an X-ray-selected sample of galaxy clusters for cosmological studies, the authors have assembled a sample of 495 X-ray sources which were found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region with declination &gt;=0 degrees and Galactic latitude |b| &gt;= 20 degrees, and comprises sources with a Position Sensitive Proportional Counter (PSPC) count rate &gt;= 0.06 counts/s and a source extent likelihood of L &gt;= 7. In an optical follow-up identification program, the authors found 378 (76%) of these sources to be clusters of galaxies. It was necessary to reanalyze the sources in this sample with a new X-ray source characterization technique to provide more precise values for the X-ray flux and source extent than obtained from the standard processing. This new method, termed growth curve analysis (GCA), has the advantage over previous methods in its ability to be robust, to be easy to model and to integrate into simulations, to provide diagnostic plots for visual inspection, and to make extensive use of the X-ray data. The source parameters obtained assist the source identification and provide more precise X-ray fluxes. This reanalysis is based on data from the more recent second processing of the ROSAT Survey, RASS II. The authors present a catalog of the cluster sources with the X-ray properties obtained as well as a list of the previously flagged extended sources that are found to have a non-cluster counterpart. In their paper, they discuss the process of source identification from the combination of optical and X-ray data. To investigate the overall completeness of the cluster sample as a function of the X-ray flux limit, they extended the search for X-ray cluster sources to the RASS II data for the northern sky region between 9 and 14 hours in right ascension. They included the search for X-ray emission from known galaxy clusters as well as a new investigation of extended X-ray sources. In the course of this search, they found X-ray emission from 85 additional Abell clusters and 56 very probable cluster candidates among the newly found extended sources. A comparison of the X-ray cluster number counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX) Cluster Survey results leads to an estimate of the completeness of the NORAS sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s^-1 cm^-2. The estimated completeness achieved by adding the supplementary sample in the study area amounts to about 82% in comparison to REFLEX. The low completeness introduces an uncertainty in the use of the sample for cosmological statistical studies that will be cured with the completion of the continuing Northern ROSAT All-Sky (NORAS) Cluster Survey project.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/noras#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/noras</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/noras.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NORASGalClus [2]</TD>
            <TD>Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog</TD>
            <TD>In the construction of an X-ray-selected sample of galaxy clusters for cosmological studies, the authors have assembled a sample of 495 X-ray sources which were found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region with declination &gt;=0 degrees and Galactic latitude |b| &gt;= 20 degrees, and comprises sources with a Position Sensitive Proportional Counter (PSPC) count rate &gt;= 0.06 counts/s and a source extent likelihood of L &gt;= 7. In an optical follow-up identification program, the authors found 378 (76%) of these sources to be clusters of galaxies. It was necessary to reanalyze the sources in this sample with a new X-ray source characterization technique to provide more precise values for the X-ray flux and source extent than obtained from the standard processing. This new method, termed growth curve analysis (GCA), has the advantage over previous methods in its ability to be robust, to be easy to model and to integrate into simulations, to provide diagnostic plots for visual inspection, and to make extensive use of the X-ray data. The source parameters obtained assist the source identification and provide more precise X-ray fluxes. This reanalysis is based on data from the more recent second processing of the ROSAT Survey, RASS II. The authors present a catalog of the cluster sources with the X-ray properties obtained as well as a list of the previously flagged extended sources that are found to have a non-cluster counterpart. In their paper, they discuss the process of source identification from the combination of optical and X-ray data. To investigate the overall completeness of the cluster sample as a function of the X-ray flux limit, they extended the search for X-ray cluster sources to the RASS II data for the northern sky region between 9 and 14 hours in right ascension. They included the search for X-ray emission from known galaxy clusters as well as a new investigation of extended X-ray sources. In the course of this search, they found X-ray emission from 85 additional Abell clusters and 56 very probable cluster candidates among the newly found extended sources. A comparison of the X-ray cluster number counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX) Cluster Survey results leads to an estimate of the completeness of the NORAS sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s^-1 cm^-2. The estimated completeness achieved by adding the supplementary sample in the study area amounts to about 82% in comparison to REFLEX. The low completeness introduces an uncertainty in the use of the sample for cosmological statistical studies that will be cured with the completion of the continuing Northern ROSAT All-Sky (NORAS) Cluster Survey project.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/noras#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/noras</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=noras&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/noras.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NORASGalClus [3]</TD>
            <TD>Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog</TD>
            <TD>In the construction of an X-ray-selected sample of galaxy clusters for cosmological studies, the authors have assembled a sample of 495 X-ray sources which were found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region with declination &gt;=0 degrees and Galactic latitude |b| &gt;= 20 degrees, and comprises sources with a Position Sensitive Proportional Counter (PSPC) count rate &gt;= 0.06 counts/s and a source extent likelihood of L &gt;= 7. In an optical follow-up identification program, the authors found 378 (76%) of these sources to be clusters of galaxies. It was necessary to reanalyze the sources in this sample with a new X-ray source characterization technique to provide more precise values for the X-ray flux and source extent than obtained from the standard processing. This new method, termed growth curve analysis (GCA), has the advantage over previous methods in its ability to be robust, to be easy to model and to integrate into simulations, to provide diagnostic plots for visual inspection, and to make extensive use of the X-ray data. The source parameters obtained assist the source identification and provide more precise X-ray fluxes. This reanalysis is based on data from the more recent second processing of the ROSAT Survey, RASS II. The authors present a catalog of the cluster sources with the X-ray properties obtained as well as a list of the previously flagged extended sources that are found to have a non-cluster counterpart. In their paper, they discuss the process of source identification from the combination of optical and X-ray data. To investigate the overall completeness of the cluster sample as a function of the X-ray flux limit, they extended the search for X-ray cluster sources to the RASS II data for the northern sky region between 9 and 14 hours in right ascension. They included the search for X-ray emission from known galaxy clusters as well as a new investigation of extended X-ray sources. In the course of this search, they found X-ray emission from 85 additional Abell clusters and 56 very probable cluster candidates among the newly found extended sources. A comparison of the X-ray cluster number counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX) Cluster Survey results leads to an estimate of the completeness of the NORAS sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s^-1 cm^-2. The estimated completeness achieved by adding the supplementary sample in the study area amounts to about 82% in comparison to REFLEX. The low completeness introduces an uncertainty in the use of the sample for cosmological statistical studies that will be cured with the completion of the continuing Northern ROSAT All-Sky (NORAS) Cluster Survey project.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/noras#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/noras</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_noras&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/noras.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NORASGalClus [1]</TD>
            <TD>Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog</TD>
            <TD>In the construction of an X-ray-selected sample of galaxy clusters for cosmological studies, the authors have assembled a sample of 495 X-ray sources which were found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region with declination &gt;=0 degrees and Galactic latitude |b| &gt;= 20 degrees, and comprises sources with a Position Sensitive Proportional Counter (PSPC) count rate &gt;= 0.06 counts/s and a source extent likelihood of L &gt;= 7. In an optical follow-up identification program, the authors found 378 (76%) of these sources to be clusters of galaxies. It was necessary to reanalyze the sources in this sample with a new X-ray source characterization technique to provide more precise values for the X-ray flux and source extent than obtained from the standard processing. This new method, termed growth curve analysis (GCA), has the advantage over previous methods in its ability to be robust, to be easy to model and to integrate into simulations, to provide diagnostic plots for visual inspection, and to make extensive use of the X-ray data. The source parameters obtained assist the source identification and provide more precise X-ray fluxes. This reanalysis is based on data from the more recent second processing of the ROSAT Survey, RASS II. The authors present a catalog of the cluster sources with the X-ray properties obtained as well as a list of the previously flagged extended sources that are found to have a non-cluster counterpart. In their paper, they discuss the process of source identification from the combination of optical and X-ray data. To investigate the overall completeness of the cluster sample as a function of the X-ray flux limit, they extended the search for X-ray cluster sources to the RASS II data for the northern sky region between 9 and 14 hours in right ascension. They included the search for X-ray emission from known galaxy clusters as well as a new investigation of extended X-ray sources. In the course of this search, they found X-ray emission from 85 additional Abell clusters and 56 very probable cluster candidates among the newly found extended sources. A comparison of the X-ray cluster number counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX) Cluster Survey results leads to an estimate of the completeness of the NORAS sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s^-1 cm^-2. The estimated completeness achieved by adding the supplementary sample in the study area amounts to about 82% in comparison to REFLEX. The low completeness introduces an uncertainty in the use of the sample for cosmological statistical studies that will be cured with the completion of the continuing Northern ROSAT All-Sky (NORAS) Cluster Survey project.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/noras#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/noras</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=noras&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/noras.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NORASGalClus [2]</TD>
            <TD>Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog</TD>
            <TD>In the construction of an X-ray-selected sample of galaxy clusters for cosmological studies, the authors have assembled a sample of 495 X-ray sources which were found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region with declination &gt;=0 degrees and Galactic latitude |b| &gt;= 20 degrees, and comprises sources with a Position Sensitive Proportional Counter (PSPC) count rate &gt;= 0.06 counts/s and a source extent likelihood of L &gt;= 7. In an optical follow-up identification program, the authors found 378 (76%) of these sources to be clusters of galaxies. It was necessary to reanalyze the sources in this sample with a new X-ray source characterization technique to provide more precise values for the X-ray flux and source extent than obtained from the standard processing. This new method, termed growth curve analysis (GCA), has the advantage over previous methods in its ability to be robust, to be easy to model and to integrate into simulations, to provide diagnostic plots for visual inspection, and to make extensive use of the X-ray data. The source parameters obtained assist the source identification and provide more precise X-ray fluxes. This reanalysis is based on data from the more recent second processing of the ROSAT Survey, RASS II. The authors present a catalog of the cluster sources with the X-ray properties obtained as well as a list of the previously flagged extended sources that are found to have a non-cluster counterpart. In their paper, they discuss the process of source identification from the combination of optical and X-ray data. To investigate the overall completeness of the cluster sample as a function of the X-ray flux limit, they extended the search for X-ray cluster sources to the RASS II data for the northern sky region between 9 and 14 hours in right ascension. They included the search for X-ray emission from known galaxy clusters as well as a new investigation of extended X-ray sources. In the course of this search, they found X-ray emission from 85 additional Abell clusters and 56 very probable cluster candidates among the newly found extended sources. A comparison of the X-ray cluster number counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX) Cluster Survey results leads to an estimate of the completeness of the NORAS sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s^-1 cm^-2. The estimated completeness achieved by adding the supplementary sample in the study area amounts to about 82% in comparison to REFLEX. The low completeness introduces an uncertainty in the use of the sample for cosmological statistical studies that will be cured with the completion of the continuing Northern ROSAT All-Sky (NORAS) Cluster Survey project.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/noras#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/noras</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=noras&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/noras.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NORASGalClus [3]</TD>
            <TD>Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog</TD>
            <TD>In the construction of an X-ray-selected sample of galaxy clusters for cosmological studies, the authors have assembled a sample of 495 X-ray sources which were found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region with declination &gt;=0 degrees and Galactic latitude |b| &gt;= 20 degrees, and comprises sources with a Position Sensitive Proportional Counter (PSPC) count rate &gt;= 0.06 counts/s and a source extent likelihood of L &gt;= 7. In an optical follow-up identification program, the authors found 378 (76%) of these sources to be clusters of galaxies. It was necessary to reanalyze the sources in this sample with a new X-ray source characterization technique to provide more precise values for the X-ray flux and source extent than obtained from the standard processing. This new method, termed growth curve analysis (GCA), has the advantage over previous methods in its ability to be robust, to be easy to model and to integrate into simulations, to provide diagnostic plots for visual inspection, and to make extensive use of the X-ray data. The source parameters obtained assist the source identification and provide more precise X-ray fluxes. This reanalysis is based on data from the more recent second processing of the ROSAT Survey, RASS II. The authors present a catalog of the cluster sources with the X-ray properties obtained as well as a list of the previously flagged extended sources that are found to have a non-cluster counterpart. In their paper, they discuss the process of source identification from the combination of optical and X-ray data. To investigate the overall completeness of the cluster sample as a function of the X-ray flux limit, they extended the search for X-ray cluster sources to the RASS II data for the northern sky region between 9 and 14 hours in right ascension. They included the search for X-ray emission from known galaxy clusters as well as a new investigation of extended X-ray sources. In the course of this search, they found X-ray emission from 85 additional Abell clusters and 56 very probable cluster candidates among the newly found extended sources. A comparison of the X-ray cluster number counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX) Cluster Survey results leads to an estimate of the completeness of the NORAS sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s^-1 cm^-2. The estimated completeness achieved by adding the supplementary sample in the study area amounts to about 82% in comparison to REFLEX. The low completeness introduces an uncertainty in the use of the sample for cosmological statistical studies that will be cured with the completion of the continuing Northern ROSAT All-Sky (NORAS) Cluster Survey project.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/noras#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/noras</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_noras&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/noras.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>NORASGalClus [1]</TD>
            <TD>Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog</TD>
            <TD>In the construction of an X-ray-selected sample of galaxy clusters for cosmological studies, the authors have assembled a sample of 495 X-ray sources which were found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region with declination &gt;=0 degrees and Galactic latitude |b| &gt;= 20 degrees, and comprises sources with a Position Sensitive Proportional Counter (PSPC) count rate &gt;= 0.06 counts/s and a source extent likelihood of L &gt;= 7. In an optical follow-up identification program, the authors found 378 (76%) of these sources to be clusters of galaxies. It was necessary to reanalyze the sources in this sample with a new X-ray source characterization technique to provide more precise values for the X-ray flux and source extent than obtained from the standard processing. This new method, termed growth curve analysis (GCA), has the advantage over previous methods in its ability to be robust, to be easy to model and to integrate into simulations, to provide diagnostic plots for visual inspection, and to make extensive use of the X-ray data. The source parameters obtained assist the source identification and provide more precise X-ray fluxes. This reanalysis is based on data from the more recent second processing of the ROSAT Survey, RASS II. The authors present a catalog of the cluster sources with the X-ray properties obtained as well as a list of the previously flagged extended sources that are found to have a non-cluster counterpart. In their paper, they discuss the process of source identification from the combination of optical and X-ray data. To investigate the overall completeness of the cluster sample as a function of the X-ray flux limit, they extended the search for X-ray cluster sources to the RASS II data for the northern sky region between 9 and 14 hours in right ascension. They included the search for X-ray emission from known galaxy clusters as well as a new investigation of extended X-ray sources. In the course of this search, they found X-ray emission from 85 additional Abell clusters and 56 very probable cluster candidates among the newly found extended sources. A comparison of the X-ray cluster number counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX) Cluster Survey results leads to an estimate of the completeness of the NORAS sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s^-1 cm^-2. The estimated completeness achieved by adding the supplementary sample in the study area amounts to about 82% in comparison to REFLEX. The low completeness introduces an uncertainty in the use of the sample for cosmological statistical studies that will be cured with the completion of the continuing Northern ROSAT All-Sky (NORAS) Cluster Survey project.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/noras#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/noras</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=noras&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/noras.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>NORASGalClus [2]</TD>
            <TD>Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog</TD>
            <TD>In the construction of an X-ray-selected sample of galaxy clusters for cosmological studies, the authors have assembled a sample of 495 X-ray sources which were found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region with declination &gt;=0 degrees and Galactic latitude |b| &gt;= 20 degrees, and comprises sources with a Position Sensitive Proportional Counter (PSPC) count rate &gt;= 0.06 counts/s and a source extent likelihood of L &gt;= 7. In an optical follow-up identification program, the authors found 378 (76%) of these sources to be clusters of galaxies. It was necessary to reanalyze the sources in this sample with a new X-ray source characterization technique to provide more precise values for the X-ray flux and source extent than obtained from the standard processing. This new method, termed growth curve analysis (GCA), has the advantage over previous methods in its ability to be robust, to be easy to model and to integrate into simulations, to provide diagnostic plots for visual inspection, and to make extensive use of the X-ray data. The source parameters obtained assist the source identification and provide more precise X-ray fluxes. This reanalysis is based on data from the more recent second processing of the ROSAT Survey, RASS II. The authors present a catalog of the cluster sources with the X-ray properties obtained as well as a list of the previously flagged extended sources that are found to have a non-cluster counterpart. In their paper, they discuss the process of source identification from the combination of optical and X-ray data. To investigate the overall completeness of the cluster sample as a function of the X-ray flux limit, they extended the search for X-ray cluster sources to the RASS II data for the northern sky region between 9 and 14 hours in right ascension. They included the search for X-ray emission from known galaxy clusters as well as a new investigation of extended X-ray sources. In the course of this search, they found X-ray emission from 85 additional Abell clusters and 56 very probable cluster candidates among the newly found extended sources. A comparison of the X-ray cluster number counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX) Cluster Survey results leads to an estimate of the completeness of the NORAS sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s^-1 cm^-2. The estimated completeness achieved by adding the supplementary sample in the study area amounts to about 82% in comparison to REFLEX. The low completeness introduces an uncertainty in the use of the sample for cosmological statistical studies that will be cured with the completion of the continuing Northern ROSAT All-Sky (NORAS) Cluster Survey project.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/noras#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/noras</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=noras&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/noras.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>NORASGalClus [3]</TD>
            <TD>Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog</TD>
            <TD>In the construction of an X-ray-selected sample of galaxy clusters for cosmological studies, the authors have assembled a sample of 495 X-ray sources which were found to show extended X-ray emission in the first processing of the ROSAT All-Sky Survey (RASS I), the Northern ROSAT All-Sky (NORAS) Galaxy Cluster Survey Catalog. The sample covers the celestial region with declination &gt;=0 degrees and Galactic latitude |b| &gt;= 20 degrees, and comprises sources with a Position Sensitive Proportional Counter (PSPC) count rate &gt;= 0.06 counts/s and a source extent likelihood of L &gt;= 7. In an optical follow-up identification program, the authors found 378 (76%) of these sources to be clusters of galaxies. It was necessary to reanalyze the sources in this sample with a new X-ray source characterization technique to provide more precise values for the X-ray flux and source extent than obtained from the standard processing. This new method, termed growth curve analysis (GCA), has the advantage over previous methods in its ability to be robust, to be easy to model and to integrate into simulations, to provide diagnostic plots for visual inspection, and to make extensive use of the X-ray data. The source parameters obtained assist the source identification and provide more precise X-ray fluxes. This reanalysis is based on data from the more recent second processing of the ROSAT Survey, RASS II. The authors present a catalog of the cluster sources with the X-ray properties obtained as well as a list of the previously flagged extended sources that are found to have a non-cluster counterpart. In their paper, they discuss the process of source identification from the combination of optical and X-ray data. To investigate the overall completeness of the cluster sample as a function of the X-ray flux limit, they extended the search for X-ray cluster sources to the RASS II data for the northern sky region between 9 and 14 hours in right ascension. They included the search for X-ray emission from known galaxy clusters as well as a new investigation of extended X-ray sources. In the course of this search, they found X-ray emission from 85 additional Abell clusters and 56 very probable cluster candidates among the newly found extended sources. A comparison of the X-ray cluster number counts of the NORAS sample with the ROSAT-ESO Flux-limited X-ray (REFLEX) Cluster Survey results leads to an estimate of the completeness of the NORAS sample of ROSAT All-Sky Survey (RASS) I extended clusters of about 50% at an X-ray flux of FX(0.1-2.4 keV) = 3 x 10-12 ergs s^-1 cm^-2. The estimated completeness achieved by adding the supplementary sample in the study area amounts to about 82% in comparison to REFLEX. The low completeness introduces an uncertainty in the use of the sample for cosmological statistical studies that will be cured with the completion of the continuing Northern ROSAT All-Sky (NORAS) Cluster Survey project.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/noras#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/noras</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_noras&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/noras.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PGC [1]</TD>
            <TD>Principal Galaxy Catalog (PGC) 2003</TD>
            <TD>The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec&lt;sup&gt;2&lt;/sup&gt;, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, &lt;a href="http://leda.univ-lyon1.fr/"&gt;http://leda.univ-lyon1.fr/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/pgc2003#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pgc2003</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=pgc2003&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/pgc2003.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PGC [2]</TD>
            <TD>Principal Galaxy Catalog (PGC) 2003</TD>
            <TD>The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec&lt;sup&gt;2&lt;/sup&gt;, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, &lt;a href="http://leda.univ-lyon1.fr/"&gt;http://leda.univ-lyon1.fr/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/pgc2003#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pgc2003</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=pgc2003&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/pgc2003.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PGC [3]</TD>
            <TD>Principal Galaxy Catalog (PGC) 2003</TD>
            <TD>The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec&lt;sup&gt;2&lt;/sup&gt;, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, &lt;a href="http://leda.univ-lyon1.fr/"&gt;http://leda.univ-lyon1.fr/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/pgc2003#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pgc2003</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_pgc2003&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/pgc2003.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PGC [1]</TD>
            <TD>Principal Galaxy Catalog (PGC) 2003</TD>
            <TD>The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec&lt;sup&gt;2&lt;/sup&gt;, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, &lt;a href="http://leda.univ-lyon1.fr/"&gt;http://leda.univ-lyon1.fr/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/pgc2003#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pgc2003</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=pgc2003&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/pgc2003.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PGC [2]</TD>
            <TD>Principal Galaxy Catalog (PGC) 2003</TD>
            <TD>The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec&lt;sup&gt;2&lt;/sup&gt;, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, &lt;a href="http://leda.univ-lyon1.fr/"&gt;http://leda.univ-lyon1.fr/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/pgc2003#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pgc2003</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=pgc2003&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/pgc2003.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PGC [3]</TD>
            <TD>Principal Galaxy Catalog (PGC) 2003</TD>
            <TD>The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec&lt;sup&gt;2&lt;/sup&gt;, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, &lt;a href="http://leda.univ-lyon1.fr/"&gt;http://leda.univ-lyon1.fr/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/pgc2003#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pgc2003</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_pgc2003&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/pgc2003.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PGC [1]</TD>
            <TD>Principal Galaxy Catalog (PGC) 2003</TD>
            <TD>The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec&lt;sup&gt;2&lt;/sup&gt;, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, &lt;a href="http://leda.univ-lyon1.fr/"&gt;http://leda.univ-lyon1.fr/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/pgc2003#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pgc2003</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=pgc2003&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/pgc2003.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PGC [2]</TD>
            <TD>Principal Galaxy Catalog (PGC) 2003</TD>
            <TD>The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec&lt;sup&gt;2&lt;/sup&gt;, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, &lt;a href="http://leda.univ-lyon1.fr/"&gt;http://leda.univ-lyon1.fr/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/pgc2003#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pgc2003</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=pgc2003&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/pgc2003.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PGC [3]</TD>
            <TD>Principal Galaxy Catalog (PGC) 2003</TD>
            <TD>The Principal Galaxy Catalog, 2003 Version (PGC2003) is a new catalog of principal galaxies. It constitutes the framework of the HYPERLEDA database that supersedes the LEDA one, with more data and more capabilities. The catalog is still restricted to confirmed galaxies, i.e. about one million galaxies, brighter than a B-magnitude of ~18. In order to provide the best possible identification for each galaxy, the authors give accurate coordinates (typical accuracy of better than 2 arcseconds), diameters, axis ratios and position angles. Diameters and axis ratios have been homogenized to the RC2 system at the limiting surface brightness of 25 B-mag/arcsec&lt;sup&gt;2&lt;/sup&gt;, using a new method (EPIDEMIC). In order to provide the best designation for each galaxy, the authors have collected names from 50 catalogs. The compatibility of the spelling has been tested against NED and SIMBAD, and, as far as possible a spelling is used that is compatible with both. For some cases, where no consensus exists between NED, SIMBAD and LEDA, the authors have proposed some changes that could make the spelling of names fully compatible. The full catalog is distributed through the CDS and can be extracted from HYPERLEDA, &lt;a href="http://leda.univ-lyon1.fr/"&gt;http://leda.univ-lyon1.fr/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/pgc2003#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/pgc2003</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_pgc2003&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/pgc2003.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RC3 [1]</TD>
            <TD>Third Reference Catalog of Bright Galaxies</TD>
            <TD>This table contains the machine-readable version of the Third Reference Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs, H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by Springer-Verlag in 1991, and including some corrections and additions made by Corwin et al. (1994, AJ, 108, 2128). Only brief parameter descriptions are given in this help file. Detailed information about, for example, how certain quantities were derived, or exactly what a given code means, can be found in the printed version of RC3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/rc3#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rc3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rc3&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/rc3.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RC3 [2]</TD>
            <TD>Third Reference Catalog of Bright Galaxies</TD>
            <TD>This table contains the machine-readable version of the Third Reference Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs, H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by Springer-Verlag in 1991, and including some corrections and additions made by Corwin et al. (1994, AJ, 108, 2128). Only brief parameter descriptions are given in this help file. Detailed information about, for example, how certain quantities were derived, or exactly what a given code means, can be found in the printed version of RC3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/rc3#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rc3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rc3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/rc3.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RC3 [3]</TD>
            <TD>Third Reference Catalog of Bright Galaxies</TD>
            <TD>This table contains the machine-readable version of the Third Reference Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs, H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by Springer-Verlag in 1991, and including some corrections and additions made by Corwin et al. (1994, AJ, 108, 2128). Only brief parameter descriptions are given in this help file. Detailed information about, for example, how certain quantities were derived, or exactly what a given code means, can be found in the printed version of RC3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/rc3#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rc3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rc3&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/rc3.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RC3 [1]</TD>
            <TD>Third Reference Catalog of Bright Galaxies</TD>
            <TD>This table contains the machine-readable version of the Third Reference Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs, H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by Springer-Verlag in 1991, and including some corrections and additions made by Corwin et al. (1994, AJ, 108, 2128). Only brief parameter descriptions are given in this help file. Detailed information about, for example, how certain quantities were derived, or exactly what a given code means, can be found in the printed version of RC3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/rc3#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rc3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rc3&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/rc3.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RC3 [2]</TD>
            <TD>Third Reference Catalog of Bright Galaxies</TD>
            <TD>This table contains the machine-readable version of the Third Reference Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs, H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by Springer-Verlag in 1991, and including some corrections and additions made by Corwin et al. (1994, AJ, 108, 2128). Only brief parameter descriptions are given in this help file. Detailed information about, for example, how certain quantities were derived, or exactly what a given code means, can be found in the printed version of RC3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/rc3#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rc3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rc3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/rc3.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RC3 [3]</TD>
            <TD>Third Reference Catalog of Bright Galaxies</TD>
            <TD>This table contains the machine-readable version of the Third Reference Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs, H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by Springer-Verlag in 1991, and including some corrections and additions made by Corwin et al. (1994, AJ, 108, 2128). Only brief parameter descriptions are given in this help file. Detailed information about, for example, how certain quantities were derived, or exactly what a given code means, can be found in the printed version of RC3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/rc3#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rc3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rc3&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/rc3.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>RC3 [1]</TD>
            <TD>Third Reference Catalog of Bright Galaxies</TD>
            <TD>This table contains the machine-readable version of the Third Reference Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs, H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by Springer-Verlag in 1991, and including some corrections and additions made by Corwin et al. (1994, AJ, 108, 2128). Only brief parameter descriptions are given in this help file. Detailed information about, for example, how certain quantities were derived, or exactly what a given code means, can be found in the printed version of RC3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/rc3#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rc3</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=rc3&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/rc3.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>RC3 [2]</TD>
            <TD>Third Reference Catalog of Bright Galaxies</TD>
            <TD>This table contains the machine-readable version of the Third Reference Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs, H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by Springer-Verlag in 1991, and including some corrections and additions made by Corwin et al. (1994, AJ, 108, 2128). Only brief parameter descriptions are given in this help file. Detailed information about, for example, how certain quantities were derived, or exactly what a given code means, can be found in the printed version of RC3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/rc3#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rc3</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=rc3&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/rc3.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>RC3 [3]</TD>
            <TD>Third Reference Catalog of Bright Galaxies</TD>
            <TD>This table contains the machine-readable version of the Third Reference Catalogue of Bright Galaxies (RC3) by G. de Vaucouleurs, A. de Vacouleurs, H.G. Corwin, R.J. Buta, P. Fouque, and G. Paturel, originally published by Springer-Verlag in 1991, and including some corrections and additions made by Corwin et al. (1994, AJ, 108, 2128). Only brief parameter descriptions are given in this help file. Detailed information about, for example, how certain quantities were derived, or exactly what a given code means, can be found in the printed version of RC3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/rc3#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/rc3</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_rc3&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/rc3.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSSWHLGC [1]</TD>
            <TD>Sloan Digital Sky Survey DR6 Galaxy Clusters Catalog</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z &lt;= 0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify 39,716 clusters in the redshift range 0.05 &lt; z &lt; 0.6 with more than eight luminous (M_r &lt;= -21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200 &gt; 2 x 10^14 M_sun, where M_200 is the total mass within the radius in which the mean mass density is 200 times the critical cosmic mass density) clusters of z &lt;= 0.42. The false detection rate is ~5%. The authors obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of the clusters. Cluster mass is related to the richness and summed luminosity with M_200 ~ R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition, 790 new candidate X-ray clusters are found by cross-identification of these clusters with the source list of the ROSAT X-ray All-Sky Survey.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sdsswhlgc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sdsswhlgc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sdsswhlgc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sdsswhlgc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSSWHLGC [2]</TD>
            <TD>Sloan Digital Sky Survey DR6 Galaxy Clusters Catalog</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z &lt;= 0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify 39,716 clusters in the redshift range 0.05 &lt; z &lt; 0.6 with more than eight luminous (M_r &lt;= -21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200 &gt; 2 x 10^14 M_sun, where M_200 is the total mass within the radius in which the mean mass density is 200 times the critical cosmic mass density) clusters of z &lt;= 0.42. The false detection rate is ~5%. The authors obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of the clusters. Cluster mass is related to the richness and summed luminosity with M_200 ~ R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition, 790 new candidate X-ray clusters are found by cross-identification of these clusters with the source list of the ROSAT X-ray All-Sky Survey.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sdsswhlgc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sdsswhlgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sdsswhlgc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sdsswhlgc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SDSSWHLGC [3]</TD>
            <TD>Sloan Digital Sky Survey DR6 Galaxy Clusters Catalog</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z &lt;= 0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify 39,716 clusters in the redshift range 0.05 &lt; z &lt; 0.6 with more than eight luminous (M_r &lt;= -21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200 &gt; 2 x 10^14 M_sun, where M_200 is the total mass within the radius in which the mean mass density is 200 times the critical cosmic mass density) clusters of z &lt;= 0.42. The false detection rate is ~5%. The authors obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of the clusters. Cluster mass is related to the richness and summed luminosity with M_200 ~ R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition, 790 new candidate X-ray clusters are found by cross-identification of these clusters with the source list of the ROSAT X-ray All-Sky Survey.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sdsswhlgc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sdsswhlgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sdsswhlgc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sdsswhlgc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSSWHLGC [1]</TD>
            <TD>Sloan Digital Sky Survey DR6 Galaxy Clusters Catalog</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z &lt;= 0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify 39,716 clusters in the redshift range 0.05 &lt; z &lt; 0.6 with more than eight luminous (M_r &lt;= -21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200 &gt; 2 x 10^14 M_sun, where M_200 is the total mass within the radius in which the mean mass density is 200 times the critical cosmic mass density) clusters of z &lt;= 0.42. The false detection rate is ~5%. The authors obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of the clusters. Cluster mass is related to the richness and summed luminosity with M_200 ~ R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition, 790 new candidate X-ray clusters are found by cross-identification of these clusters with the source list of the ROSAT X-ray All-Sky Survey.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sdsswhlgc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sdsswhlgc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sdsswhlgc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sdsswhlgc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSSWHLGC [2]</TD>
            <TD>Sloan Digital Sky Survey DR6 Galaxy Clusters Catalog</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z &lt;= 0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify 39,716 clusters in the redshift range 0.05 &lt; z &lt; 0.6 with more than eight luminous (M_r &lt;= -21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200 &gt; 2 x 10^14 M_sun, where M_200 is the total mass within the radius in which the mean mass density is 200 times the critical cosmic mass density) clusters of z &lt;= 0.42. The false detection rate is ~5%. The authors obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of the clusters. Cluster mass is related to the richness and summed luminosity with M_200 ~ R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition, 790 new candidate X-ray clusters are found by cross-identification of these clusters with the source list of the ROSAT X-ray All-Sky Survey.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sdsswhlgc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sdsswhlgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sdsswhlgc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sdsswhlgc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SDSSWHLGC [3]</TD>
            <TD>Sloan Digital Sky Survey DR6 Galaxy Clusters Catalog</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z &lt;= 0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify 39,716 clusters in the redshift range 0.05 &lt; z &lt; 0.6 with more than eight luminous (M_r &lt;= -21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200 &gt; 2 x 10^14 M_sun, where M_200 is the total mass within the radius in which the mean mass density is 200 times the critical cosmic mass density) clusters of z &lt;= 0.42. The false detection rate is ~5%. The authors obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of the clusters. Cluster mass is related to the richness and summed luminosity with M_200 ~ R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition, 790 new candidate X-ray clusters are found by cross-identification of these clusters with the source list of the ROSAT X-ray All-Sky Survey.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sdsswhlgc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sdsswhlgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sdsswhlgc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sdsswhlgc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SDSSWHLGC [1]</TD>
            <TD>Sloan Digital Sky Survey DR6 Galaxy Clusters Catalog</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z &lt;= 0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify 39,716 clusters in the redshift range 0.05 &lt; z &lt; 0.6 with more than eight luminous (M_r &lt;= -21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200 &gt; 2 x 10^14 M_sun, where M_200 is the total mass within the radius in which the mean mass density is 200 times the critical cosmic mass density) clusters of z &lt;= 0.42. The false detection rate is ~5%. The authors obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of the clusters. Cluster mass is related to the richness and summed luminosity with M_200 ~ R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition, 790 new candidate X-ray clusters are found by cross-identification of these clusters with the source list of the ROSAT X-ray All-Sky Survey.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sdsswhlgc#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sdsswhlgc</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sdsswhlgc&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sdsswhlgc.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SDSSWHLGC [2]</TD>
            <TD>Sloan Digital Sky Survey DR6 Galaxy Clusters Catalog</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z &lt;= 0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify 39,716 clusters in the redshift range 0.05 &lt; z &lt; 0.6 with more than eight luminous (M_r &lt;= -21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200 &gt; 2 x 10^14 M_sun, where M_200 is the total mass within the radius in which the mean mass density is 200 times the critical cosmic mass density) clusters of z &lt;= 0.42. The false detection rate is ~5%. The authors obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of the clusters. Cluster mass is related to the richness and summed luminosity with M_200 ~ R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition, 790 new candidate X-ray clusters are found by cross-identification of these clusters with the source list of the ROSAT X-ray All-Sky Survey.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sdsswhlgc#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sdsswhlgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sdsswhlgc&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sdsswhlgc.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SDSSWHLGC [3]</TD>
            <TD>Sloan Digital Sky Survey DR6 Galaxy Clusters Catalog</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z &lt;= 0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), the authors identify 39,716 clusters in the redshift range 0.05 &lt; z &lt; 0.6 with more than eight luminous (M_r &lt;= -21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200 &gt; 2 x 10^14 M_sun, where M_200 is the total mass within the radius in which the mean mass density is 200 times the critical cosmic mass density) clusters of z &lt;= 0.42. The false detection rate is ~5%. The authors obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of the clusters. Cluster mass is related to the richness and summed luminosity with M_200 ~ R^(1.90+/-0.04)^ and M_200 ~ L_r^(1.64+/-0.03)^, respectively. In addition, 790 new candidate X-ray clusters are found by cross-identification of these clusters with the source list of the ROSAT X-ray All-Sky Survey.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/sdsswhlgc#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Cluster of Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sdsswhlgc</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sdsswhlgc&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/sdsswhlgc.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Shk.(Gal.) [1]</TD>
            <TD>Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shkgalaxy#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shkgalaxy</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=shkgalaxy&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shkgalaxy.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Shk.(Gal.) [2]</TD>
            <TD>Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shkgalaxy#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shkgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=shkgalaxy&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shkgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Shk.(Gal.) [3]</TD>
            <TD>Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shkgalaxy#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shkgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_shkgalaxy&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shkgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Shk.(Gal.) [1]</TD>
            <TD>Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shkgalaxy#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shkgalaxy</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=shkgalaxy&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shkgalaxy.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Shk.(Gal.) [2]</TD>
            <TD>Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shkgalaxy#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shkgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=shkgalaxy&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shkgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Shk.(Gal.) [3]</TD>
            <TD>Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shkgalaxy#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shkgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_shkgalaxy&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shkgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>Shk.(Gal.) [1]</TD>
            <TD>Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shkgalaxy#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shkgalaxy</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=shkgalaxy&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shkgalaxy.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>Shk.(Gal.) [2]</TD>
            <TD>Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shkgalaxy#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shkgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=shkgalaxy&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shkgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>Shk.(Gal.) [3]</TD>
            <TD>Shakhabazian (Shk) Compact Groups of Galaxies: Individual Galaxies Data</TD>
            <TD>The largest survey of compact galaxy groups was published by Shakhbazian et al. (the CDS catalog VII/89, implemented by the HEASARC as the SHK database table). This present catalog provides accurate positions of the individual galaxies in the groups; photometric properties of the Southern sky (delta not greater than +2.5 degrees) are evaluated on the basis of the COSMOS/UKST catalog of the Southern sky. This catalog contains 373 groups; this number differs from the number in Shakhbazian's list (377 groups) by the following: (i) there are no data for groups 001 (already published by other authors), 206 and 241 (could not be re-identified), 252 (this is identical with 214), 301 and 353 (could not be re-identified); (ii) Group 328 was published twice (in North and South); and (iii) Group 340 was divided in two parts (340 and 340a), according to Bettoni and Fasano ([BF95]=1995AJ....109...32B). This HEASARC version of the catalog contains a total of 3435 individual galaxies identified as members of the compact groups, 2574 from the northern part of this survey (taken from the ADS Catalog VII/196 file north.dat), and 861 from the southern part of this survey (extracted from the 10746 entries in the ADS Catalog VII/196 file south.dat by including only entries corresponding to bona fide group members).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/shkgalaxy#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/shkgalaxy</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_shkgalaxy&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/shkgalaxy.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VLACDFSCAT [1]</TD>
            <TD>VLA Survey of Chandra Deep Field South</TD>
            <TD>This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacdfscat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacdfscat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=vlacdfscat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacdfscat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VLACDFSCAT [2]</TD>
            <TD>VLA Survey of Chandra Deep Field South</TD>
            <TD>This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacdfscat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacdfscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=vlacdfscat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacdfscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VLACDFSCAT [3]</TD>
            <TD>VLA Survey of Chandra Deep Field South</TD>
            <TD>This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacdfscat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacdfscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_vlacdfscat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacdfscat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VLACDFSCAT [1]</TD>
            <TD>VLA Survey of Chandra Deep Field South</TD>
            <TD>This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacdfscat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacdfscat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=vlacdfscat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacdfscat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VLACDFSCAT [2]</TD>
            <TD>VLA Survey of Chandra Deep Field South</TD>
            <TD>This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacdfscat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacdfscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=vlacdfscat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacdfscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VLACDFSCAT [3]</TD>
            <TD>VLA Survey of Chandra Deep Field South</TD>
            <TD>This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacdfscat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacdfscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_vlacdfscat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacdfscat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VLACDFSCAT [1]</TD>
            <TD>VLA Survey of Chandra Deep Field South</TD>
            <TD>This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacdfscat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacdfscat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=vlacdfscat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacdfscat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VLACDFSCAT [2]</TD>
            <TD>VLA Survey of Chandra Deep Field South</TD>
            <TD>This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacdfscat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacdfscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=vlacdfscat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacdfscat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VLACDFSCAT [3]</TD>
            <TD>VLA Survey of Chandra Deep Field South</TD>
            <TD>This table contains some of the results from 20 and 6 cm VLA deep observations of the Chandra Deep Field-South (CDF-S), including the Extended CDF-S (E-CDF-S). In the reference paper, the authors discuss the radio properties of 266 cataloged radio sources, of which 198 are above a 20-cm completeness level reaching down to 43 microJanskies (uJy) at the center of the field. Survey observations made at 6 cm over a more limited region cover the original CDF-S to a comparable level of sensitivity as the 20-cm observations. Of 266 cataloged radio sources, 52 have X-ray counterparts in the CDF-S and a further 37 have counterparts in the E-CDF-S area not covered by the 1 Ms exposure. Using a wide range of material, the authors have found optical or infrared counterparts for 254 radio sources, of which 186 have either spectroscopic or photometric redshifts. Three radio sources have no apparent counterpart at any other wavelength. Measurements of the 20-cm radio flux density at the position of each CDF-S X-ray source detected a further 30 radio sources (not included in this table) above a conservative 3-sigma detection limit. X-ray and submillimeter observations have been traditionally used as a measure of AGN and star formation activity, respectively. These new observations probe the faint end of both the star formation and radio galaxy/AGN population, as well as the connection between the formation and evolution of stars and SMBHs. Both of the corresponding gravitational and nuclear fusion-driven energy sources can lead to radio synchrotron emission. AGN and radio galaxies dominate at high flux densities. Although emission from star formation becomes more prominent at the microjansky levels reached by deep radio surveys, even for the weakest sources, an apparent significant contribution from low-luminosity AGN as well as from star formation is still found. Notice that are 319 entries in this table corresponding to the 266 catalogued radio sources, due to the fact that some of these sources have multiple components. In such cases, the composite source as well as each of its components are listed as separate entries, e.g., source 7 which has 3 components (A, B and C) has 4 entries in this table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacdfscat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacdfscat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_vlacdfscat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacdfscat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VLACOSMOS [1]</TD>
            <TD>VLA-COSMOS Large Project 1.4-GHz Source Catalog</TD>
            <TD>The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N &gt;= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and &lt; 55 mas, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacosmos#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacosmos</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=vlacosmos&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacosmos.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VLACOSMOS [2]</TD>
            <TD>VLA-COSMOS Large Project 1.4-GHz Source Catalog</TD>
            <TD>The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N &gt;= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and &lt; 55 mas, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacosmos#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=vlacosmos&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacosmos.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VLACOSMOS [3]</TD>
            <TD>VLA-COSMOS Large Project 1.4-GHz Source Catalog</TD>
            <TD>The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N &gt;= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and &lt; 55 mas, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacosmos#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_vlacosmos&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacosmos.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VLACOSMOS [1]</TD>
            <TD>VLA-COSMOS Large Project 1.4-GHz Source Catalog</TD>
            <TD>The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N &gt;= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and &lt; 55 mas, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacosmos#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacosmos</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=vlacosmos&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacosmos.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VLACOSMOS [2]</TD>
            <TD>VLA-COSMOS Large Project 1.4-GHz Source Catalog</TD>
            <TD>The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N &gt;= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and &lt; 55 mas, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacosmos#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=vlacosmos&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacosmos.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VLACOSMOS [3]</TD>
            <TD>VLA-COSMOS Large Project 1.4-GHz Source Catalog</TD>
            <TD>The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N &gt;= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and &lt; 55 mas, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacosmos#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_vlacosmos&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacosmos.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VLACOSMOS [1]</TD>
            <TD>VLA-COSMOS Large Project 1.4-GHz Source Catalog</TD>
            <TD>The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N &gt;= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and &lt; 55 mas, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacosmos#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacosmos</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=vlacosmos&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacosmos.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VLACOSMOS [2]</TD>
            <TD>VLA-COSMOS Large Project 1.4-GHz Source Catalog</TD>
            <TD>The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N &gt;= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and &lt; 55 mas, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacosmos#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=vlacosmos&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacosmos.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VLACOSMOS [3]</TD>
            <TD>VLA-COSMOS Large Project 1.4-GHz Source Catalog</TD>
            <TD>The international COSMOS (Cosmic Evolution) survey (Scoville et al. 2007, ApJS, 172, 1) is a panchromatic imaging and spectroscopic survey of a 1.4 degree by 1.4 degree field designed to probe galaxy and SMBH (supermassive black hole) evolution as a function of cosmic environment. One major aspect of the COSMOS survey is the Hubble Space Telescope (HST) Treasury Project (Scoville et al. 2007, ApJS, 172, 38), entailing the largest ever allocation of HST telescope time. The equatorial location of the COSMOS field offers the critical advantage of allowing major observatories from both hemispheres to join forces in this endeavor. State-of-the-art imaging data at all wavelengths (X-ray to centimeter, plus large optical spectroscopic campaigns using the VLT VIMOS and the Magellan IMACS instruments (Lilly et al. 2007; Impey et al. 2007; Trump et al. 2007) have been or are currently being obtained for the COSMOS field. These make the COSMOS field an excellent resource for observational cosmology and galaxy evolution in the important redshift range z ~ 0.5 - 3, a time span covering ~ 75% of the lifetime of the universe. The VLA-COSMOS Large Project produced a catalog of 3643 radio sources found in the 2 square degrees COSMOS field at 1.4 GHz with a signal-to-noise threshold S/N &gt;= 4.5. The observations in the VLA A and C configurations resulted in a resolution of 1.5" by 1.4" and a mean rms noise of ~ 10.5 microJy (uJy) beam^-1 in the central 1 deg^2, and of 15 uJy in the 2 deg^2 field. Eighty radio sources are clearly extended consisting of multiple components, and most of them appear to be double-lobed radio galaxies. The astrometry of the catalog has been thoroughly tested, and the uncertainty in the relative and absolute astrometry are 130 and &lt; 55 mas, respectively.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/vlacosmos#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/vlacosmos</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_vlacosmos&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/vlacosmos.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CFAZ [1]</TD>
            <TD>CfA Redshift Catalog (June 1995 Version)</TD>
            <TD>The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/zcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/zcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=zcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/zcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CFAZ [2]</TD>
            <TD>CfA Redshift Catalog (June 1995 Version)</TD>
            <TD>The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/zcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/zcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=zcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/zcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CFAZ [3]</TD>
            <TD>CfA Redshift Catalog (June 1995 Version)</TD>
            <TD>The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/zcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/zcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_zcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/zcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CFAZ [1]</TD>
            <TD>CfA Redshift Catalog (June 1995 Version)</TD>
            <TD>The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/zcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/zcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=zcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/zcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CFAZ [2]</TD>
            <TD>CfA Redshift Catalog (June 1995 Version)</TD>
            <TD>The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/zcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/zcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=zcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/zcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CFAZ [3]</TD>
            <TD>CfA Redshift Catalog (June 1995 Version)</TD>
            <TD>The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/zcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/zcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_zcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/zcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CFAZ [1]</TD>
            <TD>CfA Redshift Catalog (June 1995 Version)</TD>
            <TD>The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/zcat#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/zcat</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=zcat&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/zcat.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CFAZ [2]</TD>
            <TD>CfA Redshift Catalog (June 1995 Version)</TD>
            <TD>The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/zcat#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/zcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=zcat&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/zcat.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CFAZ [3]</TD>
            <TD>CfA Redshift Catalog (June 1995 Version)</TD>
            <TD>The ZCAT database contains the CfA Redshift Catalog, which incorporates much of the latest velocity data from the Whipple Observatory and other sources, as well as velocities from earlier compilations such as the "Second Reference Catalog" of de Vaucouleurs, de Vaucouleurs, and Corwin; the "Index of Galaxy Spectra" of Gisler and Friel; and the "Catalog of Radial Velocities of Galaxies" of Palumbo, Tanzella-Nitti, and Vettolani. It includes BT magnitudes, some UGC numbers, and increased "accuracy" in the velocity source information. The data presented here have primarily been assembled for the purpose of studying the large scale structure of the universe, and, as such, are nearly complete in redshift information, but are not necessarily complete in such categories as diameter, magnitude, and cross-references to other catalogues.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/zcat#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Galaxy#Redshift#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/zcat</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_zcat&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galaxy-catalog/zcat.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>AAVSOVSX [1]</TD>
            <TD>AAVSO International Variable Star Index</TD>
            <TD>This table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; &lt;a href="http://www.aavso.org/vsx"&gt;http://www.aavso.org/vsx&lt;/a&gt;). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/aavsovsx#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/aavsovsx</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=aavsovsx&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/aavsovsx.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>AAVSOVSX [2]</TD>
            <TD>AAVSO International Variable Star Index</TD>
            <TD>This table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; &lt;a href="http://www.aavso.org/vsx"&gt;http://www.aavso.org/vsx&lt;/a&gt;). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/aavsovsx#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/aavsovsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=aavsovsx&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/aavsovsx.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>AAVSOVSX [3]</TD>
            <TD>AAVSO International Variable Star Index</TD>
            <TD>This table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; &lt;a href="http://www.aavso.org/vsx"&gt;http://www.aavso.org/vsx&lt;/a&gt;). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/aavsovsx#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/aavsovsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_aavsovsx&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/aavsovsx.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>AAVSOVSX [1]</TD>
            <TD>AAVSO International Variable Star Index</TD>
            <TD>This table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; &lt;a href="http://www.aavso.org/vsx"&gt;http://www.aavso.org/vsx&lt;/a&gt;). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/aavsovsx#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/aavsovsx</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=aavsovsx&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/aavsovsx.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>AAVSOVSX [2]</TD>
            <TD>AAVSO International Variable Star Index</TD>
            <TD>This table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; &lt;a href="http://www.aavso.org/vsx"&gt;http://www.aavso.org/vsx&lt;/a&gt;). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/aavsovsx#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/aavsovsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=aavsovsx&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/aavsovsx.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>AAVSOVSX [3]</TD>
            <TD>AAVSO International Variable Star Index</TD>
            <TD>This table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; &lt;a href="http://www.aavso.org/vsx"&gt;http://www.aavso.org/vsx&lt;/a&gt;). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/aavsovsx#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/aavsovsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_aavsovsx&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/aavsovsx.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>AAVSOVSX [1]</TD>
            <TD>AAVSO International Variable Star Index</TD>
            <TD>This table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; &lt;a href="http://www.aavso.org/vsx"&gt;http://www.aavso.org/vsx&lt;/a&gt;). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/aavsovsx#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/aavsovsx</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=aavsovsx&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/aavsovsx.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>AAVSOVSX [2]</TD>
            <TD>AAVSO International Variable Star Index</TD>
            <TD>This table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; &lt;a href="http://www.aavso.org/vsx"&gt;http://www.aavso.org/vsx&lt;/a&gt;). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/aavsovsx#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/aavsovsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=aavsovsx&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/aavsovsx.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>AAVSOVSX [3]</TD>
            <TD>AAVSO International Variable Star Index</TD>
            <TD>This table contains Galactic stars known or suspected to be variable. It lists all stars that have an entry in the American Association of Variable Star Observers' (AAVSO) International Variable Star Index (VSX; &lt;a href="http://www.aavso.org/vsx"&gt;http://www.aavso.org/vsx&lt;/a&gt;). The database consisted initially of the General Catalogue of Variable Stars (GCVS) and the New Catalogue of Suspected Variables (NSV) and was then supplemented with a large number of variable star catalogues, as well as individual variable star discoveries or variables found in the literature. Effort has also been invested to update the entries with the latest information regarding position, type and period and to remove duplicates. The VSX database is being continually updated and maintained. For historical reasons some objects outside of the Galaxy have been included.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#</TD>
            <TD>ivo://nasa.heasarc/aavsovsx#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0333333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/aavsovsx</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_aavsovsx&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/star-catalog/aavsovsx.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GALEXLOG [1]</TD>
            <TD>Galaxy Evolution Explorer (GALEX) Observation Log</TD>
            <TD>This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m_AB ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m_AB ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m_AB ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at &lt;a href="http://galex.stsci.edu/"&gt;http://galex.stsci.edu/&lt;/a&gt;. More information about GALEX can be found at http://www.galex.caltech.edu/ and &lt;a href="http://galexgi.gsfc.nasa.gov/"&gt;http://galexgi.gsfc.nasa.gov/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/galexlog#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.6</TD>
            <TD />
            <TD>ivo://nasa.heasarc/galexlog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=galexlog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/galexlog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GALEXLOG [2]</TD>
            <TD>Galaxy Evolution Explorer (GALEX) Observation Log</TD>
            <TD>This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m_AB ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m_AB ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m_AB ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at &lt;a href="http://galex.stsci.edu/"&gt;http://galex.stsci.edu/&lt;/a&gt;. More information about GALEX can be found at http://www.galex.caltech.edu/ and &lt;a href="http://galexgi.gsfc.nasa.gov/"&gt;http://galexgi.gsfc.nasa.gov/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/galexlog#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.6</TD>
            <TD />
            <TD>ivo://nasa.heasarc/galexlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=galexlog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/galexlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GALEXLOG [3]</TD>
            <TD>Galaxy Evolution Explorer (GALEX) Observation Log</TD>
            <TD>This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m_AB ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m_AB ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m_AB ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at &lt;a href="http://galex.stsci.edu/"&gt;http://galex.stsci.edu/&lt;/a&gt;. More information about GALEX can be found at http://www.galex.caltech.edu/ and &lt;a href="http://galexgi.gsfc.nasa.gov/"&gt;http://galexgi.gsfc.nasa.gov/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/galexlog#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.6</TD>
            <TD />
            <TD>ivo://nasa.heasarc/galexlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_galexlog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/galexlog.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GALEXLOG [1]</TD>
            <TD>Galaxy Evolution Explorer (GALEX) Observation Log</TD>
            <TD>This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m_AB ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m_AB ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m_AB ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at &lt;a href="http://galex.stsci.edu/"&gt;http://galex.stsci.edu/&lt;/a&gt;. More information about GALEX can be found at http://www.galex.caltech.edu/ and &lt;a href="http://galexgi.gsfc.nasa.gov/"&gt;http://galexgi.gsfc.nasa.gov/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/galexlog#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.6</TD>
            <TD />
            <TD>ivo://nasa.heasarc/galexlog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=galexlog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/galexlog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GALEXLOG [2]</TD>
            <TD>Galaxy Evolution Explorer (GALEX) Observation Log</TD>
            <TD>This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m_AB ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m_AB ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m_AB ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at &lt;a href="http://galex.stsci.edu/"&gt;http://galex.stsci.edu/&lt;/a&gt;. More information about GALEX can be found at http://www.galex.caltech.edu/ and &lt;a href="http://galexgi.gsfc.nasa.gov/"&gt;http://galexgi.gsfc.nasa.gov/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/galexlog#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.6</TD>
            <TD />
            <TD>ivo://nasa.heasarc/galexlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=galexlog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/galexlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GALEXLOG [3]</TD>
            <TD>Galaxy Evolution Explorer (GALEX) Observation Log</TD>
            <TD>This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m_AB ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m_AB ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m_AB ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at &lt;a href="http://galex.stsci.edu/"&gt;http://galex.stsci.edu/&lt;/a&gt;. More information about GALEX can be found at http://www.galex.caltech.edu/ and &lt;a href="http://galexgi.gsfc.nasa.gov/"&gt;http://galexgi.gsfc.nasa.gov/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/galexlog#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.6</TD>
            <TD />
            <TD>ivo://nasa.heasarc/galexlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_galexlog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/galexlog.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GALEXLOG [1]</TD>
            <TD>Galaxy Evolution Explorer (GALEX) Observation Log</TD>
            <TD>This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m_AB ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m_AB ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m_AB ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at &lt;a href="http://galex.stsci.edu/"&gt;http://galex.stsci.edu/&lt;/a&gt;. More information about GALEX can be found at http://www.galex.caltech.edu/ and &lt;a href="http://galexgi.gsfc.nasa.gov/"&gt;http://galexgi.gsfc.nasa.gov/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/galexlog#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.6</TD>
            <TD />
            <TD>ivo://nasa.heasarc/galexlog</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=galexlog&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/galexlog.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GALEXLOG [2]</TD>
            <TD>Galaxy Evolution Explorer (GALEX) Observation Log</TD>
            <TD>This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m_AB ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m_AB ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m_AB ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at &lt;a href="http://galex.stsci.edu/"&gt;http://galex.stsci.edu/&lt;/a&gt;. More information about GALEX can be found at http://www.galex.caltech.edu/ and &lt;a href="http://galexgi.gsfc.nasa.gov/"&gt;http://galexgi.gsfc.nasa.gov/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/galexlog#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.6</TD>
            <TD />
            <TD>ivo://nasa.heasarc/galexlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=galexlog&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/galexlog.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GALEXLOG [3]</TD>
            <TD>Galaxy Evolution Explorer (GALEX) Observation Log</TD>
            <TD>This table contains the Galaxy Evolution Explorer (GALEX) observation log of the extant and planned observations to be made by this satellite observatory. The Galaxy Evolution Explorer (GALEX) is a NASA Small Explorer Mission launched on April 28, 2003. GALEX has been performing the first Space Ultraviolet sky survey. Five imaging surveys in each of two bands (FUV: 1350-1750 Angstroms and NUV: 1750-2800 Angstroms) range from an all-sky survey (limiting m_AB ~ 20 - 21) to an ultra-deep survey of 4 square degrees (limiting m_AB ~ 26). Three spectroscopic grism surveys (spectral resolution R = 100 - 300) are underway with various depths (m_AB ~ 20 - 25) and sky coverage (100 to 2 square degrees) over the 1350 - 2800 Angstroms spectral range. The instrument includes a 50-cm modified Ritchey-Chretien telescope, a dichroic beam splitter and astigmatism corrector, two large, sealed-tube microchannel plate detectors to simultaneously cover the two bands and the 1.2-degree field of view. A rotating wheel provides either imaging or grism spectroscopy with transmitting optics. The GALEX mission also includes an Associate Investigator program for additional observations and supporting data analysis which supports a wide variety of investigations made possible by the first UV sky survey. The HEASARC provides this table of GALEX observations as an assistance to the high-energy astrophysics community, e.g., to enable cross-correlations of GALEX with X-ray observations. The GALEX data are available via MAST at &lt;a href="http://galex.stsci.edu/"&gt;http://galex.stsci.edu/&lt;/a&gt;. More information about GALEX can be found at http://www.galex.caltech.edu/ and &lt;a href="http://galexgi.gsfc.nasa.gov/"&gt;http://galexgi.gsfc.nasa.gov/&lt;/a&gt;.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#UV#</TD>
            <TD>ivo://nasa.heasarc/galexlog#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.6</TD>
            <TD />
            <TD>ivo://nasa.heasarc/galexlog</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_galexlog&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/galex/galexlog.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M101XMM [1]</TD>
            <TD>M 101 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D&lt;sub&gt;25&lt;/sub&gt; ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D&lt;sub&gt;25&lt;/sub&gt; ellipse of M101.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m101xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m101xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M101XMM [2]</TD>
            <TD>M 101 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D&lt;sub&gt;25&lt;/sub&gt; ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D&lt;sub&gt;25&lt;/sub&gt; ellipse of M101.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m101xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m101xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M101XMM [3]</TD>
            <TD>M 101 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D&lt;sub&gt;25&lt;/sub&gt; ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D&lt;sub&gt;25&lt;/sub&gt; ellipse of M101.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m101xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m101xmm.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M101XMM [1]</TD>
            <TD>M 101 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D&lt;sub&gt;25&lt;/sub&gt; ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D&lt;sub&gt;25&lt;/sub&gt; ellipse of M101.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m101xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m101xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M101XMM [2]</TD>
            <TD>M 101 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D&lt;sub&gt;25&lt;/sub&gt; ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D&lt;sub&gt;25&lt;/sub&gt; ellipse of M101.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m101xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m101xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M101XMM [3]</TD>
            <TD>M 101 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D&lt;sub&gt;25&lt;/sub&gt; ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D&lt;sub&gt;25&lt;/sub&gt; ellipse of M101.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m101xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m101xmm.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>M101XMM [1]</TD>
            <TD>M 101 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D&lt;sub&gt;25&lt;/sub&gt; ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D&lt;sub&gt;25&lt;/sub&gt; ellipse of M101.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=m101xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m101xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>M101XMM [2]</TD>
            <TD>M 101 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D&lt;sub&gt;25&lt;/sub&gt; ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D&lt;sub&gt;25&lt;/sub&gt; ellipse of M101.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=m101xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m101xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>M101XMM [3]</TD>
            <TD>M 101 XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>The authors describe the global X-ray properties of the point source population in the grand-design spiral galaxy M 101, as seen with XMM-Newton. 108 X-ray sources are detected within the D&lt;sub&gt;25&lt;/sub&gt; ellipse (~28.8 arcminutes diameter) of M101, of which ~24 are estimated to be background galaxies. Multiwavelength cross-correlations show that 20 sources are coincident with H II regions and/or supernova remnants (SNRs), seven have identified/candidate background galaxy counterparts, six are coincident with foreground stars and one has a radio counterpart. While the spectral and timing properties of the brightest sources were presented by Jenkins et al. (2004, MNRAS, 349, 404: Paper I), in the present analysis the authors apply an X-ray colour classification scheme to split the entire source population into different types, i.e. X-ray binaries (XRBs), SNRs, absorbed sources, background sources and supersoft sources (SSSs). Approximately 60% of the population can be classified as XRBs, although there is source contamination from background active galactic nuclei (AGN) in this category as they have similar spectral shapes in the X-ray regime. 15 sources have X-ray colours consistent with SNRs, three of which correlate with known SNR/HII radio sources. Another two are promising new candidates for SNRs, one is unidentified, and the remainder are a mixture of foreground stars, bright soft XRBs and AGN candidates. The authors also detect 14 candidate SSSs, with significant detections in the softest X-ray band (0.3 - 1 keV) only. 16 sources display short-term variability during the XMM-Newton observation, twelve of which fall into the XRB category, giving additional evidence of their accreting nature. Using archival Chandra and ROSAT High Resolution Imager data, the authors find that ~40% of the XMM sources show long-term variability over a baseline of up to ~10 yr, and eight sources display potential transient behaviour between observations. Sources with significant flux variations between the XMM and Chandra observations show a mixture of softening and hardening with increasing luminosity. The spectral and timing properties of the sources coincident with M 101 confirm that its X-ray source population is dominated by accreting XRBs. The authors cross-correlated the XMM-Newton source list with previous X-ray observations of M 101. For the Chandra observations detailed in Section 2 of the reference paper, they matched on-axis sources (whose positions are generally accurate to ~1 arcsec) to within the XMM-Newton 3-sigma errors. For off-axis sources, the decreasing Chandra positional accuracy to ~2 arcsec was also taken into account. However, given the large PSF of XMM-Newton (~6 arcsec FWHM), they also checked for any contamination from additional fainter sources detected only by Chandra by searching for sources that lie within 15 arcsec of the XMM-Newton source positions (this corresponds to the on-axis 68% energy cut-out radius used in emldetect). In total, 71 XMM-Newton sources were unambiguously matched to single Chandra sources within the 3-sigma errors, whereas the nuclear source is resolved into two sources by Chandra. These matches are listed in this table, as are additional sources matching to within 15 arcsec. For completeness, both the CXOU designations of Kilgard et al. (2005, ApJS, 159, 214) and equivalent source source numbers from Pence et al. (2001, ApJ, 561, 189) are given. M 101 was observed with XMM-Newton for 42.8 ks on 2002 June 4 (Obs ID 0104260101). The EPIC MOS-1, MOS-2 and PN cameras were operated with medium filters in the 'Prime Full Window' mode, which utilizes the full ~ 30-arcmin field of view of XMM-Newton, covering the entire D&lt;sub&gt;25&lt;/sub&gt; ellipse of M101.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/m101xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/m101xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_m101xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/m101xmm.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ASCAEGCLUS [1]</TD>
            <TD>ASCA Elliptical Galaxies and Galaxy Clusters Catalog</TD>
            <TD>Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L&lt;sub&gt;X&lt;/sub&gt; ~ (kT)&lt;sup&gt;alpha&lt;/sup&gt;, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT &gt; 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R&lt;sub&gt;1500&lt;/sub&gt; (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M&lt;sub&gt;gas&lt;/sub&gt; ~ T&lt;sup&gt;(2.33+/-0.07)&lt;/sup&gt; from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h&lt;sub&gt;50&lt;/sub&gt; km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt; and q&lt;sub&gt;0&lt;/sub&gt; to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: &lt;pre&gt; Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm&lt;sup&gt;2&lt;/sup&gt;) NGC 5018 9.8 x 10&lt;sup&gt;14&lt;/sup&gt; GHO 1322+3114 1.3 x 10&lt;sup&gt;13&lt;/sup&gt; J1888.16CL 5.9 x 10&lt;sup&gt;14&lt;/sup&gt; CL 0317+1521 4.5 x 10&lt;sup&gt;14&lt;/sup&gt; MS 1512.4+3647 1.0 x 10&lt;sup&gt;12&lt;/sup&gt; PRG 38 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; SCGG 205 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; RGH 101 9.1 x 10&lt;sup&gt;14&lt;/sup&gt; 3C 184 8.5 x 10&lt;sup&gt;14&lt;/sup&gt; RX J1756.5+6512 1.6 x 10&lt;sup&gt;13&lt;/sup&gt; 3C 324 5.4 x 10&lt;sup&gt;14&lt;/sup&gt; PDCS 01 2.8 x 10&lt;sup&gt;14&lt;/sup&gt; MS 0147.8-3941 5.0 x 10&lt;sup&gt;14&lt;/sup&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ascaegclus#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ascaegclus</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ascaegclus&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/asca/ascaegclus.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ASCAEGCLUS [2]</TD>
            <TD>ASCA Elliptical Galaxies and Galaxy Clusters Catalog</TD>
            <TD>Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L&lt;sub&gt;X&lt;/sub&gt; ~ (kT)&lt;sup&gt;alpha&lt;/sup&gt;, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT &gt; 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R&lt;sub&gt;1500&lt;/sub&gt; (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M&lt;sub&gt;gas&lt;/sub&gt; ~ T&lt;sup&gt;(2.33+/-0.07)&lt;/sup&gt; from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h&lt;sub&gt;50&lt;/sub&gt; km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt; and q&lt;sub&gt;0&lt;/sub&gt; to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: &lt;pre&gt; Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm&lt;sup&gt;2&lt;/sup&gt;) NGC 5018 9.8 x 10&lt;sup&gt;14&lt;/sup&gt; GHO 1322+3114 1.3 x 10&lt;sup&gt;13&lt;/sup&gt; J1888.16CL 5.9 x 10&lt;sup&gt;14&lt;/sup&gt; CL 0317+1521 4.5 x 10&lt;sup&gt;14&lt;/sup&gt; MS 1512.4+3647 1.0 x 10&lt;sup&gt;12&lt;/sup&gt; PRG 38 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; SCGG 205 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; RGH 101 9.1 x 10&lt;sup&gt;14&lt;/sup&gt; 3C 184 8.5 x 10&lt;sup&gt;14&lt;/sup&gt; RX J1756.5+6512 1.6 x 10&lt;sup&gt;13&lt;/sup&gt; 3C 324 5.4 x 10&lt;sup&gt;14&lt;/sup&gt; PDCS 01 2.8 x 10&lt;sup&gt;14&lt;/sup&gt; MS 0147.8-3941 5.0 x 10&lt;sup&gt;14&lt;/sup&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ascaegclus#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ascaegclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ascaegclus&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/asca/ascaegclus.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ASCAEGCLUS [3]</TD>
            <TD>ASCA Elliptical Galaxies and Galaxy Clusters Catalog</TD>
            <TD>Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L&lt;sub&gt;X&lt;/sub&gt; ~ (kT)&lt;sup&gt;alpha&lt;/sup&gt;, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT &gt; 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R&lt;sub&gt;1500&lt;/sub&gt; (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M&lt;sub&gt;gas&lt;/sub&gt; ~ T&lt;sup&gt;(2.33+/-0.07)&lt;/sup&gt; from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h&lt;sub&gt;50&lt;/sub&gt; km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt; and q&lt;sub&gt;0&lt;/sub&gt; to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: &lt;pre&gt; Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm&lt;sup&gt;2&lt;/sup&gt;) NGC 5018 9.8 x 10&lt;sup&gt;14&lt;/sup&gt; GHO 1322+3114 1.3 x 10&lt;sup&gt;13&lt;/sup&gt; J1888.16CL 5.9 x 10&lt;sup&gt;14&lt;/sup&gt; CL 0317+1521 4.5 x 10&lt;sup&gt;14&lt;/sup&gt; MS 1512.4+3647 1.0 x 10&lt;sup&gt;12&lt;/sup&gt; PRG 38 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; SCGG 205 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; RGH 101 9.1 x 10&lt;sup&gt;14&lt;/sup&gt; 3C 184 8.5 x 10&lt;sup&gt;14&lt;/sup&gt; RX J1756.5+6512 1.6 x 10&lt;sup&gt;13&lt;/sup&gt; 3C 324 5.4 x 10&lt;sup&gt;14&lt;/sup&gt; PDCS 01 2.8 x 10&lt;sup&gt;14&lt;/sup&gt; MS 0147.8-3941 5.0 x 10&lt;sup&gt;14&lt;/sup&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ascaegclus#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ascaegclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ascaegclus&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/asca/ascaegclus.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ASCAEGCLUS [1]</TD>
            <TD>ASCA Elliptical Galaxies and Galaxy Clusters Catalog</TD>
            <TD>Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L&lt;sub&gt;X&lt;/sub&gt; ~ (kT)&lt;sup&gt;alpha&lt;/sup&gt;, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT &gt; 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R&lt;sub&gt;1500&lt;/sub&gt; (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M&lt;sub&gt;gas&lt;/sub&gt; ~ T&lt;sup&gt;(2.33+/-0.07)&lt;/sup&gt; from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h&lt;sub&gt;50&lt;/sub&gt; km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt; and q&lt;sub&gt;0&lt;/sub&gt; to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: &lt;pre&gt; Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm&lt;sup&gt;2&lt;/sup&gt;) NGC 5018 9.8 x 10&lt;sup&gt;14&lt;/sup&gt; GHO 1322+3114 1.3 x 10&lt;sup&gt;13&lt;/sup&gt; J1888.16CL 5.9 x 10&lt;sup&gt;14&lt;/sup&gt; CL 0317+1521 4.5 x 10&lt;sup&gt;14&lt;/sup&gt; MS 1512.4+3647 1.0 x 10&lt;sup&gt;12&lt;/sup&gt; PRG 38 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; SCGG 205 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; RGH 101 9.1 x 10&lt;sup&gt;14&lt;/sup&gt; 3C 184 8.5 x 10&lt;sup&gt;14&lt;/sup&gt; RX J1756.5+6512 1.6 x 10&lt;sup&gt;13&lt;/sup&gt; 3C 324 5.4 x 10&lt;sup&gt;14&lt;/sup&gt; PDCS 01 2.8 x 10&lt;sup&gt;14&lt;/sup&gt; MS 0147.8-3941 5.0 x 10&lt;sup&gt;14&lt;/sup&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ascaegclus#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ascaegclus</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ascaegclus&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/asca/ascaegclus.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ASCAEGCLUS [2]</TD>
            <TD>ASCA Elliptical Galaxies and Galaxy Clusters Catalog</TD>
            <TD>Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L&lt;sub&gt;X&lt;/sub&gt; ~ (kT)&lt;sup&gt;alpha&lt;/sup&gt;, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT &gt; 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R&lt;sub&gt;1500&lt;/sub&gt; (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M&lt;sub&gt;gas&lt;/sub&gt; ~ T&lt;sup&gt;(2.33+/-0.07)&lt;/sup&gt; from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h&lt;sub&gt;50&lt;/sub&gt; km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt; and q&lt;sub&gt;0&lt;/sub&gt; to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: &lt;pre&gt; Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm&lt;sup&gt;2&lt;/sup&gt;) NGC 5018 9.8 x 10&lt;sup&gt;14&lt;/sup&gt; GHO 1322+3114 1.3 x 10&lt;sup&gt;13&lt;/sup&gt; J1888.16CL 5.9 x 10&lt;sup&gt;14&lt;/sup&gt; CL 0317+1521 4.5 x 10&lt;sup&gt;14&lt;/sup&gt; MS 1512.4+3647 1.0 x 10&lt;sup&gt;12&lt;/sup&gt; PRG 38 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; SCGG 205 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; RGH 101 9.1 x 10&lt;sup&gt;14&lt;/sup&gt; 3C 184 8.5 x 10&lt;sup&gt;14&lt;/sup&gt; RX J1756.5+6512 1.6 x 10&lt;sup&gt;13&lt;/sup&gt; 3C 324 5.4 x 10&lt;sup&gt;14&lt;/sup&gt; PDCS 01 2.8 x 10&lt;sup&gt;14&lt;/sup&gt; MS 0147.8-3941 5.0 x 10&lt;sup&gt;14&lt;/sup&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ascaegclus#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ascaegclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ascaegclus&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/asca/ascaegclus.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ASCAEGCLUS [3]</TD>
            <TD>ASCA Elliptical Galaxies and Galaxy Clusters Catalog</TD>
            <TD>Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L&lt;sub&gt;X&lt;/sub&gt; ~ (kT)&lt;sup&gt;alpha&lt;/sup&gt;, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT &gt; 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R&lt;sub&gt;1500&lt;/sub&gt; (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M&lt;sub&gt;gas&lt;/sub&gt; ~ T&lt;sup&gt;(2.33+/-0.07)&lt;/sup&gt; from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h&lt;sub&gt;50&lt;/sub&gt; km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt; and q&lt;sub&gt;0&lt;/sub&gt; to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: &lt;pre&gt; Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm&lt;sup&gt;2&lt;/sup&gt;) NGC 5018 9.8 x 10&lt;sup&gt;14&lt;/sup&gt; GHO 1322+3114 1.3 x 10&lt;sup&gt;13&lt;/sup&gt; J1888.16CL 5.9 x 10&lt;sup&gt;14&lt;/sup&gt; CL 0317+1521 4.5 x 10&lt;sup&gt;14&lt;/sup&gt; MS 1512.4+3647 1.0 x 10&lt;sup&gt;12&lt;/sup&gt; PRG 38 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; SCGG 205 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; RGH 101 9.1 x 10&lt;sup&gt;14&lt;/sup&gt; 3C 184 8.5 x 10&lt;sup&gt;14&lt;/sup&gt; RX J1756.5+6512 1.6 x 10&lt;sup&gt;13&lt;/sup&gt; 3C 324 5.4 x 10&lt;sup&gt;14&lt;/sup&gt; PDCS 01 2.8 x 10&lt;sup&gt;14&lt;/sup&gt; MS 0147.8-3941 5.0 x 10&lt;sup&gt;14&lt;/sup&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ascaegclus#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ascaegclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ascaegclus&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/asca/ascaegclus.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>ASCAEGCLUS [1]</TD>
            <TD>ASCA Elliptical Galaxies and Galaxy Clusters Catalog</TD>
            <TD>Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L&lt;sub&gt;X&lt;/sub&gt; ~ (kT)&lt;sup&gt;alpha&lt;/sup&gt;, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT &gt; 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R&lt;sub&gt;1500&lt;/sub&gt; (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M&lt;sub&gt;gas&lt;/sub&gt; ~ T&lt;sup&gt;(2.33+/-0.07)&lt;/sup&gt; from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h&lt;sub&gt;50&lt;/sub&gt; km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt; and q&lt;sub&gt;0&lt;/sub&gt; to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: &lt;pre&gt; Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm&lt;sup&gt;2&lt;/sup&gt;) NGC 5018 9.8 x 10&lt;sup&gt;14&lt;/sup&gt; GHO 1322+3114 1.3 x 10&lt;sup&gt;13&lt;/sup&gt; J1888.16CL 5.9 x 10&lt;sup&gt;14&lt;/sup&gt; CL 0317+1521 4.5 x 10&lt;sup&gt;14&lt;/sup&gt; MS 1512.4+3647 1.0 x 10&lt;sup&gt;12&lt;/sup&gt; PRG 38 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; SCGG 205 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; RGH 101 9.1 x 10&lt;sup&gt;14&lt;/sup&gt; 3C 184 8.5 x 10&lt;sup&gt;14&lt;/sup&gt; RX J1756.5+6512 1.6 x 10&lt;sup&gt;13&lt;/sup&gt; 3C 324 5.4 x 10&lt;sup&gt;14&lt;/sup&gt; PDCS 01 2.8 x 10&lt;sup&gt;14&lt;/sup&gt; MS 0147.8-3941 5.0 x 10&lt;sup&gt;14&lt;/sup&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ascaegclus#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ascaegclus</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ascaegclus&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/asca/ascaegclus.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>ASCAEGCLUS [2]</TD>
            <TD>ASCA Elliptical Galaxies and Galaxy Clusters Catalog</TD>
            <TD>Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L&lt;sub&gt;X&lt;/sub&gt; ~ (kT)&lt;sup&gt;alpha&lt;/sup&gt;, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT &gt; 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R&lt;sub&gt;1500&lt;/sub&gt; (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M&lt;sub&gt;gas&lt;/sub&gt; ~ T&lt;sup&gt;(2.33+/-0.07)&lt;/sup&gt; from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h&lt;sub&gt;50&lt;/sub&gt; km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt; and q&lt;sub&gt;0&lt;/sub&gt; to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: &lt;pre&gt; Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm&lt;sup&gt;2&lt;/sup&gt;) NGC 5018 9.8 x 10&lt;sup&gt;14&lt;/sup&gt; GHO 1322+3114 1.3 x 10&lt;sup&gt;13&lt;/sup&gt; J1888.16CL 5.9 x 10&lt;sup&gt;14&lt;/sup&gt; CL 0317+1521 4.5 x 10&lt;sup&gt;14&lt;/sup&gt; MS 1512.4+3647 1.0 x 10&lt;sup&gt;12&lt;/sup&gt; PRG 38 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; SCGG 205 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; RGH 101 9.1 x 10&lt;sup&gt;14&lt;/sup&gt; 3C 184 8.5 x 10&lt;sup&gt;14&lt;/sup&gt; RX J1756.5+6512 1.6 x 10&lt;sup&gt;13&lt;/sup&gt; 3C 324 5.4 x 10&lt;sup&gt;14&lt;/sup&gt; PDCS 01 2.8 x 10&lt;sup&gt;14&lt;/sup&gt; MS 0147.8-3941 5.0 x 10&lt;sup&gt;14&lt;/sup&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ascaegclus#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0833333333333333333</TD>
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            <TD>ivo://nasa.heasarc/ascaegclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ascaegclus&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/asca/ascaegclus.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>ASCAEGCLUS [3]</TD>
            <TD>ASCA Elliptical Galaxies and Galaxy Clusters Catalog</TD>
            <TD>Utilizing ASCA archival data of about 300 objects - elliptical galaxies, groups, and clusters of galaxies - the authors performed systematic measurements of the X-ray properties of hot gas in their systems, and compiled them in this study. The steepness (power-law slope) of the luminosity-temperature (L-T) relation, L&lt;sub&gt;X&lt;/sub&gt; ~ (kT)&lt;sup&gt;alpha&lt;/sup&gt;, in the range of kT ~ 1.5 - 15 keV is alpha = 3.17 +/- 0.15, consistent with previous measurements. In the relation, the authors find two breaks at around intracluster medium (ICM) temperatures of 1 keV and 4 keV: alpha = 2.34 +/- 0.29 above 4 keV, 3.74 +/- 0.32 in the 1.5 to 5 keV range, and 4.03 +/- 1.07 below 1.5 keV. Two such breaks are also evident in the temperature and size relation. The steepness in the L-T relation at kT &gt; 4 keV is consistent with the scale-relation derived from the CDM model, indicating that the gravitational effect is dominant in richer clusters, while poorer clusters suffer non-gravity effects. The steep L-T relation below 1 keV is mostly attributed to X-ray faint systems of elliptical galaxies and galaxy groups. The authors find that the ICM mass within the scaling radius R&lt;sub&gt;1500&lt;/sub&gt; (the radius within which the averaged mass density is 1500 times higher than the critical density) follows the relation of M&lt;sub&gt;gas&lt;/sub&gt; ~ T&lt;sup&gt;(2.33+/-0.07)&lt;/sup&gt; from X-ray faint galaxies to rich clusters. Thus, the authors speculate that even such X-ray faint systems contain large-scale hot gas, which is too faint to detect. For this project, the authors utilized all of the ASCA data of elliptical galaxies and clusters of galaxies. Several clusters were observed more than once, and they chose the observation with the longest exposure. The total number of objects that the authors identified as elliptical galaxies and clusters was 313, and these are listed in this table. Some of the objects could not be utilized for deriving various correlations, due to either having an unknown redshift (17 objects), an insignificant detection (13 objects listed below), or contamination of the environmental X-ray emission, such as cluster emission around non-cD elliptical galaxies (10 objects: NGC 4472, NGC 4406, NGC 4374, NGC 1404, NGC 499, NGC 6034, NGC 2865, NGC 4291, CL 2236-04 and RX J1031.6-2607). Thus, the authors analyzed the ASCA data for 292 objects, among which were ~ 50 elliptical galaxies and galaxy groups. In this study, the authors assumed the Hubble constant to be 50 h&lt;sub&gt;50&lt;/sub&gt; km s&lt;sup&gt;-1&lt;/sup&gt; Mpc&lt;sup&gt;-1&lt;/sup&gt; and q&lt;sub&gt;0&lt;/sub&gt; to be 0. Table 1 of the reference paper (reproduced below) lists the 13 clusters for which only 90% confidence level upper limits to the flux in the observer's frame are available: &lt;pre&gt; Name Flux (0.5 - 2 keV) Upper Limit (erg/s/cm&lt;sup&gt;2&lt;/sup&gt;) NGC 5018 9.8 x 10&lt;sup&gt;14&lt;/sup&gt; GHO 1322+3114 1.3 x 10&lt;sup&gt;13&lt;/sup&gt; J1888.16CL 5.9 x 10&lt;sup&gt;14&lt;/sup&gt; CL 0317+1521 4.5 x 10&lt;sup&gt;14&lt;/sup&gt; MS 1512.4+3647 1.0 x 10&lt;sup&gt;12&lt;/sup&gt; PRG 38 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; SCGG 205 6.9 x 10&lt;sup&gt;14&lt;/sup&gt; RGH 101 9.1 x 10&lt;sup&gt;14&lt;/sup&gt; 3C 184 8.5 x 10&lt;sup&gt;14&lt;/sup&gt; RX J1756.5+6512 1.6 x 10&lt;sup&gt;13&lt;/sup&gt; 3C 324 5.4 x 10&lt;sup&gt;14&lt;/sup&gt; PDCS 01 2.8 x 10&lt;sup&gt;14&lt;/sup&gt; MS 0147.8-3941 5.0 x 10&lt;sup&gt;14&lt;/sup&gt; &lt;/pre&gt;</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ascaegclus#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/ascaegclus</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ascaegclus&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/asca/ascaegclus.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CYGOB2XMM [1]</TD>
            <TD>Cygnus OB2 Association XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Cyg OB2 is one of the most massive associations of O-type stars in our Galaxy. Despite the large interstellar reddening towards Cyg OB2, many studies, spanning a wide range of wavelengths, have been conducted to more clearly understand this association. X-ray observations provide a powerful tool to overcome the effect of interstellar absorption and study the most energetic processes associated with the stars in Cyg OB2. The author analyses XMM-Newton data to investigate the X-ray and UV properties of massive O-type stars as well as low-mass pre-main sequence stars in Cyg OB2. Six XMM-Newton observations of the core of Cyg OB2 were obtained. In the analysis, the author paid particular attention to the variability of the X-ray bright OB stars, especially the luminous blue variable candidate Cyg OB2 #12. He found that X-ray variability is quite common among the stars in Cyg OB2. While short-term variations are restricted mostly to low-mass pre-main sequence stars, one third of the OB stars display long-term variations. The X-ray flux of CygO B2 #12 varies by 37%, over timescales from days to years, while its mean log L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt; amounts to -6.10. These properties suggest that Cyg OB2 wind. Two other X-ray bright O-type stars (MT91 516 and CPR2002A11) display variations that suggest they are interacting wind binary systems. This table lists the general properties of the X-ray sources detected in Cyg OB2 with the EPIC cameras onboard XMM-Newton as given in Table 2 of the reference paper. An additional list of the properties of the sources detected inside Cyg OB2 with the two UV filters of the OM instrument onboard XMM-Newton which was contained in Table 4 of the reference paper is not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cygob2xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/cygob2xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CYGOB2XMM [2]</TD>
            <TD>Cygnus OB2 Association XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Cyg OB2 is one of the most massive associations of O-type stars in our Galaxy. Despite the large interstellar reddening towards Cyg OB2, many studies, spanning a wide range of wavelengths, have been conducted to more clearly understand this association. X-ray observations provide a powerful tool to overcome the effect of interstellar absorption and study the most energetic processes associated with the stars in Cyg OB2. The author analyses XMM-Newton data to investigate the X-ray and UV properties of massive O-type stars as well as low-mass pre-main sequence stars in Cyg OB2. Six XMM-Newton observations of the core of Cyg OB2 were obtained. In the analysis, the author paid particular attention to the variability of the X-ray bright OB stars, especially the luminous blue variable candidate Cyg OB2 #12. He found that X-ray variability is quite common among the stars in Cyg OB2. While short-term variations are restricted mostly to low-mass pre-main sequence stars, one third of the OB stars display long-term variations. The X-ray flux of CygO B2 #12 varies by 37%, over timescales from days to years, while its mean log L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt; amounts to -6.10. These properties suggest that Cyg OB2 wind. Two other X-ray bright O-type stars (MT91 516 and CPR2002A11) display variations that suggest they are interacting wind binary systems. This table lists the general properties of the X-ray sources detected in Cyg OB2 with the EPIC cameras onboard XMM-Newton as given in Table 2 of the reference paper. An additional list of the properties of the sources detected inside Cyg OB2 with the two UV filters of the OM instrument onboard XMM-Newton which was contained in Table 4 of the reference paper is not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cygob2xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/cygob2xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CYGOB2XMM [3]</TD>
            <TD>Cygnus OB2 Association XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Cyg OB2 is one of the most massive associations of O-type stars in our Galaxy. Despite the large interstellar reddening towards Cyg OB2, many studies, spanning a wide range of wavelengths, have been conducted to more clearly understand this association. X-ray observations provide a powerful tool to overcome the effect of interstellar absorption and study the most energetic processes associated with the stars in Cyg OB2. The author analyses XMM-Newton data to investigate the X-ray and UV properties of massive O-type stars as well as low-mass pre-main sequence stars in Cyg OB2. Six XMM-Newton observations of the core of Cyg OB2 were obtained. In the analysis, the author paid particular attention to the variability of the X-ray bright OB stars, especially the luminous blue variable candidate Cyg OB2 #12. He found that X-ray variability is quite common among the stars in Cyg OB2. While short-term variations are restricted mostly to low-mass pre-main sequence stars, one third of the OB stars display long-term variations. The X-ray flux of CygO B2 #12 varies by 37%, over timescales from days to years, while its mean log L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt; amounts to -6.10. These properties suggest that Cyg OB2 wind. Two other X-ray bright O-type stars (MT91 516 and CPR2002A11) display variations that suggest they are interacting wind binary systems. This table lists the general properties of the X-ray sources detected in Cyg OB2 with the EPIC cameras onboard XMM-Newton as given in Table 2 of the reference paper. An additional list of the properties of the sources detected inside Cyg OB2 with the two UV filters of the OM instrument onboard XMM-Newton which was contained in Table 4 of the reference paper is not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cygob2xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/cygob2xmm.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CYGOB2XMM [1]</TD>
            <TD>Cygnus OB2 Association XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Cyg OB2 is one of the most massive associations of O-type stars in our Galaxy. Despite the large interstellar reddening towards Cyg OB2, many studies, spanning a wide range of wavelengths, have been conducted to more clearly understand this association. X-ray observations provide a powerful tool to overcome the effect of interstellar absorption and study the most energetic processes associated with the stars in Cyg OB2. The author analyses XMM-Newton data to investigate the X-ray and UV properties of massive O-type stars as well as low-mass pre-main sequence stars in Cyg OB2. Six XMM-Newton observations of the core of Cyg OB2 were obtained. In the analysis, the author paid particular attention to the variability of the X-ray bright OB stars, especially the luminous blue variable candidate Cyg OB2 #12. He found that X-ray variability is quite common among the stars in Cyg OB2. While short-term variations are restricted mostly to low-mass pre-main sequence stars, one third of the OB stars display long-term variations. The X-ray flux of CygO B2 #12 varies by 37%, over timescales from days to years, while its mean log L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt; amounts to -6.10. These properties suggest that Cyg OB2 wind. Two other X-ray bright O-type stars (MT91 516 and CPR2002A11) display variations that suggest they are interacting wind binary systems. This table lists the general properties of the X-ray sources detected in Cyg OB2 with the EPIC cameras onboard XMM-Newton as given in Table 2 of the reference paper. An additional list of the properties of the sources detected inside Cyg OB2 with the two UV filters of the OM instrument onboard XMM-Newton which was contained in Table 4 of the reference paper is not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cygob2xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/cygob2xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CYGOB2XMM [2]</TD>
            <TD>Cygnus OB2 Association XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Cyg OB2 is one of the most massive associations of O-type stars in our Galaxy. Despite the large interstellar reddening towards Cyg OB2, many studies, spanning a wide range of wavelengths, have been conducted to more clearly understand this association. X-ray observations provide a powerful tool to overcome the effect of interstellar absorption and study the most energetic processes associated with the stars in Cyg OB2. The author analyses XMM-Newton data to investigate the X-ray and UV properties of massive O-type stars as well as low-mass pre-main sequence stars in Cyg OB2. Six XMM-Newton observations of the core of Cyg OB2 were obtained. In the analysis, the author paid particular attention to the variability of the X-ray bright OB stars, especially the luminous blue variable candidate Cyg OB2 #12. He found that X-ray variability is quite common among the stars in Cyg OB2. While short-term variations are restricted mostly to low-mass pre-main sequence stars, one third of the OB stars display long-term variations. The X-ray flux of CygO B2 #12 varies by 37%, over timescales from days to years, while its mean log L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt; amounts to -6.10. These properties suggest that Cyg OB2 wind. Two other X-ray bright O-type stars (MT91 516 and CPR2002A11) display variations that suggest they are interacting wind binary systems. This table lists the general properties of the X-ray sources detected in Cyg OB2 with the EPIC cameras onboard XMM-Newton as given in Table 2 of the reference paper. An additional list of the properties of the sources detected inside Cyg OB2 with the two UV filters of the OM instrument onboard XMM-Newton which was contained in Table 4 of the reference paper is not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cygob2xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/cygob2xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CYGOB2XMM [3]</TD>
            <TD>Cygnus OB2 Association XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Cyg OB2 is one of the most massive associations of O-type stars in our Galaxy. Despite the large interstellar reddening towards Cyg OB2, many studies, spanning a wide range of wavelengths, have been conducted to more clearly understand this association. X-ray observations provide a powerful tool to overcome the effect of interstellar absorption and study the most energetic processes associated with the stars in Cyg OB2. The author analyses XMM-Newton data to investigate the X-ray and UV properties of massive O-type stars as well as low-mass pre-main sequence stars in Cyg OB2. Six XMM-Newton observations of the core of Cyg OB2 were obtained. In the analysis, the author paid particular attention to the variability of the X-ray bright OB stars, especially the luminous blue variable candidate Cyg OB2 #12. He found that X-ray variability is quite common among the stars in Cyg OB2. While short-term variations are restricted mostly to low-mass pre-main sequence stars, one third of the OB stars display long-term variations. The X-ray flux of CygO B2 #12 varies by 37%, over timescales from days to years, while its mean log L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt; amounts to -6.10. These properties suggest that Cyg OB2 wind. Two other X-ray bright O-type stars (MT91 516 and CPR2002A11) display variations that suggest they are interacting wind binary systems. This table lists the general properties of the X-ray sources detected in Cyg OB2 with the EPIC cameras onboard XMM-Newton as given in Table 2 of the reference paper. An additional list of the properties of the sources detected inside Cyg OB2 with the two UV filters of the OM instrument onboard XMM-Newton which was contained in Table 4 of the reference paper is not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cygob2xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/cygob2xmm.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CYGOB2XMM [1]</TD>
            <TD>Cygnus OB2 Association XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Cyg OB2 is one of the most massive associations of O-type stars in our Galaxy. Despite the large interstellar reddening towards Cyg OB2, many studies, spanning a wide range of wavelengths, have been conducted to more clearly understand this association. X-ray observations provide a powerful tool to overcome the effect of interstellar absorption and study the most energetic processes associated with the stars in Cyg OB2. The author analyses XMM-Newton data to investigate the X-ray and UV properties of massive O-type stars as well as low-mass pre-main sequence stars in Cyg OB2. Six XMM-Newton observations of the core of Cyg OB2 were obtained. In the analysis, the author paid particular attention to the variability of the X-ray bright OB stars, especially the luminous blue variable candidate Cyg OB2 #12. He found that X-ray variability is quite common among the stars in Cyg OB2. While short-term variations are restricted mostly to low-mass pre-main sequence stars, one third of the OB stars display long-term variations. The X-ray flux of CygO B2 #12 varies by 37%, over timescales from days to years, while its mean log L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt; amounts to -6.10. These properties suggest that Cyg OB2 wind. Two other X-ray bright O-type stars (MT91 516 and CPR2002A11) display variations that suggest they are interacting wind binary systems. This table lists the general properties of the X-ray sources detected in Cyg OB2 with the EPIC cameras onboard XMM-Newton as given in Table 2 of the reference paper. An additional list of the properties of the sources detected inside Cyg OB2 with the two UV filters of the OM instrument onboard XMM-Newton which was contained in Table 4 of the reference paper is not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2xmm#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2xmm</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=cygob2xmm&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/cygob2xmm.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CYGOB2XMM [2]</TD>
            <TD>Cygnus OB2 Association XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Cyg OB2 is one of the most massive associations of O-type stars in our Galaxy. Despite the large interstellar reddening towards Cyg OB2, many studies, spanning a wide range of wavelengths, have been conducted to more clearly understand this association. X-ray observations provide a powerful tool to overcome the effect of interstellar absorption and study the most energetic processes associated with the stars in Cyg OB2. The author analyses XMM-Newton data to investigate the X-ray and UV properties of massive O-type stars as well as low-mass pre-main sequence stars in Cyg OB2. Six XMM-Newton observations of the core of Cyg OB2 were obtained. In the analysis, the author paid particular attention to the variability of the X-ray bright OB stars, especially the luminous blue variable candidate Cyg OB2 #12. He found that X-ray variability is quite common among the stars in Cyg OB2. While short-term variations are restricted mostly to low-mass pre-main sequence stars, one third of the OB stars display long-term variations. The X-ray flux of CygO B2 #12 varies by 37%, over timescales from days to years, while its mean log L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt; amounts to -6.10. These properties suggest that Cyg OB2 wind. Two other X-ray bright O-type stars (MT91 516 and CPR2002A11) display variations that suggest they are interacting wind binary systems. This table lists the general properties of the X-ray sources detected in Cyg OB2 with the EPIC cameras onboard XMM-Newton as given in Table 2 of the reference paper. An additional list of the properties of the sources detected inside Cyg OB2 with the two UV filters of the OM instrument onboard XMM-Newton which was contained in Table 4 of the reference paper is not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2xmm#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=cygob2xmm&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/cygob2xmm.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CYGOB2XMM [3]</TD>
            <TD>Cygnus OB2 Association XMM-Newton X-Ray Point Source Catalog</TD>
            <TD>Cyg OB2 is one of the most massive associations of O-type stars in our Galaxy. Despite the large interstellar reddening towards Cyg OB2, many studies, spanning a wide range of wavelengths, have been conducted to more clearly understand this association. X-ray observations provide a powerful tool to overcome the effect of interstellar absorption and study the most energetic processes associated with the stars in Cyg OB2. The author analyses XMM-Newton data to investigate the X-ray and UV properties of massive O-type stars as well as low-mass pre-main sequence stars in Cyg OB2. Six XMM-Newton observations of the core of Cyg OB2 were obtained. In the analysis, the author paid particular attention to the variability of the X-ray bright OB stars, especially the luminous blue variable candidate Cyg OB2 #12. He found that X-ray variability is quite common among the stars in Cyg OB2. While short-term variations are restricted mostly to low-mass pre-main sequence stars, one third of the OB stars display long-term variations. The X-ray flux of CygO B2 #12 varies by 37%, over timescales from days to years, while its mean log L&lt;sub&gt;X&lt;/sub&gt;/L&lt;sub&gt;bol&lt;/sub&gt; amounts to -6.10. These properties suggest that Cyg OB2 wind. Two other X-ray bright O-type stars (MT91 516 and CPR2002A11) display variations that suggest they are interacting wind binary systems. This table lists the general properties of the X-ray sources detected in Cyg OB2 with the EPIC cameras onboard XMM-Newton as given in Table 2 of the reference paper. An additional list of the properties of the sources detected inside Cyg OB2 with the two UV filters of the OM instrument onboard XMM-Newton which was contained in Table 4 of the reference paper is not included herein.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/cygob2xmm#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/cygob2xmm</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_cygob2xmm&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/cygob2xmm.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CCOSRSSFAG [1]</TD>
            <TD>Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog</TD>
            <TD>X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ccosrssfag#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ccosrssfag</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ccosrssfag&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ccosrssfag.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CCOSRSSFAG [2]</TD>
            <TD>Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog</TD>
            <TD>X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ccosrssfag#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>#Research#</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ccosrssfag&amp;</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ccosrssfag.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CCOSRSSFAG [3]</TD>
            <TD>Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog</TD>
            <TD>X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ccosrssfag&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ccosrssfag.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CCOSRSSFAG [1]</TD>
            <TD>Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog</TD>
            <TD>X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ccosrssfag#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/ccosrssfag</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ccosrssfag&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ccosrssfag.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CCOSRSSFAG [2]</TD>
            <TD>Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog</TD>
            <TD>X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ccosrssfag#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ParamHTTP</TD>
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            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ccosrssfag&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ccosrssfag.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CCOSRSSFAG [3]</TD>
            <TD>Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog</TD>
            <TD>X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ccosrssfag#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ccosrssfag</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ccosrssfag&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ccosrssfag.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CCOSRSSFAG [1]</TD>
            <TD>Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog</TD>
            <TD>X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ccosrssfag#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ccosrssfag</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=ccosrssfag&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ccosrssfag.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CCOSRSSFAG [2]</TD>
            <TD>Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog</TD>
            <TD>X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ccosrssfag#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ccosrssfag</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=ccosrssfag&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ccosrssfag.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CCOSRSSFAG [3]</TD>
            <TD>Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog</TD>
            <TD>X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/ccosrssfag#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/ccosrssfag</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_ccosrssfag&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/ccosrssfag.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHAMPSDSSA [1]</TD>
            <TD>CHAMP/SDSS Nearby Low-Luminosity AGN Catalog</TD>
            <TD>The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L&lt;sub&gt;X&lt;/sub&gt; and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -&gt; Seyfert/Transition Object -&gt; LINER -&gt; Passive suggested by optical data. In particular, the authors show that both L&lt;sub&gt;X&lt;/sub&gt; and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt;, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L&lt;sub&gt;Edd&lt;/sub&gt; LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L&lt;sub&gt;Edd&lt;/sub&gt; ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt; may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L&lt;sub&gt;Edd&lt;/sub&gt; &gt;~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta &lt;0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH&lt;sub&gt;Gal&lt;/sub&gt;. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs').</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champsdssa#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/champsdssa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=champsdssa&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champsdssa.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHAMPSDSSA [2]</TD>
            <TD>CHAMP/SDSS Nearby Low-Luminosity AGN Catalog</TD>
            <TD>The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L&lt;sub&gt;X&lt;/sub&gt; and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -&gt; Seyfert/Transition Object -&gt; LINER -&gt; Passive suggested by optical data. In particular, the authors show that both L&lt;sub&gt;X&lt;/sub&gt; and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt;, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L&lt;sub&gt;Edd&lt;/sub&gt; LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L&lt;sub&gt;Edd&lt;/sub&gt; ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt; may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L&lt;sub&gt;Edd&lt;/sub&gt; &gt;~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta &lt;0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH&lt;sub&gt;Gal&lt;/sub&gt;. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs').</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champsdssa#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/champsdssa</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=champsdssa&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champsdssa.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHAMPSDSSA [3]</TD>
            <TD>CHAMP/SDSS Nearby Low-Luminosity AGN Catalog</TD>
            <TD>The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L&lt;sub&gt;X&lt;/sub&gt; and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -&gt; Seyfert/Transition Object -&gt; LINER -&gt; Passive suggested by optical data. In particular, the authors show that both L&lt;sub&gt;X&lt;/sub&gt; and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt;, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L&lt;sub&gt;Edd&lt;/sub&gt; LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L&lt;sub&gt;Edd&lt;/sub&gt; ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt; may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L&lt;sub&gt;Edd&lt;/sub&gt; &gt;~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta &lt;0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH&lt;sub&gt;Gal&lt;/sub&gt;. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs').</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champsdssa#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/champsdssa</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_champsdssa&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champsdssa.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHAMPSDSSA [1]</TD>
            <TD>CHAMP/SDSS Nearby Low-Luminosity AGN Catalog</TD>
            <TD>The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L&lt;sub&gt;X&lt;/sub&gt; and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -&gt; Seyfert/Transition Object -&gt; LINER -&gt; Passive suggested by optical data. In particular, the authors show that both L&lt;sub&gt;X&lt;/sub&gt; and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt;, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L&lt;sub&gt;Edd&lt;/sub&gt; LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L&lt;sub&gt;Edd&lt;/sub&gt; ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt; may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L&lt;sub&gt;Edd&lt;/sub&gt; &gt;~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta &lt;0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH&lt;sub&gt;Gal&lt;/sub&gt;. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs').</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champsdssa#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/champsdssa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=champsdssa&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHAMPSDSSA [2]</TD>
            <TD>CHAMP/SDSS Nearby Low-Luminosity AGN Catalog</TD>
            <TD>The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L&lt;sub&gt;X&lt;/sub&gt; and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -&gt; Seyfert/Transition Object -&gt; LINER -&gt; Passive suggested by optical data. In particular, the authors show that both L&lt;sub&gt;X&lt;/sub&gt; and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt;, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L&lt;sub&gt;Edd&lt;/sub&gt; LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L&lt;sub&gt;Edd&lt;/sub&gt; ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt; may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L&lt;sub&gt;Edd&lt;/sub&gt; &gt;~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta &lt;0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH&lt;sub&gt;Gal&lt;/sub&gt;. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs').</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champsdssa#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=champsdssa&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champsdssa.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHAMPSDSSA [3]</TD>
            <TD>CHAMP/SDSS Nearby Low-Luminosity AGN Catalog</TD>
            <TD>The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L&lt;sub&gt;X&lt;/sub&gt; and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -&gt; Seyfert/Transition Object -&gt; LINER -&gt; Passive suggested by optical data. In particular, the authors show that both L&lt;sub&gt;X&lt;/sub&gt; and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt;, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L&lt;sub&gt;Edd&lt;/sub&gt; LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L&lt;sub&gt;Edd&lt;/sub&gt; ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt; may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L&lt;sub&gt;Edd&lt;/sub&gt; &gt;~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta &lt;0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH&lt;sub&gt;Gal&lt;/sub&gt;. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs').</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champsdssa#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/champsdssa</TD>
            <TD />
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            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_champsdssa&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champsdssa.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>CHAMPSDSSA [1]</TD>
            <TD>CHAMP/SDSS Nearby Low-Luminosity AGN Catalog</TD>
            <TD>The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L&lt;sub&gt;X&lt;/sub&gt; and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -&gt; Seyfert/Transition Object -&gt; LINER -&gt; Passive suggested by optical data. In particular, the authors show that both L&lt;sub&gt;X&lt;/sub&gt; and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt;, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L&lt;sub&gt;Edd&lt;/sub&gt; LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L&lt;sub&gt;Edd&lt;/sub&gt; ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt; may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L&lt;sub&gt;Edd&lt;/sub&gt; &gt;~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta &lt;0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH&lt;sub&gt;Gal&lt;/sub&gt;. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs').</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champsdssa#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/champsdssa</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>CHAMPSDSSA [2]</TD>
            <TD>CHAMP/SDSS Nearby Low-Luminosity AGN Catalog</TD>
            <TD>The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L&lt;sub&gt;X&lt;/sub&gt; and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -&gt; Seyfert/Transition Object -&gt; LINER -&gt; Passive suggested by optical data. In particular, the authors show that both L&lt;sub&gt;X&lt;/sub&gt; and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt;, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L&lt;sub&gt;Edd&lt;/sub&gt; LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L&lt;sub&gt;Edd&lt;/sub&gt; ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt; may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L&lt;sub&gt;Edd&lt;/sub&gt; &gt;~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta &lt;0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH&lt;sub&gt;Gal&lt;/sub&gt;. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs').</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champsdssa#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champsdssa.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>CHAMPSDSSA [3]</TD>
            <TD>CHAMP/SDSS Nearby Low-Luminosity AGN Catalog</TD>
            <TD>The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L&lt;sub&gt;X&lt;/sub&gt; and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -&gt; Seyfert/Transition Object -&gt; LINER -&gt; Passive suggested by optical data. In particular, the authors show that both L&lt;sub&gt;X&lt;/sub&gt; and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt;, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L&lt;sub&gt;Edd&lt;/sub&gt; LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L&lt;sub&gt;Edd&lt;/sub&gt; ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L&lt;sub&gt;Edd&lt;/sub&gt; may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L&lt;sub&gt;Edd&lt;/sub&gt; &gt;~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta &lt;0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH&lt;sub&gt;Gal&lt;/sub&gt;. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs').</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/champsdssa#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD />
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            <TD>WebBrowser</TD>
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            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/chandra/champsdssa.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GMRTJ0916 [1]</TD>
            <TD>Giant Metrewave Radio Telescope J0916+6348 Field Radio Source Catalog</TD>
            <TD>This table contains a catalog based on deep multifrequency observations made using the Giant Metrewave Radio Telescope (GMRT) at 153, 244, 610 and 1260 MHz of a field centred on J0916+6348, to search for evidence of fossil radio lobes which could be due to an earlier cycle of episodic activity of the parent galaxy, as well as haloes and relics in clusters of galaxies. The authors do not find any unambiguous evidence of episodic activity in a list of 374 sources, suggesting that such activity is rare even in relatively deep low-frequency observations. The authors examine the spectra of all the sources by combining their observations with those from the Westerbork Northern Sky Survey (WENSS), NRAO (National Radio Astronomy Observatories) VLA (Very Large Array) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty-Centimeters Survey (FIRST). Considering only those which have measurements at a minimum of 3 different frequencies, they find that almost all sources are consistent with a straight spectrum with a median spectral index alpha ~ 0.8 (S&lt;sub&gt;nu&lt;/sub&gt; ~ nu&lt;sup&gt;-alpha&lt;/sup&gt;) which appears steeper than theoretical expectations of the injection spectral index. The authors identify 14 very-steep-spectrum sources with alpha &gt;~ 1.3. This table contains the list of 317 sources (out of the 374 sources which were within 1.5 degrees of the phase center at 153 MHz and had peak brightnesses at least 6 times larger than the local rms value) which were detected at a minimum of 3 frequencies out of the 6 frequencies (153, 244, 327, 610, 1260 and 1400 MHz) which were utilized in this study. The new observations were made on 2005 December 12 at 153 MHz, 2005 November 26 at 244 MHz and 610 MHz, and on 2008 April 22 at 1260 MHz, on the Giant Metrewave Radio Telescope (Pune, India).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/gmrtj0916#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gmrtj0916</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=gmrtj0916&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/gmrtj0916.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GMRTJ0916 [2]</TD>
            <TD>Giant Metrewave Radio Telescope J0916+6348 Field Radio Source Catalog</TD>
            <TD>This table contains a catalog based on deep multifrequency observations made using the Giant Metrewave Radio Telescope (GMRT) at 153, 244, 610 and 1260 MHz of a field centred on J0916+6348, to search for evidence of fossil radio lobes which could be due to an earlier cycle of episodic activity of the parent galaxy, as well as haloes and relics in clusters of galaxies. The authors do not find any unambiguous evidence of episodic activity in a list of 374 sources, suggesting that such activity is rare even in relatively deep low-frequency observations. The authors examine the spectra of all the sources by combining their observations with those from the Westerbork Northern Sky Survey (WENSS), NRAO (National Radio Astronomy Observatories) VLA (Very Large Array) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty-Centimeters Survey (FIRST). Considering only those which have measurements at a minimum of 3 different frequencies, they find that almost all sources are consistent with a straight spectrum with a median spectral index alpha ~ 0.8 (S&lt;sub&gt;nu&lt;/sub&gt; ~ nu&lt;sup&gt;-alpha&lt;/sup&gt;) which appears steeper than theoretical expectations of the injection spectral index. The authors identify 14 very-steep-spectrum sources with alpha &gt;~ 1.3. This table contains the list of 317 sources (out of the 374 sources which were within 1.5 degrees of the phase center at 153 MHz and had peak brightnesses at least 6 times larger than the local rms value) which were detected at a minimum of 3 frequencies out of the 6 frequencies (153, 244, 327, 610, 1260 and 1400 MHz) which were utilized in this study. The new observations were made on 2005 December 12 at 153 MHz, 2005 November 26 at 244 MHz and 610 MHz, and on 2008 April 22 at 1260 MHz, on the Giant Metrewave Radio Telescope (Pune, India).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/gmrtj0916#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gmrtj0916</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=gmrtj0916&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/gmrtj0916.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GMRTJ0916 [3]</TD>
            <TD>Giant Metrewave Radio Telescope J0916+6348 Field Radio Source Catalog</TD>
            <TD>This table contains a catalog based on deep multifrequency observations made using the Giant Metrewave Radio Telescope (GMRT) at 153, 244, 610 and 1260 MHz of a field centred on J0916+6348, to search for evidence of fossil radio lobes which could be due to an earlier cycle of episodic activity of the parent galaxy, as well as haloes and relics in clusters of galaxies. The authors do not find any unambiguous evidence of episodic activity in a list of 374 sources, suggesting that such activity is rare even in relatively deep low-frequency observations. The authors examine the spectra of all the sources by combining their observations with those from the Westerbork Northern Sky Survey (WENSS), NRAO (National Radio Astronomy Observatories) VLA (Very Large Array) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty-Centimeters Survey (FIRST). Considering only those which have measurements at a minimum of 3 different frequencies, they find that almost all sources are consistent with a straight spectrum with a median spectral index alpha ~ 0.8 (S&lt;sub&gt;nu&lt;/sub&gt; ~ nu&lt;sup&gt;-alpha&lt;/sup&gt;) which appears steeper than theoretical expectations of the injection spectral index. The authors identify 14 very-steep-spectrum sources with alpha &gt;~ 1.3. This table contains the list of 317 sources (out of the 374 sources which were within 1.5 degrees of the phase center at 153 MHz and had peak brightnesses at least 6 times larger than the local rms value) which were detected at a minimum of 3 frequencies out of the 6 frequencies (153, 244, 327, 610, 1260 and 1400 MHz) which were utilized in this study. The new observations were made on 2005 December 12 at 153 MHz, 2005 November 26 at 244 MHz and 610 MHz, and on 2008 April 22 at 1260 MHz, on the Giant Metrewave Radio Telescope (Pune, India).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/gmrtj0916#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gmrtj0916</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_gmrtj0916&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/gmrtj0916.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GMRTJ0916 [1]</TD>
            <TD>Giant Metrewave Radio Telescope J0916+6348 Field Radio Source Catalog</TD>
            <TD>This table contains a catalog based on deep multifrequency observations made using the Giant Metrewave Radio Telescope (GMRT) at 153, 244, 610 and 1260 MHz of a field centred on J0916+6348, to search for evidence of fossil radio lobes which could be due to an earlier cycle of episodic activity of the parent galaxy, as well as haloes and relics in clusters of galaxies. The authors do not find any unambiguous evidence of episodic activity in a list of 374 sources, suggesting that such activity is rare even in relatively deep low-frequency observations. The authors examine the spectra of all the sources by combining their observations with those from the Westerbork Northern Sky Survey (WENSS), NRAO (National Radio Astronomy Observatories) VLA (Very Large Array) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty-Centimeters Survey (FIRST). Considering only those which have measurements at a minimum of 3 different frequencies, they find that almost all sources are consistent with a straight spectrum with a median spectral index alpha ~ 0.8 (S&lt;sub&gt;nu&lt;/sub&gt; ~ nu&lt;sup&gt;-alpha&lt;/sup&gt;) which appears steeper than theoretical expectations of the injection spectral index. The authors identify 14 very-steep-spectrum sources with alpha &gt;~ 1.3. This table contains the list of 317 sources (out of the 374 sources which were within 1.5 degrees of the phase center at 153 MHz and had peak brightnesses at least 6 times larger than the local rms value) which were detected at a minimum of 3 frequencies out of the 6 frequencies (153, 244, 327, 610, 1260 and 1400 MHz) which were utilized in this study. The new observations were made on 2005 December 12 at 153 MHz, 2005 November 26 at 244 MHz and 610 MHz, and on 2008 April 22 at 1260 MHz, on the Giant Metrewave Radio Telescope (Pune, India).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/gmrtj0916#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gmrtj0916</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=gmrtj0916&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/gmrtj0916.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GMRTJ0916 [2]</TD>
            <TD>Giant Metrewave Radio Telescope J0916+6348 Field Radio Source Catalog</TD>
            <TD>This table contains a catalog based on deep multifrequency observations made using the Giant Metrewave Radio Telescope (GMRT) at 153, 244, 610 and 1260 MHz of a field centred on J0916+6348, to search for evidence of fossil radio lobes which could be due to an earlier cycle of episodic activity of the parent galaxy, as well as haloes and relics in clusters of galaxies. The authors do not find any unambiguous evidence of episodic activity in a list of 374 sources, suggesting that such activity is rare even in relatively deep low-frequency observations. The authors examine the spectra of all the sources by combining their observations with those from the Westerbork Northern Sky Survey (WENSS), NRAO (National Radio Astronomy Observatories) VLA (Very Large Array) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty-Centimeters Survey (FIRST). Considering only those which have measurements at a minimum of 3 different frequencies, they find that almost all sources are consistent with a straight spectrum with a median spectral index alpha ~ 0.8 (S&lt;sub&gt;nu&lt;/sub&gt; ~ nu&lt;sup&gt;-alpha&lt;/sup&gt;) which appears steeper than theoretical expectations of the injection spectral index. The authors identify 14 very-steep-spectrum sources with alpha &gt;~ 1.3. This table contains the list of 317 sources (out of the 374 sources which were within 1.5 degrees of the phase center at 153 MHz and had peak brightnesses at least 6 times larger than the local rms value) which were detected at a minimum of 3 frequencies out of the 6 frequencies (153, 244, 327, 610, 1260 and 1400 MHz) which were utilized in this study. The new observations were made on 2005 December 12 at 153 MHz, 2005 November 26 at 244 MHz and 610 MHz, and on 2008 April 22 at 1260 MHz, on the Giant Metrewave Radio Telescope (Pune, India).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/gmrtj0916#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gmrtj0916</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=gmrtj0916&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/gmrtj0916.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GMRTJ0916 [3]</TD>
            <TD>Giant Metrewave Radio Telescope J0916+6348 Field Radio Source Catalog</TD>
            <TD>This table contains a catalog based on deep multifrequency observations made using the Giant Metrewave Radio Telescope (GMRT) at 153, 244, 610 and 1260 MHz of a field centred on J0916+6348, to search for evidence of fossil radio lobes which could be due to an earlier cycle of episodic activity of the parent galaxy, as well as haloes and relics in clusters of galaxies. The authors do not find any unambiguous evidence of episodic activity in a list of 374 sources, suggesting that such activity is rare even in relatively deep low-frequency observations. The authors examine the spectra of all the sources by combining their observations with those from the Westerbork Northern Sky Survey (WENSS), NRAO (National Radio Astronomy Observatories) VLA (Very Large Array) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty-Centimeters Survey (FIRST). Considering only those which have measurements at a minimum of 3 different frequencies, they find that almost all sources are consistent with a straight spectrum with a median spectral index alpha ~ 0.8 (S&lt;sub&gt;nu&lt;/sub&gt; ~ nu&lt;sup&gt;-alpha&lt;/sup&gt;) which appears steeper than theoretical expectations of the injection spectral index. The authors identify 14 very-steep-spectrum sources with alpha &gt;~ 1.3. This table contains the list of 317 sources (out of the 374 sources which were within 1.5 degrees of the phase center at 153 MHz and had peak brightnesses at least 6 times larger than the local rms value) which were detected at a minimum of 3 frequencies out of the 6 frequencies (153, 244, 327, 610, 1260 and 1400 MHz) which were utilized in this study. The new observations were made on 2005 December 12 at 153 MHz, 2005 November 26 at 244 MHz and 610 MHz, and on 2008 April 22 at 1260 MHz, on the Giant Metrewave Radio Telescope (Pune, India).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/gmrtj0916#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gmrtj0916</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_gmrtj0916&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/gmrtj0916.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>GMRTJ0916 [1]</TD>
            <TD>Giant Metrewave Radio Telescope J0916+6348 Field Radio Source Catalog</TD>
            <TD>This table contains a catalog based on deep multifrequency observations made using the Giant Metrewave Radio Telescope (GMRT) at 153, 244, 610 and 1260 MHz of a field centred on J0916+6348, to search for evidence of fossil radio lobes which could be due to an earlier cycle of episodic activity of the parent galaxy, as well as haloes and relics in clusters of galaxies. The authors do not find any unambiguous evidence of episodic activity in a list of 374 sources, suggesting that such activity is rare even in relatively deep low-frequency observations. The authors examine the spectra of all the sources by combining their observations with those from the Westerbork Northern Sky Survey (WENSS), NRAO (National Radio Astronomy Observatories) VLA (Very Large Array) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty-Centimeters Survey (FIRST). Considering only those which have measurements at a minimum of 3 different frequencies, they find that almost all sources are consistent with a straight spectrum with a median spectral index alpha ~ 0.8 (S&lt;sub&gt;nu&lt;/sub&gt; ~ nu&lt;sup&gt;-alpha&lt;/sup&gt;) which appears steeper than theoretical expectations of the injection spectral index. The authors identify 14 very-steep-spectrum sources with alpha &gt;~ 1.3. This table contains the list of 317 sources (out of the 374 sources which were within 1.5 degrees of the phase center at 153 MHz and had peak brightnesses at least 6 times larger than the local rms value) which were detected at a minimum of 3 frequencies out of the 6 frequencies (153, 244, 327, 610, 1260 and 1400 MHz) which were utilized in this study. The new observations were made on 2005 December 12 at 153 MHz, 2005 November 26 at 244 MHz and 610 MHz, and on 2008 April 22 at 1260 MHz, on the Giant Metrewave Radio Telescope (Pune, India).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/gmrtj0916#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gmrtj0916</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=gmrtj0916&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/gmrtj0916.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GMRTJ0916 [2]</TD>
            <TD>Giant Metrewave Radio Telescope J0916+6348 Field Radio Source Catalog</TD>
            <TD>This table contains a catalog based on deep multifrequency observations made using the Giant Metrewave Radio Telescope (GMRT) at 153, 244, 610 and 1260 MHz of a field centred on J0916+6348, to search for evidence of fossil radio lobes which could be due to an earlier cycle of episodic activity of the parent galaxy, as well as haloes and relics in clusters of galaxies. The authors do not find any unambiguous evidence of episodic activity in a list of 374 sources, suggesting that such activity is rare even in relatively deep low-frequency observations. The authors examine the spectra of all the sources by combining their observations with those from the Westerbork Northern Sky Survey (WENSS), NRAO (National Radio Astronomy Observatories) VLA (Very Large Array) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty-Centimeters Survey (FIRST). Considering only those which have measurements at a minimum of 3 different frequencies, they find that almost all sources are consistent with a straight spectrum with a median spectral index alpha ~ 0.8 (S&lt;sub&gt;nu&lt;/sub&gt; ~ nu&lt;sup&gt;-alpha&lt;/sup&gt;) which appears steeper than theoretical expectations of the injection spectral index. The authors identify 14 very-steep-spectrum sources with alpha &gt;~ 1.3. This table contains the list of 317 sources (out of the 374 sources which were within 1.5 degrees of the phase center at 153 MHz and had peak brightnesses at least 6 times larger than the local rms value) which were detected at a minimum of 3 frequencies out of the 6 frequencies (153, 244, 327, 610, 1260 and 1400 MHz) which were utilized in this study. The new observations were made on 2005 December 12 at 153 MHz, 2005 November 26 at 244 MHz and 610 MHz, and on 2008 April 22 at 1260 MHz, on the Giant Metrewave Radio Telescope (Pune, India).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/gmrtj0916#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gmrtj0916</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=gmrtj0916&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/gmrtj0916.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GMRTJ0916 [3]</TD>
            <TD>Giant Metrewave Radio Telescope J0916+6348 Field Radio Source Catalog</TD>
            <TD>This table contains a catalog based on deep multifrequency observations made using the Giant Metrewave Radio Telescope (GMRT) at 153, 244, 610 and 1260 MHz of a field centred on J0916+6348, to search for evidence of fossil radio lobes which could be due to an earlier cycle of episodic activity of the parent galaxy, as well as haloes and relics in clusters of galaxies. The authors do not find any unambiguous evidence of episodic activity in a list of 374 sources, suggesting that such activity is rare even in relatively deep low-frequency observations. The authors examine the spectra of all the sources by combining their observations with those from the Westerbork Northern Sky Survey (WENSS), NRAO (National Radio Astronomy Observatories) VLA (Very Large Array) Sky Survey (NVSS) and the Faint Images of the Radio Sky at Twenty-Centimeters Survey (FIRST). Considering only those which have measurements at a minimum of 3 different frequencies, they find that almost all sources are consistent with a straight spectrum with a median spectral index alpha ~ 0.8 (S&lt;sub&gt;nu&lt;/sub&gt; ~ nu&lt;sup&gt;-alpha&lt;/sup&gt;) which appears steeper than theoretical expectations of the injection spectral index. The authors identify 14 very-steep-spectrum sources with alpha &gt;~ 1.3. This table contains the list of 317 sources (out of the 374 sources which were within 1.5 degrees of the phase center at 153 MHz and had peak brightnesses at least 6 times larger than the local rms value) which were detected at a minimum of 3 frequencies out of the 6 frequencies (153, 244, 327, 610, 1260 and 1400 MHz) which were utilized in this study. The new observations were made on 2005 December 12 at 153 MHz, 2005 November 26 at 244 MHz and 610 MHz, and on 2008 April 22 at 1260 MHz, on the Giant Metrewave Radio Telescope (Pune, India).</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/gmrtj0916#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/gmrtj0916</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_gmrtj0916&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/gmrtj0916.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LOCKMANOIR [1]</TD>
            <TD>Lockman Hole AGN Optical and Infrared Properties Catalog</TD>
            <TD>This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&amp;A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f&lt;sub&gt;x&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K and f&lt;sub&gt;24um&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, z' bands). The LBT observations were taken from February 2007 to March 2009. The R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&amp;A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lockmanoir#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lockmanoir</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lockmanoir&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/lockmanoir.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LOCKMANOIR [2]</TD>
            <TD>Lockman Hole AGN Optical and Infrared Properties Catalog</TD>
            <TD>This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&amp;A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f&lt;sub&gt;x&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K and f&lt;sub&gt;24um&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, z' bands). The LBT observations were taken from February 2007 to March 2009. The R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&amp;A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lockmanoir#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
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            <TD>ivo://nasa.heasarc/lockmanoir</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lockmanoir&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/lockmanoir.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LOCKMANOIR [3]</TD>
            <TD>Lockman Hole AGN Optical and Infrared Properties Catalog</TD>
            <TD>This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&amp;A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f&lt;sub&gt;x&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K and f&lt;sub&gt;24um&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, z' bands). The LBT observations were taken from February 2007 to March 2009. The R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&amp;A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lockmanoir#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lockmanoir</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lockmanoir&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/lockmanoir.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LOCKMANOIR [1]</TD>
            <TD>Lockman Hole AGN Optical and Infrared Properties Catalog</TD>
            <TD>This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&amp;A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f&lt;sub&gt;x&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K and f&lt;sub&gt;24um&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, z' bands). The LBT observations were taken from February 2007 to March 2009. The R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&amp;A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lockmanoir#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lockmanoir</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lockmanoir&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/lockmanoir.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LOCKMANOIR [2]</TD>
            <TD>Lockman Hole AGN Optical and Infrared Properties Catalog</TD>
            <TD>This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&amp;A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f&lt;sub&gt;x&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K and f&lt;sub&gt;24um&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, z' bands). The LBT observations were taken from February 2007 to March 2009. The R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&amp;A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lockmanoir#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lockmanoir</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lockmanoir&amp;</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/lockmanoir.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LOCKMANOIR [3]</TD>
            <TD>Lockman Hole AGN Optical and Infrared Properties Catalog</TD>
            <TD>This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&amp;A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f&lt;sub&gt;x&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K and f&lt;sub&gt;24um&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, z' bands). The LBT observations were taken from February 2007 to March 2009. The R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&amp;A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lockmanoir#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/lockmanoir</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lockmanoir&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/lockmanoir.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>LOCKMANOIR [1]</TD>
            <TD>Lockman Hole AGN Optical and Infrared Properties Catalog</TD>
            <TD>This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&amp;A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f&lt;sub&gt;x&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K and f&lt;sub&gt;24um&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, z' bands). The LBT observations were taken from February 2007 to March 2009. The R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&amp;A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lockmanoir#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lockmanoir</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=lockmanoir&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/lockmanoir.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>LOCKMANOIR [2]</TD>
            <TD>Lockman Hole AGN Optical and Infrared Properties Catalog</TD>
            <TD>This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&amp;A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f&lt;sub&gt;x&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K and f&lt;sub&gt;24um&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, z' bands). The LBT observations were taken from February 2007 to March 2009. The R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&amp;A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lockmanoir#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lockmanoir</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=lockmanoir&amp;</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/lockmanoir.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>LOCKMANOIR [3]</TD>
            <TD>Lockman Hole AGN Optical and Infrared Properties Catalog</TD>
            <TD>This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&amp;A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f&lt;sub&gt;x&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K and f&lt;sub&gt;24um&lt;/sub&gt;/f&lt;sub&gt;RC&lt;/sub&gt; vs. R&lt;sub&gt;C&lt;/sub&gt; - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, z' bands). The LBT observations were taken from February 2007 to March 2009. The R&lt;sub&gt;C&lt;/sub&gt;, I&lt;sub&gt;C&lt;/sub&gt;, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&amp;A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Infrared#Optical#X-ray#</TD>
            <TD>ivo://nasa.heasarc/lockmanoir#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/lockmanoir</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_lockmanoir&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/xmm-newton/lockmanoir.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE030 [1]</TD>
            <TD>Planck Early Release 30-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 30-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke030#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke030</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke030&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke030.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE030 [2]</TD>
            <TD>Planck Early Release 30-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 30-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke030#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke030</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke030&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke030.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE030 [3]</TD>
            <TD>Planck Early Release 30-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 30-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke030#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke030</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke030&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke030.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE030 [1]</TD>
            <TD>Planck Early Release 30-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 30-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke030#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke030</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke030&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke030.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE030 [2]</TD>
            <TD>Planck Early Release 30-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 30-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke030#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>ivo://nasa.heasarc/plancke030</TD>
            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke030&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke030.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE030 [3]</TD>
            <TD>Planck Early Release 30-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 30-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke030#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
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            <TD>#Research#</TD>
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            <TD>ivo://nasa.heasarc/plancke030</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke030&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke030.html</TD>
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            <TD>Catalog</TD>
            <TD>PLANCKE030 [1]</TD>
            <TD>Planck Early Release 30-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 30-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke030#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke030</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke030&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke030.html</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE030 [2]</TD>
            <TD>Planck Early Release 30-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 30-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke030#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke030</TD>
            <TD />
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            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke030&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke030.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE030 [3]</TD>
            <TD>Planck Early Release 30-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 30-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke030#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
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            <TD />
            <TD>ivo://nasa.heasarc/plancke030</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke030&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke030.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE044 [1]</TD>
            <TD>Planck Early Release 44-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 44-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke044#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke044&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke044.html</TD>
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            <TD>HTTP Request</TD>
            <TD>PLANCKE044 [2]</TD>
            <TD>Planck Early Release 44-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 44-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke044#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke044&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke044.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE044 [3]</TD>
            <TD>Planck Early Release 44-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 44-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke044#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/plancke044</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke044&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke044.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE044 [1]</TD>
            <TD>Planck Early Release 44-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 44-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke044#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke044</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke044&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke044.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE044 [2]</TD>
            <TD>Planck Early Release 44-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 44-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke044#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>ivo://nasa.heasarc/plancke044</TD>
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            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke044&amp;</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke044.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE044 [3]</TD>
            <TD>Planck Early Release 44-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 44-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke044#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke044</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke044&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke044.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE044 [1]</TD>
            <TD>Planck Early Release 44-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 44-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke044#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke044</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke044&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke044.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE044 [2]</TD>
            <TD>Planck Early Release 44-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 44-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke044#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke044</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke044&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke044.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE044 [3]</TD>
            <TD>Planck Early Release 44-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 44-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke044#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke044</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke044&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke044.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE070 [1]</TD>
            <TD>Planck Early Release 70-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 70-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke070#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke070</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke070&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke070.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE070 [2]</TD>
            <TD>Planck Early Release 70-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 70-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
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            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke070&amp;</TD>
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            <TD>Web Page</TD>
            <TD>PLANCKE070 [3]</TD>
            <TD>Planck Early Release 70-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 70-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke070#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/plancke070</TD>
            <TD />
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            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke070&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>PLANCKE070 [1]</TD>
            <TD>Planck Early Release 70-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 70-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke070#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
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            <TD>ParamHTTP</TD>
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            <TD>180</TD>
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            <TD>PLANCKE070 [2]</TD>
            <TD>Planck Early Release 70-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 70-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE070 [3]</TD>
            <TD>Planck Early Release 70-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). 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            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke070#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/plancke070</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke070&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke070.html</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE070 [1]</TD>
            <TD>Planck Early Release 70-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 70-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke070#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke070</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke070&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke070.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE070 [2]</TD>
            <TD>Planck Early Release 70-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 70-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke070#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke070</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke070&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke070.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE070 [3]</TD>
            <TD>Planck Early Release 70-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 70-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke070#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke070</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke070&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke070.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE100 [1]</TD>
            <TD>Planck Early Release 100-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 100-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke100#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke100&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke100.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE100 [2]</TD>
            <TD>Planck Early Release 100-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 100-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke100#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke100.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE100 [3]</TD>
            <TD>Planck Early Release 100-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 100-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke100#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke100&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke100.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE100 [1]</TD>
            <TD>Planck Early Release 100-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 100-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke100#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke100&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke100.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE100 [2]</TD>
            <TD>Planck Early Release 100-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 100-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke100#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke100</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke100&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke100.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE100 [3]</TD>
            <TD>Planck Early Release 100-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 100-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke100#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke100&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke100.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>PLANCKE100 [1]</TD>
            <TD>Planck Early Release 100-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 100-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/plancke100#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/plancke100</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=plancke100&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke100.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>PLANCKE100 [2]</TD>
            <TD>Planck Early Release 100-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 100-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
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            <TD />
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=plancke100&amp;</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
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          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>PLANCKE100 [3]</TD>
            <TD>Planck Early Release 100-GHz Compact Source Catalog</TD>
            <TD>Planck is a European Space Agency (ESA) mission with significant contributions from the U.S. National Aeronautics and Space Agency (NASA). It is the third generation of space-based cosmic microwave background (CMB) experiments, after the Cosmic Background Explorer (COBE) and the Wilkinson Microwave Anisotropy Probe (WMAP). Planck was launched on 14 May 2009 on an Ariane 5 rocket from Kourou, French Guiana. Following a cruise to the Earth-Sun L2 Lagrange point, cooling and in-orbit checkout, Planck initiated the First Light Survey on 13 August 2009. Since then, Planck has been continuously measuring the intensity of the sky over a range of frequencies from 30 to 857 GHz (wavelengths of 1 cm to 350 microns) with spatial resolutions ranging from about 33 to 4.2 arcminutes, respectively. The Low Frequency Instrument (LFI) on Planck provides temperature and polarization information using radiometers which operate between 30 and 70 GHz. The High Frequency Instrument (HFI) uses pairs of polarization-sensitive bolometers at each of four frequencies between 100 and 353 GHz but does not measure polarization information in the two upper HFI bands at 545 and 857 GHz. The lowest frequencies overlap with the frequencies of WMAP, and the highest frequencies extend far into the submillimeter in order to improve separation between Galactic foregrounds and the CMB. By extending to wavelengths longer than those at which the Infrared Astronomical Satellite (IRAS) operated, Planck is providing an unprecedented window into dust emission at far-infrared and submillimeter wavelengths. The Planck Early Release Compact Source Catalogue (ERCSC) is a list of all high reliability sources, both Galactic and extragalactic, derived from the first sky coverage. The data that went into this early release comprise all observations undertaken between 13 August 2009 and 6 June 2010, corresponding to Planck operational days 91-389. Since the Planck scan strategy results in the entire sky being observed every 6 months, the data considered in this release correspond to more than the first sky coverage. The source lists have reliability goals of &gt; 90% across the entire sky and &gt; 95% at high Galactic latitude. The goals on photometric accuracy are 30% while the positional accuracy goal translates to a positional root mean square (RMS) uncertainty that is less than 1/5 of the beam full width at half maximum (FWHM). A brief description of the methodology of the construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC) is provided in the reference paper. The catalog is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. Four source detection algorithms were run as part of the ERCSC pipeline. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is &gt;~ 90%. There is no requirement on completeness for the ERCSC. As a result of the Monte-Carlo assessment of reliability of sources from the different techniques, an implementation of the PowellSnakes source extraction technique was used at the five frequencies between 30 and 143 GHz while the SExtractor technique was used between 217 and 857 GHz. The 10-sigma photometric flux density limit of the catalogue at |b| &gt; 30 degrees is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations with stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. The entire source list, with more than 15,000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities. Detailed explanations about the mission and the catalogs included here can be found in the "Explanatory supplement" (file &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/ercsc4_3.pdf&lt;/a&gt;). Skymaps of the sources can be found in the "skymaps" subdirectory at &lt;a href="ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/"&gt;ftp://cdsarc.u-strasbg.fr/pub/cats/VIII/88/skymaps/&lt;/a&gt; . This present table contains the ERCSC 100-GHz source catalog. The parameter names as defined in the FITS files containing the source lists which were created by the Planck Project are given in parentheses and in capital letters at the end of the corresponding parameter descriptions below.</TD>
            <TD>NASA/GSFC HEASARC</TD>
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            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>ivo://nasa.heasarc/plancke100</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_plancke100&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/planck/plancke100.html</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>SZA31GHZ [1]</TD>
            <TD>Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog</TD>
            <TD>This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg&lt;sup&gt;2&lt;/sup&gt; of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(&gt;S) = (27.2 +/- 2.5) deg&lt;sup&gt;-2&lt;/sup&gt; * (S&lt;sub&gt;mJy&lt;/sub&gt;)^(-1.18 +/- 0.12)^ over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg&lt;sup&gt;-2&lt;/sup&gt;, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
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            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/sza31ghz.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SZA31GHZ [2]</TD>
            <TD>Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog</TD>
            <TD>This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg&lt;sup&gt;2&lt;/sup&gt; of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(&gt;S) = (27.2 +/- 2.5) deg&lt;sup&gt;-2&lt;/sup&gt; * (S&lt;sub&gt;mJy&lt;/sub&gt;)^(-1.18 +/- 0.12)^ over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg&lt;sup&gt;-2&lt;/sup&gt;, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/sza31ghz#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sza31ghz&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/sza31ghz.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SZA31GHZ [3]</TD>
            <TD>Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog</TD>
            <TD>This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg&lt;sup&gt;2&lt;/sup&gt; of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(&gt;S) = (27.2 +/- 2.5) deg&lt;sup&gt;-2&lt;/sup&gt; * (S&lt;sub&gt;mJy&lt;/sub&gt;)^(-1.18 +/- 0.12)^ over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg&lt;sup&gt;-2&lt;/sup&gt;, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
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            <TD />
            <TD>ivo://nasa.heasarc/sza31ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sza31ghz&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
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          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SZA31GHZ [1]</TD>
            <TD>Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog</TD>
            <TD>This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg&lt;sup&gt;2&lt;/sup&gt; of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(&gt;S) = (27.2 +/- 2.5) deg&lt;sup&gt;-2&lt;/sup&gt; * (S&lt;sub&gt;mJy&lt;/sub&gt;)^(-1.18 +/- 0.12)^ over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg&lt;sup&gt;-2&lt;/sup&gt;, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/sza31ghz#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>#Research#</TD>
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          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SZA31GHZ [2]</TD>
            <TD>Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog</TD>
            <TD>This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg&lt;sup&gt;2&lt;/sup&gt; of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(&gt;S) = (27.2 +/- 2.5) deg&lt;sup&gt;-2&lt;/sup&gt; * (S&lt;sub&gt;mJy&lt;/sub&gt;)^(-1.18 +/- 0.12)^ over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg&lt;sup&gt;-2&lt;/sup&gt;, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/sza31ghz#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
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            <TD>0.0166666666666666667</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sza31ghz&amp;</TD>
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            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/sza31ghz.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SZA31GHZ [3]</TD>
            <TD>Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog</TD>
            <TD>This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg&lt;sup&gt;2&lt;/sup&gt; of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(&gt;S) = (27.2 +/- 2.5) deg&lt;sup&gt;-2&lt;/sup&gt; * (S&lt;sub&gt;mJy&lt;/sub&gt;)^(-1.18 +/- 0.12)^ over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg&lt;sup&gt;-2&lt;/sup&gt;, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/sza31ghz#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sza31ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sza31ghz&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/sza31ghz.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>SZA31GHZ [1]</TD>
            <TD>Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog</TD>
            <TD>This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg&lt;sup&gt;2&lt;/sup&gt; of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(&gt;S) = (27.2 +/- 2.5) deg&lt;sup&gt;-2&lt;/sup&gt; * (S&lt;sub&gt;mJy&lt;/sub&gt;)^(-1.18 +/- 0.12)^ over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg&lt;sup&gt;-2&lt;/sup&gt;, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/sza31ghz#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sza31ghz</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=sza31ghz&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/sza31ghz.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>SZA31GHZ [2]</TD>
            <TD>Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog</TD>
            <TD>This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg&lt;sup&gt;2&lt;/sup&gt; of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(&gt;S) = (27.2 +/- 2.5) deg&lt;sup&gt;-2&lt;/sup&gt; * (S&lt;sub&gt;mJy&lt;/sub&gt;)^(-1.18 +/- 0.12)^ over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg&lt;sup&gt;-2&lt;/sup&gt;, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/sza31ghz#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sza31ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=sza31ghz&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/sza31ghz.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>SZA31GHZ [3]</TD>
            <TD>Sunyaev-Zeldovich Array 31-GHZ Radio Source Catalog</TD>
            <TD>This table contains the first sample of 31-GHz selected sources to flux levels of 1 mJy. From late-2005 to mid-2007, the Sunyaev-Zel'dovich Array (SZA) observed 7.7 deg&lt;sup&gt;2&lt;/sup&gt; of the sky at 31 GHz to a median rms of 0.18 mJy/beam. The authors identify 209 sources at greater than 5-sigma significance in the 31-GHz maps, ranging in flux from 0.7 mJy to ~200 mJy. Archival NRAO VLA Sky Survey (NVSS) data at 1.4 GHz and observations at 5 GHz with the Very Large Array are used to characterize the sources. The authors determine the maximum-likelihood integrated source count to be N(&gt;S) = (27.2 +/- 2.5) deg&lt;sup&gt;-2&lt;/sup&gt; * (S&lt;sub&gt;mJy&lt;/sub&gt;)^(-1.18 +/- 0.12)^ over the flux range 0.7 - 15 mJy. This result is significantly higher than predictions based on 1.4-GHz selected samples, a discrepancy which can be explained by a small shift in the spectral index distribution for faint 1.4-GHz sources. From comparison with previous measurements of sources within the central arcminute of massive clusters, the authors derive an overdensity of 6.8 +/- 4.4 deg&lt;sup&gt;-2&lt;/sup&gt;, relative to field sources. The SZA is an interferometer designed specifically for detecting and imaging the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters, and is located at the Owens Valley Radio Observatory (OVRO). The SZA is equipped with an 8-GHz wideband correlator and sensitive 26GHZ-36GHz receivers. The data in the SZA survey correspond to 1493 tracks taken between 2005 November 13 and 2007 July 25. The data in the CMB anisotropy measurements correspond to an additional 414 tracks taken between 2005 November 12 and 2007 October 25. The analysis in this paper refers to the full 1907 tracks taken in both observing modes. To complement the NVSS and FIRST observations, the authors obtained high-sensitivity VLA observations at 5 GHz between 2007 February 24 and 2007 April 15.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#Radio#</TD>
            <TD>ivo://nasa.heasarc/sza31ghz#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0166666666666666667</TD>
            <TD />
            <TD>ivo://nasa.heasarc/sza31ghz</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_sza31ghz&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/radio-catalog/sza31ghz.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WARPS2 [1]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog</TD>
            <TD>This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg&lt;sup&gt;2&lt;/sup&gt;. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z &gt;= 0.3 (29 not previously reported in the literature) and 11 clusters with z &gt;= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10&lt;sup&gt;-14&lt;/sup&gt; ergs/cm&lt;sup&gt;2&lt;/sup&gt;/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=warps2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WARPS2 [2]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog</TD>
            <TD>This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg&lt;sup&gt;2&lt;/sup&gt;. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z &gt;= 0.3 (29 not previously reported in the literature) and 11 clusters with z &gt;= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10&lt;sup&gt;-14&lt;/sup&gt; ergs/cm&lt;sup&gt;2&lt;/sup&gt;/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=warps2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WARPS2 [3]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog</TD>
            <TD>This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg&lt;sup&gt;2&lt;/sup&gt;. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z &gt;= 0.3 (29 not previously reported in the literature) and 11 clusters with z &gt;= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10&lt;sup&gt;-14&lt;/sup&gt; ergs/cm&lt;sup&gt;2&lt;/sup&gt;/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_warps2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps2.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WARPS2 [1]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog</TD>
            <TD>This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg&lt;sup&gt;2&lt;/sup&gt;. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z &gt;= 0.3 (29 not previously reported in the literature) and 11 clusters with z &gt;= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10&lt;sup&gt;-14&lt;/sup&gt; ergs/cm&lt;sup&gt;2&lt;/sup&gt;/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=warps2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WARPS2 [2]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog</TD>
            <TD>This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg&lt;sup&gt;2&lt;/sup&gt;. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z &gt;= 0.3 (29 not previously reported in the literature) and 11 clusters with z &gt;= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10&lt;sup&gt;-14&lt;/sup&gt; ergs/cm&lt;sup&gt;2&lt;/sup&gt;/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=warps2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WARPS2 [3]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog</TD>
            <TD>This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg&lt;sup&gt;2&lt;/sup&gt;. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z &gt;= 0.3 (29 not previously reported in the literature) and 11 clusters with z &gt;= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10&lt;sup&gt;-14&lt;/sup&gt; ergs/cm&lt;sup&gt;2&lt;/sup&gt;/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_warps2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps2.html</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>WARPS2 [1]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog</TD>
            <TD>This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg&lt;sup&gt;2&lt;/sup&gt;. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z &gt;= 0.3 (29 not previously reported in the literature) and 11 clusters with z &gt;= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10&lt;sup&gt;-14&lt;/sup&gt; ergs/cm&lt;sup&gt;2&lt;/sup&gt;/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps2#1</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps2</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/vo/cone/coneGet.pl?table=warps2&amp;</TD>
            <TD>180</TD>
            <TD>99999</TD>
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps2.html</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>WARPS2 [2]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog</TD>
            <TD>This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg&lt;sup&gt;2&lt;/sup&gt;. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z &gt;= 0.3 (29 not previously reported in the literature) and 11 clusters with z &gt;= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10&lt;sup&gt;-14&lt;/sup&gt; ergs/cm&lt;sup&gt;2&lt;/sup&gt;/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps2#2</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps2</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/getvotable.pl?name=warps2&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>WARPS2 [3]</TD>
            <TD>Wide Angle ROSAT Pointed Survey, Second Phase (WARPS-II) Clusters Catalog</TD>
            <TD>This table contains the galaxy cluster catalog from the second, larger phase of the Wide Angle ROSAT Pointed Survey (WARPS), an X-ray selected survey for high-redshift galaxy clusters. WARPS is among the largest deep X-ray cluster surveys and is being used to study the properties and evolution of galaxy clusters. The WARPS-II sample contains 125 clusters serendipitously detected in a survey of 301 ROSAT PSPC pointed observations and covers a sky area of 56.7 deg&lt;sup&gt;2&lt;/sup&gt;. Of these 125 clusters, 53 have not been previously reported in the literature. The authors have nearly complete spectroscopic follow-up of the clusters, which range in redshift from z = 0.029 to z = 0.92 with a median redshift of z = 0.29 and they find 59 clusters with z &gt;= 0.3 (29 not previously reported in the literature) and 11 clusters with z &gt;= 0.6 (6 not previously reported). They also define a statistically complete subsample of 102 clusters above a uniform flux limit of 6.5 x 10&lt;sup&gt;-14&lt;/sup&gt; ergs/cm&lt;sup&gt;2&lt;/sup&gt;/s (0.5 - 2.0 keV). In their paper, the authors also compare their redshifts, fluxes, and detection methods to other similar published cluster surveys and state that they find no serious issues with their measurements or completeness. The list of ROSAT pointings used in WARPS-II is given in Table 1 of the first reference paper. The WARPS-I cluster catalog (the second reference listed below) is also available in Browse as the WARPS table.</TD>
            <TD>NASA/GSFC HEASARC</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://nasa.heasarc/warps2#3</TD>
            <TD>2012-11-29T00:00:00Z</TD>
            <TD>#Survey Source#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD>0.0833333333333333333</TD>
            <TD />
            <TD>ivo://nasa.heasarc/warps2</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://heasarc.gsfc.nasa.gov/cgi-bin/W3Browse/w3query.pl?tablehead=name=heasarc_warps2&amp;Action=More+Options&amp;Action=Parameter+Search&amp;ConeAdd=1</TD>
            <TD />
            <TD />
            <TD>ivo://nasa.heasarc/ASD</TD>
            <TD>http://heasarc.gsfc.nasa.gov/W3Browse/rosat/warps2.html</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/420/1684 [1]</TD>
            <TD>End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)</TD>
            <TD>In this paper, we obtain the photometric and spectroscopic data from the SDSS DR7 (Abazajian et al., 2009, Cat. II/294) for all objects classified as `galaxy' (Strauss et al., 2002AJ....124.1810S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684#1</TD>
            <TD>2012-12-08T13:08:27Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/420/1684</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/1684</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/420/1684 [2]</TD>
            <TD>End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)</TD>
            <TD>In this paper, we obtain the photometric and spectroscopic data from the SDSS DR7 (Abazajian et al., 2009, Cat. II/294) for all objects classified as `galaxy' (Strauss et al., 2002AJ....124.1810S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684#2</TD>
            <TD>2012-12-08T13:08:27Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/420/1684&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/1684</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/420/1684 [table1]</TD>
            <TD>End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)</TD>
            <TD>In this paper, we obtain the photometric and spectroscopic data from the SDSS DR7 (Abazajian et al., 2009, Cat. II/294) for all objects classified as `galaxy' (Strauss et al., 2002AJ....124.1810S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684#table1</TD>
            <TD>2012-12-08T13:08:27Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/420/1684&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/1684</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/420/1684 [1]</TD>
            <TD>End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)</TD>
            <TD>In this paper, we obtain the photometric and spectroscopic data from the SDSS DR7 (Abazajian et al., 2009, Cat. II/294) for all objects classified as `galaxy' (Strauss et al., 2002AJ....124.1810S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684#1</TD>
            <TD>2012-12-08T13:08:27Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/420/1684</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/1684</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/420/1684 [2]</TD>
            <TD>End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)</TD>
            <TD>In this paper, we obtain the photometric and spectroscopic data from the SDSS DR7 (Abazajian et al., 2009, Cat. II/294) for all objects classified as `galaxy' (Strauss et al., 2002AJ....124.1810S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684#2</TD>
            <TD>2012-12-08T13:08:27Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/420/1684&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/1684</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/420/1684 [table1]</TD>
            <TD>End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)</TD>
            <TD>In this paper, we obtain the photometric and spectroscopic data from the SDSS DR7 (Abazajian et al., 2009, Cat. II/294) for all objects classified as `galaxy' (Strauss et al., 2002AJ....124.1810S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684#table1</TD>
            <TD>2012-12-08T13:08:27Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/420/1684&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/1684</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/420/1684 [1]</TD>
            <TD>End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)</TD>
            <TD>In this paper, we obtain the photometric and spectroscopic data from the SDSS DR7 (Abazajian et al., 2009, Cat. II/294) for all objects classified as `galaxy' (Strauss et al., 2002AJ....124.1810S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684#1</TD>
            <TD>2012-12-08T13:08:27Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/420/1684</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/1684</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/420/1684 [2]</TD>
            <TD>End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)</TD>
            <TD>In this paper, we obtain the photometric and spectroscopic data from the SDSS DR7 (Abazajian et al., 2009, Cat. II/294) for all objects classified as `galaxy' (Strauss et al., 2002AJ....124.1810S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684#2</TD>
            <TD>2012-12-08T13:08:27Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/420/1684&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/1684</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/420/1684 [table1]</TD>
            <TD>End of red sequence galaxies in Galaxy Zoo (Wong+, 2012)</TD>
            <TD>In this paper, we obtain the photometric and spectroscopic data from the SDSS DR7 (Abazajian et al., 2009, Cat. II/294) for all objects classified as `galaxy' (Strauss et al., 2002AJ....124.1810S).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684#table1</TD>
            <TD>2012-12-08T13:08:27Z</TD>
            <TD>#Galaxies:spectra#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/420/1684</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/420/1684&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/420/1684</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/316/326 [1]</TD>
            <TD>Redshifts of Ophiuchus region galaxies (Hasegawa+, 2000)</TD>
            <TD>The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre (l=0.5{deg}, b=9.5{deg}, cz=8500km/s) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 120{deg}x170{deg} area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219. In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100-{mu}m flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000km/s. Field galaxies are also distributed centred at 8500km/s. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0-5000km/s is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Bootes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326#1</TD>
            <TD>2011-09-14T19:27:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/316/326</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/316/326</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/316/326 [2]</TD>
            <TD>Redshifts of Ophiuchus region galaxies (Hasegawa+, 2000)</TD>
            <TD>The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre (l=0.5{deg}, b=9.5{deg}, cz=8500km/s) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 120{deg}x170{deg} area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219. In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100-{mu}m flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000km/s. Field galaxies are also distributed centred at 8500km/s. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0-5000km/s is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Bootes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326#2</TD>
            <TD>2011-09-14T19:27:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/316/326&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/316/326</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/316/326 [tablec1]</TD>
            <TD>Redshifts of Ophiuchus region galaxies (Hasegawa+, 2000)</TD>
            <TD>The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre (l=0.5{deg}, b=9.5{deg}, cz=8500km/s) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 120{deg}x170{deg} area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219. In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100-{mu}m flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000km/s. Field galaxies are also distributed centred at 8500km/s. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0-5000km/s is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Bootes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326#tablec1</TD>
            <TD>2011-09-14T19:27:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/316/326&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/316/326</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/316/326 [1]</TD>
            <TD>Redshifts of Ophiuchus region galaxies (Hasegawa+, 2000)</TD>
            <TD>The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre (l=0.5{deg}, b=9.5{deg}, cz=8500km/s) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 120{deg}x170{deg} area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219. In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100-{mu}m flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000km/s. Field galaxies are also distributed centred at 8500km/s. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0-5000km/s is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Bootes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326#1</TD>
            <TD>2011-09-14T19:27:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/316/326</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/316/326</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/316/326 [2]</TD>
            <TD>Redshifts of Ophiuchus region galaxies (Hasegawa+, 2000)</TD>
            <TD>The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre (l=0.5{deg}, b=9.5{deg}, cz=8500km/s) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 120{deg}x170{deg} area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219. In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100-{mu}m flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000km/s. Field galaxies are also distributed centred at 8500km/s. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0-5000km/s is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Bootes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326#2</TD>
            <TD>2011-09-14T19:27:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/316/326&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/316/326</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/316/326 [tablec1]</TD>
            <TD>Redshifts of Ophiuchus region galaxies (Hasegawa+, 2000)</TD>
            <TD>The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre (l=0.5{deg}, b=9.5{deg}, cz=8500km/s) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 120{deg}x170{deg} area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219. In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100-{mu}m flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000km/s. Field galaxies are also distributed centred at 8500km/s. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0-5000km/s is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Bootes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326#tablec1</TD>
            <TD>2011-09-14T19:27:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/316/326&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/316/326</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/316/326 [1]</TD>
            <TD>Redshifts of Ophiuchus region galaxies (Hasegawa+, 2000)</TD>
            <TD>The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre (l=0.5{deg}, b=9.5{deg}, cz=8500km/s) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 120{deg}x170{deg} area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219. In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100-{mu}m flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000km/s. Field galaxies are also distributed centred at 8500km/s. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0-5000km/s is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Bootes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326#1</TD>
            <TD>2011-09-14T19:27:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/316/326</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/316/326</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/316/326 [2]</TD>
            <TD>Redshifts of Ophiuchus region galaxies (Hasegawa+, 2000)</TD>
            <TD>The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre (l=0.5{deg}, b=9.5{deg}, cz=8500km/s) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 120{deg}x170{deg} area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219. In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100-{mu}m flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000km/s. Field galaxies are also distributed centred at 8500km/s. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0-5000km/s is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Bootes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326#2</TD>
            <TD>2011-09-14T19:27:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/316/326&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/316/326</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/316/326 [tablec1]</TD>
            <TD>Redshifts of Ophiuchus region galaxies (Hasegawa+, 2000)</TD>
            <TD>The large-scale structure around the Ophiuchus cluster of galaxies in the vicinity of the Galactic Centre (l=0.5{deg}, b=9.5{deg}, cz=8500km/s) is investigated on the basis of a galaxy survey and spectroscopic observations made for a 120{deg}x170{deg} area. The galaxy survey was performed using six ESO/SERC Sky Survey Atlas films, and 4021 galaxies were detected in total. Recession velocities were newly obtained for 179 galaxies to make the total number of galaxies in the survey area with known velocities 219. In the distribution of bright galaxies, we identified seven new clumps of galaxies. Comparing the surface number density of bright galaxies with the Galactic extinction, which is estimated from the 100-{mu}m flux density in the IRAS Sky Survey Atlas, we demonstrate that the seven clumps are not spurious as a result of the inhomogeneity of the Galactic extinction. Among the seven clumps, two are found to be clusters and four to be groups on the basis of the histogram of recession velocities and the number of member galaxies. The Ophiuchus cluster, two newly identified clusters, and four groups are all concentrated at 9000km/s. Field galaxies are also distributed centred at 8500km/s. Hence field galaxies occupy a common three-dimensional region with galaxies in the clusters and groups, and altogether they form a large-scale structure of supercluster size. As opposed to the overdensity in the supercluster region, the mean number density of galaxies in the velocity range 0-5000km/s is only 25 per cent of the mean number density of the Universe, comparable with the density of the well-known Bootes void. Hence this nearby three-dimensional region in Ophiuchus is a void of galaxies also.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326#tablec1</TD>
            <TD>2011-09-14T19:27:43Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-Oct-2000</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/316/326</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/316/326&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/316/326</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VI/112 [1]</TD>
            <TD>Optical Imaging of 57 spiral galaxies (Knapen+ 2004)</TD>
            <TD>All B, R, I and H{alpha} images described in the paper are presented electronically, along with the K_s_ images from Paper I (Knapen et al., 2003MNRAS.344..527K). The images are in FITS format, with basic parameters like pixel scale and calibration described in the FITS headers. All images have been reduced to the equivalent of 1 second exposure time. The filenames have the basic format ngc1234X.fits, where digits 4-7 identify the galaxy's NGC number, which is followed by a description of the filter used (B, V, R, I, K, Ha [not continuum subtracted], Ha_cs _[continuum subtracted], or HaCont for the 6470/115 continuum filter). Further details on, e.g., exposure times, telescopes and filters used, or Ha continuum subtraction can be found in the papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VI/112#1</TD>
            <TD>2011-09-14T19:56:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2004</TD>
            <TD>ivo://CDS.VizieR/VI/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VI/112</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/112</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VI/112 [2]</TD>
            <TD>Optical Imaging of 57 spiral galaxies (Knapen+ 2004)</TD>
            <TD>All B, R, I and H{alpha} images described in the paper are presented electronically, along with the K_s_ images from Paper I (Knapen et al., 2003MNRAS.344..527K). The images are in FITS format, with basic parameters like pixel scale and calibration described in the FITS headers. All images have been reduced to the equivalent of 1 second exposure time. The filenames have the basic format ngc1234X.fits, where digits 4-7 identify the galaxy's NGC number, which is followed by a description of the filter used (B, V, R, I, K, Ha [not continuum subtracted], Ha_cs _[continuum subtracted], or HaCont for the 6470/115 continuum filter). Further details on, e.g., exposure times, telescopes and filters used, or Ha continuum subtraction can be found in the papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VI/112#2</TD>
            <TD>2011-09-14T19:56:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2004</TD>
            <TD>ivo://CDS.VizieR/VI/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VI/112&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/112</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VI/112 [table]</TD>
            <TD>Optical Imaging of 57 spiral galaxies (Knapen+ 2004)</TD>
            <TD>All B, R, I and H{alpha} images described in the paper are presented electronically, along with the K_s_ images from Paper I (Knapen et al., 2003MNRAS.344..527K). The images are in FITS format, with basic parameters like pixel scale and calibration described in the FITS headers. All images have been reduced to the equivalent of 1 second exposure time. The filenames have the basic format ngc1234X.fits, where digits 4-7 identify the galaxy's NGC number, which is followed by a description of the filter used (B, V, R, I, K, Ha [not continuum subtracted], Ha_cs _[continuum subtracted], or HaCont for the 6470/115 continuum filter). Further details on, e.g., exposure times, telescopes and filters used, or Ha continuum subtraction can be found in the papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VI/112#table</TD>
            <TD>2011-09-14T19:56:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2004</TD>
            <TD>ivo://CDS.VizieR/VI/112</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VI/112&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/112</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VI/112 [1]</TD>
            <TD>Optical Imaging of 57 spiral galaxies (Knapen+ 2004)</TD>
            <TD>All B, R, I and H{alpha} images described in the paper are presented electronically, along with the K_s_ images from Paper I (Knapen et al., 2003MNRAS.344..527K). The images are in FITS format, with basic parameters like pixel scale and calibration described in the FITS headers. All images have been reduced to the equivalent of 1 second exposure time. The filenames have the basic format ngc1234X.fits, where digits 4-7 identify the galaxy's NGC number, which is followed by a description of the filter used (B, V, R, I, K, Ha [not continuum subtracted], Ha_cs _[continuum subtracted], or HaCont for the 6470/115 continuum filter). Further details on, e.g., exposure times, telescopes and filters used, or Ha continuum subtraction can be found in the papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VI/112#1</TD>
            <TD>2011-09-14T19:56:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2004</TD>
            <TD>ivo://CDS.VizieR/VI/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VI/112</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/112</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VI/112 [2]</TD>
            <TD>Optical Imaging of 57 spiral galaxies (Knapen+ 2004)</TD>
            <TD>All B, R, I and H{alpha} images described in the paper are presented electronically, along with the K_s_ images from Paper I (Knapen et al., 2003MNRAS.344..527K). The images are in FITS format, with basic parameters like pixel scale and calibration described in the FITS headers. All images have been reduced to the equivalent of 1 second exposure time. The filenames have the basic format ngc1234X.fits, where digits 4-7 identify the galaxy's NGC number, which is followed by a description of the filter used (B, V, R, I, K, Ha [not continuum subtracted], Ha_cs _[continuum subtracted], or HaCont for the 6470/115 continuum filter). Further details on, e.g., exposure times, telescopes and filters used, or Ha continuum subtraction can be found in the papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VI/112#2</TD>
            <TD>2011-09-14T19:56:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2004</TD>
            <TD>ivo://CDS.VizieR/VI/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VI/112&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/112</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VI/112 [table]</TD>
            <TD>Optical Imaging of 57 spiral galaxies (Knapen+ 2004)</TD>
            <TD>All B, R, I and H{alpha} images described in the paper are presented electronically, along with the K_s_ images from Paper I (Knapen et al., 2003MNRAS.344..527K). The images are in FITS format, with basic parameters like pixel scale and calibration described in the FITS headers. All images have been reduced to the equivalent of 1 second exposure time. The filenames have the basic format ngc1234X.fits, where digits 4-7 identify the galaxy's NGC number, which is followed by a description of the filter used (B, V, R, I, K, Ha [not continuum subtracted], Ha_cs _[continuum subtracted], or HaCont for the 6470/115 continuum filter). Further details on, e.g., exposure times, telescopes and filters used, or Ha continuum subtraction can be found in the papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VI/112#table</TD>
            <TD>2011-09-14T19:56:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2004</TD>
            <TD>ivo://CDS.VizieR/VI/112</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VI/112&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/112</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>VI/112 [1]</TD>
            <TD>Optical Imaging of 57 spiral galaxies (Knapen+ 2004)</TD>
            <TD>All B, R, I and H{alpha} images described in the paper are presented electronically, along with the K_s_ images from Paper I (Knapen et al., 2003MNRAS.344..527K). The images are in FITS format, with basic parameters like pixel scale and calibration described in the FITS headers. All images have been reduced to the equivalent of 1 second exposure time. The filenames have the basic format ngc1234X.fits, where digits 4-7 identify the galaxy's NGC number, which is followed by a description of the filter used (B, V, R, I, K, Ha [not continuum subtracted], Ha_cs _[continuum subtracted], or HaCont for the 6470/115 continuum filter). Further details on, e.g., exposure times, telescopes and filters used, or Ha continuum subtraction can be found in the papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VI/112#1</TD>
            <TD>2011-09-14T19:56:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2004</TD>
            <TD>ivo://CDS.VizieR/VI/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=VI/112</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/112</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>VI/112 [2]</TD>
            <TD>Optical Imaging of 57 spiral galaxies (Knapen+ 2004)</TD>
            <TD>All B, R, I and H{alpha} images described in the paper are presented electronically, along with the K_s_ images from Paper I (Knapen et al., 2003MNRAS.344..527K). The images are in FITS format, with basic parameters like pixel scale and calibration described in the FITS headers. All images have been reduced to the equivalent of 1 second exposure time. The filenames have the basic format ngc1234X.fits, where digits 4-7 identify the galaxy's NGC number, which is followed by a description of the filter used (B, V, R, I, K, Ha [not continuum subtracted], Ha_cs _[continuum subtracted], or HaCont for the 6470/115 continuum filter). Further details on, e.g., exposure times, telescopes and filters used, or Ha continuum subtraction can be found in the papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VI/112#2</TD>
            <TD>2011-09-14T19:56:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2004</TD>
            <TD>ivo://CDS.VizieR/VI/112</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=VI/112&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/112</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>VI/112 [table]</TD>
            <TD>Optical Imaging of 57 spiral galaxies (Knapen+ 2004)</TD>
            <TD>All B, R, I and H{alpha} images described in the paper are presented electronically, along with the K_s_ images from Paper I (Knapen et al., 2003MNRAS.344..527K). The images are in FITS format, with basic parameters like pixel scale and calibration described in the FITS headers. All images have been reduced to the equivalent of 1 second exposure time. The filenames have the basic format ngc1234X.fits, where digits 4-7 identify the galaxy's NGC number, which is followed by a description of the filter used (B, V, R, I, K, Ha [not continuum subtracted], Ha_cs _[continuum subtracted], or HaCont for the 6470/115 continuum filter). Further details on, e.g., exposure times, telescopes and filters used, or Ha continuum subtraction can be found in the papers.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/VI/112#table</TD>
            <TD>2011-09-14T19:56:38Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Sep-2004</TD>
            <TD>ivo://CDS.VizieR/VI/112</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=VI/112&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?VI/112</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/607/202 [1]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#1</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/607/202</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/607/202 [2]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#2</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/607/202&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/607/202 [table1]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#table1</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/607/202&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/607/202 [table2]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#table2</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/607/202&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/607/202 [1]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#1</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/607/202</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/607/202 [2]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#2</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/607/202&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/607/202 [table1]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#table1</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/607/202&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/607/202 [table2]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#table2</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/607/202&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/607/202 [1]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#1</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/607/202</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/607/202 [2]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#2</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/607/202&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/607/202 [table1]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#table1</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/607/202&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/607/202 [table2]</TD>
            <TD>Redshift survey of nearby galaxy groups (Mahdavi+, 2004)</TD>
            <TD>We obtained spectra of the 2419 target galaxies with the FAST single object spectrograph on the 1.5m Tillinghast Reflector at Whipple Observatory on Mount Hopkins, Arizona.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202#table2</TD>
            <TD>2011-09-14T19:57:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Nov-2004</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/607/202</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/607/202&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/607/202</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/128/67 [1]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#1</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/128/67</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/128/67 [2]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#2</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/128/67&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/128/67 [table1]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#table1</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/128/67&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/128/67 [table2]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#table2</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/128/67&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/128/67 [1]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#1</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
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            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/128/67</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/128/67 [2]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#2</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/128/67&amp;</TD>
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            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/128/67 [table1]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#table1</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/128/67&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/128/67 [table2]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#table2</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
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            <TD>#Research#</TD>
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            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/128/67&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/128/67 [1]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#1</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
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            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/128/67</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/128/67 [2]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#2</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
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            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/128/67&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/128/67 [table1]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#table1</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/128/67&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/128/67 [table2]</TD>
            <TD>BVR photometry of Abell 85 (Slezak+ 1998)</TD>
            <TD>We present two catalogues of galaxies in the direction of the rich cluster ABCG 85. The first one includes 4232 galaxies located in a region +/-1{deg} from the cluster centre. It has been obtained from a list of more than 25000 galaxy candidates detected by scanning a Schmidt photographic plate taken in the B_J_ band. Positions are very accurate in this catalogue but magnitudes are not. This led us to perform CCD imaging observations in the V and R bands to calibrate these photographic magnitudes. A second catalogue (805 galaxies) gives a list of galaxies with CCD magnitudes in the V and R bands for a much smaller region in the centre of the cluster. These two catalogues will be combined with a redshift catalogue of 509 galaxies by Durret et al. (1997, subm.) to investigate the cluster properties at optical wavelengths Durret et al. (1997, subm.), as a complement to our previous X-ray studies (Pislar et al., 1997A&amp;A...322...53P; Lima-Neto et al., 1997A&amp;A...327...81L).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67#table2</TD>
            <TD>2011-09-14T19:58:14Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Jun-1997</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/128/67</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/128/67&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/128/67</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/367/1261 [1]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/367/1261#1</TD>
            <TD>2011-09-14T19:58:30Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/367/1261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/367/1261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/367/1261</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/367/1261 [2]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/367/1261#2</TD>
            <TD>2011-09-14T19:58:30Z</TD>
            <TD>#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/367/1261&amp;</TD>
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            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/367/1261 [table1]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
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            <TD>#Optical#</TD>
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            <TD>26-Sep-2006</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/367/1261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/367/1261 [tab3-18]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>26-Sep-2006</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/367/1261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/367/1261</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/367/1261 [1]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>26-Sep-2006</TD>
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            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/367/1261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/367/1261</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/367/1261 [2]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/367/1261#2</TD>
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            <TD>ivo://CDS.VizieR/J/MNRAS/367/1261</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/367/1261&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/367/1261</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/367/1261 [table1]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
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            <TD>26-Sep-2006</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/367/1261&amp;</TD>
            <TD>180</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/367/1261 [tab3-18]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
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            <TD>#Optical#</TD>
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            <TD>26-Sep-2006</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/367/1261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/367/1261</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/367/1261 [1]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>26-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/367/1261</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/367/1261</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/367/1261</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/367/1261 [2]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
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            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/367/1261&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/367/1261</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/367/1261 [table1]</TD>
            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>26-Sep-2006</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/367/1261&amp;</TD>
            <TD>180</TD>
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            <TD>Redshift survey in 15 quasar fields (Morris+, 2006)</TD>
            <TD>We investigate the relative distribution of the gaseous contents of the Universe (as traced by a sample of Ly{alpha} absorbers), and the luminous baryonic matter (as traced by a redshift survey of galaxies in the same volume searched for Ly{alpha} absorbers), along 16 lines of sight (LOS) between redshifts 0 and 1. Our galaxy redshift survey was made with the multi-object spectrograph on the Canada-France-Hawaii Telescope and, when combined with galaxies from the literature in the same LOS, gives us a galaxy sample of 636 objects. By combining this with an absorption-line sample of 406 absorbing systems drawn from published works, we are able to study the relationship between gas and galaxies over the latter half of the age of the Universe.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD />
            <TD>26-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/367/1261</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/367/1261&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/367/1261</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/396/397 [1]</TD>
            <TD>Deep cluster survey in Chandra archival data (Boschin+, 2002)</TD>
            <TD>I present the first results of a search for clusters of galaxies in Chandra ACIS pointed observations at high galactic latitude with exposure times larger than 10ks. The survey is being carried out using the Voronoi Tessellation and Percolation technique, which is particularly suited for the detection and accurate quantification of extended and/or low surface brightness emission in X-ray imaging observations. A new catalogue of 36 cluster candidates has been created from 5.55deg^2^ of surveyed area. Five of these candidates have already been associated to visible enhancements of the projected galaxy distribution in low deepness DSS-II fields and are probably low-to moderate redshift systems. Three of the candidates have been identified in previous ROSAT-based surveys. I show that a significative fraction (30-40%) of the candidate clusters are probably intermediate to high redshift systems. In this paper I publish the catalogue of these first candidate clusters. I also derive the number counts of clusters and compare it with the results of deep ROSAT-based cluster surveys.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397#1</TD>
            <TD>2011-09-14T19:58:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/396/397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/396/397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/396/397 [2]</TD>
            <TD>Deep cluster survey in Chandra archival data (Boschin+, 2002)</TD>
            <TD>I present the first results of a search for clusters of galaxies in Chandra ACIS pointed observations at high galactic latitude with exposure times larger than 10ks. The survey is being carried out using the Voronoi Tessellation and Percolation technique, which is particularly suited for the detection and accurate quantification of extended and/or low surface brightness emission in X-ray imaging observations. A new catalogue of 36 cluster candidates has been created from 5.55deg^2^ of surveyed area. Five of these candidates have already been associated to visible enhancements of the projected galaxy distribution in low deepness DSS-II fields and are probably low-to moderate redshift systems. Three of the candidates have been identified in previous ROSAT-based surveys. I show that a significative fraction (30-40%) of the candidate clusters are probably intermediate to high redshift systems. In this paper I publish the catalogue of these first candidate clusters. I also derive the number counts of clusters and compare it with the results of deep ROSAT-based cluster surveys.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397#2</TD>
            <TD>2011-09-14T19:58:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/396/397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/396/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/396/397 [table1]</TD>
            <TD>Deep cluster survey in Chandra archival data (Boschin+, 2002)</TD>
            <TD>I present the first results of a search for clusters of galaxies in Chandra ACIS pointed observations at high galactic latitude with exposure times larger than 10ks. The survey is being carried out using the Voronoi Tessellation and Percolation technique, which is particularly suited for the detection and accurate quantification of extended and/or low surface brightness emission in X-ray imaging observations. A new catalogue of 36 cluster candidates has been created from 5.55deg^2^ of surveyed area. Five of these candidates have already been associated to visible enhancements of the projected galaxy distribution in low deepness DSS-II fields and are probably low-to moderate redshift systems. Three of the candidates have been identified in previous ROSAT-based surveys. I show that a significative fraction (30-40%) of the candidate clusters are probably intermediate to high redshift systems. In this paper I publish the catalogue of these first candidate clusters. I also derive the number counts of clusters and compare it with the results of deep ROSAT-based cluster surveys.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397#table1</TD>
            <TD>2011-09-14T19:58:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/396/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/396/397</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/396/397 [1]</TD>
            <TD>Deep cluster survey in Chandra archival data (Boschin+, 2002)</TD>
            <TD>I present the first results of a search for clusters of galaxies in Chandra ACIS pointed observations at high galactic latitude with exposure times larger than 10ks. The survey is being carried out using the Voronoi Tessellation and Percolation technique, which is particularly suited for the detection and accurate quantification of extended and/or low surface brightness emission in X-ray imaging observations. A new catalogue of 36 cluster candidates has been created from 5.55deg^2^ of surveyed area. Five of these candidates have already been associated to visible enhancements of the projected galaxy distribution in low deepness DSS-II fields and are probably low-to moderate redshift systems. Three of the candidates have been identified in previous ROSAT-based surveys. I show that a significative fraction (30-40%) of the candidate clusters are probably intermediate to high redshift systems. In this paper I publish the catalogue of these first candidate clusters. I also derive the number counts of clusters and compare it with the results of deep ROSAT-based cluster surveys.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397#1</TD>
            <TD>2011-09-14T19:58:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/396/397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/396/397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/396/397 [2]</TD>
            <TD>Deep cluster survey in Chandra archival data (Boschin+, 2002)</TD>
            <TD>I present the first results of a search for clusters of galaxies in Chandra ACIS pointed observations at high galactic latitude with exposure times larger than 10ks. The survey is being carried out using the Voronoi Tessellation and Percolation technique, which is particularly suited for the detection and accurate quantification of extended and/or low surface brightness emission in X-ray imaging observations. A new catalogue of 36 cluster candidates has been created from 5.55deg^2^ of surveyed area. Five of these candidates have already been associated to visible enhancements of the projected galaxy distribution in low deepness DSS-II fields and are probably low-to moderate redshift systems. Three of the candidates have been identified in previous ROSAT-based surveys. I show that a significative fraction (30-40%) of the candidate clusters are probably intermediate to high redshift systems. In this paper I publish the catalogue of these first candidate clusters. I also derive the number counts of clusters and compare it with the results of deep ROSAT-based cluster surveys.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397#2</TD>
            <TD>2011-09-14T19:58:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/396/397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/396/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/396/397 [table1]</TD>
            <TD>Deep cluster survey in Chandra archival data (Boschin+, 2002)</TD>
            <TD>I present the first results of a search for clusters of galaxies in Chandra ACIS pointed observations at high galactic latitude with exposure times larger than 10ks. The survey is being carried out using the Voronoi Tessellation and Percolation technique, which is particularly suited for the detection and accurate quantification of extended and/or low surface brightness emission in X-ray imaging observations. A new catalogue of 36 cluster candidates has been created from 5.55deg^2^ of surveyed area. Five of these candidates have already been associated to visible enhancements of the projected galaxy distribution in low deepness DSS-II fields and are probably low-to moderate redshift systems. Three of the candidates have been identified in previous ROSAT-based surveys. I show that a significative fraction (30-40%) of the candidate clusters are probably intermediate to high redshift systems. In this paper I publish the catalogue of these first candidate clusters. I also derive the number counts of clusters and compare it with the results of deep ROSAT-based cluster surveys.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397#table1</TD>
            <TD>2011-09-14T19:58:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/396/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/396/397</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/396/397 [1]</TD>
            <TD>Deep cluster survey in Chandra archival data (Boschin+, 2002)</TD>
            <TD>I present the first results of a search for clusters of galaxies in Chandra ACIS pointed observations at high galactic latitude with exposure times larger than 10ks. The survey is being carried out using the Voronoi Tessellation and Percolation technique, which is particularly suited for the detection and accurate quantification of extended and/or low surface brightness emission in X-ray imaging observations. A new catalogue of 36 cluster candidates has been created from 5.55deg^2^ of surveyed area. Five of these candidates have already been associated to visible enhancements of the projected galaxy distribution in low deepness DSS-II fields and are probably low-to moderate redshift systems. Three of the candidates have been identified in previous ROSAT-based surveys. I show that a significative fraction (30-40%) of the candidate clusters are probably intermediate to high redshift systems. In this paper I publish the catalogue of these first candidate clusters. I also derive the number counts of clusters and compare it with the results of deep ROSAT-based cluster surveys.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397#1</TD>
            <TD>2011-09-14T19:58:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/396/397</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/396/397</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/396/397 [2]</TD>
            <TD>Deep cluster survey in Chandra archival data (Boschin+, 2002)</TD>
            <TD>I present the first results of a search for clusters of galaxies in Chandra ACIS pointed observations at high galactic latitude with exposure times larger than 10ks. The survey is being carried out using the Voronoi Tessellation and Percolation technique, which is particularly suited for the detection and accurate quantification of extended and/or low surface brightness emission in X-ray imaging observations. A new catalogue of 36 cluster candidates has been created from 5.55deg^2^ of surveyed area. Five of these candidates have already been associated to visible enhancements of the projected galaxy distribution in low deepness DSS-II fields and are probably low-to moderate redshift systems. Three of the candidates have been identified in previous ROSAT-based surveys. I show that a significative fraction (30-40%) of the candidate clusters are probably intermediate to high redshift systems. In this paper I publish the catalogue of these first candidate clusters. I also derive the number counts of clusters and compare it with the results of deep ROSAT-based cluster surveys.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397#2</TD>
            <TD>2011-09-14T19:58:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/396/397&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/396/397</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/396/397 [table1]</TD>
            <TD>Deep cluster survey in Chandra archival data (Boschin+, 2002)</TD>
            <TD>I present the first results of a search for clusters of galaxies in Chandra ACIS pointed observations at high galactic latitude with exposure times larger than 10ks. The survey is being carried out using the Voronoi Tessellation and Percolation technique, which is particularly suited for the detection and accurate quantification of extended and/or low surface brightness emission in X-ray imaging observations. A new catalogue of 36 cluster candidates has been created from 5.55deg^2^ of surveyed area. Five of these candidates have already been associated to visible enhancements of the projected galaxy distribution in low deepness DSS-II fields and are probably low-to moderate redshift systems. Three of the candidates have been identified in previous ROSAT-based surveys. I show that a significative fraction (30-40%) of the candidate clusters are probably intermediate to high redshift systems. In this paper I publish the catalogue of these first candidate clusters. I also derive the number counts of clusters and compare it with the results of deep ROSAT-based cluster surveys.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397#table1</TD>
            <TD>2011-09-14T19:58:48Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>02-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/396/397</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/396/397&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/396/397</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/459/L13 [1]</TD>
            <TD>A composite HII region luminosity function (Bradley+, 2006)</TD>
            <TD>HII region catalogues for 57 face on spiral galaxies within v&lt;2600km/s are presented. For each galaxy the following information is given for the HII regions; position from the galaxy centre, logarithm of the integrated luminosity is erg/s (which is 10^-7^W in SI units), area of the HII region in units of pc^2^ and the value of the local background.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13#1</TD>
            <TD>2011-09-14T19:59:01Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/459/L13</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/L13</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/459/L13 [2]</TD>
            <TD>A composite HII region luminosity function (Bradley+, 2006)</TD>
            <TD>HII region catalogues for 57 face on spiral galaxies within v&lt;2600km/s are presented. For each galaxy the following information is given for the HII regions; position from the galaxy centre, logarithm of the integrated luminosity is erg/s (which is 10^-7^W in SI units), area of the HII region in units of pc^2^ and the value of the local background.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13#2</TD>
            <TD>2011-09-14T19:59:01Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/459/L13&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/L13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/459/L13 [galaxies]</TD>
            <TD>A composite HII region luminosity function (Bradley+, 2006)</TD>
            <TD>HII region catalogues for 57 face on spiral galaxies within v&lt;2600km/s are presented. For each galaxy the following information is given for the HII regions; position from the galaxy centre, logarithm of the integrated luminosity is erg/s (which is 10^-7^W in SI units), area of the HII region in units of pc^2^ and the value of the local background.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13#galaxies</TD>
            <TD>2011-09-14T19:59:01Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/459/L13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/L13</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/459/L13 [1]</TD>
            <TD>A composite HII region luminosity function (Bradley+, 2006)</TD>
            <TD>HII region catalogues for 57 face on spiral galaxies within v&lt;2600km/s are presented. For each galaxy the following information is given for the HII regions; position from the galaxy centre, logarithm of the integrated luminosity is erg/s (which is 10^-7^W in SI units), area of the HII region in units of pc^2^ and the value of the local background.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13#1</TD>
            <TD>2011-09-14T19:59:01Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/459/L13</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/L13</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/459/L13 [2]</TD>
            <TD>A composite HII region luminosity function (Bradley+, 2006)</TD>
            <TD>HII region catalogues for 57 face on spiral galaxies within v&lt;2600km/s are presented. For each galaxy the following information is given for the HII regions; position from the galaxy centre, logarithm of the integrated luminosity is erg/s (which is 10^-7^W in SI units), area of the HII region in units of pc^2^ and the value of the local background.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13#2</TD>
            <TD>2011-09-14T19:59:01Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/459/L13&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/L13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/459/L13 [galaxies]</TD>
            <TD>A composite HII region luminosity function (Bradley+, 2006)</TD>
            <TD>HII region catalogues for 57 face on spiral galaxies within v&lt;2600km/s are presented. For each galaxy the following information is given for the HII regions; position from the galaxy centre, logarithm of the integrated luminosity is erg/s (which is 10^-7^W in SI units), area of the HII region in units of pc^2^ and the value of the local background.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13#galaxies</TD>
            <TD>2011-09-14T19:59:01Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/459/L13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/L13</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/459/L13 [1]</TD>
            <TD>A composite HII region luminosity function (Bradley+, 2006)</TD>
            <TD>HII region catalogues for 57 face on spiral galaxies within v&lt;2600km/s are presented. For each galaxy the following information is given for the HII regions; position from the galaxy centre, logarithm of the integrated luminosity is erg/s (which is 10^-7^W in SI units), area of the HII region in units of pc^2^ and the value of the local background.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13#1</TD>
            <TD>2011-09-14T19:59:01Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/459/L13</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/L13</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/459/L13 [2]</TD>
            <TD>A composite HII region luminosity function (Bradley+, 2006)</TD>
            <TD>HII region catalogues for 57 face on spiral galaxies within v&lt;2600km/s are presented. For each galaxy the following information is given for the HII regions; position from the galaxy centre, logarithm of the integrated luminosity is erg/s (which is 10^-7^W in SI units), area of the HII region in units of pc^2^ and the value of the local background.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13#2</TD>
            <TD>2011-09-14T19:59:01Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/459/L13&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/L13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/459/L13 [galaxies]</TD>
            <TD>A composite HII region luminosity function (Bradley+, 2006)</TD>
            <TD>HII region catalogues for 57 face on spiral galaxies within v&lt;2600km/s are presented. For each galaxy the following information is given for the HII regions; position from the galaxy centre, logarithm of the integrated luminosity is erg/s (which is 10^-7^W in SI units), area of the HII region in units of pc^2^ and the value of the local background.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13#galaxies</TD>
            <TD>2011-09-14T19:59:01Z</TD>
            <TD>#Photometry:narrow-band#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>22-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/459/L13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/459/L13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/459/L13</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/456/905 [1]</TD>
            <TD>JKs, i'g'r' photometry of C stars in NGC 6822 (Demers+, 2006)</TD>
            <TD>From a 2{deg}x2{deg} survey of NGC 6822 we have previously established that this Local Group dwarf irregular galaxy possesses a huge spheroid having more than one degree in length. This spheroid is in rotation but its rotation curve is known only within ~15' from the center. It is therefore critical to identify bright stars belonging to the spheroid to characterize, as far as possible, its outer kinematics. We use the new wide field near infrared imager CPAPIR, operated by the SMARTS consortium, to acquire J, K_s_ images of two 34.8'x34.8' areas in the outer spheroid to search for C stars. The colour diagram of the fields allows the identification of 192 C stars candidates but a study of the FWHM of the images permits the rejection of numerous non-stellar objects with colours similar to C stars. We are left with 75 new C stars, their mean K_s_ magnitude and mean colour are similar to the bulk of known NGC 6822 C stars. This outer spheroid survey confirms that the intermediate-age AGB stars are a major contributor to the stellar populations of the spheroid. The discovery of some 50 C stars well beyond the limit of the previously known rotation curve calls for a promising spectroscopic follow-up to a major axis distance of 40'.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905#1</TD>
            <TD>2011-09-14T19:59:21Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/456/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/456/905 [2]</TD>
            <TD>JKs, i'g'r' photometry of C stars in NGC 6822 (Demers+, 2006)</TD>
            <TD>From a 2{deg}x2{deg} survey of NGC 6822 we have previously established that this Local Group dwarf irregular galaxy possesses a huge spheroid having more than one degree in length. This spheroid is in rotation but its rotation curve is known only within ~15' from the center. It is therefore critical to identify bright stars belonging to the spheroid to characterize, as far as possible, its outer kinematics. We use the new wide field near infrared imager CPAPIR, operated by the SMARTS consortium, to acquire J, K_s_ images of two 34.8'x34.8' areas in the outer spheroid to search for C stars. The colour diagram of the fields allows the identification of 192 C stars candidates but a study of the FWHM of the images permits the rejection of numerous non-stellar objects with colours similar to C stars. We are left with 75 new C stars, their mean K_s_ magnitude and mean colour are similar to the bulk of known NGC 6822 C stars. This outer spheroid survey confirms that the intermediate-age AGB stars are a major contributor to the stellar populations of the spheroid. The discovery of some 50 C stars well beyond the limit of the previously known rotation curve calls for a promising spectroscopic follow-up to a major axis distance of 40'.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905#2</TD>
            <TD>2011-09-14T19:59:21Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/456/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/456/905 [Cstars]</TD>
            <TD>JKs, i'g'r' photometry of C stars in NGC 6822 (Demers+, 2006)</TD>
            <TD>From a 2{deg}x2{deg} survey of NGC 6822 we have previously established that this Local Group dwarf irregular galaxy possesses a huge spheroid having more than one degree in length. This spheroid is in rotation but its rotation curve is known only within ~15' from the center. It is therefore critical to identify bright stars belonging to the spheroid to characterize, as far as possible, its outer kinematics. We use the new wide field near infrared imager CPAPIR, operated by the SMARTS consortium, to acquire J, K_s_ images of two 34.8'x34.8' areas in the outer spheroid to search for C stars. The colour diagram of the fields allows the identification of 192 C stars candidates but a study of the FWHM of the images permits the rejection of numerous non-stellar objects with colours similar to C stars. We are left with 75 new C stars, their mean K_s_ magnitude and mean colour are similar to the bulk of known NGC 6822 C stars. This outer spheroid survey confirms that the intermediate-age AGB stars are a major contributor to the stellar populations of the spheroid. The discovery of some 50 C stars well beyond the limit of the previously known rotation curve calls for a promising spectroscopic follow-up to a major axis distance of 40'.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905#Cstars</TD>
            <TD>2011-09-14T19:59:21Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/456/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/456/905 [1]</TD>
            <TD>JKs, i'g'r' photometry of C stars in NGC 6822 (Demers+, 2006)</TD>
            <TD>From a 2{deg}x2{deg} survey of NGC 6822 we have previously established that this Local Group dwarf irregular galaxy possesses a huge spheroid having more than one degree in length. This spheroid is in rotation but its rotation curve is known only within ~15' from the center. It is therefore critical to identify bright stars belonging to the spheroid to characterize, as far as possible, its outer kinematics. We use the new wide field near infrared imager CPAPIR, operated by the SMARTS consortium, to acquire J, K_s_ images of two 34.8'x34.8' areas in the outer spheroid to search for C stars. The colour diagram of the fields allows the identification of 192 C stars candidates but a study of the FWHM of the images permits the rejection of numerous non-stellar objects with colours similar to C stars. We are left with 75 new C stars, their mean K_s_ magnitude and mean colour are similar to the bulk of known NGC 6822 C stars. This outer spheroid survey confirms that the intermediate-age AGB stars are a major contributor to the stellar populations of the spheroid. The discovery of some 50 C stars well beyond the limit of the previously known rotation curve calls for a promising spectroscopic follow-up to a major axis distance of 40'.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905#1</TD>
            <TD>2011-09-14T19:59:21Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/456/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/456/905 [2]</TD>
            <TD>JKs, i'g'r' photometry of C stars in NGC 6822 (Demers+, 2006)</TD>
            <TD>From a 2{deg}x2{deg} survey of NGC 6822 we have previously established that this Local Group dwarf irregular galaxy possesses a huge spheroid having more than one degree in length. This spheroid is in rotation but its rotation curve is known only within ~15' from the center. It is therefore critical to identify bright stars belonging to the spheroid to characterize, as far as possible, its outer kinematics. We use the new wide field near infrared imager CPAPIR, operated by the SMARTS consortium, to acquire J, K_s_ images of two 34.8'x34.8' areas in the outer spheroid to search for C stars. The colour diagram of the fields allows the identification of 192 C stars candidates but a study of the FWHM of the images permits the rejection of numerous non-stellar objects with colours similar to C stars. We are left with 75 new C stars, their mean K_s_ magnitude and mean colour are similar to the bulk of known NGC 6822 C stars. This outer spheroid survey confirms that the intermediate-age AGB stars are a major contributor to the stellar populations of the spheroid. The discovery of some 50 C stars well beyond the limit of the previously known rotation curve calls for a promising spectroscopic follow-up to a major axis distance of 40'.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905#2</TD>
            <TD>2011-09-14T19:59:21Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/456/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/456/905 [Cstars]</TD>
            <TD>JKs, i'g'r' photometry of C stars in NGC 6822 (Demers+, 2006)</TD>
            <TD>From a 2{deg}x2{deg} survey of NGC 6822 we have previously established that this Local Group dwarf irregular galaxy possesses a huge spheroid having more than one degree in length. This spheroid is in rotation but its rotation curve is known only within ~15' from the center. It is therefore critical to identify bright stars belonging to the spheroid to characterize, as far as possible, its outer kinematics. We use the new wide field near infrared imager CPAPIR, operated by the SMARTS consortium, to acquire J, K_s_ images of two 34.8'x34.8' areas in the outer spheroid to search for C stars. The colour diagram of the fields allows the identification of 192 C stars candidates but a study of the FWHM of the images permits the rejection of numerous non-stellar objects with colours similar to C stars. We are left with 75 new C stars, their mean K_s_ magnitude and mean colour are similar to the bulk of known NGC 6822 C stars. This outer spheroid survey confirms that the intermediate-age AGB stars are a major contributor to the stellar populations of the spheroid. The discovery of some 50 C stars well beyond the limit of the previously known rotation curve calls for a promising spectroscopic follow-up to a major axis distance of 40'.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905#Cstars</TD>
            <TD>2011-09-14T19:59:21Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/456/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/456/905 [1]</TD>
            <TD>JKs, i'g'r' photometry of C stars in NGC 6822 (Demers+, 2006)</TD>
            <TD>From a 2{deg}x2{deg} survey of NGC 6822 we have previously established that this Local Group dwarf irregular galaxy possesses a huge spheroid having more than one degree in length. This spheroid is in rotation but its rotation curve is known only within ~15' from the center. It is therefore critical to identify bright stars belonging to the spheroid to characterize, as far as possible, its outer kinematics. We use the new wide field near infrared imager CPAPIR, operated by the SMARTS consortium, to acquire J, K_s_ images of two 34.8'x34.8' areas in the outer spheroid to search for C stars. The colour diagram of the fields allows the identification of 192 C stars candidates but a study of the FWHM of the images permits the rejection of numerous non-stellar objects with colours similar to C stars. We are left with 75 new C stars, their mean K_s_ magnitude and mean colour are similar to the bulk of known NGC 6822 C stars. This outer spheroid survey confirms that the intermediate-age AGB stars are a major contributor to the stellar populations of the spheroid. The discovery of some 50 C stars well beyond the limit of the previously known rotation curve calls for a promising spectroscopic follow-up to a major axis distance of 40'.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905#1</TD>
            <TD>2011-09-14T19:59:21Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/456/905</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/905</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/456/905 [2]</TD>
            <TD>JKs, i'g'r' photometry of C stars in NGC 6822 (Demers+, 2006)</TD>
            <TD>From a 2{deg}x2{deg} survey of NGC 6822 we have previously established that this Local Group dwarf irregular galaxy possesses a huge spheroid having more than one degree in length. This spheroid is in rotation but its rotation curve is known only within ~15' from the center. It is therefore critical to identify bright stars belonging to the spheroid to characterize, as far as possible, its outer kinematics. We use the new wide field near infrared imager CPAPIR, operated by the SMARTS consortium, to acquire J, K_s_ images of two 34.8'x34.8' areas in the outer spheroid to search for C stars. The colour diagram of the fields allows the identification of 192 C stars candidates but a study of the FWHM of the images permits the rejection of numerous non-stellar objects with colours similar to C stars. We are left with 75 new C stars, their mean K_s_ magnitude and mean colour are similar to the bulk of known NGC 6822 C stars. This outer spheroid survey confirms that the intermediate-age AGB stars are a major contributor to the stellar populations of the spheroid. The discovery of some 50 C stars well beyond the limit of the previously known rotation curve calls for a promising spectroscopic follow-up to a major axis distance of 40'.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905#2</TD>
            <TD>2011-09-14T19:59:21Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/456/905&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/905</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/456/905 [Cstars]</TD>
            <TD>JKs, i'g'r' photometry of C stars in NGC 6822 (Demers+, 2006)</TD>
            <TD>From a 2{deg}x2{deg} survey of NGC 6822 we have previously established that this Local Group dwarf irregular galaxy possesses a huge spheroid having more than one degree in length. This spheroid is in rotation but its rotation curve is known only within ~15' from the center. It is therefore critical to identify bright stars belonging to the spheroid to characterize, as far as possible, its outer kinematics. We use the new wide field near infrared imager CPAPIR, operated by the SMARTS consortium, to acquire J, K_s_ images of two 34.8'x34.8' areas in the outer spheroid to search for C stars. The colour diagram of the fields allows the identification of 192 C stars candidates but a study of the FWHM of the images permits the rejection of numerous non-stellar objects with colours similar to C stars. We are left with 75 new C stars, their mean K_s_ magnitude and mean colour are similar to the bulk of known NGC 6822 C stars. This outer spheroid survey confirms that the intermediate-age AGB stars are a major contributor to the stellar populations of the spheroid. The discovery of some 50 C stars well beyond the limit of the previously known rotation curve calls for a promising spectroscopic follow-up to a major axis distance of 40'.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905#Cstars</TD>
            <TD>2011-09-14T19:59:21Z</TD>
            <TD>#Photometry#Galaxies#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/905</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/456/905&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/905</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/455/1165 [1]</TD>
            <TD>Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)</TD>
            <TD>We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165#1</TD>
            <TD>2011-09-14T19:59:51Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/455/1165</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/455/1165</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/455/1165 [2]</TD>
            <TD>Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)</TD>
            <TD>We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165#2</TD>
            <TD>2011-09-14T19:59:51Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/455/1165&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/455/1165</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/455/1165 [table1]</TD>
            <TD>Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)</TD>
            <TD>We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165#table1</TD>
            <TD>2011-09-14T19:59:51Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/455/1165&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/455/1165</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/455/1165 [1]</TD>
            <TD>Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)</TD>
            <TD>We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165#1</TD>
            <TD>2011-09-14T19:59:51Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/455/1165</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/455/1165</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/455/1165 [2]</TD>
            <TD>Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)</TD>
            <TD>We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165#2</TD>
            <TD>2011-09-14T19:59:51Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/455/1165&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/455/1165</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/455/1165 [table1]</TD>
            <TD>Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)</TD>
            <TD>We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165#table1</TD>
            <TD>2011-09-14T19:59:51Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/455/1165&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/455/1165</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/455/1165 [1]</TD>
            <TD>Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)</TD>
            <TD>We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165#1</TD>
            <TD>2011-09-14T19:59:51Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/455/1165</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/455/1165</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/455/1165 [2]</TD>
            <TD>Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)</TD>
            <TD>We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165#2</TD>
            <TD>2011-09-14T19:59:51Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/455/1165&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/455/1165</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/455/1165 [table1]</TD>
            <TD>Catalogue of Galactic high-mass X-ray binaries (Liu+, 2006)</TD>
            <TD>We present a new edition of the catalogue of high-mass X-ray binaries in the Galaxy. The catalogue contains source name(s), coordinates, finding chart, X-ray luminosity, system parameters, and stellar parameters of the components and other characteristic properties of 114 high-mass X-ray binaries, together with a comprehensive selection of the relevant literature. The aim of this catalogue is to provide the reader with some basic information on the X-ray sources and their counterparts in other wavelength ranges (gamma-rays, UV, optical, IR, radio). About 60% of the high-mass X-ray binary candidates are known or suspected Be/X-ray binaries, while 32% are supergiant/X-ray binaries. Some sources, however, are only tentatively identified as high-mass X-ray binaries on the basis of their X-ray properties similar to the known high-mass X-ray binaries. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 October 2005 has, as far as possible, been taken into account.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165#table1</TD>
            <TD>2011-09-14T19:59:51Z</TD>
            <TD>#Binaries:cataclysmic#Stars#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-May-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/455/1165</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/455/1165&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/455/1165</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/415/2417 [1]</TD>
            <TD>ASK spectroscopic sequence of galaxies (Ascasibar+, 2011)</TD>
            <TD>We identify a spectroscopic sequence of galaxies, analogous to the Hubble sequence of morphological types, based on the Automatic Spectroscopic K-means-based (ASK) classification. Considering galaxy spectra as multidimensional vectors, the majority of the spectral classes are distributed along a well-defined curve going from the earliest to the latest types, suggesting that the optical spectra of normal galaxies can be described in terms of a single affine parameter. Optically bright active galaxies, however, appear as an independent, roughly orthogonal branch that intersects the main sequence exactly at the transition between early and late types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/2417#1</TD>
            <TD>2012-05-18T13:52:16Z</TD>
            <TD>#Models#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/2417</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/415/2417</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/2417</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/415/2417 [2]</TD>
            <TD>ASK spectroscopic sequence of galaxies (Ascasibar+, 2011)</TD>
            <TD>We identify a spectroscopic sequence of galaxies, analogous to the Hubble sequence of morphological types, based on the Automatic Spectroscopic K-means-based (ASK) classification. Considering galaxy spectra as multidimensional vectors, the majority of the spectral classes are distributed along a well-defined curve going from the earliest to the latest types, suggesting that the optical spectra of normal galaxies can be described in terms of a single affine parameter. Optically bright active galaxies, however, appear as an independent, roughly orthogonal branch that intersects the main sequence exactly at the transition between early and late types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/2417#2</TD>
            <TD>2012-05-18T13:52:16Z</TD>
            <TD>#Models#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/2417</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/415/2417&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/2417</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/415/2417 [1]</TD>
            <TD>ASK spectroscopic sequence of galaxies (Ascasibar+, 2011)</TD>
            <TD>We identify a spectroscopic sequence of galaxies, analogous to the Hubble sequence of morphological types, based on the Automatic Spectroscopic K-means-based (ASK) classification. Considering galaxy spectra as multidimensional vectors, the majority of the spectral classes are distributed along a well-defined curve going from the earliest to the latest types, suggesting that the optical spectra of normal galaxies can be described in terms of a single affine parameter. Optically bright active galaxies, however, appear as an independent, roughly orthogonal branch that intersects the main sequence exactly at the transition between early and late types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/2417#1</TD>
            <TD>2012-05-18T13:52:16Z</TD>
            <TD>#Models#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/2417</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/415/2417</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/2417</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/415/2417 [2]</TD>
            <TD>ASK spectroscopic sequence of galaxies (Ascasibar+, 2011)</TD>
            <TD>We identify a spectroscopic sequence of galaxies, analogous to the Hubble sequence of morphological types, based on the Automatic Spectroscopic K-means-based (ASK) classification. Considering galaxy spectra as multidimensional vectors, the majority of the spectral classes are distributed along a well-defined curve going from the earliest to the latest types, suggesting that the optical spectra of normal galaxies can be described in terms of a single affine parameter. Optically bright active galaxies, however, appear as an independent, roughly orthogonal branch that intersects the main sequence exactly at the transition between early and late types.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/2417#2</TD>
            <TD>2012-05-18T13:52:16Z</TD>
            <TD>#Models#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/415/2417</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/415/2417&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/415/2417</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/2840 [1]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#1</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/2840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/2840 [2]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#2</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/2840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/2840 [catalog]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#catalog</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/2840 [group]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#group</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/2840 [1]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#1</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/2840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/2840 [2]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#2</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/2840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/2840 [catalog]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#catalog</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/2840 [group]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#group</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/2840 [1]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#1</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/2840</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/2840 [2]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#2</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/2840&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/2840 [catalog]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#catalog</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/2840 [group]</TD>
            <TD>The 2M++ galaxy redshift catalogue (Lavaux+, 2011)</TD>
            <TD>Peculiar velocities arise from gravitational instability, and thus are linked to the surrounding distribution of matter. In order to understand the motion of the Local Group with respect to the cosmic microwave background, a deep all-sky map of the galaxy distribution is required. Here we present a new redshift compilation of 69160 galaxies, dubbed 2M++, to map large-scale structures of the local Universe over nearly the whole sky, and reaching depths of K&lt;=12.5, or 200h^-1^Mpc. The target catalogue is based on the Two-Micron All-Sky Survey Extended Source Catalog (2MASS-XSC). The primary sources of redshifts are the 2MASS Redshift Survey, the 6dF galaxy redshift survey and the Sloan Digital Sky Survey (Data Release 7). We assess redshift completeness in each region and compute the weights required to correct for redshift incompleteness and apparent magnitude limits, and discuss corrections for incompleteness in the zone of avoidance. We present the density field for this survey, and discuss the importance of large-scale structures such as the Shapley Concentration.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840#group</TD>
            <TD>2012-06-15T07:30:04Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Apr-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/2840</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/2840&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/2840</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/465/357 [1]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#1</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/465/357</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/465/357 [2]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#2</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/465/357&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/465/357 [table2]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#table2</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/465/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/465/357 [table6]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#table6</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/465/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/465/357 [1]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#1</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/465/357</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/465/357 [2]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#2</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/465/357&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/465/357 [table2]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#table2</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/465/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/465/357 [table6]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#table6</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/465/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/465/357 [1]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#1</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/465/357</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/465/357 [2]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#2</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/465/357&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/465/357 [table2]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#table2</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/465/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/465/357 [table6]</TD>
            <TD>Stroemgren photometry in the Draco dSph galaxy (Faria+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed during five nights in March 2000 at the 2.5m Isaac Newton Telescope (INT) on La Palma using the Wide Field Camera (WFC).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357#table6</TD>
            <TD>2011-09-14T20:17:10Z</TD>
            <TD>#Abundances#Galaxies#Photometry:intermediate-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>09-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/465/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/465/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/465/357</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/162/80 [1]</TD>
            <TD>BVRJHKgr photometry of bright spiral galaxies (Kassin+, 2006)</TD>
            <TD>We present photometrically calibrated images and surface photometry in the B, V, R, J, H, and K bands of 25, and in the g, r, and K bands of five nearby bright (B^0^_T_&lt;12.5 mag) spiral galaxies with inclinations of 30{deg}-65{deg} spanning the Hubble sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey (Eskridge et al., Cat. &lt;J/ApJS/143/73&gt;), the Two Micron All Sky Survey (2006AJ....131.1163S), and the Sloan Digital Sky Survey Second Data Release (Abazajian et al., 2004AJ....128..502A). Radial surface brightness profiles are extracted, and integrated magnitudes are measured from the profiles. Axis ratios, position angles, and scale lengths are measured from the near-infrared images. A one-dimensional bulge/disk decomposition is performed on the near-infrared images of galaxies with a nonnegligible bulge component, and an exponential disk is fit to the radial surface brightness profiles of the remaining galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80#1</TD>
            <TD>2011-09-14T20:17:26Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/162/80</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/80</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/162/80 [2]</TD>
            <TD>BVRJHKgr photometry of bright spiral galaxies (Kassin+, 2006)</TD>
            <TD>We present photometrically calibrated images and surface photometry in the B, V, R, J, H, and K bands of 25, and in the g, r, and K bands of five nearby bright (B^0^_T_&lt;12.5 mag) spiral galaxies with inclinations of 30{deg}-65{deg} spanning the Hubble sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey (Eskridge et al., Cat. &lt;J/ApJS/143/73&gt;), the Two Micron All Sky Survey (2006AJ....131.1163S), and the Sloan Digital Sky Survey Second Data Release (Abazajian et al., 2004AJ....128..502A). Radial surface brightness profiles are extracted, and integrated magnitudes are measured from the profiles. Axis ratios, position angles, and scale lengths are measured from the near-infrared images. A one-dimensional bulge/disk decomposition is performed on the near-infrared images of galaxies with a nonnegligible bulge component, and an exponential disk is fit to the radial surface brightness profiles of the remaining galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80#2</TD>
            <TD>2011-09-14T20:17:26Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/162/80&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/80</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/162/80 [galaxies]</TD>
            <TD>BVRJHKgr photometry of bright spiral galaxies (Kassin+, 2006)</TD>
            <TD>We present photometrically calibrated images and surface photometry in the B, V, R, J, H, and K bands of 25, and in the g, r, and K bands of five nearby bright (B^0^_T_&lt;12.5 mag) spiral galaxies with inclinations of 30{deg}-65{deg} spanning the Hubble sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey (Eskridge et al., Cat. &lt;J/ApJS/143/73&gt;), the Two Micron All Sky Survey (2006AJ....131.1163S), and the Sloan Digital Sky Survey Second Data Release (Abazajian et al., 2004AJ....128..502A). Radial surface brightness profiles are extracted, and integrated magnitudes are measured from the profiles. Axis ratios, position angles, and scale lengths are measured from the near-infrared images. A one-dimensional bulge/disk decomposition is performed on the near-infrared images of galaxies with a nonnegligible bulge component, and an exponential disk is fit to the radial surface brightness profiles of the remaining galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80#galaxies</TD>
            <TD>2011-09-14T20:17:26Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/162/80&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/80</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/162/80 [1]</TD>
            <TD>BVRJHKgr photometry of bright spiral galaxies (Kassin+, 2006)</TD>
            <TD>We present photometrically calibrated images and surface photometry in the B, V, R, J, H, and K bands of 25, and in the g, r, and K bands of five nearby bright (B^0^_T_&lt;12.5 mag) spiral galaxies with inclinations of 30{deg}-65{deg} spanning the Hubble sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey (Eskridge et al., Cat. &lt;J/ApJS/143/73&gt;), the Two Micron All Sky Survey (2006AJ....131.1163S), and the Sloan Digital Sky Survey Second Data Release (Abazajian et al., 2004AJ....128..502A). Radial surface brightness profiles are extracted, and integrated magnitudes are measured from the profiles. Axis ratios, position angles, and scale lengths are measured from the near-infrared images. A one-dimensional bulge/disk decomposition is performed on the near-infrared images of galaxies with a nonnegligible bulge component, and an exponential disk is fit to the radial surface brightness profiles of the remaining galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80#1</TD>
            <TD>2011-09-14T20:17:26Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/162/80</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/80</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/162/80 [2]</TD>
            <TD>BVRJHKgr photometry of bright spiral galaxies (Kassin+, 2006)</TD>
            <TD>We present photometrically calibrated images and surface photometry in the B, V, R, J, H, and K bands of 25, and in the g, r, and K bands of five nearby bright (B^0^_T_&lt;12.5 mag) spiral galaxies with inclinations of 30{deg}-65{deg} spanning the Hubble sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey (Eskridge et al., Cat. &lt;J/ApJS/143/73&gt;), the Two Micron All Sky Survey (2006AJ....131.1163S), and the Sloan Digital Sky Survey Second Data Release (Abazajian et al., 2004AJ....128..502A). Radial surface brightness profiles are extracted, and integrated magnitudes are measured from the profiles. Axis ratios, position angles, and scale lengths are measured from the near-infrared images. A one-dimensional bulge/disk decomposition is performed on the near-infrared images of galaxies with a nonnegligible bulge component, and an exponential disk is fit to the radial surface brightness profiles of the remaining galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80#2</TD>
            <TD>2011-09-14T20:17:26Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/162/80&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/80</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/162/80 [galaxies]</TD>
            <TD>BVRJHKgr photometry of bright spiral galaxies (Kassin+, 2006)</TD>
            <TD>We present photometrically calibrated images and surface photometry in the B, V, R, J, H, and K bands of 25, and in the g, r, and K bands of five nearby bright (B^0^_T_&lt;12.5 mag) spiral galaxies with inclinations of 30{deg}-65{deg} spanning the Hubble sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey (Eskridge et al., Cat. &lt;J/ApJS/143/73&gt;), the Two Micron All Sky Survey (2006AJ....131.1163S), and the Sloan Digital Sky Survey Second Data Release (Abazajian et al., 2004AJ....128..502A). Radial surface brightness profiles are extracted, and integrated magnitudes are measured from the profiles. Axis ratios, position angles, and scale lengths are measured from the near-infrared images. A one-dimensional bulge/disk decomposition is performed on the near-infrared images of galaxies with a nonnegligible bulge component, and an exponential disk is fit to the radial surface brightness profiles of the remaining galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80#galaxies</TD>
            <TD>2011-09-14T20:17:26Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/162/80&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/80</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/162/80 [1]</TD>
            <TD>BVRJHKgr photometry of bright spiral galaxies (Kassin+, 2006)</TD>
            <TD>We present photometrically calibrated images and surface photometry in the B, V, R, J, H, and K bands of 25, and in the g, r, and K bands of five nearby bright (B^0^_T_&lt;12.5 mag) spiral galaxies with inclinations of 30{deg}-65{deg} spanning the Hubble sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey (Eskridge et al., Cat. &lt;J/ApJS/143/73&gt;), the Two Micron All Sky Survey (2006AJ....131.1163S), and the Sloan Digital Sky Survey Second Data Release (Abazajian et al., 2004AJ....128..502A). Radial surface brightness profiles are extracted, and integrated magnitudes are measured from the profiles. Axis ratios, position angles, and scale lengths are measured from the near-infrared images. A one-dimensional bulge/disk decomposition is performed on the near-infrared images of galaxies with a nonnegligible bulge component, and an exponential disk is fit to the radial surface brightness profiles of the remaining galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80#1</TD>
            <TD>2011-09-14T20:17:26Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/162/80</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/80</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/162/80 [2]</TD>
            <TD>BVRJHKgr photometry of bright spiral galaxies (Kassin+, 2006)</TD>
            <TD>We present photometrically calibrated images and surface photometry in the B, V, R, J, H, and K bands of 25, and in the g, r, and K bands of five nearby bright (B^0^_T_&lt;12.5 mag) spiral galaxies with inclinations of 30{deg}-65{deg} spanning the Hubble sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey (Eskridge et al., Cat. &lt;J/ApJS/143/73&gt;), the Two Micron All Sky Survey (2006AJ....131.1163S), and the Sloan Digital Sky Survey Second Data Release (Abazajian et al., 2004AJ....128..502A). Radial surface brightness profiles are extracted, and integrated magnitudes are measured from the profiles. Axis ratios, position angles, and scale lengths are measured from the near-infrared images. A one-dimensional bulge/disk decomposition is performed on the near-infrared images of galaxies with a nonnegligible bulge component, and an exponential disk is fit to the radial surface brightness profiles of the remaining galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80#2</TD>
            <TD>2011-09-14T20:17:26Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/162/80&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/80</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/162/80 [galaxies]</TD>
            <TD>BVRJHKgr photometry of bright spiral galaxies (Kassin+, 2006)</TD>
            <TD>We present photometrically calibrated images and surface photometry in the B, V, R, J, H, and K bands of 25, and in the g, r, and K bands of five nearby bright (B^0^_T_&lt;12.5 mag) spiral galaxies with inclinations of 30{deg}-65{deg} spanning the Hubble sequence from Sa to Scd. Data are from The Ohio State University Bright Spiral Galaxy Survey (Eskridge et al., Cat. &lt;J/ApJS/143/73&gt;), the Two Micron All Sky Survey (2006AJ....131.1163S), and the Sloan Digital Sky Survey Second Data Release (Abazajian et al., 2004AJ....128..502A). Radial surface brightness profiles are extracted, and integrated magnitudes are measured from the profiles. Axis ratios, position angles, and scale lengths are measured from the near-infrared images. A one-dimensional bulge/disk decomposition is performed on the near-infrared images of galaxies with a nonnegligible bulge component, and an exponential disk is fit to the radial surface brightness profiles of the remaining galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80#galaxies</TD>
            <TD>2011-09-14T20:17:26Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Photometry:surface#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/162/80</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/162/80&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/162/80</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/2677 [1]</TD>
            <TD>Stars in the Carina dSph galaxy field (Majewski+, 2005)</TD>
            <TD>Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677#1</TD>
            <TD>2011-09-14T20:17:28Z</TD>
            <TD>#Stars#Galaxies:spectra#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/2677</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2677</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/2677 [2]</TD>
            <TD>Stars in the Carina dSph galaxy field (Majewski+, 2005)</TD>
            <TD>Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677#2</TD>
            <TD>2011-09-14T20:17:28Z</TD>
            <TD>#Stars#Galaxies:spectra#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/2677&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2677</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/2677 [table5]</TD>
            <TD>Stars in the Carina dSph galaxy field (Majewski+, 2005)</TD>
            <TD>Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677#table5</TD>
            <TD>2011-09-14T20:17:28Z</TD>
            <TD>#Stars#Galaxies:spectra#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/2677&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2677</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/2677 [1]</TD>
            <TD>Stars in the Carina dSph galaxy field (Majewski+, 2005)</TD>
            <TD>Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677#1</TD>
            <TD>2011-09-14T20:17:28Z</TD>
            <TD>#Stars#Galaxies:spectra#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/2677</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2677</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/2677 [2]</TD>
            <TD>Stars in the Carina dSph galaxy field (Majewski+, 2005)</TD>
            <TD>Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677#2</TD>
            <TD>2011-09-14T20:17:28Z</TD>
            <TD>#Stars#Galaxies:spectra#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/2677&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2677</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/2677 [table5]</TD>
            <TD>Stars in the Carina dSph galaxy field (Majewski+, 2005)</TD>
            <TD>Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677#table5</TD>
            <TD>2011-09-14T20:17:28Z</TD>
            <TD>#Stars#Galaxies:spectra#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/2677&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2677</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/2677 [1]</TD>
            <TD>Stars in the Carina dSph galaxy field (Majewski+, 2005)</TD>
            <TD>Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677#1</TD>
            <TD>2011-09-14T20:17:28Z</TD>
            <TD>#Stars#Galaxies:spectra#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/2677</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2677</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/2677 [2]</TD>
            <TD>Stars in the Carina dSph galaxy field (Majewski+, 2005)</TD>
            <TD>Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677#2</TD>
            <TD>2011-09-14T20:17:28Z</TD>
            <TD>#Stars#Galaxies:spectra#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/2677&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2677</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/2677 [table5]</TD>
            <TD>Stars in the Carina dSph galaxy field (Majewski+, 2005)</TD>
            <TD>Spectra of our Carina giant candidates have been obtained using the Blanco 4m + Hydra multifiber spectrograph system at the Cerro Tololo Inter-American Observatory on the nights of UT 2000 March 26-29, 2000 November 10-12, and 2001 October 8-11.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677#table5</TD>
            <TD>2011-09-14T20:17:28Z</TD>
            <TD>#Stars#Galaxies:spectra#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>07-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/2677</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/2677&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/2677</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/799 [1]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#1</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/799</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/799 [2]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#2</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/799&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/799 [catalog]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#catalog</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/799 [disqual]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#disqual</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/799 [candid]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#candid</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/799 [1]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#1</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/799</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/799 [2]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#2</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/799&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/799 [catalog]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#catalog</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/799 [disqual]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#disqual</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/799 [candid]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#candid</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/799 [1]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#1</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/799</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/799 [2]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#2</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/799&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/799 [catalog]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#catalog</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/799 [disqual]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#disqual</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/799 [candid]</TD>
            <TD>Torun catalog of post-AGB and related objects (Szczerba+, 2007)</TD>
            <TD>With the ongoing AKARI infrared sky survey, of much greater sensitivity than IRAS, a wealth of post-AGB objects may be discovered. It is thus time to organize our present knowledge of known post-AGB stars in the galaxy with a view to using it to search for new post-AGB objects among AKARI sources. We searched the literature available on the NASA Astrophysics Data System up to 1 October 2006, and defined criteria for classifying sources into three categories: very likely, possible and disqualified post-AGB objects. The category of very likely post-AGB objects is made up of several classes. We have created an evolutionary, on-line catalogue of Galactic post-AGB objects, to be referred to as the Torun catalogue of Galactic post-AGB and related objects. The present version of the catalogue contains 326 very likely, 107 possible and 64 disqualified objects. For the very likely post-AGB objects, the catalogue gives the available optical and infrared photometry, infrared spectroscopy and spectral types, and links to finding charts and bibliography.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799#candid</TD>
            <TD>2011-09-14T20:17:42Z</TD>
            <TD>#Stars#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>10-Sep-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/799</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/799&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/799</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/84 [1]</TD>
            <TD>AGNs and host galaxies information (Vanden Berk+, 2006)</TD>
            <TD>Using an eigenspectrum decomposition technique, we separate the host galaxy from the broad-line active galactic nucleus (AGN) in a set of 4666 spectra from the Sloan Digital Sky Survey (SDSS), from redshifts near zero up to about 0.75. The decomposition technique uses separate sets of galaxy and quasar eigenspectra to efficiently and reliably separate the AGN and host spectroscopic components. The technique accurately reproduces the host galaxy spectrum, its contributing fraction, and its classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84#1</TD>
            <TD>2011-09-14T20:18:15Z</TD>
            <TD>#AGN#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/84</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/84</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/84 [2]</TD>
            <TD>AGNs and host galaxies information (Vanden Berk+, 2006)</TD>
            <TD>Using an eigenspectrum decomposition technique, we separate the host galaxy from the broad-line active galactic nucleus (AGN) in a set of 4666 spectra from the Sloan Digital Sky Survey (SDSS), from redshifts near zero up to about 0.75. The decomposition technique uses separate sets of galaxy and quasar eigenspectra to efficiently and reliably separate the AGN and host spectroscopic components. The technique accurately reproduces the host galaxy spectrum, its contributing fraction, and its classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84#2</TD>
            <TD>2011-09-14T20:18:15Z</TD>
            <TD>#AGN#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/84&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/84</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/84 [table2]</TD>
            <TD>AGNs and host galaxies information (Vanden Berk+, 2006)</TD>
            <TD>Using an eigenspectrum decomposition technique, we separate the host galaxy from the broad-line active galactic nucleus (AGN) in a set of 4666 spectra from the Sloan Digital Sky Survey (SDSS), from redshifts near zero up to about 0.75. The decomposition technique uses separate sets of galaxy and quasar eigenspectra to efficiently and reliably separate the AGN and host spectroscopic components. The technique accurately reproduces the host galaxy spectrum, its contributing fraction, and its classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84#table2</TD>
            <TD>2011-09-14T20:18:15Z</TD>
            <TD>#AGN#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/84&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/84</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/84 [1]</TD>
            <TD>AGNs and host galaxies information (Vanden Berk+, 2006)</TD>
            <TD>Using an eigenspectrum decomposition technique, we separate the host galaxy from the broad-line active galactic nucleus (AGN) in a set of 4666 spectra from the Sloan Digital Sky Survey (SDSS), from redshifts near zero up to about 0.75. The decomposition technique uses separate sets of galaxy and quasar eigenspectra to efficiently and reliably separate the AGN and host spectroscopic components. The technique accurately reproduces the host galaxy spectrum, its contributing fraction, and its classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84#1</TD>
            <TD>2011-09-14T20:18:15Z</TD>
            <TD>#AGN#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/84</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/84</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/84 [2]</TD>
            <TD>AGNs and host galaxies information (Vanden Berk+, 2006)</TD>
            <TD>Using an eigenspectrum decomposition technique, we separate the host galaxy from the broad-line active galactic nucleus (AGN) in a set of 4666 spectra from the Sloan Digital Sky Survey (SDSS), from redshifts near zero up to about 0.75. The decomposition technique uses separate sets of galaxy and quasar eigenspectra to efficiently and reliably separate the AGN and host spectroscopic components. The technique accurately reproduces the host galaxy spectrum, its contributing fraction, and its classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84#2</TD>
            <TD>2011-09-14T20:18:15Z</TD>
            <TD>#AGN#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/84&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/84</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/84 [table2]</TD>
            <TD>AGNs and host galaxies information (Vanden Berk+, 2006)</TD>
            <TD>Using an eigenspectrum decomposition technique, we separate the host galaxy from the broad-line active galactic nucleus (AGN) in a set of 4666 spectra from the Sloan Digital Sky Survey (SDSS), from redshifts near zero up to about 0.75. The decomposition technique uses separate sets of galaxy and quasar eigenspectra to efficiently and reliably separate the AGN and host spectroscopic components. The technique accurately reproduces the host galaxy spectrum, its contributing fraction, and its classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84#table2</TD>
            <TD>2011-09-14T20:18:15Z</TD>
            <TD>#AGN#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/84&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/84</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/131/84 [1]</TD>
            <TD>AGNs and host galaxies information (Vanden Berk+, 2006)</TD>
            <TD>Using an eigenspectrum decomposition technique, we separate the host galaxy from the broad-line active galactic nucleus (AGN) in a set of 4666 spectra from the Sloan Digital Sky Survey (SDSS), from redshifts near zero up to about 0.75. The decomposition technique uses separate sets of galaxy and quasar eigenspectra to efficiently and reliably separate the AGN and host spectroscopic components. The technique accurately reproduces the host galaxy spectrum, its contributing fraction, and its classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84#1</TD>
            <TD>2011-09-14T20:18:15Z</TD>
            <TD>#AGN#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/131/84</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/84</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/131/84 [2]</TD>
            <TD>AGNs and host galaxies information (Vanden Berk+, 2006)</TD>
            <TD>Using an eigenspectrum decomposition technique, we separate the host galaxy from the broad-line active galactic nucleus (AGN) in a set of 4666 spectra from the Sloan Digital Sky Survey (SDSS), from redshifts near zero up to about 0.75. The decomposition technique uses separate sets of galaxy and quasar eigenspectra to efficiently and reliably separate the AGN and host spectroscopic components. The technique accurately reproduces the host galaxy spectrum, its contributing fraction, and its classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84#2</TD>
            <TD>2011-09-14T20:18:15Z</TD>
            <TD>#AGN#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/131/84&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/84</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/131/84 [table2]</TD>
            <TD>AGNs and host galaxies information (Vanden Berk+, 2006)</TD>
            <TD>Using an eigenspectrum decomposition technique, we separate the host galaxy from the broad-line active galactic nucleus (AGN) in a set of 4666 spectra from the Sloan Digital Sky Survey (SDSS), from redshifts near zero up to about 0.75. The decomposition technique uses separate sets of galaxy and quasar eigenspectra to efficiently and reliably separate the AGN and host spectroscopic components. The technique accurately reproduces the host galaxy spectrum, its contributing fraction, and its classification.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84#table2</TD>
            <TD>2011-09-14T20:18:15Z</TD>
            <TD>#AGN#Photometry:wide-band#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>17-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/AJ/131/84</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/131/84&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/131/84</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AN/327/365 [1]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#1</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AN/327/365</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AN/327/365 [2]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#2</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AN/327/365&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/327/365 [groups]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#groups</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/327/365&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/327/365 [grGal]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#grGal</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/327/365&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/327/365 [isoGal]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#isoGal</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/327/365&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AN/327/365 [1]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#1</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AN/327/365</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AN/327/365 [2]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#2</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AN/327/365&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/327/365 [groups]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#groups</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/327/365&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/327/365 [grGal]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#grGal</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/327/365&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/327/365 [isoGal]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#isoGal</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/327/365&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AN/327/365 [1]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#1</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AN/327/365</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AN/327/365 [2]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#2</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AN/327/365&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/327/365 [groups]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#groups</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/327/365&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/327/365 [grGal]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#grGal</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/327/365&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AN/327/365 [isoGal]</TD>
            <TD>Clusters and groups of galaxies in 2dF (Tago+, 2006)</TD>
            <TD>We create a new catalogue of groups and clusters, applying the friends-to-friends method to the 2dF GRS final release. We investigate various selection effects due to the use of a magnitude limited sample. For this purpose we follow the changes in group sizes and mean galaxy number densities within the groups when shifting nearby observed groups to larger distances. We study the distribution of sizes of dark matter haloes in N-body simulations and compare properties of these haloes and the 2dF groups.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365#isoGal</TD>
            <TD>2011-09-14T20:18:47Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/AN/327/365</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AN/327/365&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AN/327/365</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/645/955 [1]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#1</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/645/955</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/645/955 [2]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#2</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/645/955&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/645/955 [BGV2006]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#BGV2006</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/645/955&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/645/955 [ext_sources]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#ext_sources</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/645/955&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/645/955 [1]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#1</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/645/955</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/645/955 [2]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#2</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/645/955&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/645/955 [BGV2006]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#BGV2006</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/645/955&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/645/955 [ext_sources]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#ext_sources</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/645/955&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/645/955 [1]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#1</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/645/955</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/645/955 [2]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#2</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/645/955&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/645/955 [BGV2006]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#BGV2006</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/645/955&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/645/955 [ext_sources]</TD>
            <TD>ChaMP serendipitous galaxy cluster survey (Barkhouse+, 2006)</TD>
            <TD>We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg^2^, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10^-14^ergs/cm^2^/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z~0.7. From the overlapping 6.1deg^2^ X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955#ext_sources</TD>
            <TD>2011-09-14T20:19:55Z</TD>
            <TD>#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/645/955</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/645/955&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/645/955</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/381/211 [1]</TD>
            <TD>Radio galaxies in the 2SLAQ LRG Survey (Sadler+, 2007)</TD>
            <TD>We have combined optical data from the 2dF-SDSS (Sloan Digital Sky Survey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ) redshift survey with radio measurements from the 1.4GHz VLA (Very Large Array) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAO VLA Sky Survey) surveys to identify a volume-limited sample of 391 radio galaxies at redshift 0.4&lt;z&lt;0.7. By determining an accurate radio luminosity function for luminous early-type galaxies in this redshift range, we can investigate the cosmic evolution of the radio-galaxy population over a wide range in radio luminosity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211#1</TD>
            <TD>2011-09-14T20:20:26Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/381/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/381/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/381/211 [2]</TD>
            <TD>Radio galaxies in the 2SLAQ LRG Survey (Sadler+, 2007)</TD>
            <TD>We have combined optical data from the 2dF-SDSS (Sloan Digital Sky Survey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ) redshift survey with radio measurements from the 1.4GHz VLA (Very Large Array) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAO VLA Sky Survey) surveys to identify a volume-limited sample of 391 radio galaxies at redshift 0.4&lt;z&lt;0.7. By determining an accurate radio luminosity function for luminous early-type galaxies in this redshift range, we can investigate the cosmic evolution of the radio-galaxy population over a wide range in radio luminosity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211#2</TD>
            <TD>2011-09-14T20:20:26Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/381/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/381/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/381/211 [table3]</TD>
            <TD>Radio galaxies in the 2SLAQ LRG Survey (Sadler+, 2007)</TD>
            <TD>We have combined optical data from the 2dF-SDSS (Sloan Digital Sky Survey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ) redshift survey with radio measurements from the 1.4GHz VLA (Very Large Array) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAO VLA Sky Survey) surveys to identify a volume-limited sample of 391 radio galaxies at redshift 0.4&lt;z&lt;0.7. By determining an accurate radio luminosity function for luminous early-type galaxies in this redshift range, we can investigate the cosmic evolution of the radio-galaxy population over a wide range in radio luminosity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211#table3</TD>
            <TD>2011-09-14T20:20:26Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/381/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/381/211</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/381/211 [1]</TD>
            <TD>Radio galaxies in the 2SLAQ LRG Survey (Sadler+, 2007)</TD>
            <TD>We have combined optical data from the 2dF-SDSS (Sloan Digital Sky Survey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ) redshift survey with radio measurements from the 1.4GHz VLA (Very Large Array) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAO VLA Sky Survey) surveys to identify a volume-limited sample of 391 radio galaxies at redshift 0.4&lt;z&lt;0.7. By determining an accurate radio luminosity function for luminous early-type galaxies in this redshift range, we can investigate the cosmic evolution of the radio-galaxy population over a wide range in radio luminosity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211#1</TD>
            <TD>2011-09-14T20:20:26Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/381/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/381/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/381/211 [2]</TD>
            <TD>Radio galaxies in the 2SLAQ LRG Survey (Sadler+, 2007)</TD>
            <TD>We have combined optical data from the 2dF-SDSS (Sloan Digital Sky Survey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ) redshift survey with radio measurements from the 1.4GHz VLA (Very Large Array) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAO VLA Sky Survey) surveys to identify a volume-limited sample of 391 radio galaxies at redshift 0.4&lt;z&lt;0.7. By determining an accurate radio luminosity function for luminous early-type galaxies in this redshift range, we can investigate the cosmic evolution of the radio-galaxy population over a wide range in radio luminosity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211#2</TD>
            <TD>2011-09-14T20:20:26Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/381/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/381/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/381/211 [table3]</TD>
            <TD>Radio galaxies in the 2SLAQ LRG Survey (Sadler+, 2007)</TD>
            <TD>We have combined optical data from the 2dF-SDSS (Sloan Digital Sky Survey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ) redshift survey with radio measurements from the 1.4GHz VLA (Very Large Array) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAO VLA Sky Survey) surveys to identify a volume-limited sample of 391 radio galaxies at redshift 0.4&lt;z&lt;0.7. By determining an accurate radio luminosity function for luminous early-type galaxies in this redshift range, we can investigate the cosmic evolution of the radio-galaxy population over a wide range in radio luminosity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211#table3</TD>
            <TD>2011-09-14T20:20:26Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/381/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/381/211</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/381/211 [1]</TD>
            <TD>Radio galaxies in the 2SLAQ LRG Survey (Sadler+, 2007)</TD>
            <TD>We have combined optical data from the 2dF-SDSS (Sloan Digital Sky Survey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ) redshift survey with radio measurements from the 1.4GHz VLA (Very Large Array) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAO VLA Sky Survey) surveys to identify a volume-limited sample of 391 radio galaxies at redshift 0.4&lt;z&lt;0.7. By determining an accurate radio luminosity function for luminous early-type galaxies in this redshift range, we can investigate the cosmic evolution of the radio-galaxy population over a wide range in radio luminosity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211#1</TD>
            <TD>2011-09-14T20:20:26Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/381/211</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/381/211</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/381/211 [2]</TD>
            <TD>Radio galaxies in the 2SLAQ LRG Survey (Sadler+, 2007)</TD>
            <TD>We have combined optical data from the 2dF-SDSS (Sloan Digital Sky Survey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ) redshift survey with radio measurements from the 1.4GHz VLA (Very Large Array) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAO VLA Sky Survey) surveys to identify a volume-limited sample of 391 radio galaxies at redshift 0.4&lt;z&lt;0.7. By determining an accurate radio luminosity function for luminous early-type galaxies in this redshift range, we can investigate the cosmic evolution of the radio-galaxy population over a wide range in radio luminosity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211#2</TD>
            <TD>2011-09-14T20:20:26Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/381/211&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/381/211</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/381/211 [table3]</TD>
            <TD>Radio galaxies in the 2SLAQ LRG Survey (Sadler+, 2007)</TD>
            <TD>We have combined optical data from the 2dF-SDSS (Sloan Digital Sky Survey) LRG (Luminous Red Galaxy) and QSO (quasi-stellar object) (2SLAQ) redshift survey with radio measurements from the 1.4GHz VLA (Very Large Array) FIRST (Faint Images of the Radio Sky at Twenty-cm) and NVSS (NRAO VLA Sky Survey) surveys to identify a volume-limited sample of 391 radio galaxies at redshift 0.4&lt;z&lt;0.7. By determining an accurate radio luminosity function for luminous early-type galaxies in this redshift range, we can investigate the cosmic evolution of the radio-galaxy population over a wide range in radio luminosity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211#table3</TD>
            <TD>2011-09-14T20:20:26Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Jan-2008</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/381/211</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/381/211&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/381/211</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/103 [1]</TD>
            <TD>BVRI imaging of M 51-type pairs (Laurikainen+, 2000)</TD>
            <TD>We present decompositions of azimuthally averaged surface brightness profiles in optical B, V, R and I-bands for a sample of 40 M 51-type interacting galaxies. The profiles were modelled by an exponential disk and a spherical bulge described either by the R^1/4^ law or by an exponential function. Half of the galaxies were well fitted by both bulge models, whereas for 35% the exponential function was a better choice. Special care was taken on eliminating superpositions of the companion galaxies. The mean B-band central surface brightness {mu}_0_was found to be 21.5mag/arcsec^2^, which is near to the value originally found by Freeman (1970ApJ...160..811F), but the scatter was fairly large. Galaxy interactions have strongly modified the disks in many of the galaxies in the sample. For example, six of them had extremely flat brightness profiles outside the exponential part of the disk, and many showed significant isophotal twists.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103#1</TD>
            <TD>2011-09-14T20:20:57Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/103</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/103</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/103 [2]</TD>
            <TD>BVRI imaging of M 51-type pairs (Laurikainen+, 2000)</TD>
            <TD>We present decompositions of azimuthally averaged surface brightness profiles in optical B, V, R and I-bands for a sample of 40 M 51-type interacting galaxies. The profiles were modelled by an exponential disk and a spherical bulge described either by the R^1/4^ law or by an exponential function. Half of the galaxies were well fitted by both bulge models, whereas for 35% the exponential function was a better choice. Special care was taken on eliminating superpositions of the companion galaxies. The mean B-band central surface brightness {mu}_0_was found to be 21.5mag/arcsec^2^, which is near to the value originally found by Freeman (1970ApJ...160..811F), but the scatter was fairly large. Galaxy interactions have strongly modified the disks in many of the galaxies in the sample. For example, six of them had extremely flat brightness profiles outside the exponential part of the disk, and many showed significant isophotal twists.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103#2</TD>
            <TD>2011-09-14T20:20:57Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/103&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/103</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/103 [table1]</TD>
            <TD>BVRI imaging of M 51-type pairs (Laurikainen+, 2000)</TD>
            <TD>We present decompositions of azimuthally averaged surface brightness profiles in optical B, V, R and I-bands for a sample of 40 M 51-type interacting galaxies. The profiles were modelled by an exponential disk and a spherical bulge described either by the R^1/4^ law or by an exponential function. Half of the galaxies were well fitted by both bulge models, whereas for 35% the exponential function was a better choice. Special care was taken on eliminating superpositions of the companion galaxies. The mean B-band central surface brightness {mu}_0_was found to be 21.5mag/arcsec^2^, which is near to the value originally found by Freeman (1970ApJ...160..811F), but the scatter was fairly large. Galaxy interactions have strongly modified the disks in many of the galaxies in the sample. For example, six of them had extremely flat brightness profiles outside the exponential part of the disk, and many showed significant isophotal twists.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103#table1</TD>
            <TD>2011-09-14T20:20:57Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/103&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/103</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/103 [1]</TD>
            <TD>BVRI imaging of M 51-type pairs (Laurikainen+, 2000)</TD>
            <TD>We present decompositions of azimuthally averaged surface brightness profiles in optical B, V, R and I-bands for a sample of 40 M 51-type interacting galaxies. The profiles were modelled by an exponential disk and a spherical bulge described either by the R^1/4^ law or by an exponential function. Half of the galaxies were well fitted by both bulge models, whereas for 35% the exponential function was a better choice. Special care was taken on eliminating superpositions of the companion galaxies. The mean B-band central surface brightness {mu}_0_was found to be 21.5mag/arcsec^2^, which is near to the value originally found by Freeman (1970ApJ...160..811F), but the scatter was fairly large. Galaxy interactions have strongly modified the disks in many of the galaxies in the sample. For example, six of them had extremely flat brightness profiles outside the exponential part of the disk, and many showed significant isophotal twists.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103#1</TD>
            <TD>2011-09-14T20:20:57Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/103</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/103</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/103 [2]</TD>
            <TD>BVRI imaging of M 51-type pairs (Laurikainen+, 2000)</TD>
            <TD>We present decompositions of azimuthally averaged surface brightness profiles in optical B, V, R and I-bands for a sample of 40 M 51-type interacting galaxies. The profiles were modelled by an exponential disk and a spherical bulge described either by the R^1/4^ law or by an exponential function. Half of the galaxies were well fitted by both bulge models, whereas for 35% the exponential function was a better choice. Special care was taken on eliminating superpositions of the companion galaxies. The mean B-band central surface brightness {mu}_0_was found to be 21.5mag/arcsec^2^, which is near to the value originally found by Freeman (1970ApJ...160..811F), but the scatter was fairly large. Galaxy interactions have strongly modified the disks in many of the galaxies in the sample. For example, six of them had extremely flat brightness profiles outside the exponential part of the disk, and many showed significant isophotal twists.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103#2</TD>
            <TD>2011-09-14T20:20:57Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/103&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/103</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/103 [table1]</TD>
            <TD>BVRI imaging of M 51-type pairs (Laurikainen+, 2000)</TD>
            <TD>We present decompositions of azimuthally averaged surface brightness profiles in optical B, V, R and I-bands for a sample of 40 M 51-type interacting galaxies. The profiles were modelled by an exponential disk and a spherical bulge described either by the R^1/4^ law or by an exponential function. Half of the galaxies were well fitted by both bulge models, whereas for 35% the exponential function was a better choice. Special care was taken on eliminating superpositions of the companion galaxies. The mean B-band central surface brightness {mu}_0_was found to be 21.5mag/arcsec^2^, which is near to the value originally found by Freeman (1970ApJ...160..811F), but the scatter was fairly large. Galaxy interactions have strongly modified the disks in many of the galaxies in the sample. For example, six of them had extremely flat brightness profiles outside the exponential part of the disk, and many showed significant isophotal twists.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103#table1</TD>
            <TD>2011-09-14T20:20:57Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/103&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/103</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/141/103 [1]</TD>
            <TD>BVRI imaging of M 51-type pairs (Laurikainen+, 2000)</TD>
            <TD>We present decompositions of azimuthally averaged surface brightness profiles in optical B, V, R and I-bands for a sample of 40 M 51-type interacting galaxies. The profiles were modelled by an exponential disk and a spherical bulge described either by the R^1/4^ law or by an exponential function. Half of the galaxies were well fitted by both bulge models, whereas for 35% the exponential function was a better choice. Special care was taken on eliminating superpositions of the companion galaxies. The mean B-band central surface brightness {mu}_0_was found to be 21.5mag/arcsec^2^, which is near to the value originally found by Freeman (1970ApJ...160..811F), but the scatter was fairly large. Galaxy interactions have strongly modified the disks in many of the galaxies in the sample. For example, six of them had extremely flat brightness profiles outside the exponential part of the disk, and many showed significant isophotal twists.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103#1</TD>
            <TD>2011-09-14T20:20:57Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/141/103</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/103</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/141/103 [2]</TD>
            <TD>BVRI imaging of M 51-type pairs (Laurikainen+, 2000)</TD>
            <TD>We present decompositions of azimuthally averaged surface brightness profiles in optical B, V, R and I-bands for a sample of 40 M 51-type interacting galaxies. The profiles were modelled by an exponential disk and a spherical bulge described either by the R^1/4^ law or by an exponential function. Half of the galaxies were well fitted by both bulge models, whereas for 35% the exponential function was a better choice. Special care was taken on eliminating superpositions of the companion galaxies. The mean B-band central surface brightness {mu}_0_was found to be 21.5mag/arcsec^2^, which is near to the value originally found by Freeman (1970ApJ...160..811F), but the scatter was fairly large. Galaxy interactions have strongly modified the disks in many of the galaxies in the sample. For example, six of them had extremely flat brightness profiles outside the exponential part of the disk, and many showed significant isophotal twists.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103#2</TD>
            <TD>2011-09-14T20:20:57Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/141/103&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/103</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/141/103 [table1]</TD>
            <TD>BVRI imaging of M 51-type pairs (Laurikainen+, 2000)</TD>
            <TD>We present decompositions of azimuthally averaged surface brightness profiles in optical B, V, R and I-bands for a sample of 40 M 51-type interacting galaxies. The profiles were modelled by an exponential disk and a spherical bulge described either by the R^1/4^ law or by an exponential function. Half of the galaxies were well fitted by both bulge models, whereas for 35% the exponential function was a better choice. Special care was taken on eliminating superpositions of the companion galaxies. The mean B-band central surface brightness {mu}_0_was found to be 21.5mag/arcsec^2^, which is near to the value originally found by Freeman (1970ApJ...160..811F), but the scatter was fairly large. Galaxy interactions have strongly modified the disks in many of the galaxies in the sample. For example, six of them had extremely flat brightness profiles outside the exponential part of the disk, and many showed significant isophotal twists.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103#table1</TD>
            <TD>2011-09-14T20:20:57Z</TD>
            <TD>#Photometry#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jan-2000</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/141/103</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/141/103&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/141/103</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/375/831 [1]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#1</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/375/831</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/375/831 [2]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#2</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/831 [table5]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#table5</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/831 [table3]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#table3</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/831 [table2]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#table2</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/375/831 [1]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#1</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/375/831</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/375/831 [2]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#2</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/831 [table5]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#table5</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/831 [table3]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#table3</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/831 [table2]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#table2</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/375/831 [1]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#1</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/375/831</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/375/831 [2]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#2</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/831 [table5]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#table5</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/831 [table3]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#table3</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/375/831 [table2]</TD>
            <TD>Draco MegaCam, INT and HST photometry (Segall+, 2007)</TD>
            <TD>The Draco dSph galaxy was observed with the wide-field MegaCam camera at the Canada-France-Hawaii Telescope (CFHT) in service mode during the 2004A and 2005A observing seasons. MegaCam is a mosaic of 364612x2048 EEV chips, offering a field of ~0.96x0.94deg^2^.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831#table2</TD>
            <TD>2011-09-14T20:21:01Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/375/831</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/375/831&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/375/831</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/474/1081 [1]</TD>
            <TD>Stellar population gradients in bulges. I (Gorgas+, 2007)</TD>
            <TD>In the first dataset we list Lick/IDS line-strength indices along the galaxy radii measured in flux-calibrated spectra and at the natural resolution of the bulges (i.e. internal plus instrumental). In the second dataset we list all the indices converted to the Lick/IDS system, together with the dynamical parameters (radial velocity and velocity dispersions) at each galactocentric radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081#1</TD>
            <TD>2011-09-14T20:22:05Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/474/1081</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/1081</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/474/1081 [2]</TD>
            <TD>Stellar population gradients in bulges. I (Gorgas+, 2007)</TD>
            <TD>In the first dataset we list Lick/IDS line-strength indices along the galaxy radii measured in flux-calibrated spectra and at the natural resolution of the bulges (i.e. internal plus instrumental). In the second dataset we list all the indices converted to the Lick/IDS system, together with the dynamical parameters (radial velocity and velocity dispersions) at each galactocentric radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081#2</TD>
            <TD>2011-09-14T20:22:05Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/474/1081&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/1081</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/474/1081 [table1]</TD>
            <TD>Stellar population gradients in bulges. I (Gorgas+, 2007)</TD>
            <TD>In the first dataset we list Lick/IDS line-strength indices along the galaxy radii measured in flux-calibrated spectra and at the natural resolution of the bulges (i.e. internal plus instrumental). In the second dataset we list all the indices converted to the Lick/IDS system, together with the dynamical parameters (radial velocity and velocity dispersions) at each galactocentric radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081#table1</TD>
            <TD>2011-09-14T20:22:05Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/474/1081&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/1081</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/474/1081 [1]</TD>
            <TD>Stellar population gradients in bulges. I (Gorgas+, 2007)</TD>
            <TD>In the first dataset we list Lick/IDS line-strength indices along the galaxy radii measured in flux-calibrated spectra and at the natural resolution of the bulges (i.e. internal plus instrumental). In the second dataset we list all the indices converted to the Lick/IDS system, together with the dynamical parameters (radial velocity and velocity dispersions) at each galactocentric radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081#1</TD>
            <TD>2011-09-14T20:22:05Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/474/1081</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/1081</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/474/1081 [2]</TD>
            <TD>Stellar population gradients in bulges. I (Gorgas+, 2007)</TD>
            <TD>In the first dataset we list Lick/IDS line-strength indices along the galaxy radii measured in flux-calibrated spectra and at the natural resolution of the bulges (i.e. internal plus instrumental). In the second dataset we list all the indices converted to the Lick/IDS system, together with the dynamical parameters (radial velocity and velocity dispersions) at each galactocentric radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081#2</TD>
            <TD>2011-09-14T20:22:05Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/474/1081&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/1081</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/474/1081 [table1]</TD>
            <TD>Stellar population gradients in bulges. I (Gorgas+, 2007)</TD>
            <TD>In the first dataset we list Lick/IDS line-strength indices along the galaxy radii measured in flux-calibrated spectra and at the natural resolution of the bulges (i.e. internal plus instrumental). In the second dataset we list all the indices converted to the Lick/IDS system, together with the dynamical parameters (radial velocity and velocity dispersions) at each galactocentric radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081#table1</TD>
            <TD>2011-09-14T20:22:05Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/474/1081&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/1081</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/474/1081 [1]</TD>
            <TD>Stellar population gradients in bulges. I (Gorgas+, 2007)</TD>
            <TD>In the first dataset we list Lick/IDS line-strength indices along the galaxy radii measured in flux-calibrated spectra and at the natural resolution of the bulges (i.e. internal plus instrumental). In the second dataset we list all the indices converted to the Lick/IDS system, together with the dynamical parameters (radial velocity and velocity dispersions) at each galactocentric radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081#1</TD>
            <TD>2011-09-14T20:22:05Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/474/1081</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/1081</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/474/1081 [2]</TD>
            <TD>Stellar population gradients in bulges. I (Gorgas+, 2007)</TD>
            <TD>In the first dataset we list Lick/IDS line-strength indices along the galaxy radii measured in flux-calibrated spectra and at the natural resolution of the bulges (i.e. internal plus instrumental). In the second dataset we list all the indices converted to the Lick/IDS system, together with the dynamical parameters (radial velocity and velocity dispersions) at each galactocentric radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081#2</TD>
            <TD>2011-09-14T20:22:05Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/474/1081&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/1081</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/474/1081 [table1]</TD>
            <TD>Stellar population gradients in bulges. I (Gorgas+, 2007)</TD>
            <TD>In the first dataset we list Lick/IDS line-strength indices along the galaxy radii measured in flux-calibrated spectra and at the natural resolution of the bulges (i.e. internal plus instrumental). In the second dataset we list all the indices converted to the Lick/IDS system, together with the dynamical parameters (radial velocity and velocity dispersions) at each galactocentric radius.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081#table1</TD>
            <TD>2011-09-14T20:22:05Z</TD>
            <TD>#Galaxies#Galaxies:spectra#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Mar-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/474/1081</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/474/1081&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/474/1081</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/481/593 [1]</TD>
            <TD>Radial velocities in A2163 (Maurogordato+, 2008)</TD>
            <TD>Velocity measurements for 512 objects obtained by multiobject spectroscopy in a field of 30'x30' centered on the galaxy cluster Abell 2163 are presented. For each object, table1.dat provides the spectroscopic identification number, right ascension and declination (J2000.0); radial velocity and the associated error, RTR parameter (Tonry and Davis, 1981ApJ...246..680T) as an indicator of the goodness of the cross-correlation redshift, a quality flag for the redshift, a flag indicating the presence of emission lines, and a flag corresponding to the instrument used. Objects are sorted by increasing Right Ascension.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593#1</TD>
            <TD>2011-09-14T20:22:22Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/481/593</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/481/593</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/481/593 [2]</TD>
            <TD>Radial velocities in A2163 (Maurogordato+, 2008)</TD>
            <TD>Velocity measurements for 512 objects obtained by multiobject spectroscopy in a field of 30'x30' centered on the galaxy cluster Abell 2163 are presented. For each object, table1.dat provides the spectroscopic identification number, right ascension and declination (J2000.0); radial velocity and the associated error, RTR parameter (Tonry and Davis, 1981ApJ...246..680T) as an indicator of the goodness of the cross-correlation redshift, a quality flag for the redshift, a flag indicating the presence of emission lines, and a flag corresponding to the instrument used. Objects are sorted by increasing Right Ascension.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593#2</TD>
            <TD>2011-09-14T20:22:22Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/481/593&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/481/593</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/481/593 [table1]</TD>
            <TD>Radial velocities in A2163 (Maurogordato+, 2008)</TD>
            <TD>Velocity measurements for 512 objects obtained by multiobject spectroscopy in a field of 30'x30' centered on the galaxy cluster Abell 2163 are presented. For each object, table1.dat provides the spectroscopic identification number, right ascension and declination (J2000.0); radial velocity and the associated error, RTR parameter (Tonry and Davis, 1981ApJ...246..680T) as an indicator of the goodness of the cross-correlation redshift, a quality flag for the redshift, a flag indicating the presence of emission lines, and a flag corresponding to the instrument used. Objects are sorted by increasing Right Ascension.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593#table1</TD>
            <TD>2011-09-14T20:22:22Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/481/593&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/481/593</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/481/593 [1]</TD>
            <TD>Radial velocities in A2163 (Maurogordato+, 2008)</TD>
            <TD>Velocity measurements for 512 objects obtained by multiobject spectroscopy in a field of 30'x30' centered on the galaxy cluster Abell 2163 are presented. For each object, table1.dat provides the spectroscopic identification number, right ascension and declination (J2000.0); radial velocity and the associated error, RTR parameter (Tonry and Davis, 1981ApJ...246..680T) as an indicator of the goodness of the cross-correlation redshift, a quality flag for the redshift, a flag indicating the presence of emission lines, and a flag corresponding to the instrument used. Objects are sorted by increasing Right Ascension.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593#1</TD>
            <TD>2011-09-14T20:22:22Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/481/593</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/481/593</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/481/593 [2]</TD>
            <TD>Radial velocities in A2163 (Maurogordato+, 2008)</TD>
            <TD>Velocity measurements for 512 objects obtained by multiobject spectroscopy in a field of 30'x30' centered on the galaxy cluster Abell 2163 are presented. For each object, table1.dat provides the spectroscopic identification number, right ascension and declination (J2000.0); radial velocity and the associated error, RTR parameter (Tonry and Davis, 1981ApJ...246..680T) as an indicator of the goodness of the cross-correlation redshift, a quality flag for the redshift, a flag indicating the presence of emission lines, and a flag corresponding to the instrument used. Objects are sorted by increasing Right Ascension.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593#2</TD>
            <TD>2011-09-14T20:22:22Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/481/593&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/481/593</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/481/593 [table1]</TD>
            <TD>Radial velocities in A2163 (Maurogordato+, 2008)</TD>
            <TD>Velocity measurements for 512 objects obtained by multiobject spectroscopy in a field of 30'x30' centered on the galaxy cluster Abell 2163 are presented. For each object, table1.dat provides the spectroscopic identification number, right ascension and declination (J2000.0); radial velocity and the associated error, RTR parameter (Tonry and Davis, 1981ApJ...246..680T) as an indicator of the goodness of the cross-correlation redshift, a quality flag for the redshift, a flag indicating the presence of emission lines, and a flag corresponding to the instrument used. Objects are sorted by increasing Right Ascension.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593#table1</TD>
            <TD>2011-09-14T20:22:22Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/481/593&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/481/593</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/481/593 [1]</TD>
            <TD>Radial velocities in A2163 (Maurogordato+, 2008)</TD>
            <TD>Velocity measurements for 512 objects obtained by multiobject spectroscopy in a field of 30'x30' centered on the galaxy cluster Abell 2163 are presented. For each object, table1.dat provides the spectroscopic identification number, right ascension and declination (J2000.0); radial velocity and the associated error, RTR parameter (Tonry and Davis, 1981ApJ...246..680T) as an indicator of the goodness of the cross-correlation redshift, a quality flag for the redshift, a flag indicating the presence of emission lines, and a flag corresponding to the instrument used. Objects are sorted by increasing Right Ascension.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593#1</TD>
            <TD>2011-09-14T20:22:22Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/481/593</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/481/593</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/481/593 [2]</TD>
            <TD>Radial velocities in A2163 (Maurogordato+, 2008)</TD>
            <TD>Velocity measurements for 512 objects obtained by multiobject spectroscopy in a field of 30'x30' centered on the galaxy cluster Abell 2163 are presented. For each object, table1.dat provides the spectroscopic identification number, right ascension and declination (J2000.0); radial velocity and the associated error, RTR parameter (Tonry and Davis, 1981ApJ...246..680T) as an indicator of the goodness of the cross-correlation redshift, a quality flag for the redshift, a flag indicating the presence of emission lines, and a flag corresponding to the instrument used. Objects are sorted by increasing Right Ascension.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593#2</TD>
            <TD>2011-09-14T20:22:22Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/481/593&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/481/593</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/481/593 [table1]</TD>
            <TD>Radial velocities in A2163 (Maurogordato+, 2008)</TD>
            <TD>Velocity measurements for 512 objects obtained by multiobject spectroscopy in a field of 30'x30' centered on the galaxy cluster Abell 2163 are presented. For each object, table1.dat provides the spectroscopic identification number, right ascension and declination (J2000.0); radial velocity and the associated error, RTR parameter (Tonry and Davis, 1981ApJ...246..680T) as an indicator of the goodness of the cross-correlation redshift, a quality flag for the redshift, a flag indicating the presence of emission lines, and a flag corresponding to the instrument used. Objects are sorted by increasing Right Ascension.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593#table1</TD>
            <TD>2011-09-14T20:22:22Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/481/593</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/481/593&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/481/593</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/478/353 [1]</TD>
            <TD>Structural properties of disk galaxies (Mendez-Abreu+, 2008)</TD>
            <TD>A variety of formation scenarios have been proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help to constrain the dominant mechanisms at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived in order to study the correlations between bulges and disks, as well as the probability distribution function of the intrinsic equatorial ellipticity of bulges. We present a new fitting algorithm (GASP2D) to perform two-dimensional photometric decomposition of the galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images, which were available in the Two Micron All Sky Survey. The probability distribution function of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353#1</TD>
            <TD>2011-09-14T20:22:52Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/478/353</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/353</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/478/353 [2]</TD>
            <TD>Structural properties of disk galaxies (Mendez-Abreu+, 2008)</TD>
            <TD>A variety of formation scenarios have been proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help to constrain the dominant mechanisms at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived in order to study the correlations between bulges and disks, as well as the probability distribution function of the intrinsic equatorial ellipticity of bulges. We present a new fitting algorithm (GASP2D) to perform two-dimensional photometric decomposition of the galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images, which were available in the Two Micron All Sky Survey. The probability distribution function of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353#2</TD>
            <TD>2011-09-14T20:22:52Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/478/353&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/353</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/478/353 [table3]</TD>
            <TD>Structural properties of disk galaxies (Mendez-Abreu+, 2008)</TD>
            <TD>A variety of formation scenarios have been proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help to constrain the dominant mechanisms at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived in order to study the correlations between bulges and disks, as well as the probability distribution function of the intrinsic equatorial ellipticity of bulges. We present a new fitting algorithm (GASP2D) to perform two-dimensional photometric decomposition of the galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images, which were available in the Two Micron All Sky Survey. The probability distribution function of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353#table3</TD>
            <TD>2011-09-14T20:22:52Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/478/353&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/353</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/478/353 [1]</TD>
            <TD>Structural properties of disk galaxies (Mendez-Abreu+, 2008)</TD>
            <TD>A variety of formation scenarios have been proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help to constrain the dominant mechanisms at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived in order to study the correlations between bulges and disks, as well as the probability distribution function of the intrinsic equatorial ellipticity of bulges. We present a new fitting algorithm (GASP2D) to perform two-dimensional photometric decomposition of the galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images, which were available in the Two Micron All Sky Survey. The probability distribution function of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353#1</TD>
            <TD>2011-09-14T20:22:52Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/478/353</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/353</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/478/353 [2]</TD>
            <TD>Structural properties of disk galaxies (Mendez-Abreu+, 2008)</TD>
            <TD>A variety of formation scenarios have been proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help to constrain the dominant mechanisms at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived in order to study the correlations between bulges and disks, as well as the probability distribution function of the intrinsic equatorial ellipticity of bulges. We present a new fitting algorithm (GASP2D) to perform two-dimensional photometric decomposition of the galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images, which were available in the Two Micron All Sky Survey. The probability distribution function of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353#2</TD>
            <TD>2011-09-14T20:22:52Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/478/353&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/353</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/478/353 [table3]</TD>
            <TD>Structural properties of disk galaxies (Mendez-Abreu+, 2008)</TD>
            <TD>A variety of formation scenarios have been proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help to constrain the dominant mechanisms at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived in order to study the correlations between bulges and disks, as well as the probability distribution function of the intrinsic equatorial ellipticity of bulges. We present a new fitting algorithm (GASP2D) to perform two-dimensional photometric decomposition of the galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images, which were available in the Two Micron All Sky Survey. The probability distribution function of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353#table3</TD>
            <TD>2011-09-14T20:22:52Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/478/353&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/353</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/478/353 [1]</TD>
            <TD>Structural properties of disk galaxies (Mendez-Abreu+, 2008)</TD>
            <TD>A variety of formation scenarios have been proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help to constrain the dominant mechanisms at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived in order to study the correlations between bulges and disks, as well as the probability distribution function of the intrinsic equatorial ellipticity of bulges. We present a new fitting algorithm (GASP2D) to perform two-dimensional photometric decomposition of the galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images, which were available in the Two Micron All Sky Survey. The probability distribution function of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353#1</TD>
            <TD>2011-09-14T20:22:52Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/478/353</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/353</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/478/353 [2]</TD>
            <TD>Structural properties of disk galaxies (Mendez-Abreu+, 2008)</TD>
            <TD>A variety of formation scenarios have been proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help to constrain the dominant mechanisms at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived in order to study the correlations between bulges and disks, as well as the probability distribution function of the intrinsic equatorial ellipticity of bulges. We present a new fitting algorithm (GASP2D) to perform two-dimensional photometric decomposition of the galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images, which were available in the Two Micron All Sky Survey. The probability distribution function of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353#2</TD>
            <TD>2011-09-14T20:22:52Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/478/353&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/353</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/478/353 [table3]</TD>
            <TD>Structural properties of disk galaxies (Mendez-Abreu+, 2008)</TD>
            <TD>A variety of formation scenarios have been proposed to explain the diversity of properties observed in bulges. Studying their intrinsic shape can help to constrain the dominant mechanisms at the epochs of their assembly. The structural parameters of a magnitude-limited sample of 148 unbarred S0-Sb galaxies were derived in order to study the correlations between bulges and disks, as well as the probability distribution function of the intrinsic equatorial ellipticity of bulges. We present a new fitting algorithm (GASP2D) to perform two-dimensional photometric decomposition of the galaxy surface-brightness distribution. This was assumed to be the sum of the contribution of a bulge and disk component characterized by elliptical and concentric isophotes with constant (but possibly different) ellipticity and position angles. Bulge and disk parameters of the sample galaxies were derived from the J-band images, which were available in the Two Micron All Sky Survey. The probability distribution function of the equatorial ellipticity of the bulges was derived from the distribution of the observed ellipticities of bulges and misalignments between bulges and disks.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353#table3</TD>
            <TD>2011-09-14T20:22:52Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>21-Apr-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/478/353</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/478/353&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/478/353</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/631/906 [1]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#1</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/631/906</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/631/906 [2]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#2</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/631/906&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/906 [lcurves]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#lcurves</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/906&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/906 [events]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#events</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/906&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/631/906 [1]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#1</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/631/906</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/631/906 [2]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#2</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/631/906&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/906 [lcurves]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#lcurves</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/906&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/906 [events]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#events</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/906&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/631/906 [1]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#1</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/631/906</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/631/906 [2]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#2</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/631/906&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/906 [lcurves]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#lcurves</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/906&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/631/906 [events]</TD>
            <TD>MACHO Galactic Bulge microlensing events (Thomas+, 2005)</TD>
            <TD>We present a catalog of 450 relatively high signal-to-noise ratio microlensing events observed by the MACHO collaboration between 1993 and 1999. The events are distributed throughout our fields, and as expected, they show a clear concentration toward the Galactic center. No optical depth is given for this sample, since no blending efficiency calculation has been performed and we find evidence for substantial blending. In a companion paper we give optical depths for the subsample of events on clump giant source stars, where blending is a less significant effect. Several events with sources that may belong to the Sagittarius dwarf galaxy are identified. For these events even relatively low dispersion spectra could suffice to classify these events as either consistent with Sagittarius membership or as non-Sagittarius sources. Several unusual events, such as microlensing of periodic variable source stars, binary lens events, and an event showing extended source effects, are identified. We also identify a number of contaminating background events as cataclysmic variable stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906#events</TD>
            <TD>2011-09-14T20:22:55Z</TD>
            <TD>#Photometry#Stars:variable#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/631/906</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/631/906&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/631/906</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/727 [1]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#1</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/727</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/727 [2]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#2</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/727 [table2]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#table2</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/727 [table6]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#table6</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/727 [table3]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#table3</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/727 [1]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#1</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/727</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/727 [2]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#2</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/727 [table2]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#table2</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/727 [table6]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#table6</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/727 [table3]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#table3</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/416/727 [1]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#1</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/416/727</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/416/727 [2]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#2</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/727 [table2]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#table2</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/727 [table6]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#table6</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/416/727 [table3]</TD>
            <TD>Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)</TD>
            <TD>To build a catalogue that satisfies our requirements of spectroscopic and photometric completeness, we used a set of galaxies derived from the Millennium Galaxy Catalogue (MGC, Cat. VII/240), a B-band imaging survey, both deep and wide, which provides a high-quality, complete representation of the nearby galaxy populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727#table3</TD>
            <TD>2012-07-03T14:17:44Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/416/727</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/416/727&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/416/727</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1857 [1]</TD>
            <TD>Sample of major galaxy pairs at z=0.08-0.38 (Woods+, 2010)</TD>
            <TD>The SHELS magnitude-limited redshift survey includes 9825 galaxies with total R-band magnitude R&lt;20.3. The galaxies are selected from the Deep Lens Survey F2 field R-band images. We obtained spectroscopy using Hectospec at the MMT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857#1</TD>
            <TD>2012-07-04T22:00:08Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1857 [2]</TD>
            <TD>Sample of major galaxy pairs at z=0.08-0.38 (Woods+, 2010)</TD>
            <TD>The SHELS magnitude-limited redshift survey includes 9825 galaxies with total R-band magnitude R&lt;20.3. The galaxies are selected from the Deep Lens Survey F2 field R-band images. We obtained spectroscopy using Hectospec at the MMT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857#2</TD>
            <TD>2012-07-04T22:00:08Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1857 [table2]</TD>
            <TD>Sample of major galaxy pairs at z=0.08-0.38 (Woods+, 2010)</TD>
            <TD>The SHELS magnitude-limited redshift survey includes 9825 galaxies with total R-band magnitude R&lt;20.3. The galaxies are selected from the Deep Lens Survey F2 field R-band images. We obtained spectroscopy using Hectospec at the MMT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857#table2</TD>
            <TD>2012-07-04T22:00:08Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1857 [1]</TD>
            <TD>Sample of major galaxy pairs at z=0.08-0.38 (Woods+, 2010)</TD>
            <TD>The SHELS magnitude-limited redshift survey includes 9825 galaxies with total R-band magnitude R&lt;20.3. The galaxies are selected from the Deep Lens Survey F2 field R-band images. We obtained spectroscopy using Hectospec at the MMT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857#1</TD>
            <TD>2012-07-04T22:00:08Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1857 [2]</TD>
            <TD>Sample of major galaxy pairs at z=0.08-0.38 (Woods+, 2010)</TD>
            <TD>The SHELS magnitude-limited redshift survey includes 9825 galaxies with total R-band magnitude R&lt;20.3. The galaxies are selected from the Deep Lens Survey F2 field R-band images. We obtained spectroscopy using Hectospec at the MMT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857#2</TD>
            <TD>2012-07-04T22:00:08Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1857 [table2]</TD>
            <TD>Sample of major galaxy pairs at z=0.08-0.38 (Woods+, 2010)</TD>
            <TD>The SHELS magnitude-limited redshift survey includes 9825 galaxies with total R-band magnitude R&lt;20.3. The galaxies are selected from the Deep Lens Survey F2 field R-band images. We obtained spectroscopy using Hectospec at the MMT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857#table2</TD>
            <TD>2012-07-04T22:00:08Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/139/1857 [1]</TD>
            <TD>Sample of major galaxy pairs at z=0.08-0.38 (Woods+, 2010)</TD>
            <TD>The SHELS magnitude-limited redshift survey includes 9825 galaxies with total R-band magnitude R&lt;20.3. The galaxies are selected from the Deep Lens Survey F2 field R-band images. We obtained spectroscopy using Hectospec at the MMT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857#1</TD>
            <TD>2012-07-04T22:00:08Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/139/1857</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1857</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/139/1857 [2]</TD>
            <TD>Sample of major galaxy pairs at z=0.08-0.38 (Woods+, 2010)</TD>
            <TD>The SHELS magnitude-limited redshift survey includes 9825 galaxies with total R-band magnitude R&lt;20.3. The galaxies are selected from the Deep Lens Survey F2 field R-band images. We obtained spectroscopy using Hectospec at the MMT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857#2</TD>
            <TD>2012-07-04T22:00:08Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/139/1857&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1857</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/139/1857 [table2]</TD>
            <TD>Sample of major galaxy pairs at z=0.08-0.38 (Woods+, 2010)</TD>
            <TD>The SHELS magnitude-limited redshift survey includes 9825 galaxies with total R-band magnitude R&lt;20.3. The galaxies are selected from the Deep Lens Survey F2 field R-band images. We obtained spectroscopy using Hectospec at the MMT.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857#table2</TD>
            <TD>2012-07-04T22:00:08Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-May-2012</TD>
            <TD>ivo://CDS.VizieR/J/AJ/139/1857</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/139/1857&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/139/1857</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/479/927 [1]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#1</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/479/927</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/479/927 [2]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#2</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/479/927&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/479/927 [galaxies]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#galaxies</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/479/927&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/479/927 [groups]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#groups</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/479/927&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/479/927 [1]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#1</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/479/927</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/479/927 [2]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#2</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/479/927&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/479/927 [galaxies]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#galaxies</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/479/927&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/479/927 [groups]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#groups</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/479/927&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/479/927 [1]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#1</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/479/927</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/479/927 [2]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#2</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/479/927&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/479/927 [galaxies]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#galaxies</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/479/927&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/479/927 [groups]</TD>
            <TD>Group of galaxies in SDSS 5 (Tago+, 2008)</TD>
            <TD>We extract groups of galaxies from the SDSS Data Release 5 to study the supercluster-void network and environmental properties of groups therein. Groups of galaxies as density enhancements can be used to determine the luminosity density field of the supercluster-void network. We use a modified friends-of-friends (FoF) method with slightly variable linking lengths in transverse and radial directions to eliminate selection effects and to reliably find as many groups as possible. To determine the scaling of the linking length we calibrated group sizes and mean galaxy number densities within groups by shifting nearby groups to larger distances. Our final sample contains 17143 groups in the equatorial (E), and 33219 groups in the northern (N) part of the DR5 survey. The mean sizes and velocity dispersions of our groups practically do not change with their distance. This means that the selection effects have been properly taken into account when generating the group catalogue.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927#groups</TD>
            <TD>2011-09-14T20:24:01Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Dec-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/479/927</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/479/927&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/479/927</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/647/13 [1]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#1</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/647/13</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/647/13 [2]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#2</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/647/13&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/647/13 [table1]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#table1</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/647/13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/647/13 [sources]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#sources</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/647/13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/647/13 [1]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#1</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/647/13</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/647/13 [2]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#2</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/647/13&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/647/13 [table1]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#table1</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/647/13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/647/13 [sources]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#sources</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/647/13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/647/13 [1]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#1</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/647/13</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/647/13 [2]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#2</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/647/13&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/647/13 [table1]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#table1</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/647/13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/647/13 [sources]</TD>
            <TD>BIMA CMB anisotropy survey (Dawson+, 2006)</TD>
            <TD>The BIMA anisotropy survey consists of 18 fields that had not been previously observed for SZ galaxy clusters or CMB anisotropy at arcminute angular scales. Each field was observed with the BIMA array at a frequency of 28.5GHz and the VLA at a frequency of 4.8GHz. Analysis of 10 fields observed with the BIMA array during the summers of 1998, 2000, and 2001 revealed evidence for a detection of power in excess of the instrumental noise. A description of the analysis and results for the first 10 fields in the survey can be found in Dawson et al. (2002ApJ...581...86D). Eight new fields were added to the survey in the summer of 2002.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13#sources</TD>
            <TD>2011-09-14T20:26:10Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/647/13</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/647/13&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/647/13</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/486/755 [1]</TD>
            <TD>Parameters of galaxies in 8 Abell clusters (Thomas+, 2008)</TD>
            <TD>Global parameters for 227 CGCG galaxies in eight low redshift Abell clusters are presented. Galaxies in the following clusters have been observed: A262, A347, A400, A426, A569, A779, A1367, and A1656. For each galaxy the observing run and Halpha filter used, the absolute B magnitude, galaxy type, Right ascension and Declination, major-to-minor axis ratio, position angle, 24mag/arcsec^2^ isophotal radius, R band apparent magnitude, Halpha flux and EW, and global star formation rate are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755#1</TD>
            <TD>2011-09-14T20:27:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/486/755</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/755</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/486/755 [2]</TD>
            <TD>Parameters of galaxies in 8 Abell clusters (Thomas+, 2008)</TD>
            <TD>Global parameters for 227 CGCG galaxies in eight low redshift Abell clusters are presented. Galaxies in the following clusters have been observed: A262, A347, A400, A426, A569, A779, A1367, and A1656. For each galaxy the observing run and Halpha filter used, the absolute B magnitude, galaxy type, Right ascension and Declination, major-to-minor axis ratio, position angle, 24mag/arcsec^2^ isophotal radius, R band apparent magnitude, Halpha flux and EW, and global star formation rate are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755#2</TD>
            <TD>2011-09-14T20:27:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/486/755&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/755</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/486/755 [table2]</TD>
            <TD>Parameters of galaxies in 8 Abell clusters (Thomas+, 2008)</TD>
            <TD>Global parameters for 227 CGCG galaxies in eight low redshift Abell clusters are presented. Galaxies in the following clusters have been observed: A262, A347, A400, A426, A569, A779, A1367, and A1656. For each galaxy the observing run and Halpha filter used, the absolute B magnitude, galaxy type, Right ascension and Declination, major-to-minor axis ratio, position angle, 24mag/arcsec^2^ isophotal radius, R band apparent magnitude, Halpha flux and EW, and global star formation rate are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755#table2</TD>
            <TD>2011-09-14T20:27:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/486/755&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/755</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/486/755 [1]</TD>
            <TD>Parameters of galaxies in 8 Abell clusters (Thomas+, 2008)</TD>
            <TD>Global parameters for 227 CGCG galaxies in eight low redshift Abell clusters are presented. Galaxies in the following clusters have been observed: A262, A347, A400, A426, A569, A779, A1367, and A1656. For each galaxy the observing run and Halpha filter used, the absolute B magnitude, galaxy type, Right ascension and Declination, major-to-minor axis ratio, position angle, 24mag/arcsec^2^ isophotal radius, R band apparent magnitude, Halpha flux and EW, and global star formation rate are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755#1</TD>
            <TD>2011-09-14T20:27:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/486/755</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/755</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/486/755 [2]</TD>
            <TD>Parameters of galaxies in 8 Abell clusters (Thomas+, 2008)</TD>
            <TD>Global parameters for 227 CGCG galaxies in eight low redshift Abell clusters are presented. Galaxies in the following clusters have been observed: A262, A347, A400, A426, A569, A779, A1367, and A1656. For each galaxy the observing run and Halpha filter used, the absolute B magnitude, galaxy type, Right ascension and Declination, major-to-minor axis ratio, position angle, 24mag/arcsec^2^ isophotal radius, R band apparent magnitude, Halpha flux and EW, and global star formation rate are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755#2</TD>
            <TD>2011-09-14T20:27:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/486/755&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/755</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/486/755 [table2]</TD>
            <TD>Parameters of galaxies in 8 Abell clusters (Thomas+, 2008)</TD>
            <TD>Global parameters for 227 CGCG galaxies in eight low redshift Abell clusters are presented. Galaxies in the following clusters have been observed: A262, A347, A400, A426, A569, A779, A1367, and A1656. For each galaxy the observing run and Halpha filter used, the absolute B magnitude, galaxy type, Right ascension and Declination, major-to-minor axis ratio, position angle, 24mag/arcsec^2^ isophotal radius, R band apparent magnitude, Halpha flux and EW, and global star formation rate are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755#table2</TD>
            <TD>2011-09-14T20:27:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/486/755&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/755</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/486/755 [1]</TD>
            <TD>Parameters of galaxies in 8 Abell clusters (Thomas+, 2008)</TD>
            <TD>Global parameters for 227 CGCG galaxies in eight low redshift Abell clusters are presented. Galaxies in the following clusters have been observed: A262, A347, A400, A426, A569, A779, A1367, and A1656. For each galaxy the observing run and Halpha filter used, the absolute B magnitude, galaxy type, Right ascension and Declination, major-to-minor axis ratio, position angle, 24mag/arcsec^2^ isophotal radius, R band apparent magnitude, Halpha flux and EW, and global star formation rate are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755#1</TD>
            <TD>2011-09-14T20:27:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/486/755</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/755</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/486/755 [2]</TD>
            <TD>Parameters of galaxies in 8 Abell clusters (Thomas+, 2008)</TD>
            <TD>Global parameters for 227 CGCG galaxies in eight low redshift Abell clusters are presented. Galaxies in the following clusters have been observed: A262, A347, A400, A426, A569, A779, A1367, and A1656. For each galaxy the observing run and Halpha filter used, the absolute B magnitude, galaxy type, Right ascension and Declination, major-to-minor axis ratio, position angle, 24mag/arcsec^2^ isophotal radius, R band apparent magnitude, Halpha flux and EW, and global star formation rate are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755#2</TD>
            <TD>2011-09-14T20:27:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/486/755&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/755</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/486/755 [table2]</TD>
            <TD>Parameters of galaxies in 8 Abell clusters (Thomas+, 2008)</TD>
            <TD>Global parameters for 227 CGCG galaxies in eight low redshift Abell clusters are presented. Galaxies in the following clusters have been observed: A262, A347, A400, A426, A569, A779, A1367, and A1656. For each galaxy the observing run and Halpha filter used, the absolute B magnitude, galaxy type, Right ascension and Declination, major-to-minor axis ratio, position angle, 24mag/arcsec^2^ isophotal radius, R band apparent magnitude, Halpha flux and EW, and global star formation rate are given.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755#table2</TD>
            <TD>2011-09-14T20:27:28Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Jun-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/755</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/486/755&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/755</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/102 [1]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#1</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/102 [2]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#2</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/117/102 [cowie]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#cowie</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/117/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/117/102 [hff_cat]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#hff_cat</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/117/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/102 [1]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#1</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/102 [2]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#2</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/117/102 [cowie]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#cowie</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/117/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/117/102 [hff_cat]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#hff_cat</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/117/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/117/102 [1]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#1</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/117/102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/117/102 [2]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#2</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/117/102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/117/102 [cowie]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#cowie</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/117/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/117/102 [hff_cat]</TD>
            <TD>Photometry + Spectroscopy in HDF + Flanking Fields (Barger+, 1999)</TD>
            <TD>the Hubble Deep Field and its flanking fields. Our wide-field survey provides uniform coverage of a 61.8arcmin^2^ area to a depth equivalent to K=20.1 at 5{sigma}. We have also imaged the Hubble Deep Field in HK', providing uniform coverage of a 7.8arcmin^2^ area to a depth equivalent to K=21.2 at 5{sigma}. Using these data in combination with new deep University of Hawaii 8K V- and I-imaging obtained on the Canada-France-Hawaii Telescope, we find only a small population of objects with colors redder than an equivalent I-K=4mag, the color expected for an evolved elliptical galaxy at z&gt;1. We infer that only a fraction of the local field elliptical galaxy population with M_K_&lt;-23.4 could have formed in single bursts at high redshift. The HK' observations of the HDF and its flanking fields were made with the University of Hawaii 2.2m telescope (1996-02-06 to 1996-02-08 for the HDF, and 1997-04-17 to 1997-04-22 for the wider area) and the 3.6m Canada-France-Hawaii Telescope (CFHT, 1996-04-05 to 1996-04-08 for the HDF). The deep V- and I-band observations were made with the CFHT (1997-04-03 to 1997-04-08), and B-band observations with the Keck Low Resolution Imaging Spectrograph in a strip across the center of the HK wide-field image.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102#hff_cat</TD>
            <TD>2011-09-14T20:28:30Z</TD>
            <TD>#Photometry#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/117/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/117/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/117/102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/484/303 [1]</TD>
            <TD>X-ray sources close to 3C 295 galaxy cluster (D'Elia+, 2008)</TD>
            <TD>To acquire the optical spectra of the 3C 295 sources, we proposed a Multi Object Spectroscopy (MOS) programme using DOLORES@TNG (AOT 9). Two acquisition images each of exposure time 900 s and with a limiting magnitude of R~24, had already been obtained using DOLORES on March 19, 2002. We acquired the spectral data on 22 and 23 March, 2004.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303#1</TD>
            <TD>2011-09-14T20:29:32Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/484/303</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/484/303</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/484/303 [2]</TD>
            <TD>X-ray sources close to 3C 295 galaxy cluster (D'Elia+, 2008)</TD>
            <TD>To acquire the optical spectra of the 3C 295 sources, we proposed a Multi Object Spectroscopy (MOS) programme using DOLORES@TNG (AOT 9). Two acquisition images each of exposure time 900 s and with a limiting magnitude of R~24, had already been obtained using DOLORES on March 19, 2002. We acquired the spectral data on 22 and 23 March, 2004.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303#2</TD>
            <TD>2011-09-14T20:29:32Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/484/303&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/484/303</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/484/303 [table1]</TD>
            <TD>X-ray sources close to 3C 295 galaxy cluster (D'Elia+, 2008)</TD>
            <TD>To acquire the optical spectra of the 3C 295 sources, we proposed a Multi Object Spectroscopy (MOS) programme using DOLORES@TNG (AOT 9). Two acquisition images each of exposure time 900 s and with a limiting magnitude of R~24, had already been obtained using DOLORES on March 19, 2002. We acquired the spectral data on 22 and 23 March, 2004.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303#table1</TD>
            <TD>2011-09-14T20:29:32Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/484/303&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/484/303</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/484/303 [1]</TD>
            <TD>X-ray sources close to 3C 295 galaxy cluster (D'Elia+, 2008)</TD>
            <TD>To acquire the optical spectra of the 3C 295 sources, we proposed a Multi Object Spectroscopy (MOS) programme using DOLORES@TNG (AOT 9). Two acquisition images each of exposure time 900 s and with a limiting magnitude of R~24, had already been obtained using DOLORES on March 19, 2002. We acquired the spectral data on 22 and 23 March, 2004.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303#1</TD>
            <TD>2011-09-14T20:29:32Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/484/303</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/484/303</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/484/303 [2]</TD>
            <TD>X-ray sources close to 3C 295 galaxy cluster (D'Elia+, 2008)</TD>
            <TD>To acquire the optical spectra of the 3C 295 sources, we proposed a Multi Object Spectroscopy (MOS) programme using DOLORES@TNG (AOT 9). Two acquisition images each of exposure time 900 s and with a limiting magnitude of R~24, had already been obtained using DOLORES on March 19, 2002. We acquired the spectral data on 22 and 23 March, 2004.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303#2</TD>
            <TD>2011-09-14T20:29:32Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/484/303&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/484/303</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/484/303 [table1]</TD>
            <TD>X-ray sources close to 3C 295 galaxy cluster (D'Elia+, 2008)</TD>
            <TD>To acquire the optical spectra of the 3C 295 sources, we proposed a Multi Object Spectroscopy (MOS) programme using DOLORES@TNG (AOT 9). Two acquisition images each of exposure time 900 s and with a limiting magnitude of R~24, had already been obtained using DOLORES on March 19, 2002. We acquired the spectral data on 22 and 23 March, 2004.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303#table1</TD>
            <TD>2011-09-14T20:29:32Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/484/303&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/484/303</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/484/303 [1]</TD>
            <TD>X-ray sources close to 3C 295 galaxy cluster (D'Elia+, 2008)</TD>
            <TD>To acquire the optical spectra of the 3C 295 sources, we proposed a Multi Object Spectroscopy (MOS) programme using DOLORES@TNG (AOT 9). Two acquisition images each of exposure time 900 s and with a limiting magnitude of R~24, had already been obtained using DOLORES on March 19, 2002. We acquired the spectral data on 22 and 23 March, 2004.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303#1</TD>
            <TD>2011-09-14T20:29:32Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/484/303</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/484/303</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/484/303 [2]</TD>
            <TD>X-ray sources close to 3C 295 galaxy cluster (D'Elia+, 2008)</TD>
            <TD>To acquire the optical spectra of the 3C 295 sources, we proposed a Multi Object Spectroscopy (MOS) programme using DOLORES@TNG (AOT 9). Two acquisition images each of exposure time 900 s and with a limiting magnitude of R~24, had already been obtained using DOLORES on March 19, 2002. We acquired the spectral data on 22 and 23 March, 2004.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303#2</TD>
            <TD>2011-09-14T20:29:32Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/484/303&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/484/303</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/484/303 [table1]</TD>
            <TD>X-ray sources close to 3C 295 galaxy cluster (D'Elia+, 2008)</TD>
            <TD>To acquire the optical spectra of the 3C 295 sources, we proposed a Multi Object Spectroscopy (MOS) programme using DOLORES@TNG (AOT 9). Two acquisition images each of exposure time 900 s and with a limiting magnitude of R~24, had already been obtained using DOLORES on March 19, 2002. We acquired the spectral data on 22 and 23 March, 2004.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303#table1</TD>
            <TD>2011-09-14T20:29:32Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/484/303</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/484/303&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/484/303</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/486/697 [1]</TD>
            <TD>Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)</TD>
            <TD>The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein &amp; Zabludoff (2003ApJ...591..764C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697#1</TD>
            <TD>2011-09-14T20:30:36Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/486/697</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/697</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/486/697 [2]</TD>
            <TD>Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)</TD>
            <TD>The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein &amp; Zabludoff (2003ApJ...591..764C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697#2</TD>
            <TD>2011-09-14T20:30:36Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/486/697&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/697</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/486/697 [tablea2]</TD>
            <TD>Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)</TD>
            <TD>The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein &amp; Zabludoff (2003ApJ...591..764C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697#tablea2</TD>
            <TD>2011-09-14T20:30:36Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/486/697&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/697</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/486/697 [1]</TD>
            <TD>Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)</TD>
            <TD>The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein &amp; Zabludoff (2003ApJ...591..764C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697#1</TD>
            <TD>2011-09-14T20:30:36Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/486/697</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/697</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/486/697 [2]</TD>
            <TD>Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)</TD>
            <TD>The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein &amp; Zabludoff (2003ApJ...591..764C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697#2</TD>
            <TD>2011-09-14T20:30:36Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/486/697&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/697</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/486/697 [tablea2]</TD>
            <TD>Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)</TD>
            <TD>The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein &amp; Zabludoff (2003ApJ...591..764C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697#tablea2</TD>
            <TD>2011-09-14T20:30:36Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/486/697&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/697</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/486/697 [1]</TD>
            <TD>Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)</TD>
            <TD>The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein &amp; Zabludoff (2003ApJ...591..764C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697#1</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>23-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/486/697</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/697</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/486/697 [2]</TD>
            <TD>Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)</TD>
            <TD>The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein &amp; Zabludoff (2003ApJ...591..764C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697#2</TD>
            <TD>2011-09-14T20:30:36Z</TD>
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            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
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            <TD>23-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/486/697&amp;</TD>
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            <TD>ivo://CDS</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/486/697 [tablea2]</TD>
            <TD>Hydra I Cluster Catalogue (HCC) (Misgeld+, 2008)</TD>
            <TD>The obtained photometric parameters along with the available radial velocities for all early-type galaxies in our sample (111 objects) are presented in the Hydra I Cluster Catalogue (HCC). For each galaxy right ascension, declination, extinction corrected magnitude V and colour V-I, central surface brightness and scale length of an exponential fit to the surface brightness profile, effective surface brightness, effective radius and profile shape index n, as obtained from a Sersic fit, are given. The physical scale is 0.2kpc/arcsec at the assumed distance modulus of (m-M)=33.07mag. The radial velocities are taken from our study and from Christlein &amp; Zabludoff (2003ApJ...591..764C).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697#tablea2</TD>
            <TD>2011-09-14T20:30:36Z</TD>
            <TD>#Clusters_of_galaxies#Photometry#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/A+A/486/697</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/486/697&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/486/697</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/681/1163 [1]</TD>
            <TD>Late-type galaxies in Chandra deep fields (Lehmer+, 2008)</TD>
            <TD>We report on the X-ray evolution over the last ~9Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (L_X_/L_B_) and the X-ray-to-stellar mass mean ratio (L_X_/M_*_) for galaxy populations selected by L_B_ and M_*_, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L_X_/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR=1-100M_{sun}_/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z=0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that L_X_/L_B_ at z~3 is similar to its value at z=1.4.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163#1</TD>
            <TD>2011-09-14T21:04:26Z</TD>
            <TD>#AGN#Redshifts#</TD>
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            <TD />
            <TD>28-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/681/1163</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/681/1163</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/681/1163 [2]</TD>
            <TD>Late-type galaxies in Chandra deep fields (Lehmer+, 2008)</TD>
            <TD>We report on the X-ray evolution over the last ~9Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (L_X_/L_B_) and the X-ray-to-stellar mass mean ratio (L_X_/M_*_) for galaxy populations selected by L_B_ and M_*_, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L_X_/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR=1-100M_{sun}_/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z=0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that L_X_/L_B_ at z~3 is similar to its value at z=1.4.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163#2</TD>
            <TD>2011-09-14T21:04:26Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/681/1163&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/681/1163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/681/1163 [table1]</TD>
            <TD>Late-type galaxies in Chandra deep fields (Lehmer+, 2008)</TD>
            <TD>We report on the X-ray evolution over the last ~9Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (L_X_/L_B_) and the X-ray-to-stellar mass mean ratio (L_X_/M_*_) for galaxy populations selected by L_B_ and M_*_, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L_X_/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR=1-100M_{sun}_/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z=0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that L_X_/L_B_ at z~3 is similar to its value at z=1.4.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163#table1</TD>
            <TD>2011-09-14T21:04:26Z</TD>
            <TD>#AGN#Redshifts#</TD>
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            <TD>#Research#</TD>
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            <TD>28-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/681/1163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/681/1163</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/681/1163 [1]</TD>
            <TD>Late-type galaxies in Chandra deep fields (Lehmer+, 2008)</TD>
            <TD>We report on the X-ray evolution over the last ~9Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (L_X_/L_B_) and the X-ray-to-stellar mass mean ratio (L_X_/M_*_) for galaxy populations selected by L_B_ and M_*_, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L_X_/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR=1-100M_{sun}_/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z=0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that L_X_/L_B_ at z~3 is similar to its value at z=1.4.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163#1</TD>
            <TD>2011-09-14T21:04:26Z</TD>
            <TD>#AGN#Redshifts#</TD>
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            <TD>28-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/681/1163</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/681/1163</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/681/1163 [2]</TD>
            <TD>Late-type galaxies in Chandra deep fields (Lehmer+, 2008)</TD>
            <TD>We report on the X-ray evolution over the last ~9Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (L_X_/L_B_) and the X-ray-to-stellar mass mean ratio (L_X_/M_*_) for galaxy populations selected by L_B_ and M_*_, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L_X_/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR=1-100M_{sun}_/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z=0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that L_X_/L_B_ at z~3 is similar to its value at z=1.4.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163#2</TD>
            <TD>2011-09-14T21:04:26Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/681/1163&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/681/1163</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/681/1163 [table1]</TD>
            <TD>Late-type galaxies in Chandra deep fields (Lehmer+, 2008)</TD>
            <TD>We report on the X-ray evolution over the last ~9Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (L_X_/L_B_) and the X-ray-to-stellar mass mean ratio (L_X_/M_*_) for galaxy populations selected by L_B_ and M_*_, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L_X_/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR=1-100M_{sun}_/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z=0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that L_X_/L_B_ at z~3 is similar to its value at z=1.4.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
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            <TD>#AGN#Redshifts#</TD>
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            <TD>#Research#</TD>
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            <TD>28-Oct-2010</TD>
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            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/681/1163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/681/1163</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/681/1163 [1]</TD>
            <TD>Late-type galaxies in Chandra deep fields (Lehmer+, 2008)</TD>
            <TD>We report on the X-ray evolution over the last ~9Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (L_X_/L_B_) and the X-ray-to-stellar mass mean ratio (L_X_/M_*_) for galaxy populations selected by L_B_ and M_*_, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L_X_/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR=1-100M_{sun}_/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z=0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that L_X_/L_B_ at z~3 is similar to its value at z=1.4.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163#1</TD>
            <TD>2011-09-14T21:04:26Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/681/1163</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/681/1163</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/681/1163 [2]</TD>
            <TD>Late-type galaxies in Chandra deep fields (Lehmer+, 2008)</TD>
            <TD>We report on the X-ray evolution over the last ~9Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (L_X_/L_B_) and the X-ray-to-stellar mass mean ratio (L_X_/M_*_) for galaxy populations selected by L_B_ and M_*_, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L_X_/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR=1-100M_{sun}_/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z=0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that L_X_/L_B_ at z~3 is similar to its value at z=1.4.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163#2</TD>
            <TD>2011-09-14T21:04:26Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/681/1163&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/681/1163</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/681/1163 [table1]</TD>
            <TD>Late-type galaxies in Chandra deep fields (Lehmer+, 2008)</TD>
            <TD>We report on the X-ray evolution over the last ~9Gyr of cosmic history (i.e., since z=1.4) of late-type galaxy populations in the Chandra Deep Field-North and Extended Chandra Deep Field-South (CDF-N and E-CDF-S, respectively; jointly CDFs) survey fields. Our late-type galaxy sample consists of 2568 galaxies, which were identified using rest-frame optical colors and HST morphologies. We utilized X-ray stacking analyses to investigate the X-ray emission from these galaxies, emphasizing the contributions from normal galaxies that are not dominated by active galactic nuclei (AGNs). Over this redshift range, we find significant increases (factors of ~5-10) in the X-ray-to-optical mean luminosity ratio (L_X_/L_B_) and the X-ray-to-stellar mass mean ratio (L_X_/M_*_) for galaxy populations selected by L_B_ and M_*_, respectively. When analyzing galaxy samples selected via SFR, we find that the mean X-ray-to-SFR ratio (L_X_/SFR) is consistent with being constant over the entire redshift range for galaxies with SFR=1-100M_{sun}_/yr, thus demonstrating that X-ray emission can be used as a robust indicator of star formation activity out to z~1.4. We find that the star formation activity (as traced by X-ray luminosity) per unit stellar mass in a given redshift bin increases with decreasing stellar mass over the redshift range z=0.2-1, which is consistent with previous studies of how star formation activity depends on stellar mass. Finally, we extend our X-ray analyses to Lyman break galaxies at z~3 and estimate that L_X_/L_B_ at z~3 is similar to its value at z=1.4.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163#table1</TD>
            <TD>2011-09-14T21:04:26Z</TD>
            <TD>#AGN#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>28-Oct-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/681/1163</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/681/1163&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/681/1163</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/518/69 [1]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#1</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/518/69</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/518/69 [2]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#2</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/518/69&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/518/69 [table2]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#table2</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/518/69&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/518/69 [table1]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#table1</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/518/69&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/518/69 [1]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#1</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/518/69</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/518/69 [2]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#2</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/518/69&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/518/69 [table2]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#table2</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/518/69&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/518/69 [table1]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#table1</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/518/69&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/518/69 [1]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#1</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/518/69</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/518/69 [2]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#2</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/518/69&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/518/69 [table2]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#table2</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/518/69&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/518/69 [table1]</TD>
            <TD>Deep Optical Catalog of galaxy systems (Mahdavi+, 1999)</TD>
            <TD>++++Lrecl of file 'table2.dat' (45) indicates 8 extra blanks (trim!) %B We assemble and observe a sample of poor galaxy systems that is suitable for testing N-body simulations of hierarchical clustering and other dynamical halo models. We (1) determine the parameters of the density profile {Rho}(r) and the velocity dispersion profile {sigma}_p_(R), (2) separate emission-line galaxies from absorption-line galaxies, examining the model parameters, {beta}, and as a function of spectroscopic type, and (3) for the best-behaved subsample, constrain the velocity anisotropy parameter, {beta}, which determines the shapes of the galaxy orbits. Our sample consists of 20 systems, 12 of which have extended X-ray emission in the ROSAT All-Sky Survey. We measure the 877 optical spectra of galaxies brighter than m_R_~15.4 within 1.5h^-1^Mpc of the system centers (we take H_0_=100h*km/s/Mpc). Thus, we sample the system membership to a radius typically three times larger than other recent optical group surveys. The average system population is 30 galaxies, and the average line-of-sight velocity dispersion is ~300km/s. The Navarro, Frenk, &amp; White universal profile and the Hernquist model both provide good descriptions of the spatial data. In most cases an isothermal sphere is ruled out. Systems with declining {sigma}_p_(R) are well-matched by theoretical profiles in which the star-forming galaxies have predominantly radial orbits ({beta}&gt;0); many of these galaxies are probably falling in for the first time. There is significant evidence for spatial segregation of the spectroscopic classes regardless of {sigma}_p_(R).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69#table1</TD>
            <TD>2011-09-14T21:04:27Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Sep-1999</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/518/69</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/518/69&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/518/69</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/502/1015 [1]</TD>
            <TD>OB associations in IC 1613 (Garcia+, 2009)</TD>
            <TD>From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friends-of-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015#1</TD>
            <TD>2011-09-14T21:06:00Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/502/1015</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/1015</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/502/1015 [2]</TD>
            <TD>OB associations in IC 1613 (Garcia+, 2009)</TD>
            <TD>From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friends-of-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015#2</TD>
            <TD>2011-09-14T21:06:00Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/502/1015&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/1015</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/502/1015 [tablea1]</TD>
            <TD>OB associations in IC 1613 (Garcia+, 2009)</TD>
            <TD>From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friends-of-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015#tablea1</TD>
            <TD>2011-09-14T21:06:00Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/502/1015&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/1015</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/502/1015 [1]</TD>
            <TD>OB associations in IC 1613 (Garcia+, 2009)</TD>
            <TD>From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friends-of-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015#1</TD>
            <TD>2011-09-14T21:06:00Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/502/1015</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/1015</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/502/1015 [2]</TD>
            <TD>OB associations in IC 1613 (Garcia+, 2009)</TD>
            <TD>From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friends-of-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015#2</TD>
            <TD>2011-09-14T21:06:00Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/502/1015&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/1015</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/502/1015 [tablea1]</TD>
            <TD>OB associations in IC 1613 (Garcia+, 2009)</TD>
            <TD>From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friends-of-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015#tablea1</TD>
            <TD>2011-09-14T21:06:00Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/502/1015&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/1015</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/502/1015 [1]</TD>
            <TD>OB associations in IC 1613 (Garcia+, 2009)</TD>
            <TD>From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friends-of-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015#1</TD>
            <TD>2011-09-14T21:06:00Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/502/1015</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/1015</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/502/1015 [2]</TD>
            <TD>OB associations in IC 1613 (Garcia+, 2009)</TD>
            <TD>From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friends-of-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015#2</TD>
            <TD>2011-09-14T21:06:00Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/502/1015&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/1015</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/502/1015 [tablea1]</TD>
            <TD>OB associations in IC 1613 (Garcia+, 2009)</TD>
            <TD>From observations taken with the Wide Field Camera (WFC) at the Isaac Newton Telescope (INT), we have built an astrometric and photometric catalogue of stars in IC 1613. Candidate blue massive stars are preselected by their colors. A friends-of-friends algorithm is developed to find their clustering in the galaxy. While a common physical origin for all the members of the associations cannot be ensured, this is a necessary first step to place candidate OB stars in a population context.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015#tablea1</TD>
            <TD>2011-09-14T21:06:00Z</TD>
            <TD>#Associations#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/502/1015</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/502/1015&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/502/1015</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/503/357 [1]</TD>
            <TD>Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)</TD>
            <TD>Our analysis is based mainly on redshift data for 145 galaxies mostly acquired at the Telescopio Nazionale Galileo and on new photometric data acquired at the Isaac Newton Telescope. We also use X-ray data from the Chandra archive and photometric data from the Sloan Digital Sky Survey (Data Release 7). We combine galaxy velocities and positions to select 89 cluster galaxies and analyze the internal dynamics of the Abell 1237 + Abell 1240 cluster complex, Abell 1237 being a close companion of Abell 1240 in its southern direction.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357#1</TD>
            <TD>2011-09-14T21:08:41Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/503/357</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/503/357</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/503/357 [2]</TD>
            <TD>Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)</TD>
            <TD>Our analysis is based mainly on redshift data for 145 galaxies mostly acquired at the Telescopio Nazionale Galileo and on new photometric data acquired at the Isaac Newton Telescope. We also use X-ray data from the Chandra archive and photometric data from the Sloan Digital Sky Survey (Data Release 7). We combine galaxy velocities and positions to select 89 cluster galaxies and analyze the internal dynamics of the Abell 1237 + Abell 1240 cluster complex, Abell 1237 being a close companion of Abell 1240 in its southern direction.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357#2</TD>
            <TD>2011-09-14T21:08:41Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/503/357&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/503/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/503/357 [table1]</TD>
            <TD>Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)</TD>
            <TD>Our analysis is based mainly on redshift data for 145 galaxies mostly acquired at the Telescopio Nazionale Galileo and on new photometric data acquired at the Isaac Newton Telescope. We also use X-ray data from the Chandra archive and photometric data from the Sloan Digital Sky Survey (Data Release 7). We combine galaxy velocities and positions to select 89 cluster galaxies and analyze the internal dynamics of the Abell 1237 + Abell 1240 cluster complex, Abell 1237 being a close companion of Abell 1240 in its southern direction.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357#table1</TD>
            <TD>2011-09-14T21:08:41Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/503/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/503/357</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/503/357 [1]</TD>
            <TD>Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)</TD>
            <TD>Our analysis is based mainly on redshift data for 145 galaxies mostly acquired at the Telescopio Nazionale Galileo and on new photometric data acquired at the Isaac Newton Telescope. We also use X-ray data from the Chandra archive and photometric data from the Sloan Digital Sky Survey (Data Release 7). We combine galaxy velocities and positions to select 89 cluster galaxies and analyze the internal dynamics of the Abell 1237 + Abell 1240 cluster complex, Abell 1237 being a close companion of Abell 1240 in its southern direction.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357#1</TD>
            <TD>2011-09-14T21:08:41Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/503/357</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/503/357</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/503/357 [2]</TD>
            <TD>Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)</TD>
            <TD>Our analysis is based mainly on redshift data for 145 galaxies mostly acquired at the Telescopio Nazionale Galileo and on new photometric data acquired at the Isaac Newton Telescope. We also use X-ray data from the Chandra archive and photometric data from the Sloan Digital Sky Survey (Data Release 7). We combine galaxy velocities and positions to select 89 cluster galaxies and analyze the internal dynamics of the Abell 1237 + Abell 1240 cluster complex, Abell 1237 being a close companion of Abell 1240 in its southern direction.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357#2</TD>
            <TD>2011-09-14T21:08:41Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/503/357&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/503/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/503/357 [table1]</TD>
            <TD>Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)</TD>
            <TD>Our analysis is based mainly on redshift data for 145 galaxies mostly acquired at the Telescopio Nazionale Galileo and on new photometric data acquired at the Isaac Newton Telescope. We also use X-ray data from the Chandra archive and photometric data from the Sloan Digital Sky Survey (Data Release 7). We combine galaxy velocities and positions to select 89 cluster galaxies and analyze the internal dynamics of the Abell 1237 + Abell 1240 cluster complex, Abell 1237 being a close companion of Abell 1240 in its southern direction.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357#table1</TD>
            <TD>2011-09-14T21:08:41Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/503/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/503/357</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/503/357 [1]</TD>
            <TD>Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)</TD>
            <TD>Our analysis is based mainly on redshift data for 145 galaxies mostly acquired at the Telescopio Nazionale Galileo and on new photometric data acquired at the Isaac Newton Telescope. We also use X-ray data from the Chandra archive and photometric data from the Sloan Digital Sky Survey (Data Release 7). We combine galaxy velocities and positions to select 89 cluster galaxies and analyze the internal dynamics of the Abell 1237 + Abell 1240 cluster complex, Abell 1237 being a close companion of Abell 1240 in its southern direction.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357#1</TD>
            <TD>2011-09-14T21:08:41Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/503/357</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/503/357</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/503/357 [2]</TD>
            <TD>Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)</TD>
            <TD>Our analysis is based mainly on redshift data for 145 galaxies mostly acquired at the Telescopio Nazionale Galileo and on new photometric data acquired at the Isaac Newton Telescope. We also use X-ray data from the Chandra archive and photometric data from the Sloan Digital Sky Survey (Data Release 7). We combine galaxy velocities and positions to select 89 cluster galaxies and analyze the internal dynamics of the Abell 1237 + Abell 1240 cluster complex, Abell 1237 being a close companion of Abell 1240 in its southern direction.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357#2</TD>
            <TD>2011-09-14T21:08:41Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/503/357&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/503/357</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/503/357 [table1]</TD>
            <TD>Redhift catalog of A1237+A1240 galaxies (Barrena+, 2009)</TD>
            <TD>Our analysis is based mainly on redshift data for 145 galaxies mostly acquired at the Telescopio Nazionale Galileo and on new photometric data acquired at the Isaac Newton Telescope. We also use X-ray data from the Chandra archive and photometric data from the Sloan Digital Sky Survey (Data Release 7). We combine galaxy velocities and positions to select 89 cluster galaxies and analyze the internal dynamics of the Abell 1237 + Abell 1240 cluster complex, Abell 1237 being a close companion of Abell 1240 in its southern direction.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357#table1</TD>
            <TD>2011-09-14T21:08:41Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>30-Oct-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/503/357</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/503/357&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/503/357</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/ChA+A/32 [1]</TD>
            <TD>Accretion rate distributions of AGNs (Bao+, 2008)</TD>
            <TD>The redshift, central black hole mass and accretion rate are important parameters when studying the AGN evolution. The central black hole masses for 172 quasars and Seyfert galaxies are calculated in this paper using the reverberation mapping method. The distributions of central black hole masses, redshifts and the Eddington accretion rates are analyzed, to verify the transition from the quasar to the Seyfert galaxy in the course of evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351#1</TD>
            <TD>2011-09-14T21:08:57Z</TD>
            <TD>#AGN#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/ChA+A/32.351</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ChA+A/32.351</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/ChA+A/32 [2]</TD>
            <TD>Accretion rate distributions of AGNs (Bao+, 2008)</TD>
            <TD>The redshift, central black hole mass and accretion rate are important parameters when studying the AGN evolution. The central black hole masses for 172 quasars and Seyfert galaxies are calculated in this paper using the reverberation mapping method. The distributions of central black hole masses, redshifts and the Eddington accretion rates are analyzed, to verify the transition from the quasar to the Seyfert galaxy in the course of evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351#2</TD>
            <TD>2011-09-14T21:08:57Z</TD>
            <TD>#AGN#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/ChA+A/32.351&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ChA+A/32.351</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/ChA+A/32 [table1]</TD>
            <TD>Accretion rate distributions of AGNs (Bao+, 2008)</TD>
            <TD>The redshift, central black hole mass and accretion rate are important parameters when studying the AGN evolution. The central black hole masses for 172 quasars and Seyfert galaxies are calculated in this paper using the reverberation mapping method. The distributions of central black hole masses, redshifts and the Eddington accretion rates are analyzed, to verify the transition from the quasar to the Seyfert galaxy in the course of evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351#table1</TD>
            <TD>2011-09-14T21:08:57Z</TD>
            <TD>#AGN#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/ChA+A/32.351&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ChA+A/32.351</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/ChA+A/32 [1]</TD>
            <TD>Accretion rate distributions of AGNs (Bao+, 2008)</TD>
            <TD>The redshift, central black hole mass and accretion rate are important parameters when studying the AGN evolution. The central black hole masses for 172 quasars and Seyfert galaxies are calculated in this paper using the reverberation mapping method. The distributions of central black hole masses, redshifts and the Eddington accretion rates are analyzed, to verify the transition from the quasar to the Seyfert galaxy in the course of evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351#1</TD>
            <TD>2011-09-14T21:08:57Z</TD>
            <TD>#AGN#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/ChA+A/32.351</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ChA+A/32.351</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/ChA+A/32 [2]</TD>
            <TD>Accretion rate distributions of AGNs (Bao+, 2008)</TD>
            <TD>The redshift, central black hole mass and accretion rate are important parameters when studying the AGN evolution. The central black hole masses for 172 quasars and Seyfert galaxies are calculated in this paper using the reverberation mapping method. The distributions of central black hole masses, redshifts and the Eddington accretion rates are analyzed, to verify the transition from the quasar to the Seyfert galaxy in the course of evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351#2</TD>
            <TD>2011-09-14T21:08:57Z</TD>
            <TD>#AGN#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/ChA+A/32.351&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ChA+A/32.351</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/ChA+A/32 [table1]</TD>
            <TD>Accretion rate distributions of AGNs (Bao+, 2008)</TD>
            <TD>The redshift, central black hole mass and accretion rate are important parameters when studying the AGN evolution. The central black hole masses for 172 quasars and Seyfert galaxies are calculated in this paper using the reverberation mapping method. The distributions of central black hole masses, redshifts and the Eddington accretion rates are analyzed, to verify the transition from the quasar to the Seyfert galaxy in the course of evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351#table1</TD>
            <TD>2011-09-14T21:08:57Z</TD>
            <TD>#AGN#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/ChA+A/32.351&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ChA+A/32.351</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/ChA+A/32 [1]</TD>
            <TD>Accretion rate distributions of AGNs (Bao+, 2008)</TD>
            <TD>The redshift, central black hole mass and accretion rate are important parameters when studying the AGN evolution. The central black hole masses for 172 quasars and Seyfert galaxies are calculated in this paper using the reverberation mapping method. The distributions of central black hole masses, redshifts and the Eddington accretion rates are analyzed, to verify the transition from the quasar to the Seyfert galaxy in the course of evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351#1</TD>
            <TD>2011-09-14T21:08:57Z</TD>
            <TD>#AGN#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/ChA+A/32.351</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ChA+A/32.351</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/ChA+A/32 [2]</TD>
            <TD>Accretion rate distributions of AGNs (Bao+, 2008)</TD>
            <TD>The redshift, central black hole mass and accretion rate are important parameters when studying the AGN evolution. The central black hole masses for 172 quasars and Seyfert galaxies are calculated in this paper using the reverberation mapping method. The distributions of central black hole masses, redshifts and the Eddington accretion rates are analyzed, to verify the transition from the quasar to the Seyfert galaxy in the course of evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351#2</TD>
            <TD>2011-09-14T21:08:57Z</TD>
            <TD>#AGN#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/ChA+A/32.351&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ChA+A/32.351</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/ChA+A/32 [table1]</TD>
            <TD>Accretion rate distributions of AGNs (Bao+, 2008)</TD>
            <TD>The redshift, central black hole mass and accretion rate are important parameters when studying the AGN evolution. The central black hole masses for 172 quasars and Seyfert galaxies are calculated in this paper using the reverberation mapping method. The distributions of central black hole masses, redshifts and the Eddington accretion rates are analyzed, to verify the transition from the quasar to the Seyfert galaxy in the course of evolution.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351#table1</TD>
            <TD>2011-09-14T21:08:57Z</TD>
            <TD>#AGN#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-May-2010</TD>
            <TD>ivo://CDS.VizieR/J/other/ChA+A/32.351</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/ChA+A/32.351&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/ChA+A/32.351</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/520/A42 [1]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#1</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/520/A42</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/520/A42 [2]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#2</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/520/A42&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/520/A42 [table5]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#table5</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/520/A42&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/520/A42 [table4]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#table4</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/520/A42&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/520/A42 [1]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#1</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/520/A42</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/520/A42 [2]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#2</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/520/A42&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/520/A42 [table5]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#table5</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/520/A42&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/520/A42 [table4]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#table4</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/520/A42&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/520/A42 [1]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#1</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/520/A42</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/520/A42 [2]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#2</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/520/A42&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/520/A42 [table5]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#table5</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/520/A42&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/520/A42 [table4]</TD>
            <TD>Galaxy groups in the VIMOS-VLT Deep Survey (Cucciati+, 2010)</TD>
            <TD>We have compiled a homogeneous catalogue of optical galaxy groups identified in the VVDS-02h field (0.7x0.7deg^2^) by means of the VDM algorithm, in the range 0.2&lt;=z&lt;=1.0. We give the coordinates (RA, DE and z) and a few properties (velocity dispersion, number of galaxy members) of the so-found groups. We also list the galaxies that belong to these groups (ID, RA, DE, z, quality of redshift measurement).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42#table4</TD>
            <TD>2011-09-14T21:10:15Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Aug-2010</TD>
            <TD>ivo://CDS.VizieR/J/A+A/520/A42</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/520/A42&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/520/A42</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/489/923 [1]</TD>
            <TD>Abundances of stars in lower main sequence (Mishenina+, 2008)</TD>
            <TD>The aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923#1</TD>
            <TD>2011-09-14T21:12:20Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/489/923</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/923</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/489/923 [2]</TD>
            <TD>Abundances of stars in lower main sequence (Mishenina+, 2008)</TD>
            <TD>The aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923#2</TD>
            <TD>2011-09-14T21:12:20Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/489/923&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/923</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/489/923 [abund]</TD>
            <TD>Abundances of stars in lower main sequence (Mishenina+, 2008)</TD>
            <TD>The aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923#abund</TD>
            <TD>2011-09-14T21:12:20Z</TD>
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            <TD>18-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/489/923&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/923</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/489/923 [1]</TD>
            <TD>Abundances of stars in lower main sequence (Mishenina+, 2008)</TD>
            <TD>The aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923#1</TD>
            <TD>2011-09-14T21:12:20Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/489/923</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/923</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/489/923 [2]</TD>
            <TD>Abundances of stars in lower main sequence (Mishenina+, 2008)</TD>
            <TD>The aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923#2</TD>
            <TD>2011-09-14T21:12:20Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/489/923&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/923</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/489/923 [abund]</TD>
            <TD>Abundances of stars in lower main sequence (Mishenina+, 2008)</TD>
            <TD>The aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923#abund</TD>
            <TD>2011-09-14T21:12:20Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/489/923&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/923</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/489/923 [1]</TD>
            <TD>Abundances of stars in lower main sequence (Mishenina+, 2008)</TD>
            <TD>The aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923#1</TD>
            <TD>2011-09-14T21:12:20Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/489/923</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/923</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/489/923 [2]</TD>
            <TD>Abundances of stars in lower main sequence (Mishenina+, 2008)</TD>
            <TD>The aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923#2</TD>
            <TD>2011-09-14T21:12:20Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/489/923&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/923</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/489/923 [abund]</TD>
            <TD>Abundances of stars in lower main sequence (Mishenina+, 2008)</TD>
            <TD>The aim of this paper is to provide fundamental parameters and abundances with a high accuracy for a large sample of cool main sequence stars. This study is part of wider project, in which the metallicity distribution of the local thin disc is investigated from a complete sample of G and K dwarfs within 25pc. The stars were observed at high resolution and a high signal-to-noise ratio with the ELODIE echelle spectrograph. The Vsini were obtained with a calibration of the cross-correlation function. Effective temperatures were estimated by the line depth ratio method. Surface gravities (logg) were determined by two methods: parallaxes and ionization balance of iron. The Mg and Na abundances were derived using a non-LTE approximation. Abundances of other elements were obtained by measuring equivalent widths. Rotational velocities, atmospheric parameters Teff, logg, [Fe/H], Vt, and Li, O, Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Co, Ni, and Zn abundances are provided for 131 stars. Among them, more than 30 stars are active stars with a fraction of BY Dra and RS CVn type stars for which spectral peculiarities were investigated. We find the mean abundances of the majority of elements in active and non-active stars to be similar, except for Li, and possibly for Zn and Co. The lithium is reliably detected in 54% of active stars but only in 20% of non -active stars. No correlation is found between Li abundances and rotational velocities. A possible anticorrelation of log A(Li) with the index of chromospheric activity GrandS is observed. Active and non active cool dwarfs show similar dependencies of most elemental ratios vs [Fe/H]. This allows us to use such abundance ratios to study the chemical and dynamical evolution of the Galaxy. Among active stars, no clear correlation has been found between different indicators of activity for our sample stars.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923#abund</TD>
            <TD>2011-09-14T21:12:20Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>18-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/A+A/489/923</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/489/923&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/489/923</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/193/28 [1]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#1</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/193/28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/193/28 [2]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#2</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/28 [objects]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#objects</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/28 [table4]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#table4</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/28 [table1]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#table1</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/193/28 [1]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#1</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/193/28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/193/28 [2]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#2</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/28 [objects]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#objects</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/28 [table4]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#table4</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/28 [table1]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#table1</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/193/28 [1]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#1</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/193/28</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/193/28 [2]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#2</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/28 [objects]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#objects</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/28 [table4]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#table4</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/193/28 [table1]</TD>
            <TD>Galaxy survey around 20 UV-bright quasars (Prochaska+, 2011)</TD>
            <TD>We selected 20 fields accessible from Las Campanas Observatory (LCO) (DEC&lt;25{deg}) surrounding UV-bright quasars. These quasars and their UV spectroscopic data sets are summarized in Table 1. All of the fields in our survey were imaged with the Swope 40" telescope using a direct imaging camera in B and R filter. The data were obtained in a series of dithered exposures intended to map at least a 20'x20' FOV, between 2000 Oct 26 and 2003 Apr 8. We performed multi-slit spectroscopy on each field with the WFCCD spectrometer using the blue grism and the Tek 5 CCD, between 2001 Apr 17 and 2003 Jun 6.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28#table1</TD>
            <TD>2011-09-14T21:26:47Z</TD>
            <TD>#Photometry#Galaxies#Spectroscopy#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>19-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/193/28</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/193/28&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/193/28</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/404/325 [1]</TD>
            <TD>Massive galaxy clusters lensing analyse (Richard+, 2010)</TD>
            <TD>High-resolution imaging data taken with the Advanced Camera for Surveys (ACS) or Wide Field Planetary Camera 2 (WFPC2) instrument on HST are available for each selected cluster in one or two bands, either through our dedicated LoCuSS programme (GO-DD 11312, PI: G.P. Smith) or from the archive. J- and KS-band data were obtained between 2003 March and 2007 April on the following near-infrared instruments: Wide Infrared Camera (WIRC) on the Palomar-200-inch telescope, Infrared Side Port Imager (ISPI) on the CTIO Blanco 4-m telescope and Florida Infrared Imaging Multi-Object Spectrograph (FLAMINGOS) on the Kitt Peak (KPNO) 4-m telescope. We used the LRIS on the Keck-I telescope to perform long-slit and multislit observations of the clusters. The spectroscopic data used in the current paper are the outcome of six different observing runs between 2004 and 2008.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/325#1</TD>
            <TD>2011-09-14T21:26:50Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/325</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/404/325</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/325</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/404/325 [2]</TD>
            <TD>Massive galaxy clusters lensing analyse (Richard+, 2010)</TD>
            <TD>High-resolution imaging data taken with the Advanced Camera for Surveys (ACS) or Wide Field Planetary Camera 2 (WFPC2) instrument on HST are available for each selected cluster in one or two bands, either through our dedicated LoCuSS programme (GO-DD 11312, PI: G.P. Smith) or from the archive. J- and KS-band data were obtained between 2003 March and 2007 April on the following near-infrared instruments: Wide Infrared Camera (WIRC) on the Palomar-200-inch telescope, Infrared Side Port Imager (ISPI) on the CTIO Blanco 4-m telescope and Florida Infrared Imaging Multi-Object Spectrograph (FLAMINGOS) on the Kitt Peak (KPNO) 4-m telescope. We used the LRIS on the Keck-I telescope to perform long-slit and multislit observations of the clusters. The spectroscopic data used in the current paper are the outcome of six different observing runs between 2004 and 2008.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/325#2</TD>
            <TD>2011-09-14T21:26:50Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/325</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/404/325&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/325</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/404/325 [table4]</TD>
            <TD>Massive galaxy clusters lensing analyse (Richard+, 2010)</TD>
            <TD>High-resolution imaging data taken with the Advanced Camera for Surveys (ACS) or Wide Field Planetary Camera 2 (WFPC2) instrument on HST are available for each selected cluster in one or two bands, either through our dedicated LoCuSS programme (GO-DD 11312, PI: G.P. Smith) or from the archive. J- and KS-band data were obtained between 2003 March and 2007 April on the following near-infrared instruments: Wide Infrared Camera (WIRC) on the Palomar-200-inch telescope, Infrared Side Port Imager (ISPI) on the CTIO Blanco 4-m telescope and Florida Infrared Imaging Multi-Object Spectrograph (FLAMINGOS) on the Kitt Peak (KPNO) 4-m telescope. We used the LRIS on the Keck-I telescope to perform long-slit and multislit observations of the clusters. The spectroscopic data used in the current paper are the outcome of six different observing runs between 2004 and 2008.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/325#table4</TD>
            <TD>2011-09-14T21:26:50Z</TD>
            <TD>#Clusters_of_galaxies#Gravitational_lensing#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-May-2011</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/404/325</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/404/325&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/404/325</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/404/325 [1]</TD>
            <TD>Massive galaxy clusters lensing analyse (Richard+, 2010)</TD>
            <TD>High-resolution imaging data taken with the Advanced Camera for Surveys (ACS) or Wide Field Planetary Camera 2 (WFPC2) instrument on HST are available for each selected cluster in one or two bands, either through our dedicated LoCuSS programme (GO-DD 11312, PI: G.P. Smith) or from the archive. J- and KS-band data were obtained between 2003 March and 2007 April on the following near-infrared instruments: Wide Infrared Camera (WIRC) on the Palomar-200-inch telescope, Infrared Side Port Imager (ISPI) on the CTIO Blanco 4-m telescope and Florida Infrared Imaging Multi-Object Spectrograph (FLAMINGOS) on the Kitt Peak (KPNO) 4-m telescope. We used the LRIS on the Keck-I telescope to perform long-slit and multislit observations of the clusters. The spectroscopic data used in the current paper are the outcome of six different observing runs between 2004 and 2008.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>Massive galaxy clusters lensing analyse (Richard+, 2010)</TD>
            <TD>High-resolution imaging data taken with the Advanced Camera for Surveys (ACS) or Wide Field Planetary Camera 2 (WFPC2) instrument on HST are available for each selected cluster in one or two bands, either through our dedicated LoCuSS programme (GO-DD 11312, PI: G.P. Smith) or from the archive. J- and KS-band data were obtained between 2003 March and 2007 April on the following near-infrared instruments: Wide Infrared Camera (WIRC) on the Palomar-200-inch telescope, Infrared Side Port Imager (ISPI) on the CTIO Blanco 4-m telescope and Florida Infrared Imaging Multi-Object Spectrograph (FLAMINGOS) on the Kitt Peak (KPNO) 4-m telescope. We used the LRIS on the Keck-I telescope to perform long-slit and multislit observations of the clusters. The spectroscopic data used in the current paper are the outcome of six different observing runs between 2004 and 2008.</TD>
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            <TD>J/MNRAS/404/325 [1]</TD>
            <TD>Massive galaxy clusters lensing analyse (Richard+, 2010)</TD>
            <TD>High-resolution imaging data taken with the Advanced Camera for Surveys (ACS) or Wide Field Planetary Camera 2 (WFPC2) instrument on HST are available for each selected cluster in one or two bands, either through our dedicated LoCuSS programme (GO-DD 11312, PI: G.P. Smith) or from the archive. J- and KS-band data were obtained between 2003 March and 2007 April on the following near-infrared instruments: Wide Infrared Camera (WIRC) on the Palomar-200-inch telescope, Infrared Side Port Imager (ISPI) on the CTIO Blanco 4-m telescope and Florida Infrared Imaging Multi-Object Spectrograph (FLAMINGOS) on the Kitt Peak (KPNO) 4-m telescope. We used the LRIS on the Keck-I telescope to perform long-slit and multislit observations of the clusters. The spectroscopic data used in the current paper are the outcome of six different observing runs between 2004 and 2008.</TD>
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            <TD>HTTP Request</TD>
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            <TD>Massive galaxy clusters lensing analyse (Richard+, 2010)</TD>
            <TD>High-resolution imaging data taken with the Advanced Camera for Surveys (ACS) or Wide Field Planetary Camera 2 (WFPC2) instrument on HST are available for each selected cluster in one or two bands, either through our dedicated LoCuSS programme (GO-DD 11312, PI: G.P. Smith) or from the archive. J- and KS-band data were obtained between 2003 March and 2007 April on the following near-infrared instruments: Wide Infrared Camera (WIRC) on the Palomar-200-inch telescope, Infrared Side Port Imager (ISPI) on the CTIO Blanco 4-m telescope and Florida Infrared Imaging Multi-Object Spectrograph (FLAMINGOS) on the Kitt Peak (KPNO) 4-m telescope. We used the LRIS on the Keck-I telescope to perform long-slit and multislit observations of the clusters. The spectroscopic data used in the current paper are the outcome of six different observing runs between 2004 and 2008.</TD>
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            <TD>Web Page</TD>
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            <TD>Host and companion galaxies in the SDSS (Patton+, 2008)</TD>
            <TD>We measure the number of companions per galaxy (N_c_) as a function of r-band absolute magnitude for both the Sloan Digital Sky Survey (DR5) and the Croton and coworkers semianalytic catalog, 2006MNRAS.365...11C, applied to the Millennium Run simulation (Springel et al., 2005Natur.435..629S). For close pairs with projected separations of 5-20kpc/h, velocity differences less than 500km/s, and luminosity ratios between 1:2 and 2:1, we find good agreement between the observations and simulations, with N_c_ consistently close to 0.02 over the range -22&lt;M_r_&lt;-18. For larger pair separations, N_c_(M_r_) instead becomes increasingly steep toward the faint end, implying that luminosity-dependent clustering plays an important role on small scales. Using the simulations to assess and correct for projection effects, we infer that the real-space N_c_(M_r_) for close pairs peaks at about M^*^ and declines by at least a factor of 2 as M_r_ becomes fainter. Conversely, by measuring the number density of close companions, we estimate that at least 90% of all major mergers occur between galaxies which are fainter than L^*^. Finally, measurements of the luminosity density of close companions indicate that L^*^ galaxies likely dominate in terms of the overall importance of major mergers in the evolution of galaxy populations at low redshift.</TD>
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            <TD>HTTP Request</TD>
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            <TD>Host and companion galaxies in the SDSS (Patton+, 2008)</TD>
            <TD>We measure the number of companions per galaxy (N_c_) as a function of r-band absolute magnitude for both the Sloan Digital Sky Survey (DR5) and the Croton and coworkers semianalytic catalog, 2006MNRAS.365...11C, applied to the Millennium Run simulation (Springel et al., 2005Natur.435..629S). For close pairs with projected separations of 5-20kpc/h, velocity differences less than 500km/s, and luminosity ratios between 1:2 and 2:1, we find good agreement between the observations and simulations, with N_c_ consistently close to 0.02 over the range -22&lt;M_r_&lt;-18. For larger pair separations, N_c_(M_r_) instead becomes increasingly steep toward the faint end, implying that luminosity-dependent clustering plays an important role on small scales. Using the simulations to assess and correct for projection effects, we infer that the real-space N_c_(M_r_) for close pairs peaks at about M^*^ and declines by at least a factor of 2 as M_r_ becomes fainter. Conversely, by measuring the number density of close companions, we estimate that at least 90% of all major mergers occur between galaxies which are fainter than L^*^. Finally, measurements of the luminosity density of close companions indicate that L^*^ galaxies likely dominate in terms of the overall importance of major mergers in the evolution of galaxy populations at low redshift.</TD>
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            <TD>Host and companion galaxies in the SDSS (Patton+, 2008)</TD>
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            <TD>Host and companion galaxies in the SDSS (Patton+, 2008)</TD>
            <TD>We measure the number of companions per galaxy (N_c_) as a function of r-band absolute magnitude for both the Sloan Digital Sky Survey (DR5) and the Croton and coworkers semianalytic catalog, 2006MNRAS.365...11C, applied to the Millennium Run simulation (Springel et al., 2005Natur.435..629S). For close pairs with projected separations of 5-20kpc/h, velocity differences less than 500km/s, and luminosity ratios between 1:2 and 2:1, we find good agreement between the observations and simulations, with N_c_ consistently close to 0.02 over the range -22&lt;M_r_&lt;-18. For larger pair separations, N_c_(M_r_) instead becomes increasingly steep toward the faint end, implying that luminosity-dependent clustering plays an important role on small scales. Using the simulations to assess and correct for projection effects, we infer that the real-space N_c_(M_r_) for close pairs peaks at about M^*^ and declines by at least a factor of 2 as M_r_ becomes fainter. Conversely, by measuring the number density of close companions, we estimate that at least 90% of all major mergers occur between galaxies which are fainter than L^*^. Finally, measurements of the luminosity density of close companions indicate that L^*^ galaxies likely dominate in terms of the overall importance of major mergers in the evolution of galaxy populations at low redshift.</TD>
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            <TD>HTTP Request</TD>
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            <TD>Host and companion galaxies in the SDSS (Patton+, 2008)</TD>
            <TD>We measure the number of companions per galaxy (N_c_) as a function of r-band absolute magnitude for both the Sloan Digital Sky Survey (DR5) and the Croton and coworkers semianalytic catalog, 2006MNRAS.365...11C, applied to the Millennium Run simulation (Springel et al., 2005Natur.435..629S). For close pairs with projected separations of 5-20kpc/h, velocity differences less than 500km/s, and luminosity ratios between 1:2 and 2:1, we find good agreement between the observations and simulations, with N_c_ consistently close to 0.02 over the range -22&lt;M_r_&lt;-18. For larger pair separations, N_c_(M_r_) instead becomes increasingly steep toward the faint end, implying that luminosity-dependent clustering plays an important role on small scales. Using the simulations to assess and correct for projection effects, we infer that the real-space N_c_(M_r_) for close pairs peaks at about M^*^ and declines by at least a factor of 2 as M_r_ becomes fainter. Conversely, by measuring the number density of close companions, we estimate that at least 90% of all major mergers occur between galaxies which are fainter than L^*^. Finally, measurements of the luminosity density of close companions indicate that L^*^ galaxies likely dominate in terms of the overall importance of major mergers in the evolution of galaxy populations at low redshift.</TD>
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            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJ/685/235 [1]</TD>
            <TD>Host and companion galaxies in the SDSS (Patton+, 2008)</TD>
            <TD>We measure the number of companions per galaxy (N_c_) as a function of r-band absolute magnitude for both the Sloan Digital Sky Survey (DR5) and the Croton and coworkers semianalytic catalog, 2006MNRAS.365...11C, applied to the Millennium Run simulation (Springel et al., 2005Natur.435..629S). For close pairs with projected separations of 5-20kpc/h, velocity differences less than 500km/s, and luminosity ratios between 1:2 and 2:1, we find good agreement between the observations and simulations, with N_c_ consistently close to 0.02 over the range -22&lt;M_r_&lt;-18. For larger pair separations, N_c_(M_r_) instead becomes increasingly steep toward the faint end, implying that luminosity-dependent clustering plays an important role on small scales. Using the simulations to assess and correct for projection effects, we infer that the real-space N_c_(M_r_) for close pairs peaks at about M^*^ and declines by at least a factor of 2 as M_r_ becomes fainter. Conversely, by measuring the number density of close companions, we estimate that at least 90% of all major mergers occur between galaxies which are fainter than L^*^. Finally, measurements of the luminosity density of close companions indicate that L^*^ galaxies likely dominate in terms of the overall importance of major mergers in the evolution of galaxy populations at low redshift.</TD>
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            <TD>ivo://CDS.VizieR/J/ApJ/685/235#1</TD>
            <TD>2011-09-14T21:27:06Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/685/235</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/685/235</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/685/235</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/685/235 [2]</TD>
            <TD>Host and companion galaxies in the SDSS (Patton+, 2008)</TD>
            <TD>We measure the number of companions per galaxy (N_c_) as a function of r-band absolute magnitude for both the Sloan Digital Sky Survey (DR5) and the Croton and coworkers semianalytic catalog, 2006MNRAS.365...11C, applied to the Millennium Run simulation (Springel et al., 2005Natur.435..629S). For close pairs with projected separations of 5-20kpc/h, velocity differences less than 500km/s, and luminosity ratios between 1:2 and 2:1, we find good agreement between the observations and simulations, with N_c_ consistently close to 0.02 over the range -22&lt;M_r_&lt;-18. For larger pair separations, N_c_(M_r_) instead becomes increasingly steep toward the faint end, implying that luminosity-dependent clustering plays an important role on small scales. Using the simulations to assess and correct for projection effects, we infer that the real-space N_c_(M_r_) for close pairs peaks at about M^*^ and declines by at least a factor of 2 as M_r_ becomes fainter. Conversely, by measuring the number density of close companions, we estimate that at least 90% of all major mergers occur between galaxies which are fainter than L^*^. Finally, measurements of the luminosity density of close companions indicate that L^*^ galaxies likely dominate in terms of the overall importance of major mergers in the evolution of galaxy populations at low redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/685/235#2</TD>
            <TD>2011-09-14T21:27:06Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/685/235</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/685/235&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/685/235</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/685/235 [table1]</TD>
            <TD>Host and companion galaxies in the SDSS (Patton+, 2008)</TD>
            <TD>We measure the number of companions per galaxy (N_c_) as a function of r-band absolute magnitude for both the Sloan Digital Sky Survey (DR5) and the Croton and coworkers semianalytic catalog, 2006MNRAS.365...11C, applied to the Millennium Run simulation (Springel et al., 2005Natur.435..629S). For close pairs with projected separations of 5-20kpc/h, velocity differences less than 500km/s, and luminosity ratios between 1:2 and 2:1, we find good agreement between the observations and simulations, with N_c_ consistently close to 0.02 over the range -22&lt;M_r_&lt;-18. For larger pair separations, N_c_(M_r_) instead becomes increasingly steep toward the faint end, implying that luminosity-dependent clustering plays an important role on small scales. Using the simulations to assess and correct for projection effects, we infer that the real-space N_c_(M_r_) for close pairs peaks at about M^*^ and declines by at least a factor of 2 as M_r_ becomes fainter. Conversely, by measuring the number density of close companions, we estimate that at least 90% of all major mergers occur between galaxies which are fainter than L^*^. Finally, measurements of the luminosity density of close companions indicate that L^*^ galaxies likely dominate in terms of the overall importance of major mergers in the evolution of galaxy populations at low redshift.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/685/235#table1</TD>
            <TD>2011-09-14T21:27:06Z</TD>
            <TD>#Galaxies#Spectroscopy#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>13-Dec-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/685/235</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/685/235&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/685/235</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/85/805 [1]</TD>
            <TD>11cm radio continuum survey. IV. (Fuerst+ 1990)</TD>
            <TD>We analysed the 11cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 6483 radio sources with a maximum apparent size of 12' and peak flux densities &gt;40mJy/beam area. Point-like sources are almost evenly distributed over the surveyed area, except that we miss some sources in the highly confused inner part of the Galaxy and the Cygnus X complex. At Galactic longitudes l&gt;100deg the list of compact sources is almost complete above an integrated flux density limit of 70mJy. Most of them are extragalactic. Extended sources show a concentration towards the Galactic Plane. At longitudes l&lt;100deg the scale height is about 0.6deg. An excess of about 900 extended sources is most likely of Galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805#1</TD>
            <TD>2012-09-24T07:17:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/85/805</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/85/805</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/85/805 [2]</TD>
            <TD>11cm radio continuum survey. IV. (Fuerst+ 1990)</TD>
            <TD>We analysed the 11cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 6483 radio sources with a maximum apparent size of 12' and peak flux densities &gt;40mJy/beam area. Point-like sources are almost evenly distributed over the surveyed area, except that we miss some sources in the highly confused inner part of the Galaxy and the Cygnus X complex. At Galactic longitudes l&gt;100deg the list of compact sources is almost complete above an integrated flux density limit of 70mJy. Most of them are extragalactic. Extended sources show a concentration towards the Galactic Plane. At longitudes l&lt;100deg the scale height is about 0.6deg. An excess of about 900 extended sources is most likely of Galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805#2</TD>
            <TD>2012-09-24T07:17:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/85/805&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/85/805</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/85/805 [table1]</TD>
            <TD>11cm radio continuum survey. IV. (Fuerst+ 1990)</TD>
            <TD>We analysed the 11cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 6483 radio sources with a maximum apparent size of 12' and peak flux densities &gt;40mJy/beam area. Point-like sources are almost evenly distributed over the surveyed area, except that we miss some sources in the highly confused inner part of the Galaxy and the Cygnus X complex. At Galactic longitudes l&gt;100deg the list of compact sources is almost complete above an integrated flux density limit of 70mJy. Most of them are extragalactic. Extended sources show a concentration towards the Galactic Plane. At longitudes l&lt;100deg the scale height is about 0.6deg. An excess of about 900 extended sources is most likely of Galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805#table1</TD>
            <TD>2012-09-24T07:17:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/85/805&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/85/805</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/85/805 [1]</TD>
            <TD>11cm radio continuum survey. IV. (Fuerst+ 1990)</TD>
            <TD>We analysed the 11cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 6483 radio sources with a maximum apparent size of 12' and peak flux densities &gt;40mJy/beam area. Point-like sources are almost evenly distributed over the surveyed area, except that we miss some sources in the highly confused inner part of the Galaxy and the Cygnus X complex. At Galactic longitudes l&gt;100deg the list of compact sources is almost complete above an integrated flux density limit of 70mJy. Most of them are extragalactic. Extended sources show a concentration towards the Galactic Plane. At longitudes l&lt;100deg the scale height is about 0.6deg. An excess of about 900 extended sources is most likely of Galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805#1</TD>
            <TD>2012-09-24T07:17:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/85/805</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/85/805</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/85/805 [2]</TD>
            <TD>11cm radio continuum survey. IV. (Fuerst+ 1990)</TD>
            <TD>We analysed the 11cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 6483 radio sources with a maximum apparent size of 12' and peak flux densities &gt;40mJy/beam area. Point-like sources are almost evenly distributed over the surveyed area, except that we miss some sources in the highly confused inner part of the Galaxy and the Cygnus X complex. At Galactic longitudes l&gt;100deg the list of compact sources is almost complete above an integrated flux density limit of 70mJy. Most of them are extragalactic. Extended sources show a concentration towards the Galactic Plane. At longitudes l&lt;100deg the scale height is about 0.6deg. An excess of about 900 extended sources is most likely of Galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805#2</TD>
            <TD>2012-09-24T07:17:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/85/805&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/85/805</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/85/805 [table1]</TD>
            <TD>11cm radio continuum survey. IV. (Fuerst+ 1990)</TD>
            <TD>We analysed the 11cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 6483 radio sources with a maximum apparent size of 12' and peak flux densities &gt;40mJy/beam area. Point-like sources are almost evenly distributed over the surveyed area, except that we miss some sources in the highly confused inner part of the Galaxy and the Cygnus X complex. At Galactic longitudes l&gt;100deg the list of compact sources is almost complete above an integrated flux density limit of 70mJy. Most of them are extragalactic. Extended sources show a concentration towards the Galactic Plane. At longitudes l&lt;100deg the scale height is about 0.6deg. An excess of about 900 extended sources is most likely of Galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805#table1</TD>
            <TD>2012-09-24T07:17:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/85/805&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/85/805</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/85/805 [1]</TD>
            <TD>11cm radio continuum survey. IV. (Fuerst+ 1990)</TD>
            <TD>We analysed the 11cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 6483 radio sources with a maximum apparent size of 12' and peak flux densities &gt;40mJy/beam area. Point-like sources are almost evenly distributed over the surveyed area, except that we miss some sources in the highly confused inner part of the Galaxy and the Cygnus X complex. At Galactic longitudes l&gt;100deg the list of compact sources is almost complete above an integrated flux density limit of 70mJy. Most of them are extragalactic. Extended sources show a concentration towards the Galactic Plane. At longitudes l&lt;100deg the scale height is about 0.6deg. An excess of about 900 extended sources is most likely of Galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805#1</TD>
            <TD>2012-09-24T07:17:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/85/805</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/85/805</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/85/805 [2]</TD>
            <TD>11cm radio continuum survey. IV. (Fuerst+ 1990)</TD>
            <TD>We analysed the 11cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 6483 radio sources with a maximum apparent size of 12' and peak flux densities &gt;40mJy/beam area. Point-like sources are almost evenly distributed over the surveyed area, except that we miss some sources in the highly confused inner part of the Galaxy and the Cygnus X complex. At Galactic longitudes l&gt;100deg the list of compact sources is almost complete above an integrated flux density limit of 70mJy. Most of them are extragalactic. Extended sources show a concentration towards the Galactic Plane. At longitudes l&lt;100deg the scale height is about 0.6deg. An excess of about 900 extended sources is most likely of Galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805#2</TD>
            <TD>2012-09-24T07:17:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/85/805&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/85/805</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/85/805 [table1]</TD>
            <TD>11cm radio continuum survey. IV. (Fuerst+ 1990)</TD>
            <TD>We analysed the 11cm Galactic Plane survey carried out with the Effelsberg 100-m telescope for small diameter sources. We present a list of 6483 radio sources with a maximum apparent size of 12' and peak flux densities &gt;40mJy/beam area. Point-like sources are almost evenly distributed over the surveyed area, except that we miss some sources in the highly confused inner part of the Galaxy and the Cygnus X complex. At Galactic longitudes l&gt;100deg the list of compact sources is almost complete above an integrated flux density limit of 70mJy. Most of them are extragalactic. Extended sources show a concentration towards the Galactic Plane. At longitudes l&lt;100deg the scale height is about 0.6deg. An excess of about 900 extended sources is most likely of Galactic structure.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805#table1</TD>
            <TD>2012-09-24T07:17:11Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>03-Mar-1999</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/85/805</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/85/805&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/85/805</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/398/479 [1]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#1</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/398/479</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/398/479 [2]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#2</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/398/479&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/398/479 [table2]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#table2</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/398/479&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/398/479 [table1]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#table1</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/398/479&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/398/479 [1]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#1</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/398/479</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/398/479 [2]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#2</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/398/479&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/398/479 [table2]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#table2</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/398/479&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/398/479 [table1]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#table1</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/398/479&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/398/479 [1]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#1</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/398/479</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/398/479 [2]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#2</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/398/479&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/398/479 [table2]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#table2</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/398/479&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/398/479 [table1]</TD>
            <TD>Local galaxy flows within 5 Mpc (Karachentsev+, 2003)</TD>
            <TD>Images of sixteen galaxies were obtained with the Wide Field and Planetary Camera (WFPC2) aboard the Hubble Space Telescope (HST) between October 22, 1999 and July 26, 2001 as part of our HST snapshot survey of nearby galaxy candidates (Seitzer et al., 1999, BAAS, 31, 1380; Grebel et al. 2000, ASP Conf. Ser. 221, 147). The galaxies were observed with 600-second exposures taken in the F606W and F814W filters for each object. For photometric measurements we used the HSTphot stellar photometry package developed by Dolphin (2000PASP..112.1383D).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479#table1</TD>
            <TD>2012-09-24T07:25:55Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Mar-2003</TD>
            <TD>ivo://CDS.VizieR/J/A+A/398/479</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/398/479&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/398/479</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/252/102 [1]</TD>
            <TD>Radio sources in bright spiral galaxies. II. (Condon+, 1982)</TD>
            <TD>Statistically complete samples comprising 33 bright spiral galaxies that are strong radio sources were selected. Sixteen of the galaxies have integrated radio-to-optical flux ratios greater than 10 times the median value for normal spirals. The remainder contain radio cores &lt;=20" in size and stronger than 90mJy at 1415MHz or 60mJy at 2695MHz. High-resolution (2" at 1413MHz or 0.6" at 4885MHz) maps of these galaxies were made with the Very Large Array. The radio sources are usually confined to the central 1kpc of the galaxies, lying within and extending parallel to their stellar disks. There is no evidence for ejection from central components. Most of the sources appear to be coextensive with regions of intense star formation (bolometric luminosities ~10^10-10^11L_{Sun}). The typical radio luminosity, ~10^21^W/Hz/sr at 1413MHz, of the resolved sources can be explained by synchrotron radiation from supernova remnants (SNRs) produced at the rate of ~1/yr. Five of the radio sources are &lt;=1pc in size and probably are not related to star formation or SNRs. The radio and 10-{mu}m flux densities of the extended sources are roughly proportional. The bolometric mass-to luminosity ratios in some active regions are too low to have been maintained for a Hubble time. Nearly all of the strong, extended radio sources are found in galaxies with nearby companions, so most of the episodic bursts of star formation are apparently triggered by galaxy-galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102#1</TD>
            <TD>2012-09-24T07:32:05Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/252/102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/252/102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/252/102 [2]</TD>
            <TD>Radio sources in bright spiral galaxies. II. (Condon+, 1982)</TD>
            <TD>Statistically complete samples comprising 33 bright spiral galaxies that are strong radio sources were selected. Sixteen of the galaxies have integrated radio-to-optical flux ratios greater than 10 times the median value for normal spirals. The remainder contain radio cores &lt;=20" in size and stronger than 90mJy at 1415MHz or 60mJy at 2695MHz. High-resolution (2" at 1413MHz or 0.6" at 4885MHz) maps of these galaxies were made with the Very Large Array. The radio sources are usually confined to the central 1kpc of the galaxies, lying within and extending parallel to their stellar disks. There is no evidence for ejection from central components. Most of the sources appear to be coextensive with regions of intense star formation (bolometric luminosities ~10^10-10^11L_{Sun}). The typical radio luminosity, ~10^21^W/Hz/sr at 1413MHz, of the resolved sources can be explained by synchrotron radiation from supernova remnants (SNRs) produced at the rate of ~1/yr. Five of the radio sources are &lt;=1pc in size and probably are not related to star formation or SNRs. The radio and 10-{mu}m flux densities of the extended sources are roughly proportional. The bolometric mass-to luminosity ratios in some active regions are too low to have been maintained for a Hubble time. Nearly all of the strong, extended radio sources are found in galaxies with nearby companions, so most of the episodic bursts of star formation are apparently triggered by galaxy-galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102#2</TD>
            <TD>2012-09-24T07:32:05Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/252/102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/252/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/252/102 [table3]</TD>
            <TD>Radio sources in bright spiral galaxies. II. (Condon+, 1982)</TD>
            <TD>Statistically complete samples comprising 33 bright spiral galaxies that are strong radio sources were selected. Sixteen of the galaxies have integrated radio-to-optical flux ratios greater than 10 times the median value for normal spirals. The remainder contain radio cores &lt;=20" in size and stronger than 90mJy at 1415MHz or 60mJy at 2695MHz. High-resolution (2" at 1413MHz or 0.6" at 4885MHz) maps of these galaxies were made with the Very Large Array. The radio sources are usually confined to the central 1kpc of the galaxies, lying within and extending parallel to their stellar disks. There is no evidence for ejection from central components. Most of the sources appear to be coextensive with regions of intense star formation (bolometric luminosities ~10^10-10^11L_{Sun}). The typical radio luminosity, ~10^21^W/Hz/sr at 1413MHz, of the resolved sources can be explained by synchrotron radiation from supernova remnants (SNRs) produced at the rate of ~1/yr. Five of the radio sources are &lt;=1pc in size and probably are not related to star formation or SNRs. The radio and 10-{mu}m flux densities of the extended sources are roughly proportional. The bolometric mass-to luminosity ratios in some active regions are too low to have been maintained for a Hubble time. Nearly all of the strong, extended radio sources are found in galaxies with nearby companions, so most of the episodic bursts of star formation are apparently triggered by galaxy-galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102#table3</TD>
            <TD>2012-09-24T07:32:05Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/252/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/252/102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/252/102 [1]</TD>
            <TD>Radio sources in bright spiral galaxies. II. (Condon+, 1982)</TD>
            <TD>Statistically complete samples comprising 33 bright spiral galaxies that are strong radio sources were selected. Sixteen of the galaxies have integrated radio-to-optical flux ratios greater than 10 times the median value for normal spirals. The remainder contain radio cores &lt;=20" in size and stronger than 90mJy at 1415MHz or 60mJy at 2695MHz. High-resolution (2" at 1413MHz or 0.6" at 4885MHz) maps of these galaxies were made with the Very Large Array. The radio sources are usually confined to the central 1kpc of the galaxies, lying within and extending parallel to their stellar disks. There is no evidence for ejection from central components. Most of the sources appear to be coextensive with regions of intense star formation (bolometric luminosities ~10^10-10^11L_{Sun}). The typical radio luminosity, ~10^21^W/Hz/sr at 1413MHz, of the resolved sources can be explained by synchrotron radiation from supernova remnants (SNRs) produced at the rate of ~1/yr. Five of the radio sources are &lt;=1pc in size and probably are not related to star formation or SNRs. The radio and 10-{mu}m flux densities of the extended sources are roughly proportional. The bolometric mass-to luminosity ratios in some active regions are too low to have been maintained for a Hubble time. Nearly all of the strong, extended radio sources are found in galaxies with nearby companions, so most of the episodic bursts of star formation are apparently triggered by galaxy-galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102#1</TD>
            <TD>2012-09-24T07:32:05Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/252/102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/252/102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/252/102 [2]</TD>
            <TD>Radio sources in bright spiral galaxies. II. (Condon+, 1982)</TD>
            <TD>Statistically complete samples comprising 33 bright spiral galaxies that are strong radio sources were selected. Sixteen of the galaxies have integrated radio-to-optical flux ratios greater than 10 times the median value for normal spirals. The remainder contain radio cores &lt;=20" in size and stronger than 90mJy at 1415MHz or 60mJy at 2695MHz. High-resolution (2" at 1413MHz or 0.6" at 4885MHz) maps of these galaxies were made with the Very Large Array. The radio sources are usually confined to the central 1kpc of the galaxies, lying within and extending parallel to their stellar disks. There is no evidence for ejection from central components. Most of the sources appear to be coextensive with regions of intense star formation (bolometric luminosities ~10^10-10^11L_{Sun}). The typical radio luminosity, ~10^21^W/Hz/sr at 1413MHz, of the resolved sources can be explained by synchrotron radiation from supernova remnants (SNRs) produced at the rate of ~1/yr. Five of the radio sources are &lt;=1pc in size and probably are not related to star formation or SNRs. The radio and 10-{mu}m flux densities of the extended sources are roughly proportional. The bolometric mass-to luminosity ratios in some active regions are too low to have been maintained for a Hubble time. Nearly all of the strong, extended radio sources are found in galaxies with nearby companions, so most of the episodic bursts of star formation are apparently triggered by galaxy-galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102#2</TD>
            <TD>2012-09-24T07:32:05Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/252/102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/252/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/252/102 [table3]</TD>
            <TD>Radio sources in bright spiral galaxies. II. (Condon+, 1982)</TD>
            <TD>Statistically complete samples comprising 33 bright spiral galaxies that are strong radio sources were selected. Sixteen of the galaxies have integrated radio-to-optical flux ratios greater than 10 times the median value for normal spirals. The remainder contain radio cores &lt;=20" in size and stronger than 90mJy at 1415MHz or 60mJy at 2695MHz. High-resolution (2" at 1413MHz or 0.6" at 4885MHz) maps of these galaxies were made with the Very Large Array. The radio sources are usually confined to the central 1kpc of the galaxies, lying within and extending parallel to their stellar disks. There is no evidence for ejection from central components. Most of the sources appear to be coextensive with regions of intense star formation (bolometric luminosities ~10^10-10^11L_{Sun}). The typical radio luminosity, ~10^21^W/Hz/sr at 1413MHz, of the resolved sources can be explained by synchrotron radiation from supernova remnants (SNRs) produced at the rate of ~1/yr. Five of the radio sources are &lt;=1pc in size and probably are not related to star formation or SNRs. The radio and 10-{mu}m flux densities of the extended sources are roughly proportional. The bolometric mass-to luminosity ratios in some active regions are too low to have been maintained for a Hubble time. Nearly all of the strong, extended radio sources are found in galaxies with nearby companions, so most of the episodic bursts of star formation are apparently triggered by galaxy-galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102#table3</TD>
            <TD>2012-09-24T07:32:05Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/252/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/252/102</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/252/102 [1]</TD>
            <TD>Radio sources in bright spiral galaxies. II. (Condon+, 1982)</TD>
            <TD>Statistically complete samples comprising 33 bright spiral galaxies that are strong radio sources were selected. Sixteen of the galaxies have integrated radio-to-optical flux ratios greater than 10 times the median value for normal spirals. The remainder contain radio cores &lt;=20" in size and stronger than 90mJy at 1415MHz or 60mJy at 2695MHz. High-resolution (2" at 1413MHz or 0.6" at 4885MHz) maps of these galaxies were made with the Very Large Array. The radio sources are usually confined to the central 1kpc of the galaxies, lying within and extending parallel to their stellar disks. There is no evidence for ejection from central components. Most of the sources appear to be coextensive with regions of intense star formation (bolometric luminosities ~10^10-10^11L_{Sun}). The typical radio luminosity, ~10^21^W/Hz/sr at 1413MHz, of the resolved sources can be explained by synchrotron radiation from supernova remnants (SNRs) produced at the rate of ~1/yr. Five of the radio sources are &lt;=1pc in size and probably are not related to star formation or SNRs. The radio and 10-{mu}m flux densities of the extended sources are roughly proportional. The bolometric mass-to luminosity ratios in some active regions are too low to have been maintained for a Hubble time. Nearly all of the strong, extended radio sources are found in galaxies with nearby companions, so most of the episodic bursts of star formation are apparently triggered by galaxy-galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102#1</TD>
            <TD>2012-09-24T07:32:05Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/252/102</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/252/102</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/252/102 [2]</TD>
            <TD>Radio sources in bright spiral galaxies. II. (Condon+, 1982)</TD>
            <TD>Statistically complete samples comprising 33 bright spiral galaxies that are strong radio sources were selected. Sixteen of the galaxies have integrated radio-to-optical flux ratios greater than 10 times the median value for normal spirals. The remainder contain radio cores &lt;=20" in size and stronger than 90mJy at 1415MHz or 60mJy at 2695MHz. High-resolution (2" at 1413MHz or 0.6" at 4885MHz) maps of these galaxies were made with the Very Large Array. The radio sources are usually confined to the central 1kpc of the galaxies, lying within and extending parallel to their stellar disks. There is no evidence for ejection from central components. Most of the sources appear to be coextensive with regions of intense star formation (bolometric luminosities ~10^10-10^11L_{Sun}). The typical radio luminosity, ~10^21^W/Hz/sr at 1413MHz, of the resolved sources can be explained by synchrotron radiation from supernova remnants (SNRs) produced at the rate of ~1/yr. Five of the radio sources are &lt;=1pc in size and probably are not related to star formation or SNRs. The radio and 10-{mu}m flux densities of the extended sources are roughly proportional. The bolometric mass-to luminosity ratios in some active regions are too low to have been maintained for a Hubble time. Nearly all of the strong, extended radio sources are found in galaxies with nearby companions, so most of the episodic bursts of star formation are apparently triggered by galaxy-galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102#2</TD>
            <TD>2012-09-24T07:32:05Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/252/102&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/252/102</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/252/102 [table3]</TD>
            <TD>Radio sources in bright spiral galaxies. II. (Condon+, 1982)</TD>
            <TD>Statistically complete samples comprising 33 bright spiral galaxies that are strong radio sources were selected. Sixteen of the galaxies have integrated radio-to-optical flux ratios greater than 10 times the median value for normal spirals. The remainder contain radio cores &lt;=20" in size and stronger than 90mJy at 1415MHz or 60mJy at 2695MHz. High-resolution (2" at 1413MHz or 0.6" at 4885MHz) maps of these galaxies were made with the Very Large Array. The radio sources are usually confined to the central 1kpc of the galaxies, lying within and extending parallel to their stellar disks. There is no evidence for ejection from central components. Most of the sources appear to be coextensive with regions of intense star formation (bolometric luminosities ~10^10-10^11L_{Sun}). The typical radio luminosity, ~10^21^W/Hz/sr at 1413MHz, of the resolved sources can be explained by synchrotron radiation from supernova remnants (SNRs) produced at the rate of ~1/yr. Five of the radio sources are &lt;=1pc in size and probably are not related to star formation or SNRs. The radio and 10-{mu}m flux densities of the extended sources are roughly proportional. The bolometric mass-to luminosity ratios in some active regions are too low to have been maintained for a Hubble time. Nearly all of the strong, extended radio sources are found in galaxies with nearby companions, so most of the episodic bursts of star formation are apparently triggered by galaxy-galaxy interactions.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102#table3</TD>
            <TD>2012-09-24T07:32:05Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>20-Nov-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/252/102</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/252/102&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/252/102</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/61/451 [1]</TD>
            <TD>The 37W catalogue of radio sources in M31 (Walterbos+ 1985)</TD>
            <TD>The radio continuum emission of the spiral galaxy M31 has been mapped at a wavelength of 21cm with the Westerbork Synthesis Radio Telescope, at an angular resolution of 23"x35", corresponding to a linear resolution of 70x115pc. Five fields have been observed which, when combined, cover the main part of the disk of M31. A catalogue of sources inside the M31 area with a flux density larger than 1mJy (five times the rms noise) is presented.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451#1</TD>
            <TD>2012-09-24T07:48:54Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/61/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/61/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/61/451 [2]</TD>
            <TD>The 37W catalogue of radio sources in M31 (Walterbos+ 1985)</TD>
            <TD>The radio continuum emission of the spiral galaxy M31 has been mapped at a wavelength of 21cm with the Westerbork Synthesis Radio Telescope, at an angular resolution of 23"x35", corresponding to a linear resolution of 70x115pc. Five fields have been observed which, when combined, cover the main part of the disk of M31. A catalogue of sources inside the M31 area with a flux density larger than 1mJy (five times the rms noise) is presented.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451#2</TD>
            <TD>2012-09-24T07:48:54Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/61/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/61/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/61/451 [table3]</TD>
            <TD>The 37W catalogue of radio sources in M31 (Walterbos+ 1985)</TD>
            <TD>The radio continuum emission of the spiral galaxy M31 has been mapped at a wavelength of 21cm with the Westerbork Synthesis Radio Telescope, at an angular resolution of 23"x35", corresponding to a linear resolution of 70x115pc. Five fields have been observed which, when combined, cover the main part of the disk of M31. A catalogue of sources inside the M31 area with a flux density larger than 1mJy (five times the rms noise) is presented.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451#table3</TD>
            <TD>2012-09-24T07:48:54Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/61/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/61/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/61/451 [1]</TD>
            <TD>The 37W catalogue of radio sources in M31 (Walterbos+ 1985)</TD>
            <TD>The radio continuum emission of the spiral galaxy M31 has been mapped at a wavelength of 21cm with the Westerbork Synthesis Radio Telescope, at an angular resolution of 23"x35", corresponding to a linear resolution of 70x115pc. Five fields have been observed which, when combined, cover the main part of the disk of M31. A catalogue of sources inside the M31 area with a flux density larger than 1mJy (five times the rms noise) is presented.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451#1</TD>
            <TD>2012-09-24T07:48:54Z</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/61/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/61/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/61/451 [2]</TD>
            <TD>The 37W catalogue of radio sources in M31 (Walterbos+ 1985)</TD>
            <TD>The radio continuum emission of the spiral galaxy M31 has been mapped at a wavelength of 21cm with the Westerbork Synthesis Radio Telescope, at an angular resolution of 23"x35", corresponding to a linear resolution of 70x115pc. Five fields have been observed which, when combined, cover the main part of the disk of M31. A catalogue of sources inside the M31 area with a flux density larger than 1mJy (five times the rms noise) is presented.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451#2</TD>
            <TD>2012-09-24T07:48:54Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/61/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/61/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/61/451 [table3]</TD>
            <TD>The 37W catalogue of radio sources in M31 (Walterbos+ 1985)</TD>
            <TD>The radio continuum emission of the spiral galaxy M31 has been mapped at a wavelength of 21cm with the Westerbork Synthesis Radio Telescope, at an angular resolution of 23"x35", corresponding to a linear resolution of 70x115pc. Five fields have been observed which, when combined, cover the main part of the disk of M31. A catalogue of sources inside the M31 area with a flux density larger than 1mJy (five times the rms noise) is presented.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451#table3</TD>
            <TD>2012-09-24T07:48:54Z</TD>
            <TD>##</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/61/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/61/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+AS/61/451 [1]</TD>
            <TD>The 37W catalogue of radio sources in M31 (Walterbos+ 1985)</TD>
            <TD>The radio continuum emission of the spiral galaxy M31 has been mapped at a wavelength of 21cm with the Westerbork Synthesis Radio Telescope, at an angular resolution of 23"x35", corresponding to a linear resolution of 70x115pc. Five fields have been observed which, when combined, cover the main part of the disk of M31. A catalogue of sources inside the M31 area with a flux density larger than 1mJy (five times the rms noise) is presented.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451#1</TD>
            <TD>2012-09-24T07:48:54Z</TD>
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            <TD>05-Aug-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+AS/61/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/61/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+AS/61/451 [2]</TD>
            <TD>The 37W catalogue of radio sources in M31 (Walterbos+ 1985)</TD>
            <TD>The radio continuum emission of the spiral galaxy M31 has been mapped at a wavelength of 21cm with the Westerbork Synthesis Radio Telescope, at an angular resolution of 23"x35", corresponding to a linear resolution of 70x115pc. Five fields have been observed which, when combined, cover the main part of the disk of M31. A catalogue of sources inside the M31 area with a flux density larger than 1mJy (five times the rms noise) is presented.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451#2</TD>
            <TD>2012-09-24T07:48:54Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+AS/61/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+AS/61/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+AS/61/451 [table3]</TD>
            <TD>The 37W catalogue of radio sources in M31 (Walterbos+ 1985)</TD>
            <TD>The radio continuum emission of the spiral galaxy M31 has been mapped at a wavelength of 21cm with the Westerbork Synthesis Radio Telescope, at an angular resolution of 23"x35", corresponding to a linear resolution of 70x115pc. Five fields have been observed which, when combined, cover the main part of the disk of M31. A catalogue of sources inside the M31 area with a flux density larger than 1mJy (five times the rms noise) is presented.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451#table3</TD>
            <TD>2012-09-24T07:48:54Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Aug-2002</TD>
            <TD>ivo://CDS.VizieR/J/A+AS/61/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+AS/61/451&amp;</TD>
            <TD>180</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/89/57 [1]</TD>
            <TD>IRAS galaxies behind southern Milky Way (Yamada+, 1993)</TD>
            <TD>We systematically searched for IRAS galaxies with 60nm flux density larger than 0.6Jy by using the UK Schmidt Infrared and IIIa-J Atlases in the Milky Way region (|b|&lt;15{deg}) between l=210{deg} and 360{deg}. We first selected about 4000 IRAS point sources by using our far-infrared criteria, which are optimized for the search of IRAS galaxies behind the Milky Way region, and then inspected visually the optical counterparts of them on the Schmidt Atlas film copies. We found 966 IRAS sources associated with galaxy-like objects. The list of the objects is presented here with the IRAS source name, Galactic coordinates, IRAS flux densities, field number and emulsion of the Atlas, type and size of galaxy(-like) image, redshift, multiplicity, and cross-identification. Of these, 423 galaxies are already catalogued in the Catalog of Galaxies and Quasars Observed in the IRAS Survey (Cat. &lt;VII/113&gt;), and most of the remaining 543 galaxy candidates are newly identified in this search. Although the radial velocities are known for only 387 galaxies, of which 60 were newly measured by us so far, we inferred the contamination by Galactic objects to be small from the good correlation between the sky distributions of the newly identified galaxy candidates and the previously catalogued galaxies. In the regions where the Galactic molecular clouds dominate, almost all the sources were not identified as galaxies. The detected galaxies are clustered in the three regions around l=240{deg}, 280{deg}, and 315{deg}, where the projected number densities are higher than the whole-sky average of IRAS galaxies of the same flux limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57#1</TD>
            <TD>2012-09-24T08:53:10Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/89/57</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/89/57</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/89/57 [2]</TD>
            <TD>IRAS galaxies behind southern Milky Way (Yamada+, 1993)</TD>
            <TD>We systematically searched for IRAS galaxies with 60nm flux density larger than 0.6Jy by using the UK Schmidt Infrared and IIIa-J Atlases in the Milky Way region (|b|&lt;15{deg}) between l=210{deg} and 360{deg}. We first selected about 4000 IRAS point sources by using our far-infrared criteria, which are optimized for the search of IRAS galaxies behind the Milky Way region, and then inspected visually the optical counterparts of them on the Schmidt Atlas film copies. We found 966 IRAS sources associated with galaxy-like objects. The list of the objects is presented here with the IRAS source name, Galactic coordinates, IRAS flux densities, field number and emulsion of the Atlas, type and size of galaxy(-like) image, redshift, multiplicity, and cross-identification. Of these, 423 galaxies are already catalogued in the Catalog of Galaxies and Quasars Observed in the IRAS Survey (Cat. &lt;VII/113&gt;), and most of the remaining 543 galaxy candidates are newly identified in this search. Although the radial velocities are known for only 387 galaxies, of which 60 were newly measured by us so far, we inferred the contamination by Galactic objects to be small from the good correlation between the sky distributions of the newly identified galaxy candidates and the previously catalogued galaxies. In the regions where the Galactic molecular clouds dominate, almost all the sources were not identified as galaxies. The detected galaxies are clustered in the three regions around l=240{deg}, 280{deg}, and 315{deg}, where the projected number densities are higher than the whole-sky average of IRAS galaxies of the same flux limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57#2</TD>
            <TD>2012-09-24T08:53:10Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/89/57&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/89/57</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/89/57 [table5]</TD>
            <TD>IRAS galaxies behind southern Milky Way (Yamada+, 1993)</TD>
            <TD>We systematically searched for IRAS galaxies with 60nm flux density larger than 0.6Jy by using the UK Schmidt Infrared and IIIa-J Atlases in the Milky Way region (|b|&lt;15{deg}) between l=210{deg} and 360{deg}. We first selected about 4000 IRAS point sources by using our far-infrared criteria, which are optimized for the search of IRAS galaxies behind the Milky Way region, and then inspected visually the optical counterparts of them on the Schmidt Atlas film copies. We found 966 IRAS sources associated with galaxy-like objects. The list of the objects is presented here with the IRAS source name, Galactic coordinates, IRAS flux densities, field number and emulsion of the Atlas, type and size of galaxy(-like) image, redshift, multiplicity, and cross-identification. Of these, 423 galaxies are already catalogued in the Catalog of Galaxies and Quasars Observed in the IRAS Survey (Cat. &lt;VII/113&gt;), and most of the remaining 543 galaxy candidates are newly identified in this search. Although the radial velocities are known for only 387 galaxies, of which 60 were newly measured by us so far, we inferred the contamination by Galactic objects to be small from the good correlation between the sky distributions of the newly identified galaxy candidates and the previously catalogued galaxies. In the regions where the Galactic molecular clouds dominate, almost all the sources were not identified as galaxies. The detected galaxies are clustered in the three regions around l=240{deg}, 280{deg}, and 315{deg}, where the projected number densities are higher than the whole-sky average of IRAS galaxies of the same flux limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57#table5</TD>
            <TD>2012-09-24T08:53:10Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/89/57&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/89/57</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/89/57 [1]</TD>
            <TD>IRAS galaxies behind southern Milky Way (Yamada+, 1993)</TD>
            <TD>We systematically searched for IRAS galaxies with 60nm flux density larger than 0.6Jy by using the UK Schmidt Infrared and IIIa-J Atlases in the Milky Way region (|b|&lt;15{deg}) between l=210{deg} and 360{deg}. We first selected about 4000 IRAS point sources by using our far-infrared criteria, which are optimized for the search of IRAS galaxies behind the Milky Way region, and then inspected visually the optical counterparts of them on the Schmidt Atlas film copies. We found 966 IRAS sources associated with galaxy-like objects. The list of the objects is presented here with the IRAS source name, Galactic coordinates, IRAS flux densities, field number and emulsion of the Atlas, type and size of galaxy(-like) image, redshift, multiplicity, and cross-identification. Of these, 423 galaxies are already catalogued in the Catalog of Galaxies and Quasars Observed in the IRAS Survey (Cat. &lt;VII/113&gt;), and most of the remaining 543 galaxy candidates are newly identified in this search. Although the radial velocities are known for only 387 galaxies, of which 60 were newly measured by us so far, we inferred the contamination by Galactic objects to be small from the good correlation between the sky distributions of the newly identified galaxy candidates and the previously catalogued galaxies. In the regions where the Galactic molecular clouds dominate, almost all the sources were not identified as galaxies. The detected galaxies are clustered in the three regions around l=240{deg}, 280{deg}, and 315{deg}, where the projected number densities are higher than the whole-sky average of IRAS galaxies of the same flux limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57#1</TD>
            <TD>2012-09-24T08:53:10Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/89/57</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/89/57</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/89/57 [2]</TD>
            <TD>IRAS galaxies behind southern Milky Way (Yamada+, 1993)</TD>
            <TD>We systematically searched for IRAS galaxies with 60nm flux density larger than 0.6Jy by using the UK Schmidt Infrared and IIIa-J Atlases in the Milky Way region (|b|&lt;15{deg}) between l=210{deg} and 360{deg}. We first selected about 4000 IRAS point sources by using our far-infrared criteria, which are optimized for the search of IRAS galaxies behind the Milky Way region, and then inspected visually the optical counterparts of them on the Schmidt Atlas film copies. We found 966 IRAS sources associated with galaxy-like objects. The list of the objects is presented here with the IRAS source name, Galactic coordinates, IRAS flux densities, field number and emulsion of the Atlas, type and size of galaxy(-like) image, redshift, multiplicity, and cross-identification. Of these, 423 galaxies are already catalogued in the Catalog of Galaxies and Quasars Observed in the IRAS Survey (Cat. &lt;VII/113&gt;), and most of the remaining 543 galaxy candidates are newly identified in this search. Although the radial velocities are known for only 387 galaxies, of which 60 were newly measured by us so far, we inferred the contamination by Galactic objects to be small from the good correlation between the sky distributions of the newly identified galaxy candidates and the previously catalogued galaxies. In the regions where the Galactic molecular clouds dominate, almost all the sources were not identified as galaxies. The detected galaxies are clustered in the three regions around l=240{deg}, 280{deg}, and 315{deg}, where the projected number densities are higher than the whole-sky average of IRAS galaxies of the same flux limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57#2</TD>
            <TD>2012-09-24T08:53:10Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/89/57&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/89/57</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/89/57 [table5]</TD>
            <TD>IRAS galaxies behind southern Milky Way (Yamada+, 1993)</TD>
            <TD>We systematically searched for IRAS galaxies with 60nm flux density larger than 0.6Jy by using the UK Schmidt Infrared and IIIa-J Atlases in the Milky Way region (|b|&lt;15{deg}) between l=210{deg} and 360{deg}. We first selected about 4000 IRAS point sources by using our far-infrared criteria, which are optimized for the search of IRAS galaxies behind the Milky Way region, and then inspected visually the optical counterparts of them on the Schmidt Atlas film copies. We found 966 IRAS sources associated with galaxy-like objects. The list of the objects is presented here with the IRAS source name, Galactic coordinates, IRAS flux densities, field number and emulsion of the Atlas, type and size of galaxy(-like) image, redshift, multiplicity, and cross-identification. Of these, 423 galaxies are already catalogued in the Catalog of Galaxies and Quasars Observed in the IRAS Survey (Cat. &lt;VII/113&gt;), and most of the remaining 543 galaxy candidates are newly identified in this search. Although the radial velocities are known for only 387 galaxies, of which 60 were newly measured by us so far, we inferred the contamination by Galactic objects to be small from the good correlation between the sky distributions of the newly identified galaxy candidates and the previously catalogued galaxies. In the regions where the Galactic molecular clouds dominate, almost all the sources were not identified as galaxies. The detected galaxies are clustered in the three regions around l=240{deg}, 280{deg}, and 315{deg}, where the projected number densities are higher than the whole-sky average of IRAS galaxies of the same flux limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57#table5</TD>
            <TD>2012-09-24T08:53:10Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/89/57&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/89/57</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/89/57 [1]</TD>
            <TD>IRAS galaxies behind southern Milky Way (Yamada+, 1993)</TD>
            <TD>We systematically searched for IRAS galaxies with 60nm flux density larger than 0.6Jy by using the UK Schmidt Infrared and IIIa-J Atlases in the Milky Way region (|b|&lt;15{deg}) between l=210{deg} and 360{deg}. We first selected about 4000 IRAS point sources by using our far-infrared criteria, which are optimized for the search of IRAS galaxies behind the Milky Way region, and then inspected visually the optical counterparts of them on the Schmidt Atlas film copies. We found 966 IRAS sources associated with galaxy-like objects. The list of the objects is presented here with the IRAS source name, Galactic coordinates, IRAS flux densities, field number and emulsion of the Atlas, type and size of galaxy(-like) image, redshift, multiplicity, and cross-identification. Of these, 423 galaxies are already catalogued in the Catalog of Galaxies and Quasars Observed in the IRAS Survey (Cat. &lt;VII/113&gt;), and most of the remaining 543 galaxy candidates are newly identified in this search. Although the radial velocities are known for only 387 galaxies, of which 60 were newly measured by us so far, we inferred the contamination by Galactic objects to be small from the good correlation between the sky distributions of the newly identified galaxy candidates and the previously catalogued galaxies. In the regions where the Galactic molecular clouds dominate, almost all the sources were not identified as galaxies. The detected galaxies are clustered in the three regions around l=240{deg}, 280{deg}, and 315{deg}, where the projected number densities are higher than the whole-sky average of IRAS galaxies of the same flux limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57#1</TD>
            <TD>2012-09-24T08:53:10Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/89/57</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/89/57</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/89/57 [2]</TD>
            <TD>IRAS galaxies behind southern Milky Way (Yamada+, 1993)</TD>
            <TD>We systematically searched for IRAS galaxies with 60nm flux density larger than 0.6Jy by using the UK Schmidt Infrared and IIIa-J Atlases in the Milky Way region (|b|&lt;15{deg}) between l=210{deg} and 360{deg}. We first selected about 4000 IRAS point sources by using our far-infrared criteria, which are optimized for the search of IRAS galaxies behind the Milky Way region, and then inspected visually the optical counterparts of them on the Schmidt Atlas film copies. We found 966 IRAS sources associated with galaxy-like objects. The list of the objects is presented here with the IRAS source name, Galactic coordinates, IRAS flux densities, field number and emulsion of the Atlas, type and size of galaxy(-like) image, redshift, multiplicity, and cross-identification. Of these, 423 galaxies are already catalogued in the Catalog of Galaxies and Quasars Observed in the IRAS Survey (Cat. &lt;VII/113&gt;), and most of the remaining 543 galaxy candidates are newly identified in this search. Although the radial velocities are known for only 387 galaxies, of which 60 were newly measured by us so far, we inferred the contamination by Galactic objects to be small from the good correlation between the sky distributions of the newly identified galaxy candidates and the previously catalogued galaxies. In the regions where the Galactic molecular clouds dominate, almost all the sources were not identified as galaxies. The detected galaxies are clustered in the three regions around l=240{deg}, 280{deg}, and 315{deg}, where the projected number densities are higher than the whole-sky average of IRAS galaxies of the same flux limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57#2</TD>
            <TD>2012-09-24T08:53:10Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/89/57&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/89/57</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/89/57 [table5]</TD>
            <TD>IRAS galaxies behind southern Milky Way (Yamada+, 1993)</TD>
            <TD>We systematically searched for IRAS galaxies with 60nm flux density larger than 0.6Jy by using the UK Schmidt Infrared and IIIa-J Atlases in the Milky Way region (|b|&lt;15{deg}) between l=210{deg} and 360{deg}. We first selected about 4000 IRAS point sources by using our far-infrared criteria, which are optimized for the search of IRAS galaxies behind the Milky Way region, and then inspected visually the optical counterparts of them on the Schmidt Atlas film copies. We found 966 IRAS sources associated with galaxy-like objects. The list of the objects is presented here with the IRAS source name, Galactic coordinates, IRAS flux densities, field number and emulsion of the Atlas, type and size of galaxy(-like) image, redshift, multiplicity, and cross-identification. Of these, 423 galaxies are already catalogued in the Catalog of Galaxies and Quasars Observed in the IRAS Survey (Cat. &lt;VII/113&gt;), and most of the remaining 543 galaxy candidates are newly identified in this search. Although the radial velocities are known for only 387 galaxies, of which 60 were newly measured by us so far, we inferred the contamination by Galactic objects to be small from the good correlation between the sky distributions of the newly identified galaxy candidates and the previously catalogued galaxies. In the regions where the Galactic molecular clouds dominate, almost all the sources were not identified as galaxies. The detected galaxies are clustered in the three regions around l=240{deg}, 280{deg}, and 315{deg}, where the projected number densities are higher than the whole-sky average of IRAS galaxies of the same flux limit.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57#table5</TD>
            <TD>2012-09-24T08:53:10Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Jun-2000</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/89/57</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/89/57&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/89/57</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/200/8 [1]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#1</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/200/8</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/200/8 [2]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#2</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/200/8&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/8 [sources]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#sources</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/8&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/8 [table2]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#table2</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/8&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/200/8 [1]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#1</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/200/8</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/200/8 [2]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#2</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/200/8&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/8 [sources]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#sources</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/8&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/8 [table2]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#table2</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/8&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/200/8 [1]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#1</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/200/8</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/200/8 [2]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#2</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/200/8&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/8 [sources]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#sources</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/8&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/200/8 [table2]</TD>
            <TD>AGES: the AGN and Galaxy Evolution Survey (Kochanek+, 2012)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8#table2</TD>
            <TD>2012-09-28T15:18:16Z</TD>
            <TD>#AGN#Photometry#Galaxies#QSOs#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/200/8</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/200/8&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/200/8</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/727/14 [1]</TD>
            <TD>Merging galaxy cluster A2255 in mid-IR (Shim+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14#1</TD>
            <TD>2012-10-01T23:43:50Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/727/14</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/727/14</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/727/14 [2]</TD>
            <TD>Merging galaxy cluster A2255 in mid-IR (Shim+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14#2</TD>
            <TD>2012-10-01T23:43:50Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/727/14&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/727/14</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/727/14 [table2]</TD>
            <TD>Merging galaxy cluster A2255 in mid-IR (Shim+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14#table2</TD>
            <TD>2012-10-01T23:43:50Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/727/14&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/727/14</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/727/14 [1]</TD>
            <TD>Merging galaxy cluster A2255 in mid-IR (Shim+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14#1</TD>
            <TD>2012-10-01T23:43:50Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/727/14</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/727/14</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/727/14 [2]</TD>
            <TD>Merging galaxy cluster A2255 in mid-IR (Shim+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14#2</TD>
            <TD>2012-10-01T23:43:50Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/727/14&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/727/14</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/727/14 [table2]</TD>
            <TD>Merging galaxy cluster A2255 in mid-IR (Shim+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14#table2</TD>
            <TD>2012-10-01T23:43:50Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/727/14&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/727/14</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/727/14 [1]</TD>
            <TD>Merging galaxy cluster A2255 in mid-IR (Shim+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14#1</TD>
            <TD>2012-10-01T23:43:50Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/727/14</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/727/14</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/727/14 [2]</TD>
            <TD>Merging galaxy cluster A2255 in mid-IR (Shim+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14#2</TD>
            <TD>2012-10-01T23:43:50Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/727/14&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/727/14</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/727/14 [table2]</TD>
            <TD>Merging galaxy cluster A2255 in mid-IR (Shim+, 2011)</TD>
            <TD>****Returned code = -1: can't connect</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14#table2</TD>
            <TD>2012-10-01T23:43:50Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>connect</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/727/14</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/727/14&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/727/14</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/133 [1]</TD>
            <TD>Kepler Input Catalog (Kepler Mission Team, 2009)</TD>
            <TD>The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets. The KIC, or Kepler Input Catalog, is the primary source of information about objects observed as part of the ground-based Kepler Spectral Classification Program (SCP) in preparation for the selection of Kepler PI and GO targets. The KIC lists objects down to 21mag, but it is not complete to this limit. Light from only about 1/3 of these objects falls on the Kepler CCD detector. A small number of the KIC objects are calibration objects distributed across the sky. For this reason the full KIC should never be used for Kepler target selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/133#1</TD>
            <TD>2012-11-22T21:43:11Z</TD>
            <TD>#Abundances#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/V/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/133</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/133</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/133 [2]</TD>
            <TD>Kepler Input Catalog (Kepler Mission Team, 2009)</TD>
            <TD>The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets. The KIC, or Kepler Input Catalog, is the primary source of information about objects observed as part of the ground-based Kepler Spectral Classification Program (SCP) in preparation for the selection of Kepler PI and GO targets. The KIC lists objects down to 21mag, but it is not complete to this limit. Light from only about 1/3 of these objects falls on the Kepler CCD detector. A small number of the KIC objects are calibration objects distributed across the sky. For this reason the full KIC should never be used for Kepler target selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/133#2</TD>
            <TD>2012-11-22T21:43:11Z</TD>
            <TD>#Abundances#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/V/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/133&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/133</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/133 [kic]</TD>
            <TD>Kepler Input Catalog (Kepler Mission Team, 2009)</TD>
            <TD>The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets. The KIC, or Kepler Input Catalog, is the primary source of information about objects observed as part of the ground-based Kepler Spectral Classification Program (SCP) in preparation for the selection of Kepler PI and GO targets. The KIC lists objects down to 21mag, but it is not complete to this limit. Light from only about 1/3 of these objects falls on the Kepler CCD detector. A small number of the KIC objects are calibration objects distributed across the sky. For this reason the full KIC should never be used for Kepler target selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/133#kic</TD>
            <TD>2012-11-22T21:43:11Z</TD>
            <TD>#Abundances#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/V/133</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/133&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/133</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/133 [1]</TD>
            <TD>Kepler Input Catalog (Kepler Mission Team, 2009)</TD>
            <TD>The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets. The KIC, or Kepler Input Catalog, is the primary source of information about objects observed as part of the ground-based Kepler Spectral Classification Program (SCP) in preparation for the selection of Kepler PI and GO targets. The KIC lists objects down to 21mag, but it is not complete to this limit. Light from only about 1/3 of these objects falls on the Kepler CCD detector. A small number of the KIC objects are calibration objects distributed across the sky. For this reason the full KIC should never be used for Kepler target selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/133#1</TD>
            <TD>2012-11-22T21:43:11Z</TD>
            <TD>#Abundances#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/V/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/133</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/133</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/133 [2]</TD>
            <TD>Kepler Input Catalog (Kepler Mission Team, 2009)</TD>
            <TD>The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets. The KIC, or Kepler Input Catalog, is the primary source of information about objects observed as part of the ground-based Kepler Spectral Classification Program (SCP) in preparation for the selection of Kepler PI and GO targets. The KIC lists objects down to 21mag, but it is not complete to this limit. Light from only about 1/3 of these objects falls on the Kepler CCD detector. A small number of the KIC objects are calibration objects distributed across the sky. For this reason the full KIC should never be used for Kepler target selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/133#2</TD>
            <TD>2012-11-22T21:43:11Z</TD>
            <TD>#Abundances#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/V/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/133&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/133</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/133 [kic]</TD>
            <TD>Kepler Input Catalog (Kepler Mission Team, 2009)</TD>
            <TD>The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets. The KIC, or Kepler Input Catalog, is the primary source of information about objects observed as part of the ground-based Kepler Spectral Classification Program (SCP) in preparation for the selection of Kepler PI and GO targets. The KIC lists objects down to 21mag, but it is not complete to this limit. Light from only about 1/3 of these objects falls on the Kepler CCD detector. A small number of the KIC objects are calibration objects distributed across the sky. For this reason the full KIC should never be used for Kepler target selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/133#kic</TD>
            <TD>2012-11-22T21:43:11Z</TD>
            <TD>#Abundances#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/V/133</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/133&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/133</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>V/133 [1]</TD>
            <TD>Kepler Input Catalog (Kepler Mission Team, 2009)</TD>
            <TD>The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets. The KIC, or Kepler Input Catalog, is the primary source of information about objects observed as part of the ground-based Kepler Spectral Classification Program (SCP) in preparation for the selection of Kepler PI and GO targets. The KIC lists objects down to 21mag, but it is not complete to this limit. Light from only about 1/3 of these objects falls on the Kepler CCD detector. A small number of the KIC objects are calibration objects distributed across the sky. For this reason the full KIC should never be used for Kepler target selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/133#1</TD>
            <TD>2012-11-22T21:43:11Z</TD>
            <TD>#Abundances#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/V/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=V/133</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/133</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>V/133 [2]</TD>
            <TD>Kepler Input Catalog (Kepler Mission Team, 2009)</TD>
            <TD>The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets. The KIC, or Kepler Input Catalog, is the primary source of information about objects observed as part of the ground-based Kepler Spectral Classification Program (SCP) in preparation for the selection of Kepler PI and GO targets. The KIC lists objects down to 21mag, but it is not complete to this limit. Light from only about 1/3 of these objects falls on the Kepler CCD detector. A small number of the KIC objects are calibration objects distributed across the sky. For this reason the full KIC should never be used for Kepler target selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/133#2</TD>
            <TD>2012-11-22T21:43:11Z</TD>
            <TD>#Abundances#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/V/133</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=V/133&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/133</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>V/133 [kic]</TD>
            <TD>Kepler Input Catalog (Kepler Mission Team, 2009)</TD>
            <TD>The Kepler Mission, NASA Discovery mission #10, is specifically designed to survey our region of the Milky Way galaxy to discover hundreds of Earth-size and smaller planets in or near the habitable zone and determine how many of the billions of stars in our galaxy have such planets. The KIC, or Kepler Input Catalog, is the primary source of information about objects observed as part of the ground-based Kepler Spectral Classification Program (SCP) in preparation for the selection of Kepler PI and GO targets. The KIC lists objects down to 21mag, but it is not complete to this limit. Light from only about 1/3 of these objects falls on the Kepler CCD detector. A small number of the KIC objects are calibration objects distributed across the sky. For this reason the full KIC should never be used for Kepler target selection.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/V/133#kic</TD>
            <TD>2012-11-22T21:43:11Z</TD>
            <TD>#Abundances#Stars#Proper_Motions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/V/133</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=V/133&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?V/133</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/971 [1]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#1</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/971</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/971 [2]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#2</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/971&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/971 [gamacore]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#gamacore</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/971&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/971 [extra]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#extra</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/971&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/971 [1]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#1</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/971</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/971 [2]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#2</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/971&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/971 [gamacore]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#gamacore</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/971&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/971 [extra]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#extra</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/971&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/413/971 [1]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#1</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/413/971</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/413/971 [2]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#2</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/413/971&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/971 [gamacore]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#gamacore</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/971&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/413/971 [extra]</TD>
            <TD>Galaxy And Mass Assembly (GAMA) DR1 (Driver+, 2011)</TD>
            <TD>All GAMA 2dF pointings (tiles) were observed during dark or grey time with exposure times mostly ranging from 3000 to 5000s (in three to five exposures) depending on seeing and sky brightness. Observations were generally conducted at an hour angle of less than 2h (the median zenith distance of the observations is 35{deg}) and with the Atmospheric Dispersion Corrector engaged. We used the 580V and 385R gratings with central wavelengths of 4800 and 7250{AA} in the blue and red arms, respectively, separated by a 5700{AA} dichroic. This set-up yielded a continuous wavelength coverage of 3720-8850{AA} at a resolution of ~3.5{AA} (in the blue channel) and ~5.5{AA} (in the red channel).</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971#extra</TD>
            <TD>2012-12-16T06:25:35Z</TD>
            <TD>#Galaxies#Photometry:wide-band#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>16-Sep-2012</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/413/971</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/413/971&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/413/971</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/314 [1]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#1</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/314</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/314 [2]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#2</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/314&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/314 [las8]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#las8</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/314&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/314 [dxs8]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#dxs8</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/314&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/314 [gcs8]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#gcs8</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/314&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/314 [1]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#1</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/314</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/314 [2]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#2</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/314&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/314 [las8]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#las8</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/314&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/314 [dxs8]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#dxs8</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/314&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/314 [gcs8]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#gcs8</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/314&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>II/314 [1]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#1</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=II/314</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>II/314 [2]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#2</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=II/314&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/314 [las8]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#las8</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/314&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/314 [dxs8]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#dxs8</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/314&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>II/314 [gcs8]</TD>
            <TD>UKIDSS-DR8 LAS, GCS and DXS Surveys (Lawrence+ 2012)</TD>
            <TD>The UKIRT Infrared Deep Sky Survey (UKIDSS) is a large-scale near-IR survey which aim is to cover 7500 square degrees of the Northern sky. The survey is carried out using the Wide Field Camera (WFCAM), with a field of view of 0.21 square degrees, mounted on the 3.8m United Kingdom Infra-red Telescope (UKIRT) in Hawaii. The project comprises five surveys (LAS, GCS, DXS, GPS and UDS). The Large Area Survey (LAS) covers an area of 4000 square degrees in high Galactic latitudes (extragalactic) in the four bands Y(1.0um) J(1.2um) H(1.6um) and K(2.2um) to a depth of K=18.4. The Galactic Clusters Survey (GCS) aims to survey ten large open star clusters and star formation associations, covering a total of 1067 square degrees in the five bands Z (0.9um), Y(1.0um) J(1.2um) H(1.6um) and K(2.2um), plus a second pass in K for proper motions, to a depth of Z=20.4, Y=20.3, J=19.5, H=18.6, K=18.6. The Deep Extragalactic Survey (DXS) aims to map 35 square degrees of sky to a 5-{sigma} point-source sensitivity of J=22.3 and K=20.8 in four carefully selected, multi-wavelength survey areas. The central regions of each field will also be mapped to H=21.8. The primary aim of the survey is to produce a photometric galaxy sample at a redshift of 1-2, within a volume comparable to that of the SDSS, selected in the same passband (rest frame optical). Details of the surveys can be found in the in the paper by Lawrence et al. (2007MNRAS.379.1599L), and at the UKIDSS Surveys site (http://www.ukidss.org/surveys/surveys.html). The data described here represent a subset of the UKIDSS data, limited to the public data and most representative columns. In the "Byte-by-byte Description" below the original names of the columns are given as bracketed names.</TD>
            <TD>CDS</TD>
            <TD>#Infrared#</TD>
            <TD>ivo://CDS.VizieR/II/314#gcs8</TD>
            <TD>2012-12-21T22:24:40Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Mar-2012</TD>
            <TD>ivo://CDS.VizieR/II/314</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
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            <TD>ParamHTTP</TD>
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            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=II/314&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?II/314</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1811 [1]</TD>
            <TD>Catalog of SDSS compact groups of galaxies (Lee+, 2004)</TD>
            <TD>Compact groups (CGs) of galaxies - relatively poor groups of galaxies in which the typical separations between members is of the order of a galaxy diameter - offer an exceptional laboratory for the study of dense galactic environments with short (&lt;1Gyr) dynamical timescales. We present an objectively defined catalog of CGs in 153deg^2^ of the Sloan Digital Sky Survey (SDSS) Early Data Release (&lt;J/AJ/123/567&gt;). To identify CGs, we applied a modified version of Hickson's criteria of 1982 aimed at finding the highest-density CGs and thus reducing the number of chance alignments. Our catalog contains 175 CGs down to a limiting galaxy magnitude of r*=21. The resulting catalog has a median depth of z_med_~0.13, substantially deeper than previous CG catalogs. Since the SDSS will eventually image up to one-quarter of the celestial sphere, we expect our final catalog, based on the completed SDSS, will contain on the order of 5000-10000CGs. This catalog will be useful for conducting studies of the general characteristics of CGs, their environments, and their component galaxies.</TD>
            <TD>CDS</TD>
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            <TD>WebBrowser</TD>
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            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1811 [2]</TD>
            <TD>Catalog of SDSS compact groups of galaxies (Lee+, 2004)</TD>
            <TD>Compact groups (CGs) of galaxies - relatively poor groups of galaxies in which the typical separations between members is of the order of a galaxy diameter - offer an exceptional laboratory for the study of dense galactic environments with short (&lt;1Gyr) dynamical timescales. We present an objectively defined catalog of CGs in 153deg^2^ of the Sloan Digital Sky Survey (SDSS) Early Data Release (&lt;J/AJ/123/567&gt;). To identify CGs, we applied a modified version of Hickson's criteria of 1982 aimed at finding the highest-density CGs and thus reducing the number of chance alignments. Our catalog contains 175 CGs down to a limiting galaxy magnitude of r*=21. The resulting catalog has a median depth of z_med_~0.13, substantially deeper than previous CG catalogs. Since the SDSS will eventually image up to one-quarter of the celestial sphere, we expect our final catalog, based on the completed SDSS, will contain on the order of 5000-10000CGs. This catalog will be useful for conducting studies of the general characteristics of CGs, their environments, and their component galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1811</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1811 [1]</TD>
            <TD>Catalog of SDSS compact groups of galaxies (Lee+, 2004)</TD>
            <TD>Compact groups (CGs) of galaxies - relatively poor groups of galaxies in which the typical separations between members is of the order of a galaxy diameter - offer an exceptional laboratory for the study of dense galactic environments with short (&lt;1Gyr) dynamical timescales. We present an objectively defined catalog of CGs in 153deg^2^ of the Sloan Digital Sky Survey (SDSS) Early Data Release (&lt;J/AJ/123/567&gt;). To identify CGs, we applied a modified version of Hickson's criteria of 1982 aimed at finding the highest-density CGs and thus reducing the number of chance alignments. Our catalog contains 175 CGs down to a limiting galaxy magnitude of r*=21. The resulting catalog has a median depth of z_med_~0.13, substantially deeper than previous CG catalogs. Since the SDSS will eventually image up to one-quarter of the celestial sphere, we expect our final catalog, based on the completed SDSS, will contain on the order of 5000-10000CGs. This catalog will be useful for conducting studies of the general characteristics of CGs, their environments, and their component galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1811#1</TD>
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            <TD>WebBrowser</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1811 [2]</TD>
            <TD>Catalog of SDSS compact groups of galaxies (Lee+, 2004)</TD>
            <TD>Compact groups (CGs) of galaxies - relatively poor groups of galaxies in which the typical separations between members is of the order of a galaxy diameter - offer an exceptional laboratory for the study of dense galactic environments with short (&lt;1Gyr) dynamical timescales. We present an objectively defined catalog of CGs in 153deg^2^ of the Sloan Digital Sky Survey (SDSS) Early Data Release (&lt;J/AJ/123/567&gt;). To identify CGs, we applied a modified version of Hickson's criteria of 1982 aimed at finding the highest-density CGs and thus reducing the number of chance alignments. Our catalog contains 175 CGs down to a limiting galaxy magnitude of r*=21. The resulting catalog has a median depth of z_med_~0.13, substantially deeper than previous CG catalogs. Since the SDSS will eventually image up to one-quarter of the celestial sphere, we expect our final catalog, based on the completed SDSS, will contain on the order of 5000-10000CGs. This catalog will be useful for conducting studies of the general characteristics of CGs, their environments, and their component galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ParamHTTP</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1811</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1811 [1]</TD>
            <TD>Catalog of SDSS compact groups of galaxies (Lee+, 2004)</TD>
            <TD>Compact groups (CGs) of galaxies - relatively poor groups of galaxies in which the typical separations between members is of the order of a galaxy diameter - offer an exceptional laboratory for the study of dense galactic environments with short (&lt;1Gyr) dynamical timescales. We present an objectively defined catalog of CGs in 153deg^2^ of the Sloan Digital Sky Survey (SDSS) Early Data Release (&lt;J/AJ/123/567&gt;). To identify CGs, we applied a modified version of Hickson's criteria of 1982 aimed at finding the highest-density CGs and thus reducing the number of chance alignments. Our catalog contains 175 CGs down to a limiting galaxy magnitude of r*=21. The resulting catalog has a median depth of z_med_~0.13, substantially deeper than previous CG catalogs. Since the SDSS will eventually image up to one-quarter of the celestial sphere, we expect our final catalog, based on the completed SDSS, will contain on the order of 5000-10000CGs. This catalog will be useful for conducting studies of the general characteristics of CGs, their environments, and their component galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1811#1</TD>
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1811</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1811 [2]</TD>
            <TD>Catalog of SDSS compact groups of galaxies (Lee+, 2004)</TD>
            <TD>Compact groups (CGs) of galaxies - relatively poor groups of galaxies in which the typical separations between members is of the order of a galaxy diameter - offer an exceptional laboratory for the study of dense galactic environments with short (&lt;1Gyr) dynamical timescales. We present an objectively defined catalog of CGs in 153deg^2^ of the Sloan Digital Sky Survey (SDSS) Early Data Release (&lt;J/AJ/123/567&gt;). To identify CGs, we applied a modified version of Hickson's criteria of 1982 aimed at finding the highest-density CGs and thus reducing the number of chance alignments. Our catalog contains 175 CGs down to a limiting galaxy magnitude of r*=21. The resulting catalog has a median depth of z_med_~0.13, substantially deeper than previous CG catalogs. Since the SDSS will eventually image up to one-quarter of the celestial sphere, we expect our final catalog, based on the completed SDSS, will contain on the order of 5000-10000CGs. This catalog will be useful for conducting studies of the general characteristics of CGs, their environments, and their component galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1811#2</TD>
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            <TD>ivo://CDS.VizieR/J/AJ/127/1811</TD>
            <TD />
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1811&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1811</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/82/420 [1]</TD>
            <TD>Spectral study of 19 radio sources (Afanasiev+, 2005)</TD>
            <TD>We present optical identifications, classifications, and radio spectra of 19 radio sources from a complete sample in flux-density with the declinations 10{deg}-12{deg}30' (J2000) obtained with the 6-m optical telescope (4000-9000{AA}) and RATAN-600 radio telescope (0.97-21.7GHz) of the Special Astrophysical Observatory. Twelve objects with redshifts from 0.573-2.694 have been classified as quasars, and two objects with featureless spectra as BL Lac objects. Four objects are emission-line radio galaxies with redshifts from 0.204 to 0.311, one object is an absorption-line radio galaxy with redshift 0.214. Radio flux densities have been obtained at six frequencies for all sources except for two extended objects. The radio spectra of five of the sources can be separated into extended and compact components. Three objects display substantial rapid and long-term variability of their flux densities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
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            <TD>ivo://CDS.VizieR/J/AZh/82/420</TD>
            <TD />
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            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/82/420</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/82/420 [2]</TD>
            <TD>Spectral study of 19 radio sources (Afanasiev+, 2005)</TD>
            <TD>We present optical identifications, classifications, and radio spectra of 19 radio sources from a complete sample in flux-density with the declinations 10{deg}-12{deg}30' (J2000) obtained with the 6-m optical telescope (4000-9000{AA}) and RATAN-600 radio telescope (0.97-21.7GHz) of the Special Astrophysical Observatory. Twelve objects with redshifts from 0.573-2.694 have been classified as quasars, and two objects with featureless spectra as BL Lac objects. Four objects are emission-line radio galaxies with redshifts from 0.204 to 0.311, one object is an absorption-line radio galaxy with redshift 0.214. Radio flux densities have been obtained at six frequencies for all sources except for two extended objects. The radio spectra of five of the sources can be separated into extended and compact components. Three objects display substantial rapid and long-term variability of their flux densities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
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            <TD>2011-09-14T19:43:52Z</TD>
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            <TD>28-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AZh/82/420</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/82/420&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/82/420</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/82/420 [1]</TD>
            <TD>Spectral study of 19 radio sources (Afanasiev+, 2005)</TD>
            <TD>We present optical identifications, classifications, and radio spectra of 19 radio sources from a complete sample in flux-density with the declinations 10{deg}-12{deg}30' (J2000) obtained with the 6-m optical telescope (4000-9000{AA}) and RATAN-600 radio telescope (0.97-21.7GHz) of the Special Astrophysical Observatory. Twelve objects with redshifts from 0.573-2.694 have been classified as quasars, and two objects with featureless spectra as BL Lac objects. Four objects are emission-line radio galaxies with redshifts from 0.204 to 0.311, one object is an absorption-line radio galaxy with redshift 0.214. Radio flux densities have been obtained at six frequencies for all sources except for two extended objects. The radio spectra of five of the sources can be separated into extended and compact components. Three objects display substantial rapid and long-term variability of their flux densities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
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            <TD>28-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AZh/82/420</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
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            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/82/420</TD>
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          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/82/420 [2]</TD>
            <TD>Spectral study of 19 radio sources (Afanasiev+, 2005)</TD>
            <TD>We present optical identifications, classifications, and radio spectra of 19 radio sources from a complete sample in flux-density with the declinations 10{deg}-12{deg}30' (J2000) obtained with the 6-m optical telescope (4000-9000{AA}) and RATAN-600 radio telescope (0.97-21.7GHz) of the Special Astrophysical Observatory. Twelve objects with redshifts from 0.573-2.694 have been classified as quasars, and two objects with featureless spectra as BL Lac objects. Four objects are emission-line radio galaxies with redshifts from 0.204 to 0.311, one object is an absorption-line radio galaxy with redshift 0.214. Radio flux densities have been obtained at six frequencies for all sources except for two extended objects. The radio spectra of five of the sources can be separated into extended and compact components. Three objects display substantial rapid and long-term variability of their flux densities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
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            <TD>ivo://CDS.VizieR/J/AZh/82/420</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/82/420&amp;</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AZh/82/420 [1]</TD>
            <TD>Spectral study of 19 radio sources (Afanasiev+, 2005)</TD>
            <TD>We present optical identifications, classifications, and radio spectra of 19 radio sources from a complete sample in flux-density with the declinations 10{deg}-12{deg}30' (J2000) obtained with the 6-m optical telescope (4000-9000{AA}) and RATAN-600 radio telescope (0.97-21.7GHz) of the Special Astrophysical Observatory. Twelve objects with redshifts from 0.573-2.694 have been classified as quasars, and two objects with featureless spectra as BL Lac objects. Four objects are emission-line radio galaxies with redshifts from 0.204 to 0.311, one object is an absorption-line radio galaxy with redshift 0.214. Radio flux densities have been obtained at six frequencies for all sources except for two extended objects. The radio spectra of five of the sources can be separated into extended and compact components. Three objects display substantial rapid and long-term variability of their flux densities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
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            <TD>28-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AZh/82/420</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AZh/82/420</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/82/420</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AZh/82/420 [2]</TD>
            <TD>Spectral study of 19 radio sources (Afanasiev+, 2005)</TD>
            <TD>We present optical identifications, classifications, and radio spectra of 19 radio sources from a complete sample in flux-density with the declinations 10{deg}-12{deg}30' (J2000) obtained with the 6-m optical telescope (4000-9000{AA}) and RATAN-600 radio telescope (0.97-21.7GHz) of the Special Astrophysical Observatory. Twelve objects with redshifts from 0.573-2.694 have been classified as quasars, and two objects with featureless spectra as BL Lac objects. Four objects are emission-line radio galaxies with redshifts from 0.204 to 0.311, one object is an absorption-line radio galaxy with redshift 0.214. Radio flux densities have been obtained at six frequencies for all sources except for two extended objects. The radio spectra of five of the sources can be separated into extended and compact components. Three objects display substantial rapid and long-term variability of their flux densities.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
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            <TD>28-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/AZh/82/420</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AZh/82/420&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AZh/82/420</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1883 [1]</TD>
            <TD>Merging galaxies in SDSS EDR (Allam+, 2004)</TD>
            <TD>We present a new catalog of merging galaxies obtained through an automated systematic search routine. The 1479 new pairs of merging galaxies were found in ~462 square degrees of the Sloan Digital Sky Survey Early Data Release (SDSS EDR, Cat. &lt;J/AJ/123/567&gt;) photometric data, and the pair catalog is complete for galaxies in the magnitude range 16.0&lt;=g*&lt;=20. The selection algorithm, implementing a variation on the original Karachentsev criteria, proved to be very efficient and fast. Merging galaxies were selected such that the intergalaxy separations were less than the sum of the component galaxies' radii. We discuss the characteristics of the sample in terms of completeness, pair separation, and the Holmberg effect. We also present an on-line atlas of images for the SDSS EDR pairs obtained using the corrected frames from the SDSS EDR database. The atlas images also include the relevant data for each pair member. This catalog will be useful for conducting studies of the general characteristics of merging galaxies, their environments, and their component galaxies. The redshifts for a subset of the interacting and merging galaxies and the distribution of angular sizes for these systems indicate the SDSS provides a much deeper sample than almost any other wide-area catalog to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883#1</TD>
            <TD>2011-09-14T19:44:39Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1883</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1883</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1883 [2]</TD>
            <TD>Merging galaxies in SDSS EDR (Allam+, 2004)</TD>
            <TD>We present a new catalog of merging galaxies obtained through an automated systematic search routine. The 1479 new pairs of merging galaxies were found in ~462 square degrees of the Sloan Digital Sky Survey Early Data Release (SDSS EDR, Cat. &lt;J/AJ/123/567&gt;) photometric data, and the pair catalog is complete for galaxies in the magnitude range 16.0&lt;=g*&lt;=20. The selection algorithm, implementing a variation on the original Karachentsev criteria, proved to be very efficient and fast. Merging galaxies were selected such that the intergalaxy separations were less than the sum of the component galaxies' radii. We discuss the characteristics of the sample in terms of completeness, pair separation, and the Holmberg effect. We also present an on-line atlas of images for the SDSS EDR pairs obtained using the corrected frames from the SDSS EDR database. The atlas images also include the relevant data for each pair member. This catalog will be useful for conducting studies of the general characteristics of merging galaxies, their environments, and their component galaxies. The redshifts for a subset of the interacting and merging galaxies and the distribution of angular sizes for these systems indicate the SDSS provides a much deeper sample than almost any other wide-area catalog to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883#2</TD>
            <TD>2011-09-14T19:44:39Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1883&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1883</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1883 [1]</TD>
            <TD>Merging galaxies in SDSS EDR (Allam+, 2004)</TD>
            <TD>We present a new catalog of merging galaxies obtained through an automated systematic search routine. The 1479 new pairs of merging galaxies were found in ~462 square degrees of the Sloan Digital Sky Survey Early Data Release (SDSS EDR, Cat. &lt;J/AJ/123/567&gt;) photometric data, and the pair catalog is complete for galaxies in the magnitude range 16.0&lt;=g*&lt;=20. The selection algorithm, implementing a variation on the original Karachentsev criteria, proved to be very efficient and fast. Merging galaxies were selected such that the intergalaxy separations were less than the sum of the component galaxies' radii. We discuss the characteristics of the sample in terms of completeness, pair separation, and the Holmberg effect. We also present an on-line atlas of images for the SDSS EDR pairs obtained using the corrected frames from the SDSS EDR database. The atlas images also include the relevant data for each pair member. This catalog will be useful for conducting studies of the general characteristics of merging galaxies, their environments, and their component galaxies. The redshifts for a subset of the interacting and merging galaxies and the distribution of angular sizes for these systems indicate the SDSS provides a much deeper sample than almost any other wide-area catalog to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883#1</TD>
            <TD>2011-09-14T19:44:39Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1883</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1883</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1883 [2]</TD>
            <TD>Merging galaxies in SDSS EDR (Allam+, 2004)</TD>
            <TD>We present a new catalog of merging galaxies obtained through an automated systematic search routine. The 1479 new pairs of merging galaxies were found in ~462 square degrees of the Sloan Digital Sky Survey Early Data Release (SDSS EDR, Cat. &lt;J/AJ/123/567&gt;) photometric data, and the pair catalog is complete for galaxies in the magnitude range 16.0&lt;=g*&lt;=20. The selection algorithm, implementing a variation on the original Karachentsev criteria, proved to be very efficient and fast. Merging galaxies were selected such that the intergalaxy separations were less than the sum of the component galaxies' radii. We discuss the characteristics of the sample in terms of completeness, pair separation, and the Holmberg effect. We also present an on-line atlas of images for the SDSS EDR pairs obtained using the corrected frames from the SDSS EDR database. The atlas images also include the relevant data for each pair member. This catalog will be useful for conducting studies of the general characteristics of merging galaxies, their environments, and their component galaxies. The redshifts for a subset of the interacting and merging galaxies and the distribution of angular sizes for these systems indicate the SDSS provides a much deeper sample than almost any other wide-area catalog to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883#2</TD>
            <TD>2011-09-14T19:44:39Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1883&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1883</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/1883 [1]</TD>
            <TD>Merging galaxies in SDSS EDR (Allam+, 2004)</TD>
            <TD>We present a new catalog of merging galaxies obtained through an automated systematic search routine. The 1479 new pairs of merging galaxies were found in ~462 square degrees of the Sloan Digital Sky Survey Early Data Release (SDSS EDR, Cat. &lt;J/AJ/123/567&gt;) photometric data, and the pair catalog is complete for galaxies in the magnitude range 16.0&lt;=g*&lt;=20. The selection algorithm, implementing a variation on the original Karachentsev criteria, proved to be very efficient and fast. Merging galaxies were selected such that the intergalaxy separations were less than the sum of the component galaxies' radii. We discuss the characteristics of the sample in terms of completeness, pair separation, and the Holmberg effect. We also present an on-line atlas of images for the SDSS EDR pairs obtained using the corrected frames from the SDSS EDR database. The atlas images also include the relevant data for each pair member. This catalog will be useful for conducting studies of the general characteristics of merging galaxies, their environments, and their component galaxies. The redshifts for a subset of the interacting and merging galaxies and the distribution of angular sizes for these systems indicate the SDSS provides a much deeper sample than almost any other wide-area catalog to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883#1</TD>
            <TD>2011-09-14T19:44:39Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/1883</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1883</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/1883 [2]</TD>
            <TD>Merging galaxies in SDSS EDR (Allam+, 2004)</TD>
            <TD>We present a new catalog of merging galaxies obtained through an automated systematic search routine. The 1479 new pairs of merging galaxies were found in ~462 square degrees of the Sloan Digital Sky Survey Early Data Release (SDSS EDR, Cat. &lt;J/AJ/123/567&gt;) photometric data, and the pair catalog is complete for galaxies in the magnitude range 16.0&lt;=g*&lt;=20. The selection algorithm, implementing a variation on the original Karachentsev criteria, proved to be very efficient and fast. Merging galaxies were selected such that the intergalaxy separations were less than the sum of the component galaxies' radii. We discuss the characteristics of the sample in terms of completeness, pair separation, and the Holmberg effect. We also present an on-line atlas of images for the SDSS EDR pairs obtained using the corrected frames from the SDSS EDR database. The atlas images also include the relevant data for each pair member. This catalog will be useful for conducting studies of the general characteristics of merging galaxies, their environments, and their component galaxies. The redshifts for a subset of the interacting and merging galaxies and the distribution of angular sizes for these systems indicate the SDSS provides a much deeper sample than almost any other wide-area catalog to date.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883#2</TD>
            <TD>2011-09-14T19:44:39Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/1883</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/1883&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/1883</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/591/850 [1]</TD>
            <TD>Radial velocities of M49 globular clusters (Cote+, 2003)</TD>
            <TD>Using the Low Resolution Imaging Spectrometer on the Keck I and II telescopes, we have measured radial velocities for 196 globular clusters (GCs) around M49 (NGC 4472), the brightest member of the Virgo Cluster. Combined with published data, they bring the total number of GCs with measured radial velocities in this galaxy to 263. In terms of sample size, spatial coverage, velocity precision, and the availability of metallicity estimates from Washington photometry, this radial velocity database resembles that presented recently for M87 (NGC 4486), Virgo's cD galaxy and its second-ranked member. We extract the projected kinematics of the full sample of GCs and of separate subsamples of 158 metal-poor and 105 metal-rich GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850#1</TD>
            <TD>2011-09-14T19:45:57Z</TD>
            <TD>#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/591/850</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/850</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/591/850 [2]</TD>
            <TD>Radial velocities of M49 globular clusters (Cote+, 2003)</TD>
            <TD>Using the Low Resolution Imaging Spectrometer on the Keck I and II telescopes, we have measured radial velocities for 196 globular clusters (GCs) around M49 (NGC 4472), the brightest member of the Virgo Cluster. Combined with published data, they bring the total number of GCs with measured radial velocities in this galaxy to 263. In terms of sample size, spatial coverage, velocity precision, and the availability of metallicity estimates from Washington photometry, this radial velocity database resembles that presented recently for M87 (NGC 4486), Virgo's cD galaxy and its second-ranked member. We extract the projected kinematics of the full sample of GCs and of separate subsamples of 158 metal-poor and 105 metal-rich GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850#2</TD>
            <TD>2011-09-14T19:45:57Z</TD>
            <TD>#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/591/850&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/850</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/591/850 [1]</TD>
            <TD>Radial velocities of M49 globular clusters (Cote+, 2003)</TD>
            <TD>Using the Low Resolution Imaging Spectrometer on the Keck I and II telescopes, we have measured radial velocities for 196 globular clusters (GCs) around M49 (NGC 4472), the brightest member of the Virgo Cluster. Combined with published data, they bring the total number of GCs with measured radial velocities in this galaxy to 263. In terms of sample size, spatial coverage, velocity precision, and the availability of metallicity estimates from Washington photometry, this radial velocity database resembles that presented recently for M87 (NGC 4486), Virgo's cD galaxy and its second-ranked member. We extract the projected kinematics of the full sample of GCs and of separate subsamples of 158 metal-poor and 105 metal-rich GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850#1</TD>
            <TD>2011-09-14T19:45:57Z</TD>
            <TD>#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/591/850</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/850</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/591/850 [2]</TD>
            <TD>Radial velocities of M49 globular clusters (Cote+, 2003)</TD>
            <TD>Using the Low Resolution Imaging Spectrometer on the Keck I and II telescopes, we have measured radial velocities for 196 globular clusters (GCs) around M49 (NGC 4472), the brightest member of the Virgo Cluster. Combined with published data, they bring the total number of GCs with measured radial velocities in this galaxy to 263. In terms of sample size, spatial coverage, velocity precision, and the availability of metallicity estimates from Washington photometry, this radial velocity database resembles that presented recently for M87 (NGC 4486), Virgo's cD galaxy and its second-ranked member. We extract the projected kinematics of the full sample of GCs and of separate subsamples of 158 metal-poor and 105 metal-rich GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850#2</TD>
            <TD>2011-09-14T19:45:57Z</TD>
            <TD>#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/591/850&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/850</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/591/850 [1]</TD>
            <TD>Radial velocities of M49 globular clusters (Cote+, 2003)</TD>
            <TD>Using the Low Resolution Imaging Spectrometer on the Keck I and II telescopes, we have measured radial velocities for 196 globular clusters (GCs) around M49 (NGC 4472), the brightest member of the Virgo Cluster. Combined with published data, they bring the total number of GCs with measured radial velocities in this galaxy to 263. In terms of sample size, spatial coverage, velocity precision, and the availability of metallicity estimates from Washington photometry, this radial velocity database resembles that presented recently for M87 (NGC 4486), Virgo's cD galaxy and its second-ranked member. We extract the projected kinematics of the full sample of GCs and of separate subsamples of 158 metal-poor and 105 metal-rich GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850#1</TD>
            <TD>2011-09-14T19:45:57Z</TD>
            <TD>#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/591/850</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/850</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/591/850 [2]</TD>
            <TD>Radial velocities of M49 globular clusters (Cote+, 2003)</TD>
            <TD>Using the Low Resolution Imaging Spectrometer on the Keck I and II telescopes, we have measured radial velocities for 196 globular clusters (GCs) around M49 (NGC 4472), the brightest member of the Virgo Cluster. Combined with published data, they bring the total number of GCs with measured radial velocities in this galaxy to 263. In terms of sample size, spatial coverage, velocity precision, and the availability of metallicity estimates from Washington photometry, this radial velocity database resembles that presented recently for M87 (NGC 4486), Virgo's cD galaxy and its second-ranked member. We extract the projected kinematics of the full sample of GCs and of separate subsamples of 158 metal-poor and 105 metal-rich GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850#2</TD>
            <TD>2011-09-14T19:45:57Z</TD>
            <TD>#Globular_Clusters#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/591/850</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/591/850&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/591/850</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/588/824 [1]</TD>
            <TD>Velocities of blue stars near (l,b)=(198,-27) (Yanny+, 2003)</TD>
            <TD>We present evidence for a ring of stars in the plane of the Milky Way, extending at least from l=180{deg} to 227{deg} with turnoff magnitude g~19.5; the ring could encircle the Galaxy. We infer that the low Galactic latitude structure is at a fairly constant distance of R=18+/-2kpc from the Galactic center above the Galactic plane and has R=20+/-2kpc in the region sampled below the Galactic plane. The evidence includes 500 Sloan Digital Sky Survey spectroscopic radial velocities of stars within 30{deg} of the plane. The velocity dispersion of the stars associated with this structure is found to be 27km/s at (l, b)=(198, -27), 22km/s at (l, b)=(225, 28), 30km/s at (l, b)=(188, 24), and 30km/s at (l, b)=(182, 27). The structure rotates in the same prograde direction as the Galactic disk stars but with a circular velocity of 110+/-25km/s. The narrow measured velocity dispersion is inconsistent with power-law spheroid or thick-disk populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824#1</TD>
            <TD>2011-09-14T19:45:59Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/588/824</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/824</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/588/824 [2]</TD>
            <TD>Velocities of blue stars near (l,b)=(198,-27) (Yanny+, 2003)</TD>
            <TD>We present evidence for a ring of stars in the plane of the Milky Way, extending at least from l=180{deg} to 227{deg} with turnoff magnitude g~19.5; the ring could encircle the Galaxy. We infer that the low Galactic latitude structure is at a fairly constant distance of R=18+/-2kpc from the Galactic center above the Galactic plane and has R=20+/-2kpc in the region sampled below the Galactic plane. The evidence includes 500 Sloan Digital Sky Survey spectroscopic radial velocities of stars within 30{deg} of the plane. The velocity dispersion of the stars associated with this structure is found to be 27km/s at (l, b)=(198, -27), 22km/s at (l, b)=(225, 28), 30km/s at (l, b)=(188, 24), and 30km/s at (l, b)=(182, 27). The structure rotates in the same prograde direction as the Galactic disk stars but with a circular velocity of 110+/-25km/s. The narrow measured velocity dispersion is inconsistent with power-law spheroid or thick-disk populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824#2</TD>
            <TD>2011-09-14T19:45:59Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/588/824&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/824</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/588/824 [1]</TD>
            <TD>Velocities of blue stars near (l,b)=(198,-27) (Yanny+, 2003)</TD>
            <TD>We present evidence for a ring of stars in the plane of the Milky Way, extending at least from l=180{deg} to 227{deg} with turnoff magnitude g~19.5; the ring could encircle the Galaxy. We infer that the low Galactic latitude structure is at a fairly constant distance of R=18+/-2kpc from the Galactic center above the Galactic plane and has R=20+/-2kpc in the region sampled below the Galactic plane. The evidence includes 500 Sloan Digital Sky Survey spectroscopic radial velocities of stars within 30{deg} of the plane. The velocity dispersion of the stars associated with this structure is found to be 27km/s at (l, b)=(198, -27), 22km/s at (l, b)=(225, 28), 30km/s at (l, b)=(188, 24), and 30km/s at (l, b)=(182, 27). The structure rotates in the same prograde direction as the Galactic disk stars but with a circular velocity of 110+/-25km/s. The narrow measured velocity dispersion is inconsistent with power-law spheroid or thick-disk populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824#1</TD>
            <TD>2011-09-14T19:45:59Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#</TD>
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            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/588/824</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/824</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/588/824 [2]</TD>
            <TD>Velocities of blue stars near (l,b)=(198,-27) (Yanny+, 2003)</TD>
            <TD>We present evidence for a ring of stars in the plane of the Milky Way, extending at least from l=180{deg} to 227{deg} with turnoff magnitude g~19.5; the ring could encircle the Galaxy. We infer that the low Galactic latitude structure is at a fairly constant distance of R=18+/-2kpc from the Galactic center above the Galactic plane and has R=20+/-2kpc in the region sampled below the Galactic plane. The evidence includes 500 Sloan Digital Sky Survey spectroscopic radial velocities of stars within 30{deg} of the plane. The velocity dispersion of the stars associated with this structure is found to be 27km/s at (l, b)=(198, -27), 22km/s at (l, b)=(225, 28), 30km/s at (l, b)=(188, 24), and 30km/s at (l, b)=(182, 27). The structure rotates in the same prograde direction as the Galactic disk stars but with a circular velocity of 110+/-25km/s. The narrow measured velocity dispersion is inconsistent with power-law spheroid or thick-disk populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824#2</TD>
            <TD>2011-09-14T19:45:59Z</TD>
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            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/588/824&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/824</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/588/824 [1]</TD>
            <TD>Velocities of blue stars near (l,b)=(198,-27) (Yanny+, 2003)</TD>
            <TD>We present evidence for a ring of stars in the plane of the Milky Way, extending at least from l=180{deg} to 227{deg} with turnoff magnitude g~19.5; the ring could encircle the Galaxy. We infer that the low Galactic latitude structure is at a fairly constant distance of R=18+/-2kpc from the Galactic center above the Galactic plane and has R=20+/-2kpc in the region sampled below the Galactic plane. The evidence includes 500 Sloan Digital Sky Survey spectroscopic radial velocities of stars within 30{deg} of the plane. The velocity dispersion of the stars associated with this structure is found to be 27km/s at (l, b)=(198, -27), 22km/s at (l, b)=(225, 28), 30km/s at (l, b)=(188, 24), and 30km/s at (l, b)=(182, 27). The structure rotates in the same prograde direction as the Galactic disk stars but with a circular velocity of 110+/-25km/s. The narrow measured velocity dispersion is inconsistent with power-law spheroid or thick-disk populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824#1</TD>
            <TD>2011-09-14T19:45:59Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/588/824</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/824</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/588/824 [2]</TD>
            <TD>Velocities of blue stars near (l,b)=(198,-27) (Yanny+, 2003)</TD>
            <TD>We present evidence for a ring of stars in the plane of the Milky Way, extending at least from l=180{deg} to 227{deg} with turnoff magnitude g~19.5; the ring could encircle the Galaxy. We infer that the low Galactic latitude structure is at a fairly constant distance of R=18+/-2kpc from the Galactic center above the Galactic plane and has R=20+/-2kpc in the region sampled below the Galactic plane. The evidence includes 500 Sloan Digital Sky Survey spectroscopic radial velocities of stars within 30{deg} of the plane. The velocity dispersion of the stars associated with this structure is found to be 27km/s at (l, b)=(198, -27), 22km/s at (l, b)=(225, 28), 30km/s at (l, b)=(188, 24), and 30km/s at (l, b)=(182, 27). The structure rotates in the same prograde direction as the Galactic disk stars but with a circular velocity of 110+/-25km/s. The narrow measured velocity dispersion is inconsistent with power-law spheroid or thick-disk populations.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824#2</TD>
            <TD>2011-09-14T19:45:59Z</TD>
            <TD>#Stars#Photometry:wide-band#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2003</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/588/824</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/588/824&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/588/824</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/622/187 [1]</TD>
            <TD>Velocity of eight RASSCALS galaxy groups (Mahdavi+, 2005)</TD>
            <TD>We study the distribution of gas pressure and entropy in eight groups of galaxies belonging to the ROSAT All-Sky Survey/Center for Astrophysics Loose Systems (RASSCALS, Cat. &lt;J/ApJ/534/114&gt;). We use archival and proprietary XMM-Newton observations, supplementing the X-ray data with redshifts derived from the literature; we also list 125 new redshifts measured with the Gemini North telescope.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187#1</TD>
            <TD>2011-09-14T19:46:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/622/187</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/622/187</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/622/187 [2]</TD>
            <TD>Velocity of eight RASSCALS galaxy groups (Mahdavi+, 2005)</TD>
            <TD>We study the distribution of gas pressure and entropy in eight groups of galaxies belonging to the ROSAT All-Sky Survey/Center for Astrophysics Loose Systems (RASSCALS, Cat. &lt;J/ApJ/534/114&gt;). We use archival and proprietary XMM-Newton observations, supplementing the X-ray data with redshifts derived from the literature; we also list 125 new redshifts measured with the Gemini North telescope.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187#2</TD>
            <TD>2011-09-14T19:46:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/622/187&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/622/187</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/622/187 [1]</TD>
            <TD>Velocity of eight RASSCALS galaxy groups (Mahdavi+, 2005)</TD>
            <TD>We study the distribution of gas pressure and entropy in eight groups of galaxies belonging to the ROSAT All-Sky Survey/Center for Astrophysics Loose Systems (RASSCALS, Cat. &lt;J/ApJ/534/114&gt;). We use archival and proprietary XMM-Newton observations, supplementing the X-ray data with redshifts derived from the literature; we also list 125 new redshifts measured with the Gemini North telescope.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187#1</TD>
            <TD>2011-09-14T19:46:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>01-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/622/187</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/622/187</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/622/187 [2]</TD>
            <TD>Velocity of eight RASSCALS galaxy groups (Mahdavi+, 2005)</TD>
            <TD>We study the distribution of gas pressure and entropy in eight groups of galaxies belonging to the ROSAT All-Sky Survey/Center for Astrophysics Loose Systems (RASSCALS, Cat. &lt;J/ApJ/534/114&gt;). We use archival and proprietary XMM-Newton observations, supplementing the X-ray data with redshifts derived from the literature; we also list 125 new redshifts measured with the Gemini North telescope.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187#2</TD>
            <TD>2011-09-14T19:46:32Z</TD>
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            <TD />
            <TD>01-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/622/187&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/622/187</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/622/187 [1]</TD>
            <TD>Velocity of eight RASSCALS galaxy groups (Mahdavi+, 2005)</TD>
            <TD>We study the distribution of gas pressure and entropy in eight groups of galaxies belonging to the ROSAT All-Sky Survey/Center for Astrophysics Loose Systems (RASSCALS, Cat. &lt;J/ApJ/534/114&gt;). We use archival and proprietary XMM-Newton observations, supplementing the X-ray data with redshifts derived from the literature; we also list 125 new redshifts measured with the Gemini North telescope.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187#1</TD>
            <TD>2011-09-14T19:46:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/622/187</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/622/187</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/622/187 [2]</TD>
            <TD>Velocity of eight RASSCALS galaxy groups (Mahdavi+, 2005)</TD>
            <TD>We study the distribution of gas pressure and entropy in eight groups of galaxies belonging to the ROSAT All-Sky Survey/Center for Astrophysics Loose Systems (RASSCALS, Cat. &lt;J/ApJ/534/114&gt;). We use archival and proprietary XMM-Newton observations, supplementing the X-ray data with redshifts derived from the literature; we also list 125 new redshifts measured with the Gemini North telescope.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187#2</TD>
            <TD>2011-09-14T19:46:32Z</TD>
            <TD>#Clusters_of_galaxies#Redshifts#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2005</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/622/187</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/622/187&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/622/187</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/2031 [1]</TD>
            <TD>Catalog of neighboring galaxies (Karachentsev+, 2004)</TD>
            <TD>We present an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D&lt;~10Mpc or a radial velocity V_LG_&lt;550km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. We expect the catalog completeness to be roughly 70%-80% within 8Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031#1</TD>
            <TD>2011-09-14T19:47:02Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/2031</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2031</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/2031 [2]</TD>
            <TD>Catalog of neighboring galaxies (Karachentsev+, 2004)</TD>
            <TD>We present an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D&lt;~10Mpc or a radial velocity V_LG_&lt;550km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. We expect the catalog completeness to be roughly 70%-80% within 8Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031#2</TD>
            <TD>2011-09-14T19:47:02Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/2031&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2031</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/2031 [1]</TD>
            <TD>Catalog of neighboring galaxies (Karachentsev+, 2004)</TD>
            <TD>We present an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D&lt;~10Mpc or a radial velocity V_LG_&lt;550km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. We expect the catalog completeness to be roughly 70%-80% within 8Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031#1</TD>
            <TD>2011-09-14T19:47:02Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/2031</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2031</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/2031 [2]</TD>
            <TD>Catalog of neighboring galaxies (Karachentsev+, 2004)</TD>
            <TD>We present an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D&lt;~10Mpc or a radial velocity V_LG_&lt;550km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. We expect the catalog completeness to be roughly 70%-80% within 8Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031#2</TD>
            <TD>2011-09-14T19:47:02Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/2031&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2031</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/127/2031 [1]</TD>
            <TD>Catalog of neighboring galaxies (Karachentsev+, 2004)</TD>
            <TD>We present an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D&lt;~10Mpc or a radial velocity V_LG_&lt;550km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. We expect the catalog completeness to be roughly 70%-80% within 8Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031#1</TD>
            <TD>2011-09-14T19:47:02Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/127/2031</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2031</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/127/2031 [2]</TD>
            <TD>Catalog of neighboring galaxies (Karachentsev+, 2004)</TD>
            <TD>We present an all-sky catalog of 451 nearby galaxies, each having an individual distance estimate D&lt;~10Mpc or a radial velocity V_LG_&lt;550km/s. The catalog contains data on basic optical and H I properties of the galaxies, in particular, their diameters, absolute magnitudes, morphological types, circumnuclear region types, optical and H I surface brightnesses, rotational velocities, and indicative mass-to-luminosity and H I mass-to-luminosity ratios, as well as a so-called tidal index, which quantifies the galaxy environment. We expect the catalog completeness to be roughly 70%-80% within 8Mpc.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031#2</TD>
            <TD>2011-09-14T19:47:02Z</TD>
            <TD>#Galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>06-Jul-2004</TD>
            <TD>ivo://CDS.VizieR/J/AJ/127/2031</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/127/2031&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/127/2031</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/456/985 [1]</TD>
            <TD>Radial velocities of 76 M31 candidate clusters (Galleti+, 2006)</TD>
            <TD>We present the first results of a large spectroscopic survey of globular clusters and candidate globular clusters in the nearby M31 galaxy. The survey is aimed at the classification of known candidate M31 clusters and at the study of their kinematic properties. We obtained low-resolution spectroscopy for 133 targets, including 76 yet-to-be-confirmed candidate clusters (i.e. with no previous spectroscopic information), 55 already-confirmed genuine M31 clusters, and 2 uncertain candidates. Our observations allowed a reliable estimate of the target radial velocity, within a typical accuracy of ~+/-20Km/s. The observed candidates have been robustly classified according to their radial velocity and shape parameters that allowed us to confidently discriminate between point sources and extended objects even from low-spatial-resolution imagery. In our set of 76 candidate clusters we found: 42 newly-confirmed bona-fide M31 clusters, 12 background galaxies, 17 foreground Galactic stars, 2 HII regions belonging to M31 and 3 unclassified (possibly M31 clusters or foreground stars) objects. The classification of a few other candidates not included in our survey has been also reassessed on various observational bases. All the sources of radial velocity estimates for M31 known globular clusters available in the literature have been compared and checked, and a homogeneous general list has been obtained for 349 confirmed clusters with radial velocity. Our results suggest that a significant number of genuine clusters (~&gt;100) is still hidden among the plethora of known candidates proposed by various authors. Hence our knowledge of the globular cluster system of the M31 galaxy is still far from complete even in terms of simple membership.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985#1</TD>
            <TD>2011-09-14T20:01:30Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/456/985</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/985</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/456/985 [2]</TD>
            <TD>Radial velocities of 76 M31 candidate clusters (Galleti+, 2006)</TD>
            <TD>We present the first results of a large spectroscopic survey of globular clusters and candidate globular clusters in the nearby M31 galaxy. The survey is aimed at the classification of known candidate M31 clusters and at the study of their kinematic properties. We obtained low-resolution spectroscopy for 133 targets, including 76 yet-to-be-confirmed candidate clusters (i.e. with no previous spectroscopic information), 55 already-confirmed genuine M31 clusters, and 2 uncertain candidates. Our observations allowed a reliable estimate of the target radial velocity, within a typical accuracy of ~+/-20Km/s. The observed candidates have been robustly classified according to their radial velocity and shape parameters that allowed us to confidently discriminate between point sources and extended objects even from low-spatial-resolution imagery. In our set of 76 candidate clusters we found: 42 newly-confirmed bona-fide M31 clusters, 12 background galaxies, 17 foreground Galactic stars, 2 HII regions belonging to M31 and 3 unclassified (possibly M31 clusters or foreground stars) objects. The classification of a few other candidates not included in our survey has been also reassessed on various observational bases. All the sources of radial velocity estimates for M31 known globular clusters available in the literature have been compared and checked, and a homogeneous general list has been obtained for 349 confirmed clusters with radial velocity. Our results suggest that a significant number of genuine clusters (~&gt;100) is still hidden among the plethora of known candidates proposed by various authors. Hence our knowledge of the globular cluster system of the M31 galaxy is still far from complete even in terms of simple membership.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985#2</TD>
            <TD>2011-09-14T20:01:30Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/456/985&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/985</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/456/985 [table5]</TD>
            <TD>Radial velocities of 76 M31 candidate clusters (Galleti+, 2006)</TD>
            <TD>We present the first results of a large spectroscopic survey of globular clusters and candidate globular clusters in the nearby M31 galaxy. The survey is aimed at the classification of known candidate M31 clusters and at the study of their kinematic properties. We obtained low-resolution spectroscopy for 133 targets, including 76 yet-to-be-confirmed candidate clusters (i.e. with no previous spectroscopic information), 55 already-confirmed genuine M31 clusters, and 2 uncertain candidates. Our observations allowed a reliable estimate of the target radial velocity, within a typical accuracy of ~+/-20Km/s. The observed candidates have been robustly classified according to their radial velocity and shape parameters that allowed us to confidently discriminate between point sources and extended objects even from low-spatial-resolution imagery. In our set of 76 candidate clusters we found: 42 newly-confirmed bona-fide M31 clusters, 12 background galaxies, 17 foreground Galactic stars, 2 HII regions belonging to M31 and 3 unclassified (possibly M31 clusters or foreground stars) objects. The classification of a few other candidates not included in our survey has been also reassessed on various observational bases. All the sources of radial velocity estimates for M31 known globular clusters available in the literature have been compared and checked, and a homogeneous general list has been obtained for 349 confirmed clusters with radial velocity. Our results suggest that a significant number of genuine clusters (~&gt;100) is still hidden among the plethora of known candidates proposed by various authors. Hence our knowledge of the globular cluster system of the M31 galaxy is still far from complete even in terms of simple membership.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985#table5</TD>
            <TD>2011-09-14T20:01:30Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/456/985&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/985</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/456/985 [1]</TD>
            <TD>Radial velocities of 76 M31 candidate clusters (Galleti+, 2006)</TD>
            <TD>We present the first results of a large spectroscopic survey of globular clusters and candidate globular clusters in the nearby M31 galaxy. The survey is aimed at the classification of known candidate M31 clusters and at the study of their kinematic properties. We obtained low-resolution spectroscopy for 133 targets, including 76 yet-to-be-confirmed candidate clusters (i.e. with no previous spectroscopic information), 55 already-confirmed genuine M31 clusters, and 2 uncertain candidates. Our observations allowed a reliable estimate of the target radial velocity, within a typical accuracy of ~+/-20Km/s. The observed candidates have been robustly classified according to their radial velocity and shape parameters that allowed us to confidently discriminate between point sources and extended objects even from low-spatial-resolution imagery. In our set of 76 candidate clusters we found: 42 newly-confirmed bona-fide M31 clusters, 12 background galaxies, 17 foreground Galactic stars, 2 HII regions belonging to M31 and 3 unclassified (possibly M31 clusters or foreground stars) objects. The classification of a few other candidates not included in our survey has been also reassessed on various observational bases. All the sources of radial velocity estimates for M31 known globular clusters available in the literature have been compared and checked, and a homogeneous general list has been obtained for 349 confirmed clusters with radial velocity. Our results suggest that a significant number of genuine clusters (~&gt;100) is still hidden among the plethora of known candidates proposed by various authors. Hence our knowledge of the globular cluster system of the M31 galaxy is still far from complete even in terms of simple membership.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985#1</TD>
            <TD>2011-09-14T20:01:30Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/456/985</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/985</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/456/985 [2]</TD>
            <TD>Radial velocities of 76 M31 candidate clusters (Galleti+, 2006)</TD>
            <TD>We present the first results of a large spectroscopic survey of globular clusters and candidate globular clusters in the nearby M31 galaxy. The survey is aimed at the classification of known candidate M31 clusters and at the study of their kinematic properties. We obtained low-resolution spectroscopy for 133 targets, including 76 yet-to-be-confirmed candidate clusters (i.e. with no previous spectroscopic information), 55 already-confirmed genuine M31 clusters, and 2 uncertain candidates. Our observations allowed a reliable estimate of the target radial velocity, within a typical accuracy of ~+/-20Km/s. The observed candidates have been robustly classified according to their radial velocity and shape parameters that allowed us to confidently discriminate between point sources and extended objects even from low-spatial-resolution imagery. In our set of 76 candidate clusters we found: 42 newly-confirmed bona-fide M31 clusters, 12 background galaxies, 17 foreground Galactic stars, 2 HII regions belonging to M31 and 3 unclassified (possibly M31 clusters or foreground stars) objects. The classification of a few other candidates not included in our survey has been also reassessed on various observational bases. All the sources of radial velocity estimates for M31 known globular clusters available in the literature have been compared and checked, and a homogeneous general list has been obtained for 349 confirmed clusters with radial velocity. Our results suggest that a significant number of genuine clusters (~&gt;100) is still hidden among the plethora of known candidates proposed by various authors. Hence our knowledge of the globular cluster system of the M31 galaxy is still far from complete even in terms of simple membership.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985#2</TD>
            <TD>2011-09-14T20:01:30Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/456/985&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/985</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/456/985 [table5]</TD>
            <TD>Radial velocities of 76 M31 candidate clusters (Galleti+, 2006)</TD>
            <TD>We present the first results of a large spectroscopic survey of globular clusters and candidate globular clusters in the nearby M31 galaxy. The survey is aimed at the classification of known candidate M31 clusters and at the study of their kinematic properties. We obtained low-resolution spectroscopy for 133 targets, including 76 yet-to-be-confirmed candidate clusters (i.e. with no previous spectroscopic information), 55 already-confirmed genuine M31 clusters, and 2 uncertain candidates. Our observations allowed a reliable estimate of the target radial velocity, within a typical accuracy of ~+/-20Km/s. The observed candidates have been robustly classified according to their radial velocity and shape parameters that allowed us to confidently discriminate between point sources and extended objects even from low-spatial-resolution imagery. In our set of 76 candidate clusters we found: 42 newly-confirmed bona-fide M31 clusters, 12 background galaxies, 17 foreground Galactic stars, 2 HII regions belonging to M31 and 3 unclassified (possibly M31 clusters or foreground stars) objects. The classification of a few other candidates not included in our survey has been also reassessed on various observational bases. All the sources of radial velocity estimates for M31 known globular clusters available in the literature have been compared and checked, and a homogeneous general list has been obtained for 349 confirmed clusters with radial velocity. Our results suggest that a significant number of genuine clusters (~&gt;100) is still hidden among the plethora of known candidates proposed by various authors. Hence our knowledge of the globular cluster system of the M31 galaxy is still far from complete even in terms of simple membership.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985#table5</TD>
            <TD>2011-09-14T20:01:30Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/456/985&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/985</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/456/985 [1]</TD>
            <TD>Radial velocities of 76 M31 candidate clusters (Galleti+, 2006)</TD>
            <TD>We present the first results of a large spectroscopic survey of globular clusters and candidate globular clusters in the nearby M31 galaxy. The survey is aimed at the classification of known candidate M31 clusters and at the study of their kinematic properties. We obtained low-resolution spectroscopy for 133 targets, including 76 yet-to-be-confirmed candidate clusters (i.e. with no previous spectroscopic information), 55 already-confirmed genuine M31 clusters, and 2 uncertain candidates. Our observations allowed a reliable estimate of the target radial velocity, within a typical accuracy of ~+/-20Km/s. The observed candidates have been robustly classified according to their radial velocity and shape parameters that allowed us to confidently discriminate between point sources and extended objects even from low-spatial-resolution imagery. In our set of 76 candidate clusters we found: 42 newly-confirmed bona-fide M31 clusters, 12 background galaxies, 17 foreground Galactic stars, 2 HII regions belonging to M31 and 3 unclassified (possibly M31 clusters or foreground stars) objects. The classification of a few other candidates not included in our survey has been also reassessed on various observational bases. All the sources of radial velocity estimates for M31 known globular clusters available in the literature have been compared and checked, and a homogeneous general list has been obtained for 349 confirmed clusters with radial velocity. Our results suggest that a significant number of genuine clusters (~&gt;100) is still hidden among the plethora of known candidates proposed by various authors. Hence our knowledge of the globular cluster system of the M31 galaxy is still far from complete even in terms of simple membership.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985#1</TD>
            <TD>2011-09-14T20:01:30Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/456/985</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/985</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/456/985 [2]</TD>
            <TD>Radial velocities of 76 M31 candidate clusters (Galleti+, 2006)</TD>
            <TD>We present the first results of a large spectroscopic survey of globular clusters and candidate globular clusters in the nearby M31 galaxy. The survey is aimed at the classification of known candidate M31 clusters and at the study of their kinematic properties. We obtained low-resolution spectroscopy for 133 targets, including 76 yet-to-be-confirmed candidate clusters (i.e. with no previous spectroscopic information), 55 already-confirmed genuine M31 clusters, and 2 uncertain candidates. Our observations allowed a reliable estimate of the target radial velocity, within a typical accuracy of ~+/-20Km/s. The observed candidates have been robustly classified according to their radial velocity and shape parameters that allowed us to confidently discriminate between point sources and extended objects even from low-spatial-resolution imagery. In our set of 76 candidate clusters we found: 42 newly-confirmed bona-fide M31 clusters, 12 background galaxies, 17 foreground Galactic stars, 2 HII regions belonging to M31 and 3 unclassified (possibly M31 clusters or foreground stars) objects. The classification of a few other candidates not included in our survey has been also reassessed on various observational bases. All the sources of radial velocity estimates for M31 known globular clusters available in the literature have been compared and checked, and a homogeneous general list has been obtained for 349 confirmed clusters with radial velocity. Our results suggest that a significant number of genuine clusters (~&gt;100) is still hidden among the plethora of known candidates proposed by various authors. Hence our knowledge of the globular cluster system of the M31 galaxy is still far from complete even in terms of simple membership.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985#2</TD>
            <TD>2011-09-14T20:01:30Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/456/985&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/985</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/456/985 [table5]</TD>
            <TD>Radial velocities of 76 M31 candidate clusters (Galleti+, 2006)</TD>
            <TD>We present the first results of a large spectroscopic survey of globular clusters and candidate globular clusters in the nearby M31 galaxy. The survey is aimed at the classification of known candidate M31 clusters and at the study of their kinematic properties. We obtained low-resolution spectroscopy for 133 targets, including 76 yet-to-be-confirmed candidate clusters (i.e. with no previous spectroscopic information), 55 already-confirmed genuine M31 clusters, and 2 uncertain candidates. Our observations allowed a reliable estimate of the target radial velocity, within a typical accuracy of ~+/-20Km/s. The observed candidates have been robustly classified according to their radial velocity and shape parameters that allowed us to confidently discriminate between point sources and extended objects even from low-spatial-resolution imagery. In our set of 76 candidate clusters we found: 42 newly-confirmed bona-fide M31 clusters, 12 background galaxies, 17 foreground Galactic stars, 2 HII regions belonging to M31 and 3 unclassified (possibly M31 clusters or foreground stars) objects. The classification of a few other candidates not included in our survey has been also reassessed on various observational bases. All the sources of radial velocity estimates for M31 known globular clusters available in the literature have been compared and checked, and a homogeneous general list has been obtained for 349 confirmed clusters with radial velocity. Our results suggest that a significant number of genuine clusters (~&gt;100) is still hidden among the plethora of known candidates proposed by various authors. Hence our knowledge of the globular cluster system of the M31 galaxy is still far from complete even in terms of simple membership.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985#table5</TD>
            <TD>2011-09-14T20:01:30Z</TD>
            <TD>#Globular_Clusters#Photometry#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jun-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/456/985</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/456/985&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/456/985</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/462/811 [1]</TD>
            <TD>Superclusters of galaxies from 2dF (Einasto+, 2007)</TD>
            <TD>Tables contain data on superclusters, selected from the 2dFGRS survey. Catalogues consist of four lists, two for each Galaxy hemisphere, the main lists A for superclusters up to distance 520Mpc/h, and supplementary lists B for more distant systems. The lists are ordered according to increasing RA, a common id-numeration for lists A and B. Distance and sizes are given in Mpc/h, luminosities in Solar units L_{sun}_/h^2, where h is the Hubble constant in units of 100km/s/Mpc</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811#1</TD>
            <TD>2011-09-14T20:02:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/462/811</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/811</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/462/811 [2]</TD>
            <TD>Superclusters of galaxies from 2dF (Einasto+, 2007)</TD>
            <TD>Tables contain data on superclusters, selected from the 2dFGRS survey. Catalogues consist of four lists, two for each Galaxy hemisphere, the main lists A for superclusters up to distance 520Mpc/h, and supplementary lists B for more distant systems. The lists are ordered according to increasing RA, a common id-numeration for lists A and B. Distance and sizes are given in Mpc/h, luminosities in Solar units L_{sun}_/h^2, where h is the Hubble constant in units of 100km/s/Mpc</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811#2</TD>
            <TD>2011-09-14T20:02:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/462/811&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/811</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/462/811 [SCl]</TD>
            <TD>Superclusters of galaxies from 2dF (Einasto+, 2007)</TD>
            <TD>Tables contain data on superclusters, selected from the 2dFGRS survey. Catalogues consist of four lists, two for each Galaxy hemisphere, the main lists A for superclusters up to distance 520Mpc/h, and supplementary lists B for more distant systems. The lists are ordered according to increasing RA, a common id-numeration for lists A and B. Distance and sizes are given in Mpc/h, luminosities in Solar units L_{sun}_/h^2, where h is the Hubble constant in units of 100km/s/Mpc</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811#SCl</TD>
            <TD>2011-09-14T20:02:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/462/811&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/811</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/462/811 [1]</TD>
            <TD>Superclusters of galaxies from 2dF (Einasto+, 2007)</TD>
            <TD>Tables contain data on superclusters, selected from the 2dFGRS survey. Catalogues consist of four lists, two for each Galaxy hemisphere, the main lists A for superclusters up to distance 520Mpc/h, and supplementary lists B for more distant systems. The lists are ordered according to increasing RA, a common id-numeration for lists A and B. Distance and sizes are given in Mpc/h, luminosities in Solar units L_{sun}_/h^2, where h is the Hubble constant in units of 100km/s/Mpc</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811#1</TD>
            <TD>2011-09-14T20:02:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/462/811</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/811</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/462/811 [2]</TD>
            <TD>Superclusters of galaxies from 2dF (Einasto+, 2007)</TD>
            <TD>Tables contain data on superclusters, selected from the 2dFGRS survey. Catalogues consist of four lists, two for each Galaxy hemisphere, the main lists A for superclusters up to distance 520Mpc/h, and supplementary lists B for more distant systems. The lists are ordered according to increasing RA, a common id-numeration for lists A and B. Distance and sizes are given in Mpc/h, luminosities in Solar units L_{sun}_/h^2, where h is the Hubble constant in units of 100km/s/Mpc</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811#2</TD>
            <TD>2011-09-14T20:02:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/462/811&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/811</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/462/811 [SCl]</TD>
            <TD>Superclusters of galaxies from 2dF (Einasto+, 2007)</TD>
            <TD>Tables contain data on superclusters, selected from the 2dFGRS survey. Catalogues consist of four lists, two for each Galaxy hemisphere, the main lists A for superclusters up to distance 520Mpc/h, and supplementary lists B for more distant systems. The lists are ordered according to increasing RA, a common id-numeration for lists A and B. Distance and sizes are given in Mpc/h, luminosities in Solar units L_{sun}_/h^2, where h is the Hubble constant in units of 100km/s/Mpc</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811#SCl</TD>
            <TD>2011-09-14T20:02:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/462/811&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/811</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/462/811 [1]</TD>
            <TD>Superclusters of galaxies from 2dF (Einasto+, 2007)</TD>
            <TD>Tables contain data on superclusters, selected from the 2dFGRS survey. Catalogues consist of four lists, two for each Galaxy hemisphere, the main lists A for superclusters up to distance 520Mpc/h, and supplementary lists B for more distant systems. The lists are ordered according to increasing RA, a common id-numeration for lists A and B. Distance and sizes are given in Mpc/h, luminosities in Solar units L_{sun}_/h^2, where h is the Hubble constant in units of 100km/s/Mpc</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811#1</TD>
            <TD>2011-09-14T20:02:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/462/811</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/811</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/462/811 [2]</TD>
            <TD>Superclusters of galaxies from 2dF (Einasto+, 2007)</TD>
            <TD>Tables contain data on superclusters, selected from the 2dFGRS survey. Catalogues consist of four lists, two for each Galaxy hemisphere, the main lists A for superclusters up to distance 520Mpc/h, and supplementary lists B for more distant systems. The lists are ordered according to increasing RA, a common id-numeration for lists A and B. Distance and sizes are given in Mpc/h, luminosities in Solar units L_{sun}_/h^2, where h is the Hubble constant in units of 100km/s/Mpc</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811#2</TD>
            <TD>2011-09-14T20:02:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/462/811&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/811</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/462/811 [SCl]</TD>
            <TD>Superclusters of galaxies from 2dF (Einasto+, 2007)</TD>
            <TD>Tables contain data on superclusters, selected from the 2dFGRS survey. Catalogues consist of four lists, two for each Galaxy hemisphere, the main lists A for superclusters up to distance 520Mpc/h, and supplementary lists B for more distant systems. The lists are ordered according to increasing RA, a common id-numeration for lists A and B. Distance and sizes are given in Mpc/h, luminosities in Solar units L_{sun}_/h^2, where h is the Hubble constant in units of 100km/s/Mpc</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811#SCl</TD>
            <TD>2011-09-14T20:02:02Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Dec-2006</TD>
            <TD>ivo://CDS.VizieR/J/A+A/462/811</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/462/811&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/462/811</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/451 [1]</TD>
            <TD>Radio continuum spectra of GPS galaxies (Torniainen+, 2007)</TD>
            <TD>Radio continuum spectral properties of a sample of 96 galaxy-type gigahertz-peaked spectrum (GPS) sources are presented. When available, also the redshifts of the sources are listed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451#1</TD>
            <TD>2011-09-14T20:11:31Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/451 [2]</TD>
            <TD>Radio continuum spectra of GPS galaxies (Torniainen+, 2007)</TD>
            <TD>Radio continuum spectral properties of a sample of 96 galaxy-type gigahertz-peaked spectrum (GPS) sources are presented. When available, also the redshifts of the sources are listed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451#2</TD>
            <TD>2011-09-14T20:11:31Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/451 [table2]</TD>
            <TD>Radio continuum spectra of GPS galaxies (Torniainen+, 2007)</TD>
            <TD>Radio continuum spectral properties of a sample of 96 galaxy-type gigahertz-peaked spectrum (GPS) sources are presented. When available, also the redshifts of the sources are listed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451#table2</TD>
            <TD>2011-09-14T20:11:31Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/469/451 [1]</TD>
            <TD>Radio continuum spectra of GPS galaxies (Torniainen+, 2007)</TD>
            <TD>Radio continuum spectral properties of a sample of 96 galaxy-type gigahertz-peaked spectrum (GPS) sources are presented. When available, also the redshifts of the sources are listed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451#1</TD>
            <TD>2011-09-14T20:11:31Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/469/451</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/451</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/469/451 [2]</TD>
            <TD>Radio continuum spectra of GPS galaxies (Torniainen+, 2007)</TD>
            <TD>Radio continuum spectral properties of a sample of 96 galaxy-type gigahertz-peaked spectrum (GPS) sources are presented. When available, also the redshifts of the sources are listed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451#2</TD>
            <TD>2011-09-14T20:11:31Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/469/451&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/451</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/469/451 [table2]</TD>
            <TD>Radio continuum spectra of GPS galaxies (Torniainen+, 2007)</TD>
            <TD>Radio continuum spectral properties of a sample of 96 galaxy-type gigahertz-peaked spectrum (GPS) sources are presented. When available, also the redshifts of the sources are listed.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451#table2</TD>
            <TD>2011-09-14T20:11:31Z</TD>
            <TD>#Galaxies#QSOs#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>25-Apr-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/469/451</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/469/451&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/469/451</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/1065 [1]</TD>
            <TD>Members of the Sculptor dwarf spheroidal galaxy (Coleman+, 2005)</TD>
            <TD>Images of the Sculptor region were obtained at the Siding Spring Observatory 1m telescope equipped with the Wide Field Imager (WFI). Sixteen fields were observed in two filters (V and I), thereby covering a 3.1{deg}x3.1{deg} area on the sky using a 4x4 mosaic of WFI fields. The 2dF instrument at the prime focus of the Anglo-Australian Telescope allows the simultaneous spectroscopy of up to 400 targets over a field of view 2{deg} in diameter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065#1</TD>
            <TD>2011-09-14T20:11:43Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/1065</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1065</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/1065 [2]</TD>
            <TD>Members of the Sculptor dwarf spheroidal galaxy (Coleman+, 2005)</TD>
            <TD>Images of the Sculptor region were obtained at the Siding Spring Observatory 1m telescope equipped with the Wide Field Imager (WFI). Sixteen fields were observed in two filters (V and I), thereby covering a 3.1{deg}x3.1{deg} area on the sky using a 4x4 mosaic of WFI fields. The 2dF instrument at the prime focus of the Anglo-Australian Telescope allows the simultaneous spectroscopy of up to 400 targets over a field of view 2{deg} in diameter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065#2</TD>
            <TD>2011-09-14T20:11:43Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/1065&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1065</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/1065 [table7]</TD>
            <TD>Members of the Sculptor dwarf spheroidal galaxy (Coleman+, 2005)</TD>
            <TD>Images of the Sculptor region were obtained at the Siding Spring Observatory 1m telescope equipped with the Wide Field Imager (WFI). Sixteen fields were observed in two filters (V and I), thereby covering a 3.1{deg}x3.1{deg} area on the sky using a 4x4 mosaic of WFI fields. The 2dF instrument at the prime focus of the Anglo-Australian Telescope allows the simultaneous spectroscopy of up to 400 targets over a field of view 2{deg} in diameter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065#table7</TD>
            <TD>2011-09-14T20:11:43Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/1065&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1065</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/1065 [1]</TD>
            <TD>Members of the Sculptor dwarf spheroidal galaxy (Coleman+, 2005)</TD>
            <TD>Images of the Sculptor region were obtained at the Siding Spring Observatory 1m telescope equipped with the Wide Field Imager (WFI). Sixteen fields were observed in two filters (V and I), thereby covering a 3.1{deg}x3.1{deg} area on the sky using a 4x4 mosaic of WFI fields. The 2dF instrument at the prime focus of the Anglo-Australian Telescope allows the simultaneous spectroscopy of up to 400 targets over a field of view 2{deg} in diameter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065#1</TD>
            <TD>2011-09-14T20:11:43Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/1065</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1065</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/1065 [2]</TD>
            <TD>Members of the Sculptor dwarf spheroidal galaxy (Coleman+, 2005)</TD>
            <TD>Images of the Sculptor region were obtained at the Siding Spring Observatory 1m telescope equipped with the Wide Field Imager (WFI). Sixteen fields were observed in two filters (V and I), thereby covering a 3.1{deg}x3.1{deg} area on the sky using a 4x4 mosaic of WFI fields. The 2dF instrument at the prime focus of the Anglo-Australian Telescope allows the simultaneous spectroscopy of up to 400 targets over a field of view 2{deg} in diameter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065#2</TD>
            <TD>2011-09-14T20:11:43Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/1065&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1065</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/1065 [table7]</TD>
            <TD>Members of the Sculptor dwarf spheroidal galaxy (Coleman+, 2005)</TD>
            <TD>Images of the Sculptor region were obtained at the Siding Spring Observatory 1m telescope equipped with the Wide Field Imager (WFI). Sixteen fields were observed in two filters (V and I), thereby covering a 3.1{deg}x3.1{deg} area on the sky using a 4x4 mosaic of WFI fields. The 2dF instrument at the prime focus of the Anglo-Australian Telescope allows the simultaneous spectroscopy of up to 400 targets over a field of view 2{deg} in diameter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065#table7</TD>
            <TD>2011-09-14T20:11:43Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/1065&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1065</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/1065 [1]</TD>
            <TD>Members of the Sculptor dwarf spheroidal galaxy (Coleman+, 2005)</TD>
            <TD>Images of the Sculptor region were obtained at the Siding Spring Observatory 1m telescope equipped with the Wide Field Imager (WFI). Sixteen fields were observed in two filters (V and I), thereby covering a 3.1{deg}x3.1{deg} area on the sky using a 4x4 mosaic of WFI fields. The 2dF instrument at the prime focus of the Anglo-Australian Telescope allows the simultaneous spectroscopy of up to 400 targets over a field of view 2{deg} in diameter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065#1</TD>
            <TD>2011-09-14T20:11:43Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/1065</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1065</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/1065 [2]</TD>
            <TD>Members of the Sculptor dwarf spheroidal galaxy (Coleman+, 2005)</TD>
            <TD>Images of the Sculptor region were obtained at the Siding Spring Observatory 1m telescope equipped with the Wide Field Imager (WFI). Sixteen fields were observed in two filters (V and I), thereby covering a 3.1{deg}x3.1{deg} area on the sky using a 4x4 mosaic of WFI fields. The 2dF instrument at the prime focus of the Anglo-Australian Telescope allows the simultaneous spectroscopy of up to 400 targets over a field of view 2{deg} in diameter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065#2</TD>
            <TD>2011-09-14T20:11:43Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/1065&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1065</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/1065 [table7]</TD>
            <TD>Members of the Sculptor dwarf spheroidal galaxy (Coleman+, 2005)</TD>
            <TD>Images of the Sculptor region were obtained at the Siding Spring Observatory 1m telescope equipped with the Wide Field Imager (WFI). Sixteen fields were observed in two filters (V and I), thereby covering a 3.1{deg}x3.1{deg} area on the sky using a 4x4 mosaic of WFI fields. The 2dF instrument at the prime focus of the Anglo-Australian Telescope allows the simultaneous spectroscopy of up to 400 targets over a field of view 2{deg} in diameter.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065#table7</TD>
            <TD>2011-09-14T20:11:43Z</TD>
            <TD>#Abundances#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/1065</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/1065&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/1065</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/957 [1]</TD>
            <TD>Radial velocities of 6dF galaxies (Fleenor+, 2005)</TD>
            <TD>Observations covering the 12{deg}x14{deg} area in the HRS were carried out on the 1.2m UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) in 2002 October and November. All observations were carried out as part of the 6dF Galaxy Survey (6dFGS) program being undertaken by the AAO (Wakamatsu et al. 2003ASPC..289...97W).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957#1</TD>
            <TD>2011-09-14T20:11:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/957</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/957</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/957 [2]</TD>
            <TD>Radial velocities of 6dF galaxies (Fleenor+, 2005)</TD>
            <TD>Observations covering the 12{deg}x14{deg} area in the HRS were carried out on the 1.2m UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) in 2002 October and November. All observations were carried out as part of the 6dF Galaxy Survey (6dFGS) program being undertaken by the AAO (Wakamatsu et al. 2003ASPC..289...97W).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957#2</TD>
            <TD>2011-09-14T20:11:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/957&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/957</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/957 [table2]</TD>
            <TD>Radial velocities of 6dF galaxies (Fleenor+, 2005)</TD>
            <TD>Observations covering the 12{deg}x14{deg} area in the HRS were carried out on the 1.2m UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) in 2002 October and November. All observations were carried out as part of the 6dF Galaxy Survey (6dFGS) program being undertaken by the AAO (Wakamatsu et al. 2003ASPC..289...97W).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957#table2</TD>
            <TD>2011-09-14T20:11:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/957&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/957</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/957 [1]</TD>
            <TD>Radial velocities of 6dF galaxies (Fleenor+, 2005)</TD>
            <TD>Observations covering the 12{deg}x14{deg} area in the HRS were carried out on the 1.2m UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) in 2002 October and November. All observations were carried out as part of the 6dF Galaxy Survey (6dFGS) program being undertaken by the AAO (Wakamatsu et al. 2003ASPC..289...97W).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957#1</TD>
            <TD>2011-09-14T20:11:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/957</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/957</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/957 [2]</TD>
            <TD>Radial velocities of 6dF galaxies (Fleenor+, 2005)</TD>
            <TD>Observations covering the 12{deg}x14{deg} area in the HRS were carried out on the 1.2m UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) in 2002 October and November. All observations were carried out as part of the 6dF Galaxy Survey (6dFGS) program being undertaken by the AAO (Wakamatsu et al. 2003ASPC..289...97W).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957#2</TD>
            <TD>2011-09-14T20:11:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/957&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/957</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/957 [table2]</TD>
            <TD>Radial velocities of 6dF galaxies (Fleenor+, 2005)</TD>
            <TD>Observations covering the 12{deg}x14{deg} area in the HRS were carried out on the 1.2m UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) in 2002 October and November. All observations were carried out as part of the 6dF Galaxy Survey (6dFGS) program being undertaken by the AAO (Wakamatsu et al. 2003ASPC..289...97W).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957#table2</TD>
            <TD>2011-09-14T20:11:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/957&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/957</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/130/957 [1]</TD>
            <TD>Radial velocities of 6dF galaxies (Fleenor+, 2005)</TD>
            <TD>Observations covering the 12{deg}x14{deg} area in the HRS were carried out on the 1.2m UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) in 2002 October and November. All observations were carried out as part of the 6dF Galaxy Survey (6dFGS) program being undertaken by the AAO (Wakamatsu et al. 2003ASPC..289...97W).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957#1</TD>
            <TD>2011-09-14T20:11:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/130/957</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/957</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/130/957 [2]</TD>
            <TD>Radial velocities of 6dF galaxies (Fleenor+, 2005)</TD>
            <TD>Observations covering the 12{deg}x14{deg} area in the HRS were carried out on the 1.2m UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) in 2002 October and November. All observations were carried out as part of the 6dF Galaxy Survey (6dFGS) program being undertaken by the AAO (Wakamatsu et al. 2003ASPC..289...97W).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957#2</TD>
            <TD>2011-09-14T20:11:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/130/957&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/957</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/130/957 [table2]</TD>
            <TD>Radial velocities of 6dF galaxies (Fleenor+, 2005)</TD>
            <TD>Observations covering the 12{deg}x14{deg} area in the HRS were carried out on the 1.2m UK Schmidt Telescope (UKST) of the Anglo-Australian Observatory (AAO) in 2002 October and November. All observations were carried out as part of the 6dF Galaxy Survey (6dFGS) program being undertaken by the AAO (Wakamatsu et al. 2003ASPC..289...97W).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957#table2</TD>
            <TD>2011-09-14T20:11:44Z</TD>
            <TD>#Clusters_of_galaxies#Velocities#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>14-Nov-2005</TD>
            <TD>ivo://CDS.VizieR/J/AJ/130/957</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/130/957&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/130/957</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/372/1259 [1]</TD>
            <TD>Abundances of extragalactic globular clusters (Sharina+, 2006)</TD>
            <TD>We present measurements of ages, metallicities and [alpha/Fe] ratios for 16 globular clusters (GCs) in NGC 147, 185 and 205 and of the central regions of the diffuse galaxy light in NGC 185 and 205. Our results are based on spectra obtained with the SCORPIO multislit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality Hubble Space Telescope/WFPC2 photometry of individual stars in the studied GCs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. All our sample GCs appear to be old (T&gt;8Gyr) and metal-poor ([Z/H]&lt;1.1), except for the GCs Hubble V in NGC 205 (T=1.2+/-0.6Gyr, [Z/H]=0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2Gyr, [Z/H]=0.8+/-0.2) and FJJVII in NGC 185 (T=7+/-3Gyr, [Z/H]=0.8+/-0.2). The majority of our GCs sample has solar [alpha/Fe] enhancement in contrast to the halo population of GCs in M31 and the Milky Way. The HB morphologies for our sample GCs follow the same behaviour with metallicity as younger halo Galactic GCs. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Spectroscopic ages and metallicities of the central regions in NGC 205 and 185 coincide with those obtained from colour-magnitude diagrams. The central field stellar populations in these galaxies have approximately the same age as their most central GCs (Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the central GCs.</TD>
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            <TD>HTTP Request</TD>
            <TD>J/MNRAS/372/1259 [2]</TD>
            <TD>Abundances of extragalactic globular clusters (Sharina+, 2006)</TD>
            <TD>We present measurements of ages, metallicities and [alpha/Fe] ratios for 16 globular clusters (GCs) in NGC 147, 185 and 205 and of the central regions of the diffuse galaxy light in NGC 185 and 205. Our results are based on spectra obtained with the SCORPIO multislit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality Hubble Space Telescope/WFPC2 photometry of individual stars in the studied GCs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. All our sample GCs appear to be old (T&gt;8Gyr) and metal-poor ([Z/H]&lt;1.1), except for the GCs Hubble V in NGC 205 (T=1.2+/-0.6Gyr, [Z/H]=0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2Gyr, [Z/H]=0.8+/-0.2) and FJJVII in NGC 185 (T=7+/-3Gyr, [Z/H]=0.8+/-0.2). The majority of our GCs sample has solar [alpha/Fe] enhancement in contrast to the halo population of GCs in M31 and the Milky Way. The HB morphologies for our sample GCs follow the same behaviour with metallicity as younger halo Galactic GCs. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Spectroscopic ages and metallicities of the central regions in NGC 205 and 185 coincide with those obtained from colour-magnitude diagrams. The central field stellar populations in these galaxies have approximately the same age as their most central GCs (Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the central GCs.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ParamHTTP</TD>
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            <TD>Catalog</TD>
            <TD>J/MNRAS/372/1259 [objects]</TD>
            <TD>Abundances of extragalactic globular clusters (Sharina+, 2006)</TD>
            <TD>We present measurements of ages, metallicities and [alpha/Fe] ratios for 16 globular clusters (GCs) in NGC 147, 185 and 205 and of the central regions of the diffuse galaxy light in NGC 185 and 205. Our results are based on spectra obtained with the SCORPIO multislit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality Hubble Space Telescope/WFPC2 photometry of individual stars in the studied GCs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. All our sample GCs appear to be old (T&gt;8Gyr) and metal-poor ([Z/H]&lt;1.1), except for the GCs Hubble V in NGC 205 (T=1.2+/-0.6Gyr, [Z/H]=0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2Gyr, [Z/H]=0.8+/-0.2) and FJJVII in NGC 185 (T=7+/-3Gyr, [Z/H]=0.8+/-0.2). The majority of our GCs sample has solar [alpha/Fe] enhancement in contrast to the halo population of GCs in M31 and the Milky Way. The HB morphologies for our sample GCs follow the same behaviour with metallicity as younger halo Galactic GCs. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Spectroscopic ages and metallicities of the central regions in NGC 205 and 185 coincide with those obtained from colour-magnitude diagrams. The central field stellar populations in these galaxies have approximately the same age as their most central GCs (Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the central GCs.</TD>
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            <TD>Web Page</TD>
            <TD>J/MNRAS/372/1259 [1]</TD>
            <TD>Abundances of extragalactic globular clusters (Sharina+, 2006)</TD>
            <TD>We present measurements of ages, metallicities and [alpha/Fe] ratios for 16 globular clusters (GCs) in NGC 147, 185 and 205 and of the central regions of the diffuse galaxy light in NGC 185 and 205. Our results are based on spectra obtained with the SCORPIO multislit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality Hubble Space Telescope/WFPC2 photometry of individual stars in the studied GCs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. All our sample GCs appear to be old (T&gt;8Gyr) and metal-poor ([Z/H]&lt;1.1), except for the GCs Hubble V in NGC 205 (T=1.2+/-0.6Gyr, [Z/H]=0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2Gyr, [Z/H]=0.8+/-0.2) and FJJVII in NGC 185 (T=7+/-3Gyr, [Z/H]=0.8+/-0.2). The majority of our GCs sample has solar [alpha/Fe] enhancement in contrast to the halo population of GCs in M31 and the Milky Way. The HB morphologies for our sample GCs follow the same behaviour with metallicity as younger halo Galactic GCs. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Spectroscopic ages and metallicities of the central regions in NGC 205 and 185 coincide with those obtained from colour-magnitude diagrams. The central field stellar populations in these galaxies have approximately the same age as their most central GCs (Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the central GCs.</TD>
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            <TD>HTTP Request</TD>
            <TD>J/MNRAS/372/1259 [2]</TD>
            <TD>Abundances of extragalactic globular clusters (Sharina+, 2006)</TD>
            <TD>We present measurements of ages, metallicities and [alpha/Fe] ratios for 16 globular clusters (GCs) in NGC 147, 185 and 205 and of the central regions of the diffuse galaxy light in NGC 185 and 205. Our results are based on spectra obtained with the SCORPIO multislit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality Hubble Space Telescope/WFPC2 photometry of individual stars in the studied GCs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. All our sample GCs appear to be old (T&gt;8Gyr) and metal-poor ([Z/H]&lt;1.1), except for the GCs Hubble V in NGC 205 (T=1.2+/-0.6Gyr, [Z/H]=0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2Gyr, [Z/H]=0.8+/-0.2) and FJJVII in NGC 185 (T=7+/-3Gyr, [Z/H]=0.8+/-0.2). The majority of our GCs sample has solar [alpha/Fe] enhancement in contrast to the halo population of GCs in M31 and the Milky Way. The HB morphologies for our sample GCs follow the same behaviour with metallicity as younger halo Galactic GCs. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Spectroscopic ages and metallicities of the central regions in NGC 205 and 185 coincide with those obtained from colour-magnitude diagrams. The central field stellar populations in these galaxies have approximately the same age as their most central GCs (Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the central GCs.</TD>
            <TD>CDS</TD>
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            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/372/1259&amp;</TD>
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            <TD>Catalog</TD>
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            <TD>Abundances of extragalactic globular clusters (Sharina+, 2006)</TD>
            <TD>We present measurements of ages, metallicities and [alpha/Fe] ratios for 16 globular clusters (GCs) in NGC 147, 185 and 205 and of the central regions of the diffuse galaxy light in NGC 185 and 205. Our results are based on spectra obtained with the SCORPIO multislit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality Hubble Space Telescope/WFPC2 photometry of individual stars in the studied GCs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. All our sample GCs appear to be old (T&gt;8Gyr) and metal-poor ([Z/H]&lt;1.1), except for the GCs Hubble V in NGC 205 (T=1.2+/-0.6Gyr, [Z/H]=0.6+/-0.2), Hubble VI in NGC 205 (T=4+/-2Gyr, [Z/H]=0.8+/-0.2) and FJJVII in NGC 185 (T=7+/-3Gyr, [Z/H]=0.8+/-0.2). The majority of our GCs sample has solar [alpha/Fe] enhancement in contrast to the halo population of GCs in M31 and the Milky Way. The HB morphologies for our sample GCs follow the same behaviour with metallicity as younger halo Galactic GCs. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Spectroscopic ages and metallicities of the central regions in NGC 205 and 185 coincide with those obtained from colour-magnitude diagrams. The central field stellar populations in these galaxies have approximately the same age as their most central GCs (Hubble V in NGC 205 and FJJIII in NGC 185), but are more metal-rich than the central GCs.</TD>
            <TD>CDS</TD>
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            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJ/634/1319 [1]</TD>
            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
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            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
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            <TD />
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            <TD>std</TD>
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            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
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            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>Web Page</TD>
            <TD>J/ApJ/634/1319 [1]</TD>
            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
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            <TD>HTTP Request</TD>
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            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
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            <TD>ParamHTTP</TD>
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            <TD>std</TD>
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            <TD>Catalog</TD>
            <TD>J/ApJ/634/1319 [table4]</TD>
            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319#table4</TD>
            <TD>2011-09-14T20:15:49Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/634/1319&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/1319</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/634/1319 [1]</TD>
            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319#1</TD>
            <TD>2011-09-14T20:15:49Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/634/1319</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/1319</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/634/1319 [2]</TD>
            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319#2</TD>
            <TD>2011-09-14T20:15:49Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/634/1319&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/1319</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/634/1319 [table2]</TD>
            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319#table2</TD>
            <TD>2011-09-14T20:15:49Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/634/1319&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/1319</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/634/1319 [table4]</TD>
            <TD>Synthetic Lick indices of alpha-enhanced stars (Franchini+ 2005)</TD>
            <TD>A sample of 119 F, G, and K solar neighborhood stars, selected under the condition [Fe/H]&gt;0.00, is investigated in order to detect which of them, if any, present {alpha}-enhanced characteristics. According to the kinematics, the sample represents stars of the thin-disk component of the Galaxy.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319#table4</TD>
            <TD>2011-09-14T20:15:49Z</TD>
            <TD>#Abundances#Stars:late-type#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Aug-2006</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/634/1319</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/634/1319&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/634/1319</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/379/289 [1]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz. II. (Kerton+, 2007)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to construct a new catalogue of extended radio sources found near the Galactic plane in the second quadrant of our Galaxy. In addition cross-identifications are made with other major radio catalogues and information is provided to facilitate the recovery of CGPS image data associated with each catalogued source.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289#1</TD>
            <TD>2011-09-14T20:15:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/379/289</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/289</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/379/289 [2]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz. II. (Kerton+, 2007)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to construct a new catalogue of extended radio sources found near the Galactic plane in the second quadrant of our Galaxy. In addition cross-identifications are made with other major radio catalogues and information is provided to facilitate the recovery of CGPS image data associated with each catalogued source.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289#2</TD>
            <TD>2011-09-14T20:15:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/379/289&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/289</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/379/289 [tables]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz. II. (Kerton+, 2007)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to construct a new catalogue of extended radio sources found near the Galactic plane in the second quadrant of our Galaxy. In addition cross-identifications are made with other major radio catalogues and information is provided to facilitate the recovery of CGPS image data associated with each catalogued source.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289#tables</TD>
            <TD>2011-09-14T20:15:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/379/289&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/289</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/379/289 [1]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz. II. (Kerton+, 2007)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to construct a new catalogue of extended radio sources found near the Galactic plane in the second quadrant of our Galaxy. In addition cross-identifications are made with other major radio catalogues and information is provided to facilitate the recovery of CGPS image data associated with each catalogued source.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289#1</TD>
            <TD>2011-09-14T20:15:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/379/289</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/289</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/379/289 [2]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz. II. (Kerton+, 2007)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to construct a new catalogue of extended radio sources found near the Galactic plane in the second quadrant of our Galaxy. In addition cross-identifications are made with other major radio catalogues and information is provided to facilitate the recovery of CGPS image data associated with each catalogued source.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289#2</TD>
            <TD>2011-09-14T20:15:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/379/289&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/289</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/379/289 [tables]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz. II. (Kerton+, 2007)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to construct a new catalogue of extended radio sources found near the Galactic plane in the second quadrant of our Galaxy. In addition cross-identifications are made with other major radio catalogues and information is provided to facilitate the recovery of CGPS image data associated with each catalogued source.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289#tables</TD>
            <TD>2011-09-14T20:15:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/379/289&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/289</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/379/289 [1]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz. II. (Kerton+, 2007)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to construct a new catalogue of extended radio sources found near the Galactic plane in the second quadrant of our Galaxy. In addition cross-identifications are made with other major radio catalogues and information is provided to facilitate the recovery of CGPS image data associated with each catalogued source.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289#1</TD>
            <TD>2011-09-14T20:15:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/379/289</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/289</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/379/289 [2]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz. II. (Kerton+, 2007)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to construct a new catalogue of extended radio sources found near the Galactic plane in the second quadrant of our Galaxy. In addition cross-identifications are made with other major radio catalogues and information is provided to facilitate the recovery of CGPS image data associated with each catalogued source.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289#2</TD>
            <TD>2011-09-14T20:15:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/379/289&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/289</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/379/289 [tables]</TD>
            <TD>The outer Galaxy at 1420 and 408MHz. II. (Kerton+, 2007)</TD>
            <TD>Arcminute-resolution radio continuum images at 408 and 1420MHz from the Canadian Galactic Plane Survey (CGPS) have been used to construct a new catalogue of extended radio sources found near the Galactic plane in the second quadrant of our Galaxy. In addition cross-identifications are made with other major radio catalogues and information is provided to facilitate the recovery of CGPS image data associated with each catalogued source.</TD>
            <TD>CDS</TD>
            <TD>#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289#tables</TD>
            <TD>2011-09-14T20:15:51Z</TD>
            <TD>##</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>24-Aug-2007</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/379/289</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/379/289&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/379/289</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/473/399 [1]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#1</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/473/399</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/473/399 [2]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#2</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/473/399&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/473/399 [table1]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#table1</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/473/399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/473/399 [table8]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#table8</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/473/399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/473/399 [1]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#1</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/473/399</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/473/399 [2]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#2</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/473/399&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/473/399 [table1]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#table1</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/473/399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/473/399 [table8]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#table8</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/473/399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/A+A/473/399 [1]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#1</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/A+A/473/399</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/A+A/473/399 [2]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#2</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/A+A/473/399&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/473/399 [table1]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#table1</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/473/399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/A+A/473/399 [table8]</TD>
            <TD>Optical and HI data of 6 southern galaxy groups (Pompei+, 2007)</TD>
            <TD>Multi-wavelength observations of Hickson's Compact Groups (HCGs) have shown that many of these groups are physical bound structures and are in different stage of evolution, from spiral-dominated systems to almost merged objects. Very few studies have analysed the Southern Compact Groups (SCGs) sample, which is thought to be younger that HCGs, due to an on average higher number of spiral galaxies. We present here the first results from optical and radio observations on a pilot sample of SCGs. Optical observations of SCGs obtained with ESO telescopes and radio data from the ATCA allow us to probe the distribution of the warm intra-group medium and the evolutionary stage of each group, by means of morphological studies and via measurements of star formation and other types of nuclear activity.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399#table8</TD>
            <TD>2011-09-14T20:16:24Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>05-Oct-2007</TD>
            <TD>ivo://CDS.VizieR/J/A+A/473/399</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/A+A/473/399&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/A+A/473/399</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>GHOSTS [1]</TD>
            <TD>Galaxy Halos, Outer disks, Substructure, Thick disks and Star clusters (GHOSTS)</TD>
            <TD>The GHOSTS survey is the largest study to date of the resolved stellar populations in the outskirts of disk galaxies. The sample consists of 14 disk galaxies within 17 Mpc, whose outer disks and halos are imaged with the Hubble Space Telescope Advanced Camera for Surveys (ACS).</TD>
            <TD>Space Telescope Science Institute Archive</TD>
            <TD>#Optical#</TD>
            <TD>ivo://archive.stsci.edu/ghosts#1</TD>
            <TD>2012-04-30T20:48:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://archive.stsci.edu/ghosts</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD>1.0</TD>
            <TD>STD</TD>
            <TD>http://archive.stsci.edu/siap/search.php?id=ghosts&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://archive.stsci.edu/stsci-arc</TD>
            <TD>http://archive.stsci.edu/prepds/ghosts</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>GHOSTS [2]</TD>
            <TD>Galaxy Halos, Outer disks, Substructure, Thick disks and Star clusters (GHOSTS)</TD>
            <TD>The GHOSTS survey is the largest study to date of the resolved stellar populations in the outskirts of disk galaxies. The sample consists of 14 disk galaxies within 17 Mpc, whose outer disks and halos are imaged with the Hubble Space Telescope Advanced Camera for Surveys (ACS).</TD>
            <TD>Space Telescope Science Institute Archive</TD>
            <TD>#Optical#</TD>
            <TD>ivo://archive.stsci.edu/ghosts#2</TD>
            <TD>2012-04-30T20:48:59Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD />
            <TD>ivo://archive.stsci.edu/ghosts</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://archive.stsci.edu/prepds/ghosts/display_page.html</TD>
            <TD />
            <TD />
            <TD>ivo://archive.stsci.edu/stsci-arc</TD>
            <TD>http://archive.stsci.edu/prepds/ghosts</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/504 [1]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#1</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/504</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/504 [2]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#2</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/504&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/504 [table1]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#table1</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/504&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/504 [table2]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#table2</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/504&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/504 [1]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#1</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/504</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/504 [2]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#2</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/504&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/504 [table1]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#table1</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/504&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/504 [table2]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#table2</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/504&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/504 [1]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#1</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/504</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/504 [2]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#2</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/504&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/504 [table1]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#table1</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/504&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/504 [table2]</TD>
            <TD>Galaxies around CenA/M83 galaxy complex (Karachentsev+, 2007)</TD>
            <TD>We have observed 24 galaxies with the Advanced Camera for Surveys (ACS) during HST Cycles 12 and 13 (proposals 9771 and 10235).</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504#table2</TD>
            <TD>2011-09-14T20:34:22Z</TD>
            <TD>#Clusters_of_galaxies#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/504</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/504&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/504</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1729 [1]</TD>
            <TD>Hubble Ultra Deep Field BVI-dropout sources (Beckwith+, 2006)</TD>
            <TD>This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million secs exposure of an 11arcmin^2^ region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i775), and F850LP (z850), to give approximately uniform limiting magnitudes m_AB_~29 for point sources. The image contains at least 10000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ~4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729#1</TD>
            <TD>2011-09-14T20:36:42Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1729</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1729</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1729 [2]</TD>
            <TD>Hubble Ultra Deep Field BVI-dropout sources (Beckwith+, 2006)</TD>
            <TD>This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million secs exposure of an 11arcmin^2^ region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i775), and F850LP (z850), to give approximately uniform limiting magnitudes m_AB_~29 for point sources. The image contains at least 10000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ~4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729#2</TD>
            <TD>2011-09-14T20:36:42Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1729&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1729</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1729 [bvi]</TD>
            <TD>Hubble Ultra Deep Field BVI-dropout sources (Beckwith+, 2006)</TD>
            <TD>This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million secs exposure of an 11arcmin^2^ region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i775), and F850LP (z850), to give approximately uniform limiting magnitudes m_AB_~29 for point sources. The image contains at least 10000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ~4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729#bvi</TD>
            <TD>2011-09-14T20:36:42Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1729&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1729</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1729 [1]</TD>
            <TD>Hubble Ultra Deep Field BVI-dropout sources (Beckwith+, 2006)</TD>
            <TD>This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million secs exposure of an 11arcmin^2^ region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i775), and F850LP (z850), to give approximately uniform limiting magnitudes m_AB_~29 for point sources. The image contains at least 10000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ~4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729#1</TD>
            <TD>2011-09-14T20:36:42Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1729</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1729</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1729 [2]</TD>
            <TD>Hubble Ultra Deep Field BVI-dropout sources (Beckwith+, 2006)</TD>
            <TD>This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million secs exposure of an 11arcmin^2^ region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i775), and F850LP (z850), to give approximately uniform limiting magnitudes m_AB_~29 for point sources. The image contains at least 10000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ~4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729#2</TD>
            <TD>2011-09-14T20:36:42Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1729&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1729</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1729 [bvi]</TD>
            <TD>Hubble Ultra Deep Field BVI-dropout sources (Beckwith+, 2006)</TD>
            <TD>This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million secs exposure of an 11arcmin^2^ region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i775), and F850LP (z850), to give approximately uniform limiting magnitudes m_AB_~29 for point sources. The image contains at least 10000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ~4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729#bvi</TD>
            <TD>2011-09-14T20:36:42Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1729&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1729</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/132/1729 [1]</TD>
            <TD>Hubble Ultra Deep Field BVI-dropout sources (Beckwith+, 2006)</TD>
            <TD>This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million secs exposure of an 11arcmin^2^ region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i775), and F850LP (z850), to give approximately uniform limiting magnitudes m_AB_~29 for point sources. The image contains at least 10000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ~4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729#1</TD>
            <TD>2011-09-14T20:36:42Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/132/1729</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1729</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/132/1729 [2]</TD>
            <TD>Hubble Ultra Deep Field BVI-dropout sources (Beckwith+, 2006)</TD>
            <TD>This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million secs exposure of an 11arcmin^2^ region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i775), and F850LP (z850), to give approximately uniform limiting magnitudes m_AB_~29 for point sources. The image contains at least 10000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ~4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729#2</TD>
            <TD>2011-09-14T20:36:42Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/132/1729&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1729</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/132/1729 [bvi]</TD>
            <TD>Hubble Ultra Deep Field BVI-dropout sources (Beckwith+, 2006)</TD>
            <TD>This paper presents the Hubble Ultra Deep Field (HUDF), a 1 million secs exposure of an 11arcmin^2^ region in the southern sky with the Advanced Camera for Surveys on the Hubble Space Telescope using Director's Discretionary Time. The exposure time was divided among four filters, F435W (B435), F606W (V606), F775W (i775), and F850LP (z850), to give approximately uniform limiting magnitudes m_AB_~29 for point sources. The image contains at least 10000 objects, presented here as a catalog, the vast majority of which are galaxies. Visual inspection of the images shows few if any galaxies at redshifts greater than ~4 that resemble present-day spiral or elliptical galaxies. The image reinforces the conclusion from the original Hubble Deep Field that galaxies evolved strongly during the first few billion years in the infancy of the universe. Using the Lyman break dropout method to derive samples of galaxies at redshifts between 4 and 7, it is possible to study the apparent evolution of the galaxy luminosity function and number density.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729#bvi</TD>
            <TD>2011-09-14T20:36:42Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Sep-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/132/1729</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/132/1729&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/132/1729</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/185 [1]</TD>
            <TD>GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007)</TD>
            <TD>We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; lambda_eff_=1516{AA}) and near-ultraviolet (NUV; lambda_eff_=2267{AA}) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185#1</TD>
            <TD>2011-09-14T20:36:57Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/185</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/185</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/185 [2]</TD>
            <TD>GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007)</TD>
            <TD>We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; lambda_eff_=1516{AA}) and near-ultraviolet (NUV; lambda_eff_=2267{AA}) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185#2</TD>
            <TD>2011-09-14T20:36:57Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/185&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/185</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/173/185 [galex]</TD>
            <TD>GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007)</TD>
            <TD>We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; lambda_eff_=1516{AA}) and near-ultraviolet (NUV; lambda_eff_=2267{AA}) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185#galex</TD>
            <TD>2011-09-14T20:36:57Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/173/185&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/185</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/185 [1]</TD>
            <TD>GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007)</TD>
            <TD>We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; lambda_eff_=1516{AA}) and near-ultraviolet (NUV; lambda_eff_=2267{AA}) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185#1</TD>
            <TD>2011-09-14T20:36:57Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/185</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/185</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/185 [2]</TD>
            <TD>GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007)</TD>
            <TD>We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; lambda_eff_=1516{AA}) and near-ultraviolet (NUV; lambda_eff_=2267{AA}) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185#2</TD>
            <TD>2011-09-14T20:36:57Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/185&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/185</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/173/185 [galex]</TD>
            <TD>GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007)</TD>
            <TD>We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; lambda_eff_=1516{AA}) and near-ultraviolet (NUV; lambda_eff_=2267{AA}) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185#galex</TD>
            <TD>2011-09-14T20:36:57Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/173/185&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/185</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/173/185 [1]</TD>
            <TD>GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007)</TD>
            <TD>We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; lambda_eff_=1516{AA}) and near-ultraviolet (NUV; lambda_eff_=2267{AA}) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185#1</TD>
            <TD>2011-09-14T20:36:57Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/173/185</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/185</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/173/185 [2]</TD>
            <TD>GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007)</TD>
            <TD>We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; lambda_eff_=1516{AA}) and near-ultraviolet (NUV; lambda_eff_=2267{AA}) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185#2</TD>
            <TD>2011-09-14T20:36:57Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/173/185&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/185</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/173/185 [galex]</TD>
            <TD>GALEX ultraviolet atlas of nearby galaxies (Gil de Paz+, 2007)</TD>
            <TD>We present images, integrated photometry, and surface-brightness and color profiles for a total of 1034 nearby galaxies recently observed by the Galaxy Evolution Explorer (GALEX) satellite in its far-ultraviolet (FUV; lambda_eff_=1516{AA}) and near-ultraviolet (NUV; lambda_eff_=2267{AA}) bands. Our catalog of objects is derived primarily from the GALEX Nearby Galaxies Survey (NGS) supplemented by galaxies larger than 1' in diameter serendipitously found in these fields and in other GALEX exposures of similar of greater depth. The sample analyzed here adequately describes the distribution and full range of properties (luminosity, color, star formation rate [SFR]) of galaxies in the local universe.</TD>
            <TD>CDS</TD>
            <TD>#UV#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185#galex</TD>
            <TD>2011-09-14T20:36:57Z</TD>
            <TD>#Galaxies#Photometry:wide-band#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>23-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/173/185</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/173/185&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/173/185</TD>
          </TR>
          <TR>
            <TD>Images</TD>
            <TD>HST.SGAL</TD>
            <TD>HST WFPC2 Spiral Galaxies</TD>
            <TD>Holwerda et al. examined 32 HST/WFPC2 archival fields of 29 spiral galaxies (Sab and later) for their paper The Opacity of Spiral Galaxy Disks. IV. Radial Extinction Profiles from Counts of Distant Galaxies Seen through Foreground Disks (2005, AJ,129:1396-1411). The majority of the data are from the Cepheid distance scale Key Project. The explicit goal was to provide deep mosaics in both V- and I-band with a better sampling in order to identify background galaxies through the foreground disk.</TD>
            <TD>MAST</TD>
            <TD>#Optical#</TD>
            <TD>ivo://mast.stsci/siap/hst.sgal#1</TD>
            <TD>2011-09-14T20:37:27Z</TD>
            <TD>#Optical Astronomy#</TD>
            <TD>#Archive#</TD>
            <TD>#Research#</TD>
            <TD>0.0500000007450581</TD>
            <TD>1.0</TD>
            <TD>ivo://mast.stsci/siap/hst.sgal</TD>
            <TD>SimpleImageAccess</TD>
            <TD>ivo://ivoa.net/std/SIA</TD>
            <TD>2</TD>
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://archive.stsci.edu/siap/search.php?id=sgal&amp;</TD>
            <TD />
            <TD>100</TD>
            <TD />
            <TD>http://archive.stsci.edu/prepds/sgal</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/174/117 [1]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#1</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/174/117</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/174/117 [2]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#2</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/174/117&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/174/117 [clusters]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#clusters</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/174/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/174/117 [table1]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#table1</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/174/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/174/117 [1]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#1</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/174/117</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/174/117 [2]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#2</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/174/117&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/174/117 [clusters]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#clusters</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/174/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/174/117 [table1]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#table1</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/174/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/174/117 [1]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#1</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/174/117</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/174/117 [2]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#2</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/174/117&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/174/117 [clusters]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#clusters</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/174/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/174/117 [table1]</TD>
            <TD>Properties and metal abundances of clusters (Maughan+, 2008)</TD>
            <TD>We have assembled a sample of 115 galaxy clusters at 0.1&lt;z&lt;1.3 with archived Chandra ACIS-I observations. We present X-ray images of the clusters and make available region files containing contours of the smoothed X-ray emission. The structural properties of the clusters were investigated, and we found a significant absence of relaxed clusters (as determined by centroid shift measurements) at z&gt;0.5. The slope of the surface brightness profiles at large radii were steeper on average by 15% than the slope obtained by fitting a simple {beta}-model to the emission. This slope was also found to be correlated with cluster temperature, with some indication that the correlation is weaker for the clusters at z&gt;0.5. We measured the mean metal abundance of the cluster gas as a function of redshift and found significant evolution, with the abundances dropping by 50% between z=0.1 and z~1. This evolution was still present (although less significant) when the cluster cores were excluded from the abundance measurements, indicating that the evolution is not solely due to the disappearance of relaxed, cool core clusters (which are known to have enhanced core metal abundances) from the population at z&gt;~0.5.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117#table1</TD>
            <TD>2011-09-14T20:37:42Z</TD>
            <TD>#Abundances#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jun-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/174/117</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/174/117&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/174/117</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/791 [1]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#1</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/791</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/791 [2]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#2</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/791&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/791 [table1]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#table1</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/791 [table2]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#table2</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/791 [1]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#1</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/791</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/791 [2]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#2</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/791&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/791 [table1]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#table1</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/791 [table2]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#table2</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/791 [1]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#1</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/791</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/791 [2]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#2</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/791&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/791 [table1]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#table1</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/791 [table2]</TD>
            <TD>Spitzer photometry of normal &amp; interacting galaxies (Smith+, 2007)</TD>
            <TD>We present Spitzer mid-infrared imaging of a sample of 35 tidally distorted premerger interacting galaxy pairs selected from the Arp Atlas. We compare their global mid-infrared properties with those of normal galaxies from the SINGS Spitzer Legacy survey, and separate the disk emission from that of the tidal features. The [8.0um]-[24um], [3.6um]-[24um], and [5.8um]-[8.0um] colors of these optically selected interacting galaxies are redder on average than those of spirals, implying enhancements to the mass-normalized star formation rates (SFRs) of a factor of ~2.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791#table2</TD>
            <TD>2011-09-14T20:42:15Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Jan-2009</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/791</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/791&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/791</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/220 [1]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#1</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/220</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/220 [2]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#2</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/220&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/220 [Xray]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#Xray</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/220&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/220 [table1]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#table1</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/220&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/220 [faintmm]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#faintmm</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/220&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/220 [1]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#1</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/220</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/220 [2]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#2</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/220&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/220 [Xray]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#Xray</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/220&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/220 [table1]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#table1</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/220&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/220 [faintmm]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#faintmm</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/220&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/AJ/133/220 [1]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#1</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/AJ/133/220</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/AJ/133/220 [2]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#2</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/AJ/133/220&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/220 [Xray]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#Xray</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/220&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/220 [table1]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#table1</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/220&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/AJ/133/220 [faintmm]</TD>
            <TD>X-ray sources in galaxy pairs (Gruetzbauch+, 2007)</TD>
            <TD>We obtained XMM-Newton observations of RR 143 on 2003 Oct 19 and RR 242 with on 2003 Jul 17 EPIC in the medium filter.</TD>
            <TD>CDS</TD>
            <TD>#X-ray#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220#faintmm</TD>
            <TD>2011-09-14T20:42:31Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>11-Dec-2008</TD>
            <TD>ivo://CDS.VizieR/J/AJ/133/220</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/AJ/133/220&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/AJ/133/220</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/660/1151 [1]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#1</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/660/1151</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/660/1151 [2]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#2</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/660/1151&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/660/1151 [table1]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#table1</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/660/1151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/660/1151 [table2]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#table2</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/660/1151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/660/1151 [1]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#1</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/660/1151</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/660/1151 [2]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#2</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/660/1151&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/660/1151 [table1]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#table1</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/660/1151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/660/1151 [table2]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#table2</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/660/1151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/660/1151 [1]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#1</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/660/1151</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/660/1151 [2]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#2</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/660/1151&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/660/1151 [table1]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#table1</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/660/1151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/660/1151 [table2]</TD>
            <TD>Morphology of galaxies in 10 EDisCS clusters (Desai+, 2007)</TD>
            <TD>The 10 clusters included in this study are a subset of the ESO Distant Cluster Survey, an extensive program to obtain spectroscopy and multiwavelength photometry for 20 galaxy clusters at 0.4&lt;z&lt;1. Details of the goals and data sets associated with this survey are documented by White et al. (2005, Cat. &lt;J/A+A/444/365&gt;)</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151#table2</TD>
            <TD>2011-09-14T20:42:43Z</TD>
            <TD>#Clusters_of_galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>08-Mar-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/660/1151</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/660/1151&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/660/1151</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/177/465 [1]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#1</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/177/465</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/177/465 [2]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#2</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/177/465&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/177/465 [ngc6946]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#ngc6946</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/177/465&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/177/465 [ngc4485]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#ngc4485</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/177/465&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/177/465 [1]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#1</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/177/465</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/177/465 [2]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#2</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/177/465&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/177/465 [ngc6946]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#ngc6946</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/177/465&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/177/465 [ngc4485]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#ngc4485</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/177/465&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/177/465 [1]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#1</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/177/465</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/177/465 [2]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#2</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD />
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            <TD />
            <TD>ParamHTTP</TD>
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            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/177/465&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/177/465 [ngc6946]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#ngc6946</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
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            <TD>#Research#</TD>
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            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/177/465&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/177/465 [ngc4485]</TD>
            <TD>X-ray variability in NGC 6946, NGC 4485/90 (Fridriksson+, 2008)</TD>
            <TD>++++Lrecl of file 'table6.dat' (103) increased to 107 %B We analyze data from five Chandra observations of the spiral galaxy NGC 6946 and from three Chandra observations of the irregular/spiral interacting galaxy pair NGC 4485/4490, with an emphasis on investigating the long-term variability exhibited by the source populations. We detect 90 point sources coincident with NGC 6946 down to luminosities of a few times 10^36^ergs/s, and 38 sources coincident with NGC 4485/90 down to a luminosity of ~1x10^37^ergs/s. Twenty-five (15) sources in NGC 6946 (NGC 4485/90) exhibit long-term (i.e., weeks to years) variability in luminosity; 11 (4) are transient candidates. The single ultraluminous X-ray source (ULX) in NGC 6946 and all but one of the eight ULXs in NGC 4485/90 exhibit long-term flux variability. Two of the ULXs in NGC 4485/90 have not been identified before as ultraluminous sources. The widespread variability in both systems is indicative of the populations being dominated by X-ray binaries, and this is supported by the X-ray colors of the sources. The distribution of colors among the sources indicates a large fraction of high-mass X-ray binaries in both systems. The shapes of the X-ray luminosity functions of the galaxies do not change significantly between observations and can be described by power laws with cumulative slopes ~0.6-0.7 (NGC 6946) and ~0.4 (NGC 4485/90).</TD>
            <TD>CDS</TD>
            <TD>#X-ray#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465#ngc4485</TD>
            <TD>2011-09-14T20:46:58Z</TD>
            <TD>#Binaries:cataclysmic#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>01-Sep-2009</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/177/465</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/177/465&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/177/465</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/SerAJ/17 [1]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87#1</TD>
            <TD>2011-09-14T20:53:42Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
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            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/SerAJ/179.87</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/SerAJ/179.87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/SerAJ/17 [2]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87#2</TD>
            <TD>2011-09-14T20:53:42Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
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            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/SerAJ/179.87&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/SerAJ/179.87</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/other/SerAJ/17 [table5]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87#table5</TD>
            <TD>2011-09-14T20:53:42Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/SerAJ/179.87&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/SerAJ/179.87</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/SerAJ/17 [1]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87#1</TD>
            <TD>2011-09-14T20:53:42Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
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            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/SerAJ/179.87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/SerAJ/179.87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/SerAJ/17 [2]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87#2</TD>
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            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/SerAJ/179.87&amp;</TD>
            <TD />
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/SerAJ/179.87</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/other/SerAJ/17 [table5]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87#table5</TD>
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            <TD>#Galaxies#HII_regions#</TD>
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            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/SerAJ/179.87&amp;</TD>
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            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/SerAJ/179.87</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/other/SerAJ/17 [1]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87#1</TD>
            <TD>2011-09-14T20:53:42Z</TD>
            <TD>#Galaxies#HII_regions#</TD>
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            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/other/SerAJ/179.87</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/SerAJ/179.87</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/other/SerAJ/17 [2]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
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            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/other/SerAJ/179.87&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/SerAJ/179.87</TD>
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          <TR>
            <TD>Catalog</TD>
            <TD>J/other/SerAJ/17 [table5]</TD>
            <TD>H{alpha} in HII regions of Holmberg IX (Arbutina+, 2009)</TD>
            <TD>We present observations of the nearby tidal dwarf galaxy Holmberg IX in M81 galaxy group in narrow band [SII] and H{alpha} filters, carried out in March and November 2008 with the 2m RCC telescope at NAO Rozhen, Bulgaria. Our search for resident supernova remnants (identified as sources with enhanced [SII] emission relative to their H{alpha} emission) in this galaxy yielded no sources of this kind, besides M&amp;H 10-11 or HoIX X-1. Nevertheless, we found a number of objects with significant H{alpha} emission that probably represent uncatalogued HII regions.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87#table5</TD>
            <TD>2011-09-14T20:53:42Z</TD>
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            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/other/SerAJ/179.87</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/other/SerAJ/179.87&amp;</TD>
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            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/other/SerAJ/179.87</TD>
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          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/653/240 [1]</TD>
            <TD>Low-mass SDSS dwarf galaxy properties (Geha+, 2006)</TD>
            <TD>We investigate the gas content and baryonic Tully-Fisher relationship for extremely low luminosity dwarf galaxies in the absolute magnitude range -13.5&gt;M_r_-5logh_70_&gt;-16. The sample is selected from the Sloan Digital Sky Survey and consists of 101 galaxies for which we have obtained follow-up HI observations using the Arecibo Observatory and Green Bank Telescope. This represents the largest homogeneous sample of dwarf galaxies at low luminosities with well-measured HI and optical properties. The sample spans a range of environments, from dense groups to truly isolated galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240#1</TD>
            <TD>2011-09-14T20:54:12Z</TD>
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            <TD />
            <TD>31-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/653/240</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/653/240</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/653/240 [2]</TD>
            <TD>Low-mass SDSS dwarf galaxy properties (Geha+, 2006)</TD>
            <TD>We investigate the gas content and baryonic Tully-Fisher relationship for extremely low luminosity dwarf galaxies in the absolute magnitude range -13.5&gt;M_r_-5logh_70_&gt;-16. The sample is selected from the Sloan Digital Sky Survey and consists of 101 galaxies for which we have obtained follow-up HI observations using the Arecibo Observatory and Green Bank Telescope. This represents the largest homogeneous sample of dwarf galaxies at low luminosities with well-measured HI and optical properties. The sample spans a range of environments, from dense groups to truly isolated galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240#2</TD>
            <TD>2011-09-14T20:54:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
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            <TD>31-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/653/240&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/653/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/653/240 [table1]</TD>
            <TD>Low-mass SDSS dwarf galaxy properties (Geha+, 2006)</TD>
            <TD>We investigate the gas content and baryonic Tully-Fisher relationship for extremely low luminosity dwarf galaxies in the absolute magnitude range -13.5&gt;M_r_-5logh_70_&gt;-16. The sample is selected from the Sloan Digital Sky Survey and consists of 101 galaxies for which we have obtained follow-up HI observations using the Arecibo Observatory and Green Bank Telescope. This represents the largest homogeneous sample of dwarf galaxies at low luminosities with well-measured HI and optical properties. The sample spans a range of environments, from dense groups to truly isolated galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240#table1</TD>
            <TD>2011-09-14T20:54:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/653/240&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/653/240</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/653/240 [1]</TD>
            <TD>Low-mass SDSS dwarf galaxy properties (Geha+, 2006)</TD>
            <TD>We investigate the gas content and baryonic Tully-Fisher relationship for extremely low luminosity dwarf galaxies in the absolute magnitude range -13.5&gt;M_r_-5logh_70_&gt;-16. The sample is selected from the Sloan Digital Sky Survey and consists of 101 galaxies for which we have obtained follow-up HI observations using the Arecibo Observatory and Green Bank Telescope. This represents the largest homogeneous sample of dwarf galaxies at low luminosities with well-measured HI and optical properties. The sample spans a range of environments, from dense groups to truly isolated galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240#1</TD>
            <TD>2011-09-14T20:54:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/653/240</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/653/240</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/653/240 [2]</TD>
            <TD>Low-mass SDSS dwarf galaxy properties (Geha+, 2006)</TD>
            <TD>We investigate the gas content and baryonic Tully-Fisher relationship for extremely low luminosity dwarf galaxies in the absolute magnitude range -13.5&gt;M_r_-5logh_70_&gt;-16. The sample is selected from the Sloan Digital Sky Survey and consists of 101 galaxies for which we have obtained follow-up HI observations using the Arecibo Observatory and Green Bank Telescope. This represents the largest homogeneous sample of dwarf galaxies at low luminosities with well-measured HI and optical properties. The sample spans a range of environments, from dense groups to truly isolated galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240#2</TD>
            <TD>2011-09-14T20:54:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/653/240&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/653/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/653/240 [table1]</TD>
            <TD>Low-mass SDSS dwarf galaxy properties (Geha+, 2006)</TD>
            <TD>We investigate the gas content and baryonic Tully-Fisher relationship for extremely low luminosity dwarf galaxies in the absolute magnitude range -13.5&gt;M_r_-5logh_70_&gt;-16. The sample is selected from the Sloan Digital Sky Survey and consists of 101 galaxies for which we have obtained follow-up HI observations using the Arecibo Observatory and Green Bank Telescope. This represents the largest homogeneous sample of dwarf galaxies at low luminosities with well-measured HI and optical properties. The sample spans a range of environments, from dense groups to truly isolated galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240#table1</TD>
            <TD>2011-09-14T20:54:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/653/240&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/653/240</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/653/240 [1]</TD>
            <TD>Low-mass SDSS dwarf galaxy properties (Geha+, 2006)</TD>
            <TD>We investigate the gas content and baryonic Tully-Fisher relationship for extremely low luminosity dwarf galaxies in the absolute magnitude range -13.5&gt;M_r_-5logh_70_&gt;-16. The sample is selected from the Sloan Digital Sky Survey and consists of 101 galaxies for which we have obtained follow-up HI observations using the Arecibo Observatory and Green Bank Telescope. This represents the largest homogeneous sample of dwarf galaxies at low luminosities with well-measured HI and optical properties. The sample spans a range of environments, from dense groups to truly isolated galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240#1</TD>
            <TD>2011-09-14T20:54:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/653/240</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/653/240</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/653/240 [2]</TD>
            <TD>Low-mass SDSS dwarf galaxy properties (Geha+, 2006)</TD>
            <TD>We investigate the gas content and baryonic Tully-Fisher relationship for extremely low luminosity dwarf galaxies in the absolute magnitude range -13.5&gt;M_r_-5logh_70_&gt;-16. The sample is selected from the Sloan Digital Sky Survey and consists of 101 galaxies for which we have obtained follow-up HI observations using the Arecibo Observatory and Green Bank Telescope. This represents the largest homogeneous sample of dwarf galaxies at low luminosities with well-measured HI and optical properties. The sample spans a range of environments, from dense groups to truly isolated galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240#2</TD>
            <TD>2011-09-14T20:54:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/653/240&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/653/240</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/653/240 [table1]</TD>
            <TD>Low-mass SDSS dwarf galaxy properties (Geha+, 2006)</TD>
            <TD>We investigate the gas content and baryonic Tully-Fisher relationship for extremely low luminosity dwarf galaxies in the absolute magnitude range -13.5&gt;M_r_-5logh_70_&gt;-16. The sample is selected from the Sloan Digital Sky Survey and consists of 101 galaxies for which we have obtained follow-up HI observations using the Arecibo Observatory and Green Bank Telescope. This represents the largest homogeneous sample of dwarf galaxies at low luminosities with well-measured HI and optical properties. The sample spans a range of environments, from dense groups to truly isolated galaxies.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240#table1</TD>
            <TD>2011-09-14T20:54:12Z</TD>
            <TD>#Photometry#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>31-Jul-2008</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/653/240</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/653/240&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/653/240</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/182/559 [1]</TD>
            <TD>Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)</TD>
            <TD>In this paper, we apply the phase-shift method to a much larger sample of galaxies than in Paper I: the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;). This survey includes all RC3 (de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;) galaxies having a type in the range S0/a to Sm, total blue magnitude B_T_&lt;=12.0, blue light isophotal diameter D_25_&lt;=6.5', and declination in the range -80&lt;{delta}&lt;+50{dd}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559#1</TD>
            <TD>2011-09-14T20:57:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/182/559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/182/559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/182/559 [2]</TD>
            <TD>Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)</TD>
            <TD>In this paper, we apply the phase-shift method to a much larger sample of galaxies than in Paper I: the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;). This survey includes all RC3 (de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;) galaxies having a type in the range S0/a to Sm, total blue magnitude B_T_&lt;=12.0, blue light isophotal diameter D_25_&lt;=6.5', and declination in the range -80&lt;{delta}&lt;+50{dd}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559#2</TD>
            <TD>2011-09-14T20:57:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/182/559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/182/559</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/182/559 [table1]</TD>
            <TD>Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)</TD>
            <TD>In this paper, we apply the phase-shift method to a much larger sample of galaxies than in Paper I: the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;). This survey includes all RC3 (de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;) galaxies having a type in the range S0/a to Sm, total blue magnitude B_T_&lt;=12.0, blue light isophotal diameter D_25_&lt;=6.5', and declination in the range -80&lt;{delta}&lt;+50{dd}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559#table1</TD>
            <TD>2011-09-14T20:57:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/182/559&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/182/559</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/182/559 [1]</TD>
            <TD>Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)</TD>
            <TD>In this paper, we apply the phase-shift method to a much larger sample of galaxies than in Paper I: the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;). This survey includes all RC3 (de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;) galaxies having a type in the range S0/a to Sm, total blue magnitude B_T_&lt;=12.0, blue light isophotal diameter D_25_&lt;=6.5', and declination in the range -80&lt;{delta}&lt;+50{dd}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559#1</TD>
            <TD>2011-09-14T20:57:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/182/559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/182/559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/182/559 [2]</TD>
            <TD>Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)</TD>
            <TD>In this paper, we apply the phase-shift method to a much larger sample of galaxies than in Paper I: the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;). This survey includes all RC3 (de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;) galaxies having a type in the range S0/a to Sm, total blue magnitude B_T_&lt;=12.0, blue light isophotal diameter D_25_&lt;=6.5', and declination in the range -80&lt;{delta}&lt;+50{dd}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559#2</TD>
            <TD>2011-09-14T20:57:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/182/559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/182/559</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/182/559 [table1]</TD>
            <TD>Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)</TD>
            <TD>In this paper, we apply the phase-shift method to a much larger sample of galaxies than in Paper I: the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;). This survey includes all RC3 (de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;) galaxies having a type in the range S0/a to Sm, total blue magnitude B_T_&lt;=12.0, blue light isophotal diameter D_25_&lt;=6.5', and declination in the range -80&lt;{delta}&lt;+50{dd}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559#table1</TD>
            <TD>2011-09-14T20:57:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/182/559&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/182/559</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/182/559 [1]</TD>
            <TD>Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)</TD>
            <TD>In this paper, we apply the phase-shift method to a much larger sample of galaxies than in Paper I: the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;). This survey includes all RC3 (de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;) galaxies having a type in the range S0/a to Sm, total blue magnitude B_T_&lt;=12.0, blue light isophotal diameter D_25_&lt;=6.5', and declination in the range -80&lt;{delta}&lt;+50{dd}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559#1</TD>
            <TD>2011-09-14T20:57:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/182/559</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/182/559</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/182/559 [2]</TD>
            <TD>Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)</TD>
            <TD>In this paper, we apply the phase-shift method to a much larger sample of galaxies than in Paper I: the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;). This survey includes all RC3 (de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;) galaxies having a type in the range S0/a to Sm, total blue magnitude B_T_&lt;=12.0, blue light isophotal diameter D_25_&lt;=6.5', and declination in the range -80&lt;{delta}&lt;+50{dd}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559#2</TD>
            <TD>2011-09-14T20:57:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/182/559&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/182/559</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/182/559 [table1]</TD>
            <TD>Corotation radii for 153 galaxies of OSUBSGS (Buta+, 2009)</TD>
            <TD>In this paper, we apply the phase-shift method to a much larger sample of galaxies than in Paper I: the Ohio State University Bright Spiral Galaxy Survey (OSUBSGS; Eskridge et al. 2002, Cat. &lt;J/ApJS/143/73&gt;). This survey includes all RC3 (de Vaucouleurs et al., 1991, Cat. &lt;VII/155&gt;) galaxies having a type in the range S0/a to Sm, total blue magnitude B_T_&lt;=12.0, blue light isophotal diameter D_25_&lt;=6.5', and declination in the range -80&lt;{delta}&lt;+50{dd}.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559#table1</TD>
            <TD>2011-09-14T20:57:07Z</TD>
            <TD>#Galaxies#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>04-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/182/559</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/182/559&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/182/559</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/183/197 [1]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#1</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/183/197</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/183/197 [2]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#2</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/183/197&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/183/197 [table1]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#table1</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/183/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/183/197 [table2]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#table2</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/183/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/183/197 [1]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#1</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/183/197</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/183/197 [2]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#2</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/183/197&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/183/197 [table1]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#table1</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/183/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/183/197 [table2]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#table2</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/183/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJS/183/197 [1]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#1</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJS/183/197</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJS/183/197 [2]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#2</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJS/183/197&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/183/197 [table1]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#table1</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/183/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJS/183/197 [table2]</TD>
            <TD>Galaxy clusters identified from the SDSS-DR6 (Wen+, 2009)</TD>
            <TD>Clusters of galaxies in most of the previous catalogs have redshifts z&lt;=0.3. Using the photometric redshifts of galaxies from the Sloan Digital Sky Survey Data Release 6 (SDSS DR6), we identify 39716 clusters in the redshift range 0.05&lt;z&lt;0.6 with more than eight luminous (M_r_&lt;=-21) member galaxies. Cluster redshifts are estimated accurately with an uncertainty of less than 0.022. The contamination rate of member galaxies is found to be roughly 20%, and the completeness of member galaxy detection reaches ~90%. Monte Carlo simulations show that the cluster detection rate is more than 90% for massive (M_200_&gt;2x10^14^M_{sun}_) clusters of z&lt;=0.42. The false detection rate is ~5%. We obtain the richness, the summed luminosity, and the gross galaxy number within the determined radius for identified clusters. They are tightly related to the X-ray luminosity and temperature of clusters. Cluster mass is related to the richness and summed luminosity with M_200_{prop.to}R^1.90+/-0.04^ and M_200_{prop.to}L^1.64+/-0.03^_r_, respectively. In addition, 790 new candidates of X-ray clusters are found by cross-identification of our clusters with the source list of the ROSAT X-ray survey.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197#table2</TD>
            <TD>2011-09-14T20:57:08Z</TD>
            <TD>#Clusters_of_galaxies#Stars#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>12-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJS/183/197</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJS/183/197&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJS/183/197</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/670/346 [1]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)</TD>
            <TD>We present reliable measurements of the metallicity distribution function (MDF) at different points along the tidal stream of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy, based on high-resolution, echelle spectroscopy of candidate M giant members of the Sgr system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346#1</TD>
            <TD>2011-09-14T20:57:43Z</TD>
            <TD>#Stars#Equivalent_widths#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/670/346</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/670/346</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/670/346 [2]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)</TD>
            <TD>We present reliable measurements of the metallicity distribution function (MDF) at different points along the tidal stream of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy, based on high-resolution, echelle spectroscopy of candidate M giant members of the Sgr system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346#2</TD>
            <TD>2011-09-14T20:57:43Z</TD>
            <TD>#Stars#Equivalent_widths#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/670/346&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/670/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/670/346 [Mstars]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)</TD>
            <TD>We present reliable measurements of the metallicity distribution function (MDF) at different points along the tidal stream of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy, based on high-resolution, echelle spectroscopy of candidate M giant members of the Sgr system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346#Mstars</TD>
            <TD>2011-09-14T20:57:43Z</TD>
            <TD>#Stars#Equivalent_widths#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/670/346&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/670/346</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/670/346 [1]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)</TD>
            <TD>We present reliable measurements of the metallicity distribution function (MDF) at different points along the tidal stream of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy, based on high-resolution, echelle spectroscopy of candidate M giant members of the Sgr system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346#1</TD>
            <TD>2011-09-14T20:57:43Z</TD>
            <TD>#Stars#Equivalent_widths#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/670/346</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/670/346</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/670/346 [2]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)</TD>
            <TD>We present reliable measurements of the metallicity distribution function (MDF) at different points along the tidal stream of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy, based on high-resolution, echelle spectroscopy of candidate M giant members of the Sgr system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346#2</TD>
            <TD>2011-09-14T20:57:43Z</TD>
            <TD>#Stars#Equivalent_widths#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/670/346&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/670/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/670/346 [Mstars]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)</TD>
            <TD>We present reliable measurements of the metallicity distribution function (MDF) at different points along the tidal stream of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy, based on high-resolution, echelle spectroscopy of candidate M giant members of the Sgr system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346#Mstars</TD>
            <TD>2011-09-14T20:57:43Z</TD>
            <TD>#Stars#Equivalent_widths#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/670/346&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/670/346</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/ApJ/670/346 [1]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)</TD>
            <TD>We present reliable measurements of the metallicity distribution function (MDF) at different points along the tidal stream of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy, based on high-resolution, echelle spectroscopy of candidate M giant members of the Sgr system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346#1</TD>
            <TD>2011-09-14T20:57:43Z</TD>
            <TD>#Stars#Equivalent_widths#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/ApJ/670/346</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/670/346</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/ApJ/670/346 [2]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)</TD>
            <TD>We present reliable measurements of the metallicity distribution function (MDF) at different points along the tidal stream of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy, based on high-resolution, echelle spectroscopy of candidate M giant members of the Sgr system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346#2</TD>
            <TD>2011-09-14T20:57:43Z</TD>
            <TD>#Stars#Equivalent_widths#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/ApJ/670/346&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/670/346</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/ApJ/670/346 [Mstars]</TD>
            <TD>M giant stars in the Sagittarius dwarf galaxy. V. (Chou+, 2007)</TD>
            <TD>We present reliable measurements of the metallicity distribution function (MDF) at different points along the tidal stream of the Sagittarius (Sgr) dwarf spheroidal (dSph) galaxy, based on high-resolution, echelle spectroscopy of candidate M giant members of the Sgr system.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346#Mstars</TD>
            <TD>2011-09-14T20:57:43Z</TD>
            <TD>#Stars#Equivalent_widths#Spectroscopy#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>27-Jan-2010</TD>
            <TD>ivo://CDS.VizieR/J/ApJ/670/346</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/ApJ/670/346&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/ApJ/670/346</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/398/109 [1]</TD>
            <TD>Imperial IRAS-FSC redshift catalogue (IIFSCz) (Wang+, 2009)</TD>
            <TD>We present a new catalogue, the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), of 60303 galaxies selected at 60um from the IRAS Faint Source Catalogue (FSC). The IIFSCz consists of accurate position, optical, near-infrared and/or radio identifications, spectroscopic redshift (if available) or photometric redshift (if possible), predicted far-infrared (FIR) and submillimetre (submm) fluxes ranging from 12 to 1380um based upon the best-fitting infrared template. About 55% of the galaxies in the IIFSCz have spectroscopic redshifts, and a further 20% have photometric redshifts obtained through either the training set or the template-fitting method. For S(60)&gt;0.36Jy, the 90% completeness limit of the FSC, 90% of the sources have either spectroscopic or photometric redshifts. Scientific applications of the IIFSCz include validation of current and forthcoming infrared and submm/mm surveys such as AKARI, Planck and Herschel, follow-up studies of rare source populations, large-scale structure and galaxy bias, local multiwavelength luminosity functions and source counts. The catalogue is publicly available at http://astro.imperial.ac.uk/~mrr/fss/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109#1</TD>
            <TD>2011-09-14T20:57:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/398/109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/398/109 [2]</TD>
            <TD>Imperial IRAS-FSC redshift catalogue (IIFSCz) (Wang+, 2009)</TD>
            <TD>We present a new catalogue, the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), of 60303 galaxies selected at 60um from the IRAS Faint Source Catalogue (FSC). The IIFSCz consists of accurate position, optical, near-infrared and/or radio identifications, spectroscopic redshift (if available) or photometric redshift (if possible), predicted far-infrared (FIR) and submillimetre (submm) fluxes ranging from 12 to 1380um based upon the best-fitting infrared template. About 55% of the galaxies in the IIFSCz have spectroscopic redshifts, and a further 20% have photometric redshifts obtained through either the training set or the template-fitting method. For S(60)&gt;0.36Jy, the 90% completeness limit of the FSC, 90% of the sources have either spectroscopic or photometric redshifts. Scientific applications of the IIFSCz include validation of current and forthcoming infrared and submm/mm surveys such as AKARI, Planck and Herschel, follow-up studies of rare source populations, large-scale structure and galaxy bias, local multiwavelength luminosity functions and source counts. The catalogue is publicly available at http://astro.imperial.ac.uk/~mrr/fss/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109#2</TD>
            <TD>2011-09-14T20:57:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/398/109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/109</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/398/109 [iifsczv4]</TD>
            <TD>Imperial IRAS-FSC redshift catalogue (IIFSCz) (Wang+, 2009)</TD>
            <TD>We present a new catalogue, the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), of 60303 galaxies selected at 60um from the IRAS Faint Source Catalogue (FSC). The IIFSCz consists of accurate position, optical, near-infrared and/or radio identifications, spectroscopic redshift (if available) or photometric redshift (if possible), predicted far-infrared (FIR) and submillimetre (submm) fluxes ranging from 12 to 1380um based upon the best-fitting infrared template. About 55% of the galaxies in the IIFSCz have spectroscopic redshifts, and a further 20% have photometric redshifts obtained through either the training set or the template-fitting method. For S(60)&gt;0.36Jy, the 90% completeness limit of the FSC, 90% of the sources have either spectroscopic or photometric redshifts. Scientific applications of the IIFSCz include validation of current and forthcoming infrared and submm/mm surveys such as AKARI, Planck and Herschel, follow-up studies of rare source populations, large-scale structure and galaxy bias, local multiwavelength luminosity functions and source counts. The catalogue is publicly available at http://astro.imperial.ac.uk/~mrr/fss/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109#iifsczv4</TD>
            <TD>2011-09-14T20:57:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/398/109&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/398/109 [1]</TD>
            <TD>Imperial IRAS-FSC redshift catalogue (IIFSCz) (Wang+, 2009)</TD>
            <TD>We present a new catalogue, the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), of 60303 galaxies selected at 60um from the IRAS Faint Source Catalogue (FSC). The IIFSCz consists of accurate position, optical, near-infrared and/or radio identifications, spectroscopic redshift (if available) or photometric redshift (if possible), predicted far-infrared (FIR) and submillimetre (submm) fluxes ranging from 12 to 1380um based upon the best-fitting infrared template. About 55% of the galaxies in the IIFSCz have spectroscopic redshifts, and a further 20% have photometric redshifts obtained through either the training set or the template-fitting method. For S(60)&gt;0.36Jy, the 90% completeness limit of the FSC, 90% of the sources have either spectroscopic or photometric redshifts. Scientific applications of the IIFSCz include validation of current and forthcoming infrared and submm/mm surveys such as AKARI, Planck and Herschel, follow-up studies of rare source populations, large-scale structure and galaxy bias, local multiwavelength luminosity functions and source counts. The catalogue is publicly available at http://astro.imperial.ac.uk/~mrr/fss/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109#1</TD>
            <TD>2011-09-14T20:57:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/398/109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/398/109 [2]</TD>
            <TD>Imperial IRAS-FSC redshift catalogue (IIFSCz) (Wang+, 2009)</TD>
            <TD>We present a new catalogue, the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), of 60303 galaxies selected at 60um from the IRAS Faint Source Catalogue (FSC). The IIFSCz consists of accurate position, optical, near-infrared and/or radio identifications, spectroscopic redshift (if available) or photometric redshift (if possible), predicted far-infrared (FIR) and submillimetre (submm) fluxes ranging from 12 to 1380um based upon the best-fitting infrared template. About 55% of the galaxies in the IIFSCz have spectroscopic redshifts, and a further 20% have photometric redshifts obtained through either the training set or the template-fitting method. For S(60)&gt;0.36Jy, the 90% completeness limit of the FSC, 90% of the sources have either spectroscopic or photometric redshifts. Scientific applications of the IIFSCz include validation of current and forthcoming infrared and submm/mm surveys such as AKARI, Planck and Herschel, follow-up studies of rare source populations, large-scale structure and galaxy bias, local multiwavelength luminosity functions and source counts. The catalogue is publicly available at http://astro.imperial.ac.uk/~mrr/fss/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109#2</TD>
            <TD>2011-09-14T20:57:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/398/109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/109</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/398/109 [iifsczv4]</TD>
            <TD>Imperial IRAS-FSC redshift catalogue (IIFSCz) (Wang+, 2009)</TD>
            <TD>We present a new catalogue, the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), of 60303 galaxies selected at 60um from the IRAS Faint Source Catalogue (FSC). The IIFSCz consists of accurate position, optical, near-infrared and/or radio identifications, spectroscopic redshift (if available) or photometric redshift (if possible), predicted far-infrared (FIR) and submillimetre (submm) fluxes ranging from 12 to 1380um based upon the best-fitting infrared template. About 55% of the galaxies in the IIFSCz have spectroscopic redshifts, and a further 20% have photometric redshifts obtained through either the training set or the template-fitting method. For S(60)&gt;0.36Jy, the 90% completeness limit of the FSC, 90% of the sources have either spectroscopic or photometric redshifts. Scientific applications of the IIFSCz include validation of current and forthcoming infrared and submm/mm surveys such as AKARI, Planck and Herschel, follow-up studies of rare source populations, large-scale structure and galaxy bias, local multiwavelength luminosity functions and source counts. The catalogue is publicly available at http://astro.imperial.ac.uk/~mrr/fss/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109#iifsczv4</TD>
            <TD>2011-09-14T20:57:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/398/109&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/MNRAS/398/109 [1]</TD>
            <TD>Imperial IRAS-FSC redshift catalogue (IIFSCz) (Wang+, 2009)</TD>
            <TD>We present a new catalogue, the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), of 60303 galaxies selected at 60um from the IRAS Faint Source Catalogue (FSC). The IIFSCz consists of accurate position, optical, near-infrared and/or radio identifications, spectroscopic redshift (if available) or photometric redshift (if possible), predicted far-infrared (FIR) and submillimetre (submm) fluxes ranging from 12 to 1380um based upon the best-fitting infrared template. About 55% of the galaxies in the IIFSCz have spectroscopic redshifts, and a further 20% have photometric redshifts obtained through either the training set or the template-fitting method. For S(60)&gt;0.36Jy, the 90% completeness limit of the FSC, 90% of the sources have either spectroscopic or photometric redshifts. Scientific applications of the IIFSCz include validation of current and forthcoming infrared and submm/mm surveys such as AKARI, Planck and Herschel, follow-up studies of rare source populations, large-scale structure and galaxy bias, local multiwavelength luminosity functions and source counts. The catalogue is publicly available at http://astro.imperial.ac.uk/~mrr/fss/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109#1</TD>
            <TD>2011-09-14T20:57:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/MNRAS/398/109</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/109</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/MNRAS/398/109 [2]</TD>
            <TD>Imperial IRAS-FSC redshift catalogue (IIFSCz) (Wang+, 2009)</TD>
            <TD>We present a new catalogue, the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), of 60303 galaxies selected at 60um from the IRAS Faint Source Catalogue (FSC). The IIFSCz consists of accurate position, optical, near-infrared and/or radio identifications, spectroscopic redshift (if available) or photometric redshift (if possible), predicted far-infrared (FIR) and submillimetre (submm) fluxes ranging from 12 to 1380um based upon the best-fitting infrared template. About 55% of the galaxies in the IIFSCz have spectroscopic redshifts, and a further 20% have photometric redshifts obtained through either the training set or the template-fitting method. For S(60)&gt;0.36Jy, the 90% completeness limit of the FSC, 90% of the sources have either spectroscopic or photometric redshifts. Scientific applications of the IIFSCz include validation of current and forthcoming infrared and submm/mm surveys such as AKARI, Planck and Herschel, follow-up studies of rare source populations, large-scale structure and galaxy bias, local multiwavelength luminosity functions and source counts. The catalogue is publicly available at http://astro.imperial.ac.uk/~mrr/fss/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109#2</TD>
            <TD>2011-09-14T20:57:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/MNRAS/398/109&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/109</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/MNRAS/398/109 [iifsczv4]</TD>
            <TD>Imperial IRAS-FSC redshift catalogue (IIFSCz) (Wang+, 2009)</TD>
            <TD>We present a new catalogue, the Imperial IRAS-FSC Redshift Catalogue (IIFSCz), of 60303 galaxies selected at 60um from the IRAS Faint Source Catalogue (FSC). The IIFSCz consists of accurate position, optical, near-infrared and/or radio identifications, spectroscopic redshift (if available) or photometric redshift (if possible), predicted far-infrared (FIR) and submillimetre (submm) fluxes ranging from 12 to 1380um based upon the best-fitting infrared template. About 55% of the galaxies in the IIFSCz have spectroscopic redshifts, and a further 20% have photometric redshifts obtained through either the training set or the template-fitting method. For S(60)&gt;0.36Jy, the 90% completeness limit of the FSC, 90% of the sources have either spectroscopic or photometric redshifts. Scientific applications of the IIFSCz include validation of current and forthcoming infrared and submm/mm surveys such as AKARI, Planck and Herschel, follow-up studies of rare source populations, large-scale structure and galaxy bias, local multiwavelength luminosity functions and source counts. The catalogue is publicly available at http://astro.imperial.ac.uk/~mrr/fss/.</TD>
            <TD>CDS</TD>
            <TD>#Optical#Infrared#Radio#</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109#iifsczv4</TD>
            <TD>2011-09-14T20:57:56Z</TD>
            <TD>#Galaxies#Redshifts#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>26-Apr-2010</TD>
            <TD>ivo://CDS.VizieR/J/MNRAS/398/109</TD>
            <TD>ConeSearch</TD>
            <TD>ivo://ivoa.net/std/ConeSearch</TD>
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD>std</TD>
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-A?-source=J/MNRAS/398/109&amp;</TD>
            <TD>180</TD>
            <TD>9999</TD>
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/MNRAS/398/109</TD>
          </TR>
          <TR>
            <TD>Web Page</TD>
            <TD>J/PAZh/35/574 [1]</TD>
            <TD>He, C, N and O abundances in planetary nebulae (Milanova+, 2009)</TD>
            <TD>The He, C, N, and O abundances in more than 120 planetary nebulae (PNe) of our Galaxy and the Magellanic Clouds have been redetermined by analyzing new PNe observations. The characteristics of PNe obtained by modeling their spectra have been used to compile a new catalog of parameters for Galactic and extragalactic PNe, which is accessible at http://www.astro.spbu.ru/staff/afk/GalChemEvol.html. The errors in the parameters of PNe and their elemental abundances related to inaccuracies in the observational data have been analyzed. The He abundance is determined with an accuracy of 0.06dex, while the errors in the C, N, and O abundances are 0.1-0.2dex. Taking into account the inaccuracies in the corrections for the ionization stages of the elements whose lines are absent in the PNe spectra increases the errors in the He abundance to 0.1dex and in the C, N, and O abundances to 0.2-0.3dex. The elemental abundances in PNe of various Galactic subsystems and the Magellanic Clouds have been analyzed. This analysis suggests that the Galactic bulge objects are similar to type II PNe in Peimbert's classification, whose progenitor stars belong to the thin-disk population with ages of at least 4-6Gyr. A similarity between the elemental abundances in PNe of the Magellanic Clouds and the Galactic halo has been established.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/574#1</TD>
            <TD>2011-09-14T20:58:15Z</TD>
            <TD>#Abundances#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/574</TD>
            <TD />
            <TD />
            <TD />
            <TD>WebBrowser</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/cgi-bin/VizieR-2?-source=J/PAZh/35/574</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/574</TD>
          </TR>
          <TR>
            <TD>HTTP Request</TD>
            <TD>J/PAZh/35/574 [2]</TD>
            <TD>He, C, N and O abundances in planetary nebulae (Milanova+, 2009)</TD>
            <TD>The He, C, N, and O abundances in more than 120 planetary nebulae (PNe) of our Galaxy and the Magellanic Clouds have been redetermined by analyzing new PNe observations. The characteristics of PNe obtained by modeling their spectra have been used to compile a new catalog of parameters for Galactic and extragalactic PNe, which is accessible at http://www.astro.spbu.ru/staff/afk/GalChemEvol.html. The errors in the parameters of PNe and their elemental abundances related to inaccuracies in the observational data have been analyzed. The He abundance is determined with an accuracy of 0.06dex, while the errors in the C, N, and O abundances are 0.1-0.2dex. Taking into account the inaccuracies in the corrections for the ionization stages of the elements whose lines are absent in the PNe spectra increases the errors in the He abundance to 0.1dex and in the C, N, and O abundances to 0.2-0.3dex. The elemental abundances in PNe of various Galactic subsystems and the Magellanic Clouds have been analyzed. This analysis suggests that the Galactic bulge objects are similar to type II PNe in Peimbert's classification, whose progenitor stars belong to the thin-disk population with ages of at least 4-6Gyr. A similarity between the elemental abundances in PNe of the Magellanic Clouds and the Galactic halo has been established.</TD>
            <TD>CDS</TD>
            <TD>#Optical#</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/574#2</TD>
            <TD>2011-09-14T20:58:15Z</TD>
            <TD>#Abundances#Planetary_Nebulae#</TD>
            <TD>#Catalog#</TD>
            <TD>#Research#</TD>
            <TD />
            <TD>29-Dec-2009</TD>
            <TD>ivo://CDS.VizieR/J/PAZh/35/574</TD>
            <TD />
            <TD />
            <TD />
            <TD>ParamHTTP</TD>
            <TD />
            <TD />
            <TD>http://vizier.u-strasbg.fr/viz-bin/votable/-dtd/-A?-source=J/PAZh/35/574&amp;</TD>
            <TD />
            <TD />
            <TD>ivo://CDS</TD>
            <TD>http://cdsarc.u-strasbg.fr/cgi-bin/Cat?J/PAZh/35/574</TD>
          </TR>
          <TR>
            <TD>Catalog</TD>
            <TD>J/PAZh/35/574 [all_PNe]</TD>
            <TD>He, C, N and O abundances in planetary nebulae (Milanova+, 2009)</TD>
            <TD>The He, C, N, and O abundances in more than 120 planetary nebulae (PNe) of our Galaxy and the Magellanic Clouds have been redetermined by analyzin
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